The evolving relation between star formation rate and stellar mass in the VIDEO survey since<i>z</i> = 3

Johnston, Russell; Vaccari, M.; Jarvis, Matt J.; Smith, M.; Giovannoli, É.; Häußler, Boris; Prescott, M.

doi:10.1093/mnras/stv1715

Cited by 78 publications

(87 citation statements)

References 119 publications

(259 reference statements)

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“…Elbaz et al 2007Elbaz et al , 2011Schreiber et al 2015;Johnston et al 2015) we can examine whether QSOs have SFRs that are consistent with being selected from the overall star forming galaxy population. To make this comparison we use the Schreiber et al (2015) definition of the 'main sequence' at z ∼ 1 (see Eq.…”

Section: The Star Formation Dependence On Agn Activitymentioning

confidence: 99%

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Several studies support the existence of a link between the AGN and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9 < z < 1.1 which span over two decades in optical luminosity. By decoupling luminosity from evolutionary effects, we investigate how the star formation rate (SFR) depends on AGN luminosity, radio-loudness and orientation. We find that: 1) the SFR shows a weak correlation with the bolometric luminosity for all AGN sub-samples, 2) the RLQs show a SFR excess of about a factor of 1.4 compared to the RQQs, matched in terms of black hole mass and bolometric luminosity, suggesting that either positive radio-jet feedback or radio AGN triggering are linked to star-formation triggering and 3) RGs have lower SFRs by a factor of 2.5 than the RLQ sub-sample with the same BH mass and bolometric luminosity. We suggest that there is some jet power threshold at which radio-jet feedback switches from enhancing star formation (by compressing gas) to suppressing it (by ejecting gas). This threshold depends on both galaxy mass and jet power.

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Section: The Star Formation Dependence On Agn Activitymentioning

confidence: 99%

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Only model galaxies with sSFR> 0.3/tH are used for this analysis. Gray symbols correspond to different observational measurements based on Hα (Elbaz et al 2007;Sobral et al 2014), UV (Salim et al 2007;Johnston et al 2015), UV+IR (Salmi et al 2012;Santini et al 2009), and FUV (Magdis et al 2010;Lee et al 2011Lee et al , 2012. Symbols and error bars correspond to the best fitting and standard deviation given in Speagle et al (2014).…”

Section: Galaxy Stellar Mass -Cold Gas Metallicity Relationmentioning

confidence: 99%

H2-based star formation laws in hierarchical models of galaxy formation

Xie

Lucia

Hirschmann

et al. 2017

Monthly Notices of the Royal Astronomical Society

101

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We update our recently published model for GAlaxy Evolution and Assembly (GAEA), to include a self-consistent treatment of the partition of cold gas in atomic and molecular hydrogen. Our model provides significant improvements with respect to previous ones used for similar studies. In particular, GAEA (i) includes a sophisticated chemical enrichment scheme accounting for non-instantaneous recycling of gas, metals, and energy; (ii) reproduces the measured evolution of the galaxy stellar mass function; (iii) reasonably reproduces the observed correlation between galaxy stellar mass and gas metallicity at different redshifts. These are important prerequisites for models considering a metallicity dependent efficiency of molecular gas formation. We also update our model for disk sizes and show that model predictions are in nice agreement with observational estimates for the gas, stellar and star forming disks at different cosmic epochs. We analyse the influence of different star formation laws including empirical relations based on the hydrostatic pressure of the disk, analytic models, and prescriptions derived from detailed hydrodynamical simulations. We find that modifying the star formation law does not affect significantly the global properties of model galaxies, neither their distributions. The only quantity showing significant deviations in different models is the cosmic molecular-to-atomic hydrogen ratio, particularly at high redshift. Unfortunately, however, this quantity also depends strongly on the modelling adopted for additional physical processes. Useful constraints on the physical processes regulating star formation can be obtained focusing on low mass galaxies and/or at higher redshift. In this case, self-regulation has not yet washed out differences imprinted at early time.

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“…To test how outshining would affect SMD measurements, we first took the best-fit Schecter function parameters for all galaxy morphologies listed in Table 2 of Huertas-Company et al (2016), which were divided at different redshifts into star-forming and passive mass functions. We estimated the star-formation rate of the star-forming galaxies of a given mass and redshift using the main sequence relation of Johnston et al (2015). Then, with estimates of the sSFRs of the star-forming population of galaxies, we used Equation 6 to correct the star-forming mass function at each redshift for the mass bias found in this work.…”

Section: The Missing Mass Problemmentioning

confidence: 99%

Spatially unresolved SED fitting can underestimate galaxy masses: a solution to the missing mass problem

Sorba

Sawicki

2018

Monthly Notices of the Royal Astronomical Society

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We perform spatially-resolved, pixel-by-pixel SED fitting on galaxies up to z ∼ 2.5 in the Hubble Extreme Deep Field (XDF). Comparing stellar mass estimates from spatially resolved and spatially unresolved photometry we find that unresolved masses can be systematically underestimated by factors of up to 5. The ratio of the unresolved to resolved mass measurement depends on the galaxy's specific star formation rate (sSFR): at low sSFRs the bias is small, but above sSFR ∼ 10 −9.5 yr −1 the discrepancy increases rapidly such that galaxies with sSFRs ∼ 10 −8 yr −1 have unresolved mass estimates of only one half to one fifth of the resolved value. This result indicates that stellar masses estimated from spatially-unresolved datasets need to be systematically corrected, in some cases by large amounts, and we provide an analytic prescription for applying this correction. We show that correcting stellar mass measurements for this bias changes the normalization and slope of the star-forming main sequence and reduces its intrinsic width; most dramatically, correcting for the mass bias increases the stellar mass density of the Universe at high redshift and can resolve the long-standing discrepancy between the directly-measured cosmic star formation rate density at z > ∼ 1 and that inferred from stellar mass densities ("the missing mass problem").

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The evolving relation between star formation rate and stellar mass in the VIDEO survey sincez = 3

Cited by 78 publications

References 119 publications

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

H2-based star formation laws in hierarchical models of galaxy formation

Spatially unresolved SED fitting can underestimate galaxy masses: a solution to the missing mass problem

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