! File: 2417C.PROP ! Database: PEPDB ! Date: 17-FEB-1994:06:08:00 coverpage: title_1: CAS A: THE REMNANT OF A MASSIVE SUPERNOVA sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO 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: ABUNDANCES, NUCLEOSYNTHESIS, SUPERNOVA REMNANTS hours_pri: 9.00 num_pri: 2 wf_pc: Y funds_amount: 51000 funds_length: 12 funds_date: JAN-91 pi_position: PROFESSOR OF ASTRON. ! end of coverpage abstract: line_1: The remnants of recent supernovae provide the best opportunity to probe the line_2: evolution of massive stars and the synthesis of heavy elements. line_3: Among the remnants with fast moving, undiluted debris, line_4: the best known is Cas A. line_5: We have obtained extensive ground-based data on Cas A. line_7: The results provide valuable insights into the ages, line_8: composition, and kinematics of the remnant, but are imcomplete in line_9: tantalizing ways that HST can resolve. While we are confident Cas A line_10: results from the violent destruction of a massive star after advanced line_11: nuclear burning, essential features of the explosion physics, the line_12: excitation of the debris, the chemical composition of the ejecta, and line_13: the age, distance, and kinematics still elude our grasp. HST images line_14: will allow us to isolate the chemical inhomogeneities in the debris. line_15: The images will allow an unprecedented line_16: probe of the excitation mechanism, and will provide 10 times the angular line_17: resolution for proper motion studies to determine ages. ! ! end of abstract general_form_proposers: lname: BLAIR fname: WILLIAM mi: P. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: LONG fname: KNOX mi: S. inst: JOHNS HOPKINS UNIVERSITY country: USA ! lname: WINKLER fname: P. mi: F. inst: MIDDLEBURY COLLEGE country: USA ! lname: KIRSHNER fname: ROBERT title: P.I. mi: P. inst: CFA country: USA ! lname: RAYMOND fname: JOHN mi: C. inst: CFA country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 0 line_1: No new scientific justification is needed. ! question: 3 section: 1 line_1: Imaging observations will be carried out with line_2: WFC of the supernova remnant Cas A. The filters line_3: selected will give images in [O I], [O III], [S II] line_4: H-alpha, and a continuum band. These will allow us line_5: to separate the fast-moving oxygen rich ejecta from line_6: the slow moving flocculi that emit in H-alpha. In line_7: addition, the sulfur-rich knots can be separated from line_8: the oxygen-rich knots, and all the knots can be distinguished line_9: from background stars by using the continuum image. line_10: We expect to resolve the shocks, search for a stellar line_11: remnant, and set the stage for the most accurate measurement line_12: of the expansion of this recent supernova. ! question: 4 section: 1 line_1: The spatial resolution of HST is 10 times better than our line_2: ground-based data. We have extensive spectra of Cas A from line_3: 3300 angstroms out to 10000 angstroms. ! question: 5 section: 1 line_1: We have just one target, and aim to get good images of the line_2: brightest filaments. We know the surface brightness, at least line_3: as measured from the ground. Since the remnant is clumpy, we line_4: expect the surface birghtness as imaged with WFC to be higher. line_5: Scaling from our 4-m images, we expect about 300 photons per pixel line_6: in a 2500s integration. Basically, we would like to expose as long line_7: possible in the emission lines of interest- but 1 orbit seems a line_8: natural way to set the integration time. ! question: 7 section: 1 line_1: The image data from HST are similar to data we have from current line_2: TI CCD's. We have IRAF line_3: going on a Decstation 3100. It should be no special line_4: problem to get STSDAS going on the same machines. On the other hand, line_5: we expect to spend a large amount of effort characterising the line_6: individual knots and their spectra. In principle, this can be combined line_7: with the kinematic survey that Winkler has carried out. We also line_8: expect to use the continuum image to remove all the stars from all the line_9: emission-line images, and to try image resoration using a maximum line_10: entropy technique. This is a lot of processing, so even though the line_11: number of images is small, it will occupy somebody for most of a year line_12: to get the most out of the data. That is why the budget request is for line_13: the support of a student for a year. ! question: 8 section: 1 line_1: Our intent with Cas A is to measure proper motions and to monitor line_2: long-term changes, which are known to take place on a scale of line_3: years. We would like to retain the data rights to proper motion line_4: analysis, which will require a repeat observation in the next decade. ! question: 10 section: 1 line_1: The current computer facilities were all purchased by Harvard, line_2: and we expect a Harvard graduate student will undertake the detailed line_3: analysis under Kirshner's direct supervision. Support for the Co-I's, line_4: or for Kirshner is not requested. The use of all the local talent line_5: and facilities for image processing, and the interactions with a wide line_6: range of people interested in stellar evolution, nuclear astrophysics, line_7: atomic physics, and X-ray astronomy at the CfA is an important, if line_8: intangible contribution. ! !end of general form text general_form_address: lname: KIRSHNER fname: ROBERT mi: P. title: PROF. category: PI inst: HARVARD COLLEGE OBSERVATORY addr_1: 60 GARDEN STREET city: CAMBRIDGE state: MA zip: 02138 country: USA ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: CASSIOPEIA-A-NE descr_1: INTERSTELLAR MEDIUM descr_2: SUPERNOVA REMNANT pos_1: RA = 23H 21M 17.0S +/- 0.1S, pos_2: DEC = +58D 33' 25.0" +/- 1" equinox: 1950.0 rv_or_z: V = 0 comment_1: THIS IS A PURE EMISSION-LINE comment_2: OBJECT THAT IS VERY CLUMPY. comment_3: THE LINES ARE (USUSALLY) NARROWER comment_4: THAN THE FILTERS,BUT THE LINE WIDTH comment_5: GIVEN IS FICTITIOUS. comment_6: WHEN THE LINE WIDTH GIVEN IS comment_7: MULTIPLIED BY THE SURF_BRIGHTNESS comment_8: GIVEN, THE OBSERVED FLUX RESULTS. comment_9: PLEASE DO NOT ALTER EXPOSURE TIMES comment_10: WITHOUT UNDERSTANDING THESE ISSUES fluxnum_1: 1 fluxval_1: SURF-LINE(5007) = 3 +/- 3 E-16 fluxnum_2: 2 fluxval_2: W-LINE(5007) = 10 +/- 5 fluxnum_3: 3 fluxval_3: SURF-LINE(6300) = 1 +/- 1 E-16 fluxnum_4: 4 fluxval_4: W-LINE(6300) = 10 +/- 5 fluxnum_5: 5 fluxval_5: SURF-LINE(6732) = 3 +/- 3 E-16 fluxnum_6: 6 fluxval_6: W-LINE(6732) = 10 +/- 5 fluxnum_7: 7 fluxval_7: SURF-LINE(6562) = 1 +/- 1 E-16 fluxnum_8: 8 fluxval_8: W-LINE(6562) = 10 +/- 5 ! targnum: 2 name_1: HD3360-CALIB descr_1: STAR pos_1: RA = 0H 36M 58.2S +/- 0.1S, pos_2: DEC = +53D 53' 49.0" +/- 1" equinox: 2000.0 rv_or_z: V = 0 comment_1: TO MEASURE PSF THROUGH FILTERS fluxnum_1: 1 fluxval_1: V = 3.67 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: CASSIOPEIA-A-NE config: WFC opmode: IMAGE aperture: ALL sp_element: F502N wavelength: 5019 num_exp: 1 time_per_exp: 1900S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PRE-FLASH=YES, param_2: CLOCKS=YES param_3: CR-SPLIT=NO req_1: CYCLE 1 / 1-9 ; req_2: SEQUENTIAL 1-9 NO GAP ! linenum: 1.100 targname: CASSIOPEIA-A-NE config: WFC opmode: IMAGE aperture: ALL sp_element: F502N wavelength: 5019 num_exp: 2 time_per_exp: 2100S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PRE-FLASH=YES, param_2: CLOCKS=YES param_3: CR-SPLIT=NO req_1: CYCLE 1 / 1-9 ; req_2: SEQUENTIAL 1-9 NO GAP ! linenum: 2.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F656N wavelength: 6559 num_exp: 3 time_per_exp: 2100S s_to_n: ^ fluxnum_1: 7 fluxnum_2: 8 priority: 2 param_1: ^ req_1: SAME ORIENT FOR 2-5 AS 1 ! linenum: 3.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F631N wavelength: 6307 num_exp: 3 time_per_exp: 2100S s_to_n: ^ fluxnum_1: 3 fluxnum_2: 4 priority: 2 param_1: ^ req_1: ^ ! linenum: 4.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F673N wavelength: 6727 num_exp: 3 time_per_exp: 2100S s_to_n: ^ fluxnum_1: 5 fluxnum_2: 6 priority: 1 param_1: ^ req_1: ^ ! linenum: 5.000 sequence_1: ^ targname: ^ config: ^ opmode: ^ aperture: ^ sp_element: F547M wavelength: 5462 num_exp: 2 time_per_exp: 500S s_to_n: ^ fluxnum_1: ^ priority: 2 param_1: ^ req_1: ^ ! linenum: 6.000 targname: HD3360-CALIB config: WFC opmode: IMAGE aperture: ALL sp_element: F502N wavelength: 5019 num_exp: 1 time_per_exp: 0.11S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_3: CR-SPLIT=NO req_2: GUID TOL 0.1" / 6-9 ! linenum: 7.000 targname: HD3360-CALIB config: WFC opmode: IMAGE aperture: ALL sp_element: F656N wavelength: 6559 num_exp: 1 time_per_exp: 0.11S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_3: CR-SPLIT=NO ! linenum: 8.000 targname: HD3360-CALIB config: WFC opmode: IMAGE aperture: ALL sp_element: F631N wavelength: 6307 num_exp: 1 time_per_exp: 0.11S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_3: CR-SPLIT=NO ! linenum: 9.000 targname: HD3360-CALIB config: WFC opmode: IMAGE aperture: ALL sp_element: F673N wavelength: 6727 num_exp: 1 time_per_exp: 0.11S fluxnum_1: 1 priority: 1 param_1: PRE-FLASH=YES, param_3: CR-SPLIT=NO ! ! end of exposure logsheet ! No scan data records found