Quiescent galaxies cluster more strongly than star-forming ones by 0.5-1 dex after halo-mass matching, with one-halo conformity up to z~2 that disappears at higher redshifts.
CANDELS Multi-wavelength Catalogs: Source Detection and Photometry in the GOODS-South Field
4 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We present a UV-to-mid infrared multi-wavelength catalog in the CANDELS/GOODS-S field, combining the newly obtained CANDELS HST/WFC3 F105W, F125W, and F160W data with existing public data. The catalog is based on source detection in the WFC3 F160W band. The F160W mosaic includes the data from CANDELS deep and wide observations as well as previous ERS and HUDF09 programs. The mosaic reaches a 5$\sigma$ limiting depth (within an aperture of radius 0.17 arcsec) of 27.4, 28.2, and 29.7 AB for CANDELS wide, deep, and HUDF regions, respectively. The catalog contains 34930 sources with the representative 50% completeness reaching 25.9, 26.6, and 28.1 AB in the F160W band for the three regions. In addition to WFC3 bands, the catalog also includes data from UV (U-band from both CTIO/MOSAIC and VLT/VIMOS), optical (HST/ACS F435W, F606W, F775W, F814W, and F850LP), and infrared (HST/WFC3 F098M, VLT/ISAAC Ks, VLT/HAWK-I Ks, and Spitzer/IRAC 3.6, 4.5, 5.8, 8.0 $\mu$m) observations. The catalog is validated via stellar colors, comparison with other published catalogs, zeropoint offsets determined from the best-fit templates of the spectral energy distribution of spectroscopically observed objects, and the accuracy of photometric redshifts. The catalog is able to detect unreddened star-forming (passive) galaxies with stellar mass of 10^{10}M_\odot at a 50% completeness level to z$\sim$3.4 (2.8), 4.6 (3.2), and 7.0 (4.2) in the three regions. As an example of application, the catalog is used to select both star-forming and passive galaxies at z$\sim$2--4 via the Balmer break. It is also used to study the color--magnitude diagram of galaxies at 0<z<4.
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TNG100 and EAGLE hydrodynamical simulations underproduce faint compact galaxies at z>3 relative to CANDELS observations even after forward modeling and completeness corrections, with the mismatch linked to both detection effects and simulation physics.
JWST observations show larger average rest-UV than rest-optical sizes in z=1.5-3 galaxies, supporting inside-out disk formation after dust correction.
Mock CSST images yield 95% completeness limits of 26.3-28.5 mag for point sources and 24.4-27.1 mag for galaxies, with fainter objects showing systematic overestimates in magnitude, size, and surface brightness and underestimates in Sersic index and axis ratio.
citing papers explorer
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COSMOS-Web: does halo mass alone shape the clustering of star-forming and quiescent galaxies?
Quiescent galaxies cluster more strongly than star-forming ones by 0.5-1 dex after halo-mass matching, with one-halo conformity up to z~2 that disappears at higher redshifts.
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Probing the faint end of simulated galaxy counts at z>3
TNG100 and EAGLE hydrodynamical simulations underproduce faint compact galaxies at z>3 relative to CANDELS observations even after forward modeling and completeness corrections, with the mismatch linked to both detection effects and simulation physics.
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Quantifying the inside-out formation of disk galaxies at $1.5 \le z \le 3.0$
JWST observations show larger average rest-UV than rest-optical sizes in z=1.5-3 galaxies, supporting inside-out disk formation after dust correction.
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CSST Preparations: Galaxy Completeness and S\'ersic Profile Fitting across the Wide, Deep, and Extreme Fields
Mock CSST images yield 95% completeness limits of 26.3-28.5 mag for point sources and 24.4-27.1 mag for galaxies, with fainter objects showing systematic overestimates in magnitude, size, and surface brightness and underestimates in Sersic index and axis ratio.