! 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