Deep Extragalactic VIsible Legacy Survey (DEVILS): SED fitting in the D10-COSMOS field and the evolution of the stellar mass function and SFR–<i>M</i>⋆ relation

Thorne, Jessica E.; Robotham, Aaron S. G.; Davies, Luke J. M.; Bellstedt, Sabine; Driver, Simon P.; Bravo, Matías; Bremer, M. N.; Holwerda, Benne W.; Hopkins, A. M.; Lagos, Claudia del P.; Phillipps, Steven; Siudek, M.; Taylor, Edward N.; Wright, Angus H.

doi:10.1093/mnras/stab1294

Cited by 81 publications

(154 citation statements)

References 177 publications

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“…Figure 21 shows the distribution of these spec-zs. In the future, there will be more public spectroscopic redshifts from surveys such as CSI (e.g., Kelson et al 2014), DEVILS (e.g., Davies et al 2018;Thorne et al 2021), DESI (e.g., Levi et al 2019), MOONS (e.g., Maiolino et al 2020), andWAVES (e.g., Driver et al 2019).…”

Section: Spectroscopic Redshiftsmentioning

confidence: 99%

The XMM-SERVS Survey: XMM-Newton Point-source Catalogs for the W-CDF-S and ELAIS-S1 Fields

Brandt

Chen

et al. 2021

ApJS

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We present the X-ray point-source catalogs in two of the XMM-Spitzer Extragalactic Representative Volume Survey (XMM-SERVS) fields, W-CDF-S (4.6 deg 2 ) and ELAIS-S1 (3.2 deg 2 ), aiming to fill the gap between deep pencil-beam X-ray surveys and shallow X-ray surveys over large areas. The W-CDF-S and ELAIS-S1 regions were targeted with 2.3 and 1.0 Ms of XMM-Newton observations, respectively; 1.8 and 0.9 Ms exposures remain after flare filtering. The survey in W-CDF-S has a flux limit of 1.0 × 10 −14 erg cm −2 s −1 over 90% of its area in the 0.5-10 keV band; 4053 sources are detected in total. The survey in ELAIS-S1 has a flux limit of 1.3 × 10 −14 erg cm −2 s −1 over 90% of its area in the 0.5-10 keV band; 2630 sources are detected in total. Reliable optical-to-IR multiwavelength counterpart candidates are identified for ≈89% of the sources in W-CDF-S and ≈87% of the sources in ELAIS-S1. A total of 3129 sources in W-CDF-S and 1957 sources in ELAIS-S1 are classified as active galactic nuclei (AGNs). We also provide photometric redshifts for X-ray sources; ≈84% of the 3319/2001 sources in W-CDF-S/ELAIS-S1 with optical-to-near-IR forced photometry available have either spectroscopic redshifts or high-quality photometric redshifts. The completion of the XMM-Newton observations in the W-CDF-S and ELAIS-S1 fields marks the end of the XMM-SERVS survey data gathering. The ≈12,000 pointlike X-ray sources detected in the whole ≈13 deg 2 XMM-SERVS survey will benefit future large-sample AGN studies.

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Section: Spectroscopic Redshiftsmentioning

confidence: 99%

The XMM-SERVS Survey: XMM-Newton Point-source Catalogs for the W-CDF-S and ELAIS-S1 Fields

Brandt

Chen

et al. 2021

ApJS

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“…In this work, we utilize the derived galaxy properties and redshifts for galaxies in the D10 region discussed in Thorne et al ( 2021 ). Briefly, Thorne et al ( 2021 ) fit galaxies in the D10 region using the PROSPECT (Robotham et al 2020 ) SED fitting code to derive galaxy properties such as stellar mass, SFR, SFH, and metallicity from FUV-FIR photometry derived using PROFOUND (Robotham et al 2018 ). They discuss the validity of these measurements and then perform a detailed analysis of the evolution of the SFR-M * relation and stellar mass function.…”

Section: Sample Selection and Fitting Rangesmentioning

confidence: 99%

“…Man y studies have measured the non-linearity and flattening of the SFS at high stellar masses (e.g. Rodighiero et al 2010 ;Elbaz et al 2011 ;Whitaker et al 2012 ;Lee et al 2015 ;Katsianis, Tescari & Wyithe 2016 ;Grootes et al 2017Grootes et al , 2018Thorne et al 2021 ), and various astrophysical processes ha ve been inv oked that dri ve the most massi v e galaxies a way from the linear SFS (e.g. Abramson et al 2014 ;Willett et al 2015 ;Erf anianf ar et al 2016 ;Cook et al 2020 ).…”

Section: Introductionmentioning

confidence: 99%

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Deep Extragalactic VIsible Legacy Survey (DEVILS): evolution of the σSFR–M⋆ relation and implications for self-regulated star formation

Davies

Thorne

Bellstedt

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the evolution of the star-formation dispersion - stellar mass relation (σSFR-M⋆) in the DEVILS D10 region using new measurements derived using the ProSpect spectral energy distribution fitting code. We find that σSFR-M⋆ shows the characteristic ‘U-shape’ at intermediate stellar masses from 0.1 < z < 0.7 for a number of metrics, including using the deconvolved intrinsic dispersion. A physical interpretation of this relation is the combination of stochastic star-formation and stellar feedback causing large scatter at low stellar masses and AGN feedback causing asymmetric scatter at high stellar masses. As such, the shape of this distribution and its evolution encodes detailed information about the astrophysical processes affecting star-formation, feedback and the lifecycle of galaxies. We find that the stellar mass that the minimum σSFR occurs evolves linearly with redshift, moving to higher stellar masses with increasing lookback time and traces the turnover in the star-forming sequence. This minimum σSFR point is also found to occur at a fixed specific star-formation rate (sSFR) at all epochs (sSFR∼10−9.6 Gyr−1). The physical interpretation of this is that there exists a maximum sSFR at which galaxies can internally self-regulate on the tight sequence of star-formation. At higher sSFRs, stochastic stellar processes begin to cause galaxies to be pushed both above and below the star-forming sequence leading to increased SFR dispersion. As the Universe evolves, a higher fraction of galaxies will drop below this sSFR threshold, causing the dispersion of the low-stellar mass end of the star-forming sequence to decrease with time.

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“…Pier & Krolik 1992 ;Granato & Danese 1994 ;Efstathiou & Rowan-Robinson 1995 ;Fritz, Franceschini & Hatziminaoglou 2006 ;Nenkova et al 2008 ;Stalevski et al 2012Stalevski et al , 2016Siebenmorgen, Heymann & Efstathiou 2015 ;Tanimoto et al 2019 ), which are fitted together with dust emissions and stellar populations (e.g. Calistro Rivera et al 2016 ;Leja et al 2018 ;Boquien et al 2019 ) in different configurations (check Thorne et al 2021 ;P érez-Torres et al 2021 , for an o v erview of the most popular SED fitting codes). SED models without an AGN contribution do not provide the adequate physical properties of AGNs (e.g.…”

mentioning

confidence: 99%

The viewing angle in AGN SED models: a data-driven analysis

Padilla

Wang

Małek

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The validity of the unified active galactic nuclei (AGN) model has been challenged in the last decade, especially when different types of AGNs are considered to only differ in the viewing angle to the torus. We aim to assess the importance of the viewing angle in classifying different types of Seyfert galaxies in spectral energy distribution (SED) modelling. We retrieve photometric data from publicly available astronomical databases: CDS and NED, to model SEDs with X-CIGALE in a sample of 13 173 Seyfert galaxies located at redshift range from z = 0 to z = 3.5, with a median redshift of z ≈ 0.2. We assess whether the estimated viewing angle from the SED models reflects different Seyfert classifications. Two AGN models with either a smooth or clumpy torus structure are adopted in this paper. We find that the viewing angle in Type-1 AGNs is better constrained than in Type-2 AGNs. Limiting the viewing angles representing these two types of AGNs do not affect the physical parameter estimates such as star-formation rate (SFR) or AGN fractional contribution (fAGN). In addition, the viewing angle is not the most discriminating physical parameter to differentiate Seyfert types. We suggest that the observed and intrinsic AGN disc luminosity can: i) be used in z < 0.5 studies to distinguish between Type-1 and Type-2 AGNs, and ii) explain the probable evolutionary path between these AGN types. Finally, we propose the use of X-CIGALE for AGN galaxy classification tasks. All data from the 13 173 SED fits are available at Zenodo.†

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Deep Extragalactic VIsible Legacy Survey (DEVILS): SED fitting in the D10-COSMOS field and the evolution of the stellar mass function and SFR–M⋆ relation

Cited by 81 publications

References 177 publications

The XMM-SERVS Survey: XMM-Newton Point-source Catalogs for the W-CDF-S and ELAIS-S1 Fields

The XMM-SERVS Survey: XMM-Newton Point-source Catalogs for the W-CDF-S and ELAIS-S1 Fields

Deep Extragalactic VIsible Legacy Survey (DEVILS): evolution of the σSFR–M⋆ relation and implications for self-regulated star formation

The viewing angle in AGN SED models: a data-driven analysis

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