  The Nele group, formerly known as the Iannini family, is one of the youngest
asteroid families in the main belt. Previously, it has been noted that the
pericenter longitudes $\varpi$ and nodal longitudes $\Omega$ of its largest
member asteroids are clustered at the present time, therefore suggesting that
the collisional breakup of parent body must have happened recently. Here we
verify this conclusion by detailed orbit-propagation of a synthetic Nele family
and show that the current level of clustering of secular angles of the largest
Nele family members requires an approximate age limit of $4.5$ Myr.
Additionally, we make use of an updated and largely extended Nele membership to
obtain, for the first time, an age estimate of this family using the Backward
Integration Method (BIM). Convergence of the secular angles in a purely
gravitational model and in a model including the non-gravitational forces
caused by the Yarkovsky effect are both compatible with an age younger than $7$
Myr. More accurate determination of the Nele family age would require
additional data about the spin state of its members.
