! File: 2237C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:03:49:12 coverpage: title_1: OBSERVATIONS OF THE ECLIPSING MILLISECOND PULSAR sci_cat: STELLAR ASTROPHYSICS proposal_for: GO pi_title: DR. pi_fname: JAY pi_lname: BOOKBINDER pi_inst: CFA pi_country: USA pi_phone: (617) 495-7058 keywords_1: PULSARS, PULSARS: BINARY, PULSARS: MILLISECOND keywords_2: BINARIES: LOW MASS X-RAY, NEUTRON STARS. hours_pri: 7.42 num_pri: 1 wf_pc: X fos: X time_crit: X funds_amount: 48706 funds_length: 12 funds_date: JAN-91 pi_position: ASTROPHYSICIST off_fname: GEORGE off_mi: D. off_lname: DICK off_title: MANAGER off_inst: SMITHSONIAN off_addr_1: 60 GARDEN STREET off_city: CAMBRIDGE off_state: MA off_zip: 02138 off_country: USA off_phone: (617) 495-7401 off_telex: 921428 SATELLITE CAM ! end of coverpage abstract: line_1: FRUCHTER et al. (1988a) HAVE RECENTLY DISCOVERED a 1.6 MSEC PULSAR (PSR line_2: 1957+20) IN A 9.2 HOUR ECLIPSING BINARY SYSTEM. THE UNUSUAL BEHAVIOR OF THE line_3: DISPERSION MEASURE AS A FUNCTION OF ORBITAL PHASE, AND THE DISAPPEARANCE OF THE line_4: PULSAR SIGNAL FOR 50 MINUTES DURING EACH ORBIT, IMPLIES THAT THE ECLIPSES ARE line_5: DUE TO A PULSAR-INDUCED WIND FLOWING OFF OF THE COMPANION. THE OPTICAL line_6: COUNTERPART IS A 21ST MAGNITUDE OBJECT WHICH VARIES IN INTENSITY OVER THE line_7: BINARY PERIOD; ACCURATE GROUND-BASED OBSERVATIONS ARE PREVENTED BY THE line_8: PROXIMITY (0.7") OF A 20TH MAGNITUDE K DWARF. WE PROPOSE TO OBSERVE THE line_9: OPTICAL COUNTERPART IN A TWO-PART STUDY. FIRST, THE WF/PC WILL PROVIDE line_10: ACCURATE MULTICOLOR PHOTOMETRY, ENABLING US TO DETERMINE UNCONTAMINATED line_11: MAGNITUDES AND COLORS BOTH AT MAXIMUM (ANTI-ECLIPSE) AS WELL AS AT MINIMUM line_12: (ECLIPSE). SECOND, WE PROPOSE TO OBSERVE THE EXPECTED UV LINE EMISSION WITH line_13: FOS, ALLOWING FOR AN INTIAL DETERMINATION OF THE TEMPERATURE AND DENSITY line_14: STRUCTURE AND ABUNDANCES OF THE WIND THAT IS BEING ABLATED FROM THE COMPANION. line_15: STUDY OF THIS UNIQUE SYSTEM HOLDS ENORMOUS POTENTIAL FOR THE UNDERSTANDING OF line_16: THE RADIATION FIELD OF A MILLISECOND PULSAR AND THE EVOLUTION OF LMXRBs AND line_17: MSPs IN GENERAL. WE EXPECT THESE OBSERVATIONS TO PLACE VERY SIGNIFICANT line_18: CONTRAINTS ON MODELS OF THIS UNIQUE OBJECT. ! ! end of abstract general_form_proposers: lname: TAYLOR fname: JOSEPH title: PROF. inst: PRINCETON UNIVERSITY country: USA ! lname: JUDGE fname: PHILLIP title: PROF. mi: D. inst: COLORADO, UNIVERSITY OF country: USA ! lname: BOOKBINDER fname: JAY title: P.I. inst: CFA country: USA ! lname: BAILYN fname: CHARLES inst: CFA country: USA ! lname: FRUCHTER fname: ANDREW title: PROF. inst: DEPARTMENT OF TERRESTRIAL MAGNETISM, CARNEGIE INST. country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We are proposing two sets of science observations using the PC and FOS. line_2: Our science observations with the PC will be performed to obtain line_3: wide-band colors of the companion. RI colors will be obtained using the line_4: PC mode and the ``standard'' R, and I filters F675W, F791W. These line_5: observations consisting of the ``R'' and ``I'' bands will be obtained at line_6: eclipse (optical minimum). The goal of the PC observations is to line_7: acquire accurate color temperatures of the pulsar's optical companion. line_8: The magnitude and color of the companion line_9: at minimum can be used to constrain the geometry of the orbit, under the line_10: assumption that there is a lit and unlit face of the secondary. The line_11: observations at minimum may also allow us to deduce information about line_12: the intrinsic luminosity and nature of the secondary. ! question: 3 section: 2 line_1: Second, we propose to obtain a deep, low resolution FOS UV spectrum to line_2: obtain the overall flux levels in the UV regime, and to identify line_3: lines of C, O, S, Si, N, or He. To obtain this spectrum, line_4: we will use the low resolution G160L grating (6.5 A/diode over 1150 A -- line_5: 2523 A) and the blue digicon camera on the FOS. This configuration will line_6: provide high sensitivity with sufficient spectral resolution for this line_7: experiment. This region of the UV spectrum covers the transition line_8: region temperature lines of N V, C IV, Si IV, O IV], He II. The range of line_9: temperatures sampled is from 7000 to 2 x 10(5). Additionally, several line_10: lines that sample plasma at coronal temperatures may be present (e.g., line_11: Fe XXI 1354 A (at 10(7)K), Fe XII 1349 A (at 1.6 x 10(6)), OV 1371 A line_12: (about 2 x 10(5) K). Standard mode on the FOS will allow us to obtain line_13: a spectrum every four minutes. While we are unlikely to detect line_14: the pulsar in individual scans, it is possible that variability line_15: is present that we would be sensitive to. ! question: 6 section: 1 line_1: At maximum, the pulsar has a V magnitude of 20.3 (Fruchter et al 1988b), line_2: although confusion from the neighboring G star (0.7" away) makes this line_3: somewhat uncertain. Estimated exposure times are based on the WF/PC line_4: Instrument description, using conservative assumptions regarding line_5: both magnitude and flux distribution of the pulsar's optical companion. line_6: The requested PC observations at system maximum - 600 seconds with the line_7: F569W filter (approx. V-band) - will yield a line_8: magnitude error less than 5 percent. Since the magnitude and colors are line_9: totally unknown at optical minimum, we will apportion 1000 seconds to line_10: each of three I exposures and one R exposures. This will result in at line_11: least 5 sigma sensitivity down to 24 magnitude in I. ! question: 6 section: 2 line_1: Good astrometry of the field will be required to distinguish between the line_2: pulsar's optical counterpart and its near neighbor for the purpose of line_3: the FOS observation. This will be accomplished by scheduling the line_4: pulsar system maximum PC observations well before the line_5: FOS observation. line_6: Although our observations must be performed at specific orbital phases, line_7: there is a great deal of flexibility in scheduling the primary science line_8: observations, since the orbital period is 9.2 hours, and we are line_9: insensitive to which orbit(s) are selected for observation. However, we line_10: must obtain PC observations both at system maximum and minimum, and line_11: FOS observations at system maximum. An accurate ephemeris is available line_12: for detailed scheduling information. ! !end of general form text general_form_address: lname: BOOKBINDER fname: JAY title: DR. category: PI inst: SMITHSONIAN ASTROPHYS. OBS. addr_1: 60 GARDEN STREET city: CAMBRIDGE state: MA zip: 02138 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PSR1957+20 name_2: ECLIPSING-MILLISECOND-PULSAR descr_1: PULSAR, NEUTRON STAR, ECLIPSING BINARY descr_2: INTERACTING BINARY pos_1: RA = 19H 59M 36.77S +/-0.1S, pos_2: DEC = +20D 48' 15.16" +/-1.0" equinox: 2000 pos_epoch_yr: 1988.00 acqpr_1: COMP comment_1: B, V, R, B-V ARE AT MAX. LIGHT comment_2: TOTAL VARIATION IS +/- 4 MAG fluxnum_1: 1 fluxval_1: B = 21.0 +/- 0.5 fluxnum_2: 2 fluxval_2: V = 20.3 +/- 0.5 fluxnum_3: 3 fluxval_3: R = 19.4 +/- 0.5 fluxnum_4: 4 fluxval_4: B-V = 1.0 +/- 0.3 fluxnum_5: 5 fluxval_5: A(V) = 1.5 +/- 1.0 fluxnum_6: 6 fluxval_6: E(B-V) = 0.5 +/- 0.35 ! targnum: 2 name_1: PSR1957+20-SPEC name_2: ECLIPSING-MILLISECOND-PULSAR descr_1: PULSAR, NEUTRON STAR, ECLIPSING BINARY descr_2: INTERACTING BINARY pos_1: TBD-EARLY, pos_2: RA-OFF = 1.37S +/- 0.1S, pos_3: DEC-OFF = -3.06" +/- 0.5", pos_4: FROM 3 equinox: 1950 pos_epoch_yr: 1988.00 acqpr_1: COMP comment_1: B,V,R,B-V AT MAX. LIGHT comment_2: TOTAL VARIATION IS +/- 4 MAG fluxnum_1: 1 fluxval_1: B = 21.0 +/- 0.5 fluxnum_2: 2 fluxval_2: V = 20.3 +/- 0.5 fluxnum_3: 3 fluxval_3: R = 19.4 +/- 0.5 fluxnum_4: 4 fluxval_4: B-V = 1.0 +/- 0.3 fluxnum_5: 5 fluxval_5: A(V) = 1.5 +/- 1 fluxnum_6: 6 fluxval_6: E(B-V) = 0.5 +/- 0.35 ! targnum: 3 name_1: SOMESTAR-OFFSET descr_1: STAR pos_1: TBD-EARLY, pos_2: RA = 19H 59M 35.431S +/- 0.01S, pos_3: DEC = +20D 48' 18.04" +/- 0.02" equinox: 2000 comment_1: STAR "B" ON FINDING CHRTS fluxnum_1: 1 fluxval_1: V = 17.00 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F569W num_exp: 1 time_per_exp: 600S s_to_n: 100 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: POS TARG 10,-10 / 1-2; req_2: ORIENT 45D +/- 55D / 1-6; req_3: GUID TOL 0.020S / 1-6; req_4: ZERO-PHASE JD2447245.0846808 +/- 0.0001D; req_5: PERIOD 33001.9167S +/- 0.0004S; req_6: PHASE 0.75 +/- 0.01; req_7: EARLY ACQ FOR 7-12; req_8: CYCLE 1 comment_1: SYSTEM MAXIMUM; "V" FILTER comment_2: EPHEMERIS WILL BE UPDATED comment_3: LATER. OFFSET ANGLE comment_4: USED FOR P8 WAS 0.0 ! linenum: 2.000 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F791W num_exp: 2 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: PHASE 0.22 +/- 0.01 OF REF 1; req_2: SEQ 2-6; req_3: CYCLE 1 comment_1: OPTICAL MINIMUM; "I" FILTER comment_2: PHASE IS GIVEN FOR START OF comment_3: OBSERVATION. ! linenum: 2.500 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F791W num_exp: 1 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: POS TARG 9,-9 / 3-6; req_2: PHASE 0.07 +/- 0.01 OF REF 1; req_3: AFTER 2 BY 70D; req_4: SEQ 2.5-6 NO GAP; req_5: CYCLE 1 comment_1: NEAR OPTICAL MINIM; "I" FLTR comment_2: PHASE IS GIVEN FOR START OF comment_3: OBSERVATION. THIS EXPOSURE IS TO comment_4: FORCE THE ACQUISITION INTO THE comment_5: PREVIOUS ORBIT. ! linenum: 3.000 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F675W num_exp: 1 time_per_exp: 600S s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: SEQ 3-4 NON-INT; req_2: CYCLE 1 comment_1: NEAR OPTICAL MINIM; "R" FLTR comment_2: PHASE IS GIVEN FOR START OF comment_3: OBSERVATION. comment_4: THIS MAY BE MADE INTO AN "I" comment_5: FILTER, DEPENDING ON RESULTS comment_6: OF LINE 2. ! linenum: 4.000 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F791W num_exp: 1 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: CYCLE 1 comment_1: OPTICAL MINIMUM; "I" FILTER ! linenum: 5.000 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F791W num_exp: 1 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: SEQ 5-6 NON-INT; req_2: CYCLE 1 comment_1: OPTICAL MINIMUM; "I" FILTER ! linenum: 6.000 targname: PSR1957+20 config: PC opmode: IMAGE aperture: P8 sp_element: F675W num_exp: 1 time_per_exp: 600S s_to_n: 10 fluxnum_1: 3 priority: 1 param_1: PRE-FLASH=YES param_2: CR-SPLIT=DEF req_1: CYCLE 1 comment_1: NEAR OPTICAL MINIMUM; comment_2: "R" FILTER comment_3: THIS MAY BE MADE INTO AN "I" comment_4: FILTER, DEPENDING ON RESULTS comment_5: OF LINE 2. ! linenum: 7.000 targname: SOMESTAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 1 req_1: AFTER 1 BY 90D; req_2: ONBOARD ACQ FOR 8; req_3: SEQ 7-8 NO GAP; req_4: CYCLE 1 comment_1: ONBOARD ACQ PRIOR TO OFFSET TO comment_2: SCIENCE TARGET. FINAL COORDS TBD comment_3: BY EARLY ACQ. FINAL ACQUISITION comment_4: STRATEGY TBD AFTER PC IMAGE IS comment_5: STUDIED.BRIGHT,FAINT,TIME_PER_EXP comment_6: MAY ALSO BE MODIFIED ! linenum: 8.000 targname: PSR1957+20-SPEC config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G160L wavelength: 1150-2524 num_exp: 2 time_per_exp: 1320S s_to_n: 4 fluxnum_1: 1 priority: 1 req_1: PHASE 0.65 +/- 0.05 OF REF 1; req_2: ORIENT 143.2D +/- 5D; req_3: DARK TIME; req_4: CYCLE 1 comment_1: COORDS, ORIENT TBD VIA EARLY ACQ. comment_2: ORIENT +180 OK. OFFSET ANGLE OF comment_3: SLIT WAS 98.19D. PHASE IS FOR comment_4: START OF OBS. EXPOSURE MUST OCCUR comment_5: BETWN PHASES 0.60-0.90.DARK TIME comment_6: LESS IMPORTANT THAN PHASE, ORIENT ! linenum: 9.000 targname: SOMESTAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 1 req_1: AFTER 1 BY 90D; req_2: ONBOARD ACQ FOR 10; req_3: SEQ 9-10 NO GAP; req_4: CYCLE 1 comment_1: ONBOARD ACQ PRIOR TO OFFSET TO comment_2: SCIENCE TARGET. FINAL COORDS TBD comment_3: BY EARLY ACQ. FINAL ACQUISITION comment_4: STRATEGY TBD AFTER PC IMAGE IS comment_5: STUDIED.BRIGHT,FAINT,TIME_PER_EXP comment_6: MAY ALSO BE MODIFIED ! linenum: 10.000 targname: PSR1957+20-SPEC config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G160L wavelength: 1150-2524 num_exp: 2 time_per_exp: 1320S s_to_n: 4 fluxnum_1: 1 priority: 1 req_1: PHASE 0.65 +/- 0.05 OF REF 1; req_2: ORIENT 143.2D +/- 5D; req_3: DARK TIME; req_4: CYCLE 1 comment_1: COORDS, ORIENT TBD VIA EARLY ACQ. comment_2: ORIENT +180 OK. OFFSET ANGLE OF comment_3: SLIT WAS 98.19D. PHASE IS FOR comment_4: START OF OBS. EXPOSURE MUST OCCUR comment_5: BETWN PHASES 0.60-0.90.DARK TIME comment_6: LESS IMPORTANT THAN PHASE, ORIENT ! linenum: 11.000 targname: SOMESTAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 1 req_1: AFTER 1 BY 90D; req_2: ONBOARD ACQ FOR 12; req_3: SEQ 11-12 NO GAP; req_4: CYCLE 1 comment_1: ONBOARD ACQ PRIOR TO OFFSET TO comment_2: SCIENCE TARGET. FINAL COORDS TBD comment_3: BY EARLY ACQ. FINAL ACQUISITION comment_4: STRATEGY TBD AFTER PC IMAGE IS comment_5: STUDIED.BRIGHT,FAINT,TIME_PER_EXP comment_6: MAY ALSO BE MODIFIED ! linenum: 12.000 targname: PSR1957+20-SPEC config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G160L wavelength: 1150-2524 num_exp: 2 time_per_exp: 1320S s_to_n: 4 fluxnum_1: 1 priority: 1 req_1: PHASE 0.65 +/- 0.05 OF REF 1; req_2: ORIENT 143.2D +/- 5D; req_3: DARK TIME; req_4: CYCLE 1 comment_1: COORDS, ORIENT TBD VIA EARLY ACQ. comment_2: ORIENT +180 OK. OFFSET ANGLE OF comment_3: SLIT WAS 98.19D. PHASE IS FOR comment_4: START OF OBS. EXPOSURE MUST OCCUR comment_5: BETWN PHASES 0.60-0.90.DARK TIME comment_6: LESS IMPORTANT THAN PHASE, ORIENT ! linenum: 13.000 targname: SOMESTAR-OFFSET config: FOS/BL opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 90S fluxnum_1: 1 priority: 1 req_1: AFTER 1 BY 90D; req_2: ONBOARD ACQ FOR 14; req_3: SEQ 13-14 NO GAP; req_4: CYCLE 1 comment_1: ONBOARD ACQ PRIOR TO OFFSET TO comment_2: SCIENCE TARGET. FINAL COORDS TBD comment_3: BY EARLY ACQ. FINAL ACQUISITION comment_4: STRATEGY TBD AFTER PC IMAGE IS comment_5: STUDIED.BRIGHT,FAINT,TIME_PER_EXP comment_6: MAY ALSO BE MODIFIED ! linenum: 14.000 targname: PSR1957+20-SPEC config: FOS/BL opmode: ACCUM aperture: 0.25X2.0 sp_element: G160L wavelength: 1150-2524 num_exp: 2 time_per_exp: 1320S s_to_n: 4 fluxnum_1: 1 priority: 1 req_1: PHASE 0.65 +/- 0.05 OF REF 1; req_2: ORIENT 143.2D +/- 5D; req_3: DARK TIME; req_4: CYCLE 1 comment_1: COORDS, ORIENT TBD VIA EARLY ACQ. comment_2: ORIENT +180 OK. OFFSET ANGLE OF comment_3: SLIT WAS 98.19D. PHASE IS FOR comment_4: START OF OBS. EXPOSURE MUST OCCUR comment_5: BETWN PHASES 0.60-0.90.DARK TIME comment_6: LESS IMPORTANT THAN PHASE, ORIENT ! ! end of exposure logsheet ! No scan data records found