Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/24306
Title: | Searching in the dark: the dark mass content of the Milky Way globular clusters NGC288 and NGC6218 | Authors: | SOLLIMA, ANTONIO LUIGI Ferraro, F. R. Lovisi, L. Contenta, F. Vesperini, E. ORIGLIA, Livia Lapenna, E. Lanzoni, B. Mucciarelli, A. Dalessandro, Emanuele Pallanca, C. |
Issue Date: | 2016 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 462 | Issue: | 2 | First Page: | 1937 | Abstract: | We present an observational estimate of the fraction and distribution of dark mass in the innermost region of the two Galactic globular clusters NGC 6218 (M12) and NGC 288. Such an assessment has been made by comparing the dynamical and luminous mass profiles derived from an accurate analysis of the most extensive spectroscopic and photometric surveys performed on these stellar systems. We find that non-luminous matter constitutes more than 60 per cent of the total mass in the region probed by our data (R < 1.6 arcmin ∼ r<SUB>h</SUB>) in both clusters. We have carefully analysed the effects of binaries and tidal heating on our estimate and ruled out the possibility that our result is a spurious consequence of these effects. The dark component appears to be more concentrated than the most massive stars suggesting that it is likely composed of dark remnants segregated in the cluster core. | URI: | http://hdl.handle.net/20.500.12386/24306 | URL: | https://academic.oup.com/mnras/article/462/2/1937/2589898 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stw1779 | Bibcode ADS: | 2016MNRAS.462.1937S | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
stw1779.pdf | PDF editoriale | 1.52 MB | Adobe PDF | View/Open |
Page view(s)
48
checked on May 2, 2024
Download(s)
13
checked on May 2, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.