Observations of the interacting galaxy pair NGC 4490/85

Details Observations of the interacting galaxy pair NGC 4490/85 Observations of the interacting galaxy pair NGC 4490/85

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...121..150k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 121, no. 1, May 1983, p. 150-152.

Astronomy and Astrophysics

Astrophysics

15

Continuous Spectra, Galactic Clusters, Galactic Radio Waves, Hydrogen Clouds, Interacting Galaxies, Radio Galaxies, Stellar Evolution, Centimeter Waves, H Alpha Line, Lyman Spectra, Nonthermal Radiation, O Stars, Photon Density, Star Formation Rate, Thermal Emission

Scientific paper

The interacting galaxy pair NGC 4490/85 (Arp, 269) has been observed with the Effelsberg 100-m telescope at 24.5 GHz. The radio emission at that frequency is strongly correlated with the regions of ionized gas that can be seen in Hα. The fraction of thermal emission at 1.2 cm wavelength is 38 ± 12%. This suggests that also an appreciable amount of non-thermal emission originates in the H II complexes of this double system. Supernovae resulting from tidally triggered star formation bursts must be the sources of relativistic electrons. Some 2×105 O5 stars are required to account for the observed production rate of Lyman continuum photons. The derived present star formation rate is consistent with models of galaxy evolution.

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