Do YSOs host a wide-angled wind?- NIR imaging spectroscopy of H2 emission -

3. Spectro-Imaging using Gemini-NIFS

Subaru UM, 1/30/2008

Hiro Takami (ASIAA)

2. Long-Slit Spectroscopy using Subaru-IRCS

1. Introduction

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)

Schematic view ofSchematic view of

an X-ray binaryan X-ray binary(Credit: ULTRACAM/VLT (Credit: ULTRACAM/VLT

ESO)ESO)

Schematic view of an AGN & Schematic view of an AGN & jetjet

(http://www.phys.hawaii.edu/~jgl/(http://www.phys.hawaii.edu/~jgl/post/)post/)

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)

Magnetic pressure (Uchida & Shibata 1985)

1. Introduction

Key Questions (I) What is the mechanism of mass ejection/accretion?

Magnetic Stress (Hayashi et al. 1996)

1. Introduction

Key Questions (I) What is the mechanism of mass ejection/accretion?

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 arenot sufficient to resolve the central engine.

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?

1. Introduction

Observations of a wide-angled wind would be useful toto tackle these issues, but they are not directly observed.

Line + Cont. Line

Shocked H2 at the cavity walls?

Shocked H2 at the cavity walls?

H2 2.12 μm @ L1551-IRS5 (Davis et al. 2002) UV H2 @ T Tau

(Saucedo et al. 2003)

R=1.1x104 (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=5x103 (v ~60 km s-1)

Gemini-NIFS

AO-corrected FWHM=0”.1-0”.2

2. Long-Slit Spectroscopy using Subaru-IRCS

One of the most active T Tauri stars known.

H2 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)

2. Long-Slit Spectroscopy using Subaru-IRCS

One of the most active T Tauri stars known.

H2 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 H2 emission associated with outflow.

Emission from the other objects are associated with the disk (or quiescent gas)

2. Long-Slit Spectroscopy using Subaru-IRCS

Spectral Resolution(30 km s-1)

(Along the Jet)

Continuum (seeing)

H2

H2 emission toward DG Tau (Takami et al.

2004, A&A)

2. Long-Slit Spectroscopy using Subaru-IRCS

(Perpendicular to the Jet)

H2

Continuum (seeing)

H2 emission toward DG Tau (Takami et al.

2004, A&A)

0”.3

0”.9

0”.6

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 H2 outflow result from a wide-angled wind.

H2 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

2. Long-Slit Spectroscopy using Subaru-IRCS

H2 & [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)

VLSR (km s-1)100-300 -200 -100 0 200 300

01

2-1

-2

X (

arcs

ec)

[Fe II] 1.64 um

H2 2.12 um

Jet

VLSR (km s-1)300100-300 -200 -100 0 200

01

2-1

-2[Fe II] 1.64 um

H2 2.12 um

Jet

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).

VLSR (km s-1)300100-300 -200 -100 0 200

030

060

0-3

00X

(A

U)

VLSR (km s-1)300100-300 -200 -100 0 200

VLSR (km s-1)300100-300 -200 -100 0 200

VLSR (km s-1)300100-300 -200 -100 0 200

VLSR (km s-1)300100-300 -200 -100 0 200

VLSR (km s-1)300100-300 -200 -100 0 200

030

060

0-3

00X

(A

U)

H2 & [Fe II] emission @ HH sources (Takami et al.

2006, ApJ)

3. Integral-Field Spectroscopy using Gemini-NIFS

H2 emission toward six T Tauri stars(Beck, McGregor, Takami, Pyo 2008, ApJ)

H2 (color)

Continuum(blue contour)

jet

3. Integral-Field Spectroscopy using Gemini-NIFS

H2 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

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)

(x10)

(x5)

H2

H2[Fe II]

H2 (gray)

[Fe II] (contour)

H2 (gray)

Cont. 1.64μm (contour)

[Fe II] H2

-200 -100 0 100VHel (km s-1)

Spectralresolution

1”

3. Integral-Field Spectroscopy using Gemini-NIFS

Detailed Study for HL Tau (Takami et al. 2007, ApJL)

Presence of “micro molecular bipolar H2 flow” is revealed H2 emission in some regions are associated with the cavit

y walls. There is no evidence for kinematic interaction with the coll

imated jet.

A wide-angled wind interacts with ambient material,opening up cavities.

Conclusion and Future Directions

NIR H2 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 H2 (blue)

SO NJ=56-45 (red)

CO J=1-0 (white)

SiO J=2-1 (white)