seen only in the inclination. The gap between the MON and NOO is also visible in Figure 1. The $q-i$ phase space and the dispersion of orbits from the mean orbit of each shower imply that the NOO exhibit wider dispersion. The cometary orbit is located within MON elements and, therefore, the NOO meteoroids seem to be older than MON. The inclination exhibits interesting behavior. The nominal orbit of the parent comet lies within the MON orbits, while the NOO orbits are less inclined and are apparently well separated from the MON orbits. There seems to be no overlapping in the inclination between the two clumps representing the MON and NOO in Figure 2.

   elements     a       e        q        i     $\omega$   $\Omega$   $v_{g}$\[km/s\]   mass\[g\]      activity       No     author
  ---------- ------- -------- -------- ------- ---------- ---------- ----------------- ----------- ----------------- ----- -----------
   **MON**    8.86    0.979    0.186    34.7     129.6       77.9          41.2            0.6      Nov 26 - Dec 21   111   this work
    s.dev             0.018    0.029     3.9      4.3        5.4            1.7                                            
              19.88   0.991    0.188    34.9     128.9       80.1          41.6                                       15      OH89
    s.dev     7.49    0.026    0.012     3.1      2.1        2.2            1.8                                            
              20.79   0.990    0.187    34.9     128.9       80.4          41.82                    Nov 27 - Dec 17   12     LIND90
   **NOO**    11.36   0.989    0.125    23.51    139.3       69.3          