Erratum: Recovering galaxy stellar population properties from broad-band spectral energy distribution fitting

By J. Pforr, C. Maraston, Chiara Tonini Institute of Cosmology, Gravitation, Portsmouth, Uk, National Optical Astronomy Observatory, Tucson, Usa, Centre for Gravitational Astrophysics and 3 more. 2012

188 citations recorded by the source corpus.

This is an erratum to the paper entitled ‘Recovering galaxy stellar population properties from broad-band spectral energy distribution fitting’, published in MNRAS, 422, 3285 (2012).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e44e027b03db050bcc7f6dfaf48c0bf3cae9ff60

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Citations in the corpus

The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields (2015, background): “3.1, we have considered separately the classical exponential declining model, the exponentially increasing SFH (Maraston et al. 2010; Pforr et al. 2012) and the “delayed” SFH that increases at early ages and then shows a declining phase at later epochs.”
Galaxy Masses: A Review (2013, background): “Pforr et al. (2012) also show that - when the template star formation history matches the real one - as is the case for positive tau models for high-redshift galaxies (Maraston et al. 2010), the mass recovery from spectral fit is excellent and mostly independent of the waveband used in the fit.”
An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey (2018, unknown): “…uncertainty in stellar masses derived from SED-fitting codes (Papovich et al. 2001; Marchesini et al. 2009; Wuyts et al. 2009; Behroozi et al. 2010; Pforr et al. 2012; Conroy 2013; Mitchell et al. 2013; Leja et al. 2015, 2019; Mobasher et al. 2015; Santini et al. 2015; Tomczak et al. 2016; Carnall…”
How to Measure Galaxy Star Formation Histories. II. Nonparametric Models (2018, background): “The first is “outshining” (Papovich et al. 2001; Maraston et al. 2010; Pforr et al. 2012; Conroy 2013), whereby it is difficult to distinguish the presence of old, dim stars behind luminous young blue stars.”
Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe (2016, background): “SFH recovery is critical to accurately recover stellar masses (Lee et al. 2009; Maraston et al. 2010; Pforr et al. 2012), and simple exponentially declining SFHs fail to reproduce the mass function of galaxies at earlier epochs by several orders of magnitude (Wuyts et al. 2011a).”
Inferring the star formation histories of massive quiescent galaxies with bagpipes: evidence for multiple quenching mechanisms (2017, background): “…however Maraston et al. (2010) and Reddy et al. (2012) have shown by that it becomes less effective at higher redshifts, and Wuyts et al. (2011) and Pforr et al. (2012) have shown that the biases on the estimated SFH parameters (e.g. the ongoing SFR) are highly dependent on the permitted ranges of…”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, unknown): “In this section we quantify the degeneracies in those parameters (see also Pirzkal et al. 2012; Pforr et al. 2012) along with the modest constraints we obtain on them, assuming that MACS0647-JD is indeed at high redshift.”
A CANDELS–3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5 (2013, unknown): “The performance and limitations of broad-band SED modeling as a tool to infer stellar population properties have been abundantly tested on synthetic observations of simulated galaxies (Wuyts et al. 2009; Lee et al. 2009; Pforr et al. 2012; Mitchell et al. 2013).”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, background): “…a fixed IMF, uncertainties in the stellar evolution models used to infer stellar masses are ∼ 0.3 dex (e.g. Conroy et al. 2009; Behroozi et al. 2010; Pforr et al. 2012; Mitchell et al. 2013), there is perhaps little point in trying to improve the agreement between the models and the data further.”
AN ATLAS OF GALAXY SPECTRAL ENERGY DISTRIBUTIONS FROM THE ULTRAVIOLET TO THE MID-INFRARED (2013, background): “Unfortunately, SED models with a large number of free parameters cannot be expected to reproduce the SED of a galaxy with a complex star formation history when only limited photometry is available (e.g., Pforr et al. 2012).”
STELLAR MASSES FROM THE CANDELS SURVEY: THE GOODS-SOUTH AND UDS FIELDS (2014, result): “However, discrepant results were found by other groups (Maraston et al. 2010; Pforr et al. 2012), who reported an underestimation of the stellar mass when parameterizing the SFH as direct-τ models compared to the mass predicted by semianalytical models.”
A unified multiwavelength model of galaxy formation (2015, background): “All of these are cur- c© 0000 RAS, MNRAS000, 000–000 rently uncertain, as analysed in various papers (e.g. Conroy et al. 2009; Gallazzi & Bell 2009; Zibetti et al. 2009; Pforr et al. 2012; Mitchell et al. 2013).”
The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations (2015, methodology): “This precision is comparable to the systematic uncertainty associated with spectrophotometric techniques for inferring galaxy stellar masses, indicating that MNRAS 450, 1937–1961 (2015) a more precise reproduction of the GSMF may be unwarranted11 (e.g. Conroy et al. 2009; Pforr et al. 2012).”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, background): “For example, Pforr et al. (2012) find that unbiased stellar masses can only be recovered when the true star formation history (SFH) of a galaxy is known.”
A CATALOG OF BULGE, DISK, AND TOTAL STELLAR MASS ESTIMATES FOR THE SLOAN DIGITAL SKY SURVEY (2013, methodology): “…curves leads to variations in total mass of 0.1–0.2 dex depending on the wavelengths used in the SED fitting procedure (e.g., Marchesini et al. 2009; Ilbert et al. 2010; Swindle et al. 2011; Pforr et al. 2012); differences are typically largest when incorporating data which extend into the far-UV.”
Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, methodology): “Without a strong constraint on the dust attenuation, a degeneracy between the age of the old stellar population (which is directly linked to the stellar mass) and the attenuation appears (Pforr et al. 2012; Conroy 2013; Buat et al. 2014).”
Stellar masses of SDSS-III/BOSS galaxies at z ∼ 0.5 and constraints to galaxy formation models (2012, methodology): “These mock galaxies coincide with the mock star forming option as used in Pforr et al. (2012).”