Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3

Shen, Lu; Lemaux, B. C.; Lubin, Lori M.; Cucciati, O.; Fèvre, O. Le; Liu, Guilin; Fang, Wenjuan; Pelliccia, Debora; Tomczak, Adam; McKean, J. P.; Miller, Neal A.; Fassnacht, C. D.; Gal, R. R.; Hung, Denise; Hathi, N. P.; Bardelli, S.; Vergani, D.; Zucca, E.

doi:10.3847/1538-4357/abee75

Cited by 17 publications

(8 citation statements)

References 125 publications

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“…This result is consistent with the idea that Hot DOGs may not be the central galaxies of the overdensities traced by themselves (Assef et al 2015). It is worth noting that Shen et al (2021) also found similar results in the protostructure at z = 3.3 traced by radio-detected AGNs. They proposed a scenario where merging might already have happened in this case and lowered the local density of their surrounding region.…”

Section: Local Overdensity Of Drgssupporting

confidence: 89%

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

Luo

Fan

Zou

et al. 2022

ApJ

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Wide-field Infrared Survey Explorer all-sky survey has discovered a new population of hot dust-obscured galaxies (Hot DOGs), which have been confirmed to be dusty quasars. Previous statistical studies have found significant overdensities of submillimeter and mid-IR-selected galaxies around Hot DOGs, indicating they may reside in dense regions. Here we present the near-infrared (J and K s bands) observations over a 7 .′ 5 × 7 .′ 5 field centered on a Hot DOG W1835+4355 at z ∼ 2.3 using the wide-field infrared camera on the Palomar 200 inch telescope. We use the color criterion J − K s > 2.3 for objects with K S < 20 , to select distant red galaxies (DRGs). We find a significant excess of number density of DRGs in the W1835+4355 field compared to three control fields, by a factor of about two. The overdensity of red galaxies around W1835+4355 is consistent with the multiwavelength environment of Hot DOGs, suggesting that Hot DOGs may be a good tracer for dense regions at high redshift. We find that W1835+4355 does not reside in the densest region of the dense environment traced by itself. A possible scenario is that W1835+4355 is undergoing a merging process, which lowers the local number density of galaxies in its surrounding region.

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Section: Local Overdensity Of Drgssupporting

confidence: 89%

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

Luo

Fan

Zou

et al. 2022

ApJ

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“…Navarro et al 1995;Borgani et al 2001), as well as the intergalactic medium (IGM; Borgani & Viel 2009), helping to narrow down the possible mechanisms that can lie behind the non-gravitational heat injection. Recently, a radio AGN has been found in a proto-cluster at redshift z = 3.3 (Shen et al 2021), which adds to the growing consensus that black hole feedback already plays a significant role in the early stages of the evolution of the ICM.…”

Section: Introductionmentioning

confidence: 84%

Detecting preheating in proto-clusters with Lyman-$α$ Forest Tomography

Kooistra,

Inoue,

Lee

et al. 2021

Preprint

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Studies of low redshift galaxy clusters suggest the intra-cluster medium (ICM) has experienced non-gravitational heating during the formation phase of the clusters. Using simple phenomenological heating prescriptions, we simulate the effect of this preheating of the nascent ICM in galaxy protoclusters and examine its effect on Lyman-α (Lyα) forest tomographic maps. We analyse a series of cosmological zoom-in simulations of proto-clusters within the framework of the Lyα transmission-dark matter (DM) density distribution. We find that the more energy is injected into the proto-ICM at z = 3, the more the distribution at high DM density tilts towards higher Lyα transmission. This effect has been confirmed in both low-resolution simulations adopting a preheating scheme based on entropy floors, as well as in higher-resolution simulations with another scheme based on energy floors. The evolution of the slope of this distribution is shown to vary with redshift. The methodology developed here can be applied to current and upcoming Lyα forest tomographic survey data to help constrain feedback models in galaxy proto-clusters.

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“…We complement DC 881725 with nine additional galaxies at z ∼ 4. et al 2009 ) surv e y (C3VO; Lemaux et al 2020 ;Shen et al 2021 ).…”

Section: [O II ] Measurements From Narrow-band Imagingmentioning

confidence: 99%

The ALPINE-ALMA [C ii] survey: Investigation of 10 galaxies at z ∼ 4.5 with [O ii] and [C ii] line emission − ISM properties and [O ii]−SFR relation

Vanderhoof

Faisst

Shen

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present 10 main-sequence ALPINE galaxies (log (M/M⊙) = 9.2 − 11.1 and SFR = 23 − 190 M⊙ yr−1) at z ∼ 4.5 with optical [O ii] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band imaging. This is the largest such multi-wavelength sample at these redshifts, combining various measurements in the ultra-violet, optical, and far-infrared including [C ii]158μm line emission and dust continuum from ALMA and Hα emission from Spitzer photometry. For the first time, this unique sample allows us to analyse the relation between [O ii] and total star-formation rate (SFR) and the interstellar medium (ISM) properties via [O ii]/[C ii] and [O ii]/Hα luminosity ratios at z ∼ 4.5. The [O ii]−SFR relation at z ∼ 4.5 cannot be described using standard local descriptions, but is consistent with a metal-dependent relation assuming metallicities around $50{{\ \rm per\ cent}}$ solar. To explain the measured dust-corrected luminosity ratios of $\log (L_{\rm [OII]}/L_{\rm [CII]}) \sim 0.98^{+0.21}_{-0.22}$ and $\log (L_{\rm [OII]}/L_{\rm H\alpha }) \sim -0.22^{+0.13}_{-0.15}$ for our sample, ionisation parameters log (U) < −2 and electron densities $\log (\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required. The former is consistent with galaxies at z ∼ 2 − 3, however lower than at z > 6. The latter may be slightly higher than expected given the galaxies’ specific SFR. The analysis of this pilot sample suggests that typical log (M/M⊙) > 9 galaxies at z ∼ 4.5 to have broadly similar ISM properties as their descendants at z ∼ 2 and suggest a strong evolution of ISM properties since the Epoch of Reionisation at z > 6.

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Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3

Cited by 17 publications

References 125 publications

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

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

Detecting preheating in proto-clusters with Lyman-$α$ Forest Tomography

The ALPINE-ALMA [C ii] survey: Investigation of 10 galaxies at z ∼ 4.5 with [O ii] and [C ii] line emission − ISM properties and [O ii]−SFR relation

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