Filamentary star formation in NGC 1275

Canning, R. E. A.; Ryon, J. E.; Gallagher, John S.; Kotulla, Ralf; O’Connell, R. W.; Fabian, A. C.; Johnstone, R. M.; Conselice, Christopher J.; Hicks, A. K.; Rosario, D. J.; Wyse, Rosemary F. Ġ.

doi:10.1093/mnras/stu1191

Cited by 55 publications

(61 citation statements)

References 94 publications

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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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“…Star formation also occurs in a minority of the extended cool gas filaments in the Perseus cluster despite their substantial molecular gas mass (Canning et al 2014). Only three separate regions of the outer filaments have been disrupted by an unknown mechanism and rapidly collapsed into stars < 50 Myr ago (Canning et al at University of Durham on March 17, 2016 http://mnras.oxfordjournals.org/ Downloaded from 2014).…”

Section: Forming Molecular Gas In Extended Filamentsmentioning

confidence: 99%

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Russell

McNamara

Fabian

et al. 2016

Mon. Not. R. Astron. Soc.

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105

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We present ALMA observations of the CO(1-0) and CO(3-2) line emission tracing filaments of cold molecular gas in the central galaxy of the cluster PKS 0745-191. The total molecular gas mass of 4.6±0.3×10 9 M , assuming a Galactic X CO factor, is divided roughly equally between three filaments each extending radially 3 − 5 kpc from the galaxy centre. The emission peak is located in the SE filament ∼ 1 arcsec (2 kpc) from the nucleus. The velocities of the molecular clouds in the filaments are low, lying within ±100 km s −1 of the galaxy's systemic velocity. Their FWHMs are less than 150 km s −1 , which is significantly below the stellar velocity dispersion. Although the molecular mass of each filament is comparable to a rich spiral galaxy, such low velocities show that the filaments are transient and the clouds would disperse on < 10 7 yr timescales unless supported, likely by the indirect effect of magnetic fields. The velocity structure is inconsistent with a merger origin or gravitational free-fall of cooling gas in this massive central galaxy. If the molecular clouds originated in gas cooling even a few kpc from their current locations their velocities would exceed those observed. Instead, the projection of the N and SE filaments underneath X-ray cavities suggests they formed in the updraft behind bubbles buoyantly rising through the cluster atmosphere. Direct uplift of the dense gas by the radio bubbles appears to require an implausibly high coupling efficiency. The filaments are coincident with low temperature X-ray gas, bright optical line emission and dust lanes indicating that the molecular gas could have formed from lifted warmer gas that cooled in situ.

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“…Moreover, some blue star-forming filaments apparently lack cospatial Hα emission (e.g. the 'blue loop' in Perseus; Fabian et al 2008;Canning et al 2010Canning et al , 2014. Hα traces the contemporary SFR via the instantaneous flux of ionizing photons from the most massive (M 15 M ) O and early B-type stars, while the more heavily extincted UV excess associated with the photospheres of less massive (M 5 M ) young stars can shine long after those most massive stars powering the Hα flux are gone.…”

Section: Comparison Of Fuv Lyα and Hα Morphologymentioning

confidence: 99%

“…Fabian 2003;Hatch et al 2006;Canning et al 2010Canning et al , 2014McDonald et al 2011b). The spatial associations are certainly compelling, and filament uplift by cavities may indeed be an important and even common effect.…”

Section: Spatial Correlations and Anti-correlations Of Star-forming Fmentioning

confidence: 99%

“…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).…”

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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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Filamentary star formation in NGC 1275

Cited by 55 publications

References 94 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

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

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

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