! File: 4642C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:20:52:38 coverpage: title_1: INTEGRATED DYNAMICAL AND SPECTROSCOPIC OBSERVATIONS OF JUPITER AND SAT title_2: URN-CYC3 sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GO pi_fname: RETA pi_mi: F. pi_lname: BEEBE pi_inst: NEW MEXICO STATE UNIVERSITY pi_country: USA hours_pri: 10.55 num_pri: 2 wf_pc: Y fos: Y time_crit: Y funds_length: 12 off_fname: J. off_mi: M. off_lname: ADAMS off_title: DIR. A&S RES. CENT. off_inst: 2960 off_addr_1: BOX 30001/ DEPT. RC off_city: LAS CRUCES off_state: NM off_zip: 88003 off_country: USA off_phone: 505-646-2611 ! end of coverpage abstract: line_1: The design of our Cycle 3 program for Jupiter and Saturn is driven by the line_2: spectroscopic results from Cycle 1 observations of Jupiter, and from line_3: wind field analysis of the Saturn Target-of-Opportunity and Jupiter Cycle 0 line_4: WF/PC data. Early analysis of the Cycle 1 FOS spectra has revealed variation line_5: that is dependent on latitude as well as the viewing aspect of the region line_6: within the aperture. Because of the greater sensitivity of the FOS these line_7: results were obtained with smaller apertures than had been possible with line_8: previously available instruments. Several of the FOS results were unexpected line_9: and will provide constraints for studying dynamical phenomena in the line_10: atmospheres of these planets. We are requesting specific observations with the line_11: FOS and coordinated multicolor observations with the WF/PC to relate the line_12: variation in the aerosol properties of the atmospheres to the morphological line_13: features and possible changes in zonal wind speed. The data will help to line_14: constrain the meridional circulation and local dynamics. The proposed sequences line_15: will add significantly to the content of the data base that will be acquired line_16: in proposal 2560. No facility other than HST has the spatial resolution and line_17: sensitivity in the FUV to obtain the spectra requested in this study. ! ! end of abstract general_form_proposers: lname: BEEBE fname: RETA title: PI mi: F. inst: NEW MEXICO STATE UNIVERSITY country: USA ! lname: ATREYA fname: SUSHIL inst: UNIVERSITY OF MICHIGAN country: USA ! lname: CALDWELL fname: JOHN inst: YORK UNIVERSITY country: CANADA ! lname: BARNET fname: CHRISTOPHER inst: NASA GODDARD SPACE FLIGHT CENTER country: USA ! lname: LIMAYE fname: SANJAY inst: UNIVERSITY OF WISCONSIN country: USA ! lname: NOLL fname: KEITH inst: STSCI country: USA ! lname: TRAFTON fname: LAURENCE inst: UNIVERSITY OF TEXAS country: USA ! lname: WEST fname: ROBERT inst: JPL country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: FOS observations at 4, 6, 8 and 10 degrees N latitude using the G190H grating wi line_2: ll provide information concerning the latitudinal distribution of ammonia gas. A line_3: set of multicolor images, spanning one rotation of the planet, will be followed line_4: 20 hours later by two 5-color sets covering longitudes excluding the Red Spot i line_5: n order to derive the undisturbed zonal wind profile. ! question: 3 section: 2 line_1: Cycle 3 Jupiter Primary Hours:5.1 Exposures:150 ! question: 4 section: 1 line_1: Only HST can obtain these FUV observations with the required spatial(0.5-1") and line_2: spectral resolution. IUE does not have the spatial resolution or sensitivity to line_3: obtain usable spectra below 2500A of Saturn or Jupiter. The FUV is needed to re line_4: veal the upper atmospheric aerosol and minor gas absorptions. Rayleigh scatterin line_5: g in the FUV permits the atmosphere to be probed to different depths at differen line_6: t wavelengths; this capability is needed for dynamical studies. line_8: Our Cycle 1 and 2 data will not realize the spatial resolution requested here. line_9: The PC F230W filter is not good and in any event, its single bandpass integrates line_10: over all sensible atmospheric depths. line_12: Analysis of Cycle 0 data has established that the PC images can be successfully line_13: deconvolved, revealing the small scale convective structures that are needed to line_14: detect the wind speeds associated with the maximum and minimum jets. ! question: 4 section: 2 line_1: The above exposure times are based on actual empirical results obtained from our line_2: Cycle 1 Jupiter data for the same gratings and apertures of the FOS. The S/N ra line_3: tios, varying strongly across each grating's wavelength region, are adequate to line_4: characterize the phenomena discovered in Cycle 1. The overhead for the FOS obser line_5: vations and WF/PC images and the onboard acquisitions are the main contributions line_6: to the S/C time beyond the exposure time. line_8: The PC exposures are based on Cycle 2 results for Jupiter. They are grouped in line_9: sets of 5 to optimize color information while maximizing spacecraft efficiency. ! question: 6 section: 1 line_1: Standard HST in-house calibrations will be adequate. ! question: 7 section: 1 line_1: R. Beebe and Graduate Student L. Huber at New Mexico State University will be in line_2: charge of distributing the data and serving as a central coordination site for line_3: all investigators. They will also have responsibility for monitoring the calibr line_4: ation and coordinating and evaluating the processing of the PC images. L. Trafto line_5: n will be in charge of the preliminary reduction, calibration and evaluation of line_6: the FOS data. line_8: Atreya, Caldwell, Noll and Trafton will carry the lead role in reducing the spec line_9: troscopic data. Each will bring his own expertise and knowledge to the problem. line_10: Barnet, with full access to the Voyager IRIS spectra, will contribute to the an line_11: alysis and C. Barnet, R. Beebe and S. Limaye will be involved in deconvolution o line_12: f the PC images and subsequent analysis of the horizontal wind data. line_14: R. West will lead the studies for modeling of aerosol scattering and will intera line_15: ct with others during our efforts to define the limit to which we can specify ph line_16: otometric properties. ! question: 8 section: 1 line_1: We are submitting a Cycle 3 archival proposal that proposes to process and analy line_2: ze Cycle 0 and Cycle 1 PC imaging data of Jupiter to extend the dynamical timeli line_3: ne using the data from our Cycle 1 and 2 imaging results. ! question: 9 section: 1 line_1: Beebe and Caldwell, with J. Westphal, W. Baum, G. Danielson and A. Ingersoll--DD line_2: proposal #3090 and #3109 "The 1990 Saturn equatorial storm" Related to this wor line_3: k. See below for results. line_5: Atreya, Beebe, Limaye, Trafton and West--Cycle 1 #2560 and Cycle 2 #3887 "Integr line_6: ated Dynamical and Spectroscopic Observations of Jupiter and Saturn" related to line_7: this work and described in question 2. line_9: Trafton--Cycle 2 no number yet- "Pluto's FUV Spectrum: CO Abundance and FUV Surv line_10: ey" not related to this work. line_12: West--Cycle 1 #2564 with M. Tomasko. "Aerosols in Planetary Atmospheres". Relate line_13: d to this work and deals with WF/PC imaging and modelling of the scattering prop line_14: erties. line_16: Caldwell--GTO with the Observatory Scientist team. In addition to his original line_17: forty hours of GTO, he was awarded another 25 hours of AUG time in 1991. ! question: 9 section: 2 line_1: Results from 3090 and 3109 have been processed and analyzed. See question 9c for line_2: publications. Data from 2560 was received in May 1992 and preliminary analysis line_3: is underway and is discussed in this proposal. line_5: L. Trafton presented preliminary results of 2560 and R. Beebe reviewed results f line_6: rom 3109 and 3090 as invited papers at the ESA/HST Workshop in Sardinia, Italy, line_7: June 29-July 7, 1992. line_9: Caldwell's GTO program is devoted to auroral study. Successful observations were line_10: made at the time of the Ulysses Jupiter encounter.A publication is in press wit line_11: h SCIENCE. ! question: 9 section: 3 line_1: Hubble Space Telescope observations of the 1990 equatorial disturbance on Saturn line_2: : zonal winds and central meridian albedos. Barnet, C.D., J.A. Westphal, R.F. Be line_3: ebe and L.F. Huber. Icarus (accepted 8/1992). line_5: The onset and growth of the 1990 equatorial disturbance on Saturn. Beebe, R.F., line_6: C.D. Barnet, P.V. Sada and A.S. Murrell. Icarus v.96 p.163-172 1992. line_8: Hubble Space Telescope observations of the 1990 equatorial disturbance on Saturn line_9: : images, albedos, and limb darkening. Westphal, J.A., W.A. Baum, A.P. Ingersoll line_10: , C.D. Barnet, E.M. De Jong, G. Edward Danielson and J. Caldwell. Icarus (submit line_11: ted 7/1992). line_13: Titan: Evidence for Seasonal Change - A Comparison of Hubble Space Telescope an line_14: d Voyager Images, J. Caldwell et al., Icarus 96, 1-9, 1992. line_16: Hubble Space Telescope Imaging of the North Polar Aurora On Jupiter, J. Caldwell line_17: , B. Turgeon, H.-M. Hua, Science, in press, 1992. ! question: 10 section: 1 line_1: The PI and Co-I's are experienced in data reductions of this type. Each individu line_2: al has his/her own workstation at the home sites. line_4: A collaborative workshop will be held at NMSU about 6 months after the receipt o line_5: f these data. NMSU will provide the facilities and host this meeting. ! !end of general form text general_form_address: lname: BEEBE fname: RETA mi: F. category: PI inst: New Mexico State University addr_1: BOX 30001, DEPARTMENT 4500 city: LAS CRUCES state: NM zip: 88003 country: USA phone: 505-646-1938 ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: BL-JUP-4DEGN-CM-FOS-CYC3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 0.1 lev2_1: TYPE = TORUS, RAD = 71380.9, lev2_2: LAT = +3.50, LONG = 0 comment_1: OBSERVE JUPITER AT 4 DEG NLAT comment_2: ON CENTRAL MERIDIAN fluxnum_1: 1 fluxval_1: V=-2.5 fluxnum_2: 2 fluxval_2: SURF(1900)=2.1+/-1.0E-14 ! targnum: 2 name_1: BL-JUP-6DEGN-CM-FOS-CYC3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 0.1 lev2_1: TYPE = TORUS, RAD = 71357.1, lev2_2: LAT = +5.25, LONG = 0 comment_1: OBSERVE JUPITER AT 6 DEG NLAT comment_2: ON CENTRAL MERIDIAN fluxnum_1: 1 fluxval_1: V=-2.5 fluxnum_2: 2 fluxval_2: SURF(1900)=2.1+/-1.0E-14 ! targnum: 3 name_1: BL-JUP-8DEGN-CM-FOS-CYC3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 0.1 lev2_1: TYPE = TORUS, RAD = 71324.1, lev2_2: LAT = +7.00, LONG = 0 comment_1: OBSERVE JUPITER AT 8 DEG NLAT comment_2: ON CENTRAL MERIDIAN fluxnum_1: 1 fluxval_1: V=-2.5 fluxnum_2: 2 fluxval_2: SURF(1900)=2.1+/-1.0E-14 ! targnum: 4 name_1: BL-JUP-10DEGN-CM-FOS-CYC3 descr_1: FEATURE JUPITER lev1_1: STD = JUPITER, ACQ = 0.1 lev2_1: TYPE = TORUS, RAD = 71281.3, lev2_2: LAT = +8.77, LONG = 0 comment_1: OBSERVE JUPITER AT 10 DEG NLAT comment_2: ON CENTRAL MERIDIAN fluxnum_1: 1 fluxval_1: V=-2.5 fluxnum_2: 2 fluxval_2: SURF(1900)=2.1+/-1.0E-14 ! targnum: 5 name_1: JUPITER-PC-CYC3 descr_1: PLANET JUPITER lev1_1: STD = JUPITER comment_1: IMAGE JUPITER IN MULTIPLE FILTERS FOR 6 comment_2: CONTIGUOUS ORBITS TO OBTAIN ONE comment_3: COMPLETE MULTICOLOR MAP OF THE PLANET comment_4: FOLLOWED LATER BY 2 CONTIGUOUS ORBITS comment_5: AWAY FROM RED SPOT FOR DYNAMICS comment_6: OMIT FILTERS AT THE END OF A SEQUENCE comment_7: DURING A GIVEN ORBIT WHEN GUIDE STAR comment_8: ACQUISITION IS NECESSARY comment_9: FLUX VALUES ARE FOR PLANET CENTER fluxnum_1: 1 fluxval_1: V=-2.5 fluxnum_2: 2 fluxval_2: SURF(8890)=1.6+/-0.3E-12 fluxnum_3: 3 fluxval_3: SURF(7180)=1.5+/-0.3E-11 fluxnum_4: 4 fluxval_4: SURF(4130)=3.5+/-0.6E-11 fluxnum_5: 5 fluxval_5: SURF(3360)=9.6+/-2.0E-12 fluxnum_6: 6 fluxval_6: SURF(5470)=4.0+/-0.5E-11 fluxnum_7: 7 fluxval_7: SURF(6310)=4.5+/-0.9E-11 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 sequence_1: DEFINE sequence_2: PCJUP-C3-1 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 14.0S fluxnum_1: 5 priority: 1 req_1: SEQ 1-5 NON-INT; req_2: GUID TOL 0.025"; req_3: CYCLE 3 / 1-51 ! linenum: 2.000 sequence_1: DEFINE sequence_2: PCJUP-C3-1 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F547M num_exp: 1 time_per_exp: 0.33S fluxnum_1: 6 priority: 1 req_1: GUID TOL 0.025" ! linenum: 3.000 sequence_1: DEFINE sequence_2: PCJUP-C3-1 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F889N num_exp: 1 time_per_exp: 60S fluxnum_1: 2 priority: 1 req_1: GUID TOL 0.025" ! linenum: 4.000 sequence_1: DEFINE sequence_2: PCJUP-C3-1 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F631N num_exp: 1 time_per_exp: 8.0S fluxnum_1: 7 priority: 1 req_1: GUID TOL 0.025" ! linenum: 5.000 sequence_1: DEFINE sequence_2: PCJUP-C3-1 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F718M num_exp: 1 time_per_exp: 0.46S fluxnum_1: 3 priority: 1 req_1: GUID TOL 0.025" comment_1: THIS GENERATES A COMPLETE MAP comment_2: OF THE PLANET WHEN IT IS comment_3: REPEATED 5 MORE TIMES ! linenum: 11.000 sequence_1: DEFINE sequence_2: PCJUP-C3-2 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F336W num_exp: 1 time_per_exp: 14.0S fluxnum_1: 5 priority: 1 req_1: SEQ 11-15 NON-INT; req_2: GUID TOL 0.025"; ! linenum: 12.000 sequence_1: DEFINE sequence_2: PCJUP-C3-2 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F547M num_exp: 1 time_per_exp: 0.33S fluxnum_1: 6 priority: 1 req_1: GUID TOL 0.025" ! linenum: 13.000 sequence_1: DEFINE sequence_2: PCJUP-C3-2 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F889N num_exp: 1 time_per_exp: 60S fluxnum_1: 2 priority: 1 req_1: GUID TOL 0.025" ! linenum: 14.000 sequence_1: DEFINE sequence_2: PCJUP-C3-2 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F631N num_exp: 1 time_per_exp: 8.0S fluxnum_1: 7 priority: 1 req_1: GUID TOL 0.025" ! linenum: 15.000 sequence_1: DEFINE sequence_2: PCJUP-C3-2 targname: # config: PC opmode: IMAGE aperture: ALL sp_element: F718M num_exp: 1 time_per_exp: 0.46S fluxnum_1: 3 priority: 1 req_1: GUID TOL 0.025" comment_1: COMBINED WITH 1-5 THIS ALLOWS comment_2: COLOR RATIOS AND MAPPING OF THE comment_3: HORIZONTAL WINDS ! linenum: 20.000 sequence_1: DEFINE sequence_2: FOSBG190H targname: # config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G190H num_exp: 1 time_per_exp: 25M fluxnum_1: 2 priority: 1 ! linenum: 21.000 sequence_1: USE sequence_2: FOSBG190H targname: BL-JUP-4DEGN-CM-FOS-CYC3 req_1: SEQ 21-24 NO GAP; comment_1: PLACE APERTURE ON CENTRAL comment_2: MERIDIAN AT 4 DEG N LATITUDE comment_3: USE SAME GUIDE STAR FOR 21-24 ! linenum: 22.000 sequence_1: USE sequence_2: FOSBG190H targname: BL-JUP-6DEGN-CM-FOS-CYC3 comment_1: PLACE APERTURE ON CENTRAL comment_2: MERIDIAN AT 6 DEG N LATITUDE ! linenum: 23.000 sequence_1: USE sequence_2: FOSBG190H targname: BL-JUP-8DEGN-CM-FOS-CYC3 comment_1: PLACE APERTURE NEAR CENTRAL comment_2: MERIDIAN AT 8 DEG N LATITUDE ! linenum: 24.000 sequence_1: USE sequence_2: FOSBG190H targname: BL-JUP-10DEGN-CM-FOS-CYC3 comment_1: PLACE APERTURE ON CENTRAL comment_2: MERIDIAN AT 10 DEG N LATITUDE ! linenum: 40.000 sequence_1: USE sequence_2: PCJUP-C3-1 targname: JUPITER-PC-CYC3 req_1: SEQ 40-45 NO GAP; comment_1: 40-45 GENERATES A COMPLETE MAP comment_2: OF THE PLANET. ! linenum: 41.000 sequence_1: USE sequence_2: PCJUP-C3-1 targname: JUPITER-PC-CYC3 ! linenum: 42.000 sequence_1: USE sequence_2: PCJUP-C3-1 targname: JUPITER-PC-CYC3 ! linenum: 43.000 sequence_1: USE sequence_2: PCJUP-C3-1 targname: JUPITER-PC-CYC3 ! linenum: 44.000 sequence_1: USE sequence_2: PCJUP-C3-1 targname: JUPITER-PC-CYC3 ! linenum: 45.000 sequence_1: USE sequence_2: PCJUP-C3-1 targname: JUPITER-PC-CYC3 ! linenum: 50.000 sequence_1: USE sequence_2: PCJUP-C3-2 targname: JUPITER-PC-CYC3 req_1: SEQ 50-51 NO GAP; req_2: AFTER 40 BY 19.3H +/-0.5H comment_1: AVOID RED SPOT ! linenum: 51.000 sequence_1: USE sequence_2: PCJUP-C3-2 targname: JUPITER-PC-CYC3 ! ! end of exposure logsheet ! No scan data records found