HST NICMOS Coronagraphic Polarimetry of AFGL 2591, S140 IRS1, and MON R2 IRS3

Details HST NICMOS Coronagraphic Polarimetry of AFGL 2591, S140 IRS1, and MON R2 IRS3 HST NICMOS Coronagraphic Polarimetry of AFGL 2591, S140 IRS1, and MON R2 IRS3

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21341316s&link_type=abstract

American Astronomical Society, AAS Meeting #213, #413.16; Bulletin of the American Astronomical Society, Vol. 41, p.223

Astronomy and Astrophysics

Astronomy

Scientific paper

Whereas the nearby low-mass young stellar objects (YSOs) can be isolated
and not have substantial interaction from other stars, most, if not all, massive stars (> 8 Msun) are observed to form in clusters. This combination of massive stars and clusters has led to the suggestions that massive stars form by coalescence after stellar collisions
or by enhanced accretion due to the gravitational potential of the cluster. It is still possible that massive stars form by accretion through a disk, similar to the formation of low-mass stars, although the presence of a disk in any star with mass > 25 Msun (earlier than O8) has not been observed and the existance of disks is still controversial. We are studying the massive YSOs in the nearest star-forming regions using 2 micron polarimetry with the 0.2" resolution of the Near-Infrared Camera and Multi-Object Spectrometer (NICMOS) on Hubble Space Telescope (HST). These stars, which are still embedded in dense envelopes, have lobes
of scattered light along their outflow axes. Because these nearby massive YSOs are bright, their point-spread functions
(PSFs) put substantial scattered light, usually polarized, into their immediate vicinity on the array. Because our goal is to determine any effects of interactions with other stars on possible disk structure, these PSFs must be removed; the best way is by coronagraphic imaging. We find that AFGL 2591, S 140 IRS1, and the two components of Mon R2 IRS3 all have very wide opening angles, asymmetric structure near the stars, and indications of episodic outflows.
Support for program 10519 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

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