  Rapid magnetic upflows in the quiet-Sun photosphere were recently uncovered
from both SUNRISE/IMaX and Hinode/SOT observations. Here, we study magnetic
upflow events (MUEs) from high-quality, high- (spatial, temporal, and spectral)
resolution, and full Stokes observations in four photospheric magnetically
sensitive Fe I lines centered at 525.021, 617.334, 630.151, and 630.250 nm
acquired with the Swedish Solar Telescope (SST)/CRISP. We detect MUEs by
subtracting in-line Stokes V signals from those in far blue wing whose
signal-to-noise ratio (S/N) >= 7. We find a larger number of MUEs at any given
time (0.02 per square arcsec), larger by one to two orders of magnitude, than
previously reported. The MUEs appear to fall into four classes presenting
different shapes of Stokes V profiles with (I) asymmetric double lobes, (II)
single lobes, (III) double-humped (two same-polarity lobes), and (IV) three
lobes (an extra blue-shifted bump in addition to double-lobes), of which less
than half are single-lobed. We also find that MUEs are almost equally
distributed in network and internetwork areas and they appear in the interior
or at the edge of granules in both regions. Distributions of physical
properties, except that of horizontal velocity, of the MUEs (namely, Stokes V
signal, size, line-of-sight velocity, and lifetime) are almost identical for
the different spectral lines in our data. A bisector analysis of our spectrally
resolved observations shows that these events host modest upflows and do not
show direct indication of the presence of supersonic upflows reported earlier.
Our findings reveal that numbers, types (classes), and properties determined
for MUEs can strongly depend on the detection techniques used and the
properties of the employed data, namely, S/Ns, resolutions, and wavelengths.
