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Extra info for AN 08-10-209 BC-348 series Radio Receiver (maintenance)

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I ••• ,:. . 1 'ID • 120 __"'_ . :' "7; 1;0 ~-... -'". / -;1- -'f ' . - '. "" ' . , or' Figs. 2a- b. (a) A photographic presentation of the distribution of HI column density in the sky over the velocity range - 20 to + 20 km s - 1 (LSR). From Heiles and Jenkins (1974). (b) The directions of polarization of optical starlight, and hence presumably the direction of the interstellar magnetic field . From Mathewson and Ford (1970). -.. - .. -1. J i· 2. f - ,~. ~ 'W IV rn ~ ffi (j o .. '" . , -JO -,.

Yet another large filament rises perpendicular to the galactic plane near the north celestial pole (l~ 120°, b~ 30°); again, optical polarization data is scanty here, but suggests alignment. This filament has appreciable velocity structure both along and perpendicular to its axis. Some of the filamentary structures are extremely long, extending up to 80° or so in projection on the sky. A typical large filament has density ~ 30 cm - 3, diameter ~ 2 pc, and mass ~ 6 M 0 per parsec of length. Long filamentary structures similar to those seen in Figure 2 have been observed in regions other than the solar neighborhood.

I ~~~~ o ________________________________ 270 ~ I B 0 ____ .. -~ ~~_ o (c) Regions referred to in the text. (d) The locations of dust clouds catalogued by Lynds (1962). Made from computer cards recently generated by Lynds. o Velo cit y. k m/sec Figs. 3a-b. Contour maps of antenna temperature vs. galactic longitude and velocity, for fixed galactic latitude. Each covers a star showing an interstellar CaD line with no corresponding Hlline. The position of the star and the velocity of the line are located at the tip of the arrow.

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