! File: 4382C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:09:17:03 coverpage: title_1: HST IMAGERY AND SPECTROSCOPY OF THE DUSTY SMC title_2: HII REGION N88A: CYCLE3HIGH sci_cat: INTERSTELLAR MEDIUM sci_subcat: DUST proposal_for: GO pi_fname: REGINALD pi_mi: J. pi_lname: DUFOUR pi_inst: RICE UNIVERSITY pi_country: USA hours_pri: 0.74 hours_par: 0.74 num_pri: 2 num_par: 2 wf_pc: Y foc: Y funds_length: 12 off_fname: G. off_mi: A. off_lname: GORRY off_title: VP FOR RESEARCH off_inst: 3240 off_addr_1: OFFICE OF SPONSORED RESEARCH off_addr_2: RICE UNIVERSITY off_addr_3: 6100 MAIN ST. off_city: HOUSTON off_state: TX off_zip: 77251 off_country: USA off_phone: 713 527 6054 ! end of coverpage abstract: line_1: Extensive imagery and spectroscopic observations of the DUSTY SMC HII region line_2: N88A (Henize 1956 catalog) are proposed with HST in order to study its line_3: UV-optical spectrum (FOS), the morphology of its gas and dust (WFC & FOC), line_4: and the characteristics of the surrounding stellar population (WFC). line_5: This object is unique among the HII region population of the SMC in line_6: that it contains significant amounts of internal dust and shows a very line_7: stratified ionization structure and spectrum. By virtue of its high surface line_8: brightness and small angular size, it is particularly well suited for the high line_9: spatial resolution imagery and combined UV-optical spectroscopic capabilities line_10: of HST. From these observations we will model both the ionized gas and line_11: dust in N88A in detail. These models will provide fundamental information line_12: regarding the nature and origin of the dust and its effect on the line_13: composition and physical conditions of the ionized gas local to N88A line_14: and the fainter nebulosities surrounding it. Similar observations of line_15: another compact SMC HII region, N81, will provide a compariso n. SMC N81 line_16: does not contain any internal or surrounding dust, but has a very high surface line_17: brightness and similar single-star ionizing source, making it particularly line_18: suitable for modeling and for comparisons with N88A. This study should line_19: have wide importance related to the nature and origin of dust in the ISM of line_20: metal-poor irregular galaxies. ! ! end of abstract general_form_proposers: lname: DUFOUR fname: REGINALD title: PI mi: J. inst: RICE UNIVERSITY country: USA ! lname: GARNETT fname: DONALD mi: R. inst: UNIVERSITY OF MINNESOTA country: USA ! lname: MATHIS fname: JOHN mi: S. inst: UNIVERSITY OF WISCONSIN country: USA ! lname: PEIMBERT fname: MANUEL inst: INSTITUTO DE ASTRONOMIA country: MEXICO ! lname: SKILLMAN fname: EVAN mi: D. inst: UNIVERSITY OF MINNESOTA country: USA ! lname: TORRES-PEIMBERT fname: SILVIA inst: INSTITUTO DE ASTRONOMIA country: MEXICO ! lname: WALTER fname: DONALD mi: K. inst: RICE UNIVERSITY country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: THIS IS AN EARLY ACQUISITION REQUEST PART OF THE G0-4382 PROGRAM WHICH line_2: IS BEING SUBMITTED IN TWO PARTS: (a) EARLY ACQ WFC IMAGERY AND line_3: (b) FOLLOW-ON FOS SPECTROSCOPY OF TWO SMALL HII REGIONS IN THE SMC line_4: Since the scientific justification is optional, we choose to omit it here. line_5: However, we include a table of data on the two target objects: line_7: TABLE 1 - FLUX AND SURFACE BRIGHTNESS DATA FOR SMC N88A AND N81 line_8: _______________________________________________________________________________ line_9: C(1400) C(2200) F(1909) F(2326) F(3727) F(4861) F(5007) F(6563) line_10: _______________________________________________________________________________ line_11: N88AINT F 5.5 3.2 92. 42. 64. 320. 2600. 1870. line_12: N88ACEN S (5) (3) 37. 17. 26. 128. 1040. 748. line_13: N81INT F 8.0 2.7 222. 42. 1680. 1450. 7600. 4422. line_14: N81CEN S (8) (3) 7.4 1.4 56. 48. 254. 148. line_16: FOS G130H/B G190H/R G190H/R G270H/R G400H/R G570H/R G570H/R G570H/R line_17: Effic. 0.007 0.070 0.035 0.065 0.067 0.049 0.048 0.013 line_19: N88A CPS 1.3* 5.3* 28. 29. 74. 695. 2850. 728. line_20: Exposure 800S 400S 400S 400S 150S 20S 20S 20S line_21: NETCOUNTS 1040 2100 11,200 11,600 18,800 13,900 57,000 14,600 line_22: S/N 30* 45* 95* 85* 130 115 230 120 ! question: 2 section: 2 line_1: N81 CPS 1.8 5. 10.2 4.8 320. 260. 1400. 290. line_2: Exposure 800S 1000S 1000S 600S 100S 45S 45S 45S line_3: NETCOUNTS 1400 5000 10,200 2900 32,000 11,700 63,000 13,000 line_4: S/N 35* 70* 71* 48* 175 105 250 110 line_5: _______________________________________________________________________________ line_7: Notes: At the top "F" is the integrated flux of the nebulae in units of 10^-14 line_8: ergs cm^-2 sec^-1 (A^-1 for continuum); "S" is the estimated central surface line_9: brightness in above F units per square arcsec. "CPS" is detected counts per sec line_10: through an aperture of approximately 1-square arcsec area centered on the line_11: nebula. See discussion for details and references. The S/N values for the UV line_12: lines consider the noise(*) in the underlying continuum from IUE spectra with line_13: the exciting star(s) included. line_14: _______________________________________________________________________________ ! question: 3 section: 1 line_1: The primary observations are (a) FOS spectroscopy (1" square aperture) of line_2: the center of N88A and of an (arbitrary) offset position 3" off center with 5 line_3: gratings G130H, G190H, G270H, G400H, and G570H; (b) similar FOS spectroscopy line_4: of the center of N81; (c) WFC imagery of N88A through 5 filters: F502N (for 5007 line_5: [OIII]), F656N (for Halpha), F336W ("U"), F439W ("B"), and F555W ("V"); (d) line_6: similar WFC imagery of N81 through 5 filters: F502N, F656N, F336W, F439W, and line_7: and F555W. [Note that we have deleted originally proposed FOC/48 UV imagery.] line_9: All are proposed for Cycle 3; with the WFC imagery (observation sets c & d) line_10: of N88A and N81 being requested [THIS RPS FILE] early in the cycle in order to line_11: have the imagery available for precise positional measurement and determination line_12: of the best acquisition mode for the two sets of FOS spectra later. We are line_13: requesting that the five WFC exposures of each nebula be done consecatively in line_14: a "half-orbit" sequence, since not only are they necessary for FOS offset and line_15: acquisition purposes -but science as well (and we need similar orientations for line_16: the frames to minimize problems with alignment and rebinning of the imagery). line_17: Finally, doing a sequence of five in a "half-orbit" maximizes HST efficiency. line_19: We feel that an important adjunct to our primary science program on N88A and line_20: N81 is the parallel WFC and FOC imagery of "Serendipity Fields" located in the line_21: Shapley Wing east of the main body of the SMC --to be taken primarily during the line_22: FOS spectroscopy. Altogether, we calculate that some 18 parallel WFC and FOC/48 line_23: imagery exposures are possible to accomplish during the 21 direct observations. ! question: 3 section: 2 line_1: The WFC imagery proposed are generally with F656N (searching for emission-line line_2: objects), F336W (U-band photometry), F439W (B-band photometry), F555W (V-band line_3: photometry), and some with F702W (R-band photometry). The FOC/48 parallel line_4: imagery (to be done in parallel with the WFC directed imagery) will be through line_5: PRISM1, F342W, F430W, and F130LP filters (UV-vis spectra & "U" - "B"). These line_6: parallel imagery data will be used by a graduate student at Rice to study line_7: the stellar population characteristics of the SMC wing fields as part of a line_8: (hopefully Ph. D.) dissertation project. They offer an important secondary line_9: scientific program in itself, but one which space limitations in the proposal line_10: format do not permit us to fully justify (essentially the same now for the SMC line_11: regions as for Dufour's Cycle 1 program on the irregular galaxy GR8, noted line_12: later.) line_14: THIS PARTICULAR RPS SUBMISSION PROPOSES ONLY THE WFC AND PARALLEL IMAGERY FOR line_15: PARTS OF THE ENTIRE PROGRAM --NEEDED FOR THE FOLLOW-UP FOS SPECTROSCOPY ! question: 4 section: 1 line_1: The three most important capabilities of HST which we require for our line_2: proposed science are (a) UV spectroscopic capabilities (FOS) with small line_3: apertures, (b) UV imagery capabilites (FOC), and (c) high spatial resolution line_4: (WFC, FOC, & FOS) compared to nominal ground-based seeing limited observations. line_5: Even with the spherical aberration problems, HST imagery of nebulae (eg. Eta line_6: Carina, Orion Nebula, the PN NGC2440) show outstanding improvements in detail line_7: with rather straightforward image deconvolution techniques. Since both N88A and line_8: N81 are rather small objects, we expect to be able to perform very good Lucy and line_9: Weiner deconvolution on the primary targets, since the PSF variation problem line_10: will be rather minimal compared to larger nebulae. line_12: However, the most important capability is the ability to obtain FOS UV- line_13: optical spectra spanning the entire range 1150-6840A through small 1" apertures line_14: near the center and "edge" of N88A. This capability is crucial to understanding line_15: the nature of the object and its dust in N88A since it shows exceptionally high line_16: stratification in physical conditions. During the past several years we have line_17: accumulated longslit spectra, CCD imagery, and IUE spectra of these two objects line_18: and it is clear that sub-arcsecond resolution high S/N observations, possible line_19: only with HST, will be required to determine accurate C-N-Si abundances from line_20: high-S/N observations of the UV lines (notably NIII]1747-54, SiIII]1882-93, line_21: CIII]1907-9, CII]2324-29, etc.) continuum scattering and absorption by the line_22: dust. ! question: 4 section: 2 line_1: Table 1 (in our scientific justification at top here) gives various line_2: line and continuum surface brightness data for SMC N88A and N81. These were line_3: derived from published imagery and spectrophotometry data, CTIO 4m and 1.5m line_4: longslit and scanner spectrophotometry, and IUE SWP and LWR (both low and high line_5: dispersion) spectra. The bottom part of Table 1 lists expected counts for line_6: various emission lines and UV continuum points, based on our proposed exposure line_7: times. These were calculated per the Ver2.0 FOS Handbook instructions (p.15). line_9: The determining factor for the G190H/RD spectra was to accumulate 10,000+ line_10: counts in the important CIII]1909 lines, resulting in a S/N of approximately 100 line_11: (some 10 times better than our IUE spectra). The short exposures on the line_12: G570H/RD spectra are such so as not to overexpose [OIII]5007 (<64,000 counts). line_13: The G130H/BL exposures are to get approximately 1000+ counts per diode in the UV line_14: continuum, and the G270H/RD and G400H/RD exposures were set to get adequate line_15: counts for the CII]2326 multiplet and [OII]3727, respectively. Finally, the line_16: exposures for the N88A offset position (3" S of center) are approximately 3X line_17: longer than the center to compensate for the expected drop in surface line_18: brightness compared to the center. line_20: The WFC exposure times for N88A and N81 are based on the longest exposure line_21: possible so as not to saturate a V=12.5 BO star in the wide-band (F336W, F439W, line_22: F555W) imagery (reasonable for the brightest stars in our field). To estimate line_23: exposures for WFC F486N, F502N, and F656N, we took the integrated fluxes in ! question: 4 section: 3 line_1: Table 1 and filter-CCD+OTA efficiencies in the WFC/PC Instrument Handbook and line_2: calculated net count rates for the two nebulae, then determined reasonable line_3: exposure times of 600S for F502N and F656N. The total WFC imagery electrons line_4: detected are expected to be (M=10^6, K=10^3): [N88A...F502N-12.6M, F656N-9.1M; line_5: N81...F502N-37.6M, F656N-22.0M]; for uniform surface brightness circular line_6: nebulae of radii 1.2" (N88A) and 6.1" (N81), the detected electrons per pixel line_7: reduce to: [N88A..., F502N-23.9K, F6563N-20.2K; N81...F502N-3.24K, F656N-1.86K]. line_8: Of course the surface brightness will not be uniform -the point is that we will line_9: have excellent S/N in our images. line_11: The parallel imagery exposure times are set by (a) the net time available line_12: during the primary instrument observations and (b) consideration of the relative line_13: filter+detector responses among each group of filters (appropriate for A0V). ! question: 5 section: 1 line_1: Our only "special request" is that the WFC imagery be performed first in the line_2: Cycle so that we can use the data to accurately map the surface brightness line_3: structure of the two nebulae and the locations of surrounding stars for line_4: precisely determining the positions for the two sets of FOS spectra. line_6: THEREFORE, AS PER THE PHASE II INSTRUCTIONS AND CONSULTATION WITH STSCI line_7: WE SUBMIT THE WFC IMAGERY AS AN EARLY ACQUISITION REQUEST. SINCE THE PI IS line_8: FAMILIAR WITH "OFFSET ASTROMETRY" USING WFC IMAGERY, HE EXPECTS THAT THE FOS line_9: ACQUISION PARAMETERS COULD BE DONE WITHIN A WEEK AFTER RECEIVING THE IMAGERY. ! question: 6 section: 1 line_1: NONE ARE EXPECTED TO BE NEEDED line_2: WE EXPECT THE WFC IMAGERY WILL CALIBRATE THE ZERO POINT OF THE 1.0-PAIR line_3: APERTURES IF SUCH IS NOT PROVIDED BY STSCI BY THE END OF 1993. ! question: 7 section: 1 line_1: The WFC-FOC imagery will be analyzed using standard IRAF/SDAS packages line_2: (the PI and a student recently finished processing WF and FOC imagery of the line_3: galaxy GR8) for which we have some experience based on a Cycle 1 program. The line_4: FOS spectra (and some existing IUE spectra) will be used to calibrate the FOC line_5: UV imagery. Ground-based imagery and spectroscopy will be used to calibrate the line_6: WFC imagery. line_8: The FOS spectra will be processed with IRAF/STSDAS software as well, whereby line_9: the emission line strengths and continuum levels will be measured on all three line_10: sets of spectra. Exposures are calculated to give adequate S/N (>10) for the line_11: important weak UV lines of NIV1488, [OIII]1663-6, NIII]1750, SiIII]1882-93, line_12: CII]2326, [OII]2470, etc; and S/N >100 for CIII]1909. These, coupled with the line_13: many optical emission lines expected in the longer wavelength FOS spectra will line_14: give a set of empirical diagnostics for ionic abundance ratios, temperatures, line_15: and densities for the positions in each nebula. However, the scientific line_16: analysis will be strongest in our modeling capabilities, which is discussed line_17: below. line_19: The spatial variation of the optical depth of the dust within N88A line_20: follows from the UV fluxes of the early-type stars, since their intrinsic line_21: energy distributions for wavelengths longer than Lyman-alpha are fairly line_22: independent of composition and temperature. The Balmer line ratios also line_23: provide the spatial variation of the optical reddening and of the ! question: 7 section: 2 line_1: recombination rate of nebular gas. From this recombination rate the nebular line_2: (two-photon) continuum can be predicted from standard theory and line_3: subtracted from the observed continuum, yielding the scattering from the line_4: dust (if the star is not in the aperture). line_6: The dust scattering provides a comparison of the optical properties of line_7: this dust, found in an extreme environment as regards radiation and line_8: chemical composition, with Galactic dust. The calculation will proceed line_9: similar to that for the diffuse galactic light (Mathis 1973) or in the Orion line_10: Nebula (Mathis et al 1981). The calculations begin by a tentative assumption line_11: of the albedo and phase parameter (the mean cosine of the scattering angle) line_12: of the dust in a model nebula. The actual spatial distribution of the stars will line_13: be used to determine the first scattering, and each subsequent scattering line_14: follows from the previous by the equations of radiative transport. line_15: Agreement of the emergent intensity with observations determines line_16: acceptable values of the optical properties of the dust. It will be most line_17: interesting to see if SMC dust is radically different from Galactic. line_19: Photoionization models of the nebulae will be calculated similar to line_20: Mathis (1982), Mathis and Rosa (1991), and similar papers. Radiation line_21: transport for the ionizing radiation is used to determine the ionization line_22: fractions of 13 elements in various stages of ionization. The opacity of the line_23: dust can be fully taken into account, and alters the type of ionization ! question: 7 section: 3 line_1: structure that a given spectral type star produces (Mathis 1986). ! question: 8 section: 1 line_1: It would be most expedient to obtain the WFC EARLY ACQ imagery before line_2: 1993 August 1 -since the PI will subsequently be in Mexico on sabbatical line_3: and he could more speedily do the astrometry on his Rice SparcStation line_4: before then. line_6: Because the SMC is at 1hr RA and -73 Dec, it is observable throughout line_7: the year with HST. ! question: 9 section: 1 line_1: None of the programs below are related to this project. line_2: P2416: "Imagery and Spectroscopy of the Super-Metal-Poor Galaxy GR8", line_3: Cycle 1, PI: R. J. Dufour. Not directly related to this project. line_4: P3589: "Parallel High Resolution Imaging of Diffuse Objects in the line_5: Magellanic Clouds", Cycle 2, PI: J. Walsh (Garnett is a CoI) line_6: "Massive Stars in Starburst Galaxies", Cycle 2, PI: T. Heckman, line_7: (Garnett is a CoI) line_8: P3840: "Abundances and Time Evolution of C, N, and O in Star Forming line_9: Galaxies", Cycle 2, PI: E. Skillman (Dufour, Garnett, Peimbert, and line_10: Torres-Peimbert are among the CoIs) line_12: WFC and FOC/48 imagery of the nearby (1Mpc) blue dwarf irregular galaxy GR8 line_13: was successfully obtained in 1991 July. Two 1200s (CR-SPLIT) exposures of the line_14: entire galaxy were obtained with WF/PC using F336W, F439W, F555W, F702W, F785LP, line_15: F502N, and F656N filters. Moreover, similar exposures of two associations in line_16: GR8 were obtained with FOC/48 using the F150W filter. Despite lack of flat- line_17: fields, during the 2nd half of 1991 stellar "core" photometry of over a thousand line_18: stars in GR8 down to V~24.5 was performed using DAOFIND AND APPHOT algorithms line_19: and the results presented in a poster paper at the 1992 January AAS meeting in line_20: Atlanta. The preliminary color-magnitude diagrams suggested that there have line_21: been three recent bursts of star formation in GR8, all withing the past 100 line_22: million years (uncorrected for light travel time), and that the galaxy does not line_23: contain any red supergiants and has an unexpectedly low red giant tip ! question: 9 section: 2 line_1: population. Hence, we concluded that GR8 is truly a young galaxy with no line_2: evidence whatsoever for having an old faint stellar population. line_4: Finally, in 1992 April, the WFC flat-field and other calibration data line_5: arrived from STScI, and during mid-1992 we removed the instrumental signatures line_6: from the WFC imagery. Currently we are (re-)doing the stellar photometry using line_7: DAOPHOT-II using PSF-weighted apertures and calibrations based on ground-based line_8: CCD imagery of the brightest stars obtained at McDonald in 1992 March. We line_9: expect to submit for publication the final results in late 1992, which a line_10: graduate student at Rice will further defend as his M.S. dissertation. Lastly, line_11: the FOS spectra (originally delayed due to FOS-safing problems in mid-1991) of line_12: the brightest HII region has now been scheduled for 1993 February in the (Cycle line_13: 2 line_15: No refereed publications to date; the abstract of our Atlanta AAS Meeting line_16: poster paper is published as: line_17: "HST WFC/FOC Imagery of the Irregulus Galaxy GR8", by R. J. Dufour, P. A. line_18: Scowen, K. Davidson, E. D. Skillman, J.-R. Roy, G. A. Shields, M. L. McCall, line_19: D. D. Clayton, and C.-C. Wu 1991, BAAS, 23,1456 ! question: 10 section: 1 line_1: Rice: Dufour has a SparcStation 2GX which was 50% funded by the University line_2: (remainder by STScI and IUE-related grants) which has the full IRAF/STSDAS line_3: software package installed. Rice supports the PI with a 9-month academic line_4: salary, of which approximately 40% time is available for research. The likely line_5: graduate student to be involved in this project had his entire tuition and line_6: stipend supported by the University last year and a tuition waiver for him is line_7: likely possible during the period of this research (which we hope will be part line_8: of his Ph.D. dissertation). line_10: Minnesota: Skillman has a SparcStation paid for by the University as part line_11: of a start-up grant available for his HST-related research herein. UMN also line_12: supports 9M/M of his salary with significant release time for research. Garnett line_13: has a Hubble Fellowship supporting his entire annual salary, for which he line_14: divides his time roughly equally between UMN and STScI in his research. line_16: Wisconsin: Mathis also receives 9M/M of academic salary support with line_17: approximately half time available for research. His graduate student involved line_18: with the nebular modeling may receive tuition waivers during the period, as well line_19: as significant amounts of computer time necessary to pursue model-development line_20: and applications to the proposed research. line_22: UNAM(Mexico): Peimbert and Torres-Peimbert receive full 12-month salary line_23: support from Mexico for their research and teaching. They further have a ! question: 10 section: 2 line_1: variety of Sun workstations paid from UNAM funds available for the proposed line_2: research. line_4: All four institutions are major astronomy research centers with the line_5: necessary facilities available (libraries, computers, support personnel, etc.) line_6: necessary for successful attainment of the scientific objectives proposed. ! !end of general form text general_form_address: lname: DUFOUR fname: REGINALD mi: J. category: PI inst: Rice University addr_1: DEPT. OF SPACE PHYSICS & ASTRONOMY addr_2: RICE UNIVERSITY addr_3: PO BOX 1892 city: HOUSTON state: TX zip: 77251 country: USA phone: 713 527 4944 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SMC-N88A descr_1: H,503 pos_1: RA = 01H 24M 09.2S +/- 0.1S, pos_2: DEC = -73D 09' 17" +/- 1", pos_3: TBD-EARLY equinox: 2000 rv_or_z: V = +110 acqpr_1: EXT acqpr_2: BKG comment_1: MAG/COLOR IS FOR CENTRAL STAR comment_2: SURF-LINES ARE FOR H II REGION comment_3: RMS N88A J2000 POSITIONS ARE: comment_4: RA = 01H 24M 09.2S +/- 0.1S comment_5: DEC = -73D 09' 17" +/- 1" comment_6: THESE ARE INADEQUATE FOR FOS OBS. fluxnum_1: 1 fluxval_1: V = 13.0, TYPE = B0 V, E(B-V) = 0.6 fluxnum_2: 2 fluxval_2: B-V = -0.3, U-B = -1.1 fluxnum_3: 3 fluxval_3: SURF-LINE(6563) = 7.5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 1.0 E-11 fluxnum_5: 5 fluxval_5: SURF-LINE(4861) = 1.3 E-12 fluxnum_6: 6 fluxval_6: SURF-LINE(3727) = 2.6 E-13 fluxnum_7: 7 fluxval_7: SURF-LINE(2326) = 1.7 E-13 fluxnum_8: 8 fluxval_8: SURF-LINE(1909) = 3.7 E-13 fluxnum_9: 9 fluxval_9: SURF-CONT(1400) = 5.0 E-14 fluxnum_10: 10 fluxval_10: W-LINE(5019) = 1 ! targnum: 2 name_1: SMC-N83 name_2: NGC456 descr_1: H,503 pos_1: RA = 01H 13M 49.18S +/- 0.2S, pos_2: DEC = -73D 17' 27.40" +/- 2.0", pos_3: TBD-EARLY equinox: 2000 rv_or_z: V = +167 acqpr_1: EXT acqpr_2: BKG comment_1: THIS TARGET REPLACES SMC-N81 DUE comment_2: TO GUIDE STAR AVAILABILITY. fluxnum_1: 1 fluxval_1: V = 13.0, TYPE = B0 V, E(B-V) = 0.02 fluxnum_2: 2 fluxval_2: B-V = -0.3, U-B = -1.1 fluxnum_3: 3 fluxval_3: SURF-LINE(6563) = 1.5 E-12 fluxnum_4: 4 fluxval_4: SURF-LINE(5007) = 2.5 E-12 fluxnum_5: 5 fluxval_5: SURF-LINE(4861) = 4.8 E-13 fluxnum_6: 6 fluxval_6: SURF-LINE(3727) = 5.6 E-13 fluxnum_7: 7 fluxval_7: SURF-LINE(2326) = 1.4 E-14 fluxnum_8: 8 fluxval_8: SURF-LINE(1909) = 7.4 E-14 fluxnum_9: 9 fluxval_9: SURF-CONT(1400) = 8.0 E-14 fluxnum_10: 10 fluxval_10: W-LINE(5019) = 1 ! ! end of fixed targets ! No solar system records found generic_targets: targnum_1: 3 name_1: SMC-N83-GEN descr_1: H,503 criteria_1: RA = 01H 13M 49.18S, criteria_2: DEC = -73D 17' 27.40", criteria_3: R = 20' ! targnum_1: 4 name_1: SMC-N88A-GEN descr_1: H,503 criteria_1: RA = 01H 24M 09.2S, criteria_2: DEC = -73D 09' 17", criteria_3: R = 20' ! ! end of generic targets exposure_logsheet: linenum: 1.100 targname: SMC-N88A config: WFC opmode: IMAGE aperture: WFALL sp_element: F502N num_exp: 1 time_per_exp: 600S s_to_n: 100 fluxnum_1: 4 priority: 1 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = 0.5 req_1: GROUP 1.1,1.2,1.3,1.4,1.5 NO GAP; req_2: CYCLE 3 ! linenum: 1.110 targname: SMC-N88A-GEN config: FOC/96 opmode: IMAGE aperture: 256X1024 sp_element: PRISM1 num_exp: 1 time_per_exp: 1200S s_to_n: 10 fluxnum_1: 1 fluxnum_2: 2 priority: 5 req_1: PAR; req_2: CYCLE 3 comment_1: PARALLEL WITH 1.10 & 1.20 EXPOSURES ! linenum: 1.200 targname: SMC-N88A config: WFC opmode: IMAGE aperture: WFALL sp_element: F656N num_exp: 1 time_per_exp: 600S s_to_n: 100 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = 0.5 req_1: GROUP 1.1,1.2,1.3,1.4,1.5 NO GAP; req_2: CYCLE 3 ! linenum: 1.300 targname: SMC-N88A config: WFC opmode: IMAGE aperture: WFALL sp_element: F336W num_exp: 1 time_per_exp: 100S s_to_n: 300 fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = NO req_1: GROUP 1.1,1.2,1.3,1.4,1.5 NO GAP; req_2: CYCLE 3 ! linenum: 1.310 targname: SMC-N88A-GEN config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 100S s_to_n: 100 fluxnum_1: 1 fluxnum_2: 2 priority: 5 req_1: PAR; req_2: CYCLE 3 comment_1: PARALLEL WITH 1.30 WFC EXPOSURE ! linenum: 1.400 targname: SMC-N88A config: WFC opmode: IMAGE aperture: WFALL sp_element: F439W num_exp: 1 time_per_exp: 30S s_to_n: 500 fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = NO req_1: GROUP 1.1,1.2,1.3,1.4,1.5 NO GAP; req_2: CYCLE 3 ! linenum: 1.500 targname: SMC-N88A config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 10S s_to_n: 1000 fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = NO req_1: GROUP 1.1,1.2,1.3,1.4,1.5 NO GAP; req_2: CYCLE 3 ! linenum: 2.100 targname: SMC-N83 config: WFC opmode: IMAGE aperture: WFALL sp_element: F502N num_exp: 1 time_per_exp: 600S s_to_n: 100 fluxnum_1: 4 priority: 2 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = 0.5 req_1: GROUP 2.1,2.2,2.3,2.4,2.5 NO GAP; req_2: CYCLE 3 ! linenum: 2.110 targname: SMC-N83-GEN config: FOC/96 opmode: IMAGE aperture: 256X1024 sp_element: PRISM1 num_exp: 1 time_per_exp: 1200S s_to_n: 10 fluxnum_1: 1 fluxnum_2: 2 priority: 5 req_1: PAR; req_2: CYCLE 3 comment_1: PARALLEL WITH 2.10 & 2.20 EXPOSURES ! linenum: 2.200 targname: SMC-N83 config: WFC opmode: IMAGE aperture: WFALL sp_element: F656N num_exp: 1 time_per_exp: 600S s_to_n: 100 fluxnum_1: 3 priority: 2 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = 0.5 req_1: GROUP 2.1,2.2,2.3,2.4,2.5 NO GAP; req_2: CYCLE 3 ! linenum: 2.300 targname: SMC-N83 config: WFC opmode: IMAGE aperture: WFALL sp_element: F336W num_exp: 1 time_per_exp: 100S s_to_n: 300 fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = NO req_1: GROUP 2.1,2.2,2.3,2.4,2.5 NO GAP; req_2: CYCLE 3 ! linenum: 2.310 targname: SMC-N83-GEN config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 100S s_to_n: 100 fluxnum_1: 1 fluxnum_2: 2 priority: 5 req_1: PAR; req_2: CYCLE 3 comment_1: PARALLEL WITH 2.30 WFC EXPOSURE ! linenum: 2.400 targname: SMC-N83 config: WFC opmode: IMAGE aperture: WFALL sp_element: F439W num_exp: 1 time_per_exp: 30S s_to_n: 500 fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = NO req_1: GROUP 2.1,2.2,2.3,2.4,2.5 NO GAP; req_2: CYCLE 3 ! linenum: 2.500 targname: SMC-N83 config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 10S s_to_n: 1000 fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: PRE-FLASH = YES, param_2: CR-SPLIT = NO req_1: GROUP 2.1,2.2,2.3,2.4,2.5 NO GAP; req_2: CYCLE 3 ! ! end of exposure logsheet ! No scan data records found