CARMA mm view over three selected star-forming regions: intrigues of outflow activity
Manuel Fernández-López
University of Illinois at Urbana-Champaign CARMA mm view over three selected star-forming regions: intrigues of outflow activity
Manuel Fernández-López
University of Illinois at Urbana-Champaign CARMA mm view over two selected star-forming regions: intrigues of outflow activity
Manuel Fernández-López
University of Illinois at Urbana-Champaign 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 1st round: CARMA vs GGD27 Massive stars
4 Massive stars: >8 MΘ and >10 LΘ Form HII regions (photodisociate & ionize) Inject large scale turbulence Could trigger star formation Massive stars
Before 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 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). HH80-81/GGD27: summary
Very large >10 pc at Martí et al. 1993; Qiu et al. 2008 1.7 kpc HH80-81/GGD27: summary
Carrasco-González et al. (2012)
Green lines indicate magnetic field direction inferred by the polarization of the synchrotron emission. HH80-81/GGD27: summary
Aspin et al. 1991 (UKIT, 3.8m)
Linz et al. 2003 HH80-81/GGD27: summary
Fernández-López et al. 2011 (a)
1.3mm
-two main sources (luminosidad) -compact and extended emission: different evolutive stages Asymmetric Outflows
(Fernández-López et al. 2013 submitted) Asymmetric Outflows
•Characterization of the 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. Asymmetric Outflows
•CO(3-2) - 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.
Collaborators: M. Fernández-López J.M. Girart (ICE-CSIC), S. Curiel (IA-UNAM), L.A. Zapata (CryA-UNAM), P. Fonfria (IA-UNAM), K. Qiu (Nanjing U.) 2nd round: CARMA vs L1157 L1157
- 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 ? • • •
Gueth et al. 1997 L1157
•- A bipolar precessing jet along with a wide Bachiller et al. 2001 open and slow wind L1157
Looney et al. 2007
Kwon et al. 2013 (in prep.) L1157
• -CO (2-1): 0.5km/s per channel and 5”~1000AU
-High velocity gas “fingers” clearly indicating: ballistic ejections & precession L1157
• -CO (2-1): 0.5km/s per channel and 5”~1000AU
-High velocity gas “fingers” clearly indicating: ballistic ejections & precession 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? L1157
- Multiple outflow in the literature: Soker et al. (2012, 2013, arXiv) Klaasen et al. (2013) 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. L1157
•
Collaborators: W. Kwon (U.Groningen), M. Fernández-López (UIUC) I. Stephens (UIUC), L. Looney (UIUC) L1157
• Two independent fits THANKS 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