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

I., Georgantopoulos,; E., Pouliasis,; Mountrichas, G.; Wel, Arjen van der; S., Marchesi,; Lanzuisi, G.

doi:10.1051/0004-6361/202244875

Cited by 14 publications

(27 citation statements)

References 126 publications

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“…These studies have shown that X-ray absorbed AGN exhibit, on average, lower n Edd compared to their X-ray unabsorbed counterparts (Ricci et al 2017;Ananna et al 2022;Georgantopoulos et al 2023), in agreement with our findings.…”

Section: Obscuration and Eddington Ratiosupporting

confidence: 93%

“…Mountrichas et al (submitted) built upon these insights by employing X-ray AGN data from the 4XMM catalog and implementing rigorous X-ray criteria for AGN classification. Their results closely mirrored those obtained by Georgantopoulos et al (2023), reinforcing the observed differences in host galaxy properties between X-ray obscured and unobscured AGN. Moreover, their analysis highlighted that these distinctions tend to diminish for luminous AGN.…”

Section: Introductionsupporting

confidence: 82%

“…Our findings align with the results of these previous studies. Different M * for the different AGN populations have also been reported by studies that used X-ray classifcation criteria (Lanzuisi et al 2017;Georgantopoulos et al 2023, but see Masoura et al 2021;Mountrichas et al 2021a).…”

Section: Discussionmentioning

confidence: 65%

“…For instance, using the hydrogen column density , N H , and a threshold at N H = 10 21.5 cm −2 (or N H = 10 22 cm −2 ), previous studies found no significant differences regarding the SFR and stellar mass, M * , of galaxies hosting Xray absorbed and unabsorbed AGN (e.g., Masoura et al 2021;Mountrichas et al 2021c). More recently, Georgantopoulos et al (2023), adopted a higher N H threshold (N H = 10 23 cm −2 ) and found that the two AGN populations live in galaxies with statistically significant differences (> 2σ) in terms of their SFR and M * . Moreover, X-ray absorbed sources tend to exhibit lower specific black hole accretion rates, λ sBHAR , which serves as a proxy for the Eddington ratio, compared to their unabsorbed counterparts.…”

Section: Introductionmentioning

confidence: 99%

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The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

Mountrichas

2023

A&A

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It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, M BH , and the galaxy bulge or stellar mass, M * . The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the M BH −M * relation, using 687 X-ray luminous (median log [L X,2−10keV (ergs −1 )] = 44.3), broad-line active galactic nuclei (AGN), at 0.2 < z < 4.0 (median z ≈ 1.4) that lie in the XMM-XXL field. Their M BH and M * range from 7.5 < log [M BH (M )] < 9.5 and 10 < log [M * (M )] < 12, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that M BH and M * are correlated (r = 0.47 ± 0.21, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the M BH and M * does not evolve with redshift, at least up to z = 2 and has a value of log(M BH /M * ) = −2.44. The majority of the AGN (75%) are in a SMBH mass growth-dominant phase. In these systems, the M BH −M * correlation is weaker and their M * tends to be lower (for the same M BH ) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.

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Section: Obscuration and Eddington Ratiosupporting

confidence: 93%

Section: Introductionsupporting

confidence: 82%

Section: Discussionmentioning

confidence: 65%

Section: Introductionmentioning

confidence: 99%

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The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

Mountrichas

2023

A&A

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“…Our findings align with this trend, yet the distinction is less prominent, despite being consistently observed across various L X . Previous studies have found differences in the SFR of AGN host galaxies for different obscuration levels, in particular for AGN with modest L X (Georgantopoulos et al 2023;Mountrichas & Georgantopoulos 2024;Mountrichas et al 2024b). The COSMOS field benefits from deeper observations compared to the XMM-XXL, resulting in a higher number of AGN in COSMOS that exhibit elevated obscuration levels.…”

Section: Comparison Of the Sfr Of Agn And Non-agn Galaxies As A Funct...mentioning

confidence: 95%

Comparison of star formation histories of AGN and non-AGN galaxies

Mountrichas

Buat

Yang

et al. 2022

A&A

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We use AGN with X-ray luminosities, L X,2−10keV ∼ 10 42.5−44 erg s −1 , from the COSMOS-Legacy survey that lie within the UltraVISTA region and cross match them with the LEGA-C catalogue. The latter provides measurements of the calcium break, D n 4000, and H δ Balmer line that allow us to study the stellar populations of AGN and compare them with a galaxy reference catalogue. Our samples consist of 69 AGN and 2176 non-AGN systems, within 0.6 < z < 1.3, that satisfy the same photometric selection criteria. We construct the SEDs of both population and use the CIGALE code to investigate the effect of the two indices in the SED fitting process. Our analysis shows that the inclusion of D n 4000 and H δ allows CIGALE to constrain better the ages of the stellar populations. Furthermore, we find an increase of the estimated stellar masses by, on average, ∼ 0.2 dex, in particular for systems with young stars (D n 4000 < 1.5), when the two indices are included in the SED fitting. We then compare the D n 4000 and H δ of AGN with sources in the reference catalogue, accounting for the different stellar mass of the two populations. Our analysis reveals that low to moderate L X AGN tend to reside in galaxies with older stellar populations and are less likely to have experienced a recent star formation burst, compared to galaxies in the control sample. Finally, we compare the two populations as a function of their morphology (bulgedominated, BD, vs. non-BD) and compactness (mass-to-size ratio). A similar fraction of AGN and non-AGN systems are classified as non-BD (∼ 70%). Our analysis shows that BD AGN tend to have younger stellar populations compared to BD, non-AGN systems. On the other hand, non-BD AGN have, on average, older stellar populations and are less likely to have experienced a burst compared to non-BD sources in the reference sample. Furthermore, AGN tend to prefer more compact systems compared to non-AGN.

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Link between star formation and the properties of supermassive black holes

Mountrichas,

Buat

2023

A&A

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It is well known that supermassive black holes (SMBHs) and their host galaxies undergo a process of co-evolution. Feedback from active galactic nuclei (AGNs) plays an important role in this symbiosis. To study the effect of AGN feedback on the host galaxy, one popular method is to study the star formation rate (SFR) as a function of the X-ray luminosity (LX). However, hydrodynamical simulations suggest that the cumulative impact of AGN feedback on a galaxy is encapsulated in the mass of the SMBH, MBH, rather than the LX. In this study, we compare the SFRs of AGN and non-AGN galaxies as a function of LX, MBH, the Eddington ratio (nEdd), and the specific black hole accretion rate (λsBHAR). For that purpose, we used 122 X-ray AGN in the XMM-XXL field and 3371 galaxies from the VIPERS survey to calculate the SFRnorm parameter, defined as the ratio of the SFR of AGN to the SFR of non-AGN galaxies with similar stellar mass, M*, and redshift. Our datasets span a redshift range of 0.5 ≤ z ≤ 1.2. The results show that the correlation between SFRnorm and MBH is stronger compared to that between SFRnorm and LX. A weaker correlation is found between SFRnorm and λsBHAR. No correlation is detected between SFRnorm and nEdd. These results corroborate the notion that the MBH is a more robust tracer of the cumulative impact of the AGN feedback, compared to the instantaneous accretion rate (LX). Thus, it may serve as a better predictive parameter of changes in the SFR of the host galaxy.

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

Cited by 14 publications

References 126 publications

The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

Comparison of star formation histories of AGN and non-AGN galaxies

Link between star formation and the properties of supermassive black holes

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