Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.stsci.edu/institute/org/telescopes/Reports/ISR-TEL-2010-02.pdf Äàòà èçìåíåíèÿ: Wed Dec 8 20:28:27 2010 Äàòà èíäåêñèðîâàíèÿ: Fri Feb 11 13:25:56 2011 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: m 31

Instrument Science Report TEL 2010-02

HST Focus in SMOV4: Strategy for OTA adjustment & SI Focus
M. Lallo, R. van der Marel, C. Cox, G. Hartig, S.-M. Niemi Dec 10, 2010

ABSTRACT This report documents in summary the observatory-level effort to produce optimal focus during Servicing Mission Observatory Verification 4 (SMOV4). It describes the extrapolation of monitor data available prior to SMOV4, and the resulting decision to adjust the HST Secondary Mirror +3 µm away from the Primary in concert with the active optical alignment of WFC3 and COS in order to maximize image quality and confocality among the instruments. It also provides the historical HST focus dataset used for such long term focus predictions.

1. Introduction
HST focus has been monitored and adjusted throughout the Observatory's life. The monitoring normally consists of phase retrieval determinations of the amount of defocus present in images taken with one or more Science Instruments (SI). Since deployment, the HST Optical Telescope Assembly (OTA) has shrunk by ~150 µm (3x10-5 of its length). This has resulted in ~25 Secondary Mirror (SM) adjustments away from the Primary Mirror (PM) to maintain the focus to the SIs. On top of this long term trend, operational temperature fluctuations produce focus changes which add "noise" to our estimates of the overall focal length of the OTA, some of which can be modeled (Lallo et al. 2005, DiNino et al. 2008). This long-term shrinkage is ongoing, and upon entering SMOV4, our trending analysis of ACS phase retrieval data indicated a defocus of ­2.5 µm at the SM (1µm @ SM = 6.1nm rms wave front error @ SIs). A negative focus value indicates the SM is too close to the PM. Comparable amounts of defocus (positive or negative) are frequently experienced in normal science operations due to thermal variations, but it was desired to remove any systematic offset during SMOV, in order to pass through Cycle 17 and 18 with the new and existing SIs as close as possible to their best focus.
Copyright© 2010 The Association of Universities for Research in Astronomy, Inc. All Rights Reserved.


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To accomplish this, STScI produced a plan to offset the best-focus position for COS and WFC3 found during their SMOV4 optical alignment by an amount equivalent to the ­2.5 µm estimated amount of defocus at ACS. This would leave the old and new SIs confocal within our errors, but ~ ­2.5 µm out of focus. This activity was followed by a ~ 3.0 µm OTA refocus on 20 July 2009, in order to leave the SIs at an estimated ~ +0.5 µm focus, slightly overshooting best focus, with the intention of passing through zero and evolving slightly negative over the Cycle 17/18 period. For a detailed discussion of subsequent camera focus and confocality estimates, and focus trending over this period see Niemi & Lallo (2010).

2. The Data
The body of HST focus-monitor data spans back to a few months after HST deployment on 24 April 1990. It comprises data from various CCD imaging instruments over the mission life. With some exceptions prior to WFPC2 commissioning in 1994, the data is typically obtained approximately monthly, with multiple exposures taken over some significant fraction of an HST orbit. The targets are normally one or more isolated, bright, non-saturating point sources, observed through filters with central wavelengths between ~0.4 and ~0.8 µm. Proposal numbers for the more recent incarnations of the routine focus monitoring program are CAL/OTA 11877, 11316, 11020, and 10752. From observations such as these, we perform a parametric phase retrieval analysis to recover presumed optical aberrations. See appendix 1 and Niemi & Lallo (2010). The phase retrieval is usually configured to solve for focus, but is also used to fit coma and astigmatism when appropriate to the nature of a particular study. A phase retrieval analysis is performed on each exposure in the visit, often sampling much of an orbit. This has allowed an accurate characterization of the temperature-driven focus changes during HST orbits, and has facilitated the development of a temperature-based focus model (DiNino et al 2008). Using data obtained from the HST engineering telemetry, the model takes temperatures from a number of sensors throughout HST to predict focus. A purely temperature-based model gives some success in explaining short-term focus variations but does not follow long term trends, most or all of which are not thermally driven nor reversible. This requires the addition of a secular function that is obtained by fitting such trends. For the data and analysis discussed here, when we apply the model, we do not include the long term secular component since this is what we are seeking to determine. When used, the model is only applied to data from 2003 onward since this is the time period over which it was developed and fit to observations. For the purpose of OTA focus maintenance, we desire independent (uncorrelated) measurements, so the data is processed to replace the multiple values for each visit with the single mean value for that visit. The resulting data file records mean focus values and corresponding time stamps. Over the duration of our monitoring, we have utilized various cameras so the file contains results from WF/PC-1, WFPC2/PC, ACS/HRC, and ACS/WFC, as well as a small number of STIS imaging observations. Since there are small focus offsets (non-confocality) between the SIs, the data in this file has been processed to express results with respect to best ACS/WFC fo2


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cus. This required adding ­1.0 µm to ACS/HRC data, ­1.4 µm to WFPC2/PC, and +5.7 µm to STIS image data. WF/PC-1 results were used "as-is" since a reliable estimate does not exist for confocality between WF/PC1 and the other imagers. The large offset for STIS is due to STIS focus being optimized at the slit plane which is not confocal with the image plane, and it is this image focus that is measured by phase retrieval as reported here. The resulting file currently contains 363 independent measurements spanning from 1990 to March 2009. It is provided in appendix A3. ACS observations (WFC or HRC) are indicated by a "j" as the first character in the filename. WFPC2 data begins with a "u", WF/PC-1 is identified as "pre94", and in some instances (as well as for STIS) the points are named by the proposal and visit number or other descriptive label. As already described, the HST OTA exhibits a long-term shrinkage, which is periodically corrected by commanding the SM away from the PM. Thus, in order to fit the long term behavior to make predictions used for effective control of the OTA focus, the measured focus values in this file must have accumulated offsets removed in order to reproduce the continuous focus trend rather than observed focus as maintained by periodic OTA refocusing. The history since 1994 of such mirror moves, their amounts and dates can be found at:
http://www.stsci.edu/hst/observatory/focus/mirrormoves.html

A peculiarity in the historical record should be pointed out here; mirror moves prior to 1994 are already captured in our input file. This can be seen in the first 44 rows identified as "pre94" (appendix 3). These values reflect the accumulated defocus up to 1994, rather than the measured values, so do not require piecewise processing to account for mirror moves prior to 1994. This processing of the file is accomplished by simply adding to each measured value the sum of all Secondary Mirror moves that occurred after the date of that observation. This recovers the smooth lifetime behavior whose predictive utility is discussed in the next section. Finally, we maintain ancillary data files where aberrations such as coma and astigmatism are tracked, along with a number of other characteristics and correlations of interest, but for the purpose of OTA focus maintenance and prediction, the focus aberration is of interest, and the simple file reproduced in appendix 3 comprises the basic input.

3. SMOV4 Focus Estimate
Plotting the mission-life focus data, after removing the OTA refocusings, produces a trend, with real focus variations creating "noise" about this otherwise monotonic behavior. In fig. 1 below we see this focus data evaluated prior to SM4. The best fitting double exponential,
Eqn. 1: S = -5.04 + 56.26e­t/364.53 + 106.24e­t/2237.2

(where SM is the change in SM position in microns and t is the number of days since 24 April 1990) produced a reasonable fit to the long-term data up to the cessation of HST science in May 2009 in anticipation of SMOV4 (last points plotted). The overall shrinkage of the HST OTA can be seen as ~150 µm. In practice, we have executed OTA refocusings listed in the provided URL to counteract this trend and maintain focus to typically within ~5 µm maximum at the SM.

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Figure 1: Accumulated defocus of the OTA over the mission lifetime prior to SM4 (April 1990 - April 2009), and the best fitting double exponential.
HST lifetime focus trend

Although the lifetime fit is illuminating for understanding long-term behavior, its rms residuals of 2.7 µm (after focus model correction discussed in sect. 2) is too high to accurately base an OTA refocus determination. Systematic long-term displacements above and below the best fitting curve can be seen in figure 1. Because of this, fits to more recent data are often used when determining the overall OTA focus for the purposes of planning an OTA refocusing. This was the case for determining the SMOV4 focus. We examined only the portion of the focus data taken after the December 2002 OTA refocus. The data spans two OTA refocusings indicated in figure 2 by dotted vertical lines. These focus adjustments of +4.16 µm (22 Dec 2004) and +5.34 µm (31 July 2006) were added back into the observed focus values to produce a continuous dataset. This was then best fit with a single exponential,
Eqn. 2: S = -6.16 + 201.64e­t/1754.4

This fit had rms residuals of 1.7 µm and predicted a focus value of ­2.5 µm for 1 August 2009 (rough date for the intended OTA refocus). A straight line fit had slightly higher rms residuals of 1.8 µm and predicted ­3.4 µm on 1 August. For comparison, the double exponential fit to the lifetime data predicted ­1.5 µm with 2.7 µm rms residuals, clearly underestimating the amount of actual defocus seen in monitoring data for the past 1.5 years. An exponential fit performed without model correcting the data increased the rms residuals to 2.0 µm but did not result

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in a significantly different fit or focus prediction, confirming that the temperature-based focus model was not introducing a systematic offset over the timescale being considered. It is interesting to note that the constant term in both exponential fits given in equations 1 & 2 imply a total future shrinkage of the HST OTA of only another 5 to 6 µm.
Figure 2: Accumulated defocus of the OTA from 2 December 2002 up to and including SMOV data points (identified with red arrows). Data have been model-corrected. Best fitting exponential predicted a focus of ­2.5 microns on 1 August 2009. Best fitting straight line is dashed and included for reference.

The best estimate of ­2.5 µm of defocus at ACS implied an equivalent amount of defocus at the STIS slit plane, since STIS and ACS were both originally focused to be confocal with WFPC2 and thus should remain confocal within the errors to each other. Early SMOV calibration results included a phase retrieval measurement of a STIS CCD OII image, which indicated that, like ACS, the resurrected SI had not seen a noticeable focus change since the last time it was operational. After correcting by the 5.7 µm to express this measurement at the STIS slit focus (see sect. 2), this point was seen to be slightly more positive than expected, though it was not "out of family" with other outliers seen throughout our monitoring history. Additionally, STIS CCD phase retrieval results have carried higher errors than seen with the more frequently utilized imagers due to coarser calibrations of the algorithms consistent with their less frequent application to that SI, along with uncertainty associated with the focus offset between the imaging and
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spectral modes. The STIS image-plane focus check made during SMOV was thus performed more as a gross indicator of any possibly new large focus offset within the instrument, rather than as a sensitive measurement of OTA focus state.

4. SMOV4 Focus Adjustments
The SMOV focusing plan that emerged from this estimate of ­2.5 µm at the SM was as follows: offset WFC3 & COS foci during SI SMOV fine alignment by the equivalent of ­2.5 µm to achieve confocality with ACS/WFC, then follow up with a +3.0 µm OTA refocus (prior to WFC3 PSF specification tests and Early Release Science). This OTA adjustment would then leave the SIs at ~ +0.5 µm focus, intentionally slightly overshooting best focus. Predictions using the best fitting exponential (eqn. 2) put best focus for the SIs near mid cycle 17 (summer 2010). Focus monitoring throughout cycle 17 would then establish the success to which confocality and best focus was achieved. During SMOV4, between 7­9 July 2009, WFC3 UVIS & IR Fine Optical Alignment proposals 11434 & 11435, and COS NUV Optical alignment 11469 executed. These programs featured near-real-time "ops requests" to actively command the instruments' optics into their final positions for best overall image quality based upon analysis performed on images obtained earlier in the same programs. The final uploaded positions for the SI optics were biased at that time by the equivalent of ­2.5 µm focus. The actual commanded values associated with the optical alignment of these instruments are described in Hartig (2009a, 2009b, 2010). On 20 July 2009, a Secondary Mirror move of +3.0 µm away from the PM was executed by engineers at GSFC. The actual commanded amount of this move was +2.97 µm due to SM actuator quantization. This OTA refocus was smaller than most of the routine shrinkage-compensating adjustments that had been applied in the past. However, WFC3's imaging performance is believed to require tighter focus control than other HST imaging instruments, and the initial desire to stay within 2 µm of defocus was adopted. After experience with WFC3 images in cycle 17 there is some evidence that a tighter focus control (e.g. +/­1 µm) may realize measurable improvement. This will be investigated further in cycle 18. The timeline and decision tree specific to SMOV4 focus that was developed to prescribe contingency plans for focusing new or existing SIs is reproduced in appendix A2. In fact, other than the described biasing of the new-SIs followed by the OTA adjustment to optimize focus and confocality, no other active focusing activities were performed during (and since) SMOV4. The OTA and the repaired SIs (STIS and ACS) were found to not have experienced any gross changes across the Servicing Mission boundary, or while inactive prior to repair.

5. Post-SMOV4 Focus Monitoring
Since the SMOV focusing activities, proposal CAL/OTA 11877 has been used as the primary monitor of overall focus. The data are analyzed using phase retrieval analysis of images taken with WFC3/UVIS and ACS/WFC, either in parallel or within the same orbit. The phase retrieval

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code requires SI-specific information in order to accurately characterize apparent optical aberrations like focus, and considerable investment was made during cycle 17 to adapt and calibrate the algorithms for WFC3. Niemi et al. (2010) give a thorough review of this. Figure 3 plots focus monitoring data obtained since the SMOV4 period, illustrating the success of our SMOV4 focus initiative at restoring overall focus and producing practically confocal main imagers. A full treatment of findings & results since the SMOV4 focusing initiative can be found in Niemi & Lallo (2010).
Figure 3: Defocus of the OTA from 2 December 2002 up to June 2010, including data taken since the 2009 Secondary Mirror Move in late SMOV. Evident is the resulting overall state of WFC3/ UVIS and ACS/WFC near best focus through cycle 17 (mirror moves prior to the last are indicated but have been removed to show a continuous trend).
Focus Trend Since Dec 2002 Mirror Move
Mirror Movement No Breathing correction No Breathing correction (WFC3) Linear Regression Exponent Fit Exponent Fit Cont.

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Accumulated Defocus [S M µm]

5

0

-5
4.16µm 5.34µm 2.97µm
6500 7000

3.6µm

5000

5500

Days since HST deployment

6000

7500

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References
Burrows, C., Hubble Space Telescope Optical Telescope Assembly Handbook, V1.0, 5/1990 Di Nino, D., Makidon, R. B., Lallo, M., Sahu, K., Sirianni, M., Casertano, S., HST Focus Variations with Temperature, ISR ACS 2008-03, 5/2008 Hartig, G., Dressel, L., Delker, T., WFC3 SMOV Programs 11424, 11434: UVIS Channel Onorbit Alignment, ISR WFC3 2009-45, 12/2009 Hartig, G., Dressel, L., Delker, T., WFC3 SMOV Programs 11425, 11435: IR Channel On-orbit Alignment, ISR WFC3 2009-46, 12/2009 Hartig, G., Delker, T., Keyes, C., SMOV: COS NUV On-orbit Optical Alignment, ISR COS 201004, 2/2010 Krist, J. E., Burrows, C. J., Phase Retrieval analysis of pre- and post-repair Hubble Space Telescope images, Appl. Opt. 34, 4951­4963 {1995} Lallo, M., Makidon, R. B., Casertano, S., Gilliland, R., Stys, J., HST Temporal Optical Behavior & Current Focus Status, ISR TEL 2005-03, 10/2005 Niemi, S.-M. Lallo, M., Phase Retrieval to Monitor HST Focus: II. First Results Post-Servicing Mission 4, ISR TEL 2010-02, 10/2010 Niemi, S.-M. Lallo, M., Hartig, G., Cox, C., Phase Retrieval to Monitor HST Focus: I. WFC3 UVIS Software Implementation , ISR TEL 2010-01, 7/2010

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Appendix
A1. Phase Retrieval Routine optical monitoring of HST is performed using IDL code to perform parametric (model-fitting) phase retrieval of a nearly in-focus PSF. The technique iteratively generates model PSFs and compares them with the observed data (Krist & Burrows 1995). The wavefront is characterized by the series of Mahajan Zernike polynomials modified for the 0.33 obscuration applicable to HST. They are listed below and discussed in greater detail in the OTA handbook (Burrows 1990). Current application and adaptation for WFC3 is described by Niemi et al. (2010). The phase retrieval process produces an estimated wavefront described by the series: (1)

where Zn are the Zernike polynomials, n are the normalization factors sometimes seen included as part of the Zernike polynomial, and cn are the solved-for coefficients representing wavefront error in microns. For n = 4 to 8, n Zn are given below: 4 5 6 7 8 Z Z Z Z Z
4 5 6 7 8

= = = = =

3.89 2.31 2.31 8.33 8.33

(r2 - 0.55445) r2 cos2 r2 sin2 (r3 - 0.673796r) cos (r3 - 0.673796r) sin

In the case of focus (n = 4) the c4 coefficient can be expressed as: (2)

where F = 24 = HST focal ratio, 4 = 3.89, m = magnification = F/fprimary = 24/2.3 =10.43. Thus c4 = 0.0061 ·
SM

Total rms wavefront error is (cn2)

1/2

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1st focus check in SMOV STIS image quality acceptable 5/30 (1st visit), 6/15 (2nd visit) ACS/SBC image quality verification ACS-16, 11378 NGC6681, NGC604 (SBC PSF gives only coarse focus check) 6/27 ACS/HRC Image Quality verification ACS-17, 11379 NGC188 6/11 (1st visit) 6/27 (2nd visit) ACS/WFC CTE Monitor 11510-03 6/21 ACS/WFC Image Quality verification ACS-17, 11379 NGC188

5/29 STIS focus check (CCD) STIS-11, 11386

ACS & STIS image quality acceptable

ACS Image quality nominal but STIS's is not.

Image quality appears degraded but STIS SMOV activities can proceed

STIS Optical Alignment Contingency STIS-12 11387 6/26 ACS/HRC&WFC Geometric Distortion ACS-11, 11397 47 Tuc ACS Image quality unacceptable

Image quality too poor to continue STIS SMOV activities Note: ACS CTE obs likely to be moved forward by a few days to immediately follow BEA-end

Deferred contingency pending other SI results

Y

STIS also unacceptable, and WFC3 & COS mechanism displacements all indicate consistent defocus magnitude and N direction?

STIS Optical Alignment Contingency STIS-12 11387
Schedule Placement TBD

6/22 ACS CTE Monitor 11510-04 47 Tuc If focus as measured by STIS and ACS up to and including this activity is acceptable but indicating a consistent, significant offset, then inform new SI alignments with this delta to increase confocality

STIS focus nominal? Y

N

ACS Optical Alignment Contingency ACS-13 11375 6/13 ­ 6/25 COS/NUV Optical Alignment COS-09 parts 1 - 5, 11469 COS cannot focus within OSM1's desirable range

Instrument Science Report TEL 2010-02

Decision Tree: Details & Timeline
A2. SMOV4 Focus Decision Tree
Assumes: · May 12 launch · NICMOS unavailable for external obser vations during SMOV Note: All boxes' left sides align with approximate start time unless otherwise noted. COS & WFC3 box lengths indicate approximate duration of activity and analysis. All others activities are comparatively short.

OTA Refocus Contingency Assessment

Schedule Placement TBD

6/14 ­ 6/21 WFC3/UVIS Initial Optical Alignment WF-11, 11424

6/26 COS/FUV Optical Alignment COS-26,11484

CAL/OTA Cycle 17 Focus Monitor, visit-01 initiates. Uses ACS/HRC, WFC3/UVIS, & STIS/CCD

WFC3/UVIS cannot focus within M1's desirable range

6/15 ­ 6/21 WFC3/IR Initial Optical Alignment WF-12, 11425

6/22 ­ 6/29 WFC3/UVIS Fine Alignment WF-21, 11434 WFC3/IR cannot focus within M2's desirable range

6/28 ­ 7/4 WFC3/IR Fine Alignment WF-22, 11435

Assess relative focii of all SIs, including NICMOS, and consider OTA and/or SI adjustment in early cycle 17 to increase confocality and/or better position SI mechanism(s )

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A3. HST Focus History Data File
Measured defocus, expressed with respect to best ACS/WFC focus (see section 2). No focus model correction.

ObsName, Date, Modified pre94 pre94 48110 pre94 pre94 48183 pre94 pre94 48219 pre94 pre94 48231 pre94 pre94 48292 pre94 pre94 48371 pre94 pre94 48402 pre94 pre94 48486 pre94 pre94 48511 pre94 pre94 48513 pre94 pre94 48536 pre94 pre94 48566 pre94 pre94 48584 pre94 pre94 48591 pre94 pre94 48621 pre94 pre94 48656 pre94 pre94 48671 pre94 pre94 48695 pre94 pre94 48698 pre94 pre94 48730 pre94 pre94 48761 pre94 pre94 48762 pre94 pre94 48786 pre94 pre94 48803 pre94 pre94 48840 pre94 pre94 48876 pre94 pre94 48901 pre94 pre94 48909 pre94 pre94 48936 pre94 pre94 48956 pre94 pre94 48986 pre94 pre94 49016 pre94 pre94 49036 pre94 pre94 49066 pre94 pre94 49126 pre94 pre94 49132 pre94 pre94 49161 pre94 pre94 49208 pre94 pre94 49236 pre94 pre94 49261 pre94 pre94 49279 pre94 pre94 49281 pre94 pre94 49301 pre94 pre94 49314 u2a70305t 8/03/94 49419 u2a70605t 20/03/94 49431 u2a70905t 25/03/94 49436 u2a70c05p 1/04/94 49443 u2a70i05t 21/04/94 49463 u2a70l05t 1/05/94 49473 u2a70o05t 8/06/94 49511 u2a70r05t 14/06/94 49517 u2a70u05t 4/07/94 49537 u2a70x05t 16/07/94 49549 u2a71005p 25/07/94 49558

JD, Microns of Secondary Mirror despace -1.00 -23.00 -32.00 -28.00 -39.00 -51.00 -48.00 -57.00 -61.00 -55.00 -59.00 -58.00 -61.00 -57.00 -51.00 -66.00 -69.00 -73.00 -74.00 -66.00 -72.00 -72.00 -72.00 -76.00 -78.00 -77.00 -78.00 -73.00 -70.50 -78.00 -78.00 -81.00 -77.00 -81.00 -82.00 -84.00 -86.00 -86.00 -87.00 -90.00 -91.00 -89.00 -93.00 -88.00 -2.40 -0.50 -0.70 -1.10 -2.30 -12.40 -4.10 -3.50 1.10 -0.50 -0.50

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u2a71305t u2a71605t u2a71905t u2a71c05t u2a71f05t u2a71i05t u2a71l05t u2a71o05t u2a71r05t u2a71u05t u2a71x05t u2a72605t u2a72905t u2a72c05t u2a72f05t u2n10203p u2n10403t u2o00501t u2s61101t u2s61201t u2s61301t u2s61401t u2s61501t u2s61601t u2s61701t u2s61801t u2s62101t u2s62201t u2s62301t u2s62401t u2s62501t u2s62601t u2s62701t u2s62801t u2s63101t u2s63201t u2s63301t u2s63401t u2s63501t u2s63601t u2s63701t u2s63801t u2s63901t u2s64001t u3dy0103t u3dy0203t u3dy0403t u3dy0503t u3dy0603t u3dy0702t u3dy0802t u3dy0904t u3dy1004t u3dy1102t u3dy1403t u3dy1502t u3dy1602t u3sr0102r u3sr0202r u3sa1107r u3sa1308r u3sr2602r u3t9810hr 4/08/94 23/08/94 2/09/94 21/09/94 26/09/94 20/10/94 25/10/94 14/11/94 21/11/94 12/12/94 20/12/94 11/01/95 21/01/95 11/02/95 13/02/95 7/03/95 13/03/95 7/05/95 27/07/95 6/08/95 21/08/95 31/08/95 18/09/95 28/09/95 16/10/95 29/10/95 13/11/95 22/11/95 12/12/95 18/12/95 10/01/96 15/01/96 8/02/96 15/02/96 6/03/96 17/03/96 28/03/96 7/04/96 2/05/96 7/05/96 27/05/96 6/06/96 17/06/96 24/06/96 27/07/96 30/07/96 8/09/96 17/09/96 29/09/96 15/10/96 19/10/96 11/11/96 21/11/96 9/12/96 9/01/97 5/02/97 9/02/97 23/02/97 25/02/97 27/02/97 28/02/97 3/03/97 4/03/97 49568 49587 49597 49616 49621 49645 49650 49670 49677 49698 49706 49728 49738 49759 49761 49783 49789 49844 49925 49935 49950 49960 49978 49988 50006 50019 50034 50043 50063 50069 50092 50097 50121 50128 50148 50159 50170 50180 50205 50210 50230 50240 50251 50258 50291 50294 50334 50343 50355 50371 50375 50398 50408 50426 50457 50484 50488 50502 50504 50506 50507 50510 50511 -0.70 -1.80 -0.30 -1.70 -1.40 -3.00 -4.90 -4.10 -2.00 -2.70 -5.20 -4.70 -0.80 -1.90 -3.00 1.20 -1.30 -1.50 -2.70 -3.90 -6.30 -2.20 1.00 -0.20 0.10 -1.20 -1.60 -0.40 -2.00 0.20 -1.80 -5.20 -0.70 -2.90 -6.30 -0.60 -0.50 2.90 0.70 -2.20 0.80 3.30 -0.20 2.20 0.17 -0.13 -2.57 -0.77 -0.87 -1.85 -1.45 6.50 1.23 4.30 4.27 3.35 4.55 3.90 3.45 3.92 4.31 4.13 4.00

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Instrument Science Report TEL 2010-02
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Instrument Science Report TEL 2010-02
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Instrument Science Report TEL 2010-02
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Instrument Science Report TEL 2010-02
j94g11k1q u94g120cm j94g07p7q u9i4020cm u9i4040cm j9i405mhq j9i406swq j9i407lzq j9i408cfq j9i409djq j9i410a2q j9i411ubq j9i412jrq j9i413bwq u9i4140cm u9vg010cm j9vg02d0q j9vg03usq j9vg03w0q u9vg040mm u9vg060hm u9vg070pm u9vg080pm u9vg090km u9vg100cm u9vg110om u9vg120pm u9vg130pm u9vg140pm u9vg150pm u9vg160pm u9vg170pm u9vg180pm ua5t010om ua5t020om ua5t030nm ua5t040om ua5t050om ua5t160om ua5t180nm ua5t270om ua5t190nm ua5t200nm ua5t210mn ua5t220om ua5t280om ua5t290om ua5t300om ua5t310om ua5t320om ua5t330om STIS_SMOV ACS_SMOV ACS_SMOV ACS_11501 27/07/05 26/08/05 09/09/05 1/10/05 11/12/05 30/12/05 22/01/06 23/02/06 13/03/06 19/04/06 25/05/06 09/06/06 05/07/06 07/08/06 9/09/06 6/11/06 27/11/06 20/01/07 21/01/07 6/03/07 25/04/07 28/05/07 7/07/07 7/08/07 18/09/07 6/11/07 2/12/07 15/12/07 17/01/08 28/01/08 2/03/08 16/03/08 20/04/08 1/05/08 13/06/08 23/06/08 31/07/08 15/08/08 24/09/08 19/12/08 1/01/09 28/01/09 23/02/09 22/03/09 3/04/09 6/04/09 10/04/09 23/04/09 25/04/09 1/05/09 7/05/09 4/06/09 14/06/09 9/07/09 24/07/09 53578 53608 53622 53644 53715 53734 53757 53789 53807 53844 53881 53895 53921 53954 53987 54045 54066 54120 54121 54165 54215 54248 54288 54319 54361 54410 54436 54449 54482 54493 54527 54541 54576 54587 54630 54640 54678 54693 54733 54819 54832 54859 54885 54912 54924 54927 54931 54944 54946 54952 54958 54986 54996 55021 55036 -0.62 -2.33 -4.62 0.53 -1.00 -3.89 -3.14 -6.70 -1.80 -8.40 -4.04 -3.99 -5.05 -1.54 -1.11 0.67 3.60 1.02 -0.76 -3.18 -2.81 -4.02 -1.21 -1.12 -1.58 -2.95 2.80 -0.48 1.74 0.45 -1.13 -0.16 0.81 -1.96 0.36 -0.59 -0.93 -3.27 -3.07 -2.87 -1.48 -2.93 -5.18 -3.49 -4.07 -2.87 -1.53 -1.54 -1.39 -1.33 -1.40 -2.30 -0.62 -2.20 0.40

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