THE INTRINSIC SCATTER ALONG THE MAIN SEQUENCE OF STAR-FORMING GALAXIES AT<i>z</i>∼ 0.7

Guo, Kaihua; Zheng, Xian Zhong; Fu, Hai

doi:10.1088/0004-637x/778/1/23

Cited by 68 publications

(100 citation statements)

References 82 publications

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“…Our finding also provides a window to interpret the intrinsic scatter of the star formation main sequence (MS) of local SFGs. Recently, Guo et al (2013Guo et al ( , 2015 found that the intrinsic scatter of the low-z MS increases with M * , which is not reported in other similar studies (e.g., Whitaker et al 2012). In the context of this work, Guo et al's findings seem to be more reasonable since many massive SFGs have been partly quenched (see Figure 5).…”

Section: Sample Selectionmentioning

confidence: 81%

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: Sample Selectionmentioning

confidence: 81%

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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“…We use the ultra-deep H-band catalogs provided by the CANDELS-HST team (Grogin et al 2011;Koekemoer et al 2011) in three of the CANDELS fields, namely GOODSSouth (GS Guo et al 2013), UDS (Galametz et al 2013), and COSMOS (Nayyeri et al, in prep.). With the GOODS-North (GN) CANDELS catalog not being finalized at the time of writing, we fall back to a ground-based K s -band catalog.…”

Section: Sample and Observationsmentioning

confidence: 99%

“…In GOODS-South, UDS and COSMOS CANDELS we use the official CANDELS catalogs presented, respectively, in Guo et al (2013;version 121114), Galametz et al (2013;version 120720) and Nayyeri et al (in prep., version 130701). They are built using SExtractor in dual image mode, using the HST H-band image as the detection image to extract the photometry at the other HST bands.…”

Section: Goods-south Uds and Cosmos Candelsmentioning

confidence: 99%

TheHerschelview of the dominant mode of galaxy growth fromz= 4 to the present day

Schreiber

Pannella

Elbaz

et al. 2015

A&A

803

181

1,372

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We present an analysis of the deepest Herschel images in four major extragalactic fields GOODS-North, GOODS-South, UDS, and COSMOS obtained within the GOODS-Herschel and CANDELS-Herschel key programs. The star formation picture provided by a total of 10 497 individual far-infrared detections is supplemented by the stacking analysis of a mass complete sample of 62 361 starforming galaxies from the Hubble Space Telescope (HST) H band-selected catalogs of the CANDELS survey and from two deep ground-based K s band-selected catalogs in the GOODS-North and the COSMOS-wide field to obtain one of the most accurate and unbiased understanding to date of the stellar mass growth over the cosmic history. We show, for the first time, that stacking also provides a powerful tool to determine the dispersion of a physical correlation and describe our method called "scatter stacking", which may be easily generalized to other experiments. The combination of direct UV and far-infrared UV-reprocessed light provides a complete census on the star formation rates (SFRs), allowing us to demonstrate that galaxies at z = 4 to 0 of all stellar masses (M * ) follow a universal scaling law, the so-called main sequence of star-forming galaxies. We find a universal close-to-linear slope of the log 10 (SFR)-log 10 (M * ) relation, with evidence for a flattening of the main sequence at high masses (log 10 (M * /M ) > 10.5) that becomes less prominent with increasing redshift and almost vanishes by z 2. This flattening may be due to the parallel stellar growth of quiescent bulges in star-forming galaxies, which mostly happens over the same redshift range. Within the main sequence, we measure a nonvarying SFR dispersion of 0.3 dex: at a fixed redshift and stellar mass, about 68% of star-forming galaxies form stars at a universal rate within a factor 2. The specific SFR (sSFR = SFR/M * ) of star-forming galaxies is found to continuously increase from z = 0 to 4. Finally we discuss the implications of our findings on the cosmic SFR history and on the origin of present-day stars: more than two-thirds of present-day stars must have formed in a regime dominated by the "main sequence" mode. As a consequence we conclude that, although omnipresent in the distant Universe, galaxy mergers had little impact in shaping the global star formation history over the last 12.5 billion years.

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“…Additionally, the slope and redshift evolution of the MS normalization have been discussed in the context of feedback processes and gas exhaustion with cosmic time, respectively (e.g. Noeske et al 2007a;Zheng et al 2007;Tacconi et al 2013;Guo et al 2013). Correlations between galaxy structural parameters, SFR and stellar mass (e.g.…”

Section: Introductionmentioning

confidence: 99%

Constraining the properties of AGN host galaxies with spectral energy distribution modelling

Ciesla

Charmandaris

Georgakakis

et al. 2015

A&A

233

354

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Detailed studies of the spectral energy distribution (SED) of normal galaxies have increasingly been used to understand the physical mechanism dominating their integrated emission, mainly owing to the availability of high quality multi-wavelength data from the UV to the far-infrared (FIR). However, systems hosting dust-enshrouded nuclear starbursts and/or an accreting supermassive black hole (an active galactic nucleus or AGN) are especially challenging to study. This is due to the complex interplay between the heating by massive stars and the AGN, the absorption and emission of radiation from dust, as well as the presence of the underlying old stellar population. We used the latest release of CIGALE, a fast state-of-the-art galaxy SED-fitting model relying on energy balance, to study the influence of an AGN in a self consistent manner in estimating both the star formation rate (SFR) and stellar mass in galaxies, as well as to calculate the contribution of the AGN to the power output of the host. Using the semi-analytical galaxy formation model , we created a suite of mock galaxy SEDs using realistic star formation histories (SFH). We also added an AGN of Type-1, Type-2, or intermediate-type whose contribution to the bolometric luminosity can be variable. We performed an SED-fitting of these catalogues with CIGALE, assuming three different SFHs: a single-exponentially-decreasing (1τ-dec), a double-exponentiallydecreasing (2τ-dec), and a delayed SFH. Constraining the overall contribution of an AGN to the total infrared luminosity (frac AGN ) is very challenging for frac AGN < 20%, with uncertainties of ∼5-30% for higher fractions depending on the AGN type, while FIR and sub-mm are essential. The AGN power has an impact on the estimation of M * in Type-1 and intermediate-type AGNs but has no effect on galaxies hosting Type-2 AGNs. We find that in the absence of AGN emission, the best estimates of M * are obtained using the 2τ-dec model but at the expense of realistic ages of the stellar population. The delayed SFH model provides good estimates of M * and SFR, with a maximum offset of 10% as well as better estimates of the age. Our analysis shows that the under-estimation of the SFR increases with frac AGN for Type-1 systems, as well as for low contributions of an intermediate AGN type, but it is quite insensitive to the emission of Type-2 AGNs up to frac AGN ∼ 45%. A lack of sampling the FIR, or sub-mm domain systematically over-estimates the SFR (<20%), independent of the contribution of the AGN. Similarly, the UV emission is critical in accurately retrieving both the M * for Type-1 and intermediate-type AGN and the SFR of all three AGN types. We show that the presence of AGN emission introduces a scatter to the SFR-M * main sequence relation derived from SED-fitting, which is driven by the uncertainties on M * . Finally, we used our mock catalogues to test the popular IR SED-fitting code DIR and show that frac AGN is under-estimated but that the SFR is recovered well for Type-1 and intermedia...

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THE INTRINSIC SCATTER ALONG THE MAIN SEQUENCE OF STAR-FORMING GALAXIES ATz∼ 0.7

Cited by 68 publications

References 82 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

TheHerschelview of the dominant mode of galaxy growth fromz= 4 to the present day

Constraining the properties of AGN host galaxies with spectral energy distribution modelling

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