The W4 Superbubble

Worms in CGPS-I


Worms are wiggly looking bits of HI sticking out of the Galactic plane. Chances are that some of them are walls of superbubbles or chimneys. There are two catalogues of worms and worm candidates in existence. Koo et al (1992) used low resolution HI surveys, and IRAS 60 and 100 micron data. The HI was integrated over all velocities and all three data sets were median filtered. Series of connected positive pixels were extracted; an object is a worm candidate if it is present in all three images. Heiles et al (1996) catalogue 27 worms using the Effelsberg 11 cm survey and Radio Recombination Line measurements made with the now defunct Hat Creek telescope.

The objective of this subproject is to look for new worms. The best method to do this has not yet been devised but I (MN) don't believe that the Koo et al method is particularly useful, mainly because of the integration over all velocities.

Previously catalogued in the CGPS longitude range

From Koo, Heiles & Reach
ObjectCGPS-I field(s)Comments
GW 78.1-4.7O2-N7Too low for much C21 & S21
GW 89.7-2.4K7 
GW 90.3+7.6 Too high
GW 93.7+3.0J9 
GW 93.8+7.6 Too high
GW 99.4-1.7I2 
GW 103.6-3.9H2-G7Too low for much C21 & S21
GW 104.2-9.0 Too low
GW 107.4-3.3G2-F7Too low for much C21 & S21
GW 108.9-8.2 Too low
GW 112.7-4.0E7-E2Too low for much C21 & S21
GW 118.6-5.1D2-C7Too low for much C21 & S21
GW 123.4-1.5B7 
GW 128.9-4.8A2Too low for much C21 & S21
GW 129.8+1.6A1 
GW 131.3-2.2Y7-Y2 
GW 132.6-0.9Y2 
GW 134.6-4.7Y2-X7Too low for much C21 & S21
GW 135.5-8.2 Too low

Searching the Dwingeloo data

What was done


Lightest: structure correlated in one pairing, medium: structure correlated in two pairings, darkest: structure correlated in all 3 pairings. Only the intersections are coloured.

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