! File: 4182C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:12:23:36 coverpage: title_1: DYNAMICS AND ENERGY BALANCE IN STELLAR TRANSITION REGIONS title_2: CYCLE 3 AUGMENTATION sci_cat: STELLAR ASTROPHYSICS sci_subcat: COOL STARS proposal_for: AUG/HRS cont_id: 1176 pi_fname: JEFFREY pi_mi: L. pi_lname: LINSKY pi_inst: COLORADO, UNIVERSITY OF pi_country: USA pi_phone: (303)492-7838 keywords_1: HYDROGEN COLUMN DENSITY, DEUTERIUM COLUMN DENSITY, keywords_2: DEUTERIUM ABUNDANCE hours_pri: 6.61 num_pri: 1 time_crit: X pi_position: ASTROPHYSICST ! end of coverpage abstract: line_1: We will observe with 20,000 spectral resolution the stellar line_2: Lyman alpha emission line and interstellar hydrogen and line_3: deuterium absorption towards local late-type stars to line_4: derive the H and D column densities and D/H ratios along line_5: different lines of sight. High resolution (90,000) spectra of the line_6: MgII and FeII lines will help determine the interstellar line_7: line broadening and whether material along each line of line_8: sight has more than one velocity component. This is critical line_9: for accurate measurements of D/H, because both the D and H line_10: lines are on or near the flat part of the curve of growth. line_11: Previous IUE and Copernicus observations, which had low line_12: signal/noise and inadequate spectral resolution, provided line_13: very crude D/H values and suggested that the D/H ratio may line_14: vary within a few parsecs of the Sun. We will measure D/H line_15: with at least one order of magnitude improved precision and line_16: determine whether the proposed local variations are real. The line_17: local value(s) of D/H may be extrapolated to zero metal line_18: abundance to estimate the primordial value, which is line_19: valuable for constraining cosmological models. ! ! end of abstract general_form_proposers: lname: JURA fname: MICHAEL inst: UC, LOS ANGELES country: USA ! lname: SAVAGE fname: BLAIR mi: D. inst: WISCONSIN, UNIVERSITY OF country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! lname: HEAP fname: SARA mi: R. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! lname: LANDSMAN fname: WAYNE inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! lname: SMITH fname: ANDREW mi: M. inst: NASA, GODDARD SPACE FLIGHT CENTER country: USA ! lname: BROWN fname: ALEXANDER inst: COLORADO, UNIVERSITY OF country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We intend to observe 5 stars at 1.0E+5 resolution with the HRS in 3 line_2: grating settings. Two stars (Capella and HR 1099) are spectroscopic line_3: binary systems that will be observed at orbital quadrature in line_4: order to shift the interstellar absorption feature relative to line_5: the stellar emission line. For most observations a signal-to-noise of 100 is line_6: desired. This requirement requires special care for the Lyman alpha line_7: observations because of fixed pattern noise in the D1 detector. Our solution to line_8: this problem involves (1) placing the Lyman alpha feature on the right hand line_9: half of the digicon (diodes 300-500) where the fixed pattern noise is lower, line_10: and (2) obtaining many individual spectra with small shifts of the grating so line_11: that the spectrum will be placed on different portions of the digicon. line_12: Acceptable observing windows for each star are listed on the target sheet. line_13: Capella was observed in Cycle 0. ! question: 4 section: 1 line_1: The required spectral lines cannot be observed from the ground. ! question: 5 section: 1 line_1: Two targets (Capella and HR 1099) are spectroscopic binaries and must be line_2: observed each near one conjunction (PHI=0.0 or 0.5) and one quadrature line_3: (PHI=0.75 for HR 1099 and PHI=0.25 for Capella). Ephemeris for HR1099 is line_4: PHI=0.00 at JD (helio) = 2,442,766.069 + 2d.83782E. Ephemeris for Capella is line_5: PHI=0.00 at JD (helio) = 2,442,039.4 + 104d.0204E. Also there are preferred line_6: times of the year for each target so as to center the geocoronal emission in line_7: the Lyman alpha interstellar absorption core. These observing windows line_8: are given on the Target List. ! question: 7 section: 1 line_1: We have developed data analysis software to separate the interstellar line_2: absorption and stellar emission line features so as to determine column line_3: densities for interstellar H and D. ! question: 8 section: 1 line_1: Several stars are targets for our other GTO programs. In these cases contiguous line_2: observing of the same star for all programs will mean only one acquisition per line_3: target with a saving of HST observing time. ! question: 10 section: 1 line_1: Data analysis programs and postdoctoral research associates supported by the line_2: HRS GTO program. ! question: 12 section: 1 line_1: The total observing time includes overhead of 435 seconds for each use of the line_2: LISM sequence. ! question: 13 section: 1 line_1: We will observe the Lyman alpha line at 90,000 spectral resolution towards 7 line_2: late-type local stars. The purpose is to derive the hydrogen and deuterium line_3: column densities and D/H ratios along lines of sight towards nearby stars. High line_4: resolution spectra of MgII and FeII lines will be obtained to help determine line_5: the broadening parameter and whether material along these lines of sight has line_6: more than one velocity component. ! !end of general form text general_form_address: lname: LINSKY fname: JEFFREY mi: L. category: PI inst: JILA, UNIVERSITY OF COLORADO addr_1: CAMPUS BOX 440 city: BOULDER state: CO zip: 80309 country: USA phone: (303) 492-7838 telex: 755842 JILA ! ! end of general_form_address records fixed_targets: targnum: 5 name_1: HD22468 name_2: HR1099 descr_1: KO IV+G5 V BINARY SYSTEM pos_1: RA=03H34M13.169S+/-0.01S, pos_2: DEC=+00D25'33.17"+/-0.1" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: -0.002000 ra_pm_unct: 0.000067 dec_pm_val: -0.1610 dec_pm_unct: 0.0010 an_prlx_val: 0.0320 rv_or_z: V=-23 fluxnum_1: 1 fluxval_1: V=5.71 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: LISM1 targname: # config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1223.70 num_exp: # time_per_exp: 108.8S s_to_n: 100 priority: # param_1: STEP-PATT=5, param_2: FP-SPLIT=STD ! linenum: 5.000 sequence_1: DEFINE sequence_2: LISM2 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ECH-B20 wavelength: 2800 num_exp: ^ time_per_exp: 54.4S s_to_n: ^ priority: ^ param_1: STEP-PATT=7 ! linenum: 6.000 sequence_1: DEFINE sequence_2: LISM3 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ECH-B22 wavelength: 2600 num_exp: ^ time_per_exp: 54.4S s_to_n: ^ priority: ^ param_1: STEP-PATT=7 ! linenum: 33.000 targname: HD22468 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 1.8S priority: 2 param_1: SEARCH-SIZE=3, param_2: BRIGHT=RETURN req_1: ONBOARD ACQ FOR 34; req_2: ZERO-PHASE JD2446795.5 +/- 0.001D; req_3: PERIOD 365.25D +/- 0.01D; req_4: PHASE 0.62 +/- 0.23; req_5: CYCLE 3/33-55; req_6: GROUP 33-55 NO GAP comment_1: STEP TIME = 200 MSEC comment_2: FAINT=900 ! linenum: 34.000 targname: HD22468 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 163.2S fluxnum_1: 1 priority: 2 req_1: ONBOARD ACQ FOR 35.0-55.0 comment_1: STEP-TIME=1.6 SEC comment_2: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 35.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G200M wavelength: 1900 num_exp: 1 time_per_exp: 32S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 36 NO SLEW; req_2: SEQ 35-36 NO GAP ! linenum: 36.000 targname: HD22468 config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 2 time_per_exp: 245S priority: ^ param_1: STEP-PATT=5 ! linenum: 36.400 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1402 num_exp: 1 time_per_exp: 59.2S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 36.5 NO SLEW; req_2: SEQ 36.4-36.5 NO GAP ! linenum: 36.500 targname: HD22468 config: ^ opmode: ^ aperture: 2.0 sp_element: G160M wavelength: 1402 num_exp: 4 time_per_exp: 300S priority: ^ param_1: STEP-PATT=5 ! linenum: 50.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1223.70 num_exp: 1 time_per_exp: 64S priority: 2 param_1: STEP-PATT=3 req_1: CALIB FOR 51 NO SLEW; req_2: SEQ 50-51 NO GAP comment_1: NO CARROUSEL MOTION BETWEEN 50 AND 51 ! linenum: 51.000 sequence_1: USE sequence_2: LISM1 targname: HD22468 num_exp: 4 time_per_exp: X9 priority: ^ req_1: ZERO-PHASE JD 2442766.069 +/- .001D; req_2: PERIOD 2.83782D +/- .00001D; req_3: PHASE 0.75 +/- 0.02 comment_1: THIS TARGET MUST BE OBSERVED comment_2: BETWEEN 19 MAY AND 8 NOV. ! linenum: 52.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B20 wavelength: 2800 num_exp: 1 time_per_exp: 32S priority: ^ param_1: STEP-PATT=3 req_1: CALIB FOR 53 NO SLEW; req_2: SEQ 52-53 NO GAP ! linenum: 53.000 sequence_1: USE sequence_2: LISM2 targname: HD22468 num_exp: 1 time_per_exp: X26 priority: 2 req_1: PHASE 0.75 +/- 0.02 OF REF 51 comment_1: THIS TARGET MUST BE OBSERVED comment_2: BETWEEN 19 MAY AND 8 NOV. ! linenum: 54.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B22 wavelength: 2600 num_exp: ^ time_per_exp: 32S priority: ^ param_1: STEP-PATT=3 req_1: CALIB FOR 55 NO SLEW; req_2: SEQ 54-55 NO GAP ! linenum: 55.000 sequence_1: USE sequence_2: LISM3 targname: HD22468 num_exp: 1 time_per_exp: X18 priority: 2 req_1: PHASE 0.75 +/- 0.02 OF REF 51 comment_1: THIS TARGET MUST BE OBSERVED comment_2: BETWEEN 19 MAY AND 8 NOV. ! ! end of exposure logsheet ! No scan data records found