Measuring the Hubble Flow Hubble Constant
We propose to use the Wide Field Camera 3 to extend our Cycle 15 program to phase
Cepheid variables in a spiral galaxy in the core of the Coma cluster. With an
investment of just 34 orbits, we will obtain a Cepheid distance to Coma accurate to 5%.
A direct application of the canonical primary distance indicator at 100 Mpc
will measure the far-field Hubble constant free of many of the systematic
uncertainties which beset current determinations relying on secondary indicators.
Establishing the far-field Hubble constant with Cepheids will provide one of the
strongest links in the extragalactic distance scale and will robustly calibrate the
fiducial fundamental plane of elliptical galaxies and type Ia supernovae.
From five epochs prior to ACS failure in Cycle 15, our WFC observations of NGC4921
in Coma produced at least 50 Cepheid candidates with S/N=5 to 10 or better and
periods of 40d to 70d. Efficient phasing of these and discovery of additional
Cepheids can be done with 12 epochs of observations with WFC3, optimally spaced for
long-period Cepheids. The better spatial sampling of WFC3 will improve on our
already robust detections and the F350LP filter allows a dramatic reduction in the
required observing time. We will supplement these data with two additional F606W
(wide-V) epochs to tie in with and leverage our Cycle 15 data to obtain accurate
mean magnitudes in standard bandpasses.
The primary science observations consist of a dozen two-orbit visits
using F350LP, supplemented by two five-orbit visits using F606W,
targeting the entire disk of NGC4921, a luminous spiral in the Coma
cluster. The F606W imaging is to tie the WFC3 photometry into the
Cycle 15 ACS imaging in the same band; it is desirable to execute each
F606W visit as close in time as possible to one of the F350LP visits,
and also to space the two F606W visits well apart in time, 45-65 days.
These data provide near optimum imaging for detection and phasing of
Cepheids with periods of 45 to 90 days. Each F350LP orbit will
consist of a dithered pair of exposures. Each F606W orbit will be a
single CRsplit exposure. The dither steps use the same postarg moves
from the dither-box sequence; for our science, it is preferable to
minimize the footprint of the gap rather than dither it away. Each
orbit has roughly 53 minutes of visibility or longer so each two-orbit
visit will total 5000s of open shutter time.
All available windows from mid-December to March with visibility
periods of 53 minutes or longer are acceptable (needed) for this
program. We have found it necessary to use three orients (290, 252.5,
and 222) to schedule the observations over the 90d window needed to
phase the longest period Cepheids. We have optimized the sampling
intervals for maximum detection and phasing efficiency for Cepheids
with periods of 45-90d; the success of the program is contingent upon
maintaining these spacings as closely as possible.
The 252.5 orient is the only one of the three orients which is
critical; this orient aligns the WFC3 CCD gap with the ACS CCD gap
from our Cycle 15 data, thereby maximizing our overlap between the two
instruments.
The parallel ACS imaging observing strategy is dictated by the Cepheid
observations. The time will be divided roughly equally among the
F475W, F606W, F814W, and G800L. Only the F606W exposures will be
CRsplit, in conjunction with the grism imaging, to obtain a clean
zero-order image. For the orient=222 parallels, we will use only
F475W and F814W to image the large elliptical galaxy in the field to
maximum depth in those two filters for SBF and GCLF studies.
COSMOLOGY
12
false
0.0
0.0
false
false
false
false
AVAILABLE
GALAXY
SPIRAL
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
GALAXY
SPIRAL
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
GALAXY
SPIRAL
This object was generated by the targetselector and retrieved from the SIMBAD database.
J2000
J2000
WFC3/UVIS
Imaging
No
No
F350LP
WFC3/UVIS
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
F814W
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Same orient constraint links visits (31 32 33 34)
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