LAUSR

Green Pea galaxies are compact galaxies with high star formation rates. However, limited samples of Green Pea galaxies have HI 21 cm measurements. Whether the HI gas fraction (fHi ≡ MHI/M⋆) of Green Pea galaxies follows the existing scaling relations be- tween the fHi and NUV-r colour or linear combinations of colour and other physical quanti- ties needs checking. Using archival data of HI 21cm observations, we investigate the scaling relation of the NUV-r colour with the MHI/M⋆ of 38 Green Pea galaxies, including 17 de- tections and 21 non-detections. The HI to stellar mass ratios (fHi) of Green Pea galaxies deviate from the polynomial form, where a higher HI gas fraction is predicted given the cur- rent NUV-r colour, even with the emission lines removed. The blue sources (NUV-r<1) from the comparison sample (ALFALFA-SDSS) follow a similar trend. The HI gas fraction scal- ing relations with linear combination forms of −0.34(NUV − r) − 0.64 log(μ⋆,z) + 5.94 and −0.77 log μ⋆,i + 0.26 log SFR/M⋆ + 8.53, better predict the HI gas fraction of the Green Pea galaxies. In order to obtain accurate linear combined forms, higher-resolution photometry from space-based telescopes is needed.