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Multi-color photometry of the stellar populations in five fields in the thirdGalactic quadrant centred on the clusters NGC 2215, NGC 2354, Haffner 22,Ruprecht 11, and ESO489SC01 is interpreted in terms of a warped and flaredGalactic disk, without resort to an external entity such as the popularMonoceros or Canis Major overdensities. Except for NGC 2215, the clusters arepoorly or unstudied previously. The data generate basic parameters for eachcluster, including the distribution of stars along the line of sight. We usestar counts and photometric analysis, without recourse to Galactic-model-basedpredictions or interpretations, and confirms earlier results for NGC 2215 andNGC 2354. ESO489SC01 is not a real cluster, while Haffner~22 is an overlookedcluster aged about 2.5 Gyr. Conclusions for Ruprecht~11 are preliminary,evidence for a cluster being marginal. Fields surrounding the clusters showsignatures of young and intermediate-age stellar populations. The youngpopulation background to NGC~2354 and Ruprecht~11 lies 8-9 kpc from the Sun and$\sim$1 kpc below the formal Galactic plane, tracing a portion of theNorma-Cygnus arm, challenging Galactic models that adopt a sharp cut-off of thedisk 12-14 kpc from the Galactic center. The old population is metal poor withan age of 2-3 Gyr, resembling star clusters like Tombaugh 2 or NGC 2158. It hasa large color spread and is difficult to locate precisely. Young and oldpopulations follow a pattern that depends critically on the vertical locationof the thin and/or thick disk, and whether or not a particular line of sightintersects one, both, or none.

The complex stellar populations in the lines of sight to open clusters in the third Galactic quadrant