! File: 2955C.PROP ! Database: PEPDB ! Date: 18-FEB-1994:00:44:05 coverpage: title_1: UV IMAGING AND SPECTROSCOPY OF S ANDROMEDAE IN M31 sci_cat: INTERSTELLAR MEDIUM proposal_for: GO/DD pi_title: DR. pi_fname: ROBERT pi_mi: A. pi_lname: FESEN pi_inst: DARTMOUTH COLLEGE pi_country: USA pi_phone: 603-646-2949 keywords_1: SUPERNOVA REMNANT, SUPERNOVAE, M31 hours_pri: 3.50 num_pri: 1 foc: Y fos: Y funds_amount: 44210 funds_length: 12 funds_date: SEP-91 pi_position: ASSISTANT PROFESSOR off_fname: JOHN off_mi: F. off_lname: KAVANAUGH off_title: DIRECTOR off_inst: DARTMOUTH COLLEGE off_addr_1: GRANTS AND CONTRACTS off_addr_2: BOX 7 off_city: HANOVER off_state: NH off_zip: 03755 off_country: USA off_phone: 603-646-3007 ! end of coverpage abstract: line_1: We recently discovered the long sought after remnant line_2: of the famous historical supernova, commonly known as line_3: S Andromedae, which occurred in 1885 in the bulge of M31. line_4: The remnant is detected optically as a dark spot of Fe I line_5: absorption at precisely the observed position of the SN event. line_6: Our detection shows that S And contains a large quantity line_7: of cold iron freely expanding at velocities up to 5000 km/s, line_8: consistent with its historical Type I classification. The line_9: remnant's inferred diameter is 0.3 - 0.5 arcsec. line_10: We propose to obtain UV FOC imaging and FOS spectroscopy line_11: of S And's remnant. From observed absorption line profiles it line_12: should be possible to determine directly density and composition line_13: as a function of radius in the freely expanding ejecta. line_14: This is a uniquely powerful observation made possible line_15: by HST's UV capability. It is important to line_16: establish first epoch observations of S And's evolving remnant line_17: at the earliest opportunity. ! ! end of abstract general_form_proposers: lname: FESEN fname: ROBERT title: DR. mi: A. inst: DARTMOUTH COLLEGE country: USA ! lname: HAMILTON fname: ANDREW title: DR. mi: J. inst: UNIVERSITY OF COLORADO, BOULDER country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: IN ORDER TO DETERMINE S AND'S PRECISE SIZE AND LOCATION, line_2: WE WILL OBTAIN AN FOC IMAGE TAKEN THROUGH THE line_3: F231M + F220W FILTER COMBINATION WHICH YIELDS A NEARLY line_4: IDEAL BANDPASS FOR OUR PURPOSE TOGETHER WITH EXCELLENT SUPPRESSION line_5: OF M31'S BULGE LIGHT ABOVE 2600 A. THIS FILTER COMBO HAS A PEAK line_6: TRANSMISSION AT 2340 A WHICH IS VERY CLOSE TO THE STRONG line_7: 2343, 2374, AND 2382 FE II LINES. (CF. FOC HANDBOOK, PG. 74). line_8: WE WILL OBTAIN A 100 MINUTE EXPOSURE WITH THE FOC AT F/96. line_9: THIS IMAGE WILL YIELD S AND'S ANGULAR SIZE line_10: AND TELL WHETHER THERE ARE ANY SMALL NEARBY DUST FEATURES TO WORRY line_11: ABOUT. ! question: 3 section: 2 line_1: WE WILL USE THE FOS/RD WITH THE line_2: 1.0" PAIR APERTURES AND G270H GRAING TO OBTAIN A SPECTRUM line_3: OF THE 2230-3309 A REGION FOR BOTH THE OBJECT (S AND) AND line_4: THE BULGE (BACKGROUND SKY). THESE SPECTRA WILL PERMIT line_5: THE DETECTION OF THE REMNANT'S FE II RESONANCE LINES line_6: AT 2343, 2383, 2586, AND 2599 A PLUS FE I RESONANCE LINES AT line_7: 2483, 2522, AND 2719 A. line_8: DUE TO THE ONE SIDED TAN S AND IS RECEIVING FROM M31'S BULGE, line_9: WE EXPECT THAT THE REMNANT'S FE I LINES WILL BE BLUESHIFTED, line_10: WHILE THE FE II LINES WILL BE REDSHIFTED. line_11: DUE TO THE `GIMP' PROBLEM, THE 2 HR TOTAL line_12: EXPOSURE TIME WILL BE BROKEN INTO MANY SHORT, 4 MIN EXPOSURES TO line_13: MITIGATE THE GIMP PROBLEM WHICH IS SEVERE FOR THE 1.0'' APERTURES. ! question: 4 section: 1 line_1: UV absorption observations of the 0.5 arcsec diameter line_2: remnant of S And use HST's UV capilities line_3: to great advantage. While some Fe I lines can line_4: be observed from the ground, all the Fe II resonance lines line_5: lie in the UV. IUE's relatively low sensitivity and large line_6: 3 arcsec aperture make spectral observations with IUE line_7: only marginal. ! question: 5 section: 1 line_1: Imaging with the FOC: line_2: Using the F231M + F220W filter combination, line_3: we estimate over 1000 cts on M31's line_4: bright nucleus and around 750 cts at S And's location in a line_5: 100 min exposure per 0.1'' resolution element. We line_6: estimate a S/N of around 25 at S And's psoition. ! question: 5 section: 2 line_1: FOS SPECTRA: line_2: At 2500 A, flux at S And's bulge position is 4E-15 ergs/s cm2 A. line_3: Using the FOS/RD digicon and the G270H grating, a total exposure line_4: time of 120 minutes in star-sky mode (i.e. 60 min on each) line_5: will result in a total of around 4000 cts on target and line_6: a S/N of 50 at 2500 A. ! question: 6 section: 1 line_1: N/A ! question: 7 section: 1 line_1: The FOC image will be useful in determining S And's precise line_2: location but not needed for offset positioning of the 1.0 arcsec line_3: aperture pairs of the FOS/RD. S And's position will be line_4: measured relative to a 14th mag star to the SW. line_5: The FOC image be also searched for evidence of other small sysmetric line_6: absorption features. We will collaborate with GTO programs line_7: obtaining WFC or FOC images of M31's bulge to help to distinguish line_8: Fe II absorbing features (other old Type I SNRs) from bulge line_9: dust clouds. FOS spectral data reduction will include accurate line_10: flux and wavelength calibrations, and equivalent width and line_11: profile measurements for both Fe I and Fe II absorption lines line_12: detected. HST data will be combined with optical ground-based line_13: Fe I spectral data to construct a detailed observational picture LINE_14: line_15: of the remnant's composition and ionization structure as a line_16: function of radius in the ejecta. These data will then be compared line_17: to deflagration and detonation exploding white dwarf models. ! question: 8 section: 1 line_1: We note that a GTO program (#1044) is planning to observe S And. line_2: Their goal, however, is the detection of the remnant through line_3: emission lines, not absorption lines, using the FOS/BL. line_4: Our discovery of the remnant supersedes their observational search line_5: and the stated exposure time for this GTO program (700 sec) is line_6: quite inadequate to detect any of the Fe I or Fe II absorption line_7: features. Moreover, the chosen grating (G130H) misses the line_8: crcial lines of Fe II at 2380 and 2600 A. ! question: 9 section: 1 line_1: NO ! question: 10 section: 1 line_1: The resources provided by Dartmouth include computer time line_2: and programming assistance for data reduction and analysis: line_3: software development, graphics, and post-processing will line_4: be carried out at the home institution. ! !end of general form text general_form_address: lname: FESEN fname: ROBERT mi: A title: DR. category: PI inst: DARTMOUTH COLLEGE addr_1: DEPARTMENT OF PHYSICS AND ASTRONOMY addr_2: WILDER HALL city: HANOVER state: NH zip: 03755 country: USA ! lname: FESEN fname: ROBERT mi: A. title: DR. category: PI inst: DARTMOUTH COLLEGE addr_1: DEPARTMENT OF PHYSICS AND ASTRONOMY addr_2: WILDER LAB city: HANOVER state: NH zip: 03755 country: USA phone: 603-646-2949 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: S-AND-FIELD name_2: SN1885 name_3: M31 descr_1: EXT-MEDIUM; DARK NEBULA; SN pos_1: RA = 00H 39M 58.84S +/- 0.2S, pos_2: DEC = +40D 59' 38.5" +/- 0.5" equinox: 1950 pm_or_par: N acqpr_1: BKG comment_1: V FLUX NOT GIVEN BECAUSE WE WILL comment_2: NOT ACQUIRE DIRECTLY ON OUR TARGET fluxnum_1: 1 fluxval_1: SURF(2500) = 4 +/-1 E-15 ! targnum: 2 name_1: S-AND-OFFSET-STAR descr_1: STAR; OFFSET STAR pos_1: RA = 00H 39M 49.4S +/-0.4S, pos_2: DEC = +40D 59' 24.0" +/-0.5" equinox: 1950 acqpr_1: BKG comment_1: CLOSER BUT FAINTER OFFSET STAR CAN comment_2: BE CHOSEN IF NEEDED. fluxnum_1: 1 fluxval_1: V = 12.32 +/- 0.1 ! targnum: 3 name_1: S-ANDROMEDAE name_2: SN1885-SNR descr_1: EXT-MEDIUM; DARK NEBULA; SN pos_1: TBD-EARLY, pos_2: RA = 00H 39M 58.84S +/- 0.2S, pos_3: DEC = +40D 59' 38.5" +/-0.5" equinox: 1950 acqpr_1: BKG comment_1: COORDINATES MAY BE UPDATED comment_2: BASED ON FOC IMAGES fluxnum_1: 1 fluxval_1: SURF(2500) = 4 +/-1 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: S-AND-FIELD config: FOC/96 opmode: IMAGE aperture: 512X512 sp_element: F231M,F220W wavelength: 2340 num_exp: 10 time_per_exp: 600S s_to_n: 15 s_to_n_time: 6000S fluxnum_1: 1 priority: 1 req_1: CYCLE 1 comment_1: M31'S NUCLEUS MAY PRODUCE comment_2: 120 CTS PER 0.1'' ELEMENT comment_3: DURING EACH 20 MIN EXPOSURE. ! linenum: 2.000 targname: S-AND-OFFSET-STAR config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 3.0S priority: 1 param_1: BRIGHT = 330000, param_2: FAINT = 3300 req_1: CYCLE 1; req_2: ONBOARD ACQ FOR 3; comment_1: STAR FOR USE IN BLIND comment_2: OFFSET FOR FOS OBS. ! linenum: 3.000 targname: S-ANDROMEDAE config: FOS/RD opmode: ACCUM aperture: 1.0-PAIR sp_element: G270H wavelength: 2400 num_exp: 1 time_per_exp: 7200S s_to_n: 10 fluxnum_1: 1 priority: 1 param_1: STEP-PATT = STAR-SKY req_1: CYCLE 1 comment_1: POSITION MIGHT BE UPDATED comment_2: BASED ON FOC IMAGE. ! ! end of exposure logsheet ! No scan data records found