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Strongly Doppler-shifted Stokes $V$ profiles have been detected in the quietSun with the IMaX instrument on-board the SUNRISE stratospheric balloon-bornetelescope. High velocities are required in order to produce such signals, hencethese events have been interpreted as jets, although other sources are alsopossible. We aim to characterize the variation of the main properties of theseevents (occurrence rate, lifetime, size and velocities) with their position onthe solar disk between disk centre and the solar limb. These events have beenidentified in Sunrise/IMaX data according to the same objective criteria at allavailable positions on the solar disk. Their properties were determined usingstandard techniques. Our study yielded a number of new insights into thisphenomenon. Most importantly, the number density of these events is independentof the heliocentric angle, i.e. the investigated supersonic flows are nearlyisotropically distributed. Size and lifetime are also nearly independent of theheliocentric angle, while their intensity contrast increases towards the solarlimb. The Stokes $V$ jets are associated with upflow velocities deduced fromStokes $I$, which are stronger towards the limb. Their intensity decreases withtime, while their line-of-sight (LOS) velocity does not display a cleartemporal evolution. Their association with linear polarization signalsdecreases towards the limb. The density of events appears to be independent ofheliocentric angle, establishing that they are directed nearly randomly. Ifthese events are jets triggered by magnetic reconnection between emergingmagnetic flux and the ambient field, then our results suggest that there is nopreferred geometry for the reconnection process.

Centre-to-limb properties of small, photospheric quiet Sun jets