1. JVN observations of (NLS1s and) BAL quasars 2009Mar18-20 EAVN-WS 2009 @ Seoul Akihiro Doi ( 土居 明広 ) （ ASTRO-G/JAXA ） Keiichi Asada, Kenta Fujisawa, Noriyuki Kawaguchi, Hiroshi Nagai, and JVN/OCTAVE collaborators.

2. Coevolution of SMBH & Galaxy? Kormendy+2000, Credit: K. Cordes & S. Brown (STScI)STScI

3. Coevolution of SMBH & Galaxy? Di Matteo+(2005) Nature Remaining galaxy with very little gas but a large SMBH. ← Simulation - Color: temperature - Brightness: gas density When the galaxies and their black holes collide a quasar is ignited which expels most of the gas in a strong wind.

4. Rapidly growing Black Holes Log (M BH / M ◎ ) Log (L/L Edd ) 5 6 7 8 9 10 0 － 1 － 2 － 3 － 4 － 5 － 6 Low-luminosity AGN （ Seyfert ） Quasar NLS1 BALQSO ■ Narrow-Line Seyfert 1 Galaxy (NLS1) ■ Broad Absorption Line Quasar (BALQSO)

5. Broad Absorption Line (BAL) quasars 2,000 km/s – 0.3c blue-shifted absorption line -> high-velocity outflow C IV

6. Why BAL in ~30% of QSO? Evolutionary scenario Some quasars in an episodic or young phase have BAL outflows. = depending on the duration of the phase e.g, Becker et al., 2000; Gregg et al., 2000 Orientation scenario Every quasar has BAL outflowing toward nearly edge-on directions. = depending on viewing angle e.g, Elvis 2000; Murray et al., 1995 KEY measurement: ORIENTATION / AGE

7. Photon-pressure-driven outflow Simulation: Proga, Stone, and Kallman (2000) densityvelocity ~ 0.1 pc BHdisk BAL could be found, when observed from edge-on ?

8. Orientation Measurement by VLBI imaging 1. Doppler Boosting 2. Super-Luminal motion Ex., NGC 4261 （ Piner et al. 2001 ） Approaching jets 1. boosted, 2. faster Receding jets 1. deboosted, 2. slower ■ Apparent asymmetry : δ, β app ( φ, β)

9. Kameno 2000 CSSGPS ～ 1-10 kpc > 100 kpc < 1 kpc Spectral Peak Frequency Size (Age) GPS CSS RG CSS GPS RG Flux density Frequency [GHz] Size (Age) Measurement by VLBI imaging Radio Galaxy

10. Only 4 VLBI images for BALQSO (2006) VLBA 5 GHz 1045+352J1556+3517 EVN 1.6 GHz J0957+2356J1312+2319 EVN 1.6 GHz Jiang & Wang 2003 Kunert- Bajraszewska 2006

11. Sample Selection Radio Identification ・ VLA FIRST 1.4 GHz ・ 1 mJy Parent sample （ optical ） ・ SDSS 3DR ・ ⇒ Quasars: 46,420 ・ ⇒ BAL quasars: 4,784 (Trump et al. 2006) SDSS VLA

12. Sample Selection: Result ■ VLA covered the area for 4374/4784 objects (91.4%) ■ 492 objects found (FIRST BAL = 11.2% SDSS BAL) 1 st priority: 23 object （ >100 mJy ） Histogram of radio-detected BAL quasars N

13. OCTAVE, broad-band subarray in JVN Tsukuba 32 ｍ Usuda 64 ｍ Kashima 34 ｍ Yamaguchi 32 ｍ 7 σ Baseline Sensitivity ~3 mJy ( X-band, 9 min integ. ) 2.4 Gbps Optically ConnecTed Array for VLBI Exploration 岐阜 11m Correlator (NAOJ) Nobeyama 45 ｍ Tomakomai 11 ｍ

14. Result: Baseline-detection snapshots ■ 21/23 detected → T B ＞ 10^6 K ■ 4/21 showing inverted spectra ( S vs. S ) ⇒ core dominated ⇒ beaming? ( ν obs = δ rest ν ) Coexistence: nonthermal jet & thermal outflow (magnetic-pressure-driven & radiative-pressure-driven) Some BAL quasars have pole-on viewed relativistic jets? Doi & Asada et al. submitted to PASJ VLBI 8GHz VLA 1.4GHz

15. Multi-Freq. VLBI imaging ■ Sample 2 BAL quasars (inverted spectrum) ■ Observations - 1.7 GHzEVN+MERLIN2008 Mar - 2.3 & 8.4 GHzJVN2008 Aug - 6.4 GHzJVN2008 May

16. Japanese VLBI Network (JVN) ■ Bands (N ant ) ・ 6.7 GHz (6) ・ 8.4 GHz(9) ・ 22 GHz(9) + 2.3 GHz ?(8) + 43 GHz ?(5) ~ 3 mas (8.4 GHz)

17. Results: Multi-Freq. JVN imaging Giga-hertz Peaked Spectrum (GPS) sources ? ( Young Radio Sources?) Doi & Asada in prep. unresolved

18. Summary ■ VLBI contributions to studies of BALQSOs - Jet Asymmetry -> ORIENTATION - Size -> AGE ■ our JVN/OCTAVE observations - 21/23 detections - coexistence of nonthermal/thermal outflows - 2/4 inverted spectra - unresolved - pole-on viewed? / young? ■ A VLBA proposal accepted !! (L/C/X-bands) for 6 BALQSOs

19. radio-quiet NLS1s (Doi et al. submitted) radio-loud NLS1s (Doi et al. 2006 PASJ, Doi et al. to be submitted.) NLS1s can generate nonthermal jets; highly relativistic (Dopper-beamed) in some sources DESPITE OF SMALL BHs !!