! 6584_hopr.prop - RAL 10/08/96 - For HOPR repeat of Visit 01 ( now Visit 51 ) ! due to GS loss of lock. ! ! 6584_EA_update.prop - RAL 8/22/96 ! ! This version contains the updates to targets 4 and 5 from the EARLY ACQ ! imaging. ! ! Set Visit 02 ORIENT to U3=105D as this is the one that seems obtainable ! every day from 1996.197-1996.216 and which also still keeps the position ! of Target 4 (SN1979C-OFFSET) on WF3 and well away from the WF3-WF4 chip ! boundary when Target 3 (SN1979C-CLUSTER) is centered in the PC1 aperture ! as desired by the PI. The target enters the Solar Exclusion Zone on 1996.217. ! ! Added further detailed info to target comments for Target 3, SN1979C-CLUSTER, ! based on extensive telephone conversation with PI on 22/23 June, 1996. ! ! Inserted target comments about pedigree of GASP Plate IDs. They are merely ! the GS Plate IDs from which the finder charts were made. The target coords ! were NOT measured from these plates. PLATE-ID=0000 had previously been used ! for all targets in the original submitted version of the program file and ! was causing the Spike LRP scheduling system to think that no guide stars ! were available, and therefore it was impossible for the LRP to obtain any ! plan windows. ! ! - Ray Lucas - 23 June, 1996 ! ! Updated coords for Target 1 to those I measured from GASP images with GASP ! s/w. ! ! - Ray Lucas - 27 June, 1996 ! ! Applied slight offset to coords for Target 1 based on fact that both PI and ! I see a slight shift wrt the crosshairs and target still appears not to be ! centered quite perfectly. Maybe the centroid was slightly wrong for some ! reason, but now the crosshairs should appear centered better on the offset ! star. Also applied a small offset to Target 4 on instructions from the PI ! again in order to make the crosshairs line up more exactly as seen on the ! GASP chart. ! ! Also inserted the modified Visit 1 Exp Log lines provided by Michael Dahlem ! ( all of Visit 1 ). The only thing I changed was to add the optional ! parameter STEP-PATT=SINGLE to all the exposure lines using the FOS paired ! apertures. It is the default for the acquisitions, but it is not the default ! for the ACCUM mode and therefore must be specified explicitly. I decided to ! specify it explicitly for all lines in Visit 1 including the acquisitions ! just to be sure and make it very clear for anyone reading the propsal file. ! ! - Ray Lucas - 28 June, 1996 ! ! Updated Targets 4 and 5 information based on EARLY ACQ results supplied by ! the PI. ! ! - Ray Lucas - 21 August, 1996 ! ! ! Proposal 6584, submission 1 ! PI: Alex Filippenko ! Received Tue Feb 20 22:47:24 EST 1996 ! From: alex@beast.berkeley.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6584,v 11.1 1996/10/08 19:36:18 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6584,v 11.1 1996/10/08 19:36:18 pepsa Exp $ ! ! Refer to the HST Phase II Proposal Instructions to fill this out ! ! Anything after a "!" is ignored, and may be deleted ! ! All keywords with multiple entries are comma delimited except the ! Visit_Requirements and Special_Requirements keywords which can be ! delimited with carriage returns or semi-colons, but not commas ! ! For help call your Program Coordinator: Lucas ! Phone: 410-338-4716 , E-mail: lucas@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0501.filippenko.prop ! Date generated: Fri Dec 22 16:32:59 EST 1995 ! Proposal_Information ! Section 4 Title: Interaction of Supernovae with Circumstellar Material Proposal_Category: GO Scientific_Category: INTERSTELLAR MEDIUM Cycle: 6 Investigators PI_name: Alex 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: Douglas Leonard CoI_Institution: University of California, Berkeley 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 SNs (1979C and 1980K) whose optical and radio characteristics reveal them to be especially well suited for an investigation of the interaction between ejecta and circumstellar gas. We will also observe a more recent SN II (1995N) showing strong evidence for early interaction with circumstellar gas. The fluxes and intensity ratios of UV emission lines will be used to test theoretical models of the interaction. In addition, we will obtain UBVRI and HAlpha images of SN 1979C to obtain a precise offset from an offset star (for the subsequent FOS spectroscopy), to determine background contamination corrections for previous photometry, to measure accurate current magnitudes, to search for light echoes, and to investigate the stellar population and structure of H II regions in its vicinity. The HST observations will shed light on differences among the 3 objects, as well as on the mass-loss histories of their progenitors. Questions ! Free format text (please update) Observing_Description: (1) We wish to obtain broad-band "optical" (UBVRI) images of SN 1979C and its surroundings, as well as a narrow-band H-alpha image. The use of five standard bands (WFPC2 Handbook, p. 24) will permit direct comparisons with other HST observations. To achieve high spatial resolution, the PC is requested. The continuum V magnitude of SN 1979C is about 24, but we should go a magnitude deeper in case it fades and to study the surrounding stellar population. We would like to reach relatively high signal-to-noise ratios (SNRs), at least 20 in VRI and 15 in UB, for sufficiently accurate measurement of magnitudes and colors. We will remove cosmic rays by comparing pairs of exposures made through the same filter. Consider the F814W (I) filter. From the WFPC2 Handbook, we find that QT d\lambda/\lambda = 0.01799. Using eq. 6.1 in the Handbook, we calculate a count rate of 0.45 s^{-1}. The sky background is small by comparison (29.2 mag/pixel, or about 26.7 mag over the compact core of 10 pixels). We find that SNR = 20 is achieved in about 900~s. (Note that the readout noise, 5 electrons/pixel, is negligible.) Similarly, we find that 800~s, 600~s, 1900~s, and 2300~s are required with the F675W (R), F555W (V), F439W (B), and F336W (U) filters, respectively. The narrow-band H-alpha image will be obtained through the F658N filter. At the redshift of NGC 4321 (cz = 1600 km/s), the observed wavelength of H-alpha is 6598~\AA, well within the flat part of the transmission profile (WFPC2 Handbook, p. 104). The continuum will be subtracted from the narrow-band image by appropriately scaling the broad-band images. From our ground-based images, the H$\alpha$ flux is about 5 x 10^{-15} ergs/s/cm^2. If this is spread over about 3 square arcsec we have 0.34 x 10^{-17} ergs/s/cm^2/pixel, since each PC2 pixel subtends 0.002 square arcsec. Averaged over the effective bandpass of the filter, we have 1.8 x 10^{-19} ergs/s/cm^2/pixel/\AA, which corresponds to about 25.2 mag/pixel. Using the estimated transmission of the filter and the CCD efficiency, we calculate that about 20 electrons will be detected in 65 minutes (1.5 orbits), yielding SNR = 3 per pixel. (2) We wish to obtain UV FOS spectra of all three SNe. 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 H-alpha or H-beta flux (e.g., Fesen \& Matonick 1994) and extinction. Extrapolations into Cycle 6 were based on previous observations of SN 1995N, and on the observed light curves of SNe 1979C and 1980K. Ideally, we would obtain spectra of each object with the high-resolution UV gratings (G130H, G190H, G270H, G400H), in order to get accurate emission-line profiles. However, calculations show that in the UV, the signal will be substantially less than the dark current, even with the low-resolution G160L grating in two of the objects. Thus, we must compromise. For each of SN 1979C and SN 1980K, we request 5 orbits: 1 for target acquisition, 3 with G270H, and 1 with G400H. For SN 1995N, we request 7 orbits: 1 for target acquisition, 3 with G160L, 2 with G270H, and 1 with G400H. All exposures except G160L will be done with the red arm of the FOS. The G400H spectra are useful for lines in the near-UV (3200--4000~\AA), and to help tie our ground-based Keck and Lick spectra (\lambda > 4000~\AA) to the HST data; moreover, they require only a small fraction of time relative to the UV settings. The total number of orbits for FOS spectroscopy is 17. Here we give a sample calculation of the exposure time. For SN 1980K we have a measured flux density (f_\lambda) of 3 (in units of 10^{-17} erg s^{-1} cm^{-2} \AA^{-1}) at 2400~\AA, and this may decrease to 1 by a year from now. From the Cycle 6 FOS Handbook, we find that the throughput (T_\lambda) of the 0.86^{\prime\prime} aperture is 0.91, and the inverse sensitivity (S_\lambda) at 2400~\AA\ is 2.82 x 10^{-15} erg s^{-1} cm^{-2} count^{-1}. Thus, the expected count rate (N_\lambda) is f_\lambda T_\lambda/S_\lambda = 0.00327 counts s^{-1} diode^{-1}, less than the dark current (D) of 0.01 counts s^{-1} diode^{-1}. The required integration time is given by t = (SNR)^2 (N_\lambda +D)/N_\lambda^2, which in this case is 8000 sec (3 orbits) for SNR = 2.5 per diode. (Note that the emission lines in which we are interested will have higher SNRs!) A similar calculation shows that with the G400H grating, a total integration time of 2700 sec (1 orbit) will be sufficient. Note that our original proposal called for observations of SN 1994Y instead of SN 1980K. However, our Cycle 5 spectrum of SN 1980K was not successful due to an incorrect offset. Since SN 1980K has higher priority than SN 1994Y, we requested (and received) a change of targets. Real_Time_Justification: Calibration_Justification: Additional_Comments: (1) Visit 2, the WFPC2 imaging of SN 1979C-CLUSTER (target 3), must be done at least 2 months prior to the FOS spectroscopy, since we need to measure a more accurate offset from the offset star (target 4) to SN1979C (target 5) using these images. THUS, THE IMAGING OBSERVATIONS OF SN1979C (VISIT 2) MUST BE SCHEDULED AS SOON AS POSSIBLE, PREFERABLY EVEN BEFORE THE OFFICIAL BEGINNING OF CYCLE 6 (JULY 1). The three main windows of opportunity are (a) a week in April 1996, (b) May/June 1996, and (c) July 1996. I would prefer to have the imaging observations scheduled either in April or in May, since the follow-up FOS observations could then be performed in July 1996. Otherwise, we have to wait for November 1996 to obtain the FOS spectra, and if something goes wrong (e.g., HST safing event, or a target of opportunity), then there's little chance to re-schedule for January 1997 (the last possible window for the FOS spectra). NOTE: For LRP and scheduling purposes, the ORIENT has been set to 105.0D which means mid-late July. - Ray Lucas - 6/22-23/96 (2) Note that the offset star (SN1979C-OFFSET, target 4) is at PA = 305 deg with respect to SN1979C-CLUSTER (that is, west and north of SN1979C-CLUSTER). If SN1979C-CLUSTER (target 3) is positioned in the geometric center of the PC chip, I want to BE SURE that SN1979C-OFFSET (target 4) lands somewhere on one of the WFC chips. Thus, I have specified the visit requirement "ORIENT 65D TO 185D" for VISIT 2. This has a midpoint of 125 deg, or 180 deg from the PA of SN1979C-OFFSET with respect to SN1979C-CLUSTER (305D). Looking at pages 7-11, 7-12, and 9-14 in the Phase II Proposal Instructions, I think this is correct, but please check it for me. Thanks! - NOTE: Verified to be OK with ORIENT 105.0D which is the value that has been placed in the program for LRP and scheduling purposes. - Ray Lucas - 6/22-23/96. (3) Note that SN1979C-OFFSET (target 4) is quite far (80") from SN1979C (target 5). I want to offset from target 4 to target 5 and then get an FOS spectrum of target 5. If it turns out (during scheduling) that the guide stars used for target 4 are no longer in the pickles when HST is pointing at target 5, PLEASE CONTACT ME and I will choose a different (closer) offset star. However, all of the other candidate offset stars are VERY faint, and would require 2 to 3 orbits of acquisition time (out of 5 orbits allocated to this Visit!). Thus, I prefer to use the chosen offset star (target 4) if possible. Fixed_Targets ! Section 5.1 Target_Number: 1 Target_Name: SN1995N-OFFSET Alternate_Names: Description: STAR, G V-IV Position: RA=14H 49M 29.275S +/- 0.05S, ! Most common specification format is DEC=-10D 10' 36.00" +/- 0.5", ! RA=0H 0M 0.00S +/- 0S, PLATE-ID=04MV ! DEC=0D 0' 0.0" +/- 0", ! PLATE-ID=0000 Equinox: 2000 RV_or_Z: Flux: V = 17.45 +/- 0.2 ! Include at least V and B-V B-V = 0.58 +/- 0.2 R-I = 0.68 +/- 0.2 Comments: G5 OFFSET STAR FOR SN1995N. These coordinates are GASP coords but the seconds of time and arc have been changed slightly to still make the cross-hairs line up properly with the target. The centroided coords appeared to be slightly off, and the GASP coords were measured from the same GS Plate as the finder charts, so the reference frame is the same. The coords have just been tweaked very slightly ( from 29.314s to 29.275s and from 36.14" to 36.00" ). Target_Number: 2 Target_Name: SN1995N Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA-OFF = -0.942S +/- 0.01S, DEC-OFF = +22.11" +/- 0.15", FROM 1, PLATE-ID=04MV Equinox: 2000 RV_or_Z: V = +1800 Flux: V = 22 +/- 1 ! Include at least V and B-V B-V = 0.5 +/- 0.5 F-LINE(2800) = 2 +/- 1 E-15 W-LINE(2800) = 4 +/- 1 Comments: MAGNITUDES AND COLORS VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. PLATE-ID is merely the one from the GASP finder chart which was the best one to use in terms of GSSS plate x,y. Position was not measured from this plate, however. Target_Number: 3 Target_Name: SN1979C-CLUSTER Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA=12H 22M 58.63S +/- 0.1S, DEC=+15D 47' 51.7" +/- 1.0", PLATE-ID=00G0 Equinox: 2000 RV_or_Z: V = +1600 Flux: V = 24 +/- 1 B-V = 0.5 +/- 0.5 Comments: MAGNITUDES AND COLORS VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. PLATE-ID is merely the one from the GASP finder chart which was the best one to use in terms of GSSS plate x,y. Position was not measured from this plate, however. The actual science target ( Target 5 = SN1979C ) is somewhere in this cluster and will have to be identified by comparing all the EARLY ACQ images in the different filters, hence ALL the imaging is a prerequisite as EARLY ACQ for the spectroscopy. They are also all required to be contemporaneous since SN remnant is fading over time. - Ray Lucas - 6/22-23/96. Target_Number: 4 Target_Name: SN1979C-OFFSET Alternate_Names: Description: STAR, G V-IV Position: RA=12H 22M 54.05S +/- 0.02S, DEC=+15D 48' 40.20" +/- 0.3", PLATE-ID=00G0 Equinox: 2000 RV_or_Z: Flux: V = 17.8 +/- 0.3 B-V = 0.8 +/- 0.1 Comments: Further flux info includes U-B=0.2 +/- 0.1 and B-I = 2.6 +/- 0.1. These are based on EARLY ACQ results. G5 OFFSET STAR FOR SN1979C. IF THIS OFFSET STAR ENDS UP BEING TOO FAR AWAY FROM THE TARGET (SUCH THAT THE GUIDE STARS ARE LOST), I WILL CHOOSE A DIFFERENT OFFSET STAR --- BUT ALL OF THEM ARE MUCH FAINTER THAN THIS ONE. SEE "ADDITIONAL COMMENTS" SECTION FOR MORE DETAILS. PLATE-ID is the one from the GASP finder chart and EARLY ACQ. The coords have been updated by the PI based on the results of the EARLY ACQ imaging. Target_Number: 5 Target_Name: SN1979C Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA-OFF = +4.661S +/- 0.01S, DEC-OFF = -47.79" +/- 0.2", FROM 4, PLATE-ID=00G0 Equinox: 2000 RV_or_Z: V = +1600 Flux: V = 24 +/- 1 B-V = 0.5 +/- 0.5 F-LINE(2800) = 2 +/- 1 E-15 W-LINE(2800) = 4 +/- 1 Comments: MAGNITUDES AND FLUXES VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. PLATE-ID is the one from the GASP finder chart which was the best one to use in terms of GSSS plate x,y and it is also the one from which the EARLY ACQ guide stars came. These target offset coords are the ones measured by the PI from the EARLY ACQ images. Target_Number: 6 Target_Name: SN1980K-OFFSET Alternate_Names: Description: STAR, K V-IV Position: RA=20H 35M 30.87S +/- 0.05S, DEC=+60D 06' 20.9" +/- 0.5", PLATE-ID=02RK Equinox: 2000 RV_or_Z: Flux: V = 18.19 +/- 0.05 ! Include at least V and B-V B-V = 1.09 +/- 0.03 Comments: K3 OFFSET STAR FOR SN1980K. PLATE-ID is merely the one from the GASP finder chart which was the best one to use in terms of GSSS plate x,y. Position was not measured from this plate, however. Target_Number: 7 Target_Name: SN1980K Alternate_Names: Description: EXT-STAR, SUPERNOVA TYPE II Position: RA-OFF = -0.770S +/- 0.01S, DEC-OFF = +3.024" +/- 0.05", FROM 6, PLATE-ID=02RK Equinox: 2000 RV_or_Z: V = +50 Flux: V = 24 +/- 1 B-V = 0.5 +/- 0.5 F-LINE(2800) = 2 +/- 1 E-15 W-LINE(2800) = 4 +/- 1 Comments: MAGNITUDES AND FLUXES VERY APPROXIMATE; OBJECT SLOWLY FADING WITH TIME. PLATE-ID is merely the one from the GASP finder chart which was the best one to use in terms of GSSS plate x,y. Position was not measured from this plate, however. ! This is a template for a single containing a single exposure ! Repeat exposure and visit blocks as needed ! Visit 1 edited by M. Dahlem, 06/28/96; replaced single apertures by PAIR-A. ! STEP-PATT=SINGLE optional parameter added to paired aperture exposures ! by Ray Lucas, 6/28/96. Visits ! Section 6 Visit_Number: 1 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: Exposure_Number: 1 ! Section 6.5 Target_Name: SN1995N-OFFSET Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 45S Special_Requirements: ONBOARD ACQ FOR 2 ! Section 7.2 Comments: Exposure_Number: 2 Target_Name: SN1995N-OFFSET Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.25-PAIR-A Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 SCAN-STEP-X=0.12 SCAN-STEP-Y=0.12 STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 6S Special_Requirements: ONBOARD ACQ FOR 3-5 Comments: NEED TO OFFSET FROM THIS STAR TO THE TARGET. Exposure_Number: 3 Target_Name: SN1995N Config: FOS/RD Opmode: ACCUM Aperture: 1.0-PAIR-A Sp_Element: G400H Wavelength: Optional_Parameters: STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 48M Special_Requirements: EXPAND Exposure_Number: 4 Target_Name: SN1995N Config: FOS/RD Opmode: ACCUM Aperture: 1.0-PAIR-A Sp_Element: G270H Wavelength: Optional_Parameters: STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 80M Special_Requirements: EXPAND Exposure_Number: 5 Target_Name: SN1995N Config: FOS/BL Opmode: ACCUM Aperture: 1.0-PAIR-A Sp_Element: G160L Wavelength: Optional_Parameters: STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 116M Special_Requirements: Visit_Number: 2 Visit_Requirements: ORIENT 105.0D TO 105.0D On_Hold_Comments: Visit_Comments: THIS VISIT NEEDS TO BE DONE AT LEAST 2 MONTHS BEFORE VISIT 3, SO THAT OFFSET USED IN VISIT 3 CAN BE DETERMINED MORE ACCURATELY. ALSO, I WANT THE OFFSET STAR, SN1979C-OFFSET (TARGET 4), WHICH IS AT PA = 305D RELATIVE TO SN1979C-CLUSTER, TO FALL SOMEWHERE ON A WFC CHIP; HENCE THE "ORIENT 65D TO 185D" VISIT REQUIREMENT (WHICH HAS A MIDPOINT OF 125D, OR 180D FROM THE PA OF SN1979C-OFFSET). SEE "ADDITIONAL COMMENTS" SECTION FOR MORE DETAILS. NOTE: ORIENT WAS FIXED AT 105.0D FOR SCHEDULING PURPOSES BY RAY LUCAS ON 6/22-23/96. SEE ALSO TARGET 3 COMMENTS. Exposure_Number: 1 ! Section 6.5 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F439W Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2400S Special_Requirements: EXPAND MAX DUR 130% Comments: Exposure_Number: 2 ! Section 6.5 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F336W Wavelength: Optional_Parameters: CR-TOLERANCE=0.1 Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: EXPAND MAX DUR 130% Comments: Exposure_Number: 3 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F814W Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 10S Special_Requirements: Comments: THIS SHORT EXPOSURE WILL BE USED TO DETERMINE THE CENTROID OF THE BRIGHT OFFSET STAR, SN1979C-OFFSET, IF THE OTHERS ARE SATURATED Exposure_Number: 4 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F814W Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1200S Special_Requirements: Comments: Exposure_Number: 5 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F555W Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 800S Special_Requirements: EXPAND MAX DUR 130% Comments: Exposure_Number: 6 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F675W Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 1000S Special_Requirements: Comments: Exposure_Number: 7 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F658N Wavelength: Optional_Parameters: CR-SPLIT=NO Number_of_Iterations: 1 Time_Per_Exposure: 1200S Special_Requirements: EXPAND MAX DUR 130% Comments: Exposure_Number: 8 Target_Name: SN1979C-CLUSTER Config: WFPC2 Opmode: IMAGE Aperture: PC1-FIX Sp_Element: F658N Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 2600S Special_Requirements: EXPAND MAX DUR 130% Comments: Visit_Number: 3 Visit_Requirements: AFTER 2 BY 60D TO 200D ! Section 7.1 On_Hold_Comments: Visit_Comments: THIS VISIT SHOULD BE DONE AT LEAST 60 DAYS AFTER VISIT 2, BUT BEFORE THE HST SERVICING MISSION (SINCE IT IS AN FOS OBSERVATION). SEE "ADDITIONAL COMMENTS" SECTION FOR MORE DETAILS. Exposure_Number: 1 ! Section 6.5 Target_Name: SN1979C-OFFSET Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 46S Special_Requirements: ONBOARD ACQ FOR 2 ! Section 7.2 Comments: Exposure_Number: 2 Target_Name: SN1979C-OFFSET Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 SCAN-STEP-X=0.11 SCAN-STEP-Y=0.11 Number_of_Iterations: 1 Time_Per_Exposure: 9S Special_Requirements: ONBOARD ACQ FOR 3-4 Comments: NEED TO OFFSET FROM THIS STAR TO THE TARGET. Exposure_Number: 3 Target_Name: SN1979C Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G400H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 50M Special_Requirements: END ORBIT Exposure_Number: 4 Target_Name: SN1979C Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 120M Special_Requirements: Visit_Number: 4 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: 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: 90S Special_Requirements: ONBOARD ACQ FOR 2 ! Section 7.2 Comments: Exposure_Number: 2 Target_Name: SN1980K-OFFSET Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 SCAN-STEP-X=0.11 SCAN-STEP-Y=0.11 Number_of_Iterations: 1 Time_Per_Exposure: 15S Special_Requirements: ONBOARD ACQ FOR 3-4 Comments: NEED TO OFFSET FROM THIS STAR TO THE TARGET. Exposure_Number: 3 Target_Name: SN1980K Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G400H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 50M Special_Requirements: END ORBIT Exposure_Number: 4 Target_Name: SN1980K Config: FOS/RD Opmode: ACCUM Aperture: 1.0 Sp_Element: G270H Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 130M Special_Requirements: Visit_Number: 51 Visit_Requirements: ! Section 7.1 On_Hold_Comments: Visit_Comments: HOPR Repeat due to GS loss of lock in Visit 01 execution. Exposure_Number: 1 ! Section 6.5 Target_Name: SN1995N-OFFSET Config: FOS/RD Opmode: ACQ/BINARY Aperture: 4.3 Sp_Element: MIRROR Wavelength: Optional_Parameters: Number_of_Iterations: 1 Time_Per_Exposure: 45S Special_Requirements: ONBOARD ACQ FOR 2 ! Section 7.2 Comments: Exposure_Number: 2 Target_Name: SN1995N-OFFSET Config: FOS/RD Opmode: ACQ/PEAK Aperture: 0.25-PAIR-A Sp_Element: MIRROR Wavelength: Optional_Parameters: TYPE=UP SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 SCAN-STEP-X=0.12 SCAN-STEP-Y=0.12 STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 6S Special_Requirements: ONBOARD ACQ FOR 3-5 Comments: NEED TO OFFSET FROM THIS STAR TO THE TARGET. Exposure_Number: 3 Target_Name: SN1995N Config: FOS/RD Opmode: ACCUM Aperture: 1.0-PAIR-A Sp_Element: G400H Wavelength: Optional_Parameters: STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 48M Special_Requirements: EXPAND Exposure_Number: 4 Target_Name: SN1995N Config: FOS/RD Opmode: ACCUM Aperture: 1.0-PAIR-A Sp_Element: G270H Wavelength: Optional_Parameters: STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 80M Special_Requirements: EXPAND Exposure_Number: 5 Target_Name: SN1995N Config: FOS/BL Opmode: ACCUM Aperture: 1.0-PAIR-A Sp_Element: G160L Wavelength: Optional_Parameters: STEP-PATT=SINGLE Number_of_Iterations: 1 Time_Per_Exposure: 116M Special_Requirements: 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: ! ! University of California, Berkeley ! Department of Astronomy ! 601 Campbell Hall ! Berkeley, CA 94720-3411, USA ! 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! ! Please send a list of your likes and dislikes to your Program Coordinator