! $Id: 5393,v 9.1 1994/07/27 17:27:53 pepsa Exp $ coverpage: title_1: THE NATURE OF THE HOST GALAXIES OF HIGH-REDSHIFT, title_2: RADIO-LOUD QUASARS sci_cat: QUASARS & AGN sci_subcat: HOST GALAXIES proposal_for: GO pi_fname: MATTHEW pi_mi: D pi_lname: LEHNERT pi_inst: INSTITUTE FOR GEOPHYSICS AND PLANETARY PHYSICS pi_country: US pi_phone: (510) 423-6013 hours_pri: 9.25 num_pri: 5 wf_pc: Y off_fname: CHARLES off_lname: ALCOCK off_title: DIRECTOR OF IGPP off_inst: 2460 off_addr_1: INSTITUTE FOR GEOPHYSICS AND PLANETARY PHYSICS off_addr_2: LAWRENCE LIVERMORE NATIONAL LAB off_addr_3: 7000 EAST AVE., P.O. BOX 808, L-413 off_city: LIVERMORE off_state: CA off_zip: 94550 off_country: US off_phone: (510) 423-0621 ! end of coverpage abstract: line_1: The co-moving space density of highly luminous radio-loud quasars has line_2: decreased by roughly 3 orders of magnitude from z=2-3 to the current line_3: epoch. Understanding the physical processes responsible for this line_4: decrease could profoundly influence how we think the universe and line_5: galaxies have evolved. In order to make the first steps in line_6: understanding these physical processes, we propose to conduct a narrow line_7: (at Lyman alpha) and broad-band imaging survey of five radio-loud, line_8: high-z (z=2) quasars using WFPC2. HST observations are crucial for line_9: separating the "blinding" nuclear emission (AGN) from that of the line_10: extended "fuzz" (parent galaxy). They will allow quantitative line_11: comparisons of the emission-line and continuum morphologies of the host line_12: galaxies of high-z quasars to those of comparable high-z radio line_13: galaxies, and of low-z quasars. Such comparisons will allow us to line_14: investigate whether or not radio-loud quasars and radio galaxies are line_15: members of the same parent population as is fashionable in the AGN line_16: unification schemes and how luminous AGN have evolved from redshifts of line_17: 2-3. ! ! end of abstract general_form_proposers: lname: LEHNERT fname: MATTHEW mi: D inst: 2460 country: US ! lname: HECKMAN fname: TIMOTHY mi: M inst: 2380 country: US ! lname: VAN BREUGEL fname: WIL inst: 2460 country: US ! lname: MILEY fname: GEORGE mi: K inst: 6870 country: NL esa: Y ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observational plan can be summarized as obtaining deep optical line_2: broad and narrow-band images of 5 high-redshift radio-loud quasars line_3: The continuum broad-band images will be taken using the planetary line_4: camera in combination with the filter F555W. The narrow-band filters line_5: were choosen to correspond to the wavelength of redshifted Lyman-alpha line_6: in each of these quasars. The narrow-band images will be obtained line_7: with the wide field camera. The main two observational constraints line_8: on this program is our desire to detect faint emission line gas and line_9: continuum emission and yet not saturate the active galactic nucleus line_10: of these quasars. To meet these constraints we have chosen to split line_11: the exposures in to sets of 3 each for the continuum and the narrow-band line_12: imaging. This technique has the added advantage that it will aid in line_13: cosmic ray removal. To detect continuum emission down to 28 V mag per line_14: HST PSF requires total integration times of 30 minutes. Thus for line_15: each quasar we will obtain 3 exposures x 10 minutes per exposure line_16: for 30 minutes of exposure time, except for 4C57.29, the brightest line_17: of the quasars, for which we will obtain 6 exposures x 5 minutes line_18: per exposure. For the narrow-band imaging, exposures of about line_19: an hour will allow us to probe Lyman-alpha emitting line_20: structures down few times 10E-17 ergs per sec per square cm per line_21: HST PSF. Such fluxes are sufficient to meet our scientific goals. line_22: We therefore have decided to split to images into sets of 3 images line_23: per quasar through the narrow-band filter to aid in cosmic ray ! question: 3 section: 2 line_1: removal and to ensure that the images do not saturate the bright quasar line_2: nucleus. Each quasar will be exposed for a hour following the line_3: prescription 3 exposures x 20 minutes per exposure. To match the line_4: wavelength of redshifted Lyman-alpha in these quasars we will use the line_5: quadrant filter, "redshifted [OII]" (FQUVN) for four of the quasars and line_6: F437N for PKS2338+042. The details of the quasar-filter combinations line_7: are: For PKS0445+097 at z=2.110, we would like to use the "redshifted line_8: [OII]" filter rotated by -33 degrees and use WF2 for its aperature. line_9: This should give a central wavelength of 3763 angstroms for the filter line_10: which is close to the wavelength of redshifted Lyman-alpha in line_11: PKS0445+097 (3781 angstroms). For MRC0549-213 at z=2.245, we would line_12: like to use the "redshifted [OII]" filter in its nominal position and line_13: use WF2 for the aperature. This aperature corresponds to a central line_14: wavelength of 3986 angstroms (Lyman-alpha in MRC0549-213 is at 3945 line_15: angstroms). For PKS1318+113 at z=2.171, we would again like to use the line_16: FQUVN filter in its nominal position and use WF4 for the aperature. line_17: This aperature corresponds to a central wavelength of 3839 angstroms line_18: (redshifted Lyman-alpha for PKS1318+113 is at 3855 angstroms). For line_19: 4C57.29, again we would like to use FQUVN in its nominal position and line_21: use WF4 as the aperature to give a central wavelength of 3839 angstroms line_22: (Lyman-alpha for 4C57.29 is at 3857 angstroms). For PKS2338+042 line_23: we would like to use the narrow-band filter F437N. ! question: 4 section: 1 line_1: The observational constraint that limits our ability to say anything line_2: meaningful about the properties of the extended emission ("fuzz") line_3: around high-redshift quasars is the limit of how well we can separate line_4: the bright, nuclear emission from the AGN from the fuzz. At typical line_5: ground based seeing (1 arc second), the nuclear light is spread over the line_6: central 10 kpc of the fuzz. Previous ground-based data has shown that line_7: quasars at redshifts of 2 to 3, typically have isophotal radii of at line_8: most 9 arc seconds in the rest-frame UV (typically down to 27th mag line_9: per square arc seconds at B) and about 12 arc seconds in Lyman alpha line_10: (down to 10E-17 ergs per sec per square cm). This implies that seeing line_11: of an arc second is required just to show that the quasars are extended line_12: (never mind actually showing the detailed morphology). HST is crucial line_13: if we are to make secure detections of the host galaxies of line_14: high-redshift quasars by allowing us to rather unambiguously remove the line_15: contribution of the AGN by, roughly speaking, restricting its light to line_16: 0.1 arc seconds in diameter. Thus HST observations will allow us to line_17: probe the near-nuclear environments that are literally impossible to line_18: probe from the ground. Moreover, such high-resolution observations will line_19: also allow us to make meaningful comparisons at similar spatial line_20: resolutions as the ground-based observations of low redshift quasars line_21: (approximately 1 kpc), will allow us to compare the radio and line_22: rest-frame UV morphologies at similar angular resolutions (few tenths of line_23: an arc second), and allow us to probe the important nuclear environment ! question: 4 section: 2 line_1: on present-day galaxy scales (less than about 1 to 10 kpc). Thus, while line_2: HST data would be unique in the type of information it is able to line_3: provide, it also is a strong compliment to the data in the radio, line_4: optical and IR that has already been obtained. ! question: 5 section: 1 line_1: No special scheduling is required. ! question: 6 section: 1 line_1: No special calibration exposures are required. ! ! ! question: 8 section: 1 line_1: We we originally proposed this project, we asked for 7.50 hours of line_2: exposure time and were granted the full amount of spacecraft time line_3: estimated during Phase I (13.23 hours). However, the Phase II line_4: resource estimator claims that our 7.50 hours of exposure time line_5: only requires about 10.1 hours of spacecraft time. We thus adjusted line_6: the number of exposures to fill out the rest of the time. line_7: To prevent a lot of work, we keep the original estimates in line_8: the written portions of Phase II, namely one hour in the line_9: narrow-band images and a half an hour in each of the broad line_10: band images. Our sensitivity estimates are also based on these line_11: original numbers. In case of a conflict between what we have line_12: done here and our original PhaseI estimates, we have a completed line_13: PhaseII form with our original exposure break-up in it. Thus line_14: if there is a problem, please write Matt Lehnert at line_15: lehnert@sunlight.llnl.gov for a copy of the Phase II form line_16: with the original numbers. ! question: 9 section: 1 line_1: Heckman -- PI on 3591. FOC images of sample delivered a few months ago. line_2: FOS spectra of a subset will be obtained later in Cycle 3. line_3: PI on 4370. No data yet obtained. line_4: Miley -- PI on 2438. "Hubble Space Telescope Imaging of Distant line_5: Galaxies: 4C 41.17 at z = 3.8" Miley, G. K., Chambers, K. C., line_6: van Bruegel, W., and Macchetto, D., ApJ, 401, L69, 1993. ! question: 10 section: 1 line_1: The reduction of the images will take place IGPP and the various line_2: participating institutions. STSDAS/IRAF is running at all of them. line_3: Additionally, normal institutional support is provided for each line_4: participating investigator by their respective host institutions. ! !end of general form text general_form_address: lname: Lehnert fname: Matthew mi: D category: PI inst: 2460 addr_1: Institute for Geophysics and Planetary Physics addr_2: Lawrence Livermore National Lab addr_3: 7000 East Ave., P. O. Box 808, L-413 city: Livermore state: CA zip: 94550 country: US phone: (510) 423-6013 telex: lehnert@sunlight.llnl.gov ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PKS0445+097 name_2: 4C+09.17 descr_1: E,314,325 pos_1: RA=04H 45M 37.07S +/- 0.05S, pos_2: DEC=+09D 45' 36.2" +/-0.3" equinox: B1950 rv_or_z: Z=2.114 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE THE comment_2: DESIRED 3 SIGMA DETECTION LIMITS comment_3: OF THE CONTINUUM AND LYMAN-ALPHA comment_4: IMAGING (LYMAN-ALPHA IN UNITS comment_5: OF FLUX, NOT FLUX DENSITY). comment_6: FLUXVAL_3 IS THE TOTAL V MAG comment_7: OF THE QUASAR. fluxnum_1: 1 fluxval_1: SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 0.05 fluxnum_2: 2 fluxval_2: SURF(1216)=5 +/- 2 E-17 fluxnum_3: 3 fluxval_3: V=19.55 +/- 0.1 ! targnum: 2 name_1: MRC0549-213 descr_1: E,314,325 pos_1: RA=05H 49M 50.56S +/- 0.05S, pos_2: DEC=-21D 20' 29.6" +/- 0.3" equinox: B1950 rv_or_z: Z=2.245 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE THE comment_2: DESIRED 3 SIGMA DETECTION LIMITS comment_3: OF THE CONTINUUM AND LYMAN-ALPHA comment_4: IMAGING (LYMAN-ALPHA IN UNITS comment_5: OF FLUX PER HST PSF, NOT FLUX comment_6: DENSITY). FLUXVAL_3 IS THE TOTAL V comment_7: MAG OF THE QUASAR. fluxnum_1: 1 fluxval_1: SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 0.05 fluxnum_2: 2 fluxval_2: SURF(1216)=5 +/- 2 E-17 fluxnum_3: 3 fluxval_3: V=20.0 +/- 0.5 ! targnum: 3 name_1: PKS1318+113 name_2: 4C11.45 descr_1: E,314,325 pos_1: RA=13H 18M 49.63S +/- 0.05S, pos_2: DEC=+11D 22' 31.5" +/- 0.3" equinox: B1950 rv_or_z: Z=2.175 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE THE comment_2: DESIRED 3 SIGMA DETECTION LIMITS comment_3: OF THE CONTINUUM AND LYMAN-ALPHA comment_4: IMAGING (LYMAN-ALPHA IN UNITS comment_5: OF FLUX PER HST PSF, NOT FLUX comment_6: DENSITY). FLUXVAL_3 IS THE TOTAL V comment_7: MAG OF THE QUASAR. fluxnum_1: 1 fluxval_1: SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 0.05 fluxnum_2: 2 fluxval_2: SURF(1216)=5 +/- 2 E-17 fluxnum_3: 3 fluxval_3: V=19.13 +/- 0.1 ! targnum: 4 name_1: 4C57.29 name_2: 1658+575 descr_1: E,314,325 pos_1: RA=16H 58M 53.44S +/- 0.05S, pos_2: DEC=57D 35' 52.4" +/- 0.3" equinox: B1950 rv_or_z: Z=2.174 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE THE comment_2: DESIRED 3 SIGMA DETECTION LIMITS comment_3: OF THE CONTINUUM AND LYMAN-ALPHA comment_4: IMAGING (LYMAN-ALPHA IN UNITS comment_5: OF FLUX PER HST PSF, NOT FLUX comment_6: DENSITY). FLUXVAL_3 IS THE TOTAL V comment_7: MAG OF THE QUASAR. fluxnum_1: 1 fluxval_1: SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 0.05 fluxnum_2: 2 fluxval_2: SURF(1216)=5 +/- 2 E-17 fluxnum_3: 3 fluxval_3: V=17.9 +/- 0.2 ! targnum: 5 name_1: PKS2338+042 name_2: 4C04.81 descr_1: E,314,325 pos_1: RA=23H 38M 24.66S +/- 0.05S, pos_2: DEC=+04D 14' 37.2" +/- 0.3" equinox: B1950 rv_or_z: Z=2.591 comment_1: FLUXVAL_1 AND FLUXVAL_2 ARE THE comment_2: DESIRED 3 SIGMA DETECTION LIMITS comment_3: OF THE CONTINUUM AND LYMAN-ALPHA comment_4: IMAGING (LYMAN-ALPHA IN UNITS comment_5: OF FLUX PER HST PSF, NOT FLUX comment_6: DENSITY). FLUXVAL_3 IS THE TOTAL V comment_7: MAG OF THE QUASAR. fluxnum_1: 1 fluxval_1: SURF(V)=28.0 +/- 0.3,SIZE=0.1 +/- 0.05 fluxnum_2: 2 fluxval_2: SURF(1216)=5 +/- 2 E-17 fluxnum_3: 3 fluxval_3: V=19.5 +/- 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PKS0445+097 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F555W wavelength: 5407 num_exp: 3 time_per_exp: 700S s_to_n: 3 s_to_n_time: 1800S fluxnum_1: 1 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 2 AS 1 comment_1: CONTINUUM IMAGE OF QUASAR IN THE comment_2: PLANETARY CAMERA WITH F555W. SHOULD comment_3: BE 3 EXPOSURES OF 600SEC. ! linenum: 2.000 targname: PKS0445+097 config: WFPC2 opmode: IMAGE aperture: FQUVN33 sp_element: FQUVN33 wavelength: 3765 num_exp: 5 time_per_exp: 1000S s_to_n: 3 s_to_n_time: 4800S fluxnum_1: 2 priority: 1 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: FOR THESE EXPOSURES, THE REDSHIFTED comment_2: [OII] FILTER SHOULD BE ROTATED BY comment_3: -33 DEGREES. THE FILTER NAME IS comment_4: FQUVN33. PLEASE MAKE SURE THAT comment_5: OBJECT FALLS ON THE FILTER. ! linenum: 3.000 targname: MRC0549-213 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F555W wavelength: 5407 num_exp: 3 time_per_exp: 700S s_to_n: 3 s_to_n_time: 1800S fluxnum_1: 1 priority: 3 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 4 AS 3 comment_1: CONTINUUM IMAGE OF QUASAR IN THE comment_2: PLANETARY CAMERA WITH F555W. SHOULD comment_3: BE 3 EXPOSURES OF 600SEC. ! linenum: 4.000 targname: MRC0549-213 config: WFPC2 opmode: IMAGE aperture: WF2 sp_element: FQUVN wavelength: 3986 num_exp: 5 time_per_exp: 1000S s_to_n: 3 s_to_n_time: 4800S fluxnum_1: 2 priority: 3 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: THIS IS A NARROW-BAND EXPOSURE OF comment_2: QUASAR USING THE QUAD REDSHIFTED comment_3: [OII] FILTER. THE WAVELENGTH OF comment_4: THE FILTER SHOULD MATCH THAT OF comment_5: REDSHIFTED LYMAN ALPHA AT Z=2.245. ! linenum: 5.000 targname: PKS1318+113 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F555W wavelength: 5407 num_exp: 3 time_per_exp: 700S s_to_n: 3 s_to_n_time: 1800S fluxnum_1: 1 priority: 2 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 6 AS 5 comment_1: CONTINUUM IMAGING OF QUASAR IN comment_2: F555W AND THE PLANETARY CAMERA. ! linenum: 6.000 targname: PKS1318+113 config: WFPC2 opmode: IMAGE aperture: WF4 sp_element: FQUVN wavelength: 3839 num_exp: 5 time_per_exp: 1000S s_to_n: 3 s_to_n_time: 4800S fluxnum_1: 2 priority: 2 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: EXPOSURES OF REDSHIFTED LYMAN-ALPHA comment_2: OF THIS QUASAR. THE REDSHIFT comment_3: IS 2.171. ! linenum: 7.000 targname: 4C57.29 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F555W wavelength: 5407 num_exp: 7 time_per_exp: 300S s_to_n: 3 s_to_n_time: 1800S fluxnum_1: 1 priority: 5 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 8 AS 7 comment_1: CONTINUUM IMAGING OF 4C57.29 comment_2: USING THE PLANETARY CAMERA. comment_3: THIS IS THE BRIGHTEST QSO AND comment_4: SO IT IS 5 EXPOSURES X 6 MIN IN THE comment_5: CONTINUUM INSTEAD OF 3 comment_6: EXPOSURES X 10 MIN. ! linenum: 8.000 targname: 4C57.29 config: WFPC2 opmode: IMAGE aperture: WF4 sp_element: FQUVN wavelength: 3839 num_exp: 5 time_per_exp: 1000S s_to_n: 3 s_to_n_time: 4800S fluxnum_1: 2 priority: 5 param_1: CR-SPLIT = NO req_1: CYCLE 4; comment_1: NARROW-BAND IMAGING USING THE comment_2: QUAD REDSHIFTED [OII] FILTER OF comment_3: QUASAR AT REDSHIFTED LYMAN comment_4: ALPHA. THE REDSHIFT IS 2.173. ! linenum: 9.000 targname: PKS2338+042 config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F555W wavelength: 5407 num_exp: 3 time_per_exp: 700S s_to_n: 3 s_to_n_time: 1800S fluxnum_1: 1 priority: 4 param_1: CR-SPLIT = NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 10 AS 9 comment_1: CONTINUUM IMAGING OF comment_2: PKS2338+042 USING F555W comment_3: AND THE PLANETARY CAMERA. ! linenum: 10.000 targname: PKS2338+042 config: WFPC2 opmode: IMAGE aperture: WF3 sp_element: F437N wavelength: 4369 num_exp: 5 time_per_exp: 1000S s_to_n: 3 s_to_n_time: 4800S fluxnum_1: 2 priority: 4 param_1: CR-SPLIT = NO req_1: CYCLE 4 comment_1: NARROW-BAND IMAGING OF comment_2: PKS2338+042 AT REDSHIFTED LYMAN comment_3: ALPHA. THE REDSHIFT IS 2.594 comment_4: AND REDSHIFTED LYMAN ALPHA comment_5: IS AT APPROXIMATELY 4367 ANGSTROMS. ! ! end of exposure logsheet ! No scan data records found