Selection and Photometric Properties of K+A Galaxies

By A. D. Quintero, David W. Hogg, M. Blanton, David Schlegel, Daniel J. Eisenstein, James E. Gunn, J. Brinkmann, M. Fukugita, Karl Glazebrook, Tomotsugu Goto. 2003

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Two different simple measurements of galaxy star formation rate with different timescales are compared empirically on 156,395 fiber spectra of galaxies with r < 17.77 mag taken from the Sloan Digital Sky Survey in the redshift range 0.05 < z < 0.20: a ratio A/K found by fitting a linear sum of an average old stellar population spectrum (K) and average A star spectrum (A) to the galaxy spectrum, and the equivalent width (EW) of the Hα emission line. The two measures are strongly correlated, but there is a small, clearly separated population of outliers from the median correlation that display excess A/K relative to Hα EW. These "K+A" (or "E+A") galaxies must have dramatically decreased their star formation rates over the last ~1 Gyr. The K+A luminosity distribution is similar to that of the total galaxy population. The K+A population appears to be bulge-dominated, but bluer and with higher surface brightness than normal bulge-dominated galaxies; it appears that K+A galaxies will fade with time into normal bulge-dominated galaxies. The inferred rate density for K+A galaxy formation is ~10-4 h3 Mpc-3 Gyr-1 at redshift z ~ 0.1. These events are taking place in the field; the K+A galaxies found in this study do not primarily lie in the high-density environments or clusters typical of bulge-dominated populations.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Active Galactic Nuclei in the Sloan Digital Sky Survey. I. Sample Selection (2005, background): “One possible resolution would be to make sure that the PCA sample includes enough E+A galaxies, which contain young stellar populations and do not have emission lines (Goto et al. 2003; Quintero et al. 2004).”
THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, background): “These objects possess blue colors and strong Balmer absorption yet weak Hα, signifying recent quenching, and their Sérsic indices are high (Quintero et al. 2004; Yang et al. 2008).”
The Bimodal Galaxy Color Distribution: Dependence on Luminosity and Environment (2004, background): “…predicted to be in the transition phase is comparable to the fraction of spectroscopically identified post-starburst galaxies (Goto et al. 2003a; Quintero et al. 2004), and anemic (passively evolving) spirals (van den Bergh 1976; Goto et al. 2003b) which may be the signature of such…”
CAIRNS: The Cluster and Infall Region Nearby Survey. I. Redshifts and Mass Profiles (2003, result): “The frequency of E+As among bright galaxies in nearby clusters is therefore .0.1%, crudely consistent with other studies of local galaxies in all environments (Zabludoff et al. 1996; Quintero et al. 2004).”
Post-starburst galaxies: more than just an interesting curiosity (2008, methodology): “Classes of galaxies which could be transitioning between the blue and red sequences are ‘post-starburst (PSB)’ galaxies (e.g. Tran et al. 2004; Quintero et al. 2004; Le Borgne et al. 2006; Kaviraj et al. 2007) and ‘green valley’ galaxies (e.g. Martin et al. 2007).”
Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “…result for z ∼ 1) whereas only 4% of the blue cloud lie below the SF sequence (these may be post-starburst galaxies, those that exhibit no signs of ongoing star formation but experienced recent star formation within the last ∼Gyr - see for example, Dressler & Gunn 1983; Quintero et al. 2004).”
Passively Evolving Early-Type Galaxies at 1.4 ≲ z ≲ 2.5 in the Hubble Ultra Deep Field (2005, unknown): “This single object in the 1:4 < z < 2 redshift range corresponds, however, to a volume density that is 2 to 3 orders of magnitude higher than the local density of E+A galaxies above similar luminosities (Quintero et al. 2004).”
A LINK BETWEEN STAR FORMATION QUENCHING AND INNER STELLAR MASS DENSITY IN SLOAN DIGITAL SKY SURVEY CENTRAL GALAXIES (2013, background): “Post-starburst (or E+A) galaxies (Dressler & Gunn 1983; Quintero et al. 2004; Goto 2005) are rapidly quenched objects that likely underwent a recent merger-induced starburst (e.g., Hopkins et al. 2006; Snyder et al. 2011).”
Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey (2006, background): “Early types with central star formation activities have been studied and some of them are E + A galaxies (Goto et al. 2003c; Fukugita et al. 2004; Quintero et al. 2004; Goto 2005; Park & Choi 2005; Yamauchi & Goto 2005).”
266 E+A galaxies selected from the Sloan Digital Sky Survey Data Release 2: the origin of E+A galaxies (2005, result): “In the literature, there are some recent work which found consistent results with ours; Quintero et al. (2004) reported that K+A galaxies do not lie in high-density regions using a K/A star ratio to select ∼1000 K+A galaxies from the SDSS data (However, note that they did not apply constraints on…”
On the Origin of [O II] Emission in Red-Sequence and Poststarburst Galaxies (2005, methodology): “In the top panel of Figure 12,11 we reproduce Figure 3 of Quintero et al. (2004) with our ownmeasurements for all galaxies that arewithin 0:07 < z < 0:1 and have both [O ii] andH visible in their spectra.”
Physical properties and environments of nearby galaxies (2009, methodology): “These galaxies tend to be high in surface brightness and to be highly concentrated, yet blue (Norton et al. 2001; Quintero et al. 2004), with a strong possibility that as their stellar population fades they will become consistent with the red sequence, and become elliptical galaxies.”