Quasar Jet Surveys with Chandra Herman L. Marshall (MIT) D. - - PowerPoint PPT Presentation

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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.

SLIDE 1

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. CXC

Schwartz et al. 2000 Marshall et al. 2001

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Overview

History of FR II jet surveys using Chandra
Results from 2 recent surveys
Individual studies
see also poster by Leith Godfrey

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Overview

History of FR II jet surveys using Chandra
Results from 2 recent surveys
Individual studies
see also poster by Leith Godfrey

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

First Chandra Jet

Contours: Radio Color: X-ray Contours: Radio Color: Optical

S y n c h r

e l I C

f C M B S S C

Schwartz et al. 2000

Observed for focussing
Jet flux is 7% of core flux
3C 273: 0.5% in jet
Optical jet emission is weak
Rules out simple synchrotron
Rules out SSC
Inverse Compton of CMB
Jet is 10° to line of sight
Bulk Γ ~ 15
Γ, θ like pc scale VLBI

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

First Chandra Jet

Contours: Radio Color: X-ray Contours: Radio Color: Optical

S y n c h r

e l I C

f C M B S S C

Schwartz et al. 2000

Observed for focussing
Jet flux is 7% of core flux
3C 273: 0.5% in jet
Optical jet emission is weak
Rules out simple synchrotron
Rules out SSC
Inverse Compton of CMB
Jet is 10° to line of sight
Bulk Γ ~ 15
Γ, θ like pc scale VLBI

SLIDE 6

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

First Chandra Jet

Contours: Radio Color: X-ray Contours: Radio Color: Optical

S y n c h r

e l I C

f C M B S S C

Schwartz et al. 2000

Observed for focussing
Jet flux is 7% of core flux
3C 273: 0.5% in jet
Optical jet emission is weak
Rules out simple synchrotron
Rules out SSC
Inverse Compton of CMB
Jet is 10° to line of sight
Bulk Γ ~ 15
Γ, θ like pc scale VLBI

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

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
Estimate B’me in jet frame
based on Bme in observed frame
Bme depends (weakly) on Lr, V of a jet knot
Assume Lx is iC from CMB:
Match B to B’me, giving δ from observables

δ = 1/(Γ[1 − β cos θ]) B′

me = Bme/δ

LS LIC = νrSr νxSx = uB uν uB = B2 8π = a[(1 + z)T]4Γ2 LS LIC ≅ aT 4(1 + z)4δ2 νrSr νxSx

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

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),

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Survey Examples

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Jet Survey Results I

Sx/Sr distribution is broad
<Sx/Sr> depends weakly on z
IC-CMB: <Sx/Sr> ∝ (1+z)α+3, but not found

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Jet Survey Results I

Sx/Sr distribution is broad
<Sx/Sr> depends weakly on z
IC-CMB: <Sx/Sr> ∝ (1+z)α+3, but not found

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Mojave Survey

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

Hogan+ 2011

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

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

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Deeper Imaging II

Radio-OIR fits simple

synchrotron

X-ray peak fit by IC-

CMB after bend

knot is elongated along jet
total power --> e+/e-
Γ = 6

Godfrey+ ’11

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Deepest Imaging

Schwartz+ ’06

3C 273 PKS 1127-145 4C 19.44 Q1055+201

Harris + ’11 Siemiginowska+ ’07 Jester+ ’06

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Width changes along jet
A1, B1: point-like
Rest is broad channel
Spectral indices differ
Spine-sheath structure?

Jester et al. 2006

Marshall et al. 2006

3C 273 Jet 2nd part

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Bonus: Pictor A

New radio map, HST images
Galactic tidal tail, long offset 1.6µ knot in jet

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Bonus: Pictor A

New radio map, HST images
Galactic tidal tail, long offset 1.6µ knot in jet

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Summary

Chandra surveys: jets in 60% of FSRQs (z<2.5)
Distribution of Sx/Sr 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, αx are problematic
Need large survey with z>2.5, z>4
Need UV, X-ray polarization

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Barcelona

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HEPRO 3 — June 30, 2011 Marshall — Quasar Jets

Barcelona

15 Montserrat