ChandraObservations of Kiloparsec-ScaleJets

Dan Schwartz

Chandra X-ray Center Harvard/Smithsonian Center for

Astrophysics

Calibration Workshop Cambridge, MA

26 October, 2004

INTRODUCTION

• What Do Jets Do?

– Carry large quantities of energy, to supply radio lobes

– Interact with gas in galaxies and clusters of galaxies

• What Do We Want to Learn?

– Particle composition and acceleration

– Jet acceleration and collimation

• Why Do We Need Multiwavelength Data?

– Spectral Energy Distribution (SED) gives mechanism

– Particle lifetimes change with observed band

IMAGING ISSUES

• Morphology

– Radio/Optical/X-ray comparison

– Knots vs. hotspots vs. continuum

• Detailed Spatial Relations

– How do we define a region?

– Where are acceleration sites?

– Lifetime issues

• Change of Direction

Outline1. Nearby Jets

• Cen A, 3.4 Mpc

• M87, 16 Mpc

• 3C 273, 750 Mpc

2. Quasar/FRII Jets

3. Jets at Large Redshift

Cen A, Kraft et al.

M87 Nucleus and Inner Jet

12:30:49.049.249.4 48.8 48.6 48.4 48.2

2:23:30

31

32

33

34

35

36

29

28

27

26

C + G

B

A

FE

knot D

HST-1

core

Gaussian smoothing: FWHM=0.25 asec

1/10 native ACIS pixels

No pixel randomization

M87 Sum of 6 Chandra observations

0.8asec

D. Harris, et al.

Marshall et al. 2001ApJ...549L.167M

Outline1. Nearby Jets

2. Quasar/FRII Jets

• Spatially resolved analysis

• Broadband SED

• Interpretation as IC/CMB

• Kinetic flux and efficiency

3. Jets at Large Redshift

PKS 0208-512 PKS 0920-397

PKS 1030-357

PKS 1202-262

Outline1. Nearby Jets

2. Quasar/FRII Jets

3. Jets at Large Redshift• Beacons to Large Redshift?

• Radio quiet X-ray jets?

J0841

30" = 273 kpc

Schwartz et al., 2004ApJ...605L.105S

3" = 20kpc

GB 1508+5714

z=4.3

Siemiginowska et al., 2003ApJ...598L..15S

DE

CL

INA

TIO

N (

J200

0)

RIGHT ASCENSION (J2000)13 25 33 32 31 30 29 28

-43 00 15

30

45

01 00

15

Hardcastle et al., 2003ApJ...593..169H

Cen A

8.4 GHz0.4–7 keV

1 kpc

29

10 arcsec

C+G

B

AF

E

D

HST-1

CORE

Harris et al., 2003ApJ...586L..41H

M87 Jet

0.77 kpc

Core HST-1

10 arcsec

C+G

B

AF

E

D

HST-1

CORE

Harris et al., 2003ApJ...586L..41H

M87 Jet

0.77 kpc

Core HST-1

E

B C

D F

A

0 5 100

200

400

600

1 10

Multiwavelength observations of FR II Jets

0723+679

1136-13.5

1150+497

1354+195

Sambruna et al. (2002ApJ...571..206S; astro-ph/0401475)

PKS 0208-512

PKS 2101-490

PKS 0920-397

PKS 1030-357PKS 1202-262

3C 273

Schwartz et al. (2000ApJ...540L..69S,2003agnc.conf..359S)

Marshall et al.(2001ApJ...549L.167M)

2 4 6 8 10

50

100

150

200

K 2

PKS 0208-512

Quasar

5" = 43 kpc

K 1

K 3

0.5 to 7 keV

0.492′′pixels

1.23′′↔ 95%

z=0.999

PKS 0920-397

K 2

K 1

Quasar

10" = 72 kpc

H0=65Ωm =0.3ΩΛ =0.7

z=0.591

12" = 109 kpc

Quasar

PKS 1030-357

K 3

K 1

K 2

z=1.455

Knot 1

5" = 40.3 kpc

Knot 2

PKS 1202-262

Quasar

z=0.789

0.5-7 keV X-rays

z=0.653PKS 0637-752

K4K3

8.6 GHz

11"=76 kpc

K2K1

Spectral Energy Distribution often indicates against Synchrotron X-rays

Spectral Energy Distribution often indicates against Synchrotron X-rays

Sambruna et al., 2002ApJ...571..206S

Spectral Energy Distribution often indicates against Synchrotron X-rays

Sambruna et al., 2002ApJ...571..206S

Inverse Compton X-rays from the CMB:

γx ≈102−3

γr ≈104−5

Some jets may be de-tectable by GLAST,at 10−13 to 10−12 ergscm−2 s−1

1 10 100 10000.1

1

10

100

1 10 100 10000.1

1

10

100

1 10 100 10000.1

1

10

100

The intersection gives a solution

for the magnetic field, B, in the

rest frame, and for the apparent

Doppler factor,

δ = (Γ(1− β cos(θ))−1.

Uncertainties in the Magnetic Field Estimates

Uncertainties in the Magnetic Field Estimates

Equipartition

Uncertainties in the Magnetic Field Estimates

Equipartition Inverse Compton

1 10 100 10000.1

1

10

100

• Determined B and δ

within a factor of 2

• Kinetic flux is ∝ (Bδ)2,

for equipartition

5 10 15 20 25 30

5

10

15

20

5 10 15 20 25 30

5

10

15

20

Kinetic Flux

• K =Γ2π r 2β c U

• U is total internal energy

density, UB+Ue+Up

• For equipartition,

U= B2

8π(2 + k)

• NOTE: K constant ⇒(B Γ)2 = constant

5 10 15 20 25 30

5

10

15

20

Kinetic Flux

• K =Γ2π r 2β c U

• U is total internal energy

density, UB+Ue+Up

• For equipartition,

U= B2

8π(2 + k)

• NOTE: K constant ⇒(B Γ)2 = constant

• We takeΓ ≈ δδ = (Γ(1− β cos(θ)))−1

• cos(θmax) = δ−1/δ√(δ2−1)

100 10000.1

1

10

Kinetic Flux

From K = Γ2π r 2β c U,

K ∝ δ2θ2r (3 B2/(8 π))

Kinetic Flux

From K = Γ2π r 2β c U,

K ∝ δ2θ2r (3 B2/(8 π))

Kinetic flux is a signif-

icant, even dominant,

portion of the accretion

energy budget.

Implications of the FR II Jets

• Eddington Luminosity might not limitAccretion Rate

• Jets may Power Cluster Cavities – StopCooling Flows

• IC/CMB X-ray jets Maintain ConstantSurface Brightness vs. z. We will detectthem at Arbitrarily Large Redshift.

PERSEUS AFabian et al. (2000MNRAS.318L..65F)

3h19m40s3h19m50s3h20m00s

41:29:00

41:30:00

41:31:00

41:32:00

41:33:00

RA

Dec

50′′=18.4 kpc

1.4 GHz VLA

PERSEUS AFabian et al. (2000MNRAS.318L..65F)

3h19m40s3h19m50s3h20m00s

41:29:00

41:30:00

41:31:00

41:32:00

41:33:00

RA

Dec

50′′=18.4 kpc

1.4 GHz VLA

Hot cluster Gas

Cavities

Cooler Gas!

PERSEUS AFabian et al. (2000MNRAS.318L..65F)

3h19m40s3h19m50s3h20m00s

41:29:00

41:30:00

41:31:00

41:32:00

41:33:00

RA

Dec

50′′=18.4 kpc

1.4 GHz VLA

Hot cluster Gas

Cavities

Cooler Gas!

Fossil Cavities

Fabian et al., (2002MNRAS.331..369F)74 MHz

PERSEUS AFabian et al. (2000MNRAS.318L..65F)

3h19m40s3h19m50s3h20m00s

41:29:00

41:30:00

41:31:00

41:32:00

41:33:00

RA

Dec

50′′=18.4 kpc

1.4 GHz VLA

Hot cluster Gas

Cavities

Cooler Gas!

Fossil Cavities

Fabian et al., (2002MNRAS.331..369F)74 MHz

p ∆V ≈ 2× 1058 ergsume ∆V ≈ 4× 1056 ergsPressure equality⇒ k/f≥180Lifetimes⇒ B≤ Bme/4

Do Sound Waves Provide the Energy?

3h19m30s3h19m40s3h19m50s3h20m00s

41:28

41:30

41:32

41:34

RA

DEC

Fabian et al. 2003astro-ph/0306036

0.1 1 10

10

100

0.1 1 10

10

100

0.1 1 10

10

100

0.1 1 10

10

100

Where ARE the bright X-ray Jets at High Redshift?

• Unidentified ROSAT sources?

• Bright ROSAT, ASCA, EINSTEIN quasar identifications?

• Extreme X-ray/Optical sources (Koekemoer et al.

2004ApJ...600L.123K) in Chandra Deep Surveys?

Where ARE the bright X-ray Jets at High Redshift?

3" = 20kpc

GB 1508+5714

z=4.3

Siemiginowska et al. 2003ApJ...598L..15SCheung,2004ApJ...600L..23C

There Should Be Radio Quiet X-Ray Jets!

• 1 keV X-rays produced byγ ≈ 1000/Γ

• ν = 4.2×10−6γ2 H[µG] ≈ 10 MHz

A Radio Quiet X-Ray Jet?

EMSS 0841+1314

30"

J0841

30" = 273 kpc

A Radio Quiet X-Ray Jet?

EMSS 0841+1314

30"

J0841

30" = 273 kpc

z=1.8661

DE

CL

INA

TIO

N (

J200

0)

RIGHT ASCENSION (J2000)08 41 29.0 28.5 28.0 27.5

13 11 20

15

10

05

00

10 55

A Radio Quiet X-Ray Jet?

EMSS 0841+1314

30"

J0841

30" = 273 kpc

z=1.8661

DE

CL

INA

TIO

N (

J200

0)

RIGHT ASCENSION (J2000)08 41 29.0 28.5 28.0 27.5

13 11 20

15

10

05

00

10 55

DE

CL

INA

TIO

N (

J200

0)

13 11 30

15

00

10 45 f8.6GHz ≤ 100µJy

Correlation of X-ray Jet and Radio Flux Densities

Significance of the X-ray Emission

1. X-rays typically radiate the most energy

2. Quasar/Black hole core X-ray emission may be dominated

by jets (in radio sources)

If emission is inverse Compton on CMB,

and emission region is in equipartition:

3. X-rays give the effective Doppler factor and rest frame B

4. X-ray jets will be detectable at arbitrarily large redshift