JVN observations of (NLS1s and) BAL quasars2009Mar18-20 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.

Coevolution of SMBH & Galaxy?

Kormendy+2000, Credit: K. Cordes & S. Brown (STScI)

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.

Rapidly growing Black Holes

Log (MBH / M◎ )

Log

(L

/LE

dd

)

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)

Broad Absorption Line (BAL) quasars

2,000 km/s – 0.3c blue-shifted absorption line

-> high-velocity outflow

CIV

Why BAL in ~30% of QSO?

Evolutionary scenarioSome 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 scenarioEvery 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

Photon-pressure-driven outflow

Simulation: Proga, Stone, and Kallman (2000)

density velocity

~ 0.1 pc

BH disk

BAL could be found,when observed from edge-on ?

Orientation Measurement by VLBI imaging

　　 1. Doppler Boosting

　　 2. Super-Luminal motion 　　　

Ex., NGC 4261 （ Piner et al. 2001 ）

Approaching jets1. boosted, 2. faster

Receding jets1. deboosted, 2. slower

■ Apparent asymmetry : δ, βapp

cos1

1 2

cos1

sin

app

(φ, β)

Kameno 2000

CSSGPS

～ 1-10 kpc

> 100 kpc

< 1 kpc

Spectral Peak Frequency

Size (Age)

GPS

CSS

RG

CSS

GPS

RG

Flu

x d

en

sity

Frequency [GHz]

Size (Age) Measurement by VLBI imaging

Radio Galaxy

Only 4 VLBI images for BALQSO (2006)

VLBA 5 GHz

1045+352 J1556+3517

EVN 1.6 GHz

J0957+2356J1312+2319

EVN 1.6 GHzEVN 1.6 GHz

Jiang & Wang 2003

Kunert-Bajraszewska2006

Sample Selection

Radio Identification

・ VLA FIRST 1.4 GHz・ <10” , >1 mJy

Parent sample 　（ optical ）

・ SDSS 3DR ・ ⇒ Quasars: 46,420・ ⇒ BAL quasars: 4,784 　　　 (Trump et al. 2006)

SDSS

VLA

Sample Selection: Result

■ VLA covered the area for 4374/4784 objects (91.4%)■ 492 objects found　　　　　 (FIRST BAL = 11.2% SDSS BAL)

BAL (mJ y/ beam) 電波源 ピーク強度 度数分布

0102030405060708090

100

1.00

1.

58

2.51

3.

98

6.31

10

.00

15.8

25

.1

39.8

63

.1

100

158

251

398

631

1000

次

の級

mJ y/ beam

天体

数

1st priority: 23 object

（ >100 mJy ）

Histogram of radio-detected BAL quasars

N

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 ｍTomakomai 11 ｍ

Result: Baseline-detection snapshots

■ 21/23 detected → TB ＞ 10^6 K

■ 4/21 showing inverted spectra ( S vs. S )　　　 ⇒　 core dominated　　　 ⇒ beaming? ( νobs = δrest 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

VLBI8GHz

VLA1.4GHz

Multi-Freq. VLBI imaging

■ Sample

2 BAL quasars (inverted spectrum)

■ Observations

- 1.7 GHz EVN+MERLIN2008 Mar- 2.3 & 8.4 GHz JVN

2008 Aug- 6.4 GHz JVN 2008

May

Japanese VLBI Network (JVN)

■ Bands (Nant)

・ 6.7 GHz (6)・ 8.4 GHz (9)・ 22 GHz (9)+ 2.3 GHz ? (8)+ 43 GHz ? (5)

~3 mas(8.4 GHz)

Results: Multi-Freq. JVN imaging

Giga-hertz Peaked Spectrum (GPS) sources ?( Young Radio Sources?)

Doi & Asada in prep.

unresolved unresolved

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

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 sourcesDESPITE OF SMALL BHs !!