3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES

By R. Skelton, K. Whitaker, Ivelina G. Momcheva, G. Brammer, P. V. van Dokkum, I. Labbé, M. Franx, A. van der Wel, R. Bezanson, E. da Cunha and 17 more. 2014

772 citations recorded by the source corpus.

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).

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/531e8eff28e314be0da8f523405bd74201451861

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. P. V. van Dokkum
6. C. Conroy
7. A. Dekel
8. M. Franx

In Electrical and Electronic Engineering

1. Richard S. Ellis
2. R. Bouwens
3. J. Dunlop
4. D. Stark
5. P. Oesch
6. G. Illingworth
7. M. Ouchi
8. R. McLure

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. P. V. van Dokkum
4. C. Conroy
5. R. Dav'e
6. M. Franx
7. R. Somerville
8. A. Dekel

Citations in the corpus

• COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, methodology): “…al. 2007, 2009), including the recent CANDELS J- and Hband HST imaging (Grogin et al. 2011, Koekemoer et al. 2011) and 3D-HST grism spectroscopy (Brammer et al. 2012, Skelton et al. 2014), as well as D3a (Kong et al. 2006) and the BX/BM samples of Steidel et al. (2004) and Adelberger et al. (2004).”
• THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR ∼1500 H-SELECTED GALAXIES AT 1.37 ≤ z ≤ 3.8 ?> (2014, methodology): “The parent catalogs are the trimmed versions of the 3D-HST catalogs by Skelton et al. (2014), by imposing the redshift and magnitude criteria for each redshift interval.”
• PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, methodology): “…et al. 2004, Berta et al. 2010) and COSMOS fields (Scoville et al. 2007, Lilly et al. 2007, 2009), including the recent CANDELS J- and H-band HST imaging (Grogin et al. 2011, Koekemoer et al. 2011) and 3D-HST grism spectroscopy (Brammer et al. 2012, Skelton et al. 2014, Momcheva et al. 2016).”
• A deep ALMA image of the Hubble Ultra Deep Field (2016, methodology): “…grism spectroscopy has also made an important contribution, with a combination of the 3D-HST programme, and CANDELS supernovae grism follow-up observations delivering ' 1000 redshifts in the GOODS-South field (Brammer et al. 2012; Skelton et al. 2014; Morris et al. 2015; Momcheva et al. 2016).”
• Lyα EMISSION FROM A LUMINOUS z = 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION (2015, methodology): “The absolute calibration for each night was derived by comparing the spectroscopic magnitude of the stars on the slitmask with photometric measures in the J-band obtained from the 3D-HST catalog (Brammer et al. 2012; Skelton et al. 2014).”
• FORMING COMPACT MASSIVE GALAXIES (2015, methodology): “Finally, stellar masses were determined from fits of stellar population synthesis models to the 0.3µm – 8µm photometry, as described in Skelton et al. (2014).”
• (Star)bursts of FIRE: observational signatures of bursty star formation in galaxies (2015, methodology): “Using data from this survey and ancillary 3D-HST UV photometry (Skelton et al. 2014), the SFR–”
• THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, methodology): “Survey design & sample selection We select KMOS3D targets from the 3D-HST Treasury Survey (Brammer et al. 2012; Skelton et al. 2014) in the fields accessible from the VLT (GOODS-S, COSMOS, UDS).”
• THE MOSDEF SURVEY: EXCITATION PROPERTIES OF z ∼ 2.3 STAR-FORMING GALAXIES (2014, methodology): “Stellar masses (M∗) were estimated using the preexisting multi-wavelength photometry assembled by the 3D-HST team (Skelton et al. 2014), with spectroscopic redshifts fixed by our MOSFIRE measurements.”
• JADES Initial Data Release for the Hubble Ultra Deep Field: Revealing the Faint Infrared Sky with Deep JWST NIRCam Imaging (2023, methodology): “Pixel correlations are dif fi cult to avoid on projected and recombined images, but as judged by these scalings, the overall level of correlated noise present in our images is comparable to or better than other space-based data sets ( e.g., Skelton et al. 2014; Whitaker et al. 2019 ) .”
• THE MOSDEF SURVEY: MASS, METALLICITY, AND STAR-FORMATION RATE AT z ∼ 2.3 (2014, methodology): “Stellar masses were estimated using the MOSDEF redshifts and pre-existing photometric data assembled by the 3D-HST team (Skelton et al. 2014).”
• A Census of Photometrically Selected Little Red Dots at 4 < z < 9 in JWST Blank Fields (2024, methodology): “We generate our F444W PSFs empirically for each field by following the methodology described in Skelton et al. (2014), Whitaker et al. (2019) and Weaver et al. (2023a).”
• ZFIRE: THE KINEMATICS OF STAR-FORMING GALAXIES AS A FUNCTION OF ENVIRONMENT AT z ∼ 2 (2016, methodology): “For details on the reduction of CANDELS imaging, see Skelton et al. (2014).”
• THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, methodology): “…the stellar population synthesis models of Conroy et al. (2009) with the SED-fitting code FAST (Kriek et al. 2009) using the measured MOSDEF spectroscopic redshifts and broadband photometric catalogs assembled by the 3D-HST team (Skelton et al. 2014) spanning observed optical to mid-infrared.”
• Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies (2018, methodology): “The photometry in these catalogs was assembled with the same tools and approaches, namely aperture photometry on residual images cleaned of neighboring sources (see Skelton et al. 2014; Straatman et al. 2016).”
• THE 3D-HST SURVEY: HUBBLE SPACE TELESCOPE WFC3/G141 GRISM SPECTRA, REDSHIFTS, AND EMISSION LINE MEASUREMENTS FOR ∼100,000 GALAXIES (2015, methodology): “The spectroscopic redshifts come from the entire CANDELS area (see Skelton et al. 2014), and are not limited to the area with grism coverage.”