! File: 1186C.PROP ! Database: PEPDB ! Date: 16-FEB-1994:05:08:34 coverpage: title_1: IMAGERY AND UV SPECTROSCOPY OF MATTER EJECTED FROM ETA CARINAE sci_cat: STELLAR ASTROPHYSICS sci_subcat: HOT STARS proposal_for: GTO/HRS pi_title: DR. pi_fname: DENNIS pi_mi: C. pi_lname: EBBETS pi_inst: BALL AEROSPACE CORPORATION pi_country: USA pi_phone: (303) 939-5964 keywords_1: STELLAR EVOLUTION, MASS LOSS, NUCLEOSYNTHESIS hours_pri: 5.37 num_pri: 3 pi_position: PRIN MEM TECH STAFF ! end of coverpage abstract: line_1: The Planetary Camera and the High Resolution Spectrograph will be used to line_2: study the knots of material which have been ejected from Eta Carinae. Two sets line_3: of PC images in the light of H-Alpha will be taken at widely separated epochs. line_4: Analysis of the images will provide new information about the distribution, line_5: morphology and motions of the ejecta. Ultraviolet spectra of two bright knots line_6: will be obtained with the HRS. The spectral region 1150-1950A will be observed line_7: with configuration G140L, allowing emission line fluxes, profiles, and line_8: velocities to be studied. A signal to noise ratio of 25 in the brighter lines line_9: is anticipated. Searches for as yet undetected lines of carbon and oxygen will line_10: be possible to much fainter limits on the fluxes. line_12: REVISED 7/20/88 FOR PHASE 2 line_13: UPDATED 9/15/89 FOR CYCLE 1 PHASE 2 line_14: WF/PC images revised 10/89 line_15: REVISED 11/16/90 FOR CYCLE 0 WFC AND PC IMAGES ! ! end of abstract general_form_proposers: lname: EBBETS fname: DENNIS mi: C. inst: BALL AEROSPACE CORPORATION country: USA ! lname: WALBORN fname: NOLAN mi: R. inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: DAVIDSON fname: KRIS inst: UNIV OF MINNESOTA country: USA ! lname: WARNOCK fname: ARCHIE inst: NASA/GSFC country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Two sets of observations will be made for this project. Images of the line_2: nebulosity surrounding Eta Carinae will be obtained using the Planetary Camera line_3: with H Alpha and R filters. Two sets of images will obtained, the first during line_4: cycle 0 of GTO observations, and a "second epoch" image during the last line_5: phase. The images will be used to study with high spatial resolution and line_6: sensitivity the distribution, morphology, and motions of the numerous knots of line_7: ejected material. The initial image will be used to measure the size and line_8: precise location of two bright knots, the "S" and "W" condensations, relative line_9: to nearby stars. These offsets will be used for target acquisition by the HRS. line_10: Both knots will be observed with the low resolution, R=2000, configuration, line_11: G140L. Ultraviolet spectra in the spectral range 1150-1950A will be obtained, line_12: with 3 carrousel settings. Signal to noise ratio of roughly 25 will be obtained line_13: in the brighter emission lines. The Large Science Aperture, 2.0 arcsec, will be line_14: used to maximize the flux and simplify target acquisiton. The HRS observations line_15: should be made during cycles 1 and 2. line_17: Cycle 0: exposures 8.5, 8.6, 9 1.52 hours priority 1 line_18: Cycle 1: exposures 10-16 1.65 hours priority 1 line_19: Cycle 2: exposures 17-23 1.65 hours priority 3 line_20: Cycle 3: exposure 24 0.55 hours priority 1 line_22: TOTAL = 5.37 hours ! question: 3 section: 2 line_1: Here is description of what we intend to mean with the pointing line_2: requests for the cycle 0 exposures, lines 4 - 9. line_4: For the two PC F336W exposures, lines 4 and 5, we would like the bright line_5: central object of Eta Carina placed at the center of P6. We do however line_6: want the data from all four chips. That is why we said "ALL" for the line_7: "aperture" and requested POS TARG -16.0,+16.0. The documentation indicates line_8: that P6 is the cosmetically best chip. In this wavelength band most of the line_9: interesting structure should be within a few arc seconds of the core. Centering line_10: in P6 gives us a full 16 arc second radius around the object without line_11: crossing a chip boundary. line_13: For the three red exposures, lines 6,7,8, we would like the bright central line_14: object to be placed near the center of the full four chip format, but line_15: all in one chip. The inner region is bright in the red, and there will line_16: probably be some saturation. By putting the bright object at -3.0,+3.0, line_17: any bleeding of columns will be confined to one chip. Fainter sources line_18: nearby will be on different chips, and should not be contaminated. ! question: 3 section: 3 line_1: For the two WFC images, lines 8.5 and 8.6, we would like the bright object line_2: on or near the ND spot. We recognize that the spherical aberation reduces line_3: the effectiveness of the spot, and that its position has not been carefully line_4: calibrated astrometrically. We understand that this pointing may not be line_5: terribly effective. However, it can't hurt the observation either, so... line_6: We would like to try for the spot and will accept whatever suppression of line_7: the bright light we get. We do not want to do an interactive target line_8: acquisition. line_13: In all three cases, when I refer to the bright central object, I mean line_14: target #1, ETA-CARINAE, on the fixed target list. line_16: Also note that my coinvestigator, Kris Davidson, has supplied Conrad Sturch line_17: with a special catalog of astrometric measurements from which the coordinates line_18: of the central object and guide stars must be extracted. Kris, Conrad and I line_19: have been discussing this for over two years, so Conrad is well aware of line_20: what's going on. The special catalog is designated ZZZQ. This special catalog line_21: should be used for all target positions. ! question: 4 section: 1 line_1: HRS will provide the spatial resolution, sensitivity, and spectral resolution line_2: to record the ultraviolet spectra of these faint objects. The most important line_3: lines of Nitrogen, Helium, and Silicon are found in this spectral region. line_4: Spectra have been obtained with the IUE, but are limited by the poor spatial line_5: resolution, low spectral resolution, and lower photometric accuracy of that line_6: instrument. The PC images will allow more precise measurements of the positions line_7: and proper motions of the ejecta, and will likely detect fainter material and line_8: smaller scale structures which have escaped detection by the previous ground line_9: based studies. Precise positions are required for an efficient HRS target line_10: acquisition to be planned. ! question: 5 section: 1 line_1: An interval of several months is requested between the initial PC images and line_2: the HRS observations, to allow careful planning of the HRS target acquisition line_3: sequence. line_5: Two sets of PC images should be scheduled as early and as late in the GTO line_6: program as possible, to maximize the effect of proper motions of the ejecta. line_8: Kris Davidson's special catalog ZZZQ should be used for guide line_9: star selection. line_11: The WFC and PC images should be taken after the UV flood. ! question: 7 section: 1 line_1: The calibration and reduction of the PC images will be accomplished with line_2: RSDP, SDAS and GASP routines. The positions of astrometric standard stars line_3: (Walborn, Blanco, Thackeray 1978, Ap.J., 219, 498) and several stars closer to line_4: Eta Carinae will be measured from the WFC images (see comment 8 below). The line_5: closer stars will be used as fiducials for study of the proper motions of the line_6: ejecta, and as target acquisition offsets for the HRS. The PC R band and H line_7: Alpha images will be scaled and differenced to suppress continuum sources and line_8: emphasize material emitting in H Alpha. The knots of nebular material will be line_9: studied in these processed images. line_11: The HRS spectra will be processed with standard techniques using either RSDP or line_12: IDT facilities. Emission lines will be analyzed with respect to fluxes, line line_13: profiles, and radial velocities. Corrections for extinction will be applied line_14: where appropriate. The various ionization stages of nitrogen will be studied to line_15: estimate the abundance. Presently undetected lines of Carbon and Oxygen will be line_16: searched for, and fluxes, or at least upper limits, will be determined. ! question: 9 section: 1 line_1: D. Ebbets in involved with several other GTO projects ! question: 10 section: 1 line_1: Access to data reduction, image analysis facilities, part-time research line_2: assistant, preparation of manuscript, support of publication costs. ! question: 12 section: 1 line_1: First set of PC observations should be scheduled for cycle 0 interleaved line_2: SV-GTO time. line_4: HRS observations should be scheduled for cycles 1 and 2, beginning several line_5: months after the initial PC observations. line_7: Second epoch PC observations should be scheduled for cycle 3, during the final line_8: months of GTO time. line_11: Prerequisite SV tests: line_13: HRS-05.3 Mode II Target Acquisition - offset (or verification of non flight line_14: s/w offset capability) line_16: HRS-08 HRS Low Resolution Calibration ! question: 13 section: 1 line_1: The knots of nebular material which appear to have been ejected from Eta line_2: Carinae will be studied using the Planetary camera and the High Resolution line_3: Spectrograph. PC images in the light of H Alpha taken at two widely separated line_4: epochs will allow the distribution, morphology, and proper motions of the line_5: ejecta to be studied. UV spectra in the range 1150-1950 A will be used to study line_6: the composition and nature of the "S" and "W" condensations. ! !end of general form text general_form_address: lname: WALBORN fname: NOLAN mi: R. category: CON inst: SPACE TELESCOPE SCIENCE INSTITUTE addr_1: HOMEWOOD CAMPUS city: BALTIMORE state: MD zip: 21218 country: USA phone: (301) 338-4915 telex: 6849101 ! lname: EBBETS fname: DENNIS mi: C. title: DR. category: PI inst: BALL AEROSPACE SYSTEMS GROUP addr_1: HRS PROJECT AR-1 addr_2: P.O. BOX 1062 city: BOULDER state: CO zip: 80306 country: USA phone: (303) 939-5964 ! lname: DAVIDSON fname: KRIS category: CON inst: UNIV. OF MINNESOTA addr_1: SCHOOL OF PHYS. AND ASTRON. addr_2: 116 CHURCH ST SE city: MINNEAPOLIS state: MN zip: 55455 country: USA phone: (612) 624-5711 ! lname: WARNOCK fname: ARCHIE category: CON inst: NASA GSFC addr_1: CODE 681 city: GREENBELT state: MD zip: 20771 country: USA phone: (301) 286-8968 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: ETA-CARINAE name_2: HD93308 descr_1: CENTRAL OBJECT pos_1: RA = 10H 45M 03.615S +/- 0.1S, pos_2: DEC = -59D 41' 03.96" +/- 0.5", pos_3: PLATE-ID=ZZZQ equinox: 2000 pm_or_par: NO comment_1: COORDINATES OF CENTRAL OBJECT comment_2: FROM DAVIDSON'S CCD ASTROMETRY ! targnum: 2 name_1: S-CONDENSATION descr_1: KNOT OF EJECTED MATTER pos_1: RA = 10H 43M 05.608S +/- 0.02S, pos_2: DEC = -59D 25' 19.72" +/- 0.1", pos_3: PLATE-ID=ZZZQ equinox: 1950 pm_or_par: NO acqpr_1: EXT acqpr_2: BKG fluxnum_1: 1 fluxval_1: F-LINE(1240)=1.5E-13 fluxnum_2: 2 fluxval_2: F-LINE(1486)=1.5E-13 fluxnum_3: 3 fluxval_3: F-LINE(1749)=2.6E-13 ! targnum: 3 name_1: W-CONDENSATION descr_1: ^ pos_1: RA = 10H 43M 05.491S +/- 0.02S, pos_2: DEC = -59D 25' 02.55" +/- 0.1", pos_3: PLATE-ID=ZZZQ equinox: ^ pm_or_par: ^ acqpr_1: ^ comment_1: POSITIONS OF KNOTS FROM WALBORN comment_2: AND BLANCO MEAS. FROM PLATES comment_3: OBTAINED IN 1985. comment_4: PRECISE POS. WILL BE MEASURED comment_5: FROM WF/PC IMAGES PRIOR TO HRS comment_6: OBSERVATIONS. comment_7: ATTEMPTS TO MEASURE KNOTS WITH comment_8: GASP WERE NOT SUCCESSFUL fluxnum_1: 1 fluxval_1: F-LINE(1240)=3.0E-14 fluxnum_2: 2 fluxval_2: F-LINE(1486)=3.0E-14 fluxnum_3: 3 fluxval_3: F-LINE(1749)=3.0E-14 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 4.000 sequence_1: DEFINE sequence_2: PCETA targname: # config: PC opmode: IMAGE aperture: P6 sp_element: F336W num_exp: 1 time_per_exp: 2S s_to_n: # priority: # param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: POS TARG -14.0,+14.0 ! linenum: 5.000 sequence_1: DEFINE sequence_2: PCETA targname: # config: PC opmode: IMAGE aperture: P6 sp_element: F336W num_exp: 1 time_per_exp: 30S s_to_n: # priority: # param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: POS TARG -14.0,+14.0 ! linenum: 6.000 sequence_1: DEFINE sequence_2: PCETA targname: # config: PC opmode: IMAGE aperture: P6 sp_element: F675W num_exp: 1 time_per_exp: 4S s_to_n: # priority: # param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: POS TARG -3.0,+3.0 / 6-8 ! linenum: 7.000 sequence_1: DEFINE sequence_2: PCETA targname: # config: PC opmode: IMAGE aperture: P6 sp_element: F675W num_exp: 1 time_per_exp: 100S s_to_n: # priority: # param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES ! linenum: 8.000 sequence_1: DEFINE sequence_2: PCETA targname: # config: PC opmode: IMAGE aperture: P6 sp_element: F658N num_exp: 1 time_per_exp: 100S s_to_n: # priority: # param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES comment_1: THIS SEQUENCE DEFINES THE PC IMAGES comment_2: OF ETA CARINAE AND ITS SURROUNDINGS. comment_3: SEE GENERAL FORM SECTION 3 FOR comment_4: INFORMATION ON WHAT IS BEING comment_5: REQUESTED WITH POS TARG (LINES comment_6: 4-8.6). ! linenum: 8.500 targname: ETA-CARINAE config: WFC opmode: IMAGE aperture: ALL-ND sp_element: F675W num_exp: 1 time_per_exp: 3S s_to_n: 50 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: CYCLE 0 / 8.5,8.6; req_3: UNPROTECTED; req_4: EARLY ACQ FOR 9; ! linenum: 8.600 targname: ETA-CARINAE config: WFC opmode: IMAGE aperture: ALL-ND sp_element: F658N num_exp: 1 time_per_exp: 10S s_to_n: 50 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: UNPROTECTED ! linenum: 9.000 sequence_1: USE sequence_2: PCETA targname: ETA-CARINAE s_to_n: 50 priority: 1 req_1: CYCLE 0; req_2: EARLY ACQ FOR 10-23; ! linenum: 10.000 targname: S-CONDENSATION config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 273S priority: 1 param_1: MAP=END-POINT, param_2: FAINT=100, req_1: ONBOARD ACQ FOR 11-16; req_2: AFTER 9 BY 120D; req_3: CYCLE 1 /10-16 ! linenum: 11.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1300 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=2 req_1: CALIB FOR 12; req_2: SEQ 11-12 NO GAP comment_1: WAVELENGTH CALIBRATIONS LINES 11, 13, comment_2: 15 TO INCLUDE SPECTRUM Y BALANCE. ! linenum: 12.000 targname: S-CONDENSATION config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1300 num_exp: 1 time_per_exp: 20M s_to_n: 25 fluxnum_1: 1 priority: 1 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD ! linenum: 13.000 targname: WAVE config: ^ opmode: ^ aperture: SC2 sp_element: ^ wavelength: 1550 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=2 req_1: CALIB FOR 14; req_2: SEQ 13-14 NO GAP ! linenum: 14.000 targname: S-CONDENSATION config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 20M s_to_n: 25 fluxnum_1: 2 priority: 1 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD ! linenum: 15.000 targname: WAVE config: ^ opmode: ^ aperture: SC2 sp_element: ^ wavelength: 1800 num_exp: 1 time_per_exp: 30S priority: 1 param_1: STEP-PATT=2 req_1: CALIB FOR 16; req_2: SEQ 15-16 NO GAP ! linenum: 16.000 targname: S-CONDENSATION config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 30M s_to_n: 25 fluxnum_1: 3 priority: 1 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD comment_1: SCHEDULE 10-16 DURING CYCLE 1 comment_2: UNOCCULTED SC TIME APPROX. 1.65 comment_3: HOURS FOR 10-16. ! linenum: 17.000 targname: W-CONDENSATION config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 time_per_exp: 289S priority: 3 param_1: MAP=END-POINT req_1: ONBOARD ACQ FOR 18-23; req_2: CYCLE 2 /17-23 ! linenum: 18.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1300 num_exp: 1 time_per_exp: 30S priority: 3 param_1: STEP-PATT=2 req_1: CALIB FOR 19; req_2: SEQ 18-19 NO GAP ! linenum: 19.000 targname: W-CONDENSATION config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 20M s_to_n: 25 fluxnum_1: 1 priority: 3 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD ! linenum: 20.000 targname: WAVE config: ^ opmode: ^ aperture: SC2 sp_element: ^ wavelength: 1550 num_exp: 1 time_per_exp: 30S priority: 3 param_1: STEP-PATT=2 req_1: CALIB FOR 21; req_2: SEQ 20-21 NO GAP ! linenum: 21.000 targname: W-CONDENSATION config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1550 num_exp: 1 time_per_exp: 20M s_to_n: 25 fluxnum_1: 2 priority: 3 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD ! linenum: 22.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1800 num_exp: 1 time_per_exp: 30S priority: 3 param_1: STEP-PATT=2 req_1: CALIB FOR 23; req_2: SEQ 22-23 NO GAP ! linenum: 23.000 targname: W-CONDENSATION config: ^ opmode: ^ aperture: 2.0 sp_element: ^ wavelength: ^ num_exp: 1 time_per_exp: 30M s_to_n: 25 fluxnum_1: 3 priority: 3 param_1: STEP-PATT=2, param_2: FP-SPLIT=STD comment_1: SCHEDULE 17 - 23 DURING CYCLE 2. comment_2: UNOCCULTED SC TIME APPROX. 1.65 comment_3: HOURS FOR 17-23 ! linenum: 24.000 sequence_1: USE sequence_2: PCETA targname: ETA-CARINAE s_to_n: 50 priority: 1 req_1: AFTER 9 BY 730D; req_2: CYCLE 3 comment_1: SCHEDULE 24 DURING GTO CYCLE 3. comment_2: UNOCCULTED SC TIME APPROX. 0.55 comment_3: HOURS FOR 24 ! ! end of exposure logsheet ! No scan data records found