Galaxy properties of type 1 and 2 X-ray selected AGN and comparison among different classification criteria

Mountrichas, G.; Buat, V.; Georgantopoulos, I.; Yang, G.; Masoura, V. A.; Boquien, M.; Burgarella, D.

doi:10.48550/arxiv.2106.11579

Cited by 3 publications

(3 citation statements)

References 51 publications

(91 reference statements)

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“…Furthermore, there are no differences between the PDFs for SFR of Type-I and Type-II QSOs, consistent with previous work (e.g. Shangguan & Ho 2019;Mountrichas et al 2021).…”

Section: The Star Formation Rates Of Radio Agnssupporting

confidence: 91%

Quantifying the cool ISM in radio AGNs: evidence for late-time re-triggering by galaxy mergers and interactions

Bernhard,

Tadhunter,

Pierce

et al. 2022

Preprint

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We use deep Herschel observations of the complete 2Jy sample of powerful radio AGNs in the local universe (0.05 < z < 0.7) to probe their cool interstellar medium (ISM) contents and star-forming properties, comparing them against other samples of nearby luminous AGNs and quiescent galaxies. This allows us to investigate triggering and feedback mechanisms. We find that the dust masses of the strong-line radio galaxies (SLRGs) in our sample are similar to those of radio-quiet quasars, and that their median dust mass (M dust = 2 × 10 7 M ) is enhanced by a factor ∼200 compared to that of non-AGN ellipticals, but lower by a factor ∼16 relative to that of local ultra-luminous infrared galaxies (UILRGs). Along with compelling evidence for merger signatures in optical images, the SLRGs in our sample also show relatively high starformation efficiencies, despite the fact that many of them fall below the main sequence for star forming galaxies. Together, these results suggest that most of our SLRGs have been re-triggered by late-time mergers that are relatively minor in terms of their gas contents. In comparison with the SLRGs, the radio AGNs with weak optical emission lines (WLRGs) and edge-darkened radio jets (FRIs) have both lower cool ISM masses and star-formation rates (by a factor of >30), consistent with being fuelled by a different mechanism (e.g. the direct accretion of hot gas).

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“…Furthermore, there are no differences between the PDFs for SFR of Type-I and Type-II QSOs, consistent with previous work (e.g. Shangguan & Ho 2019;Mountrichas et al 2021).…”

Section: The Star Formation Rates Of Radio Agnssupporting

confidence: 91%

Quantifying the cool ISM in radio AGNs: evidence for late-time re-triggering by galaxy mergers and interactions

Bernhard,

Tadhunter,

Pierce

et al. 2022

Preprint

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“…Studying the link between galaxies and black holes requires us to measure physical properties associated with both, and has been attempted in numerous previous works (e.g. Merloni et al 2010;Bongiorno et al 2012;Azadi et al 2015;Circosta, C. et al 2019;Mountrichas et al 2021;Pouliasis et al 2020).…”

Section: Introductionmentioning

confidence: 99%

“…Bayesian techniques are also increasingly being employed to constrain SED properties (e.g. Calistro Rivera et al 2016) with greater awareness of some of the potential pitfalls of interpreting simple maximum likelihood estimates (Mountrichas et al 2021).…”

Section: Introductionmentioning

confidence: 99%

A fresh look at AGN spectral energy distribution fitting with the XMM-SERVS AGN sample

Marshall

Auger-Williams

Banerji

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We perform spectral energy distribution (SED) fitting to 711 luminous X-ray AGN at 0.7 < z < 4.5 using 10-bands of optical and infra-red photometric data for objects within XMM-SERVS. This fitting provided 510 reliable (reduced χ2 < 3) inferences on AGN and host galaxy properties. The AGN optical (3000 Å) luminosity inferred from SED-fitting is found to correlate with the measured X-ray (2–10 keV) luminosity, in good agreement with previous work. Using X-ray hardness as a proxy for AGN obscuration, we also study the differences in the host galaxy properties of obscured and unobscured AGNs. Both populations have consistent stellar masses (log10(M*/M⊙) = 10.88 $\pm 0.09\, {\rm M}_\odot$ and log10(M*/M⊙) = 10.8 $\pm 0.1\, {\rm M}_\odot$ for unobscured and obscured AGNs, respectively). We also find evidence for varying AGN emission line properties from a standard AGN template in 18.8 per cent of the sample with a reduced χ2 < 3 where the inclusion of an additional emission line strength free parameter was found to improve the quality of the fit. Comparison of these fits to SDSS spectra showed that emission line properties inferred from broad-band photometry were consistent with the results from spectroscopy for 91 per cent of objects. We find that the presence of weaker, more blueshifted emission lines as inferred from the SED fits are associated with more negative values of αox. While the correlation between the hardness of the ionizing SED and the emission line properties has been known for some time, we are able to derive this correlation purely from broad-band photometry.

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A Fresh Look at AGN Spectral Energy Distribution Fitting with the XMM-SERVS AGN Sample

Marshall,

Auger-Williams,

Banerji

et al. 2022

Preprint

View full text Add to dashboard Cite

We perform spectral energy distribution (SED) fitting to 711 luminous X-ray AGN at 0.7 < 𝑧 < 4.5 using 10-bands of optical and infra-red photometric data for objects within XMM-SERVS. This fitting provided 510 reliable (reduced 𝜒 2 < 3) inferences on AGN and host galaxy properties. The AGN optical (3000Å) luminosity inferred from SED-fitting is found to correlate with the measured X-ray (2-10 keV) luminosity, in good agreement with previous work. Using X-ray hardness as a proxy for AGN obscuration, we also study the differences in the host galaxy properties of obscured and unobscured AGN. Both populations have consistent stellar masses (log 10 (𝑀 * /𝑀 ) = 10.88 ±0.09𝑀 and log 10 (𝑀 * /𝑀 ) = 10.8 ±0.1𝑀 for unobscured and obscured AGN respectively). We also find evidence for varying AGN emission line properties from a standard AGN template in 18.8% of the sample with a reduced 𝜒 2 < 3 where the inclusion of an additional emission line strength free parameter was found to improve the quality of the fit. Comparison of these fits to SDSS spectra showed that emission line properties inferred from broadband photometry were consistent with the results from spectroscopy for 91% of objects. We find that the presence of weaker, more blueshifted emission lines as inferred from the SED fits are associated with more negative values of 𝛼 𝑜𝑥 . While the correlation between the hardness of the ionising SED and the emission line properties has been known for some time, we are able to derive this correlation purely from broadband photometry.

show abstract

Galaxy properties of type 1 and 2 X-ray selected AGN and comparison among different classification criteria

Cited by 3 publications

References 51 publications

Quantifying the cool ISM in radio AGNs: evidence for late-time re-triggering by galaxy mergers and interactions

Quantifying the cool ISM in radio AGNs: evidence for late-time re-triggering by galaxy mergers and interactions

A fresh look at AGN spectral energy distribution fitting with the XMM-SERVS AGN sample

A Fresh Look at AGN Spectral Energy Distribution Fitting with the XMM-SERVS AGN Sample

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