The star formation history of K-selected galaxies

By L. Dunne, R. Ivison, S. Maddox, M. Cirasuolo, A. Mortier, S. Foucaud, E. Ibar, O. Almaini, C. Simpson, R. McLure. 2008

137 citations recorded by the source corpus.

We have studied the μJy radio properties of K-selected galaxy populations detected in the Ultra-Deep Survey (UDS) portion of the United Kingdom Infrared Telescope (UKIRT) Deep Sky Survey using 610- and 1400-MHz images from the Very Large Array and the Giant Metre-wave Telescope. These deep radio mosaics, combined with the largest and deepest K-band image currently available, allow high signal-to-noise ratio (S/N) detections of many K-selected subpopulations, including sBzK and pBzK star-forming and passive galaxies. We find a strong correlation between the radio and K-band fluxes and a linear relationship between star formation rate (SFR) and K-band luminosity. We find no evidence, either from radio spectral indices or a comparison with submm-derived SFRs, that the full sample is strongly contaminated by active galactic nuclei (AGN) at these low flux densities, though this is very difficult to determine from this data set. The photometric redshift distributions for the BzK galaxies place 37 (29) per cent of pBzK (sBzK) galaxies at z 1.4, the pBzK galaxies become difficult to detect in the radio stack, though the implied SFRs are still much higher than expected for passively evolving galaxies. It may be that their radio emission comes from low-luminosity AGN. Extremely red objects (EROs) straddle the passive and star-forming regions of the BzK diagram and also straddle the two groups in terms of their radio properties. We find that K-bright ERO samples are dominated by passive galaxies and faint ERO samples contain more star-forming galaxies. The star formation history (SFH) from stacking all K-band sources in the UDS agrees well with that derived for other wavebands and other radio surveys, at least out to z ∼ 2. The radio-derived SFH then appears to fall more steeply than that measured at other wavelengths. The SSFR for K-selected sources rises strongly with redshift at all stellar masses, and shows a weak dependence on stellar mass. High- and low-mass galaxies show a similar decline in SSFR since z ∼ 2.

Subfields: Astronomy and Astrophysics, Instrumentation

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. R. Dav'e
4. R. Somerville
5. D. M. Alexander
6. P. V. van Dokkum
7. C. Conroy
8. A. Dekel

In Instrumentation

1. R. Dav'e
2. P. Hopkins
3. L. Hernquist
4. R. Somerville
5. P. V. van Dokkum
6. C. Conroy
7. A. Dekel
8. Christopher J. Conselice

Citations in the corpus

• GOODS-Herschel: the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3 (2011, background): “…formation. are roughly proportional to galaxy stellar mass (e.g., Noeske et al. 2007; Elbaz et al. 2007; Daddi et al. 2007; Pannella et al. 2009a; Dunne et al. 2009; Magdis et al. 2010), meaning systematic differences in the stellar masses of difference populations of galaxies (such as AGNs…”
• Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschel observations (2012, background): “…with redshift up toz ∼ 2 − 3, an epoch which corresponds to the peak of SF (e.g. Hopkins & Beacom 2006), and to flatten at higher redshifts, its slope is still debated (see discussion in Dunne et al. 2009; Pannella et al. 2009; Santini et al. 2009; Rodighiero et al. 2010; Karim et al. 2011).”
• GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “15Here, we assume an intrinsic dispersion of 0.3 dex (Speagle et al. 2014) and a slope of 0.8 in the stellar-mass range below 1010 M (Dunne et al. 2009; Santini et al. 2009; Sobral et al. 2014) and 0.55 above (Whitaker et al. 2012).”
• UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, unknown): “…(2011b) 1-3 UV 0.24 I Kajisawa et al. (2010) 0.5-3.5 UV/IR 0.03 I Schreiber et al. (2015) 0-4 FIR 1.75 IN Planck Collab. et al. (2014) 0-4 FIR 2240 IN Dunne et al. (2009) 0-4 Radio 0.8 I Cucciati et al. (2012) 0-5 UV 0.6 I Le Borgne et al. (2009) 0-5 IR-mm varies I van der Burg et al. (2010) 3-5…”
• WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, background): “At a given stellar mass, the SFR of galaxies depends strongly on redshift, evolving by a factor of 5–10 byz∼ 1 and another factor of 4 or so out toz∼ 2 (Zheng et al. 2007; Noeske et al. 2007; Dunne et al. 2009; Karim et al. 2011).”
• MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION IN SDSS AND zCOSMOS AND THE ORIGIN OF THE SCHECHTER FUNCTION (2010, background): “…of the sSFR described in the two previous subsections, is also seen at much higher redshifts, (e.g. Daddi et al., 2007, Elbaz et al., 2007, Dunne et al. 2009; Pannella et al. 2009; Santini et al. 2009), but with a characteristic sSFR that is substantially elevated, by a factor of about 7…”
• Star formation and mass assembly in high-redshift galaxies (2009, background): “However, we note that deep radio observations (Dunne et al. 2009) appear to conflict with thisscenario.”
• HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “This implies that dust forms very rapidly after the onset of the main episode of star formation, either in the ISM (Draine et al. 2009; Dunne et al. 2011) or by effect of Type-II SNae (Dunne et al. 2003, 2009; Matsuura et al. 2011).”
• A fundamental problem in our understanding of low-mass galaxy evolution (2012, background): “We also find that the observed evolution of the low mass end of the mass function is consistent with the sSFR-stellar mass relation as observed by Dunne et al. (2009), Daddi et al. (2007) and Elbaz et al. (2007), who find β ∼-0.1.”
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• THE COSMOS-WIRCam NEAR-INFRARED IMAGING SURVEY. I. BzK-SELECTED PASSIVE AND STAR-FORMING GALAXY CANDIDATES AT z ≳ 1.4 (2009, methodology): “…control sample lie in the (B − z) and (z − K) plane and considerations of galaxy evolutionary tracks, it has been adopted and tested in several subsequent studies (e.g., Kong et al. (2006); Lane et al. (2007); Hayashi et al. (2007); Blanc et al. (2008); Dunne et al. (2009); Popesso et al. (2009)).”
• A TURNOVER IN THE GALAXY MAIN SEQUENCE OF STAR FORMATION AT M* ∼ 1010 M☉ FOR REDSHIFTS z < 1.3 (2015, background): “…of the SFR/M∗ mainsequence with redshift.15 The scaling of the main sequence has been found in the literature to evolve as (1 + z)n, with the exponent n varying from 2.2 < n < 5 (Erb et al. 2006; Daddi et al. 2007; Damen et al. 2009; Dunne et al. 2009; Pannella et al. 2009; Karim et al. 2011).”
• THE RELATION BETWEEN STAR FORMATION RATE AND STELLAR MASS FOR GALAXIES AT 3.5 ⩽ z ⩽ 6.5 IN CANDELS (2014, result): “2 (Daddi et al. 2007; Noeske et al. 2007; Dunne et al. 2009; Oliver et al. 2010; Rodighiero et al. 2010), opposing results have been observed in the literature for higher redshift (z > 2) galaxies.”
• Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA (2013, background): “The other points are a compilation by Stark et al. (2013) including also data from Dunne et al. (2009) and Reddy et al. (2012) atlog(M) ∼ 9.7.”
• EMU: Evolutionary Map of the Universe (2011, unknown): “Stacking at radio wavelengths has been used very successfully (e.g. White 2007; Ivison et al. 2007; Ivison et al. 2010; Dunne et al. 2009; Messias et al. 2010; Bourne et al. 2011) on highresolution data for the purpose of studying faint populations which are below the detection threshold of the…”
• THE SFR–M* RELATION AND EMPIRICAL STAR FORMATION HISTORIES FROM ZFOURGE AT 0.5 < z < 4 (2015, background): “Thus, many studies over the past several years have turned to measuring SFRs from stacked data in order to compensate for this disparity (e.g. Dunne et al. 2009; Rodighiero et al. 2010; Karim et al. 2011; Whitaker et al. 2014; Schreiber et al. 2015).”
• The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, unknown): “…and gas content etc. of these galaxies (e.g. Doherty et al. 2004, 2006; Bell et al. 2005, 2012; Erb et al. 2006a,b; Kassin et al. 2007, 2012; Buitrago et al. 2008; Dunne et al. 2009; Peng et al. 2010; Geach et al. 2011; van Dokkum et al. 2011; Stott et al. 2013a,b; Sobral et al. 2014).”