Multi-Time Scale Spectral Monitoring of Seyferts with RXTE...N4051 N3516 N3227 N4151 CenA N4258 FormostX-ray-bright,nearby Seyferts: Power-lawsoftensas ﬂuxincreases(e.g.,Papadakis

RXTE Database Absorption Fe Kα Lines Corona Jets End

Multi-Time Scale Spectral MonitoringMulti-Time Scale Spectral Monitoringof Seyferts with RXTEof Seyferts with RXTE

Alex MarkowitzAlex MarkowitzUC San Diego, Center for Astrophysics & Space SciencesUC San Diego, Center for Astrophysics & Space Sciences

Karl Remeis Observatory, Bamberg, & ECAPKarl Remeis Observatory, Bamberg, & ECAP

Karl Remeis Sternwarte


RXTE’s Legacy: The AGN Variability Database1996 2000 2004 2008

0

5

10NGC 4051

F2

−1

0

0

5

10NGC 3516

F2

−1

0

0

5

10 NGC 3227

F2

−1

0

0

2

4Mkn 79

F2

−1

0

1996 2000 2004 2008

10

20

30 3C 273

Time

F2

−1

0

Sy1 Sy2 Blzr# Visited 57 47 51# Monitored 39 15 45Tot. Mon. (obj · yr) 152.5 39.6 68.6

• Average flux & typicalflux range for each object

Time scales of months–years are interesting for AGN!


RXTE’s Legacy: The AGN Spectral Variability Database1996 2000 2004 2008

0

5

10 NGC 4051

F2−

10

0

5

10 NGC 3516

F2−

10

0

5

10 NGC 3227

F2−

10

0

2

4Mkn 79

F2−

10

1996 2000 2004 2008

10

20

30 3C 273

Time

F2−

10

2.5

2.1

1.7

1.3

0.9

0.5

Γsimple

• Long-term avg. spectralproperties (Rivers et al.2011a; SEE POSTER!)



RXTE’s Legacy: The AGN Spectral Variability Database1996 2000 2004 2008

0

5

10 NGC 4051

F2−

10

0

5

10 NGC 3516

F2−

10

0

5

10 NGC 3227

F2−

10

0

2

4Mkn 79

F2−

10

1996 2000 2004 2008

10

20

30 3C 273

Time

F2−

10

2.5

2.1

1.7

1.3

0.9

0.5

Γsimple

• Long-term avg. spectralproperties (Rivers et al.2011a; SEE POSTER!)

• Monitoring → Γ(t),IFeKα(t), NH(t)



Variability in Line of Sight Absorbers

• Variations in X-ray absorbing columns in both Sy 1s & 2s, on timescales of hours–years (Risaliti+ 2002, Puccetti+ 2007, Turner+ 2008)

20

40

60

F(2

−1

0)

2010 2010.4 2010.8 2011.20.5

1

1.5

F(2

−4

)F

(7−

10

)

2010 2010.4 2010.8 2011.21.6

1.8

2

Γ

15

20

25

30

NH

Lamer+ ’03: NGC 3227:3-month eclipse, 2000–1

∆NH = 3× 1023 cm−2

R ∼ 10− 100 lt.-daysBLR cloud likely

Rivers+ ’11b: Cen A6-month eclipse, 2010–1

∆NH = 8× 1022 cm−2

R ∼ 0.1− 0.3 pcTorus cloud likely

NH monitoring with RXTE: complementary to short-term results


Absorption Variability in Cen A: From weeks to a decade

1998 2001 2004 2007 2010

15

20

25

30

NH (

/10

22 c

m−

2)

10 100 10000

5

10

15

Cen A

∆T(days)

∆N

H (

/10

23 c

m−

2)

2010−2011 Monitoring

13 Campaigns (1996−2009)+ Monitoring

(monitoring of Cen A on even longer timescales would be ideal....)

ALSO: NGC 6300 changed from C-thick to C-thin over 2.5 years(Leighly et al. 1999, 2000 & Guainazzi et al. 2002)


RXTE Spectral Monitoring of NGC 4151, 1996–2004

10

20

30

F2−

10

(/10

−10 e

rg c

m−

2 s

−1)

1996 1997 1998 1999 2000 2001 2002 2003 2004

1

2

3

4

Year

F7−

10/F

2−

4

NGC 4151: Complex, absorbed X-ray spectrum (e.g., full-covering+ partial-coverer):

Can variations in absorption explain the observed trends inHardness Ratio?


RXTE Spectral Monitoring of NGC 4151, 1996–2004

10

20

30

Full−Coverer (constant) + Partial Coverer (variable)

F2−10

(Absd)

1

1.5

2

2.5

3

3.5

1

1.5

2

2.5

3

3.5

/

0.2

0.4

0.6

0.8Covering

Fraction

1996 1998 2000 2002 2004

20

40NH

(/1022 cm−2)

Year

Markowitz et al., in prep.: Yes: Changes in covering fraction ofpartial coverer drive Hardness Ratio trends (consistent with DeRosa

et al. 2007, 5 BeppoSAX observations)


Clumpy torus models

(Urry & Padovani 1995)

→

e.g., Nenvoka et al. 2002, 2008;Elitzur & Schlossmann 2006


Reverberation Mapping with the Fe Kα Line

NGC 3227 (Markowitz et al. 2009)

3C 111 (Chatterjee et al. 2011)

50%/80% of lineflux responds tocontinuumvariations; variableportion of lineoriginates in gas< 700/< 60 light-daysfrom central engine

(Related: see also: Markowitz, Edelson & Vaughan 2003; Vaughan & Edelson 2001; Nandra et al. 2000)


Coronal Power Law Component

Nandra et al. (2000), 32-dayRXTE+IUE campaign onNGC 7469:•ΓX & FUV correlated• Consistent with Comptonizationin a corona• But also supports thermalreprocessing of SX/EUV photonsinto UV continuum photons

(Related: see also: Chiang et al. 2000, RXTE+ASCA+EUVE campaign on NGC 5548)


Coronal Power Law Component: Links to accretion inGBHs?

2.5 2 1.5

10−4

10−3

0.01

0.1

1

ΓX

LB

ol/L

Edd

Ark564

PKS0558

Mkn766

Mkn335

3C

120

PG0804

Mkn79

3C390.3

N5

54

8

3C111

N4051

N3516

N3227

N4151

CenA

N4258

• For most X-ray-bright, nearbySeyferts: Power-law softens asflux increases (e.g., Papadakiset al. 2002)• FUTURE: Need to accessmore LLAGN/ lower-ṁ sources(which are more slowly variable)


Constraints on Blazar Jet Emission Models

(Abdo et al. 2011) (Giebels et al. 2007) (Grube 2007)

• RXTE’s flexible scheduling → participation in many ToOcampaigns on flaring blazars

• RXTE spectral monitoring → better model SED(t) → constrainmodels of particle acceleration, jet emission


Summary

• RXTE has been the only mission to provide sustained X-ray• RXTE has been the only mission to provide sustained X-raycontinuum & spectral monitoring, covering timescales fromcontinuum & spectral monitoring, covering timescales fromhours to &a decade.hours to &a decade.• (multi-band light curves usually not sufficient!)• (multi-band light curves usually not sufficient!)• Variability of Fe Kα line, absorption, coronal power-law• Variability of Fe Kα line, absorption, coronal power-lawcomponent, Compton reflectioncomponent, Compton reflection• Constraints on geometry of circumnuclear (absorbing,• Constraints on geometry of circumnuclear (absorbing,line-emitting) gasline-emitting) gas• Pathfinder investigations for eROSITA (launch 2013; 0.2–10 keV)• Pathfinder investigations for eROSITA (launch 2013; 0.2–10 keV)and brightest AGN accessible to MIRAX-HXI (launch ∼2016,and brightest AGN accessible to MIRAX-HXI (launch ∼2016,hopefully; ∼5–200 keV). (& maybe LOFT?)hopefully; ∼5–200 keV). (& maybe LOFT?)


References & Back-up Slides

Abdo, A., et al. (Fermi LAT collaboration), 2011,ApJ, 736, 131Chatterjee, R., Marscher, A.P., Jorstad, S.G., etal., 2011, ApJ, 734, 43Chiang, J., Reynolds, C.S., Blaes, O., et al., 2000,ApJ, 528, 292de Rosa, A., Piro, L., Perola, G.C., et al., 2007,A&A, 463, 903Elitzur, M. & Shlosman, I. 2006, ApJ, 648, L101Giebels, B., et al 2007, A&A, 462, 29Grube, J., 2007, PhD thesisGuainazzi, M., 2002, MNRAS, 329, L13Lamer, G., Uttley, P. & McHardy, I.M. 2003,MNRAS, 342, L41Leighly, K.M., et al., 1999, ApJ, 522, 209Leighly, K.M., et al., 2000, Rossi2000 conferenceMarkowitz, A., Edelson, R. & Vaughan, S. 2003,ApJ, 598, 935Markowitz, A., Reeves, J.N., George, I.M., et al.2009, ApJ, 691, 922Nandra, K., Le, T., George, I.M., et al., 2000,

ApJ, 544, 734Nenkova, M., Ivezić, Z. & Elitzur, M. 2002, ApJ,570, L9Nenkova, M., Sirocky, M.M., Nikutta, R., et al.2008, ApJ, 685, 160Papadakis, I.E., et al., 2002, ApJ, 573, 92Puccetti, S., Fiore, F., Risaliti, G., et al. 2007,MNRAS, 377, 607Risaliti, G., Elvis, M., & Nicastro, F. 2002 ApJ,571, 234Rivers, E., Markowitz, A., Rothschild, R.E.,2011a, ApJS, 193, 3Rivers, E., Markowitz, A., Rothschild, R.E.,2011b, ApJ, 742, L29Turner, T.J., Reeves, J.N., Kraemer, S.B. &Miller, L. 2008, A&A, 483, 161Urry, C.M. & Padovani, P. 1995, PASP, 107, 803Vaughan, S. & Edelson, R. 2001, ApJ, 548, 694Zdziarski, A.A., et al., 1999, MNRAS, 30, L11Zdziarski, A.A., et al., 2003, MNRAS, 342, 355


R − Γ CorrelationGlobal correlations and correlation within individual objects:

2.42.221.81.61.4

-0.5

-1

-1.5

-2

-2.5

Γ

R

Zdziarksi et al. (2003) Rivers et al. (2011) Markowitz et al., in prep.

PCA+HEXTE NGC 4151; PCA

•Other examples: Chiang et al. (2000); Zdziarski et al. (1999, Ginga)•CAUTIONS: See Vaughan & Edelson (2001) and Nandra et al.(2000), and run those Monte Carlo sims!

RXTE DatabaseAbsorptionFe K LinesCoronaJetsEnd

Documents

Multi-Time Scale Spectral Monitoring of Seyferts with RXTE...N4051 N3516 N3227 N4151 CenA N4258 FormostX-ray-bright,nearby Seyferts: Power-lawsoftensas ﬂuxincreases(e.g.,Papadakis