Page 1 PROPOSAL FOR HUBBLE SPACE TELESCOPE OBSERVATIONS ST ScI Use Only ID 5623 Report Date: 18-Jul-95:17:45 Version: ********** Check-in Date: ********** 1.Proposal Title: SINS: THE SUPERNOVA INTENSIVE STUDY TARGET OF OPPORTUNITY - CYCLE 4 ------------------------------------------------------------------------------------ 2. Scientific Category 3. Proposal For 4. Proposal Type 5. Continuation ID INTERSTELLAR MEDIUM GO 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 plan in this program is 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 5623 PI: Robert P. Kirshner Proposal Title: SINS: THE SUPERNOVA INTENSIVE STUDY TARGET OF OPPORTUNITY - CYCLE 4 ------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------ 3. Description of proposed observations. We will observe one TARG OF OPP supernova in Cycle 4 which we will call SN 1994N. Our intention here is to give a narrative description of the observations described in the exposure log sheets. 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 3 ------------------------------------------------------------------------------------ 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. 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. In the past, we have done well by assembling ground-based images and IUE spectra of newly-discovered bright supernovae to prepare for the HST observations. We have worked effectively with the STScI staff to insert the new supernova into the next available slot in the telescope schedule. Page 4 ------------------------------------------------------------------------------------ 6. Description of special calibration exposures. Since all evidence is that the UV fades rapidly in supernovae, there is a premium on rapid response, but observations that begin within about 10 days of discovery are likely to be of great value. Our plan calls for follow-up in both FOS and WFPC observations 30 days after the first set of data, and again at about 300 days. We are quite flexible on the date of this late observation to avoid observing constraints. ------------------------------------------------------------------------------------ 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 5 ------------------------------------------------------------------------------------ 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 6 ------------------------------------------------------------------------------------ 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 = 5623 [ 7] ------------------------------------------------------------------------------------------------------------------------------------ 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| | | | | | | | | ------------------------------------------------------------------------------------------------------------------------------------ 1 SN1994I A,182 ra=13h 27m 47.82s +/- 0.1s, 1950 dec=+47d 26' 58.2" +/- 0.1" ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5623 [ 8] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 501 DEFINE # FOS/RD ACCUM 1.0 G190H 1650- 1 2000S 10 1 1 SEQ 501.0-503.0 NO SN94NSP 2311 GAP EC1 TARG OF OPP / 501- 531 cycle 4 / 501-531 ------------------------------------------------------------------------------------------------------------------------------------ 502 DEFINE # FOS/RD ACCUM 1.0 G270H 2223- 1 2000S 10 1 1 SN94NSP 3278 EC1 ------------------------------------------------------------------------------------------------------------------------------------ 503 DEFINE # FOS/RD ACCUM 1.0 G400H 3240- 1 600S 10 1 1 SN94NSP 4784 EC1 ------------------------------------------------------------------------------------------------------------------------------------ 504 DEFINE # FOS/RD ACCUM 1.0 G190H 1650- 1 2500S 10 1 1 SEQ 504.0-506.0 NO SN94NSP 2311 GAP EC2 ------------------------------------------------------------------------------------------------------------------------------------ 505 DEFINE # FOS/RD ACCUM 1.0 G270H 2223- 1 2500S 10 1 1 SN94NSP 3278 EC2 ------------------------------------------------------------------------------------------------------------------------------------ 506 DEFINE # FOS/RD ACCUM 1.0 G400H 3240- 1 1000S 10 1 1 SN94NSP 4784 EC2 ------------------------------------------------------------------------------------------------------------------------------------ 507 DEFINE SN1994I FOS/RD ACQ/ 0.3 MIRROR SCAN-STEP- 1 12S 1 1 ONBOARD ACQ FOR SN94NSP PEAK X=.172 507.2-507.3 EC3 SCAN-STEP- SEQ 507.0-507.3 Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 ------------------------------------------------------------------------------------------------------------------------------------ 507.2 DEFINE SN1994I FOS/RD ACCUM 1.0 G270H 2223- 1 4000S 10 1 1 SN94NSP 3278 EC3 ------------------------------------------------------------------------------------------------------------------------------------ 507.3 DEFINE SN1994I FOS/RD ACCUM 1.0 G400H 3240- 1 2000S 10 1 1 SN94NSP 4784 EC3 ------------------------------------------------------------------------------------------------------------------------------------ 510.1 SN1994I FOS/RD ACQ/ 4.3 G570H SEARCH-SIZE-X=1 1 5S 10 1 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 510.2 SCAN-STEP- Y=1.204 ------------------------------------------------------------------------------------------------------------------------------------ 510.2 SN1994I FOS/RD ACQ/ 1.0 G570H SEARCH-SIZE-X=6 1 5S 10 1 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 510.3 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5623 [ 9] ------------------------------------------------------------------------------------------------------------------------------------ 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 ------------------------------------------------------------------------------------------------------------------------------------ 510.3 SN1994I FOS/RD ACQ/ 0.3 G570H SEARCH-SIZE-X=5 1 5S 10 1 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=5 511 SCAN-STEP-X=.06 SCAN-STEP-Y=.06 ------------------------------------------------------------------------------------------------------------------------------------ 511 USE SN1994I SN94NSP EC1 Comments: BEGIN SERIES OF 1994N SPECTRA 511.0 TO BE EXECUTED AS SOON AS POSSIBLE AFTER DISCOVERY ------------------------------------------------------------------------------------------------------------------------------------ 512.1 SN1994I FOS/RD ACQ/ 4.3 G570H SEARCH-SIZE-X=1 1 5S 10 1 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=3 512.2 SCAN-STEP- Y=1.204 ------------------------------------------------------------------------------------------------------------------------------------ 512.2 SN1994I FOS/RD ACQ/ 1.0 G570H SEARCH-SIZE-X=6 1 5S 10 1 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=2 512.3 SCAN-STEP- X=.602 SCAN-STEP- Y=.602 ------------------------------------------------------------------------------------------------------------------------------------ 512.3 SN1994I FOS/RD ACQ/ 0.3 G570H SEARCH-SIZE-X=5 1 5S 10 1 1 ONBOARD ACQ FOR PEAK SEARCH-SIZE-Y=5 513 SCAN-STEP-X=.06 SCAN-STEP-Y=.06 ------------------------------------------------------------------------------------------------------------------------------------ 513 USE SN1994I AFTER 511 BY 30D + SN94NSP /- 7D EC2 Comments: BEGIN SERIES OF 1994N SPECTRA ------------------------------------------------------------------------------------------------------------------------------------ 520.1 DEFINE # WFPC2 IMAGE PC1 F160BW 1 2000s 30 1 1 GROUP 520.1-520.3 SN94NPH NO GAP OT1 ------------------------------------------------------------------------------------------------------------------------------------ 520.2 DEFINE # WFPC2 IMAGE PC1 F255W 1 500S 30 1 1 SN94NPH OT1 ------------------------------------------------------------------------------------------------------------------------------------ 520.3 DEFINE # WFPC2 IMAGE PC1 F336W 1 180S 30 1 1 SN94NPH OT1 ------------------------------------------------------------------------------------------------------------------------------------ 522.1 DEFINE # WFPC2 IMAGE PC1 F160BW 1 2000s 30 1 1 GROUP 522.1-522.3 SN94NPH NO GAP OT2 ------------------------------------------------------------------------------------------------------------------------------------ EXPOSURE LOGSHEET ID = 5623 [ 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 ------------------------------------------------------------------------------------------------------------------------------------ 522.2 DEFINE # WFPC2 IMAGE PC1 F255W 1 1000S 30 1 1 SN94NPH OT2 ------------------------------------------------------------------------------------------------------------------------------------ 522.3 DEFINE # WFPC2 IMAGE PC1 F336W 1 300S 30 1 1 GROUP 522.1-522.3 SN94NPH NO GAP OT2 ------------------------------------------------------------------------------------------------------------------------------------ 524.1 DEFINE # WFPC2 IMAGE PC1 F160BW 1 2000s 30 1 1 SN94NPH OT3 ------------------------------------------------------------------------------------------------------------------------------------ 524.2 DEFINE # WFPC2 IMAGE PC1 F255W 1 1000S 30 1 1 SN94NPH OT3 ------------------------------------------------------------------------------------------------------------------------------------ 524.3 DEFINE # WFPC2 IMAGE PC1 F336W 1 600S 30 1 1 GROUP 524.1-524.3 SN94NPH NO GAP OT3 ------------------------------------------------------------------------------------------------------------------------------------ 530 USE SN1994I SN94NPH OT1 Comments: BEGIN PHOTOMETRY OF 94N 530.0 TO BE EXECUTED AS SOON AS POSSIBLE AFTER DISCOVERY ------------------------------------------------------------------------------------------------------------------------------------ 531 USE SN1994I AFTER 530 BY 30D + SN94NPH /- 7D OT2 Comments: BEGIN PHOTOMETRY OF 94N ------------------------------------------------------------------------------------------------------------------------------------ Summary Form for Proposal 5623 [ 11] Item Used in this proposal ------------------------------------------------------------------------------------------------------------------------------------ Configurations FOS/RD WFPC2 ------------------------------------------------------------------------------------------------------------------------------------ Opmodes ACCUM ACQ/PEAK IMAGE ------------------------------------------------------------------------------------------------------------------------------------ Optional Parameters SCAN-STEP-X=.172 SCAN-STEP-Y=.172 SEARCH-SIZE-X=5 SEARCH-SIZE-Y=5 SEARCH-SIZE-X=1 SEARCH-SIZE-Y=3 SCAN-STEP-Y=1.204 SEARCH-SIZE-X=6 SEARCH-SIZE-Y=2 SCAN-STEP-X=.602 SCAN-STEP-Y=.602 SCAN-STEP-X=.06 SCAN-STEP-Y=.06 ------------------------------------------------------------------------------------------------------------------------------------ Proposal for GO ------------------------------------------------------------------------------------------------------------------------------------ S/C Hours 40.00 ------------------------------------------------------------------------------------------------------------------------------------ Scientific Category INTERSTELLAR MEDIUM ------------------------------------------------------------------------------------------------------------------------------------ Scientific Sub-category SN & SNR ------------------------------------------------------------------------------------------------------------------------------------ Special Requirements SEQ 501.0-503.0 NO GAP; TARG OF OPP / 501-531; cycle 4 / 501-531; SEQ 504.0-506.0 NO GAP; ONBOARD ACQ FOR 507.2-507.3; SEQ 507.0-507.3 ONBOARD ACQ FOR 510.2 ONBOARD ACQ FOR 510.3 ONBOARD ACQ FOR 511 ONBOARD ACQ FOR 512.2 ONBOARD ACQ FOR 512.3 ONBOARD ACQ FOR 513 AFTER 511 BY 30D +/- 7D GROUP 520.1-520.3 NO GAP GROUP 522.1-522.3 NO GAP GROUP 524.1-524.3 NO GAP AFTER 530 BY 30D +/- 7D ------------------------------------------------------------------------------------------------------------------------------------ Spectral Elements G190H G270H G400H MIRROR G570H F160BW F255W F336W ------------------------------------------------------------------------------------------------------------------------------------ Target Names SN1994I ------------------------------------------------------------------------------------------------------------------------------------