High-energy monitoring of Seyfert galaxies: the case of NGC 5548 - - PowerPoint PPT Presentation

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High-energy monitoring of Seyfert galaxies: the case of NGC 5548 - - PowerPoint PPT Presentation

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High-energy monitoring of Seyfert galaxies: the case of NGC 5548 and NGC 4593 Francesco Ursini Univ. Grenoble - Alpes, IPAG Universit Roma T re The Extremes of Black Hole Accretion Madrid, June 8 2015 NGC 5548 Object of a

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SLIDE 1

High-energy monitoring

  • f Seyfert galaxies: the case of

NGC 5548 and NGC 4593

Francesco Ursini

  • Univ. Grenoble-Alpes, IPAG

Università Roma T re The Extremes of Black Hole Accretion Madrid, June 8 2015

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SLIDE 2

NGC 5548

The logs of the simultaneous XMM-Newton, NuSTAR and/or INTEGRAL ob- servations of NGC 5548 during our campaign. Obs. Satellites

  • Obs. Id.

Start time (UTC) Net exp. yyyy-mm-dd (ks) 1 XMM-Newton 0720110401 2013-06-30 38 INTEGRAL 10700010001 2013-06-29 62 2 XMM-Newton 0720110601 2013-07-11 37 NuSTAR 60002044002/3 2013-07-11 50 INTEGRAL 10700010002 2013-07-11 50 3 XMM-Newton 0720110701 2013-07-15 37 INTEGRAL 10700010003 2013-07-15 50 4 XMM-Newton 0720111101 2013-07-23 38 NuSTAR 60002044005 2013-07-23 50 INTEGRAL 10700010004 2013-07-23 52 5 Chandra 16314 2013-09-10 120 NuSTAR 60002044006 2013-09-10 50 6 XMM-Newton 0720111501 2013-12-20 38 NuSTAR 60002044008 2013-12-20 50 7 XMM-Newton 0720111601 2014-02-04 38 INTEGRAL 11200110001 2014-01-17 94 11200110002 2014-01-22 40 11200110003 2014-02-09 30

Object of a multiwavelength campaign in 2013 The nucleus appeared

  • bscured by a clumpy

stream of ionized gas - a disc wind? (Kaastra+15; see talk by M. Cappi) 7 high-energy observations with XMM, NuSTAR and INTEGRAL (Ursini+15)

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SLIDE 3

NGC 5548: high-energy view

10−4 10−3 0.01 0.1 1 Counts s−1 keV−1

  • Obs. 2: Broad−band fit, residuals and best−fit model.

XMM−Newton/pn NuSTAR/FPMA NuSTAR/FPMB INTEGRAL

−10 −5 5 2 1 10 100 10−6 10−5 10−4 10−3 0.01 keV2 Ph/(cm2 s keV) Energy (keV)

good constraints

  • n both

the primary power law and the reflection component

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SLIDE 4

1.5 2 2.5 100 1000 PEXMON Cut−off energy (keV) PEXMON Photon Index 1.5 2 2.5 100 1000 1.5 2 2.5 100 1000 1.5 2 2.5 100 1000 5 2 6 4 Te 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 PEXMON Norm. PEXMON Photon Index 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 5 2 4 6

reflection component

PEXMON Photon index PEXMON Norm. PEXMON Photon index PEXMON Ec (keV)

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SLIDE 5

1.5 2 2.5 100 1000 PEXMON Cut−off energy (keV) PEXMON Photon Index 1.5 2 2.5 100 1000 1.5 2 2.5 100 1000 1.5 2 2.5 100 1000 5 2 6 4 Te 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 PEXMON Norm. PEXMON Photon Index 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 5 2 4 6

reflection component

PEXMON Photon index PEXMON Norm. PEXMON Photon index PEXMON Ec (keV)

1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1 2 3 4 5 6 7

Cut−off Energy (keV) Photon Index

Photon index Cut-off energy (keV)

primary power law

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SLIDE 6

1.5 2 2.5 100 1000 PEXMON Cut−off energy (keV) PEXMON Photon Index 1.5 2 2.5 100 1000 1.5 2 2.5 100 1000 1.5 2 2.5 100 1000 5 2 6 4 Te 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 PEXMON Norm. PEXMON Photon Index 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 1.4 1.6 1.8 2 2.2 5×10−3 0.01 0.015 5 2 4 6

reflection component

PEXMON Photon index PEXMON Norm. PEXMON Photon index PEXMON Ec (keV)

1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1.5 1.6 1.7 100 200 300 400 500 1 2 3 4 5 6 7

Cut−off Energy (keV) Photon Index

Photon index Cut-off energy (keV)

+ +

kTe (keV)

+

100 200 300 400 0.4 0.6 0.8 1.0

2013 campaign 2007 Suzaku 1997 BeppoSAX Compton parameter y

primary power law

Temperature (keV) Compton parameter

y-kT of the hot corona

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SLIDE 7

NGC 4593: XMM/NuSTAR monitoring program

a strong reflection hump above 10 keV and a prominent, non- relativistic Fe Kα line (truncated disc? distant material?) a significant soft X-ray excess below 1 keV (Comptonization?) a lower limit for the high- energy cut-off of 150 keV Past observations by BeppoSAX (1998: Guainazzi+98), XMM (2002: Reynolds+04, Brenneman+07), Suzaku (2007: Markowitz&Reeves09) show:

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SLIDE 8

NGC 4593: XMM/NuSTAR monitoring program

a strong reflection hump above 10 keV and a prominent, non- relativistic Fe Kα line (truncated disc? distant material?) a significant soft X-ray excess below 1 keV (Comptonization?) a lower limit for the high- energy cut-off of 150 keV

The logs of the joint XMM-Newton and NuSTAR observations of NGC 4593. Obs. Satellites

  • Obs. Id.

Start time (UTC) Net exp. yyyy-mm-dd (ks) 1 XMM-Newton 0740920201 2014-12-29 16 NuSTAR 60001149002 22 2 XMM-Newton 0740920301 2014-12-31 17 NuSTAR 60001149004 22 3 XMM-Newton 0740920401 2015-01-02 17 NuSTAR 60001149006 21 4 XMM-Newton 0740920501 2015-01-04 15 NuSTAR 60001149008 23 5 XMM-Newton 0740920601 2015-01-06 21 NuSTAR 60001149010 21

Past observations by BeppoSAX (1998: Guainazzi+98), XMM (2002: Reynolds+04, Brenneman+07), Suzaku (2007: Markowitz&Reeves09) show:

5 × 20 ks joint observations in early 2015

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SLIDE 9

Significant flux variability Significant spectral variability in the soft band (0.5-10 keV) … not much in the hard band (3-50 keV)

2.5 5.0 7.5 10.0 12.5 Counts/s

XMM/pn and NuSTAR/FPMA+FPMB light curves and hardness ratios

XMM/pn 0.5−2 keV 2.0 3.0 4.0 Counts/s XMM/pn 2−10 keV 0.30 0.35 0.40 0.45 Hardness ratio XMM/pn 2−10 keV/0.5−2 keV 0.8 1.2 1.6 Counts/s NuSTAR 3−10 keV 0.30 0.45 0.60 0.75 Counts/s NuSTAR 10−50 keV 0.2 0.4 0.6 1×105 2×105 3×105 Hardness ratio Time (s) NuSTAR 10−50 keV/3−10 keV

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SLIDE 10

Each spectrum is fitted separately; we divide the first

  • bservation into

two intervals

2.5 5.0 7.5 10.0 12.5 Counts/s

XMM/pn and NuSTAR/FPMA+FPMB light curves and hardness ratios

XMM/pn 0.5−2 keV 2.0 3.0 4.0 Counts/s XMM/pn 2−10 keV 0.30 0.35 0.40 0.45 Hardness ratio XMM/pn 2−10 keV/0.5−2 keV 0.8 1.2 1.6 Counts/s NuSTAR 3−10 keV 0.30 0.45 0.60 0.75 Counts/s NuSTAR 10−50 keV 0.2 0.4 0.6 1×105 2×105 3×105 Hardness ratio Time (s) NuSTAR 10−50 keV/3−10 keV

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SLIDE 11

10−6 10−5 10−4 10−3 10−2 Counts s−1 keV−1 cm−2

XMM/pn and NuSTAR/FPMA data fitted with a power law

  • Obs. 1−I
  • Obs. 1−II
  • Obs. 2
  • Obs. 3
  • Obs. 4
  • Obs. 5

1.5 0.5 1.0 2.0 5 50 1 10 Data/model ratio Energy (keV) 1.5 0.5 1.0 2.0 5 50 1 10 Data/model ratio Energy (keV)

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SLIDE 12

Baseline model: warm abs.*(soft excess + cut-off power law + reflection)

bbody xillver

AFe free

10−5 10−4 10−3 0.01 Counts/(s keV cm2)

  • Obs. 2: Broad−band fit, residuals and best−fit model

XMM−Newton/pn NuSTAR/FPMA NuSTAR/FPMB

−5 5 2 1 10 10−4 10−3 0.01 keV2 Ph/(cm2 s keV) Energy (keV)

weak hump (R ~ 0.2-0.3)

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SLIDE 13

AFe ' 2-3

2.4×10−5 3.0×10−5 3.6×10−5 4.2×10−5 4.8×10−5 Fe K line flux

Fe K line flux and EW, primary flux (3−10 keV), photon index

2.4×10−5 3.0×10−5 3.6×10−5 4.2×10−5 4.8×10−5 Fe K line flux

Fe K line flux and EW, primary flux (3−10 keV), photon index

(A) 100 150 200 250 Fe K line EW 100 150 200 250 Fe K line EW (B) 1.2×10−11 1.5×10−11 1.8×10−11 2.1×10−11 F(3−10 keV) 1.2×10−11 1.5×10−11 1.8×10−11 2.1×10−11 F(3−10 keV) (C) 1.60 1.65 1.70 1.75 1.80 1.85 1−I 1−II 2 3 4 5

  • Observation number

1.60 1.65 1.70 1.75 1.80 1.85 1−I 1−II 2 3 4 5

  • Observation number

(D)

Line flux Line EW F(3-10 keV) Γ

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SLIDE 14

2.4×10−5 3.0×10−5 3.6×10−5 4.2×10−5 4.8×10−5 Fe K Flux

Anticorrelation between EW of the Fe K line and primary flux

2.4×10−5 3.0×10−5 3.6×10−5 4.2×10−5 4.8×10−5 Fe K Flux

Anticorrelation between EW of the Fe K line and primary flux

(A) 100 150 200 250 1.2×10−11 1.5×10−11 1.8×10−11 2.1×10−11 Fe K EW F(3−10 keV) 100 150 200 250 1.2×10−11 1.5×10−11 1.8×10−11 2.1×10−11 Fe K EW F(3−10 keV) (B)

p-value = 0.009 ρ = −0.92

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SLIDE 15

1.2×10−11 1.5×10−11 1.8×10−11 2.1×10−11 Flux(3−10 keV)

Correlation between soft excess and primary flux

1.2×10−11 1.5×10−11 1.8×10−11 2.1×10−11 Flux(3−10 keV)

Correlation between soft excess and primary flux

3.0×10−11 3.5×10−11 4.0×10−11 4.5×10−11 1.5×10−12 2.5×10−12 3.5×10−12 4.5×10−12 5.5×10−12 Flux(10−50 keV) Soft Excess Flux 3.0×10−11 3.5×10−11 4.0×10−11 4.5×10−11 1.5×10−12 2.5×10−12 3.5×10−12 4.5×10−12 5.5×10−12 Flux(10−50 keV) Soft Excess Flux

ρ = 0.97 ρ = 0.93 p-value = 0.001 p-value = 0.007

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SLIDE 16

Conclusions

NGC 5548 (see Kaastra+15; Mehdipour+15; Arav+15; Ursini+15; di Gesu+15) Distant reflector (~ light months) Evidence of variable photon index and high-energy cut-off Temperature and optical depth of the hot corona show long-term (~15 yrs) variability Next step: detailed test of Comptonization models NGC 4593 Strong spectral variability in the soft band on a time-scale of days Neutral Fe Kα line: flux ~ constant; equivalent width anticorrelated with primary flux accompanied by a weak reflection hump ⇒ two line components? Soft excess below 1 keV correlated with the primary emission Work in progress!