! $Id: 5312,v 46.1 1994/07/27 16:28:01 pepsa Exp $ coverpage: title_1: A DEEP IMAGING SEARCH FOR THE SOURCE OF THE SHORT PERIOD COMETS: title_2: CYCLE 4 HIGH sci_cat: SOLAR SYSTEM sci_subcat: COMETS proposal_for: GO pi_fname: ANITA pi_mi: L. pi_lname: COCHRAN pi_inst: 3550 pi_country: USA pi_phone: 512-471-1471 hours_pri: 10.00 num_pri: 2 wf_pc: Y time_crit: Y off_fname: STEPHEN off_lname: MONTI off_title: SPONSORED PROJECTS off_addr_1: UNIVERSITY OF TEXAS off_city: AUSTIN off_state: TX off_zip: 78712 off_country: USA off_phone: 512-471-4363 ! end of coverpage abstract: line_1: We propose to perform a deep WFPC2 imaging search for the Kuiper Belt, line_2: the probable source of the short period comets. The search will consist line_3: of two sets of thirty 10-min exposures. Each set (total exposure time line_4: for each is 5-hour) will reach a limiting magnitude of 28.5, or down line_5: to objects of radius = 11 km if they have albedo = 0.04 and are at 40 AU. line_6: The search will be complete down to this size. line_7: If reasonable assumptions are made about initial surface density line_8: distribution, albedo and minimum size of a body which could be seen line_9: as a short period comet, we would expect to see between 12 and 65 line_10: Kuiper belt objects. This is in marked contrast to ground-based line_11: studies which are limited to relatively large objects (radius > 55 km) line_12: which are atypical of short period comets. Whereas the ground-based line_13: searches have proved the existence of bodies in the region of the line_14: Kuiper belt, they are unable to prove the belt contains objects that line_15: are the size of short period comets, nor can they define the size line_16: distribution. The HST survey we propose will either confirm the link line_17: between short period comets and the Kuiper belt, or it will place line_18: severe constraints on the size distribution of objects in the belt. ! ! end of abstract general_form_proposers: lname: COCHRAN fname: ANITA mi: L. inst: 3550 country: USA esa: N ! lname: DUNCAN fname: MARTIN mi: J. inst: 3440 country: USA esa: N ! lname: LEVISON fname: HAROLD mi: F, inst: 3440 country: USA esa: N ! lname: STERN fname: SOL mi: A. inst: 3440 country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We propose 2 sets of observations with WFPC2. Each set of WFPC2 observations line_2: consists of thirty 10-min integration ``Wide V'' (F606W) frames which total line_3: to 5-hours total integration per set. Each individual 5-hour set needs to line_4: be collected in a single 24-hour period. There should be no spacecraft roll line_5: between frames in a set of observations. We will collect data with all three line_6: WF chips and the PC chip. The combined field of view is 5.3 arcmin**2. line_8: The fields to be imaged consist of fields along the ecliptic but not within line_9: 20 deg of the galactic plane. Fields will be chosen to be of dark clouds line_10: to minimize the number of background stars. We have a list of two dozen such line_11: fields spread over 24 hours of RA. We specify here one such field which line_12: was chosen because of its good position and blankness. We propose to observe line_13: this field twice, 6 months apart, at quadrature. This is our preferred line_14: field but we can supply coordinates of any of the other fields on our line_15: list in the event that it is not possible to obtain the observations of line_16: this particular field. line_18: This program should be run in fine lock. ! question: 4 section: 1 line_1: Objects in the Kuiper belt are expected to have albedos of a few percent. line_2: With an inner distance of the belt of 40 au, objects should line_3: be quite faint. Several ground-based searches have been performed line_4: with limiting magnitudes up to m=25. Objects of this magnitude line_5: at 40 au and 4% albedo would have radii of 55km. It is not expected that line_6: ground-based searches can reach fainter limiting magnitudes for moving line_7: objects in the foreseeable future because they are limited by sky line_8: brightness and seeing. Indeed, even the Keck telescope will suffer from line_9: sky-brightness limits which will dominate the signal of these faint objects. line_10: Additionally, very long observations of moving objects suffer from line_11: confusion limits due to motion of the object resulting in substantial line_12: star trails. Still, ground-based searches DID find 2 objects with line_13: radii ~100km. Most SPCs are much smaller than 55km so, in order line_14: to search for progenitors of the typical SPC, it is necessary to push line_15: the limiting magnitudes down as far as possible, but to do this with line_16: integrations which don't span such a long time that objects disappear line_17: from the field of view. This last constraint makes an orbiting telescope line_18: necessary. HST is the only orbiting telescope with deep-sky imaging line_19: capabilities. ! question: 5 section: 1 line_1: We require that there be no roll during or between 10-min exposures for each line_2: 30-exposure set. This is necessary so that we can co-register the images line_3: to reach our deep limiting magnitude. line_5: We also require that each complete set of thirty 10-min exposures line_6: be completed within a 24-hour period. The objects will be moving line_7: 5-6 pixels/hour so in a 24-hour period they will move 120-144 pixels. line_8: This will result in objects being lost in some of the 10-min exposures. line_9: However, even in 24-hours, at most 7% of the Kuiper belt field would line_10: suffer from decreased S/N. We would prefer if the observations could line_11: be completed in the minimum possible time, allowing for earth occultations line_12: and guide star reacquisitions. ! question: 6 section: 1 line_1: No special calibrations required. Normal flat fields will be sufficient. line_2: We will also use the standard calibration standard area for approximate line_3: photometry. ! ! ! question: 8 section: 1 line_1: NONE ! question: 9 section: 1 line_1: Cycle 1: P4024 High Resolution UV Spectroscopy of Triton (Stern, PI); line_2: Cycle 1: P2560 UV Rotational Light Curves of Pluto, and Charon's line_3: UV Spectrum (Stern, CoI); line_4: Cycle 2: P3803 CO Abundance and FUV Survey (Stern, CoI). line_5: Cycle 2: P4005 Observations of Jovian Aurora in Support of Ulysses (Stern, PI); line_6: Cycle 3: P4462 Deep UV Spectroscopy of Triton (Stern, CoI); line_8: None of the above programs are related to this proposal. line_10: To date, the Pluto observations have not been completed. However, line_11: the final Triton Cycle 1 (P4024) FOS data were obtained in May 1992, and have line_12: now been analyzed (Stern et al. 1993). This spectrum was made at a different line_13: orbital longitude (and therefore rotational epoch) than the IUE data, and line_14: has been compared to the reduced IUE spectra. It (i) confirms that Triton's line_15: UV lightcurve amplitude is higher than in any of the Voyager color filters, line_16: (ii) shows that Triton's UV color slope varies with rotational aspect, and line_17: (iii) most importantly, reveals a suite of complex absorption features not line_18: detectable in previous, IUE studies. Our Cycle 3 Triton program, which will line_19: make more detailed studies of Triton's UV spectrum, has not yet been carried line_20: out. line_22: The Jupiter program (GO P4005) yielded eight FOC F130M/F145W line_23: images of the aurora of Jupiter taken in conjunction with the flyby of the ! question: 9 section: 2 line_1: Ulysses spacecraft in 1992. We have reduced and analyzed these images. line_2: Results were presented at a workshop in 1992 (Waite et al. 1992) and are now line_3: being prepared for publication (Waite, Stern et al. 1993). The images line_4: clearly demonstrate that the spatial morphology of the Jovian aurora are line_5: significantly more complex than IUE-investigators were led to believe. line_7: Papers Published: line_8: "HST Ultraviolet Spectroscopy of Triton: Evidence for Complex Surface line_9: Absorbers", Stern, S. A., L. M. Trafton, and D. Cruikshank. line_10: Astrophysical J. Lett. Submitted, 1993. line_12: "Multispectral Observations of the Jupiter Aurora", Waite, J. H., line_13: M. McGrath, L.M. Trafton, S. A. Stern, and G. R. Gladstone line_14: Proc. International Workshop on Time Variable Phenomena in the Jovian line_15: Planetary System, Annapolis, Md. July 13-16, 1992. line_17: "HST and ROSAT Images of the Jovian Aurora: A New Paradigm?", line_18: Waite, J. H., S. A. Stern, F. Bagenal, M. McGrath, L. M. Trafton, and line_19: G. R. Gladstone. JGR In preparation, 1993. ! question: 10 section: 1 line_1: The nominal data reduction will be performed on a SPARCStation 10 model 41 line_2: which was obtained from NASA Planetary Astronomy funds and is currently line_3: on-site and operational at The University of Texas. The software line_4: to perform the reduction will be the IRAF and STSDAS packages. line_5: These packages are installed and operational and fully supported by line_6: staff at The University of Texas. line_8: The search for moving objects will be performed independently at line_9: two sites, The University of Texas and Southwest Research Institute line_10: (SwRI). The equipment used at The University of Texas is described line_11: above. SwRI will supply a SPARCStation IPC for this purpose. This line_12: workstation was purchased through internal capital equipment funds. line_14: Modeling of the Kuiper belt will be performed on an HP9000 model line_15: 735 and an HP9000 model 720 at SwRI. These workstations were purchased line_16: through internal capital equipment funds. line_18: SwRI will not charge overhead on travel. ! !end of general form text general_form_address: lname: COCHRAN fname: ANITA mi: L. category: PI inst: 3550 addr_1: DEPARTMENT OF ASTRONOMY addr_2: UNIVERISITY OF TEXAS city: AUSTIN state: TX zip: 78712 country: USA phone: 512-471-1471 telex: 512-471-6016 ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: FIELD-034120+193441 descr_1: G,505 pos_1: RA = 03H 41M 20.0S +/- 0.25S, pos_2: DEC = +019D 34' 41" +/- 03" equinox: 2000 pm_or_par: N pos_epoch_bj: B pos_epoch_yr: 2000.00 comment_1: TARGET IS A DARK CLOUD BORDERING comment_2: BETWEEN PISCES & ARIES, ESSENTIALLY comment_3: ON THE ECLIPTIC. WE ARE USING THIS comment_4: DARK CLOUD AS A SUITABLE BACKGROUND comment_5: TO SEARCH FOR OBJECTS IN THE THIN, comment_6: ECLIPTIC-CENTERED KUIPER COMET BELT fluxnum_1: 1 fluxval_1: V=26.5+/-2.0 fluxnum_2: 1 fluxval_2: B-V=0.7 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 30M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES req_1: CYCLE 4 /1-2.8; req_2: PCS MODE F / 1-2.8; req_3: POS TARG -28.7, 10.3 /1.0-1.8; req_4: SAME ORIENT FOR 1.1-1.8 AS 1.0; req_5: SEQ 1.0-1.8 within 24h; comment_1: 1) ROLL ORIENTATION MUST BE FIXED FOR comment_2: THE 30 EXPOSURES. WE TAKE DATA IN ALL comment_3: 4 WFPC2 CHIPS. ALL 30 OF THE 10M comment_4: EXPOSURES SHOULD OCCUR IN THE MINIMUM comment_5: TIME, AND MUST OCCUR IN <24 TO FINISH. comment_6: AT 20-AUG-94+/-3D ! linenum: 1.100 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 2 ! linenum: 1.20 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 3 ! linenum: 1.300 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 4 ! linenum: 1.400 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 30M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 5 ! linenum: 1.500 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 6 ! linenum: 1.600 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 7 ! linenum: 1.700 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 8 ! linenum: 1.800 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 1 param_1: CLOCKS=YES comment_1: ORBIT 9 ! ! Six months later... ! linenum: 2.000 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 30M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES req_1: ORIENT 180D +/- 0D FROM 1.000; req_2: POS TARG -28.7, 10.3 /2.000; req_3: SAME ORIENT FOR 2.1-2.8 AS 2.0; req_4: SEQ 2.0-2.8 within 24h; comment_1: 1) ROLL ORIENTATION MUST BE FIXED FOR comment_2: THE 30 EXPOSURES. WE TAKE DATA IN ALL comment_3: 4 WFPC2 CHIPS. ALL 30 OF THE 10M comment_4: EXPOSURES SHOULD OCCUR IN THE MINIMUM comment_5: TIME, AND MUST OCCUR IN <24 TO FINISH. comment_6: AT 16-FEB-95+/-3D ! linenum: 2.100 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 2 ! linenum: 2.200 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 3 ! linenum: 2.300 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 4 ! linenum: 2.400 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 30M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 5 ! linenum: 2.500 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 6 ! linenum: 2.600 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 7 ! linenum: 2.700 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 8 ! linenum: 2.800 targname: FIELD-034120+193441 config: WFPC2 opmode: IMAGE aperture: WFALL-FIX sp_element: F606W num_exp: 1 time_per_exp: 34M s_to_n: 4 s_to_n_time: 300M fluxnum_1: 1 priority: 2 param_1: CLOCKS=YES comment_1: ORBIT 9 ! ! end of exposure logsheet ! No scan data records found