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Extremely metal-poor stars from the cosmic dawn in the bulge of the Milky Way.

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Title: Extremely metal-poor stars from the cosmic dawn in the bulge of the Milky Way.
Authors: Howes, L. M., Casey, A. R., Asplund, M., Keller, S. C., Yong, D., Nataf, D. M., Poleski, R., Lind, K., Kobayashi, C., Owen, C. I., Ness, M., Bessell, M. S., Da Costa, G. S., Schmidt, B. P., Tisserand, P., Udalski, A., Szymański, M. K., Soszyński, I., Pietrzyński, G., Ulaczyk, K.
Source: Nature. 11/26/2015, Vol. 527 Issue 7579, p484-487. 4p. 6 Charts, 4 Graphs.
Subjects: Metal-poor stars, Helium, Big bang theory, Galactic Center, Halos (Meteorology)
Abstract: The first stars are predicted to have formed within 200 million years after the Big Bang, initiating the cosmic dawn. A true first star has not yet been discovered, although stars with tiny amounts of elements heavier than helium ('metals') have been found in the outer regions ('halo') of the Milky Way. The first stars and their immediate successors should, however, preferentially be found today in the central regions ('bulges') of galaxies, because they formed in the largest over-densities that grew gravitationally with time. The Milky Way bulge underwent a rapid chemical enrichment during the first 1-2 billion years, leading to a dearth of early, metal-poor stars. Here we report observations of extremely metal-poor stars in the Milky Way bulge, including one star with an iron abundance about 10,000 times lower than the solar value without noticeable carbon enhancement. We confirm that most of the metal-poor bulge stars are on tight orbits around the Galactic Centre, rather than being halo stars passing through the bulge, as expected for stars formed at redshifts greater than 15. Their chemical compositions are in general similar to typical halo stars of the same metallicity although intriguing differences exist, including lower abundances of carbon. [ABSTRACT FROM AUTHOR]
Copyright of Nature is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Database: Psychology and Behavioral Sciences Collection
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  Data: Extremely metal-poor stars from the cosmic dawn in the bulge of the Milky Way.
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  Data: <searchLink fieldCode="AR" term="%22Howes%2C+L%2E+M%2E%22">Howes, L. M.</searchLink><br /><searchLink fieldCode="AR" term="%22Casey%2C+A%2E+R%2E%22">Casey, A. R.</searchLink><br /><searchLink fieldCode="AR" term="%22Asplund%2C+M%2E%22">Asplund, M.</searchLink><br /><searchLink fieldCode="AR" term="%22Keller%2C+S%2E+C%2E%22">Keller, S. C.</searchLink><br /><searchLink fieldCode="AR" term="%22Yong%2C+D%2E%22">Yong, D.</searchLink><br /><searchLink fieldCode="AR" term="%22Nataf%2C+D%2E+M%2E%22">Nataf, D. M.</searchLink><br /><searchLink fieldCode="AR" term="%22Poleski%2C+R%2E%22">Poleski, R.</searchLink><br /><searchLink fieldCode="AR" term="%22Lind%2C+K%2E%22">Lind, K.</searchLink><br /><searchLink fieldCode="AR" term="%22Kobayashi%2C+C%2E%22">Kobayashi, C.</searchLink><br /><searchLink fieldCode="AR" term="%22Owen%2C+C%2E+I%2E%22">Owen, C. I.</searchLink><br /><searchLink fieldCode="AR" term="%22Ness%2C+M%2E%22">Ness, M.</searchLink><br /><searchLink fieldCode="AR" term="%22Bessell%2C+M%2E+S%2E%22">Bessell, M. S.</searchLink><br /><searchLink fieldCode="AR" term="%22Da+Costa%2C+G%2E+S%2E%22">Da Costa, G. S.</searchLink><br /><searchLink fieldCode="AR" term="%22Schmidt%2C+B%2E+P%2E%22">Schmidt, B. P.</searchLink><br /><searchLink fieldCode="AR" term="%22Tisserand%2C+P%2E%22">Tisserand, P.</searchLink><br /><searchLink fieldCode="AR" term="%22Udalski%2C+A%2E%22">Udalski, A.</searchLink><br /><searchLink fieldCode="AR" term="%22Szymański%2C+M%2E+K%2E%22">Szymański, M. K.</searchLink><br /><searchLink fieldCode="AR" term="%22Soszyński%2C+I%2E%22">Soszyński, I.</searchLink><br /><searchLink fieldCode="AR" term="%22Pietrzyński%2C+G%2E%22">Pietrzyński, G.</searchLink><br /><searchLink fieldCode="AR" term="%22Ulaczyk%2C+K%2E%22">Ulaczyk, K.</searchLink>
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  Data: The first stars are predicted to have formed within 200 million years after the Big Bang, initiating the cosmic dawn. A true first star has not yet been discovered, although stars with tiny amounts of elements heavier than helium ('metals') have been found in the outer regions ('halo') of the Milky Way. The first stars and their immediate successors should, however, preferentially be found today in the central regions ('bulges') of galaxies, because they formed in the largest over-densities that grew gravitationally with time. The Milky Way bulge underwent a rapid chemical enrichment during the first 1-2 billion years, leading to a dearth of early, metal-poor stars. Here we report observations of extremely metal-poor stars in the Milky Way bulge, including one star with an iron abundance about 10,000 times lower than the solar value without noticeable carbon enhancement. We confirm that most of the metal-poor bulge stars are on tight orbits around the Galactic Centre, rather than being halo stars passing through the bulge, as expected for stars formed at redshifts greater than 15. Their chemical compositions are in general similar to typical halo stars of the same metallicity although intriguing differences exist, including lower abundances of carbon. [ABSTRACT FROM AUTHOR]
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  Data: <i>Copyright of Nature is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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