Star Formation Rates in Interacting Starburst Galaxies

Dopita, Michael A.; Pereira, M. J.; Kewley, Lisa J.; Capaccioli, M.

doi:10.1086/342624

Cited by 105 publications

(139 citation statements)

References 84 publications

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“…Thus, the Hα line might be dimmed by dust and appears weaker. The derived star formation rates lies within the range covered by the interacting starburst galaxy sample of Dopita et al (2002). In most of our observed galaxies the star formation is enhanced, probably due to the merger.…”

Section: Optical Spectroscopysupporting

confidence: 75%

The Structure and Interaction History of Moderate Luminosity Mergers

Hüttemeister¹,

Manthey²

2006

Proc. IAU

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Interaction and merging are the two most important driving forces of galaxy evolution. In contrast to the well studied major mergers of two large gas-rich disk galaxies, which may lead to Ultraluminous Infrared Galaxies (ULIRGs, LFIR>1012 L⊙), mergers between galaxies of unequal mass or a spiral and an elliptical (S+E mergers) are still poorly understood. These moderate luminosity mergers typically have LFIR > 1011 L⊙. Here, we present the results of our multiwavelength study of a sample of such kind of mergers, including interferometric HI and single-dish CO observations, optical and near-infrared imaging as well as optical spectroscopy.

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Section: Optical Spectroscopysupporting

confidence: 75%

The Structure and Interaction History of Moderate Luminosity Mergers

Hüttemeister¹,

Manthey²

2006

Proc. IAU

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“…(5). The majority of the galaxies show the typical value for starforming galaxies, log R = 1.3 ± 0.4 Dopita et al (2002). The low value in R found in POX 4 and NGC 5253 may be because the Hα flux has been overestimated, although the situation of NGC 5253 is far from clear ).…”

Section: Fir/radio Correlationmentioning

confidence: 89%

“…These observations also permit detecting of extremely young, dense, heavily embedded star clusters (Kobulnicky & Johnson 1999;Johnson & Kobulnicky 2003). Although radio data at frequencies different from 1.4 GHz are not usually available for this kind of galaxy, we applied the equation provided by Dopita et al (2002),…”

Section: Radio-continuum Datamentioning

confidence: 99%

“…Condon (1992) and Niklas et al (1997) indicated that the nonthermal component is more than 90% of the total at this frequency. It is common to consider the nonthermal to thermal ratio, R; Dopita et al (2002) report that the average value in starburst galaxies is log R = 1.3 ± 0.4. Radio continuum and FIR data help to discern the normal or active (that is, a galaxy hosting an AGN) nature.…”

Section: Radio-continuum Datamentioning

confidence: 99%

“…As previous authors have pointed out (i.e. Dopita et al 2002;James et al 2005), the correction of the Hα fluxes for both extinction and [N ii] emission is vital to a reliable estimation of the SFR using Hα-images.…”

Section: Analysis Of the Star-formation Ratesmentioning

confidence: 99%

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Massive star formation in Wolf-Rayet galaxies

López-Sánchez

2010

A&A

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Aims. We performed a comprehensive analysis of a sample of 20 starburst galaxies that show a substantial population of very young massive stars, most of them classified as Wolf-Rayet galaxies. Methods. In this paper, the last in the series, we analyze the global properties of our galaxy sample using multiwavelength data extracted from our own observations (Hα fluxes, B and H-band magnitudes) and from the literature, which include X-ray, FUV, FIR, and radio (both H i spectral line and 1.4 GHz radio-continuum) measurements.Results. The agreement between our Hα-based star-formation rates (Sfr) and those provided by indicators at other wavelengths is remarkable, but we consider that the new Hα-based calibration provided by Calzetti et al. (2007, ApJ, 666, 870) should be preferred to older calibrations. The FUV-based Sfr provides a powerful tool for analyzing the star-formation activity on both global and local scales independently to the Hα emission. We provide empirical relationships between the ionized gas mass, neutral gas mass, dust mass, stellar mass, and dynamical mass with the B-luminosity. Although all mass estimations increase with increasing luminosity, we find important deviations to the general trend in some objects, which seem to be the consequence of their particular evolutionary histories. The analysis of the mass-to-light ratios give similar results. We investigate the mass-metallicity relations and conclude that both the nature and the star-formation history are needed to understand the relationships between both properties. The majority of the galaxies follow a Schmidt-Kennicutt scaling law of star-formation that agrees with that reported in individual star-forming regions within M 51 but not with that found in normal spiral galaxies. Dwarf galaxies seem to be forming stars more efficiently than the outskirts of spiral galaxies. We find a relation between the reddening coefficient and the warm dust mass indicating that the extinction is mainly internal to the galaxies. The comparison with the closed-box model also indicates that the environment has strongly affected their evolution. Conclusions. Considering all multiwavelength data, we found that 17 up to 20 galaxies are clearly interacting or merging with lowluminosity dwarf objects or H i clouds. The remaining three galaxies (Mkn 5, SBS 1054+364, and SBS 1415+437) show considerable divergences of some properties when comparing with similar objects. Many of the interacting/merging features are only detected when deep optical spectroscopy and a detailed multiwavelength analysis, including H i observations, are obtained. We conclude that interactions do play a fundamental role in the triggering mechanism of the strong star-formation activity observed in dwarf starburst galaxies.

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