do ysos host a wide-angled wind? - nir imaging spectroscopy of h 2 emission -
DESCRIPTION
Subaru UM, 1/30/2008. Do YSOs host a wide-angled wind? - NIR imaging spectroscopy of H 2 emission -. Hiro Takami (ASIAA). 3. Spectro-Imaging using Gemini-NIFS. 1. Introduction. 2. Long-Slit Spectroscopy using Subaru-IRCS. Young stellar objects (HST Public Pictures). Nearby AGN - PowerPoint PPT PresentationTRANSCRIPT
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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
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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)
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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/)
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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)
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Magnetic pressure (Uchida & Shibata 1985)
1. Introduction
Key Questions (I) What is the mechanism of mass ejection/accretion?
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Magnetic Stress (Hayashi et al. 1996)
1. Introduction
Key Questions (I) What is the mechanism of mass ejection/accretion?
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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.
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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?
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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)
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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
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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)
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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)
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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)
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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
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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
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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
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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)
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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
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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
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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]
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H2 (gray)
[Fe II] (contour)
H2 (gray)
Cont. 1.64μm (contour)
[Fe II] H2
-200 -100 0 100VHel (km s-1)
Spectralresolution
1”
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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.
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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)