The XXL Survey XLV: Linking the ages of optically selected groups to their X-ray emission

J. P. Crossett; S. L. McGee; Trevor J. Ponman; M. E. Ramos-Ceja; M. J. I. Brown; B. J. Maughan; A. S. G. Robotham; J. P. Willis; C. Wood; J Bland-Hawthorn; S. Brough; S. P. Driver; B. W. Holwerda; A. M. Hopkins; J. Loveday; M. S. Owers; S. Phillipps; M Pierre; K. A. Pimbblet

doi:10.1051/0004-6361/202142057

The XXL Survey XLV: Linking the ages of optically selected groups to their X-ray emission

J. P. Crossett^*, S. L. McGee, Trevor J. Ponman, M. E. Ramos-Ceja, M. J. I. Brown, B. J. Maughan, A. S. G. Robotham, J. P. Willis, C. Wood, J Bland-Hawthorn, S. Brough, S. P. Driver, B. W. Holwerda, A. M. Hopkins, J. Loveday, M. S. Owers, S. Phillipps, M Pierre, K. A. Pimbblet

^*Corresponding author for this work

School of Physics

Research output: Contribution to journal › Article (Academic Journal) › peer-review

5 Citations (Scopus)

Abstract

We investigate the properties of 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. 142 of these groups are 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 0.22 mag larger than in underluminous groups. The central galaxy in overluminous groups also lies closer to the 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 trends with X-ray emission in some of these properties despite the high stochastic noise from the limited number of group galaxies. We attribute the trends we see 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, a minority of X-ray underluminous groups have properties that suggest them to be dynamically mature. 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.

Original language	English
Article number	A2
Pages (from-to)	1-18
Number of pages	18
Journal	Astronomy and Astrophysics
Volume	663
DOIs	https://doi.org/10.1051/0004-6361/202142057
Publication status	Published - 1 Jul 2022

Bibliographical note

Accepted for Publication in A&A. 18 pages, 17 figures

Funding Information:
Acknowledgements. The authors thank the anonymous referee for their suggestions which improved the paper. We also wish to thank L. Chiappetti and E. Pompei for their helpful comments and feedback. JPC and SLM acknowl- edge support from the Science and Technology Facilities Council through grant number ST/N000633/1. JPC acknowledges support from the University of Birmingham, as well as support from Comité Mixto ESO-Gobierno de Chile. MP thanks the Centre National d’Etudes Spatiales for long-term support. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http:// www.gama-survey.org/. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. XXL is an international project based around an XMM Very Large Programme surveying two 25 deg2 extragalactic fields at a depth of ∼6 × 10−15 erg cm−2 s−1 in the [0.5−2] keV band for point-like sources. The XXL website is http://irfu.cea.fr/xxl. Multiband information and spectroscopic follow-up of the X-ray sources are obtained through a number of survey programmes, summarised at http://xxlmultiwave.pbworks.com/.

Publisher Copyright:
© ESO 2022.

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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. (2022). The XXL Survey XLV: Linking the ages of optically selected groups to their X-ray emission. Astronomy and Astrophysics, 663, 1-18. Article A2. https://doi.org/10.1051/0004-6361/202142057

@article{45cea02d7c3d4158b2f23f05d3b1bca8,

title = "The XXL Survey XLV: Linking the ages of optically selected groups to their X-ray emission",

abstract = "We investigate the properties of 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. 142 of these groups are 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 0.22 mag larger than in underluminous groups. The central galaxy in overluminous groups also lies closer to the 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 trends with X-ray emission in some of these properties despite the high stochastic noise from the limited number of group galaxies. We attribute the trends we see 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, a minority of X-ray underluminous groups have properties that suggest them to be dynamically mature. 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.",

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author = "Crossett, {J. P.} and McGee, {S. L.} and Ponman, {Trevor J.} and Ramos-Ceja, {M. E.} and Brown, {M. J. I.} and Maughan, {B. J.} and Robotham, {A. S. G.} and Willis, {J. P.} and C. Wood and J Bland-Hawthorn and S. Brough and Driver, {S. P.} and Holwerda, {B. W.} and Hopkins, {A. M.} and J. Loveday and Owers, {M. S.} and S. Phillipps and M Pierre and Pimbblet, {K. A.}",

note = "Accepted for Publication in A&A. 18 pages, 17 figures Funding Information: Acknowledgements. The authors thank the anonymous referee for their suggestions which improved the paper. We also wish to thank L. Chiappetti and E. Pompei for their helpful comments and feedback. JPC and SLM acknowl- edge support from the Science and Technology Facilities Council through grant number ST/N000633/1. JPC acknowledges support from the University of Birmingham, as well as support from Comit{\'e} Mixto ESO-Gobierno de Chile. MP thanks the Centre National d{\textquoteright}Etudes Spatiales for long-term support. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http:// www.gama-survey.org/. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. XXL is an international project based around an XMM Very Large Programme surveying two 25 deg2 extragalactic fields at a depth of ∼6 × 10−15 erg cm−2 s−1 in the [0.5−2] keV band for point-like sources. The XXL website is http://irfu.cea.fr/xxl. Multiband information and spectroscopic follow-up of the X-ray sources are obtained through a number of survey programmes, summarised at http://xxlmultiwave.pbworks.com/. Publisher Copyright: {\textcopyright} ESO 2022.",

year = "2022",

month = jul,

day = "1",

doi = "10.1051/0004-6361/202142057",

language = "English",

volume = "663",

pages = "1--18",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Crossett, JP, McGee, SL, Ponman, TJ, Ramos-Ceja, ME, Brown, MJI, Maughan, BJ, Robotham, ASG, Willis, JP, Wood, C, Bland-Hawthorn, J, Brough, S, Driver, SP, Holwerda, BW, Hopkins, AM, Loveday, J, Owers, MS, Phillipps, S, Pierre, M & Pimbblet, KA 2022, 'The XXL Survey XLV: Linking the ages of optically selected groups to their X-ray emission', Astronomy and Astrophysics, vol. 663, A2, pp. 1-18. https://doi.org/10.1051/0004-6361/202142057

TY - JOUR

T1 - The XXL Survey XLV

T2 - Linking the ages of optically selected groups to their X-ray emission

AU - Crossett, J. P.

AU - McGee, S. L.

AU - Ponman, Trevor J.

AU - Ramos-Ceja, M. E.

AU - Brown, M. J. I.

AU - Maughan, B. J.

AU - Robotham, A. S. G.

AU - Willis, J. P.

AU - Wood, C.

AU - Bland-Hawthorn, J

AU - Brough, S.

AU - Driver, S. P.

AU - Holwerda, B. W.

AU - Hopkins, A. M.

AU - Loveday, J.

AU - Owers, M. S.

AU - Phillipps, S.

AU - Pierre, M

AU - Pimbblet, K. A.

N1 - Accepted for Publication in A&A. 18 pages, 17 figures Funding Information: Acknowledgements. The authors thank the anonymous referee for their suggestions which improved the paper. We also wish to thank L. Chiappetti and E. Pompei for their helpful comments and feedback. JPC and SLM acknowl- edge support from the Science and Technology Facilities Council through grant number ST/N000633/1. JPC acknowledges support from the University of Birmingham, as well as support from Comité Mixto ESO-Gobierno de Chile. MP thanks the Centre National d’Etudes Spatiales for long-term support. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http:// www.gama-survey.org/. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. XXL is an international project based around an XMM Very Large Programme surveying two 25 deg2 extragalactic fields at a depth of ∼6 × 10−15 erg cm−2 s−1 in the [0.5−2] keV band for point-like sources. The XXL website is http://irfu.cea.fr/xxl. Multiband information and spectroscopic follow-up of the X-ray sources are obtained through a number of survey programmes, summarised at http://xxlmultiwave.pbworks.com/. Publisher Copyright: © ESO 2022.

PY - 2022/7/1

Y1 - 2022/7/1

N2 - We investigate the properties of 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. 142 of these groups are 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 0.22 mag larger than in underluminous groups. The central galaxy in overluminous groups also lies closer to the 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 trends with X-ray emission in some of these properties despite the high stochastic noise from the limited number of group galaxies. We attribute the trends we see 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, a minority of X-ray underluminous groups have properties that suggest them to be dynamically mature. 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.

AB - We investigate the properties of 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. 142 of these groups are 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 0.22 mag larger than in underluminous groups. The central galaxy in overluminous groups also lies closer to the 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 trends with X-ray emission in some of these properties despite the high stochastic noise from the limited number of group galaxies. We attribute the trends we see 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, a minority of X-ray underluminous groups have properties that suggest them to be dynamically mature. 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.

KW - astro-ph.GA

U2 - 10.1051/0004-6361/202142057

DO - 10.1051/0004-6361/202142057

M3 - Article (Academic Journal)

SN - 0004-6361

VL - 663

SP - 1

EP - 18

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A2

ER -

The XXL Survey XLV: Linking the ages of optically selected groups to their X-ray emission

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