! $Id: 5377,v 11.1 1994/07/27 17:16:50 pepsa Exp $ coverpage: title_1: UV OBSERVATIONS OF PULSARS: CYCLE4MEDIUM sci_cat: HOT STARS sci_subcat: NEUTRON STARS proposal_for: GO pi_fname: FRANCE pi_mi: A. pi_lname: CORDOVA pi_inst: 3150 pi_country: USA pi_phone: 814-865-0418 hours_pri: 4.25 num_pri: 3 foc: Y off_fname: ROBERT off_lname: KILLOREN off_title: DIRECTOR off_inst: 3150 off_addr_1: SPONSORED PROGRAMS AND CONTACTS OFFICE off_addr_2: 118 BARBARA BUILDING II off_city: UNIVERSITY PARK off_state: PA off_zip: 16802 off_country: USA off_phone: 814-865-1027 ! end of coverpage abstract: line_1: We propose to make UV observations of three nearby pulsars - line_2: PSR 0656+14, PSR 0950+08 and PSR 1929+10. The former one is a line_3: relatively young soft X-ray pulsar which shows the highest intensity line_4: of the soft X-ray flux and has a thermal-like spectrum. The latter line_5: two are the nearest old radio and soft X-ray pulsars. None of these line_6: objects have been imaged in the UV. Preliminary estimates of their line_7: surface temperatures, made with the aid of X-ray observations and line_8: theoretical cooling scenarios, indicate they should be sufficiently line_9: hot objects, and their thermal-like UV radiation should be line_10: observable with the HST Faint Object Camera. The UV spectra, line_11: together with the soft X-ray spectra, will be fitted with a new line_12: generation of neutron star atmosphere models that we are developing. line_13: This will allow us to determine parameters of the atmospheres line_14: (effective temperature, magnetic field, chemical composition), line_15: to study the thermal evolution of neutron stars and to investigate line_16: properties of the super-high-density matter in their interiors. ! ! end of abstract general_form_proposers: lname: CORDOVA fname: FRANCE mi: A. inst: 3150 country: USA ! lname: PAVLOV fname: GEORGE mi: G. inst: 3150 country: USA ! lname: STRINGFELLOW fname: GUY mi: S. inst: 3150 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to use FOC/96 for detection of the nearby pulsars line_2: 0656+14, 0950+08 and 1929+10. These objects have not yet been line_3: detected in the optical/UV range so that actual values of their line_4: fluxes are unknown. To detect them firmly and to evaluate the total line_5: UV flux, we propose to use the long pass F130LP filter (the filter line_6: is used to cut off the airglow background). To estimate the line_7: exposure times, we used ROSAT data and neutron star atmosphere line_8: models. The models yield optical/UV fluxes close to Rayleigh-Jeans line_9: fluxes corresponding to surface temperatures of the neutron stars. line_10: Extending the soft X-ray spectrum of PSR 0656+14 down to the UV line_11: range yields an estimate U=26.5-27.5 (Anderson et al., 1993, line_12: Ap.J., 414, 867). The 85 min exposure with F130LP would then provide line_13: a signal-to-noise ratio S/N=7-14 (at n=21 pixels). This estimate line_14: is obtained assuming a background rate R_B/n=0.002 counts/s/pix. line_15: The main contribution to the background comes from the zodiacal line_16: light; its intensity was assumed to be 200 S10 units, which is line_17: close to the maximum value over a half-year period when the difference line_18: between the target ecliptic longitude (105D) and the longitude of line_19: the Sun exceeds 90D. ROSAT data available on the old cooler pulsars line_20: 0950+08 and 1929+10 give only upper limits on their surface line_21: temperatures. We chose the same exposures for these, which would line_22: allow significant detections if the temperatures are 100000 and line_23: 200000 K, respectively. ! question: 4 section: 1 line_1: All the proposed objects are expected to be so hot that they are line_2: brighter in the UV range unobservable from the ground. The old line_3: pulsars, 0950+08 and 1929+10, are too faint, V > 27 - 28, for line_4: ground-based or other space observations. At least, all attempts line_5: to detect the radio pulsars with ground-based telescopes (Perriman line_6: et al., 1989, Astron. Astrophys, 215, 195; Van Kerkwijk, 1992, line_7: private communication) have been so far unsuccessful. For PSR 0656+14 line_8: only limiting magnitudes, R > 23 and V > 25, are known. Thus the line_9: presently proposed FOC observations are justified on the basis of line_10: the need to obtain ULTRAVIOLET imaging at wavelengths as short line_11: as 1300 A, and to ensure that the source is detected with a S/N line_12: ratio high enough to measure the broadband spectrum of the object line_13: and to constrain the surface temperature of the neutron star. ! question: 5 section: 1 line_1: To reach the faint source limit with the F130LP filter which line_2: is sensitive to 1304 A airglow, we request nighttime observations line_3: for all three exposures. Since the targets lie at low ecliptic line_4: latitudes (-8.5D, -4.6D and 32.3D for 0656+14, 0950+08 and 1929+10, line_5: respectively) where the zodiacal light is rather intense, it is line_6: very desirable to observe in seasons when the ecliptic longitudes line_7: of the targets (105D, 145D and 297D, respectively) are sufficiently line_8: far from the longitude of the Sun. ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: F. Cordova is a Co-I on the HST proposals: line_2: ID 3578, "Line Eclipse Mapping of an Accretion Disk Wind", line_3: ID 3579, "The UV Orbital Light Curve of the X-ray Binary X 1822-371". line_4: G. Stringfellow is a Co-I on the HST proposal: line_5: ID 2590, "Deep Imaging of the Site of SN 1961V". line_6: These observations are not related to the present project. ! question: 10 section: 1 line_1: Penn State's Astronomy and Astrophysics department will provide line_2: computing capabilities including a network of Sun workstations line_3: connected by Ethernet, as well as access to mainframes and line_4: supercomputers outside the department. ! !end of general form text general_form_address: lname: CORDOVA fname: FRANCE mi: A. category: PI inst: 3150 addr_1: DEPARTMENT OF ASTRONOMY AND ASTROPHYSICS addr_2: 525 DAVEY LABORATORY city: UNIVERSITY PARK state: PA zip: 16802 country: USA phone: 814-865-0418 telex: cordova@astro.psu.edu ! lname: LUMB fname: DAVID mi: H. category: CON inst: 3150 addr_1: DEPARTMENT OF ASTRONOMY AND ASTROPHYSICS addr_2: 525 DAVEY LABORATORY city: UNIVERSITY PARK state: PA zip: 16802 country: USA phone: 814-863-6041 telex: dlumb@astro.psu.edu ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: PSR0656+14 descr_1: A,160 pos_1: RA = 6H 59M 48.148S +/- 0.004S, pos_2: DEC = +14D 14' 21.31" +/- 0.04" equinox: J2000 fluxnum_1: 1 fluxval_1: V=28.3 +/- 1, E(B-V)= 0.02 +/- 0.02 fluxnum_2: 2 fluxval_2: B-V= -0.3 +/- 0.1, U-B= -1.1 +/- 0.2 fluxnum_3: 2 fluxval_3: A(U)= 0.15 +/- 0.1 fluxnum_4: 3 fluxval_4: F(3450)= 7 +/- 6 E-20 ! targnum: 2 name_1: PSR0950+08 descr_1: A,160 pos_1: RA = 9H 53M 09.326S +/- 0.008S, pos_2: DEC = +7D 55' 35.91" +/- 0.09" equinox: J2000 fluxnum_1: 1 fluxval_1: V=28.4 +/- 2, E(B-V)=0.01 +/- 0.01 fluxnum_2: 2 fluxval_2: B-V= -0.3 +/- 0.1, U-B= -1.1 +/- 0.2 fluxnum_3: 2 fluxval_3: A(U)= 0.05 +/- 0.05 fluxnum_4: 3 fluxval_4: F(3450)= 7 +/- 6 E-20 ! targnum: 3 name_1: PSR1929+10 descr_1: A,160 pos_1: RA = 19H 32M 13.924S +/- 0.009S, pos_2: DEC = +10D 59' 32.07" +/- 0.19" equinox: J2000 fluxnum_1: 1 fluxval_1: V=28.2 +/- 2, E(B-V)= 0.1 +/- 0.05 fluxnum_2: 2 fluxval_2: B-V=0.2 +/- 0.1, U-B=1.0 +/- 0.2 fluxnum_3: 2 fluxval_3: A(U)= 0.5 +/- 0.3 fluxnum_4: 3 fluxval_4: F(3450)= 7 +/-6 E-20 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: PSR0656+14 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F130LP num_exp: 1 time_per_exp: 85M s_to_n: 10 fluxnum_1: 3 priority: 1 req_1: CYCLE 4; req_2: DARK TIME; req_3: AT 5-JAN-95 +/- 90D comment_1: THE EXPOSURE MAY BE TAKEN ALSO BEFORE comment_2: 5-APR-1994, I.E., REQ_3 CAN BE comment_3: REPLACED BY "AT 18-MAR-94 +/- 18D". comment_4: THE LATTER PERIOD IS CHOSEN comment_5: ASSUMING CYCLE 4 STARTS comment_6: AT 1-MAR-94. ! linenum: 2.000 targname: PSR0950+08 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F130LP num_exp: 1 time_per_exp: 85M s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: DARK TIME; req_3: AT 1-MAR-94 +/- 75D comment_1: REQ_3 CAN BE comment_2: REPLACED BY "AT 15-FEB-95 +/- 90D". ! linenum: 3.000 targname: PSR1929+10 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F130LP num_exp: 1 time_per_exp: 85M s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: DARK TIME; req_3: AT 19-JUL-94 +/- 140D comment_1: THE EXPOSURE MAY BE TAKEN ALSO AFTER comment_2: 1-MAR-95, I.E., REQ_3 CAN BE comment_3: REPLACED BY "AT APR-10-95 +/- 41D". comment_4: THE LATTER PERIOD IS CHOSEN comment_5: ASSUMING CYCLE 4 IS COMPLETED comment_6: AT 1-JUL-95. ! linenum: 4.000 targname: PSR1929+10 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F130LP num_exp: 1 time_per_exp: 1449S s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: AT 19-JUL-94 +/- 20D comment_1: SCIENCE SHOULD BE DONE IN DARK TIME; ! linenum: 4.100 targname: PSR1929+10 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F430W param_1: PIXEL=50X25 num_exp: 1 time_per_exp: 10M s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: AT 19-JUL-94 +/- 140D ! linenum: 4.200 targname: INTFLAT config: FOC/96 opmode: RESEAU aperture: 512X1024 sp_element: F430W param_1: PIXEL=50X25 param_2: LED=GREEN-2 param_3: LED-STEP=32 num_exp: 1 time_per_exp: 5M s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: AT 19-JUL-94 +/- 140D ! linenum: 4.300 targname: INTFLAT config: FOC/96 opmode: RESEAU aperture: 512X512 sp_element: F430W param_1: PIXEL=25X25 param_2: LED=GREEN-2 param_3: LED-STEP=96 num_exp: 1 time_per_exp: 5M s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: AT 19-JUL-94 +/- 140D ! linenum: 5.000 targname: PSR1929+10 config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 61M s_to_n: 10 fluxnum_1: 3 priority: 2 req_1: CYCLE 4; req_2: DARK TIME; req_3: AT 19-JUL-94 +/- 20D ! ! end of exposure logsheet ! No scan data records found