Connection between Galaxies and H i in Circumgalactic and Intergalactic Media: Variation according to Galaxy Stellar Mass and Star Formation Activity

Momose, Rieko; Shimizu, Ikkoh; Nagamine, Kentaro; Shimasaku, Kazuhiro; Kashikawa, Nobunari; Kusakabe, Haruka

doi:10.3847/1538-4357/abe1b9

Cited by 8 publications

(6 citation statements)

References 78 publications

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“…Several groups have already demonstrated the feasibility of this approach (e.g., Lee et al 2014Lee et al , 2018Cai et al 2016;Mukae et al 2020), and massive protoclusters at redshifts z = 2 − 3 have been identified (Lee et al 2016;Cai et al 2017). Moreover, this technique enables the derivation of the correlation between galaxy overdensity and Hi overdensity, providing valuable insights into the relationship between galaxies/AGNs and the surrounding Hi gas (Mukae et al 2017;Liang et al 2021;Momose et al 2021).…”

Section: Probing the Impact Of Feedback By Cosmological Simulationsmentioning

confidence: 98%

Feedback models in galaxy simulations and probing their impact by cosmological hydrodynamic simulations

Nagamine¹

2021

Proc. IAU

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Feedback effects by supernovae (SNe) and active galactic nuclei (AGNs) are believed to be essential for galaxy evolution and shaping present-day galaxies, but their exact mechanisms on galactic scales and their impact on CGM/IGM are not well understood yet. In galaxy formation simulations, it is still challenging to resolve sub-parsec scales, and we need to implement subgrid models to account for the physics on small scales. In this article, we summarize some of the efforts to build more physically based feedback models, discuss about pushing the resolution to its limits in galaxy simulations, testing galaxy formation codes under the AGORA code comparison project, and how to probe the impact of feedback using cosmological hydrodynamic simulations via Lyα absorption and CGM/IGM tomography technique. We also discuss our future directions of research in this field and how we make progress by comparing our simulations with observations.

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Section: Probing the Impact Of Feedback By Cosmological Simulationsmentioning

confidence: 98%

Feedback models in galaxy simulations and probing their impact by cosmological hydrodynamic simulations

Nagamine¹

2021

Proc. IAU

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“…On the other hand, the HI and dust column densities should be sufficiently low that we can observe their Lyα emission and identify the structure of LAEs (e.g., Shimakawa et al 2017a). In fact, several studies reported that the large-scale (tens of Mpc) HI gas traced by Lyα absorption is associated with high-density structures of LAEs (Cucciati et al 2014;Mawatari et al 2017;Liang et al 2021), while the high optical depth of Lyα emission could lead to a deficit of LAEs at small scales (e.g., Momose et al 2021aMomose et al , 2021b. The most massive galaxies with M s > 10 11 M e in the 53W002 field tend to avoid high-density peaks of LAEs, but they show similar wide distribution along the SW-NE direction (Figure 15).…”

Section: Comparisons With Previous Studiesmentioning

confidence: 99%

A Search for Massive Galaxy Population in a Protocluster of LAEs at z = 2.39 near the Radio Galaxy 53W002

Yonekura

Kajisawa

Hamaguchi

et al. 2022

ApJ

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We searched for massive galaxy population in the known large-scale high-density structure of Lyα emitters (LAEs) at z = 2.39 near the radio galaxy 53W002 by using imaging data from B , V , i ′ , J , H , and K s bands taken with Suprime-Cam and MOIRCS on the Subaru telescope. We selected 62 protocluster member candidates by their JHK s -band colors and spectral energy distribution (SED) fitting analysis (JHK s -selected galaxies) in our survey field of 70.2 arcmin 2 and compared their physical properties estimated from the SED fitting with a comparison sample in the COSMOS field. We found significant number density excesses for the JHK s -selected galaxies in the 53W002 field at K s < 22.25, J − K s > 2, or V − K s > 4. In particular, the number density of the JHK s -selected galaxies with K s < 22.25 and J − K s > 2 in the 53W002 field is nine times higher than the comparison sample. Most of those with K s < 22.25 and J − K s > 2 are massive galaxies with M s > 1011 M ⊙, and their specific star formation rates (sSFRs) of 10−11–10−10 yr−1 suggest that the star formation has not yet stopped completely. We also found a density excess of quiescent galaxies with M s = 5 × 1010 M ⊙ to 1011 M ⊙ and sSFR < 10−11 yr−1, as well as that of low-mass galaxies with M s = 109.75–1010 M ⊙ and various sSFRs. The massive galaxies with M s > 1011 M ⊙ are not located at the density peaks of LAEs but widely distributed along a similar direction to the structure of LAEs over ∼15–20 comoving Mpc. On the other hand, the quiescent galaxies with sSFR < 10−11 yr−1 clearly avoid the structure of LAEs. Our results suggest that massive galaxies also exist in this protocluster discovered by the moderate overdensity of LAEs and their star formation activities depend on location in the protocluster.

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“…These studies have examined the galaxy-H I correlation at small separations to constrain the spatial extent, kinematics, and temperature of inflows and outflows in the circumgalactic region. At separations well beyond ∼1 cMpc (comoving Mpc), on the other hand, the correlation is instead dominated by large-scale structure and is expected to depend mainly on the halo mass (Momose et al 2021b). Kim & Croft (2008) made an initial estimate of the halo mass of LBGs based on the surrounding Lyα absorption, although the data of Adelberger et al (2003) permitted only loose constraints with an uncertainty of 0.6 dex.…”

Section: Introductionmentioning

confidence: 99%

LATIS: Constraints on the Galaxy–Halo Connection at z ∼ 2.5 from Galaxy–Galaxy and Galaxy–Lyα Clustering

Newman,

Qezlou,

Chartab

et al. 2024

ApJ

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The connection between galaxies and dark matter halos is often quantified using the stellar mass–halo mass (SMHM) relation. Optical and near-infrared imaging surveys have led to a broadly consistent picture of the evolving SMHM relation based on measurements of galaxy abundances and angular correlation functions. Spectroscopic surveys at z ≳ 2 can also constrain the SMHM relation via the galaxy autocorrelation function and through the cross-correlation between galaxies and Lyα absorption measured in transverse sight lines; however, such studies are very few and have produced some unexpected or inconclusive results. We use ∼3000 spectra of z ∼ 2.5 galaxies from the Lyα Tomography IMACS Survey (LATIS) to measure the galaxy–galaxy and galaxy–Lyα correlation functions in four bins of stellar mass spanning 109.2 ≲ M */M ⊙ ≲ 1010.5. Parallel analyses of the MultiDark N-body and ASTRID hydrodynamic cosmological simulations allow us to model the correlation functions, estimate covariance matrices, and infer halo masses. We find that results of the two methods are mutually consistent and broadly accord with standard SMHM relations. This consistency demonstrates that we are able to measure and model Lyα transmission fluctuations δ F in LATIS accurately. We also show that the galaxy–Lyα cross-correlation, a free by-product of optical spectroscopic galaxy surveys at these redshifts, can constrain halo masses with similar precision to galaxy–galaxy clustering.

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Connection between Galaxies and H i in Circumgalactic and Intergalactic Media: Variation according to Galaxy Stellar Mass and Star Formation Activity

Cited by 8 publications

References 78 publications

Feedback models in galaxy simulations and probing their impact by cosmological hydrodynamic simulations

Feedback models in galaxy simulations and probing their impact by cosmological hydrodynamic simulations

A Search for Massive Galaxy Population in a Protocluster of LAEs at z = 2.39 near the Radio Galaxy 53W002

LATIS: Constraints on the Galaxy–Halo Connection at z ∼ 2.5 from Galaxy–Galaxy and Galaxy–Lyα Clustering

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