! Proposal 6600, submission 1 ! PI: Dr. Elizabeth M. Puchnarewicz ! Received Thu Feb 8 17:14:48 EST 1996 ! From: kom@msslac.mssl.ucl.ac.uk ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6600,v 3.1 1996/02/12 15:29:12 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6600,v 3.1 1996/02/12 15:29:12 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: Bremmer ! Phone: 410-338-4458 , E-mail: bremmer@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0538.puchnarewicz.pro ! Date generated: Fri Dec 22 15:38:32 EST 1995 ! Proposal_Information ! Section 4 Title: Investigating high-temperature big bumps in AGN Proposal_Category: GO Scientific_Category: AGN Cycle: 6 Investigators PI_name: Dr. Elizabeth M. Puchnarewicz PI_Institution: Mullard Space Science Laboratory CoI_Name: Dr. Aneta Siemiginowska CoI_Institution: Harvard-Smithsonian Center for Astrophysics Contact: ! Y or N (designate at most one contact) CoI_Name: Professor Keith O. Mason CoI_Institution: Mullard Space Science Laboratory Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose HST-FOS observations of an AGN which has one of the hottest optical to soft X-ray `big bumps' identified to date. QSO1034+3938 is a narrow-line Seyfert 1 galaxy (z=0.042) which shows no trace of the big blue bump in the optical and a high energy turnover of the big bump in soft X-rays; these properties are both highly unusual. The existence of such high-temperature components stretches models of the optical to X-ray big bump to unprecedented limits. HST-FOS spectra of this AGN will provide key observational tests for these models as well as diagnostics of the effect of the big bump on UV line emission in the high- temperature extreme. We plan to investigate the UV spectrum of QSO1034+3938 and: (1) characterize the continuum shape; (2) measure UV line FWHM and fluxes; and (3) search for the low energy tail of the big bump and investigate a possible optical/UV power-law component in QSO1034+3938. Questions ! Free format text (please update) Observing_Description: We request an observation with the G130H+Blue Digicon to extend as far into the UV as possible to search for the big bump, and to measure Lyalpha (which will be shifted sufficiently from the geocoronal Lyalpha line). In addition, we wish to measure CIV1549 with the G190H+Blue Digicon (CIII]1909 also falls within this range) and MgII2798 with the G270H+Blue Digicon. Since the Hbeta FWHM is quite narrow (~1500 km s-1), and since this may be a physical consequence of the unusual continuum spectrum, we anticipate that the UV line FWHM may also be small. The ability to resolve the FWHM of Lyalpha and CIV is essential if we are to establish whether the high-ionization UV lines follow the same trend as the low-ionization Balmer lines, thus we require the high resolution gratings. We also require a PRISM+Blue Digicon exposure to make any renormalizations due to variability. Requested exposure times are also given in Table 1 for a S/N=10 per diode in the continuum (assuming that there is no big bump emission, in which case it would be higher), and at least this in Lyalpha, CIV and CIII]. These times have been calculated using the inverse sensitivities and other information in Version 6.0 of the FOS Instrument Handbook. Count rates were calculated assuming mV=15.6 and alpha=1.4. These observations will require 4HST orbits (one primarily for target acquisition and three for obtaining science data). The amount of absorption along the line of sight to QSO1034+3938 is small both within our Galaxy and locally to the AGN (NH=1.2e20 cm-2), therefore we expect any reddening in the spectra to be minimal. Although the galaxy component in QSO1034+3938 (z=0.04) is strong, its contribution will be negligible in the short wavelength regions we propose, therefore the 1.0 arcsecond circular aperture is appropriate in this case. We request the ACQ/PEAK mode for target acquisition with a pointing accuracy >0.1 arcsec. Although QSO1034+3938 lies at low redshift (z=0.04), the host galaxy emission is negligible in the 2000-5000A region and will be dominated by the unresolved nuclear source. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: ZW212.025 Alternate_Names: REJ1034+396 Description: GALAXY,SEYFERT,ACCRETION DISK,BLR Position: RA=10H 34M 38.63S +/-0.1S, ! Most common specification format is DEC=39D 38' 28.36" +/-0.1", ! RA=0H 0M 0.00S +/- 0S, PLATE-ID=000B ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: J2000 RV_or_Z: Z=0.042 RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=15.6+/-0.5 ! Include at least V and B-V B-V=0.6+/-0.3 F-CONT(1300)=2+/-1E-15 F-CONT(1600)=2+/-1E-15 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 ! 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