2023A&A...671A...5H


Query : 2023A&A...671A...5H

2023A&A...671A...5H - Astronomy and Astrophysics, volume 671A, 5 (2023/3-1)

Clustering dependence on Lyα luminosity from MUSE surveys at 3 < z < 6.

HERRERO ALONSO Y., MIYAJI T., WISOTZKI L., KRUMPE M., MATTHEE J., SCHAYE J., ACEVES H., KUSAKABE H. and URRUTIA T.

Abstract (from CDS):

We investigate the dependence of Lyα emitter (LAE) clustering on Lyα luminosity and connect the clustering properties of ≈L LAEs with those of much fainter ones, namely, ≈0.04L. We use 1030 LAEs from the MUSE-Wide survey, 679 LAEs from MUSE-Deep, and 367 LAEs from the to-date deepest ever spectroscopic survey, the MUSE Extremely Deep Field. All objects have spectroscopic redshifts of 3 < z < 6 and cover a large dynamic range of Lyα luminosities: 40.15 < log(LLyα/erg s–1) < 43.35. We apply the Adelberger et al. K-estimator as the clustering statistic and fit the measurements with state-of-the-art halo occupation distribution (HOD) models. We find that the large-scale bias factor increases weakly with an increasing line luminosity. For the low-luminosity (log⟨LLyα/[erg s–1]⟩ = 41.22) and intermediate-luminosity (log⟨LLyα/[erg s–1]⟩ = 41.64) LAEs, we compute consistent bias factors $ b_\mathrm{{low}}=2.43^{+0.15}_{-0.15} $ and $ b_\mathrm{{interm.}}=2.42^{+0.10}_{-0.09} $, whereas for the high-luminosity (log⟨LLyα/[erg s–1]⟩ = 42.34) LAEs we calculated $ b_\mathrm{{high}}=2.65^{+0.13}_{-0.11} $. Consequently, high-luminosity LAEs occupy dark matter halos (DMHs) with typical masses of $ \log (M_{\mathrm{h}}/[h^{-1}M_\odot])=11.09^{+0.10}_{-0.09} $, while low-luminosity LAEs reside in halos of $ \log (M_{\mathrm{h}}/[h^{-1}M_\odot])=10.77^{+0.13}_{-0.15} $. The minimum masses to host one central LAE, Mmin, and (on average) one satellite LAE, M1, also vary with Lyα luminosity, growing from $ \log (M_\mathrm{{min}}/[h^{-1}M_\odot])=10.3^{+0.2}_{-0.3} $ and $ \log (M_1/[h^{-1}M_\odot])=11.7^{+0.3}_{-0.2} $ to $ \log (M_\mathrm{{min}}/[h^{-1}M_\odot])=10.7^{+0.2}_{-0.3} $ and $ \log (M_1/[h^{-1}M_\odot])=12.4^{+0.4}_{-0.6} $ from low- to high-luminosity samples, respectively. The satellite fractions are ≲10% (≲20%) at 1σ (3σ) confidence level, supporting a scenario in which DMHs typically host one single LAE. We next bisected the three main samples into disjoint subsets to thoroughly explore the dependence of the clustering properties on LLyα. We report a strong (8σ) clustering dependence on Lyα luminosity, not accounting for cosmic variance effects, where the highest luminosity LAE subsample (log(LLyα/erg s–1) ≈ 42.53) clusters more strongly ($ b_\mathrm{{highest}}=3.13^{+0.08}_{-0.15} $) and resides in more massive DMHs ($ \log(M_\mathrm{{h}} / [h^{-1}{M}_{\odot}])=11.43^{+0.04}_{-0.10} $) than the lowest luminosity one (log(LLyα/erg s–1) ≈ 40.97), which presents a bias of $ b_\mathrm{{lowest}}=1.79^{+0.08}_{-0.06} $ and occupies $ \log(M_\mathrm{{h}} / [h^{-1}{M}_{\odot}])=10.00^{+0.12}_{-0.09} $ halos. We discuss the implications of these results for evolving Lyα luminosity functions, halo mass dependent Lyα escape fractions, and incomplete reionization signatures.

Abstract Copyright: © The Authors 2023

Journal keyword(s): large-scale structure of Universe - galaxies: high-redshift - galaxies: evolution - cosmology: observations - dark matter

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1675 0

Query : 2023A&A...671A...5H

Basic data :
NAME Hubble Ultra Deep Field -- Region defined in the Sky
Origin of the objects types :

(Ref) Object type as listed in the reference "Ref"
(acronym) Object type linked to the acronym according to the original reference
() Anterior to 2007, before we can link the objet type to a reference, or given by the CDS team in some particular cases

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reg ()
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
ICRS coord. (ep=J2000) :
03 32 39.0 -27 47 29 [ ] D ~
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
FK4 coord. (ep=B1950 eq=1950) :
03 30 33.4 -27 57 34 [ ]
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
Gal coord. (ep=J2000) :
223.5548 -54.3948 [ ]
SIMBAD within arcmin
', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay Simbad points in this preview
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Identifiers (3) :
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NAME UDF NAME HUDF NAME Hubble Ultra Deep Field

References (1675 between 1850 and 2024) (Total 1675)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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