Reversal or no reversal: the evolution of the star formation rate–density relation up to z ∼ 1.6

Ziparo, F.; Popesso, P.; Finoguenov, A.; Biviano, A.; Wuyts, Stijn; Wilman, David J.; Salvato, M.; Tanaka, Masayuki; Nandra, K.; Lutz, D.; Elbaz, D.; Dickinson, Mark; Altiéri, B.; Aussel, H.; Berta, S.; Cimatti, A.; Fadda, D.; Genzel, R.; Floc’h, E. Le; Magnelli, B.; Nordon, R.; Poglitsch, A.; Pozzi, F.; Portal, M. Sánchez; Tacconi, L. J.; Bauer, F. E.; Brandt, W. N.; Cappelluti, N.; Cooper, Michael C.; Mulchaey, John S.

doi:10.1093/mnras/stt1901

Cited by 40 publications

(48 citation statements)

References 93 publications

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“…The slightly higher L * of the group galaxy LF indicates a potentially higher mean SFR in groups than in the field, at least in the star-forming galaxy population. This would be consistent with a flattening of the SFR-density relation at this redshift, as found by Ziparo et al (2014), but also with a potential reversal of the same relation, though the difference between the total and group galaxy luminosity distribution is not very significant (∼2σ, see Fig. 8).…”

Section: Figsupporting

confidence: 89%

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The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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Context. There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low mass galaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly. Aims. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whether the observed "galaxy downsizing" could be interpreted as a "halo downsizing", whereas the most massive haloes, and their galaxy populations, evolve more rapidly than the haloes with lower mass. Methods. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of the evolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ∼1.6. We used a sample of 39 X-rayselected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field, where the deepest available mid-and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel satellite. Results. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. Their IR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. At redshift 1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a reversal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxies contribute 60-80% of the CSFH, i.e. much more than at lower redshifts. Below z ∼ 1, the comoving number and SFR densities of IR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies. Conclusions. Our results are consistent with a "halo downsizing" scenario and highlight the significant role of "environment" quenching in shaping the CSFH.

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Section: Figsupporting

confidence: 89%

“…On the other hand, Feruglio et al (2010) find no reversal in the COSMOS A&A 574, A105 (2015) field and argue that the reversal, if any, must occur at z ∼ 2. Similarly, Ziparo et al (2014) find that the local anti-correlation tends to flatten towards high redshift rather than reversing.…”

Section: Introductionmentioning

confidence: 59%

The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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“…This evidence has also been supported by simulations A&A 592, A108 (2016) from Tonnesen & Cen (2014). However, there is some controversy since Ziparo et al (2014) find no clear evidence of this type of reversal when studying the evolution of the SF-density relation in the ECDFS and GOODS fields up to z ∼ 1.6.…”

Section: Introductionmentioning

confidence: 55%

Multi-wavelength landscape of the young galaxy cluster RXJ 1257.2+4738 atz= 0.866

Pintos-Castro

Pović

Sánchez‐Portal

et al. 2016

A&A

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Studying the evolution of the morphological distribution of galaxies in different environments can provide important information about the effects of the environment and the physical mechanisms responsible for the morphological transformations. As part of a complete analysis of the young cluster RXJ 1257+4738 at z ∼ 0.9, in this work we study the morphological properties of its galaxies. We used non-parametric methods of morphological classification, as implemented in the galSVM code. The classification with the applied method was possible even using ground-based observations, as the r -band imaging from OSIRIS/GTC. We defined very conservative probability limits, taking into account the probability errors, to obtain a trustworthy classification. In this way we were able to classify ∼30% of all cluster members and to separate between late-type (LT) and early-type (ET) galaxies. Additionally, when analysing the colour-magnitude diagram, we observed a significant population of blue ET galaxies among the classified ones. We discussed possible explanations for finding this population. Moreover, we studied different physical properties of LT, ET, and blue ET galaxies. They turn out to be comparable, with the exception of the stellar mass that shows that the red ET population is more massive. We also analysed the morphology-density and morphology-radius relations observing that, only when considering the morphological separation between ET and LT galaxies, a mild classical behaviour is obtained. RXJ 1257+4738 is a young galaxy cluster, showing a clumpy structure, which is still in the process of formation, and which could explain the lack of some of the standard morphological relations. This makes this cluster a very attractive case for obtaining higher resolution data and for studying the morphological properties of the entire cluster in more detail and their relation to the environment.

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“…Cucciati et al 2006;Cooper et al 2008;Grützbauch et al 2011;Ziparo et al 2013). Beyond z ∼ 1.4, clusters host large numbers of highly star forming galaxies (e.g.…”

Section: Introductionmentioning

confidence: 99%

The impact of protocluster environments atz= 1.6

Hatch

Cooke

Muldrew

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate the effects of dense environments on galaxy evolution by examining how the properties of galaxies in the z = 1.6 protocluster Cl 0218.3−0510 depend on their location. We determine galaxy properties using spectral energy distribution fitting to 14-band photometry, including data at three wavelengths that tightly bracket the Balmer and 4000Å breaks of the protocluster galaxies. We find that two-thirds of the protocluster galaxies, which lie between several compact groups, are indistinguishable from field galaxies. The other third, which reside within the groups, differ significantly from the intergroup galaxies in both colour and specific star formation rate. We find that the fraction of red galaxies within the massive protocluster groups is twice that of the intergroup region. These excess red galaxies are due to enhanced fractions of both passive galaxies (1.7 times that of the intergroup region) and dusty star-forming galaxies (3 times that of the intergroup region). We infer that some protocluster galaxies are processed in the groups before the cluster collapses. These processes act to suppress star formation and change the mode of star formation from unobscured to obscured.

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Reversal or no reversal: the evolution of the star formation rate–density relation up to z ∼ 1.6

Cited by 40 publications

References 93 publications

The evolution of galaxy star formation activity in massive haloes

The evolution of galaxy star formation activity in massive haloes

Multi-wavelength landscape of the young galaxy cluster RXJ 1257.2+4738 atz= 0.866

The impact of protocluster environments atz= 1.6

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