Proposal_Information ! Section 4 Title: The Interaction of Supernovae with their Circumstellar Medium Proposal_Category: GO Scientific_Category: Interstellar Medium Cycle: 5 Investigators PI_name: Alexei Filippenko PI_Institution: University of California, Berkeley CoI_Name: Roger Chevalier CoI_Institution: University of Virginia Contact: ! Y or N (designate at most one contact) CoI_Name: Robert Fesen CoI_Institution: Dartmouth College Contact: ! Y or N (designate at most one contact) CoI_Name: Claes Fransson CoI_Institution: Stockholm Observatory Contact: ! Y or N (designate at most one contact) CoI_Name: Robert Kirshner CoI_Institution: Harvard University Contact: ! Y or N (designate at most one contact) CoI_Name: Bruno Leibundgut CoI_Institution: European Southern Observatory Contact: ! Y or N (designate at most one contact) CoI_Name: Thomas Matheson CoI_Institution: University of California, Berkeley Contact: ! Y or N (designate at most one contact) CoI_Name: Schuyler Van Dyk CoI_Institution: University of California, Berkeley Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) The interaction of supernova (SN) ejecta with circumstellar material supplied by the wind of the evolved progenitor star can sometimes provide enough energy to sustain the SN luminosity for several decades. Existing observations of certain Type II SNe strongly favor such an interpretation over other possible late-time energy sources. Some peculiar SNe II have such dense circumstellar winds that interaction with the ejecta substantially alters their observed properties even at early times. The UV spectrum is a powerful diagnostic for probing the conditions in the shocked outer ejecta and circumstellar gas. We propose to observe two old SNe (t = 7- 15 years) which, due to their extensive radio and optical data records, are particularly well suited for an investigation of the interaction between ejecta and circumstellar gas. We will also observe one of the most recent SNe II (SN 1994Y), which shows strong evidence for very early interaction with its circumstellar medium. The fluxes and intensity ratios of UV emission lines measured in FOS spectra will be used to test theoretical models of the interaction. HST observations of these objects will shed light on differences among them and their shocks, as well as on the mass-loss histories of their progenitor stars. Questions ! Free format text (please update) Observing_Description: We wish to obtain UV FOS spectra of two old SNe, as well as the new one, SN 1994Y. The expected fluxes of UV emission lines were calculated according to the predictions of CF94 (power-law and RSG models), in each case using the known HAlpha or HBeta flux and extinction (see below). The flux of SN 1980K is from Fesen & Matonick (1994); the HBeta flux of SN 1988Z was 6 * 10^-16 erg/s/cm^2 in a June 1994 Keck spectrum (Fig. 5). Extrapolations into Cycle 5 were generally simple: in recent years the observed fluxes have been staying nearly constant or declining very slowly. An exception is SN 1994Y, which was discovered only in August 1994; thus, we adopted a distance of 34 Mpc and the HBeta luminosity predicted by CF94 at t = 1.5 years (corresponding to the middle of Cycle 5). Ideally, we would obtain spectra of each SN with all three high-resolution UV gratings (G130H, G190H, G270H), in order to get accurate emission-line profiles. However, calculations show that in some cases the signal will be substantially less than the dark current. Thus, we must compromise. (a) SN 1980K, in the outskirts of NGC 6946, suffers from a Galactic reddening of E(B-V) = 0.40 mag (Burstein & Heiles 1984; BH84). This makes it too time consuming to obtain any UV spectra except with the G270H grating. (b) From BH84, we find that Galactic E(B-V) < 0.01 mag for SN 1988Z. Internal reddening, estimated from the Balmer decrements of H II regions adjacent to the SN, is negligible. High-resolution G190H and G270H FOS spectra are feasible. (c) From BH84, we find that E(B-V) < 0.01 mag for SN 1994Y. Extinction due to dust in the parent galaxy is also probably low, based on the object's location. Interstellar Na I D absorption is weak in the spectrum. We assume E(B-V) = 0.1 mag, and find that observations with the high-resolution gratings can easily be obtained. To maximize throughput while excluding most contaminants (H II regions, adjacent stars, etc.), we will use the 0.86 arcsec circular aperture. Target acquisition will generally be done by centering on a neighboring star and subsequently offsetting to the SN; the offsets are determined from ground-based images. Scattered red light should not be a significant problem in the spectra because we will be looking primarily at emission lines. We estimate that SN 1988Z requires 5 orbits for 2 spectra. The G190H setting will be observed with the blue digicon, rather than red, since the red digicon is not sensitive near 1600 Ang, where the CIV 1549 line of SN 1988Z falls. Since SN 1980K is in a CVZ, the G270H spectrum will require only 1 orbit. The three spectra of SN 1994Y will be obtained in the remaining 6 orbits, for a grand total of 12 orbits (as allocated). Note that we had listed SN 1994W rather than SN 1994Y in the original proposal, but SN 1994W subsequently faded unexpectedly fast. A better object of the same type is SN 1994Y. Several weeks ago we sought and obtained approval from STScI to swap SN 1994Y for SN 1994W. See the e-mail message below: ! From: SMTP%"WALBORN@stsci.edu" 3-FEB-1995 13:52:11.89 ! To: alex@bkyast.berkeley.edu, wms@stsci.edu, downes@stsci.edu ! Subj: GO 6043 Target Change Request ! Hi. Bob Williams has approved your request to substitute ! SN 1994Y for SN 1994W, subject to final duplication checks on ! the Phase II database. ! Regards. Real_Time_Justification: Since we have access to many observatories, we will continue to maintain our ground-based work on these SNe between now and the time of the HST observations. Complementary optical spectra of the two old SNe will be obtained at the Keck telescope, while SN 1994Y will be observed with the Lick 3-m reflector. Calibration_Justification: ! Move appropriate text from Real_Time_Justification Additional_Comments: Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: SN1980K-OFFSET Alternate_Names: Description: STAR, K V-IV Position: RA = 20H 35M 30.10S +/- 0.05S, DEC = 60D 06' 02.2" +/- 0.5", PLATE-ID=02RK Equinox: J2000 RV_or_Z: Flux: V = 16.33 +/- 0.1 ! Include at least V and B-V B-V = 1.13 +/- 0.1 U-B = 0.61 +/- 0.15 Comments: K3 OFFSET STAR FOR SN1980K. Target_Number: 2 Target_Name: SN1980K Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA-OFF = -0.027S +/- 0.02S, DEC-OFF = +21.58" +/- 0.15", FROM 1, !PLATE-ID= Equinox: 2000 RV_or_Z: V = +50 Flux: V = 24 +/- 1 B-V = 0.5 +/- 0.3 F-LINE(2800) = 2 +/- 1 E-15 W-LINE(2800) = 4 +/- 1 Comments: MAGNITUDES AND FLUXES VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. Target_Number: 3 Target_Name: SN1988Z-OFFSET Alternate_Names: Description: STAR, G V-IV Position: RA = 10H 51M 51.12S +/- 0.03S, DEC = 15D 59' 28.18" +/- 0.4", PLATE-ID=01AJ Equinox: J2000 RV_or_Z: Flux: V = 15.9 +/- 0.2 B-V = 0.8 +/- 0.15 V-R = 0.62 +/- 0.1 V-I = 1.24 +/- 0.1 U-B = 0.2 +/- 0.15 Comments: G5 OFFSET STAR FOR SN1988Z. Target_Number: 4 Target_Name: SN1988Z Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA-OFF = -0.944S +/- 0.01S, DEC-OFF = +31.58" +/- 0.15", FROM 3, !PLATE-ID= Equinox: 2000 RV_or_Z: V = 6600 Flux: V = 23.5 +/- 1.0 B-V = 0.0 +/- 0.5 F-LINE(1549) = 3 +/- 2 E-15 W-LINE(1549) = 4 +/- 1 Comments: MAGNITUDES AND FLUXES VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. Target_Number: 5 Target_Name: SN1994Y Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA = 13H 53M 30.58S +/- 0.07S, DEC = 40D 42' 33.0" +/- 0.4", !PLATE-ID= Equinox: 1950 RV_or_Z: V = +2560 Flux: V = 19 +/- 1 B-V = 0.5 +/- 0.3 F-LINE(1549) = 2 +/- 1 E-13 W-LINE(1549) = 10 +/- 5 Comments: MAGNITUDES AND FLUXES VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. Visits ! Section 6 Visit_Number: 1 Visit_Requirements: CVZ On_Hold_Comments: Visit_Comments: OBJECT FALLS IN CVZ, AS DISCUSSED IN ORIGINAL PROPOSAL. Exposure_Number: 1 ! Section 6.5 Target_Name: SN1980K-OFFSET Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 22S Special_Requirements: ONBOARD ACQ FOR 2 Comments: NEED TO OFFSET FROM THIS STAR TO THE TARGET. Exposure_Number: 2 ! Section 6.5 Target_Name: SN1980K Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 59.8M Special_Requirements: Comments: Visit_Number: 2 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 ! Section 6.5 Target_Name: SN1988Z-OFFSET Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 12S Special_Requirements: ONBOARD ACQ FOR 2-3 Comments: NEED TO OFFSET FROM THIS STAR TO THE TARGET. Exposure_Number: 2 ! Section 6.5 Target_Name: SN1988Z Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 40M Special_Requirements: MAX DUR 200% END ORBIT Comments: Exposure_Number: 3 ! Section 6.5 Target_Name: SN1988Z Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 120M Special_Requirements: END ORBIT Comments: Visit_Number: 3 Visit_Requirements: On_Hold_Comments: Visit_Comments: Exposure_Number: 1 ! Section 6.5 Target_Name: SN1994Y Config: FOS/RD Opmode: ACQ/PEAK Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP SCAN-STEP-Y=1.23 SEARCH-SIZE-X=1 SEARCH-SIZE-Y=3 Number_of_Iterations: 1 Time_Per_Exposure: 40S Special_Requirements: ONBOARD ACQ FOR 2 Comments: Exposure_Number: 2 ! Section 6.5 Target_Name: SN1994Y Config: FOS/RD Opmode: ACQ/PEAK Aperture: 1.0 Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP SCAN-STEP-X=0.61 SCAN-STEP-Y=0.61 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 Number_of_Iterations: 1 Time_Per_Exposure: 40S Special_Requirements: ONBOARD ACQ FOR 3 Comments: Exposure_Number: 3 ! Section 6.5 Target_Name: SN1994Y Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.5 Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP ! SCAN-STEP-X=0.17 ! SCAN-STEP-Y=0.17 ! SEARCH-SIZE-X=5 ! SEARCH-SIZE-Y=5 SCAN-STEP-X=0.29 SCAN-STEP-Y=0.29 SEARCH-SIZE-X=3 SEARCH-SIZE-Y=3 Number_of_Iterations: 1 Time_Per_Exposure: 46S Special_Requirements: ONBOARD ACQ FOR 4-6 Comments: Exposure_Number: 4 ! Section 6.5 Target_Name: SN1994Y Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 26M Special_Requirements: Comments: Exposure_Number: 5 ! Section 6.5 Target_Name: SN1994Y Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G190H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 58M Special_Requirements: END ORBIT MAX DUR 200% EXPAND Comments: Exposure_Number: 6 ! Section 6.5 Target_Name: SN1994Y Config: FOS/BL Opmode: ACCUM Aperture: 1.0 Sp_Element: G130H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 123M Special_Requirements: END ORBIT Comments: Data_Distribution ! Defaults indicated; change if desired Medium: 8MM ! 8MM or 6250BPI or 1600BPI Blocking_Factor: 10 ! 10 or 1 ! Only astronomers with very old 9- ! track tape drives should consider ! a blocking factor of 1 Ship_To: PI_Address ! STSCI or PI_Address or ! PI Address from Phase I is: ! !Department of Astronomy, !601 Campbell Hall, !University of California, !Berkeley, CA 94720 ! ! Ship_Via: UPS ! UPS (2-day) or OVERNIGHT ! Overnight shipping done at PI expense !Recipient_Email: ! Needed if Ship_To: is not PI_Address ! ! Let us know what you think of this template and software! ! 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