! File: 4951C.PROP ! Database: PEPDB ! Date: 23-FEB-1994:12:03:42 coverpage: title_1: KING, AUGMENTATION, STELLAR POPULATIONS, PART 2 sci_cat: STELLAR POPULATIONS sci_subcat: GLOBULAR CLUSTERS proposal_for: AUG/OS cont_id: 3684 pi_fname: IVAN pi_lname: KING pi_inst: UNIVERSITY OF CALIFORNIA, BERKELEY pi_country: USA pi_phone: 510-642-2206 keywords_1: GLOBULAR CLUSTER hours_pri: 1.84 hours_par: 1.83 num_pri: 4 num_par: 3 wf_pc: Y hsp: Y pi_position: PROF. OF ASTRONOMY ! end of coverpage abstract: line_1: This proposal is a followup to the UV imaging in 3218, which discovered line_2: a UV and visible counterpart to the X-ray burster in NGC 6624. With the line_3: HSP, using a wide band in the UV, a 30-min data stream will be taken at line_4: the highest available rate, and two 40-min streams at about 300 mu-sec. line_5: The data will be analyzed over the known 11-minute binary orbit, the line_6: 30-40 Hz QPO range, and the 5 mu-sec period of a neighboring pulsar line_7: which may fall in the field of view. The S/N will be high enough to line_8: search for any other possible periodicities. line_10: The WFC will do parallel imaging at the edge of the cluster, in V and I. ! ! end of abstract general_form_proposers: lname: KING fname: IVAN title: PI inst: UNIV. OF CALIFORNIA country: U.S.A. ! lname: BLESS fname: ROBERT title: DR. inst: UNIV. OF WISCONSIN country: U.S.A. ! lname: FRUCHTER fname: ANDREW title: DR. inst: UNIV. OF CALIFORNIA country: U.S.A. ! lname: ARONS fname: JONATHAN title: PROF. inst: UNIV. OF CALIFORNIA country: U.S.A. ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: FOC imaging with F140W, F430W, and F480LP has revealed an optical line_2: counterpart to the notorious X-ray burster 4U 1820-30 in the line_3: globular cluster NGC 6624. The star, which has B=18.6, cannot be line_4: observed from the ground, because it is surrounded by many red line_5: giants within an arcsec. It is proposed to observe it in the UV line_6: with the HSP, with high time resolution and also with the highest line_7: time resolution. line_9: The behavior of 4U 1820-30 is bizarre in many ways. Besides being line_10: an X-ray burster, it shows quasi-periodic oscillations at 30-40 Hz, line_11: which might possibly be a beat period between the rotation period of line_12: the neutron star and the Keplerian periods of condensations in its line_13: accretion disk. It also emits "shots" with a decay time of 17 sec. line_14: And its radiation varies slightly in its 11-min binary orbit (the line_15: shortest known) with its companion. All this in X-rays; in the line_16: optical all we have so far is the detection. line_18: The 11-minute orbital-period variation in X-ray flux is only 3%. UV line_19: variations should be much larger, since the companion must have a line_20: hot side and a cold side. According to a recent unpublished model by line_21: J. Arons, the companion should be contributing about 1/4 of the line_22: total UV light. ! question: 4 section: 1 line_1: The partial orbit is to get the finest possible detail if there is line_2: any millisecond-scale activity. The other two orbits are to study line_3: time variations at all scales, from a few milliseconds to 11 minutes line_4: or more. ! question: 5 section: 1 line_1: Exposure line 2 requires TDRSS contact. ! question: 6 section: 1 line_1: Note that THE HSP exposures have parallel WFC exposures (so that the line_2: true efficiency of HST usage is much higher than indicated by the line_3: percentage quoted in Phase I.) ! question: 6 section: 2 line_1: The highest data-taking rate of the HSP requires TDRSS contact. ! question: 7 section: 1 line_1: At Berkeley we have a VMS cluster and a Sun cluster. I have a line_2: Microvax II GPX and a Sun IPC with a gigabyte disk. For software we line_3: have been using Vista, DAOPHOT, and IRAF/STSDAS. Although it is an line_4: unhappy fact that no one has yet arrived at the ideal method of line_5: doing stellar photometry on HST images, I am doing at least as well line_6: as anyone else and am in contact with most of those who are making line_7: efforts in this direction. line_9: Bless has ample equipment and support in Madison. ! question: 8 section: 1 line_1: Note that this should get high priority in Cycle 3, because after line_2: Cycle 3 there will be no more HSP. ! question: 9 section: 1 line_1: Previous HST observing time: line_3: SAO-3121, MORPHOLOGY OF FAINT GALAXIES - PART II line_4: GTO-1277, IMAGING OF M31-GROUP GALAXIES line_5: GTO-1278, SPECTROSCOPY OF THE CENTERS OF M31, M32, AND NGC 205 line_6: GTO-1279, STRUCTURE OF GLOBULAR CLUSTERS line_7: AUG-3684, KING, AUGMENTATION, STELLAR POPULATIONS line_8: GTO-1281, THE FAINT POPULATION IN BAADE'S WINDOW line_9: AUG-3685, IMAGING OF HIGH-REDSHIFT FIELD GALAXIES AND CLUSTERS line_10: GTO-3218, (continuation of 1279) line_11: AUG-3870, (continuation of 1277) line_12: GTO-3325, (continuation of 1279, 3218) line_14: 3218 is closely related to this proposal, having discovered line_15: the object that is being studied here. line_17: Bless of course has many HSP proposals. ! question: 9 section: 2 line_1: Main results from previous related programs: line_3: 3121 produced a report that I am told was quite useful to the Cycle line_4: 1 Re-TAC, and also the publication below. ! question: 9 section: 3 line_1: "The Current Ability of HST to Reveal Morphological Structure in line_2: Medium-Redshift Galaxies", King, I.R., et al. (8 other authors), line_3: Astron. J. 102, 1553, 1992. ! question: 10 section: 1 line_1: Hardware/software as above. Postdoc + RA's. GTO funding (from line_2: NASA). ! !end of general form text general_form_address: lname: KING fname: IVAN title: PROF. category: PI inst: UNIVERSITY OF CALIFORNIA, BERKELEY addr_1: ASTRONOMY DEPARTMENT addr_2: UNIVERSITY OF CALIFORNIA city: BERKELEY state: CA zip: 94720 country: U.S.A. phone: (510)642-2206 telex: (910)366-7114 from_date: 15-MAR-92 to_date: 31-DEC-99 ! ! end of general_form_address records fixed_targets: targnum: 1 name_1: NGC6624 descr_1: C,201 pos_1: RA = 18H 20M 27.8S +/- 0.1S, pos_2: DEC = -30D 23' 16" +/-1" equinox: 1950 ! targnum: 2 name_1: NGC6624-OUTER descr_1: C,201,911 pos_1: RA = 18H 20M 27.9S, pos_2: DEC = -30D 23' 15", pos_3: REGION, pos_4: R = 7' equinox: 1950 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 1.000 targname: NGC6624 config: HSP/UV2 opmode: ACQ num_exp: 1 time_per_exp: 4S fluxnum_1: 1 priority: 1 param_1: DATA-FORMAT=WORD, req_1: ONBOARD ACQ FOR 2.000; req_2: CYCLE 3 / 1-16; req_3: SEQ 1-6 NO GAP ! linenum: 2.000 targname: NGC6624 config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 30M priority: 1 param_1: DATA-FORMAT=BYTE, param_2: SAMPLE-TIME=0.0000108, req_1: RT ANALYSIS; comment_1: EXPOSURE IS SHORT ENOUGH comment_2: THAT GSACQ CAN BE DONE ON comment_3: SAME ORBIT. comment_4: TDRSS DOWNLINK REQUIRED. ! linenum: 4.000 targname: NGC6624 config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 40M priority: 1 param_1: DATA-FORMAT=BYTE, param_2: SAMPLE-TIME=0.0002916, req_1: SAME ORIENT FOR 4 AS 2; comment_1: TARGET VISIBILITY IS 50M. THIS ALLOWS comment_2: TIME FOR GSREAC+EXP IN A SINGLE ORBIT. ! linenum: 6.000 targname: NGC6624 config: HSP/UV2 opmode: SINGLE aperture: 10.0 sp_element: F140LP num_exp: 1 time_per_exp: 40M priority: 1 param_1: DATA-FORMAT=BYTE, param_2: SAMPLE-TIME=0.0002916, req_1: SAME ORIENT FOR 6 AS 2; comment_1: TARGET VISIBILITY IS 50M. THIS ALLOWS comment_2: TIME FOR GSREAC+EXP IN A SINGLE ORBIT. ! linenum: 12.000 targname: NGC6624-OUTER config: WFC opmode: IMAGE aperture: WFALL sp_element: F785LP num_exp: 1 time_per_exp: 30M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO, req_1: PAR; comment_1: INTENDED TO BE PARALLEL WITH LINE 2. comment_2: IF WFC EXPOSURES CAUSE DATA RATE comment_3: TO BE EXCESSIVE, OMIT LINES 12,14,16. ! linenum: 14.000 targname: NGC6624-OUTER config: WFC opmode: IMAGE aperture: WFALL sp_element: F785LP num_exp: 1 time_per_exp: 40M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO, req_1: PAR; comment_1: INTENDED TO BE PARALLEL WITH LINE 4. ! linenum: 16.000 targname: NGC6624-OUTER config: WFC opmode: IMAGE aperture: WFALL sp_element: F555W num_exp: 1 time_per_exp: 40M priority: 1 param_1: CR-SPLIT=NO, param_2: PRE-FLASH=NO, req_1: PAR; comment_1: INTENDED TO BE PARALLEL WITH LINE 6. ! ! end of exposure logsheet ! No scan data records found