Galaxy And Mass Assembly (GAMA): witnessing the assembly of the cluster ABELL 1882

M. S. Owers; I. K. Baldry; A. E. Bauer; J. Bland-Hawthorn; M. J. I. Brown; M. E. Cluver; M. Colless; S. P. Driver; A. C. Edge; A. M. Hopkins; E. van Kampen; M. A. Lara-Lopez; J. Liske; J. Loveday; K. A. Pimbblet; T. Ponman; A. S. G. Robotham

doi:10.1088/0004-637X/772/2/104

Galaxy And Mass Assembly (GAMA): witnessing the assembly of the cluster ABELL 1882

M. S. Owers^*, I. K. Baldry, A. E. Bauer, J. Bland-Hawthorn, M. J. I. Brown, M. E. Cluver, M. Colless, S. P. Driver, A. C. Edge, A. M. Hopkins, E. van Kampen, M. A. Lara-Lopez, J. Liske, J. Loveday, K. A. Pimbblet, T. Ponman, A. S. G. Robotham

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

We present a combined optical and X-ray analysis of the rich cluster ABELL 1882 (A1882) with the aim of identifying merging substructure and understanding the recent assembly history of this system. Our optical data consist of spectra drawn from the Galaxy and Mass Assembly survey, which lends itself to this kind of detailed study thanks to its depth and high spectroscopic completeness. We use 283 spectroscopically confirmed cluster members to detect and characterize substructure. We complement the optical data with X-ray data taken with both Chandra and XMM. Our analysis reveals that A1882 harbors two main components, A1882A and A1882B, which have a projected separation of similar to ~2 Mpc and a line of sight velocity difference of ν_los~ -428⁺¹⁸⁷_-139km s^-1. The primary system, A1882A, has velocity dispersion σ_v = 500_-26⁺²³ km s^-1 and Chandra (XMM) temperature kT = 3.57 ± 0.17 keV (3.31_-0.27^+0.28 keV) while the secondary, A1882B, has σ_v = 457_-101⁺¹⁰⁸ km s^-1 and Chandra (XMM) temperature kT = 2.39 +/- 0.28 keV (2.12 +/- 0.20 keV). The optical and X-ray estimates for the masses of the two systems are consistent within the uncertainties and indicate that there is twice as much mass in A1882A (M₅₀₀ = 1.5-1.9 x 10¹⁴ M _☉) when compared with A1882B (M₅₀₀ = 0.8-1.0 x 10¹⁴ M _☉). We interpret the A1882A/A1882B system as being observed prior to a core passage. Supporting this interpretation is the large projected separation of A1882A and A1882B and the dearth of evidence for a recent (<2 Gyr) major interaction in the X-ray data. Two-body analyses indicate that A1882A and A1882B form a bound system with bound incoming solutions strongly favored. We compute blue fractions of f_b= 0.28 ± 0.09 and 0.18 ± 0.07 for the spectroscopically confirmed member galaxies within r ₅₀₀ of the centers of A1882A and A1882B, respectively. These blue fractions do not differ significantly from the blue fraction measured from an ensemble of 20 clusters with similar mass and redshift.

Original language	English
Article number	104
Number of pages	18
Journal	Astrophysical Journal
Volume	772
Issue number	2
Early online date	11 Jul 2013
DOIs	https://doi.org/10.1088/0004-637X/772/2/104
Publication status	Published - 1 Aug 2013

Keywords

Galaxies: clusters: individual (ABELL 1882)
Surveys
X-rays: galaxies: clusters
Digital sky survey
XMM-Newton obervations
Cold-front cluster
X-ray-clusters
Star-formation
Merging clusters
Rich clusters
Radio halo
Shapely concentration
Intracluster medium

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Owers, M. S., Baldry, I. K., Bauer, A. E., Bland-Hawthorn, J., Brown, M. J. I., Cluver, M. E., Colless, M., Driver, S. P., Edge, A. C., Hopkins, A. M., van Kampen, E., Lara-Lopez, M. A., Liske, J., Loveday, J., Pimbblet, K. A., Ponman, T., & Robotham, A. S. G. (2013). Galaxy And Mass Assembly (GAMA): witnessing the assembly of the cluster ABELL 1882. Astrophysical Journal, 772(2), Article 104. https://doi.org/10.1088/0004-637X/772/2/104

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title = "Galaxy And Mass Assembly (GAMA): witnessing the assembly of the cluster ABELL 1882",

abstract = "We present a combined optical and X-ray analysis of the rich cluster ABELL 1882 (A1882) with the aim of identifying merging substructure and understanding the recent assembly history of this system. Our optical data consist of spectra drawn from the Galaxy and Mass Assembly survey, which lends itself to this kind of detailed study thanks to its depth and high spectroscopic completeness. We use 283 spectroscopically confirmed cluster members to detect and characterize substructure. We complement the optical data with X-ray data taken with both Chandra and XMM. Our analysis reveals that A1882 harbors two main components, A1882A and A1882B, which have a projected separation of similar to ~2 Mpc and a line of sight velocity difference of νlos~ -428+187-139km s-1. The primary system, A1882A, has velocity dispersion σv = 500-26+23 km s-1 and Chandra (XMM) temperature kT = 3.57 ± 0.17 keV (3.31-0.27+0.28 keV) while the secondary, A1882B, has σv = 457-101+108 km s-1 and Chandra (XMM) temperature kT = 2.39 +/- 0.28 keV (2.12 +/- 0.20 keV). The optical and X-ray estimates for the masses of the two systems are consistent within the uncertainties and indicate that there is twice as much mass in A1882A (M500 = 1.5-1.9 x 1014 M ☉) when compared with A1882B (M500 = 0.8-1.0 x 1014 M ☉). We interpret the A1882A/A1882B system as being observed prior to a core passage. Supporting this interpretation is the large projected separation of A1882A and A1882B and the dearth of evidence for a recent (<2 Gyr) major interaction in the X-ray data. Two-body analyses indicate that A1882A and A1882B form a bound system with bound incoming solutions strongly favored. We compute blue fractions of fb= 0.28 ± 0.09 and 0.18 ± 0.07 for the spectroscopically confirmed member galaxies within r 500 of the centers of A1882A and A1882B, respectively. These blue fractions do not differ significantly from the blue fraction measured from an ensemble of 20 clusters with similar mass and redshift.",

keywords = "Galaxies: clusters: individual (ABELL 1882), Surveys, X-rays: galaxies: clusters, Digital sky survey, XMM-Newton obervations, Cold-front cluster, X-ray-clusters, Star-formation, Merging clusters, Rich clusters, Radio halo, Shapely concentration, Intracluster medium",

author = "Owers, {M. S.} and Baldry, {I. K.} and Bauer, {A. E.} and J. Bland-Hawthorn and Brown, {M. J. I.} and Cluver, {M. E.} and M. Colless and Driver, {S. P.} and Edge, {A. C.} and Hopkins, {A. M.} and {van Kampen}, E. and Lara-Lopez, {M. A.} and J. Liske and J. Loveday and Pimbblet, {K. A.} and T. Ponman and Robotham, {A. S. G.}",

year = "2013",

month = aug,

day = "1",

doi = "10.1088/0004-637X/772/2/104",

language = "English",

volume = "772",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Owers, MS, Baldry, IK, Bauer, AE, Bland-Hawthorn, J, Brown, MJI, Cluver, ME, Colless, M, Driver, SP, Edge, AC, Hopkins, AM, van Kampen, E, Lara-Lopez, MA, Liske, J, Loveday, J, Pimbblet, KA, Ponman, T & Robotham, ASG 2013, 'Galaxy And Mass Assembly (GAMA): witnessing the assembly of the cluster ABELL 1882', Astrophysical Journal, vol. 772, no. 2, 104. https://doi.org/10.1088/0004-637X/772/2/104

TY - JOUR

T1 - Galaxy And Mass Assembly (GAMA)

T2 - witnessing the assembly of the cluster ABELL 1882

AU - Owers, M. S.

AU - Baldry, I. K.

AU - Bauer, A. E.

AU - Bland-Hawthorn, J.

AU - Brown, M. J. I.

AU - Cluver, M. E.

AU - Colless, M.

AU - Driver, S. P.

AU - Edge, A. C.

AU - Hopkins, A. M.

AU - van Kampen, E.

AU - Lara-Lopez, M. A.

AU - Liske, J.

AU - Loveday, J.

AU - Pimbblet, K. A.

AU - Ponman, T.

AU - Robotham, A. S. G.

PY - 2013/8/1

Y1 - 2013/8/1

N2 - We present a combined optical and X-ray analysis of the rich cluster ABELL 1882 (A1882) with the aim of identifying merging substructure and understanding the recent assembly history of this system. Our optical data consist of spectra drawn from the Galaxy and Mass Assembly survey, which lends itself to this kind of detailed study thanks to its depth and high spectroscopic completeness. We use 283 spectroscopically confirmed cluster members to detect and characterize substructure. We complement the optical data with X-ray data taken with both Chandra and XMM. Our analysis reveals that A1882 harbors two main components, A1882A and A1882B, which have a projected separation of similar to ~2 Mpc and a line of sight velocity difference of νlos~ -428+187-139km s-1. The primary system, A1882A, has velocity dispersion σv = 500-26+23 km s-1 and Chandra (XMM) temperature kT = 3.57 ± 0.17 keV (3.31-0.27+0.28 keV) while the secondary, A1882B, has σv = 457-101+108 km s-1 and Chandra (XMM) temperature kT = 2.39 +/- 0.28 keV (2.12 +/- 0.20 keV). The optical and X-ray estimates for the masses of the two systems are consistent within the uncertainties and indicate that there is twice as much mass in A1882A (M500 = 1.5-1.9 x 1014 M ☉) when compared with A1882B (M500 = 0.8-1.0 x 1014 M ☉). We interpret the A1882A/A1882B system as being observed prior to a core passage. Supporting this interpretation is the large projected separation of A1882A and A1882B and the dearth of evidence for a recent (<2 Gyr) major interaction in the X-ray data. Two-body analyses indicate that A1882A and A1882B form a bound system with bound incoming solutions strongly favored. We compute blue fractions of fb= 0.28 ± 0.09 and 0.18 ± 0.07 for the spectroscopically confirmed member galaxies within r 500 of the centers of A1882A and A1882B, respectively. These blue fractions do not differ significantly from the blue fraction measured from an ensemble of 20 clusters with similar mass and redshift.

AB - We present a combined optical and X-ray analysis of the rich cluster ABELL 1882 (A1882) with the aim of identifying merging substructure and understanding the recent assembly history of this system. Our optical data consist of spectra drawn from the Galaxy and Mass Assembly survey, which lends itself to this kind of detailed study thanks to its depth and high spectroscopic completeness. We use 283 spectroscopically confirmed cluster members to detect and characterize substructure. We complement the optical data with X-ray data taken with both Chandra and XMM. Our analysis reveals that A1882 harbors two main components, A1882A and A1882B, which have a projected separation of similar to ~2 Mpc and a line of sight velocity difference of νlos~ -428+187-139km s-1. The primary system, A1882A, has velocity dispersion σv = 500-26+23 km s-1 and Chandra (XMM) temperature kT = 3.57 ± 0.17 keV (3.31-0.27+0.28 keV) while the secondary, A1882B, has σv = 457-101+108 km s-1 and Chandra (XMM) temperature kT = 2.39 +/- 0.28 keV (2.12 +/- 0.20 keV). The optical and X-ray estimates for the masses of the two systems are consistent within the uncertainties and indicate that there is twice as much mass in A1882A (M500 = 1.5-1.9 x 1014 M ☉) when compared with A1882B (M500 = 0.8-1.0 x 1014 M ☉). We interpret the A1882A/A1882B system as being observed prior to a core passage. Supporting this interpretation is the large projected separation of A1882A and A1882B and the dearth of evidence for a recent (<2 Gyr) major interaction in the X-ray data. Two-body analyses indicate that A1882A and A1882B form a bound system with bound incoming solutions strongly favored. We compute blue fractions of fb= 0.28 ± 0.09 and 0.18 ± 0.07 for the spectroscopically confirmed member galaxies within r 500 of the centers of A1882A and A1882B, respectively. These blue fractions do not differ significantly from the blue fraction measured from an ensemble of 20 clusters with similar mass and redshift.

KW - Galaxies: clusters: individual (ABELL 1882)

KW - Surveys

KW - X-rays: galaxies: clusters

KW - Digital sky survey

KW - XMM-Newton obervations

KW - Cold-front cluster

KW - X-ray-clusters

KW - Star-formation

KW - Merging clusters

KW - Rich clusters

KW - Radio halo

KW - Shapely concentration

KW - Intracluster medium

U2 - 10.1088/0004-637X/772/2/104

DO - 10.1088/0004-637X/772/2/104

M3 - Article

SN - 0004-637X

VL - 772

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 104

ER -

Galaxy And Mass Assembly (GAMA): witnessing the assembly of the cluster ABELL 1882

Abstract

Keywords

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