Observations from the Galactic Arecibo L-Band Feed Array H \scriptstyle I ( GALFA-H \scriptstyle I ) Survey of the tail of Complex C are presented and the halo clouds associated with this complex cataloged .
The properties of the Complex C clouds are compared to clouds cataloged at the tail of the Magellanic Stream to provide insight into the origin and destruction mechanism of Complex C. Magellanic Stream and Complex C clouds show similarities in their mass distributions ( slope = -0.7 and -0.6 \log ( N ( \log ( mass ) ) ) / \log ( mass ) , respectively ) and have a common linewidth of 20 - 30 km s ^ { -1 } ( indicative of a warm component ) , which may indicate a common origin and/or physical process breaking down the clouds .
The clouds cataloged at the tail of Complex C extend over a mass range of 10 ^ { 1.1 - 4.8 } { M } _ { \odot } , sizes of 10 ^ { 1.2 - 2.6 } pc , and have a median volume density and pressure of 0.065 cm ^ { -3 } and ( P/k ) = 580 K cm ^ { -3 } .
We do not see a prominent two-phase structure in Complex C , possibly due to its low metallicity and inefficient cooling compared to other halo clouds .
From assuming the Complex C clouds are in pressure equilibrium with a hot halo medium , we find a median halo density of 5.8 \times 10 ^ { -4 } cm ^ { -3 } , which given a constant distance of 10 kpc , is at a z -height of \sim 3 kpc .
Using the same argument for the Stream results in a median halo density of 8.4 \times 10 ^ { -5 } ~ { } ( 60 ~ { } kpc / d ) { cm ^ { -3 } } .
These densities are consistent with previous observational constraints and cosmological simulations .
We also assess the derived cloud and halo properties with three dimensional grid simulations of halo H \scriptstyle I clouds and find the temperature is generally consistent within a factor of 1.5 and the volume densities , pressures and halo densities are consistent within a factor of 3 .