1. 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)

2. Introduction Extragalactic Radio Sources
Radio morphology
Radiated by synchrotron radiation
Cygnus A
Lobe
Hotspot
Jet
Jet
Core
Hotspot
Lobe

3. Introduction: Main problems concerning about AGN jet
from cradle
to grave
Hada+ 2011
Nagai+ 2010
Kameno+ 2000
Nagai+ 2006 ？

4. Introduction: to grave; how to evolve to radio galaxy
GPS/CSS sources
Gigaheltz Peaked Spectrum / Compact Steep Spectrum
Compact radio sources suffer from absorption (<10kpc)
Odea+ 1998
Flux (Jy)
Frequency (GHz)
Frequency (GHz)
Snellen+ 2000
linear size
Correlation between
“linear size” and “peak frequency”
　⇒ self-similar evolution from GPS to CSS.
CSS
GPS
peak frequency

5. Introduction: to grave; how to evolve to radio galaxy
Radio 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, Ph.D.T
天体サイズ
天体年齢
Nagai, Ph.D. T
linear size
age
CTD93; Nagai+ 2006

6. Introduction: to grave; how to evolve to radio galaxy
Remaining 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 progress
Fading 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
Recurrent double-double RG
Konar+ 2006
Extended emission

7. Introduction: Broad Absorption Line (BAL) quasars
Blue-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)
⇒ Ionized AGN wind is absorber?
Gregg+ 2000
CIV
Proga+ 2000

8. Introduction: Broad Absorption Line (BAL) quasars
Radio jet in BAL quasars
Many 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 ?
FRIIが少ないことはどう説明するんだ？？
YRSのover population問題は、リカレントが原因と思われるが、
> BLA/non-BALにかかわらずリカレントは普遍的に存在するのか？すなわち、
> non-BALで見つかっているYRSは単にリカレント現象を見ているのではないか？
(Montenegro-montes+ 2008)
・Is the recurrence popular regardless whether the source is BAL or non-BAL ? ・Does the compactness of morphology indicate youngness ?

9. Introduction: Broad Absorption Line (BAL) quasars
The fraction of BAL
= covering factor
The orientation scheme
The evolution scheme
Radio jet:
v<c
Disk wind:
v～0.1c
The fraction of BAL
= time having the wind
Disk wind：
v～0.1c

10. Observation: VLBA observation BD137 on 2010 Jun 25
L, C, and X band
Dual pol.
BK131 on 2006 Jun 18
P band (90cm; non detected at 50cm)
◆ Target：J
detected by OCTAVE (Doi+ 2009)
GPS天体
(Montenegro-monte+ 2008)
Unresolved by VLA
(Montenegro-monte+ 2008)

11. Result: Total intensity map
Hayashi, Doi & Nagai in prep.
1.7 GHz
327 MHz
4.9 GHz
8.3 GHz 11

12. Result： Spectral index and polarization map
Hayashi, Doi & Nagai in prep.
500pc
1.7–4.9GHz
1.7 GHz
：E vector
：degree of polarization
Jet
Undetected
500pc

13. Discussion： As BAL quasars
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.
40pc
8.3GHz core

14. Discussion: Another example of BAL quasars
Mrk231 (Reynolds+ 2009)
(maybe) the nearest BAL quasar (Forstar+ 1995)
50pc-scale two-sided jet
Active radio core
⇒ same as J
jet
No variability
core
Violent activity
Reynolds+ 2009

15. Discussion: Orientation or Evolution ?
The fraction of BAL
= covering factor
The orientation scheme
The evolution scheme
Radio jet:
v<c
Disk wind:
v～0.1c
The fraction of BAL
= time having the wind
Disk wind：
v～0.1c

16. Summary & Future: Proposal to Japanese VLBI
Do any other extended emission exist ?
Summary
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 !!

18. Discussion: As radio jet
General property
Unpolarized core
Two-sided jet
Compact size (<1kpc)
⇒ J is a young radio source
Comparison with radio SED
CSS: kpc-scale jet
GPS: the radio core