www.drao-ofr.hia-iha.nrc-cnrc.gc.ca...
DA568 was noted in a 1420MHz survey of Galt & Kennedy (1968; AJ, 73, 135) made with the 26-m Telescope at DRAO. It was also noted in a Dwingeloo
1417MHz survey as DW2153+57 (BAN, 19, 201, 1967). Galt & Kennedy classified DA568 as a point source and, along with a number of other sources, as
being ``part of HB22''. DA568 has three qualities which then allowed it to disappear from the astronomical literature: it is big, it is thermal, and
it is not visible optically. It may be hard to believe, but after the initial two survey papers in 1967 and 1968, DA568 just drops off the catalogues
of radio sources and HII regions in the outer Galaxy. It is easily seen in the contour maps from the various Effelsberg surveys, but the size of the
object (~30' diameter) meant that it was not included in the subsequent catalogues, which focused on small diameter or point sources. As there is no
obvious optical emission associated with the object, it also does not have an associated Sh2, LBN, or BFS number. This leads to the strange result
that various ``complete'' catalogues of HII regions in the outer Galaxy do list the optically-visible, 3' diameter, BFS10 HII region, but omit the
30' diameter DA568 HII region.
Although this may upset some of our more sensitive readers' sense of completeness and tidiness, it would be of little note except for the fact that
DA568 is clearly a large area of ongoing star-formation in the Perseus arm, and not some old, worn-out, HII region that was overlooked because of its
very low surface brightness or because it has been reduced to inconsequential wisps of ionized material.
All the above was taken from the above link. Notice how this also would reflect the "wow" signal in the late 60's early 70's that was received in
the same spectrum. Notice how the "discovery" of this signal seems to correspond to the same frame of time, April through May. Possibly in relation
ship to the milky ways spin and our relative position to this emission source DA568. A maturing star cluster.
This is getting really Interesting 
