galactic star formation science
DESCRIPTION
Galactic Star Formation Science. with Integral Field Spectroscopy. Tracy Beck, STScI. Galactic Star Formation Science with Integral Field Spectroscopy. Introduction to the formation of sun-like stars in the Milky Way Studies of star formation (SF) with IFUs - PowerPoint PPT PresentationTRANSCRIPT
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Galactic Star Formation Science
with Integral Field Spectroscopy
Tracy Beck, STScI
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Galactic Star Formation Science
with Integral Field Spectroscopy
• Introduction to the formation of sun-like stars in the Milky Way
• Studies of star formation (SF) with IFUs– First uses of IFUs for SF science– Herbig Haro Objects– Young Star Binaries
• Star Formation at high contrast with IFUs: A Search for IR H2 Emission from the Disks of Young Stars
• Cutting Edge Science: Laser-Fed AO IFU spectroscopy of young stars
• Prospects for JWST and the ELTs
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Formation of Sun-like Stars in the Milky Way
Sub-mm continuum of protostellar cores
Shirley et al. (2000)
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Formation of Sun-like stars in the Milky Way
Young stars with Circumstellar disks + extended Envelopes (“Class I” Protostars)
HST NICMOS Imaging of Protostars (Padgett et al. 1999)
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Formation of Sun-like stars in the Milky Way
Young stars with Circumstellar disks, no envelope material left (“Class II” Protostars,
“Classical” T Tauri Stars)
Orion ProplydsO’Dell & Wen (1994)
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Formation of Sun-like stars in the Milky Way
Dust disk dissipates in <1Gyr timescale
Meyer et al. (2008)
Beta Pic Debris Disk
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Formation of Sun-like stars in the Milky Way
“Class II” Protostars with Disks + Outflows – “Classical T Tauri Stars”
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IFUs in Star Formation Science
Herbst et al. “A Near-Infrared Spectral Imaging Study of T Tau” 1996 AJ v.111, 2403
MPE 3D w/ Calar Alto (3.5m)H and K-band
Observations of T Tau
8”
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IFUs in Star Formation Science
Lavalley et al. “Sub-arcsecond morphology and kinematics of the DG Tauri jet in the [O I]λ6300 line” 1997 A&A v.327, 671
IFUs are very powerful tools for spatially resolving emission line structures in the environments of bright T Tauri Stars
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Herbig Haro Objects
• HH Objects: – optical/infrared tracers of YSO jets, seen where
jets from young stars plow into ambient cloud material and shock the gas into emission
– Pure emission line objects – viewed in optical/infrared permitted and
forbidden transitions – H, [O I], [N II], [S II], [FeII], trace atomic gas excited by shocks
– Shock-excited H2 emission in the IR Natural IFU Sources
Beck et al. 2004, 2007, Lopez et al. 2008, 2010 Giannini et al. 2008
HH 111
HH 46/47
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Herbig Haro Objects
• HH 99B: – Very sensitive VLT + SINFONI
observations– 170+ Emission lines detected– Many very high excitation
lines of H2 and [Fe II]– Bow-shock apex shows
extremely high temperature - T~6000K - revealing that the H2 molecule persists in these very high temperature regions
Giannini et al. “Near-infrared, IFU spectroscopy unravels the bow-shock HH99B“ 2008, A&A v.481, 123
H2 1-0 S(1) 2.12m H2 2-1S(17) 1.758m
[Fe II] 1.644 m [Fe II] 1.749 m
[P II] 1.188 mHI Pa 1.28 m
Head of the Bow Shock
Wings of the Bow Shock
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Young Star Binaries
• Most stars (50-60%) form as binary or higher order multiple systems
• Understand young star binary characteristics, particularly disk and mass accretion evolution
• The more massive primary star often has more active mass accretion, indicating a larger circumstellar disk reservoir of mass. I.e., preferential accretion from circumsystem material onto the more massive star in a binary
• Spatially Resolved Observations of Young Star binaries 0.”1 to ~1” separations, Programs ongoing using NIFS, SINFONI & OSIRIS
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Young Star Binaries – Z CMa
• OASIS observations in [OI] 6300A
Garcia et al. “Spatially resolved spectroscopy of Z Canis Majoris components” 1999, A&A v.346, 892
• Protostellar B star (Herbig Be star) primary, FU Ori eruptive variable companion
• System has become a prototype for understanding eruptive mass accretion in young star binaries
0.”1 binary observed with OASIS – 0.”11
microlenses!
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Young Star Binaries – Z CMa
• Keck OSIRIS [Fe II] 1.644m observations of Z CmaWhelan et al. “The 2008 Outburst of Z CMa: The First Detection of Twin
Jets” 2010, ApJL v.720,L119
• The Massive Herbig Be star does drive the parsec scale outflow!•The companion is discovered for the first time to drive its own small scale jet
•First detection of a collimated jet from a FU Ori outbursting variable star!
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High Contrast IFU Spectroscopy in Star Formation – Gas in Circumstellar Disks
HH 30
Dust in Circumstellar Disks – Traced by infrared excessEmission, seen in scattered light images of T Tauri starsGas in Circumstellar Disks – As much as 99% of the mass in circumstellar disks is in GAS not DUST
Disk Gas is traced by:• mm molecular observations of cold outer disk gas• IR emission species trace warm gas from ~terrestrial regions of disks
Most studies cannot spatially resolve the gas in the inner disk regions and measure trace components of the disks, ~70% of the disk by mass is in H2
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The Search for IR Molecular Hydrogen Gas in Young Star Disks
FWHM ~0.”1
Beck et al. “Spatially Resolved Molecular Hydrogen in the Inner 200 AU Environments of T Tauri Stars” 2008 ApJ, v.676, 472
Gemini + NIFS IFU
observations of six T Tauri Stars – all
known to drive YSO outflows
K-band Continuum
Images
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The Search for IR Molecular Hydrogen Gas in Young Star Disks
Herbig Haro Flows
From Classical T Tauri stars w/
outflows, H2 arises from
shocked emission
surrounding the HH flows
Beck et al. “Spatially Resolved Molecular Hydrogen in the Inner 200 AU Environments of T Tauri Stars” 2008 ApJ, v.676, 472
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IFU Observations of T Tau Across a Decade…
Herbst et al. 1996MPE 3D Data from Calar Alto 3.5m
Jan. 1995
Beck et al. 2008NIFS Data from Gemini-N 8m
Oct. 2005
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The Search for Molecular Hydrogen Gas in Young Star
Disks
• VLT + SINFONI Observations of T Tau, detection of H2 from the face-on disk around T Tau N?
Gustofsson et al. “Spatially resolved H2 emission from the disk around T Tau N”
2008
H2 EmissionFlux
H2 Velocity
H2 Velocity Dispersion
T Tau in [Fe II]
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Where is the IR Molecular Hydrogen Gas in Young Star Disks?
• Doing a Gemini + NIFS IFU survey of additional young stars, more than doubling the past sample – this includes stars that have evidence for dust disk gaps (from IR SED shapes), and/or “disk-like” H2 from past long-slit observations
Highlight = GG Tau A, 0.”3 binary young star, with the prototypical “Circumbinary Ring” of dust (Roddier et al. 1996)
Subaru CIAO Observations of GG Tau A
*
Circumbinary Ring seen in scattered light
3”
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of
Classical T Tauri Stars” (in prep.)
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The Search for IR H2 from a Disk High Contrast for Star Formation
NIFS 2.12m continuum image of the 0.”3 GG Tau A binary
IR Spectrum of GG Tau A – typical of young starsBr
H2??
Fe I
Looking for a signal of ~few 100 cts, on a continuum of 30K+ cts, with a photospheric Fe I feature in the way!
H2!!
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The Search for IR Molecular Hydrogen Gas in Young Star Disks
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)
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The Search for IR Molecular Hydrogen Gas in Young Star Disks
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)
H2 Emission in the Environment of GG Tau A
• H2 2-1 S(1) / 1-0 S(1) line ratio not indicative of fluorescent pumping by UV photons, is consistent with X-ray heating of the gas• Gas/Dust in Protostellar binaries should NOT exist (Artymowicz & Lubow 1994):
• Circumstellar: at spatial locations beyond ~1/3 of the semi-major axis of the binary (disk truncation)• Circumbinary: at spatial locations within ~3x the semi-major axis of the binary (gap clearing)
• Clearing timescale ~100’s of years!
H2 1-0 S(1) @ 2.12m
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The Search for IR Molecular Hydrogen Gas in Young Star Disks
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)
H2 1-0 S(1) @ 2.12m
40AU – Pluto’s semi-major axis
H2 1-0 Q(1) @ 2.40m
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Cutting Edge SF Science: Laser-Fed AO Observations of Young Stars
Perrin et al. “Laser Guide Star Adaptive Optics Integral Field Spectroscopy of a Tightly Collimated Bipolar Jet from the Herbig Ae star LkH 233” 2007 ApJ, v.670,
499
• Comparably few detailed spatially resolved observations of collimated outflows toward protostars with higher mass than the sun-like T Tauris.
• Keck Observatory LGS AO + OSIRIS IFU Observations of the very young Herbig Ae star LkH 233
• Investigate whether the similarity on large spatial scales between outflows from T Tauri and Herbig Ae stars still holds true on finer spatial scales.
Pushing to Higher Mass:
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Cutting Edge SF Science: Laser-Fed AO Observations of Young Stars
Perrin et al. “Laser Guide Star Adaptive Optics Integral Field Spectroscopy of a Tightly Collimated Bipolar Jet from the Herbig Ae star LkH 233” 2007 ApJ, v.670,
499
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Cutting Edge SF Science: Laser-Fed AO IFU Observations of Young Stars
• IRAS 04158+2805 = young proto-object in the Taurus SFR (d~140pc)
• Seen in the optical largely in scattered light, with a ‘bipolar’ nebula structure typical of opaque disk material along the mid-plane (Glauser et al. ’08), interpreted as a source with a disk inclined by ~63o
• YOUNG! (<~1Myo!) w./ M6 type, commonly adopted SpT for young BD limit
• HR Diagram fitting = substellar ~0.05Msolar (large uncertainty in models)
• Andrews et al ‘08 detected the disk in sub-mm, high spatial resolution dust continuum and CO gas! extends out to >~500AU from the central source - MASSIVE disk with ~1000+ AU total extent!
• Stellar mass estimate + extended massive disk! – Mdisk / Mstar ~15-20%!
HST Image From Glauser et al. 2008
Beck et al. “Laser Fed Adaptive Optics Imaging Spectroscopy of the CandidateProto-Brown Dwarf IRAS 04158+2805”
in Prep.
Pushing to Lower Mass:
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Laser-fed AO Spectral Imaging, IRAS 04158+2805
– Gemini LGS AO w/ NIFS = Goal - Determine if H2 gas traces disk material in the BD candidate environment - it doesn’t!
– Data reveals fspatially resolved 2-D spectral images of a well collimated jet from a very young BD candidate
– BLUE-shifted, collimated [Fe II] jet associated with the brighter lobe of the scattered light nebulosity - no redshifted jet detected
– Jet Orientation consistent w/ 63o viewing disk inclination
1.644m [Fe II](Jet!)
2m K-band(Scattered Light!)
2.12m H2
(Wide-Angle Outflow!)
100
AU
Beck et al. “Laser Fed Adaptive Optics Imaging Spectroscopy of the CandidateProto-Brown Dwarf IRAS 04158+2805” in Prep.
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Laser-Fed Spectral Imaging of BD Laser-Fed Spectral Imaging of BD EnvironmentsEnvironments
• Laser-Fed AO on large ground-based telescopes is a powerful means to reveal the inner environments of BDs at high spatial resolution using IR emission lines…
• Complication = BDs are optically very faint, but you need an optical tip-tilt guide star! (TTGS)
• Observations of IRAS 04158+2805 were only possible with Gemini +LGS AO because of the nearby r~17.6 magnitude guide star
AO TTGS Area
TTGS r~17.6mag IRAS 04158+2805
K~11.6 mag, R~21
Gemini Observing Tool View
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The Future: SF Science with the JWST and ELT IFUs
FAINTER!FAINTER!More Distant– Probe the Star
formation process to low mass M
stars, approaching the BD limit in the
LMC and SMC!
More Distant– Probe the Star
formation process to low mass M
stars, approaching the BD limit in the
LMC and SMC!
Higher Mass – Massive O&B stars form in very dense
cocoons of gas+dust, pierce
through the extinction to see
the forming stars!
Higher Mass – Massive O&B stars form in very dense
cocoons of gas+dust, pierce
through the extinction to see
the forming stars!
Lower Mass – BDs and Free-Floating Planets in nearby
star forming regions like Taurus
and Orion!
Lower Mass – BDs and Free-Floating Planets in nearby
star forming regions like Taurus
and Orion!
Younger – Sun-Like stars at earlier
epochs of formation – the
“Class I” phase w/ envelope material remaining, or even
younger!
Younger – Sun-Like stars at earlier
epochs of formation – the
“Class I” phase w/ envelope material remaining, or even
younger!
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Spectral Imaging of young Star Spectral Imaging of young Star Environments with Environments with JWSTJWST
• The James Webb Space Telescope - operating at L2 in ~2014
• 6.5m Segmented Primary• 4 Science Instruments:
– NIRCam - Near-InfraRed Camera
– NIRSpec - Near-InfraRed Spectrograph w/ IFU!
– TFI - Tunable Filter Imager– MIRI - Mid-InfraRed
Instrument w/ IFU
The James Webb Space Telescope
NIRSpec and MIRI have Integral Field Units for very sensitive high-contrast spectral imaging of young star environments.
A schematic view of the JWST focal plane, including the placement of the science
entrance apertures for each instrument.
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The Future: SF Science with IFUs on the ELTs
GMT
TMT
Nearby T Tauri stars are bright for large aperture telescopes – but we really need the ELT spatial resolution
to push our observations to the ~Jupiter environs!
When considering properties for IFUs for large telescopes, please don’t forget about star formation science! & Consider
a high spectral resolution IFU mode for the IR…!!
For Kinematics and spectral line detection/characterization, star formation science
greatly benefits from HIGH spectral resolution! (R~20,000 or greater)
Mandell et al. (2009) R~27,000
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The Future: Next Generation Observations of T Tau?
Herbst et al. 1996Data from Jan.
1995 Beck et al. 2008Data from Oct. 2005
?THANKS!! For Your Attention!
Next GenerationIFU View of T Tau