HI observations of nearby galaxies V. Narrow (HI) line galaxies

Abstract

Abstract. In this paper we present new HI observations with high velocity resolution for 104 nearby narrow-line galaxies with half power line widths smaller than 50 km s −1 most of which are well approximated by a Gaussian. The FWHM line width of 30 of these integrated HI profiles is less than 25 km s −1 . We present global parameters of these nearby galaxies and discuss the size dependence, the luminosity dependence, and the dependence of these parameters with the observed line width. Our sample essentially is a subsample of the Local Volume (i.e. galaxies within 10 Mpc) with declinations ≥−30 • and only a few galaxies at greater distances. It is described by the following median values of global physical parameters: total absolute blue magnitude M Bt = −12.85; linear diameter A 0 = 1.63 kpc (this corresponds to the de Vaucouleurs diameter D 25 ); half power line width W c = 29 km s −1 ; total HI mass M HI = 2 × 10 7 M ; distance D = 5.1 Mpc; HI mass-to-luminosity ratio M HI /L B = 0.9 M /L ; total mass-to luminosity ratio M t /L B = 2.9 M /L .

The chemistry of planetary nebulae and HII regions in the dwarf galaxies Sextans A and B from deep VLT spectra

“…They are consistent, within the errors, with the heliocentric radial velocity of Sextans B (300 km s −1 from NED) and with the H  observations by Huchtmeier et al (2003), confirming that the PNe belong indeed to the galaxy.…”

The M81 Group Dwarf Irregular Galaxy Ddo 165. I. High-Velocity Neutral Gas in a Post-Starburst System

“…This is 18% lower than the single dish flux integral of 28.2 Jy km s −1 found by Huchtmeier et al (2003) using Effelsberg 100 m observations. We note that our maximum single-channel flux density of 550 ± 50 mJy is in fair agreement with the corresponding maximum value from Huchtmeier et al (2003) of 601 ± 11 mJy. As discussed above, we applied residual flux scaling in the imaging process, and thus the small difference between these global flux integrals is most likely due to the lack of very short baselines in our interferometric observations, and our corresponding insensitivity to diffuse, extended neutral gas.…”

MORE GALAXIES IN THE LOCAL VOLUME IMAGED IN Hα

“…Both have low surface brightness. An irregular dwarf, KK69, is characterized by a very narrow H i emission with a line width of 16.5 ± 0.6 km s −1 (Huchtmeier et al 2003). Our Hα image shows a very red or emission star-like object within its optical boundaries.…”