STRUCTURAL PARAMETERS OF GALAXIES IN CANDELS

By A. van der Wel, E. Bell, B. Häußler, E. McGrath, Yu-Yen Chang, Yicheng Guo, Daniel H. McIntosh, Hans-Walter Rix, M. Barden, Edmond Cheung and 12 more. 2012

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We present global structural parameter measurements of 109,533 unique, HF160W-selected objects from the CANDELS multi-cycle treasury program. Sérsic model fits for these objects are produced with GALFIT in all available near-infrared filters (HF160W, JF125W and, for a subset, YF105W). The parameters of the best-fitting Sérsic models (total magnitude, half-light radius, Sérsic index, axis ratio, and position angle) are made public, along with newly constructed point-spread functions for each field and filter. Random uncertainties in the measured parameters are estimated for each individual object based on a comparison between multiple, independent measurements of the same set of objects. To quantify systematic uncertainties, we create a mosaic with simulated galaxy images with a realistic distribution of input parameters and then process and analyze the mosaic in an identical manner as the real data. We find that accurate and precise measurements—to 10% or better—of all structural parameters can typically be obtained for galaxies with HF160W < 23, with comparable fidelity for basic size and shape measurements for galaxies to HF160W ∼ 24.5.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8c2142ff5604e09ffdb9dd598ef9e8db9d42726e

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Citations in the corpus

FORMING COMPACT MASSIVE GALAXIES (2015, methodology): “Structural parameters of galaxies in the Skelton et al. catalogs were measured by van der Wel et al. (2014b), using the methodology described in van der Wel et al. (2012).”
GOODS-ALMA: 1.1 mm galaxy survey (2018, methodology): “To estimate the completeness, galaxies that do not have measured sizes in the H-band (van der Wel et al. 2012) are considered as point sources otherwise we use RcircALMA = R circ H /1.4 (see Sect.”
ZFIRE: THE KINEMATICS OF STAR-FORMING GALAXIES AS A FUNCTION OF ENVIRONMENT AT z ∼ 2 (2016, methodology): “Our constraints are adopted from the constraints in van der Wel et al. (2012), and our point-spread function is constructed by 3D-HST.”
Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies (2015, methodology): “…11 Shenyang Normal University 12 Centro de Astrobiologia, CSIC-INTA 13 Colby College mic time (Bouwens et al. 2010; Finkelstein et al. 2013; Oesch et al. 2014), and have made a pivotal contribution to the study of galaxy sizes and morphologies (e.g., van der Wel et al. 2012; Shibuya et al. 2015).”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, background): “Further details on the PSF models can be found in van der Wel et al. (2012).”
Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, background): “Constraining observations that relate galaxy stellar mass to its structural properties are the Sèrsic index n and the effective radius Reff , 9 both at z = 0 and at higher redshifts (see e.g., Bell et al. 2012; Patel et al. 2013; van der Wel et al. 2012).”
UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD (2015, methodology): “In addition, the NIR models were found to not accurately reproduce the PSF at intermediate radii compared to stars in CANDELS, thereby justifying a hybrid PSF over using a pure model PSF (van der Wel et al. 2012).”
MORPHOLOGIES OF ∼190,000 GALAXIES AT z = 0–10 REVEALED WITH HST LEGACY DATA. I. SIZE EVOLUTION (2015, methodology): “We also include the Poisson noise from the galaxy light to the sigma image (e.g., Hathi et al. 2009; van der Wel et al. 2012).”
A CANDELS–3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5 (2013, background): “For galaxies with semi-major axis lengths larger than 3 kpc (as measured with GALFIT by van der Wel et al. 2012), more than 75% shows a better match between Hα and the I band than between Hα and the H band.”
The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, methodology): “…sizes are available for 51 objects in our full SINS/zC-SINF sample and 29 of the AO targets; we use the measurements presented by Förster Schreiber et al. (2011a) and Tacchella et al. (2015b), as well as by van der Wel et al. (2012) for the other objects that fall within the CANDELS/3D-HST fields.”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, background): “This irregular morphology is also observed in some low-mass, high-z galaxies ofM∗ ≃ 109 M⊙ (van der Wel et al. 2012), although the observed distribution of galaxy shapes is quite broad.”
3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, positive): “Given this sensitivity to small shifts in size we argue that our measurements, which do not require systematic size corrections of more than a few percent (see Section 2.5 and van der Wel et al. (2012)), represent the size distribution with good ﬁdelity across the examined redshift range.”
CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD (2013, methodology): “Our F160W PSF is a hybrid of the empirical PSF from stacking stars and the simulated PSF from TinyTim (van der Wel et al. 2012).”
THE 3D-HST SURVEY: HUBBLE SPACE TELESCOPE WFC3/G141 GRISM SPECTRA, REDSHIFTS, AND EMISSION LINE MEASUREMENTS FOR ∼100,000 GALAXIES (2015, methodology): “The set of images, PSFs, and catalogs was used to measure structural parameters of the objects in the WFC3 and ACS bands, following the methodology of van der Wel et al. (2012).”
3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES (2014, methodology): “The set of images, PSFs, and catalogs is used to measure structural parameters of the objects in the WFC3 and ACS bands, following the methodology of van der Wel et al. (2012).”
THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, methodology): “In comparison, without the kinematic data a disk fraction is obtained for the resolved KMOS3D sample from the photometric data alone using singlecomponent Sérsic fits to the rest-optical photometry (van der Wel et al. 2012).”
Morphologies of z ∼ 0.7 AGN host galaxies in CANDELS: no trend of merger incidence with AGN luminosity (2014, background): “Further details on the PSF models can be found in van der Wel et al. (2012).”
BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “For a more detailed description of the used PSF, see van der Wel et al. (2012).”