The role of E+A and post-starburst galaxies - I. Models and model results

Falkenberg, M. A.; Kotulla, Ralf; Fritze, U.

doi:10.1111/j.1365-2966.2009.14416.x

Cited by 23 publications

(36 citation statements)

References 57 publications

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“…To do so, we model SFHs of a post-starburst as a superposition of an old stellar population initially starting to form at time t = 0 and following a delayed exponential SFH of the form ψ ∝ t exp(−t/τ 1 ) with e-folding time τ 1 = 1 Gyr (cf. Kriek et al 2011) plus a young stellar population formed in a recent burst at t = 12.5 Gyr (z ∼ 0.1) with exponentially declining SFH, ψ ∝ exp(−t/τ 2 ) and τ 2 = 0.1 Gyr (see Kaviraj et al 2007;Falkenberg et al 2009). The SSP models assume Chabrier (2003) initial mass function, a solar metallicity for SFH before the recent burst, and 2.5 solar metallicity for the recent burst.…”

Section: Stellar Population Modelingmentioning

confidence: 99%

“…Kriek et al 2011) and a young stellar population formed in a recent burst at t = 12.5 Gyr (z ∼ 0.1) with exponentially declining SFH, ψ ∝ exp(−t/τ 2 ), of τ 2 = 0.1 Gyr (cf. Kaviraj et al 2007;Falkenberg et al 2009). Because of the burst mass-age degeneracy, the ages of the poststarbursts depends on the decay timescale τ 2 we assumed.…”

Section: Appendix B Details Of Stellar Population Modelingmentioning

confidence: 99%

“…Using galaxy merger simulations, Snyder et al (2011) have constrained the typical K+A lifetime of merger-induced poststarbursts to be 0.1-0.3 Gyr (see Falkenberg et al 2009;Wild et al 2009). They find that the presence of AGN makes almost no difference to the evolution of the post-merger spectrum in their simulation without diffuse dust.…”

Section: Introductionmentioning

confidence: 99%

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From Starburst to Quiescence: Testing Active Galactic Nucleus Feedback in Rapidly Quenching Post-Starburst Galaxies

Yesuf

Faber

Trump

et al. 2014

ApJ

121

151

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Post-starbursts are galaxies in transition from the blue cloud to the red sequence. Although they are rare today, integrated over time they may be an important pathway to the red sequence. This work uses Sloan Digital Sky Survey, the Galaxy Evolution Explorer, and Wide-field Infrared Survey Explorer observations to identify the evolutionary sequence from starbursts to fully quenched post-starbursts (QPSBs) in the narrow mass range log M(M ) = 10.3-10.7, and identifies "transiting" post-starbursts (TPSBs) which are intermediate between these two populations. In this mass range, ∼0.3% of galaxies are starbursts, ∼0.1% are QPSBs, and ∼0.5% are the transiting types in between. The TPSBs have stellar properties that are predicted for fast-quenching starbursts and morphological characteristics that are already typical of early-type galaxies. The active galactic nucleus (AGN) fraction, as estimated from optical line ratios, of these post-starbursts is about three times higher ( 36% ± 8%) than that of normal star forming galaxies of the same mass, but there is a significant delay between the starburst phase and the peak of nuclear optical AGN activity (median age difference of 200 ± 100 Myr), in agreement with previous studies. The time delay is inferred by comparing the broadband near-NUV-to-optical photometry with stellar population synthesis models. We also find that starbursts and post-starbursts are significantly more dust obscured than normal star forming galaxies in the same mass range. About 20% of the starbursts and 15% of the TPSBs can be classified as "dust-obscured galaxies" (DOGs), with a near-UV-to-mid-IR flux ratio of 900, while only 0.8% of normal galaxies are DOGs. The time delay between the starburst phase and AGN activity suggests that AGNs do not play a primary role in the original quenching of starbursts but may be responsible for quenching later low-level star formation by removing gas and dust during the post-starburst phase.

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Section: Stellar Population Modelingmentioning

confidence: 99%

Section: Appendix B Details Of Stellar Population Modelingmentioning

confidence: 99%

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From Starburst to Quiescence: Testing Active Galactic Nucleus Feedback in Rapidly Quenching Post-Starburst Galaxies

Yesuf

Faber

Trump

et al. 2014

ApJ

121

151

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“…Major gas-rich mergers are a possible evolutionary mechanism linking compact E+As and compact quiescent galaxies. This scenario can be examined in more detail by combining state-of-the-art hydrodynamical models (e.g., Cox et al 2006) with simple stellar population synthesis techniques (e.g., Falkenberg et al 2009). The constraints and formation scenarios for compact quiescent galaxies may also be investigated with large-scale cosmological simulations (e.g., Wellons et al 2015).…”

Section: Conclusion and Future Prospectsmentioning

confidence: 99%

COMPACT E+A GALAXIES AS A PROGENITOR OF MASSIVE COMPACT QUIESCENT GALAXIES AT 0.2 < z < 0.8

Zahid

Hochmuth

Geller

et al. 2016

ApJ

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We search the Sloan Digital Sky Survey and the Baryon Oscillation Sky Survey to identify ∼ 5500 massive compact quiescent galaxy candidates at 0.2 < z < 0.8. We robustly classify a subsample of 438 E+A galaxies based on their spectral properties and make this catalog publicly available. We examine sizes, stellar population ages and kinematics of galaxies in the sample and show that the physical properties of compact E+A galaxies suggest that they are a progenitor of massive compact quiescent galaxies. Thus, two classes of objects−compact E+A and compact quiescent galaxies−may be linked by a common formation scenario. The typical stellar population age of compact E+A galaxies is < 1 Gyr. The existence of compact E+A galaxies with young stellar populations at 0.2 < z < 0.8 means that some compact quiescent galaxies first appear at intermediate redshifts. We derive a lower limit for the number density of compact E+A galaxies. Assuming passive evolution, we convert this number density into an appearance rate of new compact quiescent galaxies at 0.2 < z < 0.8. The lower limit number density of compact quiescent galaxies which may appear at z < 0.8 is comparable to the lower limit of the total number density of compact quiescent galaxies at these intermediate redshifts. Thus, a substantial fraction of the z < 0.8 massive compact quiescent galaxy population may descend from compact E+A galaxies at intermediate redshifts.

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“…At some time during the post-starburst phase and through the combined efforts of (i) large scale gravitational torques and (ii) a series of small scale internal instabilities, the cold gas can loose ∼99.99% of its angular momentum and finally fuel a quasar for a time even shorter than its journey to the supermassive black hole (for observational studies of PSQs see Cales et al 2011Cales et al , 2013. The quasar phase (∼10 7−8 yr) is short in comparison to the lifetime of post-starburst stellar populations (0.3-3 Gyr, Falkenberg, Kotulla & Fritze 2009;Wild et al 2009). (7) Eventually after a couple of billion years (Gyr), a spheroidal galaxy emerges with properties that match those of local ellipticals.…”

Section: Merger Driven Nuclear Activitymentioning

confidence: 99%

Post-starburst quasars: bridging the gap between post-starburst galaxies and quasars

Cales

Brotherton

2015

Monthly Notices of the Royal Astronomical Society

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In order to better understand the nature of post-starburst quasars (PSQs) in the context of galaxy evolution, we compare their properties to those of post-starburst galaxies and quasars from appropriately selected samples possessing similar redshift (z ∼ 0.3), luminosity (M r ∼ −23), and data quality. We consider morphologies, spectral features, and derived physical properties of the stellar populations and central supermassive black hole. PSQs themselves come in two types: the more luminous AGNs with more luminous post-starburst stellar populations hosted by elliptical galaxies, some which are clearly merger products, and the less luminous systems existing within relatively undisturbed spiral galaxies and possessing signs of a more extended period of star formation. Post-starburst galaxies (PSQs) have elliptical and disturbed/postmerger morphologies similar to those of the more luminous PSQs, display similar spectral properties, but also can have younger stellar populations for a given starburst mass. Quasars at similar redshifts and luminosities around the Seyfert/quasar transition possess similar AGN characteristics, in terms of black hole mass and accretion rate, compared with those of PSQs, but do not appear to be hosted by galaxies with significant post-starburst populations. Recent studies of more luminous quasars find hosts consistent with those of our luminous PSQs, suggesting that these PSQs may be in transition between post-starburst galaxies and a more luminous quasar stage when the post-starburst stellar population remains dominant. The lower luminosity PSQs appear to differ from lower luminosity quasars (Seyfert galaxies) in terms of more significant star formation in their past.

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The role of E+A and post-starburst galaxies - I. Models and model results

Cited by 23 publications

References 57 publications

From Starburst to Quiescence: Testing Active Galactic Nucleus Feedback in Rapidly Quenching Post-Starburst Galaxies

From Starburst to Quiescence: Testing Active Galactic Nucleus Feedback in Rapidly Quenching Post-Starburst Galaxies

COMPACT E+A GALAXIES AS A PROGENITOR OF MASSIVE COMPACT QUIESCENT GALAXIES AT 0.2 < z < 0.8

Post-starburst quasars: bridging the gap between post-starburst galaxies and quasars

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