S ources associated with Broad Absorption Line Q uasars Takayuki HAYASHI Univ of Tokyo NAOJ A member of AGN WG in SKA jp A DOI ISASJAXA H NAGAI NAOJ G Bruni ID: 378925
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Slide1
Young Radio Sources associated with Broad Absorption Line Quasars
Takayuki HAYASHI (
Univ. of
Tokyo, NAOJ)
A member of AGN WG in SKA-
jp
A. DOI
(ISAS/JAXA),
H.
NAGAI
(NAOJ)
G.
Bruni
, K.-H. Mack (IRA/INAF), F. M. Montenegro-
montes
(APEX/ESO
)Slide2
IntroductionExtragalactic Radio SourcesRadio morphologyRadiated by synchrotron radiation
2
H
otspot
C
ore
Jet
Lobe
Lobe
H
otspot
Jet
Cygnus ASlide3
Introduction:Main problems concerning about AGN jetfrom cradle
t
o grave
Nagai+ 2010
Hada
+ 2011
Kameno
+ 2000
Nagai+ 2006
？Slide4
Introduction:to grave; how to evolve to radio galaxyGPS/CSS sources
Gigaheltz
Peaked Spectrum / Compact Steep Spectrum
Compact radio sources suffer from absorption (<10kpc)
Snellen
+ 2000
Odea
+ 1998
Correlation between
“linear size” and “peak frequency”
⇒ self-similar evolution from GPS to CSS.
peak frequency
linear size
GPS
CSS
Flux (
Jy
)
Frequency (GHz)
Frequency (GHz)Slide5
Introduction:to grave; how to evolve to radio galaxyRadio galaxy and GPS/CSS
sources
GPS/CSS sources are young
Correlation between age and linear size
is kept
even for radio galaxy
⇒ GPS/CSS sources evolve even to radio galaxy self similarly.
Nagai,
P
h.D
.
T
天体サイズ
天体年齢
Nagai, Ph.D
.
T
l
inear size
age
CTD93; Nagai+
2006Slide6
Introduction:to grave; how to evolve to radio galaxyRemaining problems
Why there are more GPS/CSS sources than expected from their linear size
？
(40%
is GPS/CSS in flux limited
sample ; O’dea+ 1998
)Do all GPS/CSS sources evolve to radio galaxy ?“age of detected emitter” ≠
“age of radio activity of AGN” ?Recent progressFading young radio sources
(e.g., Orienti+ 2010)Extend emission indicating past activity (e.g., Baum+ 1990)Double-double radio galaxy showing recurrent radio activity (e.g.,
Konar+ 2006) ⇒ AGN has recurrent radio activity ?
Baum+ 1990
K
onar
+ 2006
Recurrent double-double RG
Extended emissionSlide7
Broad Absorption Line (BAL) quasarsBlue-shifted metal absorption (e.g. CIV, Mg II) at rest-UV
Very broad;
Extremely large velocity;
~15
%
of quasars have BAL
(SDSS DR5, Shen+2008)Introduction:
Broad Absorption Line (BAL) quasars
⇒
Ionized AGN wind is absorber?
Gregg
+ 2000
CIV
7
Proga
+
2000Slide8
Introduction:Broad Absorption Line (BAL) quasarsRadio jet in BAL quasarsMany GPS/CSS sources are associated with BAL quasars
(Montenegro-
montes
+ 2008)
Small number of radio galaxy compared with non-BAL quasars
(Gregg+ 2006)⇒ disk possessing AGN winds also drive young radio sources ?
(Montenegro-
montes
+ 2008)
・
Is
the recurrence popular regardless whether the source is BAL or non-BAL ?
・
Does
the compactness of morphology indicate youngness ?Slide9
Introduction: Broad Absorption Line (BAL) quasarsThe orientation scheme
The evolution scheme
9
The fraction of BAL
= covering factor
The fraction of BAL
= time having the wind
Disk wind
：
v
～
0.1c
Disk wind
:
v
～
0.1c
Radio jet:
v
<
cSlide10
Observation:VLBA observationBD137 on 2010 Jun 25
L, C, and X band
Dual pol.
BK131 on 2006 Jun 18
P band (90cm; non detected at 50cm)
Dual pol.◆
Target：J1159+0112detected by OCTAVE (Doi+ 2009)
GPS天体 (Montenegro-monte
+ 2008)Unresolved by VLA
(Montenegro-monte
+ 2008)Slide11
Result:
Total intensity map
11
11
327
M
Hz
1.7 GHz
4.9 GHz
8.3 GHz
Hayashi,
Doi
& Nagai in prep
.Slide12
Result：Spectral index and polarization map12
500pc
1.7–4.9GHz
Jet
500
pc
：
E
vector
：
degree of polarization
Undetected
1.7
GHz
Hayashi,
Doi
& Nagai in prep
.Slide13
Discussion：As BAL quasars
40
pc
8
.3GHz
core
Radio core
Is resolved into two sub component
Peak frequency is
30GHz at rest
⇒
the radio core is extremely young
Recurrent activity
Combined with the morphology
“the source has recurrent activity
and
is active phase now”
Past activity is shown in
extended emission ?
More past activity exist ?
⇒
Radio activity might not young.
Emitter is just young.
Slide14
Mrk231 (Reynolds+ 2009) (maybe) the nearest BAL quasar
(
Forstar
+ 1995)
50pc-scale two-sided jet
Active radio core ⇒ same as J1159+0112
Discussion:Another example of BAL quasars
Reynolds+ 2009
Violent activity
jet
c
ore
No variabilitySlide15
Discussion:Orientation or Evolution ?The orientation scheme
The evolution scheme
15
The fraction of BAL
= covering factor
The fraction of BAL
= time having the wind
Disk wind
：
v
～
0.1c
Disk wind
:
v
～
0.1c
Radio jet:
v
<
cSlide16
Summary & Future:Proposal to Japanese VLBISummary
GPS/CSS in
non-BAL
：
YRSs are evolve to radio galaxy but large fraction of YRSs cannot be explained
. Recurrent activity is essential.GPS/CSS in BAL：
Larger fraction of YRSs in BAL quasars exists than in non-BAL. Some
BAL quasars show recurrent activity. The situation is same as non-BAL ? BAL is more extreme case ?Towards SKA
Disk having AGN winds also drive recurrent activity ?Detection of extended emission is the key to understand the recurrence. There might be larger amount of extended emission in BAL quasars.⇒ connection between jet and disk can be proved !!
Do a
ny other extended emission exist ?Slide17Slide18
Discussion:As radio jetGeneral propertyUnpolarized core
Two-sided jet
Compact size (
<1kpc)
⇒
J1159+0112 is a young radio sourceComparison with radio SED
CSS: kpc-scale jetGPS: the radio core