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Villar-Martín, M.; Tadhunter, C. N.; Morganti, Raffaella; Axon, D. J.; Koekemoer, Anton M.

doi:10.1023/a:1002193424056

Cited by 56 publications

(124 citation statements)

References 4 publications

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“…We can also exclude shock ionisation based on the kinematics and the emission-line ratios. The line ratios for the broad shocked gas components in powerful radio galaxies are observed to have a much lower ionisation state Villar-Martín et al 1999) than observed here. Furthermore, shock-ionisation models (Dopita & Sutherland 1995;Allen et al 2008) indicate that an [O iii]/Hβ line ratio around 10 would require shock velocities >500 km s −1 for which we find no evidence in our observations (cf.…”

Section: Source Of Ionisation and Gas Metallicitycontrasting

confidence: 48%

Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Sánchez

Wisotzki²,

Jahnke

et al. 2010

A&A

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We present VIMOS integral field spectroscopy of the brightest radio-quiet QSO on the southern sky HE 1029-1401 at a redshift of z = 0.086. Standard decomposition techniques for broad-band imaging are extended to integral field data in order to deblend the QSO and host emission. We perform a tentative analysis of the stellar continuum, finding a young stellar population (<100 Myr) or a featureless continuum embedded in an old stellar population (10 Gyr) typical for a massive elliptical galaxy. The stellar velocity dispersion of σ * = 320 ± 90 km s −1 and the estimated black hole mass log(M BH /M ) = 8.7 ± 0.3 are consistent with the local M BH -σ * relation within the errors. For the first time, we map the two-dimensional ionised gas distribution and the gas velocity field around HE 1029-1401. While the stellar host morphology is purely elliptical, we find a highly structured distribution of ionised gas out to 16 kpc from the QSO. The gas is highly ionised solely by the QSO radiation and has a significantly lower metallicity than would be expected for the stellar mass of the host, indicating an external origin of the gas most likely due to minor mergers. We find a rotating gas disc around the QSO and a dispersion-dominated non-rotating gas component within the central 3 kpc. At larger distances the velocity field is heavily disturbed, which could be interpreted as another signature of past minor merger events. Alternatively, the arc-like structure seen in the ionised gas might also be indicative of a large-scale expanding bubble, centred on and possibly driven by the active nucleus.

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Section: Source Of Ionisation and Gas Metallicitycontrasting

confidence: 48%

Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Sánchez

Wisotzki²,

Jahnke

et al. 2010

A&A

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“…Villar-Martín et al 1999), by high electron temperatures leading to X-ray emission, and by radio synchrotron radiation. Radiation and collisional processes are strongly intermingled in ionizing the gas (e.g.…”

Section: Discussionmentioning

confidence: 99%

Distribution of the heavy elements throughout the extended narrow-line region of the Seyfert galaxy NGC 7212

Contini

Cracco

Ciroi

et al. 2012

A&A

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The latest observations of line and continuum spectra emitted from the extended narrow-line region (ENLR) of the Seyfert 2 galaxy NGC 7212 are analysed using models that account for photoionization from the active galactic nucleus (AGN) and shocks. The results show that relatively high (500-800 km s −1 ) shock velocities appear at the edge of the cone and beyond. The model-inferred AGN flux, which is lower than 10 −11 photons cm −2 s −1 eV −1 at the Lyman limit, is more typical of low-luminosity AGN than Seyfert 2 galaxies. The preshock densities are characteristic of the ENLR and range between 80-150 cm −3 . Nitrogen and sulphur are found to be depleted by a factor lower than 2, particularly at the eastern edge. Oxygen is depleted at several locations. The Fe/H ratio is approximately solar, whereas the Ne/H relative abundance is unusually high, 1.5-2 times the solar value. Modelling the continuum spectral energy distribution (SED), we have found radio synchrotron radiation generated by the Fermi mechanism at the shock front, whereas the X-rays are produced by the bremsstrahlung from a relatively high temperature plasma.

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“…Detailed studies of low redshift powerful radio galaxies (z <0.5) have been very useful to understand the impact of such interactions on the gaseous environment (Tadhunter 2002, Villar-Martín. et al 1999, Clark et al 1998, van Breugel et al 1985.…”

Section: Jet Gas Interactionsmentioning

confidence: 99%

Giant Lyα nebulae in the high redshift (z⩾2) Universe

Villar-Martı́n

2007

New Astronomy Reviews

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High redshift radio galaxies (z ≥2) are believed to be progenitors of the giant ellipticals of today. They are often associated with giant Lyα nebulae (sometimes >100 kpc), which have been for more than two decades valuable sources of information about the evolutionary status of the host galaxy and its chemical enrichment and star formation histories.I present in this paper a summary of the most relevant results about the giant nebulae obtained in the last ∼10 years and the implications on our understanding of the early phases of evolution of massive elliptical galaxies. An interesting earlier review can be found in McCarthy (1993).

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Untitled

Cited by 56 publications

References 4 publications

Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Mapping the ionised gas around the luminous QSO HE 1029-1401: evidence for minor merger events?

Distribution of the heavy elements throughout the extended narrow-line region of the Seyfert galaxy NGC 7212

Giant Lyα nebulae in the high redshift (z⩾2) Universe

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