! File: 4360C.PROP ! Database: PEPDB ! Date: 20-FEB-1994:23:14:50 coverpage: title_1: A SEARCH FOR VERY LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI IN NEARBY title_2: GALAXIES: CYCLE3SUPPLEMENTAL sci_cat: GALAXIES & CLUSTERS sci_subcat: NUCLEI/CORES proposal_for: GO pi_fname: WALLACE pi_mi: W. pi_lname: SARGENT pi_inst: CALTECH pi_country: USA hours_pri: 3.88 num_pri: 13 foc: Y funds_length: 12 off_fname: EARLE off_mi: J. off_lname: FREISE off_title: DIR. SPONSORED RES. off_inst: 1590 off_addr_1: MAIL CODE 213-6 off_addr_2: CALIFORNIA INSTITUTE OF TECHNOLOGY off_city: PASADENA off_state: CA off_zip: 91125 off_country: USA off_phone: 818-356-6357 ! end of coverpage abstract: line_1: Using UV (F220W + F210M) and red (F600M) images obtained with the FOC/96, line_2: we will search for spatially unresolved, UV-bright nuclei in nearby galaxies. line_3: The goals are to discover very low-luminosity AGNs, and to see whether there line_4: is a lower limit to the activity. This is a natural extension of the large line_5: spectroscopic survey we have already conducted at Palomar. Galaxies to be line_6: observed are those in which broad H-alpha emission was either NOT detected or line_7: possibly detected in our ground-based study, but whose morphology (Hubble type) line_8: and narrow emission lines appear similar to those of galaxies in which broad line_9: H-alpha WAS detected. Ultraviolet images of 13 nearby galaxies will be line_10: obtained during Cycle 3. In future cycles, we will propose spectroscopic line_11: observations of the most probable AGNs detected through the imaging study. line_12: In most galaxies, low-luminosity active nuclei are very difficult to discern line_13: at optical wavelengths due to the dominance of the stellar continuum. At UV line_14: wavelengths, on the other hand, contamination from the old stellar population line_15: is low, making it possible to detect a nonstellar continuum. As by-products line_16: of this study, we will publish UV surface photometry of the observed galaxies, line_17: and we will identify interesting morphological features (e.g., dust lanes, line_18: blue stars, HII regions). Moreover, we will be able to recognize compact cores line_19: that may be produced by massive central black holes. ! ! end of abstract general_form_proposers: lname: SARGENT fname: WALLACE title: PI mi: W. inst: CALTECH country: USA ! lname: FILIPPENKO fname: ALEXEI mi: V. inst: UC-BERKELEY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We plan to obtain two FOC images of each of 13 bright, nearby galaxies with line_2: the FOC operating in the F/96 mode with a 512 X 1024 pixel format, a 50 X 25 line_3: micron-square pixel size (0.044" X 0.022" pixels) , and a 22" X 22" field of line_4: view. The first exposure will utilize the F220W filter (in wheel 2) plus the line_5: F210M filter (in wheel 3). This combination ensures that the contribution of line_6: red leaks (normally very important with the FOC, when imaging early-type line_7: galaxies having old stellar populations) will be negligible, as discussed on line_8: pages 62-67 of the FOC Instrument Handbook. It is also better than the F220W line_9: + F231M combination originally proposed, since it avoids emission lines more line_10: completely. (The science is not altered by this minor change, however.) The line_11: second exposure will be done through the F600M filter (wheel 1), to determine line_12: the distribution of red light. line_13: In each case the red exposure is short, but quite important. At the typical line_14: distances and absolute magnitudes of our program galaxies, expected core radii line_15: based on observed core parameter relations are typically 0.2", and many are line_16: expected to my < 0.1". Therefore, since the profiles are likely to be cuspy line_17: anyway, we need to have a method for determining which cores are probably AGNs line_18: (bright in the UV relative to the red) --- the red cusps could just be star line_19: clusters. Measurements of color gradients in the nuclear regions will also line_20: help us eliminate cases in which dust rings or stellar population gradients line_21: produce unresolved (or nearly unresolved) nuclei. ! question: 3 section: 2 line_1: These data will allow us to discover galaxies having unresolved UV-bright line_2: nuclei. Approximate photometry of the nuclei will be done, and the results line_3: will be used to determine spectroscopic exposure times in future proposals. line_4: (The exposure times strongly depend on the surface brightness of the inner line_5: few tenths of an arc second; prior to HST, this was not known for any line_6: galaxies.) We will also perform surface photometry of these images, and we line_7: will look for features such as dust lanes, HII regions, and hot stars in line_8: the circumnuclear regions. ! question: 4 section: 1 line_1: It is extremely difficult to detect a faint, point-like LLAGN in ground- line_2: based images --- at visual wavelengths, the surrounding starlight completely line_3: dominates the image. Even in the U and B bands, observable from the ground, line_4: starlight contamination within the seeing disk is too severe, and in any line_5: case the contribution of a nonstellar continuum is small. Indeed, we have line_6: obtained such images of many galaxies in our sample, but unresolved nuclei line_7: are not visible in them. Ground-based spectroscopic techniques also fail at line_8: such low luminosities; we have pushed spectroscopy to its limit in our line_9: extensive survey for weak, broad H-alpha emission in nearby galactic nuclei. line_10: Around 2200 A, on the other hand, the contribution of starlight is minimal, line_11: yet the FOC on HST is quite efficient. Moreover, with good S/N ratios, a line_12: resolution of 0.1" can be achieved, despite the spherical aberration. line_13: Emission from active nuclei much weaker than currently known can easily be line_14: discerned from the bulge background, as demonstrated in Figure 3. line_15: Prior to HST, not many galaxies had been imaged in the UV. These were mainly line_16: the nearest ones (M31, M33, M83, M51, M101), using brief rocket flights and line_17: and having low (15") spatial resolution. M31 and three other galaxies (M32, line_18: NGC 1399, and M81) were imaged with improved (3") resolution during the ASTRO line_19: mission with the Ultraviolet Imaging Telescope (Bohlin, et al. 1990, ApJ, line_20: 352, 55O; O'Connell et al. 1991, BAAS, 23, 891). Only HST can give us line_21: high-resolution images of a larger sample of galaxies, optimally chosen line_22: (from our ground-based work) for the detection of low-luminosity AGNs. ! question: 4 section: 2 line_1: Quite a few nearby galaxies have already been imaged in the UV with HST; line_2: when possible, we plan to use data from the archives to supplement our line_3: proposed target list. However, most of these were not imaged through a filter line_4: combination that effectively blocks out the red leak. Moreover, red images line_5: were generally not obtained, so it is difficult to determine whether the cuspy line_6: nucleus (if present) is simply a dense concentration of stars. Finally, many line_7: of the imaged galaxies were not good candidates for LLAGNs based on our line_8: existing survey, or were previously known Seyfert galaxies. line_9: The above three limitations (red leak, no red image, galaxies not line_10: necessarily good LLAGN candidates) all apply to the "Snapshot Survey" (Maoz, line_11: PI; Filippenko and others, Co-Is) of Cycle 2. The Snapshot Survey makes line_12: excellent use of what would otherwise be HST idle time, and the results will line_13: be important and interesting, but the data will be distinct from (and line_14: complementary to) those proposed here. ! question: 4 section: 3 line_1: We estimate that the typical central UV surface brightness will be 19.5 line_2: mag per square arcsec (using AB magnitudes, defined by Oke and Gunn, 1983, ApJ, line_3: 266, 713). Adopting the sensitivity curves in the FOC handbook, an 800 sec line_4: exposure will yield a S/N ratio of about 7 per pixel in the central regions line_5: with the F220W + F210M combination. This will allow us to detect the UV line_6: point-like nuclei and to obtain very good photometry of them. The F600M line_7: observation will require only 244 seconds. line_8: The maximum photon count rate, 0.03 counts/s, is sufficiently low that the line_9: FOC/96 in the chosen format (512 X 1024 pixels, 50 microns X 25 microns) line_10: still has a linear response (FOC Instrument Handbook). A central point source line_11: will increase the count rate, but for point sources the saturation rate of line_12: the FOC is higher. We estimate that accurate, direct measurements can be line_13: made of central unresolved sources of UV magnitude 17.5-21. Brighter sources line_14: will reach the saturation rate in the central pixels, and they may also line_15: exceed the 8-bit total count limit, but their counts can subsequently be line_16: reconstructed using the less-exposed pixels in the halo of the point spread line_17: function (PSF). Based on our optical spectroscopy, however, we do not expect line_18: such "bright" AGNs to be present in our chosen sample. ! question: 4 section: 4 line_1: To evaluate the feasibility of this project, we created simulated FOC UV line_2: images of galaxies with parameters typical of our sample. The spheroid of the line_3: simulated galaxy, which fills all of the field of view, was modeled as a line_4: de Vaucouleurs law, with a central UV surface brightness taken from the line_5: recent ASTRO measurements of several galaxies (O'Connell, 1991, private line_6: communication). The image was then convolved with the observed HST PSF, and line_7: the expected amount of noise was added. Point sources of various magnitudes line_8: were added to the nucleus of the galaxy, and at various radii from the center. line_9: As an example, a central point source of mag 20 is easily visible above the line_10: background. Off-nuclear point sources, also discernable, have UV magnitudes line_11: of 22-23 and correspond to small clusters of O-type stars at the distance of line_12: our typical galaxy (10 Mpc). ! question: 5 section: 1 line_1: We had originally requested the F231M + F220W filter combination instead of line_2: the F210M + F220W combination (as requested here). The change does not affect line_3: our science. The new filter combination is slightly superior to the old one, line_4: however, since it more completely avoids any possible emission lines --- it is line_5: a better measure of the continuum. Note that no special calibrations are line_6: required with this change. ! question: 6 section: 1 line_1: None. ! question: 7 section: 1 line_1: The data will be reduced and analyzed with standard image processing line_2: software. Azimuthally averaged surface brightness profiles will be line_3: constructed; these will have very high S/N ratio. We will identify all line_4: unresolved UV sources, paying special attention to the nucleus. Photometry of line_5: these sources will be performed. With the moderately high S/N ratios (per line_6: pixel) that we will achieve, it should be possible to run image deconvolution line_7: algorithms in order to improve the effective spatial resolution of the data line_8: (e.g., King et al. 1991, AJ, 102, 1553; Macchetto et al. 1991, ApJL, 369, line_9: L55). Some algorithms achieve superior spatial resolution at the expense of line_10: less reliable photometry, whereas others preserve the photometric integrity of line_11: the data while giving only moderate resolution. We will use a variety of line_12: techniques to obtain the maximum amount of information from the data. line_13: Color gradients will be measured, and the degree to which a central cusp line_14: is visible in the red images will be quantified. The most probable LLAGNs line_15: will be those in which a very blue, unresolved nucleus is detected, yet line_16: color gradients in the circumnuclear region indicate that the blue color of line_17: the nucleus is not simply due to a centrally-concentrated cluster of hot line_18: young stars. Based on the measured UV brightness of the nucleus and on a line_19: reasonable extrapolation of the starlight component to UV wavelengths, we line_20: will estimate the flux of the unobserved ionizing continuum. This will be line_21: compared with the emission-line fluxes determined from our ground-based line_22: spectra to see whether consistent results are achieved. In future Cycles, line_23: HST spectroscopy will be proposed for the most probable LLAGNs. ! question: 8 section: 1 line_1: None. ! question: 9 section: 1 line_1: GO Program: 2078 line_2: Title: A Search for Primordial Gas: is I Zw 18 a Young Galaxy? line_3: PI: D. Kunth line_4: Co-Is: J. Lequeux, W. Sargent, F. Viallefond line_6: GO Program: 2424 line_7: Title: Quasar Absorption Line Survey (Key Project) line_8: PI: J. Bahcall line_9: Co-Is: W. Sargent, R. Weymann, D. Schneider, G. Hartig, B. Jannuzi, line_10: A. Wolfe, D. Turnshek, B. Savage, J. Bergeron, A. Boksenberg line_12: GO Program: 2590 line_13: Title: Deep Imaging of the Site of SN 1961V line_14: PI: A. Filippenko line_15: Co-Is: R. Goodrich, G. Stringfellow, A. Porter, G. Bower, L. Ho line_17: GO Program: 3507 line_18: Title: UV Spectroscopy and High-Resolution Imaging of NGC 4395. line_19: PI: A. Filippenko line_20: Co-Is: W. Sargent, L. Ho line_21: Provides some of the motivation for this project. ! question: 9 section: 2 line_1: GO Program: 3519 line_2: Title: UV Imaging of Nearby Galaxies. line_3: PI: D. Maoz line_4: Co-Is: A. Filippenko, H. Rix, J. Bahcall, D. Schneider, R. Doxsey, line_5: F. Macchetto line_6: Complementary to, but distinct from, this proposal, as explained line_7: in Sec. 2 and 4. line_9: GO Program: 3810 line_10: Title: The Stellar Population of Wolf-Rayet Galaxies line_11: PI: P. Conti line_12: Co-Is: A. Filippenko, C. Leitherer, C. Robert, W. Sargent, L. Ho, line_13: W. Vacca line_15: GO Program: 4302 line_16: Title: Supernovae and their Local Environment. (Archival) line_17: PI: A. Filippenko line_18: Co-Is: B. Leibundgut, T. Matheson, A. Barth, M. Richmond line_20: GO Program: 4312 line_21: Title: Circumstellar Material around Supernovae. line_22: PI: A. Filippenko line_23: Co-Is: T. Matheson, B. Leibundgut, R. Kirshner, R. Chevalier, R. Fesen ! question: 9 section: 3 line_1: GO Program: 4340 line_2: Title: Origin of Blue Featureless Continuum in Seyfert 2 Nuclei line_3: PI: A. Filippenko line_4: Co-I: L. Ho line_6: GO Program: 4350 line_7: Title: FOS Observations of LINER Galaxy Nuclei. line_8: PI: G. Reichert line_9: Co-Is: A. Filippenko, J. Shields, R. Mushotzky, L. Ho, K. Mason, line_10: G. Branduardi-Raymont, C. Wu, E. Puchnarewicz line_12: GO Program: 4635 line_13: Title: Accretion Disk Line-Profile Hypothesis in Arp 102B. line_14: PI: A. Filippenko line_15: Co-Is: J. Halpern, M. Eracleous, K. Chen line_17: In addition, Filippenko was involved in one of the discoveries made by line_18: the QSO Snapshot Survey (PI J. N. Bahcall). ! question: 9 section: 4 line_1: "A Gravitational Lens Candidate Discovered with the Hubble Space Telescope." line_2: D. Maoz, J. N. Bahcall, D. P. Schneider, R. Doxsey, N. A. Bahcall, A. V. line_3: Filippenko, W. M. Goss, O. Lahav, and B. Yanny; Astrophysical Journal line_4: (Letters), 386, L1, 1992. line_6: "HST Observations of NGC 4395, the Least Luminous Seyfert 1 Nucleus: line_7: Evidence Against the Starburst Hypothesis for Broad-Lined Active Galactic line_8: Nuclei." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent; Astrophysical line_9: Journal (Letters), in press (June 20, 1993 issue). line_11: "NGC 4395: Evidence Against the Starburst Hypothesis for Seyfert 1 Nuclei line_12: and QSOs." A. V. Filippenko, L. C. Ho, and W. L. W. Sargent; in 16th line_13: Texas Symposium/3rd Symposium on Particles, Strings, and Cosmology; line_14: ed. C. Akerlof and M. Srednicki (New York: New York Academy of Sciences), line_15: 1993, in press. line_17: "Was SN 1961V a Genuine Supernova?" G. C. Bower, A. V. Filippenko, L. C. line_18: Ho, G. S. Stringfellow, R. W. Goodrich, and A. C. Porter; BAAS, 1993, line_19: in press. line_21: "The HST Quasar Absorption Line Key Project I. First Observational Results, line_22: Including Lyman-alpha and Lyman Limit Systems." J. N. Bahcall, et al.; line_23: Astrophysical Journal, in press (1993). ! question: 9 section: 5 line_1: "The HST Quasar Absorption Line Key Project II. Data Calibration and Absorption line_2: Line Selection." D. P. Schneider et al.; Astrophysical Journal, in press line_3: (1993). line_5: "The HST Quasar Absorption Line Key Project III. First Observational Results line_6: on the Milky Way Gas." B. Savage et al.; Astrophysical Journal, in press line_7: (1993). line_9: "CCD Imaging of Hubble Space Telescope Quasar Fields." S. Kirhakos, W. L. W. line_10: Sargent, D. P. Schneider, J. N. Bahcall, B. T. Jannuzi, D. Maoz, and T. A. line_11: Small; Publ. Astron. Soc. Pacific, submitted (1993). line_13: "Is There Primordial Gas in I Zw 18?" D. Kunth, J. Lequeux, W. Sargent, and line_14: F. Viallefond; Astron. Astrophys., submitted (1993). ! question: 10 section: 1 line_1: Both Caltech and U.C. Berkeley have extensive computing facilities (VMS line_2: and UNIX) in their Astronomy Departments. Image-processing workstations, line_3: graphics terminals, laser printers, large disks, and tape drives are all line_4: available. Many computer programs exist for analysis of data. Both line_5: institutions also have many extremely capable graduate students and line_6: postdoctoral fellows, a few of whom may participate in various aspects of line_7: this project. Ground-based complementary observations may readily be line_8: obtained at both Palomar and Lick Observatories. The usual secretarial line_9: and technical support is available at Caltech and Berkeley. ! !end of general form text general_form_address: lname: SARGENT fname: WALLACE mi: W. category: PI inst: Caltech addr_1: ASTRONOMY/PALOMAR OBSERVATORY addr_2: MAIL CODE 105-24 addr_3: CALTECH city: PASADENA state: CA zip: 91125 country: USA phone: 818-356-4055 telex: 675425 CALTECH PSD ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC3169 descr_1: E,301,317,910 pos_1: RA = 10H 14M 15.0S +/- 0.1S, pos_2: DEC = +03D 27' 58.9" +/- 1.0" equinox: J2000 rv_or_z: V = +1240 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 10.5 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.3 ! targnum: 2 name_1: NGC3185 descr_1: E,301,312,910 pos_1: RA = 10H 17M 38.5S +/- 0.1S, pos_2: DEC = +21D 41' 17.7" +/- 1.0" equinox: J2000 rv_or_z: V = +1240 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 12.2 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.3 ! targnum: 3 name_1: NGC3254 descr_1: E,301,317,910 pos_1: RA = 10H 29M 19.9S +/- 0.1S, pos_2: DEC = +29D 29' 30.4" +/- 1.0" equinox: J2000 rv_or_z: V = +1270 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.6 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.7 +/- 0.3 ! targnum: 4 name_1: NGC3301 descr_1: E,301,317,910 pos_1: RA = 10H 36M 56.2S +/- 0.1S, pos_2: DEC = +21D 52' 54.7" +/- 1.0" equinox: J2000 rv_or_z: V = +1330 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.4 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.9 +/- 0.3 ! targnum: 5 name_1: NGC3642 descr_1: E,301,312,910 pos_1: RA = 11H 22M 18.0S +/- 0.1S, pos_2: DEC = +59D 04' 28.0" +/- 1.0" equinox: J2000 rv_or_z: V = +1620 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.1 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.5 +/- 0.3 ! targnum: 6 name_1: NGC4036 descr_1: E,301,317,910 pos_1: RA = 12H 01M 26.6S +/- 0.1S, pos_2: DEC = +61D 53' 44.5" +/- 1.0" equinox: J2000 rv_or_z: V = +1380 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 10.5 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.9 +/- 0.3 ! targnum: 7 name_1: NGC4477 descr_1: E,301,312,910 pos_1: RA = 12H 30M 02.2S +/- 0.1S, pos_2: DEC = +13D 38' 11.6" +/- 1.0" equinox: J2000 rv_or_z: V = +1260 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 10.4 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.9 +/- 0.3 ! targnum: 8 name_1: NGC4750 descr_1: E,301,317,910 pos_1: RA = 12H 50M 07.3S +/- 0.1S, pos_2: DEC = +72D 52' 28.3" +/- 1.0" equinox: J2000 rv_or_z: V = +1650 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.5 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.3 ! targnum: 9 name_1: NGC5448 descr_1: E,301,317,910 pos_1: RA = 14H 02M 50.1S +/- 0.1S, pos_2: DEC = +49D 10' 21.0" +/- 1.0" equinox: J2000 rv_or_z: V = +2020 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.5 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.7 +/- 0.3 ! targnum: 10 name_1: NGC5838 descr_1: E,301,317,910 pos_1: RA = 15H 05M 26.3S +/- 0.1S, pos_2: DEC = +02D 05' 58.2" +/- 1.0" equinox: J2000 rv_or_z: V = +1430 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 10.8 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 1.0 +/- 0.3 ! targnum: 11 name_1: NGC6951 descr_1: E,301,317,910 pos_1: RA = 20H 37M 14.2S +/- 0.1S, pos_2: DEC = +66D 06' 20.4" +/- 1.0" equinox: J2000 rv_or_z: V = +1430 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.1 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 1.1 +/- 0.3 ! targnum: 12 name_1: NGC7217 descr_1: E,301,317,910 pos_1: RA = 22H 07M 52.5S +/- 0.1S, pos_2: DEC = +31D 21' 32.6" +/- 1.0" equinox: J2000 rv_or_z: V = +950 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 10.2 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 0.9 +/- 0.3 ! targnum: 13 name_1: NGC7743 descr_1: E,301,317,910 pos_1: RA = 23H 44M 21.2S +/- 0.1S, pos_2: DEC = +09D 56' 03.0" +/- 1.0" equinox: J2000 rv_or_z: V = +1800 comment_1: MAGNITUDES AND COLORS comment_2: REFER TO ENTIRE GALAXY, comment_3: NOT JUST THE NUCLEUS comment_4: WHICH WILL BE IMAGED. fluxnum_1: 1 fluxval_1: V = 11.2 +/- 0.5 fluxnum_2: 2 fluxval_2: B-V = 1.0 +/- 0.3 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC3169 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 11 param_1: PIXEL=50X25 req_1: GROUP 1-2 NO GAP; req_2: CYCLE 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: 2.000 targname: NGC3169 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 12 param_1: PIXEL=50X25 req_1: CYCLE 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: 3.000 targname: NGC3185 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 25 param_1: PIXEL=50X25 req_1: GROUP 3-4 NO GAP; req_2: CYCLE 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: 4.000 targname: NGC3185 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 26 param_1: PIXEL=50X25 req_1: CYCLE 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: 5.000 targname: NGC3254 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 13 param_1: PIXEL=50X25 req_1: GROUP 5-6 NO GAP; req_2: CYCLE 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: 6.000 targname: NGC3254 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 14 param_1: PIXEL=50X25 req_1: CYCLE 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: 7.000 targname: NGC3301 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 15 param_1: PIXEL=50X25 req_1: GROUP 7-8 NO GAP; req_2: CYCLE 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: NGC3301 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 16 param_1: PIXEL=50X25 req_1: CYCLE 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: 9.000 targname: NGC3642 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 1100S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PIXEL=50X25 req_1: GROUP 9-10 NO GAP; req_2: CYCLE 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: 10.000 targname: NGC3642 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 345S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 2 param_1: PIXEL=50X25 req_1: CYCLE 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: 11.000 targname: NGC4036 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 7 param_1: PIXEL=50X25 req_1: GROUP 11-12 NO GAP; req_2: CYCLE 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: 12.000 targname: NGC4036 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 8 param_1: PIXEL=50X25 req_1: CYCLE 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: 13.000 targname: NGC4477 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 17 param_1: PIXEL=50X25 req_1: GROUP 13-14 NO GAP; req_2: CYCLE 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: 14.000 targname: NGC4477 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 18 param_1: PIXEL=50X25 req_1: CYCLE 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: 15.000 targname: NGC4750 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 19 param_1: PIXEL=50X25 req_1: GROUP 15-16 NO GAP; req_2: CYCLE 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: 16.000 targname: NGC4750 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 20 param_1: PIXEL=50X25 req_1: CYCLE 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: 17.000 targname: NGC5448 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 21 param_1: PIXEL=50X25 req_1: GROUP 17-18 NO GAP; req_2: CYCLE 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: 18.000 targname: NGC5448 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 22 param_1: PIXEL=50X25 req_1: CYCLE 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: 19.000 targname: NGC5838 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 23 param_1: PIXEL=50X25 req_1: GROUP 19-20 NO GAP; req_2: CYCLE 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: 20.000 targname: NGC5838 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 24 param_1: PIXEL=50X25 req_1: CYCLE 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: 21.000 targname: NGC6951 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 3 param_1: PIXEL=50X25 req_1: GROUP 21-22 NO GAP; req_2: CYCLE 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: 22.000 targname: NGC6951 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 4 param_1: PIXEL=50X25 req_1: CYCLE 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: 23.000 targname: NGC7217 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 9 param_1: PIXEL=50X25 req_1: GROUP 23-24 NO GAP; req_2: CYCLE 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: 24.000 targname: NGC7217 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 10 param_1: PIXEL=50X25 req_1: CYCLE 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: 25.000 targname: NGC7743 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F210M,F220W wavelength: 2150 num_exp: 1 time_per_exp: 800S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 5 param_1: PIXEL=50X25 req_1: GROUP 25-26 NO GAP; req_2: CYCLE 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: 26.000 targname: NGC7743 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F600M wavelength: 5800 num_exp: 1 time_per_exp: 244S s_to_n: 7 fluxnum_1: 1 fluxnum_2: 2 priority: 6 param_1: PIXEL=50X25 req_1: CYCLE 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. ! ! end of exposure logsheet ! No scan data records found