Arecibo Observation of B2 0902+343 in the 21 Centimeter Line at Redshift 3.4

Briggs, F. H.; Sorar, Ertugrul; Taramopoulos, A.

doi:10.1086/187042

Cited by 24 publications

(26 citation statements)

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“…Thus, the implied values for column density and total mass of H  absorbing material are similar to those inferred by de Bruyn (1996): N(HI) ∼ 3 × 10 21 cm −2 assuming a mean spin temperature of 1000 K, and M H i = 10 7 −10 10 M , depending on whether the gas at this column density is assumed to cover a region of only 1.5 kpc 2 , corresponding to the radio continuum hotspot, or as much as 750 kpc 2 , corresponding to the entire Ly-α emission region. The possible absorption feature detected by Briggs et al (1993) near 322.5 MHz may be present in our spectrum, but noise levels preclude any confident identification. The same is true of the broad wing component detected by de Bruyn (1996) on the blueward side of the H  line.…”

Section: H I Absorptionmentioning

confidence: 90%

“…Other complex radio features were seen by Carilli et al (1994) and Carilli (1995). CO lines, on the other hand, have not been detected (Downes et al 1996) Nevertheless, the existence of gas is implied by the significant H  absorption feature at 323 MHz first observed by Uson et al (1991) and later confirmed by Briggs et al (1993) andde Bruyn (1996), who noted a potentially significant absorption wing to the blueward side of this line. B2 0902+343 happens to be one of only two galaxies at z > 3 that exhibit an H  absorption feature.…”

Section: Introductionmentioning

confidence: 99%

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Observations of the high-redshift galaxy B2 0902+343 at 92 cm

Cody

Braun²

2003

A&A

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Abstract. We present 92 cm observations of the high-redshift galaxy B2 0902+343 (z = 3.40) with the Westerbork Synthesis Radio Telescope (WSRT). Twenty-one cm H  is detected in absorption, at a depth of 15.9 mJy (=6σ) and rest frame velocity width 120 km s −1 . We also report a null detection of OH emission or absorption at the 1665/1667 MHz rest-frame transitions. Based on our spectral sensitivity, we derive an upper limit on OH maser luminosity of log(L/L ) < 5.2. In addition, we consider the possibility of absorption, and estimate a maximum column depth N(OH) of 1 × 10 15 cm −2 , corresponding to at most 2 × 10 5 − 9 × 10 6 M of OH in the galaxy. The implications of these results are discussed in the context of current efforts to extend the OH megamaser luminosity function and galactic merger rate to high redshift.

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Section: H I Absorptionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Observations of the high-redshift galaxy B2 0902+343 at 92 cm

Cody

Braun²

2003

A&A

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“…These authors argue, however, that the absorbing material resides in a compact disc‐like structure much closer to the nucleus than the Lyα absorbers in the HzRGs. Furthermore, attempts to detect 21‐cm absorption in HzRGs have been largely unsuccessful (Röttgering et al 1999), with 0902+34 at z = 3.4 being the only source with a solid detection (Uson, Bagri & Cornwell 1991; Briggs, Sorar & Taramopoulos 1993; De Bruyn 1996).…”

Section: Discussionmentioning

confidence: 99%

H i in the protocluster environment atz> 2: absorbing haloes and the Lyα forest

Wilman

Jarvis

Röttgering

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present VLT‐UVES echelle spectra of the Lyα emission and absorption in five radio galaxies at redshifts z= 2.55–4.1. Together with data from our pilot study, we have a sample of seven such systems with radio source sizes ∼1–90 kpc with which to address the origin of the absorbing gas. Echelle resolution again reveals that some systems with NH i > 1018 cm−2 in lower‐resolution data in fact consist of several weaker absorbers with NH i < 1015 cm−2. We identify two groups of H i absorbers: strong absorbers with NH i≃ 1018–1020 cm−2 and weaker systems with NH i≃ 1013–1015 cm−2. There is none at intermediate NH i. The strong absorbers may be a byproduct of massive galaxy formation or could instead represent material cooling behind the expanding bow shock of the radio jet, as simulated by Krause. New observations are required to discriminate between these possibilities. We argue that the weaker absorbers with NH i≃ 1013–1015 cm−2 are part of the Lyα forest, as their rate of incidence is within a factor of 2–4 of that in the intergalactic medium at large. Such column densities are consistent with models of a multiphase proto‐intracluster medium at z > 2.

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“…The inferred blueshift is %100 km s À1 . This cannot be the same gas that causes H i absorption against the radio continuum, since Briggs et al (1993) and Cody & Braun (2003) infer a redshift z abs ¼ 3:3962 with N H ¼ 3 ; 10 21 cm À2 and FWHM ¼ 120 km s À1 for the absorbing gas. It is probable that the dense gas giving the H i absorption lies close to the nucleus, and any absorption that this may have produced in the Ly line is completely veiled by the frequency redistribution produced by multiple scattering events.…”

Section: Notes On Individual Objectsmentioning

confidence: 99%

Metal-Enriched Gaseous Halos around Distant Radio Galaxies: Clues to Feedback in Galaxy Formation

et al. 2007

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We present the results of an optical and near-IR spectroscopic study of giant nebular emission-line halos associated with three z > 3 radio galaxies, 4C 41.17, 4C 60.07, and B2 0902+34. Previous deep narrowband Ly imaging revealed complex morphologies with sizes up to 100 kpc, possibly connected to outflows and AGN feedback from the central regions. The outer regions of these halos show quiet kinematics with typical velocity dispersions of a few hundred km s À1 and velocity shears that can mostly be interpreted as being due to rotation. The inner regions show shocked cocoons of gas closely associated with the radio lobes. These display disturbed kinematics and have expansion velocities and /or velocity dispersions >1000 km s À1 . The core region is chemically evolved, and we also find spectroscopic evidence for the ejection of enriched material in 4C 41.17 up to a distance of %60 kpc along the radio axis. The dynamical structures traced in the Ly line are, in most cases, closely echoed in the carbon and oxygen lines. This shows that the Ly line is produced in a highly clumped medium of small filling factor and can therefore be used as a tracer of the dynamics of high-redshift radio galaxies ( HzRGs). We conclude that these HzRGs are undergoing a final jet-induced phase of star formation with ejection of most of their interstellar medium before becoming ''red and dead'' elliptical galaxies.

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Arecibo Observation of B2 0902+343 in the 21 Centimeter Line at Redshift 3.4

Cited by 24 publications

References 0 publications

Observations of the high-redshift galaxy B2 0902+343 at 92 cm

Observations of the high-redshift galaxy B2 0902+343 at 92 cm

H i in the protocluster environment atz> 2: absorbing haloes and the Lyα forest

Metal-Enriched Gaseous Halos around Distant Radio Galaxies: Clues to Feedback in Galaxy Formation

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