! $Id: 5394,v 5.1 1994/07/27 17:28:21 pepsa Exp $ coverpage: title_1: INTERSTELLAR ABUNDANCES IN THE SMC - IMPLICATIONS FOR QSO ABSORPTION- title_2: LINE SYSTEMS AND FOR CHEM EV OF UNIVERSE-CYC 4 MED EARLY ACQ FOR 5608 sci_cat: INTERSTELLAR MEDIUM sci_subcat: ABSORPTION LINES proposal_for: GO pi_fname: DANIEL pi_mi: E. pi_lname: WELTY pi_inst: UNIVERSITY OF CHICAGO pi_country: USA pi_phone: (312)702-0599 hours_pri: 7.34 num_pri: 1 wf_pc: Y hrs: Y time_crit: Y off_fname: MARY off_lname: BRANDON off_title: ACTING DIR, RESEARCH off_inst: 1710 off_addr_1: 970 EAST 58TH STREET off_city: CHICAGO off_state: IL off_zip: 60637 off_country: USA off_phone: (312)702-8604 ! end of coverpage abstract: line_1: We propose a detailed study of the interstellar (IS) abundances and depletions line_2: for one line of sight in the SMC - a nearby low metallicity, low dust-to-gas line_3: ratio system where stellar abundance data are also available. We will use the line_4: GHRS ECH-B to obtain absorption-line profiles of Zn II, Cr II, Si II, line_5: Fe II, Mn II, Mg II, and Al III, to determine both the detailed component line_6: structures and the relative abundances of those species in the various line_7: components. We will use the derived component structures to obtain similarly line_8: detailed abundances for S II, Ni II, and Al II from existing lower resolution line_9: short-wavelength IUE spectra (in which severe blending of components has to now line_10: prevented accurate abundance determinations). In addition to the intrinsic line_11: interest in obtaining detailed IS abundance and depletion data for an external line_12: galaxy quite different from our own, such data are needed for interpreting line_13: the abundance patterns found in QSO absorption-line systems. A number of the line_14: QSOALS examined to date seem to exhibit overall metallicities of about 0.1 x line_15: Solar, with some additional depletion of refractory elements. If the pattern of line_16: that depletion can be constrained, then the build-up of many elements can be line_17: traced, via the QSOALS, from redshifts 3.5 to 0.5 - with significant line_18: implications for the formation and evolution of galaxies. ! ! end of abstract general_form_proposers: lname: WELTY fname: DANIEL mi: E. inst: 1710 country: USA ! lname: BLADES fname: J. mi: C. inst: 3470 country: USA ! lname: HOBBS fname: LEWIS mi: M. inst: 1710 country: USA ! lname: LAUROESCH fname: JAMES mi: T. inst: 1710 country: USA ! lname: YORK fname: DONALD mi: G. inst: 1710 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The GHRS will be used in echelle mode, using the small science line_2: aperture and breaking long exposures into series of 5-minute sub-exposures at line_3: several slightly different central wavelengths in order to minimize the effects line_4: of magnetic drift and detector non-uniformities. The particular lines to be line_5: observed have been selected to cover a range of strengths for species usually line_6: dominant in neutral regions (both depleted and undepleted elements); tracers of line_7: ionized gas are also included. The range in line strengths is designed to line_8: enable both weak and strong components to be reliably identified and separated. line_9: The following table lists for each wavelength setting the lines to be observed, line_10: their depletion behavior, and their strength in the 3 blended features noted in line_11: IUE spectra of HD 5980 by Fitzpatrick & Savage (1983): line_12: - Strength in blend at - line_13: - Setting Ion Wavelengths depletion? 0/ 140/ 300 km/s (mA) - line_14: - - line_15: - 1) Zn II (2062) undepleted 70/ 40/ - - line_16: - Cr II (2056,2062) quite depleted 15/ 40/ - - line_17: - 2) Fe II (2586) quite depleted 310/1040/ ? - line_18: - Mn II (2593) moderately depleted 80/ 60/ - - line_19: - 3) Fe II (2260) quite depleted (weak; not reported) - line_20: - 4) Mg II (2795,2803) weakly depleted 390/1600/170 - line_21: - 5) Al III (1854) (ionized gas) 90/ 150/ - - line_22: - 6) Si II (1808) moderately depleted 110/ 230/ - - line_23: - - ! question: 3 section: 2 line_1: In order to adequately detect the individual subcomponents of these blends, we line_2: will need detection limits (2-sigma) better than about 3 mA for the weak lines line_3: (2260, 2056, 2062) and better than about 5 mA for the other, stronger lines. line_4: We will thus need S/N = 35-40 for the weak lines and 25-30 for the stronger line_5: lines. ! question: 4 section: 1 line_1: The lines for the desired species all lie in the UV; high resolution and line_2: sensitivity are essential. Eighteen short-wavelength IUE spectra exist for line_3: HD 5980 - which was one reason for its selection for this study - line_4: so that decent S/N should be achievable below about 2100 Angstroms. There are line_5: only two relatively poor long-wavelength IUE spectra, however. It is the lack line_6: of adequate spectral resolution, however, that has prevented determination of line_7: accurate abundances for the various types of regions inferred to be present line_8: along these lines of sight, due to the presence of multiple, closely spaced line_9: components. Although Wayte (1990) did not observe this star, his 5 km/s line_10: Ca II data toward other LMC and SMC stars give an indication of the IS component line_11: structure present that cannot be distinguished in the existing IUE data, but line_12: which will be distinguished at the 3.5 km/s resolution of ECH-B (see also line_13: Fig. 4). The lines to be observed span a range in strength, depletion, and line_14: environment, and should provide sufficient information for determining both the line_15: detailed component structure of this line of sight and the abundances of line_16: the various species in each of those distinct components. The Zn II and Cr II line_17: lines near 2060, which give direct, initial estimates for the metallicity and line_18: depletion, are being observed in a number of QSOALS. The other species are line_19: needed for detailed comparisons with depletion and nucleosynthesis patterns. line_20: Knowledge of the detailed component structure should enable us to derive line_21: similarly detailed column densities for species from the lower resolution (but line_22: adequate S/N) short-wavelength IUE data (e.g., Ni II, S II, Al II). line_23: Some useful information on the detailed component structure could be ! question: 4 section: 2 line_1: obtained from high-resolution ground-based observations of Na I and Ca II, but line_2: those are generally trace ionization states in neutral regions, and also are line_3: typically not strong enough to reveal some of the weaker components. line_4: For the lines to be observed, the blended features observed in existing IUE line_5: spectra range in strength from about 20 to 1600 mA - so that we will need a line_6: sensitivity of about 3 mA (2-sigma) for accurate delineation of the weakest line_7: individual components in the weakest lines (Zn II and Cr II are critical). The line_8: following table uses fluxes from low-resolution IUE spectra, line_9: the OTA + GHRS + ECH system sensitivities from the GHRS manual, line_10: a factor 2/3 to account for the loss of throughput through the SSA, a factor line_11: 0.9 to account for 10% background time, and the effects of the echelle line_12: blaze function. HD 5980 is among the brightest SMC stars in the UV, and there line_13: are short-wavelength IUE spectra of decent S/N available. line_14: - - line_15: wavelength 2060 2590 2260 2800 1855 1808 - line_16: flux (erg/cm2 s A) 1.3e-12 7.1e-13 8.5e-13 6.3e-13 1.6e-12 1.8e-12 - line_17: sensitivity 4.5e+11 1.2e+12 8.5e+11 1.2e+12 1.6e+11 1.1e+11 - line_18: blaze factor 0.70 0.80 0.95 0.95 0.85 0.97 - line_19: count rate (/min diode) 14.7 24.5 24.7 25.9 7.8 6.9 - line_20: exp. time (min) 100 60 60 40 60 90 - line_21: total counts 1474 1472 1483 1034 470 622 - line_22: S/N 38 38 39 32 22 25 - line_23: 2-sigma eq. width (mA) 2.7 3.3 2.9 4.4 4.2 3.6 - ! question: 5 section: 1 line_1: The SMC star to be observed, HD 5980, is an eclipsing binary, and should be line_2: observed at maximum brightness to maximize the S/N. The period is 19.266 +/- line_3: 0.003 days; the reference date for zero phase is JD = 2443158.771; the primary line_4: and secondary minima are at phases 0.00 and 0.36, respectively; each minimum line_5: lasts about 2 days. The observations should thus be obtained between phases line_6: 0.05 and 0.31 or between phases 0.41 and 0.95. We also plan to obtain a line_7: single WFPC2 image of the field prior to the spectroscopic observations, in line_8: order to assure a successful acquisition in the GHRS SSA (there may be a line_9: close companion). ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: 3993, 2251, 4798, "The Properties of Single Interstellar Clouds" (Cycle 1) line_2: PI = Hobbs; with Morton, Spitzer, Welty, York line_3: 3472, 4826, "The Properties of Single Interstellar Clouds" (Cycle 2) line_4: PI = Hobbs; with Morton, Spitzer, Welty, York line_5: 3482, "Variable Infalling Material on Beta Pictoris" (Cycle 2) line_6: PI = Vidal-Madjar; with Hobbs and others line_7: 4510, "The Evolution of Boron" (Cycle 3) line_8: PI = Duncan; with Hobbs and others line_9: Blades is PI or co-I on the following: line_10: 2553, 3755, "Absorption Cross-Sections of Nearby Galaxies" (1 and 2) line_11: 2563, 3853, 4016, 4022, "Supernova Intensive Study" (1 and 2) line_12: 2638, "Near-UV Spectrum of 0215+015" (1; ToO) line_13: 2644, 3676, "Environments of Starburst Galaxies" (1 and 2) line_14: 3525, "ISM of Nearby Galaxies Using SN as Probes" (2; ToO) line_15: 3761, "UV Spectroscopy of CO in Seyfert Galaxies" (2) line_16: Blades is also a part of several GTO/FOC programs (1235,3179; 1259,3231; line_17: 1263; 1265,3747,4075) and the GTO/HRS program 1306 line_18: The "Single IS Clouds" program(s) have some common goals, in that they line_19: use the echelle to determine detailed component structures for a number of line_20: elements for a set of 12 Galactic lines of sight - in order to obtain line_21: temperatures, densities, abundances, and sizes of individual IS clouds. We line_22: have received almost all of the Cycle 1 data, but none of the Cycle 2 data; line_23: reductions of the data in hand are proceding. Some initial results are the ! question: 9 section: 2 line_1: discovery of IS Tin, which with the abundances of several other heavy elements line_2: has clarified the pattern of depletion in the Galactic ISM; a detailed study of line_3: the line of sight to 23 Ori; an examination of collisionally ionized gas at high line_4: velocities in several lines of sight; and a study of the relative abundances of line_5: lightly depleted elements in individual clouds. (The latter three are in line_6: preparation.) line_8: "Heavy Elements in the Interstellar Medium: Copper, Germanium, Gallium, Krypton, line_9: and Tin", Welty, Hobbs, Morton, Spitzer, & York, poster paper given at The line_10: First Symposium on the Infrared Cirrus and Diffuse Interstellar Clouds, line_11: Tucson, AZ, April 1993 line_12: "The Interstellar Abundances of Tin and Four Other Heavy Elements", Hobbs, line_13: Welty, Morton, Spitzer, & York, ApJ, in press, 1993 line_14: "Interstellar Mg II and C IV Absorption toward Mrk 205 by NGC 4319: An line_15: 'Optically-Thick' QSO Absorption System", Bowen, & Blades, ApJ, 403, L55, line_16: 1993 line_17: "Imaging of Four Planetary Nebulae in the Magellanic Clouds Using the HST FOC", line_18: Blades et al, ApJ, 398, L41, 1992 line_19: "Preliminary Analysis of an Ultraviolet HST FOC Image of the Center of M31", line_20: King et al, ApJ, 397, L35, 1992 line_21: "Discovery of an Optical Synchrotron Jet in 3C 264", Crane et al, ApJ, 402, L37, line_22: 1993 line_23: Blades has also collaborated on 12 additional FOC papers ! question: 10 section: 1 line_1: We will have access to the necessary computational resources and line_2: software at Chicago. ! !end of general form text general_form_address: lname: WELTY fname: DANIEL mi: E. category: PI inst: 1710 addr_1: University of Chicago addr_2: Astronomy and Astrophysics Center addr_3: 5640 S. Ellis Ave. city: Chicago state: IL zip: 60637 country: USA phone: (312)702-0599 telex: welty@oddjob.uchicago.edu ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC346-E-REF descr_1: J,701,702, descr_2: D,202 pos_1: RA = 00H 59M 29.4S +/- 1.3", pos_2: DEC = -72D 10' 20.8" +/- 1.3" equinox: 2000 rv_or_z: V = 182 comment_1: FLUX IS FOR HD5980 (BRIGHTEST comment_2: STAR IN FIELD); comment_3: SHOULD ALSO INCLUDE SK 80; comment_4: THIS MAY BE A CVZ TARGET fluxnum_1: 1 fluxval_1: V=11.7 +/- 0.1 fluxnum_2: 1 fluxval_2: B-V=-0.22 +/- 0.01 fluxnum_3: 2 fluxval_3: E(B-V)=0.07 +/- 0.01 fluxnum_4: 4 fluxval_4: F-CONT(2260) = 8.5 +/- 0.1 E-13 fluxnum_5: 5 fluxval_5: F-CONT(2590) = 7.1 +/- 0.1 E-13 fluxnum_6: 6 fluxval_6: F-CONT(2800) = 6.3 +/- 0.1 E-13 ! targnum: 2 name_1: HD5980 name_2: SK78 descr_1: B,103, descr_2: H,508,509,510,506 pos_1: RA = 00H 59M 26.5S +/- 1.3", pos_2: DEC = -72D 09' 54.0" +/- 1.3" equinox: 2000 rv_or_z: V = 182 acqpr_1: COMP comment_1: ECLIPSING BINARY; comment_2: PERIOD=19.266+/-0.003 DAYS; comment_3: PHASE=0 AT JD=2443158.771; comment_4: MINIMA AT PHASE 0.0 AND 0.36; comment_5: MINIMA LAST ABOUT 2 DAYS; comment_6: MEMBER NGC346 IN SMC; comment_7: MAY HAVE CLOSE COMPANION; comment_8: THIS MAY BE A CVZ TARGET fluxnum_1: 1 fluxval_1: V=11.7 +/- 0.1 fluxnum_2: 1 fluxval_2: B-V=-0.22 +/- 0.01 fluxnum_3: 2 fluxval_3: E(B-V)=0.07 +/- 0.01 fluxnum_4: 4 fluxval_4: F-CONT(1808) = 1.8 +/- 0.1 E-12 fluxnum_5: 5 fluxval_5: F-CONT(1855) = 1.6 +/- 0.1 E-12 fluxnum_6: 6 fluxval_6: F-CONT(2060) = 1.3 +/- 0.1 E-12 fluxnum_7: 7 fluxval_7: F-CONT(2260) = 8.5 +/- 0.1 E-13 fluxnum_8: 8 fluxval_8: F-CONT(2590) = 7.1 +/- 0.1 E-13 fluxnum_9: 9 fluxval_9: F-CONT(2800) = 6.3 +/- 0.1 E-13 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 11.000 targname: NGC346-E-REF config: WFPC2 opmode: IMAGE aperture: WF3-FIX sp_element: F255W num_exp: 1 time_per_exp: 3.0S fluxnum_1: 1 priority: 1 param_1: SUM=1X1, param_2: READ=YES, param_3: CR-SPLIT=NO, param_4: CLOCKS=NO, param_5: ATD-GAIN=15 req_1: CYCLE 4; comment_1: EXPECT MAX OF 1E4-3E4 COUNTS comment_2: IN ANY SINGLE PIXEL comment_3: THIS EARLY ACQ HAS BEEN SPLIT comment_4: FROM THE GHRS SCIENCE. comment_5: EARLY ACQ FOR PROGRAM 5608 ! ! end of exposure logsheet ! No scan data records found