Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 6139 Report Date: 18-Jul-95:20:16 Version: ********** Check-in Date: ********** 1.Proposal Title: SINS: THE SUPERNOVA INTENSIVE STUDY - CYCLE4 ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID INTERSTELLAR MEDIUM GO/DD 3 Long Term yrs Sub Category Target of Oppt. SN & SNR Large Project ------------------------------------------------------------------------------------ 6. Principal Investigator Institution Country Telephone Robert P. Kirshner HARVARD COLLEGE OBSERVATORY USA 617-495-7519 ------------------------------------------------------------------------------------ 7. Abstract We are now underway in our intensive study of supernovae with HST. This long-term project promises to illuminate problems in stellar evolution, the mechanism of stellar explosion, nucleosynthesis, the energetics of interstellar gas, and the extragalactic distance scale. Initial observations, starting in the Spring of 1992, show that HST observations of SN 1987A are rich in content and that these high- minded goals can actually be achieved. Our HST observations of a new supernova, SN1992A, demonstrate that Target-of-Opportunity observations with HST are worth the effort. We were poised to observe SN 1993J in M81 and we obtained a beautiful UV/optical spectrum from an early epoch of this peculiar supernova. Our long-term plan is to continue the imaging and spectroscopy of SN 1987A, to obtain unprecedented late-time UV spectra of SN 1993J, to realize the promise of our Cycle 1 proposal by following the late-time light curves of SN 1992A and SN 1993J, and to initiate a new Target-of-Opportunity supernova for Cycle 4. SN 1992A and SN 1993J demonstrated our ability to orchestrate observations from the ground, with IUE, and from HST to investigate important issues in supernova research. ------------------------------------------------------------------------------------ ------------------------------------------------------------------------------------ 9. Est obs time (hours) pri: 40.00 par: 0 10. Num targs pri: 4 par: 0 ------------------------------------------------------------------------------------ 11. Instruments requested: FOS FOC WF/PC ------------------------------------------------------------------------------------ 12. Special sched req: Time Critical obs. Real Time obs. ------------------------------------------------------------------------------------ Page 2 I. GENERAL FORM Proposal 6139 PI: Robert P. Kirshner Proposal Title: SINS: THE SUPERNOVA INTENSIVE STUDY - CYCLE4 ------------------------------------------------------------------------------------ 1. Proposers: Proposers Institution Country ESA ------------------------------------------------------------------------------------ David Branch OKLAHOMA, UNIVERSITY OF USA Claes Fransson STOCKHOLM OBSERVATORY SWEDEN X Robert Wagoner STANFORD UNIVERSITY USA J. Craig Wheeler TEXAS, UNIVERSITY OF USA Roger Chevalier VIRGINIA, UNIVERSITY OF USA Pi Robert P. Kirshner HARVARD UNIVERSITY USA Nino Panagia STSCI USA X Alexei Filippenko CALIF. BERKELEY, UNIVERSITY OF USA Mark Phillips CTIO USA Nicholas Suntzeff CTIO USA Bruno Leibundgut SWISS NATIONAL SCIENCE USA X FOUNDATION Page 3 ------------------------------------------------------------------------------------ 3. Description of proposed observations. We will observe four different supernovae in Cycle 4: SN 1987A, SN 1992A, SN 1993J, and a generic supernova, not yet discovered, which we call SN 1994N. Our intention here is to give a narrative description of the observations described in the exposure log sheets. SN 1987A SN 1987A has been the object of our Cycle 1, 2, and 3 observing programs. Our goal is to continue this work, taking advantage of the improvements in telescope performance promised by COSTAR and WFPC2. We have used the FOS to obtain spectra from 1650-9200 angstroms using gratings G190H,G270H,G400H, G570H, and G780H with the red side detector. Since the supernova is close to two bright neighbor stars, we have used a careful offset acquisition, starting with a binary acquisition of the FOS offset star, then offsetting to the supernova debris and peaking up on the target, which should be about 19 mag in 1994. The supernova is surrounded by a ring of circumstellar material, whose spectrum we also wish to measure. We would like to move from the supernova debris to the ring (which is less than 1" away) and accumulate a spectrum at that location. It is important to keep these observations grouped so that the ring spectrum is obtained using the telescope position established by the debris spectrum This set of observations is to be made at two different times in Cycle 4: near the beginning, and approximately 200 +/- 50 days later. The other set of observations for SN 1987A is a set of photometric measures. These data will be used to continue the light curve of SN 1987A, and they should also have adequate signal to be useful for measurements of the source size and shape using PC1 in WFPC2. The filters are F160BW (the blocked Woods filter), F255W, F336W, F439W, F555W, F658N (for the ring), F675W, F814W, and F502N (also for emission from the ring). A second epoch of observations (the SN87PHOTB sequence) is requested that includes the broad band filters, but not the two narrow filters used to measure the structure of the circumstellar ring. As for the spectra, we would like the first set of observations early in Cycle 4 and the second epoch about 200 days later. The second supernova we would like to observe is SN 1993J, for which we have FOS data from 1993. Our acquisition method is to acquire an offset star using a binary search, offset to the supernova and peak up, then to accumulate the red side spectrum in a sequence of FOS gratings. The gratings are G190H, G270H, and G400H. We would also like to carry out photometry of SN 1993J, again using the PC1 chip on WPFC2. The filters are F336W, F439W, F555W, F675W, and F814W. This would be of the greatest utility if placed late in Cycle 4, as the ground-based data become more difficult to obtain. A similar set of observations, omitting only the U filter, is planned for SN 1992A, which has an extensive ground-based light curve. We will make B, V, R, I measurements with WFPC2. Observations near the beginning of Cycle 4 would be best, as we already anticipate an apparent magnitude near 24. The most difficult observations will be those of the not yet discovered supernova we call SN 1994N. Our past experience with SN 1992A and SN 1993J shows that we can assemble the information needed to make HST observations in a day or two. Our hope is to be placed into the observing schedule at the earliest available moment, and then to follow up with observations 30 days later and 300 days later. While we do not know when this supernova will be discovered, we have developed a plan for observing it. For the earliest spectrum, we use a binary acquisition on the bright supernova then accumulate an FOS spectrum in the UV using G190H, G270H, and G400H. The second spectrum, nominally at 30 days, is the same but with increased exposure times. The third spectrum, at 300 days, will use an offset star whose position we will measure in the guide star system coordinates. We will make a binary acquisition of the offset star, move to the supernova, and then peak up before accumulating the spectrum. We also will carry out UV photometry for this bright object, using F160BW, F 255W and F 336W. This set of observations will be conducted at three times, nominally at the earliest moment, at age 30 days and at age 300 days. Page 4 ------------------------------------------------------------------------------------ 4. Justification of need for HST observations. We have been very active in carrying forward this general program of research using IUE and ground-based facilities, and we know exactly what you can and cannot do with each. You cannot carry out the program of UV spectsoscopy outlined here with IUE, despite its much simpler scheduling constraints. The HST spectra go farther into the UV, they have much better spectral resolution, and the slit is much smaller so that contamination is not so serious a problem. You cannot follow a 13 mag supernova for 45 days (as we did for SN 1992A) with IUE because the flux declines by a factor of 100, and it is utterly pointless to make an observation at age 300days, which we have succesfully done with HST. While we will continue our Target-of-Opportunity work with IUE, it is of limited value compared to the outstanding data which can be obtained with HST. We have established a long-term program at KPNO on the 2.1 meter to help us get complementary photometry for the supernovae we study with HST. We have time assigned at the MMT and Mount Hopkins to obtain complementary spectroscopy and photometry from the ground and we have added observers at CTIO and at Lick to the SINS team. The HST photometry will only be carried out for magnitude 21 and below, since we can easily monitor the supernova flux from the ground down to this point. But the most interesting era is the very latest one, when the departures form a pure exponential may signal new physics in the energy supply. From mag 22 to 25, the HST data will be unique and provide the best information on the transition from a supernova to a supernova remnant. For SN 1987A, the HST data are absolutely essential, even for accurate BVRI photometry, to say nothing of resolving the debris. Our UV spectra are unique and even the spectrum in the optical region is better than any published ground based data from this epoch. All of this will continue to be true-- only more so as the supernova fades and its very close companions do not. Every previous time we have answered this question we were guessing. Now we have one set of data for each aspect of our program and we can begin to make realistic estimates based on real experience. For example, the [O III] image shown in Figure 1 is the result of summing 4700 seconds of exposure. It has about 25 counts/pixel and is none too deep for beginning image restoration or for trying to measure the rate of decline in separate knots. By the beginning of cycle 3, a comparable image will take 9000 seconds. But the chance will never come again, and it will take less time with the improved optics in Cycle 4. Investing in these data now will make the future observations more valuable. We recognize that these measurements take a lot of telescope time, and we have pared our set of filters to the essential minimum for achieving our scientific goals. The most difficult issue is not calculating a reasonable exposure time( as you can judge from some of the figures shown), but selecting the optimum interval between data sets. The supernova is fading slowly, but it changes significantly on the time scale of six months, which is comparable to the light travel time across the debris. Extremely interesting events, such as the collision of the debris with the circumstellar shell, are likely to take place on this timescale. It seems prudent to observe SN 1987A with about that frequency, and that is what we have requested. Our plan for the target-of-opportunity observations is modelled on our successful observation of SN 1992A. Our program for SN 1993J was extremely spartan, and we would like to restore early UV imaging and late-time photometry. There is reason to believe that SN II and SN Ib may have non-thermal UV continuua produced by Compton scattering, and stay bright inthe UV for longer than SN Ia. We will see. ------------------------------------------------------------------------------------ 5. Description of special scheduling requirements. WFPC2 observations of SN 1993J in cycle 4, 1995. We have received 3.5 hours of Director's Discretionary spacecraft time for WFPC2 imaging of SN 1993J. The visit will have imaging in the F255W,F336W,F439W,F555W,F675W,F814W filters. The visit should be scheduled shortly before or after the already planned/scheduled FOS observations of SN 1993J (proposal 5777). The spectrum and the WFPC images can be seperated in time by up to a 1 month difference. Page 5 ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. WFPC2 observations of SN 1993J in cycle 4, 1995. We have received 3.5 hours of Director's Discretionary spacecraft time for WFPC2 imaging of SN 1993J. The visit will have imaging in the F255W,F336W,F439W,F555W,F675W,F814W filters. The visit should be scheduled shortly before or after the already planned/scheduled FOS observations of SN 1993J (proposal 5777). The spectrum and the WFPC images can be seperated in time by up to a 1 month difference. ------------------------------------------------------------------------------------ 7. Data reduction and analysis plans. Now that we have some data, this answer has also come from the realm of creativewriting into the realm of fact. We have set up a cluster of Decstations at Harvard and hired a data specialist (Peter Challis, late of STScI) who helps us with archiving the incoming data, maintaining and running STSDAS, improving the calibration over the pipeline processing, and making the preliminary measurements of fluxes, wavelengths, and other quantities. This is just the beginning Phil Plait, a graduate student at Virginia, is working with Roger Chevlaier on the analysis of the 1987A circumstellar ring data. This includes image restoration through deconvolution and other methods to deal with the stellar light at thering location. Image modelling and subtraction appears to work best. Panagia hasled the geometric analysis of the ring and its application to the distance scale. Kirshner, assisted Challis, Harvard postdocs David Jeffery and Pilar Ruiz-Lapuente and Harvard graduate students is working on the photometry of SN 1987A, and on measurement of the expansion. They are also making the preliminary measurements of the narrow and broad line fluxes, which involves some modelling. The analysis of SN1992A was carried out using LTE models, and will be done in a more careful way by Branch at Oklahoma and by Wheeler and his colleagues at Texas. Our CTIO colleagues have been especially interested in the bolometric light curves of SN Ia, including SN 1992A. The new data will extend their work. Initial work on SN 1993J is being carried out at Harvard, and new SINS colleagues Filippenko and Leibundgut have been active in gathering additional data. Both Fransson and Wheeler have theoretical models for the late time emission from the debris and both Panagia and Fransson have modelled the circumstellar ring. Physically, these mechanisms are very different: one is heated by gamma rays from radioactive debris the other is recombination from the UV flash on day 1. The extragalactic distance scale work on SN II depends on models being calculated by the Harvard group in cooperation with Ron Eastman at Santa Cruz, and independently by Wagoner at Stanford. The SN 1993J data should prove an interesting challenge. The complete team will meet at least once a year to coordinate the connection between theory and observations, to write up the results, and to plan for future cycles. We carried this out for Cycle 1 and we found it to be a very interesting and productive way to work. The 1993 meeting will be late this summer. We believe the group is sufficiently broad, yet cohesive, that the right observations will be carried out and the data thoroughly studied with a goodunderstanding of earlier work in the field. We also intend to make the thoroughly processed data availble in a convenient form for use by other students of supernovae. We regard the use of HST for supernova research as an essential investment by astronomy in this field, and we will strive to make the results widely known and widely used. SN 1987A has provided a resonable model for this type of cooperation. Page 6 ------------------------------------------------------------------------------------ 8. Additional comments or special requests. We have very good access to ground based facilities which are essential to getting the most out of our HST data. We have the ability to get spectra from the 1.5m at Mount Hopkins, and photometry from the 1.2m telescope there. We have regular assignments on the MMT and at the KPNO 2.1m that ensure we can get the observations of the supernovae when they are faint at age 1 year. We haveen listed the CTIO and Berkeley observers to the SINS team. They have been outstandingly effective observers of supernovae. We have established a worldwidee-mail network to contact a wide variety of observers around the world. We have atarget-of-opportunity program on IUE which can help fill the gap while the HST program is being wheeled into action. Panagia is a member of the VLA group which obtains complementary radio data on bright supernovae. Recent statistics show that in 8 years there were 14 supernovae brighter than mag 14 at discovery, so with any reasonable luck there will be a good target for Cycle 4. Page 7 ------------------------------------------------------------------------------------ 9. Description of previous HST work. 2417 "CAS A: The remnant of a massive supernova" Robert Kirshner (PI), William Blair, Konx Long, P.F. Winkler, John Raymond 2563 "SINS: The Supernova Intensive Study" Robert Kirshner (PI), David Branch, Claes Fransson, Robert Wagoner, J. Craig Wheeler, Roger Chevalier, Nino Panagia, J. Chirs Blades 3853 "SINS: The Supernova Intensive Study - 87A revisit" 4016 "SINS: The Supernova Intensive Study - cyc 1 opportunity" 4022 "SINS: The Supernova Intensive Study - 87A revisit" 4252 "SINS: Late Time Observations of SN1992A" 4528 "SINS: The Supernova Intensive Study - cyc 2 opportunity" 4445 "SINS: The Supernova Intensive Study - cyc 3" Robert Kirshner (PI), David Branch, Claes Fransson, Robert Wagoner, J. Craig Wheeler, Roger Chevalier, Nino Panagia N. Panagia (CoI): GTO/FOC 1241 "A Study of the Nucleus of NGC 4321". N. Panagia (CoI): GTO/FOC 1259 and 3231 "Observations of Supernovae"; related to the present proposal. A. Sandage (PI), F.D. Macchetto (CoI), N. Panagia (CoI), A. Saha (CoI), G. Tammann (CoI): GO 2547 [Cycle 1] and GO 4444??? [Cycle 3] "Calibration of Supernovae of Type I as Standard Candles". N. Panagia (PI): GO/DD 3232 and 3381 "Observations of X-Ray Nova Muscae 1991". Although we are still receiving our Cycle 1 data, we are beginning to obtain some results. SN 1987A: The earliest observations resulted in the detection of circumstellar ring-- as described in Jakobsen et al below Subsequent use of the ring geometry and fluorescent line time delay enabled a measurement of the distance to the LMC--see Panagia et al below. Work in progress includes identification of new lines in the circumstellar spectrum and measurement of lines in the supernova debris. These will becompared tomodel calculations. This was reported at the Sardinia HST meeting byKirshner. Measurement of changes in the circumstellar shell and image restoration were reported at AAS by Phil Plait. The measurement of the debris diameter is nearly completed. For SN 1992A, we have combined the data from HST, IUE, and CTIO to write a giant paper that compares this supernova with the results of stellar evolution calculations and supernova explosion models. We conclude that SN 1992A cannot be the result of the explosion most frequently used to model supernova spectra,and it is also not the result of the ``late detonation'' model developed tomatch someother well observed SN Ia. Good data are in hand for SN 1993J, but it is too soon to cite results. P. Jakobsen, R. Albrecht, C. Barbieri, J.C. Blades, A. Boksenberg, P. Crane, J.M. Deharveng, M.J. Disney, T.M. Kamperman, I.R. King, F. Macchetto, C.D. Mackay, F. Paresce, G. Weigelt, D. Baxter, P. Greenfield, R. Jedrzejewski, A. Nota, W.B. Sparks, R.P. Kirshner, N. Panagia: ``First Results from the Faint Object Camera: Supernova 1987A", 1991, {\it Astrophys. J. (Letters)}, {\bf 369}, L59. N. Panagia, R. Gilmozzi, F.D. Macchetto, H.-M. Adorf, R.P. Kirshner: ``Properties of the SN~1987A Circumstellar Ring and the Distance to the Large Magellanic Cloud", 1991, {\it Astrophys. J. (Letters)}, {\bf 380}, L23. Cheng, F.H., Horne, K., Lund, N., Panagia, N., Shrader, C., Gilmozzi, R., Paresce, F.: ``The HST Observations of X-ray Nova Muscae 1991 and Its Spectral Evolution", 1992, {\it Astrophys. J.}, {\bf 397}, 664. A. Sandage, A. Saha, G.A. Tammann, N. Panagia, F.D. Macchetto:``The Cepheid Distance to IC 4182: Calibration of M$_V$(max) for SNIa 1937C and the value of H$_o$, 1992, {\it Astrophys. J. (Letters)}, {\bf 401}, L7. P. Jakobsen, F. Macchetto, N. Panagia: ``Faint Object Camera Observations of the Shape and Expansion of SN 1987A", 1993, {\it Astrophys. J.}, {\bf 403}, 736. R.P. Kirshner, D.J. Jeffery, B. Leibundgut, P.M. Challis, G. Sonneborn, M.M. Phillips, N.B. Suntzeff, R.C. Smith, P.F. Winkler, C. Winge, M. Hamuy, D.A. Hunter, K.C. Roth, J.C. Blades, D. Branch, R.A. Chevalier, C. Fransson, N. Panagia, R.V. Wagoner, J. Craig Wheeler, R.P. Harkness: ``The First {\sl HST} Spectra of a Type Ia Supernova", 1993, {\it Astrophys. J.}, October 1 issue. N. Panagia, D. Baxter, R. Gilmozzi, F.D. Macchetto, R.P. Kirshner, H.-M. Adorf: ``New HST Observations of SN 1987ACircumstellar Ring", 1993, in preparation. P. Jakobsen, R. Albrecht, C. Barbieri, J.C. Blades, A. Boksenberg, P. Crane, J.M. Deharveng, M.J. Disney, T.M. Kamperman, I.R. King, F. Macchetto, C.D. Mackay, F. Paresce, G. Weigelt, D. Baxter, P. Greenfield, R. Jedrzejewski, A. Nota, W.B. Sparks, R.P. Kirshner, N. Panagia: ``First Results from the Faint Object Camera: Supernova 1987A", 1990, {\it BAAS}, {\bf 22}, 1275. N. Panagia, R. Gilmozzi, F.D. Macchetto, H.-M. Adorf, R.P. Kirshner: ``Properties of the Circumstellar Ring around SN 1987A", 1990, {\it BAAS}, {\bf 22}, 1275. N. Panagia, R. Gilmozzi: ``IUE and HST Observations of Supernovae", 1991, ESO/EIPC Workshop``SN 1987A and other Supernovae", ed. I.J. Danziger and K. Kjaer, {\it ESO WCP} No. 37, p. 575- 594. R. Gilmozzi, N. Panagia: ``The Stellar Population of NGC~1850 in the LMC", 1991, Vulcano Workshop``Young Clusters and Early Stellar Evolution", ed. F. Palla, P. Persi and H. Zinnecker, {\it Mem. S.A.It.}, {\bf 62}, 695. F.H. Cheng, N. Panagia, K. Horne, R. Gilmozzi, C. Shrader: `` The HST/FOS Observations of X- ray Nova Muscae 1991", 1992, {\it B.A.A.S.}, {\bf 24}, 686. N. Panagia, A. Sandage, A. Saha, G.A. Tammann, F.D. Macchetto:``The Cepheid Distance to IC 4182 and the Absolute Magnitude of SNIa 1937C" 1992, Proc. Workshop ``Science with the Hubble SpaceTelescope", ed. P. Benvenuti and E. Schreier, p. 216. N. Panagia, R. Gilmozzi, F.D. Macchetto, H.-M. Adorf, D. Baxter, R.P. Kirshner: ``SN 1987A Circumstellar Ring", 1992, Proc. Workshop ``Science with the Hubble Space Telescope", ed. P. Benvenuti and E. Schreier, 222. Cheng, F.H., Horne, K., Panagia, N., Shrader, C., Gilmozzi, R., Paresce, F.: ``The HST Observations of X- ray Nova Muscae 1991", 1992, Proc. Workshop ``Science with the Hubble Space Telescope", ed. P. Benvenuti and E. Schreier, p. 333. D. Jeffery, R.P. Kirshner, P. Challis, J. Pun, A. Filippenko, T. Matheson, D. Branch, R. Chevalier, C. Fransson, N. Panagia, R. Wagoner, J.C. Wheeler, A. Clocchiatti: "An HST Ultraviolet Spectrum of SN 1993J", A.P.J (letters) Submitted. Page 8 ------------------------------------------------------------------------------------ 10. Resources to be supplied by investigator's institution(s). Our institutions provide the basic salary support for all the senior investigators on this project. Students typically receive tuition waivers orfellowship support from the institution in addition to their research stipend. Allof our intitutions have made significant cost-sharing contributions to supplycomputers for this work and they routinely operate extensive networks at no cost to us. At CfA, we have access to considerable software help and hardware for preparationof slides and photographs. Our institutions support the ground- basedobservatories we use to augment this HST work, most significantly CTIO, Lick, andthe MMT. We have many external benefits, such as a preprint series, anextensive astronomical library, and some visitors which are provided without cost tothis project. CfA postdoc Brian Schmidt is not supported by HST funds, butcontributes to the project. Similarly, Bruno Leibundgut is supported by the SwissNational Science Foundation, and not by the HST. Harvard handles the subcontractsto eachof the other institutions without any additional overhead charge. Butbest of all, our institutions provide a rich intellectual atmosphere includingexperts on atomic data, radiative transfer, nucleosynthesis, hydrodynamics ,numerical methods, stellar evolution, shock waves, and supernova observations at otherwavelengths. More than any details of return from the overhead pool, webenefit from the depth of our surroundings. ------------------------------------------------------------------------------------ 11. Address Information Name: ROBERT P. KIRSHNER Category: PI Institution: HARVARD COLLEGE OBSERVATORY Address: MS-19 60 GARDEN STREET City: CAMBRIDGE State: MA Zip Code: 02138 Country: USA Telephone: (617) 495-7519 Telex (or e-mail): 92-1428 ------------------------------------------------------------------------------------ TARGET LIST a) Fixed Targets ID = 6139 [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 ------------------------------------------------------------------------------------------------------------------------------------ Tar| Target | Target | Target |Coord | Radial |Acqui|FLX| Flux data No | Name | Description | Position |Eqnx | Vel. |Prblm|REF| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 300 SN-1993J RA = 09H 55M 24.95S +/- 2000.0 1 V = 19.5 +/- 0.5 .01S, 2 B-V = 1.00 DEC =69D 01' 13.8" +/- 3 E(B-V) = 0.20 0.01" ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 6139 [ 10] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 301 DEFINE SN-1993J WFPC2 IMAGE PC1 F255W cr- 1 800S 30 1 1 CYCLE 4/301.0 - SN93JPH tolerance=0.0 450.0 OTA GROUP 301-306.5 WITHIN 2D Comments: one 800 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 301.5 DEFINE SN-1993J WFPC2 IMAGE PC1 F255W cr- 1 1600S 30 1 1 SN93JPH tolerance=1.0 OTA Comments: two 800 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 302 DEFINE SN-1993J WFPC2 IMAGE PC1 F336W cr- 1 400S 30 1 1 SN93JPH tolerance=0.0 OTA Comments: one 400 second exposures ------------------------------------------------------------------------------------------------------------------------------------ 302.5 DEFINE SN-1993J WFPC2 IMAGE PC1 F336W cr- 1 800S 30 1 1 SN93JPH tolerance=1.0 OTA Comments: two 400 second exposures ------------------------------------------------------------------------------------------------------------------------------------ 303 DEFINE SN-1993J WFPC2 IMAGE PC1 F439W cr- 1 400S 30 1 1 SN93JPH tolerance=0.0 OTA Comments: one 400 second exposures ------------------------------------------------------------------------------------------------------------------------------------ 303.5 DEFINE SN-1993J WFPC2 IMAGE PC1 F439W cr- 1 800S 30 1 1 SN93JPH tolerance=1.0 OTA Comments: two 400 second exposures ------------------------------------------------------------------------------------------------------------------------------------ 304 DEFINE SN-1993J WFPC2 IMAGE PC1 F555W cr- 1 300S 30 1 1 SN93JPH tolerance=0.0 OTA Comments: one 300 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 304.5 DEFINE SN-1993J WFPC2 IMAGE PC1 F555W cr- 1 600S 30 1 1 SN93JPH tolerance=1.0 OTA Comments: two 300 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 305 DEFINE SN-1993J WFPC2 IMAGE PC1 F675W cr- 1 300S 30 1 1 SN93JPH tolerance=0.0 OTA Comments: one 300 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 305.5 DEFINE SN-1993J WFPC2 IMAGE PC1 F675W cr- 1 600S 30 1 1 SN93JPH tolerance=1.0 OTA Comments: two 300 second exposure ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 6139 [ 11] ------------------------------------------------------------------------------------------------------------------------------------ 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 |10 | 11 | 12 |13 |14| 15 ------------------------------------------------------------------------------------------------------------------------------------ Line | Seq | Target |Instr | Oper. | Aper |Spectral|Central| Optional |Num| Time | S/N |Flx|Pr| Special Number | Name | Name |Config| Mode |or FOV |Element |Waveln.| Parameters |Exp| |Rel. Time|Ref| | Requirements ------------------------------------------------------------------------------------------------------------------------------------ 306 DEFINE SN-1993J WFPC2 IMAGE PC1 F814W cr- 1 300S 30 1 1 SN93JPH tolerance=0.0 OTA Comments: one 300 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 306.5 DEFINE SN-1993J WFPC2 IMAGE PC1 F814W cr- 1 600S 30 1 1 SN93JPH tolerance=1.0 OTA Comments: two 300 second exposure ------------------------------------------------------------------------------------------------------------------------------------ 450 USE AT 15-FEB-95 +/- SN93JPH 60D OTA Comments: See question #5 section #1 for scheduling requirments ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 6139 [ 12] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations WFPC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters cr-tolerance=0.0 cr-tolerance=1.0 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO/DD ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 40.00 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category INTERSTELLAR MEDIUM ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category SN & SNR ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements CYCLE 4/301.0 - 450.0; GROUP 301-306.5 WITHIN 2D; AT 15-FEB-95 +/- 60D ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements F255W F336W F439W F555W F675W F814W ------------------------------------------------------------------------------------------------------------------------------------ Target Names SN-1993J ------------------------------------------------------------------------------------------------------------------------------------