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J/AJ/143/50 HST photometry of the globular cluster NGC 104 (Woodley+, 2012)
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Beginning of ReadMe :J/AJ/143/50 White dwarfs in 47 Tuc (NGC 104) with HST (Woodley+, 2012)
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The spectral energy distributions of white dwarfs in 47 Tucanae: the distance
to the cluster.
Woodley K.A., Goldsbury R., Kalirai J.S., Richer H.B., Tremblay P.-E.,
Anderson J., Bergeron P., Dotter A., Esteves L., Fahlman G.G.,
Hansen B.M.S., Heyl J., Hurley J., Rich R.M., Shara M.M., Stetson P.B.
<Astron. J., 143, 50 (2012)>
=2012AJ....143...50W
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ADC_Keywords: Clusters, globular ; Stars, white dwarf ; Photometry, HST
Effective temperatures
Keywords: globular clusters: individual (47 Tucanae) - stars: distances -
white dwarfs
Abstract:
We present a new distance determination to the Galactic globular
cluster 47 Tucanae (47 Tuc, NGC 104) by fitting the spectral energy
distributions of its white dwarfs (WDs) to pure hydrogen atmosphere WD
models. Our photometric data set is obtained from a 121-orbit Hubble
Space Telescope program using the Wide Field Camera 3 UVIS/IR
channels, capturing F390W, F606W, F110W, and F160W images. These
images cover more than 60 arcmin^2^ and extend over a radial range of
5-13.7arcmin (6.5-17.9pc) within the globular cluster. Using a
likelihood analysis, we obtain a best-fitting unreddened distance
modulus of (m-M)_o_=13.36+/-0.02+/-0.06 corresponding to a
distance of 4.69+/-0.04+/-0.13kpc, where the first error is random and
the second is systematic. We also search the WD photometry for
infrared excess in the F160W filter, indicative of low-mass
companions, and find no convincing cases within our sample.
Description:
We obtained HST images of the Galactic globular cluster 47 Tuc in
cycle 17 (GO-11677, PI: H. Richer) with the Advanced Camera for
Surveys (ACS) and WFC3. Our observational design and reduction are
discussed in detail in Kalirai et al. (2012AJ....143...11K).
Here we briefly review the WFC3 data set used in the present analysis:
we obtained 121 orbits covering >60arcmin^2^ and extending over 250deg
in azimuthal range of 47 Tuc. This covers a radial range of 5-13.7'
(6.5-17.9pc) within the globular cluster. For 61 orbits, we stared in
one field location in the cluster (stare field) obtaining 59 orbits of
IR images in F110W and F160W and 2 orbits of UVIS images in F390W and
F606W. We then swept out an arc around the cluster's center (swath
fields), using 5 orbits in each of our 12 additional fields, obtaining
F390W, F606W, F110W, and F160W images.