! Proposal 6835, submission 2 ! PI: Ann Zabludoff ! Received Fri Feb 9 23:30:44 EST 1996 ! From: mulchaey@ociw.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6835,v 4.1 1996/02/12 14:46:41 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6835,v 4.1 1996/02/12 14:46:41 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: Ready ! Phone: 410-338-4546 , E-mail: ready@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-1169.zabludoff.prop ! Date generated: Fri Dec 22 17:51:30 EST 1995 ! Proposal_Information ! Section 4 Title: The Detailed Morphology of Post-Merger Galaxies Proposal_Category: GO Scientific_Category: COSMOLOGY Cycle: 6 Investigators PI_name: Ann Zabludoff PI_Institution: Carnegie Observatories CoI_Name: Dennis Zaritsky CoI_Institution: Lick Observatory/University of California, Santa Cruz Contact: ! Y or N (designate at most one contact) CoI_Name: Christopher Mihos CoI_Institution: Johns Hopkins University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) From the Las Campanas Redshift Survey, the largest existing spectroscopic galaxy survey, we have drawn a unique and well- defined sample of 21 galaxies with the spectral and morphological signatures of evolved merger products. These galaxies have spectra indicating little or no on-going star formation and a significant young stellar population. Morphologically, the galaxies are disturbed, with tidal tails on scales of ~10 kpc. Because the observed tidal features survive at least ~ 1 Gyr after the merger, we are unable to use them to tightly constrain the time elapsed since the end of the starburst. This timescale is the key to determining (1) the duration and frequency of the post- starburst phase in the evolution of galaxies and (2) the fraction of the stellar mass created in the starburst. We propose to use the high spatial resolution of WFPC2 to detect the small-scale (< 1 kpc) features in five post-starburst galaxies that will enable us to measure the time since the merger to within a few 100 Myr. Questions ! Free format text (please update) Observing_Description: We propose to obtain WFPC2 observations through two filters (F439W and F702W) of the detailed morphology of post- starburst galaxies for which we have extensive ground-based imaging and spectroscopy. We require imaging in these two filters to identify the young stellar component, specifically its distribution near the nucleus and in the tidal tails where simulations predict it will accumulate after the merger. The angular size of the largest of the small-scale features described in the scientific justification corresponds to ~ 20 PC pixels for the typical redshift of our targets, z = 0.08. To conservatively estimate the significance of our detection of features at least this small in one orbit, we calculate the signal-to-noise (cf. WFPC2 Instrument Handbook) in a 2 * 2 sq PC pixel aperture for a young star cluster like those observed in NGC 1275 as point sources with the PC (M_V ~ -13; Holtzman Etal 1992). In a CR -split 30 minute exposure, we obtain a ~ 25Sigma detection in F439W and a ~ 85Sigma detection in F702W. We expect the galaxies' nuclei, non-axisymmetric features, and small scale zones of recent star formation to be at least as luminous. The ``wide'' R filter is requested, because (1) we have ground-based Johnson B and R images for calibration of the proposed images, (2) the transmission efficiency of F702W is much better than the standard Johnson R filter, and (3) the means of the transmission ranges of F439W and F702W are well separated. Because all of our targets have |b^II| > 50^degrees, galactic reddening is not a problem. Two filters are necessary since many of the non-axisymmetric features should also have distinguishing colors. At the typical redshifts of our targets, the PC field corresponds to ~ 30 kpc, enough to easily sample the features of interest within the central few kpc. From our ground-based images we know the orientation any tidal tails, which extend beyond ~ 10 kpc. We will request that the telescope be oriented so that these tidal tails, or any dwarf irregular galaxies (such as those coalescing from the tidal tails of the Antennae merging system; Mirabel, Dottori, & Lutz 1992) or globular clusters formed in these structures, are detectable with the WFC. There are no bright stars in the target fields. Real_Time_Justification: None. None. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: GAL-0217-4432 Alternate_Names: Description: GALAXY Position: RA = 02H 15M 43.24S +/- 0.1S, ! Most common specification format is DEC = -44D 46' 36.7" +/- 1.0" ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: V=+29600 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=17.7+/-0.5 ! Include at least V and B-V Comments: E+A Galaxy Fixed_Targets ! Section 5.1 Target_Number: 2 Target_Name: GAL-0400-4435 Alternate_Names: Description: GALAXY Position: RA = 03H 58M 23.42S +/- 0.1S,! Most common specification format is DEC = -44D 43' 40.3" +/- 1.0"! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: V=+30350 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=17.0+/-0.5 ! Include at least V and B-V Comments: E+A Galaxy Fixed_Targets ! Section 5.1 Target_Number: 3 Target_Name: GAL-1101-1210 Alternate_Names: Description: GALAXY Position: RA = 10H 58M 48.98S +/- 0.1S,! Most common specification format is DEC = -11D 54' 09.8" +/- 1.0"! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: V=+22380 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=18.4+/-0.5 ! Include at least V and B-V Comments: E+A Galaxy Fixed_Targets ! Section 5.1 Target_Number: 4 Target_Name: GAL-0158-4437 Alternate_Names: Description: GALAXY Position: RA = 01H 56M 00.12S +/- 0.1S,! Most common specification format is DEC = -44D 51' 49.0" +/- 1.0"! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: V=+35170 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=18.1+/-0.5 ! Include at least V and B-V Comments: E+A Galaxy Fixed_Targets ! Section 5.1 Target_Number: 5 Target_Name: GAL-1209-1222 Alternate_Names: Description: GALAXY Position: RA = 12H 06M 31.34S +/- 0.1S,! Most common specification format is DEC = -12D 05' 55.4" +/- 1.0"! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: B1950 RV_or_Z: V=+24310 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=16.4+/-0.5 ! Include at least V and B-V Comments: E+A Galaxy ! 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 ! DROP TO GYRO IF NECESSARY [NO REACQuisition] ORIENTation 0D TO 90D ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! SCHEDulability ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN