VISION – Vienna survey in Orion

Großschedl, Josefa E.; Alves, J.; Teixeira, P. S.; Bouy, H.; Forbrich, Jan; Lada, Charles J.; Meingast, Stefan; Hacar, A.; Ascenso, Joana; Ackerl, Christine; Hasenberger, Birgit; Köhler, Rainer H.; Kubiak, Karolina; Larreina, Irati; Linhardt, Lorenz; Lombardi, Marco; Möller, Torsten B.

doi:10.1051/0004-6361/201832577

Cited by 56 publications

(77 citation statements)

References 106 publications

(150 reference statements)

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“…The average fraction of disk-bearing stars in the ONC in the full catalog of 5988 stars, with the sources with disks identified by Megeath et al (2012) and Großschedl et al (2019) is ∼50% (which is consistent with e.g., Mamajek 2009), though the extinction results in a bias against reliable measurements of parallaxes and proper motions with Gaia compared to their diskless and less dusty counterparts. Thus out of 1871 stars in the final sample, only ∼40% have disks.…”

Section: Discussionsupporting

confidence: 82%

Runaway Young Stars near the Orion Nebula

McBride

Kounkel

2019

ApJ

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The star forming region of the Orion Nebula (ONC) is ideal to study the stellar dynamics of young stars in a clustered environment. Using Gaia DR2 we search for the pre-main sequence stars with unusually high proper motions that may be representative of a dynamical ejection from unstable young triple systems or other close three-body encounters. We identify twenty-six candidate stars that are likely to have had such an encounter in the last 1 Myr. Nine of these stars could be traced back to the densest central-most region of the ONC, the Trapezium, while five others have likely interactions with other OB-type stars in the cluster. Seven stars originate from other nearby populations within the Orion Complex that coincidentally scattered towards the ONC. A definitive point of origin cannot be identified for the remaining sources. These observations shed light on the frequency of the ejection events in young clusters.

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Section: Discussionsupporting

confidence: 82%

Runaway Young Stars near the Orion Nebula

McBride

Kounkel

2019

ApJ

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“…OMC1, including the Trapezium cluster, is the nearest site of active intermediate-and high-mass star formation (e.g., Hillenbrand 1997;Megeath et al 2012Megeath et al , 2016Da Rio et al 2014;Großschedl et al 2019 for discussions of the stellar content).…”

Section: Discussionmentioning

confidence: 99%

Expanding bubbles in Orion A: [C II] observations of M 42, M 43, and NGC 1977

Pabst

Goicoechea

Teyssier

et al. 2020

A&A

123

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Context. The Orion Molecular Cloud is the nearest massive-star forming region. Massive stars have profound effects on their environment due to their strong radiation fields and stellar winds. Stellar feedback is one of the most crucial cosmological parameters that determine the properties and evolution of the interstellar medium in galaxies. Aims. We aim to understand the role that feedback by stellar winds and radiation play in the evolution of the interstellar medium. Velocity-resolved observations of the [C II] 158 μm fine-structure line allow us to study the kinematics of UV-illuminated gas. Here, we present a square-degree-sized map of [C II] emission from the Orion Nebula complex at a spatial resolution of 16′′ and high spectral resolution of 0.2 km s−1, covering the entire Orion Nebula (M 42) plus M 43 and the nebulae NGC 1973, 1975, and 1977 to the north. We compare the stellar characteristics of these three regions with the kinematics of the expanding bubbles surrounding them. Methods. We use [C II] 158 μm line observations over an area of 1.2 deg2 in the Orion Nebula complex obtained by the upGREAT instrument onboard SOFIA. Results. The bubble blown by the O7V star θ1 Ori C in the Orion Nebula expands rapidly, at 13 km s−1. Simple analytical models reproduce the characteristics of the hot interior gas and the neutral shell of this wind-blown bubble and give us an estimate of the expansion time of 0.2 Myr. M 43 with the B0.5V star NU Ori also exhibits an expanding bubble structure, with an expansion velocity of 6 km s−1. Comparison with analytical models for the pressure-driven expansion of H II regions gives an age estimate of 0.02 Myr. The bubble surrounding NGC 1973, 1975, and 1977 with the central B1V star 42 Orionis expands at 1.5 km s−1, likely due to the over-pressurized ionized gas as in the case of M 43. We derive an age of 0.4 Myr for this structure. Conclusions. We conclude that the bubble of the Orion Nebula is driven by the mechanical energy input by the strong stellar wind from θ1 Ori C, while the bubbles associated with M 43 and NGC 1977 are caused by the thermal expansion of the gas ionized by their central later-type massive stars.

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“…4. The western region contains the KL-BN region and most of the YSOs in Orion A (Großschedl et al 2019), the center region contains most of the L1641 dark cloud (Polychroni et al 2013), and finally, the eastern region contains the L1647 dark cloud. Although the western and eastern regions have known differences in terms of the slope of their N H distribution and number of Class 0 protostars (Stutz & Kainulainen 2015), their behavior in terms of the relative orientation between N H and B ⊥ is very similar.…”

Section: Orionmentioning

confidence: 99%

Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure

Soler

2019

A&A

103

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We present a study of the relative orientation between the magnetic field projected onto the plane of sky (B ⊥ ) on scales down to 0.4 pc, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the distribution of gas column density (N H ) structures on scales down to 0.026 pc, derived from the observations by Herschel in submillimeter wavelengths, toward ten nearby (d < 450 pc) molecular clouds. Using the histogram of relative orientation technique in combination with tools from circular statistics, we found that the mean relative orientation between N H and B ⊥ toward these regions increases progressively from 0 • , where the N H structures lie mostly parallel to B ⊥ , with increasing N H , in many cases reaching 90 • , where the N H structures lie mostly perpendicular to B ⊥ . We also compared the relative orientation between N H and B ⊥ and the distribution of N H , which is characterized by the slope of the tail of the N H probability density functions (PDFs). We found that the slopes of the N H PDF tail are steepest in regions where N H and B ⊥ are close to perpendicular. This coupling between the N H distribution and the magnetic field suggests that the magnetic fields play a significant role in structuring the interstellar medium in and around molecular clouds. However, we found no evident correlation between the star formation rates, estimated from the counts of young stellar objects, and the relative orientation between N H and B ⊥ in these regions.

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VISION – Vienna survey in Orion

Cited by 56 publications

References 106 publications

Runaway Young Stars near the Orion Nebula

Runaway Young Stars near the Orion Nebula

Expanding bubbles in Orion A: [C II] observations of M 42, M 43, and NGC 1977

Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure

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VISION – Vienna survey in Orion

Cited by 56 publications

References 106 publications

Runaway Young Stars near the Orion Nebula

Runaway Young Stars near the Orion Nebula

Expanding bubbles in Orion A: [C II] observations of M 42, M 43, and NGC 1977

Using Herschel and Planck observations to delineate the role of magnetic fields in molecular cloud structure

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Expanding bubbles in Orion A: [C II] observations of M 42, M 43, and NGC 1977