Star formation in the hosts of GHz peaked spectrum and compact steep spectrum radio galaxies

Labiano, Á.; O’Dea, C. P.; Barthel, Pieter; Vries, W. H. de; Baum, Stefi A.

doi:10.1051/0004-6361:20077112

Cited by 34 publications

(61 citation statements)

References 84 publications

(130 reference statements)

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“…At low redshifts (z < ∼ 0.3) there might be no dependence at all on (1 + z) for both luminosities, which is consistent with Labiano et al (2008).…”

Section: Dependencies Of the Uv-excess On Source Parameterssupporting

confidence: 82%

“…Interactions of the radio source with the galaxy interstellar medium are clear from the study of the emission lines (see, e.g., Labiano et al 2005;Holt et al 2009). The presence of young stellar populations in these objects has been revealed several times (Holt 2009;Labiano et al 2008;deVries et al 2007;Tadhunter et al 2002). Their origin is attributed to the shocks generated by the young radio source expanding into the interstellar medium (Rees 1989;Mellema et al 2002;Bicknell et al 2000), and/or as the result of a galaxy merger process which, at some later epoch, also triggered the onset of the radio source (Raimann et al 2005;Holt 2009).…”

Section: Introductionmentioning

confidence: 95%

“…There are different physical processes that can be responsible for the UV-excess (Best et al 1998;Tadhunter et al 2002;Labiano et al 2008):…”

Section: The Origin Of the Uv-excess In Csos/msos Galaxiesmentioning

confidence: 99%

“…Because we do not have spatial resolution (like, e.g., in Labiano et al 2008), we cannot state whether the UV-excess comes from either an extended volume or from a nuclear point source. We cannot exclude nuclear scattered light, because not only we have no information on spatial distribution and orientation, but we also have no optical polarization information.…”

Section: Agn Contribution?mentioning

confidence: 99%

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The B3-VLA CSS sample

Fanti

Zanichelli

et al. 2011

A&A

120

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Context. Compact steep-spectrum radio sources and giga-hertz peaked spectrum radio sources (CSS/GPS) are generally considered to be mostly young radio sources. In recent years we studied at many wavelengths a sample of these objects selected from the B3-VLA catalog: the B3-VLA CSS sample. Only ≈60% of the sources were optically identified. Aims. We aim to increase the number of optical identifications and study the properties of the host galaxies of young radio sources. Methods. We cross-correlated the CSS B3-VLA sample with the Sloan Digital Sky Survey (SDSS), DR7, and complemented the SDSS photometry with available GALEX (DR 4/5 and 6) and near-IR data from UKIRT and 2MASS. Results. We obtained new identifications and photometric redshifts for eight faint galaxies and for one quasar and two quasar candidates. Overall we have 27 galaxies with SDSS photometry in five bands, for which we derived the ultraviolet-optical spectral energy distribution (UV-O-SED). We extended our investigation to additional CSS/GPS selected from the literature. Most of the galaxies show an excess of ultra-violet (UV) radiation compared with the UV-O-SED of local radio-quiet ellipticals. We found a strong dependence of the UV excess on redshift and analyzed it assuming that it is generated either from the nucleus (hidden quasar) or from a young stellar population (YSP). We also compare the UV-O-SEDs of our CSS/GPS sources with those of a selection of large size (LSO) powerful radio sources from the literature. Conclusions. If the major process of the UV excess is caused by a YSP, our conclusion is that it is the result of the merger process that also triggered the onset of the radio source with some time delay. We do not see evidence for a major contribution from a YSP triggered by the radio sources itself.

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“…At low redshifts (z < ∼ 0.3) there might be no dependence at all on (1 + z) for both luminosities, which is consistent with Labiano et al (2008).…”

Section: Dependencies Of the Uv-excess On Source Parameterssupporting

confidence: 82%

Section: Introductionmentioning

confidence: 95%

“…There are different physical processes that can be responsible for the UV-excess (Best et al 1998;Tadhunter et al 2002;Labiano et al 2008):…”

Section: The Origin Of the Uv-excess In Csos/msos Galaxiesmentioning

confidence: 99%

Section: Agn Contribution?mentioning

confidence: 99%

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The B3-VLA CSS sample

Fanti

Zanichelli

et al. 2011

A&A

120

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“…12. 5 objects in our GPS sample have spectroscopic O[iii] measurements (O'Dea 1998; Labiano et al 2005Labiano et al , 2008, and references therein). The "control sample" is a collection of Seyfert 2-galaxies measurements in Guainazzi et al (2005).…”

Section: The X-ray Obscuring Environmentmentioning

confidence: 99%

The X-ray view of giga-hertz peaked spectrum radio galaxies

Tengstrand

Guainazzi

Siemiginowska

et al. 2009

A&A

Self Cite

100

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Context. This paper presents the X-ray properties of a flux-and volume-limited complete sample of 16 giga-hertz peaked spectrum (GPS) galaxies. Aims. This study addresses three basic questions in our understanding of the nature and evolution of GPS sources: a) What is the physical origin of the X-ray emission in GPS galaxies? b) Which physical system is associated with the X-ray obscuration? c) What is the "endpoint" of the evolution of compact radio sources? Methods. We discuss in this paper the results of the X-ray spectral analysis, and compare the X-ray properties of the sample sources with radio observables. Results. We obtain a 100% (94%) detection fraction in the 0.5-2 keV (0.5-10 keV) energy band. GPS galaxy X-ray spectra are typically highly obscured ( N GPS H = 3 × 10 22 cm −2 ; σ N H 0.5 dex). The X-ray column density is larger than the HI column density measured in the radio by a factor 10 to 100. GPS galaxies lie well on the extrapolation to high radio powers of the correlation between radio and X-ray luminosity known in low-luminosity FR I radio galaxies. On the other hand, GPS galaxies exhibit a comparable X-ray luminosity to FR II radio galaxies, notwithstanding their much larger radio luminosity. Conclusions. The X-ray to radio luminosity ratio distribution in our sample is consistent with the bulk of the high-energy emission being produced by the accretion disk, as well as with dynamical models of GPS evolution where X-rays are produced by Compton upscattering of ambient photons. Further support to the former scenario comes from the location of GPS galaxies in the X-ray to O[iii] luminosity ratio versus N H plane. We propose that GPS galaxies are young radio sources, which would reach their full maturity as classical FR II radio galaxies. However, column densities ∼ > 10 22 cm −2 could lead to a significant underestimate of dynamical age determinations based on the hotspot recession velocity measurements.

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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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Star formation in the hosts of GHz peaked spectrum and compact steep spectrum radio galaxies

Cited by 34 publications

References 84 publications

The B3-VLA CSS sample

The B3-VLA CSS sample

The X-ray view of giga-hertz peaked spectrum radio galaxies

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

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