! File: 4644C.PROP ! Database: PEPDB ! Date: 22-FEB-1994:20:56:54 coverpage: title_1: THE NUCLEI OF NEARBY S0 AND SPIRAL GALAXIES-I title_2: A PC SNAPSHOT IMAGING SURVE CYCLE 3 HIGH sci_cat: GALAXIES & CLUSTERS sci_subcat: NUCLEI/CORES proposal_for: SNAP pi_fname: GARTH pi_mi: D pi_lname: ILLINGWORTH pi_inst: LICK OBSERVATORY pi_country: USA hours_pri: 8.34 num_pri: 200 wf_pc: Y realtime: N time_crit: N funds_length: 12 off_fname: MARK off_lname: COBURN off_title: MANAGER off_inst: 1552 off_addr_1: CONTRACTS AND GRANTS OFFICE off_addr_2: APPLIED SCIENCES, MS455 off_addr_3: UNIVERSITY OF CALIFORNIA off_city: SANTA CRUZ off_state: CA off_zip: 95064 off_country: USA off_phone: 408 459 2778 ! end of coverpage abstract: line_1: Striking results have been obtained from HST images of the cores of nearby line_2: galaxies, such as NGC 1068, NGC 1275, NGC 7457, M32 and M87. The diffraction- line_3: limited core of the HST PSF is uniquely suited to identifying compact line_4: structures. So far, the majority of HST observations of nuclei have been on line_5: elliptical galaxies, and on the very nearest early-type spiral galaxies. The line_6: nuclei of spiral galaxies are likely to prove as interesting as those of the line_7: elliptical sample. An excellent example of this is the PC image of M51 with line_8: its X-shaped subarcsecond dust lanes. We propose a SNAPSHOT PC imaging survey line_9: of a subset of a nearby redshift-limited sample of disk galaxies (spiral plus line_10: S0) to characterize the nuclei of galaxies over a broad range of Hubble types line_11: within a variety of environments, down to luminosities some 2 magnitudes line_12: fainter than L_star. A sample of 200 galaxies will be provided, of which we line_13: hope that at least 100 can be observed. These data will provide invaluable line_14: statistics on the presence of nuclear cusps, stellar condensations, inner line_15: stellar disks and dust lanes in disk galaxies. The properties derived for line_16: nearby "normal" galactic nuclei will also provide a reference set for studies line_17: of rarer objects, such as AGNs. Furthermore, the archival database of such line_18: observations will be a resource for more detailed study of galactic nuclei in line_19: later HST cycles, when the improved PSF will allow more comprehensive line_20: spectroscopic and imaging studies to be carried out. ! ! end of abstract general_form_proposers: lname: ILLINGWORTH fname: GARTH title: PI mi: D inst: LICK OBSERVATORY country: USA esa: N ! lname: FRANX fname: MARIJN inst: CENTER FOR ASTROPHYSICS country: USA esa: N ! lname: LAUER fname: TOD mi: R inst: KITT PEAK NATIONAL OBSERVATORY country: USA esa: N ! lname: MACKENTY fname: JOHN mi: W inst: STSCI country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: This project is a survey of the nuclei of nearby disk line_2: galaxies. Such nuclei have NOT been the subject of an line_3: extensive survey with HST, with a few exceptions amongst line_4: the nearest galaxies. The ability of HST to resolve line_5: structures FAR beyond what can be done from the ground has line_6: been demonstrated during cycle 1 and makes this program line_7: uniquely suited to the current capabilities of HST. The line_8: short exposures will be used to establish the surface line_9: brightness profile of the nucleus and to identify unusual line_10: nuclear condensations (e.g., star forming clumps), nuclear line_11: point sources, compact stellar or gaseous disks and dust line_12: lanes on subarcsecond scales. Observations will be made in line_13: SNAPSHOT mode using PC6 with Coarse Track guiding of the line_14: nuclei of a sample of S0 and Spiral galaxies. ! question: 3 section: 2 line_1: The observations are taken with the F555W filter line_2: Exposure times are typically 300s. The line_3: objects chosen for observation by the scheduling group can line_4: be selected at random from the list. The sample of ~200 line_5: galaxies is selected from the Revised Shapley Ames line_6: catalog, with input from the Third Reference Catalog, with line_7: the following constraints. line_8: (1) spiral or S0 galaxy, of RC2/RC3 type -3 to +7 (i.e., line_9: early S0 to Sd); line_10: (2) brighter than ~L* - 2 mag; line_11: (3) velocity < 1000km/s. line_12: (4) distribution of the selected subset will be a uniform line_13: fraction of the bivariate distribution over luminosity and line_14: Hubble type for S0, S and SB galaxies; line_15: (5) list complemented by a fractional selection in two line_16: higher density regions, namely in the Virgo and Fornax line_17: clusters, with such galaxies to be about 40% of the total; ! question: 4 section: 1 line_1: Several ground-based imaging programs have been carried out line_2: over the years on the nuclei of a small number of nearby line_3: galaxies. The best efforts to date have come through the line_4: use of a high-resolution camera system (HRCAM) on the CFHT line_5: 3.6 m telescope. Under good conditions this system can line_6: return images with FWHM of some 0.3 arcsec (though more line_7: typical images for modern telescopes at the best sites are line_8: closer to 0.6-0.7 arcsec). Adaptive optics systems on line_9: ground-based telescopes have great potential, but use of line_10: such systems for routinely obtaining calibrated, line_11: well-characterized astronomical observations lies in the line_12: future. As we all know from detector technology line_13: developments, the future always looks promising, but it is line_14: invariably further away from routine astronomical use than line_15: we care to admit. We can carry out a unique scientific line_16: program on galaxy nuclei now with HST, and should do so. line_17: Since this is a survey it will potentially provide a sample line_18: of objects for which further more detailed study in future line_19: HST cycles (following the recovery mission) would be of line_20: great interest. ! question: 4 section: 2 line_1: line_2: Burrows et al (1991) showed that the diffraction-limited line_3: core of the HST image has a FWHM of 70 milliarcsecs in line_4: F555W (and recent results indicate that the FWHM may be line_5: smaller than the models suggest), with a Strehl ratio of line_6: ~10% ( a measure of the energy within the diffraction line_7: limited core). Some 15% of the energy in the PSF lies line_8: within a radius of 0.1 arcsec. While slightly undersampled line_9: by the PC pixelation (43 mas pixels) this is hugely better line_10: than we can do from the ground. Ground-based images at 0.5 line_11: arcsec FWHM (a value never reached on most telescopes, and line_12: only rarely exceeded on some) with a comparable-sized line_13: telescope provide images with a Strehl ratio of ~1%, an line_14: order of magnitude worse than HST. As can be seen from line_15: Figure 1, and as other results have indicated, this line_16: difference in the PSF size is a huge one. Very valuable line_17: scientific results have been obtained in going from the line_18: typical 1-2 arcsec seeing to occasional 0.3-0.5 arcsec line_19: seeing at a few ground-based sites -- yet we have a gain in line_20: resolution from the best ground-based results to HST that line_21: is proportionally larger. As was clearly demonstrated for line_22: M32 by Lauer et al. (1992), HST remains uniquely able to line_23: carry out such imaging programs. ! question: 4 section: 3 line_1: We have selected PC6 and the F555W filter for this project line_2: as this combination is one of those chosen for PSF line_3: monitoring and for which the CCD calibration data is likely line_4: to be amongst the most well-established. The nominal line_5: center of PC6 will also be used, as in the other programs line_6: on nearby galactic nuclei (primarily on ellipticals). It line_7: is also consistent with other GTO and GO programs of line_8: imaging of nearby galactic nuclei. Thus our data can line_9: subsequently be combined with that in the archive from line_10: those surveys to give a large consistent sample of high line_11: resolution images on the nuclei of nearby galaxies. line_12: Experience with these other surveys indicates that line_13: integrations of ~300s will be a satisfactory compromise line_14: value between good S/N and the risk of saturation in the line_15: nuclei. Both NGC 7457 and M32 have unresolved, high line_16: surface brightness stellar cusps at their center. With a line_17: 300 s integration time, neither nucleus would not have line_18: saturated. While a wide dispersion in central surface line_19: brightnesses is likely, those nuclei in our sample that line_20: saturate at this integration time (if any) will be amongst line_21: the highest surface brightness nuclei known and certainly line_22: worthy of observation in future HST cycles. ! question: 5 section: 1 line_1: This is a SNAPSHOT program. No special calibration of line_2: scheduling requests are needed. ! question: 7 section: 1 line_1: The team members already have considerable experience with line_2: WF/PC data (MacKenty, Lauer), or soon will have (Franx, line_3: Illingworth). In addition, all team members are deeply line_4: involved in HST projects that are using the PC to study the line_5: nature of galactic nuclei. Thus, this survey is a very line_6: natural extension of their ongoing programs. This line_7: experience means that by the time the snapshot data line_8: acquisition commences we will have in place the procedures line_9: and software for handling PC images of nuclei. While the line_10: nuclei of the spirals will propably present us with unique line_11: problems, our experience base will ensure that we can move line_12: quickly to develop and utilize the necessary changes to our line_13: existing procedures and software. ! question: 7 section: 2 line_1: We have experience with deconvolution techniques (primarily line_2: Lucy-Richardson) and can utilize that where necessary. line_3: The use of a standard filter (F555W) and the nominal line_4: position in PC6 will ensure that we are can utilize the line_5: results of the ongoing PSF monitoring programs and also line_6: take advantage of improvements in the PSF model. Model line_7: fitting procedures will also be used. One such approach line_8: is to fit a surface brightness profile directly to the line_9: data, by an iterative procedure that convolves the profile line_10: with the PSF, determine the residuals from the fit, and line_11: then adapt the surface brightness profile. Procedures line_12: which involve both deconvolution and model fitting have line_13: been shown to yield good results and will be used for these line_14: galaxies. Different approaches will be used to verify that line_15: reliable results are being obtained from restored and/or line_16: fitted data. ! question: 7 section: 3 line_1: line_2: This project is quite interesting for the involvement of a line_3: student because of the broad scientific issues that are line_4: dealt with in the analysis and interpretation of the data. line_5: The large volume of data that can arise from this program line_6: also requires a substantial concentration of effort. The line_7: students can complement and support the team members in line_8: their areas of responsibility. ! question: 7 section: 4 line_1: In certain aspects of the program, namely definition of the line_2: sample, interpretation of the results and writing the line_3: papers, all four team members will work closely. However, line_4: to ensure timely publication of the results of the program, line_5: broad areas of responsibility have been defined and are line_6: summarised below. Areas where students are expected to line_7: play a major role are also noted. line_8: preliminary definition of sample and derivation of line_9: positions -- Franx and Illingworth; line_10: responding to any scheduling issues and preliminary line_11: evaluation of the data -- MacKenty; line_12: calibration and processing of the data -- MacKenty and line_13: Lauer (student); line_14: model fitting and deconvolutions -- Franx, Lauer and line_15: Illingworth (student); line_16: implications and interpretation -- Franx, Illingworth, line_17: Lauer and MacKenty; line_18: ground-based observations for any required kinematical line_19: data -- Franx, Illingworth and Lauer. line_20: theoretical modelling -- Franx (student); line_21: paper(s) draft -- Illingworth; line_22: paper(s) final version -- Franx,Illingworth, Lauer and MacKenty. ! question: 8 section: 1 line_1: Per request of STScI/SPD, this proposal (originally GO 4644) line_2: has been divided into four parts so that each part has about 50 line_3: targets. The titles have "-I,-II,-III,or -IV" appended line_4: to reflect this change. The cover page and all general form line_5: questions have been left the same on each proposal. line_7: Positions for the list of target galaxies will be derived line_8: initially from the Third Reference Catalog. These then line_9: require accurate positions derived from the guide star line_10: catalog with GASP, as has been done for other samples of line_11: nearby galaxies. Results to date (e.g., from program line_12: GO2600) suggest that positions accurate to approximately 2 line_13: arcseconds can be obtained. This is quite adequate for line_14: the PC observations. ! question: 9 section: 1 line_1: The PI and Co-Is are involved in other HST projects. Many line_2: of these have only begun to obtain data in the latter part line_3: of cycle 1, or are awaiting data from cycle 2. Lauer is line_4: a member of the WF/PC IDT and already has several line_5: publications resulting from IDT data obtained to date line_6: (primarily from 1105 and 1118, but also from 1105-1138). line_7: Other proposals that the team members are involved in are line_8: 2227, 2600, 2684, 3551, 3698/4093 (same proposal -- two line_9: numbers for logistical reasons) and 3538. line_10: Projects 1105, 1118, 2600, 3551, and 3698/4093 are programs line_11: which involve study of the nuclear regions of nearby line_12: galaxies (primarily ellipticals and AGNs). 3698/4093 is an line_13: AGN Snapshot survey. Comparison of the results on AGNs line_14: with those for the nearby galaxies will be of particular line_15: interest. These programs provide us with valuable line_16: experience for this project and will allow us to deal with line_17: the data in a timely fashion because of the large body of line_18: procedures and software that has been (or will already have line_19: been) developed by the time cycle 3 data becomes available. ! question: 10 section: 1 line_1: The PI and Co-I's salary support is being largely covered line_2: by their respective institutions. The extensive line_3: computational support needed for this project will be line_4: largely borne by systems acquired through the university line_5: and other grants. Only supplementary items of hardware are line_6: being requested. Extensive use will be made of software line_7: developed and funded under other programs. ! !end of general form text general_form_address: lname: ILLINGWORTH fname: GARTH mi: D category: PI inst: Lick Observatory addr_1: UNIVERSITY OF CALIFORNIA city: SANTA CRUZ state: CA zip: 95064 country: USA phone: 408 459 2843 telex: NA ! ! end of general_form_address records fixed_targets: targnum: 2 name_1: NGC55 descr_1: E,301 pos_1: RA= 0H 12M 24.0S +/- 1.0", pos_2: DEC= -39D 28' 0.0" +/- 1" equinox: 1950 rv_or_z: V = +107 fluxnum_1: 1 fluxval_1: V = 8.22 +/- 0.2 ! targnum: 4 name_1: NGC278 descr_1: E,301 pos_1: RA= 0H 49M 15.0S +/- 1.0", pos_2: DEC= 47D 16' 48.0" +/- 1" equinox: 1950 rv_or_z: V = +950 fluxnum_1: 1 fluxval_1: V = 11.51 +/- 0.2 ! targnum: 8 name_1: NGC855 descr_1: E,301 pos_1: RA= 2H 14M 3.6S +/- 1.0", pos_2: DEC= 27D 52' 37.7" +/- 1" equinox: 2000 rv_or_z: V = +807 fluxnum_1: 1 fluxval_1: V = 12.70 +/- 0.2 ! targnum: 11 name_1: NGC949 descr_1: E,301 pos_1: RA= 2H 30M 48.7S +/- 1.0", pos_2: DEC= 37D 8' 13.0" +/- 1" equinox: 2000 rv_or_z: V = +867 fluxnum_1: 1 fluxval_1: V = 12.55 +/- 0.2 ! targnum: 12 name_1: NGC959 descr_1: E,301 pos_1: RA= 2H 32M 24.0S +/- 1.0", pos_2: DEC= 35D 29' 39.4" +/- 1" equinox: 2000 rv_or_z: V = +855 fluxnum_1: 1 fluxval_1: V = 12.20 +/- 0.2 ! targnum: 15 name_1: NGC4941 descr_1: E,301 pos_1: RA= 13H 1M 37.2S +/- 1.0", pos_2: DEC= -5D 17' 0.0" +/- 1" equinox: 1950 rv_or_z: V = +938 fluxnum_1: 1 fluxval_1: V = 11.90 +/- 0.2 ! targnum: 23 name_1: NGC6689 descr_1: E,301 pos_1: RA= 18H 34M 49.8S +/- 1.0", pos_2: DEC= 70D 31' 29.9" +/- 1" equinox: 2000 rv_or_z: V = +890 fluxnum_1: 1 fluxval_1: V = 12.40 +/- 0.2 ! targnum: 24 name_1: NGC6684 descr_1: E,301 pos_1: RA= 18H 44M 1.8S +/- 1.0", pos_2: DEC= -65D 13' 48.0" +/- 1" equinox: 1950 rv_or_z: V = +772 fluxnum_1: 1 fluxval_1: V = 11.34 +/- 0.2 ! targnum: 34 name_1: NGC7741 descr_1: E,301 pos_1: RA= 23H 41M 22.8S +/- 1.0", pos_2: DEC= 25D 47' 54.0" +/- 1" equinox: 1950 rv_or_z: V = +997 fluxnum_1: 1 fluxval_1: V = 11.88 +/- 0.2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 2.000 targname: NGC55 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; req_2: CYCLE 3 / 2-34; ! linenum: 4.000 targname: NGC278 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 8.000 targname: NGC855 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 11.000 targname: NGC949 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 12.000 targname: NGC959 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 15.000 targname: NGC4941 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 23.000 targname: NGC6689 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 24.000 targname: NGC6684 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! linenum: 34.000 targname: NGC7741 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 300S s_to_n: 30 fluxnum_1: 1 priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO req_1: PCS MODE C; ! ! end of exposure logsheet ! No scan data records found