The Black Hole at the Center of Our Galaxy. Pu, Hung-Yi 2009 Nov. NTHU

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1 The Black Hole at the Center of Our Galaxy Pu, Hung-Yi 2009 Nov. NTHU

2 Outline The radio source Sgr A* seems to be a SMBH in our galactic center The Sgr West and Sgr East Multiband observation for the Sgr A*/Galactic center Image Spectrum Can ADAF (Advection Dominated Accretion Flow) explains the under-luminous SMBH in our galaxy? Gamma-ray form galactic center

3 The radio source Sagittarius A*, which is the best physical marker of the true galactic center 1992~2002 data 1995~2010 from MPE infrared group

4

5 Coordinates (l,b)=(0,0) RA=17h 45m s Dec= Sagittarius A* is located at (l,b)=( ) RA=17h 45m 40.04s Dec= Dec b=0 degree RA

6 the distance of the Galactic Center ~ 8Kpc pc 1 3 pc 1 degree 180 pc

7 Chandra ACIS image Credit: NASA/G.Garmire (PSU)/F.Baganoff (MIT) VLA 6 and 20 cm image Image courtesy of NRAO/AUI

8 Credit: NASA/G.Garmire (PSU)/F.Baganoff (MIT)/Yusef-Zadeh (NWU)

9 (Credit: NASA/Penn State/G.Garmire et al.) Credit: NASA/CXC/MIT/F.K. Baganoff et al

10 Radio continuum emission at 3.6 cm Image courtesy of NRAO/AUI VLA at 6 and 20 cm Image courtesy of NRAO/AUI VLA at 1.3 cm Image courtesy of NRAO/AUI and Jun-Hui Zhao, W. M. Goss

11 VLA at 20cm Credits: Image visualized by Raymond Plante, NCSA/Univ. of Illinois Radio continuum emission at 3.6 cm Image courtesy of NRAO/AUI VLA at 20cm Image courtesy of NRAO/AUI Image courtesy of NRAO/AUI and N.E. Kassim, Naval Research Laboratory(

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13 Launch: AGILE: 2006 Fermi: 2008

14 EGRET observation (I) In EGRET standard position estimation analysis, a fine map is obtained by rebinning the PSF array with a different offset for the source position from the center of the PSF array for each trial position. (??) Localization jumps around Mayer-Hasselwander et al. 1998

15 EGRET observation (II) For E>1GeV Hooper et al Spatially umbinned The location of the Sgr A* is excluded beyond the 99.9% confidence level as the location of the source. located at 0.2degree from Sgr A*

16 INTEGRAL observation 0.5 degree kev image from the survey. Belanger et al.2006

17 HESS observation (I) Chandra map+ point-like VHE(>100GeV) source Contour lines incidate the 68% and 95% confidence region for The source position Aharonian et al. 2004

18 HESS observation (II) TeV Contours are from molecular radio lines which shows very tight correlation with the diffuse TeV emission Aharonian et al.2006

19 HESS observation (II) The EGRET souce 3EG J located at 0.2degree from Agr A* seems too far to be the GeV counterpart for the INTEGRAL and the HESS sources!!

20 Over all Spectrum of Sgr A*

21 animation from Melia, Falcke, and Agol Accretion and ADAF (Advection Dominated Accretion Flow)

22 Original idea (Narayan & Yi 1994) In ADAF, most of the heat energy is advected with gas, entering the central BH Radiatively inefficient: t(radiation)<t(fall) H/R~1 geometrically thick, optically thin Image: A. Müller, MPE Difference from Bondi accretion(inward gravity + outward pressure): Viscosity plays a crucial role in ADAF via transport of angular momentum Expected to be important for low accretion rate; L<( )L_Eddington

23 electron emission by: S: synchrotron C: inverse Compton scattering B: bremmstrahlung accretion rate : low ---- intermediate. ~ critical accretion rate (when accretion rate > critical accretion rate, thin disk dominates)

24 Later development Strong connection between ADAFS and JETs? Narayan 1996; Esin et al. (1997) Fender, Belloni & Gallo (2003) BH paradigm: thin disk + ADAF + Jet?

25 Extreme inefficiency of Sgr A*(with bolometric luminosity <10^37 erg/s) and other SMBHs (e.x. LLAGN), and XRBs in quiescent states can be explained. For the case of Sgr A*, the spectrum can be explained by ADAF+Jet (Yuan 2000)or ADAF + nonthermal electrons (Yuan et al. 2003)

26

27 Syn. and IC emission by thermal electrons syn. By nonthermal electrons.. Sum of above two free-free from outter parts of RIAF Yuan et al. 2003

28 The GeV and TeV gamma-ray fluxes reported from the direction of the Galactic center may originate in in sources different from Sgr A*: therefore, strictly speaking, they should be considered as upper limits of radiation from Sgr A*

29 Gamma-ray from the GC Sgr A East SNR accelerate proton pion gammaray Central SMBH Proton + gamma-ray: pion gamma-ray Electron + gamma-ray: IC Dark Matter Annihilation of WIMPs

30 Gamma-ray from SMBH Illustration K. Sutliff

31 Electrons or protons dominate the gamma ray emission? Though the rate of proton-gamma (pion-production) interactions is orders of magnitude below electrongamma (inverse Compton) interactions, but the population of energetic electrons declines faster due to "synchrotron cooling. If IC dominates, the maximum observed gamma ray energy puts a lower limit on the electron energy and, in combination with the synchrotron observations provides an upper limit on the magnetic field strength This could help to break the degeneracy of the observed cutoff in the synchrotron spectrum (which contains information about both the magnetic field strength and the maximum electron energy )

32 Dark Matter Candidates Baryonic dark matter some of the dark matter MUST be baryonic, since the value Omega_baryon~0.05 (deduced from nucleosynthesis in the Big Bang), while Omega_lum~0.01 Neutrinos Axions WIMPs

33 Weakly Interacting Massive Particles The postulate of supersymmerty (SUSY) claims that all fermions (bosons) will have Bosons (fermions) partners. The ecperimental mass limits on all SUSY particles are above 100 GeV. Heavier SUSY particles would decay to lighter ones, ultimately ending up with the lightest SUSY particle (LSP) The LSP is usually identified with the neutralino, a neutral fermion Since such heavy particles are not sonstitutes of atoms or nuclei, they cannot have either EM or strong coupling and are assumed to interact only weakly!!

34

35 Thank you

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