! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 5975,v 5.1 1995/11/20 20:02:10 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 09:59:22 EST 1994 ! Proposal_Information ! Section 4 Title: HIGH SPATIAL RESOLUTION STUDIES OF Z>4 QUASARS Proposal_Category: GO Scientific_Category: Quasars Cycle: 5 Investigators PI_name: Richard McMahon PI_Institution: Institute of Astronomy CoI_Name: Esther Hu CoI_Institution: Institute for Astronomy, Hawaii Contact: ! Y or N (designate at most one contact) CoI_Name: Isobel Hook CoI_Institution: University of California, Berkeley Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) def\zsol z_\odot def\zsun z_\odot defL(sun) L_\odot defL(sun) L_\odot defM(sun) M_\odot defM(sun) M_\odot We propose to carry out high spatial resolution imaging of two carefully chosen quasars with redshifts greater than four. At these redshifts the angular scales are similar to those at z=0.3 (~10kpc per arcsec for H_0=50, q_0=0.5) and the host galaxies should be both resolvable and detectable in the I(F814W) band (rest frame ~1500ang). We shall be able to study the protogalactic material surrounding these quasars at a time when the Universe was less than a billion years old. This timescale is equivalent to the dynamical timescale for a typical 100kpc galactic halo (eg Rees 1988) and the observed surface brightness distribution, or limits thereon, will be an important constraint on both quasar formation and galaxy formation scenarios. Our targets are the recently discovered, z=4.30, radio loud quasar, GB1508+5714 and the z=4.69, radio quiet quasar BR1202-0725. The former quasar is the highest redshift radio source known and the host is likely to be the progenitor of a nearby giant Elliptical galaxy. The other quasar is radio quiet and moreover it has been detected in the 300--1200Mu m wavelength range (ie ~100--200Mu m in the rest frame) with JCMT and the IRAM 30m. The inferred FIR luminosity (sim10^14L(sun)) and dust mass estimates are similar to that obtained for the z=2.3 IRAS galaxy 10214+4724. The host of this quasar is highly likely to be a spiral galaxy or some sort of interacting system. Questions ! Free format text (please update) Observing_Description: We propose to carry out deep broad band continuum observations of two z>4 quasars. The F814W filter samples the continuum longward of the Lyman-Alpha forest in these objects. \medskip Feasibility \medskip In this program we need to consider saturation effects due to the quasar nucleus and surface brightness limits. The quasar BR1202-0725 has an observed continuum flux at 1500ang in the quasar rest frame of 1.8* 10^-27 \ergpcmpHz (ie 18mJy or AB=18.2), whereas GB1505+5714 is 1mag fainter. The expected total count rate through the WFPC2 with I filter (F814W) is: \medskip 2.5* 10^11 * 0.020 * 10^-0.4(18.2) = 283 electrons/sec \medskip Therefore, based on the figures in Table 5.1 of the WFPC handbook, if the quasar is centred on a pixel 63\ the central pixel. This drops to 20\ centred on the corner of a pixel. The ADCs saturate at 30,000electrons for gain 7 and blooming occurs at >100,000 electrons. Although saturation can be avoided by using exposures of less than 100secs, the read out noise would then dominate our observations. We propose to use exposures of 1000secs which will be sky noise limited ( cf Windhorst, Mathis & Keel, 1992) at the expense of saturating in the quasar core. \medskip Beyond a radius of 0.2arc secs the quasar contributes less than 1\ be <23.2 and 24.2 for the two quasars respectively. This is comparable with sky brightness at 8000Angstrom. \medskip A source with AB_8000=24.3 will produce a count rate of 1 ct/sec. The skybrightness at 8000Angstrom\ is 22.7 ie 4.4 ct/sec/arcsec. In 1000 seconds the targets will produce 10 counts per pixel and the sky 44 counts/pixel (ie comparable with read noise per pixel). Therefore one gets a 1 sigma detection of a point source in 1000secs. Therefore in 16 such exposures one would obtain a 4 sigma detection for a point source. This corresponds to the bf Normal galaxy formation scenario described in the scientific case. A positive detection at a level greater than this would have great significance. \medskip Total time requested We wish to obtain a total of 16,000 seconds on each quasar. This would be attained in 6 orbits for B1202-0725 and 5 orbits for GB1508+5714(near CVZ). The exposures will be split up into ~1000 second segments to facilitate Cosmic Ray removal. The quasars will be located in different places on the CCD for each orbit so that flat fielding will be improved. Real_Time_Justification: none To complement our HST program we have already obtained deep narrow band Lyman-Alpha observations and broad band B, R and K observations with the University of Hawaii 88inch telescope. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: BR1202-0725 Alternate_Names: Description: GALAXY, QSO Position:RA=12H 02M 49.19S +/- 0.1S, DEC=-07D 25'50.4" +/- 1" Equinox:1950 RV_or_Z: ! RA_PM: ! Units are seconds of time per year ! Dec_PM: ! Units are seconds of arc per year ! Epoch:1950 !Annual_Parallax: Flux: V=19 ! Include at least V and B-V Comments: Fixed_Targets ! Section 5.1 Target_Number: 2 Target_Name: GB1508+5714 Alternate_Names: Description: GALAXY, QUASAR Position:RA=15H 08M 45.20S +/- 0.1S, DEC=+57D 14' 02.6" +/- 1" Equinox:1950 RV_or_Z: ! RA_PM: ! Units are seconds of time per year ! Dec_PM: ! Units are seconds of arc per year ! Epoch:1950 !Annual_Parallax: Flux: V=19 ! Include at least V and B-V 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 TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN