Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Harris, William E.; Mulholland, Courtney J.

doi:10.3847/1538-4357/aa6a59

Cited by 4 publications

(7 citation statements)

References 80 publications

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“…The data from this annulus appears to be complete to I E = 25.8 so we limited the fit to 22.7 < I E < 25.8. We derived a turn-over magnitude of I E = 26.24 ± 0.12 and σ = 1.39±0.05 mag, which is consistent with empirical expectations (Jordán et al 2007;Villegas et al 2010;Harris et al 2014) and previous measurements of the GCLF within this galaxy (Harris & Mulholland 2017). The goodness-of-fit of the Gaussian model is given by the reduced χ 2 metric.…”

Section: Annulus [Kpc]supporting

confidence: 89%

“…Jordán et al 2007). At the distance of Perseus, this Gaussian is expected to peak at a magnitude of I E ∼ 26.3 with a σ ∼ 1.3 mag, which is consistent with measurements of NGC 1275 by Harris & Mulholland (2017).…”

Section: Luminosity Function Of the Globular Clusterssupporting

confidence: 85%

“…9, are remarkably different. Both profiles reveal a flattening towards their cores, consistent with Penny et al (2012) and Harris & Mulholland (2017), and likely due to incompleteness. However, the central 10-20 kpc region of NGC 1275 contains over twice the GC density of NGC 1272.…”

Section: Radial Profile Of the Intracluster Light And Intracluster Gl...supporting

confidence: 56%

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Structure of Brightest Cluster Galaxies and Intracluster Light

Kluge

Neureiter

Riffeser

et al. 2020

ApJS

120

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Observations of 170 local (z 0.08) galaxy clusters in the northern hemisphere have been obtained with the Wendelstein Telescope Wide Field Imager (WWFI). We correct for systematic effects such as PSF broadening, foreground stars contamination, relative bias offsets and charge persistence. Scattered light induced background inhomogeneities are reduced down to ∆SB > 31 g' mag arcsec −2 by large dithering and subtraction of night-sky flats. Residual background inhomogeneities brighter than SB σ < 27.6 g' mag arcsec −2 caused by galactic cirrus are detected in front of 23% of the clusters. However, the large field of view allows to discriminate between accretion signatures and galactic cirrus. We detect accretion signatures in form of tidal streams in 22%, shells in 9.4%, multiple nuclei in 47% and two Brightest Cluster Galaxies (BCGs) in 7% of the clusters / BCGs.We measure semi-major axis surface brightness profiles of the BCGs and their surrounding Intracluster Light (ICL) down to a limiting surface brightness of SB = 30 g' mag arcsec −2 . The spatial resolution in the inner regions is increased by combining the WWFI light profiles with those that we measured from archival Hubble Space Telescope images or deconvolved WWFI images. We find that 71% of the BCG+ICL systems have SB profiles that are well described by a single Sérsic (SS) function whereas 29% require a double Sérsic (DS) function to obtain a good fit. SS BCGs, having more symmetric isophotal shapes and fewer detected accretion signatures than DS BCGs, appear to have slightly more relaxed morphology than their DS counterparts. Members of the latter type encompass S2 = 52 ± 21% of their total light in the outer Sérsic component. There is a wide scatter in transition radii r × between the two Sérsic components and surface brightnesses at the transition radii SB(r × ). The integrated brightnesses of the BCG+ICL systems correlate only weakly with S2, r × and SB(r × ). That indicates that the outer Sérsic component is unlikely to trace the dynamically hot ICL since BCG+ICL systems grow at present epoch predominantly in their outskirts.We find that BCGs have scaling relations that differ markedly from those of normal ellipticals, likely due to their indistinguishable embedding in the ICL. The most extended BCG+ICL systems have luminosities and radii comparable to whole clusters. We use different plausible estimates for the ICL component (based on an integrated brightness threshold, SB thresholds and profile decompositions) and find that they do not affect our conclusions about the properties of the ICL. On average, the ICL seems to be better aligned than the BCG with the host cluster in terms of position angle and centering. That makes it a potential Dark Matter tracer. We find positive correlations between BCG+ICL brightness and cluster mass, cluster radius, cluster richness and integrated satellite brightness, confirming that BCG/ICL growth is indeed coupled with cluster growth.

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Section: Annulus [Kpc]supporting

confidence: 89%

Section: Luminosity Function Of the Globular Clusterssupporting

confidence: 85%

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Structure of Brightest Cluster Galaxies and Intracluster Light

Kluge

Neureiter

Riffeser

et al. 2020

ApJS

120

View full text Add to dashboard Cite

show abstract

“…West et al (2011) confirmed the presence of ∼ 1300 globular clusters in the Abell 1185 galaxy cluster that apparently are not bound to any galaxy. Recently, Harris and Mulholland (2017) estimate ∼ 50000 − 80000 intra-cluster globular clusters in the Perseus cluster, with a radial distribution extending several kiloparsecs away from the cluster center.…”

Section: Introductionmentioning

confidence: 99%

Intra-cluster Globular Clusters in a Simulated Galaxy Cluster

Ramos

Abadi

Muriel

et al. 2018

ApJ

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Using a cosmological dark matter simulation of a galaxy-cluster halo, we follow the temporal evolution of its globular cluster population. To mimic the red and blue globular cluster populations, we select at high redshift (z ∼ 1) two sets of particles from individual galactic halos constrained by the fact that, at redshift z = 0, they have density profiles similar to observed ones. At redshift z = 0, approximately 60% of our selected globular clusters were removed from their original halos building up the intra-cluster globular cluster population, while the remaining 40% are still gravitationally bound to their original galactic halos. Since the blue population is more extended than the red one, the intra-cluster globular cluster population is dominated by blue globular clusters, with a relative fraction that grows from 60% at redshift z = 0 up to 83% for redshift z ∼ 2. In agreement with observational results for the Virgo galaxy cluster, the blue intra-cluster globular cluster population is more spatially extended than the red one, pointing to a tidally disrupted origin.

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“…We recall that several compact galaxies are found in galaxy clusters, like NGC 1277, which is located in the core of the Perseus cluster . Recent HST observations seem to suggest that a significant population of intracluster stars is also present in the Perseus cluster (Harris & Mulholland 2017).…”

Section: Discussionmentioning

confidence: 99%

Ultramassive black hole feedback in compact galaxies

Ishibashi

Fabian

2017

Monthly Notices of the Royal Astronomical Society

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Recent observations confirm the existence of ultra-massive black holes (UMBH) in the nuclei of compact galaxies, with physical properties similar to NGC 1277. The nature of these objects poses a new puzzle to the 'black hole-host galaxy co-evolution' scenario. We discuss the potential link between UMBH and galaxy compactness, possibly connected via extreme active galactic nucleus (AGN) feedback at early times (z > 2). In our picture, AGN feedback is driven by radiation pressure on dust. We suggest that early UMBH feedback blows away all the gas beyond a ∼kpc or so, while triggering star formation at inner radii, eventually leaving a compact galaxy remnant. Such extreme UMBH feedback can also affect the surrounding environment on larger scales, e.g. the outflowing stars may form a diffuse stellar halo around the compact galaxy, or even escape into the intergalactic or intracluster medium. On the other hand, less massive black holes will drive less powerful feedback, such that the stars formed within the AGN feedback-driven outflow remain bound to the host galaxy, and contribute to its size growth over cosmic time.

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Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Cited by 4 publications

References 80 publications

Structure of Brightest Cluster Galaxies and Intracluster Light

Structure of Brightest Cluster Galaxies and Intracluster Light

Intra-cluster Globular Clusters in a Simulated Galaxy Cluster

Ultramassive black hole feedback in compact galaxies

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