driving extreme variability: evolvingweb.stanford.edu/~wilkinsd/docs/talks/xmmconf2015.pdf · with...

Driving Extreme Variability: Evolving coronae & evidence for jet launching

Dan WilkinsCITA National Fellow, Saint Mary’s Universitywith Luigi Gallo, Kirsten Bonson, Andy Fabian, Dirk Grupe

XMM-Newton 2015 Science Workshop, ESAC, Madrid

1. Measuring the corona

2. Long timescale variability of Markarian 335

3. Short timescale variability in 2013

4. Flaring activity

Outline

3

10.5 2 510−4

10−3

2×10

−45×

10−4

2×10

−35×

10−3

keV

2 (Ph

oton

s cm

−2 s−

1 keV

−1)

Energy (keV)

The X-ray Spectrum

4

Reflection from Disc

Iron Kα Line

Power Law Continuum

Disc Thermal Continuum

Galactic Absorption

Measuring the Corona

5

Accretion Disc Emissivity

ε(r

) / A

rbit

rary

Un

its

1

1000

106

109

1012

r / rg

1 10 100

rc = 3rg

rc = 5rg

rc = 10rg

rc = 20rg

Wilkins & Fabian 2012, MNRAS 424, 1284-1296Fabian, Zoghbi, Wilkins et al 2012, MNRAS 419, 116-123


5


ε(r

) / A

rbit

rary

Un

its

1

1000

106

109

1012

r / rg

1 10 100

rc = 3rg

rc = 5rg

rc = 10rg

rc = 20rg

Reflection Fraction

Pho

ton

Fra

ctio

n

0

0.2

0.4

0.6

0.8

Source Height / rg

1 10 100

Hit disc (to be reflected)Escape (observed in continuum)



5


ε(r

) / A

rbit

rary

Un

its

1

1000

106

109

1012

r / rg

1 10 100

rc = 3rg

rc = 5rg

rc = 10rg

rc = 20rg

Reflection Fraction

Pho

ton

Fra

ctio

n

0

0.2

0.4

0.6

0.8

Source Height / rg

1 10 100

Hit disc (to be reflected)Escape (observed in continuum)


Also X-ray reverberation (Wilkins+13, Cackett+14 & Ed Cackett’s talk)

Markarian 335 – A Variable Source!

6

Grupe et al 2007, 2012

Long Timescale Variability

7

Wilkins & Gallo 2015, MNRAS 449, 129-146

1 2 510−4

10−3

0.01

keV2 (

Photo

ns cm

−2 s−1

keV−1

)

Energy (keV)

+ XMM-Newton High (2006)+ Suzaku High (2006)+ XMM-Newton Low (2007)+ XMM-Newton Int. (2009)++ Suzaku Low (2013)


7


q = 3

Fitting 3-5keVFitting 3-10keV

ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

1

r / rg

1 10 100

XMM High

1 2 510−4

10−3

0.01

keV2 (

Photo

ns cm

−2 s−1

keV−1

)

Energy (keV)



7


q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

1

r / rg

1 10 100

XMM High

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

XMM Intermediate

1 2 510−4

10−3

0.01

keV2 (

Photo

ns cm

−2 s−1

keV−1

)

Energy (keV)



7


q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

1

r / rg

1 10 100

XMM High

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

XMM Intermediate

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

Suzaku Low

1 2 510−4

10−3

0.01

keV2 (

Photo

ns cm

−2 s−1

keV−1

)

Energy (keV)



7


q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

1

r / rg

1 10 100

XMM High

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

XMM Intermediate

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

Suzaku Low

q = 2


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

Suzaku High

1 2 510−4

10−3

0.01

keV2 (

Photo

ns cm

−2 s−1

keV−1

)

Energy (keV)



8

1 2 510−4

10−3

0.01

keV2 (

Photo

ns cm

−2 s−1

keV−1

)

Energy (keV)


XMM High

Suzaku Low Suzaku High

rb = 26+10–7 rg rb < 12 rg

XMM Intermediate


R = 1.3+ 0.5– 0.2

𝚪 = 2.52 + 0.01– 0.01

R = 1.8 + 0.4– 0.3

𝚪 = 1.90 + 0.02– 0.02

rb < 5 rgR = 6 + 4

– 3

𝚪 = 1.91 + 0.04– 0.07

R = 0.26 + 0.04– 0.02

𝚪 = 2.16 + 0.02– 0.01

1H0707-495

9

Emissivity Break Radius Continuum Spectrum

Wilkins et al. 2014, MNRAS 443, 2746-2756

0 1 2 3 4 5 6x 105

0

0.05

0.1

0.15

0.2

0.25

0.3

0.35

Time / s

Coun

t Rate

/ ct s

−1

0 1 2 3 4 5 6x 105

1.6

1.7

1.8

1.9

2

2.1

Time / s

Γ

0 1 2 3 4 5 6x 105

05

10152025303540

Time / s

Refle

ction

Frac

tion

A Flare from Markarian 335

10


0 1 2 3 4 5 6x 105

0

0.05

0.1

0.15

0.2

0.25

0.3

0.35

Time / s

Coun

t Rate

/ ct s

−1

0 1 2 3 4 5 6x 105

1.6

1.7

1.8

1.9

2

2.1

Time / s

Γ

0 1 2 3 4 5 6x 105

05

10152025303540

Time / s

Refle

ction

Frac

tion

A Flare from Markarian 335

10

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100

q = 3


ε(r

) / A

rbit

rary

Un

its

10−12

10−9

10−6

10−3

r / rg

1 10 100


Cause of the Flare?

11

01

2

12

3

0 0.05 0.1 0.15

12

3

0 0.05 0.1 0.15 0.2 0.25

00.5

11.5

counts s-1

Har

dnes

s Rat

io

0.7-0.9 keV; 7-10 keV 0.7-0.9 keV; 2-3 keV

2-3 keV; 7-10 keV0.7-0.9 keV; 5-6 keV

Gallo, Wilkins et al. 2015, MNRAS 446, 633-650Wilkins & Gallo 2015, MNRAS 449, 129-146McKinney at al. 2012, MNRAS 423, 3083-3117

12

3F Γ

(10-1

2 erg

cm

-2 s-1

)

1 1.5 2 2.5Reflected flux (10-11 erg cm-2 s-1)

0.1

110

ξ (e

rg c

m s-1

)

A Bigger Flare…

12

Wilkins et al 2015, MNRAS submitted

What caused this flare?

13

10−4

10−3

0.01

0.1

1

norm

alize

d cou

nts s−1

keV−1

1 100.5

1

1.5

2

ratio

Energy (keV)

+ Swift XRT+ NuSTAR FPMA+ NuSTAR FPMB

500.3

Continuum 𝚪 2.43

Disc rin 1.235+0.16

Ref. Frac. 0.41

+ 0.05– 0.09

+ 0.15– 0.15

What caused this flare?

14

10−4

10−3

0.01

0.1

1

norm

alize

d cou

nts s−1

keV−1

1 100.5

1

1.5

2

ratio

Energy (keV)

+ Swift XRT+ NuSTAR FPMA+ NuSTAR FPMB

500.3

Continuum 𝚪 2.43

Disc rin 1.235+0.16

Ref. Frac. 0.41

+ 0.05– 0.09

+ 0.15– 0.15

• Relativistic X-ray reflection lets us measure the geometry and energetics of the corona

• Corona expands and cools as luminosity increases

• Long timescales — radial expansion, short timescale flares — vertical collimation?

• Short timescale variability during low flux epochs can be complex: X-ray flares, corona reconfiguration and evidence for aborted jet, potentially revealing the physics of the corona

Conclusions

15

E-mail: [email protected]

mailto:[email protected]

driving extreme variability: evolvingweb.stanford.edu/~wilkinsd/docs/talks/xmmconf2015.pdf · with...

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