3D shape of Orion A from <i>Gaia</i> DR2

Großschedl, Josefa E.; Alves, J.; Meingast, Stefan; Ackerl, Christine; Ascenso, Joana; Bouy, H.; Burkert, Andreas; Forbrich, Jan; Fürnkranz, Verena; Goodman, Alyssa A.; Hacar, A.; Herbst-Kiss, Gabor; Lada, Charles J.; Larreina, Irati; Leschinski, Kieran; Lombardi, Marco; Moitinho, A.; Mortimer, Daniel J.; Zari, E.

doi:10.1051/0004-6361/201833901

Cited by 158 publications

(176 citation statements)

References 43 publications

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“…The DBSCAN groups associated with the Orion A molecular cloud are those labelled B 1 , C, and D. Group B 1 and C nearly occupy the same position in the sky and share very similar kinematic properties (see Table 1), however they are at different distances, with group B 1 being closer to the Sun than group C. This poses interesting questions about their origin: the two groups might be identified separately by DBSCAN just because of a local under-density of sources. In this case, the Orion A cloud would be even more elongated along the line of sight than previously thought (Großschedl et al 2018). The radial velocities of the embedded sources in the Orion A molecular cloud are tightly related to the motion of the molecular gas in the cloud (Hacar et al 2016).…”

Section: Orion Amentioning

confidence: 73%

Structure, kinematics, and ages of the young stellar populations in the Orion region

Zari

Brown

Zeeuw

2019

A&A

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We present a study of the three dimensional structure, kinematics, and age distribution of the Orion OB association, based on the second data release of the Gaia satellite (Gaia DR2). Our goal is to obtain a complete picture of the star formation history of the Orion complex and to relate our findings to theories of sequential and triggered star formation. We select the Orion population with simple photometric criteria, and we construct a three dimensional map in galactic Cartesian coordinates to study the physical arrangement of the stellar clusters in the Orion region. The map shows structures that extend for roughly 150 pc along the line of sight, divided in multiple sub-clusters. We separate different groups by using the density based clustering algorithm DBSCAN. We study the kinematic properties of all the groups found by DBSCAN first by inspecting their proper motion distribution, and then by applying a kinematic modelling code based on an iterative maximum likelihood approach, which we use to derive their mean velocity, velocity dispersion and isotropic expansion. By using an isochrone fitting procedure we provide ages and extinction values for all the groups. We confirm the presence of an old population (∼ 15 Myr) towards the 25 Ori region, and we find that groups with ages of 12 − 15 Myr are present also towards the Belt region. We notice the presence of a population of ∼ 10 Myr also in front of the Orion A molecular cloud. Our findings suggest that star formation in Orion does not follow a simple sequential scenario, but instead consists of multiple events, which caused kinematic and physical sub-structure. To fully explain the detailed sequence of events, specific simulations and further radial velocity data are needed.

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Section: Orion Amentioning

confidence: 73%

Structure, kinematics, and ages of the young stellar populations in the Orion region

Zari

Brown

Zeeuw

2019

A&A

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“…Target selection OMC-2/3 is part of the Orion A molecular complex and is composed of two major molecular clouds, OMC-2 and OMC-3. Those two clouds form a filament-shaped region located between the Trapezium OB stellar cluster and the NGC1977 HII region, at a distance of (393±25) pc from the Sun (Großschedl et al 2018). OMC-2 lies to the north of OMC-1, which is the molecular cloud associated with the Orion Nebula, and was identified by Gatley et al (1974).…”

Section: Targeted Sources and Molecular Tracersmentioning

confidence: 78%

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

Bouvier

López-Sepulcre

Ceccarelli

et al. 2020

A&A

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Context. Solar-like protostars are known to be chemically rich, but it is not yet clear how much their chemical composition can vary and why. So far, two chemically distinct types of Solar-like protostars have been identified: hot corinos, which are enriched in interstellar Complex Organic Molecules (iCOMs), such as methanol (CH 3 OH) or dimethyl ether (CH 3 OCH 3 ), and Warm Carbon Chain Chemistry (WCCC) objects, which are enriched in carbon chain molecules, such as butadiynyl (C 4 H) or ethynyl radical (CCH). However, none of these have been studied so far in environments similar to that in which our Sun was born, that is, one that is close to massive stars. Aims. In this work, we search for hot corinos and WCCC objects in the closest analogue to the Sun's birth environment, the Orion Molecular Cloud 2/3 (OMC-2/3) filament located in the Orion A molecular cloud. Methods. We obtained single-dish observations of CCH and CH 3 OH line emission towards nine Solar-like protostars in this region. As in other, similar studies of late, we used the [CCH]/[CH 3 OH] abundance ratio in order to determine the chemical nature of our protostar sample. Results. Unexpectedly, we found that the observed methanol and ethynyl radical emission (over a few thousands au scale) does not seem to originate from the protostars but rather from the parental cloud and its photo-dissociation region, illuminated by the OB stars of the region. Conclusions. Our results strongly suggest that caution should be taken before using [CCH]/[CH 3 OH] from single-dish observations as an indicator of the protostellar chemical nature and that there is a need for other tracers or high angular resolution observations for probing the inner protostellar layers.

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“…Orion Complex: V883 Ori, FU Ori, V2775 Ori, and IRAS 05450+0019 are located in the Orion complex. V883 Ori is located in the head of the Orion A cloud, south of the Orion Nebula Cluster, in a region where stars have an average parallax of 2.50 mas (Großschedl et al 2018), corresponding to a distance of 392 pc. FU Ori is located in the λ Ori region, which has a Gaia-based distance of 404 pc from Kounkel et al (2018).…”

Section: A1 Detected Sourcesmentioning

confidence: 99%

“…FU Ori is located in the λ Ori region, which has a Gaia-based distance of 404 pc from Kounkel et al (2018). V2775 Orionis is located in the L1641 region, near the tail of Orion A, in a region with an average parallax of 2.35 mas Großschedl et al (2018), corresponding to a distance 416 pc. IRAS 05450+0019 is located in NGC 2071.…”

Section: A1 Detected Sourcesmentioning

confidence: 99%

A Comparison of the X-Ray Properties of FU Ori-type Stars to Generic Young Stellar Objects

Kuhn

Hillenbrand

2019

ApJ

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Like other young stellar objects (YSOs), FU Ori-type stars have been detected as strong X-ray emitters. However, little is known about how the outbursts of these stars affect their X-ray properties. We assemble available X-ray data from XMM Newton and Chandra observations of 16 FU Ori stars, including a new XMM Newton observation of Gaia 17bpi during its optical rise phase. Of these stars, six were detected at least once, while 10 were non-detections, for which we calculate upper limits on intrinsic X-ray luminosity (L X ) as a function of plasma temperature (kT ) and column density (N H ). The detected FU Ori stars tend to be more X-ray luminous than typical for non-outbursting YSOs, based on comparison to a sample of low-mass stars in the Orion Nebula Cluster. FU Ori stars with high L X have been observed both at the onset of their outbursts and decades later. We use the Kaplan-Meier estimator to investigate whether the higher X-ray luminosities for FU Ori stars is characteristic or a result of selection effects, and we find the difference to be statistically significant (p < 0.01) even when non-detections are taken into account. The additional X-ray luminosity of FU Ori stars relative to non-outbursting YSOs cannot be explained by accretion shocks, given the high observed plasma temperatures. This suggests that, for many FU Ori stars, either 1) the outburst leads to a restructuring of the magnetosphere in a way that enhances X-ray emission, or 2) FU Ori outbursts are more likely to occur among YSOs with the highest quiescent X-ray luminosity.

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3D shape of Orion A from Gaia DR2

Cited by 158 publications

References 43 publications

Structure, kinematics, and ages of the young stellar populations in the Orion region

Structure, kinematics, and ages of the young stellar populations in the Orion region

Hunting for hot corinos and WCCC sources in the OMC-2/3 filament

A Comparison of the X-Ray Properties of FU Ori-type Stars to Generic Young Stellar Objects

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