! File: 3792C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:19:39:48 coverpage: title_1: UV MORPHOLOGY OF STARBURSTS IN INTERACTING title_2: GALAXIES sci_cat: GALAXIES & CLUSTERS sci_subcat: PECULIAR/INTERACTING proposal_for: GO pi_title: DR. pi_fname: SUSAN pi_mi: G. pi_lname: NEFF pi_inst: NASA / GODDARD SPACE FLIGHT CENTER pi_country: USA pi_phone: 301-286-6066 keywords_1: STARBURST hours_pri: 1.00 num_pri: 2 foc: Y pi_position: SCIENTIST off_fname: STEVEN off_mi: S. off_lname: HOLT off_title: DIR. OF SPACE SCI. off_inst: NASA / GODDARD SPACE FLIGHT CENTER off_addr_1: CODE 600 off_city: GREENBELT off_state: MD off_zip: 20771 off_country: USA off_phone: 301-286-6066 ! end of coverpage abstract: line_1: We propose UV imaging observations of the colliding galaxy system line_2: NGC 3690 / IC 694, which contains several regions of intense starburst line_3: activity. The morphology of the early-type stellar population will be line_4: used to determine the relationship between the galaxy interaction and the line_5: resultant starburst activity. The UV images will be compared with images line_6: of the system in the optical continuum, H alpha line, near IR, mid-IR, line_7: CO line, 21cm line, and radio continuum to understand the spatial line_8: relationship of the starburst component to the older stars, hot dust, line_9: and molecular and atomic gas. line_10: The UV morphology will be compared line_11: with the kinematics of the ionized and molecular gas to determine the line_12: connection of the starburst location and intensity to the system line_13: kinematics. Previous IUE observations show that this system has line_14: detectable UV emission, making it an excellent candidate for UV imaging line_15: studies. ! ! end of abstract general_form_proposers: lname: NEFF fname: SUSAN title: DR. mi: G inst: NASA / GODDARD SPACE FLIGHT CENTER country: USA ! lname: STANFORD fname: SPENCER title: DR. mi: A inst: ASTRONOMY DEPARTMENT, UC-BERKELEY country: USA ! lname: JOY fname: MARSHALL title: DR. inst: NASA / MARSHALL SPACE FLIGHT CENTER country: USA ! ! end of general_form_proposers block general_form_text: question: 2 section: 1 line_1: ! question: 3 section: 1 line_1: We propose to obtain UV imaging with the FOC of one colliding galaxy pair, line_2: NGC 3690/IC 694. The FOC provides better sensitivity than the WF/PC in the UV. line_3: The 22 arcsec field of view in the F48 mode is adequate for the chosen object. line_4: Fields at two slightly overlapping positions in the system, roughly line_5: centered on the two nuclei, would cover the region of interest. Each exposure line_6: will be split into two parts, because of the advantage of comparing line_7: deconvolutions of independent frames in establishing the reality of faint line_8: features. Because the two fields are separated by only about 20 arcsec, line_9: only one visit is needed; we expect only one initial guide star acquisition, line_10: and one subsequent reacquisition in the second orbit. line_11: Pointing errors of +/- few arcsec will not greatly affect the imaging, line_12: so blind acquistion is adequate. ! question: 4 section: 1 line_1: We need to use HST because we want to obtain UV imaging. The current PSF line_2: is not detrimental to our program because it needs to use HST for its line_3: UV capabilities, not high spatial resolution. Resolution in line_4: the range of 1-2 arcsec is adequate for the UV imaging, and is appropriate line_5: for comparison with ground-based images at other wavelengths. The study of line_6: interaction-induced starbursts has been vigorously pursued from the ground line_7: in the past decade by many groups at all wavelengths available from the line_8: optical to the radio. We have been involved in these efforts; for example the line_9: PI's PhD thesis used multiwavelength ground-based observations to study the line_10: relationship between the kinematics and the starburst morphology in the line_11: interacting galaxy system NGC 520. In particular for the target NGC3690/IC694 line_12: we have already obtained VLA 21 cm H I mapping (Stanford and Wood 1989), line_13: mid-IR mapping (Joy et al. 1989), line_14: near-IR imaging (Bushouse and Stanford 1991), near-IR and optical longslit line_15: spectroscopy (Stanford 1991), and Taurus H-alpha velocity mapping (Neff et al. line_16: 1991). Clearly, the UV imaging program can only be pursued from space with HST. ! question: 5 section: 1 line_1: ! question: 6 section: 1 line_1: ! question: 7 section: 1 line_1: The data will be analyzed at the home institution of the PI after the line_2: standard pipeline reduction of flatfielding and geometric-correction has line_3: been accomplished at STScI. Images will be examined both line_4: in original form, and after deconvolution. One co-PI has extensive experience line_5: in the analysis of FOC imaging data, including deconvolution techniques, line_6: due to his present position as a postdoctoral research assistant to Dr. Ivan line_7: King of the FOC/IDT. If the UV emission tends to be in small clumps, then line_8: deconvolution may be used to try to measure their actual sizes. At the line_9: distance of NGC 3690/IC 694, 0.135 arcsec resolution (potential fwhm after line_10: image restoration) corresponds to 35 pc, line_11: which is sufficient to resolve early-type star clusters. These sizes, line_12: along with their fluxes, would be used to determine the typical stellar line_13: temperature of the stars in each clump and thus to provide an estimate of line_14: the dominant spectral type. The age of the clump may then be estimated. line_15: The most important information to obtain from the imaging is the line_16: morphology of the UV emission, particularly with respect to other wavelength line_17: imaging, and the fluxes of individual knots of starburst activity. line_18: The flux information is important to constructing spectral energy distributions line_19: of starburst regions, because these currently lack spatially-resolved data line_20: in the UV. The fluxes will be also be used to constrain calculations of line_21: the dust extinction towards the starburst regions. ! question: 8 section: 1 line_1: ! question: 9 section: 1 line_1: ! question: 10 section: 1 line_1: Data-analysis capabilities are available at the institutions line_2: of the PI and co-Is. ! !end of general form text general_form_address: lname: Neff fname: Susan mi: G title: Dr. category: PI inst: NASA/GSFC addr_1: Code 600 city: Greenbelt state: MD zip: 20771 country: USA phone: 301-286-6066 from_date: 03-MAR-92 to_date: 31-DEC-99 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC3690 name_2: A299B descr_1: E,318,319,320 pos_1: RA = 11H 25M 41.42S +/- 0.15S, pos_2: DEC = +58D 50' 16.5" +/- 0.5" equinox: 1950.0 rv_or_z: V=+3150 fluxnum_1: 1 fluxval_1: SURF(V) = 20.0 +/- 1.0 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.3 fluxnum_3: 3 fluxval_3: E(B-V) = 0.4 +/- 0.2 fluxnum_4: 4 fluxval_4: SURF-CONT(2000) = 1 +/- 1 E-16 fluxnum_5: 5 fluxval_5: SIZE = 15 +/- 5 ! targnum: 2 name_1: IC694 name_2: A299A descr_1: E,318,319,320 pos_1: RA = 11H 28M 33.45S +/- 0.15S, pos_2: DEC = +58D 33' 38.0" +/- 0.5" equinox: 2000 rv_or_z: V=+3150 fluxnum_1: 1 fluxval_1: SURF(V) = 20.0 +/- 1.0 fluxnum_2: 2 fluxval_2: B-V = 0.8 +/- 0.3 fluxnum_3: 3 fluxval_3: E(B-V) = 0.4 +/- 0.2 fluxnum_4: 4 fluxval_4: SURF-CONT(2000) = 1 +/- 1 E-16 fluxnum_5: 5 fluxval_5: SIZE = 15 +/- 5 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC3690 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F220W num_exp: 2 time_per_exp: 15M s_to_n: 7 fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: PIXEL=50X25 req_1: CYCLE 2; req_2: GROUP 1-2 NO GAP ! linenum: 2.000 targname: IC694 config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F220W num_exp: 2 time_per_exp: 15M s_to_n: 7 fluxnum_1: 4 fluxnum_2: 5 priority: 1 param_1: PIXEL=50X25 req_1: CYCLE 2 ! ! end of exposure logsheet ! No scan data records found