Limits on the Macho Content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds

By P. Tisserand, L. Guillou, C. Afonso, J. Albert, J. Andersen, R. Ansari, E. Aubourg, P. Bareyre, J. Beaulieu, X. Charlot and 28 more. 2006

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The EROS-2 project was designed to test the hypothesis that massive compact halo objects (the so-called ''machos'') could be a major component of the dark matter halo of the Milky Way galaxy. To this end, EROS-2 monitored millions of stars in the Magellanic clouds for microlensing events caused by such objects. (abridged)

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1ce165bd8f83ae40f0ea08c52c2fa7e8047dfe33

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Citations in the corpus

WIMP dark matter candidates and searches—current status and future prospects (2017, neutral): “This strategy led to an exclusion of MACHOs with masses in the range 0.6 × 10−7–15M as the dominant form of DM in the Galaxy [26].”
New experimental approaches in the search for axion-like particles (2018, methodology): “Under some assumptions on the minicluster mass fraction in our galaxy and its neighbourhood, the EROS survey of the large magellanic cloud [248] and Subaru’s HSC survery of Andromeda (M31) [249] (originally intended as primordial black hole searches) can be used to set strong constraints on the amou”
EXPERIMENTAL LIMITS ON PRIMORDIAL BLACK HOLE DARK MATTER FROM THE FIRST 2 YR OF KEPLER DATA (2013, background): “…that together have eliminated MACHO DM (which includes PBH DM) in the mass range from 3 × 10−8 M to 30 M from being the entirety of the DM (Carr et al. 2010; Wyrzykowski et al. 2011a, 2011b; Tisserand et al. 2007; Yoo et al. 2004; Alcock et al. 1996, 1998, 2001, Renault et al. 1997; Griest 1991).”
Primordial black holes with an accurate QCD equation of state (2018, background): “Other microlensing experiments in the Magellanic Clouds [89, 96] produced conflicting results.”
Formation of Supermassive Black Hole Seeds (2016, background): “Primordial black holes may have born during the early stages of Big Bang but there is no observational evidence for their existence (Alcock et al. 2000; Afshordi et al. 2003; Tisserand et al. 2007; Ricotti et al. 2008).”
The local dark matter density (2014, background): “Microlensing constraints from the Milky Way bulge and the nearby Large and Small Magellanic Clouds put an upper bound of the mass of ‘compact object’ dark matter of Mdm 10 −7 M (e.g. Tisserand et al., 2007).”
Lectures on Dark Matter Physics (2016, background): “Such objects cause lensing events when they pass in front of bright stars and the lack of such detections [49] sets an upper bound of”
Farthest Neighbor: The Distant Milky Way Satellite Eridanus II (2016, methodology): “When the results from Eri II are combined with those from microlensing and wide binary searches (Alcock et al. 2001; Tisserand et al. 2007; Quinn et al. 2009), MACHOs with mass & 10−7 M are constrained to be a subdominant component of dark matter.”
LSST: From Science Drivers to Reference Design and Anticipated Data Products (2008, background): “Given the age 30 of the Galactic halo, a significant fraction of the mass in this component may reside in these remnant stars (e.g., Alcock et al. 2000; Tisserand et al. 2007) and therefore their discovery directly constrains the Galactic mass budget.”