Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate

Bell, Eric F.; Papovich, C.; Wolf, Christian; Floc’h, E. Le; Caldwell, J. A. R.; Barden, M.; Egami, Eiichi; McIntosh, Daniel H.; Meisenheimer, K.; Pérez‐González, Pablo G.; Rieke, G. H.; Rieke, M. J.; Rigby, J. Keith; Rix, Hans─Walter

doi:10.1086/429552

Cited by 482 publications

(589 citation statements)

References 96 publications

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“…However, we do not correct for this effect because these discrepancies are poorly constrained given that the FIR data do not probe the peak of the dust emission. We also note that this difference is less than the intrinsic uncertainty in individual star formation rate calibrations (e.g., Bell 2003;Bell et al 2005).…”

Section: Comparison To Literaturementioning

confidence: 81%

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THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Tomczak

Quadri

Tran

et al. 2016

ApJ

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320

492

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We explore star formation histories (SFHs) of galaxies based on the evolution of the star formation rate stellar mass relation (SFR-M * ). Using data from the FourStar Galaxy Evolution Survey (ZFOURGE) in combination with far-IR imaging from the Spitzer and Herschel observatories we measure the SFR-M * relation at 0.5 < z < 4. Similar to recent works we find that the average infrared spectral energy distributions of galaxies are roughly consistent with a single infrared template across a broad range of redshifts and stellar masses, with evidence for only weak deviations. We find that the SFR-M * relation is not consistent with a single power law of the form M SFR * µ a at any redshift; it has a power law slope of α ∼ 1 at low masses, and becomes shallower above a turnover mass (M 0 ) that ranges from 10 9.5 to 10 10.8 M e , with evidence that M 0 increases with redshift. We compare our measurements to results from state-of-the-art cosmological simulations, and find general agreement in the slope of the SFR-M * relation albeit with systematic offsets. We use the evolving SFR-M * sequence to generate SFHs, finding that typical SFRs of individual galaxies rise at early times and decline after reaching a peak. This peak occurs earlier for more massive galaxies. We integrate these SFHs to generate mass growth histories and compare to the implied mass growth from the evolution of the stellar mass function (SMF). We find that these two estimates are in broad qualitative agreement, but that there is room for improvement at a more detailed level. At early times the SFHs suggest mass growth rates that are as much as 10× higher than inferred from the SMF. However, at later times the SFHs under-predict the inferred evolution, as is expected in the case of additional growth due to mergers.

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Section: Comparison To Literaturementioning

confidence: 81%

“…Thus by adding its contribution to that of the unobscured UV luminosity (L UV ) the total SFR for galaxies can be calculated. We use the conversion from Bell et al (2005) scaled to a Chabrier (2003) IMF to derive SFRs from our data:…”

Section: Star Formation Rate Measurementsmentioning

confidence: 99%

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Tomczak

Quadri

Tran

et al. 2016

ApJ

Self Cite

320

492

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“…For the latter, we adopt a relation similar to that proposed by Bell et al (2005) and adjusted for a Chabrier (2003) IMF:…”

Section: The Other Physical Parameters and Luminositiesmentioning

confidence: 99%

Encoding of the infrared excess in theNUVrKcolor diagram for star-forming galaxies

Arnouts

Floc’h

Chevallard

et al. 2013

A&A

190

250

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We present an empirical method of assessing the star formation rate (SFR) of star-forming galaxies based on their locations in the rest-frame color-color diagram (NUV − r) vs. (r − K). By using the Spitzer 24 µm sample in the COSMOS field (∼16 400 galaxies with 0.2 ≤ z ≤ 1.3) and a local GALEX-SDSS-SWIRE sample (∼700 galaxies with z ≤ 0.2), we show that the mean infrared excess IRX = L IR /L UV can be described by a single vector, NRK, that combines the two colors. The calibration between IRX and NRK allows us to recover the IR luminosity, L IR , with an accuracy of σ ∼ 0.21 for the COSMOS sample and 0.27 dex for the local one. The SFRs derived with this method agree with the ones based on the observed (UV+IR) luminosities and on the spectral energy distribution (SED) fitting for the vast majority (∼85%) of the star-forming population. Thanks to a library of model galaxy SEDs with realistic prescriptions for the star formation history, we show that we need to include a two-component dust model (i.e., birth clouds and diffuse ISM) and a full distribution of galaxy inclinations in order to reproduce the behavior of the IRX stripes in the NUVrK diagram. In conclusion, the NRK method, based only on the rest-frame UV/optical colors available in most of the extragalactic fields, offers a simple alternative of assessing the SFR of star-forming galaxies in the absence of far-IR or spectral diagnostic observations.

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“…Bell et al 2005;Papovich et al 2007;Barro et al 2011) of and 3000 Å, L UV , is estimated as 1.5νf ν, 2800 , where f ν, 2800 is the rest-frame luminosity at 2800 Å. For further details of this process, see Taylor et al (in preparation).…”

Section: Long-duration Uv Continuum + Tir Luminosity Sfrmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

Davies

Robotham

Driver

et al. 2015

Mon. Not. R. Astron. Soc.

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The modification of star formation (SF) in galaxy interactions is a complex process, with SF observed to be both enhanced in major mergers and suppressed in minor pair interactions. Such changes likely to arise on short timescales and be directly related to the galaxy-galaxy interaction time. Here we investigate the link between dynamical phase and direct measures of SF on different timescales for pair galaxies, targeting numerous star-formation rate (SFR) indicators and comparing to pair separation, individual galaxy mass and pair mass ratio. We split our sample into the higher (primary) and lower (secondary) mass galaxies in each pair and find that SF is indeed enhanced in all primary galaxies but suppressed in secondaries of minor mergers. We find that changes in SF of primaries is consistent in both major and minor mergers, suggesting that SF in the more massive galaxy is agnostic to pair mass ratio.We also find that SF is enhanced/suppressed more strongly for short-time duration SFR indicators (e.g. Hα), highlighting recent changes to SF in these galaxies, which are likely to be induced by the interaction. We propose a scenario where the lower mass galaxy has its SF suppressed by gas heating or stripping, while the higher mass galaxy has its SF enhanced, potentially by tidal gas turbulence and shocks. This is consistent with the seemingly contradictory observations for both SF suppression and enhancement in close pairs.

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Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate

Cited by 482 publications

References 96 publications

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Encoding of the infrared excess in theNUVrKcolor diagram for star-forming galaxies

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

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Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate

Cited by 482 publications

References 96 publications

THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

Encoding of the infrared excess in theNUVrKcolor diagram for star-forming galaxies

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

Contact Info

Product

Resources

About

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*

THE SFR–M_* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4*