Evidence of a Non-universal Stellar Initial Mass Function. Insights from HST Optical Imaging of Six Ultra-faint Dwarf Milky Way Satellites
Using deep observations obtained with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST) , we demonstrate that the sub-solar stellar initial mass function (IMF) of six ultra-faint dwarf Milky Way satellites (UFDs) is more bottom light than the IMF of the Milky Way disk....
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Veröffentlicht in: | The Astrophysical journal 2018-03, Vol.855 (1), p.20 |
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Hauptverfasser: | , , , , , , , , , , , |
Format: | Artikel |
Sprache: | eng |
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Zusammenfassung: | Using deep observations obtained with the Advanced Camera for Surveys (ACS) on board the
Hubble Space Telescope (HST)
, we demonstrate that the sub-solar stellar initial mass function (IMF) of six ultra-faint dwarf Milky Way satellites (UFDs) is more bottom light than the IMF of the Milky Way disk. Our data have a lower-mass limit of ∼0.45
M
⊙
, while the upper limit is ∼0.8
M
⊙
, set by the turnoff mass of these old, metal-poor systems. If formulated as a single power law, we obtain a shallower IMF slope than the Salpeter value of −2.3, ranging from −1.01 for Leo IV to −1.87 for Boötes I. The significance of these deviations depends on the galaxy and is typically 95% or more. When modeled as a log-normal, the IMF fit results in a higher peak mass than in the Milky Way disk, but a Milky Way disk value for the characteristic system mass (∼0.22
M
⊙
) is excluded at only 68% significance, and only for some UFDs in the sample. We find that the IMF slope correlates well with the galaxy mean metallicity, and to a lesser degree, with the velocity dispersion and the total mass. The strength of the observed correlations is limited by shot noise in the number of observed stars, but future space-based missions like the
James Webb Space Telescope
(JWST
) and the
Wide-Field Infrared Survey Telescope (
WFIRST)
will enhance both the number of dwarf Milky Way satellites that can be studied in such detail and the observation depth for individual galaxies. |
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ISSN: | 0004-637X 1538-4357 |
DOI: | 10.3847/1538-4357/aaa973 |