1. Do YSOs host a wide-angled wind? - NIR imaging spectroscopy of H 2 emission - 3. Spectro-Imaging using Gemini-NIFS Subaru UM, 1/30/2008 Hiro Takami (ASIAA) 2. Long-Slit Spectroscopy using Subaru-IRCS 1. Introduction

2. Young stellar objects (HST Public Pictures) X-ray binary (SS 433, Courtesy of Amy J. Mioduszewski) Nearby AGN (M87, HST Public Pictures) Distant Galaxy (Subaru Press Release)

3. Schematic view of an X-ray binary (Credit: ULTRACAM/VLT ESO) Schematic view of an AGN & jet (http://www.phys.hawaii.edu/~jgl/post/)

4. 1. Introduction Key Questions (I) What is the mechanism of mass ejection/accretion? Magneto-centrifugal force (Figs: Shu et al. 1994, Cabrit et al. 1999)

5. Magnetic pressure (Uchida & Shibata 1985) 1. Introduction Key Questions (I) What is the mechanism of mass ejection/accretion?

6. Magnetic Stress (Hayashi et al. 1996) 1. Introduction Key Questions (I) What is the mechanism of mass ejection/accretion?

7. 1. Introduction Key Questions (I) What is the mechanism of mass ejection/accretion? 1” (140 AU) (HST Public Pictures) XZ Tau (Goodson et al. 1999) Angular resolutions of present facilities are not sufficient to resolve the central engine.

8. 1. Introduction Key Questions (II) How does the outflow propagate? Collimated jet (ESO Archive) Molecular Outflow (Lee et al. 2000) Are molecular outflows driven by a collimated jet, or an unseen wide-angled wind?

9. 1. Introduction Observations of a wide-angled wind would be useful to to tackle these issues, but they are not directly observed. Line + Cont. Line Shocked H 2 at the cavity walls? Shocked H 2 at the cavity walls? H 2 2.12 μ m @ L1551-IRS5 (Davis et al. 2002) UV H 2 @ T Tau (Saucedo et al. 2003)

10. R=1.1x10 4 (  v ~30 km s -1 ) for Echelle mode, 0 ”.3 slit Instruments Subaru-IRCS Seeing ~ 0 ”.7 (AO was not used for our observations) IFU (FOV=3 ” x3 ” ), R=5x10 3 (  v ~60 km s -1 ) Gemini-NIFS AO-corrected FWHM=0 ”.1-0 ”.2

11. 2. Long-Slit Spectroscopy using Subaru-IRCS One of the most active T Tauri stars known. H 2 emission toward DG Tau (Takami et al. 2004, A&A) (Bacciotti et al. 2000) +50 -70-200-320-440 (km s -1 ) (Pyo et al. 2003)

12. 2. Long-Slit Spectroscopy using Subaru-IRCS One of the most active T Tauri stars known. H 2 emission toward DG Tau (Takami et al. 2004, A&A) Before this study, only 1 star was known as a T Tauri star with NIR H 2 emission associated with outflow. Emission from the other objects are associated with the disk (or quiescent gas)

13. 2. Long-Slit Spectroscopy using Subaru-IRCS Spectral Resolution (30 km s -1 ) (Along the Jet) Continuum (seeing) H2H2 H 2 emission toward DG Tau (Takami et al. 2004, A&A)

14. 2. Long-Slit Spectroscopy using Subaru-IRCS (Perpendicular to the Jet) H2H2 Continuum (seeing) H 2 emission toward DG Tau (Takami et al. 2004, A&A) 0”.3 0”.9 0”.6

15. 2. Long-Slit Spectroscopy using Subaru-IRCS Blueshifted (~15 km s -1 ) Measured width (~0 ”.6) is comparable to the offset (~0 ”.3) These suggest that warm H 2 outflow result from a wide-angled wind. H 2 emission toward DG Tau (Takami et al. 2004, A&A) Shock-excited UV/X-ray excitation scenarii would not give momentum flux as a T Tauri star

16. 2. Long-Slit Spectroscopy using Subaru-IRCS H 2 & [Fe II] emission @ HH sources (Takami et al. 2006, ApJ) Observed kinematic structures are similar to T Tauri stars (but those at HH sources show lower excitation) V LSR (km s -1 ) 100-300-200-1000200300 0 1 2 -2 X (arcsec) [Fe II] 1.64 um H 2 2.12 um Jet V LSR (km s -1 ) 300 100-300-200-1000200 0 1 2 -2 [Fe II] 1.64 um H 2 2.12 um Jet

17. 2. Long-Slit Spectroscopy using Subaru-IRCS Acceleration over hundreds AU suggest that this is an entrained component by an unseen wide-angled wind (or jet). V LSR (km s -1 ) 300 100-300-200-1000200 0 300 600 -300 X (AU) V LSR (km s -1 ) 300 100-300-200-1000200 V LSR (km s -1 ) 300 100-300-200-1000200 V LSR (km s -1 ) 300 100-300-200-1000200 V LSR (km s -1 ) 300 100-300-200-1000200 V LSR (km s -1 ) 300 100-300-200-1000200 0 300 600 -300 X (AU) H 2 & [Fe II] emission @ HH sources (Takami et al. 2006, ApJ)

18. 3. Integral-Field Spectroscopy using Gemini-NIFS H 2 emission toward six T Tauri stars (Beck, McGregor, Takami, Pyo 2008, ApJ) H 2 (color) Continuum (blue contour) jet

19. 3. Integral-Field Spectroscopy using Gemini-NIFS H 2 emission toward six T Tauri stars (Beck, McGregor, Takami, Pyo 2008, ApJ) A variety of morphology associated with jets, winds and ambient gas Excitation temperature ~2000 K → shock excited

20. 3. Integral-Field Spectroscopy using Gemini-NIFS Detailed Study for HL Tau (Takami et al. 2007, ApJL) Continuum (1.64  m) (original)(unsharp-masked) 1” E N (x10) 1” (x10) (x5) H2H2 H2H2 [Fe II]

21. H 2 (gray) [Fe II] (contour) H 2 (gray) Cont. 1.64 μ m (contour) [Fe II]H2H2 -200-1000100 V Hel (km s -1 ) Spectral resolution 1”

22. 3. Integral-Field Spectroscopy using Gemini-NIFS Detailed Study for HL Tau (Takami et al. 2007, ApJL) Presence of “ micro molecular bipolar H 2 flow ” is revealed H 2 emission in some regions are associated with the cavity walls. There is no evidence for kinematic interaction with the collimated jet. A wide-angled wind interacts with ambient material, opening up cavities.

23. Conclusion and Future Directions NIR H 2 emission toward some active YSO results from an unseen wide-angled wind Extensive studies would be useful to discuss best strategy for ALMA studies (Dutrey et al. 1997)(Lee et al. 2006) CO J=2-1 (green) NIR H 2 (blue) SO N J =5 6 -4 5 (red) CO J=1-0 (white) SiO J=2-1 (white)