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Enhanced active galactic nucleus activity in overdense galactic environments at 2 < z < 4.

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Τίτλος: Enhanced active galactic nucleus activity in overdense galactic environments at 2 < z < 4.
Συγγραφείς: Shah, Ekta A., Lemaux, Brian C., Forrest, Ben, Hathi, Nimish, Shen, Lu, Cucciati, Olga, Hung, Denise, Giddings, Finn, Sikorski, Derek, Lubin, Lori, Gal, Roy R., Zamorani, Giovanni, Golden-Marx, Emmet, Bardelli, Sandro, Cassarà, Letizia Pasqua, Garilli, Bianca, Gururajan, Gayathri, Suh, Hyewon, Vergani, Daniela, Zucca, Elena
Πηγή: Astronomy & Astrophysics / Astronomie et Astrophysique; 2025, Vol. 704, p1-16, 16p
Θεματικοί όροι: Active galactic nuclei, Redshift, Galaxy clusters, Astronomy, Photometry, Spectrum analysis instruments
Περίληψη: We carried out a study on the relationship between galaxy environments and their active galactic nucleus (AGN) activity at high redshifts (2.0 < z < 4.0). Specifically, we studied the AGN fraction in galaxies residing in a range of environments at these redshifts, from field galaxies to the densest regions of highly overdense peaks in the GOODS-S extragalactic field. Utilizing the extensive photometric and spectroscopic observations in this field, we measured the local overdensities (σδ) and global overdensities across a broad a range of environments, including those in massive (Mtot ≥ 1014.8 M⊙) protostructures. We employed a multiwavelength AGN catalog consisting of AGNs in nine different categories. Our analysis shows a higher AGN fraction (10.9−2.3+3.6%) for galaxies in the highest local overdensity regions compared to the AGN fraction (1.9−0.3+0.4%) in the corresponding coeval field galaxies (a ∼4σ difference). This trend of increasing AGN fraction in denser environments relative to the field is present in all redshift bins. We also find this trend to be consistent across all five AGN categories that have a sufficient number of AGNs to make a meaningful comparison: the mid-infrared (MIR) spectral energy distribution (SED), MIR color, X-ray luminosity, X-ray-luminosity-to-radio-luminosity-ratio, and optical-spectroscopy. Our results also demonstrate a clear trend for higher (∼4×) AGN fractions in denser local overdensity environments for a given stellar mass. Additionally, we observe the same trend (though at a lower significance) with the global environment of galaxies, measured using a metric based on the projected distance of galaxies from their nearest massive (Mtot > 1012.8 M⊙) overdense (σδ > 5.0) peak, normalized with respect to the size of the peak. These findings indicate that the prevalence of AGN activity is highly dependent on the environment a host galaxy resides in, even at early times in the formation history of the Universe. [ABSTRACT FROM AUTHOR]
Copyright of Astronomy & Astrophysics / Astronomie et Astrophysique is the property of EDP Sciences and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Enhanced active galactic nucleus activity in overdense galactic environments at 2 &lt; z &lt; 4.
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  Data: Astronomy &amp; Astrophysics / Astronomie et Astrophysique; 2025, Vol. 704, p1-16, 16p
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  Data: We carried out a study on the relationship between galaxy environments and their active galactic nucleus (AGN) activity at high redshifts (2.0 &lt; z &lt; 4.0). Specifically, we studied the AGN fraction in galaxies residing in a range of environments at these redshifts, from field galaxies to the densest regions of highly overdense peaks in the GOODS-S extragalactic field. Utilizing the extensive photometric and spectroscopic observations in this field, we measured the local overdensities (σ&lt;subscript&gt;δ&lt;/subscript&gt;) and global overdensities across a broad a range of environments, including those in massive (M&lt;subscript&gt;tot&lt;/subscript&gt; ≥ 10&lt;superscript&gt;14.8&lt;/superscript&gt; M&lt;subscript&gt;⊙&lt;/subscript&gt;) protostructures. We employed a multiwavelength AGN catalog consisting of AGNs in nine different categories. Our analysis shows a higher AGN fraction (10.9&lt;subscript&gt;−2.3&lt;/subscript&gt;&lt;superscript&gt;+3.6&lt;/superscript&gt;%) for galaxies in the highest local overdensity regions compared to the AGN fraction (1.9&lt;subscript&gt;−0.3&lt;/subscript&gt;&lt;superscript&gt;+0.4&lt;/superscript&gt;%) in the corresponding coeval field galaxies (a ∼4σ difference). This trend of increasing AGN fraction in denser environments relative to the field is present in all redshift bins. We also find this trend to be consistent across all five AGN categories that have a sufficient number of AGNs to make a meaningful comparison: the mid-infrared (MIR) spectral energy distribution (SED), MIR color, X-ray luminosity, X-ray-luminosity-to-radio-luminosity-ratio, and optical-spectroscopy. Our results also demonstrate a clear trend for higher (∼4&#215;) AGN fractions in denser local overdensity environments for a given stellar mass. Additionally, we observe the same trend (though at a lower significance) with the global environment of galaxies, measured using a metric based on the projected distance of galaxies from their nearest massive (M&lt;subscript&gt;tot&lt;/subscript&gt; &gt; 10&lt;superscript&gt;12.8&lt;/superscript&gt; M&lt;subscript&gt;⊙&lt;/subscript&gt;) overdense (σ&lt;subscript&gt;δ&lt;/subscript&gt; &gt; 5.0) peak, normalized with respect to the size of the peak. These findings indicate that the prevalence of AGN activity is highly dependent on the environment a host galaxy resides in, even at early times in the formation history of the Universe. [ABSTRACT FROM AUTHOR]
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  Data: &lt;i&gt;Copyright of Astronomy &amp; Astrophysics / Astronomie et Astrophysique is the property of EDP Sciences and its content may not be copied or emailed to multiple sites without the copyright holder&#39;s express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.&lt;/i&gt; (Copyright applies to all Abstracts.)
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