The Quasar 1317+520: A Laboratory for Particle

Acceleration

Svetlana Jorstad IAR, Boston U

Alan Marscher IAR , Boston U

Jonathan Gelbord U. Durham

Herman Marshall MIT

Dan Schwartz SAO

Diana Worrall U. Bristol

Mark Birkinshaw U. Bristol

Eric Perlman FIT

Svetlana Jorstad IAR, Boston U

Alan Marscher IAR , Boston U

Jonathan Gelbord U. Durham

Herman Marshall MIT

Dan Schwartz SAO

Diana Worrall U. Bristol

Mark Birkinshaw U. Bristol

Eric Perlman FIT

Radio Observations with the VLARadio Observations with the VLA at 15 GHz B-Array, 2 hrat 5 GHz A-Array, 2 hr

S5GHz = 396 mJy/beamS15GHz = 347 mJy/beam rms = 0.01 mJy/beambeam = 0.5'' x 0.5'', 0

5 GHz

C5

15 GHz

z=1.06, D = 7.1 GpcS5GHz = 104±15 mJyS15GHz = 40±8 mJyrad=0.83±0.03, S = -

C5 =1.2RC5 =4.3kpc

Radio Observations with the VLBARadio Observations with the VLBA at 15 GHz B-Array, 2 hrat 5 GHz A-Array, 2 hr

app ~5.7core 5.7

5 GHz

C5

Jjet/cjet ≈ 8.7cos ≈ 0.4=1- -2

- Lorentz factor

Aars & Hough 2005

Spectral/Polarization Properties of the JetSpectral/Polarization Properties of the Jet

Magnetic Fileld Structure in the JetMagnetic Fileld Structure in the Jet

Infrared Observations with Spitzer Space Telescope Infrared Observations with Spitzer Space Telescope

IRAC with 5.4ks: 4.5m & 8m

C5:S4,5m = 9.6±2.3 JyS8m = 16.6±4.5 JyIR=0.96±0.11

X-Ray Observations with Chandra: ACIS-S3, 18 ks, 0.2-6 keV X-Ray Observations with Chandra: ACIS-S3, 18 ks, 0.2-6 keV

C5NH=1.19x1020 cm-2

C5:

x=0.75±0.30S1keV =2.5±0.7 nJy

Prominent Feature C5 at 10'' from the Core

Prominent Feature C5 at 10'' from the Core

blue contours - 0.2-6keVcolor scale - 8mpink contours - 5GHz

0.83±0.03

0.96±0.11

0.75±0.30

Compton Shop Compton Shop http://jca.umbc.edu/~markos/cs

The one-zone steady-state model:A sphere of a given radius is moving with a given Lorentz factor throughan external photon field with a blackbody spectrum.An electron distribution with a powerlaw is continuously injected in the sphere.The electrons suffer synchrotron andinverse Compton losses and eventuallyescape from the source.The system reaches a steady state whenthe equation for energy conservation issatisfied:Linj = Lloss + Lesc The code calculates synchrotron, totalinverse Compton from all sources ofphotons, i.e., SSC and EC emission

Redshift, zLorentz factor, Doppler factor, Exponent for power law of theelectron distribution, pmin, max - minimum, maximum Lorentz factor of the electron distributionComoving luminosity, Linj, erg/sMagnetic field, B, GExternal photon field Radius of the sphere, R, cmEscape time, tesc , in units of R/c

Spectral Energy Distribution of C5Spectral Energy Distribution of C5

z=1.06=1.2=1.2p=2min =10 max =107

Linj = 21046 erg/sec

B = 15 GR = 1.31022 cm tesc =5 , CMB

UB= 9.010-12 erg cm-3

Up= Linj/(4R2u)= 1.610-11 erg cm-3

u=c/tesc , =h/(mc2) tltcross=R/u=1.4106 yr

Magnetic Field Structure in C5Magnetic Field Structure in C5

ConclusionsConclusions1.The bright radio feature detected at 10 from the core has counter-parts at X-ray and IR wavelengths.2. The SED of the feature suggests that the observed emission isproduced via the synchrotron mechanism and EC/CMB process by a single population of relativistic electrons with Lorentz factors up to 107 and energy index ~3.3. The jet in this region is mildly relativistic with Doppler factor ~ 1.2 and magnetic field B ~ 15 G.4. The jet most likely decelerates on kiloparsec scales bya factor of ~3 in with respect to the parsec-scale jet flow. 5. The injection of particles of such high energies in the region seems to occur at an oblique shock front formed by the interaction of the jet with a cloud that is ramming it at an angle.6. The particles stay in the region 1.4106 yr and cool efficiently.7. The EC/CMB process should produce -ray emission that possiblycan be detected with the GLAST.