! $Id: 5203,v 4.1 1994/07/27 15:53:09 pepsa Exp $ coverpage: title_1: SUPERNOVA 1987A sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GTO/WF2 pi_title: DR. pi_fname: JOHN pi_mi: T. pi_lname: TRAUGER pi_inst: JPL pi_country: USA pi_phone: (818) 354-9594 hours_pri: 3.86 num_pri: 1 wf_pc: Y time_crit: N pi_position: PROJECT SCIENTIST off_fname: JOHN off_mi: T. off_lname: TRAUGER off_title: DR. off_inst: JET PROPULSION LABORATORY off_addr_1: 4800 OAK GROVE DRIVE off_addr_2: MAIL STOP 179-225 off_city: PASADENA off_state: CA off_zip: 91109 off_country: USA off_phone: (818) 354-9594 ! end of coverpage abstract: line_1: We observe the remnant from the SN1987A in the optical continuum, and [OIII] line_2: in order to attempt a detection of the neutron star. The [OIII] will also line_3: show the evolution of the ring nebula. We observe the envelope in line_4: the near ultraviolet and at H alpha in order to get the first detailed look at line_5: its morphology (with 7 PC pixels across the shell, and sub-pixel resolution) line_6: Asymmetries in the shell would give information about the geometry of the line_7: explosion, which may be related to the ring, which was produced by line_8: asymmetries in the winds from the precursor. On a finer scale, the line_9: observations will allow us to measure or constrain any inhomogeneities in the line_10: expanding shell, which might be caused by instabilities in the flow. The line_11: observations will enable the opacities of the metal and hydrogen gas line_12: components to be compared and their mixing from the explosion to be examined. ! ! end of abstract general_form_proposers: lname: TRAUGER fname: JOHN title: DR. mi: T. inst: JPL country: USA esa: N ! lname: BURROWS fname: CHRISTOPHER title: DR. mi: J. inst: STSCI country: USA esa: Y ! lname: CLARKE fname: JOHN inst: UNIV. OF MICHIGAN country: USA ! lname: CRISP fname: DAVID inst: JPL country: USA ! lname: HOESSEL fname: JOHN inst: UNIV. OF WISCONSIN country: USA ! lname: GALLAGHER fname: JAY inst: UNIV. OF WISCONSIN country: USA ! lname: GRIFFITHS fname: RICHARD inst: JOHNS HOPKINS UNIV country: USA ! lname: HESTER fname: JEFF inst: ARIZONA STATE UNIV. country: USA ! lname: HOLTZMAN fname: JOHN inst: LOWELL OBSERVATORY country: USA ! lname: MOULD fname: JEREMY inst: CALTECH country: USA ! lname: WESTPHAL fname: JAMES inst: CALTECH country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Observations are made in the four filters F547M, F502N, NF255W, and F656N. The line_2: first (cr split) 40 minute exposure through F547M looks very deeply line_3: specifically for the pulsar, or thermal or free-free emission from the plasma line_4: excited by it. There is much uncertainty about the expected optical line_5: luminousity from the neutron star, but this image will see any object brighter line_6: than about 26th visible magnitude. Given that the bolometric luminousity of the line_7: remnant is expected in some models to be dominated by the pulsar, and the line_8: nebula is already believed to be optically thin in this passband (which line_9: contains no nebular lines), we believe that this observation gives us an line_10: excellent chance of first detecting the pulsar. It may also image the dust line_11: that is known to be present in the nebula (from its emission in the infrared line_12: light curve) in reflection from the two nearby companion stars. ! question: 3 section: 2 line_1: The [OIII] image may not show the remnant nebula which is not expected to line_2: then contain doubly ionized lines in significant strength. It will see the line_3: outer ring, and allow us to study its evolution. The main point of the line_4: observation however, is that the pulsar can excite this line in its local line_5: environment. The 40min exposure time is based on the FOC experience (they used line_6: 2200 s, when the ring nebula was more luminous, but the FOC sensitivity before line_7: the fix is much lower). line_8: The last two filters probe the nebular emission from metal lines and H alpha line_9: respectively. The exposure times are again scaled from the FOC exposures. ! question: 4 section: 1 line_1: At present, the nebula is unresolved from the ground. On the other hand, in line_2: the WFPC2 period, it would be marginally resolvable at the best sites, but by line_3: then will be contaminated by the seeing halo particularly of star 3. In any line_4: event the resolution obtained from the ground will not approach that which line_5: we expect from HST, and would not enable the investigation proposed here. line_6: WFPC2 will therefore present the best opportunity to observe the nebula, being line_7: well matched in both resolution, dynamic range, spectral response and line_8: sensitivity. ! ! question: 10 section: 1 line_1: The proposers have workstations, software, and support for line_2: data analysis required on these images. ! !end of general form text general_form_address: lname: TRAUGER fname: JOHN mi: T. title: DR. category: PI inst: JPL addr_1: Mail stop 179-225 addr_2: 4800 Oak Grove Drive city: Pasadena state: CA zip: 91109 country: USA phone: (818) 354-9594 ! lname: BURROWS fname: CHRISTOPHER mi: J. title: DR. category: CON inst: STScI addr_1: 3700 San Martin Drive city: Baltimore state: MD zip: 21218 country: USA phone: (410) 338-4935 ! lname: KRIST fname: JOHN mi: E. category: CON inst: STScI addr_1: 3700 San Martin Drive city: Baltimore state: MD zip: 21218 country: USA phone: (410) 338-5030 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SN1987A descr_1: G,506 pos_1: RA = 5H 35M 28.0S +/- 0.1S, pos_2: DEC = -69D 16' 11" +/- 0.1" equinox: J2000 fluxnum_1: 1 fluxval_1: V=19.0 fluxnum_2: 2 fluxval_2: B-V=0.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.100 sequence_1: DEFINE sequence_2: IMAGES targname: SN1987A config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F547M num_exp: 1 time_per_exp: 40M s_to_n: 1 fluxnum_1: 1 priority: 1 param_1: ATD-GAIN=7 ! linenum: 1.200 sequence_1: DEFINE sequence_2: IMAGES targname: SN1987A config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F502N num_exp: 1 time_per_exp: 40M s_to_n: 1 fluxnum_1: 1 priority: 1 param_1: ATD-GAIN=7 ! linenum: 1.300 sequence_1: DEFINE sequence_2: IMAGES targname: SN1987A config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F255W num_exp: 1 time_per_exp: 40M s_to_n: 1 fluxnum_1: 1 priority: 1 param_1: ATD-GAIN=7 ! linenum: 1.400 sequence_1: DEFINE sequence_2: IMAGES targname: SN1987A config: WFPC2 opmode: IMAGE aperture: PC1 sp_element: F656N num_exp: 1 time_per_exp: 40M s_to_n: 1 fluxnum_1: 1 priority: 1 param_1: ATD-GAIN=7 ! linenum: 10.000 sequence_1: USE sequence_2: IMAGES req_1: CYCLE 4; req_2: SEQ 1.1-1.4 NO GAP ! ! end of exposure logsheet ! No scan data records found