Overabundance of massive stars in the Tarantula Nebula
An international team of astronomers has revealed an 'astonishing' overabundance of massive stars in a neighbouring galaxy.
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| The Tarantula Nebula [Credit: NASA, ESA, D. Lennon] |
As part of the VLT-FLAMES Tarantula Survey (VFTS), the team used ESO's Very Large Telescope to observe nearly 1,000 massive stars in 30 Doradus, a gigantic stellar nursery also known as the Tarantula Nebula. The team used detailed analyses of about 250 stars with masses between 15 and 200 times the mass of our Sun to determine the distribution of massive stars born in 30 Doradus -- the so-called initial mass function (IMF).
IAC/ULL co-authors have played a fundamental role in the determination of the massive star properties. Sergio Simon Diaz, IAC researcher, declares: "The accurate determination of the physical parameters of each star is a must. In science, the careful evaluation of our uncertainties is crucial to achieve firm conclusions."
Massive stars are particularly important for astronomers because of their enormous feedback. They can explode in spectacular supernovae at the end of their lives, forming some of the most exotic objects in the Universe -- neutron stars and black holes.
Until recently, the existence of stars up to 200 solar masses was highly disputed, and the study shows that a maximum birth mass of stars of 200-300 solar masses appears likely.
In most parts of the Universe studied by astronomers to date, stars become rarer the more massive they are. The IMF predicts that most stellar mass is in low-mass stars and that less than 1% of all stars are born with masses in excess of ten times that of the Sun. Measuring the proportion of massive stars is extremely difficult -- primarily because of their scarcity -- and there are only a handful of places in the local Universe where this can be done.
30 Doradus
The team turned to 30 Doradus, the biggest local star-forming region, which hosts some of the most massive stars ever found, and determined the masses of massive stars with unique observational, theoretical and statistical tools. This large sample allowed the scientists to derive the most accurate high-mass segment of the IMF to date, and to show that massive stars are much more abundant than previously thought. Chris Evans, the principal investigator of VFTS and a co-author of the study, said: 'In fact, our results suggest that most of the stellar mass is actually no longer in low-mass stars, but a significant fraction is in high-mass stars.'
Stars are cosmic engines and have produced most chemical elements heavier than helium, from the oxygen we breathe every day to the iron in our blood. During their lives, massive stars produce copious amounts of ionising radiation and kinetic energy through strong stellar winds. The ionising radiation of massive stars was crucial for the re-brightening of the Universe after the so-called Dark Ages, and their mechanical feedback drives the evolution of galaxies.
Artemio Herrero, IAC/ULL researcher and co-author, explains: "Understanding the physics of massive stars under the varying conditions found from the Milky Way to the early Universe is fundamental to our knowledge of the cosmos evolution and how we see it presently."
Fabian Schneider added: "Our results have far-reaching consequences for the understanding of our cosmos: there might be 70% more supernovae, a 200% increase in chemical yields and 270% more ionising radiation from massive star populations. Also, the formation rate of black holes might be increased by 180%, directly translating into a corresponding increase of binary black hole mergers that have recently been detected via their gravitational wave signals."
The team's research leaves many open questions, which they intend to investigate in the future: how universal are the findings, and have other starburst regions produced a similar overabundance of massive stars? What are the exact consequences of this for the evolution of our cosmos and also the occurrence of supernovae and gravitational wave events?
The study is published in Science.
Source: Instituto de Astrofisica de Canarias (IAC) [January 31, 2018]
