Galactic Astronomy ??????? I Lecture 2-1: Active galaxies and super massive black holes in the local universe Seminar: Gultekin et al. 2009, ApJ, 698, 198 - PowerPoint PPT Presentation

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Galactic Astronomy ??????? I Lecture 2-1: Active galaxies and super massive black holes in the local universe Seminar: Gultekin et al. 2009, ApJ, 698, 198

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Galactic Astronomy I Lecture 2-1: Active galaxies and super massive black holes in the local universe Seminar: Gultekin et al. 2009, ApJ, 698, 198 – PowerPoint PPT presentation

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Title: Galactic Astronomy ??????? I Lecture 2-1: Active galaxies and super massive black holes in the local universe Seminar: Gultekin et al. 2009, ApJ, 698, 198


1
Galactic Astronomy??????? ILecture 2-1 Active
galaxies and super massive black holes in the
local universeSeminar Gultekin et al. 2009,
ApJ, 698, 198 Lecture
2011/11/21
2
UV and optical spectra of Active Galactic Nuclei
Seyfert galaxies Permitted emission lines
(Ha,Hb,MgII,CIII,CIV,NV,Lya etc) of Seyfert 1
galaxies show broad component with FWHM of
2000-10000km/s (broad-lines). Forbidden
transition lines (???) does not have broad
component, because the gas density of the
broad-line region is higher than the critical
density of the forbidden transitions. Forbidden
emission lines as well as permitted ones show
narrow emission with FWHM100-1000km/s
(narrow-lines).
Seyfert 2 Permitted lines only
narrow-line Forbidden lines narrow-line
Seyfert 1 Permitted lines broadnarrow-line Forbi
dden lines narrow-line
3
Structure of active galactic nuclei Unified
model of Seyfert 1 and 2 galaxies is proposed by
Antonucci and Miller (1985, ApJ, 297, 621) based
on the data obtained by spectro-polarimetric
observation. Dust torus structure around the
nuclei hide the broad-line region of Seyfert 2
galaxies. Emission from the broad-line can be
observed through scattered light (though electron
or dust scattering).
Miller and Antonucci 1983, ApJL, 271, 7
Miller et al. 1980, PASP, 92, 702
4
Structure of active galactic nuclei
NGC5252 Morse et al. 1998, ApJ 505, 159
Antonucci and Miller, 1985, ApJ, 297, 621
5
Unified model of AGNs
Luminous AGN QSOs, Less-luminous AGN
Seyfert Radio-loud Radio-loud QSOs, radio
galaxies Radio-quietRadio-quiet QSOs, Seyferts
From www.cv.nrao.edu/course/astr534/ExtraGalactic.
html
6
Structure of active galactic nuclei X-ray
data Unified model with the dust torus structure
is also supported by the X-ray spectra of Seyfert
2 galaxies. Their X-ray spectra show strong soft
X-ray absorption.
Awaki et al. 1991,PASJ, 43, 195
7
Structure of active galactic nuclei FIR
view Seyfert 2 galaxies with Hidden-broad-line
region (HBLR) show hot MIR-FIR spectra similar
to Seyfert 1 galaxies. (Non-HBLR Seyfert 2
galaxies show similar F25/F60 to HII-region,
LINER, Starbursts (HLS). Non-HBLRs have lower
intrinsic luminosity).
Tran 2003, ApJ, 583, 632
8
Selecting Seyfert 2 galaxies with optical
emission line ratios
AGNs tend to have stronger highly ionized
emission lines, like OIII Solid line selection
line by Kewly et al. (2001) model calculation,
Dashed line empirical line.
Kauffmann et al. 2003, MNRAS, 346, 1055
9
UV and optical spectra of AGNi QSOs QSOs show
similar line properties to Seyfert 1 galaxies,
but they are more luminous and their continuum is
dominated by nuclear component (not by host
galaxy).
Richards et al. 2003, ApJ, 126, 1131
10
Broad-band continuum of AGNs QSOs
Standard accretion disk (UV) Inverse Compton
emission (X-ray) from coronal component of
surface of the disk.
Kawaguchi et al. 2001, ApJ, 546, 966
11
AGN and super massive black holes Black hole
massesof AGNs are determined with reverberation
mapping method. The method measures the time-lag
between the time-variation of the fluxes of the
nuclear continuum and broad emission lines. The
time lag corresponds to the typical distance
between the black hole and the line emitting
region. The black hole masses can be estimated
with the distance and the line width. The
lag-velocity diagram suggests the virialized
condition of the broad-line region.
Peterson et al. 2004, ApJ, 613, 682
12
Measuring the black hole mass with stellar
motions at the center. VLT/SINFONI observation of
velocity field of the central region of Centaurus
A . Its black hole mass is estimated to be
5.5x107 Msolar
Cappellari et al. 2009, MNRAS, 394, 660
13
Which is the primary relation ?
Ferrarese and Merritt 2000, ApJ, 539, L9
14
Which is the primary relation ? MBH-LK relation
has rms0.3 dex in logMBH, MBH-Mbulge(ReSigma2,
bulge virial mass) has 0.25 dex in logMBH.
Marconi and Hunt 2003, ApJ, 589, L21
15
Extending the MBH-Mspheroid relation to the
smaller systems Search for dwarf Seyfert 1
galaxies with SDSS spectro-scopic data.
Barth et al. 2005, ApJ, 619, L151
Greene Ho 2004, ApJ, 610, 722
16
Extending the MBH-Mspheroid relation to the
smaller systems HST/STIS observation of a
globular cluster G1 in M31. Its central velocity
dispersion is 30km/s and the estimated black
hole mass is MBH18000Msolar?
Gebhardt et al. 2005, ApJ, 634, 1093
Gebhardt et al. 2002, ApJ, 578, L41
17
Extending the MBH-Mspheroid relation to the
smaller systems A search for SMBH at the center
of the globular cluster M15 with HST STIS. If the
excess velocity dispersion is explained with
existence of SMBH, its mass is edimated to be
MBH3900Msolar. See next slide.
Gerssen et al. 2002, AJ, 124, 3270
18
Extending the MBH-Mspheroid relation to the
smaller systems Proper motion survey of the
globular cluster M15 with HST WFPC2. Comparison
with N-body simulation (Baumgardt Makino 2003,
MNRAS, 340, 227) suggest that no black hole is
necessary for the cluster. The upper limit is
500Msolar.
McNamara et al. 2003, ApJ, 595, 187
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