! $Id: 5387,v 5.1 1994/07/27 17:23:59 pepsa Exp $
coverpage:
title_1: CONSTRAINTS ON THE BOW SHOCK FROM A HIGH-VELOCITY
title_2: NEUTRON STAR
sci_cat: HOT STARS
sci_subcat: NEUTRON STARS
proposal_for: GO
pi_fname: JAMES
pi_mi: M.
pi_lname: CORDES
pi_inst: CORNELL UNIVERSITY
pi_country: USA
pi_phone: (607) 255-0608
hours_pri: 3.24
num_pri: 1
wf_pc: Y
off_fname: PETER
off_lname: CURTISS
off_title: GRANT&CONTRACT OFCR
off_inst: 1810
off_addr_1: SPONSORED PROGRAMS
off_addr_2: 123 DAY HALL
off_addr_3: CORNELL UNIVERSITY
off_city: ITHACA
off_state: NY
off_zip: 14853
off_country: USA
off_phone: (607) 255-5014
! end of coverpage
abstract:
line_1: Observations with the Wide Field Planetary Camera 2 in the
line_2: H-ALPHA line aim at probing the spatial structure near the
line_3: apex of a spectacular bow shock produced by a fast neutron star.
line_4: The nebula was discovered with the Palomar 5-meter telescope
line_5: and shows evidence for structure that is unresolved.
line_6: Theoretically, there should be structure
line_7: as fine as the resolution limit of the WFPC2 camera. Our goal
line_8: is to image details of the bow shock close to the contact
line_9: discontinuity so that we may solve for the three dimensional
line_10: orientation of the nebula and, hence, the actual direction of
line_11: motion of the pulsar. Through modeling of the geometry and
line_12: flux measurements, and including the outcome of further ground
line_13: based spectroscopy, and radio imaging, we can also put
line_14: strong constraints on the distance.
line_15: The net outcome should be a better understanding
line_16: of the structure of pulsar driven bow shocks, constraints
line_17: on density irregularities in the interstellar medium on length
line_18: scales less than 0.001 par sec, and constraints on the content
line_19: of relativistic pulsar winds.
!
! end of abstract
general_form_proposers:
lname: CORDES
fname: JAMES
mi: M
inst: 1810
country: USA
!
lname: LUNDGREN
fname: SCOTT
mi: C
inst: 1810
country: USA
!
lname: ROMANI
fname: ROGER
mi: W
inst: 3490
country: USA
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: We will obtain high-resolution images of the head of the
line_2: bow shock using the PC1 CCD of the WFPC2. A narrow
line_3: H-ALPHA filter will be sensitive to the limb-brightened
line_4: emission. A wider R-band filter will be used in a separate
line_5: exposure and with the same orientation of the camera
line_6: for the purpose of background subtraction. Placing the
line_7: head of the bow shock in PC1 requires that the spacecraft
line_8: be positioned so that the U3 axis is oriented at sky position
line_9: angle +45 degrees (i.e. toward the north east) in order
line_10: that the dimmer portions of the nebula (the guitar `body')
line_11: fall on CCDs WF2, WF3, and WF4. We have calculated that
line_12: a total of two hours be spent with the narrow H-ALPHA filter
line_13: (F656N) and 12 minutes with the R-band filter (F675W).
line_14: It is mandatory that the narrow and R-band images be
line_15: obtained with the same camera orientation on the sky.
!
question: 3
section: 2
line_1:
!
question: 4
section: 1
line_1: In July 1992, we made H$\alpha$ observations at the Palomar 5 meter
line_2: telescope of pulsar 2225+65 as part of a search for pulsar bow shocks.
line_3: This pulsar displayed a spectacular guitar shaped bow shock. In
line_4: addition to the image, we obtained a low resolution spectrum of the
line_5: apex of the shock. The spectrum demonstrated that the shock is
line_6: nonradiative, but could not resolve the details of the kinematics. We
line_7: plan to obtain higher resolution spectra this year (1993) to solve for the
line_8: kinematics. Our Very Large Array (VLA) images of the pulsar from 1985
line_9: and 1990 showed that it has a large proper motion, giving it a
line_10: velocity of 1000 km/s or more depending on the distance, making it the
line_11: fastest known star in the galaxy. To look for synchrotron emission
line_12: from particles accelerated by the shock, we have obtained VLA
line_13: data to form images at several frequencies (analysis in progress). We have
line_14: requested ROSAT time to look for X-ray emission from the hot shocked gas.
line_15: Only with the 0.1 arcsecond resolution available with WFPC2 on HST can we
line_16: hope to constrain structure of near the apex of the PSR2225+65 bow shock.
line_17: Such an observation will provide important information not available in
line_18: any of the other observations done or planned. The size of the shock
line_19: region is a crucial parameter in models of pulsar bow shock systems.
line_20: Extrapolating models of the PSR1957+20 shock, the PSR2225+65 shock is
line_21: expected to have a radius on the order of 100 AU at the tip. At its 1
line_22: kpc distance, that size makes the apex just resolvable with the
line_23: upgraded HST. Finding or limiting its size will be an important test of
!
question: 4
section: 2
line_1: current pulsar bow shock models. Even if we do not fully resolve the
line_2: most compact component of the apex, we expect to measure sufficient detail
line_3: in and near the apex that we will be able to tightly constrain the
line_4: orientation of the nebula's axis and solve for the nebula and pulsar
line_5: distance.
!
question: 5
section: 1
line_1:
!
question: 6
section: 1
line_1: Our second exposure uses the `R' filter F675W to obtain
line_2: a continuum image that may be subtracted from the
line_3: longer narrow H-ALPHA image. It is important that this
line_4: subtraction remove the two stars that appear in or
line_5: adjacent to the brighter portion of the bow-shock
line_6: nebula. We have designated this as a CALIB exposure
line_7: because the pointing is identical to that for the
line_8: H-ALPHA imaging.
!
!
question: 8
section: 1
line_1:
!
question: 9
section: 1
line_1: none
!
question: 10
section: 1
line_1: Cornell has a network of Sun workstations with IRAF and AIPS installed.
line_2: Images will be analyzed on the PI's Sparc-10 worktation
line_3: connected to the network. Stanford has comparable facilities for
line_4: data reduction. At both institutions we have colleagues who are
line_5: experts in astrophysical processes with whom we can confer.
line_6: We have ample work space and access to Internet for facilitating
line_7: the analysis of HST data, interpreting the results, and disseminating
line_8: the results through preprints and journal articles.
!
!end of general form text
general_form_address:
lname: Cordes
fname: James
mi: M
category: PI
inst: 1810
addr_1: 520 Space Sciences Bldg.
addr_2: Cornell University
city: Ithaca
state: NY
zip: 14853
country: USA
phone: (607) 255-0608
telex: cordes@astrosun.tn.cornell.edu
!
lname:
category: CON
!
! end of general_form_address records
fixed_targets:
targnum: 1
name_1: NEB-222552+653531
name_2: GUITAR-NEBULA
descr_1: A,160,905,922,929
pos_1: RA = 22H 25M 52.24S +/- 0.3S,
pos_2: DEC = +65D 35' 31.9" +/- 2"
equinox: 2000
pos_epoch_bj: J
comment_1: V IN FLUXVAL_1 IS FOR BRIGHTEST
comment_2: HST GUIDE STAR IN FIELD.
comment_3: FLUXNUM_2 VALUES ARE FOR DIFFUSE
comment_4: NEBULAR EMISSION THAT WE ARE
comment_5: TRYING TO MEASURE.
fluxnum_1: 1
fluxval_1: V=13.16 +/- 0.1
fluxnum_2: 2
fluxval_2: SURF-LINE(6563) = 1.1 +/- 0.3 E-17
fluxnum_3: 2
fluxval_3: W-LINE(6563) = 20 +/- 1
fluxnum_4: 2
fluxval_4: SIZE = 3.5 +/- 0.3
!
! end of fixed targets
! No solar system records found
! No generic target records found
exposure_logsheet:
linenum: 1.000
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F656N
num_exp: 1
time_per_exp: 1200S
s_to_n: 10
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
req_1: ORIENT 45D +/- 15D;
req_2: CYCLE 4 / 1.0-2.51
!
linenum: 1.010
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F656N
num_exp: 1
time_per_exp: 1200S
s_to_n: 10
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
req_1: SAME ORIENT FOR 1.01-2.51 AS 1.00
!
linenum: 1.020
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F656N
num_exp: 1
time_per_exp: 1200S
s_to_n: 10
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
!
linenum: 1.500
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F656N
num_exp: 1
time_per_exp: 1200S
s_to_n: 10
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
req_1: POS TARG -1.592,-1.592
!
linenum: 1.510
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F656N
num_exp: 1
time_per_exp: 1200S
s_to_n: 10
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
req_1: SAME POS FOR 1.51-1.52 AS 1.50
!
linenum: 1.520
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F656N
num_exp: 1
time_per_exp: 1200S
s_to_n: 10
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
!
linenum: 2.000
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F675W
num_exp: 1
time_per_exp: 180S
s_to_n: 20
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
!
linenum: 2.010
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F675W
num_exp: 1
time_per_exp: 180S
s_to_n: 20
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
!
linenum: 2.500
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F675W
num_exp: 1
time_per_exp: 180S
s_to_n: 20
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
req_1: POS TARG -1.592,-1.592
!
linenum: 2.510
targname: NEB-222552+653531
config: WFPC2
opmode: IMAGE
aperture: PC1
sp_element: F675W
num_exp: 1
time_per_exp: 180S
s_to_n: 20
fluxnum_1: 2
priority: 1
param_1: CR-SPLIT=NO
req_1: SAME POS FOR 2.51 AS 2.50
!
! end of exposure logsheet
! No scan data records found