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

Mountrichas, G.; Buat, V.; Yang, Guang; Boquien, M.; Ni, Quan Xing; Pouliasis, E.; Burgarella, D.; Theulé, Patrice; Georgantopoulos, I.

doi:10.1051/0004-6361/202244495

Cited by 12 publications

(22 citation statements)

References 111 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The CIGALE code provides stellar ages estimates. However, Mountrichas et al (2022b) caution that the CIGALE estimates have limited accuracy if they are not combined with D n and H δ measurements. Hence, they developed a variant of the CIGALE code which uses both these indices to estimate the mass weighted galaxy ages.…”

Section: Stellar Agesmentioning

confidence: 99%

“…As this code is not publicly available, we can rely on their galaxy age methodology. This is possible because the LEGA-C COSMOS sample used by Mountrichas et al (2022b) is practically identical to our sample and moreover they use the same parameter grid for their SED fitting. Mountrichas et al (2022b) derive the spectral age index using both the D n and EW(H δ ) measurements.…”

Section: Stellar Agesmentioning

confidence: 99%

“…This is possible because the LEGA-C COSMOS sample used by Mountrichas et al (2022b) is practically identical to our sample and moreover they use the same parameter grid for their SED fitting. Mountrichas et al (2022b) derive the spectral age index using both the D n and EW(H δ ) measurements. This index combines D n and H δ to construct the distribution of galaxies along the diagonal distribution on the D n − H δ plane (see Wu et al 2018).…”

Section: Stellar Agesmentioning

confidence: 99%

See 2 more Smart Citations

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

I.¹,

E.²,

Mountrichas³

et al. 2023

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Stellar Agesmentioning

confidence: 99%

Section: Stellar Agesmentioning

confidence: 99%

Section: Stellar Agesmentioning

confidence: 99%

See 1 more Smart Citation

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

I.¹,

E.²,

Mountrichas³

et al. 2023

A&A

View full text Add to dashboard Cite

show abstract

“…Nevertheless, in both lower mass and more massive galaxies the SFR of AGN was similar to that of non-AGN systems (Mountrichas et al 2021(Mountrichas et al , 2022c. These results were also supported by studying the stellar populations of lowto-moderate L X AGN compared to non-AGN systems (Mountrichas et al 2022b).…”

Section: Introductionmentioning

confidence: 52%

“…In Mountrichas et al (2022b), we examined the SFH of AGN and non-AGN galaxies and we found that AGN of low-to-moderate L X (log [L X,2−10keV (erg s −1 )] < 44) tend to have older stellar populations and are less likely to have experienced a recent star formation burst compared to non-AGN systems. Here, we study the SFH of the two populations, but, in addition, we take into account their cosmic environment (Sect.…”

Section: Star-formation Historymentioning

confidence: 99%

The relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

Mountrichas

Yang

Buat

et al. 2023

A&A

Self Cite

View full text Add to dashboard Cite

In this work, we study the relation of the cosmic environment and morphology with the star formation and stellar population of galaxies. Most importantly, we examine if this relation differs for systems with active and non-active supermassive black holes. For that purpose, we used 551 X-ray detected active galactic nuclei (AGNs) and 16 917 non-AGN galaxies in the COSMOS-Legacy survey for which surface-density field measurements are available. The sources lie at a redshift of 0.3 < z < 1.2, probe X-ray luminosities of 42 < log[LX,2−10 keV(erg s−1)] < 44, and have stellar masses of 10.5 < log [M*(M⊙)] < 11.5. Our results show that isolated AGNs (field) have lower star formation rates (SFRs) compared to non-AGNs at all LX spanned by our sample. However, in denser environments (filaments and clusters), moderate LX AGN (log[LX,2−10 keV(erg s−1)] > 43) and non-AGN galaxies have similar SFRs. We also examined the stellar populations and the morphology of the sources in different cosmic fields. For the same morphological type, we find that non-AGN galaxies tend to have older stellar populations and are less likely to have undergone a recent burst in denser environments compared to their field counterparts. The differences in the stellar populations concerning density field are mainly driven by quiescent systems. Moreover, low LX AGNs present negligible variations of their stellar populations in all cosmic environments, whereas moderate LX AGNs have, on average, younger stellar populations and are more likely to have undergone a recent burst in high-density fields. Finally, in the case of non-AGN galaxies, the fraction of bulge-dominated (BD) systems increases with the density field, while BD AGNs are scarce in denser environments. Our results are consistent with a scenario in which a common mechanism, such as mergers, triggers both the star-formation and the AGN activity.

show abstract

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

Mountrichas

2023

A&A

View full text Add to dashboard Cite

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.

show abstract

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

Cited by 12 publications

References 111 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 relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

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

Contact Info

Product

Resources

About