CADIS has seen the Virgo overdensity and parts of the Monoceros and ‘ Orphan ’ streams in retrospect

We reanalyze deep star counts in five CADIS fields. The data are presented as vertical density distributions of stars perpendicular to the Galactic plane. In three fields the profiles are consistent with each other, while in two fields significant overdensities of stars are found. The overdensity in one field can be associated with the Virgo overdensity which can be traced right into the disk of the Milky Way. Using this detection we estimate the mass of the Virgo overdensity and show that this is equivalent to the stellar content of a Local Group dwarf spheroidal galaxy. The overdensity in the second field is more difficult to associate with a previously known overdensity. We suggest that it is related both to the Monoceros stream and the recently discovered Orphan stream. In two previous papers (Phleps et al. 2000, 2005) we have studied the distribution of stars in the Milky Way using deep star counts based on Calar Alto Deep Imaging Survey data. For this purpose we analyzed five fields which contained in total 1627 faint stars (15.5 < R < 23). We do not repeat here any details of our analysis, but give again in Table 1 the coordinates of the fields. At the time of writing the papers we were mainly interested in determining descriptive parameters of the density distributions of the various components of the Milky Way such as the vertical scale heights of the thin and thick disks, respectively , their relative normalization and the parameters of the halo density law. We realized, however, already then that, while the 1h, 16h, and 32h fields gave very consistent results, the 9h and to a lesser degree the 13h field lead to discrepant results in the sense that the vertical density distribution of the stars in these fields had a few kpc above the midplane a shallower slope than in the three other fields. With the advent of the Data Release 5 of the Sloan Digital Sky Survey and its subsequent analyses by Juri´c et al. (2006) and Belokurov et al. (2006a, b) over-densely populated parts of the density distribution of the stars in the Milky Way have been revealed in such rich detail that we can interpret now in retrospect also the results of the 13h field in a consistent way, whereas the nature of the overdensity in 9h remains at present less clear. By pure chance two out …