! $Id: 5743,v 4.1 1994/07/27 20:48:06 pepsa Exp $ ! Revised to do G190H only; after failed GS ACQ. coverpage: title_1: PLUTOS FUV SPECTRUM: CO ABUNDANCE AND FUV title_2: SURVEY carryover from 3803 sci_cat: SOLAR SYSTEM sci_subcat: MINOR PLANETS proposal_for: GO/CAR pi_fname: LAURENCE pi_mi: M pi_lname: TRAFTON pi_inst: TEXAS, UNIVERSITY OF pi_country: USA pi_phone: 512-471-1476 hours_pri: 5.26 num_pri: 2 fos: Y time_crit: Y funds_amount: 0 funds_length: 24 ! end of coverpage abstract: line_1: We propose FUV observations of Pluto using the FOS/BL with G190H to line_2: survey the spectral region 2200-1800 A for absorption features, and line_3: the FOS/BL with G130H to survey the spectral region 1608-1200 A for line_4: emission features, or fluorescence, in Pluto's atmosphere. The spectral line_5: resolutions are delta lambda = 2.3 A and 1.6 A, respectively. A high line_6: priority will be to search for the cosmogonically important molecule line_7: CO using two vibrational Cameron bands in absorption at 2060 A and line_8: 1989 A, and the (1-0) and other 4th positive vibrational bands in line_9: emission near 1500 A, in order to determine an accurate CO column line_10: abundance and to constrain the rotational temperature of CO. line_11: Detection of both emission and absorption bands would set line_12: constraints on models of atmospheric escape by providing information line_13: on the radial distribution of CO in Pluto's lower atmosphere. We line_14: also search for other species, such as NO. Only HST has the line_15: sensitivity and spatial resolution to obtain Pluto's FUV spectrum. ! ! end of abstract general_form_proposers: lname: TRAFTON fname: LAURENCE title: PI mi: M inst: TEXAS, UNIVERSITY OF country: USA ! lname: STERN fname: S. mi: A. inst: SOUTHWEST RESEARCH INSTITUTE country: USA ! ! end of general_form_proposers block general_form_text: ! question: 3 section: 1 line_1: Description of proposed observations: line_2: We plan to acquire Pluto when Charon is near line_3: elongation and Pluto is not far from opposition. line_4: line_5: For the 2200-1800A region only, a real-time peak up will center line_6: Pluto in the 1" aperture and exclude Charon, which will be about 0.9" line_7: away and about 5 times fainter. This aperture will minimize the line_8: contamination of Pluto's spectrum by Charon. A 3.2 hr exposure will be line_9: obtained with the FOS/RD+G190H+1.0" aperture. line_10: line_11: line_12: The 1608-1200A region will be observed line_13: with FOS/BL+G130H+1"aperture over an additional 4 hr total exposure. line_14: This will survey the FUV emission spectrum of Pluto and the 4th line_15: positive CO bands near 1500A. No attempt will be made to exclude Charon line_16: from this aperture since the continuum flux from both Pluto and Charon line_17: are both negligible at 1500A owing to the weak solar flux. ! question: 4 section: 1 line_1: Justify the need for the capabilities of HST: line_2: Pluto's FUV spectrum has never been observed. Pluto is the only planet line_3: not visited by a spacecraft. IUE was able to observe Pluto's spectrum line_4: only down to 2500A before reaching its limit of sensitivity. Only HST line_5: has the sensitivity to observe Pluto's FUV spectrum. High spatial line_6: resolution is needed to separate Pluto's spectrum from Charon's. Only line_7: the UV offers molecular absorption coefficients large enough for line_8: detecting many trace constituents. Pluto's strong CH4 spectrum line_9: critically interferes with detecting CO in the infrared; only the UV line_10: allows a practicable way to measure Pluto's CO abundance. CO emission line_11: from Pluto's extended atmosphere can only be observed in the UV. ! question: 5 section: 1 line_1: Justify any special scheduling requests: line_2: The observations need to be scheduled when Charon is not far from line_3: elongation so that its continuum spectrum will not contaminate Pluto's line_4: for the longer wavelength observations using the FOS. Pluto would be line_5: available about 70% of the time. line_6: Schedule to minimize background Dark Count: Avoid the SSA and high line_7: magnetic latitudes. ! question: 6 section: 1 line_1: List any special calibration requirements for your observations line_2: line_3: line_4: line_5: line_6: line_7: line_8: line_10: line_11: line_12: line_13: line_14: line_15: ! ! ! question: 8 section: 1 line_1: Additional comments or requests: line_2: None. ! question: 9 section: 1 line_1: Description of any previous HST data: line_2: a. List HST program numbers and titles, and specify whether they are line_3: related to this project or not. line_4: Trafton: line_5: 1202 Lyman-alpha and H2 Survey; No line_6: 1203 Jovian Auroral Ly-alpha Profile; No line_7: 1204: Io Proton Aurora? No line_8: 1205: SO2 on Io; No line_9: 1206 Sulfur Near Io; No line_10: 2569: UV Rotational Light Curves for Pluto, and Charon's UV Spectrum; line_11: Yes line_12: 2957 High Resolution UV Spectropy of Triton,; No line_13: 2560: Integrated Dynamical and Spectroscopic Observations of Jupiter line_14: and Saturn; No line_15: Stern: line_16: 2957 High Resolution UV Spectropy of Triton,; No line_17: 2569: UV Rotational Light Curves for Pluto, and Charon's UV Spectrum; line_18: Yes line_19: b. Summarize the main results obtained from previous related programs. line_20: No results yet. line_21: c. List publications resulting from the above data (Format: Title, line_22: Authors,Journal, Volume, Page, and Year.) line_23: "First results from the GHRS: Resolved velocity and density structure ! question: 9 section: 2 line_1: in the beta pictoris circumstellar gas", A. Boggess, F. C. Bruhweiler, line_2: C. A. Grady, D. C. Ebbets, Y. Kondo, L. M. Trafton, J. C. Brandt, and line_3: S. R. Heap, Astrophys. J. (Letters), Aug 15 , 1991. ! question: 10 section: 1 line_1: Resources to be supplied by your institution: line_2: Facilities of the UT Computation Center and Advanced Graphics Laboratory line_3: are available to support this project, as well as a Sun 4 Sparcstation. line_4: A pool of astronomy graduate students is also available from which to line_5: draw research assistants. Ground based observations of Io are line_6: periodically made from MacDonald Observatory for related studies. The line_7: Southwest Research Institute will support this project by providing all line_8: required computing facilities for the Co-I and visiting PI. ! !end of general form text general_form_address: lname: TRAFTON fname: LAURENCE mi: M category: PI inst: UNIVERSITY OF TEXAS addr_1: ASTRONOMY DEPARTMENT addr_2: UNIVERSITY OF TEXAS AT AUSTIN city: AUSTIN state: TX zip: 78712 country: USA phone: 512-471-1476 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: PLUTO-BL descr_1: PLANET PLUTO lev1_1: STD = PLUTO, ACQ = 0.07 wind_1: WND1 = 15-APR-94 TO 30-APR-95, wind_2: SEP OF PLUTO CHARON FROM EARTH wind_3: GT 0.75" WITHIN WND1 comment_1: OBSERVE PLUTO WITH CHARON NOT FAR comment_2: FROM ELONGATION (OUT OF THE WAY). fluxnum_1: 1 fluxval_1: V = 13.9 +/- 0.5 fluxnum_2: 2 fluxval_2: TYPE = G2V fluxnum_3: 3 fluxval_3: F-CONT(2400) = 1.5 +/- 1.0 E-16 fluxnum_4: 4 fluxval_4: F-CONT(2000) = 1.8 +/- 0.5 E-17 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 targname: TALED config: FOS/BL opmode: ACQ aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 120.0S fluxnum_1: 1 fluxnum_2: 2 priority: 1 req_1: RT ANALYSIS; req_2: SEQ 1-1.3 NON-INT; req_3: CYCLE 4 / 1-2; req_4: GROUP 1-2 WITHIN 36H; ! linenum: 1.200 targname: PLUTO-BL config: FOS/BL opmode: ACQ aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 480S fluxnum_1: 1 fluxnum_2: 2 priority: 1 req_1: INT ACQ FOR 2 comment_1: MAKE A PICTURE. comment_2: FOR REAL TIME CENTERING comment_3: FIGURE DURING EARTH OCCULTATION ! linenum: 1.300 targname: TALED config: FOS/BL opmode: ACQ aperture: 0.3 sp_element: MIRROR num_exp: 1 time_per_exp: 120S fluxnum_1: 1 fluxnum_2: 2 priority: 1 req_1: RT ANALYSIS comment_1: LOCATE APERTURE. ! ! linenum: 1.500 ! targname: PLUTO-BL ! config: FOS/BL ! opmode: ACQ ! aperture: 4.3 ! sp_element: MIRROR ! num_exp: 1 ! time_per_exp: 120S ! fluxnum_1: 1 ! fluxnum_2: 2 ! priority: 1 ! comment_1: MAKE A PICTURE. ! comment_2: TO VERIFY POINTING AFTER GS REACQ ! linenum: 2.000 targname: PLUTO-BL config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1950 num_exp: 1 time_per_exp: 191M s_to_n: 12 fluxnum_1: 4 priority: 1 comment_1: EXPOSURE REDUCED FROM 239M COMMENT_2: TO ACCOUNT FOR COSTAR. ! ! end of exposure logsheet ! No scan data records found