PART III: PHASE I INSTRUCTIONS

16. How to Submit A Phase I HST Proposal

16.1 Paper and Electronic Proposal Submission

There are three options for preparing and submitting proposals:

• Submission of an electronic proposal (filled-in LaTeX template) file and PostScript file. This is an option for observing proposals only. The submission deadline is September 13, 1996.
• Submission of an electronic proposal (filled-in LaTeX template) file and two paper copies with the same September 13, 1996 submission deadline. This is the only option offered for Archival Research proposals.
• Submission of a paper proposal only. This is allowed only for the small number of observing proposers without access to electronic mail, and the deadline is September 6, 1996.

It is the responsibility of applicants to mail their proposals early enough to assure arrival at STScI by the appropriate deadline. We also urge applicants to submit their electronic versions well before the deadline, to avoid possible last-minute hardware or overloading problems.

Fully Electronic Proposal Submission

For Cycle 7 STScI is encouraging a fully electronic submission. In this mode of submission, the proposer sends via electronic mail both the filled-in LaTeX proposal template AND the PostScript file output from LaTeX (which can incorporate any desired monochrome figures as encapsulated PostScript). For large PostScript files, an ftp area is available. For PostScript submissions, a separate acknowledgment will be sent upon successful printing of the file. This fully electronic submission would be in lieu of any paper submission. This mode does not apply to Archival Research proposals, for which signed budget forms are required.

Small (< 30 orbits) observing, and Snapshot proposals should be no longer than 10 pages, medium (30-99 orbits) observing proposals should not exceed 12 pages, and Major Program proposals (. 100 orbits) should not exceed 17 pages. Panel reviewers may ignore any pages beyond these limits.

Paper-plus-Electronic Submission

Under this option, observing and 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. Archival Research proposals should not exceed 10 pages.

U.S. proposers who are requesting funding for Archival Research should also include the following:

• Budget Forms GF-97-1 through GF-97-3 (attached to both copies of the proposal), with required institutional signatures.

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.

Student Principal Investigators (PIs) should enclose one copy of the

• Certification letter from faculty advisor, as described in §5.2.

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 §17.2). 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.

Paper-only Submission

If access to electronic mail is not available to a proposer, then it is permissible to submit the Phase I information to STScI solely on the paper forms. Explanation for this mode of submission should be provided in a cover letter. Note that the submission deadline for paper-only proposals is one week earlier than for paper-plus-electronic submissions, in order to reflect the significant additional STScI processing effort.

Where to Submit Proposals

Paper forms should be sent to the following address:

Science Program Selection Office

Space Telescope Science Institute

3700 San Martin Dr.

Baltimore, MD 21218 USA

The electronic version of the Proposal Template file (and optional postcript file) should be sent via e-mail directly to one of the following proposal-submission electronic mail addresses:

INTERNET: newprop@stsci.edu

NSI/DECnet: STSCIC::NEWPROP

Proposers will receive an acknowledgement of their e-mail transmission immediately after it is received at the STScI; if no acknowledgement is received within a few days, proposers should contact the STScI Help Desk. For PostScript submissions, a separate acknowledgment will be sent after printing of the file. Again, if no second acknowledgement is received within a few days, PostScript 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

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 §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":

• the Phase I Observing Proposal Template file obstemplate.tex and the Phase I Archival Research Proposal Template file artemplate.tex,
• the style file phase1.sty and supertabular files,
• an example of a completed observing template file in obsexample.tex,
• a helpful how_to_submit file, describing the template files and what to do with them.

2. Fill out the Template File

Fill out the Phase I Proposal Template file using any text editor on the proposer's local computer. Instructions can be found in the template itself, and in §17. Electronic submission of items 12-17 is optional.

3. Prepare a Paper Copy of the Proposal

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

This is the "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 for electronic submission. Please do not e-mail the PostScript version of the proposal that was produced as output by the LaTeX formatter for this first phase of the submission.

5. Send the Complete Proposal to STScI

There are three options for the "Formatted Submission". You can either send a postscript file via e-mail (5a), a postscript file via ftp (5b), or paper copies of the proposal (5c). Please select ONE of these options. Note that Archival research proposers MUST send paper copies.

5a. PostScript Submission via E-Mail

Send one postscript file, with figures included, to the STScI by e-mail to the account named newprop before the deadline for electronic submission. All figures must be encapsulated into the postscript file (i.e., send only ONE postscript file), and we can only accomodate black and white figures. Please set the formattedsubmission keyword in the LaTeX template to EMAIL.

5b. Postscript Submission via ftp

If your postscript 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 file should be transferred to the STScI via ftp. 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/proposer.html) or contact the STScI Help Desk. Do NOT use our public ftp area for your submission. Please set the formattedsubmission keyword in the LaTeX template to FTP.

5c. Make 2 Paper Copies and Send Them to STScI

Send the paper forms to the STScI before the appropriate deadline for paper or paper-plus-electronic submissions, as appropriate. The STScI will make the requisite copies for the proposal review process. These copies will be standard black and white Xerox copies. Proposers who wish to include glossies or color material must send 20 double-sided paper copies to the STScI. Archival Research proposals must include Budget Forms GF-97-1 through GF-97-3 with each copy of the proposal, and student PIs must include one copy of the certification letter from their faculty advisor. Please set the formattedsubmission keyword in the LaTeX template to PAPER.

17. Instructions for Filling Out HST Observing Proposal Forms

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

• All proposals for HST observations must be submitted on current Cycle 7 versions of the appropriate STScI forms; the forms provided for previous proposal cycles must not be used.
• A detailed budget will be required for General Observers only in Phase II. Budget Forms will be provided to GOs after the review and approval of proposals for Cycle 7.
• All copies must be be legible and in English. For legibility, use no more than 80 characters per line and 50 lines per page, or their equivalent in a 12-point font, if using a word processor with proportional spacing.
• Page limits must be strictly observed. Small (< 30 orbits) and Snapshot proposals are limited to 10 pages total, medium proposals (30-99 orbits) to 12 pages, and Major Program proposals (. 100 orbits) to 17 pages.

17.1 Cycle 7 Observing Proposal

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

• Item #1-Give a concise title for the proposal.
• Item #2-Specify the appropriate proposal category. Valid entries are one (and only one) of the following:

SNAP-Snapshot Survey proposal

• Item #3-Select the appropriate scientific category for the proposed project. Pick one and only one category from the following list:

CATEGORIES

SOLAR SYSTEM

COOL STARS-This category refers to stars with effective temperatures less than about 10.000 K, which are single or have non-interacting companions, and which are at the Main Sequence or later in their evolution.

HOT STARS AND STELLAR CORPSES-This category refers to stars which spend a significant fraction of their observable lives at an effective temperature of about 10,000 K, such as neutron stars, white dwarfs, Wolf-Rayet stars, luminous blue variables, and blue stragglers.

BINARY STARS-This category is appropriate when the interaction between stars is their most important defining characteristic.

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., T Tauri stars, FU Orionis stars) rather than dynamical effects on surrounding material (e.g., HH Objects).

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

INTERSTELLAR MATTER-This category includes the general properties of the Galactic interstellar medium; for example, diffuse gas observed in emission or absorption, dust, atomic or molecular clouds, or ionized gas in HII regions.

STELLAR POPULATIONS-This category refers to resolved stellar populations. For example, it includes luminosity functions or color-magnitude diagrams of stellar systems in the Milky Way Galaxy-open clusters, globular clusters, halo, disk, or bulge-or in nearby galaxies.

GALAXIES-This category includes galaxies in the Hubble sequence, starburst galaxies, IR-bright galaxies, dwarf galaxies, and low-surface-brightness galaxies, as well as extragalactic interstellar media and unresolved stellar populations within such galaxies. It does not include studies of gas in external galaxies through QSO absorption lines.

CLUSTERS OF GALAXIES-This category includes groups and clusters at all redshifts, and encompasses dynamical studies, cooling flows, evolution, and gravitational lensing by clusters.

AGN/QUASARS-This category includes active galactic nuclei, excluding starburst phenomena where the activity in the nucleus is insignificant.

QUASAR ABSORPTION LINES-This category addresses the physical properties and evolution of absorption line systems detected along the line of sight to quasars.

COSMOLOGY-This category addresses the universe as a whole, including measurement of cosmological parameters, peculiar velocity studies, surveys for distant objects, evolution of galaxies, and evolution of the universe.

• Item #4-Select minimum one, maximum five, Keywords that describe the scientific goal(s) of the proposal. Keywords must be taken from the list below.

KEYWORDS

• Item #5-Identify the mode of submission for the formatted proposal (PAPER, EMAIL, or FTP).
• Item #6-Enter the name, institutional affiliation, complete address, telephone, electronic mail, and ESA member-state affiliation (if appropriate) of the PI. There must be one and only one PI for each proposal.
• Item #7-Identify which Scientific Instrument(s) (SIs) will be used in the project. The allowable choices are one or more of the following: WFPC2, FOC, STIS, NICMOS, and FGS.
• Item #8-In the case of GO observing proposals, enter the total number of orbits requested for both primary and parallel observations. The values must be calculated as described in §18. For long-term projects, provide a year-by-year breakdown of the orbits requested. For SNAP observing proposals, the proposer should specify the total number of targets requested. Only a fraction of the sample targets may actually be observed.
• Item #9-Provide a concise abstract describing the proposed observations. The abstract must fit on the first page of the printed proposal: typically this will be no more than 20 lines, 80 characters per line. Include the main scientific goals and justify the necessity of HST data.
• Item #10-List the names, institutional affiliations, and countries of all Co-Is. Also indicate whether each Co-I is affiliated with the European Space Agency or with an ESA member-state institution.
• Item #11-Observation Summary (OS)

-For Long-Term Programs (see §3.1.3), include only visits requested for Cycle 7.

-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 #13- 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.

-For each row of the observation summary, the following information must be provided:

1. TARGET NAME

Targets should be named using the conventions recommended in Appendix F.

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 Scientific Instruments typically 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 STScI Guide Star Selection System Astrometric Support Package (GASP) 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 of the Scientific Instruments have limits on the brightness of the objects that they can observe safely. For more information, refer to §13.7 and the Instruments Handbooks.

4. Scientific Instrument Configuration and Operating Mode

Enter the Scientific Instrument configuration first, and then the operating mode. All of the allowable options can be found in the Instrument Handbooks.

5. SPECTRAL ELEMENT(S) (AND

RANGE IF STIS)

All of the desired spectral element(s) (i.e., filters or gratings) should be entered (see the Instrument Handbooks for the allowable options). Several different spectral elements for different exposures may be included on the same OS exposure line, each separated with a comma and a space (e.g., F120M, F220W, F320W). If more than one element is required for the same exposure, then join the elements with a "+" (e.g., F277M+POL45). If the STIS is used, then list in parentheses (immediately following the spectral element listing) the total wavelength range in angstroms for the exposures defined on the given line; for example: (1100-1400).

6. 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 §18).

7. SPECIAL REQUIREMENT FLAGS

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

• Item #12-Scientific Justification

Program Size Total Number of Orbits Maximum Length

Small < 30 orbits 3 pages

Medium 30-99 orbits 5 pages

Major . 100 orbits 10 pages

SNAP 3 pages

Up to two additional (optional) pages for figures, references, or tables are allowed. For long-term proposals, the total number of orbits refers to all cycles combined.

For the individual items below (#13-17) there are no specific page limits; however, the total proposal page limits (given at the beginning of this section) must be observed.

• Item #13-Description of the Observations

• Item #14-Special Requirements

• Item #15-Supporting/Coordinated Observations

• Item #16-Previous HST Programs

• Item #17-Justify Duplications

18. How to Calculate Orbits for Observing Proposals

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:

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 large (> 55) changes in spacecraft roll orientation. These generally force the usage of different guide star pairs, and are therefore treated as separate visits.

4. A change in instrument (e.g., FOC/96 to STIS), except that coordinated primary and parallel observations are contained within the same visit. The switching of 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 (8 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 8 orbits must be broken into separate smaller visits, each with their own guide star and target acquisitions. If you feel that this does not apply to your program, please contact the STScI Help Desk. 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 7 below, which gives the visibility period as a function of target declination; values are also provided for moving targets, and for observations requiring shadow, 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 7). 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 7 when computing the required number of orbits. Do not enter a flag on the Observation Summary 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 shadow time 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 shadow time window (see the WFPC2 example in Appendix K).

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 Observation Summary 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 §§6.4, 14.1). If you can utilize CVZ time for your observations, then the visibility period is 96 minutes per orbit for 8 orbits, beyond which time SAA interference will limit the visibility to 75 minutes per orbit for the next 8 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 during CVZ observations. It may also 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, BETWEEN, or PHASE restrictions should therefore adopt the non-CVZ target visibility period for resource estimation. Also note that there are other limitations (e.g., data volume) that may affect CVZ availability.

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 §6.4 for a detailed discussion of CVZ related policies.

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 K, 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 NICMOS-Camera 3 SNAPs, see below), a guide-star acquisition is required, which takes 9 minutes. At the beginning of subsequent orbits in a multi-orbit visit, a shorter guide-star re-acquisition is required, which takes 6 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 NICMOS-Camera 3 (in a Snapshot proposal) and wish to utilize the gyro guiding mode (see §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, FOC: For the FGS, observations are done following a standard Spiral Search location sequence. Most WFPC2 and FOC 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 §15.2.2 and the Instrument Handbooks). Note that there are no additional overheads for the FOC bright target acquisition procedure.

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 arcseconds. For science observations taken through spectroscopic slits which are less than 3 arcseconds 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. On-board target acquisitions with STIS differ considerably from previous HST instruments such as FOS and GHRS, which required raster scans to locate the 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. This should make STIS target acquisitions more robust than with the earlier generation HST spectrographs.

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 0.1 arseconds. A typical STIS target acquisition exposure takes 8 minutes.

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 or equal to 0.2 arcseconds wide (or tall). Peakup exposures use a science slit or coronagraphic aperture and can be taken with either the CCD or one of the MAMAs as the detector and with either a mirror or a spectroscopic element in the grating wheel. Typical centering accuracies following a peakup sequence are 0.3 and 0.2 times the dimension of the slit or bar for CCD and MAMA acq/peaks, respectively. Typical STIS imaging point source peakups take ~5-10 minutes, though a peakup with the very small 0.1 x 0.09 echelle aperture will take ~20 minutes. See Chapter 8 of the STIS Instrument Handbook for more details.

NICMOS: Most of the NICMOS observations do not require a target acquisition. However, some care should be taken in specifying coordinates for observations with the NICMOS Camera 1, which has a Field of View of only 11" x 11". For observations requiring positioning of the target to an accuracy of better than 1-2", the same requirements as for WFPC2 and FOC apply.

For coronography (NICMOS Camera 2), an on-board acquisition is performed to place the target under the coronographic spot. Once the target is in the Field of View of Camera 2, the on-board software determines the position of the brightest pixel, calculates the offset between that pixel and the coronographic spot, and moves the target under the spot. The overhead required for this process is 98 seconds.

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.

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 parts-the exposure time and the instrument overhead. The exposure times were determined in Step 1, while the instrument overheads are given in Table 3 below (and on the worksheets) for each instrument operating mode.

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 when mapping out your observations, although one overhead time is required (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. Note that many short WFPC2 exposures in one orbit can overload the data paths. No more than 14 exposures per orbit are allowed.

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.

FOC: FOC exposures cannot be paused across orbits.

STIS: Some differences will be found between the overhead times presented here in Table 8 and those discussed in §9 of the STIS Instrument Handbook. While both times are based on the same preliminary data, the times presented here are a simplified, slightly more conservative version of those presented in the handbook. Our primary goal here is to ensure that you are requesting sufficient orbits for your observations. The STIS sample worksheets found in Appendix K, use the simplified method presented here in the Call for Proposals on the same examples described in §9 of the STIS Instrument Handbook.

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're 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.

NICMOS: The instrument set-up at the beginning of an orbit, each filter change, change of Camera (e.g., from 1 to 3), and dithering/chopping, involve additional overheads (see Chapter 8 of the NICMOS Instrument Handbook). For instance, the instrument set-up at the beginning of an orbit needs 12 seconds, and filter changes need 12 seconds. The overheads for Camera changes depend on the starting and ending Camera: the overhead is 102 seconds from Camera 2 to 3 (and vice versa), 55 seconds from 1 to 2, and 70 seconds from 1 to 3. Many detailed examples are presented in the NICMOS Instrument Handbook (Chapter 8) to help the proposer through these numbers. NICMOS observations cannot be paused across orbits. The overhead on the ACCUM mode is a function of the number of reads, NREAD, obtained at the beginning (and at the end) of an exposure. The range of allowed NREADs is 1 (default) to 25. The two available readout modes, FAST and SLOW, are explained in detail in the NICMOS Instrument Handbook. The overhead on the BRIGHTOBJ mode is a function of the exposure time. The ACQuisition mode is available for Camera 2 only, and, specifically, for acquiring targets under the coronographic spot.

FGS: FGS observations cannot be paused across orbits.

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 1¢-2¢, 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:

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 [(4-1) 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.

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

, 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 §3.2) will most likely take less than one orbit per observation. Proposers should make certain that each of their exposures (with overheads) requires ¸ 1visibility 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 Archival Research proposals for cases where funding is requested. See §5.3 for a discussion of the HST Archival Research Program, and refer to Appendix H for instructions on how to access the HST Archive using StarView. Consult 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 World-Wide Web at http://www.stsci.edu/archive.html.

Researchers proposing an Archival Research program that will also utilize data from other NASA centers should submit their AR proposals to the STScI if the majority of the program involves HST archival data and its analysis. Conversely, requests for support of Archival Research programs utilizing data primarily from other missions should follow the guidelines in the appropriate NASA Research Announcements.

19.2 How to Fill Out Archival Research Templates

Archival Research proposals (that request funding) should be submitted using the Cycle 7 Phase I Archival Research Proposal Template and budget forms. The scientific justification for AR proposals must be no more than 3 pages in length. Two additional pages for figures, references, and tables are also allowed. Specific instructions for filling out various items in the AR proposal form are given in this section and in the LaTeX template.

• Item #1-Give a concise title for the proposal.
• Item #2-Select the appropriate scientific category for the proposed project.
• Item #3-Enter the name, institutional affiliation, complete address, telephone, electronic mail, and ESA affiliation (if appropriate) of the PI. There must be one and only one PI for each proposal.
• Item #4-Enter the total funds (in U.S. dollars) that are requested.
• Item #5-Provide a concise abstract describing the proposed observations.
• Item #6-List the names, institutional affiliations, and countries of all Co-Is. Also indicate whether each Co-I is affiliated with the European Space Agency or with an ESA member-state institution.
• Item #7-Enter the requested information of an authorizing official of the institution assuming responsibility for the project. The authorizing official should sign and date the paper copy of the Cover Page.
• Item #8-Scientific Justification-Present the scientific justification for the proposed archival program. Do not exceed 3 pages plus an additional two pages for figures, references, and tables.
• Item #9-Description of Archival Program-Provide a generic description of the requested data, and specify the number of exposures requested from the archive.
• Item #10-Related, Funded Archival Research-If you or your Co-Investigators have received any funding for HST Archival Research which is related to this proposal, list the HST program IDs, PIs, and titles, and briefly summarize their main results. If this proposal is related to any other Cycle 7 proposals, describe how so.
• Include Budget Forms GF-97-1 through GF-97-3.

19.3 Budget Forms

STScI may provide financial support to U.S. observers and Archival Researchers, subject to availability of funds from NASA. For information concerning the allowability of costs and funding procedures, see §5.3.

Archival Researchers must indicate the need for funding on the Proposal Cover Page. Budget Forms GF-97-1 through GF-97-3 are required only for Archival Research Proposals. The instructions for filling out the Budget Forms are included on the back of the forms in Appendix L. A copy of the forms should be attached to both copies of the proposal. The forms are available in LaTeX format as well as in Lotus and Excel formats on STEIS.

Specific questions concerning the allowability of costs or the preparation of the budget should be directed to the Grants Administration Branch (410-338-4200).

APPENDICES

A. STScI, ST-ECF, and CADC Contacts

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, PRESTO Glenn Miller miller@stsci.edu 4738

Science Program Selection Office

Head Meg Urry cmu@stsci.edu 4593

Technical Manager Brett Blacker blacker@stsci.edu 1281

Science Support Division

Head Knox Long long@stsci.edu 4862

Grants Administration Branch

Chief Ray Beaser beaser@stsci.edu 4203

Data Systems Division

Archive Hotseat archive@stsci.edu 4547

Miscellaneous

Main switchboard/receptionist 4700

Fax 4767

Space Telescope European Coordinating Facility

The Space Telescope European Coordinating Facility (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-Str. 2

D-85748 Garching bei MÝnchen

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. STScI Electronic Information Service (STEIS)

STEIS is the electronic information system for HST users. This service provides access to a wide variety of HST-related information, including the latest updates on mission schedules and status, spacecraft and instrument performance, proposal deadlines, and data-analysis software (including updates and bug fixes).

There are two ways to access the information provided by STEIS to the Internet. The easier is via the World-Wide Web (WWW) using a graphical browser like Netscape, Mosaic, or Microsoft Internet Explorer, or a text-only browser like Lynx (from the University of Kansas). The URL (Universal Resource Locator) for the STEIS "home page" is:

http://www.stsci.edu/

From this page you can follow links to items of interest, including documentation updates and last-minute news.

Another way to access information on STEIS is via the anonymous file transfer protocol (FTP) mechanism. This method may be more suitable if you have a slow Internet connection. Connect to the STScI server machine (ftp.stsci.edu) to browse and retrieve files of interest. Items of particular interest to proposers can be found in the "proposers" subdirectory. Be sure to retrieve the file "how_to_submit". You may also contact the STScI Help Desk for assistance or for a copy of The STEIS Guide.

If you have any problems connecting to the STScI system, then please consult your local system administrator or network expert, or contact the STScI Help Desk. Please also forward comments or suggestions regarding this service to the STScI Help Desk. For more information on STEIS, please refer to The STEIS Guide.

C. Funding Policies

C.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.

C.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 its 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 $1000), including computers or related hardware, will be approved in special circumstances, and a detailed justification must be provided in the proposal. 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. It is expected that, in most instances, the recipient organization will provide at least half of the purchase price of any item costing over $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 L for additional information on allowable costs.

C.3 Budget Submission

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

C.4 Preparatory Funding

General Observers may request early funding of their programs if necessary to prepare for the receipt of HST data. Proposers may request up to 10% of the funds for their programs to be awarded prior to the start of the Cycle 7 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.

C.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. Such programs require an annual continuation proposal, as described in §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.

C.6 Award of Funds

Shortly before the start of Cycle 7, 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 7. Additional funding up to the approved funding allocation will be awarded after the receipt of observational data for each GO program.

C.7 Educational Supplements

Funded HST proposers are invited to apply to the Initiative to Develop Education through Astronomy (IDEA) program, which is sponsored and funded by NASA Headquarters. This program typically provides a modest supplement ($6,000) to existing NASA Astrophysics or STScI grants in order to enhance the participation of research astronomers in pre-collegiate or public outreach activities. All current Principal Investigators funded through the NASA Astrophysics Division or STScI are eligible to apply for an IDEA award. For more information, contact Carole Rest, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, or send e-mail to idea@stsci.edu.

D. Scientific Instruments Retired by End of Cycle 6

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 11,000 å. However, internal contaminants on the camera optics limited normal operation to the range from 2840 to 11,000 å.

In the Wide Field Camera (low-resolution) configuration, the FOV was 2¢.6 ¥ 2¢.6, with a pixel size of 0,.10. In the Planetary Camera (high-resolution) configuration, the FOV was 1¢.1 ¥ 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 10 ms were possible, over a broad wavelength range (1200 to 8000 å), 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 Archival Research. 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 8500 å. 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 R = 250 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).

The FOS acquired data in accumulation, rapid-readout, periodic, and image modes. 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. with a large and diverse range of high quality science observations resulting. 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 1900 å (Side 1-solar blind) and 1150 to 3200 å (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 1100-1900 å at R ~ 2,500 (285 å bandpass), four first order holographic gratings with very low scattered light covering 1150-3200 å at R ~ 25,000 (27-45 å bandpass), and cross-dispersed echelles at R ~80,000 over 1150-3200 å (6-15 å 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.

E. Instrument Handbook Changes

For each HST observing Cycle the Instrument Handbooks for all active science instruments will be updated and released. Since new versions of the Instrument Handbooks are mailed to individuals only upon request, we provide here a discussion of the changes made in the most recent version. The Instrument Handbooks themselves are also available via our Web server (see §2.2).

WFPC2 Instrument Handbook, v. 4.0, June 1996

The primary revisions to this version of the WFPC2 Instrument Handbook may be summarized as follows:

Observation Strategies: A new chapter (H§7) has been added specifically to assist observers in preparing Phase II proposals. Sections include: Observation of Faint Targets, Observation of Bright Targets, Observation of Faint Targets Near Bright Objects, Dithering Observations, Selecting Field-of-View Orientation, Polarization Observations, and Ramp Filter Observations.

Exposure Time Estimation: H§6 has been completely re-written. New material includes equations and shortcuts for signal-to-noise ratio (SNR) and exposure time calculation for point sources (both with PSF fitting and aperture photometry) and extended sources. A new Appendix gives representative SNR values for various exposures of stellar, power law, and emission line sources.

CCD Performance: Material on dark current and CTE (charge transfer error) has been updated.

Calibration: Material on UV throughput, dark current calibration, flat fielding, and impact of focus variations on photometry has been updated.

Other changes include addition of an index and acronym list.

FOC Instrument Handbook, v. 7.0, June 1996

The FOC Instrument Handbook contains new information in the following areas:

a. F/48 performance and availability. Problems with the F/48 kept it from being used in the previous cycles, however, recent tests have shown that the situation is improving so that the detector can be reliably used for science. As a result, the F/48 relay will be available AGAIN ONLY for long-slit spectroscopy in Cycle 7. The latest information describing the recent performance of the F/48 can be found in the new H§6.13.

b. Calibration accuracies. The results of the calibration activities have always been implicitly incorporated into each previous version of the handbook, however, a separate chapter (H§11) describes in more detail the present calibration program (H§11.1), along with the accuracy of the current calibrations (H§11.2). Chapter 11 also contains details on the current F/48 long slit calibration plan and expected accuracies.

c. Updated calibrations of the objective prisms. The dispersion curves for the F/96 objective prisms have been re-calibrated and the results are given in Table 5. In addition, analysis techniques and spectrophotometry accuracies are now provided in a new section (H§6.13).

d. Updated information on the performances of the Neutral Density filters. The in-flight transmission properties of the five neutral density filters available in the F/96 camera have been calibrated for the first time in Cycle 5, at optical and UV wavelengths. Details are contained in H§4.4.3.

e. New calibration of filter shifts. Most F/96 filters produce image shifts which can be as large as several pixels. These shifts have now been calibrated and the details are provided in H§4.4.3.

f. Updated information on FOC simulators. The FOC Instrument Handbook has always contained a chapter describing the software package FOCSIM, which was primarily accessible only through an account at the Institute. This chapter has been enhanced to describe the new software that has been added to determine the orientation of an FOC image on the sky. This software can be used either when planning an observation requiring a special orientation, or to determine the orientation of an image already obtained.

There are many other less significant changes throughout the handbook as well, but primarily they only served to update what was already present in earlier versions, rather than adding anything new.

FGS Instrument Handbook, v. 6.0, June 1996

The current new version of the handbook has been arranged in the following sections:

-instrument description

-instrument operation

-instrument performance

-instrument calibrations

-writing proposals

-data reduction

The section on instrument description has been expanded to include a more detailed discussion of the individual elements of the optical train of the FGS as well as the detailed workings of the Koesters prism interferometer.

The instrument calibration section has been updated to include some calibration data from Cycle 5.

The section on writing proposals has been expanded to include general guidelines and recommendations regarding observing strategies, exposure times, and Phase II special requirements and optional parameters.

The section regarding data reduction has been updated and includes references to the HST Data Handbook.

F. 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:

• Each time a distinct telescope pointing is requested, a new target name should be defined. For example, for several pointings within a galaxy, one might define target names like NGC4486-NUC, NGC4486-JET, NGC4486-POS1, and NGC4486-POS2.

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 -525 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).

Uncatalogued 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 a = 1**h 34**m 28**s d = -15531'12", the designations would be STAR-0134-1531A and STAR-0134-1531B).

2. Uncatalogued 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.

G. Astronomical Symbols Available for Use

in the Proposal Templates

H. Starview Duplication and Archival Searches

The simplest and most robust way to determine whether your proposed observations conflict with previously accepted GO or GTO observing programs is to use StarView, the interface to the HST archive. Within StarView users will find a Duplication Check Screen which they can use to perform RA and Dec based or target name based searches of all planned or completed HST observations. Searching by RA and Dec is the only reliable way to find duplications of fixed target observations. Target names do not fit a fixed standard, and can vary from proposal to proposal. Solar system observations should be found by target name, imbedded in asterisks, e.g., *Mars*. Data browsing (display of images and plotting of spectra) is available for all public HST data in the archive. Archival proposers will also find the Duplication Check screen useful for preparing their archival proposals.

StarView is a software package that can be installed on your computer. However, StarView can also be accessed via telnet to one of the two archive host computers, archive.stsci.edu (unix) or stdata.stsci.edu (VMS). If you are not a registered archive user, log in with username guest and password archive. You do not need to register as an archive user to do duplication checking or to browse the data. You need to register as an archival user only if you wish to retrieve public HST data. For those who wish to retrieve data, registration is a simple process- just type register from the command line on one of the host computers.

To begin simply type xstarview to fire up the xwindows based version of StarView (if StarView is not able to create the window on your screen you should contact your local System Manager to have necessary permissions set), or type starview to use crt StarView. While there is extensive help available within StarView (via the Strategy button and the pull down Help menu), xstarview is fairly intuitive. When StarView starts up, it places you in the Welcome Screen. Select the <Duplication Check> button from the bottom (command) portion of the screen, by clicking with the mouse on the xversion or entering Esc-2 on the crt version. This will place you in the "Duplication Check Search" screen. To search for observations of a specific fixed target, enter the RA and Dec in J2000 coordinates of the target and a search radius. If you know only the name of your fixed target, but not the coordinates, select the <Get Coordinates> button and enter your source name; the software will then connect to the SIMBAD (Set of Identifications, Measurements, and Bibliography for Astronomical Data) database or the NED (NASA Extragalactic Database) to determine the coordinates of your source. To search for observations of moving targets, specify the target name embedded between asterisks (e.g., *JUPITER*) in the target name field on the "Duplication Check Search" screen. You can also enter specifications in any of the other fields to further constrain your search. When you are ready, select <BEGIN SEARCH> from the command area. (Note: The duplication checking screen allows you to check targets one at a time or to cross correlate a list of target RA and Decs against the catalog all at once. You can employ the latter capability by selecting the <Cross Correlation> button from the command area of the "Duplication Check Search" screen. More information about the cross correlation capability is provided as part of the Strategy for the "Duplication Check" screen).

If a planned or completed HST observation is found which matches your search criteria, the screen will change to the "Duplication Check Results" screen where more detailed information about the matching observation will be displayed. You can step through matching observations one at a time by using the <Step Forward> button, or you can use the <View Result as Table> button to display the information in tabular form and step through the matching observations a page at a time. Completed observations (i.e., those having exposure status = "completed") which are public (with release dates less than the current date) can be previewed using the <Preview> button.

The duplication checking screen is designed only to identify potential conflicts; you will have to decide whether the apparent conflicts are "real". The formal duplication policy is described in §6.1. Proposed observations which duplicate any existing or planned observations must be justified in the Proposal. In particular proposed observations which conflict with GTO Cycle 7 targets, which are not specifically endorsed by the TAC, will be disallowed or restricted during Phase II checking. Planned exposures of GTO Cycle 7 targets are identified by conflict type = "GTO" and exposure status = "planned - cycle 7".

Abstracts of all proposals which have been approved for observation (including both executed and pending proposals) can be displayed using the "Abstracts" screen in StarView. This screen can be accessed via the <Other Searches> button on the "Welcome Screen" of StarView or by pulling down the "Searches" menu, in the menu bar on the top of the screen. The "Abstracts" screen is listed in the "Observation/Proposal Searches" submenu, as part of the "Archive Searches" menu. Enter the proposal id of the proposal whose abstract you wish to view, or qualify on proposal title to search for proposals of a particular type of object (e.g., type *SEYFERTS* in the title field). Push <BEGIN SEARCH> when you are ready. To find observations of a particular class of object you can also use the "General Screen" and qualify on the target description field in this same way.

More information about StarView and the HST Archive is provided in the Archive Primer. For help, documentation, or information about any aspect of the HST Archive, contact the archive hotseat (e-mail archive@stsci.edu or phone 410-338-4547).

I. Space Telescope Advisory Committee

In light of these considerations, the STAC recommended for Cycle 7:

• A strong emphasis on a new category of Major Programs, defined as 100 or more orbits per Cycle.
• A re-definition of long-term status to allow multi-cycle proposals that are not subject to scientific review by multiple TACs.
• Opportunities for new kinds of surveys, particularly when reduced proprietary periods are proposed.
• Renewed attention to proposals that expand discovery space and enhance HST's chance of producing front-line discoveries, even at the risk of a null result.

These recommendations have been incorporated into this Call for Proposals. Additional details of the STAC deliberations, including the STAC report, can be found through the STScI Web page or the STScI Newsletter.

J. Continuous Viewing Zone Tables

The tables in this Appendix will be useful for proposing observations that can take advantage of Continuous Viewing Zone (CVZ) observing (see §14.1). Included are three tables for each of northern and southern declinations for a six-month sample period:

1. the maximum duration in orbits of any single CVZ interval, and

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

3. the total number of CVZ intervals.

The sample period for these tables was taken to be July 1997 through June 1998. Proposers should be aware that near the "wings" of the CVZ area (i.e., where there is only one CVZ interval), the actual availability of CVZ observing will depend in detail on the geometry of the HST orbit during Cycle 7.

(Tables are attached on the following pages, pp. 77-82.)

K. 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 §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.

(Worksheets are attached AFTER the CVZ tables, pp. 83-100.)

L. Blank Budget Forms

The following blank forms are provided:

• Budget Forms GF-97-1, GF-97-2, and GF-97-3 (to be completed in Phase I by U.S. Archival Researchers only). Please see the attached Budget Guidelines.

(Forms are attached AFTER the worksheets, pp. 102-107.)

M. Acronyms and Abbreviations

AR Archival Research

AURA Association of Universities for Research in Astronomy, Inc.

CADC Canadian Astronomy Data Centre

CCD Charge-Coupled Device

CDB Calibration Data Base

Co-I Co-Investigator

COSTAR Corrective Optics Space Telescope Axial Replacement

CVZ Continuous Viewing Zone

DADS Data Archive and Distribution System

DD Director's Discretionary

DUP Duplicate Observation

ESA European Space Agency

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

GASP GSSS Astrometric Support Package

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

IDEA Initiative to Develop Education through Astronomy

IDT Image Dissector Tube

IRAF Image Reduction and Analysis Facility

JPL Jet Propulsion Laboratory

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

OA Operations Astronomer

OPUS Observation Support/Post-Observation Data Processing Unified System

OS Observation Summary

OTA Optical Telescope Assembly

PAR Parallel Observation

PC Planetary Camera

PCS Pointing Control System

PI Principal Investigator

PMT Photomultiplier Tube

PRESTO Project to Re-Engineer Space Telescope Observing

PSF Point-Spread Function

RPS2 Remote Proposal Submission 2

SAA South Atlantic Anomaly

SHD Shadow Time

SI Scientific Instrument

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

SMOV Servicing Mission Orbital Verification

SMS Science Mission Specification

SM97 Second HST Servicing Mission, Scheduled for February 1997

SOS Science Operations Specialist

SPSO Science Program Selection Office

SSM Support Systems Module

ST-ECF European Coordinating Facility for Space Telescope

STAC Space Telescope Advisory Committee

STEIS Space Telescope Electronic Information Service

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

TDRS Tracking and Data Relay Satellite

TDRSS Tracking and Data Relay Satellite System

TOO Target of Opportunity Observation

TIM Telescope Image Modelling

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