The radio/optical alignment of high-z radio galaxies: triggering of star formation in radio lobes

Rees, M. J.

doi:10.1093/mnras/239.1.1p

Cited by 179 publications

(119 citation statements)

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“…In a recent work Rawlings & Jarvis (2004) agreed that RG lobes will penetrate much of the relevant universe, but they argued that this may often shut off star formation by expelling gas from protoclusters. However, they assume a single-phase medium, unlike our picture or that of Rees (1989), so this negative conclusion is not surprising. Many recent observational studies (e.g., Böhringer et al 1995;Bîrzan et al 2004;Choi et al 2004;O'Dea et al 2004;Reynolds et al 2005) show depressions in X-ray surface brightness coinciding with radio lobes, cavities, and buoyant bubbles in clusters of galaxies; these are clear signatures of the interactions of radio sources with their surrounding hot intracluster gas on scales of several tens to hundreds of kiloparsecs from the AGN.…”

Section: Introductionmentioning

confidence: 53%

“…Observational investigations show remarkable radio-optical alignment in high-z RGs (e.g., McCarthy et al 1987;Chambers et al 1988aChambers et al , 1988bDey et al 1997;Venemans et al 2004Venemans et al , 2005Greve et al 2006;Overzier et al 2006;Zheng et al 2006;Ajiki et al 2006). Some studies attribute this to FR II RGs triggering extensive star formation in a multiphase intergalactic medium (IGM; e.g., Begelman & Cioffi 1989;De Young 1989;Rees 1989;Chokshi 1997;GKW01). In addition, the expanding RG lobes could easily have infused significant magnetic fields into the IGM (GKW01; GWO03; GWB04).…”

Section: Introductionmentioning

confidence: 99%

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Testing Models of Radio Galaxy Evolution and the Cosmological Impact of FR II Radio Galaxies

Barai

Wiita

2007

ApJ

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We investigate aspects of the cosmological evolution of FR II radio galaxies, focusing first on the abilities of models to match data for linear sizes, radio powers, redshifts, and spectral indices. Here we consider modifications to the theoretical models we had treated earlier, primarily by accounting for the growth of the radius of hot spots with source size. Better fits to the distributions of most of the data in three low-frequency surveys can be found with sensible choices of model parameters, but no model yet considered gives a good match to all of the survey data simultaneously, nor does any do a good job of producing the spectral index distributions. The observational data sets are too small to completely discriminate among the models. We calculate the volume fraction of the ''relevant universe'' cumulatively occupied by the expanding radio galaxy lobes over the quasar era, when these powerful radio galaxies were much more common, and when they have been argued to play an important role in triggering galaxy formation and spreading magnetic fields and metals. We found the cumulative relevant volume filling factor of radio galaxies to be $5%, so we conclude that these impacts are smaller than previously estimated but that they are still significant.

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Section: Introductionmentioning

confidence: 53%

Section: Introductionmentioning

confidence: 99%

Testing Models of Radio Galaxy Evolution and the Cosmological Impact of FR II Radio Galaxies

Barai

Wiita

2007

ApJ

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“…The gas can then collapse into clouds which are dense enough to start forming stars. The scenario was proposed by Rees (1989) for high redshift galaxies where the powerful radio jet was suggested to induce star-formation along its propagation axis. Radio jets with high Mach numbers (M ∼ 10 − 100) at their terminating shocks have too much power and entrain the lowentropy gas away from the galaxy uplifting it in buoyant bubbles (e.g.…”

Section: Cause For Enhanced Star Formation In the 'Sausage' Clustermentioning

confidence: 99%

The rise and fall of star formation in z ∼ 0.2 merging galaxy clusters

Stroe¹,

Sobral²,

Dawson³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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CIZA J2242.8+5301 ('Sausage') and 1RXS J0603.3+4213 ('Toothbrush') are two lowredshift (z ∼ 0.2), massive (∼ 2 × 10 15 M ), post-core passage merging clusters, which host shock waves traced by diffuse radio emission. To study their star-formation properties, we uniformly survey the 'Sausage' and 'Toothbrush' clusters in broad and narrow band filters and select a sample of 201 and 463 line emitters, down to a rest-frame equivalent width (13Å). We robustly separate between Hα and higher redshift emitters using a combination of optical multi-band (B, g, V, r, i, z) and spectroscopic data. We build Hα luminosity functions for the entire cluster region, near the shock fronts, and away from the shock fronts and find striking differences between the two clusters. In the dynamically younger, 1 Gyr old 'Sausage' cluster we find numerous (59) Hα emitters above a star-formation rate (SFR) of 0.17 M yr −1 surprisingly located in close proximity to the shock fronts, embedded in very hot intra-cluster medium plasma. The SFR density for the cluster population is at least at the level of typical galaxies at z ∼ 2. Down to the same star-formation rate, the possibly dynamically more evolved 'Toothbrush' cluster has only 9 Hα galaxies. The cluster Hα galaxies fall on the SFRstellar mass relation z ∼ 0.2 for the field. However, the 'Sausage' cluster has an Hα emitter density > 20 times that of blank fields. If the shock passes through gas-rich cluster galaxies, the compressed gas could collapse into dense clouds and excite star-formation for a few 100 Myr. This process ultimately leads to a rapid consumption of the molecular gas, accelerating the transformation of gas-rich field spirals into cluster S0s or ellipticals.

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“…the shock-/jet-induced star formation models by Elmegreen & Elmegreen 1978;Voit 1988;De Young 1989;McNamara & O'Connell 1993). Jet-induced star formation has for many years been considered as a plausible explanation for the high-redshift alignment effect (Rees 1989;Daly 1990). …”

Section: Star-forming Filaments Aligned With Radio Jets and Lobesmentioning

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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The radio/optical alignment of high-z radio galaxies: triggering of star formation in radio lobes

Cited by 179 publications

References 0 publications

Testing Models of Radio Galaxy Evolution and the Cosmological Impact of FR II Radio Galaxies

Testing Models of Radio Galaxy Evolution and the Cosmological Impact of FR II Radio Galaxies

The rise and fall of star formation in z ∼ 0.2 merging galaxy clusters

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

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