<i>HUBBLE SPACE TELESCOPE</i>FAR-ULTRAVIOLET OBSERVATIONS OF BRIGHTEST CLUSTER GALAXIES: THE ROLE OF STAR FORMATION IN COOLING FLOWS AND BCG EVOLUTION

O’Dea, Kieran P.; Quillen, Alice C.; O’Dea, C. P.; Tremblay, G. R.; Snios, Bradford; Baum, Stefi A.; Christiansen, Kevin; Noel-Storr, J.; Edge, A. C.; Donahue, M.; Voit, G. Mark

doi:10.1088/0004-637x/719/2/1619

Cited by 81 publications

(111 citation statements)

References 71 publications

(126 reference statements)

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“…Two of the BCGs shown in Figure 8 (SPT-CLJ0000-5748, SPT-CLJ2043-5035) appear to be in the midst of major mergers, based on both the near-IR and near-UV imaging, despite the fact that these two BCGs reside in the two most relaxed high-z clusters in our sample. None of the starforming BCGs in this high-z, relaxed cluster subsample show evidence for extended, asymmetric filaments of star formation, which are commonly found in analogous low-z systems (e.g., O'Dea et al 2010;McDonald et al 2011b;Donahue et al 2015, Tremblay et al 2015. Instead, the UV emission is concentrated in the BCG center for four out of five BCGs, perhaps indicating that these systems are experiencing either nuclear starbursts or are AGN misidentified as star-forming galaxies.…”

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

confidence: 71%

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-forminmentioning

confidence: 71%

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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“…Edge and collaborators (Edge et al 2010a,b;Mittal et al 2011Mittal et al , 2012Rawle et al 2012;Tremblay et al 2012a,b;Hamer et al 2014), selected to span a wide range of both cooling flow and BCG physical properties. The remaining five targets are from the non-overlapping sample of O'Dea et al (2010), selected from the Quillen et al (2008) sample on the basis of elevated infrared-estimated SFRs.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Tremblay et al 2012a,b), or in elevated episodes as the AGN varies in power (e.g. O'Dea et al 2010;Tremblay 2011). Relative to field galaxies or those in non-CC clusters, BCGs in CCs preferentially harbour radio sources and kpc-scale filamentary forbidden and Balmer emission line nebulae amid 10 9 -10 11 M repositories of vibrationally excited and cold molecular gas (Heckman 1981;Hu, Cowie & Wang 1985;Baum 1987;Heckman et al 1989;Burns 1990;Jaffe & Bremer 1997;Donahue et al 2000;Edge 2001;Edge & Frayer 2003;Salomé & Combes 2003;Egami et al 2006;Salomé et al 2006;Edwards et al 2007; von der Wilman, Edge & Swinbank 2009;Edge et al 2010a,b;Salomé et al 2011;McNamara et al 2014;Russell et al 2014).…”

mentioning

confidence: 99%

“…Low to moderate levels (∼1 to 10 M yr −1 ) of star formation appear to be ongoing amid these mysteriously dusty (O'Dea et al 2008;Quillen et al 2008;Edge et al 2010a,b;Mittal et al 2011;Rawle et al 2012;Tremblay et al 2012b), polycyclic aromatic hydrocarbon (PAH)-rich (Donahue et al 2011) cold reservoirs on 50 kpc scales in clumpy and filamentary distributions (e.g. Johnstone, Fabian & Nulsen 1987;McNamara et al 2004;O'Dea et al 2004O'Dea et al , 2008O'Dea et al , 2010Rafferty et al 2006;McDonald et al 2011b;Tremblay et al 2014). The ionization states of the nebulae have been a mystery for three decades, and debate continues over the roles played by stellar photoionization, shocks, thermal conduction, mixing, and cosmic ray heating (e.g.…”

mentioning

confidence: 99%

“…The ionization states of the nebulae have been a mystery for three decades, and debate continues over the roles played by stellar photoionization, shocks, thermal conduction, mixing, and cosmic ray heating (e.g. Voit & Donahue 1997;Ferland et al 2009;Sparks et al 2009Sparks et al , 2012McDonald et al 2010;O'Dea et al 2010;Fabian et al 2011b;McDonald, Veilleux & Rupke 2011a;Mittal et al 2011;Oonk et al 2011;Tremblay 2011;Johnstone et al 2012). Whatever the case, there is strong evidence that young stars might play an important (although not exclusive) role in dictating the physics of both the warm (∼10 4 K) and cold (∼100 K) phases of the filaments (Voit & Donahue 1997;Canning et al 2010Canning et al , 2014McDonald et al 2010McDonald et al , 2011aO'Dea et al 2010).…”

mentioning

confidence: 99%

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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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The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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HUBBLE SPACE TELESCOPEFAR-ULTRAVIOLET OBSERVATIONS OF BRIGHTEST CLUSTER GALAXIES: THE ROLE OF STAR FORMATION IN COOLING FLOWS AND BCG EVOLUTION

Cited by 81 publications

References 71 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

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

The jet feedback mechanism (JFM) in stars, galaxies and clusters

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