Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 4939c Report Date: 09-May-96:20:11 Version: ********** Check-in Date: ********** 1.Proposal Title: QUASAR ABSORPTION LINE SURVEY: CYCLE 2 OBSERVATIONS OBSERVATIONS OF 3C249-1 ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID QUASARS & AGN GO 3 Long Term yrs 2424 Sub Category Key Project QUASAR ABSORPTION Large Project ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone John N. Bahcall INSTITUTE FOR ADVANCED STUDY USA 609-734-8058 ------------------------------------------------------------------------------------ 7. Abstract THIS SUBMISSION is a change to P3791 to replace an object that it is not possible to acquirer with the Binary Search procedure with another object from our program. The object which has been removed is IR0450-2958. We are replacing it with 3C249-1 The Quasar Absorption Line Survey of bright sources is an efficient observing program designed to provide a homogeneous data base of absorption features. The data will reveal absorption regions in galaxies, in clusters of galaxies, in voids, in large- scale structures, in Lyman ALPHA clouds, and wi provide information about damped Lyman ALPHA and Lyman-limit systems. The survey will determine, with high SNR, the profiles of > 200 emission lines. Using the estimated numbers of observed absorption lines, including archi val data, the program was designed to determine the cosmic evolution of absorption systems. High resolution spectra of a sample of quasars will be obtained with the FOS; the spectra will have a rest frame equivalent width detection limit for unresolved absorption lines of 0.3 A. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 7.42 par: 0 10. Num targs pri: 1 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 4939c PI: John N. Bahcall Proposal Title: QUASAR ABSORPTION LINE SURVEY: CYCLE 2 OBSERVATIONS OBSERVATIONS OF 3C249-1 ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ W. Sargent CALIFORNIA INSTITUTE OF USA TECHNOLOGY Ray J. Weymann OBSERVATORY OF THE CARNEGIE USA INSTITUTION IN WASHINGTON Jacqueline Bergeron INSTITUTE FOR ASTROPHYSICS, FRANCE X PARIS A. Boksenberg ROYAL GREENWICH OBSERVATORY UK X George Hartig SPACE TELESCOPE SCIENCE USA INSTITUTE Buell T. Jannuzi INSTITUTE FOR ADVANCED STUDY, USA PRINCETON Blair Savage WISCONSIN, UNIVERSITY OF USA Donald P. Schneider INSTITUTE FOR ADVANCED STUDY, USA PRINCETON David A. Turnshek UNIVERSITY OF PITTSBURGH USA A. M. Wolfe ASTROPHYSICS AND SPACE SCIENCES, USA UCSD Pi John N. Bahcall INSTITUTE FOR ADVANCED STUDY, USA PRINCETON ------------------------------------------------------------------------------------ 3. Description of proposed observations. Observations for the Quasar Absorption Line Survey will be distributed equally over three cycles (1-3). The quasars will in general be observed at high resolution ($1300$) through the 0.25 by 2.0 arcsecond slit. For these observations the desired signal to noise ratio is 30 (per diode). The FOS red side with the G190H and G270H gratings will be used to cover the wavelength range 1600 to 3300 angstroms. The FOS blue side and G130H grating will be used to cover the range from 1100 to 1600 angstroms. Since the G130H observations require a great deal of time, for some objects low resolution G160L exposures through the 1.0 arcsecond apt. are used instead. These are designed to find targets suitable for future cycle G130H observations and do not require signal to noise of 30. For eash object a single Binary acquisition is used followed by peak up acquisitions into the slit. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. HST observations are required to observe the strong resonant absorption lines and the various emission lines of the most abundant elements, which are in the ultraviolet (inaccessible to terrestrial observations) for the small and moderate redshifts investigated in this project. Ground-based observations partially determine the character of the absorbing systems and emission line regions at larger redshifts, but spectra must be obtained in the ultraviolet to establish the cosmological evolution of the known types of absorbing systems and emission line regions, to permit optical identifications, to search for gas in known voids and clusters of galaxies, to test for large scale structure in absorbing systems, and to make possible follow-up high resolution studies of the physical conditions and of the chemical (and isotopic) abundances. IUE observations do not have sufficiently high signal-to-noise ratios for our sample of objects to permit answering the scientific questions listed in the section on scientific justification. Quasar absorption and emission lines have been studied extensively from the ground (see the review articles listed in the scientific justification), but of course only in the accessible optical region. ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. No Realtime data needed ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. We would like all observations of a given object to be obtained within a ten day interval. Since quasars are known to vary in brightness, the data for all wavelengths must be taken nearly simultaneously in order to determine the spectral energy distribution. Our observations of a given object are currently linked with NO GAP inorder to be more efficient in the use of spacecraft time (only one acquisition needed). ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. The answer to this question is too long for the RPSS format; please see the paper submission for phase 1. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. See paper submission for phase 1. ------------------------------------------------------------------------------------ 9. Description of previous HST work. See paper submission for phase 1. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). See paper submission for phase 1. ------------------------------------------------------------------------------------ 11. Address Information Name: JOHN N. BAHCALL Category: PI Institution: INSTITUTE FOR ADVANCED STUDY Address: OLDEN LANE, BUILDING E City: PRINCETON, N.J. State: NJ Zip Code: 08540 Country: U.S.A. Telephone: 609-734-8058 Telex (or e-mail): 229 734 IAS UR ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 4939c [ 4] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 3C249-1 E,314,321 RA = 11H 04M 13.9S +/- 0.1S, 2000 Z=0.311 1 V = 15.72 +/- 0.1 DEC = +76D 58' 58.2" +/- 1.0", PLATE-ID=02D3 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 4939c [ 5] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 1 3C249-1 FOS/BL ACQ/ 4.3 MIRROR 1 14.46S 1 CYCLE 2 BINARY ONBOARD ACQ FOR 1.10 ------------------------------------------------------------------------------------------------------------------------------------ 1.1 3C249-1 FOS/BL ACQ/ 0.25X2. MIRROR TYPE=UP 1 2.13S 1 CYCLE 2 PEAK 0 ONBOARD ACQ FOR 2.00 SPATIAL SCAN ------------------------------------------------------------------------------------------------------------------------------------ 2 3C249-1 FOS/BL RAPID 0.25X2. G130H 1300 READ-TIME=40 1 340M 1 1 CYCLE 2 0 ------------------------------------------------------------------------------------------------------------------------------------ Scan Paramters Form Proposal ID: 4939c [ 6] ------------------------------------------------------------------------------------------------------------------------------------ Data ID: 1 Exposure Logsheet lines: 1.10 FGS Scan: DWELL Dwell Only: dwell points/line: 7 Seconds per dwell: 1.00 Scan width (arc-secs): 0.0000 Scan length (arc-secs): 0.4000 Angle between sides (degrees) 90.00 Number of lines: 1 Scan rate (arc-sec/sec): 0.0000 PA of first scan line (degrees) 90.000 Scan frame (CEL or S/C): S/C Length Offset (arc-sec): 0.2000 Width Offset (arc-sec): 0.0000 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 4939c [ 7] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/BL ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/BINARY ACQ/PEAK RAPID ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters TYPE=UP READ-TIME=40 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 7.42 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QUASARS & AGN ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category QUASAR ABSORPTION ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 2; ONBOARD ACQ FOR 1.10 ; ONBOARD ACQ FOR 2.00; SPATIAL SCAN ; CYCLE 2 ; ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR G130H ------------------------------------------------------------------------------------------------------------------------------------ Target Names 3C249-1 ------------------------------------------------------------------------------------------------------------------------------------