3D shape explains star formation mystery of California and Orion A

Abstract

The new Gaia data release (EDR3) with improved astrometry has opened a new era in studying our Milky Way in fine detail. We use Gaia EDR3 astrometry together with 2MASS and WISE photometry to study two of the most massive molecular clouds in the solar vicinity: Orion A and California. Despite having remarkable similarities in the plane of the sky in terms of shape, size, and extinction, California has an order of magnitude lower star formation efficiency. We use our state-of-the-art dust mapping technique to derive the detailed three-dimensional (3D) structure of the two clouds, taking into account both distance and extinction uncertainties, and a full 3D spatial correlation between neighbouring points. We discover that, despite the apparent filamentary structure in the plane of the sky, California is a flat 120-pc-long sheet extending from 410 to 530 $pc$. We show that not only Orion A and California differ substantially in their 3D shapes, but also Orion A has considerably higher density substructures in 3D than California. This result presents a compelling reason why the two clouds have different star formation activities. We also demonstrate how the viewing angle of California can substantially change the cloud's position in the Kennicutt-Schmidt relation. This underlines the importance of 3D information in interpreting star formation relations and challenges studies that rely solely on the column density thresholds to determine star formation activities in molecular clouds. Finally, we provide accurate distance estimates to multiple lines of sight towards various parts of the two clouds.

Accepted for publication in ApJ Letters

References in corpus (10)

• The Gaia mission
• Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3
• A Compendium of Distances to Molecular Clouds in the Star Formation Handbook
• Resolving nearby dust clouds
• On the Three-Dimensional Structure of Local Molecular Clouds
• 3D Dust Mapping Reveals that Orion Forms Part of a Large Ring of Dust
• Inferring the three-dimensional distribution of dust in the Galaxy with a non-parametric method: Preparing for Gaia
• Detailed 3D structure of OrionA in dust with Gaia DR2
• Relationship between turbulence energy and density variance in the Solar neighbourhood molecular clouds
• The effect of viewing angle on the Kennicutt-Schmidt relation of the local molecular clouds

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