! Proposal 5982, submission 2 ! PI: David Sanders ! Received Tue Jun 27 00:19:41 EDT 1995 ! From: jason@galileo.IFA.Hawaii.Edu ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5982,v 20.1 1995/09/22 12:32:21 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Doug Van Orsow ! Phone: 410 338-4568 , E-mail: vanorsow@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Sun Dec 18 10:07:27 EST 1994 ! Proposal_Information ! Section 4 Title: Imaging of a Complete Sample of the Nearest Infrared Quasars Proposal_Category: GO Scientific_Category: Quasars Cycle: 5 Investigators PI_name: David Sanders PI_Institution: University of Hawaii CoI_Name: Sylvain Veilleux CoI_Institution: Kitt Peak National Observatory Contact: ! Y or N (designate at most one contact) CoI_Name: Joe Mazzarella CoI_Institution: California Institute of Technology Contact: ! Y or N (designate at most one contact) CoI_Name: Joshua Barnes CoI_Institution: University of Hawaii Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose high resolution imaging with the Planetary Camera (PC) of a nearly complete sample (10/12) of the nearest infrared quasars that have been discovered in the IRAS database. These objects appear to represent a critical evolutionary link between ultraluminous infrared galaxies and optical QSOs. Ground-based observations suggest that these objects contain a mixture of nuclear starburst and AGN components, both of which are fueled by a tremendous reservoir of molecular gas that has been funneled into the merger nucleus during the merger of two gas- rich galaxies. PC images in B and I filters will be used to trace the distribution of different stellar populations, to separate out point source components, to trace the effects of the merger process in these galaxies, and to search for the presence of bars or other such structures that may serve to funnel gas or stars into a putative central AGN. (Note: This proposal was awarded time in the first call for Cycle 1, but was subsequently given supplemental status in the reassessment phase to carry out a limited search for double nuclei, but it was never executed. A limited search for double nuclei in 5 objects was carried out with FOC/96 in Cycle 2.) Questions ! Free format text (please update) Observing_Description: PC images in two filters (B,I) will be obtained for the sample of 10 `infrared quasars'. For each object and each color, two exposures will be obtained with 10:1 ratio in integration time. The short exposure (4 M) will permit imaging of the brightest regions without saturation and will assist in the removal of cosmic rays, while the long exposure (30--40 M) will have sufficient integration time to detect the mean surface brightness per pixel in the central 2" regions (~3--6 kpc) of each source at a S/N ratio > 5. Our choice of filters is based of different color maps that have been made from the ground. B-I always shows the largest spatial variations, and we propose to use this color to set maximum constraints on the stellar populations. I-band images typically show more spatial detail in regions of high obscuration than can be seen at R. Comparison of images of each object in different filters will aid in the identification of point sources, and allow us to account for the possibility of variations in the extinction across the source. Extinction is much less severe in the warm infrared galaxies being observed as compared to much cooler ultraluminous infrared objects such as Arp 220, as evidenced by the large fraction of observed Seyfert 1 spectra and much less extreme U-B colors. Any remaining dust screen along the line of sight to the nuclear source will decrease its observed brightness, but is not calculated to significantly widen the images of nuclei at B and I wavelengths. We have used the WFPC2 quantum efficiency tables for the appropriate B,I filters to determine the expected S/N for different exposures. Our scientific goals require that we reach at least S/N > 5 in 0.046" pixels for each color if we are to make use of the maximum resolution of the PC. The following calculations assume an F0 spectrum (type 3): The ratio (2 / 0.046)^2 means that the average mag per 0.046" pixel is 8.2 mag fainter than the mag within the central 2". The magnitude in the central 2" is typically 1--2.5 mag fainter than the total mag. For example, in the central 2" the objects range from 15--20 mag at V and 13.5--18 mag at R. For the brightest sources we can easily reach S/N > 10 per pix in a 30--40 M integration, while for the faintest sources S/N will be ~5. Real_Time_Justification: None Over the past five years we have vigorously pursued ground- based optical and near infrared imaging of both cooler ultraluminous infrared galaxies and our proposed sample of infrared quasars. All of the cooler ultraluminous infrared galaxies have been resolved as doubles, but most of the slightly more distant, and presumably more evolved `infrared quasars' eluded separation. CCD images (B,g,r,i) were first obtained at Palomar for the complete sample of 12 infrared quasars (Figure 1), allowing us to study their morphology on ~1" scales (IRAS 0857+39 and Mrk 463A/B have double nuclei). The majority of these objects have since been imaged in 0.5- 0.7" seeing at the CFHT, and although the central brightness profiles are more oval in shape, only one additional source (PKS 1345+12) was resolved into a double. Our FOC/96 proposal (Cycle 2) that was designed as a quick search for double nuclei in 5 objects revealed 4 additional doubles (IRAS 12071 -0444, IRAS 05189-2524, IRAS 15206-3342, Mrk 1014) with separations varying from 0.15--0.3", along with multiple lower intensity `knots', and 1 dominant single nucleus object Mrk 231. It is interesting to note that the latter object has recently been claimed to have a second heavily reddened nucleus at 3" separation from the central peak (Armus et al. 1994), however our inability to observe into the red with the FOC plus the insensitivity to low level structure in the images means that we were probably insensitive to the second peak. Our current WFPC2 proposal should solve these problems. We have also obtained high-quality optical (4000-- 8500Angstrom) spectra (Veilleux et al. 1994; Kim 1994), and are in the process of obtaining near-infrared (K-band) spectra of all of the objects in Figure 1. We have proposed to obtain near/mid/far-infrared spectra of several of these objects with the ISO satellite, and we will also attempt to detect X-rays from some of these objects with the ASCA satellite. We also have obtained radio continuum images with the VLA and millimeterwave and submillimeter continuum and spectral line data for all of our objects. Finally, we hope in the next year to be able to obtain near-infrared images at ~0.2" resolution from Mauna Kea using adaptive optics techniques. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: IRAS01003-2238 Description: GALAXY, ULTRALUMINOUS IR GAL Position: RA=01H02M49.83S+/-0.06S, DEC=-22D21'56.3"+/-1" Equinox: 2000 RV_or_Z: Z=0.118 Flux: SURF(B)=22.24+/-0.5, SURF(V)=21.22+/-0.5 Comments: Target_Number: 2 Target_Name: MRK1014 Alternate_Names: IRAS01572+0009 Description: GALAXY,ULTRALUMINOUS IR GAL, QSO, INTERACTING GALAXY Position: RA=01H59M50.18S+/-0.06S, DEC=+00D23'41.5"+/-1" Equinox: 2000 RV_or_Z: Z=0.163 Flux: SURF(B)=20.90+/-0.5, SURF(V)=20.44+/-0.5 Comments: Target_Number: 3 Target_Name: IRAS05189-2524 Description: GALAXY, ULTRALUMINOUS IR GAL, INTERACTING GALAXY Position: RA=05H21M01.53S+/-0.06S, DEC=-25D21'46.7"+/-1" Equinox: 2000 RV_or_Z: Z=0.0427 Flux: SURF(B)=21.81+/-0.5, SURF(V)=20.84+/-0.5 Comments: Target_Number: 4 Target_Name: IRAS17044+6720 Description: GALAXY, ULTRALUMINOUS IR GAL, QSO Position: RA=17H04M29.5S+/-0.06S, DEC=+67D20'25.5"+/-1" Equinox: B1950 ! RV_or_Z: Flux: SURF(V)=17.2+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 5 Target_Name: IRAS08572+3915 Description: GALAXY, ULTRALUMINOUS IR GAL, INTERACTING GALAXY Position: RA=09H00M25.42S+/-0.06S, DEC=+39D03'54.2"+/-1" Equinox: 2000 RV_or_Z: Z=0.058 Flux: SURF(B)=17.3+/-0.5, SURF(V)=16.1+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 6 Target_Name: IRAS12071-0444 Description: GALAXY, ULTRALUMINOUS IR GAL, INTERACTING GALAXY Position: RA=12H09M45.1S+/-0.06S, DEC=-05D01'13.7"+/-1" Equinox: 2000 RV_or_Z: Z=0.128 Flux: SURF(B)=17.85+/-0.5, SURF(V)=16.8+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 7 Target_Name: MRK231 Description: GALAXY, ULTRALUMINOUS IR GAL, QSO, INTERACTING GALAXY Position: RA=12H56M14.24S+/-0.06S, DEC=+56D52'26.1"+/-1" Equinox: 2000 RV_or_Z: Z=0.042 Flux: SURF(B)=14.42+/-0.5, SURF(V)=13.6+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 8 Target_Name: PKS1345+12 Description: GALAXY, ULTRALUMINOUS IR GAL, RADIO GALAXY Position: RA=13H47M33.55S+/-0.06S, DEC=+12D17'24.5"+/-1" Equinox: 2000 RV_or_Z: Z=0.121 Flux: SURF(B)=16.66+/-0.5, SURF(V)=15.6+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 9 Target_Name: MRK463 Description: GALAXY, ULTRALUMINOUS IR GAL, INTERACTING GALAXY Position: RA=13H56M02.74S+/-0.06S, DEC=+18D22'18.3"+/-1" Equinox: 2000 RV_or_Z: Z=0.051 Flux: SURF(B)=14.86+/-0.5, SURF(V)=14.2+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 10 Target_Name: IRAS15206+3342 Description: GALAXY, ULTRALUMINOUS IR GAL, INTERACTING GALAXY Position: RA=15H22M37.96S+/-0.06S, DEC=+33D31'36.6"+/-1" Equinox: 2000 RV_or_Z: Z=0.118 Flux: SURF(B)=15.21+/-0.5, SURF(V)=14.7+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 11 Target_Name: IRAS01003-2238-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=01H02M51.6S+/-0.06S, DEC=-22D23'00.2"+/-0.5" Equinox: 2000 Flux: V=16.0+/-0.5 Comments: Fixed_Targets ! Section 5.1 Target_Number: 13 Target_Name: IRAS05189-2524-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=05H20M54.5S+/-0.06S, DEC=-25D20'35.8"+/-0.5" Equinox: 2000 Flux: R=13.6+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 14 Target_Name: IRAS07598+6508-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=08H04M28.0S+/-0.06S, DEC=+65D00'01.4"+/-0.5" Equinox: 2000 Flux: R=14.1+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 15 Target_Name: IRAS08572+3915-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=09H00M20.5S+/-0.06S, DEC=+39D04'05.7"+/-0.5" Equinox: 2000 Flux: R=14.0+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 16 Target_Name: IRAS12071-0444-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=12H09M39.7S+/-0.06S, DEC=-05D00'05.4"+/-0.5" Equinox: 2000 Flux: R=14.1+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 17 Target_Name: MRK231-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=12H56M05.2S+/-0.06S, DEC=+56D53'20.4"+/-0.5" Equinox: 2000 Flux: R=16.6+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 18 Target_Name: PKS1345+12-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=13H47M28.5S+/-0.06S, DEC=+12D17'57.2"+/-0.5" Equinox: 2000 Flux: R=17.0+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 19 Target_Name: MRK463-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=13H56M01.9S+/-0.06S, DEC=+18D23'28.0"+/-0.5" Equinox: 2000 Flux: V=11.8+/-0.3 Comments: Fixed_Targets ! Section 5.1 Target_Number: 20 Target_Name: IRAS15206+3342-PSF Description: CALIBRATION, POINT SPREAD FUNCTION Position: RA=15H22M43.2S+/-0.06S, DEC=+33D30'04.7"+/-0.5" Equinox: 2000 Flux: R=14.1+/-0.3 Comments: ! This is a template for a single visit containing a single exposure ! Repeat exposure and visit blocks as needed Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling ! PCS MODE [Fine | Gyro] ! GUIDing TOLerance ! ORIENTation 43D TO 47D ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN