2017ApJ...842...66W

Query : 2017ApJ...842...66W

2017ApJ...842...66W - Astrophys. J., 842, 66-66 (2017/June-2)

First results from BISTRO-A SCUBA-2 polarimeter survey of the Gould belt.

WARD-THOMPSON D., PATTLE K., BASTIEN P., FURUYA R.S., KWON W., LAI S.-P., QIU K., BERRY D., CHOI M., COUDE S., DI FRANCESCO J., HOANG T., FRANZMANN E., FRIBERG P., GRAVES S.F., GREAVES J.S., HOUDE M., JOHNSTONE D., KIRK J.M., KOCH P.M., KWON J., LEE C.W., LI D., MATTHEWS B.C., MOTTRAM J.C., PARSONS H., PON A., RAO R., RAWLINGS M., SHINNAGA H., SADAVOY S., VAN LOO S., ASO Y., BYUN D.-Y., ESWARAIAH C., CHEN H.-R., CHEN M.C.-Y., CHEN W.P., CHING T.-C., CHO J., CHRYSOSTOMOU A., CHUNG E.J., DOI Y., DRABEK-MAUNDER E., EYRES S.P.S., FIEGE J., FRIESEN R.K., FULLER G., GLEDHILL T., GRIFFIN M.J., GU Q., HASEGAWA T., HATCHELL J., HAYASHI S.S., HOLLAND W., INOUE T., INUTSUKA S.-I., IWASAKI K., JEONG I.-G., KANG J.-H., KANG M., KANG S.-J., KAWABATA K.S., KEMPER F., KIM G., KIM J., KIM K.-T., KIM K.H., KIM M.-R., KIM S., LACAILLE K.M., LEE J.-E., LEE S.-S., LI D., LI H.-B., LIU H.-L., LIU J., LIU S.-Y., LIU T., LYO A.-R., MAIRS S., MATSUMURA M., MORIARTY-SCHIEVEN G.H., NAKAMURA F., NAKANISHI H., OHASHI N., ONAKA T., PERETTO N., PYO T.-S., QIAN L., RETTER B., RICHER J., RIGBY A., ROBITAILLE J.-F., SAVINI G., SCAIFE A.M.M., SOAM A., TAMURA M., TANG Y.-W., TOMISAKA K., WANG H., WANG J.-W., WHITWORTH A.P., YEN H.-W., YOO H., YUAN J., ZHANG C.-P., ZHANG G., ZHOU J., ZHU L., ANDRE P., DOWELL C.D., FALLE S. and TSUKAMOTO Y.

Abstract (from CDS):

We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array 2 camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions that the survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the first results from the BISTRO survey in the OMC 1 region. We see that the magnetic field lies approximately perpendicular to the famous "integral filament" in the densest regions of that filament. Furthermore, we see an "hourglass" magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density northeastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): ISM: individual objects: Orion A, OMC1 - polarization - stars: formation - stars: magnetic field - submillimeter: ISM - submillimeter: ISM

Simbad objects: 14

goto Full paper

goto View the references in ADS

Number of rows : 14
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1553 0
2 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 238 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
4 NAME Orion S reg 05 35 12.9 -05 24 10           ~ 156 0
5 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1249 2
6 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2421 1
7 M 42 HII 05 35 16.8 -05 23 15           ~ 4411 0
8 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 1004 0
9 NAME Ori A MoC 05 38 -07.1           ~ 3187 0
10 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 215 1
11 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3969 1
12 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1195 1
13 IC 5146 OpC 21 53 29.3 +47 14 46           ~ 507 2
14 NAME Gould Belt PoG ~ ~           ~ 956 1

To bookmark this query, right click on this link: simbad:objects in 2017ApJ...842...66W and select 'bookmark this link' or equivalent in the popup menu