Using Machine Learning to Determine Morphologies of z &lt; 1 AGN Host Galaxies in the Hyper Suprime-Cam Wide Survey

Tian, Chan; Urry, C. Megan; Ghosh, Aritra; Ofman, Ryan; Ananna, Tonima Tasnim; Auge, Connor; Cappelluti, N.; Powell, Meredith C.; Sanders, D. B.; Schawinski, Kevin; Stark, Dominic; Tremblay, G. R.

doi:10.3847/1538-4357/acad79

Cited by 3 publications

(1 citation statement)

References 80 publications

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“…The much weaker correlation found in our data implies that the AHA sample is not dominated by bulge or spheroidal galaxies and likely has many more disk galaxies, merging systems, or point sources. A detailed analysis of the host galaxies' morphology for each one of these sources is ongoing in the AHA collaboration (Schawinski et al 2014;Powell et al 2017;Ghosh et al 2022;Tian et al 2023).…”

Section: Cold Dust Emissionmentioning

confidence: 99%

The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei

Auge,

Sanders,

Treister

et al. 2023

ApJ

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Spectral energy distributions (SEDs) from X-ray to far-infrared (FIR) wavelengths are presented for a sample of 1246 X-ray-luminous active galactic nuclei (AGNs; L 0.5–10 keV > 1043 erg s−1), with z spec < 1.2, selected from Stripe 82X, COSMOS, and GOODS-N/S. The rest-frame SEDs show a wide spread (∼2.5 dex) in the relative strengths of broad continuum features at X-ray, ultraviolet (UV), mid-infrared (MIR), and FIR wavelengths. A linear correlation (log–log slope of 0.7 ± 0.04) is found between L MIR and L X. There is significant scatter in the relation between the L UV and L X owing to heavy obscuration; however, the most luminous and unobscured AGNs show a linear correlation (log–log slope of 0.8 ± 0.06) in the relation above this scatter. The relation between L FIR and L X is predominantly flat, but with decreasing dispersion at L X > 1044 erg s−1. The ratio between the “galaxy-subtracted” bolometric luminosity and the intrinsic L X increases from a factor of ∼10 to 70 from log L bol/(erg s−1) = 44.5 to 46.5. Characteristic SED shapes have been determined by grouping AGNs based on relative strengths of the UV and MIR emission. The average L 1μm is constant for the majority of these SED shapes, while AGNs with the strongest UV and MIR emission have elevated L 1μm, consistent with the AGN emission dominating their SEDs at optical and near-infrared wavelengths. A strong correlation is found between the SED shape and both the L X and L bol, such that L bol/L X = 20.4 ± 1.8, independent of the SED shape. This is consistent with an evolutionary scenario of increasing L bol with decreasing obscuration as the AGN blows away circumnuclear gas.

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Section: Cold Dust Emissionmentioning

confidence: 99%

The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei

Auge,

Sanders,

Treister

et al. 2023

ApJ

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Resolving cosmic star formation histories of present-day bulges, discs, and spheroids with ProFuse

Bellstedt,

Robotham,

Driver

et al. 2024

Monthly Notices of the Royal Astronomical Society

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We present the first look at star formation histories of galaxy components using ProFuse, a new technique to model the 2D distribution of light across multiple wavelengths using simultaneous spectral and spatial fitting of purely imaging data. We present a number of methods to classify galaxies structurally/morphologically, showing the similarities and discrepancies between these schemes. We show the variation in component-wise mass functions that can occur simply due to the use of a different classification method, which is most dramatic in separating bulges and spheroids. Rather than identifying the best-performing scheme, we use the spread of classifications to quantify uncertainty in our results. We study the cosmic star formation history (CSFH), forensically derived using ProFuse with a sample of ∼7,000 galaxies from the Galaxy And Mass Assembly (GAMA) survey. Remarkably, the forensic CSFH recovered via both our method (ProFuse) and traditional SED fitting (ProSpect) are not only exactly consistent with each other over the past 8 Gyr, but also with the in-situ CSFH measured using ProSpect. Furthermore, we separate the CSFH by contributions from spheroids, bulges and disks. While the vast majority (70%) of present-day star formation takes place in the disk population, we show that 50% of the stars that formed at cosmic noon (8-12 Gyr ago) now reside in spheroids, and present-day bulges are composed of stars that were primarily formed in the very early Universe, with half their stars already formed ∼12 Gyr ago.

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Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses

LaMassa,

Peca,

Urry

et al. 2024

ApJ

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We present the third catalog release of the wide-area (31.3 deg2) Stripe 82 X-ray survey. This catalog combines previously published X-ray source properties with multiwavelength counterparts and photometric redshifts, presents 343 new spectroscopic redshifts, and provides black hole masses for 1297 Type 1 active galactic nuclei (AGN). With spectroscopic redshifts for 3457 out of 6181 Stripe 82X sources, the survey has a spectroscopic completeness of 56%. This completeness rises to 90% when considering the contiguous portions of the Stripe 82X survey with homogeneous X-ray coverage at an optical magnitude limit of r < 22. Within that portion of the survey, 23% of AGN can be considered obscured by being either a Type 2 AGN, reddened (R − K > 4, Vega), or X-ray obscured with a column density of N H > 1022 cm−2. Unlike other surveys, there is only an 18% overlap between Type 2 and X-ray obscured AGN. We calculated black hole masses for Type 1 AGN that have Sloan Digital Sky Survey spectra using virial mass estimators calibrated on the Hβ, Mg ii, Hα, and C iv emission lines. We find wide scatter in these black hole mass estimates, indicating that statistical analyses should use black hole masses calculated from the same formula to minimize bias. We find that the AGN with the highest X-ray luminosities are accreting at the highest Eddington ratios, consistent with the picture that most black hole mass accretion happens in the phase when the AGN is luminous (L 2−10keV > 1045 erg s−1).

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Using Machine Learning to Determine Morphologies of z < 1 AGN Host Galaxies in the Hyper Suprime-Cam Wide Survey

Cited by 3 publications

References 80 publications

The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei

The Accretion History of AGN: The Spectral Energy Distributions of X-Ray-luminous Active Galactic Nuclei

Resolving cosmic star formation histories of present-day bulges, discs, and spheroids with ProFuse

Stripe 82X Data Release 3: Multiwavelength Catalog with New Spectroscopic Redshifts and Black Hole Masses

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