Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195)

D. A. Schwartz; D. E. Harris; H. Landt; A. Siemiginowska; E. S. Perlman; C. C. Cheung; J. M. Gelbord; D. M. Worrall; M. Birkinshaw; S. G. Jorstad; A. P. Marscher; L. Stawarz

doi:10.1017/S1743921307005868

Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195)

D. A. Schwartz, D. E. Harris, H. Landt, A. Siemiginowska, E. S. Perlman, C. C. Cheung, J. M. Gelbord, D. M. Worrall, M. Birkinshaw, S. G. Jorstad, A. P. Marscher, L. Stawarz

School of Physics

Research output: Chapter in Book/Report/Conference proceeding › Conference Contribution (Conference Proceeding)

Abstract

We investigate the variations of the magnetic field, Doppler factor, and relativistic particle density along the jet of a quasar at z = 0.72. We chose 4C 19.44 for this study because of its length and very straight morphology. The 18˝ length of the jet provides many independent resolution elements in the Chandra X-ray image.The straightness suggests that geometry factors, although uncertain, are almost constant along the jet. Since published optical emission from the jet prohibits a single synchrotron spectrum producing the radio and X-ray emission, we interpret the X-ray emission as inverse Compton scattering on the cosmic microwave background. With the aid of assumptions about jet alignment, equipartition between magnetic field and relativistic electron energy, and filling factors, we find that the jet is in bulk relativistic motion with a Doppler factor ˜6 at an angle no more than 10° to the line of sight over distances ˜150-600 kpc from the quasar, and a magnetic field ˜10 μGauss. X-ray emission is also seen throughout a ˜10˝ extension to the S of the jet, in a region where the radio emission is fainter, and also in the S radio lobe.

Original language	English
Title of host publication	Black Holes
Subtitle of host publication	From Stars to Galaxies - Across the Range of Masses
Editors	Vladimir Karas, Giorgio Matt
Place of Publication	Cambridge, UK
Publisher	Cambridge University Press
Pages	443-444
ISBN (Print)	9780521863476
DOIs	https://doi.org/10.1017/S1743921307005868
Publication status	Published - 1 Aug 2007

Publication series

Name	Proceedings of the International Astronomical Union Symposia and Colloquia
Number	238

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http://adsabs.harvard.edu/abs/2007IAUS..238..443S

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Schwartz, D. A., Harris, D. E., Landt, H., Siemiginowska, A., Perlman, E. S., Cheung, C. C., Gelbord, J. M., Worrall, D. M., Birkinshaw, M., Jorstad, S. G., Marscher, A. P., & Stawarz, L. (2007). Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195). In V. Karas, & G. Matt (Eds.), Black Holes: From Stars to Galaxies - Across the Range of Masses (pp. 443-444). (Proceedings of the International Astronomical Union Symposia and Colloquia; No. 238). Cambridge University Press. https://doi.org/10.1017/S1743921307005868

@inproceedings{5c7d595207d442af9c2292c59387d7ee,

title = "Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195)",

abstract = "We investigate the variations of the magnetic field, Doppler factor, and relativistic particle density along the jet of a quasar at z = 0.72. We chose 4C 19.44 for this study because of its length and very straight morphology. The 18˝ length of the jet provides many independent resolution elements in the Chandra X-ray image.The straightness suggests that geometry factors, although uncertain, are almost constant along the jet. Since published optical emission from the jet prohibits a single synchrotron spectrum producing the radio and X-ray emission, we interpret the X-ray emission as inverse Compton scattering on the cosmic microwave background. With the aid of assumptions about jet alignment, equipartition between magnetic field and relativistic electron energy, and filling factors, we find that the jet is in bulk relativistic motion with a Doppler factor ˜6 at an angle no more than 10° to the line of sight over distances ˜150-600 kpc from the quasar, and a magnetic field ˜10 μGauss. X-ray emission is also seen throughout a ˜10˝ extension to the S of the jet, in a region where the radio emission is fainter, and also in the S radio lobe.",

author = "Schwartz, \{D. A.\} and Harris, \{D. E.\} and H. Landt and A. Siemiginowska and Perlman, \{E. S.\} and Cheung, \{C. C.\} and Gelbord, \{J. M.\} and Worrall, \{D. M.\} and M. Birkinshaw and Jorstad, \{S. G.\} and Marscher, \{A. P.\} and L. Stawarz",

year = "2007",

month = aug,

day = "1",

doi = "10.1017/S1743921307005868",

language = "English",

isbn = "9780521863476",

series = "Proceedings of the International Astronomical Union Symposia and Colloquia",

publisher = "Cambridge University Press",

number = "238",

pages = "443--444",

editor = "Vladimir Karas and Giorgio Matt",

booktitle = "Black Holes",

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}

Schwartz, DA, Harris, DE, Landt, H, Siemiginowska, A, Perlman, ES, Cheung, CC, Gelbord, JM, Worrall, DM, Birkinshaw, M, Jorstad, SG, Marscher, AP & Stawarz, L 2007, Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195). in V Karas & G Matt (eds), Black Holes: From Stars to Galaxies - Across the Range of Masses. Proceedings of the International Astronomical Union Symposia and Colloquia, no. 238, Cambridge University Press, Cambridge, UK, pp. 443-444. https://doi.org/10.1017/S1743921307005868

Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195). / Schwartz, D. A.; Harris, D. E.; Landt, H. et al.
Black Holes: From Stars to Galaxies - Across the Range of Masses. ed. / Vladimir Karas; Giorgio Matt. Cambridge, UK: Cambridge University Press, 2007. p. 443-444 (Proceedings of the International Astronomical Union Symposia and Colloquia; No. 238).

Research output: Chapter in Book/Report/Conference proceeding › Conference Contribution (Conference Proceeding)

TY - GEN

T1 - Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195)

AU - Schwartz, D. A.

AU - Harris, D. E.

AU - Landt, H.

AU - Siemiginowska, A.

AU - Perlman, E. S.

AU - Cheung, C. C.

AU - Gelbord, J. M.

AU - Worrall, D. M.

AU - Birkinshaw, M.

AU - Jorstad, S. G.

AU - Marscher, A. P.

AU - Stawarz, L.

PY - 2007/8/1

Y1 - 2007/8/1

N2 - We investigate the variations of the magnetic field, Doppler factor, and relativistic particle density along the jet of a quasar at z = 0.72. We chose 4C 19.44 for this study because of its length and very straight morphology. The 18˝ length of the jet provides many independent resolution elements in the Chandra X-ray image.The straightness suggests that geometry factors, although uncertain, are almost constant along the jet. Since published optical emission from the jet prohibits a single synchrotron spectrum producing the radio and X-ray emission, we interpret the X-ray emission as inverse Compton scattering on the cosmic microwave background. With the aid of assumptions about jet alignment, equipartition between magnetic field and relativistic electron energy, and filling factors, we find that the jet is in bulk relativistic motion with a Doppler factor ˜6 at an angle no more than 10° to the line of sight over distances ˜150-600 kpc from the quasar, and a magnetic field ˜10 μGauss. X-ray emission is also seen throughout a ˜10˝ extension to the S of the jet, in a region where the radio emission is fainter, and also in the S radio lobe.

AB - We investigate the variations of the magnetic field, Doppler factor, and relativistic particle density along the jet of a quasar at z = 0.72. We chose 4C 19.44 for this study because of its length and very straight morphology. The 18˝ length of the jet provides many independent resolution elements in the Chandra X-ray image.The straightness suggests that geometry factors, although uncertain, are almost constant along the jet. Since published optical emission from the jet prohibits a single synchrotron spectrum producing the radio and X-ray emission, we interpret the X-ray emission as inverse Compton scattering on the cosmic microwave background. With the aid of assumptions about jet alignment, equipartition between magnetic field and relativistic electron energy, and filling factors, we find that the jet is in bulk relativistic motion with a Doppler factor ˜6 at an angle no more than 10° to the line of sight over distances ˜150-600 kpc from the quasar, and a magnetic field ˜10 μGauss. X-ray emission is also seen throughout a ˜10˝ extension to the S of the jet, in a region where the radio emission is fainter, and also in the S radio lobe.

U2 - 10.1017/S1743921307005868

DO - 10.1017/S1743921307005868

M3 - Conference Contribution (Conference Proceeding)

SN - 9780521863476

T3 - Proceedings of the International Astronomical Union Symposia and Colloquia

SP - 443

EP - 444

BT - Black Holes

A2 - Karas, Vladimir

A2 - Matt, Giorgio

PB - Cambridge University Press

CY - Cambridge, UK

ER -

Schwartz DA, Harris DE, Landt H, Siemiginowska A, Perlman ES, Cheung CC et al. Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195). In Karas V, Matt G, editors, Black Holes: From Stars to Galaxies - Across the Range of Masses. Cambridge, UK: Cambridge University Press. 2007. p. 443-444. (Proceedings of the International Astronomical Union Symposia and Colloquia; 238). doi: 10.1017/S1743921307005868

Detailed structure of the X-ray jet in 4C 19.44 (PKS1354+195)

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