EDP Sciences
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Volume 398, Number 2, February I 2003
Page(s) 493 - 499
Section Galactic structure and dynamics
DOI http://dx.doi.org/10.1051/0004-6361:20021701

A&A 398, 493-499 (2003)
DOI: 10.1051/0004-6361:20021701

The cold gas properties of Markarian galaxies

R. A. Kandalyan1, 2, 3

1  V. A. Ambartsumian Byurakan Astrophysical Observatory, 378433 Byurakan, Armenia
    e-mail: rkandali@bao.sci.am
2  Isaac Newton Institute of Chile, Armenian Branch, 378433 Byurakan, Armenia
3  Institute of Astronomy and Space Sciences of the Al Al-Bayt University, PO Box 130040, Mafraq 25113, Jordan

(Received 4 June 2002 / Accepted 25 October 2002 )

A sample of 61 Markarian galaxies detected in the CO line was compiled. Using available HI, $\element{H}_{2}$, optical and radio continuum data, the analysis of the gas kinematics and the star formation properties for this sample of galaxies was performed. The main conclusion can be summarized as follows: (1) The HI and CO line widths are well correlated. Interaction between galaxies has no influence on the CO line broadening. A rapidly rotating nuclear disk in the galaxy might lead to the CO line broadening with less influence on the HI line. (2) The atomic and molecular gas surface densities are well correlated with the blue, FIR and radio continuum surface brightness; however, the correlation for molecular component is stronger. (3) In general, the galaxies with UV-excess (Markarian galaxies) do not differ in their star formation properties from the non-UV galaxies.

Key words: galaxies: ISM -- radio lines: galaxies -- ultraviolet: galaxies

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