Molecular outflows associated with young stellar objects in the L1641 region of Orion

Morgan, James A.; Schloerb, F. P.; Snell, R. L.; Bally, John

doi:10.1086/170310

Cited by 38 publications

(44 citation statements)

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“…Indicates whether the YSO drives a known jet or CO outflow (Morgan et al 1991;Dent et al 1998;Allen & Davis 2008;Davis et al 2009, and this paper).…”

Section: Stellar Spectral Typesmentioning

confidence: 99%

POISSON project

Garatti

Lopez

Antoniucci

et al. 2012

A&A

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Context. Characterising stellar and circumstellar properties of embedded young stellar objects (YSOs) is mandatory for understanding the early stages of the stellar evolution. This task requires the combination of both spectroscopy and photometry, covering the widest possible wavelength range, to disentangle the various protostellar components and activities. Aims. As part of the POISSON project (Protostellar Optical-Infrared Spectral Survey On NTT), we present a multi-wavelength spectroscopic and photometric investigation of embedded YSOs in L 1641, aimed to derive the stellar parameters and evolutionary stages and to infer their accretion properties. Methods. Our multi-wavelength database includes low-resolution optical-IR spectra from the NTT and Spitzer (0.6−40 μm) and photometric data covering a spectral range from 0.4 to 1100 μm, which allow us to construct the YSOs spectral energy distributions (SEDs) and to infer the main stellar parameters (visual extinction, spectral type, accretion, stellar, bolometric luminosity, mass accretion, and ejection rates). Results. The NTT optical-NIR spectra are rich in emission lines, which are mostly associated with YSO accretion, ejection, and chromospheric activities. A few emission lines, prominent ice (H 2 O and CO 2 ), and amorphous silicate absorption features have also been detected in the Spitzer spectra. The SED analysis allows us to group our 27 YSOs into nine Class I, eleven Flat, and seven Class II objects. However, on the basis of the derived stellar properties, only six Class I YSOs have an age of ∼10 5 yr, while the others are older (5 × 10 5 −10 6 yr), and, among the Flat sources, three out of eleven are more evolved objects (5 × 10 6 −10 7 yr), indicating that geometrical effects can significantly modify the SED shapes. Inferred mass accretion rates (Ṁ acc ) show a wide range of values (3.6 × 10 −9 to 1.2 × 10 −5 M yr −1 ), which reflects the age spread observed in our sample well. Average values of mass accretion rates, extinction, and spectral indices decrease with the YSO class. The youngest YSOs have the highestṀ acc , whereas the oldest YSOs do not show any detectable jet activity in either images and spectra. Apart from the outbursting source #25 and, marginally, #20, none of the remaining YSOs is accretion-dominated (L acc > L * ). We also observe a clear correlation among the YSOṀ acc , M * , and age. For YSOs with t > 10 5 yr and 0.4 M ≤ M * ≤ 1.2 M , a relationship betweenṀ acc and t (Ṁ acc ∝ t −1.2 ) has been inferred, consistent with mass accretion evolution in viscous disc models and indicating that the mass accretion decay is slower than previously assumed. Finally, our results suggest that episodic outbursts are required for Class I YSOs to reach typical classical T Tauri stars stellar masses.

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“…Indicates whether the YSO drives a known jet or CO outflow (Morgan et al 1991;Dent et al 1998;Allen & Davis 2008;Davis et al 2009, and this paper).…”

Section: Stellar Spectral Typesmentioning

confidence: 99%

POISSON project

Garatti

Lopez

Antoniucci

et al. 2012

A&A

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“…Position refers to the candidate driving source. 59: The H 2 features SMZ 5-28 and SMZ 6-1 form the infrared counterpart to the north-south bipolar molecular outflow V 380 Ori NE (Levreault 1988;Morgan et al 1991;Davis et al 2000). These features indicate the presence of a wellcollimated, precessing jet.…”

mentioning

confidence: 96%

An unbiased H₂survey for protostellar jets in Orion A

Stanke

McCaughrean

Zinnecker

2002

A&A

135

216

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Abstract.We have made an unbiased imaging survey of a 1.2 square degree area in the Orion A giant molecular cloud searching for molecular hydrogen emission line features seen in the v = 1-0 S(1) line at a wavelength of 2.12 µm originating in shocks in outflows from young stellar objects. This survey provides for the first time an unbiased census of outflows over a significant portion of a giant molecular cloud, and yields a sample of outflows free from selection effects and with all objects located at roughly the same, well-known distance. In this paper, we present the data gathered in the course of the survey, provide a comprehensive list of all molecular hydrogen emission features found, and give a list of the 76 candidate outflows identified in the data set.

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“…These stars generally have luminosities in the range 1-250 L 0 , suggesting that predominantly low mass stars (M ~ 3M 0 ) are forming in this part of the cloud. This has been confirmed by radio continuum measurements in the cloud (Morgan et al 1990) which failed to detect any more luminous embedded sources. L1641 contains a larger percentage of class I (steep far-infrared spectrum) sources than the Taurus-Auriga dark cloud.…”

Section: (4b) Star Formation In the L1641 Dark Cloudmentioning

confidence: 58%

“…At least ten molecular outflows are known within the L1641 cloud (Fukui et al 1986;Levreault 1988;Morgan and Bally 1991;Morgan et al 1991), as well as numerous Herbig-Haro objects. Strom et al (1986) originally suggested that the molecular outflows known then, and the identified Herbig-Haro objects, aligned with the cloud magnetic field and the long dimension of the cloud.…”

Section: (4b) Star Formation In the L1641 Dark Cloudmentioning

confidence: 99%

“…Strom et al (1986) originally suggested that the molecular outflows known then, and the identified Herbig-Haro objects, aligned with the cloud magnetic field and the long dimension of the cloud. The discovery of further molecular outflows Morgan et al 1991) and the clearer understanding of the magnetic field geometry in the cloud (discussed above) negate this result. It is now apparent that outflow phenomena in the L1641 cloud are not directed along a preferred direction.…”

Section: (4b) Star Formation In the L1641 Dark Cloudmentioning

confidence: 99%

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Star Formation in the Galaxy

McGregor¹

1992

Aust. J. Phys.

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Star formation in the Galaxy occurs on different spatial scales from single star formation events in Bok Globules to the formation of OB associations and star clusters. We review recent observations of Bok Globules and relate them to the dense NH3 cores observed in dark clouds. Recent work on the Chamaeleon I dark cloud supports quasi-static subcritical collapse models for low mass star formation. This cloud is a typical region of low mass star formation similar to the Taurus-Auriga clouds; star formation has continued in the cloud for ",107 yr, the most massive embedded stars have masses of "'2M0, and the cloud appears to be magnetically supported in its long dimension.

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Molecular outflows associated with young stellar objects in the L1641 region of Orion

Cited by 38 publications

References 0 publications

POISSON project

POISSON project

An unbiased H₂survey for protostellar jets in Orion A

Star Formation in the Galaxy

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Molecular outflows associated with young stellar objects in the L1641 region of Orion

Cited by 38 publications

References 0 publications

POISSON project

POISSON project

An unbiased H2survey for protostellar jets in Orion A

Star Formation in the Galaxy

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An unbiased H₂survey for protostellar jets in Orion A