! File: 4343C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:22:36:21 coverpage: title_1: WHITE DWARF COMPANIONS OF BARIUM AND CH STARS sci_cat: COOL STARS proposal_for: GO pi_fname: ERIKA pi_mi: HR pi_lname: BOHM-VITENSE pi_inst: UNIVERSITY OF WASHINGTON pi_country: U.S.A. hours_pri: 6.35 num_pri: 12 fos: Y funds_length: 12 off_fname: DONALD off_mi: W off_lname: ALLEN off_title: DIRECTOR off_inst: 3760 off_addr_1: GRANTS AND CONTRACT SERVICES off_addr_2: 3935 UNIVERSITY WAY NE JM-24 off_city: SEATTLE off_state: WA off_zip: 98195 off_country: U.S.A. off_phone: 206 543 4043 ! end of coverpage abstract: line_1: In 1980 Mc Clure et al.(Ap.J. 238,l35) discovered that all Ba stars line_2: show radial velocity variations indicative of binary nature. In 1984 line_3: (Ap.J. 352,709) Mc Clure found the same for subgiant CH and giant CH line_4: stars. These authors already suspected that the companions are white line_5: dwarfs. White dwarf companions were indeed detected for the Ba star line_6: zeta Cap and for the mild Ba stars zeta Cyg (Bohm-Vitense, Nemec and line_7: Proffitt, 1983) by means of IUE observations. Some indirect evidence line_8: was seen for other mild Ba stars, but except for zeta Cap, no WD line_9: companions have been seen for strong Ba stars nor for any CH stars line_10: though we have looked with IUE. If present these WD must be too faint line_11: to be observable with IUE. We would like to look for them now with line_12: HST. It seems very important to check whether indeed strong Ba stars line_13: and CH stars all have WD companions. It is now generally accepted that line_14: the chemical peculiarities on the surfaces of these stars are due to line_15: mass transfer from an evolved AGB star companion which has line_16: subsequently evolved into the present white dwarf companion. While we line_17: also believe that this is so, we would feel much more assured if line_18: WD companions could be detected for more Ba stars (not only mild line_19: ones) and if also any WD companions could be seen for subgiant and for line_20: giant CH stars. ! ! end of abstract general_form_proposers: lname: BOHM-VITENSE fname: ERIKA title: PI mi: HR inst: UNIVERSITY OF WASHINGTON country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We would like to take low resolution, short wavelength spectra line_2: with the FOS and with the G 160L grating with the 4.3" aperture. line_3: We would like to observe 4 Ba stars, one subgiant CH star, 2 giant line_4: CH stars and 2 weak G band stars in order to see and study the WD line_5: companions believed to be present. We would like to observe also 3 line_6: standard late G and early K stars with similar exposure levels as line_7: the peculiar stars for comparison, in ordeer to see whether the line_8: peculiar abundance stars show excess UV flux indicative of a WD line_9: companion. For the standard star exposure levels similar to those line_10: for the peculiar abundance stars are needed, because they might line_11: possibly bring up a faint chromospheric continuum which otherwise line_12: might not be seen. Without these observations of the standard star line_13: we might confuse such a continuum, if present, in the peculiar line_14: abundance stars, with a weak WD spectrum. According to theoretical line_15: models for early K stars the photospheric flux around 1300 A line_16: should be reduced by 13 magnitudes as compared to the visual. WDs line_17: fainter by 13 magnitudes should then be detectable, unless these line_18: cool giants have a faint chromospheric continuum. If so, the WD line_19: has to be somewhat brighter to be detected. line_20: The red leaks of the UV filters used with the WC/PC cameras do line_21: not permit to detect white dwarf companions of luminous, red line_22: giants when the WDs may be 12 to 13 magnitudes fainter than the cool line_23: giants. ! question: 4 section: 1 line_1: We need the UV capabilities of HST and the large collecting area. line_2: White dwarf companions of red giants are much too faint to be line_3: detected in the visual. The giants are much too luminous. The light line_4: of the giants drowns the light of the white dwarfs. In the line_5: ultraviolet (lambda < 2000 A ) the light of the cool giants is line_6: reduced so much that white dwarfs of temperatures > 10,000 K and line_7: possibly down to 8000K should be detectable. For IUE the exposure line_8: times become too long and the background noise too high. All line_9: program stars have been observed with IUE but the WD could not be line_10: detected. If they are there, we will be able to seee blue WD line_11: companions with HST. ! question: 4 section: 2 line_1: I have assumed a temperature of 10,000 K for the unseen WD and line_2: log L/L(sun)=-2.9. Assuming that the Ba stars have about M(V)=0, line_3: which seems about average (see Bohm-Vitense et al. 1984,ApJ 278, line_4: 726) I have estimated the apparent magnitude of a 10,000K WD as line_5: given in the exposure logsheets. For 8000K the apparent magnitude line_6: is about 2.5 magnitudes fainter, reducing the S/N by a factor of line_7: 3. We have then estimated the exposure times assuming black body line_8: energy distribution for the WD aiming at the given S/N at 1600 A line_9: where the Ba and CH star contributions are small and probably line_10: negligible. line_11: For the standard stars we need comparable exposure times for line_12: comparable brightness with the Ba and CH stars. For shorter line_13: exposure times we might not see anything for the standard stars line_14: while for the program stars we might see light from the K stars line_15: because of the longer exposure times, which we might then line_16: erroneously interpret as white dwarf light. ! question: 7 section: 1 line_1: We will measure the energy distributions for the peculiar element line_2: abundance stars and for the standard stars of the same spectral line_3: type. For the spectra, normalized to equal visual magnitude, we line_4: shall then determine the difference in the UV fluxes between the line_5: peculiar star and the normal stars. If an excess is found for the line_6: peculiar star we shall compare the measured energy distribution of line_7: the excess flux with model atmosphere fluxes for WD in order to line_8: determine the temperature.Assuming an average mass of 0.6 M(sun) line_9: for the WD the effective temperature determines its luminosity, line_10: radius and age, and thereby the time since the mass transfer to line_11: the peculiar giant. The difference between the estimated lifetime line_12: of the Ba or CH star and the cooling time of the WD gives a rough line_13: estimate of the lifetime of the mass losing AGB star until it line_14: became a white dwarf. This will give us some crude information line_15: about its original mass. line_16: From a comparison of the surface flux of the WD, known from its line_17: effective temperature, and the measured flux at any given line_18: wavelength the distance to the system and the absolute magnitude line_19: of the CH or Ba star can be estimated. ! question: 9 section: 1 line_1: We have presently an HST program to determine Cepheid masses line_2: from Cepheid binaries. We have not yet received any observations. line_3: The Cepheid program is not related to this program. ! question: 10 section: 1 line_1: Image processing hardware and software is available at our line_2: department. Graduate students for help and for introduction to line_3: HST observations are also available but will have to be supported. ! !end of general form text general_form_address: lname: BOHM_VITENSE fname: ERIKA mi: HR category: PI inst: University of Washington addr_1: ASTRONOMY DEPARTMENT addr_2: UNIVERSITY OF WASHINGTON FM-20 city: SEATTLE state: WA zip: 98195 country: USA phone: (206) 543 4858 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD65699 name_2: HR3123 name_3: 12PUP descr_1: A;120 pos_1: RA=07H59M05.7S +/-1.0", pos_2: DEC=-23D18'38.4"+/-0.5", pos_3: PLATE-ID=04NO equinox: 2000 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 2000.00 ra_pm_val: -0.001000 ra_pm_unct: 0.001000 dec_pm_unct: 0.0100 an_prlx_val: 0.0100 an_prlx_unct: 0.0100 rv_or_z: V=+11.0 comment_1: WE WANT TO SEARCH FOR A comment_2: WHITE DWARF COMPANION TO comment_3: THIS BA STAR. THE FLUX comment_4: GIVEN ASSUMES AN A0 WD. comment_5: IT COULD BE HOTTER AND comment_6: BRIGHTER.THE BA STAR HAS comment_7: M(V)=5.1 AND B-V=1.12 fluxnum_1: 1 fluxval_1: V=17.1+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.2 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=.6+/-2E-13 ! targnum: 2 name_1: HD16458 name_2: HR774 descr_1: A;120 pos_1: RA=02H47M47.6S+/-1.0", pos_2: DEC=+81D26'55"+/-1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.005000 ra_pm_unct: 0.002000 dec_pm_val: -0.0700 dec_pm_unct: 0.0200 an_prlx_val: 0.0050 an_prlx_unct: 0.0050 rv_or_z: V=18 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION TO comment_3: THIS BA STAR. THE FLUX VALUE comment_4: GIVEN IS ESTIMATED FOR AN A0 comment_5: WD. IT COULD BE CONSIDERABLY comment_6: BRIGHTER OR ALSO comment_7: SOMEWHAT FAINTER. THE BA STAR comment_8: HAS M(V)=5.8 AND B-V=1.30 fluxnum_1: 1 fluxval_1: V=17.8+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.3 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=0.5+/-1.5E-13 ! targnum: 3 name_1: HD116713 name_2: HR5058 descr_1: A;120 pos_1: RA=13H26M7.8S +/-1.0", pos_2: DEC=-39D45'19"+/-1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.016000 ra_pm_unct: 0.002000 dec_pm_val: -0.0600 dec_pm_unct: 0.0300 an_prlx_val: 0.0100 an_prlx_unct: 0.0500 rv_or_z: V=+67 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION TO comment_3: THIS BA STAR. THE FLUX comment_4: VALUES GIVEN REFER TO AN comment_5: A0 WD. IT COULD BE comment_6: BRIGHTER OR SOMEWHAT comment_7: FAINTER.THE BA STAR HAS comment_8: M(V)=5.1 AND B-V=1.20 fluxnum_1: 1 fluxval_1: V=17.1+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.2 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=0.6+/-2.E-13 ! targnum: 4 name_1: HD101013 name_2: HR4474 descr_1: A;120 pos_1: RA=11H37M53.0S+/-1.0", pos_2: DEC=50D37'05"+/-1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.006000 ra_pm_unct: 0.002000 dec_pm_val: -0.0200 dec_pm_unct: 0.0100 an_prlx_val: 0.0100 an_prlx_unct: 0.0100 rv_or_z: V=-4 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION TO comment_3: THIS BA STAR.THE FLUX VALUES comment_4: GIVEN REFER TO AN A0 WD. IT comment_5: COULD BE BRIGHTER OR comment_6: SOMEWHAT FAINTER. THE BA STAR comment_7: HAS M(V)=6.2 AND B-V=1.07. fluxnum_1: 1 fluxval_1: V=18.2+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0 +/-0.20 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=0.2 +/-1.E-13 ! targnum: 5 name_1: HD166208 name_2: HR6791 descr_1: A;120 pos_1: RA=18H07M28.8S+/-1.0", pos_2: DEC=+43D27'42"+/-1" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_unct: 0.002000 dec_pm_val: -0.0600 dec_pm_unct: 0.0200 an_prlx_val: 0.0030 an_prlx_unct: 0.0030 rv_or_z: V=-16 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION TO comment_3: THIS WEAK G BAND STAR. THE FLUX comment_4: VALUES GIVEN REFER TO AN A0 comment_5: WD. IT COULD BE BRIGHTER comment_6: OR FAINTER. THE WEAK G BAND comment_7: STAR HAS M(V)=5.0 AND B-V=0.91 fluxnum_1: 1 fluxval_1: V=17.0+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.2 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=0.7+/-2.E-13 ! targnum: 6 name_1: HD165634 name_2: HR=6766 descr_1: A;120 pos_1: RA=18H08M05.0S+/-1.0", pos_2: DEC=-28D27'25"+/-1.0" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.002000 ra_pm_unct: 0.001000 dec_pm_val: -0.0300 dec_pm_unct: 0.0100 an_prlx_val: 0.0100 an_prlx_unct: 0.0100 rv_or_z: V=-5 comment_1: WE WANT TO SEARCH FOR comment_2: THE WHITE DWARF COMPANION comment_3: TO THIS WEAK G BAND STAR. comment_4: THE FLUX ESTIMATES ARE MADE comment_5: FOR AN A0 WD. IT COULD BE comment_6: BRIGHTER OR FAINTER. comment_7: THE WEAK G BAND STAR HAS comment_8: M(V)=4.6 AND B-V=0.94 comment_9: WE AIM AT S/N=10 fluxnum_1: 1 fluxval_1: V=14.6+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.2 fluxnum_3: 2 fluxval_3: F-CONT(1500)=0.6+/-2.E-12 fluxnum_4: 3 fluxval_4: E(B-V)=0.02+/-0.02 ! targnum: 7 name_1: HD182040 descr_1: A;120 pos_1: RA=19H23M10.09S+/-1.0", pos_2: DEC=-10D42'11.2"+/-1.0", pos_3: PLATE-ID=06OD equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.001000 ra_pm_unct: 0.001000 dec_pm_val: 0.0200 dec_pm_unct: 0.0050 an_prlx_val: 0.0030 an_prlx_unct: 0.0010 rv_or_z: V=-47 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION comment_3: TO THIS CH STAR. THE GIVEN comment_4: FLUXES ASSUME AN A0 WD. comment_5: IT COULD BE comment_6: BRIGHTER OR FAINTER. WE AIM comment_7: AT S/N=5. THE CH STAR HAS comment_8: M(V)=6.99 AND B-V=1.07 fluxnum_1: 1 fluxval_1: V=19.0+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.20 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=0.1+/-0.6E-13 ! targnum: 8 name_1: HD137613 descr_1: A;120 pos_1: RA=15H27M48.32S+/-1.0", pos_2: DEC=-25D10'10"+/-1.0", pos_3: PLATE-ID=00GV equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_unct: 0.001000 dec_pm_unct: 0.1000 an_prlx_val: 0.0040 an_prlx_unct: 0.0030 rv_or_z: V=+55 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION comment_3: TO THIS CH STAR. THE FLUX comment_4: VALUES GIVEN ASSUME AN A0 comment_5: WD. IT COULD BE BRIGHTER comment_6: OR FAINTER.THE CH STAR HAS comment_7: M(V)=7.5 AND B-V=1.18. comment_8: WE AIM AT S/N=4. fluxnum_1: 1 fluxval_1: V=19.5+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.2 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=.7+/-2.5E-14 ! targnum: 9 name_1: HD89948 descr_1: A;120 pos_1: RA=10H22M21.88S+/-1", pos_2: DEC=-29D33'23.6"+/-1", pos_3: PLATE-ID=04JB equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: -0.001000 ra_pm_unct: 0.001000 dec_pm_val: 0.0800 dec_pm_unct: 0.0200 an_prlx_val: 0.0020 an_prlx_unct: 0.0020 rv_or_z: V=0.0 comment_1: WE WANT TO SEARCH FOR THE comment_2: WHITE DWARF COMPANION TO comment_3: THIS SUBGIANT CH STAR,WHICH comment_4: HAS M(V)=7.7. THE FLUX VALUES comment_5: GIVEN ASSUME AN A0 WD. IT COULD comment_6: BE BRIGHTER OR FAINTER. comment_7: WE AIM AT S/N=7. fluxnum_1: 1 fluxval_1: V=17.7+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.0+/-0.2 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 fluxnum_4: 3 fluxval_4: F-CONT(1500)=0.4+/-1.5E-13 ! targnum: 10 name_1: HD40808-CALIB name_2: HR2120 name_3: ETA COL descr_1: A;140 pos_1: RA=05H59M08.78S+/-1", pos_2: DEC=-42D48'53.5"+/-1", pos_3: PLATE-ID=01D6 equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.002000 ra_pm_unct: 0.001000 dec_pm_val: -0.0100 dec_pm_unct: 0.0050 an_prlx_val: 0.0100 an_prlx_unct: 0.0500 rv_or_z: V=+17 comment_1: THIS IS A STANDARD STAR comment_2: WHICH WE NEED FOR COMPARISON comment_3: WITH THE STARS BELIEVED comment_4: TO HAVE WD COMPANIONS. comment_5: THE EXPOSURE TIMES NEED comment_6: TO REACH SIMILAR LEVELS comment_7: AS FOR THE BA AND CH STARS. fluxnum_1: 1 fluxval_1: V=4.0+/-0.1 fluxnum_2: 1 fluxval_2: B-V=1.14+/-0.02 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 ! targnum: 11 name_1: HD163993-CALIB name_2: HR6703 name_3: XSI HER descr_1: A;138 pos_1: RA=17H57M45.9S+/-1", pos_2: DEC=+29D14'52"+/-1" equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.006000 ra_pm_unct: 0.002000 dec_pm_val: -0.0200 dec_pm_unct: 0.0100 an_prlx_val: 0.0150 an_prlx_unct: 0.0100 rv_or_z: V=-2 comment_1: THIS IS A STANDARD STAR comment_2: FOR COMPARISON WITH THE comment_3: BA AND CH STARS BELIEVED comment_4: TO HAVE WD COMPANIONS. comment_5: THE EXPOSURE LEVELS NEED TO comment_6: REACH THE SAME DEPTH AS FOR comment_7: THE BA AND CH STARS. fluxnum_1: 1 fluxval_1: V=3.7+/-0.1 fluxnum_2: 1 fluxval_2: B-V=0.94+/-0.02 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 ! targnum: 12 name_1: HD157347-CALIB name_2: HR6465 descr_1: A;137 pos_1: RA=17H22M51.4S+/-1", pos_2: DEC=-02D23'19.2"+/-1", pos_3: PLATE-ID=03US equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.003000 ra_pm_unct: 0.001000 dec_pm_val: -0.1100 dec_pm_unct: 0.0500 an_prlx_val: 0.0200 an_prlx_unct: 0.0100 rv_or_z: V=-35 comment_1: THIS IS A STANDARD STAR comment_2: FOR COMPARISON WITH THE comment_3: SUBGIANT CH AND WEAK G comment_4: BAND STARS BELIEVED TO comment_5: HAVE WD COMPANIONS. THE comment_6: EXPOSURE FOR THIS STAR comment_7: MUST REACH COMPARABLE comment_8: DEPTH TO THOSE FOR THE comment_9: PECULIAR STARS. fluxnum_1: 1 fluxval_1: V=6.3+/-0.1 fluxnum_2: 1 fluxval_2: B-V=0.68+/-0.02 fluxnum_3: 2 fluxval_3: E(B-V)=0.02+/-0.02 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 11.000 targname: HD65699 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 11.5; req_3: CYCLE 3 / 11-122 ! linenum: 11.500 targname: HD65699 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 12; req_3: CYCLE 3 / 11-122 ! linenum: 12.000 targname: HD65699 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 21M s_to_n: 7 fluxnum_1: 3 fluxnum_2: 1 priority: 1 comment_1: THE EXPOSURE TIME IS CALCULATED comment_2: USING THE V MAGNITUDE comment_3: FOR THE BA STAR ! linenum: 21.000 targname: HD16458 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 0.03S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQUISITION FOR 22; req_3: CYCLE 3 / 21-22 comment_1: THE EXPOSURE TIMES ARE comment_2: CALCULATED USING THE comment_3: M(V) OF THE BA STAR. ! linenum: 21.500 targname: HD16458 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 22; req_3: CYCLE 3 / 21-22 ! linenum: 22.000 targname: HD16458 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 40M s_to_n: 7 fluxnum_1: 1 priority: 1 ! linenum: 31.000 targname: HD116713 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 31.5; req_3: CYCLE 3 / 31-32 comment_1: THE EXPOSURE TIMES comment_2: WERE CALCULATED USING comment_3: THE V OF THE BA STAR. ! linenum: 31.500 targname: HD116713 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 32; req_3: CYCLE 3 / 31-32 ! linenum: 32.000 targname: HD116713 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 21M s_to_n: 7 fluxnum_1: 3 fluxnum_2: 1 priority: 1 req_1: CYCLE 3 / 31-32 ! linenum: 41.000 targname: HD101013 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H num_exp: 1 time_per_exp: 0.02S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 41.5; req_3: CYCLE 3 /41-42 comment_1: THE EXPOSURE TIMES comment_2: WERE CALCULATED comment_3: USING THE comment_4: V MAGNITUDE OF THE comment_5: BA STAR. ! linenum: 41.500 targname: HD101013 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.02S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 42; req_3: CYCLE 3 / 41-42 ! linenum: 42.000 targname: HD101013 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 54M s_to_n: 7 fluxnum_1: 3 fluxnum_2: 1 priority: 1 ! linenum: 51.000 targname: HD166208 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 51.5; req_3: CYCLE 3 / 51-52 comment_1: THE EXPOSURE TIME comment_2: VALUES WERE CALCULATED comment_3: USING THE V MAGNITUDE comment_4: FOR THE BA STAR ! linenum: 51.500 targname: HD166208 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 52; req_3: CYCLE 3 / 51-52 ! linenum: 52.000 targname: HD166208 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 20M s_to_n: 7 fluxnum_1: 3 fluxnum_2: 1 priority: 1 req_1: CYCLE 3 / 51-52 ! linenum: 61.000 targname: HD165634 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 61.5; req_3: CYCLE 3 / 61-62 comment_1: THE EXPOSURE TIME comment_2: VALUES WERE CALCULATED comment_3: FROM THE V MAGNITUDE comment_4: OF THE WEAK G BAND STAR ! linenum: 61.500 targname: HD165634 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 62; req_3: CYCLE 3 / 61-62 ! linenum: 62.000 targname: HD165634 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 4M s_to_n: 10 fluxnum_1: 3 priority: 1 req_1: CYCLE 3 / 61-62 ! linenum: 71.000 targname: HD182040 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.04S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 71.5; req_3: CYCLE 3 / 71-72 comment_1: THE EXPOSURE TIME WAS comment_3: CALCULATED FROM THE comment_4: V MAGNITUDE OF THE comment_5: CH STAR ! linenum: 71.500 targname: HD182040 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.04S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 72; req_3: CYCLE 3 / 71-72 ! linenum: 72.000 targname: HD182040 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 61M s_to_n: 5 fluxnum_1: 3 fluxnum_2: 1 priority: 1 ! linenum: 81.000 targname: HD137613 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.06S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 81.5; req_3: CYCLE 3 / 81-82 comment_1: THE EEXPOSURE TIME comment_2: VALUES WERE CALCULATED comment_3: USING THE V MAGNITUDE comment_4: OF THE CH STAR ! linenum: 81.500 targname: HD137613 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.06S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 82; req_3: CYCLE 3 / 81-82 ! linenum: 82.000 targname: HD137613 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 65M s_to_n: 4 fluxnum_1: 3 fluxnum_2: 1 priority: 1 ! linenum: 91.000 targname: HD89948 config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.07S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 91.5; req_3: CYCLE 3 / 91-92 comment_1: THE EXPOSURE TIME comment_2: VALUES WERE DETERMINED comment_3: USING THE V MAGNITUDE comment_4: OF THE CH STAR ! linenum: 91.500 targname: HD89948 config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.07S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 92; req_3: CYCLE 3 / 91-92 ! linenum: 92.000 targname: HD89948 config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 40M s_to_n: 7 fluxnum_1: 3 fluxnum_2: 1 priority: 1 ! linenum: 101.000 targname: HD40808-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIIAL SCAN; req_2: ONBOARD ACQ FOR 101.5; req_3: CYCLE 3 / 101-102 comment_1: THE EXPOSURE TIME comment_2: VALUES WERE CALCULATED comment_3: USING THE V MAGNITUDE ! linenum: 101.500 targname: HD40808-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 102; req_3: CYCLE 3 / 101-102 ! linenum: 102.000 targname: HD40808-CALIB config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 20M s_to_n: 7 fluxnum_1: 1 priority: 1 req_1: CYCLE 3 / 101-102 comment_1: THE S/N IS CALCULATED comment_2: FOR THE WAVELENGTH OF comment_3: 1500 A ! linenum: 111.000 targname: HD163993-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 111.5; req_3: CYCLE 3 / 111-112 ! linenum: 111.500 targname: HD163993-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.015S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 112; req_3: CYCLE 3 / 111-112 ! linenum: 112.000 targname: HD163993-CALIB config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 15M s_to_n: 7 fluxnum_1: 1 priority: 1 comment_1: THE SIGNAL TO NOISE comment_2: IS CALCULATED FOR comment_3: THE WAVELENGTH OF comment_4: 1500 A ! linenum: 121.000 targname: HD157347-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 4.3 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.02S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 121.5; req_3: CYCLE 3 / 121-122 ! linenum: 121.500 targname: HD157347-CALIB config: FOS/BL opmode: ACQ/PEAK aperture: 1.0 sp_element: G270H wavelength: 2700 num_exp: 1 time_per_exp: 0.02S fluxnum_1: 1 priority: 1 req_1: SPATIAL SCAN; req_2: ONBOARD ACQ FOR 122; req_3: CYCLE 3 / 121-122 ! linenum: 122.000 targname: HD157347-CALIB config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1600 num_exp: 1 time_per_exp: 20M s_to_n: 7 fluxnum_1: 1 priority: 1 ! ! end of exposure logsheet scan_data: line_list: 11,21,31,41,51,61,71,81,91,101,111,121 fgs_scan: cont_dwell: D dwell_pnts: 3 dwell_secs: 1.00 scan_width: 0.0000 scan_length: 2.8000 sides_angle: 90.0000 number_lines: 1 scan_rate: 0.0000 first_line_pa: 0.0000 scan_frame: S/C len_offset: +1.4 wid_offset: 0.0 ! line_list: 11.5,21.5,31.5,41.5,51.5,61.5,71.5,81.5 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: +1.75 wid_offset: 0.35 ! line_list: 91.5,101.5,111.5,121.5 fgs_scan: cont_dwell: D dwell_pnts: 6 dwell_secs: 1.00 scan_width: 0.7000 scan_length: 3.5000 sides_angle: 90.0000 number_lines: 2 scan_rate: 0.0000 first_line_pa: 90.0000 scan_frame: S/C len_offset: +1.75 wid_offset: 0.35 ! ! end of scan data