An Obscured Radio Galaxy at High Redshift

Reuland, Michiel; Breugel, Wil van; Röttgering, H. J. A.; Vries, Wim de; Breuck, C. De; Stern, Daniel

doi:10.1086/367689

Cited by 14 publications

(16 citation statements)

References 31 publications

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“…Miley & De Breuck 2008), meaning that samples selected in the above way may not be completely representative of high‐ z radio galaxies. Interestingly, it has been suggested that these ‘no‐line’ radio galaxies are very dusty, based on millimetre/submillimetre detections thereof (Reuland et al 2003b; Reuland 2005).…”

Section: Datamentioning

confidence: 99%

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AzTEC 1.1-mm images of 16 radio galaxies at 0.5 < z < 5.2 and a quasar at z= 6.3

Humphrey

Zeballos

Aretxaga

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present 1.1-mm observations for a sample of 16 powerful radio galaxies at 0.5 < z < 5.2 and a radio-quiet quasar at z = 6.3, obtained using the AzTEC bolometer array mounted on the Atacama Submillimetre Telescope Experiment (ASTE) or the James Clerk Maxwell Telescope (JCMT). This paper more than doubles the number of high-z radio galaxies imaged at millimetre/submillimetre wavelengths. We detect probable millimetre-wave counterparts for 11 of the active galaxies. The six active galaxies that do not have a probable millimetre counterpart in our images nevertheless have one or more likely associated millimetric source. Thus, we conclude that powerful (radio-loud) active galaxies at high-z are beacons for finding luminous millimetre/submillimetre galaxies at high-z. The flux densities of our AzTEC counterparts imply star formation rates ranging from <200 to ∼1300 M yr −1 . In addition, we find that for the radio galaxies the 1.1-mm flux density is anticorrelated with the largest angular size of the radio source.We also present new Spitzer imaging observations of several active galaxies in our sample. Combining these with archival data, we examine the mid-infrared colours of our sample. We find that radio galaxies for which we have detected a probable 1.1-mm counterpart have mid-infrared colours consistent with dusty starbursts, and are usually bluer than high-z Spitzerselected active galaxies. In addition, we find arcs of 24-µm sources extending across ∼200-500 kpc, apparently associated with three of the radio galaxies.

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Section: Datamentioning

confidence: 99%

“…Shown in Fig. 6 is S 1.1 versus radio size for the AzTEC counterparts together with HzRGs that have been observed at 850 m using SCUBA (Archibald et al 2001; Reuland et al 2003b, 2004; Stevens et al 2003). SCUBA 850‐m flux densities have been scaled by 1/2.5 to extrapolate their 1.1‐mm flux densities.…”

Section: Comparison With Radio and Optical Propertiesmentioning

confidence: 99%

AzTEC 1.1-mm images of 16 radio galaxies at 0.5 < z < 5.2 and a quasar at z= 6.3

Humphrey

Zeballos

Aretxaga

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…Reuland et al 2003a), or not located at the centre of the host galaxy (e.g. Quirrenbach et al 2001).…”

Section: Where Is the Agn?mentioning

confidence: 99%

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

Breuck

Neri²,

Morganti³

et al. 2003

A&A

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Abstract. We present results of a comprehensive multi-frequency study of the radio galaxy B3 J2330+3927. The 1. 9 wide radio source, consisting of 3 components, is bracketed by 2 objects in our Keck K-band image. Optical and near-IR Keck spectroscopy of these two objects yield z = 3.087 ± 0.004. The brightest (K = 18.8) object has a standard type II AGN spectrum, and is the most likely location of the AGN, which implies a one-sided jet radio morphology. Deep 113 GHz observations with the IRAM Plateau de Bure Interferometer reveal CO J = 4−3 emission, which peaks at the position of the AGN. The CO line is offset by 500 km s −1 from the systemic redshift of the AGN, but corresponds very closely to the velocity shift of an associated H I absorber seen in Lyα. This strongly suggests that both originate from the same gas reservoir surrounding the AGN host galaxy. Simultaneous 230 GHz interferometer observations find a ∼3× lower integrated flux density when compared to single dish 250 GHz observations with MAMBO at the IRAM 30 m telescope. This can be interpreted as spatially resolved thermal dust emission at scales of 0. 5 to 6 . Finally, we present a τ < 1.3% limit to the H I 21 cm absorption against the radio source, which represents the seventh nondetection out of 8 z > 2 radio galaxies observed to date with the WSRT. We present mass estimates for the atomic, neutral, and ionized hydrogen, and for the dust, ranging from M(H I) = 2 × 10 7 M derived from the associated H I absorber in Lyα up to M(H 2 ) = 7 × 10 10 M derived from the CO emission. This indicates that the host galaxy is surrounded by a massive reservoir of gas and dust. The K-band companion objects may be concentrations within this reservoir, which will eventually merge with the central galaxy hosting the AGN.

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“…This is supported by the number density evolution of quasars and radio galaxies (Wall et al 2005;Richards et al 2006a) being similar to the evolution of the star formation rate (SFR) density with redshift (e.g., Giavalisco et al 2004). Observations of significant farinfrared (IR) emission potentially suggest starbursts associated with high-z quasars and radio galaxies (e.g., Willott et al 2002;Reuland et al 2003;Beelen et al 2006) and indicate rapid growth of the host galaxy, likely fueled by mergers (Hutchings et al 2006;Hopkins et al 2006). Studies of the young stellar populations of radio galaxies also suggest merger-driven starbursts (Tadhunter et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Discovery of Radio Jets in z ~ 2 Ultraluminous Infrared Galaxies with Deep 9.7 μm Silicate Absorption

Sajina

Yan

Lacy

et al. 2007

ApJ

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Recent Spitzer observations have revealed a substantial population of z ∼ 2 ultraluminous infrared galaxies (ULIRGs) with deep silicate absorption ( ). This paper reports a 20 cm radio study of such a sample to t 1 1 9.7 elucidate their physical nature. We discover that a substantial fraction (40%) of deep silicate absorption ULIRGs at z ∼ 2 are moderately radio-loud, with W Hz Ϫ1 . This is in strong contrast with z Շ 1 radio 25 26 L p 10 -10 1.4GHz galaxies and radio-loud quasars where none of the sources with available IRS spectra have . In addition, t 1 1 9.7 we observe radio jets in two of our sources, with one having a double lobe structure ∼200 kpc in extent and the other showing a one-sided jet extending ∼90 kpc from the nucleus. The likely high inclination of the latter, coupled with its deep silicate absorption, implies the mid-IR obscuration does not share an axis with the radio jets. These sources are highly obscured quasars, observed in the transition stage after the birth of the radio source, but before feedback effects dispel the interstellar medium and halt the black hole accretion and starburst activity.

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An Obscured Radio Galaxy at High Redshift

Cited by 14 publications

References 31 publications

AzTEC 1.1-mm images of 16 radio galaxies at 0.5 < z < 5.2 and a quasar at z= 6.3

AzTEC 1.1-mm images of 16 radio galaxies at 0.5 < z < 5.2 and a quasar at z= 6.3

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

Discovery of Radio Jets in z ~ 2 Ultraluminous Infrared Galaxies with Deep 9.7 μm Silicate Absorption

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