carma mm view over three selected star-forming regions...
TRANSCRIPT
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CARMA mm view over three selected star-forming regions: intrigues of outflow activity
Manuel Fernández-López
University of Illinois at Urbana-Champaign
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CARMA mm view over three selected star-forming regions: intrigues of outflow activity
Manuel Fernández-López
University of Illinois at Urbana-Champaign
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CARMA mm view over two selected star-forming regions: intrigues of outflow activity
Manuel Fernández-López
University of Illinois at Urbana-Champaign
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CONTENTS
1. Mm observations of the molecular outflows toward GGD27 (IRAS 1812-2048): a high mass star-forming region
2. L1157: possible multiple jets from a Class 0 protostar
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1st round: CARMA vs GGD27
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Massive starsMassive stars: >8 MΘ and >104 LΘ
Form HII regions (photodisociate & ionize)
Inject large scale turbulence
Could trigger star formation
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Massive starsBefore SN >> form isotopes up to 56Fe
During explosion >> formation of heavier isotopes
SN model ISM & could also trigger star formation
Black holes
Profound impact on the life of galaxies
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Outflows from Nearby High-mass stars
Nearest massive protostars:
- Orion KL: explosive outflow?- Cepheus A: precessing/pulsating outflow?
As detail increases, complexity increases.Protostar interaction yields dynamical effects in molecular outflows and jets.
Close interactions between protostars.Revisiting the problem of accretion vs mergers.
Our approach: Detailed study of outflows from nearby regions like GGD27 (d < 2kpc; 1” < 2000 AU).
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HH80-81/GGD27: summary
Martí et al. 1993; Qiu et al. 2008
Very large
>10 pc at
1.7 kpc
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Carrasco-González et al. (2012)
HH80-81/GGD27: summary
Green lines indicate magnetic field direction inferred by the polarization of the synchrotron emission.
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Linz et al. 2003
Aspin et al. 1991 (UKIT, 3.8m)
HH80-81/GGD27: summary
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1.3mm
-two main sources (luminosidad)
-compact and extended emission: different evolutive stages
Fernández-López et al. 2011 (a)
HH80-81/GGD27: summary
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Asymmetric Outflows
(Fernández-López et al. 2013 submitted)
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•Characterization of the outflows:
•
Asymmetric Outflows
- 2 apparently monopolar molecular outflows detected in CO, SiO, HCN and HCO+.
- HH80-81 undetected, just some emission associated with reflection nebula.
- Origin close to MM2.
- Physical properties from monopolar outflows similar to massive protostars (energy, momentum, luminosity).
- Possible SW counterpart for the NE monopolar outflow.
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•CO(3-2)
•
Collaborators:M. Fernández-LópezJ.M. Girart (ICE-CSIC), S. Curiel (IA-UNAM), L.A. Zapata (CryA-UNAM), P. Fonfria (IA-UNAM), K. Qiu (Nanjing U.)
Asymmetric Outflows
- Origin of SE outflow at MM2(E) position.
- Chemical differences with other outflows of the region.
- Possible link between SE and NW monopolar outflows (deflection?).
- Precession of SE outflow.
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2nd round: CARMA vs L1157
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L1157
Gueth et al. 1997
- Classical molecular outflow from a Class 0 protostar.••- A high velocity bipolar outflow drags a cavity and what we see is the limb brightened lobes ?••
•
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L1157
Bachiller et al. 2001 •- A bipolar precessing jet along with a wide open and slow wind
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L1157Looney et al. 2007
Kwon et al. 2013 (in prep.)
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L1157
•-CO (2-1):
0.5km/s per channel and 5”~1000AU
-High velocity gas“fingers” clearly indicating:
ballistic ejections
&
precession
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L1157
•-CO (2-1):
0.5km/s per channel and 5”~1000AU
-High velocity gas“fingers” clearly indicating:
ballistic ejections
&
precession
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L1157•2011 CARMA SUMMER SCHOOL DATA•(Ian Stephens and • Dick Plambeck)•- Outflow rotation just in the inner parts of the system?
- Theoretical problems for outflow rotation far away from the protostar:Soker (2005), Belloche et al. (2013), Soker (2013, 2 arXivs),Cantó & Raga (priv. com.)
- Can magnetic fields from the protostar produce an rotation in the outflow ~2500AU away?
- Alternatives to explain the velocity gradient perpendicular to the jet axis?
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L1157
- Multiple outflow in the literature: Soker et al. (2012, 2013, arXiv) Klaasen et al. (2013)
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L1157
- Multiple ejection jet model.
- Model of precessing jet based on Raga et al. (2009) for each jet (no orbital motion included).
- In principle, precession does not require a binary star.
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L1157
•
Collaborators:W. Kwon (U.Groningen),M. Fernández-López (UIUC)I. Stephens (UIUC),L. Looney (UIUC)
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L1157
• Two independent fits
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THANKS
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Conclusions L1157
- Evidences for a ballistic and precessing jet
- Some possibilities to explain CO(2-1) emission:
•- Jet + limb brightening of the dragged cavity••- Jet + open angle slower wind ••- Rotating molecular outflow (explain only the inner part)••- Multiple jet ejection model