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Multiwavelength Observations of the Quasar Jet in PKS 1030-357

Multiwavelength Observations of the Quasar Jet in PKS 1030-357. J.M. Gelbord, H.L. Marshall (MIT Kavli Inst.) S.G. Jorstad, A.P. Marscher (Boston Univ.) D.M. Worrall, M. Birkinshaw (Univ. of Bristol/SAO) D.A. Schwartz (SAO) J.E.J. Lovell, L. Godfrey, G.V. Bicknell, D.L. Jauncey (ATNF CSIRO)

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Multiwavelength Observations of the Quasar Jet in PKS 1030-357

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  1. Multiwavelength Observations of the Quasar Jet in PKS 1030-357 J.M. Gelbord, H.L. Marshall (MIT Kavli Inst.) S.G. Jorstad, A.P. Marscher (Boston Univ.) D.M. Worrall, M. Birkinshaw (Univ. of Bristol/SAO) D.A. Schwartz (SAO) J.E.J. Lovell, L. Godfrey, G.V. Bicknell, D.L. Jauncey (ATNF CSIRO) E.S. Perlman (UMBC) S. Jester (FNAL) D.W. Murphy (JPL)

  2. Prior PKS 1030-357 details • z = 1.455 • Flat spectrum radio quasar with radio jet • Unusual X-ray structure: • Either a double hot spot with strong X-rays from both • Or bright X-ray knots following a sharp bend

  3. New PKS 1030-357 data • New radio data: southern X-ray bright features have steep spectral indices (a ~ 1.2, where Snµn-a) • No clear counterparts in infrared or optical • Strong detection of X-ray jet; more structural details

  4. New PKS 1030-357 data Synchrotron model (solid line) • e- with 100 < g < 105 • a = 1.2 (to match radio) • Bme = 0.6 mG (w/o beaming) Dashed line = SSC Dotted line = IC-CMB • If synchrotron extends to X-rays, it will dominate non-beamed Bme models of SSC or IC-CMB, but can’t provide X-ray flux. • Inverse Compton could match a = 0.9 ± 0.3 X-ray spectrum, but requires extremely non-Bme field or relativistic beaming. Stay tuned - more to come! Preprints and more available at http://space.mit.edu/~jonathan/jets/

  5. Supplemental slides

  6. Candidate optical/IR counterparts • HST places optical/IR source near SE hot spot outside of the radio contours • Faint optical source at the tip of the inner jet

  7. Diffuse structure • Significant diffuse X-ray emission around PKS 1030-357 system; good agreement with lobes seen at lower radio frequencies • Likely IC emission from lobes

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