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Relevant bibliographies by topics / Brightest cluster galaxy

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Academic literature on the topic 'Brightest cluster galaxy'

Author: Grafiati

Published: 4 June 2021

Last updated: 4 March 2023

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Journal articles on the topic "Brightest cluster galaxy"

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Wittman, David, Drake Foote, and Nathan Golovich. "Brightest Cluster Galaxy Alignments in Merging Clusters." Astrophysical Journal 874, no. 1 (2019): 84. http://dx.doi.org/10.3847/1538-4357/ab0a0a.

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Bogdán, Ákos, Lorenzo Lovisari, Patrick Ogle, et al. "Detection of a Superluminous Spiral Galaxy in the Heart of a Massive Galaxy Cluster." Astrophysical Journal 930, no. 2 (2022): 138. http://dx.doi.org/10.3847/1538-4357/ac62cd.

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Abstract It is well established that brightest cluster galaxies (BCGs), residing in the centers of galaxy clusters, are typically massive and quenched galaxies with cD or elliptical morphology. An optical survey suggested that an exotic galaxy population, superluminous spiral and lenticular galaxies, could be the BCGs of some galaxy clusters. Because the cluster membership and the centroid of a cluster cannot be accurately determined based solely on optical data, we followed up a sample of superluminous disk galaxies and their environments using XMM-Newton X-ray observations. Specifically, we explored seven superluminous spiral and lenticular galaxies that are candidate BCGs. We detected massive galaxy clusters around five superluminous disk galaxies and established that one superluminous spiral, 2MASX J16273931+3002239, is the central BCG of a galaxy cluster. The temperature and total mass of the cluster are kT 500 = 3.55 − 0.20 + 0.18 keV and M 500 = (2.39 ± 0.19) × 1014 M ⊙. We identified the central galaxies of the four clusters that do not host superluminous disk galaxies at their cores, and established that the centrals are massive elliptical galaxies. However, for two of the clusters, the offset superluminous spirals are brighter than the central galaxies, implying that the superluminous disk galaxies are the brightest cluster galaxies. Our results demonstrate that superluminous disk galaxies are rarely the central systems of galaxy clusters. This is likely because galactic disks are destroyed by major mergers, which are more frequent in high-density environments. We speculate that the disks of superluminous disk galaxies in cluster cores may have been reformed due to mergers with gas-rich satellites.

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Tucker, Gregory S., and J. B. Peterson. "Alignment of Clusters with Brightest Member Galaxies." Symposium - International Astronomical Union 130 (1988): 546. http://dx.doi.org/10.1017/s0074180900136757.

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We have obtained CCD images of the brightest elliptical galaxy in 27 clusters of galaxies with redshifts z < 0.1. For each galaxy we fitted elliptical isophotes to the galaxy image. We also measured the position angle of each cluster from the Palomar Observatory Sky Survey (POSS) prints. We find only marginal evidence for alignment of brightest cluster members (BCM) with their parent clusters, but we find that our CCD isophotes are well aligned with the POSS image.

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Graham, Alister, Tod R. Lauer, Matthew Colless, and Marc Postman. "Brightest Cluster Galaxy Profile Shapes." Astrophysical Journal 465 (July 1996): 534. http://dx.doi.org/10.1086/177440.

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Pobre, Savannah, Roohi Dalal, Michael A. Strauss, and Yen-Ting Lin. "Are Brightest Cluster Galaxies Special?" Research Notes of the AAS 7, no. 2 (2023): 19. http://dx.doi.org/10.3847/2515-5172/acb9e1.

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Abstract A longstanding question when studying Brightest Cluster Galaxies (BCGs) and their evolution is whether their luminosities are statistical extremes of the luminosity distribution of other cluster member galaxies, or whether their luminosities follow a different,“special” distribution. To explore this question, we use the two Tremaine–Richstone (TR) statistics that sometimes lead to different conclusions about BCG specialness. We run Monte Carlo simulations of galaxy clusters with varying galaxy luminosity functions and BCG properties, and explore the sensitivity of the TR statistics to the adjusted BCG properties. We identify cases where the two statistics lead to different conclusions. The first of the TR statistics, which relies on the spread of BCG luminosities, is more reliable for determining specialness than the second, which utilizes the spread in the luminosity gap between the BCG and second ranked galaxy.

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Pimbblet, K. A. "Are Dumbbell Brightest Cluster Members Signposts to Galaxy Cluster Activity?" Publications of the Astronomical Society of Australia 25, no. 4 (2008): 176–83. http://dx.doi.org/10.1071/as08016.

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AbstractWe assemble a sample of galaxy clusters whose brightest members are dumbbell galaxies and compare them with a control sample in order to investigate if they are the result of recent mergers. We show that the dumbbell sample is no more likely than other clusters to exhibit subclustering. However, they are much more likely to have at least one dumbbell component possessing a significant peculiar velocity with respect to the parent cluster than a non-dumbbell brightest cluster member. We interpret this in the context of seeing the clusters at various stages of post-merger relaxation.

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Panko, Elena, Katarzyna Bajan, Piotr Flin, and Alla Gotsulyak. "The Adopted Morphological Types of 247 Rich PF Galaxy Clusters." Proceedings of the International Astronomical Union 11, S308 (2014): 213–14. http://dx.doi.org/10.1017/s1743921316009893.

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AbstractMorphological types were determined for 247 rich galaxy clusters from the PF Catalogue of Galaxy Clusters and Groups. The adopted types are based on classical morphological schemes and consider concentration to the cluster center, the signs of preferential direction or plane in the cluster, and the positions of the brightest galaxies. It is shown that both concentration and preferential plane are significant and independent morphological criteria.

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Puddu, Emanuella, and Stefano Andreon. "Do gas-poor galaxy clusters have different galaxy populations? The positive covariance of hot and cold baryons." Monthly Notices of the Royal Astronomical Society 511, no. 2 (2021): 2968–76. http://dx.doi.org/10.1093/mnras/stab3632.

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ABSTRACT Galaxy clusters show a variety of intracluster medium properties at a fixed mass in gas fractions, X-ray luminosity and X-ray surface brightness. In this work, we investigate whether the yet-undetermined cause that produces clusters of X-ray low surface brightness also affects galaxy properties, such as richness, richness concentration, width and location of the red sequence, colour, luminosity, and dominance of the brightest cluster galaxy. We use Sloan Digital Sky Survey Data Release 12 photometry, and our analysis factors out the mass dependency to derive trends at fixed cluster mass. Clusters of low surface brightness for their mass have cluster richness in spite of their group-like luminosity. Gas-poor, low X-ray surface brightness, X-ray faint clusters for their mass display 25 per cent lower richness for their mass at the 4.4σ level. Therefore, richness and quantities depending on gas, such as gas fraction, Mgas and X-ray surface brightness, are covariant at fixed halo mass. In particular, we do not confirm the suggestion of anticorrelation of hot and cold baryons at fixed mass put forth in the literature. All the remaining optical properties show no covariance at fixed mass, within the sensitivities allowed by our data and sample size. We conclude that X-ray and optical properties are disjointed; the optical properties do not show signatures of those processes involving gas content, apart from the richness–mass scaling relation. The covariance between X-ray surface brightness and richness is useful for an effective X-ray follow-up of low-surface-brightness clusters because it allows us to pre-select clusters using optical data of survey quality and avoids expensive X-ray observations.

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Huang, Mei-Ling, and Lin-wen Chen. "Co-Evolution of Brightest Cluster Galaxies and Galaxy Activity in the Host Clusters." Proceedings of the International Astronomical Union 5, S267 (2009): 110. http://dx.doi.org/10.1017/s1743921310005715.

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AbstractWe have identified ~500 relatively relaxed galaxy clusters at low redshift (z < 0.3) from the maxBCG catalog with double radio lobes at the center; about 200 radio counterparts of brightest cluster galaxies (BCGs) of these clusters appear to be wide-angle tailed (WAT) radio sources, indicating ongoing interaction between its host galaxy and the surrounding ICM. Our analysis suggests that the radio power of WAT is positively correlated with the optical luminosities of host BCGs, and increases with redshift; whereas the cluster ellipticity-radio galaxy fraction relation shows no obvious difference between WAT and non-WAT clusters.

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Vantyghem, A. N., B. R. McNamara, A. C. Edge, et al. "A13CO Detection in a Brightest Cluster Galaxy." Astrophysical Journal 848, no. 2 (2017): 101. http://dx.doi.org/10.3847/1538-4357/aa8fd0.

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Dissertations / Theses on the topic "Brightest cluster galaxy"

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Brough, Sarah. "Environmental dependence of brightest cluster galaxy evolution." Thesis, Liverpool John Moores University, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.431286.

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Peery, Tyler Robert. "The Use of Brightest Cluster Galaxies as Standard Candles Since z~1." Ohio University Art and Sciences Honors Theses / OhioLINK, 2010. http://rave.ohiolink.edu/etdc/view?acc_num=ouashonors1276623279.

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Lynam, Paul David. "Brightest cluster galaxy properties and the search for streaming flows." Thesis, Liverpool John Moores University, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.247330.

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Schwartzenberg, Jean Marc. "Field and cluster surveys for low surface brightness galaxies." Thesis, University of Bristol, 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.336873.

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TRAVASCIO, ANDREA. "Communicating the energy: accretion properties and feedback in AGN." Doctoral thesis, 2020. http://hdl.handle.net/11573/1349452.

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This thesis focuses on investigating the role of nuclear activity in SMBH-host galaxy self-regulated growth. This work is based on an extensive collection of multi-band imaging and spectroscopic data. Indeed, it is now widely accepted that AGN activity can affect different phases of the interstellar medium making mandatory a multi-wavelength approach that combines the study of emitting/absorbing gas at increasing distance from the SMBH. I have studied the relationships between nuclear properties, AGN-driven outflows, and host galaxy properties by investigating two specific cases. The first one aims at understanding if and how the huge radiative output of a hyper-luminous QSO interacts with the circum-galactic medium (CGM) of the host galaxy. The second science case regards the formation of the so-called Brightest Cluster Galaxy (BCG). BCGs are the most massive and luminous galaxies residing at the center of the relaxed, virialized and undisturbed clusters in the local Universe.

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Farage, Catherine. "The Link Between Extended Line Emission and AGN Feedback in Brightest Cluster Galaxies." Phd thesis, 2011. http://hdl.handle.net/1885/9057.

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This thesis presents a study of the optical emission-line regions of low-redshift brightest cluster galaxies (BCGs) and how these are connected to energy feedback in cluster cores. The cores of massive galaxy clusters appear to undergo cycles of self-regulating energy feedback, in which the output of nuclear activity in BCGs offsets much of the hot cluster gas cooling. Many of the BCGs in these `cool-core' clusters are surrounded by extended filamentary nebulae that produce characteristic low-ionisation emission spectra. The origin and sources of excitation of these structures are not well understood. A sample of BCGs was observed with a new wide-field, optical integral-field spectrograph. These galaxies produce strong line emission with a range of integrated luminosities. Maps of the morphology and velocities of the line-emitting gas are constructed from these data. A deep observation of the nearby galaxy NGC4696, provides a detailed view of the complex emission nebula. In the inner nebula, a bright spiral filament coincides closely with a prominent dust lane. The data reveal velocities in this structure consistent with infalling, orbit-like trajectories encircling the nucleus. A model is presented in which some of the gas in the filaments originated in the accretion of a gas-rich dwarf galaxy. It is suggested that the filaments are excited by ~200km/s ram-pressure-driven shocks as the gas clouds fall through the halo. The shock models described reproduce the optical spectrum of the nebula. Three BCGs with intermediate line luminosities are studied to investigate how the filament structures are related to the processes of feedback in the cluster cores. Two systems, Abell 3581 and Sersic 159-03, appear to be experiencing phases of feedback dominated by AGN heating. The structure and kinematics of the emitting gas in Abell 3581 show evidence for significant interaction between the radio outflows and the optical nebula, and possible accretion flows into the nucleus. X-ray and radio data indicate that Sersic 159-03 is dominated by AGN feedback, but the kinematics of the optical nebula are consistent with infall or outflow along the filaments. The third system, 2A0335+096, is dominated by a cooling and accumulation phase of feedback. The outer nebula forms a disk-like structure, ~14kpc in radius, with a velocity field of rotation about the BCG. Overall, our data are consistent with ongoing AGN-driven feedback in these systems. A comparative study of the line-luminous galaxies in the sample is also presented. The data for several systems show evidence for a correlation between the velocity dispersions and line flux ratios in the nebulae, suggesting a strong contribution from shocks to the excitation. The large-scale excitation properties of the nebulae are assessed using optical diagnostic diagrams and discussed in the context of mixing between shock and stellar photoionisation excitation models. It is suggested that both shock and photoionisation excitation contribute significantly to the properties of the emission in these BCGs, to a degree that varies among the galaxies.

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Bildfell, Christopher John. "The Stellar Content in Clusters of Galaxies." Thesis, 2013. http://hdl.handle.net/1828/4562.

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We investigate three separate topics associated with the formation and evolution of the stellar mass component in galaxy clusters. The work presented herein is based primarily on optical imaging and spectra taken with, respectively, the Canada-France-Hawaii Telescope and Gemini North/South. We confront the result from the optical data analysis with the results from the analysis of high-resolution X-ray data taken with the Chandra and XMM-Newton space observatories. Confirming earlier results, we find that 22% of brightest cluster galaxies (BCGs) show central inversions in their optical color profiles (blue-cores), indicative of recent star formation or AGN activity. Based on the extended sizes of the blue-core regions we favour recent star formation. Comparison with the host cluster central entropies (and other X-ray properties) demonstrates that the source of cold gas required to fuel the recent activity in BCG cores is direct condensation from the rapidly cooling intra-cluster medium. We measure the giant-to-dwarf ratio (GDR) of red sequence galaxies in a sample of 97 clusters to constrain its evolution over the redshift range 0.05 < z < 0.55. We find that the GDR is evolving and can be parameterized by GDR=(0.88 +/- 0.15)z+(0.44 +/- 0.03). We find that the intrinsic scatter in this relation is consistent with zero, after accounting for measurement error, Poisson noise and contributions from large-scale structure. After correcting for cluster mass effects we investigate the evolution of the individual dwarf and giant populations in order to probe the source of the observed GDR evolution. Beyond z=0.25 the GDR evolution is driven by an increase in the number of dwarfs (consistent with interpretations from the literature), however, below z=0.2 the GDR evolution is caused by a significant reduction in the number of giants. We interpret this a evidence for a significant number of major mergers in the giant population at late times. This is supported by the relatively short dynamical friction timescales for these galaxies. We use velocity-broadened stellar template models to fit the optical spectra of 19 BCGs in order to measure their the line-of-sight component of their central velocity dispersions (sigma). The sigma values are combined with previous measurements of effective radii re and effective surface brightness <I>e to investigate the properties of the BCG fundamental plane. We measure a BCG fundamental plane parameterized by log( re )= alpha log( sigma ) + beta log( <I>e ) + gamma, with best fit parameters alpha = 1.24 +/- 0.08, beta = -0.80 +/- 0.1 and gamma = (0.3 +/- 2.0)x10-4. We constrain the intrinsic scatter in this relation to be deltaint = 0.066 +/- 0.010 in re, consistent with previous measures of the scatter in the fundamental plane for regular cluster ellipticals. Comparing the slope parameters (alpha, beta) of the BCG FP to those from previous studies of the FP for regular cluster ellipticals, we find that there is no conclusive evidence for curvature in the unified FP. We use the sigma measurements to estimate the BCG dynamical masses Mdyn. Comparing these estimates with mass proxies for the clusters (Tx, ng) we find that BCG mass is independent of cluster mass with Mdyn = (2.9 +/- 1.8)x1012 solar masses.<br>Graduate<br>0606<br>0605<br>bildfell@uvic.ca

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Book chapters on the topic "Brightest cluster galaxy"

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Collins, Chris, Sarah Brough, Doug Burke, Robert Mann, and Paul Lynam. "The Evolution of Brightest Cluster Galaxies." In Galaxy Evolution in Groups and Clusters. Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0107-6_7.

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Gonzalez, Anthony H., Ann I. Zabludoff, and Dennis Zaritsky. "Structural Properties of Brightest Cluster Galaxies." In Galaxy Evolution in Groups and Clusters. Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-010-0107-6_9.

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Aragón-Salamanca, A., C. M. Baugh, and G. Kauffmann. "The K-Band Hubble Diagram For The Brightest Cluster Galaxies: A Test Of Galaxy Formation Models." In Galaxy Interactions at Low and High Redshift. Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4665-4_109.

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Giuricin, G., F. Mardirossian, and M. Mezzetti. "Brightest member luminosities and dynamical times of galaxy clusters." In New Aspects of Galaxy Photometry. Springer Berlin Heidelberg, 1985. http://dx.doi.org/10.1007/bfb0030938.

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Schade, David. "Surface Brightness Evolution of Cluster and Field Galaxies." In Galaxy Scaling Relations: Origins, Evolution and Applications. Springer Berlin Heidelberg, 1997. http://dx.doi.org/10.1007/978-3-540-69654-4_25.

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Neilsen, Eric H., Zlatan I. Tsvetanov, and Holland C. Ford. "The surface brightness fluctuations and globular cluster populations of M87 and its companions." In The Radio Galaxy Messier 87. Springer Berlin Heidelberg, 1999. http://dx.doi.org/10.1007/bfb0106417.

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Conference papers on the topic "Brightest cluster galaxy"

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Andernach, Heinz, and Miriam E. Ramos-Ceja. "Radio Properties of Brightest Cluster Members." In Panoramic Radio Astronomy: Wide-field 1-2 GHz research on galaxy evolution. Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.089.0057.

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Simionescu, A., S. W. Allen, A. Mantz, N. Werner, and Y. Takei. "Baryons in the outskirts of the X-ray brightest galaxy cluster." In SUZAKU 2011: Exploring the X-ray Universe: Suzaku and Beyond. AIP, 2012. http://dx.doi.org/10.1063/1.3696143.

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Hilton, Matt. "SALT spectroscopic observations of galaxy clusters detected by ACT and a Type II quasar hosted by a brightest cluster galaxy." In SALT Science Conference 2015. Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.250.0042.

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Reiprich, Thomas H. "Cosmic Structure Traced by Precision Measurements of the X-Ray Brightest Galaxy Clusters in the Sky." In THE EMERGENCE OF COSMIC STRUCTURE: Thirteenth Astrophysics Conference. AIP, 2003. http://dx.doi.org/10.1063/1.1581811.

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