[PPT] - Large-scale emission from FR I jets Pol Bordas with the PowerPoint Presentation

SLIDE 1

Large-scale emission from FR I jets

Pol Bordas

with the collaboration of V. Bosch-Ramon & M. Perucho

Barcelona June 2011,

miércoles 29 de junio de 2011

SLIDE 2

The FR I/II dichotomy
FR jets/medium interaction
Large scale emission in FR I jets
Summary & conclusions

Large-scale emission in FR I jets Pol Bordas, HEPRO III

OUTLINE

miércoles 29 de junio de 2011

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Active galactic nuclei

Radio-loud (~10%), eliptical Jet stuck in matter 100 kpc scale jet L178 > 2.5·1026 W/Hz L178 < 2.5·1026 W/Hz GPS/CSS Radio quasar SSRQ FSRQ FR II radio galaxy BL Lac Blazar Radio Interm. quasar Seyfert I FR I radio galaxy Optically strong Optically weak Radio-quiet (~90%), spiral Broad Lines Narrow Lines Broad Lines Radio weak quasar Seyfert II LBLs HBLs

The FR I - FR II dichotomy

Large-scale emission in FR I jets Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 4

Active galactic nuclei

Radio-loud (~10%), eliptical Jet stuck in matter 100 kpc scale jet L178 > 2.5·1026 W/Hz L178 < 2.5·1026 W/Hz GPS/CSS Radio quasar SSRQ FSRQ FR II radio galaxy BL Lac Blazar FR I radio galaxy LBLs HBLs Radio Interm. quasar Seyfert I Optically strong Optically weak Radio-quiet (~90%), spiral Broad Lines Narrow Lines Broad Lines Radio weak quasar Seyfert II

(...) there is a sharp division in luminosity between the two classes; those with luminosities at 178 MHz below 2 x 1025 W/ Hz are nearly all of Class I, and those above nearly all of Class II

Fanaroff & Riley, 1974, MNRAS, 167, 31

“(...) radio sources were classified using the ratio (r) of the distance between the regions of highest brightness to the total extent of the source measured from the lowest (energy) contour into Class 1 (r < 0.5) and Class II (r > 0.5).

The FR I - FR II dichotomy

Large-scale emission in FR I jets Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 5

Ledlow & Owen, 1996, AJ, 112, 9 Ghisellini & Celotti, 2001, A&A, 379, L1

Large-scale emission in FR I jets

The FR I - FR II dichotomy

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 6

interaction with the medium fundamental differences

jet deceleration against the ambient gas (Begelman 1982; Gopal-Krishna & Wiita 1988, 2001)
both FR I and II jets are relativistic near the core. FR I much slower at large distances (Bicknell 1995)
jet bending is common in FR I, not in FR II
observation of hybrid sources (Gopal-Krishna & Wiita 2000)
jet composition: FR I → e+ - e- plasma (Reynolds et al. 1996); FR II → e-- p plasma (Celotti et al. 1997)
black hole spin (Blandford & Znajek 1977, Rees 1982, Meier 1999)
jet power - accretion rate (Gopal-Krishna 1988, Blandford 1996, Ghisellini & Celotti 2001)
jet magnetic field at large scales (|| to jet axis in FR II, ⊥ in FR I’s)

Large-scale emission in FR I jets

The FR I - FR II dichotomy

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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HYMORS: HYbrid MOrphology Radio Sources e.g. NGC 612: “5 GHz radio maps show that the eastern lobe has a bright hotspot near its outer edge (FR II type), whereas the western lobe exhibits a jet-like structure which widens steadily and fades into a diffuse radio plume (FR I) ”

0131-36A IPOL 4885.100 MHZ NGC612AAA.ICLN.1 DECLINATION (B1950) RIGHT ASCENSION (B1950) 01 32 00 31 45 30 15

36 42

43 44 45 46 47

Gopal-Krishna & Wiita, 2000, A&A. 363, 507

Large-scale emission in FR I jets

The FR I - FR II dichotomy

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Nucleus

Chandra HS

Large-scale emission in FR I jets

FR jets/medium interaction

VLA image of 3C351 at 1.4 GHz with Chandra X- ray contours superposed. From Brunetti et al. 2001, ApJ, 561,L157 M87 as seen by Chandra plus with 8 GHz contours. From Harris & Krawczynski, 2006, ARA&A. 44, 463 Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 9

Large-scale emission in FR I jets

FR jets/medium interaction

Hot Spots cocoon shell contact discontinuity disrupted jet shell cocoon entrainment

f external

material

FR II FR I

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 10

Large-scale emission in FR I jets

FR II jets/medium interaction: numerical simulations

Scheck et al. 2002, MNRAS, 331, 615 Perucho et al. (in preparation)

jet composition, whether e+ - e- or e-- p plasma does not affect

strongly the propagation of FR II jets plasma

Relativistic jets may be very efficient in reheating the ICM → cooling flow problem

rest-mass density temperature rest-mass density

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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shocked jet cocoon bow shock reverse shock reconfnement shock

zreconf rb l b

Large-scale emission in FR I jets

FR II jets/medium interaction: analytical models

FR II 6 7

ρ ρ0 d -β

; ρ0 ≈

[ 2 x

25 g cm
3

45 46 med med med FR II FR II

β

med med med med med med med

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 12

Large-scale emission in FR I jets

FR II jets/medium interaction: non-thermal emission

Ito et al. 2011, ApJ, 730, 120

strong photon fields: UVdisk, IRtorus, NIRhost-galaxy
moderately powerful jets (Ljet~1045 erg cm-2 s-1)
evolution through source size: R1 = 1 to 100 kpc
fixed magnetic field = 10-5 G
spectral aging
One zone model for each tsource

lobe shell lobe shell shell lobe

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 13

Large-scale emission in FR I jets

FR I jets/medium interaction: numerical simulations

Perucho & Martí, 2007, MNRAS, 382, 526 Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets Perucho & Martí, 2007, MNRAS, 382, 526 shell pressure cocoon pressure shell density cocoon density

FR I jets/medium interaction: numerical simulations

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets

FR I jets/medium interaction: radiative model

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets Bordas, Bosch-Ramon & Perucho, 2011, MNRAS. 412, 1229

FR I jets/medium interaction: radiative model

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets Bordas, Bosch-Ramon & Perucho, 2011, MNRAS. 412, 1229

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log ν Lν (erg s

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UV X-rays HE γ-rays VHE γ-rays

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cocoon cocoon RH Av

FR I jets/medium interaction: radiative model

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets Bordas, Bosch-Ramon & Perucho, 2011, MNRAS. 412, 1229 Radio X-rays

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shell cocoon total

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log L >100 GeV (erg s

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HE γ-rays VHE γ-rays

FR I jets/medium interaction: radiative model

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets

Bolometric thermal emission increases with time: despite shell density and bow shock velocity

decrease, tthermal > tsrc. Peak of thermal emission shifted to lower energies as tsrc increases

Radio: fluxes up to 10-12 (d/100 Mpc)-2 erg cm-2 s-1 (~few Jy) in a region of ~10 arcmin
3C 31: F5GHz = 3 × 1040 erg/s, Andernach et al. 1992)
3C 15: F5GHz ~ 10-14 erg cm-2 s-1 (d = 300 Mpc)
X-rays: thermal : Fluxes ~10-13 erg cm-2 s-1 for tsrc = 108 yrs. Hard X-rays in more compact regions

(~1 arcmin) along the jet apex; soft X-rays from the whole shell. non-thermal: cocoon dominates in our model, though limb brightening effects may make the shell brighter (Cen A?)

X-ray fluxes at the level of those reported, e.g., for 3C 15 (Kataoka et al. 2003)
HE gamma-rays: νLν ~1039 -40 erg/s for tsrc = 107-8 yrs, Γph ≈ 2.3
Cen A by Fermi: ~ 10-11 erg cm2 s-1=> ~1040 erg/s (d = 3 Mpc).
Distant sources --> higher non-thermal efficiencies/Ljetbut enough angular resolution?
VHE gamma-rays: νLν ~1037 - a few × 1038 erg/s for tsrc = 107-108 yrs
steep spectrum above ~1 TeV; faint extended flux => long tobs required !
angular resoultions at ~arcmin (=> CTA?)

FR I jets/medium interaction: radiative model

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets

SUMMARY & CONCLUSIONS

FRI’s vs FRII’s: HYMORS + rel. velocities in both FR I/II at sub-kpc scales ⇒ ambient medium favored?
FR I’s → jet disrupted (entrainment?); bow shock trans/sub-sonic ⇒ but can still accelerate efficiently!
The external medium profile has a strong impact on the predicted thermal/non-thermal emission
Bow shock strong up to tsrc = 108 yr ⇒ no transition to weak shock regime (see e.g. Zanni et al. 2003)

but thermal fotons do not reach the MeV energy (Kino et al. 2007)

Radiation appears extended in most of the energy bands.
Lobes/shell of FRI radio galaxies are good candidates to be detected in the whole spectral range
Thermal X-rays seem unavoidable and may dominate soft X-rays in old sources
soft thermal X-rays in the whole shell, hard thermal X-rays at the bow shock apex

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

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Large-scale emission in FR I jets Abdo et al. 2010, Science, 328, 725 Beckmann et al. 2011, arXiv 1104.4253 Croston et al. 2009, MNRAS, 325, 199 Hardcastle et al. 2011, arXiv1103.1744

IC vs Sync: soft X-rays dominated by synchrotron, IC increasing for older sources
Non-thermal fluxes dominated by cocoon; shell → limb brightening effects ?
HE and VHE gamma-rays may require long exposures/nearby sources
Cen A lobes/shell: Fermi (> 0.1 GeV) + INTEGRAL/SPI (hint: 4 sigma, > 1 MeV) + predictions @

VHE (long tobs)

SUMMARY & CONCLUSIONS

Pol Bordas, HEPRO III

miércoles 29 de junio de 2011

SLIDE 22

Backup slides

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SLIDE 23

Bosch-Ramon et al. (2011) Large-scale emission from microquasars

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Large-scale emission from microquasars

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Large-scale emission from microquasars

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Large-scale emission from microquasars

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Large-scale emission from microquasars

miércoles 29 de junio de 2011