Hubble Tarantula Treasury project: V. The star cluster Hodge 301: the old face of 30 Doradus
Based on color-magnitude diagrams (CMDs) from the Hubble Space Telescope Hubble Tarantula Treasury Project (HTTP) survey, we present the star formation history (SFH) of Hodge~301, the oldest star cluster in the Tarantula Nebula. The HTTP photometry extends faint enough to reach, for the first time,...
Gespeichert in:
| Hauptverfasser: | , , |
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| Dokumenttyp: | Article (Journal) Kapitel/Artikel |
| Sprache: | Englisch |
| Veröffentlicht: |
2016
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| In: |
Arxiv
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| Online-Zugang: | Verlag, kostenfrei, Volltext: http://arxiv.org/abs/1610.06180
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| Verfasserangaben: | M. Cignoni, E. Sabbi, R.P. van der Marel, D.J. Lennon, M. Tosi, E.K. Grebel, J.S. Gallagher, A. Aloisi, G. de Marchi, D.A. Gouliermis, S. Larsen, N. Panagia, L.J. Smith |
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| 245 | 1 | 0 | |a Hubble Tarantula Treasury project |b V. The star cluster Hodge 301: the old face of 30 Doradus |c M. Cignoni, E. Sabbi, R.P. van der Marel, D.J. Lennon, M. Tosi, E.K. Grebel, J.S. Gallagher, A. Aloisi, G. de Marchi, D.A. Gouliermis, S. Larsen, N. Panagia, L.J. Smith |
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| 520 | |a Based on color-magnitude diagrams (CMDs) from the Hubble Space Telescope Hubble Tarantula Treasury Project (HTTP) survey, we present the star formation history (SFH) of Hodge~301, the oldest star cluster in the Tarantula Nebula. The HTTP photometry extends faint enough to reach, for the first time, the cluster pre-main sequence (PMS) turn-on, where the PMS joins the main sequence. Using the location of this feature, along with synthetic CMDs generated with the latest PARSEC models, we find that Hodge~301 is older than previously thought, with an age between 26.5 and 31.5 Myr. From this age, we also estimate that between 38 and 61 supernovae Type-II exploded in the region. The same age is derived from the main sequence turn-off, whereas the age derived from the post-main sequence stars is younger and between 20 and 25 Myr. Other relevant parameters are a total stellar mass of $\approx 8800\,\pm 800$M$_{\odot}$ and average reddening E(B$-$V) $\approx 0.22-0.24$ mag, with a differential reddening $\delta$E(B$-$V)$\approx 0.04$ mag. | ||
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