! Proposal 6728, submission 1 ! PI: David V. Bowen ! Received Tue Apr 23 13:04:45 EDT 1996 ! From: lubenow@stsci.edu ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6728,v 3.1 1996/04/25 20:43:28 pepsa Exp $ ! Hubble Space Telescope Cycle 6 (1996) Phase II Proposal Template ! $Id: 6728,v 3.1 1996/04/25 20:43:28 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: Lubenow ! Phone: 410-338-4928 , E-mail: lubenow@stsci.edu ! ! This partially completed template was generated from a Phase I proposal. ! Name of Phase I Proposal: archive-0869.bowen.prop ! Date generated: Fri Dec 22 16:21:26 EST 1995 ! Proposal_Information ! Section 4 Title: The interstellar medium of nearby galaxies using supernovae as probes Proposal_Category: GO Scientific_Category: GALAXIES & CLUSTERS Cycle: 6 Investigators PI_name: David V. Bowen PI_Institution: Royal Observatory, Edinburgh CoI_Name: Katherine Roth CoI_Institution: Institute for Astronomy Contact: ! Y or N (designate at most one contact) CoI_Name: J. Chris Blades CoI_Institution: Space Telescope Science Institute Contact: ! Y or N (designate at most one contact) CoI_Name: David Meyer CoI_Institution: Northwestern University Contact: ! Y or N (designate at most one contact) Abstract: ! Free format text (please update) We propose using ECH-B and G140L gratings of the GHRS to observe the one bright (V < 12.5) supernova which is likely to occur during Cycle 6 in order to probe the interstellar gas of the host galaxy as well as gas in the local Galactic halo. We wish to observe Mg II and Mg I absorption lines with ECH-B; the 3 kms\ echelle resolution will enable us to resolve individual components within the absorption lines, study the kinematic structure of the absorbing gas, and derive accurate column densities and Doppler parameters of the absorbing clouds. We would use the G140L grating to search for C IV and Si IV absorption, as well as strong low ionization lines of O I, C II, Ni II & Si II. C IV/C II & Si IV/Si II ratios will then provide details on the ionization conditions in the gas. Information on interstellar absorption from any low-redshift galaxy other than our own is sparse, and our aim is to detect lines whose strengths and structures can be compared with Galactic absorption, and QSO absorption line systems found at higher redshift in quasar spectra. Should a SN occur with V < 11, we would add exposures of C IV with the G160M grating, Zn II, Cr II with the G190M grating, and LyAlpha absorption with the G140L grating. Such data would allow us to calculate metallicities and depletions of intervening gas clouds, values which can be compared with higher redshift abundance studies. Questions ! Free format text (please update) Observing_Description: sectionScientific Background & Previous work Bright supernovae (SNae) which explode in external galaxies offer a unique opportunity to study in detail an extragalactic interstellar medium (ISM). The supernova (SN) acts as a bright background source against which absorption from interstellar gas along the line-of-sight can be studied. These sources offer one of the few possibilities to study in detail the physical characteristics of the ISM in a galaxy other than our own, usually along sightlines close to the centers of galaxies. They also provide the brightest extragalactic objects with which to probe the Galactic halo. Unfortunately, SNae are short lived; their eruption in a particular galaxy offers a transitory opportunity to investigate the ISM of one particular galaxy. SNae have been used successfully to probe host galaxy ISMs both from the ground, using Ca II and Na I absorption lines, and more recently, from space. SN 1987A in the Large Magellanic Cloud (LMC) was one of the few SNae bright enough to be observed with IUE (Blades et al. 1988), data which showed absorption from many UV transitions never seen before from a low redshift galaxy. The first SN to be observed with HST was SN1992A, which exploded in the Fornax Cluster galaxy NGC 1380 (Kirshner et al. 1993), and for which we were able to obtain a GHRS spectrum at the wavelength of Mg II using the G270M grating (Bowen, Blades & Pettini 1994; Fig. 1). Mg II is detected from our Galaxy, yet is absent from NGC 1380 to equivalent width limits of W_rmlim ~eq 70 mAngstrom . Since Mg II lines of these equivalent widths trace H I column densities, N(H I), of a few times10^17 cm^-2 (see below), the lack of Mg II is extremely surprising. In April 1993, we executed a Cycle 2 Target of Opportunity GO program to observe Mg II and Mg I absorption along the sightline towards SN 1993J in M81, this time using ECH-B with the GHRS. These data comprise some of the highest resolution observations made in the UV (~ 4 kms\ FWHM) which we combined with ground based optical spectra of Na I D lines obtained at similarly high resolution using the KPNO Coud'e Feed (Bowen et al. 1994). Fig. 2 shows our detection of individual absorption components spanning a total velocity range of -163 < v_\odot < +225 kms , grouped into 3 subcomplexes arising in gas from the disk of M81, from our own Galactic disk and halo, and from intergalactic gas which is probably the tidal debris of interactions between M81 and M82. This sightline is discussed in more detail below. We have been granted time in Cycle 5 to continue this programme, and in this proposal we ask to again be granted ToO time to obtain data towards a suitable SN. sectionProposed Observations & Science Goals The proposed observations depend on the magnitude, V, of the SN. We discuss two possible sets of observations below, and refer to our data of SN 1993J to show what can be derived from these programmes. Case 1: SN with magnitude 11.0 < V < 12.5. We would observe Mg II and Mg I with ECH-B of the GHRS, plus far UV absorption lines with the G140L. Ly-alpha\ would be the most ideal probe of the most tenuous quantaties of gas, but the galaxies which are likely to host the brightest galaxies will be at velocities too low to resolve Ly-alpha\ from the damped absorption profile caused by our own Galaxy. However: 1. observing absorption lines of Mg II will allow us to probe both neutral and ionized gas in the host galaxy and in the Milky Way. Data from ECH-B will give detailed information on the kinematic structure of the absorbing gas. Such information is extremely important for comparisons with higher-redshift Mg II systems observed toward high redshift QSOs at similar resolutions. For example, the kinematic structure of lines observed towards identified absorbers by Lanzetta & Bowen (1992) can be used to infer that absorption may occur through galaxy disks. Until more detailed morpholgical information on the absorbing galaxies is available, comparison with Mg II absorption from low- redshift galaxies offers the best method for understanding what the line profiles actually tell us about the nature and origin of the absorbing gas. For ionized gas, kinematic information cannot be derived from ground-based data; our observations of SN 1993J showed Mg II components at +225 kms\ and -160 kms\ which do not exist in Ca II or Na I (or Mg I) data (Fig. 2). The weakest Mg II absorption lines trace smaller H I column densities. For example, a 10 mAngstrom\ limit to Mg II absorption corresponds to \log N(Mg II) ~eq 11.4 for Doppler parameters of b >= 4 kms ; from simple photoionization models (e.g. Steidel & Sargent 1992), this corresponds to \log N(H I) ~eq 17.2; 2. Absorption lines of Mg I allow us to probe both neutral gas and warm ionized gas in the host galaxy and the Milky Way. In our analysis of the SN 1993J data we showed that the Mg I traced two different phases of the ISM, as tracked from Mg I/Na I column density ratios; components with small ratios arose in neutral clouds, while those with large ratios arose in gas with T > 7000 K . This is because at such temperatures, not only is N(Na I) preferentially removed by collisional ionization, but N(Mg I) also increases through dielectronic recombination. These data provided important extra information to the analysis of gas along the sightline. In Fig. 2 we have included ground based data of Ca IILambda 3933 taken from the La Palma Data Archive (see also Vladilo et al. 1994). The Ca II line profile is very similar to the Mg I profile, which might suggest that little is gained by observing Mg I instead of Ca II. However, large Ca II/Na I ratios would normally be interpreted as being due to an increase in the calcium gas phase abundance. Yet the Mg I/Na I ratios suggests that the large Ca II/Na I ratios may at least in part arise in the Warm Ionized Medium (e.g. Reynolds 1991), in line with earlier suggestions by Routly & Spitzer (1952), Pottasch (1972) and Siluk & Silk (1974), and not simply because of changes in gas depletion; 3. Observations of far UV lines with the G140L will enable us to detect high ionization species of C IV & Si IV. At present, there is virtually no information on C IV absorption by low-redshift galaxies other than the Milky Way, except from the LMC & SMC (e.g. Blades et al. 1988; Fitzpatrick & Savage 1983; Savage & de Boer 1981), and by NGC 4319 (Bowen & Blades 1993). This is despite the fact that the majority of QSO absorption lines observed at high redshift are C IV lines, and that some of the most complex systems with components covering velocity intervals of 600-1000 kms\ are found in C IV systems (Blades et al. 1982, York et al. 1984). As yet, we do not know what types of galaxies cause such systems. The observations we propose would yield W_rmlim= 0.15 Angstrom\ (3Sigma): 70 \% of the C IV absorbing population have equivalent widths greater than this (Sargent, Boksenberg & Steidel 1988). The resolution of the G140L will not allow us to calculate accurate column densities; our aim, however, is principally to detect ions rarely seen in low redshift galaxies to compare with those seen in the Galaxy and at higher redshift. Case 2: SN occurs with V <= 11. For the same number of orbits requested, we would perform the same science described above, plus, we would use: 1. the G160M grating to search for C IV absorption from the host galaxy and from the Milky Way, and the G140L to cover LyAlpha absorption if the host galaxy is at a velocity sufficient that H I absorption will not be blended with local gas; 2. the G200M to observe Zn II and Cr II absorption lines from the host galaxy and from the Milky Way. These lines are extremely valuable diagnostics for measuring the metallicity and depletion of intervening gas clouds, and are particularly interesting for comparing with metallicities and depletions found in high redshift damped LyAlpha systems (see Meyer, Welty & York 1989, Meyer & Roth 1990, and Pettini et al. 1994). Our aim is to reach W_rmlim= 20 mAngstrom\ (3Sigma), a limit which would have enabled us to detect any of the lines observed at high-redshift by Pettini et al. (1994). sectionIs each sightline really unique? To conclude, we highlight the science that could have been performed by observing SN 1994D, to demonstrate that every line of sight to a SN is indeed unique. Unfortunately, the SN was not observed, since this proposal was not accepted by the Cycle 3 TAC. SN 1994D in NGC 4526 reached a maximum of V = 11.7. The sightline was of interest for several reasons. First, NGC 4526 is a S0 galaxy; no absorption has ever been studied towards a galaxy known a priori to have this morphology, and data obtained would have given unique information on the ISM of a galaxy of that type. Second, the sightline lies midway between the center of the Virgo Cluster (5degreespoint 3 away) and 3C 273 (5degreespoint 8 away). The discovery of weak LyAlpha lines at Virgo Cluster velocities towards 3C 273 was one of the first major results to come from the HST spectrographs (Bahcall et al. 1991; Morris et al. 1991). Clearly, the search for LyAlpha lines at similar velocities along a parallel sightline with the G140L would have been very interesting. Comparison could also have been made with the sightline towards SN 1991T which exploded in NGC 4527 5degreespoint 3 away (Meyer & Roth 1991), along which Ca II was detected from Galactic High Velocity Clouds. centerline figure=sn.fig1.ps,height=8cm,angle=270 small Figure 1. Normalised spectrum of SN 1992A observed with the G270M grating of the GHRS. Strong Mg IILambdaLambda 2796,2803 absorption is detected from our own galaxy, yet none is seen at the velocity of the host galaxy NGC 1380, to sensitive equivalent width limits. NGC 1380 lies close to the center of the Fornax Cluster, and Bowen, Blades & Pettini (1994) suggest that no absorption is seen because the gas is highly ionized. vspace*.3cm centerline figure=sn.fig2.ps,height=8cm,angle=270 small Figure 3. The frequency of SNae brighter than V = 12.5 from 1980 through July 1994 calculated from the compilation of Barbon, Capellaro & Turatto (1989) and IAU Circulars. We expect that one SN will be found with V <= 12.5 during Cycle 6. vspace*-1.3cm centerline figure=sn.fig3.ps,height=15cm vspace*-3cm small Figure 2. Normalised portions of HST and ground based spectra toward SN 1993J in M81, showing absorption from Mg II & Mg I (obtained with HST), Na I (obtained with KPNO 0.9 m coud'e feed) and Ca II (extracted from the La Palma Archive). The absorption is grouped into roughly three complexes, representing absorption from the disk of M81 (v_\odot < -100 kms), from the Galactic disk & halo (-100 < v_\odot < 0 kms) and from tidal debris (v_\odot > 0 kms), which exists as a result of interactions between M81, M82 and neighbouring galaxies. The HST data arose from a Cycle 2 ToO program, and it is this program that we ask to continue in this proposal. \references em Bahcall, J. N., Jannuzi, B. T., Schneider, D. P., Hartig, G. F., Bohlin, R., & Junkkarinen, V. 1991, ApJ (Letters), 377, L5 em Barbon, R., Cappellaro, E., & Turatto, M., A&AS, 81, 421 em Blades, J. C., Hunstead, R. W., Murdoch, H. S., Pettini, M. 1982, MNRAS, 200, 1091 em Blades, J. C., Wheatley, J. M., Panagia, N., Grewing, M., Pettini, M., & Wamsteker, W. 1988, ApJ, 334, 308 em Bowen, D. V., & Blades, J. C. 1993, ApJ (Letters), 403, 55 em Bowen, D. V., Roth, K. C., Blades, J. C., & Meyer, D. M. 1994, ApJ (Letters), 420, 71 em Bowen, D. V., & Blades, J. C., & Pettini, M., 1995, ApJ, submitted em Kirshner et al. 1993, ApJ , 415, 589 em Lanzetta, K. M., & Bowen, D. V. 1992, ApJ, 391, 48 em Meyer, D. M., Welty, D. E., & York, D. G. 1989, ApJ (Letters), 343, L3 em Meyer, D. M., & Roth, K. C. 1990, ApJ, 363, 57 em Meyer, D. M., & Roth, K. C. 1991, ApJ, 383, L41 em Morris, S. L., Weymann, R. J., Savage, B. D., & Gilliland, R. L. 1991, ApJ (Letters), 377, L21 em Pettini, M., Smith, L. J., Hunstead, R. W., & King, D. L. 1994, ApJ, 426, 79 em Pottasch, S. R. 1972, A&A, 20, 245 em Reynolds, R. J. 1991, in IAU Symp. 144, The Interstellar Disk-Halo Connection in Galaxies, ed. H. Bloemen (Dordrecht: Kluwer), 67 em Routly, P. M. & Spitzer, L., Jr. 1952, ApJ, 115, 227 em Sargent, W. L. W., Boksenberg, A., & Steidel, C. C. 1988, ApJS, 68, 539 em Siluk, R. S. & Silk, J. 1974, ApJ, 192, 51 em Steidel, C. C., & Sargent, W. L. W. 1992, ApJS, 80, 1 em Vladilo, G., Centuri'on, M., de Boer, K. S., King, D. L., Lipman, K., Stegert, J., Unger, S. W., and Walton, N. A. 1994, A&A, xxx, xxx em York, D. G., Green, R. F., Bechtold, J. & Chaffee, F. H., Jr. 1984, ApJ (Letters), 280, L1 \endreferences Real_Time_Justification: The magnitude limit which will determine whether this ToO programme would be activated is based on the frequency of V < 12.5 SNae. Fig. 3 shows the number of SNae per year within this limit frequency for the last 14 years, based on the compilation by Barbon, Capellaro & Turatto (1989) and IAU Telegrams from 1990 to June 1994. The figure shows that we can expect roughly 1 SN brighter than 12.5 during a cycle, a prediction confirmed during Cycles 2-4. As the UV flux of SNae are known to drop sharply after the explosion, we would activate our proposal immediately. Observations of SN 1993J, SN 1992A & SN1994I demonstrate that HST is well able to respond to these ToOs. We will seek to obtain ground-based optical data to complement the HST data we obtain. Calibration_Justification: ! Move appropriate text from Real_Time_Justification The most accurate wavelength calibration possible is required so that the HST data can be compared with optical data obtained at echelle resolutions from the ground. Hence WAVE exposures are requested. Additional_Comments: Generic_Targets ! Section 5.3 Target_Number:1 Target_Name:SN1996X Description:ext-star,supernova;ext-medium,absorption line system Criteria:SN must be brighter than one of the quoted fluxes to execute Flux:V=12.5,F(2800)=1.5e-14 Comments: Visits Visit_Number:10 Visit_Requirements:ON HOLD;GROUP 10-11 WITHIN 12H On_Hold_Comments:Visits 10-11 conditional on SN fainter than V=11, brighter than V=12.5 Visit_Comments:First visit for MgII and far UV ions. Visit 11 should follow visit 10 ASAP. Continuous exposures over <=3 orbits without SPYBAL are included assuming that the spectrum's drift over 3 orbits is negligible. ! ********************************ACQ begins***************************** Exposure_Number:100 Target_Name:SN1996X Config:HRS Opmode:ACQ Aperture:2.0 Sp_Element:MIRROR-N2 Wavelength: Optional_Parameters:bright=return;search-size=3 Number_of_Iterations:1 Time_Per_Exposure:18s Special_Requirements:ONBOARD ACQUISITION FOR 200-400 Comments:STEP-TIME=2s ! **********************END OF ACQ********************************* ! **********************ECH settings, MgII********************* Exposure_Number:200 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:ECH-B Wavelength:2800.5 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments:Wave calib for 300. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity Exposure_Number:300 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-B Wavelength:2800.5 Optional_Parameters:fp-split=two;step-patt=7;doppler=def;spybal=no Number_of_Iterations:30 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing MgII. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. 1st set of exposures. Exposure_Number:350 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:ECH-B Wavelength:2800.5 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments:Wave calib for 370, really to set SPYBAL again. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. When orbit length known, WAVE should not cross occultation. Exposure_Number:370 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-B Wavelength:2800.5 Optional_Parameters:fp-split=two;step-patt=7;doppler=def;spybal=no Number_of_Iterations:35 Time_Per_Exposure:217.6s ! 27.2 sec is min exp, Special_Requirements: Comments: Observing MgII. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. 2nd set of exposures. Total req=4.3hrs Exposure_Number:400 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G140L Wavelength:1421 Optional_Parameters:fp-split=two Number_of_Iterations:23 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing high ions in far UV. Total req=2.0 hrs. ! ****************************************************************** ! End of First visit, ! Start second visit to do MgI ! ******************************************************************* !Visits Visit_Number:11 Visit_Requirements:ON HOLD;GROUP 10-11 WITHIN 12H On_Hold_Comments:Conditional on SN fainter than V=11, brighter than V=12.5 Visit_Comments:Second set of orbits, observing MgI.Continuous exposures over <=3 orbits without SPYBAL are included assuming that the spectrum's drift over 3 orbits is negligible. ! **************************Re-ACQ the SN***************************** Exposure_Number:500 Target_Name:SN1996X Config:HRS Opmode:ACQ Aperture:2.0 Sp_Element:MIRROR-N2 Wavelength: Optional_Parameters:bright=return;search-size=3 Number_of_Iterations:1 Time_Per_Exposure:18s Special_Requirements:ONBOARD ACQuisition FOR 600-700 Comments: STEP-TIME=2s Exposure_Number:600 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:ECH-B Wavelength:2852.0 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments: Wave calib for 700. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. Exposure_Number:700 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-B Wavelength:2852.0 Optional_Parameters:fp-split=two;step-patt=7;doppler=def;spybal=no Number_of_Iterations:30 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing MgI. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. 1st set of exposures. Exposure_Number:750 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:ECH-B Wavelength:2852.0 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments: Wave calib for 790, really for setting SPYBAL. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. When orbit length known, WAVE should not cross occultation. Exposure_Number:790 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-B Wavelength:2852.0 Optional_Parameters:fp-split=two;step-patt=7;doppler=def;spybal=no Number_of_Iterations:35 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing MgI. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. 2nd set of exposures. Total Time Needed=4.3hrs. ! ******************************************************************** ! End of both visits for faint SN ! Second set of visits for brighter SN ! ******************************************************************** Visit_Number:20 Visit_Requirements:ON HOLD; GROUP 20-21 WITHIN 12H On_Hold_Comments:Visits 20-21 conditional on SN brighter than V=11 Visit_Comments:Visit 21 should follow 20 asap. First group to observe far UV and MgII. Continuous exposures over <=3 orbits without SPYBAL are included assuming that the spectrum's drift over 3 orbits is negligible. ! **************************Begin ACQ************************* Exposure_Number:100 Target_Name:SN1996X Config:HRS Opmode:ACQ Aperture:2.0 Sp_Element:MIRROR-N2 Wavelength: Optional_Parameters:bright=return;search-size=3 Number_of_Iterations:1 Time_Per_Exposure:18s Special_Requirements:ONBOARD ACQuisition FOR 200-700 Comments: STEP-TIME=2s ! ***********************End of ACQ*********************** Exposure_Number:200 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:G160M Wavelength:1550.0 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments: Wave calib for 300. Searching for CIV. Since UV flux of SN dies rapidly, far UV observations should be made first Exposure_Number:300 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G160M Wavelength:1550.0 Optional_Parameters:fp-split=two;spybal=no Number_of_Iterations:30 Time_Per_Exposure:217.6s Special_Requirements: Comments:Observing CIV. Total Time Needed=1.5 hrs ! ***************************Back to echs*************************** Exposure_Number:500 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:ECH-B Wavelength:2800.5 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments:Wave calib for 600. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. When orbit length known, WAVE should not cross occultation. Exposure_Number:600 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-B Wavelength:2800.5 Optional_Parameters:fp-split=two;step-patt=7;doppler=def; spybal=no Number_of_Iterations:22 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing MgII. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. Total Time Needed=1.3 hrs Exposure_Number:700 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G140L Wavelength:1310 Optional_Parameters:fp-split=two Number_of_Iterations:11 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing high ions in far UV, including Lyman-a. Total T req=0.5 hrs ! ****************************************************************** ! End of first visit; begin 2nd visit for MgI and Zn, Cr ! ****************************************************************** Visit_Number:21 Visit_Requirements:ON HOLD; GROUP 20-21 WITHIN 12H On_Hold_Comments:Visits 20-21 conditional on SN brighter than V=11 Visit_Comments:Visit 21 should follow 20 asap. Second group to observe MgI and Zn, Cr. Continuous exposures over <=3 orbits without SPYBAL are included assuming that the spectrum's drift over 3 orbits is negligible. ! ******************************Begin re-ACQ************************* Exposure_Number:700 Target_Name:SN1996X Config:HRS Opmode:ACQ Aperture:2.0 Sp_Element:MIRROR-N2 Wavelength: Optional_Parameters:bright=return;search-size=3 Number_of_Iterations:1 Time_Per_Exposure:18s Special_Requirements:ONBOARD ACQuisition FOR 800-950 Comments: STEP-TIME=2s ! *******************************End re-ACQ*************************** Exposure_Number:800 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G200M Wavelength:2060.0 Optional_Parameters:fp-split=two;spybal=yes Number_of_Iterations:29 Time_Per_Exposure:217.6s Special_Requirements: Comments:Observing Zn & Cr. Correct wavelength setting for G200M is unknown, and depends critically on host galaxy velocity. 1st set. Exposure_Number:850 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:G200M Wavelength:2060.0 Optional_Parameters:fp-split=two;spybal=yes Number_of_Iterations:38 Time_Per_Exposure:217.6s Special_Requirements: Comments:Observing Zn & Cr. Correct wavelength setting for G200M is unknown, and depends critically on host galaxy velocity. 2nd set. Total Time Needed=5.0 hrs Exposure_Number:900 Target_Name:wave Config:HRS Opmode:accum Aperture:SC2 Sp_Element:ECH-B Wavelength:2852.0 Optional_Parameters: Number_of_Iterations:1 Time_Per_Exposure:def Special_Requirements: Comments: Wave calib for 950. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. When orbit length known, WAVE should not cross occultation. Exposure_Number:950 Target_Name:SN1996X Config:HRS Opmode:ACCUM Aperture:2.0 Sp_Element:ECH-B Wavelength:2852.0 Optional_Parameters:fp-split=two;step-patt=7;doppler=def; spybal=no Number_of_Iterations:22 Time_Per_Exposure:217.6s Special_Requirements: Comments: Observing MgI. Correct wavelength setting for ECH-B is unknown, and depends on host galaxy velocity. Total Time Needed=1.3 hrs 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: Royal Observatory, Edinburgh Blackford Hill Edinburgh EH9 3HJ United Kingdom ! ! 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