J/A+A/663/A2 XXL Survey. X-ray emission in opt. select. group (Crossett+, 2022)
The XXL Survey.
XLV. Linking the ages of optically selected groups to their X-ray emission.
Crossett J.P., McGee S.L., Ponman T.J., Ramos-Ceja M.E., Brown M.J.I.,
Maughan B.J., Robotham A.S.G., Willis J.P., Wood C., Bland-Hawthorn J.,
Brough S., Driver S.P., Holwerda B.W., Hopkins A.M., Loveday J.,
Owers M.S., Phillipps S., Pierre M., Pimbblet K.A.
<Astron. Astrophys. 663, A2 (2022)>
=2022A&A...663A...2C 2022A&A...663A...2C (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources
Keywords: galaxies: evolution - galaxies: groups: general -
X-rays: galaxies: clusters - galaxies: star formation
Abstract:
Why are some galaxy groups pervaded by a hot X-ray emitting
intracluster medium, whilst others have no detectable X-ray emission?
Is the presence of hot gas a reliable indicator of dynamical maturity,
and can some virialised groups contain little or none of it? What are
the main differences between samples of groups selected in the X-ray
and optical bands? We address these questions by studying 232 optical
spectroscopically selected groups from the Galaxy And Mass Assembly
(GAMA) survey that overlap the XXL X-ray cluster survey. X-ray
aperture flux measurements combined with GAMA group data provides the
largest available sample of optical groups with detailed galaxy
membership information and consistently measured X-ray fluxes and
upper limits. A sample of 142 of these groups is divided into three
subsets based on the relative strength of X-ray and optical emission,
and we see a trend in galaxy properties between these subsets: X-ray
overluminous groups contain a lower fraction of both blue and star
forming galaxies compared with X-ray underluminous systems. X-ray
overluminous groups also have a more dominant central galaxy, with a
magnitude gap between first and second ranked galaxies on average
0.22mag larger than in underluminous groups. Moreover, the central
galaxy in overluminous groups lies closer to the luminosity-weighted
centre of the group. We examine a number of other structural
properties of our groups, such as axis ratio, velocity dispersion, and
group crossing time, and find evidence of trends with X-ray emission
in some of these properties despite the high stochastic noise arising
from the limited number of group galaxies. We attribute the trends we
see primarily to the evolutionary state of groups, with X-ray
overluminous systems being more dynamically evolved than underluminous
groups. The X-ray overluminous groups have had more time to develop a
luminous intragroup medium, quench member galaxies, and build the mass
of the central galaxy through mergers compared to underluminous
groups. However, an interesting minority of X-ray underluminous groups
have properties that suggest them to be dynamically mature. We find
that the lack of hot gas in these systems cannot be accounted for by
high star formation efficiency, suggesting that high gas entropy
resulting from feedback is the likely cause of their weak X-ray
emission.
Description:
We perform forced X-ray aperture photometry on 219 GAMA groups in
order to compare the properties of groups with strong and weak X-ray
emission using the ratio of group X-ray luminosity to group optical
luminosity.
GAMA G02 groups from Robotham et al. (2011MNRAS.416.2640R 2011MNRAS.416.2640R) with
matched 300kpc aperture photometry as used in the paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 135 219 XXL GAMMA group fluxes
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See also:
IX/49 : XXL Survey: First results (Pierre+, 2016)
IX/52 : XXL Survey. DR2 (Chiappetti+, 2018)
J/A+A/638/A46 : The XXL Survey. XLI. GMRT XXL-N 610MHz (Slaus+, 2020)
J/A+A/638/A45 : Obscuration properties of red AGNs in XXL-N (Masoura+, 2020)
J/MNRAS/452/2087 : Galaxy And Mass Assembly (GAMA): DR2 (Liske+, 2015)
J/MNRAS/474/3875 : Galaxy And Mass Assembly (GAMA): DR3 (Baldry+, 2018)
http://www.gama-survey.org/dr4/ : GAMA DR4 Home Page
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- GroupID GAMA ID of each group (1)
8- 16 F9.6 deg RAdeg Group iterative centre right ascension
(J2000) (1)
18- 26 F9.6 deg DEdeg Group iterative centre declination (J2000) (1)
28- 37 F10.8 --- z Median redshift of the group (1)
39- 52 E14.9 Msun/h2 LumBfunc Redshift corrected group optical
luminosity (1)
55- 63 E9.4 10-7W xFlux X-ray flux within 300kpc aperture (erg/s)
65- 73 E9.4 10-7W E_xFlux Positive 1 sigma uncertainty of X-ray flux
(erg/s)
75- 83 E9.4 10-7W e_xFlux Negative 1 sigma uncertainty of X-ray flux
(erg/s)
85-135 A51 --- Notes Relevant notes about each source
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Note (1): Value as per Robotham et al., 2011MNRAS.416.2640R 2011MNRAS.416.2640R.
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Acknowledgements:
Jacob P. Crossett, jacob.crossett(at)uv.cl
References:
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(End) Jacob P. Crossett [U. Valparaiso], Patricia Vannier [CDS] 26-Apr-2022