RR Lyrae in LMC Globular Clusters: Insights into the Oosterhoff ...

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Oosterhoff Groups In 1939 Oosterhoffnoticed a division inthe properties ofglobular cluster RRLyraesOOI OOII .55d .65d .32d .37dN RRc /N total .17 .44[Fe/H] >-1.7
The Oosterhoff dichotomy poses strong constraints on the Galaxy’s early history:Oo-IntermediateMilky WayOo dichotomy in fieldKMM test: Galactic distribution is bimodal(“Oosterhoff dichotomy”) with P > 99.99%Old halo 2/24Young halo 2/17Bulge/disk 0/02TOTAL 4/439.3%Oo-Intermediate“External”KMM test: single-peakeddistribution, withpeak in the middle of the Oosterhoff gap!ω Cen 0/01LMC GCs 4/12dSph, MCs 8/11For GCs 3/05Sag GCs 2/04CMa GCs 0/03The Galaxy is unlikely to have formed early on by accretion ofprotogalactic fragments resembling the early counterparts of itspresent-day dwarf satellite galaxies.TOTAL 17/3647.2%Catelan 2009, Ap&SS
Page 1 and 2: RR Lyrae in LMC Globular Clusters:I
Page 3 and 4: MW Inner 100kpc
Page 5: Bailey Types Based on shape oflight
Page 10 and 11: Target Objects 5 LMC globular clust
Page 14 and 15: NGC 1466 Periods accurate to betwee
Page 16 and 17: NGC 1466
Page 18 and 19: Reticulum Previously searched by Wa
Page 20 and 21: Other Clusters3 clusters included i
Page 22 and 23: Fourier Fits
Page 24 and 25: Fourier Derived Parameters RRab sta
Page 26 and 27: Trends in Fourier Parameters vs Clu
Page 28 and 29: Trends in Fourier Parameters vs Clu
Page 30 and 31: Summary The processes that created
Page 32 and 33: Are All Oo-Int Systems Equal?Draco

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