An Overdensity of Red Galaxies around the Hyperluminous Dust-obscured Quasar W1835+4355 at z = 2.3

Luo, Yibin; Fan, Lulu; Zou, Hu; Shen, Lu; Lin, Zhoubin; Hu, Weida; Lin, Zheyu; Tao, Bojun; Chen, Guangwen

doi:10.3847/1538-4357/ac8162

Cited by 5 publications

(8 citation statements)

References 76 publications

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“…5. The W2246−0526 overdense environment is qualitatively consistent with statistical studies of Spitzer/IRAC and submillimeter companions to Hot DOGs (Assef et al 2015;Jones et al 2014;Fan et al 2017) and with recent observational studies of the environment around the Hot DOGs W0410 at z=3.6 (Ginolfi et al 2022) and W1835 at z=2.35 (Luo et al 2022). 6.…”

Section: Discussionsupporting

confidence: 87%

“…The overdensity around high-redshift radio galaxies, quasars, and Hot DOGs as a function of redshift. We highlight the studies based on LBGs around quasars (magenta triangles,Zheng et al 2006;Morselli et al 2014;Balmaverde et al 2017;García-Vergara et al 2017), around radio galaxies (magenta circles,Miley et al 2004;Intema et al 2006;Overzier et al 2008) and Hot DOGs (magenta star, this work), those based on LAEs around quasars (blue triangles, García-Vergara et al 2019), radio galaxies (blue circles,Venemans et al 2002Venemans et al , 2004Venemans et al , 2005Venemans et al , 2007Miley et al 2004), and Hot DOGs (blue star,Ginolfi et al 2022) and a study based on DRGs around Hot DOGs (cyan star,Luo et al 2022). Overdensities of 24µm sources around high-redshift radio galaxies are also shown (gray dot,Mayo et al 2012).…”

mentioning

confidence: 84%

“…Specifically, they found the number density of Lyα emitters within 0.4 Mpc of W0410-0913 to be 14 +16 −8 times that of field galaxies with comparable Lyα luminosity. Also recently, Luo et al (2022) studied the environment of W1835+4355 at z = 2.3 and found a factor of two enhancement in the number of DRGs in its surroundings. The overdensity differences between these studies may be indicative of the diversity of the environments around Hot DOGs, but may also be driven by the specific selection methods used in each study.…”

Section: Overdensities Around Hot Dogsmentioning

confidence: 98%

“…Multiwavelength observations of Hot DOGs have statistically shown that these objects are likely to live in dense environments (Jones et al 2014;Assef et al 2015;Penney et al 2019). More recently, Luo et al (2022) found an overdensity of distant red galaxies (DRGs) around a Hot DOG at z = 2.3, while Ginolfi et al (2022) revealed an overdensity of LAEs in the environment of a z = 3.6 Hot DOG with VLT/MUSE observations. All of this evidence suggests that Hot DOGs exist in overdense regions of the Universe, where significant gas accretion can be maintained and mergers could lead to large-scale obscuration.…”

Section: Introductionmentioning

confidence: 99%

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An overdensity of Lyman break galaxies around the hot dust-obscured galaxy WISE J224607.56−052634.9

Zewdie¹,

Assef²,

Mazzucchelli³

et al. 2023

A&A

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We report the identification of Lyman Break Galaxy (LBG) candidates around the most luminous Hot Dust-Obscured Galaxy (Hot DOG) known, WISE J224607.56−052634.9 (W2246−0526) at z = 4.601, using deep r-, i-, and z-band imaging from the Gemini Multi-Object Spectrograph South (GMOS-S). We use the surface density of LBGs to probe the Mpc-scale environment of W2246−0526 to characterize its richness and evolutionary state. We identify LBG candidates in the vicinity of W2246−0526 using the selection criteria developed by Ouchi et al. (2004) and Yoshida et al. (2006) in the Subaru Deep Field and in the Subaru XMM-Newton Deep Field, slightly modified to account for the difference between the filters used, and we find 37 and 55 LBG candidates, respectively. Matching to the z-band depths of those studies, this corresponds to δ = 5.8 +2.4 −1.9 times the surface density of LBGs expected in the field. Interestingly, the Hot DOG itself, as well as a confirmed neighbor, do not satisfy either LBG selection criteria, suggesting we may be missing a large number of companion galaxies. Our analysis shows that we are most likely only finding those with higher-than-average IGM optical depth or moderately high dust obscuration. The number density of LBG candidates is not concentrated around W2246−0526, suggesting either an early evolutionary stage for the proto-cluster or that the Hot DOG may not be the most massive galaxy, or that the Hot DOG may be affecting the IGM transparency in its vicinity. The overdensity around W2246−0526 is comparable to overdensities found around other Hot DOGs and is somewhat higher than typically found for radio galaxies and luminous quasars at a similar redshift.

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Section: Discussionsupporting

confidence: 87%

mentioning

confidence: 84%

Section: Overdensities Around Hot Dogsmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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An overdensity of Lyman break galaxies around the hot dust-obscured galaxy WISE J224607.56−052634.9

Zewdie¹,

Assef²,

Mazzucchelli³

et al. 2023

A&A

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“…The X-ray observations of Hot DOGs consistently find high column densities that are close to Compton thick (Stern et al 2014;Piconcelli et al 2015;Assef et al 2016;Ricci et al 2017;Vito et al 2018;Zappacosta et al 2018;Assef et al 2020). The environments where Hot DOGs reside were found to be significantly overdense (Jones et al 2015;Silva et al 2015;Jones et al 2017;Penney et al 2019;Ginolfi et al 2022;Luo et al 2022;Zewdie et al 2023). All results are generally consistent with the merger-driven coevolution scenario.…”

Section: Introductionsupporting

confidence: 66%

Physical Properties of Hyperluminous, Dust-obscured Quasars at z ∼ 3: Multiwavelength Spectral Energy Distribution Analysis and Cold Gas Content Revealed by ALMA

Sun 孙,

Fan 范,

Han 韩

et al. 2024

ApJ

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We present a UV to millimeter spectral energy distribution (SED) analysis of 16 hyperluminous, dust-obscured quasars at z ∼ 3, selected by the Wide-field Infrared Survey Explorer. We aim to investigate the physical properties of these quasars, with a focus on their molecular gas content. We decompose the SEDs into three components: stellar, cold dust, and active galactic nucleus (AGN). By doing so, we are able to derive and analyze the relevant properties of each component. We determine the molecular gas mass from CO line emission based on Atacama Large Millimeter/submillimeter Array (ALMA) observations. By including ALMA observations in the multiwavelength SED analysis, we derive the molecular gas fractions, gas depletion timescales, and star formation efficiencies (SFEs). Their sample median and 16th–84th quartile ranges are f gas ∼ 0.33 − 0.17 + 0.33 , t depl ∼ 39 − 28 + 85 Myr, and SFE ∼ 297 − 195 + 659 K km s−1 pc−2, respectively. Compared to main-sequence galaxies, they have lower molecular gas content and higher SFEs, similar to quasars in the literature. This suggests that the gas in these quasars is rapidly depleted, likely as the result of intense starburst activity and AGN feedback. The observed correlations between these properties and the AGN luminosities further support this scenario. Additionally, we infer the black hole to stellar mass ratio and black hole mass growth rate, which indicate significant central black hole mass assembly over short timescales. Our results are consistent with the scenario that our sample represents a short transition phase toward unobscured quasars.

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A benchmark for extreme conditions of the multiphase interstellar medium in the most luminous hot dust-obscured galaxy at z = 4.6

Fernández Aranda,

Díaz Santos,

Hatziminaoglou

et al. 2024

A&A

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WISE J224607.6--052634.9 (W2246--0526) is a hot dust-obscured galaxy at $z$ = 4.601, and the most luminous obscured quasar known to date. W2246--0526 harbors a heavily obscured supermassive black hole that is most likely accreting above the Eddington limit. We present observations with the Atacama Large Millimeter/submillimeter Array (ALMA) in seven bands, including band 10, of the brightest far-infrared (FIR) fine-structure emission lines of this galaxy: OI m OIII m NII m OI m CII m NII m CI m $, and CI m $. A comparison of the data to a large grid of Cloudy radiative transfer models reveals that a high hydrogen density ($n_ H $) and extinction ($A_ V mag), together with extreme ionization ($log(U)=-0.5$) and a high X-ray to UV ratio ($ ox are required to reproduce the observed nuclear line ratios. The values of $ ox $ and $U$ are among the largest found in the literature and imply the existence of an X-ray-dominated region (XDR). In fact, this component explains the a priori very surprising non-detection of the OIII m $ emission line, which is actually suppressed, instead of boosted, in XDR environments. Interestingly, the best-fitted model implies higher X-ray emission and lower CO content than what is detected observationally, suggesting the presence of a molecular gas component that should be further obscuring the X-ray emission over larger spatial scales than the central region that is being modeled. These results highlight the need for multiline infrared observations to characterize the multiphase gas in high redshift quasars and, in particular, W2246--0526 serves as an extreme benchmark for comparisons of interstellar medium conditions with other quasar populations at cosmic noon and beyond.

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An Overdensity of Red Galaxies around the Hyperluminous Dust-obscured Quasar W1835+4355 at z = 2.3

Cited by 5 publications

References 76 publications

An overdensity of Lyman break galaxies around the hot dust-obscured galaxy WISE J224607.56−052634.9

An overdensity of Lyman break galaxies around the hot dust-obscured galaxy WISE J224607.56−052634.9

Physical Properties of Hyperluminous, Dust-obscured Quasars at z ∼ 3: Multiwavelength Spectral Energy Distribution Analysis and Cold Gas Content Revealed by ALMA

A benchmark for extreme conditions of the multiphase interstellar medium in the most luminous hot dust-obscured galaxy at z = 4.6

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