Both visit 01 and visit 03 will need to have orientation constraints added once the corresponding
first-epoch observations have been taken in GO 11697.
This version is being submitted by the Contact Scientist so that the the currently restricted mode
of charge injection on the UVIS detector can be used for visit 02 before the release of the next
version of APT, which enables the selection of charge injection by GOs.
Added the orientation constraints for visits 01 and 03.
Added charge injection for visits 01 and 03. TP 10/31/2011----- Attempting Submission 1 (Fri Jul 09 19:17:58 GMT 2010) -----
----- Attempting Submission 2 (Tue Apr 26 20:32:08 GMT 2011) -----
----- Attempting Submission 3 (Mon Aug 08 14:54:56 GMT 2011) -----
HST Phase II Proposal 12319 (prop12319-3rdsubmission.apt) successfully submitted.
----- Attempting Submission 4 (Mon Oct 31 18:18:17 GMT 2011) -----This version of the proposal is being submitted by the Contact Scientist using
restricted mode so that charge injection can be used for visit 02 before the release
of the next version of APT, which will enable GOs to select charge injection for
cycle 19. This early use of charge injection has been approved by Ken Sembach,
and was prompted by the PI's stated interest of using charge injection in the
multi-cycle phase I proposal.
Added orientation constraints for visits 01 and 03. The diagnostics are for
visit 02, which has already been observed.
Added charge injection for visits 01 and 03. The diagnostics are for visit 02,
which has already been observed.Proper Motion Survey of Classical and SDSS Local Group Dwarf GalaxiesUsing the superior resolution of HST, we propose to continue our proper
motion survey of Galactic dwarf galaxies. The target galaxies include
one classical dwarf, Leo II, and six that were recently identified in
the Sloan Digital Sky Survey data: Bootes I, Canes Venatici I, Canes
Venatici II, Coma Berenices, Leo IV, and Ursa Major II. We will
observe a total of 16 fields, each centered on a spectroscopically-
confirmed QSO. Using QSOs as standards of rest in measuring absolute
proper motions has proven to be the most accurate and most efficient
method. HST is our only option to quickly determine the space motions
of the SDSS dwarfs because suitable ground-based imaging is only a few
years old and such data need several decades to produce a proper
motion. The two most distant galaxies in our sample will require time
baselines of four years to achieve our goal of a 30-50 km/s uncertainty
in the tangential velocity; given this and the finite lifetime of HST,
it is imperative that first-epoch observations be taken in this cycle.
The SDSS dwarfs have dramatically lower surface brightnesses and
luminosities than the classical dwarfs. Proper motions are crucial for
determining orbits of the galaxies and knowing the orbits will allow us
to test theories for the formation and evolution of these galaxies and,
more generally, for the formation of the Local Group.A series of papers by Piatek et al. (2002, 2003, 2005 -- 2008)
describes our method for deriving proper motions for dwarf galaxies
using WFPC2, STIS, and ACS/HRC imaging. A known QSO in the target
field provides the reference point for measuring the motion of the
stars in the galaxy. The QSO and stars in the field are used to
construct an effective point-spread function (e.g., Anderson & King
2000). Fitting this PSF to star-like images yields positions.
Dithered exposures at each epoch both refine the PSF and provide
independent position measurements which are averaged to reduce the
final uncertainty. We prefer to minimize the effects of distortions in
the cameras by maintaining the same orientation at each epoch, though
we have successfully reduced data where this is not the case.
Our proposed exposure times will achieve S/N = 15-- 20 at V=25.5
according to the ETC and confirmed by our Draco ACS/WFC data
(GO 10812). The data for the Draco J1720+5755 field, which is close to
the center and for which we have two epochs, gives a measured surface
density of stars to V=25.5. Proper motions indicate that almost all
are members. We have used this measured surface density to predict the
central surface density to V=25.5 for our target galaxies, taking
their different distances and central surface brightnesses into
account. To determine the surface density at the locations of our
target fields, we use density profiles from the literature.
We propose to observe with the WFC3 rather than ACS/WFC because it has
smaller pixels, yields a higher S/N for a given exposure time when
used with the F350LP filter, has a less degraded CCD, and has the
possibility of mitigating CTE degradation with charge injection. We
concluded that these advantages outweighed the 1.6X larger field
of view of ACS/WFC. Our exposure times are generally determined by
the requirement that the QSO be half-way to saturation. We choose the
50% limit for the QSOs in order to provide some buffer for photometric
variability --- with this limit we have never saturated a QSO.
Our experience shows that we should have at least 12 images per epoch to
achieve the required accuracies for the proper motions. For the exposure times
needed to reach V=25.5 with S/N=15, this requires 3 orbits per field at each epoch.
Thus, our program will require 49 orbits in cycle 17, 12 orbits
in cycle 18, and 49 orbits in cycle 19. The total is 110 orbits spread
over the three cycles.12false0.00.0falsefalsefalsefalseSUPPORTEDGALAXYDWARF SPHEROIDALQSOThe coordinates are for a QSO behind the dwarf spheroidal galaxy Coma Bernices.J2000J2000GALAXYDWARF SPHEROIDALQSOThe coordinates are for a QSO behind the dwarf spheroidal galaxy Coma Bernices.J2000J2000GALAXYDWARF SPHEROIDALQSOThe coordinates are for a QSO behind the dwarf spheroidal galaxy Bootes I.J2000J2000GALAXYDWARF SPHEROIDALQSOThe coordinates are for a QSO behind the dwarf spheroidal galaxy Bootes I.J2000J2000The scheduling data was generated by CASM 19.3.CASM was run in Phase II mode./private/var/folders/sg/sgF9tEWzGJKpv2rGmZkht++++TI/-Tmp-/OPVisit8300519645833048844.xmlThe first-epoch observation of this field, data sets ib5i08voq to ib5i08wfq, have an average PA_V3 = 122.8860 degrees. Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of 122.8860+180 = 302.8860 degrees. We allow a range of 0.1 degree so that objects are shifted by no more than +-2 pixels in the corner of the chip.(Tic-Visit
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)true30/Users/pryor/Documents/OP-cache/prop12319-3rdsubmission-v02.xmlThe scheduling data was generated by CASM 19.3.CASM was run in Phase II mode.The first-epoch observations of this field, data set ib5i09e5q - ib5i09ewq, have PA_V3 = 294.1234 degrees.
Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of
294.1234-180.0 = 114.1234 degrees. I allow a range of 0.1 degrees so that objects are shifted by no more
than +-2 pixels in the corners of the chip.
The visit has been modified to use LINE10 charge injection. The exposures have been shortened by 4 or 5 sec
to fit the orbits.1307290946000114.17340000000002(Tic-Visit
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Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of
120.8367+180.0 = 300.8367 degrees. I allow a range of 0.1 degrees so that objects are shifted by no more
than +-2 pixels in the corners of the chip.1295553841000300.7867(Tic-Visit
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