  We present a systematic study of the putative hot gas corona around late-type
galaxies (LTGs) residing in the Virgo cluster, based on archival Chandra
observations. Our sample consists of 21 nearly edge-on galaxies representing a
star formation rate (SFR) range of ($0.2-3\rm~M_\odot~yr^{-1}$) a stellar mass
($M_*$) range of $(0.2-10) \times 10^{10}\rm~M_{\odot}$, the majority of which
have not been explored with high-sensitivity X-ray observations so far.
Significant extraplanar diffuse X-ray (0.5-2 keV) emission is detected in only
three LTGs, which are also the three galaxies with the highest SFR. A stacking
analysis is performed for the remaining galaxies without individual detection,
dividing the whole sample into two subsets based on SFR, stellar mass, or
specific SFR. Only the high-SFR bin yields a significant detection, which has a
value of $L\rm_X \sim3\times10^{38}\rm~erg~s^{-1}$ per galaxy. The stacked
extraplanar X-ray signals of the Virgo LTGs are consistent with the empirical
$L\rm_X - SFR$ and $L\rm_X - M_*$ relations found among highly inclined disk
galaxies in the field, but appear to be systematically lower than that of a
comparison sample of simulated cluster star-formation galaxies identified from
the Illustris-TNG100 simulation. The apparent paucity of hot gas coronae in the
sampled Virgo LTGs might be understood as the net outcome of the long-lasting
effect of ram pressure stripping exerted by the hot intra-cluster medium and
in-disk star-forming activity acting on shorter timescales. A better
understanding of the roles of environmental effects in regulating the hot gas
content of cluster galaxies invites sensitive X-ray observations for a large
galaxy sample.
