3C 279 - The case for 'superluminal' expansion

Cotton, W. D.; Counselman, C. C.; Geller, R. B.; Shapiro, I. I.; Wittels, J. J.; Hinteregger, H. F.; Knight, C. A.; Rogers, A. E. E.; Whitney, A. R.; Clark, T. A.

doi:10.1086/182942

Cited by 84 publications

(31 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Cotton (1979) confirmed the superluminal motion with a series of observations showing a expansion velocity of 0.5 mas/yr in PA ∼ −140. Later observations showed lower expansion speeds ∼0.15 mas/yr (Unwin et al 1989;Carrara et al 1993).…”

Section: C 279supporting

confidence: 77%

50 μas resolution VLBI images of AGN's at λ3 mm

Rantakyrö

Bååth

Backer

et al. 1998

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

Abstract. We present 15 images from the global mm-VLBI sessions in 1990 April at 100 GHz and 1993 April at 86 GHz. These observations probe the central engines of the 16 observed AGN's with up to 50 µas resolution. Among other sources previously observed with λ3 mm VLBI we present the first λ3 mm maps of 0735+178, 0748+126, 1055+018, 2145+067, and CTA 102, in total we have been able to image 13 out of the 16 observed sources. 6 out of the 13 imaged sources observed exhibit curvature and rapid structural changes, although the low dynamic range in two thirds of the maps limits the detection of weak features. Most of the sources have unresolved cores even at this high resolution. There is substantial evidence that the observed sources can be grouped into two general groups: A misaligned population with parsec scale jets in the form of low pitch helices and an aligned population with straight jets with small changes in PA due to intrinsic bends.

show abstract

Section: C 279supporting

confidence: 77%

50 μas resolution VLBI images of AGN's at λ3 mm

Rantakyrö

Bååth

Backer

et al. 1998

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

show abstract

“…Vol (Unwin et al 1989 ;Carrara et al 1993) to 4.8c[7.5c derived from a long-term highfrequency VLBI monitoring of six superluminal components in the relativistic jet in 3C 279 (see Wehrle et al 2001). Higher velocities have also been measured in the past : Cotton et al (1979) originally found a value of 15c (speeds have been expressed assuming km s~1 H 0 \ 70 Mpc~1 and These velocities refer, however, to q 0 \ 0.1). regions farther away along the jet, while our data concern the emission from much smaller scales.…”

Section: Discussionmentioning

confidence: 98%

Spectral Energy Distributions of 3C 279 Revisited:BeppoSAXObservations and Variability Models

Ballo

Maraschi

Tavecchio

et al. 2002

ApJ

View full text Add to dashboard Cite

We present the BeppoSAX observations of 3C 279 performed simultaneously during 1997 January 13È23 with c-ray pointings with EGRET on board the Compton Gamma Ray Observatory and optical observations at the Torino Observatory (1997 January 11È18). Infrared Space Observatory data close to this epoch are also available. We compare the derived spectral energy distribution (SED) with those obtained at all other epochs with adequate multiwavelength coverage. Simple spectral models Ðtted to the multiepoch SEDs suggest that changes in intensity can be ascribed mainly to the variation of the bulk Lorentz factor of the plasma in the jet.

show abstract

“…First, the angle between the jet and our line of sight is restricted to be ≤8Њ by the observed VLBI apparent superluminal motion of 14c (Cotton et al 1979). We note that this measurement is the fastest (and earliest) motion recorded in this quasar so far and was observed when the VLBI jet was best aligned ( ) with the position angle of the 218Њ ‫ע‬ 2Њ VLA scale jet (∼205Њ).…”

Section: Physical Conditions In the Optical/uv-emitting Regionmentioning

confidence: 91%

“…It is a bright EGRET g-ray source (Hartman et al 2001) and shows rapid variability across the entire electromagnetic spectrum (e.g., Wehrle et al 1998). One of the first early triumphs of the technique of very long baseline interferometry (VLBI) was the discovery of apparent superluminal motion in the parsec-scale jet of this quasar (Cotton et al 1979 and references therein). Subsequent superluminal ejections have been continually monitored for more than 30 years (e.g., Unwin et al 1989;Wehrle et al 2001).…”

Section: Introductionmentioning

confidence: 99%

Detection of Optical Synchrotron Emission from the Radio Jet of 3C 279

Cheung

2002

The Astrophysical Journal

View full text Add to dashboard Cite

We report the detection of optical and ultraviolet emission from the kiloparsec-scale jet of the well-known quasar 3C 279. A bright knot, discovered in archival V-and U-band Hubble Space Telescope Faint Object Camera images, is coincident with a peak in the radio jet ∼0Љ .6 from the nucleus. The detection was also confirmed in Wide Field Planetary Camera 2 images. Archival Very Large Array and MERLIN radio data are also analyzed, and these data help to show that the high-energy optical/UV continuum and the spectrum are consistent with a synchrotron origin from the same population of relativistic electrons responsible for the radio emission.

show abstract

3C 279 - The case for 'superluminal' expansion

Cited by 84 publications

References 0 publications

50 μas resolution VLBI images of AGN's at λ3 mm

50 μas resolution VLBI images of AGN's at λ3 mm

Spectral Energy Distributions of 3C 279 Revisited:BeppoSAXObservations and Variability Models

Detection of Optical Synchrotron Emission from the Radio Jet of 3C 279

Contact Info

Product

Resources

About