A high abundance of massive galaxies 3–6 billion years after the Big Bang

Glazebrook, Karl; Abraham, Roberto; McCarthy, Patrick J.; Savaglio, S.; Chen, Hsiao‐Wen; Crampton, D.; Murowinski, Rick; Jørgensen, Inger; Roth, Kathy; Hook, I. M.; Marzke, Ronald O.; Carlberg, R. G.

doi:10.1038/nature02667

Cited by 335 publications

(350 citation statements)

References 29 publications

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“…Kauffmann et al 2003) and at high redshift (e.g. Glazebrook et al 2004). In addition, Juneau et al (2005) show that the more massive galaxies start to form stars earlier than intermediate and low mass objects.…”

Section: Role Of the Environment On Galaxy Formation And Evolutionmentioning

confidence: 99%

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

152

146

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Context. For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. Aims. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z ∼ 1 using about 10 000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z ∼ 1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. Methods. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10 000 galaxies down to I AB = 22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z ∼ 1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. The evolution of the morphology-density relation in different environments is then studied for luminosity and stellar-mass selected, volume-limited samples of galaxies. The trends are described and related to the various physical processes that could play a relevant role in the build-up of the morphology-density relation. Results. We confirm that the morphological segregation is present up to z ∼ 1 for luminosity-selected, volume-limited samples. The behaviour of the morphology-density relation gets flatter at fixed masses expecially above 10 10.6 M . We suggest the existence of a critical mass above which the physical processes governing galaxy stellar mass also determine the shaping of the galaxy more than its environment. We finally show that at a fixed morphology there is still a residual variation in galaxy colours with density. Conclusions. The observed evolution with redshift of the morphology-density relation offers an opportunity to trace the effect of nature and nurture as a function of environment. Even though it is based mainly on a biased view, the environmental dependence of the morphological evolution for luminosity-selected, volume-limited samples seems to indicate that nurture is in play. On the other hand, the lack of evolution observed for earlytype and spiral galaxies that are more massive than 10 10.8 M independents of the environment indicates that nature has imprinted these properties early in the life of...

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Section: Role Of the Environment On Galaxy Formation And Evolutionmentioning

confidence: 99%

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

152

146

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“…[53] analyzed the spectra (obtained with the GMOS multi-slit spectrograph) of 25 galaxies with measured D4000 n and Hδ, in the range 0.6 < z < 1.2 and with masses M > 10 10.2 M ⊙ . Stellar masses have been derived from template fits to the multicolor photometry [54], assuming a Baldry et al (2003) IMF [55]. Masses have been scaled by -0.03 dex to convert them to a Chabrier IMF [42,53].…”

Section: Goods-s Samplementioning

confidence: 99%

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

Moresco

Cimatti

Jiménez

et al. 2012

J. Cosmol. Astropart. Phys.

749

365

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Abstract. We present new improved constraints on the Hubble parameter H(z) in the redshift range 0.15 < z < 1.1, obtained from the differential spectroscopic evolution of early-type galaxies as a function of redshift. We extract a large sample of early-type galaxies (∼ 11000) from several spectroscopic surveys, spanning almost 8 billion years of cosmic lookback time (0.15 < z < 1.42). We select the most massive, red elliptical galaxies, passively evolving and without signature of ongoing star formation. Those galaxies can be used as standard cosmic chronometers, as firstly proposed by Jimenez & Loeb (2002), whose differential age evolution as a function of cosmic time directly probesWe analyze the 4000Å break (D4000) as a function of redshift, use stellar population synthesis models to theoretically calibrate the dependence of the differential age evolution on the differential D4000, and estimate the Hubble parameter taking into account both statistical and systematical errors.We provide 8 new measurements of H(z) (see Tab. 4), and determine its change in H(z) to a precision of 5 − 12% mapping homogeneously the redshift range up to z ∼ 1.1; for the first time, we place a constraint on H(z) at z = 0 with a precision comparable with the one achieved for the Hubble constant (about 5-6% at z ∼ 0.2), and covered a redshift range (0.5 < z < 0.8) which is crucial to distinguish many different quintessence cosmologies.These measurements have been tested to best match a ΛCDM model, clearly providing a statistically robust indication that the Universe is undergoing an accelerated expansion. This method shows the potentiality to open a new avenue in constrain a variety of alternative cosmologies, especially when future surveys (e.g. Euclid) will open the possibility to extend it up to z ∼ 2.-1 -

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“…Many previous works have demonstrated that a substantial fraction (30-50%) of the stellar mass formed between z ∼ 3 and z ∼ 1 (Dickinson et al 2003;Fontana et al 2003Fontana et al , 2004Fontana et al , 2006Glazebrook et al 2004;Drory et al 2004;Rudnick et al 2006;Papovich et al 2006;Yan et al 2006;Pozzetti et al 2007). However, it is still unclear what the major channel for galaxy growth is during this period.…”

Section: Introductionmentioning

confidence: 99%

The interaction-driven starburst contribution to the cosmic star formation rate density

Lamastra

Menci

Fiore

et al. 2013

A&A

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An increasing amount of observational evidence supports the notion that there are two modes of star formation: a quiescent mode in disk-like galaxies and a starburst mode, which is generally interpreted as driven by merging. Using a semi-analytic model of galaxy formation, we derive the relative contribution to the cosmic star formation rate density of quiescently star forming and starburst galaxies, predicted under the assumption that starburst events are triggered by galaxy encounters (merging and fly-by kind) during their merging histories. We show that, within this framework, quiescently star forming galaxies dominate the cosmic star formation rate density at all redshifts. The contribution of the burst-dominated star forming galaxies increases with redshift, starting from 5% at low redshift (z 0.1) to ∼20% at z ≥ 5. We estimated that the fraction of the final (z = 0) galaxy stellar mass that is formed through the burst component of star formation is ∼10% for 10 10 M ≤ M * ≤ 10 11.5 M . Selected according to their distance from the galaxy main sequence, starburst galaxies account for ∼10% of the star formation rate density in the redshift interval 1.5 < z < 2.5, i.e., at the cosmic peak of the star formation activity.

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A high abundance of massive galaxies 3–6 billion years after the Big Bang

Cited by 335 publications

References 29 publications

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers

The interaction-driven starburst contribution to the cosmic star formation rate density

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