We present high-resolution Hα velocity fields and rotation curves of the circumnuclear star-forming regions of five barred galaxies. Two of the five objects show substantially smaller initial rises than the three others; these two objects also have spiral structure inside the circumnuclear star-forming ring.
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Circumnuclear Star-Forming Regions in Barred GalaxiesKnapen, Johan H. et al.121999
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Clear Evidence for the Presence of Second-generation Asymptotic Giant Branch Stars in Metal-poor Galactic Globular Clusters
Galactic globular clusters (GCs) are known to host multiple stellar populations: a first generation (FG) with a chemical pattern typical of halo field stars and a second generation (SG) enriched in Na and Al and depleted in O and Mg. Both stellar generations are found at different evolutionary stages (e.g., the main-sequence turnoff, the subgiant
García-Hernández, D. A. et al.Advertised on:
122015 -
Clusters in point distributions
We present a procedure for obtaining the mean density of clusters and their associated structures in a very general type of distribution. We first consider the one-dimensional case, and then use it to develop the procedure according to the d-dimensional case. These procedures require the probability that a randomly placed body should contain no
Betancort-Rijo, J. E.Advertised on:
121994 -
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CO J=1->0 mapping of the cometary nebula 1548c27.
We have acquired CO J=1->0 mapping of a region 2x2arcmin^2^ about the cometary nebula and jet outflow source 1548c27. We find little evidence for interaction between the jet and molecular cloud, although it is found that the reflection nebula is embedded within a neutral condensation of size =~10^2^arcsec. Kinematic variations across the source
Phillips, J. P. et al.Advertised on:
121996 -
Collective pulsational velocity broadening due to gravity modes as a physical explanation for macroturbulence in hot massive stars
Aims. We aimed at finding a physical explanation for the occurrence of macroturbulence in the atmospheres of hot massive stars, a phenomenon found in observations for more than a decade but that remains unexplained. Methods: We computed time series of line profiles for evolved massive stars broadened by rotation and by hundreds of low-amplitude
Aerts, C. et al.Advertised on:
122009