We present an accurate analysis of the peculiar horizontal branch (HB) of the massive Galactic globular cluster NGC2808, based on high-resolution far-UV and optical images of the central region of the cluster obtained with the Hubble Space Telescope. We confirm the multimodal distribution of stars along the HB: four sub-populations separated by gaps are distinguishable. The detailed comparison with suitable theoretical models showed that (i) it is not possible to reproduce the luminosity of the entire HB with a single helium abundance, while an appropriate modelling is possible for three HB groups by assuming different helium abundances in the range 0.24 < deltaY < 0.4 that are consistent with the multiple populations observed in the main sequence; and (ii) canonical HB models are not able to properly match the observational properties of the stars populating the hottest end of the observed HB distribution, the so-called blue hook region. These objects are probably `hot flashers', stars that peel off the red giant branch before reaching the tip and ignite helium at high Teff. Both of these conclusions are based on the luminosity of the HB in the optical and ultraviolet bands and do not depend on specific assumptions about mass loss.
Dalessandro E., Salaris M., Ferraro F. R., Cassisi S., Lanzoni B., Rood R. T., et al. (2011). The peculiar horizontal branch of NGC2808. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 410, 694-704 [10.1111/j.1365-2966.2010.17479.x].
The peculiar horizontal branch of NGC2808
DALESSANDRO, EMANUELE;FERRARO, FRANCESCO ROSARIO;LANZONI, BARBARA;
2011
Abstract
We present an accurate analysis of the peculiar horizontal branch (HB) of the massive Galactic globular cluster NGC2808, based on high-resolution far-UV and optical images of the central region of the cluster obtained with the Hubble Space Telescope. We confirm the multimodal distribution of stars along the HB: four sub-populations separated by gaps are distinguishable. The detailed comparison with suitable theoretical models showed that (i) it is not possible to reproduce the luminosity of the entire HB with a single helium abundance, while an appropriate modelling is possible for three HB groups by assuming different helium abundances in the range 0.24 < deltaY < 0.4 that are consistent with the multiple populations observed in the main sequence; and (ii) canonical HB models are not able to properly match the observational properties of the stars populating the hottest end of the observed HB distribution, the so-called blue hook region. These objects are probably `hot flashers', stars that peel off the red giant branch before reaching the tip and ignite helium at high Teff. Both of these conclusions are based on the luminosity of the HB in the optical and ultraviolet bands and do not depend on specific assumptions about mass loss.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
