! $Id: 5357,v 15.1 1994/07/27 17:02:20 pepsa Exp $ coverpage: title_1: CEPHEID MASSES -CYC4-HIGH sci_cat: COOL STARS sci_subcat: PULSATING STARS proposal_for: GO CONT_ID: 4541 TIME_CRIT: Y longterm: 3 pi_fname: ERIKA pi_mi: HR pi_lname: BOHM-VITENSE pi_inst: 3760 pi_country: USA pi_phone: 206 543 4858 hours_pri: 11.99 num_pri: 7 hrs: Y funds_length: 36 off_fname: DONALD off_mi: W off_lname: ALLEN off_title: DIRECTOR off_inst: 3760 off_addr_1: 3935 UNIVERSITY WAY NE off_addr_2: 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:For 2 decades the "Cepheid mass problem" has persisted: Mass line_2:determinations from standard evolutionary tracks and those from line_3:pulsation theory gave conflicting values. The luminosity of a Cepheid line_4:of given mass depends sensitively on the amount of convective overshoot line_5:above the core of the main sequence progenitor. Hence a good mass line_6:determination for the Cepheid with known luminosity will measure the line_7:amount of convective core overshoot. This knowledge is important for line_8:interpretation of HR diagrams of populous clusters in the LMC and line_9:especially for age determinations. It is also necessary for the line_10:understanding of the mixing processes in stars. line_11:IUE observations have revealed a number of Cepheid binaries with line_12:blue companions, whose orbits have now been determined by groundbased line_13:observations. We propose to measure the orbital radial velocities of 5 line_14:blue Cepheid companions on GHRS spectra for wavelengths shorter than line_15:2000 A. The ratios of the orbital velocities for the binaries provide line_16:the mass ratios for the stars. The effective temperature of the line_17:companion can be determined from its energy distribution. For main line_18:sequence stars this also determines its mass. With GHRS spectra the line_19:orbital velocity ratio and thereby the mass ratio can be determined line_20:with an accuracLy of +/- 10 %. ! ! end of abstract general_form_proposers: lname: BOHM-VITENSE fname: ERIKA mi: HR inst: 3760 country: U.S.A. ! lname: EVANS fname: NANCY mi: R inst: INST. SPACE & TERRESTRIAL SCIENCE, NORTH YORK country: CANADA ! lname: CARPENTER fname: KENNETH mi: G inst: 2856 country: U.S.A. GENERAL_FORM_ADDRESS: ! The PI's address: LNAME: BOHM-VITENSE FNAME: ERIKA MI: HR CATEGORY: PI INST: 3760 ADDR_1: ASTR.DEP. FM-20 ADDR_2: UNIVERSITY OF WASHINGTON CITY: SEATTLE STATE: WA ZIP: 98195 COUNTRY: USA PHONE: 206 543 4858 TELEX:206 685 0403 ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1:The purpose of this proposal is to measure the orbital velocities line_2:of the main sequence companions of 5 classical Cepheids. We would line_3:like to observe each target twice. The observations are spread out line_4:over several observing cycles in order to observe most targets both line_5:at maximum and at minimum orbital velocity. The highest accuracy will line_6:be achieved if the observations can be done close to the middle of line_7:the observing windows given. After the successful repair mission line_8:we plan to use the GHRS with the 0.25" aperture and the Echelle B line_9:at 1722 A for the observations for S Mus B which has the brightest line_10:companion. For the comparison star HD 66591 the same instrument line_11:configuration has to be used. We want to use the G200M grating at line_12:1860 A for the other stars. The star HD 172167 is the line_13:standard star for comparison with the other Cepheid companions. The line_14:G200M grating at 1860 A has to be used for those. These stars line_15:should also be observed twice to be sure that we measure the same line_16:velocity. We will have observed the standard stars once during line_17:cycle 3 and would like to observe them the second time during cycle line_18:5. We would like a wavelength calibration before each stellar line_19:observation. line_20:We need to break up the exposures into subexposures of not more line_21:than 6 minutes duration each in order to avoid geomagnetic smearing line_22:They will then be aligned by cross-correlation and co-added. ! question: 4 section: 1 line_1:We need the UV capabilities and the large collection area of HST. line_2:The Cepheid companions can only be seen in the ultraviolet because line_3:in the optical their light is drowned by the light of the luminous line_4:Cepheid. Because of the temperature difference between the components line_5:,the hotter main sequence companions dominate, however, for line_6:wavelengths shorter than 2000 A. Companion velocities can therefore line_7:be measured only on UV spectra. The companions (except for S Mus B) line_8:are too faint to be observed with IUE at high resolution, needed line_9:for radial velocity measurements. line_10:Orbits for all program stars have been determined from the ground. line_11:In some cases we are working with collaborators to obtain additional line_12:velocity data to improve the orbits. line_13:We have also observed all the program stars in low resolution line_14:with IUE to determine the spectral types and the UV absolute fluxes line_15:for the companions. For S Mus and SU Cyg we have demonstrated that line_16:the cross-correlation technique works well to measure velocity line_17:differences between the Cepheid and the companion. With IUE we have line_18:been able to measure absolute velocities with an accuracy of about line_19:+/-5 km/s. With HST we will be able to measure the companion line_20:orbital velocity directly with much higher acccuracy. line_21:For S Mus we anticipate improvements over IUE results because the line_22:Echelle dispersion should allow us to measure velocities to better line_23:than 1 km/s using fairly strong lines at 1722 A. ! question: 4 section: 2 line_1:We have estimated the exposure times from the fluxes on the IUE line_2:spectra, which are available for all the target stars. Count rates line_3:have been computed by Carpenter based on grating sensitivities and line_4:experience with observations. line_5:A signal to noise ratio of 15 is adequate for a reliable radial line_6:velocity measured by cross-correlation techniques. In addition we line_7:will be able to examine the companion spectra, which have not been line_8:observed at high resolution before. line_9:As discussed above, we plan to observe at least two standard line_10:stars to be used as primary velocity comparisons. To obtain the line_11:necessary wavelength accuracy wavelength calibration exposures line_12:will have to be taken before and after the stellar observations. ! question: 5 section: 1 line_1:In order to achieve the highest possible accuracy for the orbital line_2:velocity ratio, we need to observe the companions at phases near line_3:orbital radial velocity extrema. The orbits are typically a few line_4:years. Specific scheduling requests are detailed below. line_5: SCHEDULING REQUIREMEBTS FOR CYCLE 4 line_6: Y Car Jan.1, 1994 to April 30, 1994 line_7: V350 Sgr Jan.15, 1994 to May 1, 1994 ! corrected line_8: U Aql July 1, 1993 to March 30, 1994 line_9: S Mus July 15,1994 to Sept. 15, 1994 line_10:Generally a window of several months is available, which should line_11:assure that spacekraft constraints will not preclude our orbital line_12:requirements. Highest accuracy will be achieved in the middle of the line_13:windows. We stress that the selected intervals are set by orbital line_14:mechanics. WE THEREFORE ASK THAT THE OBSERVATION OF U AQL BE line_15:SHIFTED TO CYCLE 3 IF DUE TO THE REPAIR MISSION OBSERVATIONS CAN line_16:OTHERWISE NOT BE DONE BEFORE APRIL 1994. (Not enough time was line_17:alotted for Cycle 3 to have these observations scheduled in Cycle 3. line_18: In order to obtain an accuracy in the mass determination of 10% we line_19:require a velocity accuracy of 2 km/sec. In order to obtain this line_20:accuracy, a wavelength calibration is required before and after line_21:each stellar exposure and a breakup of the long exposures into a line_22:series of short exposures to avoid geomagnetic smearing. These line_23:will then be aligned by cross-correlation and co-added. ! question: 6 section: 1 line_1: In order to obtain an accuracy in the mass determination of line_2:+/-10% (which we consider necessary for a significant result), we line_3:require a velocity accuracy of 2 km/sec. This corresponds to a line_4:wavelength accuracy of 0.2 diode or better with the G200M grating. line_5:We believe that this can be obtained because of the results of line_6:Carpenter et al. (May 1991,HST Workshop) on the emission line line_7:spectrum of alpha Tau. In order to obtain this accuracy a wavelength line_8:calibration is required before and after each stellar exposure. line_9:In addition we intend to break the long exposures up into a series line_10:of short exposures to avoid geomagnetic smearing. These will then be line_11:aligned by cross-correlation and co-added. By the combination of the line_12:spectra and the wavelength calibrations the necessary wavelength line_13:accuracy should be possible especially now, when the small aperture line_14:can be used after the repair mission. We need to reobserve the two line_15:standard stars with known and constant radial velocities and with line_16:nearly the same spectral types as the program stars in order to line_17:determine the Cepheid companion velocities by cross-correlating the line_18:companion spectra with the standard star spectra. Because of the line_19:time constraint these observations have to be postponed to cycle line_20:5. The cross-correlation of the spectra of the same standard star line_21:will assure us that we measure the same radial velocities for these line_22:stars. This will be especially important after the repair mission. ! question: 8 section: 1 line_1: If, due to the repair mission, it is unlikely that U Aql can be line_2:observed in Cycle 4 before April 1 1994, we ask that this star be line_3:observed during Cycle 3. This program was accepted during Cycle 3 line_4:with high priority. The alotted time of 5 hours for Cycle 3 was line_5:apparently based on a timely repair mission and did not allow us to line_6:schedule the U Aql observation in Cycle 3. We therefore ask now to line_7:make this observation before the repair mission if otherwise it line_8:cannot be done in the observing window which is determined by the line_9:orbital mechanics of the U Aql system. The next chance for line_10:observations at the same orbital phase will only be 5 years later. line_11:We will lose at least a factor of 2 in accuracy if we can observe line_12:only one extremum of the orbital radial velocity. question: 9 section: 1 line_1: This proposal was accepted for Cycle 3. So far we got observations line_2:for Y Car but not yet observations for the standard stars. I under- line_3:stand that these observations were scheduled for the beginning of line_4:October, but may be moved to a later time. So far we have only line_5:seen that the spectra of Y Car look OK. line_6:As soon as we have the standard star spectra we can measure the line_7:radial velocities and get a preliminary result for the radial line_8:velocity and the mass of this beat Cepheid. If the mass turns out line_9:to be around 4 solar masses this will be a strong argument in favor line_10:of the higher, Livermore opacities. Only for the higher opacities line_11:are the measured period ratios obtained for a 4 solar mass star. line_12: The final, more accurate mass determination will only be line_13:obtained after we get the second set of observations for this line_14:star in spring 1994. line_15:For description of previous work of Ken Carpenter see attached line_16:page ! !end of general form text general_form_address: lname: BOHM-VITENSE fname: ERIKA mi: HR category: PI inst: 3760 addr_1: ASTRONOMY DEPARTMENT FM-20 addr_2: UNIVERSITY OF WASHINGTON city: SEATTLE state: WA zip: 98195 country: U.S.A. phone: (206) 543 4858 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD106111 name_2: HR4645 name_3: S-MUS-B descr_1: A,147,175,178, descr_2: 134,111 pos_1: RA= 12H 12M 47.23S +/-0.5", pos_2: DEC= -70D 09' 6.0" +/-1.0", pos_3: PLATE-ID=05ZX equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1987.00 ra_pm_val: -0.002003 ra_pm_unct: 0.000079 dec_pm_val: -0.0200 dec_pm_unct: 0.0100 an_prlx_val: 0.002 an_prlx_unct: 0.001 rv_or_z: V=11.0 fluxnum_1: 1 fluxval_1: V=8.9+/-1, TYPE=B5V fluxnum_2: 1 fluxval_2: B-V=0.07+/-0.1 fluxnum_3: 2 fluxval_3: E(B-V)=0.24+/-0.04 fluxnum_4: 3 fluxval_4: F-CONT(1722)=3.2+/-0.2E-12 comment_1: WE OBSERVE THE B5V COMPANION comment_2: OF THE F8II CEPHEID S-MUS comment_3: THE CEPHEID MWGNITUDE IS 6.7+/-1 comment_4: FOR THE CEPHEID B-V=0.5+/-0.1 ! targnum: 2 name_1: HD66591-CALIB name_2: HR3159 descr_1: A,111 pos_1: RA= 08H 00M 20.00S +/- 1.0", pos_2: DEC= -63D 34' 03.2" +/- 1.0", pos_3: PLATE-ID=00MQ equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1980.00 ra_pm_val: 0.001003 ra_pm_unct: 0.000030 dec_pm_val: 0.0200 dec_pm_unct: 0.0100 an_prlx_val: 0.0040 an_prlx_unct: 0.0010 rv_or_z: V=22.0 fluxnum_1: 1 fluxval_1: V=4.82+/-0.02, TYPE=B3V fluxnum_2: 1 fluxval_2: B-V=-0.17+/-0.02 fluxnum_3: 2 fluxval_3: E(B-V)=0.0 fluxnum_4: 3 fluxval_4: F-CONT(1722)=5.0E-10 comment_1: THIS IS A VELOCITY CALIBRATION STAR comment_2: FOR THE OBSERVATIONS OF S-MUS ! targnum: 3 name_1: HD91595 name_2: Y-CAR-B descr_1: A,147,175,178,134, descr_2: 112 pos_1: RA= 10H 33M 10.90S +/- 1.0", pos_2: DEC= -58D 29' 55.7" +/- 1.0", pos_3: PLATE-ID=06A6 equinox: 2000 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 1987.00 ra_pm_val: 0.0011 ra_pm_unct: 0.0005 dec_pm_val: 0.00 dec_pm_unct: 0.001 an_prlx_val: 0.001 an_prlx_unct: 0.001 rv_or_z: V=-14.1 fluxnum_1: 1 fluxval_1: V=11.9+/-1 fluxnum_2: 1 fluxval_2: B-V=0.09+/-0.05 fluxnum_3: 2 fluxval_3: E(B-V)=0.08+/-0.05 fluxnum_4: 3 fluxval_4: F-CONT(1860)=1.0E-13 comment_1: WE WANT TO OBSERVE THE B9V comment_2: COMPANION OF THE CEPHEID Y CAR comment_3: THE CEPHEID HAS V=7.5+/-1 ! targnum: 4 name_1: HD172167-CALIB name_2: HR7001 name_3: ALPHA-LYRAE descr_1: A,123 pos_1: RA= 18H 36M 56.3S +/-0.1S, pos_2: DEC= +38D 47' 01" +/-1" equinox: 2000.00 pm_or_par: Y pos_epoch_bj: J pos_epoch_yr: 2000.00 ra_pm_val: 0.017096 ra_pm_unct: 0.000599 dec_pm_val: 0.2900 dec_pm_unct: 0.0300 an_prlx_val: 0.1200 an_prlx_unct: 0.0100 rv_or_z: V=-14.0 fluxnum_1: 1 fluxval_1: V=0.02+/-0.02, TYPE=A0V fluxnum_2: 1 fluxval_2: B-V=0.01 fluxnum_3: 2 fluxval_3: E(B-V)=0.0 fluxnum_4: 3 fluxval_4: F-CONT(1860)=5.5E-9 comment_1: THIS IS A CALIBRATION STAR comment_2: TO MEASURE THE RADIAL comment_3: VELOCITY OF Y-CAR-B ! TARGNUM: 5 NAME_1: HD183344 NAME_2: HR7402 NAME_3: U-Aql-B DESCR_1: A,147,175,134, DESCR_2: 123 POS_1: RA= 19H 29M 21.37S +/-1.0", POS_2: DEC= -07D 02' 37.7" +/-1.0", POS_3: PLATE-ID=03UO EQUINOX: 2000 PM_OR_PAR: Y POS_EPOCH_BJ: J POS_EPOCH_YR: 1982 RA_PM_VAL: +0.0014 RA_PM_UNCT: 0.0005 DEC_PM_VAL: 0.003 DEC_PM_UNCT: 0.001 AN_PRLX_VAL: 0.001 AN_PRLX_UNCT: 0.0005 RV_OR_Z: V=-6.0 FLUXNUM_1: 1 FLUXVAL_1: V=10.8+/-1 FLUXNUM_2: 1 FLUXVAL_2: B-V=0.34+/-0.05 FLUXNUM_3: 2 FLUXVAL_3: E(B-V)=0.35 FLUXNUM_4: 3 FLUXVAL_4: F-CONT(1860)=5.5E-14 COMMENT_1: WE WANT TO OBSERVE THE A1V COMMENT_2: COMPANION OF THE CEPHEID COMMENT_3: U AQL. THE CEPHEID HAS COMMENT_4: V=6.5+/-1 ! TARGNUM: 6 NAME_1: HD173297 NAME_2: V350-SGR-B NAME_3: DESCR_1: A,147,175,178, DESCR_2: 134,112 POS_1: RA= 18H 45M 17.53S +/- 1.0", POS_2: DEC= -20D 38' 50.6" +/- 1.0", POS_3: PLATE-ID=060A EQUINOX: 2000 PM_OR_PAR: Y POS_EPOCH_BJ: J POS_EPOCH_YR: 1987 RA_PM_VAL: 0.0061 RA_PM_UNCT: 0.002 DEC_PM_VAL: -0.012 DEC_PM_UNCT: 0.0 AN_PRLX_VAL: 0.001 AN_PRLX_UNCT: 0.0005 RV_OR_Z: V=0.0 FLUXNUM_1: 1 FLUXVAL_1: V=11.5+/-1 FLUXNUM_2: 1 FLUXVAL_2: B-V=-0.05+/-0.05 FLUXNUM_3: 2 FLUXVAL_3: E(B-V)=0.30+/-0.1 FLUXNUM_4: 3 FLUXVAL_4: F-CONT(1860)=5.0E-14 COMMENT_1: WE WANT TO OBSERVE THE COMMENT_2: B9V COMPANION OF THE CEPHEID COMMENT_3: V350 SGR,WHICH HAS V=8.0. ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD106111 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=3 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 2.000; req_2: SEQ 1 - 5 NO GAP; !corrected req_3: CYCLE 4/1.-65.5; req_4: AT 15-AUG-94+/-30D comment_1: USE STEP-TIME = 0.2 SEC. comment_2: EXPECT ROUGHLY 50000.CTS/0.2S COMMENT_3: THIS STAR IS SCHEDULED TO BE COMMENT_4: OBSERVED ALSO IN OCT 93 ! linenum: 2.000 targname: HD106111 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 param_1: SEARCH-SIZE=5 num_exp: 1 time_per_exp: 10.0S fluxnum_1: 1 priority: 1 req_1: SEQ 2-5 NON-INT; ! REINSTATED comment_1: STEP-TIME = 0.2 SEC ! linenum: 3.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1722.0 param_1: STEP-PATT=3 num_exp: 1 time_per_exp: 30.0S priority: 1 req_1: CALIB FOR 4 NO SLEW; ! linenum: 4.000 targname: HD106111 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B wavelength: 1722.0 param_1: STEP-PATT=7, param_2: FP-SPLIT=NO num_exp: 6 time_per_exp: 5.0M s_to_n: 15 fluxnum_1: 2 priority: 1 comment_1: S/N IS FOR SUM OF 5 EXP'S. linenum: 5.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 1722.0 param_1: STEP-PATT=3 num_exp: 1 time_per_exp: 30.0S priority: 1 req_1: CALIB FOR 4 NO SLEW ! linenum: 11.000 targname: HD91595 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=3 num_exp: 1 time_per_exp: 1.8S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 12.000; req_2: SEQ 11.0-15.8 NO GAP; ! corrected req_3: AT 1-MAR-94+/-50D comment_1: USE STEP-TIME = 200 MSEC. comment_2: EXPECT ROUGHLY 2938 CTS/200MS COMMENT_3: THIS STAR HAS BEEN OBSERVED PREVIOUSLY ! linenum: 12.000 targname: HD91595 config: HRS opmode: ACQ/PEAKUP aperture: 0.25 sp_element: MIRROR-N2 param_1: SEARCH-SIZE=5 num_exp: 1 time_per_exp: 10.0S fluxnum_1: 1 priority: 1 req_1: SEQ 12-15 NON-INT; ! REINSTATED comment_1: STEP-TIME = 200 MSEC ! linenum: 13.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1860.0 param_1: STEP-PATT=3 num_exp: 1 time_per_exp: 30.0S priority: 1 req_1: CALIB FOR 14 NO SLEW; ! linenum: 14.000 targname: HD91595 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G200M wavelength: 1860.0 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO num_exp: 5 time_per_exp: 5.0M s_to_n: 15 fluxnum_1: 2 priority: 1 comment_1: S/N IS FOR SUM OF 5 EXP'S. linenum: 15.00 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1860.0 param_1: STEP-PATT=3 num_exp: 1 time_per_exp: 30.0S priority: 1 req_1: CALIB FOR 14 NO SLEW; ! linenum: 15.500 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1860.0 param_1: STEP-PATT=3 num_exp: 1 time_per_exp: 30.0S priority: 1 req_1: CALIB FOR 15.6 NO SLEW; req_2: SEQ 15.5-15.8 NON-INT; ! reinstated ! linenum: 15.600 targname: HD91595 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G200M wavelength: 1860.0 param_1: STEP-PATT=5, param_2: FP-SPLIT=NO num_exp: 5 time_per_exp: 5.0M s_to_n: 15 fluxnum_1: 2 priority: 1 comment_1: S/N IS FOR SUM OF 5 EXP'S. linenum: 15.80 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1860.0 param_1: STEP-PATT=3 num_exp: 1 time_per_exp: 30.0S priority: 1 req_1: CALIB FOR 15.6 NO SLEW ! LINENUM: 50.000 TARGNAME: HD183344 CONFIG: HRS OPMODE: ACQ APERTURE: 2.0 SP_ELEMENT: MIRROR-N2 param_1: LOCATE=YES, param_2: BRIGHT=RETURN, param_3: SEARCH-SIZE=3 NUM_EXP: 1 TIME_PER_EXP: 1.8S FLUXNUM_1: 1 PRIORITY: 1 REQ_1: ONBOARD ACQ FOR 52-55.2; REQ_2: SEQ 50-55.2 NO GAP; ! corrected REQ_3: AT 11-DEC-93+/-120D ! corrected COMMENT_1: USE STEP-TIME = 0.20 SEC. COMMENT_2: EXPECT ROUGHLY 50000.CTS/0.2S LINENUM: 51.000 TARGNAME: HD183344 CONFIG: HRS OPMODE: ACQ/PEAKUP APERTURE: 0.25 SP_ELEMENT: MIRROR-N2 param_1: SEARCH-SIZE=5 NUM_EXP: 1 TIME_PER_EXP: 10.0S FLUXNUM_1: 1 PRIORITY: 1 REQ_1: ONBOARD ACQ FOR 52.000-55.200; REQ_2: SEQ 52.00-53.20 NON-INT; ! reinstated COMMENT_1: STEP-TIME = 200 MSEC LINENUM: 52.000 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 53.0 NO SLEW LINENUM: 53.0 TARGNAME: HD183344 CONFIG: HRS OPMODE: ACCUM APERTURE: 0.25 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=5, PARAM_2: FP-SPLIT=STD NUM_EXP: 2 TIME_PER_EXP: 15.5M S_TO_N: 15 FLUXNUM_1: 2 PRIORITY: 1 COMMENT_1: S/N IS FOR SUM OF 4 EXP'S LINENUM: 53.200 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 53.0 NO SLEW; LINENUM: 54.800 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 55.000 NO SLEW; REQ_2: SEQ 54.8-55.2 NON-INT ! reinstated LINENUM: 55.000 TARGNAME: HD183344 CONFIG: HRS OPMODE: ACCUM APERTURE: 0.25 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=5, PARAM_2: FP-SPLIT=STD NUM_EXP: 2 TIME_PER_EXP: 15.5M S_TO_N: 15 FLUXNUM_1: 2 PRIORITY: 1 COMMENT_1: S/N IS FOR SUM OF 4 EXP'S. LINENUM: 55.20 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 55.0 NO SLEW linenum: 60.000 TARGNAME: HD173297 CONFIG: HRS OPMODE: ACQ APERTURE: 2.0 SP_ELEMENT: MIRROR-N2 PARAM_1: LOCATE=YES, PARAM_2: BRIGHT=RETURN, PARAM_3: SEARCH-SIZE=3 NUM_EXP: 1 TIME_PER_EXP: 1.8S FLUXNUM_1: 1 PRIORITY: 1 REQ_1: ONBOARD ACQ FOR 63.000; REQ_2: SEQ 60.0-65.5 NO GAP; ! CORRECTED REQ_3: AT 1-MAR-94+/-60D LINENUM: 61.000 TARGNAME: HD173297 CONFIG: HRS OPMODE: ACQ/PEAKUP APERTURE: 0.25 SP_ELEMENT: MIRROR-N2 PARAM_1: SEARCH-SIZE=5 NUM_EXP: 1 TIME_PER_EXP: 10.0S FLUXNUM_1: 1 PRIORITY: 1 REQ_1: ONBOARD ACQ FOR 62.0-64.0; REQ_2: SEQ 62.0-64.0 NON-INT; ! reinstated COMMENT_1: STEP-TIME = 200 MSEC LINENUM: 62.000 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 63.0 NO SLEW; LINENUM: 63.000 TARGNAME: HD173297 CONFIG: HRS OPMODE: ACCUM APERTURE: 0.25 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=5, PARAM_2: FP-SPLIT=STD NUM_EXP: 2 TIME_PER_EXP: 15.5M S_TO_N: 15 FLUXNUM_1: 2 PRIORITY: 1 COMMENT_1: S/N IS FOR SUM OF 4 EXP'S ! LINENUM: 64.00 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 63.0 NO SLEW; ! LINENUM: 64.800 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 65.000 NO SLEW; REQ_2: SEQ 64.8-65.5 NON-INT ! reinstated LINENUM: 65.000 TARGNAME: HD173297 CONFIG: HRS OPMODE: ACCUM APERTURE: 0.25 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=5, PARAM_2: FP-SPLIT=STD NUM_EXP: 2 TIME_PER_EXP: 15.5M S_TO_N: 15 FLUXNUM_1: 2 PRIORITY: 1 COMMENT_1: S/N IS FOR SUM OF 4 EXP'S LINENUM: 65.50 TARGNAME: WAVE CONFIG: HRS OPMODE: ACCUM APERTURE: SC2 SP_ELEMENT: G200M WAVELENGTH: 1860.0 PARAM_1: STEP-PATT=3 NUM_EXP: 1 TIME_PER_EXP: 30.0S PRIORITY: 1 REQ_1: CALIB FOR 65.00 NO SLEW ! ! end of exposure logsheet ! No scan data records found