coverpage:
title_1: BLACK HOLE BINARIES IN THE LMC
sci_cat: STELLAR ASTROPHYSICS
sci_subcat: X-RAY BINARIES
proposal_for: GO/CAR
cont_id: 3489
pi_fname: JOHN
pi_mi: B
pi_lname: HUTCHINGS
pi_inst: DOMINION ASTROPHYSICAL OBSERVATORY
pi_country: CANADA
pi_phone: 604-363-0018
hours_pri: 13.30
hours_par: 0.70
num_pri: 2
num_par: 2
wf_pc: Y
fos: Y
hrs: Y
time_crit: Y
funds_amount: 28767
funds_length: 12
off_fname: JAMES
off_mi: E
off_lname: HESSER
off_title: DIRECTOR
off_inst: DOMINION ASTROPHYSICAL OBSERVATORY
off_addr_1: 5071 W. SAANICH RD
off_city: VICTORIA
off_state: BC
off_zip: V8X 4M6
off_country: CANADA
off_phone: 604-363-0007
! end of coverpage
abstract:
line_1: The endpoints of stellar evolution - white dwarfs, neutron stars and
line_2: black holes - can be most directly studied when they occur in binary
line_3: systems such as cataclysmic variables and X-ray binaries. However, only
line_4: a handful of black-hole candidates have been found, and thus very little
line_5: is known about their physical properties and associated accretion disks.
line_6: Two black-hole X-ray binaries, LMC X-3 and CAL 87, are particularly
line_7: suitable for investigation in the UV, where important diagnostic
line_8: emission lines are present and where the disk structure can be modelled
line_9: from the continuum. LMC X-3 has recently been found to have a
line_10: precessing accretion disk (P = 200 days) allowing different parts of the
line_11: disk to be observed over a timescale of months. CAL 87 (P orb 10.6hr) is
line_12: the only known eclipsing black hole, so that observation throughout the
line_13: eclipse will yield detailed information about the disk structure,
line_14: particularly very near the collapsed star itself.
!
! end of abstract
general_form_proposers:
lname: HUTCHINGS
fname: JOHN
title: PI
mi: B
inst: DOMINION ASTROPHYSICAL OBSERVATORY
country: CANADA
!
lname: COWLEY
fname: ANNE
mi: P
inst: ARIZONA STATE UNIVERSITY
country: USA
!
lname: CRAMPTON
fname: DAVID
inst: DOMINION ASTROPHYSICAL OBSERVATORY
country: CANADA
!
lname: SCHMIDKE
fname: PAUL
mi: C
inst: ARIZONA STATE UNIVERSITY
country: USA
!
! end of general_form_proposers block
general_form_text:
question: 3
section: 1
line_1: For LMC X-3 we propose to obtain low dispersion GHRS spectra at two
line_2: wavelength settings, to cover 1160-1750A at each observation. As the star
line_3: is faint (17.5m), we will need to acquire by blind offset from a nearby
line_4: brighter star, unless HST pointing improves. The observation will be repeated
line_5: at five 200-day (disk precession) phases, at a fixed (1.7-day)
line_6: orbital phase.
line_8: If GHRS low dispersion observations are not possible, we would use the
line_9: FOS with G130H and G190H gratings to cover the same spectral range. For
line_10: FOS use, the target acquisition will be direct.
line_12: For CAL 87, we propose to obtain FOS low dispersion (G160L) spectra
line_13: at 6 binary phases, to model the continuum changes through the 10 hour
line_14: orbit. We also propose to obtain FOS high dispersion (G130H) spectra
line_15: of the C IV line at 3 binary phases, to measure the profile changes, and
line_16: model the eclipse of the line-emitting region.
line_18: We request parallel exposures with the PC to study the stellar
line_19: population of the LMC in the neighbourhood of these binaries.
!
question: 4
section: 2
line_1:
line_2: For LMC X-3, we require minimum S/N of 20 per 2A (LSA resolution) with GHRS,
line_3: and this leads to exposure estimates of 2 hours for the combined 2 grating
line_4: settings, for each visit to the star. (This is true for observation
line_5: with either GHRS or FOS, as throughput and efficiencies trade off roughly.)
line_6: The UV flux of CAL 87 is not known (but will be after the cycle 1 GTO data
line_7: are obtained). Best estimates require 10 minutes for the FOS low dispersion
line_8: spectra to achieve a mean S/N of 10 over the UV continuum. The Si IV and
line_9: C IV line data require a S/N of 20 per ~2A (1 arcsec aperture resolution)
line_10: and we estimate exposures for this grating setting of 30 mins per visit.
line_12: To sample the periods sufficiently, we require 5 or more visits to
line_13: each system, making a total of ~14 hours integration time.
!
question: 5
section: 3
line_1: The proposal requires observations at specific binary and precession
line_2: phases to accomplish its science goals. We will specify windows of these
line_3: phases as widely as possible, to facilitate scheduling, but the timing is
line_4: an essential requirement.
!
!end of general form text
general_form_address:
lname: HUTCHINGS
fname: JOHN
mi: B
category: PI
inst: DOMINION ASTROPHYSICAL OBSERVATORY
addr_1: 5071 W. SAANICH RD
city: VICTORIA
state: BC
zip: V8X 4M6
country: CANADA
phone: 604-363-0018
telex: 049-7295 NRC DAO VIC
!
! end of general_form_address records
fixed_targets:
targnum: 1
name_1: CAL87STAR
descr_1: A, 139
pos_1: PLATE-ID=05ZW,
pos_2: RA=5H 46M 50.3S+/-1",
pos_3: DEC=-71D 10' 17.70"+/-1"
equinox: 2000
fluxnum_1: 1
fluxval_1: V=12.3,TYPE=K0
!
targnum: 2
name_1: OFFSET-CAL87
descr_1: A, 133
pos_1: RA-OFF=-3.47S+/- 0.1S,
pos_2: DEC-OFF=82.6" +/- 0.3",
pos_3: FROM 1,
pos_4: PLATE-ID=05ZW
equinox: 2000
comment_1: UV FLUXES KNOWN FROM IUE.
fluxnum_1: 1
fluxval_1: V=19.0 +/- 0.4,TYPE=F
!
! end of fixed targets
! No solar system records found
generic_targets:
targnum_1: 3
name_1: FIELD-NEAR-CAL87
descr_1: LMC FIELD
criteria_1: WFPC2 PARALLEL OBSERVATION
!
! end of generic targets
exposure_logsheet:
linenum: 30.000
targname: CAL87STAR
config: FOS/BL
opmode: ACQ/BINARY
aperture: 4.3
sp_element: MIRROR
num_exp: 1
time_per_exp: 3S
priority: 1
req_1: ONBOARD ACQ FOR 30.1;
req_2: CYCLE 4 / 30-34;
req_3: SEQ 30-32.1 NO GAP;
!
linenum: 30.100
targname: CAL87STAR
config: FOS/BL
opmode: ACQ/PEAK
aperture: 0.3
sp_element: MIRROR
num_exp: 1
time_per_exp: 3S
priority: 1
param_1: SCAN-STEP-X=0.1,
param_2: SCAN-STEP-Y=0.1,
param_3: SEARCH-SIZE-X=4,
param_4: SEARCH-SIZE-Y=4
req_1: ONBOARD ACQ FOR 30.5;
!
linenum: 30.500
targname: OFFSET-CAL87
config: FOS/BL
opmode: ACQ/PEAK
aperture: 0.5
sp_element: MIRROR
num_exp: 1
time_per_exp: 30S
priority: 1
param_1: SCAN-STEP-X=0.3,
param_2: SCAN-STEP-Y=0.3,
param_3: SEARCH-SIZE-X=3,
param_4: SEARCH-SIZE-Y=3,
req_1: ONBOARD ACQ FOR 31-32.1;
!
linenum: 31.000
targname: OFFSET-CAL87
config: FOS/BL
opmode: ACCUM
aperture: 1.0
sp_element: G160L
wavelength: 1150-2510
num_exp: 1
time_per_exp: 30M
priority: 1
req_1: ZERO-PHASE JD2447506.80 +/- 0.02D;
req_2: PERIOD 0.44268D +/- 0.00001D;
req_3: PHASE 0.6 +/- 0.06
!
linenum: 32.000
targname: OFFSET-CAL87
config: FOS/BL
opmode: ACCUM
aperture: 1.0
sp_element: G160L
wavelength: 1150-2510
num_exp: 6
time_per_exp: 38M
priority: 1
!
linenum: 32.100
targname: OFFSET-CAL87
config: FOS/BL
opmode: ACCUM
aperture: 1.0
sp_element: G160L
wavelength: 1150-2510
num_exp: 1
time_per_exp: 30M
priority: 1
!
linenum: 33.000
targname: FIELD-NEAR-CAL87
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F469N
num_exp: 1
time_per_exp: 9320S
priority: 1
req_1: PAR
comment_1: INTENDED TO BE PARALLEL WITH 32
!
linenum: 34.000
targname: FIELD-NEAR-CAL87
config: WFPC2
opmode: IMAGE
aperture: WFALL
sp_element: F467M
num_exp: 1
time_per_exp: 1700S
priority: 1
param_1: CR-SPLIT=NO
req_1: PAR
comment_1: INTENDED TO BE PARALLEL WITH 31
!
! end of exposure logsheet