! $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