fixed typo in Co-I name, and added an extra visit to test for earlier opportunities
add new ephem cor number to visit 01----- Attempting Submission 1 (Wed Jan 20 22:44:34 GMT 2010) -----
HST Phase II Proposal 12053 (P2010A2_submitted.apt) successfully submitted.
----- Attempting Submission 2 (Wed Jan 20 23:29:18 GMT 2010) -----
----- Attempting Submission 4 (Thu Jan 21 12:47:20 GMT 2010) -----
HST Phase II Proposal 12053 (12053.apt) successfully submitted.
----- Attempting Submission 5 (Thu Jan 21 12:59:36 GMT 2010) -----For some reason, the observations get split across orbits when the visibility planner
is run on Hal Weaver's machine. This doesn't happen on Max Mutcher's machine, so
we're submitting it w/o running on Weaver's machine.Hubble Investigation of the Unusual Object P/2010 A2On 2010 January 6, the LINEAR survey telescope detected an extremely
unusual-looking object (P/2010 A2) that appears to be either: (1) the most
remarkable member of a new dynamical class known as the main-belt comets
(MBCs), or (2) a manifestation of a collision between two asteroids in the
Flora family. In either case, this discovery could have profound
implications for planetary science. We propose a 5-orbit Hubble
investigation of P/2010 A2, executed within the next week if possible, to
determine the nature of this strange, quickly-evolving object. Deep WFC3 (or ACS/WFC)
images taken over a 6 hr period will be used to measure the size, shape, and
rotational period of the nucleus, to characterize the near-nucleus
environment, and to perform a deep search for any decameter-sized fragments.
We will also measure the color of the nucleus in 3 different bands for
comparison with asteroids and other cometary nuclei. With its high spatial
resolution and high sensitivity, Hubble is uniquely suited to this
investigation.At its declination of +28 , P/2010 A2 will have an HST visibility window of 54 min per
orbit. We are working closely with the JPL Horizons group to ensure we have knowledge of
the object’s ephemeris to an accuracy of 10′′, or better, for the HST observations, which
is more than adequate for planning these imaging observations. (The WFC3 has a field-ofview
of 162′′ × 162′′, and the ACS/WFC has a field-of-view of 202′′ × 202′′.) At the time of
the Hubble observations, the object’s heliocentric distance will be 1.9 AU, the geocentric
distance will be 1 AU (corresponding to 29 km/pixel at the comet for the WFC3), the
solar elongation angle will be 160◦, the solar phase angle will be 10◦, and the galactic
latitude (which aects the level of background star contamination) will be 13◦. All of these
geometric parameters are currently favorable for Hubble observations, but the conditions get
progressively worse over time. The target’s apparent rate of motion is 35′′/hr, which is
easily within Hubble’s tracking capabilities. This rate of motion is also slow enough to keep
a single pair of guide stars within the FGS pickles for an entire visibility window.
This program requires both high spatial resolution and high sensitivity. The former
drives us to the WFC3 (0.′′4/pix vs 0.′′5/pix), but the latter argues for use of the ACS/WFC3
(with 2x the throughput at visible wavelengths). We have tentatively selected WFC3 for
this submission (partly because of its higher spatial resolution and partly because we figure
the degraded CTE and increased noise of the ACS/WFC might negate some of its perceived
advantage in sensitivity), but we plan to consult with the relevant STScI experts before
making a final decision on which camera to use for this investigation.
We request 5 consecutive orbits utilizing the newly commissioned WFC3. Our choice
of 5 orbits is a compromise between the desire to characterize the temporal evolution of the
object and the need to minimize the impact on Hubble’s observing schedule. Our planned
observations would cover a clock time of 6 hours, which should be sufficient to include an
entire sinusoid of a dual-peaked light curve for a “typical” rotational period of 12 hours.
During orbits #1, #3, and #5, we tentatively plan to take images in 3 different filters
(here we assume WFC3): F390W (or possibly F475W), F606W, and F814W. Orbits #2
and #4 will be used entirely for F606W. This strategy balances our attempt to go as deep
as possible, yet also obtain some color information for comparison with previously observed
asteroids and cometary nuclei.
Our nominal observing strategy will be to use a standard 2-point dither, taking a series
of images (e.g., 1-2 long F606W images and 1 long exposure each using F390W and F814W)
at one location near the center of one of the CCD chips, and an identical series at the second
dither location. Dithering mitigates the effects of bad pixels and cosmic ray events. We will
shift and add the resultant images, reaching a limiting magnitude (S/N5) of V 27.5 for
the F606W images, as determined from the WFC3 ETC assuming a total exposure time of
2000 sec and a solar-type spectrum. This latter limit corresponds to an object having a
diameter of 25-30 m, assuming an albedo of 10% and a phase law of 0.04 mag/deg. For
the F390W and F814W filters, we only require reaching S/N10 for V 24, which can be
accomplished using exposure times of 320 sec and 120 sec, respectively. We expect to
use exposure times of at least 347 sec for all of our images to “hide” the overhead associated
with dumping the data storage buffer.
We understand that we will have essentially no control over the spacecraft roll angle,
which means we won’t be able to optimize the orientation of the dust tail on the CCD (i.e., to
orient the tail along the longest dimension of the detector). The field-of-view of the camera
is large enough that we should obtain excellent data on a portion of the tail, no matter what
spacecraft roll angle is used.
The proposed observing plan features the following properties:
We will probe the spectral properties of the main component; these include the spectral
slope between the F390W and F606W bands, and the prominent silicate absorption
band in F814W – a signature of S-type asteroids. A sensitive search for fragments in F606W.
Mitigation of the brightness modulation from the body rotation; this eect will be
largely averaged-out if we change filters in the suggested manner.Observations at the earliest opportunity, possibly next week, are highly desired, since material
in P/2010 A2 is dispersing and fading. We request that observations be taken no later
than the end of January in order to connect the HST-observed morphology with the initial
morphology obtained from the ground (albeit at 10 times poorer resolution).0false0.00.0falsefalsefalsefalsefalsefalseSUPPORTEDSOLAR SYSTEMCOMETMain-belt comet or collision between two asteroidsTYPE=COMET,Q=2.0112975,E=0.1231870,I=5.28995,O=320.13138,W=133.28380,T=04-DEC-2009:07:05:09,EQUINOX=J2000,EPOCH=25-NOV-2009:00:00:00EARTHduplicate of visit 11 to see if it can go earlier than day 29.(Tic-Visit
:proposal-id 12053
:visit-id "11"
:proposal-version -1
:trans-version "20091209"
:date "20-Jan-2010 17:39:30.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 1154992
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 12053
:visit-id "11"
:obset-id "11"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 12053
:visit-id "11"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2848
:al-overhead-at-end 0
:internal-dur-at-end 670
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3234
:pcs-gap 0
)false10Using ephemeris for target 12053-11-P2010-A2ephemeris data for target 12053-11-P2010-A2 does not cover planning interval. Physical constraints are assumed to be unschedulable outside of the ephemeris data. Planning interval: 08.245 to 11.001. ephemeris interval: 09.365 to 12.001Timing link suitability includes constraints ([Sequence (11 12 13) within 1.0 days])The scheduling data was generated by CASM 18.1.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 12053
:visit-id "11"
:proposal-version -1
:trans-version "20091209"
:date "20-Jan-2010 17:39:30.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:data-volume 1154992
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
:proposal-id 12053
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(Tic-Orbit
:proposal-id 12053
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:orbit-number 1
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:si-vis-utilization 2848
:al-overhead-at-end 0
:internal-dur-at-end 670
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3234
:pcs-gap 0
)false10(Tic-Visit
:proposal-id 12053
:visit-id "12"
:proposal-version -1
:trans-version "20091209"
:date "20-Jan-2010 17:39:33.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 1
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:si-bright-earth-limb-angle 20.0
:data-volume 1154992
:tdrss-contact-duration 0
:coron NIL
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(Tic-Obset
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:visit-id "12"
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(Tic-Orbit
:proposal-id 12053
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:orbit-number 1
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)false10(Tic-Visit
:proposal-id 12053
:visit-id "13"
:proposal-version -1
:trans-version "20091209"
:date "20-Jan-2010 17:39:36.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
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(Tic-Obset
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:visit-id "13"
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(Tic-Orbit
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