THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 &lt;<i>z</i>&lt; 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 &lt;<i>z</i>&lt; 0.08

Maier, C.; Lilly, S. J.; Zamorani, G.; Scodeggio, M.; Lamareille, F.; Contini, T.; Sargent, M.; Scarlata, Claudia; Oesch, Pascal; Carollo, C. M.; Fèvre, O. Le; Renzini, A.; Kneib, Jean-Paul; Mainieri, V.; Bardelli, S.; Bolzonella, M.; Bongiorno, A.; Caputi, K.; Coppa, G.; Cucciati, O.; Torre, S. de la; Ravel, L. de; Franzetti, P.; Garilli, B.; Iovino, A.; Kampczyk, P.; Knobel, C.; Kovač, K.; Borgne, J. F. Le; Brun, V. Le; Mignoli, M.; Pelló, R.; Peng, Yingjie; Montero, E. Pérez; Ricciardelli, E.; Silverman, John D.; Tanaka, Masayuki; Tasca, L.; Tresse, L.; Vergani, D.; Zucca, E.; Abbas, U.; Bottini, D.; Cappi, A.; Cassata, P.; Cimatti, A.; Fumana, M.; Guzzo, L.; Halliday, C.; Koekemoer, Anton M.; Leauthaud, Alexie; Maccagni, D.; Marinoni, C.; McCracken, H. J.; Memeo, P.; Meneux, B.; Porciani, Cristiano; Pozzetti, L.; Scaramella, R.

doi:10.1088/0004-637x/694/2/1099

Cited by 37 publications

(43 citation statements)

References 53 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…As described in Section 3.1, we distinguish between these two populations by means of a threshold in the distance of the galaxies to the star-forming sequence at each redshift ( SFR log SFR log SFR MS D º -). This criterion has been shown to be very effective at splitting galaxy samples into two groups that accurately match known bimodalities in galaxy structure, morphology, or rest-frame colors (e.g., Maier et al 2009;Brammer et al 2011;Wuyts et al 2011b). Following a similar approach to previous works, here we study the robustness of our quiescence threshold in SFR D by comparing to an independent color-color criterion based on rest-frame optical/NIR colors, the so-called UVJ diagram (Wuyts et al 2007;Williams et al 2009).…”

Section: Discussionmentioning

confidence: 96%

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Barro

Faber

Koo

et al. 2017

ApJ

271

384

View full text Add to dashboard Cite

We study the evolution of the scaling relations that compare the effective density ( r r , e e S < ) and core density ( r , 1 1 S < kpc) to the stellar masses of star-forming galaxies (SFGs) and quiescent galaxies. These relations have been fully in place since z 3 and have exhibited almost constant slope and scatter since that time. For SFGs, the zero points in e S and 1 S decline by only 2 . This fact plus the narrowness of the relations suggests that galaxies could evolve roughly along the scaling relations. Quiescent galaxies follow different scaling relations that are offset to higher densities at the same mass and redshift. Furthermore, the zero point of their core density has declined by only 2 since z 3 , while the zero point of the effective density declines by 10 . When galaxies quench, they move from the star-forming relations to the quiescent relations. This involves an increase in the core and effective densities, which suggests that SFGs could experience a phase of significant core growth relative to the average evolution along the structural relations. The distribution of massive galaxies relative to the SFR-M and the quiescent M  Srelations exhibits an L-shape that is independent of redshift. The knee of this relation consists of a subset of "compact" SFGs that are the most likely precursors of quiescent galaxies forming at later times. The compactness selection threshold in 1 S exhibits a small variation from z=3 to 0.5, M 0.65 log 10.5 9.6 9.3 1 * S --> -( ) M e kpc −2 , allowing the most efficient identification of compact SFGs and quiescent galaxies at every redshift.

show abstract

Section: Discussionmentioning

confidence: 96%

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Barro

Faber

Koo

et al. 2017

ApJ

271

384

View full text Add to dashboard Cite

show abstract

“…The redshift evolution of this correlation was later presented in Franx et al (2008) (see also Maier et al 2009). Both works identified a threshold surface density at each redshift interval: below this threshold the sSFRs are high with little variation, and above the threshold density, galaxies have low sSFRs.…”

Section: Introductionmentioning

confidence: 82%

Predicting Quiescence: The Dependence of Specific Star Formation Rate on Galaxy Size and Central Density at 0.5 < z < 2.5

Whitaker

Bezanson

Dokkum

et al. 2017

ApJ

134

137

View full text Add to dashboard Cite

In this paper, we investigate the relationship between star formation and structure, using a mass-complete sample of 27,893 galaxies at 0.5<z<2.5 selected from 3D-HST. We confirm that star-forming galaxies are larger than quiescent galaxies at fixed stellar mass (M  ). However, in contrast with some simulations, there is only a weak relation between star formation rate (SFR) and size within the star-forming population: when dividing into quartiles based on residual offsets in SFR, we find that the sizes of star-forming galaxies in the lowest quartile are 0.27±0.06 dex smaller than the highest quartile. We show that 50% of star formation in galaxies at fixed M  takes place within a narrow range of sizes (0.26 dex). Taken together, these results suggest that there is an abrupt cessation of star formation after galaxies attain particular structural properties. Confirming earlier results, we find that central stellar density within a 1 kpc fixed physical radius is the key parameter connecting galaxy morphology and star formation histories: galaxies with high central densities are red and have increasingly lower SFR/M  , whereas galaxies with low central densities are blue and have a roughly constant (higher) SFR/M  at a given redshift. We find remarkably little scatter in the average trends and a strong evolution of >0.5 dex in the central density threshold correlated with quiescence from z∼0.7-2.0. Neither a compact size nor high-n are sufficient to assess the likelihood of quiescence for the average galaxy; instead, the combination of these two parameters together with M  results in a unique quenching threshold in central density/velocity.

show abstract

“…2 in Maier et al 2009). The same trend is observed using the SFR and SSFR derived from the fit to the multi-band photometry with synthetic models.…”

Section: Mass Functions By Galaxy Typesmentioning

confidence: 99%

“…Using estimates of the SFR and SSFR derived from the [OII] lines (Moustakas et al 2006, calibration), Maier et al (2009) find that very few zCOSMOS galaxies with masses above log(M/M ) > 10.8 have 1/SSFRs below the age of the universe at 0.5 < z < 0.7, while there exist several dozens of galaxies above the same mass that are strongly star-forming at 0.7 < z < 0.9 (see Fig. 2 in Maier et al 2009).…”

Section: Mass Functions By Galaxy Typesmentioning

confidence: 99%

zCOSMOS – 10k-bright spectroscopic sample

Pozzetti

Bolzonella

Zucca

et al. 2010

A&A

Self Cite

425

309

View full text Add to dashboard Cite

We present the galaxy stellar mass function (GSMF) to redshift z 1, based on the analysis of about 8500 galaxies with I < 22.5 (AB mag) over 1.4 deg 2 , which are part of the zCOSMOS-bright 10k spectroscopic sample. We investigate the total GSMF, as well as the contributions of early-and late-type galaxies (ETGs and LTGs, respectively), defined by different criteria (broad-band spectral energy distribution, morphology, spectral properties, or star formation activities). We unveil a galaxy bimodality in the global GSMF, whose shape is more accurately represented by 2 Schechter functions, one linked to the ETG and the other to the LTG populations. For the global population, we confirm a mass-dependent evolution ("mass-assembly downsizing"), i.e., galaxy number density increases with cosmic time by a factor of two between z = 1 and z = 0 for intermediate-to-low mass (log(M/M ) ∼ 10.5) galaxies but less than 15% for log(M/M ) > 11. We find that the GSMF evolution at intermediateto-low values of M (log(M/M ) < 10.6) is mostly explained by the growth in stellar mass driven by smoothly decreasing star formation activities, despite the redder colours predicted in particular at low redshift. The low residual evolution is consistent, on average, with ∼0.16 merger per galaxy per Gyr (of which fewer than 0.1 are major), with a hint of a decrease with cosmic time but not a clear dependence on the mass. From the analysis of different galaxy types, we find that ETGs, regardless of the classification method, increase in number density with cosmic time more rapidly with decreasing M, i.e., follow a top-down building history, with a median "building redshift" increasing with mass (z > 1 for log(M/M ) > 11), in contrast to hierarchical model predictions. For LTGs, we find that the number density of blue or spiral galaxies with log(M/M ) > 10 remains almost constant with cosmic time from z ∼ 1. Instead, the most extreme population of star-forming galaxies (with high specific star formation), at intermediate/high-mass, rapidly decreases in number density with cosmic time. Our data can be interpreted as a combination of different effects. Firstly, we suggest a transformation, driven mainly by SFH, from blue, active, spiral galaxies of intermediate mass to blue quiescent and subsequently (1−2 Gyr after) red, passive types of low specific star formation. We find an indication that the complete morphological transformation, probably driven by dynamical processes, into red spheroidal galaxies, occurred on longer timescales or followed after 1−2 Gyr. A continuous replacement of blue galaxies is expected to be accomplished by low-mass active spirals increasing their stellar mass. We estimate the growth rate in number and mass density of the red galaxies at different redshifts and masses. The corresponding fraction of blue galaxies that, at any given time, is transforming into red galaxies per Gyr, due to the quenching of their SFR, is on average ∼25% for log(M/M ) < 11. We conclude that the build-up of galaxies and in particular of...

show abstract

THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 <z< 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 <z< 0.08

Cited by 37 publications

References 53 publications

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Predicting Quiescence: The Dependence of Specific Star Formation Rate on Galaxy Size and Central Density at 0.5 < z < 2.5

zCOSMOS – 10k-bright spectroscopic sample

Contact Info

Product

Resources

About