The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit

Abstract

Spectroscopic analyses of hydrogen-rich WN 5-6 stars within the young star clusters NGC 3603 and R136 are presented, using archival Hubble Space Telescope and Very Large Telescope spectroscopy, and high spatial resolution near-IR photometry, including Multi-Conjugate Adaptive Optics Demonstrator (MAD) imaging of R136. We derive high stellar temperatures for the WN stars in NGC 3603 (T * ∼ 42 ± 2 kK) and R136 (T * ∼ 53 ± 3 kK) plus clumping-corrected mass-loss rates of 2-5 × 10 −5 M yr −1 which closely agree with theoretical predictions from Vink et al. These stars make a disproportionate contribution to the global ionizing and mechanical wind power budget of their host clusters. Indeed, R136a1 alone supplies ∼7 per cent of the ionizing flux of the entire 30 Doradus region. Comparisons with stellar models calculated for the main-sequence evolution of 85-500 M accounting for rotation suggest ages of ∼1.5 Myr and initial masses in the range 105-170 M for three systems in NGC 3603, plus 165-320 M for four stars in R136. Our high stellar masses are supported by consistent spectroscopic and dynamical mass determinations for the components of NGC 3603A1. We consider the predicted X-ray luminosity of the R136 stars if they were close, colliding wind binaries. R136c is consistent with a colliding wind binary system. However, short period, colliding wind systems are excluded for R136a WN stars if mass ratios are of order unity. Widely separated systems would have been expected to harden owing to early dynamical encounters with other massive stars within such a high-density environment. From simulated star clusters, whose constituents are randomly sampled from the Kroupa initial mass function, both NGC 3603 and R136 are consistent with an tentative upper mass limit of ∼300 M . The Arches cluster is either too old to be used to diagnose the upper mass limit, exhibits a deficiency of very massive stars, or more likely stellar masses have been underestimated -initial masses for the most luminous stars in the Arches cluster approach 200 M according to contemporary stellar and photometric results. The potential for stars greatly exceeding 150 M within metal-poor galaxies suggests that such pair-instability supernovae could occur within the local universe, as has been claimed for SN 2007bi.

Implications of the gravitational wave event GW150914

“…[107] found three stars in the Large Magellanic Cloud (metallicity ∼ 0.5 times solar) with current masses in excess of 150 M ⊙ . If this means that stars can form up to hundreds of solar masses, then [108] found that > ∼ 100 M ⊙ − 100 M ⊙ black hole mergers might originate in massive stellar binaries.…”

Narrow He II emission in star-forming galaxies at low metallicity

“…Crowther et al 2010), we estimate in total log(L He ii ) ≈ 38.6. This estimate is based on a synthetic model for the LMC WN5h star VFTS 682 from Bestenlehner et al (2011) with log(L/L ) = 6.5 and log(L He ii ) = 37.5, which was scaled to the total luminosity of the seven objects (log(L/L ) = 7.58 ± 0.03, as obtained from Crowther et al 2010;Hainich et al 2014;Bestenlehner et al 2014). We note that this value is uncertain as for some of the stars different luminosities have been obtained in different works, and one of the stars, Mk 34, is a known binary.…”

“…Hamann et al 2006;Crowther et al 2010;Hainich et al 2014;Bestenlehner et al 2014). The HRD positions of these objects suggest that they are very massive stars (VMS) with initial masses in excess of ∼100 M , and reaching up to 300 M (cf.…”

The very massive star content of the nuclear star clusters in NGC 5253

“…There are potentially two ways this can be done: the inclusion of rotating massive stars (Levesque et al 2012;Leitherer et al 2014); and/or the inclusion of very massive stars (Crowther et al 2010;Doran et al 2013). We consider each in turn.…”