Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5455 Report Date: 18-Jul-95:17:26 Version: ********** Check-in Date: ********** 1.Proposal Title: THE LEVEL OF IONIZATION AND CHEMICAL COMPOSITION OF QSO BAL REGION GAS - CYCLE 4 MEDIUM ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID QUASARS & AGN GO Sub Category QUASAR ABSORPTION ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Dr. David A. Turnshek UNIVERSITY OF PITTSBURGH USA ------------------------------------------------------------------------------------ 7. Abstract About 10% of all radio quiet QSOs exhibit broad absorption lines (BALs) in their spectra. The BALs come from a mostly highly ionized region outflowing from the central source at speeds up to many tens of thousands of km/s. Observational constraints on models require that the covering factor of the BAL region be small (e.g., normally < 0.2), therefore many QSOs must have BAL regions which do not lie along our lines-of-sight. For assumptions which should reasonably apply to BAL regions, accurate (algorithm independent) ionic column densities can be derived as a function of outflow velocity for BAL gas. This is unlike the case for broad emission lines in QSOs, which at any observed velocity originates in various components with a range of ionizations. Based on column density analyses, evidence suggests that the chemical composition of the BAL region gas is enhanced by factors of 10 to 100 or more times solar values. Since this conclusion is remarkable, we propose to carefully checked it. One possible problem is that our assumptions about the ability of BAL gas to cover the central source are not universally correct. Another problem with past analyses is that different ionic species of the same element in an object have not been studied. We will remedy these problems by observing the UV spectrum of three specially selected BAL QSOs which currently show the best evidence for enhanced abundances. Constraints on the ionization and chemical composition of the BAL region gas will be derived using Ferland's photoionization code. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 4.64 par: 0 10. Num targs pri: 6 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5455 PI: Dr. David A. Turnshek Proposal Title: THE LEVEL OF IONIZATION AND CHEMICAL COMPOSITION OF QSO BAL REGION GAS - CYCLE 4 MEDIUM ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Dr. David A Turnshek UNIVERSITY OF PITTSBURGH USA Dr. Brian R Espey UNIVERSITY OF PITTSBURGH USA Dr. Ray J Weymann 3030 USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. We propose HST observations of 4 QSOs using the FOS G270H mode in order to study the strength and shape of BAL profiles that fall in the spectral region below 3200 Angstroms. The observation of each object can be made during a single visit. The signal-to-noise ratio attained near continuum regions will be approximately 30 per resolution element with resolution R=1300 (4 pixels per resolution element with 1/4 diode substeps). Exposure times range from 34 minutes to 54 minutes. In addition we will observe 6 QSOs using the FOS G160L mode in order to follow the shapes of the continuous energy distributions into the far UV. The signal-to- noise ratio attained near continuum regions at about 1600 Angstroms will be 10 per resolution element with resolution R=200 (4 pixels per resolution element with 1/4 diode substeps), which will be adequate for our purpose. ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. First, we want to obtain high quality (STNR=30 per diode) UV data on specific ionic transitions which give rise to BAL profiles and that we have studied in optical spectra. We have discussed how analysis of these transitions can be used to study the level of ionization and metal abundances of QSO BAL region gas. Observing into the UV for these specific objects is necessary because it has not been possible to find similar objects at high enough redshift to observe these transitions from the ground (i.e., these objects are special and unique as discussed in the separate detailed scientific justification). Furthermore, if similar examples could be found at high-redshift, the larger density of Ly-alpha forest lines could make the identification of the absorption more difficult. The data must be of signal-to-noise ratio 30 per resolution element with R=1300 in order to gather detailed data on the strength and shapes of BAL profiles. Such data will allow us to derive reliable column densities. Second, we want to obtain lower quality (G160L, STNR=10 per diode at 1600 Angstroms) far UV data to study the continuous energy distributions as far as possible into the UV. This will allow us to test the dust-extinction model. These objects are much too faint to observe with IUE for the purpose of deriving reliable column densities. Several other HST observations of high-ionization BAL QSOs have been made, and these will be used in our study of the continuous energy distributions of comparative samples. The exposure times were determined using data from the FOS handbook. We have proposed to observe 6 different QSOs. In the past, we have attempted to observe all of them with IUE. When possible, we have used this low signal-to- noise information to compute the exposure times. We have also checked our exposure time computations by extrapolating the known optical flux into the UV. In all cases the exposure times are derived to achieve a STNR=30 per resolution element (R=1300) at approximately 2700 Angstroms (G270H) or a STNR=10 per resolution element (R=200) at approximately 1600 Angstroms (G160L) in the anticipated continuum level. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. Page 3 ------------------------------------------------------------------------------------ 9. Description of previous HST work. Related GTO and GO programs for Turnshek: 1146: `Spectroscopic Studies of Several High Redshift BAL QSOs' -- GTO program -- Weymann (PI), Burbidge, Cohen, Foltz, Hartig, Junkkarinen, Morris, and Turnshek (one published paper). 1145: `Imaging and Spectroscopy of the Low Redshift BAL QSO PG1700+518' GTO program -- Weymann (PI) and Turnshek (deferred program). 2649: `Spectrophotometry of the Lensed Clover Leaf BAL QSO 1413+11' -- GO Cycle 1 program -- Turnshek (PI) and Lupie (not yet executed). 3660: `The Level of Ionization and Chemical Composition of QSO BAL Region Gas' -- GO Cycle 2 program -- Turnshek (PI), Espey, and Weymann (executed in April 1992). Unrelated GO programs for Turnshek: 2424: [and also continuation program numbers] `Quasar Absorption Line Survey' -- GO Key Project - - Bahcall (PI), Bergeron, Boksenberg, Hartig, Jannuzi, Sargent, Savage, Schneider, Turnshek, Weymann, and Wolfe. (Note, however, that some BAL QSOs have been observed during this program.) 3801: `Search for QSOs Suitable for Subsequent Observation of HeII304 Absorption Arising in the IGM ...' -- GO Cycle 2 program -- Tytler (PI), Hazard, Lanzetta, McMahon, Turnshek. 4343: `Damped Ly- alpha Absorption Lines from Low-Redshift Galaxies' -- GO Cycle 3 program -- Lanzetta (PI), Turnshek, and Wolfe (not yet executed). Programs 1146 and 3660 are directly related to the present program. Program resulted in the Korista et al. publication (see below). Also, a single G270H observation of Q0932+5006 was allocated for this program and the data were successfully obtained about 2 weeks ago. For Turnshek: `HST-FOS and Ground-Based Observations of the BAL Quasar 0226- 1024' by Korista, Weymann, Morris, Kopko, Turnshek, Hartig, Foltz, Burbidge, and Junkkarinen, ApJ, 401, 529 (1992) `The HST Quasar Absorption Line Key Project I. First Observational Results Including Lyman-\ALPHA\ and Lyman-Limit Systems' by Bahcall, Bergeron, Boksenberg, Hartig, Jannuzi, Kirhakos, Sargent, Savage, Schneider, Turnshek, Weymann, and Wolfe, ApJS, in press (1993) `The HST Quasar Absorption Line Key Project II. Data Calibration and Absorption Line Selection' by Schneider, Hartig, Jannuzi, Kirhakos, Saxe, Weymann, Bahcall, Bergeron, Boksenberg, Sargent, Savage, Turnshek, and Wolfe, ApJS, in press (1993) `The HST Quasar Absorption Line Key Project III. First Observational Results on Milky Way Gas' by Savage, Lu, Bahcall, Bergeron, Boksenberg, Hartig, Jannuzi, Kirhakos, Lockman, Sargent, Schneider, Turnshek, Weymann, and Wolfe, ApJS, in press (1993). ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). At Pittsburgh, institutional support includes academic salary for the PI. The University of Pittsburgh will also supply routine secretarial assistance, administrative support, and the office space required for this project. In addition, the University has a pool of graduate and undergraduate research assistants who can be called upon to perform work for this project, providing the work can be charged to the project. The Department of Physics and Astronomy operates a SUN SPARC2 workstation as a file server for client workstations owned by various research groups. Other Departmental facilities include a laser printer, a CD reader, limited disk space, an Exabyte 8mm tape drive, and some older model workstations. The Department pays for maintenance of this facility, but the Departmental facilities are not generally used by the various physics and astronomy research groups (except for the file server capability). Their primary purpose is as an educational tool. However, they would prove to be a good backup in the event that, for example, the computing facilities of the astronomy/astrophysics group go down. Research groups must purchase and maintain their computing facilities with project funds. Institutional support for co-I Weyman, who is a member of the GHRS IDT, is proposals. ------------------------------------------------------------------------------------ 11. Address Information Page 4 Name: David A Turnshek Category: PI Institution: University of Pittsburgh Address: Department of Physics and Astronomy Allen Hall City: Pittsburgh State: PA Zip Code: 15260 Country: USA Telephone: 412-624-9015/9000 Telex (or e-mail): turnshek@vm2.cis.pitt.edu ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5455 [ 5] ------------------------------------------------------------------------------------------------------------------------------------ 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 Q0059-2735 E,313 PLATE-ID=02J4, 2000 Z = 1.60 1 V = 17.62 RA = 01H 02M 17.008S +/- 1 B-V = 0.54 0.1S, 2 F-CONT(2700) = 4.7 E-16 DEC = -27D 19' 50.06" +/- 3 F-CONT(1600) = 6.1 E-16 1.0" Comments: UV FLUXES ARE ESTIMATED FROM POWER LAW OF INDEX 1.5 EXTRAPOLATIONS ------------------------------------------------------------------------------------------------------------------------------------ 2 H0903+175 E,313 PLATE-ID=0204, 2000 Z = 2.76 1 V = 17.3 RA = 09H 06M 38.213S +/- 2 F-CONT(2700) = 6.3 E-16 0.1S, 3 F-CONT(1600) = 8.13 E-16 DEC = +17D 22' 23.16" +/- 1.0" ------------------------------------------------------------------------------------------------------------------------------------ 3 H1413+117 E,313 RA = 14H 15M 46.3S +/- 0.1S, 2000 Z = 2.54 1 V = 17.0 DEC = +11D 29' 44.1" +/- 2 F-CONT(2700) = 8.3 E-16 1.5" 3 F-CONT(1600) = 1.1 E-15 Comments: PREVIOUSLY OBSERVED WITH HST ------------------------------------------------------------------------------------------------------------------------------------ 4 Q0932+5006 E,313 RA = 09H 35M 53.13S +/- 2000 Z = 1.92 1 V = 17.24 0.1S, 2 B-V = 0.16 DEC = +49D 53' 13.6" +/- 3 F-CONT(1600) = 8.6 E-16 1.5" Comments: PREVIOUSLY OBSERVED WITH HST ------------------------------------------------------------------------------------------------------------------------------------ 5 Q0226-1024 E,313 RA = 02H 28M 39.15S +/- 2000 Z = 2.26 1 V = 17.4 0.1S, 2 F-CONT(1600) = 7.42 E-16 DEC = -10D 11' 10.3" +/- 1.5" Comments: PREVIOUSLY OBSERVED WITH HST ------------------------------------------------------------------------------------------------------------------------------------ 6 Q1309-0536 E,313 PLATE-ID=024R, 2000 Z = 2.22 1 V = 17.4 RA = 13H 11M 36.484S +/- 2 B-V = 0.41 0.1S, 3 F-CONT(2700) = 5.7 E-16 DEC = -05D 52' 38.95" +/- 4 F-CONT(1600) = 7.4 E-16 1.5" ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5455 [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 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 Q0059-2735 FOS/RD ACQ/ 4.3 MIRROR 1 21S 30 1 1 CYCLE 4 BINARY ONBOARD ACQ FOR 2- 2.1 ------------------------------------------------------------------------------------------------------------------------------------ 2 Q0059-2735 FOS/RD ACCUM 1.0 G270H 1 41.7M 30 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 2.1 Q0059-2735 FOS/RD ACCUM 1.0 G160L 1 23M 10 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 3 H0903+175 FOS/RD ACQ/ 4.3 MIRROR SCAN-STEP- 1 1.3S 30 1 1 CYCLE 4 PEAK Y=1.204 ONBOARD ACQ FOR SEARCH-SIZE-X=1 3.1 SEARCH-SIZE-Y=3 ------------------------------------------------------------------------------------------------------------------------------------ 3.1 H0903+175 FOS/RD ACQ/ 1.0 MIRROR SCAN-STEP- 1 1.4S 30 1 1 CYCLE 4 PEAK X=.602 ONBOARD ACQ FOR SCAN-STEP- 3.2 Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 ------------------------------------------------------------------------------------------------------------------------------------ 3.2 H0903+175 FOS/RD ACQ/ 0.5 MIRROR SCAN-STEP- 1 1.6S 30 1 1 CYCLE 4 PEAK X=0.172 ONBOARD ACQ FOR 4- SCAN-STEP- 4.1 Y=0.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 ------------------------------------------------------------------------------------------------------------------------------------ 4 H0903+175 FOS/RD ACCUM 1.0 G270H 1 37.7M 30 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 4.1 H0903+175 FOS/RD ACCUM 1.0 G160L 1 22M 10 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 5 H1413+117 FOS/RD ACQ/ 4.3 MIRROR SEARCH-SIZE-X=1 1 1S 30 1 1 CYCLE 4 PEAK SEARCH-SIZE-Y=3 ONBOARD ACQ FOR SCAN-STEP- 5.1 Y=1.204 ------------------------------------------------------------------------------------------------------------------------------------ 5.1 H1413+117 FOS/RD ACQ/ 1.0 MIRROR SEARCH-SIZE-X=6 1 1.4S 30 1 1 CYCLE 4 PEAK SEARCH-SIZE-Y=2 ONBOARD ACQ FOR SCAN-STEP- 5.2 Y=.602 SCAN-STEP- X=.602 ------------------------------------------------------------------------------------------------------------------------------------ 5.2 H1413+117 FOS/RD ACQ/ 0.3 MIRROR SEARCH-SIZE-X=5 1 6S 30 1 1 CYCLE 4 PEAK SEARCH-SIZE-Y=5 ONBOARD ACQ FOR 6- SCAN-STEP- 6.1 X=.172 SCAN-STEP- Y=.172 ------------------------------------------------------------------------------------------------------------------------------------ 6 H1413+117 FOS/RD ACCUM 4.3 G270H 1 29M 30 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5455 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 6.1 H1413+117 FOS/RD ACCUM 4.3 G160L 1 16M 10 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 7 Q0932+5006 FOS/RD ACQ/ 4.3 MIRROR 1 14.6S 30 1 1 CYCLE 4 BINARY ONBOARD ACQ FOR 8 SEQ 7-8 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 8 Q0932+5006 FOS/RD ACCUM 1.0 G160L 1 20M 10 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 9 Q0226-1024 FOS/RD ACQ/ 4.3 MIRROR 1 17S 30 1 1 CYCLE 4 BINARY ONBOARD ACQ FOR 10 SEQ 9-10 NO GAP ------------------------------------------------------------------------------------------------------------------------------------ 10 Q0226-1024 FOS/RD ACCUM 1.0 G160L 1 23M 10 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 11 Q1309-0536 FOS/RD ACQ/ 4.3 MIRROR 1 17S 30 1 1 CYCLE 4 BINARY ONBOARD ACQ FOR 12 -12.1 ------------------------------------------------------------------------------------------------------------------------------------ 12 Q1309-0536 FOS/RD ACCUM 1.0 G270H 1 41.7M 30 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ 12.1 Q1309-0536 FOS/RD ACCUM 1.0 G160L 1 23M 10 2 1 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5455 [ 8] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/RD ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/BINARY ACCUM ACQ/PEAK ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SCAN-STEP-Y=1.204 SEARCH-SIZE-X=1 SEARCH-SIZE-Y=3 SCAN-STEP-X=.602 SCAN-STEP-Y=.602 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 SCAN-STEP-X=0.172 SCAN-STEP-Y=0.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 SCAN-STEP-X=.172 SCAN-STEP-Y=.172 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 4.64 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QUASARS & AGN ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category QUASAR ABSORPTION ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 4; ONBOARD ACQ FOR 2-2.1 CYCLE 4 ONBOARD ACQ FOR 3.1 ONBOARD ACQ FOR 3.2 ONBOARD ACQ FOR 4-4.1; ONBOARD ACQ FOR 5.1 ONBOARD ACQ FOR 5.2 ONBOARD ACQ FOR 6-6.1 ONBOARD ACQ FOR 8; SEQ 7-8 NO GAP; ONBOARD ACQ FOR 10; SEQ 9-10 NO GAP; ONBOARD ACQ FOR 12-12.1 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR G270H G160L ------------------------------------------------------------------------------------------------------------------------------------ Target Names Q0059-2735 H0903+175 H1413+117 Q0932+5006 Q0226-1024 Q1309-0536 ------------------------------------------------------------------------------------------------------------------------------------