! $Id: 5400,v 5.1 1994/07/27 17:33:32 pepsa Exp $ coverpage: title_1: THE STARBURST GALAXY NGC 5102 sci_cat: GALAXIES & CLUSTERS sci_subcat: STARBURSTS proposal_for: GO pi_fname: KENNETH pi_mi: C pi_lname: FREEMAN pi_inst: MT STROMLO AND SIDING SPRING OBSERVATORIES pi_country: AUSTRALIA pi_phone: 61 6 2490264 hours_pri: 10.20 num_pri: 4 wf_pc: Y off_fname: DONALD off_lname: FAULKNER off_title: DR off_inst: 4140 off_addr_1: MT STROMLO AND SIDING SPRING OBSERVATORIES off_addr_2: PRIVATE BAG, WESTON CREEK PO off_city: CANBERRA off_state: ACT off_zip: 2611 off_country: AUSTRALIA off_phone: 61 6 2490258 ! end of coverpage abstract: line_1: NGC 5102 is a nearby (4 Mpc) galaxy of classical SO appearance which has line_2: undergone a recent starburst in its nucleus, bulge and disk. Because it is so line_3: close, it provides a unique opportunity to investigate the IMF of a typical line_4: starburst, the mass of starburst matter relative to the underlying older line_5: population, and the effect of the starburst on the largescale structure of line_6: this galaxy. WFPC2 images will be used to derive the luminosity function and line_7: IMF for the starburst matter in three regions of NGC 5102, at different line_8: distances from the nucleus. In the inner high surface brightness region, the line_9: crucial massive end of the mass function (stars more massive than 8 M_sun) is line_10: accessible. In the outer disk, where the surface brightness is lower, we will line_11: be able to derive the mass function for stars more massive than 5 M_sun. This line_12: proposal is part of a larger program on this important galaxy, involving line_13: extensive groundbased optical and radio observations. The HST is required line_14: for its high spatial resolution, which enables faint stars of the starburst line_15: to be detected against the high background surface brightness of this line_16: galaxy. This proposal was accepted for Cycle 1 (#2436) but was not retained line_17: when the Cycle 1 program was reassessed because of the primary mirror flaw. ! ! end of abstract general_form_proposers: lname: FREEMAN fname: KENNETH mi: C inst: 4140 country: AUSTRALIA ! lname: NORMAN fname: COLIN mi: A inst: 2380 country: USA ! lname: SCOVILLE fname: NICHOLAS mi: Z inst: 1590 country: USA ! lname: QUINN fname: PETER mi: J inst: 4140 country: AUSTRALIA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: The observations will be made with the PC because its small pixel line_2: size is needed for adequate S/N ratio in the high surface line_3: brightness inner regions of NGC 5102. The WFC data obtained at the line_4: same time will have lower S/N ratio in the inner regions of NGC line_5: 5102 but will be useful in the outer regions where the diffuse line_6: surface brightness is not so high. We will use the F450W and F569W line_7: filters, because they provide satisfactory transformations to the line_8: standard BV system amd they give the best S/N ratio for line_9: observations of our blue stars against the redder diffuse line_10: background of this galaxy. line_12: The first field is centered on the nucleus of NGC 5102, for the line_13: purpose of deriving the luminosity function in the inner bulge line_14: region. A total exposure of 3000 sec in each filter will give a line_15: S/N ratio larger than 3 for early type stars with V = 26 at 3 line_16: arcsec from the nucleus, and correspondingly fainter at larger line_17: distances. The 3000 sec exposure will be split into two equal line_18: parts to minimize blooming from foreground stars and to allow line_19: discrimination of the fainter cosmic ray events. The nucleus itself line_20: will produce blooming and local saturation, but the amount of field line_21: so affected is negligible. The second and third fields are centered line_22: at about 66 and 132 arcsec from the nucleus, along the major axis line_23: towards the SW. The 66 arcsec center is located in the transition ! question: 3 section: 2 line_1: region between the bulge and disk, and the 132 arcsec field lies in line_2: disk. The field centers have been chosen to minimize the number of line_3: stars in the PC field that are bright enough to cause blooming, and line_4: the field area affected by blooming will be negligible. We have also line_5: chosen a field outside the galaxy, to be observed in an identical line_6: way to the first three fields, in order to derive accurately the line_7: local Galactic background luminosity function. ! question: 4 section: 1 line_1: The HST is required for this program, because its high spatial line_2: resolution allows photometry of faint stars against the background line_3: surface brightness distribution of this galaxy. From the ground, line_4: such photometry is so limited that our program would be impossible. line_5: For example, even in the disk of NGC 5102, where the surface line_6: brightness is about 21.2 B mag arcsec**-2, the limiting magnitude line_7: from the ground would be about B = 24.5, and only a very restricted line_8: portion of the upper end of the mass function would be observable line_9: (about 16 to 40 M_sun). However, the innermost parts of NGC 5102 line_10: are particularly important, because of the likely connection of line_11: starbursts and bulge formation, and in these regions groundbased line_12: work is impossible. For example, at about 5 arcsec from the line_13: nucleus, the background surface brightness is about 18.5 B mag line_14: arcsec**-2, and the faintest stars that could be detected under line_15: the best groundbased conditions would have B = 22. (We recall line_16: that the brightest stars that have been detected in the disk of line_17: NGC 5102 have B = 22) line_19: GTO PC observations of the nucleus of NGC 5102 (program numbers line_20: 1118/3229) with the F555W and F785LP filters have quite different line_21: science goals from ours. These filters are not optimal for studying line_22: the luminosity function of the starburst, and the exposure times line_23: are too short to be of significant use for this work. ! question: 5 section: 1 line_1: We would like the B and V images for each field to be taken at line_2: the same orientation, to allow matching of the B and V images. line_3: From field to field, the orientation need not be the same. ! question: 6 section: 1 line_1: ! ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: The Environments of Starburst Galaxies, C. Norman, 2644 line_3: Disk and Halo Globular Clusters in the Edge-on Spiral line_4: galaxy NGC 5170, K. Freeman, 3532 line_6: Quasar Absorption Line Studies of Starburst Galaxy line_7: Environments, C. Norman, 3676 ! question: 10 section: 1 line_1: The data analysis capabilities of our institutions will be used for line_2: data analysis. The software and most of the hardware is already line_3: available and in use. Graduate students at MSSSO and JHU will work line_4: on particular aspects of this project. Australian radio and optical line_5: facilities (the Australia Telescope, MSSSO 2.3-m telescope, AAT) will line_6: be used for the associated ground based observations. ! !end of general form text general_form_address: lname: FREEMAN fname: KENNETH mi: C category: PI inst: 4140 addr_1: MOUNT STROMLO AND SIDING SPRING OBSERVATORIES addr_2: PRIVATE BAG, WESTON CREEK PO city: CANBERRA state: AC zip: 2611 country: AUSTRALIA phone: 61 6 2490264 telex: KCF@MSO.ANU.EDU.AU ! lname: category: CON ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC5102-FIELD1 descr_1: E,302,318,928 pos_1: RA = 13H 19M 07.2S +/- 0.15S, pos_2: DEC = -36D 22' 09" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: V=26.0 +/- 0.5 fluxnum_2: 1 fluxval_2: B-V=-0.2 +/- 0.1 fluxnum_3: 2 fluxval_3: E(B-V)=0.1 +/- 0.05 fluxnum_4: 3 fluxval_4: SURF-BKG(V) = 17.4 +/- 0.8 ! targnum: 2 name_1: NGC5102-FIELD2 descr_1: E,302,318,928 pos_1: RA = 13H 19M 03.5S +/- 0.15S, pos_2: DEC = -36D 22' 59" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: V=26.0 +/- 0.5 fluxnum_2: 1 fluxval_2: B-V=-0.2 +/- 0.1 fluxnum_3: 2 fluxval_3: E(B-V)=0.1 +/- 0.05 fluxnum_4: 3 fluxval_4: SURF-BKG(V) = 20.7 +/- 0.5 ! targnum: 3 name_1: NGC5102-FIELD3 descr_1: E,302,318,928 pos_1: RA = 13H 18M 59.2S +/- 0.15S, pos_2: DEC = -36D 23' 40" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: V=26.0 +/- 0.5 fluxnum_2: 1 fluxval_2: B-V=-0.2 +/- 0.1 fluxnum_3: 2 fluxval_3: E(B-V)=0.1 +/- 0.05 fluxnum_4: 3 fluxval_4: SURF-BKG(V) = 21.9 +/- 0.2 ! targnum: 4 name_1: NGC5102-FIELD4 descr_1: J,702,E,302,318,928 pos_1: RA = 13H 19M 32.7S +/- 0.15S, pos_2: DEC = -36D 21' 37" +/- 2" equinox: 1950 fluxnum_1: 1 fluxval_1: V=26.0 +/- 0.5 fluxnum_2: 1 fluxval_2: B-V=-0.2 +/- 0.1 fluxnum_3: 2 fluxval_3: E(B-V)=0.1 +/- 0.05 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC5102-FIELD1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F450W wavelength: 4520 num_exp: 4 time_per_exp: 900S s_to_n: 5 s_to_n_time: 3600S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 param_1: CR-TOLERANCE=0.0 req_1: CYCLE 4; ! linenum: 2.000 targname: NGC5102-FIELD1 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F569W wavelength: 5623 num_exp: 4 time_per_exp: 1000S s_to_n: 4 s_to_n_time: 4000S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 param_1: CR-TOLERANCE=0.0 req_1: CYCLE 4; req_2: SAME ORIENT FOR 2 AS 1; ! linenum: 3.000 targname: NGC5102-FIELD2 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F450W wavelength: 4520 num_exp: 3 time_per_exp: 1100S s_to_n: 9 s_to_n_time: 3000S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; ! linenum: 4.000 targname: NGC5102-FIELD2 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F569W wavelength: 5623 num_exp: 3 time_per_exp: 1100S s_to_n: 8 s_to_n_time: 3000S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 4 AS 3; ! linenum: 5.000 targname: NGC5102-FIELD3 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F450W wavelength: 4520 num_exp: 3 time_per_exp: 1100S s_to_n: 9 s_to_n_time: 3000S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; ! linenum: 6.000 targname: NGC5102-FIELD3 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F569W wavelength: 5623 num_exp: 3 time_per_exp: 1100S s_to_n: 9 s_to_n_time: 3000S fluxnum_1: 1 fluxnum_2: 2 fluxnum_3: 3 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 6 AS 5; ! linenum: 7.000 targname: NGC5102-FIELD4 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F450W wavelength: 4520 num_exp: 3 time_per_exp: 1100S s_to_n: 9 s_to_n_time: 3000S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; ! linenum: 8.000 targname: NGC5102-FIELD4 config: WFPC2 opmode: IMAGE aperture: PC1-FIX sp_element: F569W wavelength: 5623 num_exp: 3 time_per_exp: 1100S s_to_n: 9 s_to_n_time: 3000S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 4; req_2: SAME ORIENT FOR 8 AS 7; ! ! end of exposure logsheet ! No scan data records found