! File: 4571C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:18:09:24 coverpage: title_1: SPECTROSCOPIC IDENTIFICATION OF CANDIDATE OPTICAL COUNTERPARTS OF title_2: ROSAT X-RAY SOURCES IN THE NEARBY COLLAPSED GLOBULAR CLUSTER NGC6397 CYC3MEDIUM sci_cat: HOT STARS sci_subcat: X-RAY BINARIES proposal_for: GO pi_title: PROF pi_fname: JONATHAN pi_mi: E pi_lname: GRINDLAY pi_inst: HARVARD UNIVERSITY pi_country: USA pi_phone: 617 4967204 hours_pri: 3.40 num_pri: 3 fos: Y funds_amount: 35924 funds_length: 7 funds_date: JAN-94 pi_position: PROF off_fname: CONSTANCE off_lname: GALANIS off_title: ASSISTANT DIRECTOR off_inst: 2170 off_addr_1: HARVARD UNIVERSITY off_addr_2: OFFICE FOR SPONSORED RESEARCH off_addr_3: HOLYOKE CENTER 441 off_city: CAMBRIDGE off_state: MA off_zip: 02138 off_country: USA off_phone: 617-495-5501 ! end of coverpage abstract: line_1: We propose to obtain FOS spectra of a candidate counterpart to a line_2: faint X-ray source that we have detected in the nearby, collapsed- line_3: core globular cluster NGC 6397 using the ROSAT High Resolution Imager (HRI). line_5: This object is likely to be either a cataclysmic line_6: variables (CVs), that was produced by tidal capture events in the dense core of line_7: the cluster, or an RS CVn binary that has been hardened by interactions with line_8: other stars. line_10: Due to the extreme crowding at the center of NGC 6397, spectroscopic study of line_11: faint candidate requires the angular resolution provided by HST. This study line_12: will provide a critical test of theories for the formation and evolution in line_13: clusters of interacting binaries and their progeny -- CVs, RS CVns, low-mass line_14: X-ray binaries (LMXBs), and millisecond pulsars. ! ! end of abstract general_form_proposers: lname: GRINDLAY fname: JONATHAN title: PI mi: E. inst: 2170 country: USA ! lname: CALLANAN fname: PAUL mi: J. inst: 2170 country: USA ! lname: COOL fname: ADRIENNE mi: M. inst: 2170 country: USA ! lname: BAILYN fname: CHARLES mi: D. inst: 3900 country: USA ! lname: COHN fname: HALDAN mi: N. inst: 2270 country: USA ! lname: LUGGER fname: PHYLLIS mi: M. inst: 2270 country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose to use the FOS with the red detector and G570H grating line_2: (covering the wavelength range 4571-6820 A), enabling us to cover line_3: H-alpha, H-beta and HeII 4686. The sequence of three targets is line_4: designed to provide accurate and reliable pointing in the extreme line_5: crowding in this globular cluster. The first star is used for line_6: pointing exclusively; the second is used to improve the pointing line_7: accuracy and to obtain a spectrum of the background light in the line_8: vicinity of the third target. The third target is the primary line_9: science target, and requires that the pointing be accurate to 0.1" or line_10: better. The first target star was chosen because it is isolated line_11: enough to allow the use of the ACQ/BINARY target acquisition method line_12: reliably. The GASP group at STScI has measured our PC frames line_13: containing this star (in PC7) as well as the second and third targets line_14: (in PC6) relative to the Guide Star Catalog system. Following line_15: ACQ/BINARY (pointing accuracy less or equal to 0.2") on this star, we line_16: OFFSET to a second star close to target 3, and do a fine pointing on line_17: it using the ACQ/PEAK mode, and the 0.3" circular aperture in order to line_18: obtain pointing accurate to less or equal to 0.1", which is critical line_19: for the observation of target 3. The 5x5 SPATIAL SCAN we perform with line_20: the 0.3" aperture relies on there being an additional error of less line_21: than 0.2" due to offsetting and inaccuracies in relative positions of line_22: the targets. Following ACQ/PEAK on the second target, we OFFSET FROM line_23: IT to the final target (1.3" away). ! question: 4 section: 1 line_1: The extreme crowding in this globuar cluster field requires the line_2: HST (see Question 3). ! question: 5 section: 1 line_1: The 5 "exposures" that make up this observation MUST BE DONE IN THE line_2: ORDER SPECIFIED (linenum 1 through linenum 5). The ONLY POSSIBLE EXCEPTION to line_3: this is that linenum 4 and 5 could be interchanged. This sequence (SEQ) is line_4: designed to obtain reliable and accurate pointing in this very crowded line_5: field at the center of a globular cluster (see Question 3). We give line_6: absolute positions of only the first target (measured for us at STScI line_7: relative to the GSC on PC frames we had previously obtained). It is line_8: the only target of the three that is sufficiently isolated to permit a line_9: reliable intial pointing. Once we have acquired this target we OFFSET line_10: to the second target, which we use to improve the accuracy of the line_11: pointing (using AQC/PEAK). We then OFFSET from this position to the line_12: final (and principal science) target just 1.3" away. ! question: 7 section: 1 line_1: The spectra will be searched for evidence for any emission features line_2: which would indicate an interacting binary system. The data will be line_3: reduced using the standard IRAF reduction routines: all proposers have line_4: experience reducing HST data using IRAF on SUN and VMS systems. ! question: 9 section: 1 line_1: We have successfully proposed for two photometry proposals and line_2: one archival research proposal for work related to this investigation: line_4: Cycle 1: Program P2555, ``Cataclysmic Variables and Millisecond Pulsars line_5: in Globular Cluster Cusps" (J. Grindlay, PI). line_6: Cycle 2: Program GO-3851, ``Deep Search for CVs and Compact Binaries line_7: in the Collapsed Close Globular NGC6397" (J. Grindlay, PI). line_8: Cycle 2, archival research: Program AR-3793, ``Comparison of HST Data line_9: on Globular Clusters with Other Data Sets" (C. Bailyn, PI). line_11: The P2555 program was for a preliminary H-alpha vs. R image of the line_12: core of NGC6752. A total of about 2 hours exposure was obtained with line_13: PC, yielding a senistivity limit of about Mv = 5. The data were line_14: incorrectly processed (at STScI) originally in that the wrong bias line_15: frames were used. The re-processed bias frames and flats were received line_16: only in January 1992, and we are currently still in the process of line_17: carrying out a DAOPHOT analsysis of the images. ! question: 10 section: 1 line_1: CfA is fully equipped to reduce HST data (with IRAF). Co-I's also have line_2: access to similar HST data reduction facilities. ! !end of general form text general_form_address: lname: GRINDLAY fname: JONATHAN mi: E. title: PROF category: PI inst: 2170 addr_1: HARVARD COLLEGE OBSERVATORY addr_2: CENTER FOR ASTROPHYSICS addr_3: 60 GARDEN STREET city: CAMBRIDGE state: MA zip: 02138 country: USA phone: 617-495-7204 telex: 921428 from_date: 31-JAN-94 to_date: 30-JUN-94 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC6397-STAR1-OFFSET descr_1: A,138,C,201 pos_1: PLATE-ID=0688, pos_2: RA = 17H 40M 40.639S +/- 0.100S, pos_3: DEC = -53D 40' 01.707" +/- 1.00" equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 fluxnum_1: 1 fluxval_1: V = 14, B-V=0.85, TYPE=G5III fluxnum_2: 2 fluxval_2: E(B-V) = 0.2 ! targnum: 2 name_1: NGC6397-STAR2-OFFSET descr_1: A,138,C,201 pos_1: PLATE-ID=0688, pos_2: RA-OFF = 0.8622S +/- 0.005S, pos_3: DEC-OFF = -20.246" +/- 0.05", pos_4: FROM 1 equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 fluxnum_1: 1 fluxval_1: V = 14, B-V=0.85, TYPE=G5III fluxnum_2: 2 fluxval_2: E(B-V) = 0.2 ! targnum: 3 name_1: NGC6397-STAR3 descr_1: A,161,C,201 pos_1: PLATE-ID=0688, pos_2: RA-OFF = 0.8852S +/- 0.005S, pos_3: DEC-OFF = -18.960" +/- 0.05", pos_4: FROM 1 equinox: J2000 pos_epoch_bj: J pos_epoch_yr: 2000.00 fluxnum_1: 1 fluxval_1: V = 18 fluxnum_2: 2 fluxval_2: E(B-V) = 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC6397-STAR1-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3S fluxnum_1: 1 priority: 1 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 2; req_3: SEQ 1-5 NO GAP ! linenum: 2.000 targname: NGC6397-STAR2-OFFSET config: FOS/RD opmode: ACQ/PEAK aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 4.5S fluxnum_1: 1 priority: 1 param_1: TYPE=UP, param_2: SEARCH-SIZE=5, param_3: SCAN-STEP=0.2 req_1: CYCLE 3; req_2: ONBOARD ACQ FOR 3; ! linenum: 3.000 targname: NGC6397-STAR2-OFFSET config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: G570H wavelength: 4571-6815 num_exp: 1 time_per_exp: 7M fluxnum_1: 1 priority: 1 req_1: CYCLE 3 ! linenum: 4.000 targname: NGC6397-STAR3 config: FOS/RD opmode: ACCUM aperture: 0.5 sp_element: G570H wavelength: 4571-6815 num_exp: 1 time_per_exp: 50M fluxnum_1: 1 priority: 1 req_1: CYCLE 3 ! linenum: 5.000 targname: NGC6397-STAR3 config: FOS/RD opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 2.2M fluxnum_1: 1 priority: 1 req_1: CYCLE 3 ! ! end of exposure logsheet ! No scan data records found