XXL-HSC: Link between AGN activity and star formation in the early Universe (<i>z</i>⩾ 3.5)

Pouliasis, E.; Mountrichas, G.; Georgantopoulos, I.; Ruiz, Ángel Liceras; Gilli, R.; Koulouridis, E.; Akiyama, Masayuki; Ueda, Yoshihiro; Garrel, C.; Nagao, Tohru; Paltani, S.; Pierre, M.; Toba, Yoshiki; Vignali, C.

doi:10.1051/0004-6361/202243502

Cited by 16 publications

(6 citation statements)

References 137 publications

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“…This method has been applied by Shimizu et al (2015Shimizu et al ( , 2017 in hard (14-195 keV) X-ray selected AGN from the Swift Burst Alert Telescope (BAT) and more recently by Mountrichas et al (2021cMountrichas et al ( , 2022c. The limitation of this method is the available number of reference galaxies at a given M , z bin (Pouliasis et al 2022). Here, we compare the SFR of X-ray AGN with that of normal galaxies.…”

Section: Derivation Of the Normalised Star-formationmentioning

confidence: 99%

Comparing the host galaxy ages of X-ray selected AGN in COSMOS

I.¹,

E.²,

Mountrichas³

et al. 2023

A&A

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We explore the properties of the host galaxies of X-ray selected AGN in the COSMOS field using the Chandra Legacy sample and the LEGA-C survey VLT optical spectra. Our main goal is to compare the relative ages of the host galaxies of the obscured and unobscured AGN by means of the calcium break D n (4000) and the H δ Balmer line. The host galaxy ages are examined in conjunction with other properties such as the galaxy stellar mass, and star-formation rate as well as the AGN Eddington ratio. Our sample consists of 50 unobscured or mildly obscured (N H < 10 23 cm −2 ) and 23 heavily obscured AGN (N H > 10 23 cm −2 ) in the redshift range z = 0.6 − 1. We take specific caution to create control samples in order to match the exact luminosity and redshift distributions for the obscured and unobscured AGN. The majority of unobscured AGN appear to live in young galaxies in contrast to the obscured AGN which appear to live in galaxies located between the young and old galaxy populations. This finding may be in contrast to those evolutionary AGN unification models which postulate that the AGN begin their life in a heavy obscuration phase. The host galaxies of the obscured AGN have significantly lower levels of specific star-formation. At the same time the obscured AGN have lower Eddington ratios indicating a link between the star-formation and the black hole accretion. We find that the distribution of the stellar masses of the host galaxies of obscured AGN is skewed towards higher stellar masses in agreement with previous findings. Our results on the relative age of obscured AGN are valid when we match our obscured and unobscured AGN samples according to the stellar mass of their host galaxies. All the above results become less conspicuous when a lower column density (log N H (cm −2 ) = 21.5 or 22) is used to separate the obscured and unobscured AGN populations.

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Section: Derivation Of the Normalised Star-formationmentioning

confidence: 99%

Comparing the host galaxy ages of X-ray selected AGN in COSMOS

I.¹,

E.²,

Mountrichas³

et al. 2023

A&A

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“…This value has been used in previous studies (e.g. Masoura et al 2018;Buat et al 2021;Mountrichas et al 2022c,a;Koutoulidis et al 2022;Pouliasis et al 2022) and is based on visual inspection of the SEDs. This requirement was met by 78% of the sources.…”

Section: Selection Criteria and Final Samplesmentioning

confidence: 99%

“…Previous studies have employed these ranges for the selection of reliable SFR and M * estimations while leveraging the CIGALE code (e.g. Mountrichas et al 2021aMountrichas et al ,c, 2022cMountrichas et al ,a,b, 2023Mountrichas & Shankar 2023;Buat et al 2021;Koutoulidis et al 2022;Pouliasis et al 2022). Mountrichas et al (2021c) explored variations in the range, considering 0.1−0.33 for the lower limit and 3−10 for the upper limit.…”

Section: Selection Criteria and Final Samplesmentioning

confidence: 99%

The link among X-ray spectral properties, AGN structure, and the host galaxy

Mountrichas,

Viitanen,

Carrera

et al. 2024

A&A

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In this work, we compare the supermassive black hole (SMBH) and host galaxy properties of X-ray obscured and unobscured AGN. For that purpose, we used $ 35\,000$ X-ray detected AGN in the 4XMM-DR11 catalogue for which there are available measurements for their X-ray spectral parameters, such as the hydrogen column density, N$_H$, and photon index, Gamma , from the XMM2Athena Horizon 2020 European project. We constructed the spectral energy distributions (SEDs) of the sources, and we calculated the host galaxy properties via SED fitting analysis, utilising the CIGALE code. We applied strict photometric requirements and quality selection criteria to include only sources with robust X-ray and SED fitting measurements. Our sample consists of 1\,443 AGN. In the first part of our analysis, we used different N$_H$ thresholds $) while also taking into account the uncertainties associated with the N$_H$ measurements in order to classify these sources as obscured and unobscured (or mildly obscured). We find that obscured AGN tend to live in more massive systems (by $ 0.1$\,dex) that have a lower star-formation rate, SFR, (by $ 0.25$\,dex) compared to their unobscured counterparts. However, only the difference in stellar mass, M$_*$, appears statistically significant ($>2 The results do not depend on the N$_H$ threshold used to classify AGN. The differences in M$_*$ and SFR are not statistically significant for luminous AGN ($ X,2-10\,KeV )> 44$). Our findings also show that unobscured AGN have, on average, higher specific black hole accretion rates, $ sBHAR $, compared to their obscured counterparts, a parameter which is often used as a proxy of the Eddington ratio. In the second part of our analysis, we cross-matched the 1\,443 X-ray AGN with the SDSS DR16 quasar catalogue of Wu and Shen to obtain information on the SMBH properties of our sources. This resulted in 271 type 1 AGN at $ z<1.9$. Our findings show that type 1 AGN with increased N$_H$ $) tend to have higher black hole masses, M$_ BH $, compared to AGN with lower N$_H$ values at similar M$_*$. The M$_ BH $, but it exhibits signs of increasing at higher N$_H$ values. Finally, we detected a correlation between Gamma and Eddington ratios, but only for type 1 sources with N$_H<10^

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“…Through this analysis, the reliability of the obtained estimations for the physical parameters was estimated. A full description of this process can be found in a paper by Boquien et al (2019; see also Ciesla et al 2015Ciesla et al , 2016Toba et al 2019bToba et al , 2020aPouliasis et al 2022).…”

Section: Mock Analysismentioning

confidence: 99%

Active Galactic Nucleus Properties of ∼1 Million Member Galaxies of Galaxy Groups and Clusters at z < 1.4 Based on the Subaru Hyper Suprime-Cam Survey

Toba,

Hashiguchi,

Ota

et al. 2024

ApJ

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Herein, we present the statistical properties of active galactic nuclei (AGNs) for approximately 1 million member galaxies of galaxy groups and clusters with 0.1 < cluster redshift (z cl) < 1.4 selected using the Subaru Hyper Suprime-Cam, the so-called CAMIRA clusters. In this research, we focused on the AGN power fraction (f AGN), which is defined as the proportion of the contribution of AGNs to the total infrared (IR) luminosity, L IR (AGN)/L IR, and examined how f AGN depends on (i) z cl and (ii) the distance from the cluster center. We compiled multiwavelength data using the ultraviolet–mid-IR range. Moreover, we performed spectral energy distribution fits to determine f AGN using the CIGALE code with the SKIRTOR AGN model. We found that (i) the value of f AGN in the CAMIRA clusters is positively correlated with z cl, with the correlation slope being steeper than that for field galaxies, and (ii) f AGN exhibits a high value at the cluster outskirts. These results indicate that the emergence of the AGN population depends on the redshift and environment and that galaxy groups and clusters at high redshifts are important in AGN evolution. Additionally, we demonstrated that cluster–cluster mergers may enhance AGN activity at the outskirts of particularly massive galaxy clusters. Our findings are consistent with a related study on the CAMIRA clusters that was based on the AGN number fraction.

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XXL-HSC: Link between AGN activity and star formation in the early Universe (z⩾ 3.5)

Cited by 16 publications

References 137 publications

Comparing the host galaxy ages of X-ray selected AGN in COSMOS

Comparing the host galaxy ages of X-ray selected AGN in COSMOS

The link among X-ray spectral properties, AGN structure, and the host galaxy

Active Galactic Nucleus Properties of ∼1 Million Member Galaxies of Galaxy Groups and Clusters at z < 1.4 Based on the Subaru Hyper Suprime-Cam Survey

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