! File: 4252C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:19:06:41 coverpage: title_1: SINS: LATE TIME OBSERVATION OF SN1992A sci_cat: INTERSTELLAR MEDIUM proposal_for: GO large_proj: X targ_of_opp: X longterm: 3 cont_id: 4016 pi_title: PROF. pi_fname: ROBERT pi_mi: P. pi_lname: KIRSHNER pi_inst: CFA pi_country: USA pi_phone: 617-495-7519 keywords_1: SUPERNOVA, NUCLEOSYNTHESIS, keywords_2: INTERSTELLAR ABSORPTION, GALAXY DISTANCES hours_pri: 180.70 num_pri: 4 wf_pc: N foc: Y fos: Y hrs: N hsp: N realtime: N time_crit: Y funds_amount: 1 funds_length: 36 funds_date: JAN-91 pi_position: PROFESSOR ! end of coverpage abstract: line_1: Supernovae are stars at the end of stellar evolution. They mark the moment of line_2: stellar destruction, act as the key process in the chemical evolution of the line_3: universe, serve as agitators and probes of the interstellar medium, and provide line_4: sharp and useful tools for cosmological investigations. The spatial resolution line_5: and ultraviolet ability of Space Telecope make it an essential tool in line_6: furthering all of these aspects of supernova research. As SN 1987A has line_7: demonstrated, the best progress in this field comes from the detailed study line_8: of the brightest objects. Many of the central problems of supernova research can line_9: be attacked by intensive and extensive observations of a handful of moderately line_10: bright supernovae using the HST cameras and spectrographs over an extended line_11: period of time. Observations at the latest times may be the simplest to line_12: interpret and provide the best probe of the stellar interior. SN 1987A provides line_13: a unique opportunity to connect the evolution of a supernova with the line_14: development of a supernova remnant and will be studied in this program. Because line_15: supernovae touch on so many fields of astronomy, the results of this line_16: study will affect a broad range of areas from stellar line_17: interiors to cosmology. ! ! end of abstract general_form_proposers: lname: BRANCH fname: DAVID inst: OKLAHOMA, UNIVERSITY OF country: USA ! lname: FRANSSON fname: CLAES inst: STOCKHOLM OBSERVATORY country: SWEDEN esa: X ! lname: WAGONER fname: ROBERT inst: STANFORD UNIVERSITY country: USA ! lname: WHEELER fname: J. CRAIG inst: TEXAS, UNIVERSITY OF country: USA ! lname: CHEVALIER fname: R. inst: VIRGINIA, UNIVERSITY OF country: USA ! lname: KIRSHNER fname: ROBERT title: P.I. mi: P. inst: CFA country: USA ! lname: PANAGIA fname: NINO inst: STSCI country: USA esa: X ! lname: BLADES fname: J. CHRIS inst: STSCI country: USA esa: X ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: HST observations of supernovae will advance understanding of stellar evolution line_2: nucleosynthesis, the interstellar gas of our Galaxy, and other galaxies, line_3: and extragalactic distances. Intense study of a few bright objects is the way line_4: to make the best progress, as SN 1987A has shown. We intend to use the superb line_5: imaging and unparalleled ultraviolet capabilities of HST on a few bright line_6: supernovae, including SN 1987A, to gather long sets of observations that will line_7: help answer important questions over a broad range of astrophysics. line_9: Supernovae are the ultimate event in stellar evolution: our goal is to line_10: discover which stars explode, by what mechanism and with what nuclear products. line_11: Type II supernovae appear to be massive stars which have suffered a core line_12: collapse. SN Ib seem to be similar stars which have had an extensive episode line_13: of mass loss before the collapse, and SN Ia seem to result from the line_14: thermonuclear deflagration of white dwarf stars. Direct evidence on these line_15: mechanisms will result from spectroscopy and photometry of the events with line_16: HST. line_18: Supernovae are also the best probes of the interstellar gas, both in our Galaxy line_19: and in the galaxy that hosts the supernova. A proper analysis of the UV line_20: spectrum can provide information on the ionization, gas-phase abundances, and line_21: kinematics of the interstellar gas. ! question: 3 section: 1 line_1: As approved by the time allocation committee, we will concentrate line_2: on SN 1987A in the first year. In addition, we will carry out late time line_3: observations of a supernova studied at early times line_4: Macchetto et al., which we call SN 1991N. line_6: The SN 1987A observations will include spectroscopy and photometry of the line_7: supernova and the circumstellar gas, as well as a few special observations. line_8: Brief FOS observations of stars 2 and star 3 are substituted for the HRS line_9: observations orignally proposed. These will be very helpful in separating line_10: the contribution of SN 1987A from its neighbors. ! question: 3 section: 2 line_1: In each of the subsequent years of the SINS project, we intend to observe one line_2: new supernova as a target of opportunity. This will include the extensive HRS line_3: study that will be omitted in the first year's work. In addition, we will line_4: continue to follow SN 1987A. line_6: In the third year of this project, we will continue the observations of SN 1990N line_7: if practical, follow the late evolution of the supernova from the second year, line_8: and add a third object as a target of opportunity. ! question: 4 section: 1 line_1: HST is much more powerful for UV spectroscopy than IUE, which line_2: we have employed in the past. We can use its excellent imaging to create long line_3: light curves that test the models for energy sources at late times. line_5: For SN1987A, HST observations will be possible just at the time when line_6: ground-based observations become very difficult due to the two neighbor stars. ! question: 5 section: 1 line_1: This project has many uncertainties in the exposure times, and the positions line_2: of the targets. For SN 1987A, we have some clues, but we may have to revise our line_3: estimates based on information obtained from the ground in 1991 or from the line_4: earliest GTO work. We have been allocated 33h for SN 1987A in C1. line_5: For SN 1991N, we hope to circumvent some of the difficulties of a Target of line_6: opportunity by restricting observations to 12h of an object already studied on line_7: the ground. line_8: The Target of Opportunity observations will not begin until 1992. line_9: on reasonable, though uncertain, estimates of the UV flux and other supernova line_10: properties. We expect to use 44.6 hours in the first year (C2) and 14.5 h in line_11: the second year (C3). ! question: 6 section: 1 line_1: The SN1987A observations do not require real time observations, nor do the line_2: of SN 1991N planned for the first year. The newly-discovered supernovae of line_3: 1992 and of 1993 will require real time observations in order to move promptly line_4: to establish the position of the object and begin to gather the UV line_5: spectra before the object fades. ! question: 7 section: 1 line_1: The supernovae we study will be those that are bright enough and suitably line_2: located for thorough work from the ground and from HST. We have rapid access to line_3: reports of new supernovae to the IAU in Cambridge. Panagia and Blades are at line_4: ST ScI to initiate real-time work. Spectroscopic and image data can be reduced line_5: in Cambridge, we already have IRAF in routine use, and expect to get STSDAS. line_6: Each team site will have a similar workstation so that data display and transfer line_7: is easy. Analysis will include use of model atmopsheres by Branch, Wheeler, and line_8: Wagoner. Interstellar observations will be of special interest to Blades, line_9: Panagia, Chevalier, and Fransson. line_10: Kirshner will handle the late-time light curves and low-resolution line_11: spectra for use in determining the energy supply at late times and the line_12: chemistry of the star's interior. The complete team will meet at least once line_13: each year to prepare publications and discuss future plans. ! question: 8 section: 1 line_1: We will obtain coordinated ground-based data using the MMT and the VLA. line_2: We have proposed for the use of KPNO to follow light curve to the point where line_3: only HST can continue. We continue to press forward with our IUE observations line_4: that should help with the inital work on SN 1987A. ! question: 9 section: 1 line_1: We have not received any previous HST time. ! question: 10 section: 1 line_1: Our institutions provide the ground-based observatories for this work. line_2: They also provide salary support for many of the Co-I's: salary requests line_3: for senior people reflect only a fraction of their effort on this project. line_4: Students typically receive tuition waivers or fellowship support. We have line_5: requested workstations for the US Co_I's which will be connected to file servers line_6: purchased by the universities. Although our budget provides for a programmer or line_7: data aide to help get the computers set up and keep them running as the data line_8: flows in, a great deal of support comes from other systems people at the CfA who line_9: are not supported by this project. The telescope allocation committee made a line_10: minor change in the time for this project, but the basic types of work to be line_11: carried out are not changed, and the full participation of each member line_12: of the team is required. For that reason, we have not altered our proposed line_13: budget. ! !end of general form text general_form_address: lname: KIRSHNER fname: ROBERT mi: P. title: PROF. category: PI inst: CFA addr_1: 60 GARDEN STREET city: CAMBRIDGE state: MA zip: 02138 country: USA ! ! end of general_form_address records fixed_targets: targnum: 5 name_1: SN1992A descr_1: EXT-STAR descr_2: SUPERNOVA pos_1: RA = 3H 34M 31.52S +/- 0.4S, pos_2: DEC = -35D 7' 22.5" +/- 0.6" equinox: 1950.0 acqpr_1: COMP comment_1: THE SUPERNOVA IS FADING, SO comment_2: MAGNITUDE DEPENDS ON TIME. I comment_3: ASSUME SEPT 92. fluxnum_1: 1 fluxval_1: V = 19.0 +/- 1.0 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 54.100 sequence_1: DEFINE sequence_2: SN91SPEC2 targname: SN1992A config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 100S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: BRIGHT = 33000 param_2: FAINT = 330 req_1: ONBOARD ACQ FOR 54.200; req_2: SEQ 54.1-54.4 NO GAP; comment_1: 54.1- 54.4 HAVE ACQ-BINARY ! linenum: 54.200 sequence_1: DEFINE sequence_2: SN91SPEC2 targname: # config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G160L wavelength: 1650-2503 num_exp: 1 time_per_exp: 1500S s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 54.300 sequence_1: DEFINE sequence_2: SN91SPEC2 targname: # config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G270H wavelength: 2230-3309 num_exp: 1 time_per_exp: 1500S s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 54.400 sequence_1: DEFINE sequence_2: SN91SPEC2 targname: # config: FOS/RD opmode: ACCUM aperture: 4.3 sp_element: G400H wavelength: 3250-4831 num_exp: 1 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 57.000 sequence_1: USE sequence_2: SN91SPEC2 targname: SN1992A time_per_exp: X4.0 req_1: AT 15-SEP-92 +/- 60D; req_2: CYCLE 1 / 57; comment_1: SEQUENCE HAS BINARY ACQ ! linenum: 62.000 sequence_1: DEFINE sequence_2: SN91PHOT targname: # config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F342W num_exp: 1 time_per_exp: 500S s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 63.000 sequence_1: DEFINE sequence_2: SN91PHOT targname: # config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F275W num_exp: 1 time_per_exp: 500S s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 64.000 sequence_1: DEFINE sequence_2: SN91PHOT targname: # config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F175W num_exp: 1 time_per_exp: 1000S s_to_n: 10 fluxnum_1: 1 priority: 2 ! linenum: 68.000 sequence_1: USE sequence_2: SN91PHOT targname: SN1992A time_per_exp: X2.0 req_1: AT 15-SEP-92 +/- 60D; req_2: CYCLE 1 / 68; ! ! end of exposure logsheet ! No scan data records found