HST/STIS low dispersion spectroscopy of three Compact Steep Spectrum sources

Labiano, Á.; O’Dea, C. P.; Gelderman, Richard; Vries, W. H. de; Axon, D. J.; Barthel, P. D.; Baum, Stefi A.; Capetti, A.; Fanti, R.; Koekemoer, Anton M.; Morganti, Raffaella; Tadhunter, C. N.

doi:10.1051/0004-6361:20042425

Cited by 52 publications

(71 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This also supports the claim that the shock contribution to [O iii] luminosity may not be important, and the [O iii] luminosity can still be regarded as a good indicator of central thermal emission in these small radio-sized GPS sources. Labiano et al (2005) found that the contribution to narrow line luminosity from the shocked gas is between 30% and 70% for the CSS source 3C 303.1, and this ratio is even lower in other two CSS sources (3C 67 and 3C 277.1), based on the ionization diagnostics of different narrow emission lines. Therefore, the bolometric luminosities of nine CSS sources calculated from the [O iii] luminosities may not be overestimated too much, which will not change our main conclusion.…”

Section: Summary and Discussionmentioning

confidence: 93%

Observational Evidence for Young Radio Galaxies Is Triggered by Accretion Disk Instability

2009

ApJ

View full text Add to dashboard Cite

Bolometric luminosities and black hole (BH) masses are estimated by various methods for a sample of young radio galaxies with known ages. We find that the ages are positively correlated with the bolometric luminosities in these young radio galaxies. This positive correlation is consistent with the theoretical prediction based on the radiation pressure instability of accretion disks in Czerny et al. The ages of young radio galaxies are also found to be consistent with the theoretical durations of outbursts in BH mass and accretion rate (in Eddington unit) plane, where the outbursts are assumed to be triggered by the radiation pressure instabilities. Our results provide observational evidence for the radiation pressure instability, which causes limitcycle behavior, as a physical mechanism that may be responsible for these short-lived young radio galaxies.

show abstract

Section: Summary and Discussionmentioning

confidence: 93%

Observational Evidence for Young Radio Galaxies Is Triggered by Accretion Disk Instability

2009

ApJ

View full text Add to dashboard Cite

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

“…de Vries et al (1998Vries et al ( , 2000 showed that the hosts are old giant ellipticals. 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).…”

Section: Introductionmentioning

confidence: 99%

The B3-VLA CSS sample

Fanti

Zanichelli

et al. 2011

A&A

Self Cite

120

View full text Add to dashboard Cite

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.

show abstract

HST/STIS low dispersion spectroscopy of three Compact Steep Spectrum sources

Cited by 52 publications

References 38 publications

Observational Evidence for Young Radio Galaxies Is Triggered by Accretion Disk Instability

Observational Evidence for Young Radio Galaxies Is Triggered by Accretion Disk Instability

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

The B3-VLA CSS sample

Contact Info

Product

Resources

About