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Hubble Space Telescope Cycle 8 Call for Proposals

 

 

Hubble Space Telescope

Cycle 8

Call for Proposals

and

Phase I Proposal Instructions

 

Deadline: September 11, 1998, 8:00 pm EDT

Issued June 1998

 

 

 

This is the Cycle 8 Call for Proposals for astronomical observations with the Hubble Space Telescope by members of the international scientific community. The Call for Proposals was prepared by the Science Program Selection Office at the Space Telescope Science Institute (STScI).

The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc., under contract NAS5-26555 with the National Aeronautics and Space Administration.

 

Table of Contents

PART I. POLICIES AND PROCEDURES

1. Introduction

This document invites proposals for participation in the eighth round ("Cycle 8") of the General Observer (GO), Snapshot, and funded Archival Research (AR) programs of the Hubble Space Telescope (HST). The telescope and its instruments were built under the auspices of the National Aeronautics and Space Administration (NASA) and the European Space Agency (ESA), and management of HST's scientific program has been assigned to the Space Telescope Science Institute (STScI).

HST is a 2.4-m telescope that was carried into orbit on April 24, 1990, aboard the orbiter Discovery. The first HST servicing mission, carried out by the Endeavour astronauts in December 1993, improved its optical performance via the Corrective Optics Space Telescope Axial Replacement (COSTAR) and Wide Field Planetary Camera 2 (WFPC2). The second HST servicing mission (SM2), carried out by the Discovery astronauts in February 1997, replaced the Goddard High Resolution Spectrograph (GHRS) and the Faint Object Spectrograph (FOS) with two new science instruments: the Space Telescope Imaging Spectrograph (STIS), and the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). NICMOS is working well, but the cryogen is expected to be exhausted well before Cycle 8 starts. A new Solid-State Recorder (SSR) and a refurbished analog tape recorder were installed, providing much improved data transfer capabilities; and a refurbished Fine Guidance Sensor, FGS1R, with improved optics and resulting greater sensitivity replaced FGS-1. The instruments continuing operations after the second servicing mission are the WFPC2, the Faint Object Camera (FOC), and the astrometric Fine Guidance Sensor (FGS-3). The principal capabilities of the present HST observatory include high-resolution ultraviolet, optical and near-infrared imaging and a broad range of spectroscopic capabilities over these wavelength domains. The third HST servicing mission (SM3) is currently planned for Spring 2000. The Advanced Camera for Surveys (ACS) will then replace the FOC, and the NICMOS may resume operations if a new cryo-cooling system is successfully installed.

Part I of this Call for Proposals (CP) summarizes the policies and procedures for proposing for Cycle 8 HST observations and for requesting funding to support research on archival HST data. Part II provides an overview of HST's current technical capabilities. Further detailed information about the telescope and each Scientific Instrument (SI) is provided on-line or in documents that are available from STScI, as described in section 2. Part III of this document is the Phase I Proposal Instructions, including detailed instructions for obtaining the proposal templates, preparing and submitting them electronically.

Although the proposal forms and submission procedures have been modified only slightly for Cycle 8, it is still important that all proposers, including those who proposed in previous Cycles, read this document carefully. Proposers should particularly note the following features of Cycle 8:

Proposal submission for Cycle 8 is entirely electronic, except for Archival Research proposals where a partial paper submission is requested (see Part III, section 16.1 and 16.2).

The Cycle 8 deadline for GO/AR proposals is: September 11, 1998, 8:00 pm EDT

The Cycle 8 deadline for E/PO proposals is: January 18, 1999, 8:00 pm EDT

Late proposals will not be considered.

 

2. Getting Started

It is important that all proposers read the entire Call for Proposals in order to understand the policies and procedures for preparing and submitting observing proposals, and to gain an overview of the HST and its capabilities.

Observing proposals must contain a summary of the proposed observing program, including the targets that are to be observed and their celestial coordinates, and the desired instrument modes and filters or dispersers. In addition, a calculation of the number of spacecraft orbits needed to accomplish the observing program must be carried out and summarized in the proposal. Thus it is important that proposers consult technical documentation about the capabilities and sensitivities of the instrument(s) that will be used to obtain the observations. Where necessary, proposers should discuss their requirements with appropriate STScI experts (contacts provided via the STScI Help Desk at help@stsci.edu) before submitting their proposals. The following subsections describe the various sources of information that are available to proposers.

 

2.1 Technical Documentation

The current set of technical documents is listed below:

The following manuals are of interest primarily for archival proposers:

Users will need to consult the Instrument Handbooks for detailed technical information on how to observe with the HST instruments. Users should be aware that the STIS and FGS handbooks have been rewritten for Cycle 8 and older versions should not be used. However, because the operational capabilities and performance of WFPC2 have not changed much, the handbook for WFPC2 is the same as was used in Cycle 7. There have been a few changes though, and therefore WFPC2 proposers are advised to read the Update to the WFPC2 Instrument Handbook that is posted on the Web.

Although the Cycle 9 Call for Proposals will be the first opportunity to propose for the Advanced Camera for Surveys (ACS), a preview of the expected performance of ACS is presented in the Instrument Mini-Handbook, which has been prepared for the Cycle 8 Call for Proposals.

The STScI supports a broad range of WWW information pages which may be found under: http://www.stsci.edu/. Of particular interest for proposing for HST observing time are the Instruments pages which provide access to electronic versions of the Instrument Handbooks, extensive technical documentation, and the Web tools for estimating instrument count rates and exposure times. These tools also provide warnings about rates that exceed any linearity or safety limits. All may be reached through the individual instrument pages.

An HST Data Handbook is available, describing the data that are produced by each of the current SIs. In addition there are documents describing the Space Telescope Science Data Analysis Software (STSDAS).

For Archival Researchers, a "primer" and a detailed manual are available which describe how to gain access to the HST data Archive through StarView. There is also a catalog of the GO and Guaranteed Time Observer (GTO) programs that have already been accepted, which is available electronically (see section 10.1). Proposers with no network access may obtain a hardcopy of this catalog from the STScI Help Desk.

Proposers may find it convenient to order personalcopies of the manuals they will be using extensively. To order documentation, please fill out the form on the Phase I Web Documentation Server available at URL http://www.stsci.edu/observing/proposing.html, or contact the STScI Help Desk (help@stsci.edu).

Please note that documentation requested within 2 - 3 weeks prior to the deadline might not reach the requestor in time.

Updates to the technical information contained in these documents are provided on the Web.

 

3. Proposal Categories

Proposals will be selected for General Observer (GO) programs, Snapshots and funded Archival Research (AR) programs through a competitive peer-review process. A portion of the observing time has been allocated for Guaranteed Time Observers (GTOs). It is also possible to submit requests at any time for Director's Discretionary time for extremely urgent observations. In addition, U.S. proposers are strongly encouraged to submit Education/Public Outreach proposals in conjunction with their GO/AR proposals. These various proposal categories are described in section 3.1 through 3.6.

 

3.1 General Observer Proposals

3.1.1 Scope of GO Proposals

Observing proposals may request any scientifically justified amount of observing time. In past Cycles the Space Telescope Advisory Committee (STAC) advised that the best scientific use of the HST required a mix of programs of different sizes, and that in particular "Major Programs" should be encouraged. However the TAC will monitor the overall distribution to ensure that a reasonable number of "Medium" programs is also selected.

Major Programs are those requiring more than 60 orbits, and should be strongly justified, well-thought-out proposals that would lead to a clear advance in our understanding.

Smaller proposals will be classified according to the number of orbits requested per cycle as either "Small" (< 30 orbits), or "Medium" (30 to 60 orbits). The classification will be determined by the number of orbits requested in Cycle 8 (or for long-term proposals, the largest number of orbits requested in any one cycle).

3.1.2 Major Programs (> 60 orbits in Cycle 8)

Major Programs must address important scientific questions which cannot be carried out in smaller time allocations and which utilize the unique capabilities of the HST. If scientifically justified, a Major Program may extend beyond the proposal Cycle subject only to review for progress by the STScI. The Major Programs will be evaluated for scientific merit by the appropriate Peer Review Panels, and all will then be forwarded to the TAC. The TAC will recommend the actual allocation of HST time, which will not be counted against any Panel's primary allotment.

The STAC was confident that at least three Major Programs would be ranked sufficiently highly to be awarded time in Cycle 8 and beyond and, in the steady state, approximately 10 - 20% of the GO time would be devoted to such programs. The STAC did not identify particular Major Program topics to be targeted, primarily because it did not wish to restrict the creativity of the community in formulating imaginative new projects.

Selection of a Major Program for implementation does not rule out acceptance of smaller projects to do similar science, although target duplication and overall program balance will be considered.

3.1.3 Long-Term Programs and Continuation Proposals

GO programs will normally be completed within the current scheduling Cycle. However, long-term programs (i.e., observing programs having a duration of more than one Cycle) may also be accepted.

Long-term programs may include projects that require a long time baseline, but not necessarily a large total number of spacecraft orbits, in order to achieve their scientific goals. Typical examples of such projects might be astrometric observations or long-term monitoring of variable stars or active galactic nuclei. Proposals for long-term status should be limited to cases where such status is clearly required to optimize the scientific return of the project. The scientific necessity for an allocation of time extending beyond Cycle 8 should be presented in detail.

Long-term programs may be approved for durations of up to three observing Cycles. New long-term proposals should describe the entire requested program and should provide a Cycle-by-Cycle breakdown of the number of orbits requested. However, the observation summary table in the proposal should specify only the visits for Cycle 8, not the proposed visits for future Cycles nor those approved for past observing Cycles. See section 17.1 for details. A Cycle 8 long-term proposal is not allowed to request the use of instruments other than those presently offered, even if requested for future Cycles.

The Cycle 8 TAC can award limited amounts of time in Cycles 9 and 10, where the scientific justification is compelling, with no re-submission of proposals in those Cycles.

A Cycle 8 continuation proposal is required from GOs who wish to continue long-term programs for which Cycle 8 time was already tentatively approved in Cycle 6. If satisfactory progress is being made, and the need for continuing HST observations is justified, the TAC may recommend that the program continue to receive observing time in Cycle 8. However, because of the large oversubscription of HST time, the TAC will consider the scientific importance of the continuation requests relative to newly proposed programs, and it may modify the proposed continuation program or, in some cases, not recommend further observations. Note that no continuation proposal is required from GOs who had Cycle 8 time approved in Cycle 7.

 

3.1.4 Surveys and Innovative Proposals

Survey Programs are those that, while well-justified with a clear scientific program, also produce large, uniform databases having significant archival value for a large number of investigations. Proposers are advised that a commitment to waive part or all of the proprietary period will be considered positively in selecting such programs.

Innovative Programs have the potential for considerable scientific payoff but are scientifically risky, i.e. have less than 100% probability of success. Note that these are altogether different than technically risky programs, which could endanger the safety of an instrument or of the spacecraft (e.g., observations of Mercury), and which therefore will not be considered for execution.

3.1.5 Target-of-Opportunity Proposals

Targets of opportunity (TOO) are astronomical objects undergoing unexpected or unpredictable transient phenomena. They include objects that can be identified before the onset of such phenomena (e.g. cataclysmic variables, variable stars, etc.), and objects that cannot be identified in advance (e.g. novae, supernovae, gamma ray burst (GRB) sources, newly discovered comets, etc.). For such proposals it may not be possible to include a list of specific objects; instead, the proposer may specify "generic targets" (see section 17.1, Item #12). The proposal should present a detailed plan of observations that will be implemented if the specified event occurs; it should also provide an estimate of the probability of occurrence of the specified event during the 12-month observing Cycle.

Because of the heavy impact that TOO observations have on the short- and medium-term HST schedule, no more than 6 rapid (i.e., 3 weeks turn-around) TOO programs will be awarded time in Cycle 8. The Principal Investigator (PI) should include as part of the proposal the required turn-around time and, if that time is short, strong justification of the same.

TOO proposals will be peer reviewed through the normal procedures. An accepted program will be executed only in the event that the specified phenomenon actually occurs, and it will be the responsibility of the GO to inform STScI of the occurrence of the phenomenon. If the event does not occur during the observing Cycle, the program will be deactivated at the end of the Cycle. No carry-over of the TOO unused time will be allowed.

Accepted programs will require submission of a Phase II proposal before the event occurs. If there is uncertainty in the filter, exposure time, or other exposure parameters, the Phase II proposal should include a selection of preplanned contingencies from which the observer will make a selection. When notifying STScI of the appearance of the target of opportunity, the GO must provide an accurate target position.

A review of the completed proposal will be made to assure the safety of the observations, to verify that the program complies with the original observing-time allocation and scientific objectives, and to identify execution opportunities. Note that TOO proposals that utilize the STIS MAMA detectors need to pass bright object checking before they can be scheduled. For rapid turn-around proposals, where the target may be varying in intensity, a strategy will need to be developed to ensure the safety of the TOO observations. A description of how the proposer plans to deal with this issue should be provided in the Special Requirements section of the proposal. After approval by the Director, of a request to activate a TOO observation, the schedule of observations will be replanned to contain the new observations. The time necessary to conduct these activities will vary with the particular circumstances, but the minimum response time will be roughly 25 days, and this will be achievable only if all details of the proposal (except the target position) are available in advance. If the program requires submission of a new, detailed Phase II proposal, then the response time will be substantially longer.

In the event of a sudden phenomenon of a nature that could not have been anticipated, for which it is felt that HST observations should be initiated on an urgent basis, a request for Director's Discretionary time may be submitted (see section 3.5).

 

3.2 "Snapshot" Proposals

In the process of optimizing the HST observing schedule, the scheduling algorithm occasionally finds short time intervals during which it is impossible to schedule any exposures from the pool of accepted programs. In order to utilize these intervals for scientific observations, STScI has developed the capability to take short exposures ("snapshots") on objects selected from a large list of candidates.

Snapshot observations are placed on the schedule only after the observing sequence has been determined for the higher-priority targets. In the HST schedule the distribution of gaps suitable for snap observations is broad and flat between 20 and 45 minutes. However, this distribution depends on the primary observation schedule, the operating characteristics of the instruments, and on other factors; it is therefore not predictable at the time of program submission.

In certain cases, the guide-star acquisition can be omitted for snapshot exposures, which will then be taken under gyroscopic control (tracking performance is described in section 12.2). Past experience shows that there are roughly ten opportunities each week for snapshot exposures.

Astronomers are invited to propose scientific programs which can be carried out based on observations of a set of such snapshot exposures. Proposers are advised that a commitment to waive part, or all, of the proprietary period will be included in the selection criteria for such programs. Snapshot proposers should consider the following guidelines:

Snapshot proposers should be aware that snapshot time allocations are not guaranteed. The number of observations actually executed will depend on the availability of appropriate schedule gaps, therefore only a fraction of the sample targets may actually be observed. Typical completion rates are far less than 70% and there is no commitment to obtain any completion factor for snapshot programs. If a snapshot exposure fails during execution it will not be repeated.

 

3.3 Archival Research Proposals

Completed HST observations, including both GO and GTO data, become available to the community upon expiration of their proprietary periods. The data are archived at STScI and are available for analysis by interested scientists through direct retrieval (which is free and does not provide financial support) or the HST Archival Research (AR) program (which provides financial support for the analysis of the data). A copy of the HST Archive is also maintained at the Space Telescope - European Coordinating Facility (ST-ECF) in Garching, to which European requests should normally be addressed. The Canadian Astronomy Data Centre (CADC) also maintains a copy of HST science data (only), and is the preferred source for Canadian astronomers. See section 10 for an overview of the present contents of the Archive, and for details of the procedures for accessing archival HST data.

Funding for U.S. astronomers to support the analysis of archival data is expected to be available during Cycle 8. Proposals for funded Archival Research may be submitted only by scientists affiliated with U.S. institutions. Proposals for AR funding during Cycle 8 will be considered at the same time, and by the same reviewers, as proposals for observing time for Cycle 8, and the deadline for submission is the same for all proposals. The review of AR proposals will be based on scientific merit and other appropriate criteria, as discussed in section 7.2.3.

The data must be already residing in the Archive and released from proprietary rights, or to be released by the time of the funding allocation (approximately February 1999). Researchers proposing an AR program that will also utilize data from other NASA centers should submit their AR proposal to the STScI if the majority of the program involves HST archival data and its analysis. Conversely, requests for support of AR programs utilizing data primarily from other missions should follow the guidelines in the appropriate NASA Research Announcements.

Cycle 8 proposers are informed of data available from the Archival Pure Parallel Program, described in section 4.2 and on the Web (http://archive.stsci.edu/hst/parallels). In addition, observation of the Hubble Deep Field South (HDF-S) is planned to occur in October 1998, and the data will be available for Cycle 8 Archival Research proposals. Detailed information regarding the HDF-S is available on the Web (http://www.stsci.edu/ftp/science/hdf/hdfsouth/hdfs.html).

Proposals for funded AR should be submitted on the special AR proposal form, both in hardcopy (two copies) and by electronic mail. Detailed Budget Forms should be submitted with the paper copies of the proposal. Instructions for preparing AR proposals are given in section 19. For AR proposals submitted by non-U.S. PIs with U.S. Co- Investigators (Co-Is) who request funding, one of the U.S. Co-Is should be designated as administratively responsible for the STScI funding, and should collect and submit the budget forms for all of the U.S. Co-Is.

Scientific programs that require both funding for Archival Research and new observations should be submitted as two separate proposals, one requesting funding for the Archival Research, and the other proposing the new observations. The proposals should refer to each other so that the reviewers will be aware of both components of the proposed project.

 

3.4 Education/Public Outreach Proposals

The NASA Office of Space Science (OSS) has developed a comprehensive approach for making education at all levels (with a particular emphasis on pre-college education) and the enhancement of public understanding of space science integral parts of all of its missions and research programs.

In line with these NASA OSS policies, the STScI is announcing the opportunity for U.S. PI's to submit E/PO proposals in conjunction with an approved HST Cycle 8 proposal (see Appendix J for details).

 

3.5 Director's Discretionary Proposals

Up to 10% of the available HST observing time may be reserved for Director's Discretionary (DD) allocation.

A proposal for DD time might be appropriate in cases where a truly unexpected transient phenomenon occurs or when developments since the last proposal cycle make a time-critical observation necessary. Under no circumstances should a request for DD time be used to resubmit all or part of a proposal that was rejected by the normal peer review process.

The Director will usually seek advice on the scientific merit and technical feasibility of such requests from STScI staff or outside specialists before taking action. The primary criteria for acceptance are extremely high scientific merit and a strong demonstration of the urgency of the observations. Very few non-time-critical DD proposals are approved; in general, the proposers are encouraged to resubmit their proposals for the next peer review cycle.

The HST observing schedule is determined several weeks in advance of the actual observations. Although it is technically feasible to interrupt the schedule and initiate observations of a new target, short-notice interruptions place very severe demands on the planning and scheduling process, decrease overall observing efficiency, and delay other programs, and are therefore restricted. Hence, requests for DD time must be extremely well justified and, if at all possible, submitted at least three months before the date of the requested observations. Proposals for observations already covered under the Target-of-Opportunity category will generally not be acceptable. In view of the long lead times, it will in many cases be more appropriate to submit a proposal through the normal GO procedure (e.g. as a Target-of-Opportunity program) than to request DD time.

Proprietary periods for DD programs will generally be three months or shorter; especially in the case of an unexpected target of opportunity, the Director may make the data non-proprietary and available immediately to the astronomical community. However, DD proposers may request and justify longer proprietary periods in their proposals.

Scientists wishing to request DD time should do so by using the DD Submission Template on the Web at the following URL: http://www.stsci.edu/observing/proposing.html. If you do not have access to a Web browser, then you may inquire about DD procedures from the STScI Help Desk (help@stsci.edu).

 

3.6 Guaranteed Time Observer Programs

The National Aeronautics and Space Administration has awarded a portion of the observing time during the first three years of HST operations following SM2, to scientists involved in the development of the new instruments.

 

4. HST Observation Types

4.1 Primary Observations

4.1.1 Overview

Primary observations are defined as those that determine the telescope pointing and orientation. Since all of the SIs are located at fixed positions in the telescope focal plane, it is possible simultaneously to observe with one or more instruments in addition to the primary instrument; those additional observations are named parallel observations (see section 4.2).

4.1.2 Time-Critical Observations

Proposals may request that HST observations be made at a specific date and time, or within a range of specific dates. Examples of time-critical observations for which such requests would be appropriate include, but are not limited to, the following: (1) astrometric observations; (2) observations of specific phases of binary or pulsating stars; (3) monitoring of variable stars or galactic nuclei; (4) imaging of surface features on rotating solar-system bodies; (5) observations that require a specific telescope orientation (since the orientation is fixed by the date of observation, as discussed in section 11.2); (6) observations that must coincide with simultaneous ground-based or other space-based experiments; (7) observations in support of planetary missions; and (8) observations required to be repeated at some time interval.

Time-critical events that occur over short time intervals compared to the orbital period of HST (such as eclipses of very short-period binary stars) introduce an additional complication because it will not be known to sufficient accuracy, until a few weeks in advance, where HST will be in its orbit at the time of the event, and hence whether it will occur above or below the spacecraft's horizon (see section 14.3). Proposals to observe such events can therefore be accepted only conditionally.

Because of the constraints that time-critical observations impose on the HST scheduling system, the scientific justification for such requests should be presented in detail in the observing proposal.

4.1.3 Real-Time Observations

A limited capability is available for real-time interactions during HST observing. Interactive target acquisitions (section 15.2.2), late ephemeris improvements, and real-time analysis for science purposes are permitted in real-time.

The usual purpose of a real-time interaction will be to carry out an interactive target acquisition, either with the same SI to be used for the scientific observations, or with a camera SI followed by an offset to the required SI (see the Instrument Handbooks for technical details). This type of pointing improvement is required when the target must be positioned more accurately than can be done with the guide stars alone (typically about 1"), and when there is no on-board mechanism available to accomplish that task, or when early acquisition techniques cannot be used.

Small maneuvers without target acquisition are typically used to improve the telescope pointing without requiring an observation to measure the target location. The need for this type of improved pointing arises most often for solar-system targets, because of uncertainties in the target's ephemeris, and because the HST orbital decay causes changes in the times of observations after the planning and telescope scheduling have been completed. In general, the size of all real-time maneuvers is limited by the requirement that the same pair of guide stars be used to accomplish all such pointings, usually less than 1 arcmin.

Real-time analysis may be requested for either science data or engineering telemetry associated with an observation for reasons other than target acquisition. The scientific necessity of seeing the data immediately must be fully justified in the proposal.

Availability of the Tracking and Data Relay Satellite System and other constraints limit the number of real-time interactions to a few per week. Real-time observations generally require additional operational overheads, and thus reduce observing efficiency. However, some scientific programs require this activity for success and it should be requested for them. In those cases, the scientific and operational justification for such interactions should be presented clearly in the observing proposal because real-time interactions are a limited resource. Furthermore, failure of one of the SSA transmitters in 1998 reduces the opportunity to schedule real-time contacts and generally precludes two contacts in a single orbit. This transmitter is likely to be replaced in the next servicing mission.

Real-time observations will generally require the GO's presence at STScI during the exposures. STScI personnel will be present to assist the GO, and to execute the command requests.

 

4.2 Parallel Observations

Parallel observations provide a mechanism for increasing the productivity of the HST observatory. Parallel observations are observations made with one or more additional SIs while another SI is carrying out a primary observation. Depending on whether a parallel observation is or is not related to any specific primary observation, it is defined as coordinated parallel or pure parallel, respectively. Parallel observations are made solely on a basis of non-interference with the associated primary observations.

Since each SI samples a different portion of the HST focal plane (see Fig.2, section 13.4), an SI used in parallel mode will normally be pointing at a "random" area of sky several minutes of arc away from the primary target. Thus parallel observations are usually of a survey nature. However, many HST targets lie within extended objects such as star clusters or galaxies, making it possible to conduct parallel observations of nearby portions of, or even specific targets within, these objects.

Following the recommendations of the Cycle 7 HST Time Allocation Committee, an HST Archival Pure Parallel Program was begun at the start of the Cycle 7 GO observing era (June 1997), and it is ongoing. This program seeks to maximize the scientific return from HST to the community, by taking parallel data with STIS, NICMOS and WFPC2, whenever these instruments are not prime. The data are non-proprietary and are placed immediately into the HST Archive. The Archival Pure Parallel observing programs are designed with the intent of building consistent and coherent datasets for the HST Archive. A detailed description of the HST Archival Pure Parallel Program can be found on the Web (http://archive.stsci.edu/hst/parallels).

Parallel observations of the following types may be proposed:

1. Pure parallel observations. In this case, a proposal is submitted for parallel observations that are unrelated to any specific primary observations. Proposals for such programs may involve either specific or generic targets; however, the latter are more common. Proposers must justify how the proposed program is different from or significantly enhances the existing HST Pure Parallel Program. Appropriate scheduling opportunities for such observations will be identified by STScI.

2. Coordinated parallel observations. In this case, the GO requests use of two or more SIs simultaneously, typically in order to observe several adjacent targets or regions within an extended object. Proposals for coordinated parallel observations should present a description of a coherent scientific program that clearly requires simultaneous usage of multiple SIs.

The effective aperture locations are listed in Table 3 and shown in Figure 2 (section 13.4).

Technical discussions of parallel observations are given in the Instrument Handbooks. Proposers are not allowed to add, in Phase II, coordinated parallels not included in the Phase I proposal.

Parallel observations are not permitted to interfere significantly with primary observations; this restriction applies both to concurrent and subsequent observations. Some examples of this policy are the following:

The WFPC2 and STIS modes may be used for pure parallel programs in any combination of primary and parallel instruments. The STIS MAMAs and the FGS may be used together with any other instrument for coordinated parallel observations (within the same proposal) with a specified orient, but not for pure parallel observations.

The spacecraft computers automatically correct the telescope pointing of the primary observing aperture for the effect of differential velocity aberration. This means that image shifts at the parallel aperture of 10 to 20mas can occur during parallel exposures. The effect of the shift can be minimized by using the SI with the lower spatial resolution for the parallel exposure.

 

5. Proposal Submission

5.1 Who May Submit

Proposals for HST observing time may be submitted by scientists of any nationality or affiliation, and may request use of any of the available SIs. Each proposal must identify a single individual who will act as PI, but should also list all Co-Is who will be involved in the analysis of the data. The PI will be responsible for the scientific and administrative conduct of the project, and will be the formal contact for all communications with STScI. All proposals will be reviewed without regard to the nationalities or affiliations of the proposers.

An agreement between NASA and ESA states that a minimum of 15% of HST observing time (on average over the lifetime of the HST project) will be allocated to scientists from ESA member states. It is anticipated that this requirement will continue to be satisfied via the normal selection process, as it has been in previous Cycles. In order to monitor the allocation to scientists from ESA member states, STScI requests that each PI and Co-I whose affiliation is with an ESA member-state institution be identified as such in the list of investigators contained in the proposal.

 

5.2 Endorsements

Endorsement signatures are not required for Phase I observing proposals (unless required by the regulations of the proposing institution); such endorsements will be requested in Phase II from successful GOs only.

Proposals for observing time from student PIs will be considered. Each such proposal should be accompanied by a written statement from the student's faculty advisor certifying (1) that the student is qualified to conduct the observing program and data analysis; and (2) that the student is in good academic standing. This letter from the advisor should be sent by the deadline to SPSO, c/o L. Spurrier, either by paper, e-mail or fax (e-mail: spurrier@stsci.edu; FAX: 410-338-5085). If the research is part of a doctoral thesis, the proposal should so indicate. (The faculty advisor's statement is not required in cases where a student is listed in the proposal only as a Co-I.) Students should, however, be particularly aware of the inherent uncertainties of space-based research and of the possible impact of delays upon their educational progress.

 

5.3 Funding of U.S. Observers and Archival Researchers

Subject to availability of funds from NASA, STScI will provide financial support for scientists affiliated with U.S. institutions. Detailed policies that apply to such funding are discussed in Appendix B of this document. Successful GOs will be requested to provide the Budget Forms as part of their Phase II submissions. Archival Researchers wishing to apply for such support should submit Budget Forms, as described in section 16 and section 19.

For proposals submitted by non-U.S. PIs with U.S. Co-Is who request funding, one of the U.S. Co-Is should be designated as administratively responsible for the STScI funding, and should collect and submit the budget forms for all of the U.S. Co-Is in Phase II.

Proposers from ESA member states should note that ESA does not fund HST research programs. Therefore, successful ESA member-state proposers should seek any necessary resources from their respective home institutions or national funding agencies. ESA observers do, however, have access to the data-analysis facilities and technical support of the staff of the ST ECF (see Appendix A).

 

5.4 Proposal Confidentiality

Proposals submitted to STScI will be kept confidential to the maximum extent consistent with the review process described below. However, all Phase II information for accepted programs will be publicly accessible, including PI and Co-I names, project titles, abstracts, description of observations, special scheduling requirements, and details of all targets and exposures.

 

 

6. Policy Summary

6.1 Duplications of Observations

This subsection discusses several aspects of observations that may duplicate observations that have already been obtained with HST, or are currently in the pool of accepted HST programs. An observation is defined as duplicating a previous one if it is on the same astronomical target or field, with the same or similar instrument, a similar instrument mode, similar sensitivity, similar spectral resolution, and a similar spectral range. It is the responsibility of proposers to check their proposed observations against the catalog of previously executed or accepted programs (see below), and, if any duplications exist, to identify and justify them in the Phase I proposal. Any case of unjustified duplication that may come to the attention of the peer reviewers could lead to rejection during the Phase I deliberations. A final systematic computer-aided check for duplications of previous observations is carried out in Phase II, and duplicate observations will be rejected.

Under NASA policy, the GTO programs (see section 3.6) are protected against contemporaneous acquisition by the GOs of duplicate observations. Proposed GO observations that are judged to infringe upon this protection will be disallowed. However, the duplication protection is as specifically defined above; entire classes of objects or broad scientific programs are not protected. The GTOs are entitled to revise their programs after each Cycle of GO selection, but they in turn may not duplicate the previously approved GO programs. GTOs may not modify their programs in the time interval between the publication of the GTO/GO catalog in each Cycle and the final submission of the Phase II GO programs selected for that Cycle. The protection of each observation is in force throughout its proprietary data-rights period (see section 6.2), and then expires.

A catalog of all past and planned GO and GTO observing programs is available on the Web, or it can be examined interactively using StarView (see section 10.1).

Prospective GOs should examine the catalog and exposure lists carefully before submitting their proposals, to ensure that they have not duplicated these programs. If there are duplications, they must be identified and justified strongly as meeting significantly different and compelling scientific objectives. Without specific TAC recommendation to retain such exposures, STScI will remove or restrict them during the duplication checks that are made in Phase II (section 8). In these cases, no compensatory observing time will be allowed and the associated observing time will be removed from the allocation.

Snapshot targets may not duplicate approved GO or GTO programs. Following selection, investigators will define the target samples and may be called upon to assist in the elimination of target duplications. Duplicating observations will be disallowed.

It may occasionally happen that a proposer requests an acquisition image that is already contained in a GTO program, which would be protected according to the NASA policies outlined above; if an early-acquisition image is determined to be in conflict with a protected GTO image, the GO-requested image may still be permitted, but may only be used for acquisition purposes.

 

6.2 Data Rights

GOs and GTOs have exclusive access to their scientific data during a proprietary period. Normally this period is the 12 months following the date on which the data, for each target, are archived and made available to the investigator after routine data processing (section 9.2). At the end of the proprietary period, data are available for analysis by any interested scientist through the HST Archive (see section 3.3 and section 10).

Proprietary periods longer than 12 months may occasionally be appropriate for long-term programs (defined in section 3.1.3 as programs whose observations extend over more than one Cycle) if there is a need to have most or all of the data available before any significant scientific results can be obtained. Since a proprietary period longer than 12 months is not supported by the related keyword on the proposal cover page (section 17.1), requests for data-rights extensions beyond 12 months must be made in the proposal scientific justification, and will be subject to the initial TAC review.

Proposers who wish to request a proprietary period shorter than one year, or to waive their proprietary rights, should specify it in the cover page of their proposals. Because of the potential benefit to the community at large, particularly in the case of large projects, proposers are asked to give this possibility serious consideration whenever they feel that such waivers would not be harmful to their programs.

 

6.3 Use of the Continuous Viewing Zone (CVZ)

Observations of targets that lie in the CVZ (see section 14.1 and Appendix G) have been shown to be more than a factor of two more efficient than the ensemble of non-CVZ observations; hence observers are encouraged to use the CVZ when possible, in order to maximize the scientific return and efficiency of their observations. The allocation of spacecraft orbits allows proposers to evaluate straightforwardly the efficiency gains realized through observations made in the CVZ. It will often be found that use of the CVZ will allow a significant increase in the exposure time possible during a given number of spacecraft orbits, and hence its exploitation is to the proposer's advantage. Note however, that the CVZ is considered to be a limited resource and requires specific TAC approval. If TAC approval for use of the CVZ is not obtained, it will not be possible to require CVZ observations in Phase II. Therefore requests for the CVZ must be made and justified in the Phase I proposal. Proposers should also be aware that it is not possible to use the SHADOW TIME and LOW SKY special requirements in the CVZ, and that special timing requirements are not generally compatible with CVZ observations. Hence, observations requiring low background should not be proposed for execution in the CVZ (see section 18.2).

There may be occasional instances where TAC-awarded CVZ time cannot be implemented due to conflicts in scheduling during these limited opportunities. Therefore, the proposer must choose from two options:

1. Propose observations with the explicit assumption of 96 minutes per orbit (i.e. CVZ flag) in Phase I. If approved, in Phase II the proposal must then include the CVZ special requirement. If we are not able to schedule the observations in CVZ, then depending on feasibility and the TAC recommendation, the observations may be dropped entirely or rescheduled much later. The proposer must decide whether the competitive advantage of assuming CVZ for the proposal is worth the risk.

2. Use the standard orbit visibility (Table 5 in section 18.2). The observation might still be executed while in the CVZ for reasons of overall efficiency but the time saved will not be added to the observer's allocations.

 

6.4 Unschedulable or Infeasible Programs

Successful proposers should be aware that the actual execution of their observations may, in some cases, prove impossible. Possible reasons include the following: (1) the accepted observation could be found technically extremely difficult or infeasible only after receipt of the Phase II information; (2 ) the observing mode or instrument selected may not be operational; or (3) it might be found that suitable guide stars do not exist. Therefore, all observations are accepted for the HST program with the understanding that there can be no guarantee that the observations will actually be obtained. Target-of-opportunity and time-critical observations can be particularly complex to plan and execute, and will be completed only to the extent that circumstances allow. Proposers should contact the STScI Help Desk if they have questions about whether an observation is feasible. Furthermore, observations are scheduled to optimize the overall HST efficiency. The STScI will not contemplate requests to advance the scheduling of individual programs based on other considerations.

 

6.5 Special Calibrations

The Instrument Handbooks contain details on the standard calibrations. Any special calibration needs not met by the advertised standard calibration program are the responsibility of the proposer and will require a direct request for additional observing time in the Phase I submission. Proposers are encouraged to contact the STScI Help Desk to obtain information on calibration of specific SIs, especially if they have demanding calibration requirements that may go beyond standard levels.

Data flagged as having been acquired for calibration purposes will normally be made non-proprietary. All HST data may be accessed and analyzed by appropriate Instrument Scientists to assess instrument performance and to develop calibrations. If proprietary data are used in this way strict confidentiality is maintained.

 

6.6 Failed Observations

HST observations fail at the rate of a few percent. Some of these failures result from occasional guide stars that cannot be acquired, or from an instrument anomaly, or the telescope happening to be in a suspended mode when a particular observation was scheduled. Such failures that are obviously beyond the proposer's control are usually rescheduled for an automatic repeat; when this is the case, the proposer will receive a notice to this effect from the Observation Support/ Post-Observation Data Processing Unified System (OPUS). A smaller fraction of failures do not have a clear cause, and may not be evident from our internal reviews of data quality. If you believe your observation has failed or is seriously degraded, then you may request a repeat by filing a Hubble Observation Problem Report (HOPR). The HOPR must be filed within 90 days of data receipt (short time limit is imposed in order for us to learn about, and thus correct if possible, subtle problems). It is standard policy that for sets of observations to be repeated, the proposer should be willing to have the degraded/failed observations be made public. In cases where the failure resulted from proposer error, say incorrect coordinates, a repeat will not be granted. In cases where the failure was a result of incorrect instrument performance, or incorrect information provided by the Institute, a repeat will usually be granted. A 90% completion rule also usually applies, such that if you have obtained more than 90% of the planned observations and the missing data is not uniquely important, then a repeat is not normally granted.

 

6.7 Publication of HST Results

It is expected that the results of HST observations and Archival Research will be published in the scientific literature. All publications based on HST data must carry the following footnote (with the phrase in brackets included in the case of Archival Research):

"Based on observations made with the NASA/ESA Hubble Space Telescope, obtained [from the data Archive] at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555."

If the research was supported by a grant from STScI, the publication should also carry the following acknowledgment at the end of the text:

"Support for this work was provided by NASA through grant number [###] from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555."

One preprint or reprint of each refereed publication based on HST research must be sent to the following address:

Librarian
Space Telescope Science Institute
3700 San Martin Dr.
Baltimore, MD 21218 USA

In addition, one preprint of each publication based on HST research should be sent to the following address:

Dr. David Leckrone
HST Senior Scientist
Code 440
Goddard Space Flight Center
Greenbelt, MD 20771 USA

This advance information is important for planning and evaluation of the scientific operation of the HST mission. We also remind HST observers that they have a responsibility to share interesting results of their HST investigations with the public at large. The Office of Public Outreach of the STScI is available to help observers use their HST data for public information and education purposes.

 

7. Phase I: Proposal Evaluation and Selection

The process by which HST proposals will be reviewed and selected for implementation is described in this section. Prospective GOs will find it useful to have an understanding of this process as they prepare their proposals.

The review of proposals for use of the Hubble Space Telescope (HST) is managed by the Space Telescope Science Institute (STScI) and carried out in two phases. In Phase I, proposers submit a scientific justification and observation summary for review by the Telescope Allocation Committee (TAC). The TAC review recommends a list of programs to the STScI Director for preliminary approval and implementation. During Phase II, GOs whose projects have been recommended provide complete details of their proposed observations, to allow the STScI to conduct a full technical feasibility review of the programs, and a cross-proposal exposure duplication test to search for similar exposures among previous and current HST programs. Up-to-date Exposure Catalogs are made available to proposers prior to the Phase I deadline in order to avoid duplication-related problems during the Phase II implementation and review. Upon final approval by the Director, the Phase II information is then used to schedule and obtain the actual observations.

"Phase I" refers to the process from proposal preparation and submission through the peer-review selection of a recommended list of programs to the Director's approval. "Phase II" (see section 8) refers to the detailed program preparations (including specifications of the actual HST exposures in complete detail) that are subsequently carried out by the GOs who have been approved for observing time. Programs are not fully accepted until the Phase II has been submitted and the conflict checking and feasibility reviews are completed. Failure to submit the Phase II by the required deadline will result in the loss of time allocation.

Since a portion of the proposal processing will be accomplished by computer, it is essential that the proposal forms and electronic files be filled out in accordance with the instructions given in Part III.

 

7.1 Technical Review

The first step in the evaluation of a proposal is its technical review by STScI. This is carried out by a careful reading of the proposal by STScI staff members who look for particularly complex, or human and technical resource-intensive observations, or those requiring the use of limited resources (such as real-time acquisitions or TOO programs). Any technical or feasibility problems that become apparent will be brought to the attention of the peer reviewers.

 

7.2 Scientific Review

The evaluation of the scientific merit of proposals is accomplished via a two-stage peer-review process. Proposals are ranked according to a well-defined set of criteria (section 7.2.3) by scientists chosen from the international astronomical community, in order that a final recommended HST program may be transmitted to the STScI Director.

7.2.1 Subdiscipline Review Panels

In the first stage of the scientific review, each proposal will be considered in detail by the appropriate expert panel. The outcome of the panels' deliberations will be recommended allocations of spacecraft orbits and ranked lists of proposals.

7.2.2 Telescope Allocation Committee

The final recommended GO and AR programs will be selected from the ranked lists by the TAC, which will be composed of the chairpersons of the review panels plus additional interdisciplinary scientists who were not members of individual panels. The aim of the TAC will be to integrate the panel recommendations into a balanced overall scientific program for HST.

7.2.3 Selection Criteria

The peer reviewers will be advised to generally accept or reject proposals as they are and minimize orbit/object trimming. Therefore it is very important to justify both the selection and number of targets, and the number of orbits requested. Unjustified requests of time may result in rejection of the entire proposal.

The review panels and TAC will base their evaluations of HST observing proposals on the following criteria:

In the evaluation of large proposals the panels and TAC will use the following additional criteria:

The most important evaluation criteria for Archival Research proposals will be:

 

7.3 Allocation of HST Observing Time

Based on the TAC recommendations, the STScI Director will make the final allocation of observing time. The time recommended by the TAC and approved by the Director will be in units of "orbits." Directions and worksheets for calculating the required number of orbits are given in section 18 and Appendix H; they take into account the actual on-target exposure time, plus the overhead time spent acquiring guide stars and placing the targets in the desired instrument apertures, reacquiring guide stars after Earth occultation, preparing the instruments for the observations, and reading out the data.

All proposers will receive electronic notification of the outcome of the selection process. It is anticipated that the panels and TAC will meet approximately two months after the proposal submission deadline, and that notification of the Phase I outcome will be sent shortly thereafter.

 

8. Phase II Procedures

The information supplied by GOs in their Phase I proposal forms enables the scientific and preliminary technical review of the project, but is not detailed enough for flight implementation and scheduling of the observations. Successful GOs will be asked to submit additional detailed "Phase II" observation specifications so that their programs can be placed on the observing schedule for execution. The Phase II submission deadline will be approximately eight weeks after notification of the TAC outcome. Failure to submit the Phase II by the required deadline will result in the loss of time allocation.

Detailed budgets (U.S. GOs only) will be requested for submission with the Phase II material. GOs are notified of the results of review of their submitted Phase II budgets approximately 3 months after the Phase II deadline.

For complex or difficult programs, observers may visit STScI before the Phase II deadline. U.S. GOs may incur pre-award travel costs to support such visits, and financial support for such visits, where appropriate, may be included in the Phase II budget and in a preparatory funding request. However, it should be noted that all pre-award expenditures are incurred at the risk of the PI and that all funding is contingent upon the availability of funds from NASA at the time the award is made.

 

9. Data Processing and Analysis

This section outlines the sources of technical/scientific support that STScI provides to assist GOs with analysis of their data. It also briefly describes the routine processing applied to all HST data and the data products that observers will receive.

 

9.1 Program Coordinator and Contact Scientist Support

Cycle 8 observers will be assigned two points of contact - a Program Coordinator (PC) and a Contact Scientist (CS) - when their programs are approved. The role of the PC is to help the observer deliver a Phase II proposal which is syntactically correct and will schedule successfully on the telescope. The role of the CS is to provide advice on observing strategies which will ensure the scientific objectives of the program will be carried out, to answer specific questions about instrument performance, and to provide technical help in the data analysis phase of the observing program. The CS will be an Instrument Scientist involved in the calibration and characterization of the primary instrument used in the observer's program.

New GOs (and experienced GOs who may be confronting complicated new data-analysis issues) may find a 3 - 5 days post-observation visit to STScI useful for the purpose of learning how to work with their data.

 

9.2 Routine Scientific Data Processing

Scientific data are routed from HST to the Tracking and Data Relay Satellite System (TDRSS), through the TDRSS ground station at White Sands, New Mexico, to the Data Distribution Facility (DDF) at Goddard Space Flight Center in Greenbelt, Maryland, and finally to STScI. At STScI the production pipeline of OPUS provides standard processing for data editing, calibration, and product generation. These functions, performed automatically, include the following:

The data are stored in the Hubble Data Archive after processing by OPUS, and they become available to other researchers after expiration of the proprietary period. Any further processing or scientific analysis is the responsibility of the GO. One tape copy (usually 8mm Exabyte or DAT tape) of the raw and processed data is made and sent to the PI or his/her designee. The PIs may also request electronic access to the data for themselves or anyone else. This access can be obtained by sending e-mail to archive@stsci.edu. Access must be specifically requested for each proposal.

As described below, STScI provides assistance with data analysis and Archive access, either by e-mail or telephone, or during GO visits to Baltimore.

 

9.3 Space Telescope Science Data Analysis System

STSDAS is a set of tools and support software used to calibrate and analyze HST data. A companion package, TABLES, is a set of tools for creating and manipulating tabular data, reading and writing FITS images and tables, and creating customized graphics. STSDAS and TABLES are layered onto the Image Reduction and Analysis Facility (IRAF) software from the National Optical Astronomy Observatories (NOAO); one must be running IRAF in order to run STSDAS and TABLES.

STSDAS and TABLES are portable, and because they are layered onto IRAF, should run on any system for which an IRAF port exists. STScI, in conjunction with NOAO, actively supports STSDAS and TABLES on Sun workstations and file servers running SunOS and Solaris, DEC Alpha and VAX systems running OpenVMS and OSF-1, x86 PCs running Linux, Decstations running Ultrix, and HP, SGI, and IBM RISC workstations. The current version of IRAF varies with platform and can be found in the IRAF Web pages at http://iraf.noao.edu. Information on the most recent version of IRAF for OpenVMS may be requested from help@stsci.edu; NOAO will be responsible for porting the next version of IRAF (V2.11) to OpenVMS.

STSDAS and TABLES provide a large range of data-analysis tools, including the following:

The STSDAS calibration software is the same as used in the OPUS pipeline. HST observers can, therefore, recalibrate their data, examine intermediate calibration steps, and re-run the pipeline using different calibration switch settings and reference data. STSDAS includes the software needed to generate new versions of calibration reference data and calibration parameters. STSDAS also provides tools for on-site users to access the Calibration Data Base and the Data Archive.

Observers should use up-to-date software, especially if it is used for analysis of positions from HST imaging data. Current software is backward compatible with all HST archival data. However, use of software with old release dates (e.g., pre-1994 for analysis of WFPC2 data) could return spurious results. The current release of STSDAS (version 2.0) is available for downloading from the Web, or it may be obtained on magnetic tape through a request to help@stsci.edu. Further information is contained in the STSDAS User's Guide, available from the STScI as described in section 2.1. Questions about STSDAS may be addressed to help@stsci.edu.

 

10. Facilities for Archival Research

Policies for submitting requests for archival HST data, and for proposing funded Archival Research (AR), were discussed in section 3.3. The following subsections give an overview of the Archive facilities available at the STScI and methods for accessing them. Further information is given in the HST Archive Primer and in more detail in the HST Archive Manual (section 2.1).

All science and calibration data, along with a large fraction of the engineering data, are placed in the Hubble Data Archive. As of May 1st, 1998, the Archive contained approximately 4.7 Terabytes of data, comprising over one million individual datasets. About 5 Gbytes of new data are archived each day. Over half the Archive (in byte volume) is science data, with about 138,000 datasets covering more than 15,000 different targets. The science data in the Archive currently comprise about 26,000 NICMOS observations, 8,000 STIS observations, 41,000 WFPC2 images, 8,000 WF/PC images, 5,000 FOC images, 16,000 FOS spectra, 15,000 GHRS spectra, 15,000 FGS observations, and 4,000 HSP scans. Most of the data in the Archive are public and may be retrieved by any user.

 

10.1 Browsing the STScI Data Archive Catalog

The STScI Data Archive is the primary storage and distribution point for science, calibration, and engineering data from the Hubble Space Telescope. The heart of the Archive is the Data Archive and Distribution Service (DADS). DADS is the collection of optical disks on which the data are stored, the databases which comprise the Archive catalog, and the hardware and software to support the ingest and distribution of HST data.

You may browse the Archive catalog through the Web or by using a special user interface, StarView. The Web interface is available at http://archive.stsci.edu/hst/ and provides a fast means for doing simple searches on the Archive. Data may be retrieved through this interface, as well as the corresponding calibration and observatory monitoring files.

StarView is an X-Windows interface for doing more sophisticated searches on the Archive. StarView provides a wide variety of search screens, including screens to assess the calibration of observations and for searching the text of HST observing proposal abstracts. There is also a facility for creating your own custom queries, and a cross-correlation capability for large lists of targets. Search results may be displayed in single-record or table formats, and may be saved to a file.

You can easily install StarView on your own computer. Versions are available for SunOS, Solaris, Digital UNIX for Alpha, and OpenVMS for VAX and Alpha. The software may be downloaded via anonymous ftp from archive.stsci.edu in pub/starview/, or through the Web at http://archive.stsci.edu/dist_starview.html. You may also run StarView through a guest account on the archive host machine at STScI: Logon to archive.stsci.edu with the username guest and password archive, and type "StarView" to begin. The archive host also offers a non-graphical CRT-based version: type "starview" to start it. The CRT version of the software is not available for distribution.

In both the Web interface and StarView, preview images and spectra are available for most public observations. Previews are not available through the CRT-based version of StarView. Both interfaces also offer integrated access to the Digitized Sky Survey, and both allow you to use SIMBAD (Set of Identifications, Measurements, and Bibliography for Astronomical Data) or NED (NASA/IPAC Extragalactic Database) to look up the coordinates of an object by name.

An alternative method for browsing the Archive is the Archived Exposures Catalog (AEC). This is a set of flat ASCII files containing summary information about exposures, including the target name, position, instrument mode, and the date on which the data became (or will become) public. The AEC may be examined by any text editor or used as a local database of HST observations. The AEC is updated monthly, and is available via anonymous ftp from archive.stsci.edu in pub/catalogs, or through the Web at http://archive.stsci.edu/aec.html.

STScI maintains an "Archive Hotseat" (archive@stsci.edu or 410-338-4547) which operates during normal office hours. Any archive-related questions, problems, or comments should be referred to the Hotseat.

 

10.2 Archival Data Analysis

After browsing the Archive catalog using the Web interface, StarView, or the AEC, you may retrieve any data which is public or proprietary data which you have been authorized to access. PIs can request authorization by sending e-mail to archive@stsci.edu. Currently, you will need to register as an archive user to retrieve data. Registration is simple and quick. You may register through the Web at http://archive.stsci.edu/registration.html, or by typing "register" while logged into the guest account on archive.stsci.edu, or by downloading a form via anonymous ftp from archive.stsci.edu in pub/forms.

After finding suitable datasets in the Web interface or StarView and marking them for retrieval, you may initiate the retrieval process by simply pressing the "Retrieve marked datasets" button in either interface. You will be given the option of having the data retrieved either to the staging area archive.stsci.edu, from which you may transfer it via anonymous ftp, or to have the data delivered over the Internet directly to a disk on your computer.

In either interface, you may opt for having your data written to 8mm Exabyte or DAT tape and sent via FedEx, rather than transferring it electronically. This option is recommended for users whose network bandwidth is limited, and for whom it may not be practical to have all the data they need delivered electronically.

Datasets selected from the AEC may be retrieved by extracting the dataset names of the desired observations and uploading them to either StarView or the Web interface. Both interfaces can be given a list of dataset names, either explicitly or from a file. See the Archive Manual or contact the Archive Hotseat for more information.

STScI provides limited assistance in the reduction and analysis of archival data, and encourages archival researchers to visit the Institute. Most PIs will find that they will be able to obtain sufficient advice through help@stsci.edu. New HST users may find that a visit to STScI is needed; visits can be arranged through help@stsci.edu. Although we will not as a matter of course assign a Contact Scientist to a funded AR program, we will do so upon request; this individual will serve as a single point of contact to help resolve calibration and data analysis issues. However, proposers should plan to conduct the bulk of their archival research at their home institutions, and should request funds accordingly. Limited resources preclude extensive assistance in the reduction and analysis of data obtained by non-funded archival researchers.

 

PART II. THE HUBBLE SPACE TELESCOPE

11. System Overview

11.1 Telescope Description

As shown in Fig.1, HST's SIs are mounted in bays behind the primary mirror. The Wide Field Planetary Camera 2 occupies one of the radial bays, with an attached 45 degree pickoff mirror that allows it to receive the on-axis beam. Three SIs (Faint Object Camera, Near Infrared Camera and Multi-Object Spectrometer, and Space Telescope Imaging Spectrograph) are mounted in the axial bays and receive images several arcminutes off-axis.

Figure 1: The Hubble Space Telescope

Major components are labelled, and definitions of V1,V2,V3 spacecraft axes are indicated

(see also Figure 2).

 

HST receives electrical power from two solar arrays (see Fig. 1), which are turned (and the spacecraft rolled about its optical axis) so that the panels face the incident sunlight. During the 1993 servicing mission the astronauts installed new solar arrays, which have significantly reduced the thermally induced vibrations that the old arrays had been producing. Nickel-hydrogen batteries provide power during orbital night. The two high-gain antennas shown in Fig. 1 provide communications with the ground (via the Tracking and Data Relay Satellite System). Power, control, and communications functions are carried out by the Support Systems Module (SSM), which encircles the primary mirror.

During the servicing mission in December 1993, the astronauts installed COSTAR in the fourth axial bay (in place of the High Speed Photometer). COSTAR deployed corrective reflecting optics in the optical paths in front of the FOC, GHRS, and FOS, thus removing the effects of the primary mirror's spherical aberration. In addition WF/PC was replaced by the WFPC2, which contains internal optics to correct the spherical aberration.

The Fine Guidance Sensors (FGSs) occupy the other three radial bays and receive light 10-14 arcminutes off-axis. Since at most two FGSs are required to guide the telescope, it is possible to conduct astrometric observations with a third FGS. Their performance is unaffected by the installation of COSTAR.

In addition to STIS and NICMOS, the second servicing mission has replaced several additional pieces of equipment. One of the FGSs (FGS-1) has been replaced with an enhanced FGS, called FGS1R. The new FGS1R has an adjustable folding flat mirror which is commandable from the ground and affords the opportunity to re-align critical components in the FGS optical path and thus lessen the effects of spherical aberration. As a result, FGS1R is expected to significantly exceed FGS-3 in astrometric performance. As noted earlier, a final decision whether to commission FGS1R for astrometry will be made by July 1. A solid state recorder (SSR) has replaced ESTR-1, and provides a factor of 10 greater on-board data storage volume. It also provides increased flexibility in scheduling HST observations, reducing the coupling with the TDRSS system.

The precise date for the third servicing mission (SM3) is somewhat uncertain due to shuttle schedules, but is currently expected to occur in the Spring of 2000. During this mission, the Advanced Camera for Surveys (ACS) will be installed, replacing the FOC. A mechanical cooling system is planned for installation which, if successful, will allow further use of the NICMOS. Enhanced thermal control for the axial instruments will be provided with the installation of an aft-shroud cooling system. In addition, a number of repairs and replacements to the spacecraft equipment will be made, including new Solar Arrays, a new spacecraft computer, the replacement FGS-2, a replacement gyro, an S-band transmitter, and an additional solid state recorder. Based on the current schedule, SM3 will occur during Cycle 8. If necessary, Cycle 8 science observations will resume about one month after SM3, and Cycle 8 observations with WFPC2, STIS, and FGS will be interleaved with commissioning activities for ACS, possibly NICMOS, and FGS2R. ACS and the revived NICMOS will be available for GOs in Cycle 9, which nominally will start in July of 2000, along with STIS, WFPC2 and FGS.

 

11.2 HST Maneuvering and Pointing

In principle, HST is free to roll about its optical axis. However, this freedom is limited by the need to keep sunlight shining on the solar arrays, and by a thermal design that assumes that the Sun always heats the same side of the telescope.

To discuss HST pointing, it is useful to define a coordinate system that is fixed to the telescope. This system consists of three orthogonal axes: V1, V2, and V3. V1 lies along the optical axis, V2 is parallel to the solar-array rotation axis, and V3 is perpendicular to the solar-array axis (see Fig. 1). Power and thermal constraints are satisfied when the telescope is oriented such that the Sun is in the half-plane defined by the ±V1 axis and the positive V3 axis. The orientation that optimizes the solar-array positioning with respect to the Sun is called the "nominal orientation."

It should be noted that the nominal orientation angle required for a particular observation depends on the location of the target and the date of the observation. Observations of the same target made at different times will, in general, be made at different orientations.

Some departures from nominal orientation are permitted during HST observing (e.g., if a specific orientation is required at a specific date, or if the same orientation is required for observations made at different times). Off nominal roll is defined as the angle about the V1 axis between a given orientation and nominal orientation. Off nominal rolls are restricted to approximately 5 degrees when the sun angle is between 50 degrees and 90 degrees, < 30 degrees when the sun angle is between 90 degrees and 178 degrees and is unlimited at anti-sun pointings of 178 degrees to 180 degrees (note that in order to achieve an anti-sun pointing of 178 - 180 degrees the target must lie in or near the plane of the sun's orbit).

HST utilizes electrically driven reaction wheels to perform all maneuvering required for guide-star acquisition and pointing control. A separate set of rate gyroscopes is used to provide attitude information to the pointing control system.

The slew rate is limited to approximately 6 degrees per minute of time. Thus, about one hour is needed to go full circle in pitch, yaw, or roll. Upon arrival at a new target, up to 5 additional minutes must be allowed for the FGSs to acquire a new pair of guide stars. As a result, large maneuvers are costly in time and are generally scheduled for periods of Earth occultation or crossing of the South Atlantic Anomaly (see section 14.2).

The telescope does not generally observe targets within 50 degrees of the Sun, 15.5 degrees of any illuminated portion of the Earth, 7.6 degrees of the dark limb of the Earth, nor 9 degrees of the Moon.

There are exceptions to these rules for HST pointing in certain cases. For instance, the bright Earth is a useful flat-field calibration source. However, there are onboard safety features that cannot be overridden. The most important of these is that the aperture door shown in Fig. 1 will close automatically whenever HST is pointed within 35 degrees of the Sun, in order to prevent direct sunlight from reaching the optics and focal plane.

Objects in the inner solar system, such as Venus or comets near perihelion, are unfortunately difficult or impossible to observe with HST, because of the 50 degree solar limit. When the scientific justification is compelling, observations of Venus and time-critical observations of other solar-system objects lying between 46 degrees and 50 degrees of the Sun may be carried out (this capability was successfully demonstrated in Cycle 4).

 

11.3 Data Storage and Transmission

The HST observing schedule is constructed at STScI and command loads are forwarded to the Goddard Space Flight Center (GSFC) in Greenbelt, Maryland, where the Space Telescope Operations Control Center (STOCC) is located. Communication with the spacecraft is via the Tracking and Data Relay Satellite System (TDRSS), which consists of a set of satellites in geosynchronous orbit.

The TDRSS network supports many spacecraft in addition to HST. Therefore, use of the network, either to send commands or return data, must be scheduled. Because of limited TDRSS availability, command sequences for HST observations are normally uplinked periodically and stored in the onboard computers. HST then executes the observations automatically.

It is possible for observers at STScI to interact in real-time with HST for specific purposes, such as certain target acquisitions. In practice, real-time interactions are difficult to schedule (see section 4.1.3). During normal operations, fewer than 25 real-time interactions have been required in each of the past two years.

HST currently uses a large capacity Solid State Recorder to store scientific data before transmission to the ground. Except when real-time access is required, most HST observations are stored to the SSR and read back to the ground several hours later. Some scientific programs requiring very high data-acquisition rates cannot be accommodated, because the SIs would generate more data than either the links or ground system could handle.

 

12. Telescope Performance

12.1 Optical Performance

Because the primary mirror has about one-half wave of spherical aberration, the Optical Telescope Assembly (OTA) did not achieve its design performance until after the December 1993 servicing mission. From this time on, SI detectors (FGSs excluded) have viewed a corrected beam, either via COSTAR in the past or internal optics on current cycle SIs. Table 1 gives a summary of general OTA characteristics, independent of SIs.

Table 1: HST Optical Characteristics and Performance 

Design                                 Ritchey-Chretien Cassegrain             
Aperture                               2.4 m                                   
Wavelength Coverage                    From 1100 Å  (MgF2 limited)             
                                       To ~3 microns (self-emission limited)   
Focal Ratio                            f /24                                   
Plate Scale (on axis)                  3.58 arcsec/mm                          
PSF FWHM at 5000 Å                     0.043 arcsec                            
Encircled Energy within 0.1" at 5000   87% (60%-80% at detectors)

Instrumental effects mean that realized encircled energy values will be instrument and observing technique specific. For instrument specific Point Spread Function (PSF) characteristics over various wavelength ranges, please consult the Instrument Handbooks. The TinyTim software, developed at STScI and at ST-ECF, is available for detailed simulations of HST images which agree well with observation. This software can be downloaded from the Web site http://scivax.stsci.edu/~KRIST/tinytim.html.

 

12.2 Guiding Performance

HST's Pointing Control System (PCS) has two principal hardware components. Rate gyros are the guidance sensors for large maneuvers and high-frequency (> 1Hz) pointing control. At lower frequencies, the optical Fine Guidance Sensors (FGSs) provide for pointing stability, as well as for precision maneuvers such as moving-target tracking and offsets and spatial scans.

Each of the three FGSs covers a 90degree sector in the outer portion of the HST field of view (FOV), as shown in Fig. 2 (section 13.4). Optics within the FGS, using precision motor-encoder combinations, select a 5" x 5" region of sky into an x,y interferometer system. Once an FGS is locked onto a star, the motor-encoders are driven to track the interference fringe of the guide star. The encoder positions are used by the PCS software to update the current telescope attitude and correct the pointing.

The FGSs have two guiding modes: Fine Lock and Coarse Track. Fine Lock was designed to keep telescope jitter below 0.007" rms, which is now routinely achieved. A drift of up to 0.05" may occur over a timescale of 12 hours and is attributed to thermal effects as the spacecraft and FGSs are heated or cooled. Observers planning extended observations in 0.1" or smaller STIS slits should execute a target peak up maneuver every 4 orbits.

Coarse Track is now believed to cause degradation in mechanical bearings in the FGSs, and accordingly is no longer available as a guiding mode.

Guide-star acquisition times are typically 6 minutes. Reacquisitions following interruptions due to Earth occultations take about 5 minutes. It is also possible to take observations (primarily WFPC2 or STIS CCD "snapshot" exposures) without guide stars, using only gyro pointing control. The absolute pointing accuracy using gyros is about 14" (one sigma). The pointing drifts at a rate typically of 1.4 +/- 0.7 mas/sec, but it can be somewhat larger depending on the slew history of HST.

An option to be considered is provided by single FGS guide star acquisition, where the translational motion of the HST is controlled by the FGS finelock on a guide star and the roll motion is left to gyro control. A gyro drift will therefore be present in the pointing performance, however the drift is of order 1.5 mas/sec around the dominant guide star and so introduces a much smaller translational drift into the pointing. Note however that gyro drift can build up through occultations.

 

12.3 Observing Time Availability

HST's "observing efficiency" may be defined as the fraction of the total time that is devoted to acquiring guide stars, acquiring astronomical targets, and exposing on them.

The main factors that limit the observing efficiency are (1) the low spacecraft orbit, with attendant frequent Earth occultation of most targets; (2) interruptions by passages through the South Atlantic Anomaly; (3) the relatively slow slew rate; and (4) the performance of the scheduling algorithm.

During Cycle 8, it is anticipated that the observing efficiency will be about 50%. About 80% of the spacecraft time is allocated to scientific observations, with the remainder devoted to calibration and engineering observations (10%), and DD programs and repeats of failed observations (also 10%).

SM3 will occur during the second half of Cycle 8 (section 11.1). This will have an additional impact on the total number of available orbits for science observations. We anticipate allocating approximately 2500 to 3500 orbits for Cycle 8 GO observations, depending on when SM3 occurs within the Cycle.

The procedure for estimating (and minimizing) the number of spacecraft orbits required for a given set of exposures is provided in section 18. In addition to the on-target exposure time, the procedure takes into account target visibility durations, time required for guide-star acquisitions and reacquisitions and for target acquisitions, and instrument overheads and readout times.

 

13. Scientific Instrument Overview

The following Scientific Instruments will be available for Cycle 8 proposals:

All of the SIs are mounted at the HST focal plane, so that all except the WFPC2 receive light that is slightly off-axis. A schematic diagram of the telescope focal plane is given in Fig. 2 (section 13.4).

Tables 2 (a)(e) provide a summary of the capabilities of the SIs. For some applications, more than one instrument can accomplish a given task, but not necessarily with equal quality or speed.

The following subsections (13.1 through 13.3) contain brief descriptions of the three SIs offered in Cycle 8. After examining Tables 2 (a)(e), prospective proposers should read these descriptions in order to determine which SIs are likely to be most suitable for their programs. Revised or updated Instrument Handbooks, which discuss the SIs in detail, have been distributed to institutional libraries, and are available from STScI as described in section 2.1. The Instrument Handbooks must be consulted before actual preparation of observing proposals. In addition, exposure time calculators for WFPC2 and STIS can be found on the Web instrument pages to assist in the estimation of exposure times.

Data from the following SIs, which were removed from HST during the December 1993 servicing mission (WF/PC, HSP), or in February 1997 (FOS, GHRS), or which are still on board of HST but not offered in Cycle 8, are now available only in archival form:

Overviews of the capabilities of these six instruments are provided in Appendix D, which should be consulted by persons interested in proposing Archival Research funding with WF/PC, HSP, FOS, GHRS, FOC, and NICMOS data. Archival data from the WFPC2 , STIS, and FGS are, of course, also available from past Cycles.

The following Table 2 describes the capabilities of the SIs that will be available on HST during Cycle 8. This table is provided as an overview. There may be small differences between these numbers and those in the Instrument Handbooks: the Instrument Handbook numbers should take precedence.

Table 2: HST Instrument Capabilities

(a) Direct Imaging[1] 
                                                                    
                       Field of View  Projected Pixel Spacing on   Wavelength  Magnitude  
Instrument             (arcsec)       Sky (arcsec)                 Range (Å)   Limit[2]   
WFPC2[3]               150 x 150      0.10                         1200-11,000  28.0       
                       35 x 35        0.0455                       1200-11,000  27.7       
STIS                   51 x 51        0.05                         2500-11,000  28.5       
                       25 x 25        0.024                        1650-3100    24.8       
                       25 x 25        0.024                        1150-1700    24.4       

(b) Slit Spectroscopy
                                                                       
                                                      Resolving[4]                            
                       Projected                      Power         Wavelength  Magnitude     
Instrument             Aperture Size                                Range (Å)   Limit[2]      
STIS[5]                optical 51" x (0.05-2)"         ~100,000      1150-3100    11.8-13.0      
                       UV first order 28" x (0.05-2)"  through ~150  1150-3100    22.1          
                       UV echelle .2" x (0.03-.2)"     ~30,000       1150-3100    12.7-15.2      
                                                       ~8000         1150-11,000  15.2-16.1-19.5  
                                                       ~700          1150-11,000  18.6-20.1-22.4  

(c) Slitless Spectroscopy 
                                                               
                           Projected Pixel  Resolving[4]  Wavelength  Magnitude          
Instrument                 Spacing on Sky   Power         Range (Å)   Limit              
WFPC2[6]                   0.1"             ~100           3700-9800    25                 
STIS                       0.05"            ~700-8000      2000-11,000  See slit spectro-  
                           0.024"           ~700-8000      1150-3100    scopy above        
 

(d) Positional Astrometry
                                                                
                           Field of        Precision        Wavelength  Faint Magnitude  
Instrument                 View            (single measure  Range (Å)   Limit[7]         
                                           ment)                                         
FGS1R[8]                   69 sq arcmin,   1.2 - 2 mas      4700-7100    14.5             
                           5x5" IFOV       3 mas                         17.0             
FGS-3                      69 sq arcmin,   1.2-2 mas        4700-7100    14.5             
                           5x5" IFOV       3 mas                         17.5             
 


                          (e) Binary Star Transfer Mode Astrometry                                      
 
Instrument     Field of   Separation                                Accuracy  Delta      Primary star   
                 View          (mas)                                (mas)     magnitude  magnitude      
FGS1R[8]       aperture         10                                  1         1.6        14.0           
               center                                                                                   
            5x5" IFOV           10                                  1         0.0        15.5           
                                15                                  1         2.3        13.0           
                                20                                  1         0.0        16.0           
                                20                                  1         4.0        14.0           
FGS3                            20                                  1-2       0.0        14.5           
                                20                                  1-2       2.0        12.5           
                                50                                  1-2       0.0        15.0           
                                50                                  1-2       3.2        14.5

Notes to Tables 2(a)(e):
[1] WFPC2 has polarimetric imaging capabilities. STIS has coronographic capabilities.

[2] Limiting V magnitude for an unreddened A0V star in order to achieve a S/N ratio of 5 in an exposure time of 1 hour assuming low-background conditions (low-sky). The limiting magnitude in imaging in the visual is strongly affected by the sky background; under normal observing conditions, the limiting magnitude can be about 0.5 brighter than listed here. Please note that low-sky conditions limit flexibility in scheduling, and are not compatible with CVZ. Single entries refer to wavelengths near the center of the indicated wavelength range. STIS direct imaging entries assume use of a clear filter for the CCD and the quartz filter for the UV (for sky suppression). For STIS spectroscopy to achieve the specified S/N per wavelength pixel with a 0.5" slit, multiple values are given corresponding to 1300, 2800, and 6000Å respectively (if in range).

[3] The WFPC2 has four CCD chips that are exposed simultaneously. Three are "wide-field" chips, each covering a 75"x75" field and arranged in an "L" shape, and the fourth is a "planetary" chip covering a 35"x35" field.

[4] The resolving power is lambda/resolution, which for WFPC2 is lambda/delta lambda where delta lambda is the FWHM of the filter, while for STIS it is lambda/2delta lambda where delta lambda is the dispersion scale in Angstroms/pixel.

[5] The 25" slit is for the MAMA detectors, the 51" slit is for the CCD. The R~150 entry for the prism on the near-UV MAMA is given for 2300Å. More accurate and up to date values for spectroscopic limiting magnitudes can be found in the STIS Instrument Handbook.

[6] All STIS modes can be operated in a slitless manner by replacing the slit by a clear aperture. WFPC2 has a capability of obtaining low-resolution "spectra" by placing a target successively at various locations in the WFPC2 linear ramp filter. STIS also has a PRISM for use in the UV.

[7] For S/N = 1 in Fine Lock with default settings.

[8] FGS1R values are predicted performance.

 

13.1 Wide Field Planetary Camera 2 (WFPC2)

The WFPC2 is designed to provide digital imaging over a wide field of view. It has three "wide-field" charge-coupled devices (CCDs), and one high-resolution (or "planetary") CCD. Each CCD covers 800 x 800 pixels and is sensitive from 1200 to 11,000Å. All four CCDs are exposed simultaneously, with the target of interest being placed as desired within the FOV.

The three Wide Field Camera (WFC) CCDs are arranged in an "L"-shaped FOV whose long side projects to 2.5', with a projected pixel size of 0.10". The Planetary Camera (PC) CCD has a FOV of 35" x 35", and a projected pixel size of 0.0455". A variety of filters may be inserted into the optical path. Polarimetry may be performed by placing a polarizer into the beam. A ramp filter exists that effectively allows one to image a ~10" region in an arbitrary 1.3% bandpass at any wavelength between 3700 and 9800Å, by appropriately positioning the target within the FOV.

The WFC configuration provides the largest imaging FOV available on HST, but undersamples the cores of stellar images; the PC configuration samples the images better, over its smaller FOV.

 

13.2 Space Telescope Imaging Spectrograph (STIS)

STIS uses two-dimensional detectors operating from the ultraviolet to the near-infrared (1150 - 11,000Å) in support of a broad range of spectroscopic capabilities. STIS can be used to obtain spatially resolved, long slit (or slitless) spectroscopy from the full 1150 - 11,000Å range at low to medium spectral resolutions of R~400 to 14,000 with first order gratings. Echelle spectroscopy at medium and high (R ~ 24,000 and 100,000) resolutions covering broad spectral ranges of delta lambda ~800 or 250Å respectively is available in the ultraviolet (1150 - 3100Å). STIS can also be used for deep optical and solar blind ultraviolet imaging.

The three 1024 x 1024 pixel detectors supporting spectroscopy and imaging applications are:

 

The MAMA detectors support time resolutions down to 125 micro-sec in TIME-TAG mode, and the CCD can be cycled in < 28 sec with use of small subarrays. The CCD also provides visible light, and the MAMA ultraviolet light, coronographic spectroscopy. Coronographic CCD imaging is also supported.

 

13.3 Fine Guidance Sensors (FGS)

In normal operation, two of the FGSs are used for spacecraft pointing control. The FGS can also be used as a science instrument to support astrometric and photometric observations. The FGS is a white light shearing interferometer. This is a significantly different method of interferometry as compared to the long baseline Michelson Stellar Interferometer. The FGS determines the angle of the incoming beam with respect to HST's optical axis by measuring the tilt of the collimated wavefront presented to the face of the Koesters Prisms. This allows the instrument to make full use of HST's light gathering capability. An additional advantage of using Koesters prisms is that interferometric measurements can be made simultaneously in two mutually orthogonal directions (the long baseline approach is one-dimensional).

The FGS, operating in POSITION mode, can measure the relative angular separations of point sources anywhere in its 69 square arcmin field of view to an accuracy of about 1.2 mas over a magnitude range of 3 < V < 14.5, and to about 3 mas for stars as faint as V=17. The FGS can also be used in TRANSFER mode to sample the entire interferometric fringe pattern of extended objects or binary systems. Using the fringe pattern of a point source as reference, the composite fringe pattern of a non-point source object can be deconvolved to determine the size of an extended object or the angular separation and differential photometry of the components of a binary system. FGS-3, the astrometer up to HST's Cycle 7, has been successfully used to study binary systems with a combined magnitude as faint as V=14.5, with separations as small as 20 mas and magnitude differences as large as 3.5. For brighter systems with larger separations, magnitude differences as large as 4 are measurable. Likewise, systems as faint as V=16 can be studied if the magnitude difference is less than 2. It is expected that FGS1R, described below, will exceed FGS-3's performance, yielding successful observations of binary systems with angular separations perhaps as small as 6 mas (provided the magnitude differences do not exceed 1.5 or so).

Parallax, proper motion, position and photometric studies can be carried out using the FGS in POSITION mode. In this mode an object is acquired and tracked in FineLock for an extended period of time (on the order of 30 seconds for bright objects, V < 13.5, and up to 2 minutes for V > 15.5). Two dimensional positional and photometric data are gathered every 25 msec (40 Hz). In TRANSFER mode the FGS acquires an object and then repeatedly scans across it (in two dimensions) to sample the two mutually orthogonal interference patterns (referred to as the "S-curves"). TRANSFER mode observing is appropriate for detecting companions, measuring the angular separations and relative brightness of a binary's components, and measuring the angular diameters of nearby giant stars (if the angular extent is greater than about 15 mas).

TRANSFER mode observations of a binary system are used to determine the true relative orbit (inclination, period, and eccentricity) as well as the magnitude differences of the components. If TRANSFER mode observations are supplemented with POSITION mode observations of reference stars distributed about the instrument's total field of view, it is possible that the binary's parallax can be determined, thereby yielding the physical size of the semi-major axis and therefore the total mass of the system. If measurements are sufficiently accurate, then it may even be possible to measure the reflex motion of each component which determines the absolute mass of each as well as the mass/luminosity ratio.

In March 1997, an enhanced flight spare, FGS1R, was inserted into HST, to replace FGS-1 which was mechanically degrading. The enhancement, an articulating mirror, adjustable from the ground, was designed, built, and inserted into FGS1R by the instrument's manufacturer, Hughes Danbury Optical Systems. This articulating mirror provides the ability to re-align critical optical components (whose alignment degrades from the stress of launch and on-orbit desorption of optical bench's graphite-epoxy composites). STScI expects that FGS1R, once properly aligned for optical performance, will become the new astrometer (provided the instrument is temporally stable) for Cycle 8. Simulations have indicated that FGS1R will be able to successfully measure the angular separations of point sources to about 6 mas with an accuracy of about 1 mas (provided the magnitude difference is less than about 1.5).

 

13.4 The HST Field of View

Fig. 2 shows the layout of the instrument entrance apertures in the telescope focal plane, as projected onto the sky. The Instrument Handbooks should be consulted for details of each instrument's aperture sizes and orientations. The figure shows the physical locations of the WFPC2, STIS, and FGS apertures in the focal plane.

We define two new axes in Fig. 2, U2 and U3, which are fixed in the focal plane as projected onto the sky. At nominal roll (see section 11.2), the U3 axis points toward the anti-Sun.

Table 3 lists the relative effective locations of the SI apertures; the U2,U3 coordinate system of Fig. 2 is used, and the linear dimensions have been converted to arcseconds using a plate scale of 3.58 arcsec/mm. The locations of the apertures listed in Table 3 are accurate to about+/- 1 arcsec.

 

Figure 2: Layout of the aperture locations for the instruments after SM2

 

Table 3: Nominal Effective Relative Aperture Locations

(locations accurate to about +/- 1 arcsec)

Instrument  Aperture  U2        U3        
                      (arcsec)  (arcsec)  
WFPC2       PC        2         +30       
            WF2       51        6         
            WF3       0         48        
            WF4       55        6         
                                          
STIS                  214       225       
                                          
FGS         FGS1R     726       0         
            FGS-2     0         726       
            FGS-3     726       0

13.5 Bright-Object Constraints

Some of the SIs must be protected against over-illumination; these constraints are discussed below. Observations that violate these constraints should not be proposed. Note however that there may be non-linearity, saturation, or residual-image effects that set in at substantially fainter limits than the safety limits discussed below; the Instrument Handbooks should be consulted for details.

1. WFPC2. No safety-related brightness limits.

2. STIS. No safety-related brightness limits for the CCD. The STIS MAMA detectors can be damaged by excessive levels of illumination and are therefore protected by hardware safety mechanisms. In order to avoid triggering these safety mechanisms, absolute limits on the brightest targets which can be observed by STIS will be enforced by proposal screening. It is the GO's responsibility to provide accurate information to facilitate this process. It is STScI policy that observations lost due to MAMA bright object violations not be repeated. MAMA bright object limits are mode dependent. The specific count rate observing limits and example magnitude screening limits for astronomical objects observed in the most commonly used modes are in the STIS Instrument Handbook. In addition, the STIS Exposure Time Calculator on the STIS Web page can be used to determine if a particular instrument/target combination exceeds the screening limit.

3. FGS. Objects as bright as V=3.0 may be observed if the 5-mag neutral-density filter is used. Observations on all objects brighter than V=8.0 should be performed with this filter. There is a hardware limitation which prevents the FGS target acquisition from succeeding for any target brighter than V=8.0 (3.0 with F5ND).

 

14. Orbital Constraints

HST is in a relatively low orbit. The low orbit imposes a number of constraints upon scientific programs, which will be discussed in the following subsections.

 

14.1 Target Viewing Times and Continuous Viewing Zones

As seen from HST, targets in most of the sky are occulted by the Earth for varying lengths of time during each 96-min orbit. Targets lying in the orbital plane are occulted for the longest interval, about 36 min per orbit. However, this is a purely geometric limit and does not include the additional time lost due to Earth-limb avoidance limits (see section 11.2), guide-star acquisition or reacquisition, instrument setup, and South Atlantic Anomaly avoidance (section 14.2). These orbital occultations are analogous to the diurnal cycle for ground-based observing and impose the most serious constraint limiting the efficiency of most HST observations.

The length of target occultation decreases with angle from the spacecraft orbital plane. Targets lying within 24 degrees of the orbital poles are not geometrically occulted at all during the HST orbit. However, the size of the resulting "Continuous Viewing Zones" (CVZs) is substantially reduced by the Earth-limb avoidance angles. Note also that scattered Earth light may be significant when HST observes near the bright Earth limb.

Since the orbital poles lie 28.5 degrees from the celestial poles, any target located in the two declination zones near +/- 61.5 degrees will be in the CVZ at some time during the 56-day HST precessional Cycle. The maximum uninterrupted length of an observation may then be up to 7 days, although passages through the SAA (see below) will force gaps in coverage after a maximum of 5 - 6 orbits.

 

14.2 South Atlantic Anomaly

Above South America and the South Atlantic Ocean lies a lower extension of the Van Allen radiation belts called the South Atlantic Anomaly (SAA). No astronomical or calibration observations are possible during passages of the spacecraft through the SAA because of the high background induced in the detectors. SAA passages limit the longest possible uninterrupted exposures, even in the CVZs, to about 8 - 9 hours (or 5 - 6 orbits).

 

14.3 Spacecraft Position in Orbit

Because HST's orbit is low, atmospheric drag is significant. Moreover, the amount of drag varies, depending on the orientation of the telescope and the density of the atmosphere, which depends on the level of solar activity. The chief manifestation of this effect is that it is difficult to predict in advance where HST will be in its orbit at a given time. The position error may be as large as 30km within two days of a determination of the position of the spacecraft in its orbit. A predicted position 44 days in the future may be up to ~4000 km (95% confidence level) in error.

This positional uncertainty affects observers of time-critical phenomena, since the target could be behind the Earth at the time of the event. In the worst case, it will not be known if a given event will be observable until a few days before the event.

 

15. Guide Stars and Target Acquisition

As described in section 12.2, HST uses guide stars located at the edge of its field of view. Unlike ground-based telescopes, however, HST uses two guide stars in order to control the pitch, yaw, and roll axes of the telescope. It is also possible to control the telescope pointing in pitch and yaw with one guide star, with the rate gyros controlling the roll angle. In that configuration, the telescope orientation may slowly roll about the axis defined by the direction to the star. The guide star(s) are selected in advance by STScI for each observation.

 

15.1 Guide Stars

Selection of guide stars (GSs) is carried out by the Guide Star Selection System (GSSS) at STScI. The required whole-sky coverage made it necessary for STScI to assemble a collection of survey plates as the basis for construction of a catalog of GS candidates. For the northern hemisphere (for which proper motions have now outdated the Palomar Sky Atlas), a special "Quick-V" survey was conducted for STScI with the 1.2-m Schmidt telescope at Palomar Observatory. The equatorial region and the southern hemisphere are covered by the SERC-J survey and its equatorial extension.

The Guide Star Catalog (GSC), which resulted from the digitalization and analysis of the plate collection, contains information, including coordinates and magnitudes, on about 18 million objects to 14.5 mag. Version 1.1 of the Guide Star Catalog (distributed on CD-ROM and on the STScI Web site) is used for HST operations. The use of Version 1.2 is not supported at this time.

 

15.2 Target Acquisitions

Target acquisition is the method used to assure that the target is in the field of view of the requested aperture to the level of accuracy required by the science. There are several distinct methods of target acquisition; each has a different approach and different accuracy, and will take different amounts of time and resources to complete. The level of accuracy required depends most strongly on the size of the aperture to be used to take the science data and the nature of the scientific program.

15.2.1 Target Acquisition without the Ground System

Blind acquisition means that guide stars are acquired and the FGSs are used for pointing control. The pointing is accurate to the guide star position uncertainty, which is about 1".

Onboard acquisition means that software onboard the spacecraft specific to the science instrument in use will be used to center the fiducial point onto the target. On-board target acquisitions will be needed for all STIS spectroscopic observations. The WFPC2 does not have onboard acquisition capabilities. For specific information on methods and expected pointing accuracies, see the Instrument Handbook for the instrument to be used.

Early acquisition means using an image taken on an earlier visit to provide improved target coordinates for use with subsequent visits.

15.2.2 Target Acquisition with the Ground System (OPUS)

Target acquisitions that cannot be accomplished reliably or efficiently via one of the above methods may still be possible by transmitting relevant data to the STScI, analyzing it to determine the needed pointing corrections, and then providing those corrections to the telescope. This description covers two kinds of activities, the "interactive acquisition" and the "reuse target offset", both of which are described briefly here.

Interactive acquisition, or real-time target acquisition, uses the ground system software to calculate the small angle maneuver to move the aperture onto the target. This method is available for all science instruments except the astrometry FGS. High data rate TDRSS links are required at the time the data is read out of the instrument to transmit the data to the ground, and at a subsequent time to re-point the telescope before the science observations, which adds a constraint to the scheduling. The GO, or a designated representative, must be present at the STScI at the time of the acquisition. The acquisition data, usually an image, is analyzed by OPUS personnel to compute the image coordinates and centering slew for the target identified by the GO.

Reuse target offset means using an offset slew derived from an onboard acquisition or image done on a previous visit to reduce the amount of time required for subsequent visits to the same target. The data from the initial visit are analyzed by OPUS personnel to provide the offset slew to be repeated for subsequent visits. All subsequent visits to the target must use the same guide stars as the initial visit, which limits the time span of all visits to a few weeks. There are additional instrument-specific requirements. The GO is advised to contact the STScI Help Desk if this capability is required. Justification for the use of this capability must be included in the Phase I Proposal.

 

15.3 Solar-System Targets

Objects within the solar system have apparent motions with respect to the fixed stars. HST has the capability to point at and track moving targets, including planets, their satellites, and surface features on them, with sub-arcsecond accuracy. However, there are a variety of practical limitations on the use of these capabilities that must be considered before addressing the feasibility of any particular investigation.

Two specific aspects of solar-system observations are discussed below: the initial acquisition of a moving target, and the subsequent tracking of the target during the scientific observations. Only an overview of the current moving-target capabilities is given here. Phase I proposers are encouraged to consult the STScI Help Desk for more detailed information.

15.3.1 Tracking Capabilities

HST is capable of tracking moving targets with the same precision as for fixed targets (see section 12.2). This is accomplished by maintaining FGS Fine Lock on guide stars, and driving the FGS star sensors in the appropriate path, thus moving HST so as to track the target. Tracking under FGS control is technically possible for apparent target motions up to 5 arcsec/sec. In practice, however, this technique becomes infeasible for targets moving more than a few tenths of an arcsec/sec. It is currently possible to begin observations under FGS control and then switch over to gyros when the guide stars have moved out of the FGS field of view. If sufficient guide stars are available, it is possible to "hand off" from one pair to another, but this will typically incur an additional pointing error of about 0.3".

Targets moving too fast for FGS control, but slower than 7.8 arcsec/sec, can be observed under gyro control, with a loss in precision that depends on the length of the observation.

The track for a moving target is derived from its orbital elements. Orbital elements for all of the planets and their satellites are available at STScI. For other objects, the GO must provide orbital elements for the target in Phase II.

 

15.4 Offsets and Spatial Scans

Offsets (using the same guide stars and performed under the same guide star acquisition) can be performed to an accuracy of about +/- 0.02" for the larger slews. The size of the offset is limited by the requirement that both guide stars remain within the respective FOVs of their FGSs. Offsets within single detectors (most common type) can be performed to within +/- 0.003". Offsets that continue across separate visits (including visits executed with the same guide stars), will typically encounter accuracy of ~0.3".

It is also possible to obtain data while HST scans across a small region of the sky. In all cases the region scanned must be a parallelogram (or a single scan line). Two types of "spatial scans" (i.e., raster scans) may be requested:

The possible scan area is limited by the requirement that the same guide stars be used throughout the scan, and the maximum possible scan rate for continuous scans is 1arcsec/sec. Continuous spatial scan lines cannot be interrupted and must therefore be completed within one orbital target-visibility period. Spatial scans requiring more than 45 minutes of spacecraft time should be avoided.

Note that spatial scans are not available for STIS observations.

 

PART III: PHASE I INSTRUCTIONS

16. How to Submit a Phase I HST Proposal

16.1 Proposal Submission

These are the only options for preparing and submitting proposals for Cycle 8:

INTERNET: newprop@stsci.edu

NSI/DECnet: STSCIC::NEWPROP

 

Science Program Selection Office
Space Telescope Science Institute
3700 San Martin Dr.
Baltimore, MD 21218 USA

Do not submit a Postscript or PDF file in the case of AR proposals.

The deadline for submission is: September 11, 1998, 8:00pm EDT.

We urge applicants to submit their electronic versions well before the deadline, to avoid possible last-minute hardware or overloading problems, or network delays/outages.

Maximum total number of pages is 10. This includes no more than 3 pages of text for the scientific justification, plus up to 2 additional pages for figures and references. Font size should not be smaller than 12 pt. Note however that target lists longer than 1 page and the list of previously approved HST programs are not counted against the total page limit. Student Principal Investigators should enclose one copy of the certification letter from faculty advisor, as described in section 5.2.

Fully Electronic Proposal Submission - Observing Proposals

The proposer sends via electronic mail both the filled-in LaTeX proposal template AND the PostScript or PDF file output from LaTeX (which can incorporate any desired monochrome figures). For large PostScript or PDF files, an ftp area is available (see the following URL for FTP instructions: http://www.stsci.edu/ftp/proposer/cycle8/ftp_instructions). This mode does not apply to Archival Research proposals, for which signed budget forms are required (see below). Note that the Budget Forms are not required in Phase I for observing proposals. Budget Forms will be requested in Phase II from successful U.S. observers only.

 

Paper-plus-Electronic Submission - AR Proposals

Archival Research proposals are submitted in both electronic and paper form. Two (2) complete, single-sided copies of the paper proposal should be submitted to STScI. Proposers who wish to include glossies or color illustrations must make and send 20 double-sided copies of the proposal.

U.S. proposers who are requesting funding for Archival Research should also include the Budget Forms GF-97-1 through GF-97-3 (attached to both copies of the proposal), with the required institutional signatures.

The following options exist for preparing the paper forms. All of them are acceptable, but the format and contents of the forms should not be changed in any way.

1. Request the proposal templates and the style file by return e-mail (see section 16.2). Fill out the templates using standard text-editing software, run LaTeX, and then print out the proposal forms for submission. This option will be the most advantageous for the majority of proposers, since the identical template files can also be sent electronically to STScI to satisfy the electronic-submission requirement.

2. Use word-processing equipment or a typewriter to prepare facsimiles of the Phase I proposal. Note that the format of the submitted proposal should not deviate from that produced by the LaTeX form.

 

16.2 Preparation and Submission Instructions

This subsection discusses general procedures for proposal preparation and submission. Specific instructions for filling out the electronic proposal template can be found in section 17.

The computer software used in the review and feasibility analysis of proposed HST observations can interpret the proposal information only if it is in the correct format. It is therefore essential that the proposal template be filled out carefully, accurately, completely, and in accordance with the instructions.

Step-by-step Instructions

1. Obtain the Template and Style Files

To obtain electronic copies of the LaTeX template files and the style files, please send an e-mail message to newprop@stsci.edu or STSCIC::NEWPROP containing the words "request templates" in the subject line. Proposers will receive the following files by automatic "return e-mail":

2. Fill out the Template File

Fill out the appropriate Proposal Template file using any text editor on the proposer's local computer. Instructions can be found in the template itself, and in section 17 and 19.

3. Prepare a Paper Copy of the Proposal

This step is optional, for your own convenience, if you are a GO proposer, and is mandatory if you are an AR proposer. For most proposers, the easiest way to produce a paper copy of the proposal is to run LaTeX and then print the formatted proposal. If you are not familiar with LaTeX, please check with your system manager for how to run it on your system, and how to use PostScript encapsulation for any figures. The STScI Help Desk may also be contacted for assistance with any questions or problems. Rather than completing the LaTeX template version, some proposers may prefer to use different word processing software to produce a paper copy of the proposal.

4. Send the Template File Electronically - "Unformatted Submission"

Send the completed Phase I proposal LaTeX template file to the STScI by e-mail to the account named newprop (see Step 1 above) before the deadline. This is the first step of the submission. After this, you need to submit a formatted version of your proposal.

5. Send the formatted version of your Proposal to STScI - "Formatted Submission"

For GO proposals, you can either send a PostScript or PDF file via e-mail (5a), or a PostScript or PDF file via ftp (5b). Please select ONE of these options. For AR proposals, you MUST send paper copies (5c).

5a. PostScript or PDF Submission via E-Mail - for GO proposals only

Send one PostScript or PDF file, with figures included, to the STScI by e-mail to the account named newprop before the deadline. All figures must be encapsulated into the PostScript or PDF file (i.e., send only ONE PostScript or PDF file). Color figures will be printed on grey scales. Please set the formattedsubmission keyword in the LaTeX template to EMAIL.

5b. PostScript or PDF Submission via ftp - for GO proposals only

If your PostScript or PDF file contains large figures some e-mail facilities may lead to truncation or corruption of the file. If you think this may be a problem for your submission, your PostScript or PDF file should be transferred to the STScI via ftp rather than by e-mail. We have assigned a high security area for this purpose, and although you can put your files there, only the appropriate STScI staff can retrieve them. If you wish to use this option, please refer to the instructions given on-line (http://www.stsci.edu/ftp/proposer/cycle8/ftp_instructions) or contact the STScI Help Desk. Do NOT put the LaTeX template in the ftp area. Please set the formattedsubmission keyword in the LaTeX template to FTP.

5c. Make 2 Paper Copies and Send Them to STScI - for AR proposals only

Send the paper forms to the STScI before the deadline. The STScI will make the requisite copies for the proposal review process. These copies will be standard black and white Xerox copies. Budget Forms GF-97-1 through GF-97-3 must be included with each copy of the proposal. The formattedsubmission keyword in the LaTeX template is set to PAPER by default.

Proposers will receive an acknowledgment of their e-mail transmission immediately after it is received at the STScI; due to network problems, especially in the immediate vicinity of the deadline, the acknowledgment messages may be delayed. Proposers are kindly requested not to re-submit their proposals without checking with SPSO or waiting at least 2-3 hours, to avoid multiple submission of the same proposal. If no acknowledgment is received within a few days, proposers should contact the STScI Help Desk. For PostScript or PDF submissions, a separate acknowledgment will be sent after printing of the file. Again, if no second acknowledgment is received within a week, PostScript or PDF submitters should contact the STScI Help Desk. The electronic-mail user-id for general correspondence is help@stsci.edu, and the telephone number is 800-544-8125 (toll-free within the U.S.) or 410-338-1082.

European PIs and Co-Is should send an additional electronic version of the proposal template file to the ESA Project Scientist (for accounting and statistical purposes). The ESA HST Project Scientist electronic mail address is:

INTERNET: esahstps@eso.org

NSI/DECnet: ESO::ESAHSTPS

Alternatively, a paper copy should be sent to:

ESA HST Project Scientist
Space Telescope European Co-ordinating Facility
European Southern Observatory
Karl-Schwarzschild-Strasse 2
D-85748 Garching
Germany

 

17. Instructions for Filling Out HST Observing Proposal Forms

This section provides guidelines for filling out the various observing proposal forms, beginning with some general comments pertaining to all forms, and followed by more specific instructions for each form. Archival Researchers should skip section 17 and section 18 and go directly to section 19 where complete instructions for the AR proposal forms are provided.

Proposers should observe the following general instructions and conventions when filling out the forms:

17.1 Cycle 8 Observing Proposal

Specific instructions for filling out various items in the proposal are given in this section and in the LaTeX template.

 

CATEGORIES

SOLAR SYSTEM: this category refers to all objects belonging to the solar system (except the Sun and Mercury), such as planets, comets, minor planets, asteroids, planetary satellites, etc.

COOL STARS: This category refers to stars with effective temperatures less than about 10,000K. It includes low-mass pre-MS stars (T Tauri stars), early evolution, subdwarfs, subgiants, giants, supergiants, AGB stars, pulsating/variable stars, brown dwarfs, stellar activity (coronas/flares), atmospheres/chromospheres, mass loss, winds, abundances.

HOT STARS: This category refers to stars which spend a significant fraction of their observable lives at an effective temperature higher than about 10,000K. It includes OB stars, neutron stars, white dwarfs, Wolf-Rayet stars, blue stragglers, central stars of PN, variable hot stars, luminous blue variables, hot subdwarfs, high and medium mass pre-MS stars (Herbig Ae/Be), novae, supernovae, pulsars, OB associations, mass loss and winds from hot/massive stars.

BINARY STARS: This category is appropriate when the interaction between stars is their most important defining characteristics. It includes low-mass binaries, massive and eruptive binaries, X-ray binaries, CVs, black-hole candidates.

YOUNG STARS AND CIRCUMSTELLAR MATERIAL: This category refers to newly formed stars and the material surrounding them. Proposals in this category must be mainly concerned with collapsing material surrounding the star (e.g., proto-planetary disks, extra-solar planets) or the star itself (e.g., TTauri stars, FU Orionis stars) rather than the dynamical effects on surrounding material (e.g., HH Objects).

STELLAR EJECTA: This category refers to the material ejected from stars or former stars. For example, it includes nova shells, supernova remnants, stellar jets, HH objects, winds and outflows, planetary and proto-planetary nebulae.

INTERSTELLAR AND INTERGALACTIC MATTER: This category includes the general properties of the Galactic and intergalactic interstellar medium; for example, HII regions, globules, protostars, star-forming regions, giant molecular clouds, diffuse and translucent clouds, ionized gas in halo, diffuse gas observed in emission or absorption, dust, dust extinction properties, dark clouds, deuterium abundance.

STELLAR POPULATIONS IN CLUSTERS: This category refers to resolved stellar populations in globular clusters, open clusters or associations. The clusters may be in the Milky Way or in external galaxies. Included are studies of color-magnitude diagrams, luminosity functions, internal dynamics and proper motions.

FIELD STELLAR POPULATIONS: This category refers to resolved stellar populations outside clusters. It includes studies of populations in the disk, halo or bulge of the Milky Way, in satellites of the Milky Way, the Magellanic Clouds, Andromeda and its satellites, local group (dwarf) galaxies, and other nearby galaxies with resolved populations. Included are studies of color-magnitude diagrams, luminosity functions, internal dynamics and proper motions.

GALAXY POPULATIONS AND INTERACTIONS: This category includes topics related either to unresolved stellar populations in galaxies or to galaxy interactions. It includes: studies of stellar populations and star formation from integrated colors or line strength indices; studies of galaxy mergers and interactions, starburst galaxies, and IR-bright galaxies; studies of of globular clusters populations in galaxies.

GALAXY STRUCTURE AND DYNAMICS: This category refers to the structure and dynamics of galaxies, including those in the Hubble sequence, dwarf galaxies and low-surface brightness galaxies. It addresses structural components, disks, bulges, halos, central black holes, etc., and the constituents that make up and reveal these components, such as stars, gas and dust. It includes studies of morphology, kinematics, brightness profiles, dust properties, and physical conditions of the neutral and ionized gas. All studies aimed at finding and determining the masses of black holes from kinematical measurements fall in this category, independent of whether they deal with quiescent or active galaxies.

AGN HOSTS AND ENVIRONMENT: This category refers to those studies of active galaxies where the emphasis is on the properties of the host galaxy and its environment rather than on the phenomena that define a galaxy as active. The category includes host galaxy imaging, the alignment effect, and searches and surveys. It contains Seyfert galaxies, BL Lac objects, radio galaxies, quasars, blazars, etc., and also LINERS.

AGN PHYSICS: This category refers to the active phenomena in AGNs, e.g, studies of the BLR and NLR, ionization mechanisms, ionization cones, jets, nebulae, non-thermal emission, and intrinsic UV absorption. It contains Seyfert galaxies, BL Lac objects, radio galaxies, quasars, blazars, etc., and also LINERS.

QUASAR ABSORPTION LINES: This category addresses the physical properties and evolution of absorption line systems detected along the line of sight to quasars. It includes not only spectroscopy, but also, e.g., imaging of damped Ly-alpha systems

CLUSTERS OF GALAXIES AND LENSING: This category includes studies of the structure and properties of clusters and groups of galaxies, and of gravitational lensing. Clusters topics include luminosity functions, the morphology-density relation, the fundamental plane, and cooling flows. Clusters may be at any redshift, with emphasis on the structure of the cluster (not on the structure and evolution of its constituent galaxies). Lensing topics cover all lensing of high redshifts objects (background galaxies or quasars) by intermediate redshift objects (clusters of galaxies or individual galaxies), including weak lensing, strong lensing and arcs, and observations of multiply imaged sources aimed at understanding the lens, the background source, or the Hubble constant.

DISTANT GALAXIES: This category refers to studies of galaxy evolution through observations of distant objects and galaxies. It includes studies of the structure, morphology, and dynamics of galaxies at intermediate and high redshifts, deep fields, and surveys for distant objects. Studies of gamma-ray bursts should also be submitted to this category

COSMOLOGY: This category addresses the structure of the universe as a whole. It includes measurements of cosmological parameters and the extra-galactic distance scale through, e.g., Cepheids, surface brightness fluctuations, or supernovae, and measurements that aim at refining the calibrations of these techniques. This category also includes large scale structure, peculiar velocity studies and extragalactic backgrounds.

 

KEYWORDS

GENERIC 
                                                                                                                                              
ABSORPTION LINES                    EVOLUTION                              
ACCRETION DISKS                     GRAVITATIONAL LENSING                  
ASTROMETRY                          JETS                                   
CHEMICAL ABUNDANCES                 MAGELLANIC CLOUD                       
DARK MATTER                         MILKY WAY                              
DYNAMICS                            MULTIWAVELENGTH STUDY                  
DUST                                SURVEY                                 
EMISSION LINES                                                             
                                                                          
SOLAR SYSTEM 
                                                              
                                                                           
ASTEROIDS                           PLANETARY SATELLITES                   
COMETS                              RINGS AROUND PLANETS                   
EXOSPHERIC ATMOSPHERES              SUPPORT OF NASA PLANETARY MISSIONS     
PLANETARY ATMOSPHERES               SURFACES OF PLANETS/MOONS/OTHER        
PLANETARY PLASMAS                                                          
                                                                           
GALACTIC
                                                                   
                                                                           
ATMOSPHERES & WINDS             	  O, B, AND A STARS                      
BLUE STRAGGLERS                     OLD FIELD STARS                        
CENTRAL STARS OF PLANETARY NEBULAE  OLD STAR CLUSTERS                      
CLUSTER BINARY STARS                OPEN STAR CLUSTERS                     
DETACHED BINARIES                   PLANETARY NEBULAE                      
ECLIPSING BINARIES                  PROTO-PLANETARY DISKS                  
ERUPTIVE BINARY STARS               PROTO-PLANETARY NEBULAE                
EXTRA-SOLAR PLANETS                 PROTOSTELLAR OBJECTS                   
FU ORIONIS STARS                    NOVA SHELLS                            
GALACTIC BULGE                      STAR COUNTS                            
GALACTIC CENTER                     STELLAR ACTIVITY                       
GALACTIC DISK                       SUBDWARFS                              
GALACTIC HALO                       SUPERNOVAE                             
GAMMA-RAY BURSTERS                  SUPERNOVA REMNANTS                     
GLOBULAR CLUSTERS                   T TAURI STARS                          
H II REGIONS                        UV-BRIGHT STARS                        
HERBIG AE/BE STARS                  VERY LOW MASS STARS/JUPITERS           
HERBIG-HARO OBJECTS                 WHITE DWARFS                           
LUMINOUS BLUE VARIABLES             WOLF-RAYET STARS                       
MASSIVE STARS                       X-RAY BINARIES                         
MOLECULAR CLOUDS                    YOUNG FIELD STARS                      
NEUTRON STARS                       YOUNG STAR CLUSTERS                    
PECULIAR BINARY STARS                                                      
                                                                           
EXTRA-GALACTIC
                                                             
                                                                           
BAL QUASARS                         IR-BRIGHT GALAXIES                     
BL LAC OBJECTS                      IR-LUMINOUS GALAXIES                   
CLUSTER SUBSTRUCTURE                IRREGULAR GALAXIES                     
COOLING FLOWS                       LINERS                                 
COSMOLOGICAL DISTANCE SCALE         LOW SURFACE BRIGHTNESS GALAXIES        
DAMPED LYMAN-ALPHA ABSORPTION SYS   LYMAN-ALPHA FOREST CLOUDS              
TEMS                                                                       
DIFFUSE INTERGALACTIC MEDIUM        METAL ABSORPTION SYSTEMS               
DWARF GALAXIES                      PECULIAR VELOCITIES                    
ELLIPTICAL GALAXIES                 PROTO-GALAXIES                         
EXTRAGALACTIC CLUSTERS              RADIO GALAXIES                         
GALAXY CENTERS                      RADIO-LOUD QUASARS                     
GALAXY DISKS                        RADIO-QUIET QUASARS                    
GALAXY HALOS                        SEYFERT GALAXIES                       
GALAXY MORPHOLOGY                   SPIRAL BULGES                          
GROUPS OF GALAXIES                  SPIRAL GALAXIES                        
HOST GALAXIES                       STARBURST GALAXIES                     
INTERACTING GALAXIES                STELLAR POPULATIONS IN EXTERNAL GALAX  
                                    IES                                    
INTRACLUSTER MEDIUM 
 

The OS accommodates observations of (a) fixed targets (i.e., all targets outside the solar system whose positions can be defined by specific celestial coordinates), (b) generic targets (i.e., targets defined by certain general properties, rather than by specific coordinates), and (c) solar-system targets (i.e., moving targets).

For Long-Term or Continuation Programs (see section 3.1.3), include only visits requested for Cycle 8.

All visits and exposures for a given target that use the same instrument and mode may be summarized using a single OS line.

Special calibration exposures on internal sources and calibration exposures using the Earth should not be indicated here, but should be listed only in Item #14 Description of the Observations of the proposal form. They also should not be counted toward the total number of orbits given on the Cover Page; these additional orbits will be estimated by STScI staff and then communicated to the TAC reviewers. External astronomical calibration targets should be entered as separate lines on the OS, with the appropriate number of orbits.

For SNAP proposals, the OS should be filled out with a typical example of a snapshot exposure (less than one orbit), including spectral element, etc. A complete description of the target list should be provided in the scientific justification (see section 3.2).

For each row of the OS, the following information must be provided:

1. TARGET NAME

Targets should be named using the conventions recommended in Appendix E, and the adopted naming should be used consistently throughout the proposal.

2. TARGET RA AND DEC (J2000)

Supply the coordinates for fixed targets only. For generic targets use a very short text description either of the target location (e.g., HIGH-GALACTIC LATITUDE FIELD) or of the target itself.

It is important to note that the HST SIs may have very small apertures and fields of view. Target-acquisition apertures in some cases are only a few seconds of arc in size. It will be the successful proposer's responsibility in Phase II to provide coordinates accurate to about 1" for all approved targets which require onboard acquisition. Proposers can use the extraction available on-line from the STSDAS to obtain this accuracy in Phase II. For Phase I, however, target positions with accuracies better than 1' are sufficient for the TAC review (except in crowded fields where the identity of the target may be in question).

3. TARGET MAGNITUDE

Supply the apparent total magnitude in the V passband for the entire target (galaxy, planet, etc.), if known. This information is used only for scientific review, not for exposure-time calculations.

Note that some observing modes of STIS have limits on the brightness of the objects that can observe safely. For more information, refer to section 13.5 and the STIS Instruments Handbook.

4. SCIENTIFIC INSTRUMENT CONFIGURATION AND OPERATING MODE

Enter the SI configuration first, and then the operating mode. All of the allowable options can be found in Appendix C.

5. SPECTRAL ELEMENT(S) (AND CENTRAL WAVELENGTH IF STIS)

All of the desired spectral element(s) (i.e., filters and gratings) should be entered (see Appendix C for the allowable options). Several different spectral elements for different exposures may be included on the same OS exposure line, each separated by a comma (e.g., F555W,F656N). If more than one element is required for the same exposure, then join the elements with a "+" (e.g., F255W+POL45). If a STIS grating is used, then list in parentheses (immediately following the spectral element listing) the central wavelength in angstroms for the exposures defined on the given line; for example: G430M (4781, 4961).

6.APERTURE

For STIS proposals only, all the desired apertures should be entered (see Appendix C for the allowable options). Several different apertures from different exposures may be included on the same OS exposure line, each separated with a comma (e.g., 52X0.1, 52X0.2).

7.TOTAL NUMBER OF ORBITS

Specify the total number of orbits (i.e., the sum of the orbits for all of the exposures from all target visits requested) (see section 18).

8.SPECIAL REQUIREMENT FLAGS

Enter the flags listed in the Table below, where applicable. These six options are the only allowable entries.

Table 4. Flags for the Observation Summary

Parame   Description                                                                               
ter                                                                                                
CVZ      Continuous Viewing Zones observations. See section 6.3, 14.1, and 18.2.                         
DUP      Observations which duplicate previous or upcoming GO and/or GTO exposures.                
         See Item #17 Justify Duplications below and section 6.1.                                           
SHD      Shadow Time observations. See section 18.2.                                                      
PPAR     Parallel observations. All of the exposures specified on this OS line are to be done in   
CPAR     pure (PPAR) or coordinated (CPAR) parallel mode. List them both, if needed. See           
         section 4.2.                                                                                     
TOO      Target of Opportunity observations. See section 3.1.5.

This section should include a balanced discussion of both background information and the program's goals and significance to astronomy (see section 7.2.3). For SNAP proposals, the scientific justification should describe the nature of the target sample and the potential use of the survey images by the investigator and the astronomical community (see section 3.2). The description of the scientific justification should be no more than 3 pages, irrespective of the number of orbits requested, and no more than 5 pages including (optional) figures, tables and references.

For the individual items below (#14 - 17) there are no specific page limits; however, the total proposal page limits of 10 pages must be observed (without counting the information provided in item #18, and target lists longer than 1 page).

Provide a short description of the proposed observations. Explain the amount of exposure time and number of orbits requested (e.g., number of objects, examples of exposure-time calculations and orbit estimations for some typical observations, etc.). You should summarize your STIS target acquisition strategy and durations. List any special internal or Earth calibration requirements (see section 6.5) for the proposed observations here. The additional number of orbits required for these special calibrations will be estimated by STScI staff and considered by the TAC. Snapshot proposals should specifically identify the requested guiding mode and the requested proprietary data-rights period for the exposures. Long-Term and Continuation projects should provide summary information for the entire project, along with a Cycle-by-Cycle breakdown of the requested spacecraft orbits, including previously allocated time.

Justify any special scheduling requirements for early acquisitions, real-time, shadowtime, time-critical, CVZ, and target-of-opportunity (TOO) observations. For TOO objects, indicate their probability of occurrence during Cycle 8, and how soon HST must begin observing them after occurrence. Note that the earliest HST can begin TOO observations is 2 - 5 days after notification.

Describe plans for conducting coordinated and/or supporting observations with other facilities, and whether these observations put constraints on the scheduling of HST observations, such as, simultaneous or coordinated observations with other spacecraft or ground-based campaigns, or at a fixed time.

Justify, on a target-by-target basis, any possible or potential duplication with previously accepted GO or GTO observing programs (see section 6.1). Use the DUP (Duplicate Observation) flag in the OS to identify the duplicated observations.

The following material is not included in the page count for length limits. List GO proposal number (only) and status of the data (especially publications) for each accepted HST proposal of the PI (e.g., GO-4975 - 24 Orbits - Ap.J. 441, 672, 1995). Identify allocations of time related to the proposal. Unpublished data from early Cycles should be explained. A significant publication record will be regarded by Panels and TAC as a strong plus. GTO programs and publications may be included at the PI's discretion.

 

18. How to Calculate Orbits for Observing Proposals

An HST orbit normally contains 52 - 60 minutes (depending on the declination of the target) of useful observing time - the "visibility period". Some fraction of this time must be used for various overheads. The exact amount of overhead time is determined by several different factors. This section describes a simple way of determining the number of orbits required for your proposal, taking all these factors into account. Before we explain how this is done we first need to define the concept of a visit.

18.1 Visits

A visit is an exposure or series of consecutive exposures, with overheads, on a given target, and may consist of the following parts:

1. guide-star acquisition (to point HST at the target)

2. target acquisition (to place the target in an instrument aperture)

3. science exposure(s) (to obtain the data)

4. instrument overheads (to set up the instrument and read out the data)

5. instrument calibrations/overheads (if more than standard calibration is required)

 

If the visit lasts more than one orbit, it will continue with the following for each subsequent orbit:

6. guide-star re-acquisition (to keep HST pointed and locked after earth occultation)

7. science exposure(s)

8. instrument overheads

9. instrument calibrations/overheads

 

Thus, a typical visit for a spectroscopic observation (for the cameras, a target acquisition is usually not required) may look schematically like the following:


Orbit  G.S.   Tar   Sci    Over-  Sci    Over-  Earth  
1      Acq.   get   ence   head   ence   head   Occult.  
              Acq.  Exp.          Exp.               

Orbit  G.S.   Sci   Over-  Sci    Over-  End           
2      Reacq  ence  head   ence   head   of            
              Exp.         Exp.          Visit

Note that some portion of the overheads may occur before the science exposure, but for the purposes of this calculation the overheads are all assumed to follow.

 

A new visit is required whenever a new set of guide stars must be acquired. Thus, whenever the following occurs, a new visit must be defined:

1. A change in target position of greater than 2'. Note that solar-system objects that move more than 2' during the observations may not necessarily require a new visit.

2. Repeated, periodic, or other time-separated observations with an interval between exposures such that one or more empty visibility periods would otherwise be required (e.g., to obtain an image of an object every 30 days for 5 times, or to obtain a spectrum of an object at phases 0.0, 0.3, 0.6). No visit should contain empty visibility periods.

3. Required changes in spacecraft roll orientation.

4. A change in instrument (e.g., WFPC2 to STIS), except that coordinated primary and parallel observations are contained within the same visit. The switching of primary instruments requires a change of guide stars.

The maximum duration for a single visit is generally limited by the number of consecutive South Atlantic Anomaly (SAA)-free orbits (5 - 6 orbits); for shorter visits the impact of the SAA can be eliminated or minimized by careful scheduling (to place the SAA in the portion of the orbit when the target is occulted). Visits longer than 5 - 6 orbits must be broken into separate smaller visits, each with their own guide star and target acquisitions, and will be scheduled at least a day apart. If you feel that this does not apply to your program, please contact the STScI Help Desk. For STIS programs containing both CCD and MAMA science (excluding target acquisition) exposures, in which there are more than 30 minutes of science observing time using the CCD at a single target position (inclusive of overheads), and for which that target is observed for more than a single orbit, you must split the exposures into visits which separate the CCD science exposures from the MAMA exposures. If you believe your science requires CCD and MAMA science exposures in the same visit (e.g. variability monitoring programs), you should provide an explanation in the Special Requirements section of the proposal. For astrometric observations using the FGS, each individual set (consisting of target object and reference objects) may be obtained in one visit if there is no telescope motion made during the sequence.

 

18.2 How to Calculate the Number of Orbits

Step 1. Define your Observations and Group them into Visits

The first step in determining the number of orbits is to define the observations (instrument, mode, disperser, number of exposures, and exposure time) you need to execute on each target to accomplish your scientific objectives. You will then need to group your observations into separate visits following the rules given above.

Step 2. Determine the Visibility Period

The second step is for you to determine the "visibility period" for each target, which is defined as the amount of unocculted time per orbit (i.e., the amount of time per orbit during which observations can be made). This is done by using Table 5 below, which gives the visibility period as a function of target declination; values are also provided for moving targets, and for observations requiring SHD, low-sky, or CVZ observing conditions.

LOW-SKY: If the noise in your measurement will be dominated by zodiacal light, then you may wish to use the LOW - SKY scheduling restriction, which will assure that the sky background is within 30% of the yearly minimum for your target. This is achieved by restricting an observation to times that minimize both Zodiacal Light and Earthshine scattered by the OTA. The Zodiacal Light is minimized with a seasonal restriction, and the Earthshine is minimized by reducing the orbital visibility of the target by approximately 15% (the exact reduction depends on declination as shown in Table 5). If the LOW - SKY restriction is not used, for example, the Zodiacal Light background for low-ecliptic latitude targets can be as much as four times greater than the minimum value. Earthshine at the standard limb avoidance angle (20 degrees) exceeds the Zodiacal minimum by a similar factor. Use the orbital visibility given in the last column of Table 5 when computing the required number of orbits. Do not enter a flag on the OS for this condition.

SHADOW TIME: This refers to observing when HST is in Earth shadow, which can be useful for reducing the geocoronal Lyman alpha background. If you require low continuum background, use the LOW-SKY Special Requirement described above. If you require shadowtime for your observations, then you have 25 minutes in which to obtain your science exposures regardless of target declination. Note that you may perform guide-star acquisitions/re-acquisitions, as well as end-of-orbit overheads, outside the narrower shadowtime window (see the WFPC2 example in Appendix G).

MT (Moving Targets): These objects are generally in or near the ecliptic plane, so the visibility period will be ~ 53 minutes. Do not enter a flag on the OS for this condition.

CVZ (Continuous Viewing Zone): The CVZ includes the parts of the sky where the telescope can point continuously for the entire orbit(s) without being occulted by the Earth (see section 6.3, 14.1). If you can utilize CVZ time for your observations, then the visibility period is 96 minutes per orbit for 5-6 orbits, beyond which time SAA interference will limit the visibility to 75 minutes per orbit for the next 5-6 orbits. It may be to the proposer's advantage to select CVZ targets if possible, since the long visibility period of 96 minutes per orbit will allow a factor of two competitive advantage in terms of required resource charge (orbits) to perform the same science observations relative to non-CVZ targets. However, in practice the utility of CVZ observations could be reduced because the special requirements SHADOW TIME and LOW-SKY are inconsistent with CVZ observations. While the brightness of the scattered Earthshine background during CVZ observations is not greater than during non-CVZ observations (since the same bright limb avoidance angle is used), the duration of high background can be considerably greater since the line of sight can graze the bright Earth limb avoidance zone during CVZ observations. Also, it may not be possible to schedule observations that require special timing as CVZ targets. Observation sets that will use Phase II Special Requirements: ORIENT, ON HOLD (for targets of opportunity), AFTER, BEFORE, BETWEEN, or PHASE restrictions should therefore adopt the non-CVZ target visibility period for resource estimation.

Requests to remove the CVZ requirement in Phase II will be considered only in extraordinary circumstances. Similarly, requests to add the CVZ special requirement in Phase II will not generally be considered. See section 6.3 for a detailed discussion of CVZ related policies.

Table 5. Orbital Visibility

|Declination|                Visibility (minutes)  LOW-SKY Visibility (minutes)  
0  - 18                          52                    47                            
18 - 33                          53                    48                            
33 - 43                          54                    48                            
43 - 48                          55                    45                            
48 - 53                          56                    45                            
53 - 58                          57                    45                            
58 - 63                          56                    46                            
63 - 68                          57                    45                            
68 - 73                          58                    43                            
73 - 88                          59                    42                            
88 - 90                          60                    41                                                                                                   

See text for the following:                                                      
SHADOW TIME                      25                                                  
MT                               53                                                  
CVZ                              96

Step 3. Map out the Orbits in each Visit

The third step is to fit science exposures and necessary overheads into the visibility period of each orbit, for all the visits required. The better you can pack your orbits, the more efficient your proposal will be. Examples of how this can be done for each instrument, and for several observing modes, are provided in Appendix G, as are standard worksheets for each science instrument. Do not submit the worksheets with your Phase I proposal.

Step 3.1 Guide Star Acquisitions

For all observations (except WFPC2 and STIS SNAPs, see below), a guide-star acquisition is required, which takes 6 minutes. At the beginning of subsequent orbits in a multi-orbit visit, a shorter guide-star re-acquisition is required, which takes 5 minutes. For CVZ observations in which the visibility period is 96 minutes, guide-star re-acquisitions are not required; however, if your CVZ observation extends into SAA-impacted orbits, then guide-star re-acquisitions are required for those orbits. If you are obtaining very short exposures with the WFPC2 or STIS (in a Snapshot proposal) and wish to utilize the gyro guiding mode (see section 12.2 for pointing accuracy information), then use of guide stars is not required.

Step 3.2 Target Acquisitions

Following the guide-star acquisition, a target acquisition may be required, depending on the instrument used.

FGS, WFPC2: For the FGS, observations are done following a standard Spiral Search location sequence. Most WFPC2 observations also do not require a target acquisition. However, if you require precise positioning of the target (accuracy better than 1 - 2" ) with the cameras, you will need an interactive acquisition (see section 15.2.2 and the Instrument Handbooks).

STIS: Following the initial guide star acquisition for your visit, the target location in the aperture plane will be known to an accuracy of 1 - 2" . For science observations taken through spectroscopic slits which are less than 3" in either dimension and for imaging observations taken using one of the coronagraphic apertures, you will need to use an on-board STIS target acquisition and possibly an acquisition peakup exposure to center your target. STIS target acquisitions employ the CCD camera to image the target's field directly and onboard flight software processes the image to locate the position of the target.

Acquisitions: STIS target acquisition exposures (MODE=ACQ) always use the CCD, one of the filtered or unfiltered apertures for CCD imaging and a mirror as the optical element in the grating wheel. Acquisition exposures center your target in the slit or behind a coronographic bar to an accuracy of 0.01" for points sources . For a DIFFUSE source, the accuracy depends on the size of the target, and can be as large as 0.1" . A typical STIS target acquisition exposure takes 6 minutes. However, if you are acquiring a very faint target (V>21, where the exposure time on the target is not negligible), you should add 4*exposure time to the overhead. For diffuse targets see Chapters 8 and 9 of the STIS Instrument Handbook.

Peakups: Additionally, an acquisition peakup exposure (MODE=ACQ/PEAKUP) must be taken following the target acquisition exposure to refine the target centering of point or point-like sources in slits less than 0.2" wide (or tall). Peakup exposures use a science slit or coronagraphic aperture and are taken with the CCD as the detector and with either a mirror or a spectroscopic element in the grating wheel. The typical centering accuracy following a peakup sequence is 5% of the slit dimension. Typical STIS imaging point source peakups (V>21) will take ~6 minutes.

Early Acquisitions: Early Acquisitions are simply science images obtained in visit 1, followed by science images/spectra obtained in visit 2 (scheduled at a later time).

Interactive Acquisition: If you require an interactive acquisition, treat the image obtained as a science exposure (see below), then add 30 minutes for the realtime contact (which may overlap the occultation interval at the end of an orbit). If you feel you need to utilize this capability, please consult the Instrument Handbooks and contact the STScI Help Desk; you will also have to justify the need for this type of acquisition in your proposal as this is a limited resource.

Step 3.3 Science Exposures and Instrument Overheads

Following the target acquisition, you should place the science exposures in the orbit. The time allocation for these exposures consists of two partsthe exposure time and the instrument overhead. The exposure times were determined in Step 1, while the instrument overheads are given in Table 6 below (and on the worksheets) for each instrument operating mode

Table 6. Instrument Overheads

SI     Mode           Time (minutes)  Notes                                     
WFPC2 IMAGE           3               NO CR-SPLIT                               
                       5               CR-SPLIT (2 exposures)                    
                       2               LRF exposures                             

FGS    POS             1               V < 14                                 
                       2               14 < V < 15                         
                       3               15 < V < 16                         
                       4               16 < V < 16.5                       
                       8               V > 16.5                               
       TRANS           2               any                                       

STIS  CCD ACCUM      6                                                         
                      1               if no change from previous exposure       
       MAMA-spectro.  6                                                         
                      1               if no change from previous exposure       
       MAMA-imaging   5                                                         
                      1               if no change from previous exposure       
       ACQ            6               add 4 * acq. exp. time for faint targets  
       ACQ/PEAK       6               add 4 * acq. exp. time for faint targets

WFPC2: Note that all WFPC2 images with exposure times longer than 10 minutes will be split (by default in the ratio 0.5 +/- 0.2) to allow for cosmic-ray subtraction (CR-SPLIT). These should be counted as separate exposures with an overhead of 5 min when mapping out your observations, (this time accounts for the fact that there are two exposures). If you have exposures shorter than 10 minutes, or do not wish to split your exposures, then use the NO CR-SPLIT overhead time. All exposures with the Linear Ramp Filters (LRF) require an additional 2 minutes of overhead due to repositioning of the telescope.

When placing the science observations into the visit, it is important to note that WFPC2 exposures cannot be paused across orbits. This means that if you have 20 minutes left in an orbit, you can only insert an exposure that takes 20 minutes or less (including overhead). If you wish to obtain a 30 minute exposure, then you can either put it all into the next orbit, or you can specify, e.g., a 20 minute exposure in the first orbit, and a second exposure of 10 minutes in the next orbit (and thus include two exposure overheads).

A number of WFPC2 users have employed dithering, or small spatial displacements, to allow better removal of chip defects and the reconstruction of sub-pixel resolution. During Phase II the user will be given access to "canned" dithering routines, which will avoid many of the tricky details involved in planning spatial scans. The overhead for dithering, however, can be noticeable, about 1 minute for each move. The advantages, disadvantages, and overhead associated with dithering are discussed in more detail in the WFPC2 Instrument Handbook.

STIS: Some differences will be found between the overhead times presented here in Table 6 and those discussed in section 9 of the STIS Instrument Handbook. While both times are based on the same data, the times presented here are a simplified version of those presented in the handbook. The STIS sample worksheets found in Appendix H, use the simplified method presented here in the Call for Proposals. For long multi-orbit or more complex programs, please consult Chapter 9 of the STIS Instrument Handbook directly.

When calculating STIS MAMA overhead times, we refer to spectroscopy and imaging. STIS MAMA spectroscopy are those observations obtained with either the NUV or FUV MAMA detector and a grating, while STIS MAMA imaging are those observations with the NUV or FUV MAMA and a mirror in place.

The overhead times are presented as those required per exposure or the overhead times required for a subsequent exposure with no change from the previous exposure. This means that the two exposures are taken with the same aperture and grating in place and that the same wavelength is specified. The exposure times can be different between the two exposures. If you are in doubt about whether or not you would need to make a change, please assume a change for these Phase I estimates to avoid an orbit allocation shortfall later.

 

FGS: Details of FGS observing strategies may be found in the FGS Instrument Handbook.

POSITION Mode Exposure Times and Overheads: an average POSITION mode visit would include observations of 5 or more reference stars, 2 or 3 drift check stars (which can also be reference stars) and the target star, the group repeated multiple times during a single target visibility period. For stars of 13th magnitude or brighter, an estimate of exposure time is 10 - 30 seconds, for stars between 14 and 15, 30 - 60 seconds, and for stars fainter than 16, approximately 2 minutes per exposure.

Overhead estimates are provided in Table 6 which are simplified and generalized. We have found many instances where the exposure time on the logsheet can be reduced somewhat since actual data acquisition time is folded into some of the overhead activities. STScI Contact Scientists will work with the GO in refining exposure times for Phase II submission.

TRANSFER Mode Exposure Times and Overheads: for an average scan length and an average step size of 0.001", the following guide should be used to estimate TRANSFER mode exposure times

 V      Exposure times (without overheads) [s]  Assuming:  
8-12    400                                     10 scans   
13-14   800                                     20 scans   
15      1200                                    30 scans   
16      2400                                    60 scans

The TRANSFER mode overhead is somewhat dependent on the number of scans obtained during a target visibility period, but on average 2 minutes of overhead is a fair assessment.

Special Calibrations: the FGS1R TRANSFER mode stability is being monitored and should be characterized by the start of the Cycle 8 program. If the TRANSFER mode observation severely stresses the resolution limitations of FGS1R, it may be prudent for the GO to request a special calibration orbit to acquire an orbit of data on an FGS library-reference star at the same epoch as the observation of the target, and use this reference star data to deconvolve the Transfer Scan data.

Moving Targets: The onboard tracking command that is used for moving-target observations does not allow an observation (exposure plus overhead) to be longer than 33 minutes. The result is that long exposures must be split into two or more shorter exposures with separate instrument overheads for each piece.

Small Angle Maneuvers: These are changes in telescope pointing of less than 2. If you are offsetting by 12, add 1 minute of overhead.

Spatial Scans: Spatial scan timing is very dependent on the type and size of the scan. A general rule of thumb that can be used to estimate the orbit time overheads associated with spatial scans is to add

(Number_of_Steps - 1) x Small_Angle_Maneuver_time

to the exposure time and overheads where SAM_time is defined as follows:

step-size                   SAM_time     
0" < step-size < 1"       10 seconds   
1" < step-size < 10"      0.5 minutes  
10" < step-size < 1'      1 minute

For example, if your exposure time + overhead/exposure is 4 minutes per exposure and you're planning a 4 point scan with 5" between points, you would allow 17.5 minutes for the total duration of the sequence:

total exposure time overhead=16 minutes

total scan overhead=1.5 minutes [(41) x 0.5]

More precise spatial scan timing information is only available by using the Phase II Remote Proposal Submission software (RPS2). Contact the STScI Help Desk if you are a new HST user and need instructions for accessing the RPS2 software. Note that spatial scans are not supported with the FGS.

Reuse Target Offset: For those programs with multiple visits to the same target within a three-week period (start to finish), you may be able to utilize the "reuse target offset" function. Please contact the STScI Help Desk if you feel your program can benefit from this capability. If reuse target offset is appropriate for your program, you should only include the target acquisition sequence in the initial visit; the subsequent visits should start with your science exposures.

Parallel Observations: These are treated just like primary observations. Although the primary program will be responsible for performing the guide-star acquisitions and target acquisitions, the time for these overheads must still be considered in mapping parallel exposures.

For coordinated parallel observations, where you know the visit structure of the prime observations, the mapping of parallels should be straightforward. For pure parallel observations, where you may not know the prime target declinations, you should use one of the following to determine the visibility period:

1. The minimum allowable visibility period based on the target selection criteria converted to a declination range (e.g., if the generic requirement calls for delta > 80 degrees, use 59 minutes)

or

2. if you cannot do the above, map out the exposures (plus overheads) you wish to obtain in an orbit for any legal visibility period (52 - 60 minutes). If you choose this method, you may need to decrease your exposure times when you are matched with the prime observation if it has a lesser visibility period than you selected; you will be contacted by your Contact Scientist if a reduction is required.

Step 4. Add up all the orbits

Once all the visits are defined, simply add the number of orbits in each visit, and insert the number of orbits for each target/instrument combination into the proposal template. Note that only whole orbits can be requested, and only whole orbits will be allocated. (The reason for this limitation is that the combined overhead for slew, guide star acquisition, and other overheads makes it very unlikely that an unused portion of a visibility period can be effectively used by another science program.)

Note that Snapshot proposals (see section 3.2) will most likely take less than one orbit per observation. Proposers should make certain that each of their exposures (with overheads) requires 1 visibility period. Although whole orbits will be allocated, the actual schedule construction may result in a few orbits per week not being completely filled. It is these holes that are candidate times for SNAPs.

 

19. Instructions for Archival Research Proposals

19.1 Opportunity for HST Archival Research

Completed HST observations whose proprietary periods have expired are available to the community through the HST Archival Research Program. Funding may also be available for U.S. astronomers to support the analysis of such data. This section describes how to prepare and submit AR proposals for cases where funding is requested. See section 3.3 for a discussion of the policies and procedures relevant to the HST AR Program. Consult section 10 and the HST Archive Primer for more detailed information about the HST Archive and for instructions on how to request archival data when funding is not requested. Additional Archive information and a registration form are available via the Web at http://www.stsci.edu/archive.html.

 

19.2 How to Fill Out Archival Research Templates

AR proposals should be submitted using the appropriate Cycle 8 AR Proposal LaTex Template and budget forms. The Proposal LaTeX template "ARtemplate.tex" and associated style file can be obtained by sending an e-mail message to newprop@stsci.edu or STSCIC::NEWPROP containing the words "request templates" in the subject lines. Proposers will receive the relevant files by automatic "return e-mail".

Proposals must contain all of the items in the template:

All proposals must be in English. Maximum total number of pages is 10. This includes no more than 3 pages of text for the scientific justification, plus up to 2 additional pages for figures and references, and no more than 1 page for the data analysis plan. Font size should not be smaller than 12 pt.

 

19.3 Proposal Submission

AR proposals should be submitted in electronic plus paper form. For each proposal, you must send:

Science Program Selection Office
Space Telescope Science Institute
3700 San Martin Drive Baltimore, MD 21218 USA

 

19.4 Budget Forms

Budget Forms and detailed instructions for their completion can be found under the Appendix I. General information on funding policies can be found under the Appendix B.

Specific questions concerning the preparation of the budget should be directed to the Grant Administration Office (beaser@stsci.edu, wagner@stsci.edu, or 410-338-4200).

 

APPENDICES

A. STScI, ST-ECF, and CADC Contacts

Telephone numbers are 410-338-XXXX.

E-mail Phone
 
STScI Help Desk help@stsci.edu 1082
	(toll free U.S. number: 1-800-544-8125)
 
Director's Office
  Director         Robert E. Williams  wms@stsci.edu       4710
  Deputy Director  Michael G. Hauser   hauser@stsci.edu    4730
  Assoc. Director for Science Programs 
                   F. Duccio Macchetto macchetto@stsci.edu 4790
 
PRESTO Project
  Lead, PRESTO Project Office 
                   Peg Stanley         pstanley@stsci.edu  4536
  Assoc. Lead,     Glenn Miller        miller@stsci.edu    4738
 
Science Program Selection Office
  Head             Mike Shara          shara@stsci.edu     4802
Technical Manager  Brett Blacker       blacker@stsci.edu   1281
 
Science Support Division
 Head              Knox Long           long@stsci.edu      4862
 
Grants Administration Office
  Branch Chief     Ray Beaser          beaser@stsci.edu    4200
  Supervisor       Elyse Wagner        wagner@stsci.edu    4200
 
Office of Public Outreach
  Head            Carol Christian      carolc@stsci.edu    4764
 
Data Systems Division
  Archive Hotseat                      archive@stsci.edu   4547
 
Miscellaneous
  Main switchboard/receptionist                            4700
  Fax	                                                   4767
Space Telescope European Coordinating Facility
The ST-ECF provides HST information to European astronomers. 
Questions and requests may be directed to the ST-ECF as 
follows:
 
Mail: The postal address is:
Space Telescope-European Coordinating Facility
European Southern Observatory
Karl-Schwarzschild-Strasse 2
D-85748 Garching bei Munchen
Germany
Telephone: +49-89-320-06-291 / FAX: +49-89-320-06-480
 
Electronic Mail: ST-ECF has a special account for HST-related
inquiries, whose address is stdesk@eso.org. There is also an anonymous
ftp account from which HST-related programs and data can be
downloaded:
ecf.hq.eso.org (or 134.171.11.4)
For details of electronic access, including access through 
the Web, see articles in recent issues of the ST-ECF 
Newsletter. The Newsletter, although aimed principally at 
European HST users, contains articles of general interest to 
the HST community. Those who wish to subscribe should contact 
the Newsletter Editor at the ST-ECF.
 
Canadian Astronomy Data Centre
 
Canadian proposers may obtain assistance from the Canadian 
Astronomy Data Centre (CADC). Questions and requests may be 
directed to the CADC as follows:
 
Mail: The postal address is:
CADC/DAO
5071 W. Saanich Rd.
Victoria, B.C. V8X 4M6
Canada
Telephone: 			604-363-0025
Electronic Mail: 	cadc@dao.nrc.ca


 

B. Funding Policies

It is anticipated that funds will be made available to STScI by NASA for the direct support of Cycle 8 HST research by U.S. scientists. This Appendix discusses the general conditions under which such funding will be awarded.

 

B.1 Eligibility for STScI Grant Funds

Funding from STScI may be requested by scientists who are (1) United States citizens residing in the U.S., or abroad if salary and support are being paid by a U.S. institution; (2) U.S. permanent residents and foreign-national scientists working in and funded by U.S. institutions in the U.S.; or (3) U.S. Co-Investigators (Co-Is) on observing projects with non-U.S. Principal Investigators (PIs).

Proposals for funding will be accepted from Universities and other nonprofit research institutions, private for-profit organizations, Federal employees, STScI employees, and unaffiliated scientists. For-profit organizations should note that profit is not an allowable cost for GO/AR grants.

STScI encourages collaboration by scientists from different institutions in order to make the best use of HST observing time and STScI financial support. Where multiple organizations are involved, it is normally required that the proposal be submitted by only one institution, with one scientist designated as PI with full responsibility for the scientific and administrative organization of the project. The proposal should clearly describe the role of the other institutions and the proposed managerial arrangements. STScI will award funding to the designated PI institution and to the Co-I institutions. In special circumstances, a single grant may be awarded to the PI institution, which will provide Co-I funding through subgrants or subcontracts.

When a U.S. PI obtains grant funds from STScI for a project involving non-U.S. Co-Is, no funding may flow through the U.S. PI to the non-U.S. Co-Is.

U.S. Co-Is requesting funds for a proposal submitted by a non-U.S. PI are required to submit the Phase II budget forms through one of the Co-I institutions. Approved funding will be awarded by STScI directly to the Co-I institutions.

B.2 Allowable Costs

Support may be requested for the acquisition, calibration, analysis, and publication of HST data, and related costs.

The following costs are allowable:

1. Salaries and wages. Salary support for project investigators is allowable, provided it is consistent with the policies of the institution assuming responsibility for the grant. STScI funds may not be used to pay more than a person's full-time salary or to pay more than an individual's hourly rate. Also, an individual may not be reimbursed for consulting or other work in addition to a regular full-time institutional salary covering the same period of employment. For faculty members in academic institutions, STScI funding will normally be limited to no more than two months of summer-salary support. Exceptions for released time during the academic year may be permitted in special circumstances, but such costs must be fully justified in the proposal. Released time for project investigators working in non-academic institutions is allowable, provided the compensation requested is reasonable and consistent with each employee's regular full-time salary or rate of compensation. It is assumed that most scientists will be affiliated with, and apply to STScI through, institutions that will make substantial support available for project activities (e.g., computer facilities, collaboration with other scientists, students, or research assistants). Salary support may be requested for unaffiliated scientists, but must be justified in the proposal, preferably in terms of the scientist's salary while most recently affiliated with an institution, or the salary that would be received if the scientist were currently employed on a full-time basis rather than working on the HST project.


2. Research assistance. Reasonable costs for graduate students, post-doctoral associates, data aides, and secretarial and technical support for the analysis of HST data are allowable. For post-doctoral associates and other professionals, each position should be listed with the number of months, percentage of time that will be spent on the project, and rate of pay (hourly, monthly, or annual). For graduate students and secretarial, clerical, and technical staff, only the total number of persons and the total amount of salaries per year in each category are required. All such salaries must be in accordance with the standard policies of the institution assuming responsibility for the project.

3. Fringe benefits. If an institution's usual accounting practices provide that it's contributions to employee "benefits" (Social Security, retirement,etc.) be treated as direct costs, STScI funds may be requested for all applicable fringe benefits.

4. Publication costs. Reasonable costs for publication of research results obtained from the analysis of HST data are allowable.

5. Travel. Transportation and subsistence costs for project personnel to obtain, analyze, and disseminate direct results of HST observations are allowable, provided such costs have been justified in the proposal and fully detailed in the budget. Such costs must be in accordance with the written travel policies of the institution assuming responsibility for the project. In lieu of an institutional travel policy, the Federal Travel Regulations may be used for guidance.

6. Computer services. The costs of computer time and software for the analysis of HST data are allowable. Details of the services and software that will be used must be fully described and justified in the proposal.

7. Permanent equipment. The purchase of permanent equipment (items costing over $5000), including computers or related hardware, will be approved in special circumstances, and a detailed justification must be provided in the budget narrative. If such equipment is requested, the proposal must certify that the equipment is not otherwise available to project personnel, and/or that the cost of renting the equipment (or usage charges) would exceed the purchase price. Institutions are encouraged to provide at least half of the purchase price of any item costing more than $10,000. Unless stated to the contrary in the Grant Award Document, title to and all responsibility for equipment purchased with grant funds will be vested in the grantee institution, provided that the grantee uses the equipment for the authorized activities of the project and provided that the grantee agrees to transfer title to the equipment to the designee of STScI or NASA if a request for such transfer should be made within 120 days after the completion of the project. However, if the grantee organization has provided at least half of the purchase price of the equipment, STScI will vest title to such equipment in the grantee institution. Normally, the purchase of equipment will not be approved in grants to unaffiliated individuals or for-profit organizations. A detailed list of equipment purchased with grant funds must be provided with the required final financial report at the end of the grant period.

8. Materials and supplies. Materials and supplies directly related to the analysis of HST data are allowable, provided such costs are not already reimbursed through indirect costs.

9. Funds to support ground-based observations. Funding for preparatory observations is allowable for the acquisition of astrometric data to obtain accurate target positions for an observer's approved HST program. Ground-based observations that are clearly essential to the interpretation of HST observations are also allowable. A description and justification of the planned observations must be provided in the Budget Narrative Form submitted in Phase II. The total cost of the ground-based observations must be only a small portion of the overall budget to analyze HST data.

10. Indirect costs (IDCs). Indirect costs are allowable, provided that the IDC rate used in the budget is based on a Negotiation Agreement with the Federal Government. STScI will exclude from the indirect cost base all subcontracts and subgrants in excess of $10,000. Should funding be approved for the project, the grantee will be requested to submit one copy of the Federal IDC Negotiation Agreement to the STScI Grants Administration Branch.

For institutions without a negotiated rate, STScI may allow a charge of 10% of direct costs, less items that would distort this base, such as major equipment purchases. However, the charge must not exceed $5,000 and documentation must be available to support the amount charged. Alternatively, such institutions may show such expenses as direct costs to the project, provided documentation will be maintained to verify such costs. Unaffiliated scientists should not use an indirect cost rate; instead, all administrative costs should be shown as direct costs of the project. Please see the budget guidelines in Appendix I for additional information on allowable costs.

B.3 Budget Submission

Questions concerning funding policies and the budget forms should be directed to the STScI Grants Administration Office.

B.4 Preparatory Funding

GOs may request early funding of their programs if necessary to prepare for the receipt of HST data. Proposers may request up to 25% of the funds for their programs to be awarded prior to the start of the Cycle 8 observing schedule. Preparatory funding may be requested in item 12 on Budget Form GF-97-2 when the budget is submitted in Phase II. Note that the preparatory funds are part of the overall funding allocated for the program, not additional funds.

B.5 Grant Period

It is anticipated that STScI will award funding for periods of one to two years, depending on the nature and complexity of the project, to complete the analysis of the current Cycle's observations. If the requested support is for more than one year, funding for the project will be on an annual basis, with additional funding for each subsequent grant year awarded after a favorable review of an annual performance report that will be required.

Long-term projects that are approved for more than one Cycle of observations will be funded on an annual basis. Long-term programs approved in Cycle 6 require an annual continuation proposal, as described in section 3.1.3. A budget for the analysis of current Cycle observations must be submitted with an estimate of the funding requirements for subsequent Cycles. Funding for subsequent Cycles will be provided through an amendment to an existing STScI grant.

B.6 Award of Funds

Shortly before the start of Cycle 8, each PI will receive notification from the Director concerning the specific funding allocation for their GO program. It is anticipated that requests for preparatory funding will be awarded prior to the start of Cycle 8. Additional funding up to the approved funding allocation will be awarded after the receipt of observational data for each GO program.

B.7 Educational Supplements

Scientific initiatives with Education and Public Outreach purposes can be funded through the Education/Public Outreach proposals, to be submitted in conjunction with a parent GO/AR research proposal (see Appendix J for details).

 

C. Scientific Instrument Parameters

C.1. Fine Guidance Sensors (FGS)

Instrument: FGS

Configuration: FGS

Mode: POS, TRANS

The following Table describes the updated Spectral Elements for FGS.

 

Table C.1.1. Spectral Elements for FGS 

Name   Comments                 Effective Wavelength   Full Width at Half   
                                (Å)                    maximum (Å)          

F583W  Clear filter             5830                   2340                 
F5ND   Neutral Density (5 mag)  .....                  .....                
F605W  Astrometry Clear filter  6050                   1900                 
F550W  Yellow filter            5500                   750                  
PUPIL  2/3 Pupil stop            5830                   2340

C.2. Wide Field/Planetary Camera 2 (WFPC2)

Instrument: WFPC2

Configuration: WFPC2

Mode: IMAGE

The following Tables describe the updated Spectral Elements for WFPC2

 

 

Table C.2.1. WFPC2 supported filters 

-------------------------------------------------------------------------------
Name      Wheel  Description                          Central         Effective  
                                                      Wavelength (Å)  Width (Å)  
-------------------------------------------------------------------------------
F122M     1      H Ly - Alpha (Red Leak)              1420            438        
F130LP    2      CaF2 Blocker (zero focus shift)      5116            4776       
F160AW    1      Sodium filter A                      1492            449        
F160BW    1      Sodium filter B                      1492            449        
F160BN15  1      Sodium filter B rotated -15 degrees  1492            449        
F165LP    2      Suprasil Blocker (zero focus shift)  5196            4541       
F170W     8                                           1750            546        
F185W     8                                           1953            335        
F218W     8      Interstellar feature                 2192            388        
F255W     8                                           2586            393        
F300W     9      "Wide U"                             2943            736        
F336W     3      "WFPC2 U", "Strömgren u"            3342            381        
F343N     5      Ne V                                 3433            27         
F375N     5      [O II]                               3738            27         
F380W     9                                           3964            673        
F390N     5      CN                                   3889            45         
F410M     3      "Strömgren v"                        4090            147        
F437N     5      [O III]                              4370            25         
F439W     4      "WFPC2 B"                            4300            473        
F450W     10     "Wide B"                             4519            957        
F467M     3      "Strömgren b"                        4669            167        
F469N     6      He II                                4694            25         
F487N     6      H Beta                               4865            26         
F502N     6      [O III]                              5012            27         
F547M     3      "Strömgren y"                        5476            483        
F555W     9      "WFPC2 V"                            5398            1226       
F569W     4      F555W is generally preferred      5614            966        
F588N     6      He I & Na I                          5894            49         
F606W     10     "Wide V"                             5935            1497       
F622W     9                                           6163            917        
F631N     7      [O I]                                6306            31         
F656N     7      H Alpha                              6564            21         
F658N     7      [N II]                               6590            29         
F673N     7      [S II]                               6732            47         
F675W     4      "WFPC2 R"                            6696            866        
F702W     10     "Wide R"                             6868            1383       
F785LP    2      F814W is generally preferred         8617            1332       
F791W     4      F814W is generally preferred         7826            1205       
F814W     10     "WFPC2 I"                            7921            1489       
F850LP    2                                           9072            986        
F953N     1      [S III]                              9545            53         
F1042M    11                                          10184           365        
                 Quadrant Filters                                                
                                                                                 
FQUVN     11     Redshifted [O II]                    3765 - 3992     63 (avg.)  
FQUVN33   11     Redshifted [O II] rotated -33        3765            73         
                 degrees                                                         
FQCH4N    11     Methane Bands (Jewel Quad)           5433 - 8929     49 (avg.)  
FQCH4N33  11     Methane quad filter rotated -33 deg  6193            44         
FQCH4N15  11     Methane quad filter rotated -15 deg  6193            44         
FQCH4P15  11     Methane quad filter rotated +15 deg  8929            64         
POLQ      11     Polarizer (0, 45, 90, 135) - zero                               
                 focus shift                                                     
POLQN33   11     Polarizer rotated -33 degrees                                   
POLQN18   11     Polarizer rotated -18 degrees                                   
POLQP15   11     Polarizer rotated +15 degrees                                   
                 Linear Ramp Filters                                             
                                                                                 
LRF       12     Linear ramp filter set               3710 - 9762     1.3% CW    
                                                                                 
                                                                                 
-------------------------------------------------------------------------------

Note: The F160BW filter is superior to the F160AW filter. If you feel you need to use the F160AW filter, please contact your Contact Scientist.

 

Table C.2.2. Linked Spectral Element/Aperture Combinations Wood's and Quadrant Filters

-------------------------------------------------------------------------
Spectral   Aperture  Central      Effective   Comments                     
Element              Wavelength   Width (Å)                                
                     (Å)                                                   
-------------------------------------------------------------------------
F160BN15   F160BN15  1600         900         on CCD WF3                   
FQUVN      WF2       3992         64          nominal rotation             
FQUVN      WF3       3913         59          nominal rotation             
FQUVN      WF4       3830         57          nominal rotation             
FQUVN33    FQUVN33   3765         73          33 degree rotation, on       
                                              CCD WF2                      
FQCH4N     FQCH4W2   5433         38          nominal rotation, on CCD     
                                              WF2                          
FQCH4N     FQCH4W3   8929         64          nominal rotation, on CCD     
                                              WF3                          
FQCH4N     FQCH4W4   7274         51          nominal rotation, on CCD     
                                              WF4                          
FQCH4N33   FQCH4N33  6193         44          33 degree rotation, on       
                                              CCD WF2                      
FQCH4N15   FQCH4N15  6193         44          15 degree rotation, on       
                                              CCD PC1                      
FQCH4P15   FQCH4P15  8929         64          +15 degree rotation, on      
                                              CCD PC1                      
POLQ       PC1                                pol. angle 135 degrees;      
                                              POS TARG +8, +8 recom        
                                              mended to avoid cross-talk   
POLQ       WF2                                pol. angle 0 degrees         
POLQ       WF3                                pol. angle 45 degrees        
POLQ       WF4                                pol. angle 90 degrees        
POLQN33    POLQN33                            pol. angle 102 degrees, on   
                                              CCD WF2                      
POLQP15    POLQP15W                           pol. angle 15 degrees, on    
                                              CCD WF2                      
POLQP15    POLQP15P                           pol. angle 15 degrees, on    
                                              CCD PC1; not recom           
                                              mended: clear FOV only 3     
                                              arcsec                       
POLQN18    POLQN18                            pol. angle 117 degrees, on   
                                              CCD WF2                      
-------------------------------------------------------------------------

C.3. Space Telescope Imaging Spectrograph (STIS)

Instrument: STIS

Configuration: STIS/FUV, STIS/NUV, STIS/CCD

Mode: ACCUM, TIMETAG

 

Table C.3.1. Spectroscopy - CCD

----------------------------------------------------------------------------------
Name      Tilts        Central Wavelength (Å)                Å per      Resolving   
                                                             exposure   Power       
----------------------------------------------------------------------------------
G750L      Prime        7751                                  5030      ~750        
G750M      Prime       5734,6252,6768,7283,7795,8311,8825,      570     ~7000       
                       9336,9851,10363                                              
           Secondary   6094,6581,8561,9286,9806                                     
G430L      Prime       4300                                   2900      ~750        
G430M      Prime       3165,3423,3680,3936,4194,4451,4706,      286     ~7000       
                       4961,5216,5471                                               
           Secondary   3305,3843,4781,5093                                          
G230LB     Prime        2375                                  1380      ~750        
G230MB     Prime       1713,1854,1995,2135,2276,2416,2557,      155     ~7000       
                       2697,2836,2976,3115                                          
           Secondary   2794                                                         
----------------------------------------------------------------------------------

Table C.3.2. Spectroscopy - NUV-MAMA 

-------------------------------------------------------------------------------
Name    Tilts         Central Wavelength (Å)               Å per     Resolving   
                                                           exposure  Power       
-------------------------------------------------------------------------------
G230L    Prime       2376                                  1610      ~700        
G230M    Prime       1687,1769,1851,1933,2014,2095,2176,       90    ~13,000     
                     2257,2338,2419,2499,2579,2659,2739,                         
                     2818,2898,2977,3055                                         
         Secondary   1884,2600,2800,2828                                         
E230M    Prime       1978,2707                              ~800     ~30,000     
         Secondary   2124,2269,2415,2561                                         
E230H    Prime       1763,2013,2263,2513,2762,3012           ~267    ~110,000    
         Secondary   1813,1863,1913,1963,2063,2113,2163,                         
                     2213,2313,2363,2413,2463,2563,2613,                         
                     2663,2713,2812,2862,2912,2962                               
PRISM    Prime       1200,2125                              1950     ~100        
-------------------------------------------------------------------------------

Table C.3.3. Spectroscopy - FUV-MAMA 

-------------------------------------------------------------------------------
Name    Tilts        Central Wavelength (Å)                (Å) per   Resolving   
                                                          exposure   Power       
-------------------------------------------------------------------------------
G140L   Prime        1425                                 610        ~1000       
G140M   Prime        1173,1222,1272,1321,1371,1420,1470,   55        ~13,000     
                     1518,1567,1616,1665,1714                                    
        Secondary    1218,1387,1400,1540,1550,1640                               
E140M   Prime        1425                                  600       ~45,000     
E140H    Prime       1234,1416,1598                       ~210       ~110,000    
         Secondary   1271,1307,1343,1380,1453,1489,1526,                         
                     1562                                                        
-------------------------------------------------------------------------------

Table C.3.4. Imaging

--------------------------------------------------------------------------
Name            Filter                      Central      FWHM    Detector   
                                            Wavelength   (Å)                
                                            (A)                             
--------------------------------------------------------------------------
50CCD           clear                       5850         4410    CCD        
F28X50LP        optical longpass             7230        2720    CCD        
F28X50OIII     [O III] *                    5007         5       CCD        
F28X50OII      [OII]                        3740         80      CCD        
25MAMA (NUV)    clear                       2220         1200    NUV        
25MAMA (FUV)   clear                        1370         320      FUV       
F25QTZ (NUV)    UV near longpass            2320         1010     NUV       
F25QTZ (FUV)   UV near longpass             1590         220      FUV       
F25SRF2 (NUV)  UV far longpass              2270         1110     NUV       
F25SRF2 (FUV)  UV far longpass              1480         280      FUV       
F25MGII        MgII*                        2800         70       NUV       
F25CN270       continuum near 2700 Å*       2700         350    NUV         
F25CIII         CIII]                       1909         70     NUV         
F25CN182        continuum near 1800A        1820         350    NUV         
F25LYA         Lyman alpha                   1216        85     FUV         
F25NDQ1**      neutral density, ND=10{-1}   1150-11000          CCD/NUV/    
                                                                FUV         
F25NDQ2**      neutral density, ND=10{-2}   1150-11000          CCD/NUV/    
                                                                FUV         
F25NDQ3**      neutral density, ND=10{-3}   1150-11000          CCD/NUV/    
                                                                FUV         
F25NDQ4**      neutral density, ND=10{-4}   1150-11000          CCD/NUV/    
                                                                FUV         
F25ND3         neutral density, ND=10{-3}   1150-11000          CCD/NUV/    
                                                                FUV         
F25ND5         neutral density, ND=10{-5}   1150-11000          CCD/NUV/    
                                                                FUV         
--------------------------------------------------------------------------

* filter has a substantial red leak

** quad filter (see Instrument Handbook)

 

Table C.3.5. CCD Imaging with the Coronograph

----------------------------------------------------------
Name        Description                                     
----------------------------------------------------------
WEDGEA1.0    wedge A in coronographic aperture; with=1.0"   
WEDGEA1.8    wedge A in coronographic aperture; with=1.8"   
WEDGEA2.0   wedge A in coronographic aperture; with=2.0"    
WEDGEA2.5    wedge A in coronographic aperture; with=2.5"   
WEDGEA2.8   wedge A in coronographic aperture; with=2.8"    
WEDGEB1.0    wedge B in coronographic aperture; with=1.0"   
WEDGEB1.8   wedge B in coronographic aperture; with=1.8"    
WEDGEB2.0    wedge B in coronographic aperture; with=2.0"   
WEDGEB2.5   wedge B in coronographic aperture; with=2.5"    
WEDGEB2.8   wedge B in coronographic aperture; with=2.8"    
BAR10       bar in coronographic aperture: 10.0"x3.0"       
----------------------------------------------------------

Table C.3.6. Supported Spectroscopic Apertures for STIS (1)

----------------------------------------------------
Name               Description                        
----------------------------------------------------
0.2X0.06            echelle slit                      
0.2X0.09            echelle slit                      
0.2X0.2             echelle slit                      
6X0.2               echelle slit                      
0.2X0.2 FP (A-E)   fpsplit echelle slit               
0.2X0.06 FP (A-E)  fpsplit echelle slit               
0.1X0.03           echelle slit                       
2X2                 first order slit                  
52X0.05            first order slit                   
52X0.1              first order slit                  
52X0.2              first order slit                  
52X0.5              first order slit                  
52X2                first order slit                  
52X0.2F1            first order slit; fiducial=0.5"   
----------------------------------------------------

Footnotes

(1)
The first order modes can also be used slitless, or with blocking filters

There are many available apertures that can be used if necessary; see the Instrument Handbook for the complete list. The need for the available apertures should be addressed in the Special Requirements section of the proposal.

 

D. Scientific Instruments not offered in Cycle 8

The following subsections describe the four instruments that were removed from HST during the servicing missions and the two instruments still on board the HST but not currently offered for observations in Cycle 8. The information may be of use to persons proposing AR. section 10 gives estimates of the amount of archival data available from these instruments. Further details for any of the instruments mentioned below may be found through consulting the most recent Instrument Handbooks and the HST Data Handbook as presented in section 2.1. Web pages are maintained for the WF/PC, HSP, GHRS, FOS, FOC and NICMOS and will be updated to facilitate AR. Assistance may also be obtained from the STScI Help Desk.

 

D.1 Wide Field and Planetary Camera (WF/PC)

The WF/PC had two configurations; in both, the FOV was covered by a mosaic of four charge-coupled devices (CCDs). Each CCD had 800 - 800 pixels and was sensitive from 1150 to 11,000Å. However, internal contaminants on the camera optics limited normal operation to the range from 2840 to 11,000Å.

In the Wide Field Camera (low-resolution) configuration, the FOV was 2.6' x 2.6', with a pixel size of 0.10". In the Planetary Camera (high-resolution) configuration, the FOV was 1.1' x 1.1', and the pixel size was 0.043". A variety of filters was available. The WF/PC received about 40% of the observing time on HST in Cycles 1 - 3, with a large and diverse range of science observations resulting. All WF/PC data was adversely affected by the existence of spherical aberration. Unique and valuable data exists in the archive, but in terms of photometric accuracy, and especially image quality, data taken with the WFPC2 from Cycle 4 and on is superior.

 

D.2 High Speed Photometer (HSP)

The HSP was designed to take advantage of the lack of atmospheric scintillation for a telescope in orbit, as well as to provide good ultraviolet performance. Integrations as short as 10ms were possible, over a broad wavelength range (1200 to 8000Å), and polarimetry was also possible. Observations were carried out through aperture diameters of 1.0" with the visual and ultraviolet detectors, and 0.65" with the polarimetry detector.

HSP had a large variety of fixed aperture/filter combinations distributed in the focal plane; selection was accomplished by moving the telescope so as to place the target in the desired aperture behind the desired filter.

The HSP detectors were four image-dissector tubes and one photomultiplier tube. A variety of ultraviolet and visual filters and polarizers was available. The HSP was used for only a relatively small fraction (5%) of HST observing in Cycles 1 - 3; the HSP science program was among the more severely compromised by spherical aberration. Only limited instrument expertise is available at STScI in support of HSP AR. The extremely high speed with which some HSP data was acquired make these still unique for either past, current or planned HST capabilities.

 

D.3 Faint Object Spectrograph (FOS)

The FOS performed low and moderate resolution spectroscopy (R~250 and 1300) in the wavelength range 1150 to 8500Å. A variety of apertures of different sizes and shapes were available which could optimize throughput and spectral or spatial resolution. Ultraviolet linear and circular spectropolarimetric capability was also present.

Two gratings and a prism were available in the low resolution mode and six gratings were available in the R=1300 mode to cover the entire spectral range. The photon-counting detectors were two 512-element Digicons, one which operated from 1150 to 5500 Å (FOS/BLUE), and the other from 1620 to 8500 Å (FOS/RED).

Most FOS data were acquired in accumulation and rapid-readout mode., periodic and image modes were only occasionally employed. Time resolutions as short as 30 msec were feasible. The electron image was magnetically stepped through a programmed pattern during the observations which provided for oversampling, compensation for sensitivity variations along the Digicon array, sky measures, and/or measurement of orthogonally polarized spectra. Normally data were read out in intervals that were short compared to the exposure time.

The FOS received about 20 - 25% of the total HST observing time over Cycles 1 - 6, carrying out a large and diverse range of science topics. Due to the polarimetric and large dynamic range capabilities a substantial fraction of these data will remain unique.

 

D.4 Goddard High Resolution Spectrograph (GHRS)

The GHRS used two, 500-element digicon detectors providing sensitivity from 1100 to 1900Å (Side 1 - solar blind) and 1150 to 3200Å (Side 2). The GHRS provided photon-noise limited data if an observing strategy was undertaken to map out photocathode response irregularities with the FP-SPLIT option. Signal-to-noise ratios of 100 or more were routinely achieved, and upwards of 1000 on occasion.

The GHRS modes include a first order grating covering 1100 to 1900Å at R~2,500 (285Å bandpass), four first order holographic gratings with very low scattered light covering 1150 - 3200Å at R~25,000 (27 - 45Å bandpass), and cross-dispersed echelles at R~80,000 over 1150 - 3200Å (6 - 15Å bandpass).

The GHRS had two apertures: the 2.0" Large Science Aperture, and 0.25" Small Science Aperture; post-COSTAR the aperture projections were reduced to 1.74" and 0.22" respectively. The small aperture projected to one resolution element, thus even pre-COSTAR data taken with this retained the as designed spectral resolution, albeit at reduced throughput.

Some data were acquired at time resolutions as short as 50 milli-seconds in a Rapid Readout mode. Most observations were acquired in accumulation mode which provided for oversampling, compensation for sensitivity variations along the Digicon array, and simultaneous monitoring of detector backgrounds. Routine observations of the on-board Pt-Ne emission line lamp provide data with well calibrated wavelengths.

The GHRS received about 20 - 25% of the total HST observing time over Cycles 1 - 6, with a large and diverse range of high quality science observations resulting. Due to the high signal-to-noise and large dynamic range capabilities in the far ultraviolet, much of this data will remain unique.

 

D.5 Faint Object Camera (FOC)

The FOC was designed to provide high-resolution images of small fields. The FOC consists of two independent optical relays that magnify the input beam by a factor of four (f/96) and two (f/48). A variety of filters, prisms (for slitless spectroscopy), and polarizers could be placed in the optical beam. The f/48 relay also has a longslit spectrograph. The FOC photocathodes limited the wavelength range from 1200 to 6000 Angstroms.

When corrected by COSTAR the field of view and pixel size of the f/96 camera are 7" x 7" (512 x 512 format) and 0.014" x 0.014", respectively; a field of 14" x 14" could be used with the 512 x 1024 pixel format and a rectangular pixel size of 0.028" x 0.014". Without COSTAR in the beam, the corresponding parameters for the f/96 camera are: 11" x 11" field of view in the 512 x 512 format, pixel size 0.0223" x 0.0223" and full-format field of 22" x 22" with 0.0446" x 0.0223" pixels. The corresponding values for the (little used) f/48 camera are twice those of the f/96 camera.

The f/96 camera was the primary FOC imaging workhorse; high voltage instability problems limited the use of the f/48 relay to mainly long-slit spectroscopic data after the installation of COSTAR.

Most of the FOC data in the archive are unique because the spatial resolution of the FOC is greater than that of any current (or planned) HST instrument. Also, the UV sensitivity was significantly higher than WFPC2, but less than STIS, although a larger variety of filters was available. Finally, the polarizers in the f/96 relay have very low instrumental polarization and excellent polarizing efficiencies.

 

D.6 Near Infrared Camera and Multi-Object Spectrometer (NICMOS)

The NICMOS provides HST's only infrared capability. It will not be available in Cycle 8, because the cryogen will have been exhausted well before the cycle begins. NASA is currently investigating the possibility of a mechanical cooler which would restore it to operational status in Cycle 9.

NICMOS has three 256 x 256 pixel cameras covering the spectral range 0.8 microns to 2.6 microns. The short wavelength cutoff is set by the choice of the HgCdTe detector array and the long wavelength cutoff by thermal background generated by HST's warm optics. Cameras 1 and 2 provide diffraction limited sampling at 1 micron and 1.75 microns, respectively, while Camera 3 is designed to obtain images over a relatively large 51" field of view.

Each camera carries 19 independent optical elements providing a wide range of filter options. Cameras 1 and 2 have polarimetric filters. Camera2 has a 0.3 arcsec radius coronographic spot and optimized cold mask. Camera 3 has three separate grisms providing slitless spectroscopy over the full NICMOS wavelength range.

NICMOS was designed to operate with all three cameras simultaneously. The capability was compromised somewhat by the fact that the thermal short which reduced the cryogen lifetime also resulted in deformations in the detector assembly which destroyed the parfocality of the three detectors. Nevertheless, there is a large body of high quality data from all three detectors which is available for archival research.

 

E. Target Naming Conventions

Target names are used to provide unique designations for the targets throughout the proposal. These names will generally also be used in Phase II, in the HST observing schedule, and ultimately to designate targets in the HST data archives. Prospective proposers and Archival researchers will use these names to determine whether HST has observed a particular object. This facility will be most useful if consistent naming conventions are used for targets.

The following convention should be followed in naming targets:

Catalog Name

The preferred order for catalogs to be used for the designation of various classes of objects is provided below. It is arranged in order of decreasing priority. If a target is not contained in these catalogs, then other catalog designations may be used (e.g., IRC or IRAS Catalog numbers, 4U X-ray Catalog designation, Villanova White-Dwarf Catalog number, etc.). The use of positional catalogs (SAO, Boss, GC, AGK3, FK4, etc.) is discouraged. For uncataloged targets, see below.

Stars

1. Henry Draper Catalog number (e.g., HD140283). HDE numbers are discouraged, except in the Magellanic Clouds.

2. Durchmusterung number (BD, CD, or CPD). In the southern hemisphere, adopt the convention of using CD north of -52 and CPD south of that limit (e.g., BD+30D3639, CD-42D14462).

3. General Catalog of Variable Stars designation, if one exists (e.g., RR-LYR, SS-CYG).

 

Star Clusters and Nebulae

1. New General Catalog (NGC) number (e.g., NGC6397, NGC7027).

2. Index Catalog (IC) number (e.g., IC418).

3. For planetary nebulae, the Perek-Kohoutek designation (e.g., PK208+33D1).

4. For H II regions, the Sharpless Catalog number (e.g., S106).

 

Galaxies and Clusters of Galaxies

1. NGC number (e.g., NGC4536).

2. IC number (e.g., IC724).

3. Uppsala Catalog number (e.g., UGC11810).

4. For clusters of galaxies, the Abell Catalog number (e.g., ABELL2029).

 

Quasars and Active Galaxies

The name defined in the compilation by Veron-Cetty and Veron (ESO Report No. 13, 1993) should be used (e.g., 3C273).

 

Uncataloged Targets

Objects that have not been catalogued or named should be assigned one of the following designations:

1. Isolated objects should be designated by a code name (the allowed codes are STAR, NEB,GAL, STAR-CLUS, GAL-CLUS, QSO, SKY, FIELD, and OBJ), followed by a hyphen and the object's J2000 equatorial coordinates, if possible, rounded to minutes of time and minutes of arc (e.g, for an optical binary star at J2000 coordinates alpha = 1**h 34**m 28**s delta = -15 31' 12", the designations would be STAR-0134-1531A and STAR-0134-1531B).

2. Uncataloged objects within star clusters, nebulae, or galaxies should be designated by the name of the parent body followed by a hyphen and a type designation of the object (e.g., for a star cluster within NGC 224, the designation would be NGC224-STARCLUS).

3. Known objects within nebulae or galaxies may also be designated by the name of the parent object followed by a hyphen and an identifier of the target object. The identifier should be brief, but informative (e.g., the jet in NGC 4486 could be designated NGC4486-JET). Other examples are: NGC5139-ROA24, LMC-R136A, ABELL30-CENSTAR, NGC205-NUC.

 

External Calibration Targets

The name of a target that is being observed only as a calibration standard for other observations should be designated by appending the code -CAL to the target name (e.g., BD28D4211-CAL). Internal calibration targets (e.g., WAVE, INTFLAT) and calibrations using the Earth should not be included in the OS, but in Item #13 Description of the Observations of the proposal form.

 

F. Astronomical Symbols Available for Use in the Proposal Templates

 

 

G. Continuous Viewing Zone Tables

The tables in this Appendix will be useful for proposing observations that can take advantage of CVZ observing (see section 14.1). Included are three tables for each of northern and southern declinations for the 12-month period June 01, 1999 - June 01, 2000 (1999.152:01:00:00 - 2000.151:22:00:00):

1. the maximum duration in orbits of any single CVZ window;

Northern Hemisphere PDF or PostScript Files

Southern Hemisphere PDF or PostScript Files

2. the total duration in orbits of all CVZ opportunities for targets at the specified RA and Declination; and

Northern Hemisphere PDF or PostScript Files

Southern Hemisphere PDF or PostScript Files

3. the total number of CVZ windows.

Northern Hemisphere PDF or PostScript Files

Southern Hemisphere PDF or PostScript Files

 

Proposers should be aware that near the "wings" of the CVZ area (i.e., where there is only one CVZ window), the actual availability of CVZ observing will depend in detail on the geometry of the HST orbit during Cycle 8.

 

H. Examples and Blank Worksheets

This Appendix contains example orbit calculations and blank "worksheets" for each instrument, that can be used to help lay out the exposures and overheads needed to calculate the number of orbits required. Detailed instructions for how to make the calculations are provided in section 18. Note that these worksheets are not for submission with the Phase I proposal, but are strictly for your convenience for calculating the number of orbits.

The following Worksheets are available:

 

I. Blank Budget Forms

The following blank forms are provided:

 

J. Education/Public Outreach Proposals

J.1. Scope of Program

The NASA Office of Space Science (OSS) has developed a comprehensive approach for making education at all levels (with a particular emphasis on pre-college education) and the enhancement of public understanding of space science integral parts of all of its missions and research programs. The two key documents that establish the basic policies and guide all OSS Education and Outreach activities are a strategic plan entitled Partners in Education: A Strategy for Integrating Education and Public Outreach Into NASA's Space Science Programs (March 1995) and an implementation plan entitled Implementing the Office of Space Science (OSS) Education/Public Outreach Strategy (October 1996). Both may be obtained either from the World Wide Web (select Education and Public Outreach from the menu on the OSS homepage at http://www.hq.nasa.gov/office/oss/), or from Dr. Jeffrey Rosendhal, Code S, Office of Space Science, NASA Headquarters, Washington, DC 20546-0001, USA.

In accord with these established OSS policies, Principal Investigators on any OSS NASA Research Announcement (NRA) are strongly encouraged to submit an Education/Public Outreach (E/PO) component. Note that the E/PO proposals are solicited only in conjunction with a "parent" research proposal, and the proposed activities should have some degree of intellectual linkage with the objectives of that parent research proposal and/or the science expertise of its Principal Investigator (PI).

In line with these NASA OSS policies, the STScI is announcing the opportunity for successful U.S. General Observers and Archival Researchers to submit E/PO proposals in conjunction with their accepted HST Cycle 8 proposals. Up to $10K per year may be proposed for an E/PO program, and the E/PO proposals will be funded using an amount not to exceed 2% of the currently available HST Cycle 8 GO/AR budget.

E/PO proposals will be due one month after the notification to Proposers, and will be evaluated (see criteria below) by appropriate scientific, education, and outreach personnel. The E/PO proposals will be in an independent review and the results will be provided to the STScI Director for final selection.

In general, the broad evaluation criteria against which a proposed E/PO activity will be considered are:

Note that originality of the proposed effort is not a criterion. Rather, NASA OSS policy seeks assurance that the PI is committed to carrying out a meaningful, effective, credible, and appropriate E/PO activity.

J.2. Assistance for the Preparation of E/PO Proposals

To directly aid space science personnel in identifying and developing high quality E/PO opportunities, and establishing partnerships between the space science and E/PO communities, NASA OSS has established a national space science education/outreach infrastructure. The purpose of this infrastructure is to provide the coordination, background, linkages, and services needed for a vital national, coordinated, long-term E/PO program. Of particular interest to proposers to this NRA are two elements of this system (which is described in more detail in the OSS education/outreach implementation plan referred to above):

  1. Four OSS science theme oriented "E/PO Forums" have been established to help orchestrate and organize in a comprehensive way the education/outreach aspects of OSS space science missions and research programs and provide ready access to relevant E/PO programs and products to both the space science and education communities. See http://origins.stsci.edu/ for the Origins Education Forum information that serves as the host OSS Forum for the HST mission.
  2. Five regional E/PO "Broker/Facilitators" have also been selected to search out and establish high leverage opportunities, arrange alliances between educators and OSS-supported scientists, and help scientists turn results from space science missions and programs into educationally-appropriate activities to be disseminated regionally and nationally.

Prospective proposers are strongly encouraged to make use of these infrastructure resources to help identify suitable E/PO opportunities and arrange appropriate alliances. Points of contact and addresses for all of these E/PO Forums and Broker/Facilitators may be found by opening Education and Public Outreach from the menu of the OSS homepage at http://www.hq.nasa.gov/office/oss/

J.3. Programmatic Information

The guidelines for the preparation and submission of the E/PO component of a research proposal submitted in response to this HST Cycle 8 Call for Proposals are:

Questions about an E/PO program associated with this Call for Proposals may be directed to:

Dr. Anne Kinney
Outreach Science Content Manager
Office of Public Outreach
Space Telescope Science Institute
3700 San Martin Drive
Baltimore, MD 21218
Telephone: (410) 338-4831
 
e-mail: cycle8epo@stsci.edu

Finally, attention is also called to the Initiative to Develop Education through Astronomy and Space Science (IDEAS) program administered by the Space Telescope Science Institute on behalf of OSS. This program, which currently selects proposals yearly, provides awards of up to $10K (with a few up to $40K) to enhance and encourage the participation of space scientists in E/PO activities. Annual solicitations for the IDEAS program are typically released in July with proposals due in October. The IDEAS program is open to any space scientist based in the U.S. regardless of whether or not they hold a research grant from NASA OSS. E-mail inquiries about IDEAS may be directed to: ideas@stsci.edu. The current request for proposals is posted on the Web at http://oposite.stsci.edu/pubinfo/edugroup/ideas.html. Inquiries also may be addressed to:

IDEAS Program
Office of Public Outreach
Space Telescope Science Institute
3700 San Martin Drive
Baltimore, MD 21218

 

K. Acronyms and Abbreviations

AEC Archived Exposures Catalog

AR Archival Research

AURA Association of Universities for Research in Astronomy, Inc.

CADC Canadian Astronomy Data Centre

CCD Charge-Coupled Device

Co-I Co-Investigator

COSTAR Corrective Optics Space Telescope Axial Replacement

CPAR Coordinated Parallel Observation

CS Contact Scientist

CVZ Continuous Viewing Zone

DADS Data Archive and Distribution System

DD Director's Discretionary

DUP Duplicate Observation

ESA European Space Agency

E/PO Education/Public Outreach

FGS Fine Guidance Sensor

FITS Flexible Image Transport System

FOC Faint Object Camera

FOV Field of View

FOS Faint Object Spectrograph

FTP File Transport Protocol

FUV Far Ultraviolet

GHRS Goddard High Resolution Spectrograph

GO General Observer

GS Guide Star

GSC Guide Star Catalog

GSFC Goddard Space Flight Center

GSSS Guide Star Selection System

GTO Guaranteed Time Observer

HSP High Speed Photometer

HST Hubble Space Telescope

IDC Indirect Cost

IDEAS Initiative to Develop Education through Astronomy and Space Science

IRAF Image Reduction and Analysis Facility

LRF Linear Ramp Filters

MAMA Multi-Anode, Microchannel Array

MT Moving Target

NASA National Aeronautics and Space Administration

NED NASA/IPAC Extragalactic Database

NICMOS Near Infrared Camera and Multi-Object Spectrometer

NOAO National Optical Astronomy Observatories

NUV Near Ultraviolet

OPUS Observation Support/Post-Observation Data Processing Unified System

OS Observation Summary

OTA Optical Telescope Assembly

PC Program Coordinator

PCS Pointing Control System

PI Principal Investigator

PPAR Pure Parallel Observation

PRESTO Project to Re-Engineer Space Telescope Observing

PSF Point-Spread Function

RPS2 Remote Proposal Submission (2nd generation)

SAA South Atlantic Anomaly

SHD Shadow Time

SI Scientific Instrument

SIMBAD Set of Identifications, Measurements, and Bibliography for Astronomical Data

SM2 Second HST Servicing Mission, carried out in February 1997

SM3 Third HST Servicing Mission, scheduled for May 2000

SPSO Science Program Selection Office

SSM Support Systems Module

ST-ECF European Coordinating Facility for Space Telescope

STAC Space Telescope Advisory Committee

STOCC Space Telescope Operations Control Center

STIS Space Telescope Imaging Spectrograph

STScI Space Telescope Science Institute

STSDAS Space Telescope Science Data Analysis Software

TAC Telescope Allocation Committee

TDRSS Tracking and Data Relay Satellite System

TOO Target of Opportunity

URL Universal Resource Locator

WFC Wide Field Camera

WF/PC Wide Field and Planetary Camera (1)

WFPC2 Wide Field Planetary Camera 2

WWW World Wide Web