! Proposal 6527, submission 1 ! PI: Roberto P. Mignani ! Received Wed Feb 14 12:34:20 EST 1996 ! From: mignani@helios.ifctr.mi.cnr.it ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6527,v 4.1 1996/03/27 18:51:49 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6527,v 4.1 1996/03/27 18:51:49 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: 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-0368.mignani.prop ! Date generated: Fri Dec 22 17:38:25 EST 1995 ! Proposal_Information ! Section 4 Title: Search for the Optical Counterpart of PSR1055-52. Proposal_Category: GO Scientific_Category: HOT STARS Cycle: 6 Investigators PI_name: Roberto P. Mignani PI_Institution: Istituto di Fisica Cosmica del CNR CoI_Name: Giovanni F. Bignami CoI_Institution: Istituto di Fisica Cosmica del CNR Contact: ! Y or N (designate at most one contact) CoI_Name: Patrizia A. Caraveo CoI_Institution: Istituto di Fisica Cosmica del CNR Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) PSR1055-52 is an Isolated Neutron Star (INS) observed through its pulsed emission from radio to Gamma rays. The region around PSR1055-52 was observed with ESO telescopes, but no optical counterpart was found, probably because the radio position falls close (~ 4sec point) to a bright (m_V =14.6) field star. We now plan to get new deep higher resolution images of the region with the HST/FOC in order to detect any emission from the pulsar, exploiting both the seeing-free HST optics and the UV sensitivity of the FOC. Detectability is supported by the case of two similar INSs, Geminga and PSR0656+14, both successfully seen with the HST/FOC. Questions ! Free format text (please update) Observing_Description: We plan to perform deep high resolution imaging around the radio position of PSR1055-52 in order to detect its UV emission with the FOC. To estimate the exposure times we used FOCSIM and, as a reference, our FOC observation of Geminga, gathered during Cycle 4. According to FOCSIM, exposure times of 4500 and 6500 sec in the F342W and F275W filters, respectively, should be adequate to detect the target with a S/N 30. Therefore, we ask for two exposures: one of 4500 sec. (F342W filter) and the other of 6500 sec (F275W filter). These exposures, split in shorter chunks to minimize cosmic rays contamination, will be fitted in 5 orbits. Real_Time_Justification: Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number:01 Target_Name:STAR-1057-5226 Alternate_Names:PSR1055-52 Description: STAR,NEUTRON STAR Position: ! Most common specification format is RA=10H 57M 58.84S +/- 0.29S, ! RA=0H 0M 0.00S +/- 0S, DEC=-52D 26' 56.28" +/- 0.29", ! DEC=0D 0' 0.0" +/- 0", PLATE-ID=03C2 Equinox:J2000 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=25 ! 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:01 Visit_Requirements: ! Section 7.1 ! Uncomment or copy visit level special requirements needed ! Most of these requirements (including ORIENT) will limit scheduling PCS MODE F ! 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