! File: 3551C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:11:46:59 coverpage: title_1: ELLIPTICALS WITH KINEMATICALLY-DISTINCT NUCLEI sci_cat: GALAXIES & CLUSTERS sci_subcat: NUCLEI/CORES proposal_for: GO pi_fname: GARTH pi_mi: D pi_lname: ILLINGWORTH pi_inst: UCO/LICK OBSERVATORY pi_country: USA pi_phone: 408-459-2843 hours_pri: 4.67 num_pri: 7 wf_pc: Y funds_amount: 49798 funds_length: 12 ! end of coverpage abstract: line_1: The discovery by Franx and Illingworth of a kinematically-distinct stellar com- line_2: ponent in the nucleus of the giant radio elliptical IC 1459, and the confirma- line_3: tion that such components are quite common, has added a valuable diagnostic tool line_4: for understanding the structure and the formation of ellipticals. Fifteen line_5: examples are now known, from a sample of 77 ellipticals. The angular momenta of line_6: the distinct components are anti-parallel, perpendicular, or parallel to the line_7: angular momenta of the outer parts. These substantial (10^10 solar masses for line_8: IC 1459) components are a valuable diagnostics of the dynamical state of the line_9: nuclei of ellipticals. Further study will address their formation by line_10: investigating whether these components could be the end result of a 'starburst' line_11: event, or of the accretion and settling of a stellar companion, or of the line_12: merging of primordial subclumps. We propose to take advantage of the high line_13: resolution imaging capability of HST through a PC imaging program of the 7 line_14: galaxies that are not part other imaging programs, with the goal of detecting line_15: central surface brightness cusps in the central regions of the galaxies with line_16: kinematically distinct cores. A comparative study of normal galaxies (observed line_17: by other programs) and galaxies with kinematically distinct cores can provide line_18: unique information on the formation of these components. These data are an line_19: essential complement to an extensive ground-based spectroscopic and CCD line_20: imaging survey, and will allow a much better modeling of the spectroscopic data. ! ! end of abstract general_form_proposers: lname: ILLINGWORTH fname: GARTH title: PI mi: D inst: UCO / LICK OBSERVATORY country: USA ! lname: FRANX fname: MARIJN inst: SMITHSONIAN ASTRONOMICAL OBSERVATORY country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: Of the fifteen ellipticals with kinematically distinct cores, eight line_2: are part of GTO programs, or approved GO programs. Thus we will line_3: observe the other seven galaxies. This will result in a doubling of line_4: the observed sample of ellipticals with distinct cores. Several of line_5: the galaxies are of special interest. IC 1459 because it is one line_6: the most extreme examples of a galaxy with a kinematically distinct line_7: core. NGC 7626 is remarkable because it has a very irregular line_8: rotation curve (Jedrzejewski and Schechter 1988, ApJ (Letters), 330, line_9: L87). It is very well possible that the central parts are not fully line_10: relaxed. It will be very interesting to see whether HST detects any line_11: sharp, high contrast features in this galaxy. NGC 1439 is the line_12: intrinsically faintest galaxy in the sample, with the lowest velocity line_13: dispersion. NGC 1427 has a rotation curve that is unresolved even at line_14: subarcsecond seeing. NGC 5982 is the only galaxy which has a line_15: distinct core that has a rotation axis parallel to the major axis. line_16: All other systems rotate around the minor axis. The galaxies will be line_17: observed with the Planetary Camera. Two exposures of comparable line_18: length need to be taken in ``V'' (F555W). It is essential to have line_19: two exposures to verify the deconvolution techniques. ! question: 3 section: 1 line_1: The use of the imaging capabilities of HST is a logical and important line_2: component of a broadly-based observational program involving ground- line_3: based long-slit spectra and ground-based CCD images of ellipticals line_4: with kinematically-distinct cores. Both the spectroscopic and the line_5: imaging results suggest that these distinct nuclear subcomponents are line_6: unresolved from the ground in typical 1-2" seeing. The cores of line_7: ellipticals are known to be at best marginally resolved from the line_8: ground, with a few notable exceptions (see, e.g., Kormendy, 1985, Ap.J. line_9: (Letters), 292, L9). If compact star clusters or black-holes are line_10: significant in these cores, the small gains in resolution possible at line_11: Hawaii and other sites will not be decisive in establishing the line_12: structure of the nuclei on scales <0.2". The results by Lauer et al line_13: (1991, ApJ 369, L41) have shown convincingly that HST can do line_14: significantly better than any ground-based facilities, if proper line_15: deconvolution is applied to the images. The HST PC images will line_16: complement the available ground-based multicolor CCD surface photometry line_17: by allowing comparison of the core structure and properties with those line_18: at larger radii. Furthermore, the early `discovery' spectroscopic line_19: observations have been supplemented by a set of higher S/N long-slit line_20: spectra taken with the highest practical ground-based spatial resolution line_21: (~1" with ~0.3-0.6" pixels) at a variety of position angles. These data line_22: have been acquired both in the Northern and Southern hemispheres, at line_23: CTIO and Lick. This combination of ground and space data is uniquely powerful. ! question: 4 section: 1 line_1: Seven elliptical galaxies are to be observed with the PC to obtain high line_2: S/N, high spatial resolution images suitable for the detection and line_3: measurement of a stellar cusps in the nuclei. For optimal image line_4: reconstruction we are taking two integrations of comparable length. line_5: We take pairs of images to verify the structures that may result from line_6: the deconvolution. Cosmic rays will be removed by intercomparison of line_7: the pairs of frames. The typical surface brightness of the galaxies line_8: cannot be predicted in advance, as it may be quite high if a cusp is line_9: present. The dynamic range of the system should be able to accommodate line_10: central surface brightnesses ~10 times greater than expected from the line_11: ground-based photometry. Extrapolating the observed central surface line_12: brightnesses of these galaxies, we expect that the count per pixel in line_13: the inner pixels will be of the order of 3000-5000 electrons in 600 sec, line_14: or about 1500-2500 in each frame of the CR-SPILT image. The signal will line_15: drop to typically a few hundred electrons at r~10". The S/N per pixel line_16: will be ~50 in each image (70 for the pair). The ``V'' filter is chosen line_17: for this study because its PSF will be well-monitored. We believe that line_18: this is important for a good deconvolution. If it were not for this line_19: constraint, the F702W filter would be optimal, as it produces a signal a line_20: factor of two higher than the F555W filter. If the policy regarding the line_21: PSF monitoring changes, we may like to adapt our choice of filter. ! question: 5 section: 1 line_1: No special scheduling requirements. ! question: 6 section: 1 line_1: The project is being organised to ensure a thorough but speedy path line_2: from acquisition of the data to publication of the papers. Both the line_3: Co.I and P.I have extensive experience with handling, processing and line_4: analysing two-dimensional CCD image data, having been involved in two line_5: major multicolor CCD surface photometry programs that together have line_6: assembled the largest set of color profiles for ellipticals available line_7: to date, with UBR maps of 59 galaxies (Franx, Illingworth and Heckman, line_8: 1989, AJ, 98, 538; and Peletier, Davies, Illingworth, Davis and Cawson, line_9: 1990, AJ, 100, 1091). Clearly, the most important task ahead is the line_10: deconvolution of the images. The results by Lauer et al (1991, ApJ 369, line_11: L41) show that even ``simple'' techniques like Lucy's algorithm provide line_12: satisfactory answers. It is clear that as experience grows, other line_13: algorithms may prove to be better suited. We are experimenting with a line_14: procedure that fits a surface brightness profile directly to the data, line_15: by an iterative procedure that convolves the profile with the PSF, line_16: determines the residuals from the fit, and adapts the surface brightness line_17: profile. This technique can circumvent the double-staged approach where line_18: the images are first deconvolved and then fitted. Broadly, the bulk of line_19: the data analysis will be done at Lick, with software design, testing line_20: and validation being done at CfA, with the modelling and papers being line_21: carried out jointly. More detail of the responsibilities of the PI and line_22: CoI will be given in the budget justification section. ! question: 7 section: 1 line_1: No additional requests. ! question: 8 section: 1 line_1: We have been assigned supplemental time for a similar proposal in Cycle 1 line_2: (# 2591). This project was designed to take multicolor images of line_3: NGC 4365, NGC 4406, and IC 1459. We have chosen not to reapply to take line_4: color images in cycle 2, because it is highly uncertain how well line_5: HST can do in that respect. ! question: 8 section: 2 line_1: No data has been taken yet, and is unlikely to be taken in Cycle 1. ! question: 8 section: 3 line_1: No data has been taken yet, and is unlikely to be taken in Cycle 1. ! question: 9 section: 1 line_1: Lick Observatory has a strong foundation for intensive image processing of line_2: large HST images. The department has a powerful host SUN 4/280 system with line_3: high performance peripherals that is the heart of a network that includes line_4: the P.I's workstation. Several staff are available to support the systems line_5: and system software development. There is also a pool of ten or more line_6: graduate students, some of whom have University Fellowships, who work line_7: intensively with optical imaging and spectroscopy. The P.I's UCSC-supplied line_8: workstation will host the student workstation. Both workstations will draw line_9: upon the departmental resources. S. Faber, an IDT WF/PC team member, is on line_10: the Lick faculty, and will be a source of the IDT team's valuable early line_11: experience in processing WF/PC data. The P.I also has access to the 3 m line_12: and 1 m telescopes on Mt. Hamilton, and to the Keck 10 m when it is in line_13: operation in 1993. Dr. Franx has a Hubble Fellowship, which includes summer line_14: salary, and some direct research support which will allow him some computing line_15: capability. ! !end of general form text general_form_address: lname: ILLINGWORTH fname: GARTH mi: D category: PI inst: UCO/ LICK OBSERVATORY addr_1: UNIVERSITY OF CALIFORNIA city: SANTA CRUZ state: CA zip: 95064 country: USA phone: (408) 459 2843 telex: 7607936 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC1427 descr_1: E,303,910 pos_1: RA = 03H 42M 19.60S +/- 0.15S, pos_2: DEC = -35D 23' 35.2" +/- 2" equinox: J2000 rv_or_z: V = +1413 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +1 fluxnum_1: 1 fluxval_1: SURF(V) = 16.1 +/- 2 ! targnum: 2 name_1: NGC1439 descr_1: E,303,910 pos_1: RA = 03H 44M 49.98S +/- 0.15S, pos_2: DEC = -21D 55' 14.7" +/- 2" equinox: J2000 rv_or_z: V = +1664 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +0.5 fluxnum_1: 1 fluxval_1: SURF(V) = 16.4 +/- 2 ! targnum: 3 name_1: NGC4494 descr_1: E,303,910 pos_1: RA = 12H 31M 24.16S +/- 0.15S, pos_2: DEC = +25D 46' 28.5" +/- 2" equinox: J2000 rv_or_z: V = +1324 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +0.5 fluxnum_1: 1 fluxval_1: SURF(V) = 15.8 +/- 2 ! targnum: 4 name_1: NGC4589 descr_1: E,303,910 pos_1: RA = 12H 37M 24.97S +/- 0.15S, pos_2: DEC = +74D 11' 31.2" +/- 2" equinox: J2000 rv_or_z: V = +1980 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +1 fluxnum_1: 1 fluxval_1: SURF(V) = 16.6 +/- 2 ! targnum: 5 name_1: NGC5982 descr_1: E,303,910 pos_1: RA = 15H 38M 39.74S +/- 0.15S, pos_2: DEC = +59D 21' 21.0" +/- 2" equinox: J2000 rv_or_z: V = +2904 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +0.5 fluxnum_1: 1 fluxval_1: SURF(V) = 16.2 +/- 2 ! targnum: 6 name_1: IC1459 descr_1: E,303,910 pos_1: RA = 22H 57M 10.49S +/- 0.15S, pos_2: DEC = -36D 27' 46.3" +/- 2" equinox: J2000 rv_or_z: V = +1691 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +0.5. fluxnum_1: 1 fluxval_1: SURF(V) = 15.2 +/- 2 ! targnum: 7 name_1: NGC7626 descr_1: E,303,910 pos_1: RA = 23H 20M 42.54S +/- 0.15S, pos_2: DEC = +08D 13' 01.7" +/- 2" equinox: J2000 rv_or_z: V = +3423 comment_1: BETTER FLUXVAL comment_2: UNCERTAINTY IS -2 TO +0.5 fluxnum_1: 1 fluxval_1: SURF(V) = 16.6 +/- 2 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: IC1459 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 500S s_to_n: 80 fluxnum_1: 1 priority: 1 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.4 req_1: CYCLE 2 / 1-7 ! linenum: 2.000 targname: NGC7626 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 810S s_to_n: 70 fluxnum_1: 1 priority: 2 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.38 ! linenum: 3.000 targname: NGC1427 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 500S s_to_n: 70 fluxnum_1: 1 priority: 2 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.4 ! linenum: 4.000 targname: NGC1439 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 640S s_to_n: 70 fluxnum_1: 1 priority: 3 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.37 ! linenum: 5.000 targname: NGC5982 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 640S s_to_n: 70 fluxnum_1: 1 priority: 3 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.37 ! linenum: 6.000 targname: NGC4494 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 500S s_to_n: 70 fluxnum_1: 1 priority: 3 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.4 ! linenum: 7.000 targname: NGC4589 config: PC opmode: IMAGE aperture: PC6 sp_element: F555W num_exp: 1 time_per_exp: 590S s_to_n: 70 fluxnum_1: 1 priority: 4 param_1: PRE-FLASH = NO, param_2: CR-SPLIT = 0.4 ! ! end of exposure logsheet ! No scan data records found