! Proposal 6827, submission 1 ! PI: S. R. Kulkarni ! Received Fri Feb 9 14:26:00 EST 1996 ! From: mhvk@astro.caltech.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6827,v 4.1 1997/05/20 17:30:49 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6827,v 4.1 1997/05/20 17:30:49 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: van Orsow ! Phone: 410-338-4568 , E-mail: vanorsow@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-1136.kulkarni.prop ! Date generated: Fri Dec 22 19:05:43 EST 1995 ! Proposal_Information ! Section 4 Title: THE ENIGMATIC SOFT GAMMA-RAY REPEATERS Proposal_Category: GO Scientific_Category: INTERSTELLAR MEDIUM Cycle: 6 Investigators PI_name: S. R. Kulkarni PI_Institution: California Institute of Technology CoI_Name: M. H. van Kerkwijk CoI_Institution: California Institute of Technology Contact: ! Y or N (designate at most one contact) CoI_Name: R. Danner CoI_Institution: Max-Planck Institut fuer Extraterrestrische Physik Contact: ! Y or N (designate at most one contact) CoI_Name: T. Murakami CoI_Institution: Institute for Space Astronautics and Sciences Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We prospose to try to identify an optical/UV counterpart of the Soft Gamma-ray Repeater (SGR) 0525-66, the most enigmatic of a class of sources, which, for reasons unknown, repeatedly show high-energy bursts. One SGR, 1806-20, has been identified with a plerionic supernova remnant, with a persistent X-ray source as well as a very luminous star coincident with the peak. For SGR 0525-60, the 5-March-1979 burst, the brightest burst ever observed, has led to a localisation to the northern part of the supernova remnant N49 in the LMC. Neither plerionic radio emission, nor a bright companion have been found, but there is a persistent X-ray source inside the error box. It is very unlikely find such a bright source in the 0.09 square arcmin error box by chance, but even so we recently found evidence for another, variable source right next to the persistent one. From SGR 1806-20, we infer that SGR events are associated not only with bursts of photons but also with strong burst of particles. For any reasonable ratio of the energy in particles to that in gamma- rays, the March 1979 event of SGR 0525-66 alone would suffice to power a small plerionic nebula. This nebula can account for the presistent X-ray source, and should also be detectable in the optical/UV. However, HST is needed to resolve it from the underlying emission of N49. With HST, we might even find that the plerion has the shape of a bow shock, due to the high transversal speed of the underlying power source. Questions ! Free format text (please update) Observing_Description: We intend to observe the error box of the ROSAT X-ray sources with the Planetary Camera of WFPC2. We chose the F547M filter to have as little overlap as possible with the emission lines from N49 (see the spectra by Vancura et al.\ (1992). Based on the analysis of the WFPC1 image in the F517N, we expect that in 180 minutes in F547M (two orbits in CVZ), we will be able to go down a factor sqrt6*12 deeper because of the wider filter and longer integration time (notice that the observations will be background limited, due to the signal from the supernova remnant). This means we can go down to 0.5 MuJy. For the blue region, it is not possible to chose a filter that is as free from lines. To compensate for that and for the lower sensitivity, we need to integrate about three times longer. The observations will all be slit in 1000 s exposures. These will be taken at slightly different positions, so that following the prescription of Freudling (1995; see also ST-ECF News Letter 22), we will be able to partly recover the resolution lost by undersampling, as well as get rid of cosmic ray hits. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: N49-052601-660435 Alternate_Names: SGR0525-66 Description: UNIDENTIFIED, GAMMA RAY EMITTER Position: RA=05H 26M 00.7S +/- 1.0S, DEC=-66D 04' 35" +/- 10" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: RA_PM: ! Units are seconds of time per year Dec_PM: ! Units are seconds of arc per year Epoch: Annual_Parallax: Flux: V=24, B-V=0 ! Include at least V and B-V Comments: We are trying to find the SGR companion and do not know its flux in advance. We have put a best guess. ! 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: CVZ ORIENTATION 295D TO 310D BETWEEN 1-SEP-1997 AND 1-OCT-1997 ! 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