The Northern Arc of ε Eridani’s Debris Ring as Seen by ALMAReport as inadecuate


The Northern Arc of ε Eridani’s Debris Ring as Seen by ALMA


The Northern Arc of ε Eridani’s Debris Ring as Seen by ALMA - Download this document for free, or read online. Document in PDF available to download.

Publication Date: 2017-05-04

Journal Title: Monthly Notices of the Royal Astronomical Society

Publisher: Oxford University Press

Volume: 469

Pages: 3200-3212

Language: English

Type: Article

This Version: VoR

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Citation: Booth, M., Dent, W., Jordán, A., Lestrade, J., Hales, A., Wyatt, M. C., Casassus, S., et al. (2017). The Northern Arc of ε Eridani’s Debris Ring as Seen by ALMA. Monthly Notices of the Royal Astronomical Society, 469 3200-3212. https://doi.org/10.1093/mnras/stx1072

Abstract: We present the first Atacama Large Millimeter/submillimeter Array (ALMA) observations of the closest known extrasolar debris disc. This disc orbits the star ε Eri, a K-type star just 3.2 pc away. Due to the proximity of the star, the entire disc cannot fit within the ALMA field of view. Therefore, the observations have been centred 18 North of the star, providing us with a clear detection of the Northern arc of the ring, at a wavelength of 1.3 mm. The observed disc emission is found to be narrow with a width of just 11–13 AU. The fractional disc width we find is comparable to that of the Solar system’s Kuiper Belt and makes this one of the narrowest debris discs known. If the inner and outer edges are due to resonances with a planet then this planet likely has a semi-major axis of 48 AU. We find tentative evidence for clumps in the ring, although there is a strong chance that at least one is a background galaxy. We confirm, at much higher significance, the previous detection of an unresolved emission at the star that is above the level of the photosphere and attribute this excess to stellar chromospheric emission.

Keywords: circumstellar matter, stars: individual: ε Eri, planetary systems, submillimetre: planetary systems, submillimetre: stars

Sponsorship: MB acknowledges support from a FONDECYT Postdoctoral Fellowship, project no. 3140479 and the Deutsche Forschungsgemeinschaft (DFG) through project no. Kr 2164/15-1. AJ and SC acknowledge financial support from the Millennium Nucleus RC130007 (Chilean Ministry of Economy). AJ acknowledges support from FONDECYT project no. 1130857, BASAL CATA PFB-06 and the Ministry for the Economy, Development, and Tourism’s Programa Iniciativa Cient´ıfica Milenio through grant no. IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). MCW acknowledges the support of the European Union through ERC grant no. 279973. GMK is supported by the Royal Society as a Royal Society University Research Fellow. JCA acknowledges support from PNP/CNES. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00645.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research made use of Astropy, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013).

Embargo Lift Date: 2100-01-01

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External DOI: https://doi.org/10.1093/mnras/stx1072

This record's URL: https://www.repository.cam.ac.uk/handle/1810/265819



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Author: Booth, MDent, WRFJordán, ALestrade, J-FHales, AS Wyatt, Mark CharlesCasassus, SErtel, SGreaves, JS Kennedy, Grant MalcolmMatrà,

Source: https://www.repository.cam.ac.uk/handle/1810/265819



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