Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5120c Report Date: 09-May-96:20:26 Version: ********** Check-in Date: ********** 1.Proposal Title: HST IMAGERY AND SPECTROSCOPY OF THE DUSTY SMC HII REGION N88A: CYCLE3HIGH ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID INTERSTELLAR MEDIUM GO 4382 Sub Category DUST ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Reginald J. Dufour RICE UNIVERSITY USA ------------------------------------------------------------------------------------ 7. Abstract Extensive imagery and spectroscopic observations of the DUSTY SMC HII region N88A (Henize 1956 catalog) are proposed with HST in order to study its UV-optical spectrum (FOS), the morphology of its gas and dust (WFC & FOC), and the characteristics of the surrounding stellar population (WFC). This object is unique among the HII region population of the SMC in that it contains significant amounts of internal dust and shows a very stratified ionization structure and spectrum. By virtue of its high surface brightness and small angular size, it is particularly well suited for the high spatial resolution imagery and combined UV-optical spectroscopic capabilities of HST. From these observations we will model both the ionized gas and dust in N88A in detail. These models will provide fundamental information regarding the nature and origin of the dust and its effect on the composition and physical conditions of the ionized gas local to N88A and the fainter nebulosities surrounding it. Similar observations of another compact SMC HII region, N81, will provide a compariso n. SMC N81 does not contain any internal or surrounding dust, but has a very high surface brightness and similar single-star ionizing source, making it particularly suitable for modeling and for comparisons with N88A. This study should have wide importance related to the nature and origin of dust in the ISM of metal-poor irregular galaxies. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 4.00 par: 1.73 10. Num targs pri: 2 par: 3 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS WF/PC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5120c PI: Reginald J. Dufour Proposal Title: HST IMAGERY AND SPECTROSCOPY OF THE DUSTY SMC HII REGION N88A: CYCLE3HIGH ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Pi Reginald J. Dufour RICE UNIVERSITY USA Donald R. Garnett UNIVERSITY OF MINNESOTA USA John S. Mathis UNIVERSITY OF WISCONSIN USA Manuel Peimbert INSTITUTO DE ASTRONOMIA MEXICO Evan D. Skillman UNIVERSITY OF MINNESOTA USA Silvia Torres-Peimbert INSTITUTO DE ASTRONOMIA MEXICO Donald K. Walter RICE UNIVERSITY USA ------------------------------------------------------------------------------------ 2. Scientific Justification. THIS IS THE SECOND (SPECTROSCOPY) PART OF PROGRAM GO-4382 WHICH IS BEING SUBMITTED IN TWO PARTS: (a) EARLY ACQ WFC IMAGERY AND (b) FOLLOW-ON FOS SPECTROSCOPY OF TWO SMALL HII REGIONS IN THE SMC Since the scientific justification is optional, we choose to omit it here. However, we include a table of data on the two target objects: TABLE 1 - FLUX AND SURFACE BRIGHTNESS DATA FOR SMC N88A AND N81 _______________________________________________________________________________ C(1400) C(2200) F(1909) F(2326) F(3727) F(4861) F(5007) F(6563) _______________________________________________________________________________ N88AINT F 5.5 3.2 92. 42. 64. 320. 2600. 1870. N88ACEN S (5) (3) 37. 17. 26. 128. 1040. 748. N81INT F 8.0 2.7 222. 42. 1680. 1450. 7600. 4422. N81CEN S (8) (3) 7.4 1.4 56. 48. 254. 148. FOS G130H/B G190H/R G190H/R G270H/R G400H/R G570H/R G570H/R G570H/R Effic. 0.007 0.070 0.035 0.065 0.067 0.049 0.048 0.013 N88A CPS 1.3* 5.3* 28. 29. 74. 695. 2850. 728. Exposure 600S 600S 600S 450S 200S 30S 30S 30S NETCOUNTS 780 3180 16,800 13,000 14,800 20,800 84,000 21,800 S/N 28* 56* 118* 100* 111 140 250sat 140 N81 CPS 1.8 5. 10.2 4.8 320. 260. 1400. 290. Exposure 0S 600S 600S 400S 100S 60S 60S 60S NETCOUNTS 3000 6100 1900 32,000 15,600 84,000 17,400 S/N 55* 55* 37* 175 120 250sat 130 _______________________________________________________________________________ Notes: At the top "F" is the integrated flux of the nebulae in units of 10^-14 ergs cm^-2 sec^-1 (A^-1 for continuum); "S" is the estimated central surface brightness in above F units per square arcsec. "CPS" is detected counts per sec through an aperture of approximately 1-square arcsec area centered on the nebula. See discussion for details and references. The S/N values for the UV lines consider the noise(*) in the underlying continuum from IUE spectra with the exciting star(s) included. _______________________________________________________________________________ Page 3 ------------------------------------------------------------------------------------ 3. Description of proposed observations. The primary observations are (a) FOS spectroscopy (1" square aperture) of the center of N88A and of an (arbitrary) offset position 3" off center with 5 gratings G130H, G190H, G270H, G400H, and G570H; (b) similar FOS spectroscopy of the center of N81; (c) WFC imagery of N88A through 5 filters: F502N (for 5007 [OIII]), F656N (for Halpha), F336W ("U"), F439W ("B"), and F555W ("V"); (d) similar WFC imagery of N81 through 5 filters: F502N, F656N, F336W, F439W, and and F555W. [Note that we have deleted originally proposed FOC/48 UV imagery.] All are proposed for Cycle 3; with the WFC imagery (observation sets c & d) of N88A and N81 being requested (another RPS file) early in the cycle to have the imagery available for precise positional measurement and determination of the best acquisition mode for the two sets of FOS spectra later. requesting that the five WFC exposures of each nebula be done consecatively in a "half-orbit" sequence, since not only are they necessary for FOS offset and acquisition purposes -but science as well (and we need similar orientations for the frames to minimize problems with alignment and rebinning of the imagery). Finally, doing a sequence of five in a "half-orbit" maximizes HST efficiency. We feel that an important adjunct to our primary science program on N88A and N81 is the parallel WFC and FOC imagery of "Serendipity Fields" located in the Shapley Wing east of the main body of the SMC --to be taken primarily during the FOS spectroscopy. Altogether, we calculate that some 18 parallel WFC and FOC/48 imagery exposures are possible to accomplish during the 21 direct observations. We are proposing using 1.0- PAIR square apertures with FOS in order to obtain spectra of two positions in each nebula during a given acquision or offset. For SMC N88A, aperture A will be positioned at or near the center of this small nebula and aperture B will be (arbitrarily) located on its "edge" 3" distant. Therefore, the "sky" will actually be a nebular spectrum. The same will be true for SMC N81, which is larger (10" diameter) and both apertures will be located near the center (specific offsets will be determined from the WFC early acquisi- tion imagery. Complete wavelength coverage from 1150-6870 A will be done in five grating settings for N88A (G130H, G190H, G270H, G400H, & G570H). Time restrictions by the TAC necessitated limiting our observations of N81 to only the 1650-6870 A range using four gratings (G190H, G270H, G400H, & G570H). The red digicon will be used for all except the G130H observation of N88A. THIS PARTICULAR RPS SUBMISSION PROPOSES ONLY THE FOS SPECTROSCOPY PARTS OF THE ENTIRE PROGRAM --TO BE DONE AFTER THE EARLY ACQ WFC IMAGERY Page 4 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. The three most important capabilities of HST which we require for our proposed science are (a) UV spectroscopic capabilities (FOS) with small apertures, (b) UV imagery capabilites (FOC), and (c) high spatial resolution (WFC, FOC, & FOS) compared to nominal ground-based seeing limited observations. Even with the spherical aberration problems, HST imagery of nebulae (eg. Eta Carina, Orion Nebula, the PN NGC2440) show outstanding improvements in detail with rather straightforward image deconvolution techniques. Since both N88A and N81 are rather small objects, we expect to be able to perform very good Lucy and Weiner deconvolution on the primary targets, since the PSF variation problem will be rather minimal compared to larger nebulae. However, the most important capability is the ability to obtain FOS UV- optical spectra spanning the entire range 1150- 6840A through small 1" apertures near the center and "edge" of N88A. This capability is crucial to understanding the nature of the object and its dust in N88A since it shows exceptionally high stratification in physical conditions. During the past several years we have accumulated longslit spectra, CCD imagery, and IUE spectra of these two objects and it is clear that sub-arcsecond resolution high S/N observations, possible only with HST, will be required to determine accurate C-N-Si abundances from high-S/N observations of the UV lines (notably NIII]1747-54, SiIII]1882-93, CIII]1907-9, CII]2324-29, etc.) continuum scattering and absorption by the dust. Table 1 (in our scientific justification at top here) gives various line and continuum surface brightness data for SMC N88A and N81. These were derived from published imagery and spectrophotometry data, CTIO 4m and 1.5m longslit and scanner spectrophotometry, and IUE SWP and LWR (both low and high dispersion) spectra. The bottom part of Table 1 lists expected counts for various emission lines and UV continuum points, based on our proposed exposure times. These were calculated per the Ver2.0 FOS Handbook instructions (p.15). The determining factor for the G190H/RD spectra was to accumulate 10,000+ counts in the important CIII]1909 lines, resulting in a S/N of approximately 100 (some 10 times better than our IUE spectra). The short exposures on the G570H/RD spectra are such so as not to overexpose [OIII]4959 (<64,000 counts). The G130H/BL exposures are to get approximately 1000+ counts per diode in the UV continuum, and the G270H/RD and G400H/RD exposures were set to get adequate counts for the CII]2326 multiplet and [OII]3727, respectively. Finally, the brightness of the N88A offset position (3" off center) is expected to be about 3 times lower, which will result in lower S/N spectra off center, but still have S/N sufficient for our science, particularly in the UV (lower extinction). The WFC exposure times for N88A and N81 are based on the longest exposure possible so as not to saturate a V=12.5 BO star in the wide-band (F336W, F439W, F555W) imagery (reasonable for the brightest stars in our field). To estimate exposures for WFC F486N, F502N, and F656N, we took the integrated fluxes in Table 1 and filter-CCD+OTA efficiencies in the WFC/PC Instrument Handbook and calculated net count rates for the two nebulae, then determined reasonable exposure times of 600S for F502N and F656N. The total WFC imagery electrons detected are expected to be (M=10^6, K=10^3): [N88A...F502N-12.6M, F656N-9.1M; N81...F502N-37.6M, F656N-22.0M]; for uniform surface brightness circular nebulae of radii 1.2" (N88A) and 6.1" (N81), the detected electrons per pixel reduce to: [N88A..., F502N-23.9K, F6563N-20.2K; N81...F502N-3.24K, F656N-1.86K]. Of course the surface brightness will not be uniform -the point is that we will have excellent S/N in our images. The parallel imagery exposure times are set by (a) the net time available during the primary instrument observations and (b) consideration of the relative filter+detector responses among each group of filters (appropriate for A0V). Page 5 ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. Our only "special request" is that the WFC imagery be performed first in the Cycle so that we can use the data to accurately map the surface brightness structure of the two nebulae and the locations of surrounding stars for precisely determining the positions for the two sets of FOS spectra. THEREFORE, AS PER THE PHASE II INSTRUCTIONS AND CONSULTATION WITH STSCI WE HAVE SUBMITTED SEPARATELY THE EARLY ACQUISITION REQUEST. SINCE THE PI IS FAMILIAR WITH "OFFSET ASTROMETRY" USING WFC IMAGERY, HE EXPECTS THAT THE FOS ACQUISION PARAMETERS COULD BE DONE WITHIN A WEEK AFTER RECEIVING THE IMAGERY. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. NONE ARE EXPECTED TO BE NEEDED WE EXPECT THE WFC IMAGERY WILL CALIBRATE THE ZERO POINT OF THE 1.0-PAIR APERTURES IF SUCH IS NOT PROVIDED BY STSCI BY THE END OF 1993. ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. The WFC-FOC imagery will be analyzed using standard IRAF/SDAS packages (the PI and a student recently finished processing WF and FOC imagery of the galaxy GR8) for which we have some experience based on a Cycle 1 program. The FOS spectra (and some existing IUE spectra) will be used to calibrate the FOC UV imagery. Ground-based imagery and spectroscopy will be used to calibrate the WFC imagery. The FOS spectra will be processed with IRAF/STSDAS software as well, whereby the emission line strengths and continuum levels will be measured on all three sets of spectra. Exposures are calculated to give adequate S/N (>10) for the important weak UV lines of NIV1488, [OIII]1663-6, NIII]1750, SiIII]1882-93, CII]2326, [OII]2470, etc; and S/N >100 for CIII]1909. These, coupled with the many optical emission lines expected in the longer wavelength FOS spectra will give a set of empirical diagnostics for ionic abundance ratios, temperatures, and densities for the positions in each nebula. However, the scientific analysis will be strongest in our modeling capabilities, which is discussed below. The spatial variation of the optical depth of the dust within N88A follows from the UV fluxes of the early-type stars, since their intrinsic energy distributions for wavelengths longer than Lyman-alpha are fairly independent of composition and temperature. The Balmer line ratios also provide the spatial variation of the optical reddening and of the recombination rate of nebular gas. From this recombination rate the nebular (two-photon) continuum can be predicted from standard theory and subtracted from the observed continuum, yielding the scattering from the dust (if the star is not in the aperture). The dust scattering provides a comparison of the optical properties of this dust, found in an extreme environment as regards radiation and chemical composition, with Galactic dust. The calculation will proceed similar to that for the diffuse galactic light (Mathis 1973) or in the Orion Nebula (Mathis et al 1981). The calculations begin by a tentative assumption of the albedo and phase parameter (the mean cosine of the scattering angle) of the dust in a model nebula. The actual spatial distribution of the stars will be used to determine the first scattering, and each subsequent scattering follows from the previous by the equations of radiative transport. Agreement of the emergent intensity with observations determines acceptable values of the optical properties of the dust. It will be most interesting to see if SMC dust is radically different from Galactic. Photoionization models of the nebulae will be calculated similar to Mathis (1982), Mathis and Rosa (1991), and similar papers. Radiation transport for the ionizing radiation is used to determine the ionization fractions of 13 elements in various stages of ionization. The opacity of the dust can be fully taken into account, and alters the type of ionization structure that a given spectral type star produces (Mathis 1986). Page 6 ------------------------------------------------------------------------------------ 8. Additional comments or special requests. It would be most expedient to obtain the WFC EARLY ACQ imagery before 1993 August 1 -since the PI will subsequently be in Mexico on sabbatical and he could more speedily do the astrometry on his Rice SparcStation before then. Because the SMC is at 1hr RA and -73 Dec, it is observable throughout the year with HST. ------------------------------------------------------------------------------------ 9. Description of previous HST work. None of the programs below are related to this project. P2416: "Imagery and Spectroscopy of the Super-Metal-Poor Galaxy GR8", Cycle 1, PI: R. J. Dufour. Not directly related to this project. P3589: "Parallel High Resolution Imaging of Diffuse Objects in the Magellanic Clouds", Cycle 2, PI: J. Walsh (Garnett is a CoI) "Massive Stars in Starburst Galaxies", Cycle 2, PI: T. Heckman, (Garnett is a CoI) P3840: "Abundances and Time Evolution of C, N, and O in Star Forming Galaxies", Cycle 2, PI: E. Skillman (Dufour, Garnett, Peimbert, and Torres- Peimbert are among the CoIs) WFC and FOC/48 imagery of the nearby (1Mpc) blue dwarf irregular galaxy GR8 was successfully obtained in 1991 July. Two 1200s (CR -SPLIT) exposures of the entire galaxy were obtained with WF/PC using F336W, F439W, F555W, F702W, F785LP, F502N, and F656N filters. Moreover, similar exposures of two associations in GR8 were obtained with FOC/48 using the F150W filter. Despite lack of flat- fields, during the 2nd half of 1991 stellar "core" photometry of over a thousand stars in GR8 down to V~24.5 was performed using DAOFIND AND APPHOT algorithms and the results presented in a poster paper at the 1992 January AAS meeting in Atlanta. The preliminary color-magnitude diagrams suggested that there have been three recent bursts of star formation in GR8, all withing the past 100 million years (uncorrected for light travel time), and that the galaxy does not contain any red supergiants and has an unexpectedly low red giant tip population. Hence, we concluded that GR8 is truly a young galaxy with no evidence whatsoever for having an old faint stellar population. Finally, in 1992 April, the WFC flat-field and other calibration data arrived from STScI, and during mid-1992 we removed the instrumental signatures from the WFC imagery. Currently we are (re-)doing the stellar photometry using DAOPHOT-II using PSF- weighted apertures and calibrations based on ground-based CCD imagery of the brightest stars obtained at McDonald in 1992 March. We expect to submit for publication the final results in late 1992, which a graduate student at Rice will further defend as his M.S. dissertation. Lastly, the FOS spectra (originally delayed due to FOS-safing problems in mid-1991) of the brightest HII region has now been scheduled for 1993 February in the (Cycle 2 No refereed publications to date; the abstract of our Atlanta AAS Meeting poster paper is published as: "HST WFC/FOC Imagery of the Irregulus Galaxy GR8", by R. J. Dufour, P. A. Scowen, K. Davidson, E. D. Skillman, J.-R. Roy, G. A. Shields, M. L. McCall, D. D. Clayton, and C.-C. Wu 1991, BAAS, 23,1456 Page 7 ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Rice: Dufour has a SparcStation 2GX which was 50% funded by the University (remainder by STScI and IUE-related grants) which has the full IRAF/STSDAS software package installed. Rice supports the PI with a 9-month academic salary, of which approximately 40% time is available for research. The likely graduate student to be involved in this project had his entire tuition and stipend supported by the University last year and a tuition waiver for him is likely possible during the period of this research (which we hope will be part of his Ph.D. dissertation). Minnesota: Skillman has a SparcStation paid for by the University as part of a start-up grant available for his HST-related research herein. UMN also supports 9M/M of his salary with significant release time for research. Garnett has a Hubble Fellowship supporting his entire annual salary, for which he divides his time roughly equally between UMN and STScI in his research. Wisconsin: Mathis also receives 9M/M of academic salary support with approximately half time available for research. His graduate student involved with the nebular modeling may receive tuition waivers during the period, as well as significant amounts of computer time necessary to pursue model-development and applications to the proposed research. UNAM(Mexico): Peimbert and Torres-Peimbert receive full 12-month salary support from Mexico for their research and teaching. They further have a variety of Sun workstations paid from UNAM funds available for the proposed research. All four institutions are major astronomy research centers with the necessary facilities available (libraries, computers, support personnel, etc.) necessary for successful attainment of the scientific objectives proposed. ------------------------------------------------------------------------------------ 11. Address Information Name: REGINALD J. DUFOUR Category: PI Institution: Rice University Address: DEPT. OF SPACE PHYSICS & ASTRONOMY RICE UNIVERSITY PO BOX 1892 City: HOUSTON State: TX Zip Code: 77251 Country: USA Telephone: 713 527 4944 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5120c [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 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 SMC-N88A H,503 RA-OFF = -3.126S +/- 0.005S, 2000 V = +110 EXT 1 V = 15.0, TYPE = B0 V, E(B-V) = DEC-OFF = +16.18" +/- 0.01", BKG 2 0.6 FROM 2 3 B-V = -0.3, U-B = -1.1 4 SURF-LINE(6563) = 7.5 E-12 5 SURF-LINE(5007) = 1.0 E-11 6 SURF-LINE(4861) = 1.3 E-12 7 SURF-LINE(3727) = 2.6 E-13 8 SURF-LINE(2326) = 1.7 E-13 9 SURF-LINE(1909) = 3.7 E-13 Comments: MAG/COLOR IS FOR CENTRAL STAR SURF-LINES SURF-CONT(1400) = 5.0 E-14 ARE FOR H II REGION ------------------------------------------------------------------------------------------------------------------------------------ 2 SMC-N88A- B,123 RA = 01H 24M 10.807S +/- 2000 V = +110 1 V = 15.40, TYPE = A0V, E(B-V) = OFFSET 0.023S, 2 0.02 DEC = -73D 09' 21.19" +/- B-V = -0.07, U-B = -0.4 0.10" Comments: OFFSET STAR FOR SMCN88A FOS SPECTRA MEASURED FROM EARLY ACQ WFC IMAGES MEASUREMENTS MADE 23 JULY 1993 -RJD ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST c)Generic Targets ID = 5120c [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 7 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Selection Criteria |Acqui|FLX| Flux data No | Name | Description | |Prblm|REF| | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 3 SMC-N88A-GEN H,503 RA = 01H 24M 10.807S, DEC = -73D 09' 21.19", R = 20' ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5120c [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 3 SMC-N88A- FOS/RD ACQ/ 4.3 MIRROR 1 14.0S 100 1 1 GROUP 3.0,3.1,3.2, OFFSET BINARY 3.3,3.4,3.5 NO GAP ONBOARD ACQ FOR 3.1 CYCLE 3 Comments: THIS IS BASED ON THE ANALYSIS OF EARLY ACQ IMAGES ------------------------------------------------------------------------------------------------------------------------------------ 3.1 SMC-N88A FOS/RD ACCUM 1.0- G190H STEP-PATT=STAR- 1 1200S 118 8 1 CYCLE 3 PAIR SKY Comments: APERTURE "B" TO BE CENTERED ON TARGET. ACCUMULATE SPECTRA IN BOTH APERTURES. ------------------------------------------------------------------------------------------------------------------------------------ 3.11 SMC-N88A- WFC IMAGE WFALL F656N PRE-FLASH=YES 1 1200S 10 3 3 PAR GEN CR-SPLIT=NO CYCLE 3 Comments: PARALLEL WITH FOS G190H SPEC 3.10 ------------------------------------------------------------------------------------------------------------------------------------ 3.2 SMC-N88A FOS/RD ACCUM 1.0- G270H STEP-PATT=STAR- 1 900S 100 7 1 CYCLE 3 PAIR SKY Comments: APERTURE "B" TO BE CENTERED ON TARGET. ACCUMULATE SPECTRA IN BOTH APERTURES. ------------------------------------------------------------------------------------------------------------------------------------ 3.21 SMC-N88A- WFC IMAGE WFALL F336W PRE-FLASH=YES 1 900S 100 1 3 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G270H SPEC 3.20 ------------------------------------------------------------------------------------------------------------------------------------ 3.3 SMC-N88A FOS/RD ACCUM 1.0- G400H STEP-PATT=STAR- 1 400S 111 6 1 CYCLE 3 PAIR SKY Comments: APERTURE "B" TO BE CENTERED ON TARGET. ACCUMULATE SPECTRA IN BOTH APERTURES. ------------------------------------------------------------------------------------------------------------------------------------ 3.31 SMC-N88A- WFC IMAGE WFALL F439W PRE-FLASH=YES 1 400S 100 1 3 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G400H SPEC 3.30 ------------------------------------------------------------------------------------------------------------------------------------ 3.4 SMC-N88A FOS/RD ACCUM 1.0- G570H STEP-PATT=STAR- 1 60S 250 3 1 CYCLE 3 PAIR SKY Comments: APERTURE "B" TO BE CENTERED ON TARGET. ACCUMULATE SPECTRA IN BOTH APERTURES. ------------------------------------------------------------------------------------------------------------------------------------ 3.41 SMC-N88A- WFC IMAGE WFALL F555W PRE-FLASH=YES 1 60S 100 1 3 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G570H SPEC 3.40 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5120c [ 11] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 3.5 SMC-N88A FOS/BL ACCUM 1.0- G130H STEP-PATT=STAR- 1 1200S 46 9 1 CYCLE 3 PAIR SKY Comments: APERTURE "B" TO BE CENTERED ON TARGET. ACCUMULATE SPECTRA IN BOTH APERTURES. ------------------------------------------------------------------------------------------------------------------------------------ 3.51 SMC-N88A- WFC IMAGE WFALL F439W PRE-FLASH=YES 1 1000S 300 1 3 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G130H SPEC 3.50 ------------------------------------------------------------------------------------------------------------------------------------ 3.52 SMC-N88A- WFC IMAGE WFALL F555W PRE-FLASH=YES 1 200S 300 1 3 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G130H SPEC 3.50 ------------------------------------------------------------------------------------------------------------------------------------ 4 SMC-N88A- FOS/RD ACQ/ 4.3 MIRROR 1 14.0S 100 1 2 GROUP 4.0,4.1,4.2, OFFSET BINARY 4.3,4.4,4.5 NO GAP ONBOARD ACQ FOR 4.1 CYCLE 3 Comments: THIS HAS BEEN MODIFIED AFTER ANALYSIS OF EARLY ACQ IMAGES ------------------------------------------------------------------------------------------------------------------------------------ 4.1 SMC-N88A FOS/RD ACCUM 0.7X2.0 G190H 1 1200S 118 8 2 CYCLE 3 -BAR Comments: ACCUMULATE ONE SPECTRUM OF OUTER NEB. ------------------------------------------------------------------------------------------------------------------------------------ 4.11 SMC-N88A- WFC IMAGE WFALL F336W PRE-FLASH=YES 1 1200S 100 1 4 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL DURING 4.10 SPECTRUM ------------------------------------------------------------------------------------------------------------------------------------ 4.2 SMC-N88A FOS/RD ACCUM 0.7X2.0 G270H 1 600S 100 7 2 CYCLE 3 -BAR Comments: ACCUMULATE ONE SPECTRUM OF OUTER NEB. ------------------------------------------------------------------------------------------------------------------------------------ 4.21 SMC-N88A- WFC IMAGE WFALL F439W PRE-FLASH=YES 1 600S 100 1 4 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL DURING 4.20 SPECTRUM ------------------------------------------------------------------------------------------------------------------------------------ 4.3 SMC-N88A FOS/RD ACCUM 0.7X2.0 G400H 1 300S 111 6 2 CYCLE 3 -BAR Comments: ACCUMULATE ONE SPECTRUM OF OUTER NEB. ------------------------------------------------------------------------------------------------------------------------------------ 4.31 SMC-N88A- WFC IMAGE WFALL F555W PRE-FLASH=YES 1 300S 100 1 4 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL DURING 4.30 SPECTRUM ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5120c [ 12] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 4.4 SMC-N88A FOS/RD ACCUM 0.7X2.0 G570H 1 60S 250 3 2 CYCLE 3 -BAR Comments: ACCUMULATE ONE SPECTRUM OF OUTER NEB. ------------------------------------------------------------------------------------------------------------------------------------ 4.41 SMC-N88A- WFC IMAGE WFALL F702W PRE-FLASH=YES 1 60S 100 1 4 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL DURING 4.40 SPECTRUM ------------------------------------------------------------------------------------------------------------------------------------ 4.5 SMC-N88A FOS/BL ACCUM 0.7X2.0 G130H 1 900S 46 9 2 CYCLE 3 -BAR Comments: ACCUMULATE ONE SPECTRUM OF OUTER NEB. ------------------------------------------------------------------------------------------------------------------------------------ 4.51 SMC-N88A- WFC IMAGE WFALL F439W PRE-FLASH=YES 1 700S 300 1 4 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G130H SPEC 4.50 ------------------------------------------------------------------------------------------------------------------------------------ 4.52 SMC-N88A- WFC IMAGE WFALL F555W PRE-FLASH=YES 1 200S 300 1 4 PAR GEN CR-SPLIT=NO 2 CYCLE 3 Comments: PARALLEL WITH FOS G130H SPEC 4.50 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5120c [ 13] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/RD WFC FOS/BL ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/BINARY ACCUM IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters STEP-PATT=STAR-SKY PRE-FLASH CR-SPLIT ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 4.00 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category INTERSTELLAR MEDIUM ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category DUST ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements GROUP 3.0,3.1,3.2,3.3,3.4,3.5 NO GAP; ONBOARD ACQ FOR 3.1; CYCLE 3 PAR; GROUP 4.0,4.1,4.2,4.3,4.4,4.5 NO GAP; ONBOARD ACQ FOR 4.1; ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR G190H F656N G270H F336W G400H F439W G570H F555W G130H F702W ------------------------------------------------------------------------------------------------------------------------------------ Target Names SMC-N88A SMC-N88A-OFFSET SMC-N88A-GEN ------------------------------------------------------------------------------------------------------------------------------------