  We present spectroscopic and imaging observations of small-scale reconnection
events on the Sun. Using the Interface Region Imaging Spectrograph (IRIS)
observations, one reconnection event is first detected as IRIS jets with fast
bi-directional velocities in the chromosphere and transition region, which are
identified as non-Gaussian broadenings with two extended wings in the line
profiles of Si iv, C ii, and Mg ii k. The magnetograms under the IRIS jets from
Helioseismic and Magnetic Images exhibit magnetic flux cancellation
simultaneously, supporting that the IRIS jets are driven by magnetic
reconnection. The Atmospheric Imaging Assembly images also show an extreme
ultraviolet (EUV) brightening which is shortly after the underlying IRIS jets,
i.e., in the 131 A, 171 A, 193 A, 211 A, and 94 A channels, implying that the
over-lying EUV brightening in the corona is caused by the IRIS jets in the
chromosphere and transition region. We also find another three reconnection
events which show the same features during this IRIS observation. Our
observational results suggest that the small-scale reconnection events might
contribute to the coronal heating. The new result is that the process of
magnetic reconnection is detected from the photosphere through chromosphere and
transition region to the corona.
