SOFIA and ALMA Investigate Magnetic Fields and Gas Structures in Massive Star Formation: The Case of the Masquerading Monster in BYF 73

被引:2
|
作者
Barnes, Peter J. [1 ,2 ]
Ryder, Stuart D. [3 ,4 ]
Novak, Giles [5 ,6 ]
Crutcher, Richard M. [7 ]
Fissel, Laura M. [8 ]
Pitts, Rebecca L. [9 ]
Schap, William J., III [10 ]
机构
[1] Space Sci Inst, 4765 Walnut St Suite B, Boulder, CO 80301 USA
[2] Univ New England, Sch Sci & Technol, Armidale, NSW 2351, Australia
[3] Macquarie Univ, Sch Math & Phys Sci, Sydney, NSW 2109, Australia
[4] Macquarie Univ, Astron Astrophys & Astrophoton Res Ctr, Sydney, NSW 2109, Australia
[5] Ctr Interdisciplinary Explorat & Res Astrophys CIE, 1800 Sherman Ave, Evanston, IL 60201 USA
[6] Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA
[7] Univ Illinois, Dept Astron, 1010 W Green St, Urbana, IL 60801 USA
[8] Queens Univ, Dept Phys Engn Phys & Astron, 64 Bader Lane, Kingston, ON K7L 3N6, Canada
[9] Univ Copenhagen, Niels Bohr Inst, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark
[10] Univ Florida, Astron Dept, POB 112055, Gainesville, FL 32611 USA
关键词
MOLECULAR CLOUDS; GALACTIC H-2-REGIONS; COLUMN DENSITY; YOUNG STARS; POLARIMETRY; ORIENTATION; DIRECTION; VELOCITY; OUTFLOWS; REGIONS;
D O I
10.3847/1538-4357/acac27
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present Stratospheric Observatory For Infrared Astronomy (SOFIA) + Atacama Large Millimeter/submillimeter Array (ALMA) continuum and spectral-line polarization data on the massive molecular cloud BYF 73, revealing important details about the magnetic field morphology, gas structures, and energetics in this unusual massive star formation laboratory. The 154 mu m HAWC+ polarization map finds a highly organized magnetic field in the densest, inner 0.55 x 0.40 pc portion of the cloud, compared to an unremarkable morphology in the cloud's outer layers. The 3 mm continuum ALMA polarization data reveal several more structures in the inner domain, including a parsec-long, similar to 500 M (circle dot) "Streamer" around the central massive protostellar object MIR 2, with magnetic fields mostly parallel to the east-west Streamer but oriented north-south across MIR 2. The magnetic field orientation changes from mostly parallel to the column density structures to mostly perpendicular, at thresholds N (crit) = 6.6 x 10(26) m(-2), n (crit) = 2.5 x 10(11) m(-3), and B (crit) = 42 +/- 7 nT. ALMA also mapped Goldreich-Kylafis polarization in (CO)-C-12 across the cloud, which traces, in both total intensity and polarized flux, a powerful bipolar outflow from MIR 2 that interacts strongly with the Streamer. The magnetic field is also strongly aligned along the outflow direction; energetically, it may dominate the outflow near MIR 2, comprising rare evidence for a magnetocentrifugal origin to such outflows. A portion of the Streamer may be in Keplerian rotation around MIR 2, implying a gravitating mass 1350 +/- 50 M (circle dot) for the protostar+disk+envelope; alternatively, these kinematics can be explained by gas in free-fall toward a 950 +/- 35 M (circle dot) object. The high accretion rate onto MIR 2 apparently occurs through the Streamer/disk, and could account for similar to 33% of MIR 2's total luminosity via gravitational energy release.
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页数:32
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