New models for a triaxial Milky Way spheroid and effect on the microlensing optical depthto the Large Magellanic Cloud

Abstract

We obtain models for a triaxial Milky Way spheroid based on data by Newberg and Yanny.The best fits to the data occur for a spheroid centre that is shifted by 3 kpc from theGalactic Centre. We investigate effects of the triaxiality on the microlensing optical depthto the Large Magellanic Cloud (LMC). The optical depth can be used to ascertain thenumber of massive compact halo objects (MACHOs); a larger spheroid contribution wouldimply fewer halo MACHOs. On the one hand, the triaxiality gives rise to more spheroidmass along the line of sight between us and the LMC and thus a larger optical depth.However, shifting the spheroid centre leads to an effect that goes in the otherdirection: the best fit to the spheroid centre is away from the line of sight to theLMC. As a consequence, these two effects tend to cancel so that the change inoptical depth due to the Newberg/Yanny triaxial halo is at most 50%. Aftersubtracting the spheroid contribution in the four models that we consider, theMACHO contribution (central value) to the mass of the Galactic Halo varies from∼(8–20)% if all excess lensing events observed by the MACHO Collaboration areassumed to be due to MACHOs. Here the maximum is due to the originalMACHO Collaboration results and the minimum is consistent with 0% at the1σ error level in the data.