The nebulosity around 3C 48

Wampler, E. J.; Burbidge, E. M.; Baldwin, J. A.; Robinson, L. B.

doi:10.1086/181808

Cited by 61 publications

(44 citation statements)

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“…spectra of many QSOs (e.g. Wampler et al 1975;Stockton 1976;Boroson & Oke 1984;Boroson et al 1985) indicating large amount of gas being photoionised by the QSO radiation. Unfortunately, spectroscopy of QSO hosts suffers invariably from the contamination of the spectrum by the emission of the active galactic nucleus (AGN) even when observed some arcseconds away from the nucleus.…”

Section: Introductionmentioning

confidence: 99%

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: Introductionmentioning

confidence: 99%

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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“…In addition, bright quasars have also been found surrounded by giant line-emitting nebulae observed in transitions such as Ly (e.g., Wampler et al 1975;Heckman et al 1991aHeckman et al , 1991bChristensen et al 2006). In this paper we investigate whether the two phenomena could originate from the same type of gas clouds around galaxies, thereby connecting gas absorption and line emission in galaxy and quasar halos.…”

Section: Introductionmentioning

confidence: 99%

On the Connection between Metal Absorbers and Quasar Nebulae

Chelouche

Ménard

Bowen

et al. 2008

Astrophysical Journal

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We establish a simple model for the distribution of cool ($10 4 K) gas around L ? galaxies using the properties of strong Mg ii absorption line systems as observational constraints. Our analysis suggests that the halos of L ? galaxies are filled with cool gas clouds having sizes of order 1 kpc and densities of $10 À2 cm À3 . We then investigate the physical conditions of a similar ensemble of clouds situated around a central quasar. We show that the flux from the quasar gives rise to (1) extended narrow line emission on $100 kpc scales and (2) an anisotropy in the properties of the absorbing gas arising from the geometry of the quasar radiation field. Provided that quasars reside in gaseous halos more massive than those of L ? galaxies, our predictions agree with the results from detections of both narrow emission line nebulae and $100 kpc Mg iiYabsorbing halos around quasars, suggesting a common origin for these phenomena. We discuss the implications of our results for understanding quasar absorption line systems, quasar environments at high redshifts, and the quasar unification scheme.

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“…3C 48, a quasar at z = 0.369, is the first quasar discovered with a luminous EELR extending out to ∼20 kpc (Wampler et al 1975). In addition to being a powerful CSS radio source, it is also shown by IRAS to be an ultraluminous IR galaxy with polycyclic aromatic hydrocarbon features indicating a very high star formation rate in the host galaxy (Fu & Stockton 2009).…”

Section: Introduction and Purposementioning

confidence: 99%

“…The first hint of a high-velocity outflow close to the center of 3C 48 came from Wampler et al (1975), who found that the [O iii] emission line is blueshifted with respect to the broad Hβ line. Chatzichristou et al (1999) and Canalizo & Stockton (2000) found that the [O iii] line is double peaked with a narrow component at the redshift of the broad Hβ line and a blueshifted broad component offset by ∼570 km s −1 and having a FWHM of ∼1000 km s −1 .…”

Section: Introduction and Purposementioning

confidence: 99%

The Resolved Outflow From 3c 48

Shih

Stockton

2014

ApJ

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We investigate the properties of the high-velocity outflow driven by the young radio jet of 3C 48, a compact-steepspectrum source. We use the Space Telescope Imaging Spectrograph on board the Hubble Space Telecope to obtain (1) low-resolution UV and optical spectra and (2) multi-slit medium-resolution spectra of the ionized outflow. With supporting data from ground-based spectrographs, we are able to accurately measure the ratios of diagnostic emission lines such as, and [Ne iii] λ3869. We fit the observed emission-line ratios using a range of ionization models, powered by active galactic nucleus (AGN) radiation and shocks, produced by the MAPPINGS code. We have determined that AGN radiation is likely the dominant ionization source. The outflow's density is estimated to be in the range n = 10 3 -10 4 cm −3 , the mass is ∼6 × 10 6 M , and the metallicity is likely equal to or higher than solar. Compared with the typical outflows associated with more evolved radio jets, this young outflow is denser, less massive, and more metal rich. Multi-slit observations allow us to construct a two-dimensional velocity map of the outflow that shows a wide range of velocities with distinct velocity components, suggesting a wide-angle clumpy outflow.

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The nebulosity around 3C 48

Cited by 61 publications

References 0 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?

On the Connection between Metal Absorbers and Quasar Nebulae

The Resolved Outflow From 3c 48

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