!__Proposal-Section__ !6126 ! Hubble Space Telescope Cycle 5 (1995) Phase II Proposal Template ! $Id: 6126,v 3.1 1995/04/11 14:38:28 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: Christian Ready ! Phone: 410 338-4546 , E-mail: ready@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Date generated: Mon Dec 19 08:29:30 EST 1994 ! Proposal_Information ! Section 4 Title: Evolution of Binary Neutron Stars and Their White Dwarf Companions Proposal_Category: GO Scientific_Category: Hot Stars Cycle: 5 Investigators PI_name: Dr. Roger Foster PI_Institution: Naval Research Laboratory CoI_Name: Dr. Scott Lundgren CoI_Institution: Naval Research Laboratory Contact: Y ! Y or N (designate at most one contact) CoI_Name: Fernando Camilo CoI_Institution: Princeton University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) Understanding the age and evolutionary history of millisecond pulsars can be greatly enhanced by careful multi-color photometry of the white dwarf companions to binary millisecond pulsars. Twenty two millisecond pulsars have been identified with low-mass companions, the majority being 0.1 to 0.6 Msun white dwarfs. We have selected the six most promising pulsar-white dwarf systems for study with HST. Photometry in B, V, and I filters will be used to determine the cooling age of the dwarf star independent of evolutionary arguments made from timing measurements of the pulsar. In several cases the estimated companion mass, determined from the luminosity, will place significant upper bounds on the neutron star mass, potentially revealing clues about both the supernova explosion which created the neutron star, and the later accretion which spun it up to millisecond periods. Astrometric observations of the white dwarfs will serve as a first epoch of proper motion measurements important for distinguishing between supernova and accretion induced collapse models for millisecond pulsar formation. Finally, the astrometry will enable us to measure the rotation of the optical reference frame relative to the radio and dynamical reference frames made from independent pulsar observations. Questions ! Free format text (please update) Observing_Description: We propose to image 2 pulsar companions in 3 colors and 4 companions in 2 colors each. In order to accurately fit for reddening and temperature, we require signal to noise ratios on the order of 20. From Palomar observations currently being reduced, PSR J1713+0747 and PSR J2145-0750 are barely detected at m_v~ 24.5-25. From their comparable ages and estimated white dwarf masses, the other pulsars are expected to have comparable luminosities. Hence, they could be up to 1 magnitude fainter due to larger distance, smaller size, or higher age. To reach the desired signal, we require 1 orbit for 2 colors or 2 orbits for 3 colors per object. Due to reddening, low white dwarf temperature, and lower telescope sensitivity, the B filter requires the longest integration. We propose two 7.5 minute exposures each for the V and I filters in the first orbit and two 20 minute exposures with the B filter in the second orbit. These exposures give 400-600 counts for a signal to noise ratio of 15-20 integrated over the point spread function (combined sky background (4), dark current (2), and read noise (25) counts amount to about 280 over the point spread function). The limiting magnitude would be 27 for each filter, significantly fainter than expected for any of the objects. For the objects in this project, the fraction of neutron star spin-down energy impinging on the companion is not sufficient to cause substantial heating. Hence, none of the recently discovered systems are expected to show orbital variability of the companion luminosity. The PSR 1957+20 system, which does show optical variability over the orbit (Fruchter et al 1988) has more spin-down energy and a smaller orbit than the recently discovered systems. Even if the energy was sufficient in the new systems, the chance is small that the spin and orbital axes are oriented favorably, such that the pulsar beam intercepts the companion. Consequently, we can safely make each observations for each filter at different orbital phase values. Real_Time_Justification: None. Radio timing observations are ongoing and will continue for all of these objects. J0034-0534 and J2145-0750 are monitored by Bailes at Parkes observatory. J1023+1004, J2019+2425, and J2229+2643 are observed at Arecibo observatory by Camilo. Foster observes J1640+2224 and J1713+0747 at Arecibo and Wolszczan monitors them at Bonn. Typically each source is observed monthly to monitor fluctuations from the fitted timing and orbital model. With a long enough time baseline these observations will be used to fit for positions and proper motions, to compare with the optical results. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number:1 Target_Name:STAR-2145-0750 Alternate_Names:PSRJ2145-0750 Description:STAR, BINARY PULSAR Position:RA=21H 45M 50.440S +/- 0.005S, DEC=-7D 50' 17.9" +/- 0.2" ! Most common specification format ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 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. +/- 1. ! Include at least V and B-V Comments: Target_Number:2 Target_Name:STAR-0034-0534 Alternate_Names:PSRJ0034-0534 Description:STAR, BINARY PULSAR Position:RA=00H 34M 21.826S +/- 0.002S, DEC=-05D 34' 36.56" +/- 0.03" !Most common specification format ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 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. +/- 1. ! Include at least V and B-V Comments: Target_Number:3 Target_Name:STAR-1022+1001 Alternate_Names:STAR-1023+1004, PSRJ1022+1001 Description:STAR, BINARY PULSAR Position:RA=10H 22M 58.095S +/- 0.15S, DEC=+10D 01' 55.8" +/- 5" ! Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 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=24.5 +/- 1. ! Include at least V and B-V Comments: The new name reflects improvements in the position from radio timing of the pulsar. An improved position with accuracy better than 1 arcsecond will be provided by April 1995. Target_Number:4 Target_Name:STAR-1640+2224 Alternate_Names:PSRJ1640+2224 Description:STAR, BINARY PULSAR Position:RA=16H 40M 16.742S +/- 0.001S, DEC=+22D 24' 09.015" +/- 0.003" !Most common specification format is ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 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=26. +/- 1. ! Include at least V and B-V Comments: Target_Number:5 Target_Name:STAR-1713+0747 Alternate_Names:PSRJ1713+0747 Description:STAR, BINARY PULSAR Position:RA=17H 13M 49.527S +/- 0.001S, DEC=+07D 47' 37.556" +/- 0.001" ! common specification format ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 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. +/- 1. ! Include at least V and B-V Comments: Target_Number:6 Target_Name:STAR-2019+2425 Alternate_Names:PSRJ2019+2425 Description:STAR, BINARY PULSAR Position:RA=20H 19M 31.951S +/- 0.001S, DEC=+24D 25' 15.366" +/- 0.01" ! common specification format ! RA=0H 0M 0.00S +/- 0S, ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 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. +/- 1. ! 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