Measurement Of Metering And Morphological Properties Of Lyman Break Galaxies After Observing Ultraviolet Light

Because of the observational limitation, all the photometric images we got are flux limit. I.e., we cannot observe all galaxies which flux is near the flux limit at a red shift range. This indicates the sample we select according to the magnitude is not complete at the faint end, which called Malmquist bias. Thus we need to correct the bias in order to get the more precise statistical properties of the galaxies. This work is based on Z. Chen et al.’s work at 2013, reconsider about the incomplete part of the sample, to study the photometrical and morphological properties of the sample.After correction, the fraction of the starburst and irregular galaxies is increase, which indicates that most of the LBGs galaxies chose with the UV-dropout method are starbursts or irregular galaxies. The average SFR is half value after the correction, and average stellar mass is similar compare to Z. Chen’s work.The Sérsic index at F606 W is a little bit smaller after correction, in contrast, the Sérsic index at F850 LP is a little bit bigger. Since the blue band indicates the compactness of star formation area, and the red band indicates the compactness of stellar mass area, this difference shows the LBGs we lost at observation have less compact star formation area and more compact stellar mass area. The effective radiuses are smaller in both band after correction, which shows the LBGs we lost at observation have smaller scale on average.In all, the statistical properties are similar in compare to Z. Chen et al.’s work. The LBGs we lost at observation have lower star formation rate, smaller scale, less compact star formation area, more compact stellar mass area, and more disk like.