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Accretion Signatures on Massive Young Stellar Objects

Published online by Cambridge University Press:  23 January 2015

F. Navarete ,
A. Damineli ,
C. L. Barbosa  and
R. D. Blum
F. Navarete
Affiliation:
IAG-USP, Rua do Matão, 1226, 05508-900, São Paulo, SPBrazil email: [email protected]
A. Damineli
Affiliation:
IAG-USP, Rua do Matão, 1226, 05508-900, São Paulo, SPBrazil email: [email protected]
C. L. Barbosa
Affiliation:
UNIVAP, São José dos Campos, SP, Brazil
R. D. Blum
Affiliation:
NOAO, 950 N Cherry Ave., Tuczon, AZ 85719USA
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Abstract

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We present preliminary results from a survey of molecular H2 (2.12 μm) emission in massive young stellar objects (MYSO) candidates selected from the Red MSX Source survey. We observed 354 MYSO candidates through the H2 S(1) 1-0 transition (2.12 μm) and an adjacent continuum narrow-band filters using the Spartan/SOAR and WIRCam/CFHT cameras. The continuum-subtracted H2 maps were analyzed and extended H2 emission was found in 50% of the sample (178 sources), and 38% of them (66) have polar morphology, suggesting collimated outflows. The polar-like structures are more likely to be driven on radio-quiet sources, indicating that these structures occur during the pre-ultra compact H ii phase. We analyzed the continuum images and found that 54% (191) of the sample displayed extended continuum emission and only ~23% (80) were associated to stellar clusters. The extended continuum emission is correlated to the H2 emission and those sources within stellar clusters does display diffuse H2 emission, which may be due to fluorescent H2 emission. These results support the accretion scenario for massive star formation, since the merging of low-mass stars would not produce jet-like structures. Also, the correlation between jet-like structures and radio-quiet sources indicates that higher inflow rates are required to form massive stars in a typical timescale less than 105 years.

Keywords

Stars: formationStars: early-typeStars: pre-main sequenceISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 431 - 436
Copyright
Copyright © International Astronomical Union 2015 

References

Bally, J., Reipurth, B., Walawender, J., & Armond, T. 2002, AJ 124, 2152Google Scholar
Bik, A. & Thi, W. F. 2004, A&A 427, L13Google Scholar
Blum, R. D., Barbosa, C. L., Damineli, A., Conti, P. S., & Ridgway, S. 2004, ApJ 617, 1167CrossRefGoogle Scholar
Bonnell, I. A., Bate, M. R., Clarke, C. J., & Pringle, J. E. 2001, MNRAS 323, 785Google Scholar
Bonnell, I. A., Bate, M. R., & Zinnecker, H. 1998, MNRAS 298, 93Google Scholar
Erben, T., Schirmer, M., Dietrich, J. P., et al. 2005, Astronomische Nachrichten 326, 432Google Scholar
Krumholz, M. R., Klein, R. I., McKee, C. F., Offner, S. S. R., & Cunningham, A. J. 2009, Science 323, 754Google Scholar
Krumholz, M. R., McKee, C. F., & Klein, R. I. 2005, ApJ 618, L33Google Scholar
Lumsden, S. L., Hoare, M. G., Oudmaijer, R. D., & Richards, D. 2002, MNRAS 336, 621CrossRefGoogle Scholar
Mottram, J. C.et al. 2011, A&A 525, A149Google Scholar
Palla, F. 1996, in Beckwith, S., Staude, J., Quetz, A., & Natta, A. (eds.), Disks and Outflows Around Young Stars, Vol. 465 of Lecture Notes in Physics, Berlin Springer Verlag, p. 143Google Scholar
Schirmer, M. 2013, ApJS 209, 21Google Scholar
Stahler, S. W., Palla, F., & Ho, P. T. P. 2000, Protostars and Planets IV p. 327Google Scholar
Urquhart, J. S., Busfield, A. L., Hoare, M. G., et al. 2007, A&A 461, 11Google Scholar
Urquhart, J. S.et al. 2009, A&A 501, 539Google Scholar
Varricatt, W. P., Davis, C. J., Ramsay, S., & Todd, S. P. 2010, MNRAS 404, 661Google Scholar