Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 3815c Report Date: 09-May-96:18:51 Version: ********** Check-in Date: ********** 1.Proposal Title: UV OBSERVATIONS OF THE HUBBLE-SANDAGE VARIABLES IN M31 AND M33 ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID STELLAR ASTROPHYSICS GO Sub Category MASSIVE STARS ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Roberta M. Humphreys UNIVERSITY OF MINNESOTA USA 612-624-6530 ------------------------------------------------------------------------------------ 7. Abstract The Hubble-Sandage variables in M31 and M33 are luminous blue variables (LBVs) -- very luminous, eruptively unstable stars in the same general class as S Dor, Eta Car, and P Cyg. UV observations of H-S variables will significantly enhance the limited information available to us concerning the evolution and structure of the most massive stars. ---- LBVs are important in several major astrophysical connections and are only beginning to be understood. Since the LBV stage of evolution is brief, only a few examples are available in our Galaxy and in the Magellanic Clouds, close enough for UV observations with IUE. Therefore our coverage of the wide parameter space embraced by LBVs has been so sparse that theoretical development has been hindered. ---- With the ST, we can significantly increase this coverage by adding the H-S variables in M31 and M33 to the set of "useful" LBVs. UV spectroscopy is needed to determine their temperatures, luminosities, and mass-loss rates. These parameters are required to clarify their relations to other LBVs and very massive stars in general, and to provide more information on evolutionary origin of LBVs, physical causes of the violent eruptions, and other problems. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 8.93 par: 0 10. Num targs pri: 8 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS FOC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 3815c PI: Roberta M. Humphreys Proposal Title: UV OBSERVATIONS OF THE HUBBLE-SANDAGE VARIABLES IN M31 AND M33 ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Roberta M. Humphreys UNIVERSITY OF MINNESOTA USA Kris Davidson UNIVERSITY OF MINNESOTA USA Nolan R. Walborn SPACE TELESCOPE SCIENCE USA INSTITUTE Bernhard Wolf LANDESSTERNWARTE, HEIDELBERG GERMANY X Immo Appenzeller LANDESSTERNWARTE, HEIDELBERG GERMANY X Otmar Stahl LANDESSTERNWARTE, HEIDELBERG GERMANY X Franz-Josef Zickgraf LANDESSTERNWARTE, HEIDELBERG GERMANY X ------------------------------------------------------------------------------------ 3. Description of proposed observations. We plan to make UV images of all 8 stars in our list with the FOC, and then to use the FOS to obtain UV spectra of only 4, chosen after inspecting the FOC results. The rationale is as follows: --- Moderately long FOS integration times are needed for these objects. Therefore we feel that it is not realistic to attempt FOS observations of all 8 stars at this time. Moreover, some of the stars may be fainter than the assumed brightness and would thus be more expensive in terms of integration time. Thus it makes sense to obtain UV spectra of just 4 stars, most likely those which are brightest in the FOC images. --- Since we do not know the UV brightnesses, which probably fluctuate, we need the FOC to observe their fluxes around 2000 A. Eight FOC images are required to observe the eight stars. These may be regarded as early- acquisition images but they also have scientific value. They will provide rough limits on the temperatures of all 8 stars (by comparing the UV brightnesses with ground-based photometry) and they may also show if other, fainter hot stars are very near any of the H-S variables. We propose to use the FOC at F/96 with filter F190M (chosen to avoid excessive count rates). It appears that a format giving a 22" field with 0.022" x 0.044" pixels is satisfactory for our purposes (see comments in OSF). 2-minute integration times are sufficient to give good images and comfortably- better-than -minimal photometry. (continued:...) --- For each of 4 stars, we propose 3 FOS exposures using the 1" circular aperture: 70 minutes with grating G190H and the RD detector, 30 m with G270H/RD, and 30 m with G160L/BL. The G190H and G270H observations will produce good spectra in the range 1700--3200 A, with nominal S/N ratios of 20 to 30 for resolutions of 1 to 2 A (of course the S/N ratios will be better for stars that are brighter than assumed here, which we hope will be the case for at least two or three of them). A number of useful spectral lines occur in this wavelength interval. Unfortunately, in order to obtain continuum fluxes and slopes extending to wavelengths shorter than 1700 A, and in case certain important emission lines appear at such wavelengths, we must switch to the BL detector for the G160L observations, despite the overhead time that this entails. (Since the resulting count rates are low, we do not attempt to obtain good resolution at the shortest wavelengths.) --- Altogether we propose 8 FOC exposures and 12 FOS exposures. Most likely the 4 stars chosen for FOS work will be those which are currently brightest at 2000 A, based on the FOC data. But an exception is possible, e.g. if a significant eruption is detected through ground-based observations. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. IUE observations of some of the visually brightest Hubble-Sandage variables have been attempted. The results have been just marginal detections even with IUE exposure times of 6 or 7 hours; they give only a few DN above background and poor S/N even for wide-band flux estimates at the wavelengths where IUE is most sensitive (Humpheys et al. 1984, 1988). These efforts have demonstrated that measurements of these stars' spectral features and accurate short-UV-wavelength fluxes cannot be done with IUE; they also confirm that the typical UV fluxes assumed in this proposal are realistic. --- Many ground-based visual-wavelength observations of H-S variables have been made since the early 1970's (see refs. in the scientific justification). Their blue-visual spectra show strong similarities to the LBVs in our Galaxy and in the LMC. If we get ST time to do the FOS observations, we hope to obtain ground-based spectra not too different in epoch. ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. No special scheduling is absolutely required; however, since our target stars do vary over timescales of years or months, advantageous scheduling would be helpful in several respects. First, it is highly desirable that the interval between FOC and FOS observations not be too long -- preferably not more than 2 months. Secondly, it is desirable to obtain the FOS observations during the months September--December, so that ground-based data can be obtained at nearly the same time -- even though this is not strictly a requirement. Finally, it is always possible that a major eruption of one of our target stars might be detected by ground-based work; if so then it would be desirable to obtain the FOS data as soon thereafter as practicable. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. There are no special calibration requirements. A small "special catalog" of acquisition stars may be advisable; if so, we will provide the needed data (most likely just a few altered flags for the sets of GSC stars in these M31 and M33 fields). ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. So far as we can predict, the data reduction will use fairly routine methods. UV brightnesses estimated from the FOC images will probably use a sampling circle with r = about 0.3". Resolution enhancement in the FOC images will only be attempted if a field has an interesting close grouping of stars in it -- we cannot predict whether this will be the case. ...Analysis of P Cyg line profiles in the UV spectra obtained with the FOS will indicate the terminal velocity of the stellar wind and the mass-loss rate (provided that the velocities are not too small). The UV flux and UV spectral features, supported by ground-based photometry at visual and infrared wavelengths, will indicate the total energy distribution and bolometric luminosity of each FOS target star. Effective temperatures can be derived from the spectra in combination with model atmospheres. ..."Strange" UV spectra are possible for stars like these, e.g. with many emission lines; this is unpredictable and analysis would depend on details. Page 4 ------------------------------------------------------------------------------------ 8. Additional comments or special requests. Considerations outlined in question 5 are pertinent. Since it is desirable (though not necessary) to take ground-based data at about the same time as the FOS data, September--January is the optimum time for these ST observations. Ground-based photometric and spectroscopic monitoring of the Hubble-Sandage variables will continue. We can obtain visual and near-IR (UBVRI + JHK) photometry of the H-S variables with the University of Minnesota 1.5-m telescope on Mt. Lemmon, and moderate-to-high-resolution blue-visual-red spectra with the Calar Alto 3.5-m telescope. September--January is of course the prime season for ground-based observations of M31 and M33. ---- We have measured accurate TARGET POSITIONS on a set of 4m-prime-focus plates, using appropriate sets of GSC stars to set up the coordinate grids. These same plates may provide altered flags for a few GSC stars which may be dangerous to use for acquisition. (Target positions were measured in February 1992; as of mid-March, the GSC star re-evaluations are not yet completed but probably will be within a few weeks.) ------------------------------------------------------------------------------------ 9. Description of previous HST work. -- Davidson is PI and Humphreys, Walborn and Wolf are CoI's on GO 2338, "Spectroscopy of the speckle-resolved Eta Car point sources." This is indirectly related in the sense that Eta Carinae is an LBV and so are the H-S variables. -- Davidson and Walborn are assisting D. Ebbets on Ebbets' GTO 1186, "Imagery and UV spectroscopy of matter ejected from Eta Carinae." Above comments apply to this project also. -- Davidson is a CoI on R. Dufour's GO 2416, "Imagery and spectroscopy of super metal poor galaxies." This is related only if some LBV- like stars are found in GR8 or I Zw 18 (unlikely). -----results from above-listed programs:----- Several good WFC and PC images of Eta Car were made in 1991, and good FOS data were obtained for project 2338 in August 1991. These all require rather tricky analyses, which are not yet completed as of mid-March 1992. Similar remarks apply to the data obtained for Dufour's program number 2416. There are no real publications yet, except that several of the images were used in poster papers at the January 1992 AAS meeting. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). The Graduate School of the University of Minnesota provided $12,000 toward the purchase of a Sun computer for the original proposal for these observations submitted in 1988. A network of Sun computers now exists in the Minnesota Astronomy department. We have IRAF running on this system. However, since these machines are very heavily used, Humphreys is requesting funds for a dedicted work station. The data analysis facilities of ESO/ST-ECF are available to Wolf, Appenzeller, Stahl, and Zickgraf. They have also the MIDAS data reduction package on the machines at the Landessternwarte, Heidelberg. ------------------------------------------------------------------------------------ 11. Address Information Name: ROBERTA M. HUMPHREYS Category: PI Institution: UNIVERSITY OF MINNESOTA Address: ASTRONOMY DEPT. UNIVERSITY OF MINNESOTA 116 CHURCH ST. S.E. City: MINNEAPOLIS State: MN Zip Code: 55455 Country: USA Telephone: 612-624-6530 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 3815c [ 5] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 AF-AND M31- B,148,159 RA = 0H 43M 33.06S +/- J2000 1 V = 17.0 +/- 1.0 AF-AND 0.03S, 2 B-V = 0.0 +/- 0.2 DEC = +41D 12' 10.2" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 0738 Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M31) GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ 2 AE-AND M31- B,148,159 RA = 0H 43M 2.58S +/- 0.03S, J2000 1 V = 17.0 +/- 1.0 AE-AND DEC = +41D 49' 11.9" +/- 2 B-V = 0.0 +/- 0.2 0.3", 3 F-CONT(2000) = 4 +/- 3 E-15 PLATE-ID = 0738 Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M31). GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ 3 M31- B,148,159 RA = 0H 44M 50.58S +/- J2000 1 V = 17.0 +/- 1.0 004451+41303 0.03S, 2 B-V = 0.0 +/- 0.2 7 M31-VAR-A1 DEC = +41D 30' 37.4" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 0738 Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M31) THERE IS A FAINTER STAR ABOUT 5" E. GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ 4 M31- B,148,159 RA = 0H 44M 19.46S +/- J2000 1 V = 17.0 +/- 1.0 004419+41224 0.03S, 2 B-V = 0.0 +/- 0.2 7 M31-VAR-15 DEC = +41D 22' 46.7" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 0738 Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M31). THERE ARE FAINTER STARS 4--6" AWAY, TO S AND SW GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ 5 M33- B,148,159 RA = 1H 34M 10.92S +/- J2000 1 V = 17.0 +/- 1.0 013411+30343 0.03S, 2 B-V = 0.0 +/- 0.2 8 M33-VAR-83 DEC = +30D 34' 37.6" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 00DV Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M33). GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ 6 M33- B,148,159 RA = 1H 33M 49.22S +/- J2000 1 V = 17.0 +/- 1.0 013349+30380 0.03S, 2 B-V = 0.0 +/- 0.2 9 M33-VAR-B DEC = +30D 38' 09.3" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 00DV Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M33). GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 3815c [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 7 M33- B,148,159 RA = 1H 33M 35.15S +/- J2000 1 V = 17.0 +/- 1.0 013335+30360 0.03S, 2 B-V = 0.0 +/- 0.2 1 M33-VAR-C DEC = +30D 36' 00.6" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 00DV Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M33). THERE IS PROBABLY A FAINTER STAR ABOUT 2" W. GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ 8 M33- B,148,159 RA = 1H 34M 18.36S +/- J2000 1 V = 17.0 +/- 1.0 013418+30383 0.03S, 2 B-V = 0.0 +/- 0.2 7 M33-VAR-2 DEC = +30D 38' 36.9" +/- 3 F-CONT(2000) = 4 +/- 3 E-15 0.3", PLATE-ID = 00DV Comments: BRIGHTNESS IS VARIABLE. SPECIAL FIELD (M33). GS VERSION 1.1 (NOT 1.0) ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 3815c [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 10 DEFINE # FOC/96 IMAGE 512X102 F190M PIXEL=50X25 1 300S 60 3 1 CYCLE 2 HS- 4 IMAGE Comments: THESE FOC IMAGES OF THE 8 TARGETS WILL BE USED TO DECIDE SUBSET OF 4 TO BE OBS WITH FOS, HENCE MAY BE REGARDED AS EARLY- ACQS. FLUXES ARE VARIABLE. S/ N IS IDEALIZED, REFERS TO ENTIRE STAR IMAGE. ------------------------------------------------------------------------------------------------------------------------------------ 20 DEFINE # FOS/RD ACQ/ 4.3 MIRROR 1 30S 1 1 GROUP 20-50 NO GAP HS- BINARY 2 ONBOARD ACQ FOR 30 SPECT -50 CYCLE 2 / 20-50 Comments: 30S EXP TIME IS OPTIMAL FOR STAR SLIGHTLY FAINTER THAN ASSUMED V=17.0; MIGHT REDUCE ACQ EXP TIME ON BASIS OF FOC IMAGE... ------------------------------------------------------------------------------------------------------------------------------------ 30 DEFINE # FOS/RD ACCUM 1.0 G190H 1650- 1 62M 27 3 1 HS- 2311 SPECT Comments: QUOTED S/N RATIOS FOR FOS ACCUM REFER TO 1/2 DIODE, AND ARE VERY CRUDE BECAUSE ASSUMED FLUXES ARE ROUGH. ------------------------------------------------------------------------------------------------------------------------------------ 40 DEFINE # FOS/RD ACCUM 1.0 G270H 2225- 1 28M 27 3 1 HS- 3281 1 SPECT 2 Comments: SEE COMMENT FOR LINE 30 ------------------------------------------------------------------------------------------------------------------------------------ 50 DEFINE # FOS/BL ACCUM 1.0 G160L 1150- 1 24M 13 3 1 HS- 2524 2 SPECT Comments: SEE COMMENT FOR LINE 30 ------------------------------------------------------------------------------------------------------------------------------------ 110 USE HS- AF-AND IMAGE Comments: SEE COMMENTS FOR LINE 10. RE SCHEDULING, SEE TEXT QUESTIONS 5 AND 8; OPTIMAL WOULD BE FOC IMAGING BETWEEN MID-JULY AND MID- SEPT, ALLOWING FOS OBS IN FALL 92. ------------------------------------------------------------------------------------------------------------------------------------ 120 USE HS- AE-AND IMAGE Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 3815c [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 130 USE HS- M31- IMAGE 004451+4130 37 Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ 140 USE HS- M31- IMAGE 004419+4122 47 Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ 150 USE HS- M33- IMAGE 013411+3034 38 Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ 160 USE HS- M33- IMAGE 013349+3038 09 Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ 170 USE HS- M33- IMAGE 013335+3036 01 Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ 180 USE HS- M33- IMAGE 013418+3038 37 Comments: SEE COMMENTS FOR LINE 10 ------------------------------------------------------------------------------------------------------------------------------------ 210 USE HS- AF-AND COND IF 110 BRIGHT SPECT ENOUGH SELECT 4 OF 210 OR 220 OR 230 OR 240 OR 250 OR Comments: SEE COMMENT LINENUM 110. FOR S/ 260 OR 270 OR 280 N, SEE SEQ DEF. ------------------------------------------------------------------------------------------------------------------------------------ 220 USE HS- AE-AND COND IF 120 BRIGHT SPECT ENOUGH Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ 230 USE HS- M31- COND IF 130 SPECT 004451+4130 BRIGHT ENOUGH 37 Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ 240 USE HS- M31- COND IF 140 BRIGHT SPECT 004419+4122 ENOUGH 47 Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 3815c [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 250 USE HS- M33- COND IF 150 SPECT 013411+3034 BRIGHT ENOUGH 38 Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ 260 USE HS- M33- COND IF 160 BRIGHT SPECT 013349+3038 ENOUGH 09 Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ 270 USE HS- M33- COND IF 170 BRIGHT SPECT 013335+3036 ENOUGH 01 Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ 280 USE HS- M33- COND IF 180 BRIGHT SPECT 013418+3038 ENOUGH 37 Comments: SEE SELECT, LINE 210 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 3815c [ 10] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOC/96 FOS/RD FOS/BL ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ACQ/BINARY ACCUM ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters PIXEL ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 8.93 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category STELLAR ASTROPHYSICS ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category MASSIVE STARS ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 2 GROUP 20-50 NO GAP; ONBOARD ACQ FOR 30-50; CYCLE 2 / 20-50 COND IF 110 BRIGHT ENOUGH; SELECT 4 OF 210 OR 220 OR 230 OR 240 OR 250 OR 260 OR 270 OR 280 COND IF 120 BRIGHT ENOUGH COND IF 130 BRIGHT ENOUGH; COND IF 140 BRIGHT ENOUGH; COND IF 150 BRIGHT ENOUGH; COND IF 160 BRIGHT ENOUGH; COND IF 170 BRIGHT ENOUGH; COND IF 180 BRIGHT ENOUGH; ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F190M MIRROR G190H G270H G160L ------------------------------------------------------------------------------------------------------------------------------------ Target Names AF-AND M31-AF-AND AE-AND M31-AE-AND M31-004451+413037 M31-VAR-A1 M31-004419+412247 M31-VAR-15 M33-013411+303438 M33-VAR-83 M33-013349+303809 M33-VAR-B M33-013335+303601 M33-VAR-C M33-013418+303837 M33-VAR-2 ------------------------------------------------------------------------------------------------------------------------------------