All Tables

Table 1: Parameters for the four M 31 models considered by Kerins (2004). Columns are the model name, the component name, the mass of the component, its central density $\rho _0$ and the adopted cut-off radius R. Additional columns give, where appropriate, the core radius a, the disk scale length h and height H, the flattening parameter q and the B-band mass-to-light ratio $M/L_{\rm B}$ in solar units.
Table 2: The threshold impact parameters $\langle u_{\rm T} \rangle _{\phi}$ and $\langle u_{\rm T}^{~2} \rangle _{\phi}$ averaged over the whole M 31 galaxy are given for different values of the superpixel dimension $N \times N$ , sky background $m_{\rm sky}$ , fraction $f_{\rm see}$ of the superpixel covered by the PSF and superpixel flux stability $\sigma _{\rm T}$ .
Table 3: The expected number of events $\langle E_{\rm p} \rangle$ per year in pixel lensing observations towards the M 31 galaxy for different locations of sources and lenses is shown. We consider the $100\times 70$ arcmin² region oriented along the major axis of M 31. and exclude events occurring within a radius of 8 arcmin of the M 31 center. Sources and lenses in the M 31 bulge and disk are indicated by indices 1 and 2, while lenses in the M 31 halo and MW disk and halo by indices 3, 5 and 6. The first and second indices refer to source and lens, respectively. The mean mass of bulge and disk stars is $\sim$ $0.31~M_{\odot}$ and $\sim$ $0.53~M_{\odot}$ , respectively. For the lenses in the M 31 and MW halos we take a mass of $\simeq$ $0.5~M_{\odot}$ and a MACHO fraction $f_{\rm MACHO} \simeq 20\%$ .
Table 4: The same as in Table 3 for lenses located in the M 31 galaxy. In the last three columns we give the calculated pixel event number for the South/North Semisphere and in brackets their ratio.
Table 5: The instantaneous number of events in pixel lensing observations towards the M 31 galaxy for different locations of sources and lenses is shown (for details see text). Numbers in brackets refer to the South Semisphere of M 31. For the MW disk and halo, lenses in the South Semisphere of the MW contribute to roughly one half of the total and so the corresponding event numbers are not given.