! File: 4315C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:21:33:07 coverpage: title_1: CIRCUMSTELLAR MATERIAL AROUND SUPERNOVAE: CYCLE3MEDIUM sci_cat: INTERSTELLAR MEDIUM sci_subcat: SN & SNR proposal_for: GO pi_title: PROF. pi_fname: ALEXEI pi_mi: V. pi_lname: FILIPPENKO pi_inst: UC-BERKELEY pi_country: USA hours_pri: 2.85 num_pri: 3 wf_pc: Y fos: Y funds_length: 12 off_fname: MARION off_mi: B. off_lname: LENTZ off_title: CONT/GRANTS OFFICER off_inst: 1500 off_addr_1: SPONSORED PROJECTS OFFICE off_addr_2: 336 SPROUL HALL off_addr_3: UNIVERSITY OF CALIFORNIA off_city: BERKELEY off_state: CA off_zip: 94720 off_country: USA off_phone: 510-642-8120 ! end of coverpage abstract: line_1: The interaction of a supernova (SN) shock wave with the remnants of the stellar line_2: wind of the progenitor can sometimes provide enough energy to sustain the SN line_3: luminosity for several years. Optical data, supplemented with radio and X-ray line_4: observations, of certain Type II SNe a few years past explosion strongly favor line_5: such an interpretation over other possible energy sources, such as a pulsar or line_6: long-lived radioactive isotopes. The UV spectrum is a powerful diagnostic for line_7: probing the conditions in the shock and the shocked material. We propose to line_8: observe SN 1988Z, the brightest and most recent member of this group. Due to line_9: its extensive radio and optical data records, it is particularly suited for an line_10: investigation of the interaction between ejecta and circumstellar gas. FOS line_11: spectra will be obtained. The UV fluxes will be used to test theoretical line_12: models of the interaction; the C IV line is predicted to be 3 times the line_13: strength of H-alpha, which will be measured from the ground. Optical and line_14: near-UV (UBVRI) images will be obtained with the PC to determine background line_15: contamination corrections for previous ground-based photometry, to measure line_16: accurate current magnitudes, and to investigate the local stellar population line_17: near the SN. HST observations of this object will shed light on the physical line_18: characteristics of its shock, as well as on the mass-loss history of its line_19: progenitor star. ! ! end of abstract general_form_proposers: lname: FILIPPENKO fname: ALEXEI title: PI mi: V. inst: UC-BERKELEY country: USA ! lname: CHEVALIER fname: ROGER mi: A. inst: UNIVERSITY OF VIRGINIA country: USA ! lname: FESEN fname: ROBERT mi: A. inst: DARTMOUTH COLLEGE country: USA ! lname: FRANSSON fname: CLAES inst: STOCKHOLM OBSERVATORY country: SWEDEN esa: Y ! lname: KIRSHNER fname: ROBERT mi: P. inst: CENTER FOR ASTROPHYSICS country: USA ! lname: LEIBUNDGUT fname: BRUNO inst: UC-BERKELEY country: USA esa: Y ! lname: MATHESON fname: THOMAS inst: UC-BERKELEY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: Since the allocated time is considerably less than requested, we will line_2: obtain data only for SN 1988Z (z = 0.022); the TAC said SN 1988Z is mandatory. line_3: We will obtain broad-band optical and near-UV images, and UV spectra. The line_4: broad-band images will be used to measure precise magnitudes and colors line_5: of the SN, to characterize the local environment of the SN (e.g., HII regions, line_6: old stellar populations, etc.), and to quantify the extent to which sources line_7: close to the SN contaminate our ground-based measurements at late times. FOS line_8: spectra will allow us to measure many emission lines and determine the shape line_9: of the continuum, for comparison with the results of theoretical models. line_10: The broad-band optical images will be obtained with the PC. The use of five line_11: standard bands will permit direct comparisons with normal stars and other SNe line_12: observed with HST: F336W (U), F439W (B), F555W (V), F702W (R), and F785LP (I). line_13: The U-band PC image replaces the originally requested FOC F152M image, since the line_14: latter would be very time consuming and the TAC allocated only 5 total hours. line_15: The FOS spectra of SN 1988Z will be obtained with the following settings: line_16: (1) FOS, G130H grating, 1150-1608 A, 1.0 A/diode, blue digicon. line_17: (2) FOS, G190H grating, 1573-2323 A, 1.5 A/diode, red digicon. line_18: (3) FOS, G270H grating, 2227-3306 A, 2.1 A/diode, red digicon. line_19: The high-resolution gratings are needed to readily distinguish the moderately line_20: narrow lines from the SN (FWHM 1500-2000 km/s) from the narrower (unresolved; line_21: FWHM less than 100 km/s) emission lines contributed by underlying HII regions. line_22: A circular aperture 1" in diameter will be used to exclude the brightest HII line_23: region, whose centroid is 1.5"-2" away from SN 1988Z. ! question: 4 section: 1 line_1: The optical ground-based images obtained of SN 1988Z are contaminated, to line_2: some extent, by adjacent HII regions and star clusters in the parent galaxy. line_3: Given the far higher spatial resolution achievable with HST (even in its line_4: currently aberrated state), we will be able to quantify the contamination. line_5: This will allow us to correct our ground-based magnitudes of SN 1988Z obtained line_6: at late times. Moreover, the HST images will provide optical magnitudes and line_7: colors at the present epoch for this faint object. line_8: UV spectra of SN 1988Z cannot be obtained with IUE; it is too faint, and line_9: the IUE aperture would include bright adjacent contaminating sources. The FOS line_10: spectra are of crucial importance for testing theoretical models of the line_11: interaction of supernova ejecta with dense circumstellar gas (Fransson & line_12: Chevalier 1992). No other SN in recent years provides such a good opportunity line_13: for exploring an important new area in SN research, and it is unlikely that line_14: an equally promising candidate will be found in the next few years. line_15: SN 1988Z has been observed extensively from the ground by the PI and line_16: several Co-Is. We anticipate combining the HST data with these results. line_17: We are in an excellent position to make substantial progress in understanding line_18: this interesting and important object; all we lack are the HST data. ! question: 4 section: 2 line_1: The estimated broad-band V mag of SN 1988Z at the time of observation is m = line_2: 22. Consider the F785LP filter (I). From the WFPC handbook, we find that the line_3: integral of QT dl/l is 0.021 for PC6, and we calculate 8.46 counts/s. However, line_4: only about 1/5 of these (i.e., 1.69 counts/s) will fall in the compact core of line_5: the HST PSF. For S/N = 26, we require 400 s. Similarly, t = 300 s is required line_6: for S/N = 40 with the F702W filter (R), t = 350 s for S/N = 38 with the F555W line_7: filter (V), t = 500 s for S/N = 19 with the F439W filter (B), and t = 1300 s line_8: for S/N = 18 with the F336W filter (U). line_9: The H-alpha flux of SN 1988Z was 2 X 10**-14 erg/s/cm**2 in January 1992, line_10: and dropping relatively slowly. The predicted C IV flux is 6 X 10**-14. SN line_11: 1988Z has a very low UV extinction; perhaps the C IV line is down by a factor line_12: of 1.5. If the flux drops and additional factor of 1.5 by the time the data line_13: are taken, the expected flux will be 2.6 X 10**-14 erg/s/cm**2. We wish to line_14: study lines a factor of 10 fainter than this, or 2.5 X 10**-15 cgs. line_15: Consider first the G130H filter, with the blue digicon, at 1400 A. The line_16: efficiency is 0.007 and the throughput of the 1" circular aperture is 0.27. line_17: Using eq. 2 of Table 1.2.1, we find that the line count rate is 0.016/s. The line_18: dark current is comparable to this. For S/N = 6 in the line, we need 75 min. line_19: G190H grating + red dig, at 1900 A: efficiency 0.035, throughput 0.33. Thus, line_20: we detect 0.13 counts/s. To get S/N = 16, we need 33 minutes. G270H grating line_21: + red dig, at 2800 A: efficiency 0.08, throughput 0.38. Thus, we detect 0.50 line_22: counts/s. To get S/N = 20 in an emission line, we require about 15 minutes. line_23: The total time for the FOS spectroscopy is therefore 123 minutes. ! question: 5 section: 1 line_1: None. ! question: 6 section: 1 line_1: None. ! question: 7 section: 1 line_1: Reduction and analysis of images will consist of standard calibrations of line_2: the PC data, followed by stellar photometry and surface photometry. Cosmic ray line_3: events will be identified and removed. Photometry will be performed on an line_4: absolute scale as much as possible. We will measure the colors of SN 1988Z, line_5: and comparisons will be made with the colors of normal stars and other SNe line_6: observed with HST. Colors and color gradients will be studied near SN 1988Z, line_7: to determine stellar populations. We will search for dust features, and line_8: contaminating background sources will be identified. This should allow us line_9: to perform some corrections to the existing light curves. Deconvolution line_10: techniques will be used to improve the effective spatial resolution. line_11: Measurement and analysis of the calibrated one-dimensional spectra will be line_12: done with an extensive program written by the PI for his studies of optical line_13: spectra. All emission lines will be measured (wavelengths, fluxes, equivalent line_14: widths, velocity widths), and the continuum shape will be determined. The line_15: final UV spectrum will be combined with an optical spectrum, to be obtained at line_16: nearly the same epoch (see below). The continuum flux will be extrapolated line_17: beyond the Lyman limit to see whether it can account for the emission lines. line_18: Photoionization codes (G. Ferland's CLOUDY, as well as C. Fransson's own line_19: calculations) will be used to analyze the overall emission-line spectrum. line_20: Extensive comparisons with the theoretical predictions of Fransson & Chevalier line_21: (1992) will be made. ! question: 8 section: 1 line_1: Target acquisition of SN 1988Z in the FOS aperture will be done by line_2: centering on a neighboring star and subsequently offsetting by the line_3: precisely measured displacement of the supernova. line_4: When our HST observing dates become known, we will request roughly line_5: contemporaneous time at Lick Observatory to obtain broad-band optical images line_6: of SN 1988Z, for comparison with the corresponding HST images. This will be line_7: particularly useful for determining correction factors applicable to previous line_8: photometric observations of the object. Also, optical spectra of SN 1988Z line_9: will be obtained, and they will be combined with the HST spectra. The line_10: ground-based observations will be done at no cost to this proposal. ! question: 9 section: 1 line_1: R. P. Kirshner, Co-I: GO 2356, "The Identification of Supernova Remnants line_2: in M83 and Other Spiral Galaxies." (PI: K. S. Long). Not related. line_3: R. P. Kirshner, PI: GO 2417, "Cas A: The Remnant of a Massive Supernova." line_4: Not related to this project; the Cas A remnant is much older. line_5: R. A. Fesen, Co-I: GO 2434, "A Study of the Chemical Composition and Velocity line_6: Structure of the Young Supernova Remnant AD 1006." (PI: C.-C. Wu). Not related. line_7: R. P. Kirshner, PI (Chevalier and Fransson, Co-Is): GO 2563 and GO 3853, line_8: "SINS: Supernova Intensive Study." Not directly related to this project, but line_9: the HST observations of SNe will be useful for comparison with our results. line_10: A. V. Filippenko, PI: GO 2590, "Deep Imaging of the Site of SN 1961V, a line_11: Possible Extragalactic Eta Carinae Analogue." Not related to this project. line_12: R. A. Fesen, PI: GO 2955, "UV Imaging and Spectroscopy of S Andromedae in M31." line_13: Not related to this project; S And was probably a Type I SN. line_14: A. V. Filippenko, Co-I: GO 3484, "Probing the Nuclear Regions of the line_15: Seyfert Galaxy NGC 5548." (PI: B. M. Peterson). Not related to this project. line_16: A. V. Filippenko, PI: GO 3507, "UV Spectroscopy and High-Resolution Imaging line_17: of NGC 4395." Not related to this project. line_18: A. V. Filippenko, Co-I: GO 3519, "UV Imaging of Nearby Galaxies." line_19: (PI: D. Maoz.) Not related to this project. line_20: A. V. Filippenko, Co-I: GO 3810, "The Stellar Content of Wolf-Rayet line_21: Galaxies." (PI: P. Conti.) Not related to this project. line_22: In addition, Filippenko was involved in one of the discoveries made by line_23: the QSO Snapshot Survey (PI: J. N. Bahcall.) ! question: 9 section: 2 line_1: GO 2434 (Fesen): Data obtained and analysed. FOS spectra show strong Fe II line_2: UV features due to multiplets 1-3 (2343, 2382, and 2599 A). These absorptions line_3: have equivalent widths of about 20 A each and indicate an Fe II expansion line_4: velocity of up to 8000 km/s. line_5: GO 2563 and GO 3853 (Kirshner): The earliest observations of SN 1987A line_6: resulted in the detection of a circumstellar ring. Subsequent use of the ring line_7: geometry and fluorescent line time delay enabled a measurement of the distance line_8: to the LMC. Measurements were made of changes in the circumstellar shell. For line_9: SN 1992A, we have combined the data from HST, IUE, and CTIO; comparisons were line_10: made with the results of stellar evolution and supernova explosion models. line_11: GO 2590 (Filippenko): Data were received a few months ago, and are currently line_12: being analyzed. An object has been detected at the position of SN 1961V; line_13: color information is being used to determine whether this is the supernova line_14: remnant, the surviving "progenitor," or an unrelated object. line_15: GO 2955 (Fesen): UV FOC image of S And site reduced. It shows a weak line_16: detection of the SNR as an absorption spot (0.5" diameter) on the M31 budge. line_17: FOS spectra taken of S And are weak and poorly exposed but may show asymmetric line_18: UV Fe II resonance line absorptions. line_19: GO 3507 (Filippenko): We recently received the data. Preliminary analysis line_20: reveals strong emission lines similar to those of luminous Seyfert 1 nuclei line_21: (e.g., C IV 1549, C III] 1909, Mg II 2800) superposed on a weak continuum. line_22: The nucleus seems unresolved on a scale of 1 pc (0.1"). line_23: Other proposals: Data not obtained yet. ! question: 9 section: 3 line_1: "First Results from the FOC: Supernova 1987A." P. Jakobsen et al. (including line_2: R. P. Kirshner); Astrophysical Journal (Letters), 369, L63, 1991. line_3: "Properties of the SN 1987A Circumstellar Ring and the Distance to the Large line_4: Magellanic Cloud." N. Panagia et al. (including R. P. Kirshner); Astrophysical line_5: Journal (Letters), 380, L23, 1991. line_6: "A Gravitational Lens Candidate Discovered with the Hubble Space Telescope." line_7: D. Maoz, J. N. Bahcall, D. P. Schneider, R. Doxsey, N. A. Bahcall, A. V. line_8: Filippenko, W. M. Goss, O. Lahav, and B. Yanny; Astrophysical Journal line_9: (Letters), 386, L1, 1992. line_10: "High-Velocity Fe II Absorption Lines in SNR 1006." C.-C. Wu, D. M. line_11: Crenshaw, R. A. Fesen, A. J. S. Hamilton, & M. Leventhal, in Proceedings of line_12: HST Conference in Elba, Italy; 1992. line_13: "HST Spectra of the Type Ia Supernova 1992A." R. P. Kirshner and the SINS line_14: team, in preparation. ! question: 10 section: 1 line_1: U. C. Berkeley, Harvard University, Dartmouth College, and the University line_2: of Virginia all have extensive computing facilities (VMS and UNIX) in their line_3: Astronomy Departments, as does Stockholm Observatory. Image-processing line_4: workstations, graphics terminals, laser printers, large disks, and tape drives line_5: are all available. Many computer programs exist for analysis of data. All the line_6: universities also have many highly capable graduate students and postdoctoral line_7: fellows, some of whom may participate in various aspects of this project. line_8: Ground-based complementary observations can readily be obtained (with short line_9: notice) at Lick and McGraw-Hill Observatories. The usual secretarial and line_10: technical support is available at all of the institutions. ! !end of general form text general_form_address: lname: FILIPPENKO fname: ALEXEI mi: V. title: PROF. category: PI inst: UC-Berkeley addr_1: DEPARTMENT OF ASTRONOMY addr_2: 601 CAMPBELL HALL addr_3: UNIVERSITY OF CALIFORNIA city: BERKELEY state: CA zip: 94720 country: USA phone: 510-642-1813 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: SN1988Z-OFFSET descr_1: A,137 pos_1: RA = 10H 51M 51.12S +/- 0.03S, pos_2: DEC = 15D 59' 28.18" +/- 0.4" equinox: 2000.0 pm_or_par: N rv_or_z: Z = 0.000 comment_1: G5 OFFSET STAR FOR SN1988Z. fluxnum_1: 1 fluxval_1: V = 15.9 +/- 0.2 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.15 fluxnum_3: 3 fluxval_3: V-R = 0.62 +/- 0.1 fluxnum_4: 4 fluxval_4: V-I = 1.24 +/- 0.1 fluxnum_5: 5 fluxval_5: U-B = 0.2 +/- 0.15 ! targnum: 2 name_1: SN1988Z descr_1: B,182,H,506 pos_1: RA-OFF = -0.943S +/- 0.015S, pos_2: DEC-OFF = +31.55" +/- 0.2", pos_3: FROM 1 equinox: 2000.0 pm_or_par: N rv_or_z: Z = 0.022 comment_1: MAGNITUDES AND FLUXES VERY comment_2: APPROXIMATE; OBJECT FADING comment_3: WITH TIME, VERY SLOWLY. fluxnum_1: 1 fluxval_1: V = 22.0 +/- 1.0 fluxnum_2: 2 fluxval_2: B-V = 0.0 +/- 0.3 fluxnum_3: 3 fluxval_3: V-R = 0.3 +/- 0.3 fluxnum_4: 4 fluxval_4: V-I = 0.0 +/- 0.3 fluxnum_5: 5 fluxval_5: F-LINE(1549) = 1.0 +/- 0.8 E-14 fluxnum_6: 6 fluxval_6: W-LINE(1549) = 6.0 +/- 3.0 ! targnum: 3 name_1: SN1988Z-REGION descr_1: B,182,H,506 pos_1: RA = 10H 51M 50.11S +/- 10", pos_2: DEC = 15D 59' 59.9" +/- 10", pos_3: REGION equinox: 2000.0 pm_or_par: N rv_or_z: Z = 0.022 comment_1: MAGNITUDE, COLOR, AND comment_2: REDSHIFT ARE OF SN1988Z ITSELF. comment_3: MAGNITUDE AND COLOR VERY comment_4: APPROXIMATE; OBJECT FADING comment_5: SLOWLY WITH TIME. fluxnum_1: 1 fluxval_1: V = 22.0 +/- 1.0 fluxnum_2: 2 fluxval_2: B-V = 0.0 +/- 0.3 fluxnum_3: 3 fluxval_3: V-R = 0.3 +/- 0.3 fluxnum_4: 4 fluxval_4: V-I = 0.0 +/- 0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: SN1988Z-REGION config: PC opmode: IMAGE aperture: PC6 sp_element: F791W wavelength: 8922 num_exp: 1 time_per_exp: 400S s_to_n: 26 fluxnum_1: 1 fluxnum_2: 4 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES req_1: CYCLE 3 / 1-9; req_2: GROUP 1-5 NO GAP comment_1: WANT DATA FROM ALL 4 CCDS. comment_2: IF THERE IS EXTRA TIME BEFORE comment_3: EARTH OCCULATION NEAR END OF comment_4: EXPOSURE, CAN INCREASE EXPOSURE comment_5: TIME TO INCREASE S/N RATIO. ! linenum: 2.000 targname: SN1988Z-REGION config: PC opmode: IMAGE aperture: PC6 sp_element: F675W wavelength: 6898 num_exp: 1 time_per_exp: 300S s_to_n: 40 fluxnum_1: 1 fluxnum_2: 4 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES comment_1: WANT DATA FROM ALL 4 CCDS. comment_2: IF THERE IS EXTRA TIME BEFORE comment_3: EARTH OCCULATION NEAR END OF comment_4: EXPOSURE, CAN INCREASE EXPOSURE comment_5: TIME TO INCREASE S/N RATIO. ! linenum: 3.000 targname: SN1988Z-REGION config: PC opmode: IMAGE aperture: PC6 sp_element: F569W wavelength: 5416 num_exp: 1 time_per_exp: 350S s_to_n: 38 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES comment_1: WANT DATA FROM ALL 4 CCDS. comment_2: IF THERE IS EXTRA TIME BEFORE comment_3: EARTH OCCULATION NEAR END OF comment_4: EXPOSURE, CAN INCREASE EXPOSURE comment_5: TIME TO INCREASE S/N RATIO. ! linenum: 4.000 targname: SN1988Z-REGION config: PC opmode: IMAGE aperture: PC6 sp_element: F439W wavelength: 4352 num_exp: 1 time_per_exp: 500S s_to_n: 19 fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES comment_1: WANT DATA FROM ALL 4 CCDS. comment_2: IF THERE IS EXTRA TIME BEFORE comment_3: EARTH OCCULATION NEAR END OF comment_4: EXPOSURE, CAN INCREASE EXPOSURE comment_5: TIME TO INCREASE S/N RATIO. ! linenum: 5.000 targname: SN1988Z-REGION config: PC opmode: IMAGE aperture: PC6 sp_element: F336W wavelength: 3360 num_exp: 1 time_per_exp: 1300S s_to_n: 18 fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=YES comment_1: WANT DATA FROM ALL 4 CCDS. comment_2: IF THERE IS EXTRA TIME BEFORE comment_3: EARTH OCCULATION NEAR END OF comment_4: EXPOSURE, CAN INCREASE EXPOSURE comment_5: TIME TO INCREASE S/N RATIO. ! linenum: 6.000 targname: SN1988Z-OFFSET config: FOS/RD opmode: ACQ/BINARY aperture: 4.3 sp_element: MIRROR num_exp: 1 time_per_exp: 17S fluxnum_1: 1 fluxnum_2: 2 priority: 3 req_1: ONBOARD ACQ FOR 7-9; req_2: GROUP 6-9 NO GAP; comment_1: BLUE SIDE ACQ/BINARY: comment_2: SP-ELEMENT=MIRROR, EXP = 79S. comment_3: NOTE THAT THIS OBSERVATION MUST comment_4: PRECEDE LINES 7-9, BUT THAT LINES comment_5: 7-9 CAN BE EXECUTED IN ANY ORDER comment_6: (PREFERABLY IN THE LISTED ORDER). ! linenum: 7.000 targname: SN1988Z config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G270H wavelength: 2760 num_exp: 1 time_per_exp: 15M s_to_n: 20 fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 5 fluxnum_4: 6 priority: 3 comment_1: IF THERE IS EXTRA TIME BEFORE comment_2: EARTH OCCULTATION NEAR END OF comment_3: EXPOSURE, CAN INCREASE EXPOSURE comment_4: TIME TO INCREASE S/N RATIO. ! linenum: 8.000 targname: SN1988Z config: FOS/RD opmode: ACCUM aperture: 1.0 sp_element: G190H wavelength: 1950 num_exp: 1 time_per_exp: 33M s_to_n: 16 fluxnum_1: 5 fluxnum_2: 6 priority: 4 comment_1: IF THERE IS EXTRA TIME BEFORE comment_2: EARTH OCCULTATION NEAR END OF comment_3: EXPOSURE, CAN INCREASE EXPOSURE comment_4: TIME TO INCREASE S/N RATIO. ! linenum: 9.000 targname: SN1988Z config: FOS/BL opmode: ACCUM aperture: 1.0 sp_element: G130H wavelength: 1380 num_exp: 1 time_per_exp: 86M s_to_n: 6 fluxnum_1: 5 fluxnum_2: 6 priority: 5 comment_1: IF THERE IS EXTRA TIME BEFORE comment_2: EARTH OCCULTATION NEAR END OF comment_3: EXPOSURE, CAN INCREASE EXPOSURE comment_4: TIME TO INCREASE S/N RATIO. ! ! end of exposure logsheet ! No scan data records found