H $$\alpha $$ α Kinematics of S $$^{4}$$ 4 G Spiral Galaxies: The Data

Erroz-Ferrer, Santiago

doi:10.1007/978-3-319-26398-4_3

Cited by 1 publication

(3 citation statements)

References 38 publications

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“…In order to compare the properties of Hii regions in interacting galaxies with those in isolated galaxies, we have included the parameters of Hii regions in a sample of 28 isolated galaxies observed with the same instrument (Erroz-Ferrer et al 2015), obtaining these parameters (the same as those for the interacting galaxies) for 1054 Hii regions. We present a subsample of the brightest Hii regions of the catalogue in TableA11 in for the interacting galaxies, and in TableA22 for the isolated galaxies.…”

Section: Discussionmentioning

confidence: 99%

“…Fig. 8 and Table4 are sorted by absolute magnitude (see Erroz-Ferrer et al (2015)), from brighter to fainter. The regime where the exponent is larger than three is again independent on the absolute magnitude of the galaxy.…”

Section: Scaling Relationsmentioning

confidence: 99%

“…We have measured the basic physical parameters (L Hα , R, and σv) of each Hii region and add equivalent data from the previous studies of interacting galaxies, Arp 270 and the Antennae galaxies, Zaragoza-Cardiel et al (2013, respectively. We have extracted the same parameters for the Hii regions of 28 isolated galaxies from Erroz-Ferrer et al (2015) in order to compare results from the two samples.…”

Section: Introductionmentioning

confidence: 99%

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Comparative internal kinematics of the H ii regions in interacting and isolated galaxies: implications for massive star formation modes

Zaragoza-Cardiel

Beckman

Font

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We have observed 10 interacting galaxy pairs using the Fabry-Perot interferometer GHαFaS (Galaxy Hα Fabry-Perot system) on the 4.2m William Herschel Telescope (WHT) at the Observatorio del Roque de los Muchachos, La Palma. We present here the Hα surface brightness, velocity and velocity dispersion maps for the 10 systems we have not previously observed using this technique, as well as the physical properties (sizes, Hα luminosities and velocity dispersion) of 1259 Hii regions from the full sample. We also derive the physical properties of 1054 Hii regions in a sample of 28 isolated galaxies observed with the same instrument in order to compare the two populations of Hii regions. We find a population of the brightest Hii regions for which the scaling relations, for example the relation between the Hα luminosity and the radius, are clearly distinct from the relations for the regions of lower luminosity. The regions in this bright population are more frequent in the interacting galaxies. We find that the turbulence, and also the star formation rate, are enhanced in the Hii regions in the interacting galaxies. We have also extracted the Hα equivalent widths for the Hii regions of both samples, and we have found that the distribution of Hii region ages coincides for the two samples of galaxies. We suggest that the SFR enhancement is brought about by gas flows induced by the interactions, which give rise to gravitationally bound gas clouds which grow further by accretion from the flowing gas, producing conditions favourable to star formation.

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Section: Discussionmentioning

confidence: 99%

Section: Scaling Relationsmentioning

confidence: 99%