Star Formation in AEGIS Field Galaxies since
                    <i>z</i>
                     = 1.1: The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-forming Galaxies

Noeske, K. G.; Weiner, Benjamin J.; Faber, S. M.; Papovich, Casey; Koo, David C.; Somerville, Rachel S.; Bundy, Kevin; Conselice, Christopher J.; Newman, Jeffrey A.; Schiminovich, David; Floc’h, E. Le; Coil, Alison L.; Rieke, G. H.; Lotz, Jennifer M.; Primack, Joel R.; Barmby, P.; Cooper, Michael C.; Davis, Marc; Ellis, Richard S.; Fazio, G. G.; Guhathakurta, Puragra; Huang, Jia-Sheng; Kassin, Susan; Martin, D. Christopher; Phillips, Andrew C.; Rich, R. Michael; Small, Todd; Willmer, Christopher; Wilson, G. W.

doi:10.1086/517926

Cited by 1,694 publications

(1,158 citation statements)

References 38 publications

(33 reference statements)

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“…Sommer-Larsen et al 2009, in preparation) invokes a formation mechanism where a large fraction of the gas is accreted onto the forming disk through both rapid cold gas accretion in filamentary structures and gradually in a cooling flow from a surrounding hot phase, rather than by rapid mergers of massive cold clumps. This is in qualitative agreement with recent results showing that smooth gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z ∼ 2 galaxies (see, e.g., Förster Genzel et al 2006Genzel et al , 2008Shapiro et al 2008;Noeske et al 2007;Elbaz et al 2007;Daddi et al 2007). As already suggested by the velocity-size relation obtained for a larger sample of SINS UV/optically selected galaxies (Bouché et al 2007), the angular momentum properties of these z ∼ 2 galaxies are very similar to local spirals and intermediate-redshift disks.…”

Section: Discussionsupporting

confidence: 92%

“…The dynamical evidence of the presence of such large, rotating, and turbulent disks is in agreement with the scenario in which rapid, smooth gas accretion from the halo may play a significant role in the formation of massive galaxies (Genzel et al 2008). This picture is also supported by recent broadband observations of high-z populations, which have found a fairly tight relation between stellar mass and SFR, a sign that steady SFRs, rather than merger-induced short luminous bursts, dominate the stellar assembly of these galaxies (Noeske et al 2007;Elbaz et al 2007;Daddi et al 2007). The most recent dark matter simulations such as the Millennium (Springel et al 2005) show that subsequent mergers are not frequent enough to convert all z ∼ 2 disks into elliptical galaxies at z = 0, and that most of the mass growth is achieved via mergers Vol.…”

Section: Resultssupporting

confidence: 67%

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THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

Cresci

Hicks

Genzel

et al. 2009

ApJ

278

542

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We present the modeling of SINFONI integral field dynamics of 18 star-forming galaxies at z ∼ 2 from Hα line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger-induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions (M gas ≈ M * ) are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity V max from the modeling to construct for the first time the stellar mass Tully-Fisher relation at z ∼ 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z ∼ 2.2 there is an offset in log(M * ) for a given rotational velocity of 0.41 ± 0.11 with respect to the local universe. This result is consistent with the predictions of the latest N-body/hydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z ∼ 2 galaxies.

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Section: Discussionsupporting

confidence: 92%

Section: Resultssupporting

confidence: 67%

THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

Cresci

Hicks

Genzel

et al. 2009

ApJ

278

542

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“…Also, as discussed above, high-z star-forming galaxies exhibit colder SEDs (e.g., Swinbank et al 2010;Hwang et al 2010;Magdis et al 2010;Symeonidis et al 2013) compared to local ULIRGs and more extended star formation (e.g., Menéndez-Delmestre et al 2009;Rujopakarn et al 2011). Finally, galaxies at all redshifts appear to follow a tight correlation between their star formation SFR and their stellar mass (e.g., Noeske et al 2007;Elbaz et al 2007;Pannella et al 2009;Daddi et al 2010a;Magdis et al 2010;Karim et al 2011). This speaks against stochastic-merger-induced starforming episodes as the main driver of star formation activity, as they would introduce a large scatter in the SFR−M * relation.…”

Section: Discussionmentioning

confidence: 79%

A Far-Infrared Spectroscopic Survey of Intermediate Redshift (Ultra) Luminous Infrared Galaxies

Magdis

Rigopoulou

Hopwood

et al. 2014

ApJ

116

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We present Herschel far-IR photometry and spectroscopy as well as ground-based CO observations of an intermediate redshift (0.21 z 0.88) sample of Herschel-selected (ultra)-luminous infrared galaxies (L IR > 10 11.5 L ). With these measurements, we trace the dust continuum, far-IR atomic line emission, in particular [C ii] 157.7 μm, as well as the molecular gas of z ∼ 0.3 luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and perform a detailed investigation of the interstellar medium of the population. We find that the majority of Herschel-selected intermediate redshift (U)LIRGs have L C ii /L FIR ratios that are a factor of about 10 higher than that of local ULIRGs and comparable to that of local normal and high-z star-forming galaxies. Using our sample to bridge local and high-z [C ii] observations, we find that the majority of galaxies at all redshifts and all luminosities follow an L C ii −L FIR relation with a slope of unity, from which local ULIRGs and high-z active-galactic-nucleus-dominated sources are clear outliers. We also confirm that the strong anti-correlation between the L C ii /L FIR ratio and the far-IR color L 60 /L 100 observed in the local universe holds over a broad range of redshifts and luminosities, in the sense that warmer sources exhibit lower L C ii /L FIR at any epoch. Intermediate redshift ULIRGs are also characterized by large molecular gas reservoirs and by lower star formation efficiencies compared to that of local ULIRGs. The high L C ii /L FIR ratios, the moderate star formation efficiencies (L IR /L CO or L IR /M H 2 ), and the relatively low dust temperatures of our sample (which are also common characteristics of high-z star-forming galaxies with ULIRG-like luminosities) indicate that the evolution of the physical properties of (U)LIRGs between the present day and z > 1 is already significant by z ∼ 0.3.

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“…The bulk of the SF galaxy population can be located on an MS locus in the plane of SFR versus * M (Noeske et al 2007b;Peng et al 2010;Rodighiero et al 2011;Whitaker et al 2012;Lee et al 2015). 19 …”

Section: Evolution Of the Sfrs And Stellar Massesmentioning

confidence: 99%

Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift

Scoville

Lee

Bout

et al. 2017

ApJ

358

614

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ALMA observations of the long wavelength dust continuum are used to estimate the interstellar medium (ISM) masses in a sample of 708 galaxies at z=0.3 to 4.5 in the COSMOS field. The galaxy sample has known farinfrared luminosities and, hence, star formation rates (SFRs) and stellar masses ( * M ) from the optical-infrared spectrum fitting. The galaxies sample SFRs from the main sequence (MS) to 50 times above the MS. The derived ISM masses are used to determine the dependence of gas mass on redshift, * M , and specific SFR (sSFR) relative to the MS. The ISM masses increase approximately with the 0.63 power of the rate of increase in SFRs with redshift and the 0.32 power of the sSFR/sSFR MS . The SF efficiencies also increase as the 0.36 power of the SFR redshift evolution and the 0.7 power of the elevation above the MS; thus the increased activities at early epochs are driven by both increased ISM masses and SF efficiency. Using the derived ISM mass function, we estimate the accretion rates of gas required to maintain continuity of the MS evolution (>  M 100 yr −1 at z > 2.5). Simple power-law dependencies are similarly derived for the gas accretion rates. We argue that the overall evolution of galaxies is driven by the rates of gas accretion. The cosmic evolution of total ISM mass is estimated and linked to the evolution of SF and active galactic nucleus activity at early epochs.

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Star Formation in AEGIS Field Galaxies since z = 1.1: The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-forming Galaxies

Cited by 1,694 publications

References 38 publications

THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

A Far-Infrared Spectroscopic Survey of Intermediate Redshift (Ultra) Luminous Infrared Galaxies

Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift

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