The radio counter-jet of the QSO 3C 48

Feng, Wenxia; An, Tao; Hong, Xiaoyu; Zhao, Jun‐Hui; Venturi, T.; Shen, Zhi-Qiang; Wang, W. H.

doi:10.1051/0004-6361:20042316

Cited by 15 publications

(29 citation statements)

References 18 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is identical with the radio position of the QSO (e.g., Feng et al 2005). The total on-source integration time was ∼6.5 h. Although the 1.2 mm receiver was tuned to the redshifted frequency of 13 CO(3-2), no 1.2 mm line signal was detected to a flux limit of 3.4 Jy km s −1 over the same velocity range of −220 to +160 km s −1 where the CO(1-0) is observed.…”

Section: Observationssupporting

confidence: 71%

“…The two nuclear components are not resolved but the peak flux of 230 mJy/beam is lower than the integrated flux density of 270 mJy, so the continuum is not a single point source. This is also evident from the cm-radio maps and spectra published by Feng et al 2005. Most of the (cm-)radio continuum flux comes from the radio jet and/or the northeast component 3C 48A.…”

Section: The 35 MM Continuummentioning

confidence: 60%

See 1 more Smart Citation

Molecular gas and continuum emission in 3C 48: evidence for two merger nuclei?

Krips¹,

Eckart²,

Neri

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract. We present new interferometer observations of the CO(1-0) line and mm continuum emission from 3C 48 -one of the nearest examples of a merger activating a quasar. Our new CO data show that most of the CO is not in a disk around the quasar 3C 48, but rather in a second nucleus associated with the source 3C 48A ∼ 1 to the north-east, recently studied in the near-IR by Zuther et al. (2004). This main CO source has a strong velocity gradient (140 km s −1 over about 1 ). Our new data also show a second, weaker CO source at the QSO itself. At 1.2 mm, the continuum emission is elongated in the direction of the radio jet and towards 3C 48A. We model the 1.2 mm continuum with three different sources in 3C 48 -the 3C 48 QSO, the 3C 48 jet, and the second nucleus 3C 48A. We suggest that the unusually bright and extended nature of the jet may be due to its interaction with the second merger nucleus 3C 48A.

show abstract

Section: Observationssupporting

confidence: 71%

Section: The 35 MM Continuummentioning

confidence: 60%

Molecular gas and continuum emission in 3C 48: evidence for two merger nuclei?

Krips¹,

Eckart²,

Neri

et al. 2005

A&A

View full text Add to dashboard Cite

show abstract

“…These images are shown in Figure 4, along with the location in the line profile each represents. We also show the radio jet (Feng et al 2005) at the same scale.…”

Section: The Distribution Of Extended Emission In the Nuclear Regionmentioning

confidence: 86%

“…The number in the upper left corner of the images gives the central velocity shift of the image, in km s À1 in the quasar frame, from the systemic redshift of 0.36933. The 5 GHz Merlin radio contours from Feng et al (2005) are shown superposed on the image near the peak of the high-velocity system in the lower right panel. All images use a common intensity mapping and have north up and east to the left.…”

Section: The Distribution Of Extended Emission In the Nuclear Regionmentioning

confidence: 99%

The Nature of Optical Features in the Inner Region of the 3C 48 Host Galaxy

Stockton

Canalizo

et al. 2007

ApJ

View full text Add to dashboard Cite

The well-known quasar 3C 48 is the most powerful compact steep-spectrum radio-loud QSO at low redshifts. It also has two unusual optical features within the radius of the radio jet ($1 00 ): (1) an anomalous, high-velocity narrow-line component, and (2) a bright continuum peak (3C 48A) $1 00 northeast of the quasar. Both of these optical features have been conjectured to be related to the radio jet. We have obtained Gemini North GMOS integral field unit (IFU ) spectroscopy of the central region around 3C 48. We use the unique features of the IFU data to remove unresolved emission at the position of the quasar. The resolved emission at the wavelength of the high-velocity component is peaked P0.25 00 north of the quasar, at the same position angle as the base of the radio jet. These observations appear to confirm that this high-velocity gas is connected with the radio jet. However, most of the emission comes from a region where the jet is still well collimated, rather than from the regions where the radio maps indicate strong disruption. We also present the results of HST STIS spectroscopy of 3C 48A. We show that 3C 48A is dominated by stars with a luminosity-weighted age of $1:4 ; 10 8 yr, substantially older than any reasonable estimate for the age of the radio source. Thus, 3C 48A almost certainly cannot be attributed to jet-induced star formation. The host galaxy of 3C 48 is clearly the result of a merger, and 3C 48A seems much more likely to be the distorted nucleus of the merging partner in which star formation was induced during the previous close passage.

show abstract

“…This might result from a projection on the plane of the sky of a helically twisted jet. Helical jets could be triggered by periodic variation in the direction of jet ejection (Linfield 1981;Stirling et al 2003;Zhao et al 2011), Kelvin-Helmboltz instabilities in the jet flow (Hardee 2003;Feng et al 2005;An et al 2010), or the magneto-hydrodynamics of the jet (Camenzind 1986) and can result in quasi-periodic flux density variability (Camenzind & Krockenberger 1992;An et al 2013;Wang et al 2014;Mohan & Mangalam 2015). The 15-GHz VLBA monitoring observation inferred superluminal motions of two jet components from 14-epoch datasets between 1995 and 2010, with a proper motion of 148 ± 15 µas yr −1 (10.1 c) at about 7 mas and 36 ± 13 µas yr −1 (2.47 c) at about 1.5 mas from the core (Lister et al 2013).…”

Section: +319 (J0205+3212)mentioning

confidence: 99%

The Most Compact Bright Radio-loud AGNs. II. VLBA Observations of 10 Sources at 43 and 86 GHz

Cheng¹,

An²,

Hong³

et al. 2018

ApJS

Self Cite

View full text Add to dashboard Cite

Radio-loud active galactic nuclei (AGNs), hosting powerful relativistic jet outflows, provide an excellent laboratory for studying jet physics. Very long baseline interferometry (VLBI) enables high-resolution imaging on milli-arcsecond (mas) and sub-mas scales, making it a powerful tool to explore the inner jet structure, shedding light on the formation, acceleration and collimation of AGN jets. In this paper, we present Very Long Baseline Array (VLBA) observations of ten radio-loud AGNs at 43 and 86 GHz, which were selected from the Planck catalogue of compact sources and are among the brightest in published VLBI images at and below 15 GHz. The image noise levels in our observations are typically 0.3 mJy beam at 43 and 86 GHz, respectively. Compared with the VLBI data observed at lower frequencies from the literature, our observations with higher resolution (the highest resolution up to 0.07 mas at 86 GHz and 0.18 mas at 43 GHz) and at higher frequencies detected new jet components at sub-parsec scales, offering valuable data for studies of the physical properties of innermost jets. These include compactness factor of the radio structure (the ratio of core flux density to total flux density), and core brightness temperature (T b ). In all these sources, the compact core accounts for a significant -2 -fraction (> 60%) of the total flux density. Their correlated flux density at the longest baselines is higher than 0.16 Jy. The compactness of these sources make them good phase calibrators of mm-wavelength ground-based and space VLBI.

show abstract

The radio counter-jet of the QSO 3C 48

Cited by 15 publications

References 18 publications

Molecular gas and continuum emission in 3C 48: evidence for two merger nuclei?

Molecular gas and continuum emission in 3C 48: evidence for two merger nuclei?

The Nature of Optical Features in the Inner Region of the 3C 48 Host Galaxy

The Most Compact Bright Radio-loud AGNs. II. VLBA Observations of 10 Sources at 43 and 86 GHz

Contact Info

Product

Resources

About