Near-infrared line imaging of the starburst galaxies NGC 520, NGC 1614 and NGC 7714

J. K. Kotilainen*, J. Reunanen, S. Laine, S. D. Ryder

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

4 Citations (Scopus)


We present high spatial resolution (∼0″.6) near-infrared broad-band JHK images and Brγ 2.1661 μm and H2 1-0 S(1) 2.122 μm emission line images of the nuclear regions in the interacting starburst galaxies NGC 520, NGC 1614 and NGC 7714. The near-infrared emission line and radio morphologies are in general agreement, although there are differences in details. In NGC 1614, we detect a nuclear double structure in Brγ, in agreement with the radio double structure. We derive average extinctions of AK = 0.41 and AK = 0.18 toward the nuclear regions of NGC 1614 and NGC 7714, respectively. For NGC 520, the extinction is much higher, AK = 1.2-1.6. The observed H2/Brγ ratios indicate that the main excitation mechanism of the molecular gas is fluorescence by intense UV radiation from clusters of hot young stars, while shock excitation can be ruled out. The starburst regions in all galaxies exhibit small Brγ equivalent widths. Assuming a constant star formation model, even with a lowered upper mass cutoff of Mu = 30 M, results in rather old ages (10-40 Myr), in disagreement with the clumpy near-infrared morphologies. We prefer a model of an instantaneous burst of star formation with Mu = 100 M, occurring ∼6-7 Myr ago, in agreement with previous determinations and with the detection of W-R features in NGC 1614 and NGC 7714. Finally, we note a possible systematic difference in the amount of hot molecular gas between starburst and Seyfert galaxies.

Original languageEnglish
Pages (from-to)439-450
Number of pages12
JournalAstronomy and Astrophysics
Issue number2
Publication statusPublished - 1 Jan 2001
Externally publishedYes


  • Galaxies: individual: NGC 1614
  • Galaxies: individual: NGC 520
  • Galaxies: individual: NGC 7714
  • Galaxies: starburst
  • Infrared: galaxies
  • Stars: formation


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