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Millisecond pulsars (MSPs) are faint X-ray sources commonly observed inGalactic globular clusters (GCs). In this work, we investigate 18 MSPs newlyfound in the GC Omega Centauri ($\omega$ Cen) and search for their X-raycounterparts using Chandra observations with a total exposure time of 290.9 ks.We identify confident X-ray counterparts for 11 of the MSPs, with 9 of themnewly identified in this work based on their positions, spectral properties,and X-ray colours. The X-ray spectra of 9 MSPs are well described by a neutronstar hydrogen atmosphere model, while 2 MSPs are well fitted by a power-lawmodel. The identified MSPs have X-ray luminosities ranging from$1.0\times10^{30}$ erg s$^{-1}$ to $1.4\times10^{31}$ erg s$^{-1}$.Additionally, for population comparison purposes, we study the X-raycounterpart to MSP E in the GC M71, and find its X-ray spectrum is welldescribed by blackbody-like models with a luminosity of $1.9\times10^{30}$ ergs$^{-1}$. We investigate the empirical correlations between X-ray luminositiesand minimum companion masses, as well as mass functions, of spider pulsars.Clear correlations are observed, with best-fit functions of $\log_{10}{L_X} =(1.0\pm0.1) \log_{10}{M_{c, min}} + (32.5\pm0.2)$ and $\log_{10}{L_X} =(0.35\pm0.04) \log_{10}{\rm MF} + (32.71\pm0.20)$, respectively, with anintrinsic scatter of $\log_{10}{L_X}$ of $\sim$0.3, where $L_X$ is the 0.5$-$10keV X-ray luminosity, $M_{c, min}$ is the minimum companion mass, and MFrepresents the mass function, in solar masses.

A Chandra X-ray study of millisecond pulsars in the globular cluster  Omega Centauri: a correlation between spider pulsar companion mass and X-ray  luminosity