University of Hertfordshire

From the same journal

From the same journal

By the same authors

Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A

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Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A. / Snios, Bradford; Wykes, Sarka; Nulsen, Paul E. J.; Kraft, Ralph P.; Meyer, Eileen T.; Birkinshaw, Mark; Worrall, Diana M.; Hardcastle, Martin J.; Roediger, Elke; Forman, William R.; Jones, Christine.

In: The Astrophysical Journal, Vol. 871, No. 2, 248, 05.02.2019.

Research output: Contribution to journalArticlepeer-review

Harvard

Snios, B, Wykes, S, Nulsen, PEJ, Kraft, RP, Meyer, ET, Birkinshaw, M, Worrall, DM, Hardcastle, MJ, Roediger, E, Forman, WR & Jones, C 2019, 'Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A', The Astrophysical Journal, vol. 871, no. 2, 248. https://doi.org/10.3847/1538-4357/aafaf3

APA

Snios, B., Wykes, S., Nulsen, P. E. J., Kraft, R. P., Meyer, E. T., Birkinshaw, M., Worrall, D. M., Hardcastle, M. J., Roediger, E., Forman, W. R., & Jones, C. (2019). Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A. The Astrophysical Journal, 871(2), [248]. https://doi.org/10.3847/1538-4357/aafaf3

Vancouver

Snios B, Wykes S, Nulsen PEJ, Kraft RP, Meyer ET, Birkinshaw M et al. Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A. The Astrophysical Journal. 2019 Feb 5;871(2). 248. https://doi.org/10.3847/1538-4357/aafaf3

Author

Snios, Bradford ; Wykes, Sarka ; Nulsen, Paul E. J. ; Kraft, Ralph P. ; Meyer, Eileen T. ; Birkinshaw, Mark ; Worrall, Diana M. ; Hardcastle, Martin J. ; Roediger, Elke ; Forman, William R. ; Jones, Christine. / Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A. In: The Astrophysical Journal. 2019 ; Vol. 871, No. 2.

Bibtex

@article{7393b3555d924e35ab308dcf3531068b,
title = "Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A",
abstract = "We report results from Chandra observations analyzed for evidence of variability and proper motion in the X-ray jet of Centaurus A. Using data spanning 15 yr, collective proper motion of 11.3 ± 3.3 mas yr -1 , or 0.68 ± 0.20c, is detected for the fainter X-ray knots and other substructure present within the jet. The three brightest knots (AX1A, AX1C, and BX2) are found to be stationary to an upper limit of . Brightness variations up to 27% are detected for several X-ray knots in the jet. For the fading knots, BX2 and AX1C, the changes in spectral slope expected to accompany synchrotron cooling are not found, ruling it out and placing upper limits of ≃80 μG for each of their magnetic field strengths. Adiabatic expansion can account for the observed decreases in brightness. Constraints on models for the origin of the knots are established. Jet plasma overrunning an obstacle is favored as the generator of stationary knots, while moving knots are likely produced either by internal differences in jet speed or the late stages of jet interaction with nebular or cloud material. ",
keywords = "galaxies: active, galaxies: individual (Centaurus A), galaxies: jets, X-rays: galaxies",
author = "Bradford Snios and Sarka Wykes and Nulsen, {Paul E. J.} and Kraft, {Ralph P.} and Meyer, {Eileen T.} and Mark Birkinshaw and Worrall, {Diana M.} and Hardcastle, {Martin J.} and Elke Roediger and Forman, {William R.} and Christine Jones",
note = "Accepted to ApJ, 14 pages, 8 figures, 2 tables",
year = "2019",
month = feb,
day = "5",
doi = "10.3847/1538-4357/aafaf3",
language = "English",
volume = "871",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

RIS

TY - JOUR

T1 - Variability and Proper Motion of X-ray Knots in the Jet of Centaurus A

AU - Snios, Bradford

AU - Wykes, Sarka

AU - Nulsen, Paul E. J.

AU - Kraft, Ralph P.

AU - Meyer, Eileen T.

AU - Birkinshaw, Mark

AU - Worrall, Diana M.

AU - Hardcastle, Martin J.

AU - Roediger, Elke

AU - Forman, William R.

AU - Jones, Christine

N1 - Accepted to ApJ, 14 pages, 8 figures, 2 tables

PY - 2019/2/5

Y1 - 2019/2/5

N2 - We report results from Chandra observations analyzed for evidence of variability and proper motion in the X-ray jet of Centaurus A. Using data spanning 15 yr, collective proper motion of 11.3 ± 3.3 mas yr -1 , or 0.68 ± 0.20c, is detected for the fainter X-ray knots and other substructure present within the jet. The three brightest knots (AX1A, AX1C, and BX2) are found to be stationary to an upper limit of . Brightness variations up to 27% are detected for several X-ray knots in the jet. For the fading knots, BX2 and AX1C, the changes in spectral slope expected to accompany synchrotron cooling are not found, ruling it out and placing upper limits of ≃80 μG for each of their magnetic field strengths. Adiabatic expansion can account for the observed decreases in brightness. Constraints on models for the origin of the knots are established. Jet plasma overrunning an obstacle is favored as the generator of stationary knots, while moving knots are likely produced either by internal differences in jet speed or the late stages of jet interaction with nebular or cloud material.

AB - We report results from Chandra observations analyzed for evidence of variability and proper motion in the X-ray jet of Centaurus A. Using data spanning 15 yr, collective proper motion of 11.3 ± 3.3 mas yr -1 , or 0.68 ± 0.20c, is detected for the fainter X-ray knots and other substructure present within the jet. The three brightest knots (AX1A, AX1C, and BX2) are found to be stationary to an upper limit of . Brightness variations up to 27% are detected for several X-ray knots in the jet. For the fading knots, BX2 and AX1C, the changes in spectral slope expected to accompany synchrotron cooling are not found, ruling it out and placing upper limits of ≃80 μG for each of their magnetic field strengths. Adiabatic expansion can account for the observed decreases in brightness. Constraints on models for the origin of the knots are established. Jet plasma overrunning an obstacle is favored as the generator of stationary knots, while moving knots are likely produced either by internal differences in jet speed or the late stages of jet interaction with nebular or cloud material.

KW - galaxies: active

KW - galaxies: individual (Centaurus A)

KW - galaxies: jets

KW - X-rays: galaxies

UR - http://www.scopus.com/inward/record.url?scp=85062008250&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/aafaf3

DO - 10.3847/1538-4357/aafaf3

M3 - Article

VL - 871

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 248

ER -