HI Imaging of LGS 3 and an Apparently Interacting High-Velocity Cloud

Details HI Imaging of LGS 3 and an Apparently Interacting High-Velocity Cloud HI Imaging of LGS 3 and an Apparently Interacting High-Velocity Cloud

2002-10-15

arxiv.org/abs/astro-ph/0210349v1

Astrophys.J. 580 (2002) L129-L132

Astronomy and Astrophysics

Astrophysics

5 pages, 2 color figures. Accepted for publication in ApJ Letters

Scientific paper

10.1086/345711

We present a 93' by 93' map of the area near the Local Group dwarf galaxy LGS 3, centered on an HI cloud 30' away from the galaxy. Previous authors associated this cloud with LGS 3 but relied on observations made with a 36' beam. Our high-resolution (3.4'), wide-field Arecibo observations of the region reveal that the HI cloud is distinct from the galaxy and suggest an interaction between the two. We point out faint emission features in the map that may be gas that has been tidally removed from the HI cloud by LGS 3. We also derive the rotation curve of the cloud and find that it is in solid-body rotation out to a radius of 10', beyond which the rotation velocity begins to decline. Assuming a spherical geometry for the cloud, the implied mass is 2.8 x 10^7 (d/Mpc) M_{Sun}, where d is the distance in Mpc. The observed HI mass is 5.5 x 10^6 (d/Mpc)^2 M_{Sun}, implying that the cloud is dark-matter dominated unless its distance is at least 1.9 Mpc. We propose that the cloud is a high-velocity cloud that is undergoing a tidal interaction with LGS 3 and therefore is located roughly 700 kpc away from the Milky Way. The cloud then contains a total mass of ~2.0 x 10^7 M_{Sun}, 82% of which consists of dark matter.

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