The AMIGA sample of isolated galaxies

VIII. The rate of asymmetric H i profiles in spiral galaxies ^⋆,⋆⋆

¹ Instituto de Astrofísica de Andalucía (IAA-CSIC), Apdo. 3004, 18080 Granada, Spain
e-mail: daniel@iaa.es
² National Astronomical Observatory of Japan (NAOJ), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
e-mail: daniel.espada@nao.ac.jp
³ Max-Planck-Institut fuer Radioastronomie, Postfach 2024, 53010 Bonn, Germany
⁴ Dept. de Física Teórica y del Cosmos, Universidad de Granada, Spain
⁵ Joint ALMA Observatory/ESO, Av. Alonso de Córdova 3107, Vitacura, Santiago, Chile
⁶ Institute for Astronomy, University of Edinburgh, Edinburgh EH9 3HJ, UK

Received: 10 November 2010
Accepted: 24 April 2011

Abstract

Context. Measures of the H i properties of a galaxy are among the most sensitive interaction diagnostic at our disposal. We report here on a study of H i profile asymmetries (e.g., lopsidedness) in a sample of some of the most isolated galaxies in the local Universe. This presents us with an excellent opportunity to quantify the range of intrinsic H i asymmetries in galaxies (i.e., those not induced by the environment) and provides us with a zero-point calibration for evaluating these measurements in less isolated samples.

Aims. We aim to characterize the H i profile asymmetries in a sample of isolated galaxies and search for correlations between H i asymmetry and their environments, as well as their optical and far infrared (FIR) properties.

Methods. We use high signal-to-noise global H i profiles for galaxies in the AMIGA project (Analysis of the Interstellar Medium of Isolated GAlaxies, http://amiga.iaa.es). We restrict our study to N = 166 galaxies (out of 312) with accurate measures of the H i shape properties. We quantify asymmetries using a flux ratio parameter.

Results. The asymmetry parameter distribution of our isolated sample is well described by a Gaussian model. The width of the distribution is σ = 0.13, and could be even smaller (σ = 0.11) if instrumental errors are reduced. Only 2% of our carefully vetted isolated galaxies sample show an asymmetry in excess of 3σ. By using this sample we minimize environmental effects as confirmed by the lack of correlation between H i asymmetry and tidal force (one-on-one interactions) and neighbor galaxy number density. On the other hand, field galaxy samples show wider distributions and deviate from a Gaussian curve. As a result we find higher asymmetry rates (~10–20%) in such samples. We find evidence that the spiral arm strength is inversely correlated with the HI asymmetry. We also find an excess of FIR luminous galaxies with larger HI asymmetries that may be spirals associated with hidden accretion events.

Conclusions. Our sample presents the smallest fraction of asymmetric H i profiles compared with any other yet studied. The width of the associated asymmetry parameter distribution can help to distinguish the frequency and processes of self-induced HI asymmetries, and serve as a baseline for studying asymmetry rates in other environments.