  Understanding the role of magnetic reconnection in the heating and dynamics
of the solar atmosphere requires detailed observational data of any observable
aspect of the reconnection process, including small-scale features such as
plasmoids. Here, we examine the capability of active and upcoming instruments
to detect plasmoids generated by reconnection in the corona including
low-density regimes. We used the Bifrost code to perform simulations of
plasmoid-mediated reconnection in the corona with a 2D idealized setup: a
fan-spine topology with uniform density including thermal conduction. Through a
forward-modeling of extreme-ultraviolet (EUV) observables, we checked whether
our simulated plasmoids could be detected with the instruments of Solar
Dynamics Observatory (SDO) and Solar Orbiter (SO), as well as the upcoming
Multi-Slit Solar Explorer (MUSE) and Solar-C missions. Short-lived (10-20 s)
small-scale (0.2-0.5 Mm) coronal plasmoids are not resolvable with the
Atmospheric Imaging Assembly (AIA) on board SDO, but could be captured with the
Extreme Ultraviolet Imager (EUI) of SO. The spatial and temporal
high-resolution planned for the MUSE spectrograph (SG) is adequate to obtain
full spectral information of these plasmoids. Detection of 0.8 MK plasmoids in
the MUSE/SG 171 {\AA} channel is possible in full-raster mode in regions with
electron densities above 10^9 cm^3 whereas on sit-and-stare mode for
lower-density regions. Solar-C could also capture these coronal plasmoids using
the EUV High-Throughput Spectroscopic Telescope (EUVST), considering rapid
changes in Doppler shift and line widths in different EUV lines caused by
plasmoid motions along the current sheet. With combined spectra of MUSE/SG and
Solar-C/EUVST in multiple emission lines, along with high-resolution images
from SO/EUI and MUSE/CI, it should be possible to gain new insights about
plasmoid formation in the corona.
