Tides, Interactions, and Fine-Scale Substructures in Galaxy Clusters

Conselice, Christopher J.; Gallagher, John S.

doi:10.1086/300697

Cited by 33 publications

(34 citation statements)

References 92 publications

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“…at approximately (X, Y) = (600, −250) in Ph-C). Extensive diffuse light and a handful of bright streams have been observed in nearby clusters (Conselice & Gallagher 1999;Feldmeier et al 2004 Melnick, Hoessel & White 1977;Thuan & Kormendy 1977;Trentham & Mobasher 1998;Adami et al 2005) which has a broad stream of length ∼130 kpc, width 15-30 kpc, μ R ∼ 25.7 mag arcsec −2 and no obvious progenitor (Gregg & West 1998). Fig.…”

Section: Imagesmentioning

confidence: 95%

Surface photometry of brightest cluster galaxies and intracluster stars in ΛCDM

Cooper

Gao

Guo

et al. 2015

Monthly Notices of the Royal Astronomical Society

141

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We simulate the phase-space distribution of stellar mass in nine massive ΛCDM galaxy clusters by applying the semi-analytic particle tagging method of Cooper et al. to the Phoenix suite of high-resolution N -body simulations (M 200 ≈ 7.5-33 × 10 14 M ). The resulting surface brightness (SB) profiles of brightest cluster galaxies (BCGs) match well to observations. On average, stars formed in galaxies accreted by the BCG account for 90 per cent of its total mass (the remainder is formed in situ). In circular BCG-centred apertures, the superposition of multiple debris clouds (each 10 per cent of the total BCG mass) from different progenitors can result in an extensive outer diffuse component, qualitatively similar to a 'cD envelope'. These clouds typically originate from tidal stripping at z 1 and comprise both streams and the extended envelopes of other massive galaxies in the cluster. Stars at very low SB contribute a significant fraction of the total cluster stellar mass budget: in the central 1 Mpc 2 of a z ∼ 0.15 cluster imaged at SDSS-like resolution, our fiducial model predicts 80-95 per cent of stellar mass below a SB of µ V ∼ 26.5 mag arcsec −2 is associated with accreted stars in the envelope of the BCG. The ratio of BCG stellar mass (including this diffuse component) to total cluster stellar mass is ∼ 30 per cent.

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Section: Imagesmentioning

confidence: 95%

Surface photometry of brightest cluster galaxies and intracluster stars in ΛCDM

Cooper

Gao

Guo

et al. 2015

Monthly Notices of the Royal Astronomical Society

141

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show abstract

“…Other distorted galaxies exist near NGC 1275 (Conselice & Gallagher 1999), demonstrating that this can be a hostile location for smaller galaxies. The large inferred cooling Ñow in the ICM would imply a higher density ICM (see, e.g., Fabian et al 1981 ;White & Sarazin 1988), o †ering an efficient mechanism for removing interstellar gas from an infalling galaxy and thereby further distorting the system.…”

Section: Hv Systemmentioning

confidence: 99%

On the Nature of the NGC 1275 System

Conselice

Gallagher

Wyse

2001

The Astronomical Journal

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290

442

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Subarcsecond images, taken in B, R, and Ha Ðlters, and area spectroscopy obtained with the WIYN 3.5 m telescope provide the basis for an investigation of the unusual structures in the stellar body and ionized gas in and around the Perseus Cluster central galaxy NGC 1275. Our Ha Ðlter is tuned to gas at the velocity of NGC 1275, revealing complex, probably unresolved, small-scale features in the extended ionized gas, located up to 50 kpc from NGC 1275. The mean Ha surface brightness varies little h 100 1 along the outer Ðlaments ; this, together with the complex excitation state demonstrated by spectra, imply that the Ðlaments are likely to be tubes, or ribbons, of gas. The morphology, location, and inferred physical parameters of the gas in the Ðlaments are consistent with a model, whereby the Ðlaments form through compression of the intracluster gas by relativistic plasma emitted from the active nucleus of NGC 1275. Imaging spectroscopy with the DensePak Ðber array on WIYN suggests partial rotational support of the inner component of low-velocity ionized gas. Our broadband data is used to derive color maps of the stellar distribution and also to investigate asymmetries in the stellar surface brightness. We conÐrm and extend evidence for features in the stellar body of NGC 1275 and identify outer stellar regions containing very blue, probably very young, star clusters. We interpret these as evidence for recent accretion of a gas-rich system, with subsequent star formation. Other star clusters are identiÐed, some of which are possibly associated with the high-velocity 8200 km s~1 emission-line system being in the same projected location. We suggest that two main processes, which may be causally connected, are responsible for the rich phenomenology of the NGC 1275 systemÈNGC 1275 experienced a recent merger and/or interaction with a group of gas-rich galaxies, and recent outÑows from its AGN have compressed the intracluster gas and perhaps the gas in the infalling galaxies to produce a complex web of Ðlaments.

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“…These interactions can result in significant mass loss (Conselice 2002), and are likely ongoing in clusters today (Conselice & Gallagher 1999;Gregg & West 2004;Adami et al 2005). This may also be an important process for forming dwarf galaxies.…”

Section: Limits On the N-body Modelsmentioning

confidence: 99%

Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints

Conselice

2006

ApJ

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196

376

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We present the results of a series of empirical computations regarding the role of major mergers in forming the stellar masses of modern galaxies based on measured galaxy merger and star formation histories from z $ 0:5 to 3. We reconstruct the merger history of normal field galaxies from z $ 3 to z $ 0 as a function of initial mass using published pair fractions and merger fractions from structural analyses. We calibrate the observed merger timescale and mass ratios for galaxy mergers using self-consistent N-body models of mergers with mass ratios from 1:1 to 1:5 at various orbital properties and viewing angles. We use these simulations to determine the timescales and mass ratios that produce structures that would be identified as major mergers. Based on these calculations, we argue that a typical massive galaxy at z $ 3 with M Ã > 10 10 M undergoes 4:4 þ1:6 À0:9 major mergers at z > 1. We find that by z $ 1:5 the stellar mass of an average massive galaxy is relatively established, a scenario qualitatively favored in a Ã-dominated universe. We argue that the final masses of these systems increase by as much as a factor of 100, allowing Lyman break galaxies, which tend to have low stellar masses, to become the most massive galaxies in today's universe with M > M Ã . Induced star formation, however, only accounts for 10%-30% of the stellar mass formed in these galaxies at z < 3. A comparison to semianalytic models of galaxy formation shows that cold dark matter (CDM ) models consistently underpredict the merger fraction, and rate of merging, of massive galaxies at high redshift. This suggests that massive galaxy formation occurs through more merging than predicted in CDM models, rather than a rapid early collapse.

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Tides, Interactions, and Fine-Scale Substructures in Galaxy Clusters

Cited by 33 publications

References 92 publications

Surface photometry of brightest cluster galaxies and intracluster stars in ΛCDM

Surface photometry of brightest cluster galaxies and intracluster stars in ΛCDM

On the Nature of the NGC 1275 System

Early and Rapid Merging as a Formation Mechanism of Massive Galaxies: Empirical Constraints

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