Discovery of an Optical Synchrotron Jet in 3C 15

Crane, P.; Peletier, Reynier F.; Baxter, D.; Sparks, W. B.; Albrecht, R.; Barbieri, C.; Blades, J. C.; Boksenberg, A.; Deharveng, J. M.; Disney, M. J.; Jakobsen, P.; Kamperman, T. M.; King, Ivan R.; Macchetto, F.; Mackay, C. D.; Paresce, F.; Weigelt, G.; Greenfield, P.; Jędrzejewski, R.; Nota, A.

doi:10.1086/305359

Cited by 57 publications

(99 citation statements)

References 18 publications

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“…The optical morphology of the jet closely matches the features of the radio jet, suggesting that the optical emission is strongly dominated by synchrotron radiation (Fig. 5 of Martel et al 1998). Three prominent knots in the jet were detected at a PA of −30…”

Section: Summary Of Previous Optical Observationssupporting

confidence: 59%

“…The HS T observations found no bright, unresolved nucleus in the core of the galaxy, in contrast to other galaxies hosting optical jets (Martel et al 1998). The radio structure of 3C 15 is intermediate between Fanaroff-Riley (FR) classes I and II, although its luminosity is above that of a number of sources showing classical FR II structure (Leahy et al 1997).…”

Section: Introductionmentioning

confidence: 87%

“…The optical counterpart of the radio jet in 3C 15 was found in HS T observations by Martel et al (1998), and we use these HS T data in this paper. The optical morphology of the jet closely matches the features of the radio jet, suggesting that the optical emission is strongly dominated by synchrotron radiation (Fig.…”

Section: Summary Of Previous Optical Observationsmentioning

confidence: 97%

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Chandradiscovery of an X-ray jet and lobes in 3C 15

Kataoka

Leahy

Edwards

et al. 2003

A&A

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Abstract.We report the Chandra detection of an X-ray jet in 3C 15. The peak of the X-ray emission in the jet is 4.1 (a projected distance of 5.1 kpc) from the nucleus, and coincident with a component previously identified in the radio and optical jets. We construct the spectral energy distribution (SED) for this component, optical knot C, and find that X-ray flux is well below the extrapolation of the radio-to-optical continuum. We examine four models for the X-ray jet emission: (I) weak synchrotron cooling in equipartition, (II) moderate synchrotron cooling in equipartition, (III) weak synchrotron plus synchrotron self-Compton (SSC) cooling, and (IV) moderate synchrotron plus SSC cooling. Given weak evidence for a concave feature in the X-ray spectrum, we argue that case (II) can most reasonably explain the overall emission from knot C. Case (III) is also possible, but requires a large departure from equipartition and for the jet power to be comparable to that of the brightest quasars. In all models, (I)−(IV), electrons must be accelerated up to γ max > ∼ 10 7 , suggesting that re-acceleration is necessary in knot C of the 3C 15 jet. Diffuse X-ray emission has also been detected, distributed widely over the full extent (63 kpc × 25 kpc) of the radio lobes. The X-ray spectrum of the diffuse emission is described by a two-component model, consisting of soft thermal plasma emission from the host galaxy halo and a hard nonthermal power-law component. The hard component can be ascribed to the inverse Comptonization of cosmic microwave background (CMB) photons by the synchrotron emitting electrons in the radio lobes. We compare the total energy contained in the lobes with the jet power estimated from knot C, and discuss the energetic link between the jet and the lobes. We argue that the fueling time (t fuel ) and the source age (t src ) are comparable for case (II), whereas t fuel t src is likely for case (III). The latter may imply that the jet has a very small filling factor, ∼10 −3 . We consider the pressure balance between the thermal galaxy halo and non-thermal relativistic electrons in the radio lobes. Finally, we show that the X-ray emission from the nucleus is not adequately fitted by a simple absorbed power-law model, but needs an additional power-law with heavy absorption (N H 10 22−23 cm −2 ) intrinsic to the source. Such a high column density is consistent with the presence of a dense, dusty torus which obscures the quasar nucleus.

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Section: Summary Of Previous Optical Observationssupporting

confidence: 59%

Section: Introductionmentioning

confidence: 87%

Section: Summary Of Previous Optical Observationsmentioning

confidence: 97%

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Chandradiscovery of an X-ray jet and lobes in 3C 15

Kataoka

Leahy

Edwards

et al. 2003

A&A

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“…3C 15.ÈAn optical synchrotron jet was recently discovered by Martel et al (1998b) 8, 15.9, 16.0, 16.1, 16.2, 16.3, 16.5, 16.7, 16.9, 17.1, 17.3, 17.5. jets, 3C 15 does not possess a bright, compact nucleus, possibly because it is enshrouded in dust. The host galaxy is a fairly unremarkable elliptical and is surrounded by several smaller companion galaxies.…”

Section: Discussionmentioning

confidence: 95%

[ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL] Snapshot Survey of 3CR Radio Source Counterparts. III. Radio Galaxies with [FORMULA][F]z<0.1[/F][/FORMULA]

Martel¹,

Baum²,

Sparks³

et al. 1999

The Astrophysical Journal Supplement Series

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170

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We present and describe optical counterparts to 46 3CR radio galaxies of redshifts less than 0.1 that were imaged with the Hubble Space T elescopeÏs (HST ) WFPC2 camera through the broadband F702W Ðlter as part of the 3CR Snapshot Survey. This is the Ðfth and last such paper describing the 252 radio galaxies of this R-band survey. At the resolution of the images, a wealth of detail is visible. Approx-0A .1 imately 89% of the galaxies are ellipticals, and nearly all reside in groups or clusters of galaxies of various richness and compactness. Nearby elliptical companions of slightly smaller size and mass are common. Dust is prevalent in the cores of the 3C hosts ; nearly half of the galaxies possess some type of dust structure, such as irregular dust lanes, Ðlaments, or disks. Besides the well-known dust disks of 3C 264 and 3C 270, we have found Ðve new candidates in 3C 31, 3C 40, 3C 296, 3C 449, and 3C 465, as well as in the central regions of the nearby neighbors of 3C 31 and 3C 465. Our sample includes six conÐrmed optical synchrotron jets in 3C 15, 3C 66B, 3C 78, 3C 264, 3C 274, and 3C 371, or approximately 13% of the sample. Unresolved nuclei, consistent with the point spread function of WFPC2, are found in 43%È54% of the galaxies and in the majority of galaxies with dust disks and optical jets.

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“…Before the present study, 14 optical jets were known. They are present in all kinds of radio source, but show common properties: they originate from bright unresolved optical nuclei (the one exception is 3C 15; Martel et al 1998); they are smaller and narrower in appearance than their radio counterparts and no counter-jets are observed. The optically detected jets are longer than expected from their synchrotron cooling times, and there is no indication of strong steepening of the radio-optical spectral index with increasing distance from the nucleus (Sparks et al 1996;Scarpa et al 1999).…”

Section: Introductionmentioning

confidence: 99%

The HST survey of the B2 sample of radio galaxies: Detection of two optical jets

Parma

Ruiter

Capetti

et al. 2002

A&A

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Abstract. We present HST observations of previously undetected optical jets in the low-luminosity radio galaxies B2 0755+37 and B2 1553+24. We show that there is accurate spatial coincidence between optical and radio emission, implying that the former is likely to be synchrotron radiation. The physical properties of the jets are similar to those known previously: their radio-optical spectral indices are ≈0.7 and in B2 0755+37, the spectrum steepens between optical and X-ray wavelengths. Our results support the hypothesis that optical emission is detectable from jets orientated within ≈20• of the line of sight for the B2 sample.

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Discovery of an Optical Synchrotron Jet in 3C 15

Cited by 57 publications

References 18 publications

Chandradiscovery of an X-ray jet and lobes in 3C 15

Chandradiscovery of an X-ray jet and lobes in 3C 15

[ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL] Snapshot Survey of 3CR Radio Source Counterparts. III. Radio Galaxies with [FORMULA][F]z<0.1[/F][/FORMULA]

The HST survey of the B2 sample of radio galaxies: Detection of two optical jets

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