4 MAINAK SINGHA ET AL. broad band, 0.5 – 7 keV and in the hard band, 2-7 keV. For each source, we defined a circular source region centered at the source position on the broad band images, with a radius R source enclosing 90% of the PSF at 1.0 keV. Backgrounds are extracted from an annulus with R source <R< 5R source , after confirming the absence of nearby bright X-ray sources. Out of the 22 observations, J162410.10-002202.5 and SHOC 486 are detected with significant X-ray emission (over 3σ confidence) in both broad and hard bands. Therefore, for the sources with no X-ray detection, extracting background from a region between R source − 5R source should not introduce any uncertainty. For 162410.10-002202.5 and SHOC 486, the background may be slightly overestimated due. However, even with the overestimated background, a source detection over 3σ strongly suggests that the detection is indeed robust. Figure 1. 2-10 keV observed X-ray luminosity for our sources (L 2−10 keV, observed ) vs. star formation rate (SFR, derived from narrow Hα flux). Curves show the expected relation of L 2−10 keV and SFR from the literature for several classes of galaxy. X-ray detections are shown with 1σ uncertainties, and nondetections are plotted as XX% confidence upper limits. If our sources are similar to LIRGs, then the observed X-ray emission cannot be described by XRBs alone. However, using the low metallicity galaxy calibration, L 2−10 keV, observed almost agrees with L 2−10 keV, observed . The low net counts restrict us from performing any effi- cient spectrum analysis. This makes the number of sources with X-ray detection over 3σ confidence to be 9. The host galaxy properties of these sources are listed in Table 1. We present the X-ray flux values in the 0.5-7 keV, 2-7 keV bands for the sources with X-ray detections and 3σ upper limits for the non-detections in Table 2. We have listed the 2-10 keV X-ray luminosity values (or the upper limits) for these sourcs as well. 3. ANALYSIS AND RESULTS 3.1. X-ray emission: We employ the Chandra-based Portable, Interactive Multi- Mission Simulator (PIMMS) to convert the 0.2-5 keV X-ray fluxes to 2-10 keV unabsorbed fluxes by applying a correc- tion factor of approximately 1.944. This correction is based on a photon index of Γ = 1.47, a typical value for starburst galaxies (Rephaeli et al. 1995), and a galactic hydrogen col- umn density N H =3 × 10 20 cm −2 . The estimated 2-10 keV X-ray luminosity for these sources spans a range of L 2−10 keV, observed =7.8 × 10 40 − 1.07 × 10 41 erg s −1 . These L 2−10 keV values are at least an order of magnitude higher than those typically observed in dwarf galaxies host- ing AGN (Reines et al. 2014; Mezcua et al. 2018; Latimer et al. 2021), where L 2−10 keV, observed < 10 40 erg s −1 . However, the SFR values in our sources are also an order of magnitude higher than their sources. In starburst galaxies, it is well-established that the X-ray binary population con- tribute to the observed X-ray emission significantly and that it increases with the galactic SFR. Therefore, it is necessary to estimate the 2-10 keV luminosity attributable to X-ray bi- naries L 2−10 keV, XRB . Despite both low mass (LMXBs) and high mass X-ray binaries (HMXBs) contributing to 2-10 keV X-ray emis- sion, the LMXB contribution is negligible compared to the HMXBs as documented by several studies (Grimm et al. 2003; Mineo et al. 2014; Svoboda et al. 2019; Lehmer et al. 2022). We conduct a comparative analysis of the 2-10 keV X-ray luminosity of our sources with the X-ray binary (XRB) contribution, employing various L 2−10 keV -SFR-Z calibra- tions sourced from the existing literature. Ranalli et al. (2003) established a correlation between the star formation rates (SFRs) of a selected group of nearby star-forming galaxies and their total X-ray luminosity in the 2-10 keV range, denoted as L 2−10 keV, observed ∼ 5 × 10 39 SFR (M ⊙ Yr −1 ). It is crucial to acknowledge that in this context, SFR values are derived only from stars with masses exceeding 5M ⊙ . A study by Grimm et al. (2003) sug- gested an XRB luminosity scaling with the SFR, expressed as L 2−10 keV, observed ∼ 1.65 × 10 39 SFR (M ⊙ Yr −1 ) in the 2-10 keV band. Lehmer et al. (2010) prescribed a calibration very similar to Grimm et al. (2003), L 2−10 keV, observed ∼ 1.62 × 10 39 SFR (M ⊙ Yr −1 ) for luminous infrared galax- ies (LIRGs). In the mid-infrared color-color diagram, the sources in our sample occupy similar regions as the luminous infrared galaxies (LIRGs) or ultra-luminous infrared galaxies (ULIRGs) as shown by Harish et al. (2021).