scholarly journals Molecular Outflows and a Mid‐Infrared Census of the Massive Star Formation Region Associated with IRAS 18507+0121

2007 ◽  
Vol 669 (1) ◽  
pp. 464-482 ◽  
Author(s):  
D. S. Shepherd ◽  
M. S. Povich ◽  
B. A. Whitney ◽  
T. P. Robitaille ◽  
D. E. A. Nurnberger ◽  
...  
2007 ◽  
Vol 3 (S242) ◽  
pp. 188-189
Author(s):  
James A. Green ◽  
A. M. S. Richards ◽  
H. Flood ◽  
W. H. T. Vlemmings ◽  
R. J. Cohen

AbstractMERLIN observations of 6.668-GHz Methanol and 6.035-GHz OH emission from the known massive star-formation region ON1 are presented. Maser components are found to lie at the southern edge of the UCHII with consistent polarization angles across the strongest features. Zeeman splitting of OH shows magnetic field strengths between +0.4 to −5.3 mG and from cross-correlation a tentative methanol magnetic field of −18mG is detected.


2007 ◽  
Vol 59 (1) ◽  
pp. 221-225 ◽  
Author(s):  
Jun Hashimoto ◽  
Motohide Tamura ◽  
Hiroshi Suto ◽  
Lyu Abe ◽  
Miki Ishii ◽  
...  

2007 ◽  
Vol 660 (1) ◽  
pp. 346-362 ◽  
Author(s):  
Matthew S. Povich ◽  
Jennifer M. Stone ◽  
Ed Churchwell ◽  
Ellen G. Zweibel ◽  
Mark G. Wolfire ◽  
...  

2016 ◽  
Vol 825 (1) ◽  
pp. 54 ◽  
Author(s):  
C. L. Barbosa ◽  
R. D. Blum ◽  
A. Damineli ◽  
P. S. Conti ◽  
D. M. Gusmão

1998 ◽  
Vol 164 ◽  
pp. 375-376
Author(s):  
S. P. Ellingsen ◽  
P.M. McCulloch ◽  
P. J. Diamond ◽  
R. P. Norris

AbstractWe have used the VLBA to image the 12.2 GHz (20-3−1 E) masing transition of methanol toward the massive star formation region G345.01+1.79. The maser spots are distributed in a curved structure with a near monotonic velocity distribution along the curve. The cluster of maser emission covers an area of approximately 200 milli-arcseconds in right ascension and 70 milli-arcseconds in declination.Comparison of the positions of the 12.2 GHz methanol maser spots in G345.01+1.79 as determined from the 1995 VLBA observations with 1988 Parkes-Tidbinbilla Interferometer observations shows that the relative positions of the maser spots detected in both epochs has changed by less than 5 milli-arcseconds during that interval. Assuming a distance of 2.3 kpc to G345.01+1.79 implies an upper limit on the relative tangential velocities of the maser spots of 7 km s−1.


2003 ◽  
Vol 287 (1-4) ◽  
pp. 191-194 ◽  
Author(s):  
M.S. Nanda Kumar ◽  
Christopher J. Davis ◽  
Rafael Bachiller

2000 ◽  
Vol 539 (2) ◽  
pp. 641-657 ◽  
Author(s):  
Michele D. Thornley ◽  
Natascha M. Forster Schreiber ◽  
Dieter Lutz ◽  
Reinhard Genzel ◽  
Henrik W. W. Spoon ◽  
...  

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