All Figures

Figure 1: Stellar surface-density (, in units of ) of representative examples of an OC identified in this work (FSR 942, left panels), uncertain case (FSR 855, middle), and possible field fluctuation (FSR 801, right). The surfaces were built for a mesh size of , centred on the coordinates in Table 1. The observed (raw) and field-star decontaminated photometry are shown in the top and bottom panels, respectively.

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In the text

Figure 2: 2MASS CMDs extracted from the region of the OC FSR 942. Top panels: observed photometry with the colours ( left) and ( right). A relatively populous MS and a giant clump are suggested, together with an important contamination by disk stars. Middle: equal-area comparison field extracted from the region - . Bottom panels: decontaminated CMDs with the 1.0 Gyr Padova isochrone (solid line), showing the enhanced cluster morphology. The colour-magnitude filter used to isolate cluster MS/evolved stars is shown as a shaded region.

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In the text

	Figure 3: Same as Fig. 2 for the first half of the subsample of previously known OCs included in this paper. Only the CMD is shown.
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In the text

	Figure 4: Same as Fig. 3 for the remaining previously known OCs.
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In the text

	Figure 5: Same as Fig. 3 for the remaining OCs identified here. FSR 942 is shown in Fig. 2.
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In the text

	Figure 6: Field-star decontaminated CMDs of the uncertain cases (Unc) and the possible field fluctuations (FF).
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In the text

	Figure 7: Stellar RDPs (filled circles) of confirmed open clusters built with photometry that results from the use of colour-magnitude filters (Sect. 4). Solid line: best-fit King profile. Horizontal shaded region: offset field stellar background level. Gray regions: King fit uncertainty. Absolute scale is used.
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In the text

	Figure 8: Same as Fig. 7 for the remaining OCs.
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In the text

	Figure 9: RDPs of the uncertain cases (unc) and the possible field fluctuations (ff), in angular units. In general, the RDPs of the possible field fluctuations are narrower and more irregular than those of the OCs (Figs. 7 and 8) and uncertain cases.
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In the text

	Figure 10: Presently derived parameters for the OCs are compared to those in previous studies. Panels d) and e): the core and RDP radii derived here are compared to those in common with Froebrich et al. (2007a); we note that the latter authors use the tidal radii. Identity is indicated by the dashed line.
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In the text

	Figure 11: Relations involving astrophysical parameters of OCs. Empty circles: nearby OCs of the reference sample. For comparison, similar FSR OCs from previous papers are shown as well (triangles). The centrally-projected OCs FSR 1744, FSR 89 and FSR 31 are shown as filled triangles. Filled circles: the OCs dealt with in this work.
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In the text

Figure 12: Spatial distribution of the present star clusters (circles) compared to the WEBDA OCs with ages younger (gray circles) and older than 1.0 Gyr (``''). Small FSR OCs, i.e. those with  pc, are shown as filled circles. Clusters are overplotted on a schematic projection of the Galaxy as seen from the North pole, with 7.2 kpc as the Sun's distance to the Galactic centre. Main structures are identified.

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In the text

	Figure 13: Cluster radii as a function of the vertical distance to the plane ( top panels) and the on-plane distance ( bottom). Empty circles: OCs with RDP radius larger than 5 pc. Filled circles:  pc. The dashed line in panel a) represents the fit . FSR 756, FSR 932, and NGC 2126 are not included in the fit. The drop in RDP radii occurs in the region of the Local + Perseus Arms (panel  c).
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In the text