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LONG‐TERM SPECTRAL OPTICAL MONITORNIG OF ACTIVE GALACTIC NUCLEIACTIVE GALACTIC NUCLEI
Dragana IlićDepartment of Astronomy Faculty of MathematicsDepartment of Astronomy, Faculty of Mathematics, University of Belgrade
Luka Č. Popović, Astronomical Observatory, Belgrade, Serbia
Alla I. Shapovalova, SAO observatory, Russia
Vahram H. Chavushyan, INAOE, Mexico
EMISSION LINESDragan
broad emission linesEMISSION LINES a Ilić ApBalmer lines of AGN Mrk 817
broad emission lines‐ permitted transitions
pril 2011
(Ilic et al.2006) ‐ FWHM 2000 ‐ 10000 km/s
[OIII]
Lo
[OIII]
ong‐term m
on
HHγ nitoring of AG
Hγ
GN
Hβ
2
narrow emissione lines permitted and forbidden‐ permitted and forbidden
‐ FWHM 200 ‐ 700 km/s
BLACK HOLE MASS MBHDraganBH
ESTIMATES
a Ilić ApvR 2 pril 2011
virial theorem: GvRfM BLR
BH
Lo
(Wandel+ 1999; Kaspi+ 2000, 2005; Peterson+ 2004, Bentz+ 2009)
ong‐term m
on
reverberation mapping→ the BLR radius: RBLR(for NGC 4151, 3c390. 3 in Shapovalova+2009, 2010)
nitoring of AG
Problem BLR geometry : f depends GN Problem BLR geometry : f depends
on geometry and kinematics
3
e.g. most common AGN spectra show i < 20°( l )(La Mura et al. 2009, ApJ, 693, 1437)
Draganin order toFWHM up to 10,000 km/s na Ilić A
in order to estimate
FWHM up to 10,000 km/scomplex region
t ?
April 2011MBH we
geometry: ?
disc / outflows / disc+wind /
Lo
need to know the
disc+spherical region
ong‐term m
on
know the geometry nitoring of AG
geometry of the BLR
GN
h d4
what do weknow about
T 104 K Ne ~ 1010 cm‐3
photoionized regionBLR?
photoionized region
(also shock heating?)
AGN – HIGHLY VARIABLE OBJECTSDraganAGN – HIGHLY VARIABLE OBJECTS
variation in the continuum and line flux
a Ilić Apvariation in the continuum and line flux
change of the galaxy type
pril 2011
line
Lo
i lineprofile
b l
ong‐term m
on
maximumactivity
minimumactivityvariability
nitoring of AG
activity
GN
5
(Shapovalova et al. 2009)
NGC 5548 (Peterson et al. 2002)3c390.3 (Shapovalova et al. 2010)
LONG‐TERM MONITORINGDraganLONG‐TERM MONITORING a Ilić A
p
PIs: Alla I Shapovalova (Russia)Vahram H. Chavushyan (Mexico)
pril 2011
y ( )
constantly observing well known AGN: NGC 5548 – 9 years (Ilić 2007 Popović et al 2008)
Lo
NGC 5548 – 9 years (Ilić 2007, Popović et al. 2008)
NGC 4151 – 11 years (Shapovalova et al. 2008, 2009, 2010a)
ong‐term m
on
3C390.3 – 13 years (Shapovalova et al. 2010b, Popović et al. 2011, Jovanović et al. 2010)
nitoring of AG
Arp 102B – 12 years (in prep.)
Ark 564 – 11 years (in prep )
GN
Ark 564 11 years (in prep.)
variability: continuum flux, line shapes, line fluxes …6
powerful tool for emission line region diagnostics
OBSERVATIONSDraganOBSERVATIONS
6m + 1m telescopes SAO RAS (Russia)
a Ilić Ap
6m + 1m telescopes ‐ SAO RAS (Russia)
2.1 m telescope ‐ Guillermo Haro Observatory, Cananea,
pril 2011
Sonora, Mexico
2 1 m telescope ‐ Observatorio Astronómico Nacional San Lo 2.1 m telescope Observatorio Astronómico Nacional, San Pedro Martir, Baja California, Mexico
ong‐term m
onnitoring of AGGN
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3C390 3Dragan3C390.3 double radio‐loud galaxy
a Ilić Ap double radio loud galaxy
with strong radio core(Leahy & Perley 1991)
pril 2011
( ea y e ey 99 )
Loong‐term m
on
double‐peaked broad line
nitoring of AG
(Eracleous & Halpern 1994)
proof of the line disc‐emission GN
p
variable line profiles different complex BLR models: binary BLR
8
complex BLR models: binary BLR, disc precession, disc perturbation, etcetc.
3C390 3Dragan3C390.3 a Ilić A
p 13‐year data pril 2011
13 year data
several max &min
Lo
CCF analysis (ZDCF, ICCF)
H 120 light days
ong‐term m
on
H 120 light days
Hβ 95 light days
nitoring of AG
stratified BLR
GN
minimum in 2002 2 characteristic periods
9
Shapovalova, Popović, Ilić, Chavushyan et al. 2010b, A&A, 517, 42
3C390 3 ‐ QPOSDragan3C390.3 ‐ QPOS a Ilić A
p quasi‐periodic oscillations (QPOs) pril 2011
quasi periodic oscillations (QPOs)
Morlet wavelet transformation
Lo
analysis of the minima and maxima of Hβ and continuum
ong‐term m
on
QPOs with periods: 10 years (Veilleux & Zheng 1991) nitoring of AG
2‐4 years
shock waves near the SMBH GN shock waves near the SMBH
spreading in the outer part of the disc OR contribution of either
10
disc OR contribution of either ejection or jets to QPOs
Shapovalova , Popović, Ilić, Chavushyanet al. 2010b, A&A, 517, 42
3C390 3 – LINE PROFILESDragan3C390.3 – LINE PROFILES
line profiles vary dramatically: disc like profile with strong
a Ilić Ap line profiles vary dramatically: disc‐like profile with strong
blue peak always present, BUT sometimes also the central peak appears additional emission region
pril 2011
peak appears additional emission region
Loong‐term m
onnitoring of AG
disc perturbation todescribe the line profiles
GN
Jovanović, Popović,S l ki Sh l
11Stalevski, Shapovalova2010, ApJ, 718, 168
3C390 3 – MODELSDragan3C390.3 – MODELS
f h di h i
a Ilić Ap
part of the disc that is emitting lines is shifted along th di
pril 2011
the radius
Loong‐term m
on
models vs. observations
4 an
d-3
nitoring of AG
Period I: the change can be explained with the change of h d k hm
ents
-4
GNthe disk position with respect
to the BH
of s
egm
12
Period II (when burst starts): disc position is fixed
fl t +4 d +3
flux
Popović, Shapovalova, Ilić, Chavushyan et al. 2011, A&A, 528,130
flux segments +4 and +3
CONCLUSIONSDraganCONCLUSIONS the broad line region is a complex region
aIlić
Apg p g
(careful with MBH estimates using reverberation mapping): disc outflows winds combination
pril 2011
mapping): disc, outflows, winds, combination...
possibility of QSOs as with stellar black‐holes Lo
Th k possibility to have disc perturbations: e g shock waves fragmented spiral waves
ong‐term m
on
Thank you!e.g. shock waves, fragmented spiral waves nitoring of AG
you!
GN
3C390.3: TWO COMPONENT BLR disc‐like BLR1
13
BLR2? =outflows,part of the jet, disc wind