Quasar Jet Surveys with Chandra Herman L. Marshall (MIT) D. Schwartz, D. WorralL, M. Birkinshaw (SAO) M. Lister, B. Hogan, P. Kharb (Purdue) & J. Gelbord, E. Perlman, L. Godfrey, J. Lovell, etc. Schwartz et al. 2000 CXC Marshall et al. 2001
Overview • History of FR II jet surveys using Chandra • Results from 2 recent surveys • Individual studies • see also poster by Leith Godfrey HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 2
Overview • History of FR II jet surveys using Chandra • Results from 2 recent surveys • Individual studies • see also poster by Leith Godfrey HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 2
First Chandra Jet • Observed for focussing Schwartz et al. 2000 Contours: Radio Color: X-ray • Jet flux is 7% of core flux • 3C 273: 0.5% in jet • Optical jet emission is weak Contours: Radio Color: Optical • Rules out simple synchrotron • Rules out SSC l e d o m • Inverse Compton of CMB n o r t o r h c n • Jet is 10° to line of sight B y M S C f f o C I • Bulk Γ ~ 15 C S S • Γ , θ like pc scale VLBI HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 3
First Chandra Jet • Observed for focussing Schwartz et al. 2000 Contours: Radio Color: X-ray • Jet flux is 7% of core flux • 3C 273: 0.5% in jet • Optical jet emission is weak Contours: Radio Color: Optical • Rules out simple synchrotron • Rules out SSC l e d o m • Inverse Compton of CMB n o r t o r h c n • Jet is 10° to line of sight B y M S C f f o C I • Bulk Γ ~ 15 C S S • Γ , θ like pc scale VLBI HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 3
First Chandra Jet • Observed for focussing Schwartz et al. 2000 Contours: Radio Color: X-ray • Jet flux is 7% of core flux • 3C 273: 0.5% in jet • Optical jet emission is weak Contours: Radio Color: Optical • Rules out simple synchrotron • Rules out SSC l e d o m • Inverse Compton of CMB n o r t o r h c n • Jet is 10° to line of sight B y M S C f f o C I • Bulk Γ ~ 15 C S S • Γ , θ like pc scale VLBI HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 3
IC-CMB Method • See Tavecchio+ ’00, Celotti+ ’01, Dermer ’95 • Based on blazar core modeling • superluminal motion --> high Γ , small θ • Doppler factor is large δ = 1 / (Γ[1 − β cos θ ]) • Estimate B’ me in jet frame • based on B me in observed frame B ′ me = B me /δ • B me depends (weakly) on L r , V of a jet knot • Assume L x is iC from CMB: u B = B 2 L S = ν r S r = u B 8 π = a [(1 + z ) T ] 4 Γ 2 L S ≅ aT 4 (1 + z ) 4 δ 2 ν r S r L IC ν x S x u ν L IC ν x S x • Match B to B’ me , giving δ from observables HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 4
Jet Surveys • Selected from VLA, ATCA maps of FSRQs • Sambruna+ 2004 • 17 objects, 10 detected in 10 ks snapshots • Marshall+ 2005, 2011, & in prep. • 56 sources, 5 ks snapshots • 32/51 detected, some overlap with Sambuna+ • Hogan+ 2011 — selected from MOJAVE • 21/27 detected, some overlap with M+ • Cheung+ 2007, Saez+ 2011 — 3 at z > 4 • Total: 48/78 = 61.5% (z<2.5), HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 5
Survey Examples HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 6
Jet Survey Results I • S x /S r distribution is broad • <S x /S r > depends weakly on z • IC-CMB: <S x /S r > ∝ (1+z) α +3 , but not found HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 7
Jet Survey Results I • S x /S r distribution is broad • <S x /S r > depends weakly on z • IC-CMB: <S x /S r > ∝ (1+z) α +3 , but not found HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 7
Mojave Survey Hogan+ 2011 • Sample from MOJAVE list • VLBI: pc-scale jet motion • Chandra survey: IC-CMB model constraints • Jets likely bend by few degrees from pc to kpc • Deceleration is most likely HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 8
Deeper Imaging I • Deep X-ray imaging: more X-rays between knots • PKS1136: decelerating by entrainment (Tavecchio 05) Sambruna et al. 2006 Sambruna et al. 2006 HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 9
Deeper Imaging II • Radio-OIR fits simple synchrotron • X-ray peak fit by IC- Godfrey+ ’11 CMB after bend • knot is elongated along jet • total power --> e+/e- • Γ = 6 HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 10
Deepest Imaging Jester+ ’06 3C 273 Siemiginowska+ ’07 PKS 1127-145 Harris + ’11 4C 19.44 Schwartz+ ’06 Q1055+201 HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 11
3C 273 Jet 2nd part • Width changes along jet • A1, B1: point-like • Rest is broad channel • Spectral indices differ • Spine-sheath structure? Marshall et al. 2006 Jester et al. 2006 HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 12 Jester et al. 2006
Bonus: Pictor A • New radio map, HST images • Galactic tidal tail, long offset 1.6 µ knot in jet HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 13
Bonus: Pictor A • New radio map, HST images • Galactic tidal tail, long offset 1.6 µ knot in jet HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 13
Summary • Chandra surveys: jets in 60% of FSRQs (z<2.5) • Distribution of S x /S r is broad • Dependence on z is not obvious • Angles to line of sight larger than on pc scale • Some jets are relativistic on Mpc scales • Follow-ups provide details • IC-CMB fits for many knots --> gives B, Γ • Deceleration, entrainment likely • Radio/X-ray offsets, α x are problematic • Need large survey with z>2.5, z>4 • Need UV, X-ray polarization HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 14
Barcelona HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15 15
Barcelona 15 Montserrat HEPRO 3 — June 30, 2011 Marshall — Quasar Jets /15
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