Physical properties of the CDFS X-ray sources through fitting spectral energy distributions

Guo, Xiaotong; Gu, Qing; Ding, Nan; Contini, E.; Chen, Yongyun

doi:10.1093/mnras/stz3589

Cited by 10 publications

(22 citation statements)

References 67 publications

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“…To further identify potentially omissive or mis-identified AGN candidates selected according to the MIR colors, we directly model the UV to far-IR SEDs of our cSFGs to constrain their AGN contribution, employing the CIGALE code (Burgarella et al 2005;Noll et al 2009;Boquien et al 2019). In this work, following Guo et al (2020), for each source in our sample we firstly fit its SED by utilizing the galaxy and galaxy+AGN templates, and then find the best-fit SED iteratively. There are 4 modules in the galaxy templates, which are the star formation history, the Calzetti et al (2000) dust attenuation, the Bruzual & Charlot (2003) stellar population synthesis models with the Chabrier (2003) IMF and solar metallicity, and the Dale et al (2014) dust emission.…”

Section: Compact Agn Selectionmentioning

confidence: 99%

“…Moreover, the SED fitting technique using the observed multi-band SED is now a widely-used technique to decompose the AGN/host components and derive properties of AGN host galaxies (Ciesla et al 2015;Ma lek et al 2018;Gao et al 2019). Guo et al (2020) derive the physical parameters of 791 X-ray sources (518 AGNs and 273 normal galaxies) by fitting their SEDs using the Code Investigating GALaxy Evolution code (CIGALE 0.12.1, Burgarella et al 2005;Noll et al 2009;Boquien et al 2019). Six AGN candidates are selected from the 273 normal galaxies based on their SEDs, and two of the six AGN candidates can also be identified by their X-ray variabilities (Ding et al 2018).…”

Section: Introductionmentioning

confidence: 99%

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The Compact Star-forming Galaxies at 2 < z < 3 in 3D-HST/CANDELS: AGN and Non-AGN Physical Properties

Fang³

et al. 2020

PASP

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We investigate the differences in the stellar population properties, the structure, and the environment between massive compact star-forming galaxies (cSFGs) with or without active galactic nucleus (AGN) at 2 < z < 3 in the five 3D-HST/CANDELS fields. In a sample of 221 massive cSFGs, we constitute the most complete AGN census so far, identifying 66 AGNs by the X-ray detection, the mid-infrared color criterion, and/or the SED fitting, while the rest (155) are non-AGNs. Further dividing these cSFGs into two redshift bins, i.e., 2 < z < 2.5 and 2.5 ≤ z < 3, we find that in each redshift bin the cSFGs with AGNs have similar distributions of the stellar mass, the specific star formation rate, and the ratio of L IR to L UV to those without AGNs. After having performed a two-dimensional surface brightness modeling for those cSFGs with X-ray-detected AGNs (37) to correct for the influence of the central point-like X-ray AGN on measuring the structural parameters of its host galaxy, we find that in each redshift bin the cSFGs with AGNs have comparable distributions of all concerned structural parameters, i.e., the Sersic index, the 20%-light radius, the Gini coefficient, and the concentration index, to those without AGNs. With a gradual consumption of available gas and dust, the structure of cSFGs, indicated by the above structural parameters, seem to be slightly more concentrated with decreasing redshift. At 2 < z < 3, the similar environment between cSFGs with and without AGNs suggests that their AGN activities are potentially triggered by internal secular processes, such as gravitational instabilities or/and dynamical friction.

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Section: Compact Agn Selectionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Compact Star-forming Galaxies at 2 < z < 3 in 3D-HST/CANDELS: AGN and Non-AGN Physical Properties

Fang³

et al. 2020

PASP

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“…Straatman et al (2016) provided photometric catalogs (from UV to IR; a total of 43 bands) for the CDFS survey. In order to obtain the photometric data of the X-ray sources in the CDFS survey, Guo et al (2020) have cross-matched the X-ray catalog (Luo et al 2017) and the photometric catalog (Straatman et al 2016) with a matching radius of 1 arcsec. The matching results contained 839 X-ray sources.…”

Section: The Agn Samplementioning

confidence: 99%

“…The matching results contained 839 X-ray sources. Based on the sample used in Guo et al (2020), we further select our AGN sample using the following three criteria: 1) A source is classified as AGN by X-ray. This source can also be selected as AGN by its spectral energy distribution (SED, Pouliasis et al 2020).…”

Section: The Agn Samplementioning

confidence: 99%

“…SED fitting technique can also constrain some crucially physical quantities of both AGNs and host galaxies, such as AGN luminosity, AGN fraction, SFR, and stellar mass (M * ). Guo et al (2020) obtained some physical quantities (including AGN luminosity, AGN fraction, SFR, M * , dust luminosity, AGN type, and rest-frame 6 µm luminosity for AGN component) of all AGNs in our sample through SED fitting using photometric data from UV to IR. Therefore, some physical quantities used in this work are from Guo et al (2020).…”

Section: Multi-band Sed Fitting and Mid-ir Datamentioning

confidence: 99%

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Multi-wavelength Selected Compton-thick AGNs in Chandra Deep Field-South Survey

Guo,

Gu,

Ding

et al. 2020

Preprint

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Even in deep X-ray surveys, Compton-thick active galactic nuclei (CT AGNs, N H 1.5 × 10 24 cm −2 ) are difficult to be identified due to X-ray flux suppression and their complex spectral shape. However, the study of CT AGNs is vital for understanding the rapid growth of black holes and the origin of cosmic X-ray background. In the local universe, the fraction of CT AGNs accounts for 30% of the whole AGN population. We may expect a higher fraction of CT AGNs in deep X-ray surveys, however, only 10% of AGNs have been identified as CT AGNs in the 7 Ms Chandra Deep Field-South (CDFS) survey. In this work, we select 51 AGNs with abundant multi-wavelength data. Using the method of the midinfrared (mid-IR) excess, we select hitherto unknown 8 CT AGN candidates in our sample. Seven of these candidates can confirm as CT AGN based on the multi-wavelength identification approach, and a new CT AGN (XID 133) is identified through the mid-IR diagnostics. We also discuss the X-ray origin of these eight CT AGNs and the reason why their column densities were underestimated in previous studies. We find that the multi-wavelength approaches of selecting CT AGNs are highly efficient, provided the high quality of observational data. We also find that CT AGNs have a higher Eddington ratio than non-CT AGNs, and that both CT AGNs and non-CT AGNs show similar properties of host galaxies.

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Tracing obscured galaxy build-up at high redshift using deep radio surveys

Amarantidis,

Afonso,

Matute

et al. 2023

A&A

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Context. A fundamental question of extra-galactic astronomy that is yet to be fully understood, concerns the evolution of the star formation rate (SFR) and supermassive black hole (SMBH) activity with cosmic time, as well as their interplay and how it impacts galaxy evolution. A primary focus that could shed more light on these questions is the study of merging systems, comprising highly star-forming galaxies (SFGs) and active galactic nuclei (AGN) at the earliest stages of galactic formation. However, considering the challenges associated with identifying these objects, it is essential to explore complementary selection methods across multiple wavelengths. Aims. The primary objective of this study is to conduct a comprehensive analysis of a sample of high-redshift (z > 3) far-infrared (far-IR) and radio-emitting galaxies in the highest possible spatial resolution. The aim is to study the properties of this population, such as their morphological characteristics, and to explore the interplay of SFR and SMBH activity at this epoch. Methods. In order to select the galactic population of our interest, we employed two selection criteria that have frequently been used as separate methods in the literature. In more detail, we selected galaxies that present relatively compact radio morphologies at 1.4 GHz (i.e., an angular size smaller than 10 arcsec) as well as a far-IR spectrum that peaks in flux at λ ≥ 350 μm (i.e., flux350 μm > flux250 μm). For these selection criteria, we used the COSMOS and ECDF-S fields, two of the most extensively observed astronomical fields currently available, which provide high spectral and spatial resolution at a multi-wavelength scale. By accepting only galaxies that satisfied these selection criteria, we derived a sample of eight galaxies that were identified either photometrically or spectroscopically at z > 3 from literature studies and by our team. Results. A thorough investigation of available optical, near-IR, and millimetre (mm) imaging reveals a possible merging scenario in five out of eight cases in our sample. Additionally, available multi-wavelength photometry strongly suggests active star formation at the 103 M⊙ yr−1 level in massive systems (stellar masses of M⋆ ∼ 1011 M⊙) co-hosting an active SMBH. Conclusions. Comparison of these results with previous studies, suggests that our selection method preferentially identifies galaxies hosting an active SMBH, as well as a strong SFG component, resulting in high SFR and IR luminosity. An additional examination of the efficacy of the radio and far-IR selection criteria provides further support for their combined application in selecting co-evolving AGN and star formation activity at high redshift. In this regard, future use of these selection criteria on radio and far-IR/mm observations of statistically larger galaxy samples is of high interest.

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Physical properties of the CDFS X-ray sources through fitting spectral energy distributions

Cited by 10 publications

References 67 publications

The Compact Star-forming Galaxies at 2 < z < 3 in 3D-HST/CANDELS: AGN and Non-AGN Physical Properties

The Compact Star-forming Galaxies at 2 < z < 3 in 3D-HST/CANDELS: AGN and Non-AGN Physical Properties

Multi-wavelength Selected Compton-thick AGNs in Chandra Deep Field-South Survey

Tracing obscured galaxy build-up at high redshift using deep radio surveys

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