! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6677,v 7.1 1996/10/18 15:02:53 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6677,v 7.1 1996/10/18 15:02:53 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-0738.mchardy.prop ! Date generated: Fri Dec 22 17:41:58 EST 1995 ! Proposal_Information ! Section 4 Title: The Origin of the X-Ray Background: What are the faintest X-Ray Galaxies? Proposal_Category: GO Scientific_Category: GALAXIES & CLUSTERS Cycle: 6 Investigators PI_name: Ian McHardy PI_Institution: Physics Department, University of Southampton CoI_Name: Andrew Newsam CoI_Institution: Physics Department, University of Southampton Contact: ! Y or N (designate at most one contact) CoI_Name: Roberto Abraham CoI_Institution: Institute of Astronomy, Cambridge Contact: ! Y or N (designate at most one contact) CoI_Name: Laurence Jones CoI_Institution: Goddard Space Flight Center Contact: ! Y or N (designate at most one contact) CoI_Name: Michael Merrifield CoI_Institution: Physics Department, University of Southampton Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) To determine the origin of the X-ray background (XRB) we have made the deepest optically identified (ROSAT) X-ray survey yet. At `bright' flux levels (ie 1 x 10**-14 ergs/cm/s) QSOs dominate the survey but below 5 x 10**-15 ergs/cm/s our sample is dominated by a population of narrow emission line galaxies (NELGs), at typical redshifts of 0.2-0.5. The NELG source counts rise rapidly at faint X-ray fluxes making them a major contributor to the XRB. The X-ray spectra of the NELGs are hard, as is required for any major contributor to the XRB. Deep sub-arcsecond CFHT images indicate that the brightest (m_R < 18.5) systems are mainly interacting galaxies, probably spirals. Here we request WFC R-band images to determine the morphologies of the remaining systems which we cannot study from the ground to determine whether the remaining non-QSO XRB might be explained by emission from interacting or disturbed spirals. Disturbed systems are thought to be responsible for the faint blue galaxy population, IRAS starburst galaxies and the sub-mJy radio sources so our observations may have implications for the unification of all these populations, including X-ray NELGs. Questions ! Free format text (please update) Observing_Description: THE SAMPLE The sample is statistically complete and well defined. The full sample consists of all 19 NELGs in our spectroscopically complete ROSAT deep survey. We remove from this list the 3 brightest NELGs (m_r < 18) which are reasonably studied from the ground. In order to keep the total HST observation time down we also remove the two faintest (m_r = 22.3 and 22.7) and most distant (both Z=0.58) objects from the sample leaving 13 NELGs in the magnitude range m_r 18.8 to 21.2. With one exception, all the remaining 13 have Z>0.2 Note that two NELGs lie within 1 arcmin and so can be observed simultaneously (so we list only 12 targets). Of these, in order to remain within the allocated time, we select the 10 with the brightest X-ray fluxes to give a statistically useful, flux-limited subset. FEASIBILITY AND OBSERVATION TIMES In the present proposal we choose the 814W filter to image all of our sample. As the mean redshift of our NELGs is 0.3, this gives us a rest-frame red image which will provide a good determination of the overall galaxy structure. One of us (Abraham) is heavily involved in the analysis of HST Medium Deep Survey images. Our experience there is that it is necessary to reach a surface brightness limit of approximately 24 mags/arcsec**2 in order to detect tidal debris and evidence of interactions. Our experience with MDS images also reveals that one needs to reach about that same surface brightness limit in order to reliably distinguish ellipticals from spirals on the basis of surface brightness profiles. Thus we take approximately 24 mags/arcsec**2 as our target surface brightness limit. Using the WWW exposure calculator we determine that, in order to reach approx. 24 mags/arcsec**2 per pixel (assuming Sbc spectra) in the WFC at a signal to noise of 2, we require total integration times in the 814W filter of 3500s. A S/N of 2 is low, but in the lower surface brightness regions we will probably average over a few pixels in order to determine the large scale structure of the galaxies. We note that 3500s is about 1.5 orbits. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 ! Obj. 36 Target_Name: GAL-133525+380536 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 35M 25.20S +/- 0.01S, ! Most common specification format is DEC=38D 05' 36.4" +/- 0.1" Equinox: 2000 RV_or_Z: Z=0.235 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=18.7+/-0.2, V-R=1.0+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 36. Target_Number: 2 ! Obj. 42 and 47 Target_Name: GAL-133502+375011 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 35M 04.35S +/- 0.02S, ! Most common specification format is DEC=37D 50' 02.1" +/- 0.2" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.368 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=19.7+/-0.2, V-R=0.8+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 42. Position is an offset so that Obj 47 is also included (ie at mid-point). Target_Number: 3 ! Obj. 43 Target_Name: GAL-133329+375558 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 33M 29.02S +/- 0.01S, ! Most common specification format is DEC=37D 55' 57.8" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.385 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=21.5+/-0.2, V-R=1.3+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 43. Target_Number: 4 ! Obj. 67 Target_Name: GAL-133500+375633 Alternate_Names: Description: GALAXY,Seyfert,Starburst,High z Gal Position: RA=13H 35M 00.20S +/- 0.01S, ! Most common specification format is DEC=37D 56' 33.2" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.558 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=20.7+/-0.2, V-R=0.9+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 67. Target_Number: 5 ! Obj. 85 Target_Name: GAL-133409+375444 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 34M 08.82S +/- 0.01S, ! Most common specification format is DEC=37D 54' 43.5" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.304 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=21.5+/-0.2, V-R=0.8+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 85. Target_Number: 6 ! Obj. 93 Target_Name: GAL-133354+380156 Alternate_Names: Description: GALAXY,Seyfert,Starburst,High z Gal Position: RA=13H 33M 53.80S +/- 0.01S, ! Most common specification format is DEC=38D 01' 56.0" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.590 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=21.8+/-0.2, V-R=0.6+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 93. Target_Number: 7 ! Obj. 94 Target_Name: GAL-133346+380025 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 33M 46.07S +/- 0.01S, ! Most common specification format is DEC=38D 00' 25.3" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.061 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=19.0+/-0.2, V-R=0.1+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 94. Target_Number: 8 ! Obj. 103 Target_Name: GAL-133331+374810 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 33M 31.07S +/- 0.01S, ! Most common specification format is DEC=37D 48' 09.8" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.200 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=19.8+/-0.2, V-R=0.5+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 103. Target_Number: 9 ! Obj. 121 Target_Name: GAL-133519+375532 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 35M 18.67S +/- 0.01S, ! Most common specification format is DEC=37D 55' 31.6" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.310 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=19.5+/-0.2, V-R=0.2+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 121. Target_Number: 10 ! Obj. 127 Target_Name: GAL-133458+374934 Alternate_Names: Description: GALAXY,Seyfert,Starburst Position: RA=13H 34M 57.67S +/- 0.01S, ! Most common specification format is DEC=37D 49' 34.2" +/- 0.1" ! RA=0H 0M 0.00S +/- 0S, ! No DSS Coords... ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Z=0.250 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=20.7+/-0.2, V-R=0.6+/-0.2 ! Include at least V and B-V Comments: Rosat UK Deep Field object 127. !Solar_System_Targets ! Section 5.2 ! Target_Number: ! Target_Name: ! Description: ! Level_1: ! Satellite of Sun ! Level_2: ! Satellite of Level_1 ! Level_3: ! Satellite of Level_2 ! Ephem_Uncert: ! Needed for REQ EPHEM CORR sp req ! Acq_Uncert: ! Needed for SAVE and USE OFFSET sp reqs ! Window: ! Flux: ! Include at least V and B-V ! Comments: !Generic_Targets ! Section 5.3 ! Target_Number: ! Target_Name: ! Description: ! Criteria: ! Flux: ! Comments: Scan_Data ! Appendix B ! Scan_Number: ! FGS_Scan: ! Cont_or_Dwell: ! Dwell_Points: ! Dwell_Secs: ! Scan_Width: ! Scan_Length: ! Sides_Angle: ! Number_Lines: ! Scan_Rate: ! First_Line_PA: ! Scan_Frame: ! Length_Offset: ! Width_Offset: ! 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 TO ! ORIENTation TO FROM ! ORIENTation TO FROM NOMINAL ! SAME ORIENTation AS ! CVZ ! PARallel ! SCHEDulability ! AFTER [BY [TO ]] ! AFTER ! BEFORE ! BETWEEN AND ! GROUP WITHIN