Proper Motion Survey of Classical and SDSS Local Group Dwarf Galaxies
Using 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.
RESOLVED STELLAR POPULATIONS
12
false
0.0
0.0
false
false
false
true
SUPPORTED
GALAXY
DWARF SPHEROIDAL
QUASAR
The target is a QSO behind the dwarf spheroidal galaxy Ursa Majoris I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QUASAR
The coordinates are for a QSO behind the dwarf spheroidal galaxy Ursa Majoris I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QUASAR
The coordinates are for a QSO behind the dwarf spheroidal galaxy Leo II.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Leo II.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QUASAR
The coordinates are for a QSO behind the dwarf spheroidal galaxy Leo IV.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Leo IV.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy LeoIV.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Coma Bernices.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Coma Berenices.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Canes Venatici II.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Canes Venatici I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Canes Venatici I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Canes Venatici I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Canes Venatici I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Bootes I.
J2000
J2000
GALAXY
DWARF SPHEROIDAL
QSO
The coordinates are for a QSO behind the dwarf spheroidal galaxy Bootes I.
J2000
J2000
WFC3/UVIS
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WFC3/UVIS
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No
F350LP
WFC3/UVIS
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No
F350LP
WFC3/UVIS
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No
F350LP
WFC3/UVIS
Imaging
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No
F350LP
WFC3/UVIS
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No
F350LP
WFC3/UVIS
Imaging
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No
F350LP
WFC3/UVIS
Imaging
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No
F350LP
WFC3/UVIS
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No
F350LP
WFC3/UVIS
Imaging
No
No
F350LP
WFC3/UVIS
Imaging
No
No
F350LP
WFC3/UVIS
Imaging
No
No
F350LP
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true
3
3
The scheduling data was generated by CASM 20.0.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i09e5q to ib5i09ewq, have an average PA_V3 = 294.1234 degrees. Since U3 = -V3, having the same orientation for the third-epoch images requires an orientation of 294.1234-180 = 114.1234 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
1336867232000
114.17340000000002
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true
3
3
The scheduling data was generated by CASM 20.0.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i10w2q to ib5i10wzq, have an average PA_V3 = 292.0981 degrees. Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of 292.0981-180 = 112.0981 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
1339490116000
112.1481
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true
3
3
The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i11ejq to ib5i11f1q, have an average PA_V3 = 106.4912 degrees. Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of 106.4912+180 = 286.4912 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
(Tic-Visit
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)
true
4
4
The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i12anq to ib5i12c2q, have an average PA_V3 = 82.2122 degrees. Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of 82.2122+180 = 262.2122 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
(Tic-Visit
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)
true
3
3
The scheduling data was generated by CASM 20.0.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i13ffq to ib5i13h3q, have an average PA_V3 = 283.9966 degrees. Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of 283.9966-180 = 103.9966 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
1340360805000
104.04660000000001
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)
true
3
3
The scheduling data was generated by CASM 20.0.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i14r4q to ib5i14tkq, have an average PA_V3 = 285.4190 degrees. Since U3 = -V3, having the same orientation for the second-epoch images requires an orientation of 285.4190-180 = 105.4190 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
1339420403000
105.46900000000011
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true
3
3
The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i15kwq to ib5i15m0q, have an average PA_V3 = 100.3617 degrees. Since U3 = -V3, having the same orientation for the third-epoch images requires an orientation of 100.3617+180 = 280.3617 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
(Tic-Visit
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true
3
3
The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
The first-epoch observations of this field, data sets ib5i16trq to ib5i16uoq, have an average PA_V3 = 120.8367 degrees. Since U3 = -V3, having the same orientation for the third-epoch images requires an orientation of 120.8367+180 = 300.8367 degrees. We allow a range of 0.1 degrees so that objects are shifted by no more than +-2 pixels in the corner of the chip.
(Tic-Visit
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true
3
3