Microlensing search towards M 31

¹ Dipartimento di Fisica “E.R. Caianiello”, Università degli Studi di Salerno, and INFN Sez. di Napoli – Gruppo Collegato di Salerno, Italy
² Osservatorio Astronomico di Capodimonte, Napoli, and INFN, Sez. di Napoli, Italy
³ Observatoire Midi-Pyrenées, France
⁴ CERN, 1211 Genève 23, Switzerland
⁵ Physique Corpusculaire et Cosmologie, Collège de France, Paris, France
⁶ Dipartimento di Scienze Fisiche, Università degli Studi di Napoli “Federico II” and INFN, Sez. di Napoli, Italy
⁷ Dipartimento di Fisica, Università di Lecce, Italy
⁸ Institute of Theoretical Physics, University of Zürich, Switzerland
⁹ Institute of Theoretical Physics, ETH, Zürich, Switzerland
¹⁰ INFN Sez. di Pavia, Pavia, Italy.

Corresponding author: S. Calchi Novati, novati@sa.infn.it

Received: 18 June 2001
Accepted: 25 October 2001

Abstract

We present the first results of the analysis of data collected during the 1998–99 observational campaign at the 1.3 meter McGraw-Hill Telescope, towards the Andromeda galaxy (M 31), aimed to detect gravitational microlensing effects as a probe for the presence of dark matter in our Galaxy and in the M 31 halo. The analysis is performed using the pixel lensing technique, which consists of the study of flux variations of unresolved sources and has been proposed and implemented by the AGAPE collaboration. We carry out a shape analysis by demanding that the detected flux variations be achromatic and compatible with a Paczyński light curve. We apply the Durbin-Watson hypothesis test to the residuals. Furthermore, we consider the background of variables sources. Finally five candidate microlensing events emerge from our selection. Comparing with the predictions of a Monte Carlo simulation, assuming a standard spherical model for the M 31 and Galactic haloes, and typical values for the MACHO mass, we find that our events are only marginally consistent with the distribution of observable parameters predicted by the simulation.