! $Id: 5430,v 11.1 1994/07/27 17:52:21 pepsa Exp $ coverpage: title_1: IMAGING THE UV STARS IN M32 AND NGC 205: CYCLE4MEDIUM sci_cat: GALAXIES & CLUSTERS sci_subcat: STELLAR POPULATIONS proposal_for: GO pi_fname: FRANCESCO pi_lname: BERTOLA pi_inst: DIPARTIMENTO DI ASTRONOMIA UNIVERSITA DI PADOVA pi_country: ITALY pi_phone: 39-49-8293473 hours_pri: 11.16 num_pri: 2 wf_pc: Y off_fname: FRANCESCO off_lname: LUCCHIN off_title: PROF. off_inst: 6470 off_addr_1: DIPARTIMENTO DI ASTRONOMIA off_addr_2: VIC. OSEERVATORIO 5 off_city: PADOVA off_country: ITALY off_phone: 39-49-8293420 ! end of coverpage abstract: line_1: We propose to image with the WFPC2 PC at two effective wavelengths, line_2: namely 1600 and 2180 A, the elliptical galaxies M32 and NGC 205. line_3: Imaging with FOC during Cycle 1 has revealed the line_4: possibility to detect individual UV bright stars on a diffuse line_5: background. Unfortunately remarkable disagreement between the nominal line_6: transmission curves and the ones we derived from our own observations has line_7: not allowed to take properly into account the effects of the readleak line_8: present in the FOC's filters. The much less readleak in WFPC2 PC+F185W line_9: and in WFPC2 PC+F255W makes this configuration the most appropriate one line_10: to investigate the nature of the UV stars, giving rise to the well-known n line_11: rising branch present in the far UV spectrum of early-type galaxies. line_12: The fainter magnitudes which can be reached and the determination of line_13: the (1600-2180) color will allow us to discriminate among the different line_14: candidates, such as P-AGB, P-EAGB, AGB manque`, contributing to the line_15: far UV light. line_16: These two galaxies are among the very few for which direct line_17: identification can be made of the UV bright stars that are line_18: known to exist in old stellar systems. These observations are line_19: prerequisite to our understanding of the source(s) of UV flux in both line_20: present-day galaxies and in galaxies at large lookback time. ! ! end of abstract general_form_proposers: lname: BERTOLA fname: FRANCESCO inst: 6470 country: ITALY esa: Y ! lname: AMICO fname: PAOLA inst: 6470 country: ITALY esa: Y ! lname: BURSTEIN fname: DAVID inst: 1220 country: USA ! lname: DI SEREGO ALIGHIERI fname: SPERELLO inst: 6420 country: ITALY esa: Y ! lname: GREGGIO fname: LAURA inst: 6460 country: ITALY esa: Y ! lname: RENZINI fname: ALVIO inst: 6460 country: ITALY esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to image the central regions of M32 and NGC 205 by using the line_2: WFPC2 centered on PC; the three WF CCD images will be used as well to line_3: obtain a more precise luminosity function and to study whether radial line_4: effects are present or not. We ask for 5 exposures of 30 (or 32) minutes line_5: each (which is the maximum exposure time available per orbit) for each line_6: target for both the F185W and F255W filters. Multiple exposures are line_7: desired for removal of cosmic rays. The F185W filter, centered at 1600 A, line_8: is highly efficient below 2000 A and has essentially no redleak beyond line_9: 2500 A. It will measure the flux from the hottest stars in the galaxies line_10: and it will cut completely off stars colder than 10,000 K, thanks to the line_11: absence of redleak. The F255W filter, centered at 2180 A, is more line_12: efficient than F185W, except for the hottest objects, and will permit a line_13: quantitative separation of the flux from the hottest stars from those of line_14: the main sequence. The F255 exposures require a redleak check for line_15: possible stellar contamination by bright, red AGB stars and for flux line_16: redder than 2800A. We will take two F675W exposures of each galaxy to line_17: detect individual bright AGB stars that could contaminate our UV images. line_18: The redder continuum flux will be determined by a combination of line_19: of IUE spectral energy distributions, HST WFPC2 F336W observations, line_20: WFPC2 efficiency curves and ground-based UBVRI CCD images. line_21: The (1600-2180) UV color given by the two WFPC2 filters never completely line_22: saturates, thus allowing better discrimination among the possible line_23: contributors to the UV light (P-AGB, P-EAGB, AGB manque`), as well ! question: 3 section: 2 line_1: as estimation of the color of the fraction of light from possible line_2: unresolved contributors (Hot-HB stars). We expect to detect individual line_3: UV bright stars in each of the two galaxies, based on our experience line_4: with the HST/FOC in Cycle 1. These WFPC2 observations will go line_5: three magnitudes deeper and permit accurate determination of the UV line_6: luminosities and colors, as well as a statistical study of the line_7: UV luminosity function for PAGB stars. All of this information can line_8: be used to constrain the ages and metallicities of these UV stars. ! question: 4 section: 1 line_1: We need the unique imaging capability of HST in the ultraviolet, since line_2: this is the wavelength range where hot stars emit most of their radiation line_3: and are not overwhelmed by the normal cool stars present in very large line_4: numbers in early-type galaxies. We should be able to detect individually line_5: all kinds of hot stars (except the Hot HB) present in our objects, due to line_6: the sharpness of the HST PSF and the good discrimination against faint line_7: red stars in the UV. High angular resolution is also necessary to isolate line_8: crowded objects against a non negligible background and to reach faint line_9: limiting magnitudes. The new Woods filter F185W and the F255W filter will line_10: provide, thanks to the improved sensitivity and to the very low redleak line_11: measurements of the color. This proposal represents an improvement of line_12: our Cycle 1 proposal, especially because it will take advantage of the line_13: UV color to discriminate among various types of UV stars. It is also a line_14: complement to our Cycle 2 proposal, where we study the main features of line_15: the UV SEDs of a sample of early-type galaxies as a function of the line_16: radius in these galaxies. The observations here proposed represent line_17: the completion of a long term project carried out by the proposers line_18: both from the ground (Lick Observatory) and from space (IUE), as well as line_19: through theoretical modelling of the late stages of stellar evolution. line_20: We plan to get ten consecutive far-UV exposures of two objects by using line_21: WFPC2 PC with F185W Woods filter for the first five exposures and with line_22: F255W filter for the other five. For redleak check of the F255W filter, line_23: we plan 2 exposures per object with F675W filter to discriminate against ! question: 4 section: 2 line_1: AGB stars, and two exposures per object in the F336W filter to measure line_2: redder continuum flux. Limiting detectable absolute bolometric magnitude, line_3: Mbol, at the distance of M32 (m-M=24.2), has been calculated for UV line_4: bright stars for: 1) The (WFPC2+F185W) filter configuration (2.5 hr line_5: exposure) using the F185W filter trasmission and the OTA+WFPC2 line_6: WFPC2 efficiency curves. Sky background is assumed to be V=23.0 line_7: mag/arcsec^2, but it is not critical as the CCD readout noise is the line_8: dominant source of noise. 2) The (WFPC2+F255W) filter configuration line_9: (2.5 hr exposure), calculated in the same way as for the F185W filter. line_10: These combinations of filter configuration + exposure time permit line_11: us to reach the Mbol values of AGB-manque' stars with a S/N considerably line_12: greater than 5 (which is the value used for our limiting magnitudes). line_13: We have also estimated the UV colors c(160-218) formed by these two line_14: filters, assuming that a star with Te=10,000K has c(160-218)=0.00. line_15: These calculations were presented in a figure inserted in the Phase I line_16: proposal. As shown in that figure, with exposure times of 2.5hr, we can line_17: detect UV bright stars at a S/N of 5 to a limiting Mbol of +1.5 to -1.0, line_18: depending on the effective temperature of the star. c(160-218) colors line_19: do not saturate for any proposed UV bright star in these galaxies: for line_20: for objects with Mbol 0.7, 2.1 and 3.3 magnitudes brighter than the line_21: limits, colors should be accurate within 0.3, 0.1 and 0.03 mag, resp. line_22: Thus both colors and magnitudes will discriminate among different line_23: proposed models for the orign of UV bright stars. ! question: 5 section: 1 line_1: No special scheduling requirements. ! question: 6 section: 1 line_1: We expect the absolute calibration provided by the routine calibrations line_2: to be within 10% for both our filters and that the relative calibration line_3: between the two filters in order, to obtain colors, be within 5%. line_4: The F675W exposures are being taken as a check against bright, red AGB line_5: stars (which have similar Mbol as the PAGB stars, but far lower effective line_6: temperatures) contaminating the UV exposures. The F336W exposures are line_7: part of the test for redleak contamination of continuum flux in the line_8: F255W filter. HST is required for both of these observations. The line_9: remaining redleak information will come from existing IUE spectral line_10: energy distributions and ground-based acquired UBVRI CCD imagery. ! ! question: 8 section: 1 line_1: No special scheduling requests. ! question: 9 section: 1 line_1: P2719:PAGB STARS IN ELLIPTICAL AND BULGE DOMINATED GALAXIES line_2: (F. Bertola, D. Burstein, S. di Serego Alighieri) It is strictly related line_3: to the present proposal as it concerned the first UV observations of the line_4: three galaxy NGC205, NGC221 and NGC224 with the FOC/48. The data were line_5: collected in October/November 1991. We have detected and measured the line_6: individual hot stars responsible for the UV rising branch in those line_7: galaxies. Unfortunately the limitations imposed by the spherically line_8: aberrated PSF made detectable only the brightest stars (PAGB), leaving line_9: unresolved the contribution of the fainter stars, hence making impossible line_10: to distinguish among all the possible contributions to thE total UV flux line_11: (PEAGB, Hot-HB, AGB-manque` stars). line_12: P2579:THE CALIBRATION OF THE WHITE DWARF DISTANCE SCALE FOR GLOBULAR line_13: CLUSTERS (A. Renzini). line_14: P2570:RECENT MASS EJECTION FROM PLANETARY NEBULA NUCLEI. (A. Renzini) line_15: P2298:STELLAR POPULATIONS OF GLOBULAR CLUSTERS & GALAXIES (D. Burstein) line_16: We obtained UV spectra of two M31 globular clusters and are in the line_17: process of analyzing these data. Little far-UV flux is detected from line_18: these clusters, revising knowledge obtained from IUE. Good spectra at line_19: 10A resolution were obtained from 2500-4800A, and will provide accurate line_20: flux distributions and line indices for stellar population models. line_21: Hence we feel our program has been partly successful. line_22: P3457:OPTICAL/ULTRAVIOLET BEAMING IN THE RADIO GALAXY PKS 2152-69 line_23: (S. di Serego Alighieri) ! question: 9 section: 2 line_1: P3728:IMAGING THE HOT STELLAR CONTENT OF EARLY-TYPE GALAXIES (F. Bertola, line_2: P. Amico, D. Burstein, S. di Serego Alighieri, L. Greggio, A. Renzini) line_3: This program is directly related to the present proposal. It is meant to line_4: derive complete SEDs, as a function of the distance from the center, for line_5: the two-dimensional images of early-type galaxies in four passbands. The line_6: calibration of our filter system will allow us to apply it to the line_7: bidimensional analisys of the general sample of early-type galaxies, it line_8: will provide important insight in the stellar populations, in particular line_9: the one responsible for the UV emission, and in their formation and line_10: evolution. The observations are scheduled in the next few months. line_11: P3448:THE ULTRAVIOLET EVOLUTION OF ELLIPTICAL GALAXIES AT MODERATE line_12: REDSHIFT.(A. Renzini) line_13: P3545:THE EVOLUTION OF THE UV SPECTRA OF EARLY-TYPE GALAXIES. line_14: (F. Bertola, A. Renzini). This program performed FOS spectroscopy and line_15: WFC or FOC imaging on 7 weak radio galaxies with z=0.1-0.6. It is meant t line_16: to study the evolution with lookback time of the UV rising branch in line_17: elliptical galaxies. 5 objects have been observed sofar.The spectra will line_18: directly trace the evolution of the ratio of the UV upturn (old stars?) line_19: and any flat spectrum component (young stars). line_20: P4559, Cycle 3: STELLAR POPULATIONS OF GLOBULAR CLUSTERS AND GALAXIES line_21: (D. Burstein). P4559: This program is a follow-up of P2298, in which we line_22: will take FOS spectra of M33 globular clusters and the nuclei of M31 and d line_23: M32. ! question: 10 section: 1 line_1: Padova: Vax 4000 + MIDAS reduction Package and SUN Sparcstation 2 GX+1.8 line_2: Gb disk + IRAF reduction package. line_3: Asu: DEC 5000-200 + DEC 3100 workstations, 3.6Gb disk; associated I/O line_4: devices; in a net with other workstations. IRAF, IDL runs on network. line_5: Arcetri: a Sun workstation running MIDAS and IRAF/STSDAS. line_6: Adequate resources are available also at the Institutions of the C0-I's. ! !end of general form text general_form_address: lname: BERTOLA fname: FRANCESCO category: PI inst: 6470 addr_1: DIPARTIMENTO DI ASTRRONOMIA addr_2: VIC. OSSERVATORIO 5 city: PADOVA country: ITALY phone: 39-49-8293473 telex: BERTOLA@ASTRPD.ASTRO.IT ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC221 descr_1: E,303,B,130,131,184 pos_1: RA = 0H 42M 41.71S +/- 0.05S, pos_2: DEC = +40D 51' 54.1" +/- 0.5" equinox: 2000 rv_or_z: V = -217 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE FOR THE comment_2: BRIGHTEST PAGB STAR. FLUXVAL_3 IS comment_3: UV FLUX FOR THE BRIGHTEST PAGB STAR comment_4: FLUXVAL_4 IS UV FLUX FOR THE comment_5: FAINTEST AGB-MANQUE` STAR. comment_6: FLUXVAL_5 IS ESTIMATED I BAND FLUX comment_7: FOR TYPICAL AGB RED STAR fluxnum_1: 1 fluxval_1: V=23 fluxnum_2: 1 fluxval_2: B-V=-0.3 fluxnum_3: 2 fluxval_3: F-CONT(1800)=7+/-5E-17 fluxnum_4: 3 fluxval_4: F-CONT(1800)=4+/-1E-18 fluxnum_5: 4 fluxval_5: I=20+/-1 ! targnum: 2 name_1: NGC205 descr_1: E,303,B,130,131,184 pos_1: RA = 0H 40M 22.03S +/- 0.05S, pos_2: DEC = +41D 41' 7.4" +/- 0.5" equinox: 2000 rv_or_z: V = -239 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE FOR THE comment_2: BRIGHTEST PAGB STAR. FLUXVAL_3 IS comment_3: UV FLUX FOR THE BRIGHTEST PAGB STAR comment_4: FLUXVAL_4 IS UV FLUX FOR THE comment_5: FAINTEST AGB-MANQUE` STAR. comment_6: FLUXVAL_5 IS ESTIMATED I BAND FLUX comment_7: FOR TYPICAL AGB RED STAR fluxnum_1: 1 fluxval_1: V=23+/-3 fluxnum_2: 1 fluxval_2: B-V=-0.3 fluxnum_3: 2 fluxval_3: F-CONT(1800)=7+/-5E-17 fluxnum_4: 3 fluxval_4: F-CONT(1800)=4+/-1E-18 fluxnum_5: 4 fluxval_5: I=20+/-1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.110 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F185W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1600S s_to_n: 5 fluxnum_1: 3 priority: 1 req_1: CYCLE 4 / 1.11-2.43; req_2: POS TARG 0,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. linenum: 1.120 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F185W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1600S s_to_n: 5 fluxnum_1: 3 priority: 1 req_1: SAME ORIENT FOR 1.12-1.43 AS 1.11; req_2: POS TARG -0.023,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. linenum: 1.130 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F185W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1600S s_to_n: 5 fluxnum_1: 3 priority: 1 req_1: POS TARG -0.0115,-0.023; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 1.210 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F255W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1500S s_to_n: 5 fluxnum_1: 3 priority: 2 req_1: POS TARG 0,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 1.220 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F255W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1500S s_to_n: 5 fluxnum_1: 3 priority: 2 req_1: POS TARG -0.023,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 1.230 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F255W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1500S s_to_n: 5 fluxnum_1: 3 priority: 2 req_1: POS TARG -0.0115,-0.023; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 1.310 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F675W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 50S s_to_n: 5 fluxnum_1: 4 priority: 3 req_1: POS TARG 0,0; comment_1: RED LEAK CHECK FOR comment_2: INDIVIDUAL RED AGB STARS comment_3: S_TO_N FOR FAINTEST AGB comment_4: STAR TO BE DETECTED ! linenum: 1.320 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F675W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 50S s_to_n: 5 fluxnum_1: 4 priority: 3 req_1: POS TARG -0.023,0; comment_1: RED LEAK CHECK FOR comment_2: INDIVIDUAL RED AGB STARS comment_3: S_TO_N FOR FAINTEST AGB comment_4: STAR TO BE DETECTED ! linenum: 1.330 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F675W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 50S s_to_n: 5 fluxnum_1: 4 priority: 3 req_1: POS TARG -0.0115,-0.023; comment_1: RED LEAK CHECK FOR comment_2: INDIVIDUAL RED AGB STARS comment_3: S_TO_N FOR FAINTEST AGB comment_4: STAR TO BE DETECTED ! linenum: 1.410 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F336W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 400S s_to_n: 5 fluxnum_1: 3 priority: 3 req_1: POS TARG 0,0; comment_1: RED LEAK CHECK FOR comment_2: CONTIUUM BETWEEN 3100A comment_3: AND 3500A. S_TO_N EST. comment_4: FOR FAINT INDIV. STAR ! linenum: 1.420 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F336W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 400S s_to_n: 5 fluxnum_1: 3 priority: 3 req_1: POS TARG -0.023,0; comment_1: RED LEAK CHECK FOR comment_2: CONTIUUM BETWEEN 3100A comment_3: AND 3500A. S_TO_N EST. comment_4: FOR FAINT INDIV. STAR ! linenum: 1.430 targname: NGC221 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F336W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 400S s_to_n: 5 fluxnum_1: 3 priority: 3 req_1: POS TARG -0.0115,-0.023; comment_1: RED LEAK CHECK FOR comment_2: CONTIUUM BETWEEN 3100A comment_3: AND 3500A. S_TO_N EST. comment_4: FOR FAINT INDIV. STAR ! linenum: 2.110 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F185W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1600S s_to_n: 5 fluxnum_1: 3 priority: 1 req_1: POS TARG 0,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 2.120 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F185W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1600S s_to_n: 5 fluxnum_1: 3 priority: 1 req_1: POS TARG -0.023,0; req_2: SAME ORIENT FOR 2.12-2.43 AS 2.11; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 2.130 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F185W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1600S s_to_n: 5 fluxnum_1: 3 priority: 1 req_1: POS TARG -0.0115,-0.023; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 2.210 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F255W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1500S s_to_n: 5 fluxnum_1: 3 priority: 2 req_1: POS TARG 0,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 2.220 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F255W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1500S s_to_n: 5 fluxnum_1: 3 priority: 2 req_1: POS TARG -0.023,0; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 2.230 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F255W param_1: CR-SPLIT=NO num_exp: 2 time_per_exp: 1500S s_to_n: 5 fluxnum_1: 3 priority: 2 req_1: POS TARG -0.0115,-0.023; comment_1: S_TO_N ESTIMATE FOR comment_2: FAINTEST UV STARS ONLY; comment_3: BRIGHTEST STARS DETECTED comment_4: AT S_TO_N FROM 10 TO 50. ! linenum: 2.310 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F675W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 50S s_to_n: 5 fluxnum_1: 4 priority: 3 req_1: POS TARG 0,0; comment_1: RED LEAK CHECK FOR comment_2: INDIVIDUAL RED AGB STARS comment_3: S_TO_N FOR FAINTEST AGB comment_4: STAR TO BE DETECTED ! linenum: 2.320 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F675W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 50S s_to_n: 5 fluxnum_1: 4 priority: 3 req_1: POS TARG -0.023,0; comment_1: RED LEAK CHECK FOR comment_2: INDIVIDUAL RED AGB STARS comment_3: S_TO_N FOR FAINTEST AGB comment_4: STAR TO BE DETECTED ! linenum: 2.330 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F675W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 50S s_to_n: 5 fluxnum_1: 4 priority: 3 req_1: POS TARG -0.0115,-0.023; comment_1: RED LEAK CHECK FOR comment_2: INDIVIDUAL RED AGB STARS comment_3: S_TO_N FOR FAINTEST AGB comment_4: STAR TO BE DETECTED ! linenum: 2.410 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F336W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 400S s_to_n: 5 fluxnum_1: 3 priority: 3 req_1: POS TARG 0,0; comment_1: RED LEAK CHECK FOR comment_2: CONTIUUM BETWEEN 3100A comment_3: AND 3500A. S_TO_N EST. comment_4: FOR FAINT INDIV. STAR ! linenum: 2.420 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F336W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 400S s_to_n: 5 fluxnum_1: 3 priority: 3 req_1: POS TARG -0.023,0; comment_1: RED LEAK CHECK FOR comment_2: CONTIUUM BETWEEN 3100A comment_3: AND 3500A. S_TO_N EST. comment_4: FOR FAINT INDIV. STAR ! linenum: 2.430 targname: NGC205 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F336W param_1: CR-SPLIT=NO num_exp: 1 time_per_exp: 400S s_to_n: 5 fluxnum_1: 3 priority: 3 req_1: POS TARG -0.0115,-0.023; comment_1: RED LEAK CHECK FOR comment_2: CONTIUUM BETWEEN 3100A comment_3: AND 3500A. S_TO_N EST. comment_4: FOR FAINT INDIV. STAR ! ! end of exposure logsheet ! No scan data records found