The Host Galaxies of X-Ray Quasars Are Not Strong Star Formers

Barger, A. J.; Cowie, L. L.; Owen, F. N.; Chen, Chian-Chou; Hasinger, G.; Hsu, Li‐Che; Li, Y.

doi:10.1088/0004-637x/801/2/87

Cited by 42 publications

(59 citation statements)

References 127 publications

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“…Observationally, there has been growing evidence that supports this scenario (Schawinski et al 2006;Fabian 2012;Maiolino et al 2012;Page et al 2012;Barger et al 2015). Recent progresses have confirmed the tight correlation between quiescence and the presence of a dense galaxy inner structure, whatever is parameterized by n (Bell et al 2004(Bell et al , 2012Driver et al 2006;Cheung et al 2012), by the inner 1 kpc stellar mass density (Cheung et al 2012;Fang et al 2013;Woo et al 2015) or by bulge mass (Bluck et al 2014;Lang et al 2014).…”

Section: Bulge Growth and Star Formation Quenchingmentioning

confidence: 95%

THE SPATIALLY RESOLVED NUV–r COLOR OF LOCAL STAR-FORMING GALAXIES AND CLUES FOR QUENCHING

Pan

Zheng

Lin

et al. 2016

ApJ

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Using a sample of ∼6000 local face-on star-forming galaxies (SFGs) we examine the correlations between the NUV-r colors both inside and outside the half-light radius, stellar mass M * , and Sérsic index n to understand how the quenching of star formation is linked to galaxy structure. For these less dust-attenuated galaxies, NUV-r is found to be linearly correlated with D 4000 n , supporting NUV-r as a good photometric indicator of stellar age (or specific star formation rate). First, we find that at M M 10 10.2 * <  the central NUV-r is on average only ∼0.25 mag redder than the outer NUV-r; the intrinsic value would be even smaller after accounting for dust correction. However, the central NUV-r becomes systematically much redder than the outer NUV-r for more massive galaxies at M M 10 10.2 * >  . Second, the central NUV-r shows no dependence on Sérsic index n at M M 10 10.2 * <  , while above this mass galaxies with a higher n tend to be redder in the central NUV-r color. These results suggest that galaxies with M M 10 10.2 * <  exhibit similar star formation activity from the inner R R 50 < region to the R R 50 > region. In contrast, a considerable fraction of the M M 10 10.2 * >  galaxies, especially those with a high n, have harbored a relatively inactive bulge component.

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Section: Bulge Growth and Star Formation Quenchingmentioning

confidence: 95%

THE SPATIALLY RESOLVED NUV–r COLOR OF LOCAL STAR-FORMING GALAXIES AND CLUES FOR QUENCHING

Pan

Zheng

Lin

et al. 2016

ApJ

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“…In Figure 13, we show the two brightest examples out of the three SCUBA-2 sources that do not have 24 μm counterparts. Since these sources are isolated, following Barger et al (2015), we used matched-filter extractions to measure the FIR fluxes for these sources.…”

Section: Mir and Fir Fluxesmentioning

confidence: 99%

A Submillimeter Perspective on the GOODS Fields (SUPER GOODS). I. An Ultradeep SCUBA-2 Survey of the GOODS-N* † ‡ §

Cowie

Barger

Hsu

et al. 2017

ApJ

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117

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In this first paper in the SUPER GOODS series on powerfully star-forming galaxies in the two GOODS fields, we present a deep SCUBA-2 survey of the GOODS-N at both 850 and 450 μm (central rms noise of 0.28 mJy and 2.6 mJy, respectively). In the central region, the 850 μm observations cover the GOODS-N to near the confusion limit of ∼1.65 mJy, while over a wider 450 arcmin2 region—well complemented by Herschel far-infrared imaging—they have a median limit of 3.5 mJy. We present catalogs of 186 850 μm and 31 450 μm selected sources. We use interferometric observations from the Submillimeter Array (SMA) and the Karl G. Jansky Very Large Array (VLA) to obtain precise positions for 114 SCUBA-2 sources (28 from the SMA, all of which are also VLA sources). We present new spectroscopic redshifts and include all existing spectroscopic or photometric redshifts. We also compare redshifts estimated using the 20 cm/850 μm and the 250 cm/850 μm flux ratios. We show that the redshift distribution increases with increasing flux, and we parameterize the dependence. We compute the star formation history and the star formation rate (SFR) density distribution functions in various redshift intervals, finding that they reach a peak at before dropping to higher redshifts. We show that the number density per unit volume of galaxies measured from the SCUBA-2 sample does not change much relative to that of lower SFR galaxies from UV selected samples over , suggesting that, apart from changes in the normalization, the shape in the number density as a function of SFR is invariant over this redshift interval.

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“…Controversial results were found for AGN host galaxies: some studies have indicated equivalent or enhanced star formation compared to normal star-forming galaxies (e.g., Silverman et al 2009;Mullaney et al 2012;Rosario et al 2012;Santini et al 2012;Juneau et al 2013), whereas some others have shown that AGN host galaxies lie below the MS of star-forming galaxies, suggesting that AGN accretion might suppress and eventually quench star formation via a process of feedback (e.g., Barger et al 2015;Mullaney et al 2015;Riguccini et al 2015;Shimizu et al 2015). Furthermore, several studies have addressed that the majority of AGN host galaxies in the local universe are preferentially found in the green valley on the color-magnitude diagram, transitioning from star-forming galaxies in the blue cloud to passive galaxies on the red sequence (e.g., Schawinski et al 2009;Trump et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching

Suh

Civano

Hasinger

et al. 2017

ApJ

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We investigate the star formation properties of a large sample of ∼2300 X-ray-selected Type 2 Active Galactic Nuclei (AGNs) host galaxies out to z 3 in the Chandra COSMOS Legacy Survey in order to understand the connection between the star formation and nuclear activity. Making use of the existing multi-wavelength photometric data available in the COSMOS field, we perform a multi-component modeling from far-infrared to near-ultraviolet using a nuclear dust torus model, a stellar population model and a starburst model of the spectral energy distributions (SEDs). Through detailed analyses of SEDs, we derive the stellar masses and the star formation rates (SFRs) of Type 2 AGN host galaxies. The stellar mass of our sample is in the range of M M 9 log 12 stellar < <  with uncertainties of ∼0.19 dex. We find that Type 2 AGN host galaxies have, on average, similar SFRs compared to the normal star-forming galaxies with similar M stellar and redshift ranges, suggesting no significant evidence for enhancement or quenching of star formation. This could be interpreted in a scenario, where the relative massive galaxies have already experienced substantial growth at higher redshift (z 3 > ), and grow slowly through secular fueling processes hosting moderate-luminosity AGNs.

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The Host Galaxies of X-Ray Quasars Are Not Strong Star Formers

Cited by 42 publications

References 127 publications

THE SPATIALLY RESOLVED NUV–r COLOR OF LOCAL STAR-FORMING GALAXIES AND CLUES FOR QUENCHING

THE SPATIALLY RESOLVED NUV–r COLOR OF LOCAL STAR-FORMING GALAXIES AND CLUES FOR QUENCHING

A Submillimeter Perspective on the GOODS Fields (SUPER GOODS). I. An Ultradeep SCUBA-2 Survey of the GOODS-N* † ‡ §

Type 2 AGN Host Galaxies in the Chandra-COSMOS Legacy Survey: No Evidence of AGN-driven Quenching

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