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Lupus I observations from the 2010 flight of the Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry

Matthews, Tristan G., Ade, Peter A. R., Angilè, Francesco E., Benton, Steven J., Chapin, Edward L., Chapman, Nicholas L., Devlin, Mark J., Fissel, Laura M., Fukui, Yasuo, Gandilo, Natalie N., Gundersen, Joshua O., Hargrave, Peter Charles, Klein, Jeffrey, Korotkov, Andrei L., Moncelsi, Lorenzo, Mroczkowski, Tony K., Netterfield, Calvin B., Novak, Giles, Nutter, David John, Olmi, Luca, Pascale, Enzo, Poidevin, Frédérick, Savini, Giorgio, Scott, Douglas, Shariff, Jamil A., Soler, Juan Diego, Tachihara, Kengo, Thomas, Nicholas E., Truch, Matthew D. P., Tucker, Carole Elizabeth, Tucker, Gregory S. and Ward-Thompson, Derek 2014. Lupus I observations from the 2010 flight of the Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry. The Astrophysical Journal 784 (2) , 116. 10.1088/0004-637X/784/2/116

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Abstract

The Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol) was created by adding polarimetric capability to the BLAST experiment that was flown in 2003, 2005, and 2006. BLASTPol inherited BLAST's 1.8 m primary and its Herschel/SPIRE heritage focal plane that allows simultaneous observation at 250, 350, and 500 μm. We flew BLASTPol in 2010 and again in 2012. Both were long duration Antarctic flights. Here we present polarimetry of the nearby filamentary dark cloud Lupus I obtained during the 2010 flight. Despite limitations imposed by the effects of a damaged optical component, we were able to clearly detect submillimeter polarization on degree scales. We compare the resulting BLASTPol magnetic field map with a similar map made via optical polarimetry. (The optical data were published in 1998 by J. Rizzo and collaborators.) The two maps partially overlap and are reasonably consistent with one another. We compare these magnetic field maps to the orientations of filaments in Lupus I, and we find that the dominant filament in the cloud is approximately perpendicular to the large-scale field, while secondary filaments appear to run parallel to the magnetic fields in their vicinities. This is similar to what is observed in Serpens South via near-IR polarimetry, and consistent with what is seen in MHD simulations by F. Nakamura and Z. Li.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Uncontrolled Keywords: ISM: magnetic fields; stars: formation; techniques: polarimetric
Publisher: IOP Publishing
ISSN: 0004-637X
Funders: Leverhulme
Date of First Compliant Deposit: 11 September 2017
Date of Acceptance: 16 February 2014
Last Modified: 16 Aug 2019 21:31
URI: http://orca-mwe.cf.ac.uk/id/eprint/59179

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