A sextet of clusters in the Vela OB2 region revealed by <i>Gaia</i>

Beccari, G.; Boffin, H. M. J.; Jeřabková, Tereza; Wright, N. J.; Kalari, V.; Carraro, G.; Marchi, Guido De; Wit, W. J. de

doi:10.1093/mnrasl/sly144

Cited by 50 publications

(44 citation statements)

References 19 publications

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“…We utilize densitybased clustering (Ester et al 1996;Kriegel et al 2011) to the data set. It is a general statistical method that recently has begun to be applied to classify astronomical sources in a multidimensional data space (e.g., Beccari et al 2018Beccari et al , 2020Jerabkova et al 2019). This method can identify clusters in a multidimensional space not only for their crests but also for their spatial extent, without assuming that their underlying spatial structures are filamentary or clumpy.…”

Section: Appendix D Identification Of Emission Features Using Densitymentioning

confidence: 99%

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Doi¹,

Hasegawa

Furuya

et al. 2020

ApJ

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We present new observations of the active star formation region NGC 1333 in the Perseus molecular cloud complex from the James Clerk Maxwell Telescope B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. The BISTRO data cover the entire NGC 1333 complex (∼1.5 pc×2 pc) at 0.02 pc resolution and spatially resolve the polarized emission from individual filamentary structures for the first time. The inferred magnetic field structure is complex as a whole, with each individual filament aligned at different position angles relative to the local field orientation. We combine the BISTRO data with low-and high-resolution data derived from Planck and interferometers to study the multiscale magnetic field structure in this region. The magnetic field morphology drastically changes below a scale of ∼1 pc and remains continuous from the scales of filaments (∼0.1 pc) to that of protostellar envelopes (∼0.005 pc or ∼1000 au). Finally, we construct simple models in which we assume that the magnetic field is always perpendicular to the long axis of the filaments. We demonstrate that the observed variation of the relative orientation between the filament axes and the magnetic field angles are well reproduced by this model, taking into account the projection effects of the magnetic field and filaments relative to the plane of the sky. These projection effects may explain the apparent complexity of the magnetic field structure observed at the resolution of BISTRO data toward the filament network.

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Section: Appendix D Identification Of Emission Features Using Densitymentioning

confidence: 99%

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Doi¹,

Hasegawa

Furuya

et al. 2020

ApJ

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“…As mentioned previously, the Vela OB2 region has been recently the subject of several works aimed at studying the complexity of the stellar populations in the region. In Beccari et al (2018) we demonstrated that NGC 2457 and the cluster around the Wolf-Rayet Star γ 2 Vel belong to a complex constellation of sub-populations confined in a region of ∼100 pc 3 of volume. Later, Cantat-Gaudin et al (2019b) extended the study on a wider area of sky in a range of distances from ∼250 to ∼550 pc.…”

Section: Relic Stellar Filamentmentioning

confidence: 87%

“…Along this line, the Vela OB2 association has recently revealed to be one of the best test-bench to study the early stages of clustered star formation (SF) at ages 10 to 35 Myr. Using a combination of Gaia DR2 astrometric information and accurate photometry, Beccari et al (2018) recently studied a 10 × 5 deg region around the Wolf-Rayet Star γ 2 Vel, including the well known clusters Gamma Vel and NGC2547. They discovered an assembly of six clusters.…”

Section: Introductionmentioning

confidence: 99%

Uncovering a 260 pc wide, 35-Myr-old filamentary relic of star formation

Beccari

Boffin

Jeřabková

2019

Monthly Notices of the Royal Astronomical Society

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Several recent studies have shown that the Vela OB2 region hosts a complex constellation of sub-populations with ages in the range 10 to 50 Myr. Such populations might represent the best example of the outcome of clustered star formation in Giant Molecular clouds (GMC). We use Gaia DR2 data over an area of 40 deg radius around the open cluster Collinder 135 to extend the study of the stellar populations of the Vela OB2 region over an area of several hundreds of parsecs on sky. Detailed clustering algorithms combined with the exquisite astrometric quality of the GAIA catalogue allow us to detect a new cluster named BBJ 1 that shows the same age as NGC 2547 (30 to 35 Myr), but located at a distance of 260 pc from it. Deeper investigation of the region via clustering in 5D parameter space and in the colour-magnitude diagram allows us to detect a filamentary structure of stars that bridges the two clusters. Given the extent in space of such structure (260 pc) and the young age (∼35 Myr), we exclude that such population originates by the same mechanism responsible to create tidal streams around older clusters. Even if we miss a complete picture of the 3D motion of the studied stellar structure because of the lack of accurate radial velocity measurements, we propose that such structure represent the detection of a 35 Myr old outcome of a mechanism of filamentary star formation in a GMC.

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“…Jeffries et al (2014) and Prisinzano et al (2016) estimate the mass of the cluster to be 100 M . Another cluster within the association, the P Puppis cluster, was identified by Caballero & Dinis (2008) and later by Beccari et al (2018).…”

Section: Structure and Agesmentioning

confidence: 99%

OB Associations and their origins

Wright

2020

New Astronomy Reviews

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OB associations are unbound groups of young stars made prominent by their bright OB members, and have long been thought to be the expanded remnants of dense star clusters. They have been important in astrophysics for over a century thanks to their luminous massive stars, though their low-mass members have not been well studied until the last couple of decades. This has changed thanks to data from X-ray observations, spectroscopic surveys and astrometry from Gaia that allows their full stellar content to be identified and their dynamics to be studied, which in turn is leading to changes in our understanding of these systems and their origins, with the old picture of Blaauw (1964a) now being superseded. It is clear now that OB associations have considerably more substructure than once envisioned, both spatially, kinematically and temporally. These changes have implications for the star formation process, the formation and evolution of planetary systems, and the build-up of stellar populations across galaxies.

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A sextet of clusters in the Vela OB2 region revealed by Gaia

Cited by 50 publications

References 19 publications

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Uncovering a 260 pc wide, 35-Myr-old filamentary relic of star formation

OB Associations and their origins

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