Star Formation in AEGIS Field Galaxies since
                    <i>z</i>
                     = 1.1: Staged Galaxy Formation and a Model of Mass-dependent Gas Exhaustion

Noeske, K. G.; Faber, S. M.; Weiner, Benjamin J.; Koo, David C.; Primack, Joel R.; Dekel, Avishai; Papovich, C.; Conselice, Christopher J.; Floc’h, E. Le; Rieke, G. H.; Coil, Alison L.; Lotz, Jennifer M.; Somerville, Rachel S.; Bundy, Kevin

doi:10.1086/517927

Cited by 444 publications

(511 citation statements)

References 25 publications

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“…12), therefore the SFH of our objects has an influence on the dispersion of the SFR − M plot. This agrees with the conclusions of Davé (2008) and Noeske et al (2007b). The specific star formation rate (SSFR) defined as the ratio between SFR and M (e.g., Kennicutt et al 2005) is also commonly used to trace the SFH in galaxies.…”

Section: Star Formation Rate and Stellar Masssupporting

confidence: 87%

“…For star-forming galaxies a correlation is observed between SFR and M with a slope near to unity from z ∼ 0 to 2 and a scatter of 0.3 dex Elbaz et al 2007;Noeske et al 2007a). The slope and scatter are expected to be a direct reflection of the similarity in the shape of galaxy SFHs among various models and at various masses (Davé 2008;Noeske et al 2007b). It is worth noting that other z = 2 observations suggest a somewhat large scatter (Shapley et al 2005;Papovich et al 2006), so the observational picture is not entirely settled.…”

Section: Star Formation Rate and Stellar Massmentioning

confidence: 97%

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Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Giovannoli

Buat

Noll

et al. 2010

A&A

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Context. Luminous InfraRed Galaxies (LIRGs) are particularly important for studying the build-up of the stellar mass from z = 1 to z = 0, and for determining physical properties of these objects at redshift 0.7. LIRGs are now identified as playing a major role in galaxy evolution from z = 1 to 0. The global star formation rate (SFR) at z ∼ 0.7 is mainly produced by LIRGs. Aims. We perform a multiwavelength study of an LIRGs sample in the Extended Chandra Deep Field South at z = 0.7, selected at 24 μm by MIPS onboard Spitzer Space Telescope and detected in 17 filters. Data go from the near-ultraviolet to the mid-infrared. This multiwavelength dataset allows us to place strong constraints on the spectral energy distributions (SEDs) of galaxies, and thus to efficiently derive physical parameters such as the SFR, the total infrared luminosity, attenuation parameters, and star formation history. We distinguish a subsample of galaxies detected at 70 μm, which we compare to the rest of the sample to investigate the relative importance of this wavelength in determining of the physical parameters. An important part of this work is elaboration of a mock catalogue that allows us to have a reliability criterion for the derived parameters. Methods. We studied LIRGs by means of the SED-fitting code CIGALE. At first, this code creates synthetic spectra from the Maraston stellar population models. The stellar population spectra are attenuated by using a synthetic Calzetti-based attenuation law before adding the dust emission as given by the infrared SED library. The originality of CIGALE is that it allows us to perform consistent fits of the dust-affected ultaviolet-to-infrared wavelength range. This technique appears to be a very powerful tool in the case where we can have access to a dataset that is well-sampled over a wide range of wavelengths. Results. We are able to derive a star formation history and to estimate the fraction of infrared luminosity reprocessed by an active galactic nucleus. We study the dust temperatures of our galaxies detected at 70 μm and find them colder than predicted by models. We also study the relation between the SFR and the stellar mass and do not find a tight correlation between either of them, but instead a flat distribution and a large scatter, which is interpreted in terms of variations in star formation history.

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Section: Star Formation Rate and Stellar Masssupporting

confidence: 87%

Section: Star Formation Rate and Stellar Massmentioning

confidence: 97%

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Giovannoli

Buat

Noll

et al. 2010

A&A

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“…At z < 1 the decrease of the SFR density might be driven by a gradual gas exhaustion as suggested by the continuous decrease of the SFR vs. M relation in this redshift range (Noeske et al 2007;Elbaz et al 2007). Between z ∼ 2 and z ∼ 1, the relatively constant SFR density still needs to be understood in the framework of large-scale structure formation, merging, and/or AGN activity.…”

Section: Resultsmentioning

confidence: 91%

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

422

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Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ∼20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L 24/(1+z) vs. L 70/(1+z) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ∼ 1.55 ± 0.25 and z ∼ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ∼ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z) 1.0±0.9 combined with a density evolution proportional to (1 + z) −1.1±1.5 . At z ∼ 2, luminous infrared galaxies (LIRGs: 10 11 L < L IR < 10 12 L ) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ∼ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10 12 L < L IR ) account for ∼49% and ∼17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.

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“…A tight correlation between the star formation rate and the stellar mass has been observed both in the local Universe (Brinchmann et al 2004;Salim et al 2007;Peng et al 2010) and at high redshift (Noeske et al 2007;Elbaz et al 2007;Rodighiero et al 2010Rodighiero et al , 2014, widely known as the Main Sequence (MS).…”

Section: Main Sequencementioning

confidence: 99%

The star formation activity in cosmic voids

Ricciardelli¹,

Cava²,

Varela³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using a sample of cosmic voids identified in the Sloan Digital Sky Survey Data Release 7, we study the star formation activity of void galaxies. The properties of galaxies living in voids are compared with those of galaxies living in the void shells and with a control sample, representing the general galaxy population. Void galaxies appear to form stars more efficiently than shell galaxies and the control sample. This result can not be interpreted as a consequence of the bias towards low masses in underdense regions, as void galaxy subsamples with the same mass distribution as the control sample also show statistically different specific star formation rates. This highlights the fact that galaxy evolution in voids is slower with respect to the evolution of the general population. Nevertheless, when only the star forming galaxies are considered, we find that the star formation rate is insensitive to the environment, as the main sequence is remarkably constant in the three samples under consideration. This fact implies that environmental effects manifest themselves as fast quenching mechanisms, while leaving the non-quenched galaxies almost unaffected, as their star formation activity is largely regulated by the mass of their halo. We also analyse galaxy properties as a function of void-centric distance and find that the enhancement in the star formation activity with respect to the control sample is observable up to a radial distance 1.5 · R void . This result can be used as a suitable definition of void shells. Finally, we find that larger voids show an enhanced star formation activity in the shells with respect to their smaller counterparts, that could be related to the different dynamical evolution experienced by voids of different sizes.

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Star Formation in AEGIS Field Galaxies since z = 1.1: Staged Galaxy Formation and a Model of Mass-dependent Gas Exhaustion

Cited by 444 publications

References 25 publications

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Population synthesis modelling of luminous infrared galaxies at intermediate redshift

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

The star formation activity in cosmic voids

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