The Draco nebula - A molecular cloud in the galactic halo?
U. Mebold, J. Cernicharo, L. Velden, K. Reif, C. Crezelius, W. Goerigk;
AaA, 1985, 151, 427
ABSTRACT:An extended and faint bright nebula (l = 91 deg, b = 38 deg) in the constellation Draco exhibits H I 21 cm, CO 2.6 mm and 2.7 mm emission and H2 CO 6.2 cm absorption lines in detailed positional agreement with the optical brightness distribution at the red and blue prints of the Palomar Observatory Sky Survey.Three color UBV photometry of about 60 stars located within the brightest part of the 'Draco nebula' indicates a distance of equal to or greater than 800 pc, or a distance of equal to or greater than 500 pc from the galactic plane.
With this distance the total mass of two of the molecular clumps in the Draco nebula is 27 and 219 solar masses and they appear to be gravitationally bound systems.
Further, positional coincidences are found with the low latitude end of the high velocity cloud complex HVC CI of Hulsbosch (1979) and with soft X-ray emission features on SAS as well as HEAO-1 satellite sky maps.
These suggest an astrophysical relationship between these phenomena.
KEYWORDS: interstellar extinction, milky way galaxy, molecular clouds, nebulae, radio sources (astronomy), radio spectra, carbon monoxide, formaldehyde, h lines, microwave emission, radial velocity, sky surveys (astronomy), ubv spectra
PERSOKEY:h_i, h2, cirrus, co, optical, xrays, draco, ,
CODE: mebold85