Journal articles: '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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Radovich, Mario, Crescenzo Tortora, Fabio Bellagamba, et al. "AMICO galaxy clusters in KiDS-DR3: galaxy population properties and their redshift dependence." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 4303–15. http://dx.doi.org/10.1093/mnras/staa2705.

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ABSTRACT A catalogue of galaxy clusters was obtained in an area of 414 $\deg ^2$ up to a redshift z ∼ 0.8 from the Data Release 3 of the Kilo-Degree Survey (KiDS-DR3), using the Adaptive Matched Identifier of Clustered Objects (amico) algorithm. The catalogue and the calibration of the richness–mass relation were presented in two companion papers. Here, we describe the selection of the cluster central galaxy and the classification of blue and red cluster members, and analyse the main cluster properties, such as the red/blue fraction, cluster mass, brightness, and stellar mass of the central galaxy, and their dependence on redshift and cluster richness. We use the Illustris-TNG simulation, which represents the state-of-the-art cosmological simulation of galaxy formation, as a benchmark for the interpretation of the results. A good agreement with simulations is found at low redshifts (z ≤ 0.4), while at higher redshifts the simulations indicate a lower fraction of blue galaxies than what found in the KiDS-amico catalogue: we argue that this may be due to an underestimate of star-forming galaxies in the simulations. The selection of clusters with a larger magnitude difference between the two brightest central galaxies, which may indicate a more relaxed cluster dynamical status, improves the agreement between the observed and simulated cluster mass and stellar mass of the central galaxy. We also find that at a given cluster mass the stellar mass of blue central galaxies is lower than that of the red ones.

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Burke, Claire, Chris Collins, John Stott, and Matt Hilton. "Evolution in cluster cores since z ~ 1." Proceedings of the International Astronomical Union 8, S295 (2012): 172–73. http://dx.doi.org/10.1017/s1743921313004602.

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AbstractA large fraction of the stellar mass in galaxy clusters is thought to be contained in the diffuse low surface brightness intracluster light (ICL). Being bound to the gravitational potential of the cluster rather than any individual galaxy, the ICL contains much information about the evolution of its host cluster and the interactions between the galaxies within. However due its low surface brightness it is notoriously difficult to study. We present the first detection and measurement of the flux contained in the ICL at z ~ 1. We find that the fraction of the total cluster light contained in the ICL may have increased by factors of 2–4 since z ~ 1, in contrast to recent findings for the lack of mass and scale size evolution found for brightest cluster galaxies. Our results suggest that late time build-up in cluster cores may occur more through stripping than merging and we discuss the implications of our results for hierarchical simulations.

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Zenteno, A., D. Hernández-Lang, M. Klein, et al. "A joint SZ–X-ray–optical analysis of the dynamical state of 288 massive galaxy clusters." Monthly Notices of the Royal Astronomical Society 495, no. 1 (2020): 705–25. http://dx.doi.org/10.1093/mnras/staa1157.

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ABSTRACT We use imaging from the first three years of the Dark Energy Survey to characterize the dynamical state of 288 galaxy clusters at 0.1 ≲ z ≲ 0.9 detected in the South Pole Telescope (SPT) Sunyaev–Zeldovich (SZ) effect survey (SPT-SZ). We examine spatial offsets between the position of the brightest cluster galaxy (BCG) and the centre of the gas distribution as traced by the SPT-SZ centroid and by the X-ray centroid/peak position from Chandra and XMM data. We show that the radial distribution of offsets provides no evidence that SPT SZ-selected cluster samples include a higher fraction of mergers than X-ray-selected cluster samples. We use the offsets to classify the dynamical state of the clusters, selecting the 43 most disturbed clusters, with half of those at z ≳ 0.5, a region seldom explored previously. We find that Schechter function fits to the galaxy population in disturbed clusters and relaxed clusters differ at z &gt; 0.55 but not at lower redshifts. Disturbed clusters at z &gt; 0.55 have steeper faint-end slopes and brighter characteristic magnitudes. Within the same redshift range, we find that the BCGs in relaxed clusters tend to be brighter than the BCGs in disturbed samples, while in agreement in the lower redshift bin. Possible explanations includes a higher merger rate, and a more efficient dynamical friction at high redshift. The red-sequence population is less affected by the cluster dynamical state than the general galaxy population.

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Oonk, J. B. R., W. Jaffe, M. N. Bremer, and N. Hatch. "Cool gas in brightest cluster galaxies." Proceedings of the International Astronomical Union 5, H15 (2009): 279. http://dx.doi.org/10.1017/s1743921310009221.

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AbstractGas in galaxy clusters requires re-heating. We study the re-heating of the cool gas phases. Ionized and molecular gas is traced out to 20 kpc and found to be strongly coupled. The observed line emission may in part be explained by excitation due to hot, young stars.

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Zinnecker, H., C. J. Keable, J. S. Dunlop, R. D. Cannon, and W. K. Griffiths. "The Nuclei of Nucleated Dwarf Elliptical Galaxies - Are they Globular Clusters?" Symposium - International Astronomical Union 126 (1988): 603–4. http://dx.doi.org/10.1017/s0074180900043254.

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It came as a great surprise that many dwarf elliptical galaxies of very low surface brightness in the Virgo Cluster have conspicuous bright star-like nuclei (Reaves 1983, Binggeli, Sandage and Tammann 1985). These nuclei are at least a factor of 10 more luminous than the brightest globular clusters in the Local Group and comparable only to the very brightest globulars surrounding M87. They contain a considerable fraction (1 to 20%) of the total light of the parent galaxy (Binggeli, priv. commun.). Their physical nature and origin are a matter of debate (Zinnecker et al. 1985, van den Bergh 1985, Norman 1986, Zinnecker 1986) but optical spectroscopy for 3 objects indicates a stellar composition with a range similar to globular clusters (Bothun et al. 1985). It has been suggested that a central nucleus is formed when off-center bound star clusters migrate to the center as a consequence of dynamical friction (Norman 1986). Support for such a scenario comes from CCD observations of IC 3475 which reveal numerous knots near the center of this dwarf irregular galaxy (Vigroux et al. 1986). These knots have the same color as the parent galaxy and are interpreted as intermediate age star clusters.

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Katayama, Haruyoshi, Kiyoshi Hayashida, Fumio Takahara, and Yutaka Fujita. "Properties of the Brightest Cluster Galaxy and Its Host Cluster." Astrophysical Journal 585, no. 2 (2003): 687–93. http://dx.doi.org/10.1086/346126.

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Khosroshahi, Habib G., and T. J. Ponman. "Fossil Galaxy Groups; Scaling Relations, Galaxy Properties and Formation of BCGs." Proceedings of the International Astronomical Union 2, S235 (2006): 214. http://dx.doi.org/10.1017/s174392130600620x.

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AbstractWe study fossil galaxy groups, their hot gas and the galaxy properties. Fossils are more X-ray luminous than non-fossil groups, however, they fall comfortably on the conventional L-T relation of galaxy groups and clusters indicating that their X-ray luminosity and temperature are both boosted, arguably, as a result of their early formation. The central dominant galaxy in fossils have optical luminosity comparable to the brightest cluster galaxies (BCGs), however, the isophotal shapes of the central galaxy in fossils are non-boxy in contrast to the isophotes of majority of the BCGs.

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Harvey, David, F. Courbin, J. P. Kneib, and Ian G. McCarthy. "A detection of wobbling brightest cluster galaxies within massive galaxy clusters." Monthly Notices of the Royal Astronomical Society 472, no. 2 (2017): 1972–80. http://dx.doi.org/10.1093/mnras/stx2084.

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Wen, Z. L., and J. L. Han. "GALAXY CLUSTERS AT HIGH REDSHIFT AND EVOLUTION OF BRIGHTEST CLUSTER GALAXIES." Astrophysical Journal 734, no. 1 (2011): 68. http://dx.doi.org/10.1088/0004-637x/734/1/68.

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Salomé, Philippe. "Brightest Cluster Galaxies & Cooling Flows." Proceedings of the International Astronomical Union 8, S292 (2012): 169–74. http://dx.doi.org/10.1017/s1743921313000975.

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AbstractIn the absence of any form of feedback heating, the gas in the central regions of massive relaxed cluster should cool and initiate a cooling flow. The presence/efficiency of an additional heating and the ultimate fate of the cooling gas is the subject of an extensive debate. In the last decade, molecular and atomic gas have been found in many Brightest Cluster Galaxies. I will review these observational results and discuss their implication for galaxy formation/evolution, in the perspective of ALMA.

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Sohn, Jubee, Margaret J. Geller, Ho Seong Hwang, Antonaldo Diaferio, Kenneth J. Rines, and Yousuke Utsumi. "The HectoMAP Cluster Survey: Spectroscopically Identified Clusters and their Brightest Cluster Galaxies (BCGs)." Astrophysical Journal 923, no. 2 (2021): 143. http://dx.doi.org/10.3847/1538-4357/ac29c3.

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Abstract We apply a friends-of-friends (FoF) algorithm to identify galaxy clusters and we use the catalog to explore the evolutionary synergy between brightest cluster galaxies (BCGs) and their host clusters. We base the cluster catalog on the dense HectoMAP redshift survey (2000 redshifts deg−2). The HectoMAP FoF catalog includes 346 clusters with 10 or more spectroscopic members within the range 0.05 < z < 0.55 and with a median z = 0.29. We list these clusters and their members. We also include central velocity dispersions (σ *,BCG) for the FoF cluster BCGs, a distinctive feature of the HectoMAP FoF catalog. HectoMAP clusters with higher galaxy number density (80 systems) are all genuine clusters with a strong concentration and a prominent BCG in Subaru/Hyper Suprime-Cam images. The phase-space diagrams show the expected elongation along the line of sight. Lower-density systems include some low reliability systems. We establish a connection between BCGs and their host clusters by demonstrating that σ *,BCG /σ cl decreases as a function of cluster velocity dispersion (σ cl), in contrast, numerical simulations predict a constant σ *,BCG/σ cl. Sets of clusters at two different redshifts show that BCG evolution in massive systems is slow over the redshift range z < 0.4. The data strongly suggest that minor mergers may play an important role in BCG evolution in clusters with σ cl ≳ 300 km s−1. For lower mass systems (σ cl < 300 km s−1), major mergers may play a significant role. The coordinated evolution of BCGs and their host clusters provides an interesting test of simulations in high-density regions of the universe.

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Martel, Hugo, Fidèle Robichaud, and Paramita Barai. "MAJOR CLUSTER MERGERS AND THE LOCATION OF THE BRIGHTEST CLUSTER GALAXY." Astrophysical Journal 786, no. 2 (2014): 79. http://dx.doi.org/10.1088/0004-637x/786/2/79.

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Chun, Kyungwon, Jihye Shin, Rory Smith, Jongwan Ko, and Jaewon Yoo. "The Formation of the Brightest Cluster Galaxy and Intracluster Light in Cosmological N-body Simulations with the Galaxy Replacement Technique." Astrophysical Journal 943, no. 2 (2023): 148. http://dx.doi.org/10.3847/1538-4357/aca890.

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Abstract We investigate the formation channels of the intracluster light (ICL) and the brightest cluster galaxy (BCG) in clusters at z = 0. For this, we perform multi-resolution cosmological N-body simulations using the “galaxy replacement technique.” We study the formation channels of the ICL and BCG as a function of distance from the cluster center and the dynamical state of the clusters at z = 0. To do this, we trace back the stars of the ICL and BCG, and identify the stellar components in which they existed when they first fell into the clusters. We find that the progenitors of the ICL and BCG in the central region of the cluster fell earlier and with a higher total mass ratio of the progenitors to the cluster compared to the outer region. This causes a negative radial gradient in the infall time and total mass ratio of the progenitors. Although stellar mass of the progenitors does not show the same radial gradient in all clusters, massive galaxies (M gal > 1010 M ⊙ h−1) are the dominant formation channel of the ICL and BCG for all clusters, except for our most relaxed cluster. For clusters that are dynamically more unrelaxed, we find that the progenitors of the ICL and BCG fall into their clusters more recently, and with a higher mass and mass ratio. Furthermore, we find that the diffuse material of massive galaxies and group-mass halos that is formed by preprocessing contributes significantly to the ICL in the outer region of the unrelaxed clusters.

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Lee, Myung Gyoon, Jang Ho Bae, and In Sung Jang. "Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39." Astrophysical Journal Letters 940, no. 1 (2022): L19. http://dx.doi.org/10.3847/2041-8213/ac990b.

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Abstract We present a survey of globular clusters (GCs) in the massive gravitational lens cluster SMACS J0723.3–7327 at z = 0.39 based on the early released JWST/NIRCam images. In the color–magnitude diagrams of the point sources, we clearly find a rich population of intracluster GCs that are spread over a wide area of the cluster. Their ages, considering the cluster redshift, are younger than 9.5 Gyr. The F200W (AB) magnitudes of these GCs, 26.5 mag < F200W0 < 29.5 mag, correspond to −15.2 mag < M F200W < −12.2 mag, showing that they belong to the brightest GCs (including ultracompact dwarfs). The spatial distributions of these GCs show a megaparsec-scale structure elongated along the major axis of the brightest cluster galaxy. In addition, they show a large number of substructures, some of which are consistent with the substructures seen in the map of diffuse intracluster light. The GC number density map is, in general, consistent with the dark matter mass density map based on the strong lensing analysis in the literature. The radial number density profile of the GCs in the outer region is steeper than the dark matter mass profile obtained from lensing models. These results are consistent with those for the GCs found in the deep HST images of A2744, another massive cluster at z = 0.308, and in simulated galaxy clusters. This shows that the intracluster GCs are an excellent independent tool to probe the dark matter distribution in galaxy clusters, as well as reveal the cluster assembly history in the JWST era.

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Lee, Myung Gyoon, Eunhyeuk Kim, and Doug Geisler. "Metallicity and Luminosity Functions of the Globular Clusters in NGC 4472." Symposium - International Astronomical Union 174 (1996): 393–94. http://dx.doi.org/10.1017/s0074180900001984.

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NGC 4472, the brightest elliptical galaxy in the Virgo cluster, has a rich globular cluster system. We present a study of the metallicity and luminosity functions of a large number of globular clusters in NGC 4472. Deep Washington CT1 photometry of a wide (16′ × 16′) field of NGC 4472 was obtained using Tek 2048 × 2048 CCD at the KPNO 4m telescope.

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Cardiel, N., J. Gorgas, and A. Aragon-Salamanca. "Spectroscopic Evidences for Star Formation in Cooling Flow Galaxies." Symposium - International Astronomical Union 171 (1996): 349. http://dx.doi.org/10.1017/s0074180900232683.

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X-ray observations have led to the conclusion that many galaxy clusters are hosting cooling flows. The brightest cluster galaxies could have accreted masses of the order of 1011–1012M⊙, but is still uncertain what the final fate of the accreted gas may be.

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Forés-Toribio, R., J. A. Muñoz, C. S. Kochanek, and E. Mediavilla. "A Mass Model for the Lensing Cluster SDSS J1004+4112: Constraints from the Third Time Delay." Astrophysical Journal 937, no. 1 (2022): 35. http://dx.doi.org/10.3847/1538-4357/ac8c40.

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Abstract We have built a new model for the lens system SDSS J1004+4112 including the recently measured time delay of the fourth quasar image. This time delay has a strong influence on the inner mass distribution of the lensing cluster (ρ ∝ r −α ) allowing us to determine α = 1.18 − 0.03 ( − 0.18 ) + 0.02 ( + 0.11 ) at the 68% (95%) confidence level in agreement with hydrodynamical simulations of massive galaxy clusters. We find an offset between the brightest cluster galaxy and the dark matter halo of 3.8 − 0.7 ( − 1.3 ) + 0.6 ( + 1.4 ) kpc at 68% (95%) confidence which is compatible with other galaxy cluster measurements. As an observational challenge, the estimated time delay between the leading image C and the faint (I = 24.7) fifth image E is roughly 8 yr.

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Giacintucci, S., T. Venturi, M. Markevitch, et al. "A Candle in the Wind: A Radio Filament in the Core of the A3562 Galaxy Cluster." Astrophysical Journal 934, no. 1 (2022): 49. http://dx.doi.org/10.3847/1538-4357/ac7805.

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Abstract Using a MeerKAT observation of the galaxy cluster A3562 (a member of the Shapley supercluster), we have discovered a narrow, long and straight, very faint radio filament, which branches out at a straight angle from the tail of a radio galaxy located in projection near the core of the cluster. The radio filament spans 200 kpc and aligns with a sloshing cold front seen in the X-rays, staying inside the front in projection. The radio spectral index along the filament appears uniform (within large uncertainties) at α ≃ −1.5. We propose that the radio galaxy is located outside the cold front but dips its tail under the front. The tangential wind that blows there may stretch the radio plasma from the radio galaxy into a filamentary structure. Some reacceleration is needed in this scenario to keep the radio spectrum uniform. Alternatively, the cosmic-ray electrons from that spot in the tail can spread along the cluster magnetic field lines, straightened by that same tangential flow, via anomalously fast diffusion. Our radio filament can provide constraints on this process. We also uncover a compact radio source at the brightest cluster galaxy that is 2–3 orders of magnitude less luminous than those in typical cluster central galaxies—probably an example of a brightest cluster galaxy starved of accretion fuel by gas sloshing.

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de Nicola, Stefano, Roberto P. Saglia, Jens Thomas, et al. "Intrinsic Shapes of Brightest Cluster Galaxies." Astrophysical Journal 933, no. 2 (2022): 215. http://dx.doi.org/10.3847/1538-4357/ac7463.

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Abstract We discuss the statistical distribution of galaxy shapes and viewing angles under the assumption of triaxiality by deprojecting observed surface brightness profiles of 56 brightest cluster galaxies (BCGs) coming from a recently published large deep-photometry sample. For the first time, we address this issue by directly measuring axis ratio profiles without limiting ourselves to a statistical analysis of average ellipticities. We show that these objects are strongly triaxial, with triaxiality parameters 0.39 ≤ T ≤ 0.72, they have average axis ratios 〈p(r)〉 = 0.84 and 〈q(r)〉 = 0.68, and they are more spherical in the central regions but flatten out at large radii. Measured shapes in the outskirts agree well with the shapes found for simulated massive galaxies and their dark matter halos from both the IllustrisTNG and the Magneticum simulations, possibly probing the nature of dark matter. In contrast, both simulations fail to reproduce the observed inner regions of BCGs, producing objects that are too flattened.

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Wen, Z. L., and J. L. Han. "Updated catalog of 132,684 galaxy clusters and evolution of brightest cluster galaxies." Proceedings of the International Astronomical Union 8, S295 (2012): 188. http://dx.doi.org/10.1017/s1743921313004754.

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AbstractWe identified 132,684 clusters in the redshift range of 0.05 < z < 0.8 from SDSS DR8. The spectroscopic redshifts of 52,683 clusters have been included in the catalog using SDSS DR9 data. We found that BCGs are more luminous in richer clusters and at higher redshifts.

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Somboonpanyakul, T., M. McDonald, A. Noble, et al. "The Evolution of AGN Activity in Brightest Cluster Galaxies." Astronomical Journal 163, no. 4 (2022): 146. http://dx.doi.org/10.3847/1538-3881/ac5030.

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Abstract We present the results of an analysis of Wide-field Infrared Survey Explorer (WISE) observations of the full 2500 deg2 South Pole Telescope (SPT)-Sunyaev–Zel’dovich cluster sample. We describe a process for identifying active galactic nuclei (AGN) in brightest cluster galaxies (BCGs) based on WISE mid-IR color and redshift. Applying this technique to the BCGs of the SPT-SZ sample, we calculate the AGN-hosting BCG fraction, which is defined as the fraction of BCGs hosting bright central AGNs over all possible BCGs. Assuming an evolving single-burst stellar population model, we find statistically significant evidence (>99.9%) for a mid-IR excess at high redshift compared to low redshift, suggesting that the fraction of AGN-hosting BCGs increases with redshift over the range of 0 < z < 1.3. The best-fit redshift trend of the AGN-hosting BCG fraction has the form (1 + z)4.1±1.0. These results are consistent with previous studies in galaxy clusters as well as as in field galaxies. One way to explain this result is that member galaxies at high redshift tend to have more cold gas. While BCGs in nearby galaxy clusters grow mostly by dry mergers with cluster members, leading to no increase in AGN activity, BCGs at high redshift could primarily merge with gas-rich satellites, providing fuel for feeding AGNs. If this observed increase in AGN activity is linked to gas-rich mergers rather than ICM cooling, we would expect to see an increase in scatter in the P cav versus L cool relation at z > 1. Last, this work confirms that the runaway cooling phase, as predicted by the classical cooling-flow model, in the Phoenix cluster is extremely rare and most BCGs have low (relative to Eddington) black hole accretion rates.

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Arnaboldi, Magda, and Ortwin Gerhard. "JD2 - Diffuse Light in Galaxy Clusters." Proceedings of the International Astronomical Union 5, H15 (2009): 97–110. http://dx.doi.org/10.1017/s174392131000846x.

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AbstractDiffuse intracluster light (ICL) has now been observed in nearby and in intermediate redshift clusters. Individual intracluster stars have been detected in the Virgo and Coma clusters and the first color-magnitude diagram and velocity measurements have been obtained. Recent studies show that the ICL contains of the order of 10% and perhaps up to 30% of the stellar mass in the cluster, but in the cores of some dense and rich clusters like Coma, the local ICL fraction can be high as 40%-50%. What can we learn from the ICL about the formation of galaxy clusters and the evolution of cluster galaxies? How and when did the ICL form? What is the connection to the central brightest cluster galaxy? Cosmological N-body and hydrodynamical simulations are beginning to make predictions for the kinematics and origin of the ICL. The ICL traces the evolution of baryonic substructures in dense environments and can thus be used to constrain some aspects of cosmological simulations that are most uncertain, such as the modeling of star formation and the mass distribution of the baryonic component in galaxies.

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Nieuwenhuizen, Theodorus M., Marceau Limousin, and Andrea Morandi. "Accurate modeling of the strong and weak lensing profiles for the galaxy clusters Abell 1689 and 1835." European Physical Journal Special Topics 230, no. 4 (2021): 1137–48. http://dx.doi.org/10.1140/epjs/s11734-021-00101-4.

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AbstractAn accurate, spherically symmetric description of the mass distribution is presented for two quite virialized galaxy clusters, Abell 1689 and Abell 1835. A suitable regularization of the small eigenvalues of the covariance matrices is introduced. A stretched exponential profile is assumed for the brightest cluster galaxy. A similar stretched exponential for the dark matter and halo galaxies combined, functions well, as do thermal fermions for the dark matter and a standard profile for the halo galaxies. To discriminate between them, sensitive tests have been identified and applied. A definite verdict can follow from sharp data near the cluster centers and beyond 1 Mpc.

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Contini, Emanuele. "On the Origin and Evolution of the Intra-Cluster Light: A Brief Review of the Most Recent Developments." Galaxies 9, no. 3 (2021): 60. http://dx.doi.org/10.3390/galaxies9030060.

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Not all the light in galaxy groups and clusters comes from stars that are bound to galaxies. A significant fraction of it constitutes the so-called intracluster or diffuse light (ICL), a low surface brightness component of groups/clusters generally found in the surroundings of the brightest cluster galaxies and intermediate/massive satellites. In this review, I will describe the mechanisms responsible for its formation and evolution, considering the large contribution given to the topic in the last decades by both the theoretical and observational sides. Starting from the methods that are commonly used to isolate the ICL, I will address the remarkable problem given by its own definition, which still makes the comparisons among different studies not trivial, to conclude by giving an overview of the most recent works that take advantage of the ICL as a luminous tracer of the dark matter distribution in galaxy groups and clusters.

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Loubser, S. I., and P. Sánchez-Blázquez. "Stellar population gradients in brightest cluster galaxies." Proceedings of the International Astronomical Union 8, S295 (2012): 316. http://dx.doi.org/10.1017/s1743921313005188.

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AbstractWe present the stellar population and velocity dispersion gradients for a sample of 24 brightest cluster galaxies (BCGs) in the nearby Universe for which we have obtained high quality long-slit spectra at the Gemini telescopes. With the aim of studying the possible connection between the formation of the BCGs and their host clusters, we explore the relations between the stellar population gradients and properties of the host clusters, as well as the possible connections between the stellar population gradients and other properties of the galaxies. We find mean stellar population gradients (negative Δ[Z/H]/log r gradient of − 0.285 ± 0.064; small positive Δlog(age)/log r gradient of +0.069 ± 0.049; and null Δ[E/Fe]/log r gradient of -0.008 ± 0.032), that are consistent with those of normal massive elliptical galaxies. However, we find a trend between metallicity gradients and velocity dispersion (with a negative slope of − 1.616 ± 0.539), that is not found for the most massive ellipticals. Furthermore, we find trends between the metallicity gradients and K-band luminosities (with a slope of 0.173 ± 0.081) as well as the distance from the BCG to the X-ray peak of the host cluster (with a slope of − 7.546 ± 2.752). The latter indicates a possible relation between the formation of the cluster and that of the central galaxy.

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Santos, J. S., I. Balestra, P. Tozzi, et al. "Starbursting brightest cluster galaxy: aHerschelview of the massive cluster MACS J1931.8−2634." Monthly Notices of the Royal Astronomical Society: Letters 456, no. 1 (2015): L99—L103. http://dx.doi.org/10.1093/mnrasl/slv179.

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Nelson, Amy E., Anthony H. Gonzalez, Dennis Zaritsky, and Julianne J. Dalcanton. "Revisiting Brightest Cluster Galaxy Evolution with the Las Campanas Distant Cluster Survey." Astrophysical Journal 566, no. 1 (2002): 103–22. http://dx.doi.org/10.1086/338054.

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Trudeau, A., C. Garrel, J. Willis, et al. "The XXL Survey." Astronomy & Astrophysics 642 (October 2020): A124. http://dx.doi.org/10.1051/0004-6361/202038982.

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Context. Distant galaxy clusters provide an effective laboratory in which to study galaxy evolution in dense environments and at early cosmic times. Aims. We aim to identify distant galaxy clusters as extended X-ray sources that are coincident with overdensities of characteristically bright galaxies. Methods. We used optical and near-infrared data from the Hyper Suprime-Cam and VISTA Deep Extragalactic Observations (VIDEO) surveys to identify distant galaxy clusters as overdensities of bright, zphot ≥ 0.8 galaxies associated with extended X-ray sources detected in the ultimate XMM extragalactic survey (XXL). Results. We identify a sample of 35 candidate clusters at 0.80 ≤ z ≤ 1.93 from an approximately 4.5 deg2 sky area. This sample includes 15 newly discovered candidate clusters, ten previously detected but unconfirmed clusters, and ten spectroscopically confirmed clusters. Although these clusters host galaxy populations that display a wide variety of quenching levels, they exhibit well-defined relations between quenching, cluster-centric distance, and galaxy luminosity. The brightest cluster galaxies (BCGs) within our sample display colours that are consistent with a bimodal population composed of an old and red sub-sample together with a bluer, more diverse sub-sample. Conclusions The relation between galaxy masses and quenching seem to already be in place at z ∼ 1, although there is no significant variation in the quenching fraction with the cluster-centric radius. The BCG bimodality might be explained by the presence of a younger stellar component in some BCGs, but additional data are needed to confirm this scenario.

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Mihos, J. Christopher. "Intragroup and Intracluster Light." Proceedings of the International Astronomical Union 11, S317 (2015): 27–34. http://dx.doi.org/10.1017/s1743921315006857.

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AbstractThe largest stellar halos in the universe are found in massive galaxy clusters, where interactions and mergers of galaxies, along with the cluster tidal field, all act to strip stars from their host galaxies and feed the diffuse intracluster light (ICL) and extended halos of brightest cluster galaxies (BCGs). Studies of the nearby Virgo Cluster reveal a variety of accretion signatures imprinted in the morphology and stellar populations of its ICL. While simulations suggest the ICL should grow with time, attempts to track this evolution across clusters spanning a range of mass and redshift have proved difficult due to a variety of observational and definitional issues. Meanwhile, studies of nearby galaxy groups reveal the earliest stages of ICL formation: the extremely diffuse tidal streams formed during interactions in the group environment.

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Tang, H., A. M. M. Scaife, O. I. Wong, et al. "Radio Galaxy Zoo: new giant radio galaxies in the RGZ DR1 catalogue." Monthly Notices of the Royal Astronomical Society 499, no. 1 (2020): 68–76. http://dx.doi.org/10.1093/mnras/staa2805.

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ABSTRACT In this paper, we present the identification of five previously unknown giant radio galaxies (GRGs) using Data Release 1 of the Radio Galaxy Zoo citizen science project and a selection method appropriate to the training and validation of deep learning algorithms for new radio surveys. We associate one of these new GRGs with the brightest cluster galaxy (BCG) in the galaxy cluster GMBCG J251.67741+36.45295 and use literature data to identify a further 13 previously known GRGs as BCG candidates, increasing the number of known BCG GRGs by $\gt 60$ per cent. By examining local galaxy number densities for the number of all known BCG GRGs, we suggest that the existence of this growing number implies that GRGs are able to reside in the centres of rich (∼1014 M⊙) galaxy clusters and challenges the hypothesis that GRGs grow to such sizes only in locally underdense environments.

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Harris, William E. "A Photometric Survey of Globular Cluster Systems in Brightest Cluster Galaxies." Astrophysical Journal Supplement Series 265, no. 1 (2023): 9. http://dx.doi.org/10.3847/1538-4365/acab5c.

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Abstract Hubble Space Telescope imaging for 26 giant early-type galaxies, all drawn from the MAST archive, is used to carry out photometry of their surrounding globular cluster (GC) systems. Most of these targets are Brightest Cluster Galaxies and their distances range from 24–210 Mpc. The catalogs of photometry, completed with DOLPHOT, are publicly available. The GC color indices are converted to [Fe/H] through a combination of 12 Gyr single stellar population models and direct spectroscopic calibration of the fiducial color index (F475W–F850LP). All of the resulting metallicity distribution functions (MDFs) can be accurately matched by bimodal-Gaussian functions. The GC systems in all of the galaxies also exhibit shallow metallicity gradients with projected galactocentric distance that average Z ∼ R gc − 0.3 . Several parameters of the MDFs including the means, dispersions, and blue/red fractions are summarized. Perhaps the most interesting new result is the trend of blue/red GC fraction with galaxy mass, which connects with predictions from recent simulations of GC formation within hierarchical assembly of large galaxies. The observed trend reveals two major transition stages: for low-mass galaxies, the metal-rich (red) GC fraction f(red) increases steadily with galaxy mass, until halo mass M h ≃ 3 × 1012 M ⊙. Above this point, more than half the metal-poor (blue) GCs come from accreted satellites and f(red) starts declining. But above a still higher transition point near M h ≃ 1014 M ⊙, the data hint that f(red) may start to increase again because the metal-rich GCs also become dominated by accreted systems.

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Meylan, G. "Anisotropy of the Velocity Dispersion in ω Centauri". Symposium - International Astronomical Union 127 (1987): 449–50. http://dx.doi.org/10.1017/s0074180900185687.

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By far the brightest and the most massive globular cluster in our Galaxy,ω Cen seems to be, in some of its properties, a kind of transition step between dwarf ellipticals and ordinary globular clusters. For this giant cluster, the comparison between observations and King-Michie multi-mass dynamical models appears possible only using models with strong anisotropy in the velocity dispersion. A more comprehensive description of this work is to be published (Meylan 1986).

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Dalal, Roohi, Michael A. Strauss, Tomomi Sunayama, et al. "Brightest cluster galaxies are statistically special from z = 0.3 to z = 1." Monthly Notices of the Royal Astronomical Society 507, no. 3 (2021): 4016–29. http://dx.doi.org/10.1093/mnras/stab2363.

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ABSTRACT We study brightest cluster galaxies (BCGs) in ∼5000 galaxy clusters from the Hyper Suprime-Cam (HSC) Subaru Strategic Program. The sample is selected over an area of 830 deg2 and is uniformly distributed in redshift over the range of z = 0.3−1.0. The clusters have stellar masses in the range of 1011.8−1012.9M⊙. We compare the stellar mass of the BCGs in each cluster to what we would expect if their masses were drawn from the mass distribution of the other member galaxies of the clusters. The BCGs are found to be ‘special’, in the sense that they are not consistent with being a statistical extreme of the mass distribution of other cluster galaxies. This result is robust over the full range of cluster stellar masses and redshifts in the sample, indicating that BCGs are special up to a redshift of z = 1.0. However, BCGs with a large separation from the centre of the cluster are found to be consistent with being statistical extremes of the cluster member mass distribution. We discuss the implications of these findings for BCG formation scenarios.

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Bharadwaj, V., T. H. Reiprich, G. Schellenberger, H. J. Eckmiller, R. Mittal, and H. Israel. "Intracluster medium cooling, AGN feedback, and brightest cluster galaxy properties of galaxy groups." Astronomy & Astrophysics 572 (November 27, 2014): A46. http://dx.doi.org/10.1051/0004-6361/201322684.

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Yee, H. K. C., and E. Ellingson. "Quasar Activity in Rich Galaxy Clusters." Highlights of Astronomy 9 (1992): 695–96. http://dx.doi.org/10.1017/s1539299600010078.

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We have carried out a number of imaging surveys of fields around quasars to study their global environments (e.g. Yee and Green 1987, Ellingson, Yee and Green 1991). The richness of the galaxy cluster environment of each quasar was determined using the galaxy-quasar spatial covariance amplitude, a quantity which is normalized for the expected luminosity and spatial distribution of galaxies (Longair and Seldner 1978, Yee and Green 1987). We find that ~40% of the brightest radio-loud quasars inhabit rich clusters of galaxies (Abell class 1 or higher) at z≳0.5 whereas only fainter AGN inhabit clusters at more recent epochs (Figure 1). This can be understood if quasars in rich clusters evolve much faster than those in poor environments.

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Contigiani, O., Y. M. Bahé, and H. Hoekstra. "The mass–size relation of galaxy clusters." Monthly Notices of the Royal Astronomical Society 505, no. 2 (2021): 2932–40. http://dx.doi.org/10.1093/mnras/stab1463.

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ABSTRACT The outskirts of accreting dark matter haloes exhibit a sudden drop in density delimiting their multistream region. Due to the dynamics of accretion, the location of this physically motivated edge strongly correlates with the halo growth rate. Using hydrodynamical zoom-in simulations of high-mass clusters, we explore this definition in realistic simulations and find an explicit connection between this feature in the dark matter and galaxy profiles. We also show that the depth of the splashback feature correlates well with the direction of filaments and, surprisingly, the orientation of the brightest cluster galaxy. Our findings suggest that galaxy profiles and weak-lensing masses can define an observationally viable mass-size scaling relation for galaxy clusters, which can be used to extract cosmological information.

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Ferrarese, Laura, and Patrick Côté. "The structure of early-type galaxies from the ACS Virgo and Fornax cluster surveys: cores, nuclei and supermassive black holes." Proceedings of the International Astronomical Union 3, S245 (2007): 203–6. http://dx.doi.org/10.1017/s1743921308017651.

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AbstractThe core structure of early-type galaxies is revisited in light of recent results from the ACS Virgo and Fornax Cluster Surveys. These surveys are comprised of HST/ACS g, z band images for a representative sample of 143 early-type galaxies, spanning a factor 720 in B-band luminosity. The data indicates a clear transition in the core structure going from the brightest to the faintest galaxies. In contrast to previous claims, however, this transition is found to be a continuous function of galaxy magnitude. We characterize the core structure in terms of deviations of the observed surface brightness profile – measured within ~ 2% of the galaxy effective radius – relative to the inner extrapolation of the Sérsic law that best fits the profiles on larger scales. Virtually all galaxies fainter than MB ~ −20 mag contain distinct stellar nuclei, and are described by surface brightness profiles that lie above the Sérsic extrapolation, while the reverse is true for brighter galaxies. The latter are also known to host supermassive black holes. A relation between SBHs and stellar nuclei is suggested by the fact that both types of “central massive objects” contain the same fraction, 0.2% of the total mass of the host galaxy.

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Lim, Sungsoon, Narae Hwang, and Myung Gyoon Lee. "Star clusters in the starburst galaxy M82." Proceedings of the International Astronomical Union 5, S266 (2009): 454–57. http://dx.doi.org/10.1017/s1743921309991682.

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AbstractWe present a study of star clusters in the starburst galaxy M82 using the BVI mosaic images taken with the Hubble Space Telescope's Advanced Camera for Surveys. We have selected about 850 clusters with V < 23 mag based on their morphological information. The brightest cluster is as bright as V ~ 16.5 mag (MV ~ −11.2 mag) and most clusters are fainter than V = 18 mag (MV = −9.7 mag). The V-band luminosity function is represented by a power law with a slope α ~ −2.0 in the range of −9.5 < MV < −7 mag. The star clusters in M82 are mainly distributed in the galaxy's disk. However, about a dozen clusters are found far from the disk and are considered to belong to the halo of M82. The color–magnitude diagrams of star clusters show that most star clusters are highly reddened. We have derived the age of the star clusters using a spectral-energy-distribution fitting method with Bruzual & Charlot simple stellar population models. We discuss the age distribution as well as the photometric properties of the star clusters in regard to the formation history of the M82 cluster population.

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Postman, Marc, Tod R. Lauer, Megan Donahue, et al. "A BRIGHTEST CLUSTER GALAXY WITH AN EXTREMELY LARGE FLAT CORE." Astrophysical Journal 756, no. 2 (2012): 159. http://dx.doi.org/10.1088/0004-637x/756/2/159.

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Loubser, S. I., and P. Sánchez-Blázquez. "Mg2 gradients as a signature of brightest cluster galaxy evolution." Monthly Notices of the Royal Astronomical Society 415, no. 4 (2011): 3013–20. http://dx.doi.org/10.1111/j.1365-2966.2011.18909.x.

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Journal articles on the topic 'Brightest cluster galaxy'

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