Observations with JVN, OCTAVE, & VSOP-2, & EAVN, APT 2008Mar20-22 East Asia VLBI workshop

1. Observations with JVN,OCTAVE, & VSOP-2, & EAVN, APT2008Mar20-22 East Asia VLBI workshop “ UV-coverages “ Akihiro Doi [土居 明広] ( VSOP-2 project, JAXA/ISAS )

2. We are going to getvery good UV-coverages !! APT 22 GHz APT+ASTRO-G 22 GHz APT = CVN + KVN + LBA + JVN 2013 Jun 01 24 hr Dec = +30 deg

3. Competitive !!-- Three major arrays -- EVN 22 GHz APT 22 GHz VLBA 22 GHz 9000 x 5000 km 5000 x 9000 km 8000 x 5000 km

4. The present capability & some scientific outputs of JVN(only continuum obs)cf. maser sciences by Imai & Sugiyama’s talks

5. A test image JVN 8 GHz (2004Dec18) [ 128-Mbps ] 1928+738 (16 hr) Sudou et al. ○ Good UV : high image dynamic range (~1000-3000) ×Narrow BW: observable only for strong sources (>200 mJy)

6. UV-coverages JVN 8/22 GHz Full track Snapshot δ=60 deg δ=20 deg δ = ―20 deg

7. The first systematic VLBI study for NLS1s (Doi+2007, PASJ 59, 703) A subclass of Seyfert-1, with small-mass BH JVN 8 GHz Phase-referencing [ Obs date] 2006/03/17 2006/03/26 2006/05/20 [ Array ] [ General properties ] － Small-mass BH, very high accretion rate. － Weak radio jets Jet Disk 3 mJy Black hole • [ Our Result] • - All of 5 targets detected, -> strong jets. • 2/5 sources showing inverted spectra, • suggesting Doppler boost in pole-on view

8. a test image OCTAVE 8 GHz (2007Dec12) Usuda 64ｍ Tsukuba32ｍ Yamaguchi32ｍ 2050+364 (5 hr) ○ Broad BW: high baseline sensitivities (~3-10 mJy, 10 min) ×Poor UV: baselines dominated in East-West direction Kashima 34ｍ

9. UV-coverages OCTAVE 8 GHz Full track Snapshot δ=60 deg δ=20 deg δ = ―20 deg

10. The first systematic VLBI survey for BAL quasars (Doi+2008 in prep) blue-shifted Broad Absorption Lines in UV OCTAVE 8 GHz [ Obs date] 2007/11/04 2007/12/02 2008/02/09 [ Array ] [ Standard Scenario ] － Equatorial outflows, and edge-on view － Weak polar radio jets Jet Disk Black hole • [ Our Result] ≠ “standard scenario” • - Strong jets in many radio loud BAL quasars • 4/23 sources showing inverted spectra, • suggesting Doppler boost in pole-on view

11. Comparisons with VLBA / EVN - current JVN - future EVN - future APT

12. The actual capabilities of current JVN EVN 22 GHz JVN 22 GHz VLBA 22 GHz 9000 x 5000 km 0.3 x 0.5 mas 1700 x 2300 km 1.6 x 1.2 mas 8000 x 5000 km 0.3 x 0.5 mas 1σ= 50 μJy/beam = 10^7.2 K (1hr) 1σ= 1100 μJy/beam = 10^7.2 K (1hr) 1σ= 200 μJy/beam = 10^7.6 K (1hr) 1024 Mbps 128 Mbps 1024 Mbps

13. The expected capabilities of EAVN EVN 22 GHz EAVN 22 GHz VLBA 22 GHz 9000 x 5000 km 0.3 x 0.5 mas 5000 x 4000 km 0.5 x 0.6 mas 8000 x 5000 km 0.3 x 0.5 mas 1σ= 50 μJy/beam = 10^7.2 K (1hr) 1σ= 150 μJy/beam = 10^7.2 K (1hr) 1σ= 200 μJy/beam = 10^7.6 K (1hr) 1024 Mbps 1024 Mbps 1024 Mbps

14. EAVN compared with VLBA / EVN

15. Competitive !!-- Three major VLBI arrays -- EVN 22 GHz APT 22 GHz VLBA 22 GHz 8000 x 5000 km 0.3 x 0.5 mas 5000 x 9000 km 0.3 x 0.5 mas 9000 x 5000 km 0.3 x 0.5 mas 1σ= 50 μJy/beam = 10^7.2 K 1σ= 90 μJy/beam = 10^7.4 K 1σ= 200 μJy/beam = 10^7.6 K 1024 Mbps 1024 Mbps 1024 Mbps

16. Competitive !!-- Three major ground arrays --

17. UV-coverages (22 GHz) EAVN APT APT + MaunaKea

18. UV-coverages (22 GHz) JVN+ASTRO-G EAVN + ASTRO-G APT + ASTRO-G APT + MK

19. Summary + JVN offers a dense UV-coverage. Science: e.g., NLS1s + OCTAVE offers a very high baseline sensitivity. Science: e.g., BALQSOs + EAVN provides - num of antennas larger than VLBA and EVN - image sensitivity better than VLBA - brightness sensitivity comparable to EVN - good space-VLBI UV-coverages + APT provides - num of antennas much larger than VLBA and EVN - angular resolutions comparable to VLBA and EVN - very good space-VLBI UV-coverages Thank you