CO emission and associated H I absorption from a massive gas reservoir surrounding the<i>z</i>= 3 radio galaxy B3 J2330+3927

Breuck, C. De; Neri, R.; Morganti, R.; Omont, A.; Rocca‐Volmerange, B.; Stern, Daniel; Reuland, Michiel; Breugel, W. J. M. van; Röttgering, H. J. A.; Stanford, S. A.; Spinrad, Hyron; Vigotti, M.; Wright, M. C. H.

doi:10.1051/0004-6361:20030171

Cited by 87 publications

(98 citation statements)

References 100 publications

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“…In particular, it is unclear whether our results can be easily extrapolated to (radio) galaxies at high redshift, which have copious amounts of molecular gas traced through CO line emission (e.g., Papadopoulos et al 2000;De Breuck et al 2003Nesvadba et al 2009), but whose gas conditions are likely very different from those in 3C 326 N. If the kinetic energy in these galaxies can be dissipated rapidly enough to allow for gas collapse and star formation, then feedback may be positive.…”

Section: Discussionmentioning

confidence: 93%

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Nesvadba¹,

Boulanger²,

Salomé

et al. 2010

A&A

138

232

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We present a detailed analysis of the gas conditions in the H 2 luminous radio galaxy 3C 326 N at z ∼ 0.1, which has a low starformation rate (SFR ∼ 0.07 M yr −1 ) in spite of a gas surface density similar to those in starburst galaxies. Its star-formation efficiency is likely a factor ∼10−50 lower than those of ordinary star-forming galaxies. Combining new IRAM CO emission-line interferometry with existing Spitzer mid-infrared spectroscopy, we find that the luminosity ratio of CO and pure rotational H 2 line emission is factors 10−100 lower than what is usually found. This suggests that most of the molecular gas is warm. The Na D absorption-line profile of 3C 326 N in the optical suggests an outflow with a terminal velocity of ∼−1800 km s −1 and a mass outflow rate of 30−40 M yr −1 , which cannot be explained by star formation. The mechanical power implied by the wind, of order 10 43 erg s −1 , is comparable to the bolometric luminosity of the emission lines of ionized and molecular gas. To explain these observations, we propose a scenario where a small fraction of the mechanical energy of the radio jet is deposited in the interstellar medium of 3C 326 N, which powers the outflow, and the line emission through a mass, momentum and energy exchange between the different gas phases of the ISM. Dissipation times are of order 10 7−8 yrs, similar or greater than the typical jet lifetime. Small ratios of CO and PAH surface brightnesses in another 7 H 2 luminous radio galaxies suggest that a similar form of AGN feedback could be lowering star-formation efficiencies in these galaxies in a similar way. The local demographics of radio-loud AGN suggests that secular gas cooling in massive early-type galaxies of ≥10 11 M could generally be regulated through a fundamentally similar form of "maintenance-phase" AGN feedback.

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Section: Discussionmentioning

confidence: 93%

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Nesvadba¹,

Boulanger²,

Salomé

et al. 2010

A&A

138

232

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“…As we only have a single observation at 246 GHz, we fix the shape of the SED by assuming a greybody that is characterised by β = 1.5 and T d = 40 K. Following the approach of De Breuck et al (2003), using…”

Section: Mass Estimatesmentioning

confidence: 99%

ALMA finds dew drops in the dusty spider’s web

Gullberg

Lehnert

Breuck

et al. 2016

A&A

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We present 0 . 5 resolution ALMA detections of the observed 246 GHz continuum, [CI] 3 P 2 → 3 P 1 fine structure line ([CI]2-1), CO(7-6), and H 2 O lines in the z = 2.161 radio galaxy MRC1138-262, the so-called Spiderweb galaxy. We detect strong [CI]2-1 emission both at the position of the radio core, and in a second component ∼4 kpc away from it. The 1100 km s −1 broad [CI]2-1 line in this latter component, combined with its H 2 mass of 1.6 × 10 10 M , implies that this emission must come from a compact region <60 pc, possibly containing a second active galactic nucleus (AGN). The combined H 2 mass derived for both objects, using the [CI]2-1 emission, is 3.3 × 10 10 M . The total CO(7-6)/[CI]2-1 line flux ratio of 0.2 suggests a low excitation molecular gas reservoir and/or enhanced atomic carbon in cosmic ray dominated regions. We detect spatially-resolved H 2 O 2 11 −2 02 emission -for the first time in a high-z unlensed galaxy -near the outer radio lobe to the east, and near the bend of the radio jet to the west of the radio galaxy. No underlying 246 GHz continuum emission is seen at either position. We suggest that the H 2 O emission is excited in the cooling region behind slow (10-40 km s −1 ) shocks in dense molecular gas (10 3−5 cm −3 ). The extended water emission is likely evidence of the radio jet's impact on cooling and forming molecules in the post-shocked gas in the halo and inter-cluster gas, similar to what is seen in low-z clusters and other high-z radio galaxies. These observations imply that the passage of the radio jet in the interstellar and inter-cluster medium not only heats gas to high temperatures, as is commonly assumed or found in simulations, but also induces cooling and dissipation, which can lead to substantial amounts of cold dense molecular gas. The formation of molecules and strong dissipation in the halo gas of MRC1138-262 may explain both the extended diffuse molecular gas and the young stars observed around MRC1138-262.

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“…Assuming a median redshift of z = 2.2 , dust temperature T d ∼ 40 K and dust emissivity index α = 2, the 870 μm flux density of 390 μJy corresponds to a far-infrared luminosity L FIR ∼ 6.4 × 10 11 L (Eq. (11) in De Breuck et al 2003). By assuming that the submm emission originates mainly from starburst phenomena, which follows a Salpeter initial mass function with a low-mass cutoff m l = 1.6 M , we can estimate a star-formation rate S FR ∼ 60 M yr −1 using Eq.…”

Section: Stacking Analysismentioning

confidence: 99%

A LABOCA survey of submillimeter galaxies behind galaxy clusters

Johansson

Sigurdarson

Horellou

2011

A&A

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Context. Submillimeter galaxies are a population of dusty star-forming galaxies at high redshift. Measuring their properties will help relate them to other types of galaxies, both at high and low redshift. This is needed in order to understand the formation and evolution of galaxies. Aims. The aim is to use gravitational lensing by galaxy clusters to probe the faint and abundant submillimeter galaxy population down to a lower flux density level than what can be achieved in blank-field observations. Methods. We use the LABOCA bolometer camera on the APEX telescope to observe five clusters of galaxies at a wavelength of 870 μm. The final maps have an angular resolution of 27.5 and a point source noise level of 1.2-2.2 mJy. We model the mass distribution in the clusters as superpositions of spherical NFW halos and derive magnification maps that we use to calculate intrinsic flux densities as well as area-weighted number counts. We also use the positions of Spitzer MIPS 24 μm sources in four of the fields for a stacking analysis. Results. We detected 37 submm sources, out of which 14 have not been previously reported. One source has a sub-mJy intrinsic flux density. The derived number counts are consistent with previous results, after correction for gravitational magnification and completeness levels. The stacking analysis reveals an intrinsic 870 μm signal of 390 ± 27 μJy at 14.5σ significance. We study the S 24 μm -S 870 μm relation by stacking on subsamples of the 24 μm sources and find a linear relation at S 24 μm < 300 μJy, followed by a flattening at higher 24 μm flux densities. The signal from the significantly detected sources in the maps accounts for 13% of the Extragalactic Background Light discovered by COBE, and the stacked signal accounts for 11%.

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CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927

Cited by 87 publications

References 100 publications

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

ALMA finds dew drops in the dusty spider’s web

A LABOCA survey of submillimeter galaxies behind galaxy clusters

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CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927

Cited by 87 publications

References 100 publications

Energetics of the molecular gas in the H2luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Energetics of the molecular gas in the H2luminous radio galaxy 3C 326: Evidence for negative AGN feedback

ALMA finds dew drops in the dusty spider’s web

A LABOCA survey of submillimeter galaxies behind galaxy clusters

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Product

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Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback

Energetics of the molecular gas in the H₂luminous radio galaxy 3C 326: Evidence for negative AGN feedback