! ! Hubble Space Telescope ! Cycle 4 (1993) Phase II Proposal Template ! ! for use with the ! Remote Proposal Submission System (RPSS) ! ! ! See the Phase II Proposal Instructions for more detailed instructions: ! ! 1. Other documents you may need include: the RPSS User's Manual, the ! RPSS Resource Estimator Instructions, the Instrument Handbooks, the ! Target Acquisition Handbook, the Solar System Target List Instructions, ! the STScI Calibration Plan, the Exposure Catalog, and the Archived ! Exposures Catalog (AEC), all of which should be available in your ! institution's library. These documents can also be obtained by contacting ! the User Support Branch at STScI (usb@stsci.edu or 800-544-8125). ! ! 2. Enter the keyword values on the same line, after the keyword and the colon. ! Leading blank spaces after keywords are ignored. Character types/limits are ! listed for most keywords: X means text, I means integer. For example, ! X20 means text string of <= 20 characters, and 4732 is legal for I4. ! ! 3. Anything after a "!" is ignored, and may be deleted before submission. ! Any unused keywords may also be deleted prior to submission. ! ! 4. After completing this template, run CHECK to search for syntax ! errors. After correcting all syntax errors, run VALIDATE . ! After correcting all the validation errors (see the .ERR files), run ! RESOURCE to estimate the amount of spacecraft time the proposal ! will require. If you need to make manual corrections to your spacecraft time ! estimate, edit the .RESOURCE file accordingly before you e-mail it to STScI. ! Once you are convinced that the proposal is complete and error-free, ! run SUBMIT from your RPS account. An acknowledgement message ! will be sent to your RPS account, containing a submission ID (ex: R123). ! ! 5. After submitting your program, fill-out an Electronic Submission Form -- ! one should be available in your RPS account. Append your Resource Summary ! (the .RESOURCE file) to the form, and e-mail it to usb@stsci.edu before ! the Phase II deadline. STScI will not begin working on your program until ! we receive your completed Submission Form. COVERPAGE: TITLE_1:INTERSTELLAR ABUNDANCES IN THE SMC - IMPLICATIONS FOR QSO ABSORPTION- TITLE_2:LINE SYSTEMS AND FOR THE CHEMICAL EVOLUTION OF THE UNIVERSE - CYCLE 4 MEDIUM SCI_CAT:INTERSTELLAR MEDIUM SCI_SUBCAT:ABSORPTION LINES PROPOSAL_FOR:GO TIME_CRIT:Y ! Item #9: Time-critical obs., or CVZ target? Y or blank PI_FNAME:DANIEL PI_MI:E. PI_LNAME:WELTY PI_INST:UNIVERSITY OF CHICAGO ! PI's institution, X60 PI_COUNTRY:USA ! PI's country, X20 PI_PHONE:(312)702-0599 HOURS_PRI: 7.34 HOURS_PAR: 0.00 NUM_PRI: 1 NUM_PAR: 0 ! Indicate which instruments are requested; enter Y or leave blank: WF_PC: ! Wide Field Planetary Camera 2 FOC: ! Faint Object Camera FOS: ! Faint Object Spectrograph HRS:Y ! (Goddard) High Resolution Spectrograph FGS: ! Fine Guidance Sensors ! Authorizing Institution Official: OFF_FNAME:MARY ! First name of authorizing official, X20 OFF_LNAME:BRANDON ! Last name of authorizing official, X20 OFF_TITLE:ACTING DIR, RESEARCH ! Title of authorizing official, X20 OFF_INST:1710 ! Institution number (or full institution name), X60 OFF_ADDR_1:970 EAST 58TH STREET ! Address of authorizing official, X60 OFF_CITY:CHICAGO ! City, X20 OFF_STATE:IL ! State, X3 OFF_ZIP:60637 ! Zip Code, X9 OFF_COUNTRY:USA ! Country, X20 OFF_PHONE:(312)702-8604 ! Telephone number of authorizing official, X20 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. LINE_19: LINE_20: GENERAL_FORM_PROPOSERS: ! Replicate the section below for each investigator (PI and CoI's): LNAME:WELTY ! Investigator's last name, X20 FNAME:DANIEL ! Investigator's first name, X20 MI:E. INST:1710 ! Institution code number (or full institution name), X60 COUNTRY:USA ! Investigator's country, X20 LNAME:BLADES ! Investigator's last name, X20 FNAME:J. ! Investigator's first name, X20 MI:C. INST:3470 ! Institution code number (or full institution name), X60 COUNTRY:USA ! Investigator's country, X20 LNAME:HOBBS ! Investigator's last name, X20 FNAME:LEWIS ! Investigator's first name, X20 MI:M. INST:1710 ! Institution code number (or full institution name), X60 COUNTRY:USA ! Investigator's country, X20 LNAME:LAUROESCH ! Investigator's last name, X20 FNAME:JAMES ! Investigator's first name, X20 MI:T. INST:1710 ! Institution code number (or full institution name), X60 COUNTRY:USA ! Investigator's country, X20 LNAME:YORK ! Investigator's last name, X20 FNAME:DONALD ! Investigator's first name, X20 MI:G. INST:1710 ! Institution code number (or full institution name), X60 COUNTRY:USA ! Investigator's country, X20 GENERAL_FORM_ADDRESS: ! Address information for the Principal Investigator (PI): LNAME:WELTY ! PI's last name, X20 FNAME:DANIEL ! PI's first name, X20 MI:E. CATEGORY: PI ! (do not change this entry!) INST:1710 ! PI's institution number (or full institution name), X60 ADDR_1:University of Chicago ADDR_2:Astronomy and Astrophysics Center ADDR_3:5640 S. Ellis Ave. CITY:Chicago ! X30 STATE:IL ! X3 ZIP:60637 ! X9 COUNTRY:USA ! X20 PHONE:(312)702-0599 ! PI's telephone number, X20 TELEX:welty@oddjob.uchicago.edu GENERAL_FORM_TEXT: QUESTION: 3 ! Description of proposed observations. SECTION: 1 ! Provide a detailed description of the proposed observing plan. ! This description is used during scheduling to ensure that the ! observations are implemented properly, so please answer with care. 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 ! Justification of need for HST observations. 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 ! Description of special scheduling requirements. SECTION: 1 ! Describe any special scheduling requirements such as real-time, time-critical,! dark time, uninterrupted, Target of Opportunity, or Continuous Viewing Zone ! observations. 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 ! Description of special calibration exposures. SECTION: 1 QUESTION: 7 ! Data reduction and analysis plans. SECTION: 1 LINE_1:We will use the calibrated science data provided by STScI. Those data will LINE_2:be analyzed using absorption-line profile-fitting software developed and LINE_3:extensively used for the analysis of similar optical and UV data (including LINE_4:GHRS ECH-B and G160M data from Cycle 1). We will determine self-consistent LINE_5:models for the component structures of this line of sight by comparing the LINE_6:structures derived from both weak and strong, and both depleted and undepleted LINE_7:species (Zn II, Cr II, Mn II, Fe II, Mg II), and using Al III to trace ionized LINE_8:regions. Only the strongest components will be detected in the weakest lines; LINE_9:lines of increasing strength will reveal weaker and weaker components. LINE_10:The derived component structure will then be used to model the lower LINE_11:resolution short-wavelength IUE data for other dominant H I region species LINE_12:(Si II, S II, Ni II, Al II, and perhaps O I, N I, and C II). The resulting LINE_13:set of abundance patterns for the different components (regions) will be LINE_14:compared with abundances inferred from SMC stars and nebulae to determine LINE_15:depletions, which will then be compared with depletion patterns observed in the LINE_16:Galaxy. If the depletion patterns observed in the SMC (a lower LINE_17:metallicity, lower dust-to-gas ratio system) are similar to those observed in LINE_18:the Galaxy, then separation of depletion and nucleosynthetic effects in QSOALS LINE_19:abundances should be more secure. QUESTION: 8 ! Additional comments or special requests. SECTION: 1 QUESTION: 9 ! Description of previous HST work. 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_7: 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 ! Resources to be supplied by investigator's institution(s). SECTION: 1 LINE_1:We will have access to the necessary computational resources and LINE_2:software at Chicago. ! This is the end of the General Form FIXED_TARGETS: ! Replicate this section as needed for each Fixed Target. ! Delete this entire section if none of your targets are fixed targets. ! See Section 5.1 of the Proposal Instructions for detailed instructions. TARGNUM: 1 ! Target number (must be a unique integer), I3 NAME_1:NGC346-E-REF ! Catalog target name (see Section 5.1.2), X31 NAME_2: ! Common target name (optional), X31 NAME_3: ! Common target name (optional), X31 DESCR_1:J,701,702, ! Target category code letter (Section 5.1.3), X42 DESCR_2:D,202 ! Target keyword code numbers, X42 DESCR_3: ! Target keyword code numbers, X42 POS_1:RA = 00H 59M 29.5S +/- 1.3", ! Target position, X40 POS_2:DEC = -72D 10' 20.8" +/- 1.3" POS_3: POS_4: EQUINOX:2000 ! Equinox, X7 RV_OR_Z:V = 182 ! Radial velocity or redshift, X15 ACQPR_1: ! Target acquisition problems, X4 ACQPR_2: ! Enter any of EXT COMP BKG or leave blank ACQPR_3: ! FLUXNUM_1: 1 ! Flux reference number, I2 FLUXVAL_1: V=11.7 +/- 0.1 ! Flux data: V, B-V, E(B-V)..., X40 FLUXNUM_2: 1 ! Additional flux reference number (if needed), I2 FLUXVAL_2: B-V=-0.22 +/- 0.01 ! Additional flux data (if needed), X40 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 COMMENT_1:FLUX IS FOR HD5980 (BRIGHTEST ! Fixed target comments, X35 COMMENT_2:STAR IN FIELD); ! If this target can be observed in HST's COMMENT_3:This may be a CVZ target ! Continuous Viewing Zone (CVZ), add the COMMENT_4: ! following statement to this section: COMMENT_5: ! "This is a CVZ target" TARGNUM: 2 ! Target number (must be a unique integer), I3 NAME_1:HD5980 ! Catalog target name (see Section 5.1.2), X31 NAME_2:SK78 ! Common target name (optional), X31 NAME_3: ! Common target name (optional), X31 DESCR_1:B,103, ! Target category code letter (Section 5.1.3), X42 DESCR_2:H,508,509,510,506 ! Target keyword code numbers, X42 DESCR_3: ! Target keyword code numbers, X42 POS_1:RA = 00H 59M 26.66S +/- 1.2", ! Target position, X40 POS_2:DEC = -72D 09' 55.3" +/- 1.2" POS_3: POS_4: EQUINOX:2000 ! Equinox, X7 RV_OR_Z:V = 182 ! Radial velocity or redshift, X15 ACQPR_1: ! Target acquisition problems, X4 ACQPR_2: ! Enter any of EXT COMP BKG or leave blank ACQPR_3: ! FLUXNUM_1: 1 ! Flux reference number, I2 FLUXVAL_1: V=11.7 +/- 0.1 ! Flux data: V, B-V, E(B-V)..., X40 FLUXNUM_2: 1 ! Additional flux reference number (if needed), I2 FLUXVAL_2: B-V=-0.22 +/- 0.01 ! Additional flux data (if needed), X40 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 COMMENT_1:ECLIPSING BINARY; ! Fixed target comments, X35 COMMENT_2:PERIOD=19.266+/-0.003 DAYS;! If this target can be observed in HST's COMMENT_3:PHASE=0 AT JD=2443158.771; ! Continuous Viewing Zone (CVZ), add the COMMENT_4:MINIMA AT PHASE 0.0 AND 0.36;! following statement to this section: COMMENT_5:MINIMA LAST ABOUT 2 DAYS; ! "This is a CVZ target" COMMENT_6:MEMBER NGC346 IN SMC; COMMENT_7:This may be a CVZ target COMMENT_8: COMMENT_9: COMMENT_10: TARGNUM: 3 ! Target number (must be a unique integer), I3 NAME_1:SK108 ! Catalog target name (see Section 5.1.2), X31 NAME_2:GSC9138-01898 ! Common target name (optional), X31 NAME_3:R31 ! Common target name (optional), X31 DESCR_1:B,103, ! Target category code letter (Section 5.1.3), X42 DESCR_2:H,508,509,510 ! Target keyword code numbers, X42 DESCR_3: ! Target keyword code numbers, X42 POS_1:RA = 01H 03M 25.25S +/- 1.0", ! Target position, X40 POS_2:DEC = -72D 06' 43.0" +/- 1.0" POS_3: POS_4: EQUINOX:2000 ! Equinox, X7 RV_OR_Z:V = 135 ! Radial velocity or redshift, X15 ACQPR_1: ! Target acquisition problems, X4 ACQPR_2: ! Enter any of EXT COMP BKG or leave blank ACQPR_3: ! FLUXNUM_1: 1 ! Flux reference number, I2 FLUXVAL_1: V=12.3 +/- 0.1 ! Flux data: V, B-V, E(B-V)..., X40 FLUXNUM_2: 1 ! Additional flux reference number (if needed), I2 FLUXVAL_2: B-V=-0.23 +/- 0.01 ! Additional flux data (if needed), X40 FLUXNUM_3: 2 FLUXVAL_3: E(B-V)=0.07 +/- 0.02 FLUXNUM_4: 4 FLUXVAL_4: F-CONT(1808) = 1.3 +/- 0.1 E-12 FLUXNUM_5: 5 FLUXVAL_5: F-CONT(2060) = 7.9 +/- 0.1 E-13 FLUXNUM_6: 6 FLUXVAL_6: F-CONT(2260) = 5.7 +/- 0.1 E-13 FLUXNUM_7: 7 FLUXVAL_7: F-CONT(2590) = 4.7 +/- 0.1 E-13 FLUXNUM_8: 8 FLUXVAL_8: F-CONT(1250) = 3.0 +/- 0.1 E-12 FLUXNUM_9: 9 FLUXVAL_9: F-CONT(1320) = 2.5 +/- 0.1 E-12 COMMENT_1:This may be a CVZ target ! Fixed target comments, X35 COMMENT_2: ! If this target can be observed in HST's COMMENT_3: ! Continuous Viewing Zone (CVZ), add the COMMENT_4: ! following statement to this section: COMMENT_5: ! "This is a CVZ target" COMMENT_6: COMMENT_7: COMMENT_8: COMMENT_9: COMMENT_10: EXPOSURE_LOGSHEET: ! Replicate this section as needed for each exposure. ! See Section 6 for detailed instructions. LINENUM:101.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACQ ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:MIRROR-N2 ! Spectral element/s (use commas if needed), X30 WAVELENGTH: ! Central wavelength or range, X15 PARAM_1:BRIGHT=RETURN,! Optional parameters, X32 PARAM_2:SEARCH-SIZE=5, PARAM_3:LOCATE=YES PARAM_4: NUM_EXP: 1 ! Number of exposures, I3 TIME_PER_EXP:7.5S ! Time per exposure, X9 S_TO_N: ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME: ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 1 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4; ! Special Requirements (see Section 7), X41. REQ_2:ONBOARD ACQ FOR 102 ! The CYCLE must be specified for all lines. REQ_3: ! separate requirements with semi-colons (;) REQ_4: REQ_5: COMMENT_1:STEP-TIME=0.3S; ! Exposure logsheet line comments, X38 COMMENT_2:EXPECT 14000 COUNTS IN STEP-TIME COMMENT_3: COMMENT_4: LINENUM:102.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACQ/PEAKUP ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:MIRROR-N2 ! Spectral element/s (use commas if needed), X30 WAVELENGTH: ! Central wavelength or range, X15 PARAM_1: ! Optional parameters, X32 PARAM_2: PARAM_3: PARAM_4: NUM_EXP: 1 ! Number of exposures, I3 TIME_PER_EXP:30.6S ! Time per exposure, X9 S_TO_N: ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME: ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 1 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4; ! Special Requirements (see Section 7), X41. REQ_2:ONBOARD ACQ FOR 103-209 ! The CYCLE must be specified for all lines. REQ_3: ! sep requirements with semi-colons (;) REQ_4: REQ_5: COMMENT_1:STEP-TIME=0.3S ! Exposure logsheet line comments, X38 LINENUM:103.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:IMAGE ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:MIRROR-N2 ! Spectral element/s (use commas if needed), X30 WAVELENGTH: ! Central wavelength or range, X15 PARAM_1:NX=16, NY=16 ! Optional parameters, X32 PARAM_2: PARAM_3: PARAM_4: NUM_EXP: 1 ! Number of exposures, I3 TIME_PER_EXP:384.0S ! Time per exposure, X9 S_TO_N: ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME: ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 1 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:STEP-TIME=1.5S ! Exposure logsheet line comments, X38 LINENUM:201.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACCUM ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:ECH-B ! Spectral element/s (use commas if needed), X30 WAVELENGTH:1806.7 ! Central wavelength or range, X15 PARAM_1:FP-SPLIT=DSFOUR, ! Optional parameters, X32 PARAM_2:STEP-PATT=9, PARAM_3:STEP-TIME=0.2, PARAM_4:COMB=FOUR PARAM_5: NUM_EXP: 5 ! Number of exposures, I3 TIME_PER_EXP:25.72M ! Time per exposure, X9 S_TO_N:22 ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME:128.6M ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 4 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:FIVE SETS OF 4x6.43-MIN FP-SPLIT ! Exposure logsheet comments, X38 COMMENT_2:EXPOSURES; COMMENT_3:S/N IS PER HALF DIODE; COMMENT_4:Si II 1808.0126 LINENUM:204.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACCUM ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:ECH-B ! Spectral element/s (use commas if needed), X30 WAVELENGTH:2059.95 ! Central wavelength or range, X15 PARAM_1:FP-SPLIT=DSFOUR, ! Optional parameters, X32 PARAM_2:STEP-PATT=7, PARAM_3:STEP-TIME=0.2, PARAM_4:COMB=FOUR PARAM_5: NUM_EXP: 5 ! Number of exposures, I3 TIME_PER_EXP:21.28M ! Time per exposure, X9 S_TO_N:27 ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME:106.4M ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 5 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:FIVE SETS OF 4x5.32-MIN FP-SPLIT ! Exposure logsheet comments, X38 COMMENT_2:EXPOSURES; COMMENT_3:S/N IS PER HALF DIODE; COMMENT_4:AIR WAVELENGTHS; COMMENT_5:Cr II 2055.596, 2061.575; COMMENT_6:Zn II 2062.005 LINENUM:205.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACCUM ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:ECH-B ! Spectral element/s (use commas if needed), X30 WAVELENGTH:2258.6 ! Central wavelength or range, X15 PARAM_1:FP-SPLIT=DSFOUR, ! Optional parameters, X32 PARAM_2:STEP-PATT=7, PARAM_3:STEP-TIME=0.2, PARAM_4:COMB=FOUR PARAM_5: NUM_EXP: 3 ! Number of exposures, I3 TIME_PER_EXP:21.8M ! Time per exposure, X9 S_TO_N:29 ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME:65.4M ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 6 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:THREE SETS OF 4x5.45-MIN FP-SPLIT ! Exposure logsheet comments, X38 COMMENT_2:EXPOSURES; COMMENT_3:S/N IS PER HALF DIODE; COMMENT_4:AIR WAVELENGTHS; COMMENT_5:Fe II 2260.0808 LINENUM:207.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACCUM ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:ECH-B ! Spectral element/s (use commas if needed), X30 WAVELENGTH:2590.8 ! Central wavelength or range, X15 PARAM_1:FP-SPLIT=DSFOUR, ! Optional parameters, X32 PARAM_2:STEP-PATT=7, PARAM_3:STEP-TIME=0.2, PARAM_4:COMB=FOUR PARAM_5: NUM_EXP: 3 ! Number of exposures, I3 TIME_PER_EXP:20.0M ! Time per exposure, X9 S_TO_N:29 ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME:60.0M ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 7 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:THREE SETS OF 4x5-MIN FP-SPLIT ! Exposure logsheet comments, X38 COMMENT_2:EXPOSURES; COMMENT_3:S/N IS PER HALF DIODE; COMMENT_4:AIR WAVELENGTHS; COMMENT_5:Fe II 2585.8763; COMMENT_6:Mn II 2593.724 LINENUM:208.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACCUM ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:G160M ! Spectral element/s (use commas if needed), X30 WAVELENGTH:1252.0 ! Central wavelength or range, X15 PARAM_1:FP-SPLIT=DSFOUR, ! Optional parameters, X32 PARAM_2:STEP-PATT=5, PARAM_3:STEP-TIME=0.2, PARAM_4:COMB=FOUR PARAM_5: NUM_EXP: 2 ! Number of exposures, I3 TIME_PER_EXP:20.0M ! Time per exposure, X9 S_TO_N:44 ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME:40.0M ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 8 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:TWO SETS OF 4x5-MIN FP-SPLIT ! Exposure logsheet comments, X38 COMMENT_2:EXPOSURES; COMMENT_3:S/N IS PER HALF DIODE; COMMENT_4:S II 1250, 1253, 1259; COMMENT_5:Mg II 1239, 1240; COMMENT_6:Si II 1260 LINENUM:209.0 ! Exposure logsheet line number, F3.3 SEQUENCE_1: ! Sequence definition or usage (see Section 6.2) SEQUENCE_2: ! X10 TARGNAME:SK108 ! Target name (from Target List), X31 CONFIG:HRS ! Instrument Configuration (see Table 6.4) , X13 OPMODE:ACCUM ! Operating Mode (see Table 6.4), X15 APERTURE:2.0 ! Aperture or FOV (see Table 6.5), X14 SP_ELEMENT:G160M ! Spectral element/s (use commas if needed), X30 WAVELENGTH:1316.0 ! Central wavelength or range, X15 PARAM_1:FP-SPLIT=DSFOUR, ! Optional parameters, X32 PARAM_2:STEP-PATT=5, PARAM_3:STEP-TIME=0.2, PARAM_4:COMB=FOUR PARAM_5: NUM_EXP: 2 ! Number of exposures, I3 TIME_PER_EXP:20.0M ! Time per exposure, X9 S_TO_N:44 ! Signal-to-noise required (Section 6.12), X4 S_TO_N_TIME:40.0M ! Relevant time for signal-to-noise calculation, X9 FLUXNUM_1: 9 ! Flux reference number, I3 FLUXNUM_2: PRIORITY: 1 ! Exposure priority (1 is highest, 99 is lowest), I2 REQ_1: CYCLE 4 ! Special Requirements (see Section 7), X41. REQ_2: REQ_3: ! Remember to separate requirements with semi-colons (;) REQ_4: COMMENT_1:TWO SETS OF 4x5-MIN FP-SPLIT ! Exposure logsheet comments, X38 COMMENT_2:EXPOSURES; COMMENT_3:S/N IS PER HALF DIODE; COMMENT_4:O I 1302; COMMENT_5:Si II 1304; COMMENT_6:Ni II 1317 ! End of RPSS template