TY - JOUR
T1 - Infrared reflection nebula in W75N
AU - Yamashita, T.
AU - Sato, S.
AU - Tamura, M.
AU - Suzuki, H.
AU - Gatley, I.
AU - Hough, J.
AU - Mountain, C.M.
AU - Moore, T.J.T.
N1 - Original article can be found via: http://cdsads.u-strasbg.fr/ Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA]
PY - 1988
Y1 - 1988
N2 - A new infrared reflection nebula is identified in the W75N region. The K-band polarization map shows a centrosymmetric pattern of the vectors extending over a region 2 arcmin in size, with large values of degrees of polarization, up to 50 per cent. The illuminating source is identified with the ultracompact H II region W75N(B) which is located at the center of polarization pattern. The intensity peak, IRS-1, is not a self-luminous source but is rather a bright knot in the reflection nebula. The northern peak, IRS-4, located on a second ultracompact H II region, W75N(A), extends for more than 30 arcsec and is less polarized (5-10 percent). The near-infrared light of IRS-4 is attributed to thermal emission from small (about 10 A) dust grains. The different polarization and spatial distribution of the near-infrared emission around these two ultracompact H II regions are explained by the different dust densities around them, probably due to their different evolutionary stages.
AB - A new infrared reflection nebula is identified in the W75N region. The K-band polarization map shows a centrosymmetric pattern of the vectors extending over a region 2 arcmin in size, with large values of degrees of polarization, up to 50 per cent. The illuminating source is identified with the ultracompact H II region W75N(B) which is located at the center of polarization pattern. The intensity peak, IRS-1, is not a self-luminous source but is rather a bright knot in the reflection nebula. The northern peak, IRS-4, located on a second ultracompact H II region, W75N(A), extends for more than 30 arcsec and is less polarized (5-10 percent). The near-infrared light of IRS-4 is attributed to thermal emission from small (about 10 A) dust grains. The different polarization and spatial distribution of the near-infrared emission around these two ultracompact H II regions are explained by the different dust densities around them, probably due to their different evolutionary stages.
M3 - Article
SN - 0035-8711
VL - 233
SP - 899
EP - 905
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -