Star formation and mass assembly in high-redshift galaxies

By P. Santini, A. Fontana, A. Grazian, S. Salimbeni, Fabrizio Fiore, F. Fontanot, K. Boutsia, M. Castellano, S. Cristiani, C. Santis and 19 more. 2009

278 citations recorded by the source corpus.

Aims. The goal of this work is to infer the star formation properties and the mass assembly process of high redshift (0.3 ≤ z 0.3, the star formation rate is correlated well with stellar mass, and this relationship seems to steepen with redshift if one relies on IR-based estimates of the SFR; b) the contribution to the global SFRD by massive galaxies increases with redshift up to � 2.5, more rapidly than for galaxies of lower mass, but appears to flatten at higher z; c) despite this increase, the most important contributors to the SFRD at any z are galaxies of about, or immediately lower than, the characteristic stellar mass;

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/caf2c8724d22c9b94323dc0e580a65cc6455d9f6

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

On the evolution and environmental dependence of the star formation rate versus stellar mass relation since z ∼ 2 (2013, background): “…rate (SFR) andM∗ for star-forming galaxies in the local Universe (e.g. Brinchmann et al. 2004; Peng et al. 2010), as well as in the distant Universe outtoz >∼ 2 (e.g. Noeske et al. 2007; Daddi et al. 2007; Santini et al. 2009; Kajisawa et al. 2010; Bauer et al. 2011; Whitaker et al. 2012).”
THE STAR FORMATION HISTORY OF MASS-SELECTED GALAXIES IN THE COSMOS FIELD (2010, methodology): “…bimodality (whereby quiescent galaxies preferentially populate the high-mass end) in the SSFR-M∗ plane confirmed at various redshifts for galaxy samples with individually measured SFRs (e.g. Brinchmann et al. 2004; Salim et al. 2007; Elbaz et al. 2007; Santini et al. 2009; Rodighiero et al. 2010a).”
Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers (2012, methodology): “[48], where the adopted Salpeter IMF was rescaled to a Chabrier IMF as previously discussed.”
Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, background): “In fact, Santini et al. (2009) and Wuyts et al. (2011) have studied a sample of galaxies at high redshift (up to z ∼ 3) and they have found an overall good correspondence between SFRUV+IR and SFRSED up to intermediate SFRs, while at the largest SFR (>50 M yr−1) the discrepancy was significant and…”
The star formation activity of IllustrisTNG galaxies: main sequence, UVJ diagram, quenched fractions, and systematics (2018, result): “By allowing for larger apertures and smaller averaging timescales (light blue dashed curves), the TNG MS becomes progressively more consistent with the results by Santini et al. (2009) and Pannella et al. (2009), in which galaxy SFRs are derived from UV+IR and from radio, respectively.”
KECK SPECTROSCOPY OF 3 < z < 7 FAINT LYMAN BREAK GALAXIES: THE IMPORTANCE OF NEBULAR EMISSION IN UNDERSTANDING THE SPECIFIC STAR FORMATION RATE AND STELLAR MASS DENSITY (2012, methodology): “Recognizing that selecting only isolated IRAC sources limits the size of our eventual sample, we included IRAC flux measurements for galaxies in GOODS-South from the MUSIC catalog (Grazian et al. 2006; Santini et al. 2009).”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “As noted in Section 1, there are marginal indications that p varies from near 0.7 at z = 0 − 1 (Brinchmann et al. 2004; Noeske et al. 2007a) to about 0.9 at z ∼ 2 (Daddi et al. 2007; Santini et al. 2009; Pannella et al. 2009).”
CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD (2013, methodology): “Such method can be implemented with standard astronomical tools for image analysis and has been successfully used for the GOODS-MUSIC (Grazian et al. 2006; Santini et al. 2009) and GOODS-ERS database (Santini et al. 2012).”
Morphologies of z ∼ 0.7 AGN host galaxies in CANDELS: no trend of merger incidence with AGN luminosity (2014, methodology): “The stellar masses are derived by fitting the spectral energy distributions (SEDs) of the AGN with a mixture of galaxy and quasi-stellar object (QSO) templates, for a more detailed description of the process, we refer the reader to Santini et al. (2009, 2012).”
Mid- and far-infrared luminosity functions and galaxy evolution from multiwavelength Spitzer observations up to z ~ 2.5 (2009, result): “This finding is consistent with the results of previousSpitzer studies of the specific SF for star-forming galaxies (e.g. Perez-Gonzalez et al. 2005, P. Santini et al.2009).”
CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD (2013, background): “Two multi-wavelength catalogs in the literature cover (almost) the entire GOODS-S field as well as include most of our bands: GOODS-MUSIC (GM, Grazian et al. 2006; Santini et al. 2009) and FIREWORKS (FW, Wuyts et al. 2008).”
The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, background): “Since SFR correlates quite strongly with stellar mass (Noeske et al. 2007; Daddi et al. 2007; Santini et al. 2009) and AGN hosts are preferentially hosted by massive galaxies (Alonso-Herrero et al. 2008), stellar mass selection effects can bias any inferences about SF in AGN hosts (Silverman et al.…”
GOODS-Herschel: the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3 (2011, methodology): “We refer the reader to Santini et al. (2009) for a detailed description of the catalog content.”
UVUDF: ULTRAVIOLET THROUGH NEAR-INFRARED CATALOG AND PHOTOMETRIC REDSHIFTS OF GALAXIES IN THE HUBBLE ULTRA DEEP FIELD (2015, methodology): “The Bayesian prior is based on luminosity functions observed in COSMOS (Ilbert et al. 2009), GOODS-MUSIC (Grazian et al. 2006; Santini et al. 2009), and the UDF (Coe et al. 2006).”
REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE (2013, unknown): “…charted its evolution to z∼ 2.5 using different SFR tracers and selection criteria (e.g., Damen et al. 2009, Dunne et al. 2009, Pannella et al. 2009, Santini et al. 2009, Kajisawa et al. 2010, Oliver et al. 2010, Elbaz et al. 2011, Lee et al. 2011, Rodighiero et al. 2011, Wuyts et al. 2011,…”
UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, unknown): “Observational Constraints on Average SSFRs Publication Redshifts Type Area (deg2) Notes Salim et al. (2007) 0-0.2 UV 741 Bauer et al. (2013) 0-0.35 Hα 144 N Whitaker et al. (2014) 0-2.5 UV/IR 0.25 N Zwart et al. (2014) 0-3 Radio 1 IN Karim et al. (2011) 0.2-3 Radio 2 Kajisawa et al. (2010) 0.5-3.5 U”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, result): “They also found that at the highest SFRs & 100M⊙ yr −1 the SED-based values tended to underpredict the SFR, compared to the mixed indicator (see also Santini et al. 2009).”
A HIGHLY CONSISTENT FRAMEWORK FOR THE EVOLUTION OF THE STAR-FORMING “MAIN SEQUENCE” FROM z ∼ 0–6 (2014, methodology): “…et al. 2007 (S07); Noeske et al. 2007b (N07); Elbaz et al. 2007 (E07); Daddi et al. 2007 (D07); Chen et al. 2009 (C09); Pannella et al. 2009 (P09); Santini et al. 2009 (S09); Oliver et al. 2010 (O10); Magdis et al. 2010 (M10); Lee et al. 2011 (L11); Rodighiero et al. 2011 (R11); Elbaz et al.…”
An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source (2015, background): “As shown in Figure 1, we are able to put an upper limit to the MIPS 24µm flux (S/N < 2, mAB = 22.27 ± 0.90, Santini et al. 2009), while it is undetected in Herschel bands (< 1.2mJy, < 1.2mJy, < 2.4mJy in the 70µm 100µm, and 160µm bands, respectively, 5σ upper limits).”