J/A+A/686/A137 Cosmic Web properties for radio galaxies (Oei+, 2024)
Luminous giants populate the dense Cosmic Web. The radio
luminosity-environmental density relation for radio galaxies in action.
Oei M.S.S.L., van Weeren R.J., Hardcastle M.J., Gast A.R.D.J.G.I.B.,
Leclercq F., Roettgering H.J.A., Dabhade P., Shimwell T.W., Botteon A.
<Astron. Astrophys. 686, A137 (2024)>
=2024A&A...686A.137O 2024A&A...686A.137O (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, radio ; Redshifts
Keywords: methods: statistical - galaxies: active - intergalactic medium -
galaxies: jets - large-scale structure of Universe -
radio continuum: galaxies
Abstract:
Giant radio galaxies (GRGs, giant RGs, or giants) are
megaparsec-scale, jet-driven outflows from accretion disks of
supermassive black holes, and represent the most extreme pathway by
which galaxies can impact the Cosmic Web around them. A long-standing
but unresolved question is why giants are so much larger than other
radio galaxies.
It has been proposed that, in addition to having higher jet powers
than most RGs, giants might live in especially low-density Cosmic Web
environments. In this work, we aim to test this hypothesis by
pinpointing Local Universe giants and other RGs in physically
principled, Bayesian large-scale structure reconstructions.
More specifically, we localised a LOFAR Two-metre Sky Survey (LoTSS)
DR2-dominated sample of luminous (lν(ν=150MHz≥1024W/Hz))
giants and a control sample of LoTSS DR1 RGs, both with spectroscopic
redshifts up to zmax=0.16, in the BORG SDSS CosmicWeb
reconstructions.We measured the CosmicWeb density on a smoothing scale
of 2.9Mpc/h for each RG; for the control sample, we then
quantified the relation between RG radio luminosity and Cosmic Web
density. With the BORG SDSS tidal tensor, we also measured for each RG
whether the gravitational dynamics of its Cosmic Web environment
resemble those of clusters, filaments, sheets, or voids.
For both luminous giants and general RGs, the Cosmic Web density
distribution is gamma distribution-like. Luminous giants populate
large-scale environments that tend to be denser than those of general
RGs. This result is corroborated by gravitational dynamics
classification and a cluster catalogue crossmatching analysis. We find
that the Cosmic Web density around RGs with 150 MHz radio luminosity
lν is distributed as
1+{DELTA}RG|Lν=lν~{GAMMA}(k,θ), where k=4.8+0.2.l,
θ=1.4+0.02.L, and L:=log10(lν(1023W/Hz)-1).
This work presents more than a thousand inferred megaparsec-scale
densities around radio galaxies, which may be correct up to a factor
of order unity - except in clusters of galaxies, where the densities
can be more than an order of magnitude too low. We pave the way to a
future in which megaparsec-scale densities around RGs are common
inferred quantities, which help to better understand their dynamics,
morphology, and interaction with the enveloping Cosmic Web. Our data
demonstrate that luminous giants inhabit denser environments than
general RGs. This shows that - at least at high jet powers -
low-density environments are no prerequisite for giant growth. Using
general RGs, we quantified the relation between radio luminosity at
150MHz and Cosmic Web density on a smoothing scale of ∼2.9Mpc/h. This
positive relation, combined with the discrepancy in radio luminosity
between known giants and general RGs, reproduces the discrepancy in
Cosmic Web density between known giants and general RGs. Our findings
are consistent with the view that giants are regular, rather than
mechanistically special, members of the radio galaxy population.
Description:
Using Bayesian Cosmic Web reconstructions of the Local Universe, we
compared the large-scale environments of giant radio galaxies with
those of the radio galaxy population in general. In particular, we
measured multi-megaparsec-scale Cosmic Web densities around the hosts
of ∼102 luminous giants and ∼103 general RGs.
The data presented here are combinations of data from these sources:
M.S.S.L. Oei et al. (2023A&A...672A.163O 2023A&A...672A.163O) for giant RGs
M.J. Hardcastle et al. (2019A&A...622A..12H 2019A&A...622A..12H) for general RGs
J. Jasche et al. (2015JCAP...01..036J 2015JCAP...01..036J) for Cosmic Web density
F. Leclercq et al. (2015JCAP...06..015L 2015JCAP...06..015L) for Cosmic Web class
Z.L. Wen et al. (2015ApJ...807..178W 2015ApJ...807..178W) for Cosmic Web clusters
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tab1grs.dat 93 260 Cosmic Web properties for BORG SDSS-constrained
giant radio galaxies (table 1)
tab1rg.dat 93 1443 Cosmic Web properties for BORG SDSS-constrained
radio galaxies (table 1)
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See also:
J/A+A/672/A163 : Properties of the 2060 giant radio galaxies (Oei+, 2023)
J/ApJ/807/178 : Newly rich galaxy clusters identified in SDSS-DR12 (Wen+ 2015)
Byte-by-byte Description of file: tab1grs.dat tab1rg.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 F15.11 deg RAdeg Host right ascension (J2000)
(hostrightascensionJ2000(deg))
17- 31 F15.11 deg DEdeg Host declination (J2000)
(hostdeclinationJ2000_(deg))
33- 41 F9.7 --- zspHost Host spectroscopic redshift
(hostspectroscopicredshift_(1))
43- 49 F7.5 --- e_zspHost ?=- Host spectroscopic redshift uncertainty
(hostspectroscopicredshiftuncertainty(1))
51- 55 F5.2 --- muFix Cosmic Web density distribution lognormal
fit MLE mu (fixed voxel method; unit: 1)
(CosmicWebdensitymufixed_(1)) (1)
57- 60 F4.2 --- sigma2Fix Cosmic Web density distribution lognormal
fit MLE sigma2
(fixed voxel method; unit: 1) (1)
(CosmicWebdensitysigma2fixed_(1))
62- 66 F5.2 --- muFlex Cosmic Web density distribution lognormal
fit MLE mu (flexible voxel method; unit: 1)
(CosmicWebdensitymuflexible_(1)) (1)
68- 71 F4.2 --- sigma2Flex Cosmic Web density distribution lognormal
fit MLE sigma2
(flexible voxel method; unit: 1) (1)
(CosmicWebdensitysigma2flexible_(1))
73- 75 F3.1 --- Pcluster [0/1] Cosmic Web dynamical environment
cluster probability (unit: 1)
(CosmicWebprobabilitycluster(1)) (2)
77- 79 F3.1 --- Pfilament [0/1] Cosmic Web dynamical environment
filament probability (unit: 1)
(CosmicWebprobabilityfilament(1)) (2)
81- 83 F3.1 --- Psheet [0/1] Cosmic Web dynamical environment
sheet probability (unit: 1)
(CosmicWebprobabilitysheet(1)) (2)
85- 87 F3.1 --- Pvoid [0/1] Cosmic Web dynamical environment void
probability (unit: 1)
(CosmicWebprobabilityvoid(1)) (2)
89- 91 F3.1 10+14Msun MassHost ?=- Cosmic Web host galaxy cluster mass
(CosmicWebclustermass(1e14Solarmass))
93 I1 --- PBCG [0/1] Cosmic Web host galaxy is brightest
cluster galaxy (1: yes, 0: no)
(CosmicWebclusterhostis_BCG)
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Note (1): The Cosmic Web densities comprise both baryonic and dark matter and
are relative to today's cosmic mean value. They represent averages in cubic
volumes of 4.2 Mpc per side.
The Cosmic Web densities are biased low for (G)RGs in clusters.
See Section 5.1: Cosmic Web density accuracy.
Note (2): The Cosmic Web dynamical environment probabilities refer to
clusters, filaments, sheets, and voids in the T-web sense.
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Acknowledgements:
Martijn Simon Soen Liong Oei, oei(at)caltech.edu, oei(at)strw.leidenuniv.nl
(End) Patricia Vannier [CDS] 06-Mar-2024