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 starsMassive stars: >8 MΘ and >104 LΘ

Form HII regions (photodisociate & ionize)

Inject large scale turbulence

Could trigger star formation

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

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

Martí et al. 1993; Qiu et al. 2008

Very large

>10 pc at

1.7 kpc

Carrasco-González et al. (2012)

HH80-81/GGD27: summary

Green lines indicate magnetic field direction inferred by the polarization of the synchrotron emission.

Linz et al. 2003

Aspin et al. 1991 (UKIT, 3.8m)‏

HH80-81/GGD27: summary

1.3mm

-two main sources (luminosidad)‏

-compact and extended emission: different evolutive stages

Fernández-López et al. 2011 (a)

HH80-81/GGD27: summary

Asymmetric Outflows

(Fernández-López et al. 2013 submitted)

•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.

•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.

2nd round: CARMA vs L1157

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 ?••

•

L1157

Bachiller et al. 2001 •- A bipolar precessing jet along with a wide open and slow wind

L1157Looney 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