Gas and stars in compact (young) radio sources

Morganti, Raffaella; Emonts, Bjorn; Holt, J.; Tadhunter, C. N.; Oosterloo, Thomas; Struve, Christian

doi:10.1002/asna.200811164

Cited by 8 publications

(11 citation statements)

References 17 publications

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“…The H i mass of the emission is 6.8 × 10 7 M and the peak column density is 1.0 × 10 20 cm −2 . NGC 315 is, therefore, similar to other FRI radio galaxies (Morganti et al 2009;Emonts et al in preparation). Radio galaxies of this type do not appear to have large amounts of H i associated with the host galaxy (Emonts 2006;Emonts et al 2006).…”

Section: Hi Emission and The Environmentsupporting

confidence: 76%

Is cold gas fuelling the radio galaxy NGC 315?

Morganti

Peck

Oosterloo

et al. 2009

A&A

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We present WSRT, VLA and VLBI observations of the H i absorption in the radio galaxy NGC 315. The main result is that two H i absorbing systems are detected against the central region. In addition to the known highly redshifted, very narrow component, we detect relatively broad (FWZI ∼ 150 km s −1 ) absorption. This broad component is redshifted by ∼80 km s −1 compared to the systemic velocity, while the narrow absorption is redshifted ∼490 km s −1 . Both H i absorption components are spatially resolved at the pcscale of the VLBI observations. The broad component shows strong gradients in density (or excitation) and velocity along the jet. We conclude that this gas is physically close to the AGN, although the nature of the gas resulting in the broad absorption is not completely clear. The possibility that it is entrained by the radio jet (and partly responsible of the deceleration of the jet) appears unlikely. Gas located in a thick circumnuclear toroidal structure, with orientation similar to the dusty, circumnuclear disk observed with HST, cannot be completely ruled out although it appears difficult to reconcile with the observed morphology and kinematics of the H i. A perhaps more likely scenario is that the gas producing the broad absorption could be (directly or indirectly) connected with the fueling of the AGN, i.e. gas that is falling into the nucleus. If this is the case, the accretion rate derived is similar (considering all uncertainties) to that found for other X-ray luminous elliptical galaxies, although lower than that derived from the radio core luminosity for NGC 315. The data also show that, in contrast to the broad component, the density distribution of the narrow component is featureless. Moreover, in the WSRT observations we do detect a small amount of H i in emission a few kpc SW of the AGN, coincident with faint optical absorption features and at velocities very similar to the narrow absorption. This suggests that the gas causing the narrow absorption is not close to the AGN and is more likely caused by clouds falling into NGC 315. The environment of NGC 315 turns out to be indeed quite gas rich since we detect five gas-rich companion galaxies in the immediate vicinity of NGC 315.

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Section: Hi Emission and The Environmentsupporting

confidence: 76%

Is cold gas fuelling the radio galaxy NGC 315?

Morganti

Peck

Oosterloo

et al. 2009

A&A

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“…The sensitivity of present day radio telescopes is the main limitation for the detection of H I in emission, although, very recently, Morganti et al (2009) succeeded in detecting large H I disks and rings, around 6 out of a sample of 21 low power B2 radio galaxies. All six are compact objects.…”

Section: Neutral Hydrogenmentioning

confidence: 99%

Radio properties of CSSs and GPSs

Fanti¹

2009

Astron Nachr

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“…Unfortunately, the line profiles are highly complex, precluding accurate measurements using the traditional [S II] λ6716/λ6731 ratio. Work is currently underway to measure the gas densities using alternative diagnostics (Holt et al 2009). High gas temperatures: Electron temperatures are estimated to be T e ∼ few ×10 4 K, although line measurements suffer from similar issues to those discussed above (Holt 2005;Holt et al 2008b).…”

Section: Physical Conditionsmentioning

confidence: 99%

The host galaxies of Compact Steep Spectrum and Gigahertz‐Peaked Spectrum radio sources

Holt¹

2009

Astron Nachr

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I will review some of the developments in studies of the host galaxy properties of Compact Steep Spectrum (CSS) and Gigahertz‐Peaked Spectrum (GPS) radio sources. In contrast to previous reviews structured around observational technique, I will discuss the host galaxy properties in terms of morphology, stellar content and warm gas properties and discuss how compact, young radio‐loud AGN are key objects for understanding galaxy evolution (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Gas and stars in compact (young) radio sources

Cited by 8 publications

References 17 publications

Is cold gas fuelling the radio galaxy NGC 315?

Is cold gas fuelling the radio galaxy NGC 315?

Radio properties of CSSs and GPSs

The host galaxies of Compact Steep Spectrum and Gigahertz‐Peaked Spectrum radio sources

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