| Abstract: | The various processes and evolutionary phases experienced by galaxies show emissions spanning the entire electromagnetic spectrum. Consequently, a comprehensive understanding of these phenomena requires a multi-wavelength approach.
In this work, I used the 100% ALFALFA catalog in conjunction with its optical counterparts(Durbala et al. 2020). Optical counterparts have been matched in SDSS, GALEX and WISE. These can be used in conjugation to give better estimates for the stellar mass. We have Stellar Mass Estimates derived with
Kcorrect based on optical ugriz bands, and GSWLC-2 mass estimates(Salim et al. 2016) which utilize all three surveys in optical, UV, and infrared bands.GSWLC provides more accurate stellar mass estimates because of two additional bands.
We use non-parametric method to constrain the stellar mass function of gas-rich galaxies in the ALFALFA 100% sample for both stellar mass estimates and compare their results.
The data is consistent with the Schechter function with the best-fit parameters Mstar , ϕstar /103 and α(=10.85,2.84,-1.22). Additionally, we look at the contribution to the total stellar mass function of these galaxies from the red(=10.82,2.19,-1.03) and blue(=10.73,1.39,-1.32) population of galaxies.
Compared to the overall population, the red population is 60% of the total stellar mass while blue pop-
ulation contributes rest. The gas-rich population of galaxies consists of 15% of the total stellar mass.
In this process, we have developed a method to predict the stellar mass function and can extend it to other optical properties.
We have then used Stellar Mass Function to determine the underlying scaling relation between MHI and Mstar across different galaxy populations, including complete samples, as well as blue and red galaxies. This approach helps us understand how the relationship between cold gas and stellar mass changes across different types of galaxies in an unbiased manner. |
