Sh 2-196
Coordinates: (136.45°, 2.53°)
[ Catalog | Explorer | SIMBAD ]
According to one source, this HII region, which is most likely ionised by a B2.5 V class star, lies at the edge of a 1000 solar mass molecular cloud in a similar direction to the Sh 2-192 to Sh 2-194 group of nebulae.
According to a 2007 paper by Russeil, Sh 2-196 may lie at the same distance as Sh 2-192 and Sh 2-193 (2400 +/- 320 parsecs), however she has identified a possible O9.5 class ionising star with a photometric distance of 5670 +/- 590 parsecs, suggesting that it may be much further away than the other nebulae.
Avedisova places Sh 2-196 in star formation region SFR 136.45+2.53 with 21 components, including the radio source KR 147B, 4 masers and 9 infrared sources. Among the infrared sources are three distinct young stellar objects.
According to a 2007 paper by Russeil, Sh 2-196 may lie at the same distance as Sh 2-192 and Sh 2-193 (2400 +/- 320 parsecs), however she has identified a possible O9.5 class ionising star with a photometric distance of 5670 +/- 590 parsecs, suggesting that it may be much further away than the other nebulae.
Avedisova places Sh 2-196 in star formation region SFR 136.45+2.53 with 21 components, including the radio source KR 147B, 4 masers and 9 infrared sources. Among the infrared sources are three distinct young stellar objects.
Russeil paper. [1]
Most likely ionised by a B2.5 V class star.[2]
Lies at the edge of a 1000 solar mass molecular cloud.[3]
This HII region lies between W4 and W5.[4]
Most likely ionised by a B2.5 V class star.[2]
Lies at the edge of a 1000 solar mass molecular cloud.[3]
This HII region lies between W4 and W5.[4]
Notes
1. ^ Russeil, D., Adami, C., & Georgelin, Y. M. (2007). "Revised distances of Northern HII regions", Astronomy and Astrophysics, Vol. 470, 161-171. [2007A&A...470..161R]
2. ^ Hunter, Deidre A. & Massey, Philip (1990). "Small Galactic H II regions. I - Spectral classifications of massive stars", The Astronomical Journal, Vol. 99, 846-856. [1990AJ.....99..846H]
3. ^ Hunter, Deidre A., Thronson, Harley A., Jr., & Wilton, Charles (1990). "Small Galactic H II regions. II - The molecular clouds and star formation", The Astronomical Journal, Vol. 100, 1915-1926. [1990AJ....100.1915H]
4. ^ Digel, Seth W., Lyder, David A., Philbrick, Amy J., et al. (1996). "A Large-Scale CO Survey toward W3, W4, and W5", The Astrophysical Journal, Vol. 458, 561. [1996ApJ...458..561D]
Distance estimates
3200 pc [2003A&A...397..133R]Links
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Most of the sources used to create these nebula descriptions are listed in the
notes section for each description. In some cases,
for example the Avedisova, Humphreys and Reed catalogs, the source is used extensively and is not listed in the
individual nebula descriptions. See this catalog overview
for more information on the catalogs and the general sources used
to create these descriptions and this introduction to HII regions
on the general history of this area of astronomy.
This image was created using the POSS-II/UKSTU data of the Digitized Sky Survey and SuperCOSMOS using the process described here.
According to my correspondence with the Royal Observatory Edinburgh and the Space Telescope Science Institute, I am allowed to use the POSS-II/UKSTU data to create and display images for non-commercial purposes so long as I include this fine print for the SuperCOSMOS data:
Use of these images is courtesy of the UK Schmidt Telescope (copyright in which is owned by the Particle Physics and Astronomy Research Council of the UK and the Anglo-Australian Telescope Board) and the Southern Sky Survey as created by the SuperCOSMOS measuring machine and are reproduced here with permission from the Royal Observatory Edinburgh.
and this acknowledgement taken from the DSS site:
The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions.
The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation.
The UK Schmidt Telescope was operated by the Royal Observatory Edinburgh, with funding from the UK Science and Engineering Research Council (later the UK Particle Physics and Astronomy Research Council), until 1988 June, and thereafter by the Anglo-Australian Observatory. The blue plates of the southern Sky Atlas and its Equatorial Extension (together known as the SERC-J), as well as the Equatorial Red (ER), and the Second Epoch [red] Survey (SES) were all taken with the UK Schmidt.
The "Second Epoch Survey" of the southern sky was made by the Anglo-Australian Observatory (AAO) with the UK Schmidt Telescope. Plates from this survey have been digitized and compressed by the ST ScI. The digitized images are copyright ? 1993-5 by the Anglo-Australian Observatory Board, and are distributed herein by agreement.
The "Equatorial Red Atlas" of the southern sky was made with the UK Schmidt Telescope. Plates from this survey have been digitized and compressed by the ST ScI. The digitized images are copyright ? 1992-5, jointly by the UK SERC/PPARC (Particle Physics and Astronomy Research Council, formerly Science and Engineering Research Council) and the Anglo-Australian Telescope Board, and are distributed herein by agreement.
The compressed files of the "Palomar Observatory - Space Telescope Science Institute Digital Sky Survey" of the northern sky, based on scans of the Second Palomar Sky Survey are copyright ? 1993-1995 by the California Institute of Technology and are distributed herein by agreement. The compressed files of the "Palomar Observatory - Space Telescope Science Institute Digital Sky Survey" of the northern sky, based on scans of the Second Palomar Sky Survey are copyright ? 1993-1995 by the California Institute of Technology and are distributed herein by agreement.