Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5682 Report Date: 18-Jul-95:17:51 Version: ********** Check-in Date: ********** 1.Proposal Title: UV SPECTRA OF LOW-REDSHIFT-QSOS AUGMENTATION: CYCLE 4 CARRYOVER ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID QUASARS & AGN AUG/FOS 4079 Sub Category AUG/FOS ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone E. margaret Burbidge UNIVERSITY OF CALIFORNIA, SA USA 619-534-4477 ------------------------------------------------------------------------------------ 7. Abstract This proposal contains observations which will help to complete a number of FOS IDT scientific programs. These programs are not in direct conflict with approved GO or GTO programs, but explore wavelength or signal-to-noise regimes not covered by other programs, or else they concentrate on objects of special interest. These programs will lead to a better understanding of the structure and kinematics of the broad- line region by studies of very high signal-to-noise line profiles in low redshift QSOs. The same data will also provide measurements of weak lines which will lead to improved photoionization models. This data set will yield high quality absorption line data for studies of specific absorption line systems and an independent sample for studies of absorption line evolution. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 5.38 par: 0 10. Num targs pri: 2 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS WF/PC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5682 PI: E. margaret Burbidge Proposal Title: UV SPECTRA OF LOW-REDSHIFT-QSOS AUGMENTATION: CYCLE 4 CARRYOVER ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Richard J. Harms APPLIED RESEARCH CORPORATION USA Richard G. Allen UNIVERSITY OF ARIZONA USA J. Roger P. Angel UNIVERSITY OF ARIZONA USA Frank Bartko UNAFFILIATED USA Edward Beaver UC, SAN DIEGO USA Ralph C. Bohlin SPACE TELESCOPE SCIENCE USA INSTITUTE Pi E. Margaret Burbidge UC, SAN DIEGO USA Ross D. Cohen UC, SAN DIEGO USA Aurthur F. Davidsen JOHNS HOPKINS UNIVERSITY USA Holland C. Ford SPACE TELESCOPE SCIENCE USA INSTITUTE George F. Hartig SPACE TELESCOPE SCIENCE USA INSTITUTE Vesa T. Junkkarinen UC, SAN DIEGO USA Bruce H. Margon UNIVERSITY OF WASHINGTON USA ------------------------------------------------------------------------------------ 3. Description of proposed observations. PG0026+12: After a binary search target acquisition with the blue detector, the following exposure will be taken in ACCUM mode: Blue G130H, 1.0" aperture. Then switch to the red side and do a peak up with the 0.5" aperture followed by spectra with G270H and G190H with the 1.0" aperture. The order of sides may be switched. MC1548+114A: 25 minute WFC exposure with F702W. Place the 8" off the the standard center of WF3 to ensure that the entire region of interest avoids the charge trap. ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. The HST UV capability is needed to measure Lyman-alpha and C IV lambda1549 and other lines in low redshift QSOs. By combining HST and optical spectra, it is possible to study line pairs such as Lyman-alpha and H-alpha with accurate wavelengths, good sampling of broad lines and good signal to noise. HST and optical spectra are needed to measure accurate emission line intensities for weak lines over a large range of rest wavelengths in individual objects. Emission line velocity differences cannot be easily determined from IUE data combined with ground based data because the IUE wavelength calibration is uncertain. QSO emission line profile studies using IR data or IUE data are limited by the available low signal to noise. The evolution of C IV lambda1549 absorption systems and the Lyman-alpha forest at redshifts from 0.0 to 1.06 and 1.63 respectively can only be studied from space. The collecting area of HST and the sensitivity of the FOS and GHRS make it possible to obtain spectra with the signal to noise needed to carry out these studies of QSOs at wavelengths below the atmospheric cutoff. Page 3 ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. These observations will be reduced using the standard spectroscopy and polarimetry reduction software available for FOS data. Calibration will be done using the results of SV observations. The emission lines in the spectra of QSOs will be analyzed by using IRAF / STSDAS and other existing software to measure line strengths. Blended lines and the continuum will be subtracted from the strong broad emission lines to determine line profiles which will be compared to emission lines observed in the optical and to the predictions of kinematical models. The line strengths will be compared to results from photoionization models. Additional analysis will be done by dividing broad line profiles to obtain line ratios as a function of velocity (Shuder 1982). The absorption features in QSO spectra will be measured using existing software that has been used for optical data and the early HST spectra. The evolution of C IV lambda1549 absorption systems with redshift will be studied by counting these systems and carrying out the necessary statistical analysis. Unidentified lines below Ly- alpha emission are candidate Ly-alpha forest lines and will contribute to studies of the evolution of these absorbers. Metal line systems will be studied by using curves of growth to obtain estimates and limits to column densities. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. Optical polarimetry and photometry will be performed using the facilities of Steward Observatory. Optical spectroscopy and photometry will be performed using the facilities of Lick Observatory. We will try to make the optical observations simultaneous with the HST UV observations if possible. This imposes no requirements on HST scheduling except as noted in question 5. Coordinates for a few objects need to be determined to the accuracy required for target acquisition. These can easily be obtained from the guide star data base using the existing software. There are a number of related FOS IDT GTO proposals in cycles 0, 1, and 2. Most of these observations were originally written as portions of observations begun in those proposals. Thus the observations included here contain both the baseline and augmented portions. Some observations were moved from augmented to baseline proposals to balance this. Page 4 ------------------------------------------------------------------------------------ 9. Description of previous HST work. Collaborators have received data from a number of GTO programs, SAT, and ERO programs. Related programs which have had observations are as follows: 1026 - ``UV Spectra of Low-Redshift-QSOs'', 1027 - ``UV Spectra of QSOs with z> 3.1'', 1029 - ``Spectropolarimetry of QSOs, Blazars, and AGN'', and 1033 - ``Search for Misdirected BL Lac Objects''. Low resolution observations of three high redshift QSOs have not revealed any with light at He II lambda 304. Observations of UM 675 have shown that any He I Gunn--Peterson effect is small, that He I absorption lines are not strong, that predictions of the ``Lyman valley'' may be correct, and that low redshift Ly-alpha is more prevalent than expected. Observations of low redshift QSOs (including 3C 273) have shown even more clearly that Ly-alpha absorption occurs in greater numbers than expected, as well as showing emission-- line profile differences more clearly than from earlier data. Unexpectedly, Ly- alpha is narrower than H-alpha. ``HST Imaging of the Inner 3 Arcseconds of NGC 1068 in the Light of [O III] lambda5007'', I.N.Evans, H.C.Ford, A.L.Kinney, R.R.J.Antonucci, L.Armus, and S.Caganoff, {\it Ap.J.(Lett.)}, {\bf 369}, L27, 1991. ``Faint Object Camera Observations of a Globular Cluster Nova Field'', B.Margon, S.F.Anderson, R.A.Downes, R.C.Bohlin, and P.Jakobsen, {\it Ap.J.(Lett.)}, {\bf 369}, L71, 1991. ``Far--Ultraviolet Spectroscopy of the Quasar UM 675 with the Faint Object Spectrograph on the Hubble Space Telescope'', E.A.Beaver, E.M.Burbidge, R.D.Cohen, V.T.Junkkarinen, R.W.Lyons, E.I.Rosenblatt, G.F.Hartig, B.Margon, and A.F.Davidsen, {\it Ap.J.(Lett.)}, {\bf 377}, L1, 1991. ``The Ultraviolet Absorption Spectrum of 3C 273'', J.N.Bahcall, B.T.Jannuzi, D.P.Schneider, G.F.Hartig, R.Bohlin, and V.Junkkarinen, {\it Ap.J.(Lett.)}, {\bf 377}, L5, 1991. ``Faint Object Spectrograph Spectroscopy of Resolved Structure in the Nucleus of NGC 1068'', S.Caganoff, R.R.J.Antonucci, H.C.Ford, G.A.Kriss, G.Hartig, L.Armus, I.N.Evans, E.Rosenblatt, R.C.Bohlin, and A.L.Kinney, {\it Ap.J.(Lett.)}, {\bf 377}, L9, 1991. ``Faint Object Spectrograph Observations of the Low-Luminosity Seyfert Galaxy NGC 1566'', G.A.Kriss, G.F.Hartig, L.Armus, W.P.Blair, S.Caganoff, and L.Dressel, {\it Ap.J.(Lett.)}, {\bf 377}, L13, 1991. ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). The majority of the resources required for this project other than the normal facilities of a university (librarys, offices, etc.) were supplied by NASA to the members of the FOS IDT for these projects. These include all the computing facilities required for the completion of data reduction and analysis. Optical and IR ground--based observing facilities and support are provided by the University of California and the University of Arizona. ------------------------------------------------------------------------------------ 11. Address Information Name: E. MARGARET BURBIDGE Category: PI Institution: UNIVERSITY OF CALIFORNIA, SAN DIE Address: CASS 0111, UCSD 9500 GILMAN DRIVE City: LA JOLLA State: CA Zip Code: 920930111 Country: USA Telephone: 619-534-4477 Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5682 [ 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 PG0026+12 E,313,321,923, RA = 0H 29M 13.710S +/- 2000 Z=0.142 1 V=15.14 +/- 0.05 GSC-I 602 H,515,519 0.3", 2 F(1500)=2.0 +/- 0.5 E-14 1173 DEC = 13D 16' 3.86" +/- 0.3", PLATE-ID = 028X ------------------------------------------------------------------------------------------------------------------------------------ 9 MC1548+114A E,314,321, RA = 15H 50M 43.599S +/- 2000 Z=0.436 COMP 1 V=17.0 +/- 1.0 H,515,519 1.0", DEC = 11D 20' 47.74" +/- 1.0", PLATE-ID = 00J1 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5682 [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 1.5 PG0026+12 FOS/BL ACQ/ 4.3 MIRROR BRIGHT=700000 1 6.5S 2 1 ONBOARD ACQ FOR BINARY FAINT=330 1.55 GROUP 1.5-1.9 NO GAP CYCLE 4 / 1.5-1.9 Comments: red side time would be 1.7S ------------------------------------------------------------------------------------------------------------------------------------ 1.55 PG0026+12 FOS/BL ACCUM 1.0 G130H 1300 1 9600S 15 2 1 ------------------------------------------------------------------------------------------------------------------------------------ 1.56 PG0026+12 FOS/RD ACQ/ 0.5 MIRROR SCAN-STEP-X=0.3 1 5S 2 1 ONBOARD ACQ FOR PEAK SCAN-STEP-Y=0.3 1.59-1.9 SEARCH-SIZE-X=3 SEARCH-SIZE-Y=3 Comments: peak up after side switch recommended by instrument scientist A new BSTA is OK with us if it is easier to schedule. ------------------------------------------------------------------------------------------------------------------------------------ 1.59 PG0026+12 FOS/RD ACCUM 1.0 G270H 2700 1 540S 15 2 1 ------------------------------------------------------------------------------------------------------------------------------------ 1.9 PG0026+12 FOS/RD ACCUM 1.0 G190H 1900 1 828S 15 2 1 ------------------------------------------------------------------------------------------------------------------------------------ 20 MC1548+114A WFPC2 IMAGE WF3 F702W 1 1500S 1 1 CYCLE 4 POS TARG -5.66,- 5.66 Comments: pos target should move the object 8" off nominal in the V3 direction. ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5682 [ 7] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/BL FOS/RD WFPC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACQ/BINARY ACCUM ACQ/PEAK IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters BRIGHT FAINT SCAN-STEP-X=0.3 SCAN-STEP-Y=0.3 SEARCH-SIZE-X=3 SEARCH-SIZE-Y=3 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for AUG/FOS ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 5.38 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QUASARS & AGN ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category AUG/FOS ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements ONBOARD ACQ FOR 1.55; GROUP 1.5-1.9 NO GAP; CYCLE 4 / 1.5-1.9 ONBOARD ACQ FOR 1.59-1.9; CYCLE 4; POS TARG -5.66,-5.66 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements MIRROR G130H G270H G190H F702W ------------------------------------------------------------------------------------------------------------------------------------ Target Names PG0026+12 GSC-I 602 1173 MC1548+114A ------------------------------------------------------------------------------------------------------------------------------------