Distribution and motions of atomic hydrogen in lenticular galaxies

Details Distribution and motions of atomic hydrogen in lenticular galaxies Distribution and motions of atomic hydrogen in lenticular galaxies

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...199...41v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 199, no. 1-2, June 1988, p. 41-60. ZWO-supported research.

Astronomy and Astrophysics

Astrophysics

12

Galactic Evolution, Galactic Structure, Gas Dynamics, Hydrogen Atoms, Lenticular Bodies, Spiral Galaxies, H Alpha Line, Infrared Photometry, Luminosity, Stellar Evolution

Scientific paper

The authors mapped the distribution of H I gas in and around the SO galaxy NGC 4026 and the nearby low-luminosity spirals UGC 6917, 6922 and 6956 in the 21-cm H I line with a spatial resolution of 25arcsec×32arcsec (α×δ) and a velocity resolution of 20 km s-1. No H I was detected in the SO galaxy. The H I distribution and kinematics of the three spirals show no evidence of tidal interaction. The authors detected a ≡40 kpc long filament of H I near the SO, which contains 2×108M_sun; of H I. They also mapped the H I distribution in the interacting Sab/SO galaxy pair NGC 6500/6501 with a spatial resolution of 13arcsec×39arcsec(α×δ) and a velocity resolution of 40 km s-1. They found a (kinematically) disturbed H I distribution in the Sab galaxy NGC 6500, with an H I filament curving towards the SO galaxy, in which no H I gas was detected. The observations are consistent with a capture scenario, in which gas-rich SO galaxies have formed through the accretion of gas from a nearby galaxy.

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