3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND S℡LAR MASSES. Skelton, R. E., Whitaker, K. E., Momcheva, I. G., Brammer, G. B., Dokkum, P. G. v., Labbé, I., Franx, M., Wel, A. v. d., Bezanson, R., Cunha, E. D., Fumagalli, M., Schreiber, N. F., Kriek, M., Leja, J., Lundgren, B. F., Magee, D., Marchesini, D., Maseda, M. V., Nelson, E. J., Oesch, P., Pacifici, C., Patel, S. G., Price, S., Rix, H., Tal, T., Wake, D. A., & Wuyts, S. The Astrophysical Journal Supplement Series, 214(2):24, October, 2014. ![3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND S℡LAR MASSES [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper doi abstract bibtex The 3D-HST and CANDELS programs have provided WFC3 and ACS spectroscopy and photometry over ≈900 arcmin2 in five fields: AEGIS, COSMOS, GOODS-North, GOODS-South, and the UKIDSS UDS field. All these fields have a wealth of publicly available imaging data sets in addition to the Hubble Space Telescope (HST) data, which makes it possible to construct the spectral energy distributions (SEDs) of objects over a wide wavelength range. In this paper we describe a photometric analysis of the CANDELS and 3D-HST HST imaging and the ancillary imaging data at wavelengths 0.3-8 μm. Objects were selected in the WFC3 near-IR bands, and their SEDs were determined by carefully taking the effects of the point-spread function in each observation into account. A total of 147 distinct imaging data sets were used in the analysis. The photometry is made available in the form of six catalogs: one for each field, as well as a master catalog containing all objects in the entire survey. We also provide derived data products: photometric redshifts, determined with the EAZY code, and stellar population parameters determined with the FAST code. We make all the imaging data that were used in the analysis available, including our reductions of the WFC3 imaging in all five fields. 3D-HST is a spectroscopic survey with the WFC3 and ACS grisms, and the photometric catalogs presented here constitute a necessary first step in the analysis of these grism data. All the data presented in this paper are available through the 3D-HST Web site (http://3dhst.research.yale.edu).
@article{skelton_3d-hst_2014,
title = {{3D}-{HST} {WFC3}-{SELECTED} {PHOTOMETRIC} {CATALOGS} {IN} {THE} {FIVE} {CANDELS}/{3D}-{HST} {FIELDS}: {PHOTOMETRY}, {PHOTOMETRIC} {REDSHIFTS}, {AND} {S}℡{LAR} {MASSES}},
volume = {214},
issn = {0067-0049},
shorttitle = {{3D}-{HST} {WFC3}-{SELECTED} {PHOTOMETRIC} {CATALOGS} {IN} {THE} {FIVE} {CANDELS}/{3D}-{HST} {FIELDS}},
url = {https://doi.org/10.1088%2F0067-0049%2F214%2F2%2F24},
doi = {10.1088/0067-0049/214/2/24},
abstract = {The 3D-HST and CANDELS programs have provided WFC3 and ACS spectroscopy and photometry over ≈900 arcmin2 in five fields: AEGIS, COSMOS, GOODS-North, GOODS-South, and the UKIDSS UDS field. All these fields have a wealth of publicly available imaging data sets in addition to the Hubble Space Telescope (HST) data, which makes it possible to construct the spectral energy distributions (SEDs) of objects over a wide wavelength range. In this paper we describe a photometric analysis of the CANDELS and 3D-HST HST imaging and the ancillary imaging data at wavelengths 0.3-8 μm. Objects were selected in the WFC3 near-IR bands, and their SEDs were determined by carefully taking the effects of the point-spread function in each observation into account. A total of 147 distinct imaging data sets were used in the analysis. The photometry is made available in the form of six catalogs: one for each field, as well as a master catalog containing all objects in the entire survey. We also provide derived data products: photometric redshifts, determined with the EAZY code, and stellar population parameters determined with the FAST code. We make all the imaging data that were used in the analysis available, including our reductions of the WFC3 imaging in all five fields. 3D-HST is a spectroscopic survey with the WFC3 and ACS grisms, and the photometric catalogs presented here constitute a necessary first step in the analysis of these grism data. All the data presented in this paper are available through the 3D-HST Web site (http://3dhst.research.yale.edu).},
language = {en},
number = {2},
urldate = {2019-08-06},
journal = {The Astrophysical Journal Supplement Series},
author = {Skelton, Rosalind E. and Whitaker, Katherine E. and Momcheva, Ivelina G. and Brammer, Gabriel B. and Dokkum, Pieter G. van and Labbé, Ivo and Franx, Marijn and Wel, Arjen van der and Bezanson, Rachel and Cunha, Elisabete Da and Fumagalli, Mattia and Schreiber, Natascha Förster and Kriek, Mariska and Leja, Joel and Lundgren, Britt F. and Magee, Daniel and Marchesini, Danilo and Maseda, Michael V. and Nelson, Erica J. and Oesch, Pascal and Pacifici, Camilla and Patel, Shannon G. and Price, Sedona and Rix, Hans-Walter and Tal, Tomer and Wake, David A. and Wuyts, Stijn},
month = oct,
year = {2014},
keywords = {catalogs, galaxies: evolution, galaxies: general, methods: data analysis, techniques: photometric},
pages = {24},
}
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