! Proposal 6736, submission 3
! PI: Michael Combi
! Received Fri Feb 23 13:29:33 EST 1996
! From: mcombi@engin.umich.edu
! Proposal 6736, submission 2
! PI: Michael Combi
! Received Wed Feb 14 18:17:31 EST 1996
! From: mcombi@engin.umich.edu
! +====================+
! | PED OUTPUT PRODUCT |
! +====================+
!
! /afs/engin.umich.edu/u/m/c/mcombi/6736.HST/6736.prop
! Generated by PREPROCESSOR, version 6.0e
! Date: Fri Feb 9 13:48:53 EST 1996
Proposal_Information
Title: A Comprehensive Study of the H Ly--Alpha Line Profile and Water Photochemistry in a TOO Comet
Proposal_Category: GO
Scientific_Category: SOLAR SYSTEM
Cycle: 6
Investigators
PI_Name: Michael Combi
PI_Institution: University of Michigan
CoI_Name: Michael Brown
CoI_Institution: California Institute of Technology
Contact:
CoI_Name: Paul Feldman
CoI_Institution: Johns Hopkins University
Contact:
CoI_Name: H. Uwe Keller
CoI_Institution: Max Planck Institute fur Aeronomie
Contact:
CoI_Name: Robert Meier
CoI_Institution: Naval Research Laboratory
Contact:
CoI_Name: William Smyth
CoI_Institution: Atmospheric & Environmental Research, Inc.
Contact:
Abstract:
We propose to undertake a comprehensive study of water
production and photochemistry in comets using coordinated HST
and ground-based echelle spectroscopic measurements of a
bright comet. The brightness and shape of the H LyAlpha line
profile will be measured at various locations in the inner
coma using GHRS, which has a factor of 4 better spectral
resolution than has ever been obtained for LyAlpha in comets
and 2 better than ground-based observations of HAlpha. FOS
will be used to measure the OH(0-0) emission brightness and
monitor any short-term variations. A LyAlpha image of the
whole inner coma will be constructed with WFPC 2 using the
F160BW and F130LP filters. The HST LyAlpha and OH(0-0)
measurements will be coordinated with a ground-based echelle-
spectroscopy campaign of observing the HAlpha line profile and
the OI 6300Angstrom emission and monitoring the longer term
variability of the comet. It is only through the self-
consistent analysis of such a coordinated set of observations
that we can hope to gain a better quantitative understanding
of the details of the production and photochemistry of water
in comets, such as: (1) the ejection velocity distribution of
H atoms and (via conservation of momentum) OH radicals, (2)
the branching ratio of the two main dissociation branches, (3)
the effects of collisional thermalization of H atoms, and (4)
any spatial and line profile asymmetries from aspherical
outgassing.
Questions
Observing_Description:
The observations of the TOO comet will be scheduled at a time
of reasonably large geocentric velocity, to minimize
interference by any signal from geocoronal hydrogen seen by
HST from low earth orbit which should be small compared with
the comet in any case. The time of the session would
correspond to as optimal an observation as possible given the
intrinsic brightness of the comet and the observational
geometry constraints. For planning purposes we have adopted
the following scenario: a comet with heliocentric and
geocentric distances of 1 AU and a water production rate of 2
x 10^29s^-1. The following observations would be made. 1-WFPC
2 image with F675W for targeting the comet 3-FOS spectra of
the OH(0-0) band near beginning, middle and end of session 6-
GHRS spectra of LyAlpha with ECH-A, side 1 2-WFPC 2 images
with F160BW (CR-SPLIT on one orbit) 1-WFPC 2 image with a
combination of F160BW and F130LP The comet will be targeted
using a WFPC2 image using filter F675W for the purpose of
recalibrating the pre-observation ephemeris. The acquisition
time has improved to 7.5 minutes, so even for a fast moving
comet that needs to be reacquired on each orbit not much time
is lost. On the next orbit one FOS spectrum will be taken to
obtain a baseline water production rate from the OH (0--0)
band emission at 3090Angstrom. Two more will be taken,
roughly in the middle and at the end of each session to
monitor the short term production rate variation. Our
hydrogen coma model has been used to generate an estimated
LyAlpha intensity map (see Fig 2). Assuming that an average
FWHM of 0.1Angstrom for the intrinsic cometary LyAlpha line,
based on the past LyAlpha and HAlpha measurements, and the
sensitivity at LyAlpha listed in the GHRS handbook, we have
estimated reasonable values for the integration time for each
observation and the corresponding count rate and mean signal-
to-noise ratio. The background from the combined sources of
dark current, radiation noise and random count statistics
were also estimated from the information provided in the GHRS
handbook. A series of GHRS spectra would begin on the third
orbit, consisting of a nucleus-centered spectrum and various
offset spectra shown in Table 1. , Table 1 GHRS Comet
Observations begintabbing hspace0.1in\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\=Position(km)
.2in\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\=Brightness(kR) .2in\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\=Integration
Time(s)hspace0.2in\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\=Counts/Diode .2in\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\=Orbits .2in\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\=S/N ,
\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>1. Nucleus>>80\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>2000\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>>300\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>1\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>>14 , \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>2.
5x10^3a>65\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>3000\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>320\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>1\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>14 , \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>3.
5x10^3b>65\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>3000\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>320\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>1\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>14 , \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>4.
5x10^3c>65\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>3000\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>320\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>1\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>14 , \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>5.
3x10^4>35\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>6000\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>336\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>2\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>15 , \\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>6. 10^5>20\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>12000\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>390\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\!
\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>5\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\\>13
, endtabbing The three spectra taken at 5x10^3 km (a to c)
correspond to 3 directions with respect to the nucleus:
sunward, antisunward, and a perpendicular directions (see
also Fig. 2). These observations are designed to test for
coma asymmetry, which could be due to non-spherical
outgassing, optical depth effects or both. In the most
general case one could expect both the integrated line
intensity as well as the line shape to vary around an
optically thick coma, even if the gas is spherically
symmetric. In the case of aspherical gas ejection, the line
itself could display a Doppler shifted offset. For a comet
at 1 AU from the sun the spectrum at an offset of 10^5 km
should contain equal contributions of H produced directly
from water and that produced by OH. The coma at that
distance should also be much less optically thick. After
this, two WFPC 2 images in WF 3 with aperture F160BN15 (i.e.,
rotated 15 degrees), will be taken. With these a LyAlpha
image can be constructed (Clarke et al. 1995). First an
image (actually 2 images assuming CR-SPLIT) will be recorded
using the F160BW (Woods) filter. This yields an image of the
entire far UV spectrum of the comet ( dominated by LyAlpha.
Next an image using the combination of F160BW with F130LP
will be taken. This yields an image with a slightly reduced
throughput of the far UV less the LyAlpha ( light and light
leak. This can all be accomplished on one orbit. All
observations can be acquired in 15 orbits: 11 for the GHRS
spectra, 1 for the targeting WFPC 2 (G675W)image, 1 for the
three far UV WFPC 2 images (2-F160BW and 1-F160BW+F130LP) and
2 for the OH FOS spectrum. All estimates for numbers of
orbits account for a realistic 35 minutes per orbit for
target reacquisition and integration on a moving target at
the declination of the comet, given the theoretical upper
limit of 53 minutes per orbit for all maneuvers.
sectionReferences Brown and Spinrad (1993) Icarus, 104, 197
Budzien, Festou and Feldman (1994) Icarus, 107, 164
Carruthers et al. (1974) Icarus, 23, 526 Clarke et al. (1995)
``Far UV Imaging with the HST WFPC2'' (preprint) Cochran and
Schleicher (1993) Icarus, 105, 235 Code, Houcke and Lillie
(1972) NASA SP-310, pp. 109-114 Combi (1989) Icarus, 81, 41
Combi and Feldman (1992) Icarus, 97, 260 Combi and Feldman
(1993) Icarus, 105, 557 Combi and Smyth (1988a&b) ApJ, 327,
1026 & ApJ, 327, 1044 Crovisier (1989) A&A, 213, 459 Feldman
et al. (1974) Science, 185, 705 Festou et al. (1979) ApJ,
232, 318 Huppler et al. (1975) ApJ, 202, 276 Keller and Meier
(1976) A&A, 52, 272 Meier et al. (1976) A&A, 52, 283
Schleicher and A'Hearn (1982 & 1988) ApJ, 258, 864, & ApJ,
331, 1058 Smyth et al. (1993) ApJ, 413, 756 Smyth et al.
(1995) ApJ, 440, 349 van Dishoeck and Dalgarno (1984) Icarus,
59, 305 Wu and Chen (1993) JGR-Planets, 98, 7415
Real_Time_Justification:
In order to coordinate with the ground-based observations it
would be most desirable to have some forewarning as to the
scheduling of the comet observation. As a target-of-
opportunity object scheduling would occur after
identification of a suitable comet. The probability of
occurrence of a moderate comet could be about once in 2 or 3
years. Since GHRS will only be available for about the half
of Cycle 6 before the shuttle service mission the probability
is about 1/6 to 1/4. The recently discovered comet Hale-Bopp
has the potential to be a fairly bright comet, but its
proximity to the sun in the sky will probably make HST
observations difficult when (or if) the comet is bright.
Along with the HST measurements, we will obtain simultaneous
ground-based measurements of the HAlpha line with the
Hamilton echelle spectrograph on the coude auxiliary
telescope (CAT) at Lick Observatory. The CAT is
undersubscribed, so we expect to be able to mount an
intensive observing campaign on short notice. The ability to
simultaneously match observations at LyAlpha and HAlpha will
provide a vital constraint on the hydrogen coma model and
optical depth calculations. In addition, the relative
advantages and disadvantages of the HST and ground-based
measurements precisely complement one another. One primary
difficulty in the HST measurement is the optical depth at the
LyAlpha line center. A comet, however, is a factor of about
5 less optically thick to solar LyBeta which excites the
HAlpha emission than to solar LyAlpha. With the long-slit
HAlpha spectrum we will then be able to precisely connect
LyAlpha measurements taken at locations in the coma with high
optical depth with those at low optical depth. On the other
hand, the HAlpha measurement suffers from the difficulty of
the subtraction of the strong dust continuum and from the
large numbers of unidentified spectral lines in the vicinity
(see Fig 1). These difficulties make it particularly hard to
use the HAlpha observations to measure the velocities in the
faint wings of the line (Brown & Spinrad 1993). The HST
measurement will have neither of these problems -- and
LyAlpha is optically thin in the line wings -- so it will
provide the first reliable direct measurement of the high-
velocity hydrogen.
Calibration_Justification:
Additional_Comments:
Fixed_Targets
Solar_System_Targets
Target_Number: 1
Target_Name: B2
Description: COMET B2-NUCLEUS
Level_1: TYPE=COMET,Q=0.2294915,E=1.0000000,I=124.65024,O=188.15597,W=130.29556,T=01-May-1996:13:16:14.0,EQUINOX=J2000,EPOCH=07-Feb-1996
Level_2:
Level_3:
Window: RVEL B2 EARTH GT 40
RANGE B2 EARTH LT 0.6
RANGE B2 SUN LT 1.2
Ephem_Uncert: 10000 KM
Acq_Uncert: 20 "
Flux:
V = 10
B-V = 0.8
V-R = 0.4
Comments: Requires ephemeris correction.
Target_Number: 2
Target_Name: B2-OFFSET-2
Description: COMET B2-OFFSET-2
Level_1: TYPE=COMET,Q=0.2294915,E=1.0000000,I=124.65024,O=188.15597,W=130.29556,T=01-May-1996:13:16:14.0,EQUINOX=J2000,EPOCH=07-Feb-1996
Level_2: TYPE=POS_ANGLE,RAD=23.0,ANG=0.0,REF=SUN
Level_3:
Window: R_VEL B2 EARTH GT 40
RANGE B2 EARTH LT 0.6
RANGE B2 SUN LT 1.2
Ephem_Uncert: 10000 KM
Acq_Uncert: 20 "
Flux:
V = 10
B-V = 0.8
V-R = 0.4
Comments: Requires ephemeris correction.
Target_Number: 3
Target_Name: B2-OFFSET-3
Description: COMET B2-OFFSET-3
Level_1: TYPE=COMET,Q=0.2294915,E=1.0000000,I=124.65024,O=188.15597,W=130.29556,T=01-May-1996:13:16:14.0,EQUINOX=J2000,EPOCH=07-Feb-1996
Level_2: TYPE=POS_ANGLE,RAD=23.0,ANG=180.0,REF=SUN
Level_3:
Window: R_VEL B2 EARTH GT 40
RANGE B2 EARTH LT 0.6
RANGE B2 SUN LT 1.2
Ephem_Uncert: 10000 KM
Acq_Uncert: 20 "
Flux:
V = 10
B-V = 0.8
V-R = 0.4
Comments: Requires ephemeris correction.
Target_Number: 4
Target_Name: B2-OFFSET-4
Description: COMET B2-OFFSET-4
Level_1: TYPE=COMET,Q=0.2294915,E=1.0000000,I=124.65024,O=188.15597,W=130.29556,T=01-May-1996:13:16:14.0,EQUINOX=J2000,EPOCH=07-Feb-1996
Level_2: TYPE=POS_ANGLE,RAD=23.0,ANG=90.0,REF=SUN
Level_3:
Window: R_VEL B2 EARTH GT 40
RANGE B2 EARTH LT 0.6
RANGE B2 SUN LT 1.2
Ephem_Uncert: 10000 KM
Acq_Uncert: 20 "
Flux:
V = 10
B-V = 0.8
V-R = 0.4
Comments: Requires ephemeris correction.
Target_Number: 5
Target_Name: B2-OFFSET-5
Description: COMET B2-OFFSET-5
Level_1: TYPE=COMET,Q=0.2294915,E=1.0000000,I=124.65024,O=188.15597,W=130.29556,T=01-May-1996:13:16:14.0,EQUINOX=J2000,EPOCH=07-Feb-1996
Level_2: TYPE=POS_ANGLE,RAD=138.0,ANG=0.0,REF=SUN
Level_3:
Window: R_VEL B2 EARTH GT 40
RANGE B2 EARTH LT 0.6
RANGE B2 SUN LT 1.2
Ephem_Uncert: 10000 KM
Acq_Uncert: 20 "
Flux:
V = 10
B-V = 0.8
V-R = 0.4
Comments: Requires ephemeris correction.
Target_Number: 6
Target_Name: B2-OFFSET-6
Description: COMET B2-OFFSET-6
Level_1: TYPE=COMET,Q=0.2294915,E=1.0000000,I=124.65024,O=188.15597,W=130.29556,T=01-May-1996:13:16:14.0,EQUINOX=J2000,EPOCH=07-Feb-1996
Level_2: TYPE=POS_ANGLE,RAD=461,ANG=0.0,REF=SUN
Level_3:
Window: R_VEL B2 EARTH GT 40
RANGE B2 EARTH LT 0.6
RANGE B2 SUN LT 1.2
Ephem_Uncert: 10000 KM
Acq_Uncert: 20 "
Flux:
V = 10
B-V = 0.8
V-R = 0.4
Comments: Requires ephemeris correction.
Generic_Targets
Scan_Data
Visits
Visit_Number: 01
Visit_Requirements:
GUID TOL 0.2"
GROUP 1-15 WITHIN 36H
BETWEEN 29-MAR-96 AND 4-APR-96
SCHED 100%
On_Hold_Comments:
Visit_Comments: Visit should be completed in one orbit.
Uplink offset correction to comet ephemeris before next Visit.
RANGE and BETWEEN requirements define same window.
Exposure_Number: 11
Target_Name: B2
Config: WFPC2
Opmode: IMAGE
Aperture: WF3
Sp_Element: F675W
Wavelength:
Optional_Parameters: CR-SPLIT=NO
Number_of_Iterations: 1
Time_Per_Exposure: 5S
Special_Requirements: SAVE OFFSET B2
REQ EPHEM CORR B2A
Comments: Determines ephemeris corrections for all other visits.
Exposure_Number: 12
Target_Name: B2
Config: WFPC2
Opmode: IMAGE
Aperture: WF3
Sp_Element: F675W
Wavelength:
Optional_Parameters: CR-SPLIT=NO
Number_of_Iterations: 1
Time_Per_Exposure: 10S
Special_Requirements: REQ EPHEM CORR B2A
Comments: Determines ephemeris corrections for all other visits.
Exposure_Number: 13
Target_Name: B2
Config: WFPC2
Opmode: IMAGE
Aperture: WF3
Sp_Element: F675W
Wavelength:
Optional_Parameters: CR-SPLIT=NO
Number_of_Iterations: 1
Time_Per_Exposure: 20S
Special_Requirements: REQ EPHEM CORR B2A
Comments: Determines ephemeris corrections for all other visits.
Exposure_Number: 14
Target_Name: B2
Config: WFPC2
Opmode: IMAGE
Aperture: F160BN15
Sp_Element: F160BN15
Wavelength:
Optional_Parameters: CR-SPLIT=DEF,ATD-GAIN=7
Number_of_Iterations: 1
Time_Per_Exposure: 20M
Special_Requirements: REQ EPHEM CORR B2A
Visit_Number: 02
Visit_Requirements:
GUID TOL 0.2"
GROUP 2-7 WITHIN 11H
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Before Visit 02 enough time is needed to uplink comet offset
corrections based on images from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 21
Target_Name: B2
Config: FOS/RD
Opmode: IMAGE
Aperture: 4.3
Sp_Element: G270H
Wavelength:
Optional_Parameters: Y-SIZE=5
Y-SPACE=128
COMB=YES
SUB-STEP=4
Number_of_Iterations: 1
Time_Per_Exposure: 300S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Assumes V=10.3 for the comet in a 0.7" diameter FOV
Exposure_Number: 22
Target_Name: B2
Config: FOS/RD
Opmode: ACCUM
Aperture: 4.3
Sp_Element: G270H
Wavelength:
Optional_Parameters:
Number_of_Iterations: 1
Time_Per_Exposure: 19M
Special_Requirements: EXPAND
END ORBIT
USE OFFSET B2
REQ EPHEM CORR B2A
MIN DUR 18M
Comments:
Visit_Number: 03
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 30
Target_Name: B2
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 1
Time_Per_Exposure: 652.8S
Special_Requirements:
USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Nucleus-centered spectrum.
Exposure_Number: 31
Target_Name: B2
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 1
Time_Per_Exposure: 652.8S
Special_Requirements: SEQ 31-32 NON-INT
USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Nucleus-centered spectrum.
Exposure_Number: 32
Target_Name: WAVE
Config: HRS
Opmode: ACCUM
Aperture: SC2
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: SPYBAL=NO
Number_of_Iterations: 1
Time_Per_Exposure: DEF
Special_Requirements: SAME POS AS 31
USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Wavelength Calibration
Visit_Number: 04
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 41
Target_Name: B2-OFFSET-2
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 5000 km sunward.
Visit_Number: 05
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 51
Target_Name: B2-OFFSET-3
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 5000 km antisunward.
Visit_Number: 06
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 61
Target_Name: B2-OFFSET-4
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 5000 km normal to sun-comet line.
Visit_Number: 07
Visit_Requirements:
GUID TOL 1.0"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 71
Target_Name: B2-OFFSET-5
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 30000 km sunward.
Visit_Number: 08
Visit_Requirements:
GUID TOL 1.0"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 81
Target_Name: B2-OFFSET-5
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 30000 km sunward.
Visit_Number: 09
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 91
Target_Name: B2
Config: FOS/RD
Opmode: IMAGE
Aperture: 4.3
Sp_Element: G270H
Wavelength:
Optional_Parameters: Y-SIZE=5
Y-SPACE=128
COMB=YES
SUB-STEP=4
Number_of_Iterations: 1
Time_Per_Exposure: 300S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Assumes V=10.3 for the comet in a 0.7" diameter FOV
Exposure_Number: 92
Target_Name: B2
Config: FOS/RD
Opmode: ACCUM
Aperture: 4.3
Sp_Element: G270H
Wavelength:
Optional_Parameters:
Number_of_Iterations: 1
Time_Per_Exposure: 19M
Special_Requirements: EXPAND
END ORBIT
USE OFFSET B2
REQ EPHEM CORR B2A
MIN DUR 18M
Comments:
Visit_Number: 10
Visit_Requirements:
GUID TOL 2.0"
GROUP 10-15 WITHIN 11H
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 100
Target_Name: B2-OFFSET-6
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 1
Time_Per_Exposure: 652.8S
Special_Requirements:
USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 100000 km sunward.
Exposure_Number: 101
Target_Name: B2-OFFSET-6
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 1
Time_Per_Exposure: 652.8S
Special_Requirements: SEQ 101-102 NON-INT
USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 100000 km sunward.
Exposure_Number: 102
Target_Name: WAVE
Config: HRS
Opmode: ACCUM
Aperture: SC2
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: SPYBAL=NO
Number_of_Iterations: 1
Time_Per_Exposure: DEF
Special_Requirements: SAME POS AS 101
USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Wavelength Calibration
Visit_Number: 11
Visit_Requirements:
GUID TOL 2.0"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 111
Target_Name: B2-OFFSET-6
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 100000 km sunward.
Visit_Number: 12
Visit_Requirements:
GUID TOL 2.0"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 121
Target_Name: B2-OFFSET-6
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 100000 km sunward.
Visit_Number: 13
Visit_Requirements:
GUID TOL 2.0"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 131
Target_Name: B2-OFFSET-6
Config: HRS
Opmode: ACCUM
Aperture: 0.25
Sp_Element: ECH-A
Wavelength: 1215
Optional_Parameters: FP-SPLIT=TWO
Number_of_Iterations: 3
Time_Per_Exposure: 489.6S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Offset 100000 km sunward.
Visit_Number: 14
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 141
Target_Name: B2
Config: WFPC2
Opmode: IMAGE
Aperture: F160BN15
Sp_Element: F130LP,F160BN15
Wavelength:
Optional_Parameters: CR-SPLIT=NO,ATD-GAIN=7
Number_of_Iterations: 1
Time_Per_Exposure: 7M
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments:
Exposure_Number: 142
Target_Name: B2
Config: WFPC2
Opmode: IMAGE
Aperture: F160BN15
Sp_Element: F160BN15
Wavelength:
Optional_Parameters: CR-SPLIT=DEF,ATD-GAIN=7
Number_of_Iterations: 1
Time_Per_Exposure: 15M
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments:
Visit_Number: 15
Visit_Requirements:
GUID TOL 0.2"
after 1 by 5h to 36h
SCHED 100%
On_Hold_Comments:
Visit_Comments: Requires ephemeris corrections from Visit 01.
Use "use offset" for all exposures this visit.
Exposure_Number: 151
Target_Name: B2
Config: FOS/RD
Opmode: IMAGE
Aperture: 4.3
Sp_Element: G270H
Wavelength:
Optional_Parameters: Y-SIZE=5
Y-SPACE=128
COMB=YES
SUB-STEP=4
Number_of_Iterations: 1
Time_Per_Exposure: 300S
Special_Requirements: USE OFFSET B2
REQ EPHEM CORR B2A
Comments: Assumes V=10.3 for the comet in a 0.7" diameter FOV
Exposure_Number: 152
Target_Name: B2
Config: FOS/RD
Opmode: ACCUM
Aperture: 4.3
Sp_Element: G270H
Wavelength:
Optional_Parameters:
Number_of_Iterations: 1
Time_Per_Exposure: 19M
Special_Requirements: EXPAND
END ORBIT
USE OFFSET B2
REQ EPHEM CORR B2A
MIN DUR 18M
Comments:
Data_Distribution ! Defaults indicated; change if desired
Medium: 8MM
Blocking_Factor: 10
Ship_To: PI_Address
Ship_Via: UPS
Recipient_Email:
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