! File: 3807C.PROP ! Database: PEPDB ! Date: 19-FEB-1994:20:11:23 coverpage: title_1: MINKOWSKI'S OBJECT sci_cat: GALAXIES & CLUSTERS sci_subcat: STARBURSTS proposal_for: GO pi_fname: KENNETH pi_mi: C. pi_lname: CHAMBERS pi_inst: INSTITUTE FOR ASTRONOMY, UNIV. OF HAWAII pi_country: USA pi_phone: 808-956-8566 hours_pri: 8.00 num_pri: 1 wf_pc: Y foc: Y funds_amount: 82159 funds_length: 12 off_fname: DONALD off_mi: N. off_lname: HALL off_title: DIRECTOR off_inst: INSTITUTE FOR ASTRONOMY off_addr_1: UNIVERSITY OF HAWAII off_addr_2: 2680 WOODLAWN DRIVE off_city: HONOLULU off_state: HI off_zip: 96822 off_country: USA off_phone: 808-956-8566 ! end of coverpage abstract: line_1: Minkowski's Object is the best low redshift example of a rare line_2: phenomena - a starburst triggered by a radio jet. line_3: Our recent IUE observations of MO (Chambers et al. 1992) have line_4: detected Lyman alpha emission and SIV and CIV absorption, line_5: confirming that Minkowski's Object is undergoing a line_6: spectacular starburst. Ultraviolet and high spatial line_7: resolution images by HST will provide an extraordinary view line_8: of this potentially very important physical process. We line_9: propose to trace spatially the star formation history along line_10: the path of the shock front. We will model this stellar line_11: chromography with the recent stellar population synthesis line_12: code of Charlot and Bruzual 1991. With this tool, and multi- line_13: color HST data we will be able to: (1) investigate the nature line_14: of the star burst and its stellar population, (2) date the line_15: evolution and thus the speed of propagation of star formation line_16: outward with the radio jet, and (3) study the details of the line_17: jet interaction with the star forming regions at the bow line_18: shock. This will provide absolutely unique data on stellar line_19: populations, the propogation of radio jets in dense media, line_20: and on starbursts triggered by radio jets. ! ! end of abstract general_form_proposers: lname: CHAMBERS fname: KENNETH title: PI mi: C. inst: INSTITUTE FOR ASTRONOMY, UNIVERSITY OF HAWAII country: U.S.A. ! lname: CHARLOT fname: STEPHANE inst: STSCI country: USA esa: N ! lname: VAN BREUGEL fname: WIL mi: J. inst: IGGP country: USA esa: N ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: In order to investigate the details of the detonation line_2: wave of starformation we need spatially resolved spectral line_3: energy distributions from the UV to the near-IR. It is line_4: crucial to obtain UV images where we are sensitive to the line_5: hottest and youngest population of stars, but also B-V line_6: colors to examine the 4000 A break, and I to distinguish line_7: any older underlying stellar population from a red supergiant line_8: population. Thus we plan to take 5 broad band images, line_9: UV15,UV22,BVI and one narrow band image centered on H-alpha line_10: and NII to determine the morphology of the very strong line line_11: emission. This will enable us to construct spectral energy line_12: distributions as a function of distance along the path of star line_13: formation wave. If necessary, we can also spatially average line_14: over the object in the direction perpendicular to color line_15: gradient; i.e. if necessary we can sacrifice HST's spatial line_16: resolution in ONE DIRECTION in order to obtain sufficient line_17: signal to noise. We will use the FOC/48 and filters line_18: F150W,F220W,F439W for UV15,UV22, and B images. line_19: We will use the PC and filters F569W, F791W for line_20: V, I colors and F664N to image the H-alpha emission line. ! question: 4 section: 1 line_1: Ultraviolet and high spatial resolution images by HST are crucial line_2: to disentagle the features of this unique and potentially very line_3: important object. Only in the space ultraviolet can we image line_4: directly the hottest and youngest star forming regions. The barely line_5: resolved (from the ground) bright optical blue star forming region line_6: along the leading edge of the radio jet is a prime target for line_7: HST observations. We have pursued all possible avenues available line_8: from the ground and space: (i) 16 hour IUE integration, (ii) line_9: high resolution VLA radio maps of total intensity and polarization, line_10: (iii) VLA maps of neutral hydrogen, (iv) ground based broad line_11: and narrow band images, and (v) near infrared images. ! question: 5 section: 1 line_1: Justify any real-time or special scheduling requirements or line_2: requests such as special ORIENTs etc. here. ( May need to line_3: include special ORIENT info, or GROUP WITHIN or NO GAP requests line_4: in Question 3, above, also. ) line_6: The ORIENT requirement is in order to fit the oblong shaped line_7: object in the field of view. The FOC images all need to line_8: be taken at the exact same ORIENT so they can be combined line_9: unambigously. The same is true for the PC images, but line_10: the PC and FOC can be taken at different position angles. line_11: In both cases, the intent is to place the axis of each detector line_12: at a position angle of 36 degrees east of north. ! question: 6 section: 1 line_1: Justify uninterupted exposures line_2: or use of dark time: line_3: The dark time is required for the FOC F150W filter in order line_4: to limit the geo coronal Lyman alpha. This is preferable line_5: to putting in the LP130 filter which will pull down the line_6: transmission by 40% at a crucial wavelength. ! question: 7 section: 1 line_1: We have two conflicting objectives, ginven the current mirror line_2: aberation problem with HST: the highest possible spatial line_3: resolution, and the best photometry possible. Thus we expect to line_4: experiment with all available deconvolution algorithms, since some line_5: will be better for different objectives than others (i.e. maximum line_6: resolution vs. photometry vs. surface brightness). For each line_7: algorithm (e.g. Wiener filter, Lucy-Richardson, Maximum Entropy) line_8: we will have to try various PSF's (observed and modeled). We line_9: can also put some constrains on surface brightness emission from line_10: our ground based images of these objects. Simulations of the line_11: registration, cosmic ray, and deconvolution algorithms with line_12: artifical data and models of the underlying profiles will be line_13: necessary to test our results. All of the HST optical images will line_14: be related to (i) comparable resolution VLA radio maps of total line_17: intensity and polarization, (ii) VLA maps of neutal hydrogen, line_18: (iii) ground based broad-band and narrow band images, line_19: (iv) ground based infra-red images, (v) our IUE spectra. line_20: The color gradients will be extensively modeled with the stellar line_21: population synthesis code of Charlot and Bruzual (1991). ! question: 8 section: 1 line_1: No additional comments. ! question: 9 section: 1 line_1: Description of previous HST data. line_2: (a) P2438, "The Most Distant Galaxies", PI, George Miley. line_3: Proposal P2438 is not related to this proposal (3807) line_4: (b) Some of the observations have taken place, and Chambers line_5: has recalibrated the data, and begun deconvolution and line_6: analysis of the data. line_7: (c) No publications have been submitted yet. ! question: 10 section: 1 line_1: The major part of the reduction will take place at the University line_2: of Hawaii, where IRAF/STSDAS is installed, and normal institutional line_3: support is available. ! !end of general form text general_form_address: lname: CHAMBERS fname: KENNETH mi: C. category: PI inst: INSTITUTE FOR ASTRONOMY addr_1: UNIVERSITY OF HAWAII addr_2: 2680 WOODLAWN DRIVE city: HONOLULU state: HI zip: 96822 country: USA phone: 808-956-8566 telex: 723-8459 UHAST HR ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: MINKOWSKI-OBJECT descr_1: E, descr_2: 318, descr_3: 320 pos_1: RA = 01H 25M 47.33S +/- 1S, pos_2: DEC = -01D 22' 19.98" +/- 1", pos_3: PLATE-ID=00WT equinox: 2000 comment_1: MINKOWSK'S OBJECT IS A PECULIAR comment_2: STARBURST INTERACTING WITH A RADIO comment_3: JET FROM ANOTHER GALAXY (NGC 541) comment_4: IN THE CLUSTER ABELL 194. fluxnum_1: 1 fluxval_1: V = 17.0 +/- 0.1 fluxnum_2: 2 fluxval_2: B-V = 0.1 +/- 0.1 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: MINKOWSKI-OBJECT config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F165W wavelength: 1612 num_exp: 3 time_per_exp: 1900S s_to_n: 10 s_to_n_time: 6300S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PIXEL=50X25 req_1: CYCLE 2 / 1-3; req_2: SAME ORIENT FOR 2-3 AS 1; req_3: ORIENT 69D +/- 15D /1-3; comment_1: CAN USE COARSE TRACK IF NO FINE LOCK comment_2: GUIDE STARS AVAILABLE. comment_3: ORIENT CAN ALSO BE 159D, 249D, OR comment_4: 339D ALL +/- 15D. ! linenum: 2.000 targname: MINKOWSKI-OBJECT config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F220W wavelength: 2201 num_exp: 3 time_per_exp: 2000S s_to_n: 10 s_to_n_time: 6300S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PIXEL=50X25 comment_1: CAN USE COARSE TRACK IF NO FINE LOCK comment_2: GUIDE STARS AVAILABLE. ! linenum: 3.000 targname: MINKOWSKI-OBJECT config: FOC/96 opmode: IMAGE aperture: 512X1024 sp_element: F430W wavelength: 3960 num_exp: 1 time_per_exp: 2000S s_to_n: 10 s_to_n_time: 2200S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: PIXEL=50X25 comment_1: CAN USE COARSE TRACK IF NO FINE LOCK comment_2: GUIDE STARS AVAILABLE. ! linenum: 4.000 targname: MINKOWSKI-OBJECT config: PC opmode: IMAGE aperture: PC5 sp_element: F569W wavelength: 5609 num_exp: 3 time_per_exp: 700S s_to_n: 10 s_to_n_time: 2200S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO req_1: CYCLE 2 / 4-6; req_2: SAME ORIENT FOR 5-6 AS 4; req_3: GROUP 4-6 WITHIN 7D; req_4: ORIENT 36D +/- 15D /4-6; comment_1: ALL PC IMAGES TO BE TAKEN WITH SAME comment_2: SPACECRAFT ORIENTATION. TARGET IN comment_3: CENTER OF PC5. CAN USE COARSE TRACK comment_4: IF NO FINE LOCK GUIDE STARS comment_5: AVAILABLE. ! linenum: 5.000 targname: MINKOWSKI-OBJECT config: PC opmode: IMAGE aperture: PC5 sp_element: F791W wavelength: 7935 num_exp: 3 time_per_exp: 700S s_to_n: 10 s_to_n_time: 2200S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO comment_1: TARGET SHOULD BE PLACED IN comment_2: CENTER OF PC5. COARSE TRACK CAN BE comment_3: USED IF NO FINE LOCK GUIDE STARS comment_4: AVAILABLE. ORIENT CAN ALSO BE 216D comment_5: +/- 15D USING PC7 APERTURE OR 306D comment_6: +/- 15D USING PC6 APERTURE FOR 4-6. ! linenum: 6.000 targname: MINKOWSKI-OBJECT config: PC opmode: IMAGE aperture: PC5 sp_element: F664N wavelength: 6638 num_exp: 3 time_per_exp: 350S s_to_n: 10 s_to_n_time: 1000S fluxnum_1: 1 fluxnum_2: 2 priority: 1 param_1: CR-SPLIT=NO comment_1: TARGET SHOULD BE PLACED IN comment_2: CENTER OF PC5. COARSE TRACK CAN BE comment_3: USED IF NO FINE LOCK GUIDE STARS comment_4: AVAILABLE. ! ! end of exposure logsheet ! No scan data records found