On the Nature of the NGC 1275 System

Conselice, Christopher J.; Gallagher, John S.; Wyse, Rosemary F. Ġ.

doi:10.1086/323534

Cited by 290 publications

(486 citation statements)

References 81 publications

(200 reference statements)

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“…In particular, SPT-CLJ0102-4915 and SPT-CLJ2106-5844 exhibit clumpy UV emission extending 61 and 57 kpc from the BCG center, respectively. This is comparable to the most extended star-forming filaments found in Abell1795 (50 kpc; McDonald & Veilleux 2009) and Perseus (60 kpc; Conselice et al 2001;Canning et al 2014). In all five Figure 10.…”

Section: Comparing X-ray and Uv Morphology For Individual Star-forminsupporting

confidence: 72%

STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

McDonald

Stalder

Bayliss

et al. 2016

ApJ

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We present a multiwavelength study of the 90 brightest cluster galaxies (BCGs) in a sample of galaxy clusters selected via the Sunyaev Zel'dovich effect by the South Pole Telescope, utilizing data from various ground-and space-based facilities. We infer the star-formation rate (SFR) for the BCG in each cluster-based on the UV and IR continuum luminosity, as well as the [O II]λλ3726,3729 emission line luminosity in cases where spectroscopy is available-and find seven systems with SFR > 100 M e yr −1 . We find that the BCG SFR exceeds 10 M e yr −1 in 31 of 90 (34%) cases at 0.25<z<1.25, compared to ∼1%-5% at z∼0 from the literature. At z1, this fraction increases to 92 31 6 -+ %, implying a steady decrease in the BCG SFR over the past ∼9 Gyr. At low-z, we find that the specific SFR in BCGs is declining more slowly with time than for field or cluster galaxies, which is most likely due to the replenishing fuel from the cooling ICM in relaxed, cool core clusters. At z0.6, the correlation between the cluster central entropy and BCG star formation-which is well established at z∼0-is not present. Instead, we find that the most star-forming BCGs at high-z are found in the cores of dynamically unrelaxed clusters. We use data from the Hubble Space Telescope to investigate the rest-frame near-UV morphology of a subsample of the most star-forming BCGs, and find complex, highly asymmetric UV morphologies on scales as large as ∼50-60 kpc. The high fraction of star-forming BCGs hosted in unrelaxed, non-cool core clusters at early times suggests that the dominant mode of fueling star formation in BCGs may have recently transitioned from galaxygalaxy interactions to ICM cooling.

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Section: Comparing X-ray and Uv Morphology For Individual Star-forminsupporting

confidence: 72%

STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

McDonald

Stalder

Bayliss

et al. 2016

ApJ

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“…Our simulations suggest that the former is capable of producing extended filaments out to aradius of 40-50 kpc from the cluster center, as seen in some clusters (Conselice et al 2001;McDonald et al 2011McDonald et al , 2015. On the other hand, the cold gas is condensed out only within the inner 20-30 kpc, consistent with the radius within which t c / t ff  10 (ºr TI ).…”

Section: Distribution Of Cold Gassupporting

confidence: 66%

“…Such a wide range of structures are also found in observations of cold gas (e.g., Donahue et al 2000;McDonald et al 2011;Werner et al 2014) and stellar populations (e.g., Donahue et al 2015;Tremblay et al 2015) in CC clusters. In particular, the long, nearly isotropic filaments extending tens of kiloparsecs in the Perseus cluster (Conselice et al 2001) are reproduced (second panel in the bottom row).…”

Section: Distribution Of Cold Gasmentioning

confidence: 92%

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Yang

Reynolds

2016

ApJ

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Feedback from the active galactic nuclei (AGNs) is one of the most promising heating mechanisms to circumvent the cooling-flow problem in galaxy clusters. However, the role of thermal conduction remains unclear. Previous studies have shown that anisotropic thermal conduction in cluster cool cores (CCs) could drive the heat-flux-driven buoyancy instabilities (HBIs) that reorient the field lines in the azimuthal directions and isolate the cores from conductive heating from the outskirts. However, how the AGN interacts with the HBI is still unknown. To understand these interwined processes, we perform the first 3D magnetohydrodynamic simulations of isolated CC clusters that include anisotropic conduction, radiative cooling, and AGN feedback. We find the following: (1) For realistic magnetic field strengths in clusters, magnetic tension can suppress a significant portion of HBI-unstable modes, and thus the HBI is either completely inhibited or significantly impaired, depending on the unknown magnetic field coherence length. (2) Turbulence driven by AGN jets can effectively randomize magnetic field lines and sustain conductivity at ∼1/3 of the Spitzer value; however, the AGN-driven turbulence is not volumefilling. (3) Conductive heating within the cores could contribute to ∼10% of the radiative losses in Perseus-like clusters and up to ∼50% for clusters twice the mass of Perseus. (4) Thermal conduction has various impacts on the AGN activity and intracluster medium properties for the hottest clusters, which may be searched by future observations to constrain the level of conductivity in clusters. The distribution of cold gas and the implications are also discussed.

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“…This can make Lyα morphology difficult to interpret in a physical sense, though it does serve as an excellent (although 'tip-of-the-iceberg') tracer for neutral hydrogen. We leverage these Lyα data for this purpose in many of the multiwavelength comparison figures listed in column (7) Conselice et al (2001), and in orange we show the FUV continuum images after Gaussian smoothing to (approximately) match the spatial resolution of the Hα maps. All image pairs are aligned and shown on a common spatial scale, with east left and north up.…”

Section: Comparison Of Fuv Lyα and Hα Morphologymentioning

confidence: 99%

Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies

Tremblay

O’Dea

Baum

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a multiwavelength morphological analysis of star forming clouds and filaments in the central (< ∼ 50 kpc) regions of 16 low redshift (z < 0.3) cool core brightest cluster galaxies (BCGs). The sample spans decades-wide ranges of X-ray mass deposition and star formation rates as well as active galactic nucleus (AGN) mechanical power, encompassing both high and low extremes of the supposed intracluster medium (ICM) cooling and AGN heating feedback cycle. New Hubble Space Telescope (HST) imaging of far ultraviolet continuum emission from young (< ∼ 10 Myr), massive (> ∼ 5 M ) stars reveals filamentary and clumpy morphologies, which we quantify by means of structural indices. The FUV data are compared with X-ray, Lyα, narrowband Hα, broadband optical/IR, and radio maps, providing a high spatial resolution atlas of star formation locales relative to the ambient hot (∼ 10 7−8 K) and warm ionised (∼ 10 4 K) gas phases, as well as the old stellar population and radio-bright AGN outflows. Nearly half of the sample possesses kpc-scale filaments that, in projection, extend toward and around radio lobes and/or X-ray cavities. These filaments may have been uplifted by the propagating jet or buoyant X-ray bubble, or may have formed in situ by cloud collapse at the interface of a radio lobe or rapid cooling in a cavity's compressed shell. Many other extended filaments, however, show no such spatial correlation, and the dominant driver of their morphology remains unclear. We nevertheless show that the morphological diversity of nearly the entire FUV sample is reproduced by recent hydrodynamical simulations in which the AGN powers a self-regulating rain of thermally unstable star forming clouds that precipitate from the hot atmosphere. In this model, precipitation triggers where the cooling-to-freefall time ratio is t cool /t ff ∼ 10. This condition is roughly met at the maxmial projected FUV radius for more than half of our sample, and clustering about this ratio is stronger for sources with higher star formation rates.

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On the Nature of the NGC 1275 System

Cited by 290 publications

References 81 publications

STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

STAR-FORMING BRIGHTEST CLUSTER GALAXIES AT 0.25 < z < 1.25: A TRANSITIONING FUEL SUPPLY

Interplay Among Cooling, Agn Feedback, and Anisotropic Conduction in the Cool Cores of Galaxy Clusters

Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies

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