! File: 2238C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:03:51:38 coverpage: title_1: LYMAN-ALPHA OBSERVATIONS OF HIGH RADIAL VELOCITY STARS sci_cat: STELLAR ASTROPHYSICS proposal_for: GO pi_title: DR. pi_fname: JAY pi_lname: BOOKBINDER pi_inst: CFA pi_country: USA pi_phone: (617) 495-7058 keywords_1: STARS: CHROMOSPHERES; STARS: LYMAN-ALPHA EMISSION, keywords_2: STARS: FLUORESCENCE, ISM: DEUTERIUM ABUNDANCE. hours_pri: 3.00 num_pri: 2 hrs: X funds_amount: 64536 funds_length: 12 funds_date: JAN-91 pi_position: ASTROPHYSICIST off_fname: GEORGE off_mi: D. off_lname: DICK off_title: MANAGER off_inst: SMITHSONIAN off_addr_1: 60 GARDEN ST. off_city: CAMBRIDGE off_state: MA off_zip: 02138 off_country: USA off_phone: (617) 495-7401 off_telex: 921428 SATALLITE CAM ! end of coverpage abstract: line_1: H I LYMAN -ALPHA (LY-A) IS ONE OF THE MOST IMPORTANT LINES EMITTED BY line_2: PLASMA IN THE TEMPERATURE RANGE OF 7000 TO 10 TO THE FIFTH POWER K IN LATE-TYPE line_3: STARS. IT IS A MAJOR COMPONENT OF THE TOTAL RADIATIVE LOSS RATE, AND IT PLAYS line_4: A CRUCIAL ROLE IN DETERMINING THE ATMOSPHERIC STRUCTURE AND IN FLUORESCING line_5: OTHER UV LINES. YET IT IS ALSO THE LEAST STUDIED MAJOR LINE IN THE FAR UV, line_6: BECAUSE MOST OF THE LINE FLUX IS ABSORBED BY THE ISM ALONG THE LINE OF SIGHT line_7: AND BECAUSE IT IS STRONGLY COMTAMINATED BY THE GEOCORONAL BACKGROUND. A line_8: KNOWLEDGE OF THE Ly-A PROFILE IS ALSO IMPORTANT FOR STUDIES OF DEUTERIUM IN line_9: THE INTERSTELLAR MEDIUM. BY OBSERVING HIGH RADIAL VELOCITY STARS WE WILL line_10: OBTAIN FOR THE FIRST TIME HIGH RESOLUTION SPECTRA OF THE CORE OF A STELLAR H I line_11: LYMAN-A EMISSION LINE PROFILE. ! ! end of abstract general_form_proposers: lname: BROWN fname: ALEXANDER title: PROF. inst: COLORADO, UNIVERSITY OF country: USA ! lname: LANDSMAN fname: WAYNE title: PROF. inst: ST SYSTEMS CORPORATION country: USA ! lname: JUDGE fname: PHILLIP title: PROF. mi: D. inst: COLORADO, UNIVERSITY OF country: USA ! lname: LINSKY fname: JEFFREY title: PROF. mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! lname: BOOKBINDER fname: JAY title: P.I. inst: CFA country: USA ! lname: NEFF fname: JAMES title: PROF. mi: E. inst: NASA, GODDARD country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observational goal of this program is twofold: (1) obtain good S/N line_2: spectra of intrinsic Ly-alpha and Mg II line profiles, line_3: and (2) to observe diagnostic lines that will constrain the atmospheric line_4: modeling. line_6: Three spectra line_7: for each target star will be obtained. The first will be a moderate line_8: dispersion (R=20,000) spectrum using G160M (centered at 1213 A) to line_9: obtain the Ly-alpha line. To minimize contamination of the Ly-alpha line_10: line profile by geocoronal emission, we will use line_11: the SSA (0.25") for this exposure. Our second spectrum will line_12: use G270M grating (centered at 2800 A) and the SSA to obtain the line_13: Mg II emission lines. Our final exposure, using G140L (centered at line_14: 1530 A), will cover the range from 1388 A to 1673 A, including line_15: emission lines of Si IV, O IV], C IV, He II, O I, C I, O III],and lines line_16: of neutral elements. These lines act as diagnostics of the temperature line_17: structure within the atmosphere; the intersystem lines O IV] and O III] line_18: provide density constraints. We will use the LSA to maximize the line_19: signal in faint lines. ! question: 5 section: 1 line_1: IUE measurements of low dispersion spectra of two high radial velocity line_2: stars, HD 39364 (delta Lep) and HD 41312 have been obtatined. HD 39364 line_3: has an integrated Ly-alpha flux of 5 x 10(-12) erg/sec/cm**2. Its Mg line_4: II k line flux is 6 x 10(-12) erg/sec/cm**2 with a FWHM of about 1 A. line_5: Its radial velocity relative to the ISM flow velocity (Crutcher 1982) line_6: is +120 km/s, which corresponds (at Ly-alpha ) to 0.4 A. Moreover, this line_7: star is in the third galactic quadrant, where N(H) is intrinsically low, line_8: on the order of 10(18) cm**-3. HD 41312 has an integrated Ly-alpha flux line_9: of 2 x 10(-12) erg/s/cm**2, a radial velocity relative to the LISM of line_10: +200 km/s, and it lies along a line of sight similar to that toward line_11: HD 39364. No Mg II observation exists for this star. ! question: 5 section: 2 line_1: For HD 39364, a GHRS moderate resolution (R = 20,000) exposure time of 8 line_2: minutes has been estimated on the basis of its IUE low-dispersion flux, line_3: an expected FWHM (1.6 A) of the Ly-alpha line, use of the small science line_4: aperture, and the sensitivities quoted for the G160M grating on the GHRS line_5: (neither scattered light nor dark counts are important in this line_6: experiment). This observation will be of sufficient duration to produce line_7: a spectrum with a S/N about 15 at the half-power point, which is line_8: desirable for modeling. line_9: More S/N is not required since the Ly-alpha line of giants is line_10: relatively broad and will therefore cover many pixels. The Mg II lines line_11: for HD 39364 (also R=20,000) can be obtained with a 2 minute exposure line_12: (S/N about 50 near the half-power point), based on the observed IUE line_13: flux and GHRS handbook sensitivities of the G270M grating using the line_14: large science aperture. For HD 41312, with slightly fainter lines, line_15: the estimated GHRS exposure times for the two medium dispersion line_16: gratings are 20 minutes and 5 minutes. Finally, a 15 minute line_17: low-dispersion spectrum from 1388 A to 1673 A will be obtained (using line_18: the LSA), and will provide information on many line_19: emission lines formed over a wide range of temperature down to a line_20: limiting flux (S/N above 3) about 6 x 10(-16) erg/s/cm**(2)/A. line_21: Our sensitivity calculations are based on recent revisions line_22: and we recognize that these values are still uncertain line_23: below 3000 A. ! question: 6 section: 1 line_1: To avoid Lyman alpha contamination by the geocorona, we request line_2: "dark time" for the appropriate exposures (G160M gratings). ! !end of general form text general_form_address: lname: BOOKBINDER fname: JAY title: DR. category: PI inst: SMITHSONIAN ASTROPHYS. OBS. addr_1: 60 GARDEN ST city: CAMBRIDGE state: MA zip: 01238 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: HD41312 descr_1: A,140 pos_1: RA = 06H 01M 14.578S +/- 0.02S, pos_2: DEC = -26D 16' 58.55" +/- 0.22" equinox: 1950.0 pm_or_par: Y pos_epoch_yr: 1950.00 ra_pm_val: 0.003800 ra_pm_unct: 0.000267 dec_pm_val: 0.0910 dec_pm_unct: 0.0040 rv_or_z: V=182.6 fluxnum_1: 1 fluxval_1: V = 5.04 +/- 0.05 fluxnum_2: 2 fluxval_2: B-V = 1.34 +/- 0.01 fluxnum_3: 3 fluxval_3: U-B = 1.44 +/- 0.02 fluxnum_4: 4 fluxval_4: F-LINE(1216) = 1.5 +/- 1 E-12 fluxnum_5: 5 fluxval_5: W-LINE(1216) = 2.5 +/- 0.5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: HD41312 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 25S fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: SEARCH-SIZE=3, param_2: BRIGHT=65535.0, param_3: FAINT=13000.0, param_4: LOCATE=YES req_1: ONBOARD ACQ FOR 1.1; req_2: SEQ 1.0-4.1 NO GAP; req_3: DARK TIME; req_4: CYCLE 1 ! linenum: 1.100 targname: HD41312 config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 46S fluxnum_1: 2 fluxnum_2: 3 priority: 1 req_1: ONBOARD ACQ FOR 2.0-4.1; req_2: DARK TIME; req_3: CYCLE 1 ! linenum: 2.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: ECH-B wavelength: 2802.0 num_exp: 1 time_per_exp: DEF s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT=7 req_1: SEQ 2.0-2.1 NON-INT; req_2: CALIB FOR 2.1; req_3: CYCLE 1 comment_1: WAVE CAL FOR THE MGII LINES ! linenum: 2.100 targname: HD41312 config: HRS opmode: ACCUM aperture: 2.0 sp_element: ECH-B wavelength: 2802.0 num_exp: 4 time_per_exp: 326.4S s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 priority: 1 param_1: STEP-PATT=7 param_2: FP-SPLIT=STD req_1: CYCLE 1 comment_1: THE MGII LINES ! linenum: 3.000 targname: HD41312 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1550.5 num_exp: 8 time_per_exp: 326.4S s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 1 comment_1: THE C IV LINE ! linenum: 3.100 targname: HD41312 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G200M wavelength: 1901.7 num_exp: 8 time_per_exp: 326.4S s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: CYCLE 1 comment_1: THE SI III AND C III LINES ! linenum: 4.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G160M wavelength: 1223.9 num_exp: 1 time_per_exp: DEF s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: STEP-PATT=5 req_1: SEQ 4.0-4.1 NO GAP; req_2: CALIB FOR 4.1; req_3: CYCLE 1 comment_1: WAVE CAL FOR THE LYMAN ALPHA LINE ! linenum: 4.100 targname: HD41312 config: HRS opmode: ACCUM aperture: 0.25 sp_element: G160M wavelength: 1223.9 num_exp: 19 time_per_exp: 326.4S s_to_n: 20 fluxnum_1: 2 fluxnum_2: 3 fluxnum_3: 4 priority: 1 param_1: STEP-PATT=5 param_2: FP-SPLIT=STD req_1: DARK-TIME; req_2: CYCLE 1 comment_1: THE LYMAN ALPHA LINE ! ! end of exposure logsheet ! No scan data records found