Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5393 Report Date: 18-Jul-95:17:17 Version: ********** Check-in Date: ********** 1.Proposal Title: THE NATURE OF THE HOST GALAXIES OF HIGH-REDSHIFT, RADIO-LOUD QUASARS ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID QUASARS & AGN GO Sub Category HOST GALAXIES ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Matthew D Lehnert INSTITUTE FOR GEOPHYSICS AND US (510) 423-6013 ------------------------------------------------------------------------------------ 7. Abstract The co-moving space density of highly luminous radio-loud quasars has decreased by roughly 3 orders of magnitude from z=2-3 to the current epoch. Understanding the physical processes responsible for this decrease could profoundly influence how we think the universe and galaxies have evolved. In order to make the first steps in understanding these physical processes, we propose to conduct a narrow (at Lyman alpha) and broad-band imaging survey of five radio-loud, high-z (z=2) quasars using WFPC2. HST observations are crucial for separating the "blinding" nuclear emission (AGN) from that of the extended "fuzz" (parent galaxy). They will allow quantitative comparisons of the emission-line and continuum morphologies of the host galaxies of high-z quasars to those of comparable high-z radio galaxies, and of low-z quasars. Such comparisons will allow us to investigate whether or not radio-loud quasars and radio galaxies are members of the same parent population as is fashionable in the AGN unification schemes and how luminous AGN have evolved from redshifts of 2-3. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 9.25 par: 0 10. Num targs pri: 5 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: WF/PC ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 5393 PI: Matthew D Lehnert Proposal Title: THE NATURE OF THE HOST GALAXIES OF HIGH-REDSHIFT, RADIO-LOUD QUASARS ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ Matthew D Lehnert 2460 US Timothy M Heckman 2380 US Wil Van Breugel 2460 US George K Miley 6870 NL X ------------------------------------------------------------------------------------ 3. Description of proposed observations. The observational plan can be summarized as obtaining deep optical broad and narrow-band images of 5 high-redshift radio-loud quasars The continuum broad-band images will be taken using the planetary camera in combination with the filter F555W. The narrow-band filters were choosen to correspond to the wavelength of redshifted Lyman-alpha in each of these quasars. The narrow-band images will be obtained with the wide field camera. The main two observational constraints on this program is our desire to detect faint emission line gas and continuum emission and yet not saturate the active galactic nucleus of these quasars. To meet these constraints we have chosen to split the exposures in to sets of 3 each for the continuum and the narrow-band imaging. This technique has the added advantage that it will aid in cosmic ray removal. To detect continuum emission down to 28 V mag per HST PSF requires total integration times of 30 minutes. Thus for each quasar we will obtain 3 exposures x 10 minutes per exposure for 30 minutes of exposure time, except for 4C57.29, the brightest of the quasars, for which we will obtain 6 exposures x 5 minutes per exposure. For the narrow-band imaging, exposures of about an hour will allow us to probe Lyman-alpha emitting structures down few times 10E-17 ergs per sec per square cm per HST PSF. Such fluxes are sufficient to meet our scientific goals. We therefore have decided to split to images into sets of 3 images per quasar through the narrow-band filter to aid in cosmic ray removal and to ensure that the images do not saturate the bright quasar nucleus. Each quasar will be exposed for a hour following the prescription 3 exposures x 20 minutes per exposure. To match the wavelength of redshifted Lyman-alpha in these quasars we will use the quadrant filter, "redshifted [OII]" (FQUVN) for four of the quasars and F437N for PKS2338+042. The details of the quasar-filter combinations are: For PKS0445+097 at z=2.110, we would like to use the "redshifted [OII]" filter rotated by -33 degrees and use WF2 for its aperature. This should give a central wavelength of 3763 angstroms for the filter which is close to the wavelength of redshifted Lyman-alpha in PKS0445+097 (3781 angstroms). For MRC0549-213 at z=2.245, we would like to use the "redshifted [OII]" filter in its nominal position and use WF2 for the aperature. This aperature corresponds to a central wavelength of 3986 angstroms (Lyman-alpha in MRC0549-213 is at 3945 angstroms). For PKS1318+113 at z=2.171, we would again like to use the FQUVN filter in its nominal position and use WF4 for the aperature. This aperature corresponds to a central wavelength of 3839 angstroms (redshifted Lyman-alpha for PKS1318+113 is at 3855 angstroms). For 4C57.29, again we would like to use FQUVN in its nominal position and use WF4 as the aperature to give a central wavelength of 3839 angstroms (Lyman-alpha for 4C57.29 is at 3857 angstroms). For PKS2338+042 we would like to use the narrow- band filter F437N. Page 3 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. The observational constraint that limits our ability to say anything meaningful about the properties of the extended emission ("fuzz") around high-redshift quasars is the limit of how well we can separate the bright, nuclear emission from the AGN from the fuzz. At typical ground based seeing (1 arc second), the nuclear light is spread over the central 10 kpc of the fuzz. Previous ground- based data has shown that quasars at redshifts of 2 to 3, typically have isophotal radii of at most 9 arc seconds in the rest-frame UV (typically down to 27th mag per square arc seconds at B) and about 12 arc seconds in Lyman alpha (down to 10E-17 ergs per sec per square cm). This implies that seeing of an arc second is required just to show that the quasars are extended (never mind actually showing the detailed morphology). HST is crucial if we are to make secure detections of the host galaxies of high-redshift quasars by allowing us to rather unambiguously remove the contribution of the AGN by, roughly speaking, restricting its light to 0.1 arc seconds in diameter. Thus HST observations will allow us to probe the near-nuclear environments that are literally impossible to probe from the ground. Moreover, such high-resolution observations will also allow us to make meaningful comparisons at similar spatial resolutions as the ground-based observations of low redshift quasars (approximately 1 kpc), will allow us to compare the radio and rest-frame UV morphologies at similar angular resolutions (few tenths of an arc second), and allow us to probe the important nuclear environment on present-day galaxy scales (less than about 1 to 10 kpc). Thus, while HST data would be unique in the type of information it is able to provide, it also is a strong compliment to the data in the radio, optical and IR that has already been obtained. ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. No special scheduling is required. ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. No special calibration exposures are required. ------------------------------------------------------------------------------------ 8. Additional comments or special requests. We we originally proposed this project, we asked for 7.50 hours of exposure time and were granted the full amount of spacecraft time estimated during Phase I (13.23 hours). However, the Phase II resource estimator claims that our 7.50 hours of exposure time only requires about 10.1 hours of spacecraft time. We thus adjusted the number of exposures to fill out the rest of the time. To prevent a lot of work, we keep the original estimates in the written portions of Phase II, namely one hour in the narrow-band images and a half an hour in each of the broad band images. Our sensitivity estimates are also based on these original numbers. In case of a conflict between what we have done here and our original PhaseI estimates, we have a completed PhaseII form with our original exposure break-up in it. Thus if there is a problem, please write Matt Lehnert at lehnert@sunlight.llnl.gov for a copy of the Phase II form with the original numbers. ------------------------------------------------------------------------------------ 9. Description of previous HST work. Heckman -- PI on 3591. FOC images of sample delivered a few months ago. FOS spectra of a subset will be obtained later in Cycle 3. PI on 4370. No data yet obtained. Miley -- PI on 2438. "Hubble Space Telescope Imaging of Distant Galaxies: 4C 41.17 at z = 3.8" Miley, G. K., Chambers, K. C., van Bruegel, W., and Macchetto, D., ApJ, 401, L69, 1993. Page 4 ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). The reduction of the images will take place IGPP and the various participating institutions. STSDAS/IRAF is running at all of them. Additionally, normal institutional support is provided for each participating investigator by their respective host institutions. ------------------------------------------------------------------------------------ 11. Address Information Name: Matthew D Lehnert Category: PI Institution: 2460 Address: Institute for Geophysics and Planetary Physics Lawrence Livermore National Lab 7000 East Ave., P. O. Box 808, L-413 City: Livermore State: CA Zip Code: 94550 Country: US Telephone: (510) 423-6013 Telex (or e-mail): lehnert@sunlight.llnl.gov ------------------------------------------------------------------------------------ Name: Category: CON Institution: Address: City: State: Zip Code: Country: Telephone: Telex (or e-mail): ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5393 [ 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 PKS0445+097 E,314,325 RA=04H 45M 37.07S +/- 0.05S, B1950 Z=2.114 1 SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 4C+09.17 DEC=+09D 45' 36.2" +/-0.3" 2 0.05 3 SURF(1216)=5 +/- 2 E-17 V=19.55 +/- 0.1 Comments: FLUXVAL_1 AND FLUXVAL_2 ARE THE DESIRED 3 SIGMA DETECTION LIMITS OF THE CONTINUUM AND LYMAN-ALPHA IMAGING (LYMAN-ALPHA IN UNITS OF FLUX, NOT FLUX DENSITY). FLUXVAL_3 IS THE TOTAL V MAG OF THE QUASAR. ------------------------------------------------------------------------------------------------------------------------------------ 2 MRC0549-213 E,314,325 RA=05H 49M 50.56S +/- 0.05S, B1950 Z=2.245 1 SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- DEC=-21D 20' 29.6" +/- 0.3" 2 0.05 3 SURF(1216)=5 +/- 2 E-17 V=20.0 +/- 0.5 Comments: FLUXVAL_1 AND FLUXVAL_2 ARE THE DESIRED 3 SIGMA DETECTION LIMITS OF THE CONTINUUM AND LYMAN-ALPHA IMAGING (LYMAN-ALPHA IN UNITS OF FLUX PER HST PSF, NOT FLUX DENSITY). FLUXVAL_3 IS THE TOTAL V MAG OF THE QUASAR. ------------------------------------------------------------------------------------------------------------------------------------ 3 PKS1318+113 E,314,325 RA=13H 18M 49.63S +/- 0.05S, B1950 Z=2.175 1 SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 4C11.45 DEC=+11D 22' 31.5" +/- 0.3" 2 0.05 3 SURF(1216)=5 +/- 2 E-17 V=19.13 +/- 0.1 Comments: FLUXVAL_1 AND FLUXVAL_2 ARE THE DESIRED 3 SIGMA DETECTION LIMITS OF THE CONTINUUM AND LYMAN-ALPHA IMAGING (LYMAN-ALPHA IN UNITS OF FLUX PER HST PSF, NOT FLUX DENSITY). FLUXVAL_3 IS THE TOTAL V MAG OF THE QUASAR. ------------------------------------------------------------------------------------------------------------------------------------ 4 4C57.29 E,314,325 RA=16H 58M 53.44S +/- 0.05S, B1950 Z=2.174 1 SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 1658+575 DEC=57D 35' 52.4" +/- 0.3" 2 0.05 3 SURF(1216)=5 +/- 2 E-17 V=17.9 +/- 0.2 Comments: FLUXVAL_1 AND FLUXVAL_2 ARE THE DESIRED 3 SIGMA DETECTION LIMITS OF THE CONTINUUM AND LYMAN-ALPHA IMAGING (LYMAN-ALPHA IN UNITS OF FLUX PER HST PSF, NOT FLUX DENSITY). FLUXVAL_3 IS THE TOTAL V MAG OF THE QUASAR. ------------------------------------------------------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 5393 [ 6] ------------------------------------------------------------------------------------------------------------------------------------ 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| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 5 PKS2338+042 E,314,325 RA=23H 38M 24.66S +/- 0.05S, B1950 Z=2.591 1 SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 4C04.81 DEC=+04D 14' 37.2" +/- 0.3" 2 0.05 3 SURF(1216)=5 +/- 2 E-17 V=19.5 +/- 0.2 Comments: FLUXVAL_1 AND FLUXVAL_2 ARE THE DESIRED 3 SIGMA DETECTION LIMITS OF THE CONTINUUM AND LYMAN-ALPHA IMAGING (LYMAN-ALPHA IN UNITS OF FLUX PER HST PSF, NOT FLUX DENSITY). FLUXVAL_3 IS THE TOTAL V MAG OF THE QUASAR. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5393 [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 1 PKS0445+097 WFPC2 IMAGE PC1 F555W 5407 CR-SPLIT=NO 3 700S 3 1 1 CYCLE 4 1800S SAME ORIENT FOR 2 AS 1 Comments: CONTINUUM IMAGE OF QUASAR IN THE PLANETARY CAMERA WITH F555W. SHOULD BE 3 EXPOSURES OF 600SEC. ------------------------------------------------------------------------------------------------------------------------------------ 2 PKS0445+097 WFPC2 IMAGE FQUVN33 FQUVN33 3765 CR-SPLIT=NO 5 1000S 3 2 1 CYCLE 4 4800S Comments: FOR THESE EXPOSURES, THE REDSHIFTED [OII] FILTER SHOULD BE ROTATED BY -33 DEGREES. THE FILTER NAME IS FQUVN33. PLEASE MAKE SURE THAT OBJECT FALLS ON THE FILTER. ------------------------------------------------------------------------------------------------------------------------------------ 3 MRC0549-213 WFPC2 IMAGE PC1 F555W 5407 CR-SPLIT=NO 3 700S 3 1 3 CYCLE 4 1800S SAME ORIENT FOR 4 AS 3 Comments: CONTINUUM IMAGE OF QUASAR IN THE PLANETARY CAMERA WITH F555W. SHOULD BE 3 EXPOSURES OF 600SEC. ------------------------------------------------------------------------------------------------------------------------------------ 4 MRC0549-213 WFPC2 IMAGE WF2 FQUVN 3986 CR-SPLIT=NO 5 1000S 3 2 3 CYCLE 4 4800S Comments: THIS IS A NARROW-BAND EXPOSURE OF QUASAR USING THE QUAD REDSHIFTED [OII] FILTER. THE WAVELENGTH OF THE FILTER SHOULD MATCH THAT OF REDSHIFTED LYMAN ALPHA AT Z=2.245. ------------------------------------------------------------------------------------------------------------------------------------ 5 PKS1318+113 WFPC2 IMAGE PC1 F555W 5407 CR-SPLIT=NO 3 700S 3 1 2 CYCLE 4 1800S SAME ORIENT FOR 6 AS 5 Comments: CONTINUUM IMAGING OF QUASAR IN F555W AND THE PLANETARY CAMERA. ------------------------------------------------------------------------------------------------------------------------------------ 6 PKS1318+113 WFPC2 IMAGE WF4 FQUVN 3839 CR-SPLIT=NO 5 1000S 3 2 2 CYCLE 4 4800S Comments: EXPOSURES OF REDSHIFTED LYMAN- ALPHA OF THIS QUASAR. THE REDSHIFT IS 2.171. ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5393 [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 7 4C57.29 WFPC2 IMAGE PC1 F555W 5407 CR-SPLIT=NO 7 300S 3 1 5 CYCLE 4 1800S SAME ORIENT FOR 8 AS 7 Comments: CONTINUUM IMAGING OF 4C57.29 USING THE PLANETARY CAMERA. THIS IS THE BRIGHTEST QSO AND SO IT IS 5 EXPOSURES X 6 MIN IN THE CONTINUUM INSTEAD OF 3 EXPOSURES X 10 MIN. ------------------------------------------------------------------------------------------------------------------------------------ 8 4C57.29 WFPC2 IMAGE WF4 FQUVN 3839 CR-SPLIT=NO 5 1000S 3 2 5 CYCLE 4 4800S Comments: NARROW-BAND IMAGING USING THE QUAD REDSHIFTED [OII] FILTER OF QUASAR AT REDSHIFTED LYMAN ALPHA. THE REDSHIFT IS 2.173. ------------------------------------------------------------------------------------------------------------------------------------ 9 PKS2338+042 WFPC2 IMAGE PC1 F555W 5407 CR-SPLIT=NO 3 700S 3 1 4 CYCLE 4 1800S SAME ORIENT FOR 10 AS 9 Comments: CONTINUUM IMAGING OF PKS2338+042 USING F555W AND THE PLANETARY CAMERA. ------------------------------------------------------------------------------------------------------------------------------------ 10 PKS2338+042 WFPC2 IMAGE WF3 F437N 4369 CR-SPLIT=NO 5 1000S 3 2 4 CYCLE 4 4800S Comments: NARROW-BAND IMAGING OF PKS2338+042 AT REDSHIFTED LYMAN ALPHA. THE REDSHIFT IS 2.594 AND REDSHIFTED LYMAN ALPHA IS AT APPROXIMATELY 4367 ANGSTROMS. ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5393 [ 9] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations WFPC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters CR-SPLIT ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 9.25 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category QUASARS & AGN ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category HOST GALAXIES ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 4; SAME ORIENT FOR 2 AS 1 SAME ORIENT FOR 4 AS 3 SAME ORIENT FOR 6 AS 5 SAME ORIENT FOR 8 AS 7 SAME ORIENT FOR 10 AS 9 CYCLE 4 ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F555W FQUVN33 FQUVN F437N ------------------------------------------------------------------------------------------------------------------------------------ Target Names PKS0445+097 4C+09.17 MRC0549-213 PKS1318+113 4C11.45 4C57.29 1658+575 PKS2338+042 4C04.81 ------------------------------------------------------------------------------------------------------------------------------------