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)

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

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

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

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

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

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

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 ?

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

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：J1159+0112 detected by OCTAVE (Doi+ 2009) GPS天体 (Montenegro-monte+ 2008) Unresolved by VLA (Montenegro-monte+ 2008)

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

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

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

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 J1159+0112 jet No variability core Violent activity Reynolds+ 2009

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

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 !!

Discussion: As radio jet General property Unpolarized core Two-sided jet Compact size (<1kpc) ⇒ J1159+0112 is a young radio source Comparison with radio SED CSS: kpc-scale jet GPS: the radio core