The star formation histories of galaxies in the sloan digital sky survey

By B. Panter, Raul Jimenez, Alan Heavens, S. Charlot. 2006

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We present the results of a MOPED analysis of ∼3 × 10 5 galaxy spectra from the Sloan Digital Sky Survey Data Release 3 (SDSS DR3), with a number of improvements in data, modelling and analysis compared with our previous analysis of DR1. The improvements include: modelling the galaxies with theoretical models at a higher spectral resolution of 3 A, better calibrated data, an extended list of excluded emission lines and a wider range of dust models. We present new estimates of the cosmic star formation rate (SFR), the evolution of stellar mass density and the stellar mass function from the fossil record. In contrast to our earlier work the results show no conclusive peak in the SFR out to a redshift around 2 but continue to show conclusive evidence for ‘downsizing’ in the SDSS fossil record. The star formation history is now in good agreement with more traditional instantaneous measures. The galaxy stellar mass function is determined over five decades of mass, and an updated estimate of the current stellar mass density is presented. We also investigate the systematic effects of changes in the stellar population modelling, the spectral resolution, dust modelling, sky lines, spectral resolution and the change of data set. We find that the main changes in the results are due to the improvements in the calibration of the SDSS data, changes in the initial mass function and the theoretical models

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7eec744a43d8320710b325d1fc75c3598a946482

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Citations in the corpus

The evolution of stellar mass and the implied star formation history (2008, methodology): “Fossil History results are from Panter et al. (2007) (dark green).”
Generalized massive optimal data compression (2017, background): “…in astronomy and cosmology, including determining star formation histories of galaxies (Reichardt et al. 2001; Heavens et al. © 2018 The Authors 2004; Panter et al. 2007), cosmic microwave background data analysis (Gupta & Heavens 2002; Zablocki & Dodelson 2016), gravitational waves (Graff et al.…”
How to Measure Galaxy Star Formation Histories. II. Nonparametric Models (2018, background): “The SFHs of star-forming galaxies inform us about the timescales on which star formation rates change and the rate at which stellar mass is assembled on the starforming sequence (Gallazzi et al. 2005; Panter et al. 2007; Leitner 2012).”
The distribution of stellar mass in the low‐redshift Universe (2009, methodology): “There have been previous studies of the first of these statistics, the so-called mass function of galaxies (e.g. Cole et al. 2001; Bell et al. 2003; Wang et al. 2006; Panter et al. 2007; Baldry et al. 2008).”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “1 therein and Bell et al. 2003b; Drory et al. 2005; Borch et al. 2006; Fontana et al. 2006; Panter et al. 2007; Pérez-González et al. 2008b).”
Massive optimal data compression and density estimation for scalable, likelihood-free inference in cosmology (2018, methodology): “…used in astronomy and cosmology, with applications spanning determining galaxy star formation histories (Reichardt et al. 2001; Heavens et al. 2004; Panter et al. 2007), CMB data analysis (Gupta & Heavens 2002; Zablocki & Dodelson 2016), gravitational waves (Graff et al. 2011), transient detection…”
A census of metals and baryons in stars in the local universe (2007, methodology): “…et al. (2001), (3) Fukugita et al. (1998) from the compilation of Pagel (2002), (4) Glazebrook et al. (2003), (5) Bell et al. (2003), (6) Rudnick et al. (2003), (7) Rudnick et al. (2006), (8) Panter et al. (2007), (9) Driver et al. (2007a), (10) Driver et al. (2007b), (11) Shankar et al. (2006).”
THE MAJOR AND MINOR GALAXY MERGER RATES AT z < 1.5 (2011, background): “St09 adopts the sub-halo mass - stellar mass matching relationship from Conroy & Wechsler (2009), based upon the observed stellar mass functions at 0 < z < 2 (Bell et al. 2003, Panter et al. 2007, Dory et al. 2005, Borsch et al. 2006, Pérez-González et al. 2008, Fontana et al. 2006).”
Recovering galaxy star formation and metallicity histories from spectra using VESPA (2007, background): “The effect of the choice of modelling should not be overlooked, and we refer the reader to a discussion in Section 4.5 of Panter et al. (2007), where these issues are discussed.”
The star formation history of CALIFA galaxies: Radial structures (2013, methodology): “…the paper by Bruzual & Charlot (2003), and was one of the main tools employed in the mining of the SDSS spectroscopic database, leading to the derivation of physical properties and SFHs of galaxies (e.g.; Panter et al. 2003, 2007; Mateus et al. 2007; Vale Asari et al. 2009; Tojeiro et al. 2009).”
A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4 (2010, background): “Panter et al. (2007) found a similar difference between Calzetti et al. and models based on extinction curves from the Small and Large Magellanic Clouds.”
The Star Formation History of the Universe as Revealed by Deep Radio Observations (2008, methodology): “Many authors have observed the evolution of the distribution of star formation moving high mass galaxies at high redshift to lower mass galaxies at lower redshifts (e.g. Cowie et al. 1996; Panter et al. 2004; Juneau et al. 2005; Panter et al. 2007; Noeske et al. 2007).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, methodology): “More examples of the use of PCA and other sophisticated techniques for extraction of information about the stellar content and star-formation history from the SDSS galaxy spectra include Panter et al. (2003, 2007), Cid Fernandes et al. (2005), and Yip et al. (2004).”
The many manifestations of downsizing: hierarchical galaxy formation models confront observations (2009, methodology): “When high signal-to-noise ratio spectroscopy is available, galaxy stellar masses can be estimated by comparison of the observed spectra with theoretical SEDs (e.g. Panter et al. 2007 for Sloan Digital Sky Survey (SDSS) data).”
Environment and self-regulation in galaxy formation (2009, background): “Note that the latter is a universal characteristic of galaxy formation and is not restricted to early-types (Gavazzi et al. 2002; Heavens et al. 2004; Cid Fernandes et al. 2007; Panter et al. 2007).”
Erratum: Recovering galaxy stellar population properties from broad-band spectral energy distribution fitting (2012, methodology): “…in which population parameters are extracted by fitting the full available spectrum (Heavens et al. 2000; Cid Fernandes et al. 2004; Ocvirk et al. 2006; Panter et al. 2007; Tojeiro et al. 2007, 2009; Chen et al. 2012) and which also requires high quality and high S/N spectra in order to succeed.”
Inferring the star formation histories of massive quiescent galaxies with bagpipes: evidence for multiple quenching mechanisms (2017, background): “Question (i) has been studied by extracting the star formation histories (SFHs) of local galaxies from the fossil records imprinted in their spectra (e.g. Heavens et al. 2004; Panter et al. 2007; Thomas et al. 2010; Carson &Nichol 2010; Citro et al. 2016).”