dc.contributor.author | Grossschedl, Josefa E. | |
dc.contributor.author | Alves, Joao | |
dc.contributor.author | Meingast, Stefan | |
dc.contributor.author | Ackerl, Christine | |
dc.contributor.author | Ascenso, Joana | |
dc.contributor.author | Bouy, Herve | |
dc.contributor.author | Burkert, Andreas | |
dc.contributor.author | Forbrich, Jan | |
dc.contributor.author | Fuernkranz, Verena | |
dc.contributor.author | Goodman, Alyssa | |
dc.contributor.author | Hacar, Alvaro | |
dc.contributor.author | Herbst-Kiss, Gabor | |
dc.contributor.author | Lada, Charles J. | |
dc.contributor.author | Larreina, Irati | |
dc.contributor.author | Leschinski, Kieran | |
dc.contributor.author | Lombardi, Marco | |
dc.contributor.author | Moitinho, Andre | |
dc.contributor.author | Mortimer, Daniel | |
dc.contributor.author | Zari, Eleonora | |
dc.date.accessioned | 2018-12-20T01:15:54Z | |
dc.date.available | 2018-12-20T01:15:54Z | |
dc.date.issued | 2018-11-14 | |
dc.identifier.citation | Grossschedl , J E , Alves , J , Meingast , S , Ackerl , C , Ascenso , J , Bouy , H , Burkert , A , Forbrich , J , Fuernkranz , V , Goodman , A , Hacar , A , Herbst-Kiss , G , Lada , C J , Larreina , I , Leschinski , K , Lombardi , M , Moitinho , A , Mortimer , D & Zari , E 2018 , ' 3D shape of Orion A from Gaia DR2 ' , Astronomy & Astrophysics , vol. 619 , A106 . https://doi.org/10.1051/0004-6361/201833901 | |
dc.identifier.issn | 0004-6361 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1808.05952v1 | |
dc.identifier.other | ORCID: /0000-0001-8694-4966/work/62751206 | |
dc.identifier.uri | http://hdl.handle.net/2299/20873 | |
dc.description | Reproduced with permission from Astronomy & Astrophysics. © 2018 ESO. | |
dc.description.abstract | We use the Gaia DR2 distances of about 700 mid-infrared selected young stellar objects in the benchmark giant molecular cloud Orion A to infer its 3D shape and orientation. We find that Orion A is not the fairly straight filamentary cloud that we see in (2D) projection, but instead a cometary-like cloud oriented toward the Galactic plane, with two distinct components: a denser and enhanced star-forming (bent) Head, and a lower density and star-formation quieter ~75 pc long Tail. The true extent of Orion A is not the projected ~40 pc but ~90 pc, making it by far the largest molecular cloud in the local neighborhood. Its aspect ratio (~30:1) and high column-density fraction (~45%) make it similar to large-scale Milky Way filaments ("bones"), despite its distance to the galactic mid-plane being an order of magnitude larger than typically found for these structures. | en |
dc.format.extent | 9 | |
dc.format.extent | 7428511 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomy & Astrophysics | |
dc.subject | Local insterstellar matter | |
dc.subject | Methods: Observational | |
dc.subject | Methods: Statistical | |
dc.subject | Parallaxes | |
dc.subject | Stars: Distances | |
dc.subject | Stars: Formation | |
dc.subject | Astronomy and Astrophysics | |
dc.subject | Space and Planetary Science | |
dc.title | 3D shape of Orion A from Gaia DR2 | en |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
dc.identifier.url | http://www.scopus.com/inward/record.url?scp=85056789055&partnerID=8YFLogxK | |
rioxxterms.versionofrecord | 10.1051/0004-6361/201833901 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |