TY - JOUR

T1 - Modeling x-ray emission of a straight jet

T2 - PKS 0920-397

AU - Schwartz, D. A.

AU - Massaro, F.

AU - Siemiginowska, A.

AU - Worrall, D. M.

AU - Birkinshaw, M.

AU - Marshall, H.

AU - Evans, D.

AU - Perlman, E.

AU - Gelbord, J. M.

AU - Lovell, J. E.J.

AU - Godfrey, L.

AU - Bicknell, G.

AU - Ojha, R.

AU - Hardcastle, M.

AU - Jester, S.

AU - Jorstad, S.

AU - Stawarz, L.

N1 - Funding Information: This work was supported by NASA contract NAS8-03060 and SAO grants GO9-0121B and GO7-8107X. F. Massaro acknowledges a grant from the Foundation BLANCEFLOR Boncompagni-Ludovisi, n’ee Bildt.

PY - 2010/6

Y1 - 2010/6

N2 - We summarize a study of PKS 0920-397 using our 42 ks Chandra observation in conjunction with our ATCA 20GHz image, and HST/ACS F814W and F475W images. We investigate the hypothesis that the jet X-ray emission is due to inverse-Compton (IC) scattering on the cosmic microwave background (CMB) from the same population of relativistic electrons that give rise to the radio emission. To calculate parameters intrinsic to the source, one must finesse the fact that we do not know the true angle of the jet to our line of sight. Typical assumptions are that the Doppler factor equals the bulk Lorentz factor, or that the Lorentz factor takes some fixed numerical value. While giving useful estimates, neither assumption can be exact in general. We try different constraints to determine the jet quantities. It is plausible that the kinetic flux is constant along the jet, prior to a terminal hotspot or lobe, and with minimal bending of the jet. Alternatively, because PKS 0920-397 appears straight in projection on the sky, we might assume the jet maintains a constant angle to our line of sight. Either approach gives bulk Lorentz factors of 6 to 8, with kinetic energy flux of order 1046 erg s-1, and with the jet at an angle 2° to 4° from our line of sight.

AB - We summarize a study of PKS 0920-397 using our 42 ks Chandra observation in conjunction with our ATCA 20GHz image, and HST/ACS F814W and F475W images. We investigate the hypothesis that the jet X-ray emission is due to inverse-Compton (IC) scattering on the cosmic microwave background (CMB) from the same population of relativistic electrons that give rise to the radio emission. To calculate parameters intrinsic to the source, one must finesse the fact that we do not know the true angle of the jet to our line of sight. Typical assumptions are that the Doppler factor equals the bulk Lorentz factor, or that the Lorentz factor takes some fixed numerical value. While giving useful estimates, neither assumption can be exact in general. We try different constraints to determine the jet quantities. It is plausible that the kinetic flux is constant along the jet, prior to a terminal hotspot or lobe, and with minimal bending of the jet. Alternatively, because PKS 0920-397 appears straight in projection on the sky, we might assume the jet maintains a constant angle to our line of sight. Either approach gives bulk Lorentz factors of 6 to 8, with kinetic energy flux of order 1046 erg s-1, and with the jet at an angle 2° to 4° from our line of sight.

KW - jet emission mechanisms

KW - Quasar jets

KW - X-ray jets

UR - http://www.scopus.com/inward/record.url?scp=77955235362&partnerID=8YFLogxK

U2 - 10.1142/S0218271810017147

DO - 10.1142/S0218271810017147

M3 - Article

AN - SCOPUS:77955235362

VL - 19

SP - 879

EP - 885

JO - International Journal of Modern Physics D

JF - International Journal of Modern Physics D

SN - 0218-2718

IS - 6

ER -