! File: 1195C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:05:31:11 coverpage: title_1: WINDS OF COOL LUMINOUS STARS: DENSITIES, TEMPERATURES, GEOMETRIC title_2: EXTENTS, AND VELOCITY STRUCTURES -- CYCLE 0 sci_cat: STELLAR ASTROPHYSICS sci_subcat: COOL STARS proposal_for: GTO/HRS pi_fname: KENNETH pi_mi: G. pi_lname: CARPENTER pi_inst: NASA - GODDARD SPACE FLIGHT CENTER pi_country: USA pi_phone: (301)-286-3453 keywords_1: COOL STARS: WINDS, CHROMOSPHERES, MASS-LOSS. hours_pri: 7.00 num_pri: 6 hrs: X realtime: Y pi_position: ASTROPHYSICIST ! end of coverpage abstract: line_1: The goals of this program are to determine the physical characteristics of the line_2: winds/chromospheres around cool luminous stars. GHRS observations of the line_3: C II (UV 1) 1335 A and (UV 0.01) 2325 A multiplets will be used along with line_4: observations of the C I lines near 1655 and 1994 A to constrain the temperatures line_5: and densities in model chromospheres. The C II (UV 0.01) lines will also be line_6: used to estimate the turbulence in these chromospheres. The (confusing) far UV line_7: spectrum of the M supergiants will be explored with the GHRS. line_8: GHRS echelle observations of a set of Fe II lines in the 2700 - 2800 A line_9: region will be used to study the dependence of the wind velocity on radial line_10: distance above the photosphere. High quality Mg II profiles will be line_11: acquired to search for discrete velocity features and the presence of line_12: circumstellar absorption within the profiles. line_13: The photospheric absorption-line spectrum (2579-2675 A) of Arcturus will be line_14: observed in the echelle mode. Medium resolution observations of Fe II and line_15: Mg II in the dusty, very luminous star Mu Cep will provide information on the line_16: effect of dust and very low gravity on the wind velocity field. ! ! end of abstract general_form_proposers: lname: CARPENTER fname: KENNETH mi: G. inst: NASA - GODDARD SPACE FLIGHT CENTER country: USA ! lname: LINSKY fname: JEFFREY mi: L. inst: COLORADO, UNIVERSITY OF country: USA ! lname: ROBINSON fname: RICHARD mi: D. inst: CSC - ASTRONOMY PROGRAM country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Target: AlphaOri AlphaSco A GammaCru AlphaTau AlphaBoo LambdaVel line_2: Grating Wavel. exposure time (min) line_3: G140L 1314 17.7min 7.8 9.1 10.9 5.9 12.7 line_4: G140L 1550 17.7 7.25 5.9 - - - line_5: G140L 1800 17.7 7.25 5.9 - - - line_6: G200M 1655 23.6 5.0 5.0 5.0 0.9 - line_7: G200M 1994 4.6 7.8 7.25 9.1 7.8 10.0 line_8: ECH-B 2327 12.7 8.7 13.6 15.0 11.4 6.4 line_9: ECH-B 2759# - 8.7 - 8.7 - 5.5 line_10: ECH-B 2770# - 8.7 - 8.7 - 5.5 line_11: ECH-B 2596# 3.20 - 7.8 - - - line_12: ECH-B 2736# 3.20 - 3.2 - - - line_13: ECH-B 2759# 3.20 - 4.55 - - - line_14: ECH-B 2772# 3.20 - 4.55 - - - line_15: ECH-B 2799# 5.5 1.4 1.4 1.4 0.45 2.27 line_16: Cycle: 0 1 2 1 3 1 3 line_17: Priority: 1 1 2 2 3 2 3 line_18: # = to be accompanied by wavelength calibration exposures line_19: Cycle 0 Alpha Ori obs. adjusted for spherical aberration. line_20: Cycle 1 and later obs. not adjusted for any target yet. ! question: 3 section: 2 line_1: line_2: In addition, a G270M WSCAN of the 2012 - 2200 A region in line_3: Gamma Cru will be obtained and an echelle-B WSCAN of the line_4: 2579 - 2675 A region of Arcturus. line_5: Mu Cep will be observed with G270M at 2609, 2753, and 2802 A in line_6: Cycle 2. ! question: 4 section: 1 line_1: The data required for this program consists of UV spectra not obtainable from line_2: the ground. IUE has been used for a preliminary reconnaissance of all these line_3: targets, except for AlphaSco A (which has a hot companion that cannot be line_4: excluded from the larger IUE apertures). We now require the higher sensitivity, line_5: wavelength resolution, and S/N attainable with the HRS and ST to improve and line_6: extend our studies of the physical conditions characterising the outer line_7: atmospheres of these cool luminous stars. Only HRS is capable of providing us line_8: with the very high precision line profiles, fluxes, and absolute velocities line_9: required for our program. ! question: 5 section: 1 line_1: line_8: An interactive acquisition of HD148478 is required after the line_9: blind offset from HD148478-offset to ensure that the former line_10: target (i.e. the M-supergiant) will be properly located line_11: in the Small Science Aperture despite the presence of the line_12: nearby main-sequence B-star (HD148478-offset) and its line_13: scattered light and the uncertain orbital elements of the line_14: system. ! question: 6 section: 1 line_1: Wavelength calibration exposures for all the echelle observations are needed to line_2: provide us with a velocity scale accurate to about 1 km/sec. This accuracy is line_3: required to allow us to study the dependence of the wind flow velocities on line_4: distance above the photosphere of each star. ! question: 7 section: 1 line_1: The data will be reduced and analyzed primarily with in-house software line_2: developed for analysis of IUE data and with new software to be developed line_3: in-house. Software developed by the GHRS IDT and the proposers will be line_4: used in the reduction and analysis of these observations. The NLTE line_5: MULTI code will be used to construct model chromospheres and spectra which line_6: will be compared with the observations. line_7: References documenting the methods of analysis to be used in this investigation line_8: are given in the Scientific Justification section of this proposal. ! question: 10 section: 1 line_1: See section 7. ! question: 12 section: 1 line_1: The targets observed in this program are: line_3: 1. Alpha Ori line_4: 2. Alpha Sco A line_5: 3. Gamma Cru line_6: 4. Alpha Tau line_7: 5. Alpha Boo line_8: 6. Lambda Vel line_9: 7. Mu Cep ! question: 13 section: 1 line_1: We plan UV spectroscopic observations with GHRS of a sample of 7 cool luminous line_2: stars. Our goals are to determine, from analysis of chromospheric emission line_3: lines, the physical conditions in their wind regions/chromospheres and to study line_4: the dependence of wind velocity on radial distance above the photosphere. The line_5: UV photospheric absorption line spectrum of Arcturus will also be studied at line_6: very high resolution. ! !end of general form text general_form_address: lname: CARPENTER fname: KENNETH mi: G. category: PI inst: NASA-GODDARD SPACE FLIGHT CENTER addr_1: CODE 681 city: GREENBELT state: MD zip: 20771 country: USA phone: 301-286-3453 ! lname: ROBINSON fname: RICHARD mi: D. inst: CSC @ NASA-GODDARD SPACE FLIGHT CENTER addr_1: CODE 681 city: GREENBELT state: MD zip: 20771 country: USA phone: (301)-286-4530 ! lname: LINSKY fname: JEFFREY mi: L. inst: JILA - UNIVERSITY OF COLORADO addr_1: CAMPUS BOX 440 city: BOULDER state: CO zip: 80309 country: USA phone: (303)-492-7838 ! ! end of general_form_address records fixed_targets: targnum: 2 name_1: HD39801 name_2: ALPHA-ORI descr_1: M2 IAB pos_1: RA=05H52M27.809S+/-0.1", pos_2: DEC=07D23'57.92"+/-0.1" equinox: 1950 pm_or_par: Y pos_epoch_bj: B pos_epoch_yr: 1950.00 ra_pm_val: 0.001667 ra_pm_unct: 0.000067 dec_pm_val: 0.0100 dec_pm_unct: 0.0010 rv_or_z: V=+21 comment_1: FLUXVAL 2-6 ARE FOR BASE OF LINES comment_2: FLUXVAL 9 IS FOR MIDDLE OF VIOLET comment_3: PEAK OF K-LINE fluxnum_1: 1 fluxval_1: V=0.8+/-.5,TYPE=M2 IAB fluxnum_2: 2 fluxval_2: F(1314)=3.E-14 fluxnum_3: 3 fluxval_3: F(1550)=5.0E-14 fluxnum_4: 4 fluxval_4: F(1800)=1.3E-13 fluxnum_5: 5 fluxval_5: F(1655)=1.5E-13 fluxnum_6: 6 fluxval_6: F(1994)=5.0E-13 fluxnum_7: 7 fluxval_7: F(2327)=1.E-11 fluxnum_8: 8 fluxval_8: F(2740)=8.E-12 fluxnum_9: 9 fluxval_9: F(2799)=2.5E-11 fluxnum_10: 10 fluxval_10: F(2600)=2.0E-12 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 23.000 targname: HD39801 config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 115.6S fluxnum_1: 1 priority: 1 param_1: FAINT=80, param_2: MAP=END-POINT, param_3: SEARCH-SIZE=5, param_4: LOCATE=YES req_1: CYCLE 0 / 23.0-28.3; req_2: ONBOARD ACQ FOR 23.25; req_3: SEQ 23.0-28.3 NO GAP comment_1: EXPECT 200 CTS/400 MSEC WITH SA comment_2: STEP-TIME=0.4 ! linenum: 23.250 targname: ^ config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 73.6S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 23.50-28.030 comment_1: CENTER IN LSA AFTER NEW DEFCAL comment_2: STEP-TIME=1.6SEC ! linenum: 23.500 targname: ^ config: HRS opmode: IMAGE aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 96.8S fluxnum_1: 1 priority: 1 comment_1: TAKE MAP AFTER CENTERING comment_2: 200 MSEC INTEGRATIONS ! linenum: 24.000 targname: ^ config: ^ opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1314 num_exp: 3 time_per_exp: 5.9M s_to_n: 20 fluxnum_1: 2 priority: ^ param_1: STEP-PATT=5, param_2: METER=YES,HIGH-COUNT=120000, param_3: METER-WAVE=1305 comment_1: FOR MODES G140L, G160M, G200M (LINES comment_2: 24-28.0), SPYBAL SHOULD BE COMPUTED AS comment_3: NECESSARY (PER STANDARD OPERATIONS) comment_4: ON STSCI-INSERTED WAVE OBSERVATIONS. comment_5: TARGET IS TOO FAINT FOR DIRECT comment_6: SPYBALS. S/N IS FOR SUM OF 3 OBS. ! linenum: 25.000 targname: HD39801 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1550 num_exp: 3 time_per_exp: 5.9M s_to_n: 20 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=5, param_2: METER=YES,HIGH-COUNT=120000, param_3: METER-WAVE=1540 comment_1: S/N IS FOR SUM OF 3 OBS. ! linenum: 26.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: ^ wavelength: 1800 num_exp: 3 time_per_exp: 5.9M s_to_n: 20 fluxnum_1: 4 priority: ^ param_1: STEP-PATT=5, param_2: METER=YES,HIGH-COUNT=120000, param_3: METER-WAVE=1820 comment_1: S/N IS FOR SUM OF 3 OBS. ! linenum: 27.000 targname: HD39801 config: HRS opmode: ACCUM aperture: 2.0 sp_element: G160M wavelength: 1655 num_exp: 4 time_per_exp: 5.9M s_to_n: 10 fluxnum_1: 5 priority: 1 param_1: STEP-PATT=5, param_2: METER=YES,HIGH-COUNT=120000, param_3: METER-WAVE=DEF comment_1: S/N IS FOR SUM OF 4 OBS. ! linenum: 28.000 targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: G200M wavelength: 1994 num_exp: 1 time_per_exp: 4.6M s_to_n: 10 fluxnum_1: 6 priority: ^ param_1: STEP-PATT=5, param_2: METER=YES,HIGH-COUNT=120000, param_3: METER-WAVE=DEF ! linenum: 28.030 targname: ^ config: HRS opmode: ACQ/PEAKUP aperture: 2.0 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 73.6S fluxnum_1: 1 priority: 1 req_1: ONBOARD ACQ FOR 28.1-28.3 comment_1: CENTER IN LSA AFTER NEW DEFCAL ! linenum: 28.100 targname: HD39801 config: HRS opmode: IMAGE aperture: 0.25 sp_element: MIRROR-A2 num_exp: 1 time_per_exp: 80.0S fluxnum_1: 1 priority: 1 param_1: NX=9,NY=9 comment_1: STEP-TIME=1.6 SEC, comment_2: USE ONLY IF SSA PEAKUP VALIDATED, comment_3: OTHERWISE REPLACE WITH SSA MAP comment_4: AND USE BLIND OFFSET TO SSA. ! linenum: 28.200 targname: HD39801 config: HRS opmode: ACCUM aperture: 0.25 sp_element: ECH-B20 wavelength: 2799.0 num_exp: 1 time_per_exp: 656.0S s_to_n: 55 fluxnum_1: 9 priority: 1 param_1: STEP-PATT=7, param_2: METER=YES,HIGH-COUNT=480000, param_3: METER-WAVE=2802.7, param_4: FP-SPLIT=STD req_1: SEQ 28.2-28.3 NON-INT; ! linenum: 28.300 targname: WAVE config: HRS opmode: ACCUM aperture: SC1 sp_element: ECH-B20 wavelength: 2799.0 num_exp: 1 time_per_exp: 3.2S priority: 1 param_1: STEP-PATT=3 req_1: CALIB FOR 28.2 NO SLEW ! ! end of exposure logsheet ! No scan data records found