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Title: HUBBLE TARANTULA TREASURY PROJECT. V. THE STAR CLUSTER HODGE 301: THE OLD FACE OF 30 DORADUS

Journal Article · · Astrophysical Journal
 [1]; ; ; ;  [2];  [3];  [4];  [5];  [6];  [7];  [8];  [9]
  1. Department of Physics—University of Pisa, Largo Pontecorvo, 3 Pisa, I-56127 (Italy)
  2. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, 21218 (United States)
  3. European Space Astronomy Centre, Apdo. de Correo 78, E-28691 Villanueva de la Canada, Madrid (Spain)
  4. INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna (Italy)
  5. Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12-14, D-69120 Heidelberg (Germany)
  6. Department of Astronomy, University of Wisconsin-Madison, WI 53706 (United States)
  7. European Space Research and Technology Centre, Keplerlaan 1, NL-2200 AG Noordwijk (Netherlands)
  8. Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle-Str. 2, D-69120 Heidelberg (Germany)
  9. Department of Astrophysics, Radboud University, P.O. Box 9010, NL-6500 GL Nijmegen (Netherlands)

Based on color–magnitude diagrams (CMDs) from the Hubble Space Telescope  Hubble Tarantula Treasury Project (HTTP) survey, we present the star formation history 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 Type II supernovae 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 ≈8800 ± 800  M {sub ⊙} and average reddening E ( B − V ) ≈ 0.22–0.24 mag, with a differential reddening δE ( B − V ) ≈ 0.04 mag.

OSTI ID:
22660893
Journal Information:
Astrophysical Journal, Vol. 833, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
Country of Publication:
United States
Language:
English