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We report a tentative detection of the circumgalactic medium (CGM) of WLM, anisolated, low-mass (log$M_*/M_\odot\approx7.6$), dwarf irregular galaxy in theLocal Group (LG). We analyze an HST/COS archival spectrum of a quasar sightline(PHL2525), which is 45 kpc (0.5 virial radius) from WLM and close to theMagellanic Stream (MS). Along this sightline, two ion absorbers are detected inSi II, Si III, Si IV, C II, and C IV at velocities of $\sim$-220 km s$^{-1}$(Component v-220) and $\sim$-150 km s$^{-1}$ (Component v-150). To identifytheir origins, we study the position-velocity alignment of the components withWLM and the nearby MS. Near the Magellanic longitude of PHL2525, the MS-relatedneutral and ionized gas moves at $\lesssim-190$ km s$^{-1}$, suggesting an MSorigin for Component v-220, but not for Component v-150. Because PHL2525 passesnear WLM and Component v-150 is close to WLM's systemic velocity ($\sim$-132 kms$^{-1}$), it is likely that Component v-150 arises from the galaxy's CGM. Thisresults in a total Si mass in WLM's CGM of $M_{\rm Si}^{\rmCGM}\sim(0.2-1.0)\times10^5~M_\odot$ using assumption from other COS dwarfstudies. Comparing $M_{\rm Si}^{\rm CGM}$ to the total Si mass synthesized inWLM over its lifetime ($\sim$1.3$\times10^5~M_\odot$), we find $\sim$3% islocked in stars, $\sim$6% in the ISM, $\sim$15%-77% in the CGM, and the rest($\sim$14%-76%) is likely lost beyond the virial radius. Our finding resonateswith other COS dwarf galaxy studies and theoretical predictions that low-massgalaxies can easily lose metals into their CGM due to stellar feedback andshallow gravitational potential.

Tentative Detection of the Circumgalactic Medium of the Isolated Low-Mass Dwarf Galaxy WLM