! File: 3307C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:02:28:25 coverpage: title_1: URANUS AND NEPTUNE BELOW 3000 A: CYCLE 2 sci_cat: SOLAR SYSTEM sci_subcat: GIANT PLANETS proposal_for: GTO/OS cont_id: 1290 pi_fname: JOHN pi_mi: J. pi_lname: CALDWELL pi_inst: YORK UNIVERSITY pi_country: CANADA pi_phone: (416)665-5449 keywords_1: URANUS, NEPTUNE, ATMOSPHERIC CHEMISTRY, AURORAE hours_pri: 5.75 num_pri: 2 pi_position: PROFESSOR ! end of coverpage abstract: line_1: Both these planets will be observed spectroscopically from 1515 to 2280 A to line_2: search for atmospheric absorption features, including such possible trace gas line_3: constituents as C2H2, and also for H2 auroral emission. For Neptune, the line_4: auroral search would be in the discovery mode. For Uranus, there are already line_5: indications from other wavelengths that there is an aurora there, and the HST line_6: observations will follow the Voyager encounter, so the Uranian observations line_7: will be to improve the understanding of an established phenomenon. A line_8: complementary ultraviolet image of Uranus will be obtained, to look for line_9: structure that may be associated with the reflection spectrum. ! ! end of abstract general_form_proposers: lname: CALDWELL fname: JOHN mi: J. inst: YORK UNIVERSITY country: CANADA ! ! end of general_form_proposers block general_form_text: question: 3 section: 0 line_1: For each planet, any interactive acquisition image will be taken with the PC, line_2: and then FOS and HRS spectra will be taken. The spectra must await the results line_3: of the SV test "Spectrograph Red Leak Test," however. ! question: 4 section: 0 line_1: ST observations are required for their access to the ultraviolet. Previous line_2: space craft attempts to make these observations have been hopelessly inadequate line_3: because of low signal levels. Ground-based observations are s imply not line_4: relevant. ! question: 5 section: 0 line_1: Interactive acquisitions are needed. Otherwise, there are not special line_2: scheduling requirements. ! question: 6 section: 0 line_1: There are no special requirements ! question: 7 section: 0 line_1: Spectra will be divided by a published solar spectrum to generate an albedo line_2: curve, which will then be examined for evidence of absorption by specific line_3: molecules, of which C(sub)2H(sub)2 is the most prominent candidate, and for line_4: evidence of continuum absorption, which would probably be attributed to an line_5: aerosol. It is well known what the albedo of a clear atmosphere should be. line_7: The Uranus image will be examined for evidence of non-uniformdistribution in line_8: the continuum absorber. line_10: Toward 1600 A, auroral emission from H(sub)2 is possible. This is quickly line_11: revealed in albedo curves, because the planetary emission is much higher than line_12: any physically realistic albedo could produce. Neptune's albe do curve will be line_13: examined for any evidence of this emission. To date, there have been no line_14: detections of auroral activity on that planet by any observational technique. ! question: 8 section: 0 line_1: No additional requirements. ! question: 10 section: 0 line_1: We have a dedicated SUN computer for data reduction. ! question: 13 section: 1 line_1: FOS and HRS spectra of both planets from 1515 to 2280 A will be examined line_2: both for auroral emission and atmospheric absorption features. The latter line_3: potentially include C2H2. A complementary ultraviolet image of Uranus line_4: will also be obtained. ! !end of general form text general_form_address: lname: CALDWELL fname: JOHN mi: J. category: PI inst: YORK UNIVERSITY ! ! end of general_form_address records ! No fixed target records found solar_system_targets: targnum: 1 name_1: URANUS descr_1: PLANET URANUS lev1_1: STD = URANUS fluxnum_1: 1 fluxval_1: V=5.5 fluxnum_2: 2 fluxval_2: F(1800)=8E-15 fluxnum_3: 3 fluxval_3: F(2200)=2E-13 ! targnum: 2 name_1: NEPTUNE descr_1: PLANET NEPTUNE lev1_1: STD = NEPTUNE wind_1: WND1=22-MAY-91 TO 20-AUG-91 fluxnum_1: 1 fluxval_1: V=7.7 fluxnum_2: 2 fluxval_2: F(1800)=1.3E-15 ! ! end of solar system targets ! No generic target records found exposure_logsheet: linenum: 1.000 targname: URANUS config: PC opmode: IMAGE aperture: ANY sp_element: F555W num_exp: 1 time_per_exp: 15S fluxnum_1: 1 priority: 1 req_1: CYCLE 2 / 1-4; INT ACQ FOR 2-3; req_2: GUID TOL 0.02" ! linenum: 2.000 targname: URANUS config: FOS/BL opmode: ACCUM aperture: 4.3 sp_element: G190H wavelength: 1900 num_exp: 5 time_per_exp: 6M s_to_n: 40 fluxnum_1: 2 priority: 1 req_1: GUID TOL 0.1" comment_1: DEPENDS ON THE SV "SPECTROGRAPH RED comment_2: LEAK TEST" ! linenum: 3.000 targname: URANUS config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1657 num_exp: 8 time_per_exp: 15M s_to_n: 6 fluxnum_1: 2 priority: 1 req_1: GUID TOL 0.05" ! linenum: 4.000 targname: URANUS config: FOC/288 opmode: IMAGE aperture: 512X512 sp_element: F220W num_exp: 1 time_per_exp: 15M s_to_n: 30 fluxnum_1: 3 priority: 1 req_1: GROUP 2 - 4 WITHIN 4D; GUID TOL 0.01" ! ! end of exposure logsheet ! No scan data records found