A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151
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1 A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 411 T. Beuchert, A.G. Markowitz, T. Dauser, J.A. García, M.L. Keck, J. Wilms, M. Kadler, L.W. Brenneman, & A.A. Zdziarski 17 June 8 X-ray Universe 17, Roma
2 NGC Source Properties Well-studied nearby Seyfert 1. Brightest radio-quiet Seyfert < kev Non-variable soft emission from extended, photo-/collisionally ionized environment (e.g., Ogle et al., 00; Yang et al., 01; Schurch et al., 04; Wang et al., 11a,b,c) Strongly variable hard X-ray spectrum (e.g., Caballero-Garcia et al., 12) Strongly variable neutral absorbers (days to years) (e.g., Holt et al., 1980; Yaqoob et al., 1989; Yaqoob et al., 1991; Schurch et al., 02; Puccetti et al., 07; de Rosa et al., 07; Wang et al., ) Seyfert 1 properties: variability, broad Fe K α line (e.g., Yaqoob et al., 199; Zdziarski et al., 02; Keck et al., 1) Tobias Beuchert X-ray Universe 17
3 NGC Source Properties Well-studied nearby Seyfert 1. Brightest radio-quiet Seyfert < kev Non-variable soft emission from extended, photo-/collisionally ionized environment (e.g., Ogle et al., 00; Yang et al., 01; Schurch et al., 04; Wang et al., 11a,b,c) Strongly variable hard X-ray spectrum (e.g., Caballero-Garcia et al., 12) Strongly variable neutral absorbers (days to years) (e.g., Holt et al., 1980; Yaqoob et al., 1989; Yaqoob et al., 1991; Schurch et al., 02; Puccetti et al., 07; de Rosa et al., 07; Wang et al., ) Seyfert 1 properties: variability, broad Fe K α line (e.g., Yaqoob et al., 199; Zdziarski et al., 02; Keck et al., 1) Our aim: symbiosis of strong gravity and variable absorption in NGC 411 (compare width NGC 136: Risaliti et al. 09a, 13; Brenneman et al. 13; Walton et al. 14) Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
4 Inner-Disk Reflection xillver relconv Dauser et al. () García et al. (14)?? Keck et al. (1) ε r Tobias Beuchert X-ray Universe 17
5 Inner-Disk Reflection relxilllp_cp Dauser et al. (13) García et al. (14)!!! Keck et al. (1) Observed emissivity profiles self-consistently explained in lamp-post geometry see also: Svoboda et al. (12) and refs. therein poster J by Marco Fink et al. talk by T. Dauser at 18:1 Tobias Beuchert X-ray Universe 17
6 Establishing a Baseline Model Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
7 Establishing a Baseline Model Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
8 Establishing a Baseline Model Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
9 Establishing a Baseline Model Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
10 Establishing a Baseline Model Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
11 Establishing a Baseline Model Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17
12 Establishing a Baseline Model Self-consistent lamp-post solution works well Require two point-sources with a maximal height of 1.0 r g Strong arguments for vertically extended corona! consistent with reverberation lags: Cackett et al., 14 Tobias Beuchert X-ray Universe 17
13 Beuchert et al., 17 (arxiv: ) Time-Resolved Spectroscopy XMM-Newton Suzaku NuSTAR 11.4 Tobias Beuchert X-ray Universe Time [years]
14 Beuchert et al., 17 (arxiv: ) Time-Resolved Spectroscopy Blurred Fe K α feature visible in nearly all observations Apply baseline model to all spectra Major free parameters: NH,1, NH,1, incident flux Tobias Beuchert X-ray Universe 17
15 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks MJD 60
16 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks MJD 60
17 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks MJD 60
18 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks MJD 60
19 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks MJD 60
20 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks XMM 6 ks MJD 60
21 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks XMM 6 ks XMM 9 ks MJD 60
22 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks XMM 6 ks XMM 9 ks Suzaku+ NuSTAR 10 ks MJD 60
23 Time-Resolved Spectroscopy Energy [kev] Beuchert et al., 17 (arxiv: ) Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks XMM 6 ks XMM 9 ks Suzaku+ NuSTAR 10 ks XMM 4 ks MJD 60
24 Time-Resolved Spectroscopy Energy [kev] Variability of... absorption (months years) incident flux Tobias Beuchert X-ray Universe 17 0 NH [ 22 cm 2 ] NH [ 22 cm 2 ] 3 Photons cm 2 s 1 kev XMM 2 ks XMM 6 ks XMM 7 ks XMM 6 ks XMM 9 ks Suzaku+ NuSTAR 10 ks XMM 4 ks XMM 7 ks MJD 60 Lack of strong variability for... soft emission
25 Constraining the Absorber Distance Assume Keplerian motion of distinct cloud Dynamical time-scale t : days to years distance R M BH nh 2 N 2 H t 2 for t = 2 days: R 6 4 to 6 2 pc Compare: R BLR 8 3 pc (Maoz et al., 1991) for t years: outer BLR or inner torus Tobias Beuchert X-ray Universe 17
![CA1 [ 22 cm 2 ] 3 30 2 1 Beuchert et al., 17 (arxiv:1703.86) Is the absorbing structure... 3 30 2 1 CA2 [ 22 cm 2 ] clumpy/filamentary? radiatively driven?](/docs-images/92/108137218/images/26-2.jpg "changing its ionization state with changing irradiation? see also: Couto et al.")
26 CA1 [ 22 cm 2 ] Beuchert et al., 17 (arxiv: ) Is the absorbing structure CA2 [ 22 cm 2 ] clumpy/filamentary? radiatively driven? changing its ionization state with changing irradiation? see also: Couto et al., Flux HXCOMP 7 kev [erg cm 2 s 1 ] Tobias Beuchert X-ray Universe 17
27 see also, e.g., Markowitz et al., 14; Miniutti et al., 14; Beuchert et al., 1; Svoboda et al., 1; Sanfrutos et al., 16 Tobias Beuchert X-ray Universe 17
28 Conclusions Disentangled complex absorbers from relativistically blurred reflection Self-consistent double-lamp-post solution Strong arguments for a coherent and vertically extended X-ray source Absorption variability on timescales from days to years Dynamic BLR or radiatively driven structures Tobias Beuchert X-ray Universe 17
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