The X-Ray Universe. The X-Ray Universe
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1 The X-Ray Universe The X-Ray Universe Potsdam University Dr. Lidia Oskinova Sommersemester 2017 astro.physik.uni-potsdam.de ~lida/vorlesungxrayso17.html Chandra X-ray, HST optical, Spitzer IR NGC602 in the SMC d=60pc
2 Milky Way Center 01 National Geographic
3 Mass of the Black Hole 2.2 micron animation of the stellar orbits in the central parsec 02 Use Kepler s III Law to determine the mass of the BH: a 3 =M BH P 2 For this one needs to determine for many stars: a) the period P b) the size of the orbit s semimajor axis a Current best estimate M BH =7.2 millions M
4 Composite image of Galactic Center in near IR (HST) and X-ray (Chandra) 03 X-ray luminosity of Sgr A* is ~10 32 erg/s
5 Activity of our Black Hole 04 see flare at SINFONI VLT image
6 Fermi Bubbles: evidence of previous activity 05
7 Active Galactic Nuclei 06
8 Credit: X-ray: NASA/CXC/MIT/H.Marshall et al. Radio: F. Zhou, F.Owen (NRAO), J.Biretta (STScI) Opt 07
9 08 The nearest active galaxy: Centaurus A 08
10 09 AGNs are scaled up XRBs 09 L X =η GMṀ R X-ray luminosity of QSO is 10 orders of magnitude higher than XRB Eddington luminosity L Edd M M erg/s. The mass of central object should be orders of magnitude higher XRB: M BH ~10M AGN: M BH ~ M
11 10 Observed properties of AGN 10 High luminosity L bol = ; Size << 1pc; Variabilty; Emission & Absorption lines see Dan Schwartz heasarc.gsfc.nasa.gov/docs/xrayschool/
12 11 AGN is common name for: 11 Quasars (quasi-stars) QSOs (quasi-stellar objects) QSRSs (quasi-stellar radio sources) BL Lac objects Blazars (BL Lac type quasars) OVV (Optically Violent Variables) Seyfert Galaxies (which may be Type 1, Type 2, Type 1.x, Narrow line type 1) Narrow Emission Line galaxies LINER s (Low ionization nuclear emission region) LLAGN (Low Luminosity AGN)
13 12 Famous sketch (unification model) 12 AGN with 10 8 M BH R G 3x10 13 cm Accretion disk cm BLR cm Torus cm?? NLR cm Jets cm Urry & Padovani 1995 PASP 107, 803
14 13 X-ray observations 13 Time Variability Size of emitting region, and regions where radiation is reprocessed. QPOs relativisitc effects X-ray Spectra: Absorption: amount of absorbing material; velocity field (inflow/outflow); cold/warm absorbers; ionization state Thermal emission: from hot gas, accretion physics Non-thermal emission: synchrotron, Comptonisation, relativisitc effects, acceleration, magnetic fields Emission lines: relativistic effects X-ray Images: Nucleus Extended emission on scale of 1 pc to 100 kpc Jets and radiolobes Correlstion between different components.
15 14 Schematic X-ray spectrum of AGN From W.N.Brandt "X-raying Active Galaxies" AAS
16 15 A Structure for Quasars 15 Elvis ApJ 545,63
17 16 Examples of obsevred AGN X-ray spectra 16 From W.N.Brandt "X-raying Active Galaxies" AAS 04
18 17 The speed of matter within the jets is large fraction of c. SR s effects must be taken into accout: relativistic beaming, relativistic Doppler effect, superluminal motion The inner parts of the discs are close to the BH. GR effects must be taken into account: gravitational red-shift. The emitted radiation interacts with the discs and the surrounding matter Wikipedia
19 18 Relativisitc broadening Fe-line 18 Fabian et al PASP 112, 1145
20 19
21 20 Time average (ASCA) observations of AGN MGC / average 1997 / average Lightcurve minimum Flare Fabian et al PASP 112, 1145
22 21 Cosmic X-ray background and AGN 21 Black holes in centra of galaxies M= powered by accretion. 600 obscured and 700 unobscured AGN agree with standard scheme X-ray surveys deep or wide many ongoing automatic selection
23 22 XMM spectra of the X-ray background with a relativistic iron line 22
24 23 RASS 23
25 Spectrum of Cosmic X-ray Background 24 Sazonov etal. 2008, arxiv
26 25
27 26 Summary 26 SMBH in center of galaxies are scaled up stellar mass BH AGN luminous accros the EM spectrum Responsible for CXB Unification model seems to explain obsevraitions X-rays spectra: contribution from a varaiety of processes Absorption complex geometry Emission accretion, reprocessing Relativisitc line broadening Imaging: multiwavelength approach
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