Advanced morphology of vipers galaxies

We calculated morphological parameters for a test sample of 4659 galaxies from VIPERS (spectroscopic galaxy survey performed on VIMOS spectroscope at VLT). These parameters include Gini, M$_{20}$, Concentration, Asymmetry, and Smoothness, also known as CAS parameters. The results correlate with the distribution of these parameters for other simulated and observed samples. We also studied the dependence of these parameters with the Sersic power index of the radial distribution of the surface brightness of the galaxy image. Our aim was to find a clear division of VIPERS galaxies into elliptical and spiral. This is necessary for testing the method of the Sersic index (ns) calculation in the statmorph program. To find such bimodality, we use B-V color index from VIPERS database. To perform the error analysis of morphological parameters, we simulated galaxy images with a random background of different magnitudes and estimated the errors as the dispersion of the parameters. We also found asymptotic values of errors of morphological parameters by increasing the numbers of mock images. To analyse the possible variation of each morphological parameter during the convolution of close galactic images, we have simulated them to research. As a result of this investigation, we have analysed the dependence of every morphological parameter from CAS and Gini-M$_{20}$ statistics, from the distance between galactic centers.The differences between our results for VIPERS and Gini-M$_{20}$ distribution for PanStarrs galaxies at z 0.5 which corresponds to VIPERS sample. Also we concluded that galaxy mergers were more frequent in the early Universe

Advanced morphology of vipers galaxies

We calculated morphological parameters for a test sample of 4659 galaxies from VIPERS (spectroscopic galaxy survey performed on VIMOS spectroscope at VLT). These parameters include Gini, M$_{20}$, Concentration, Asymmetry, and Smoothness, also known as CAS parameters. The results correlate with the distribution of these parameters for other simulated and observed samples. We also studied the dependence of these parameters with the Sersic power index of the radial distribution of the surface brightness of the galaxy image. Our aim was to find a clear division of VIPERS galaxies into elliptical and spiral. This is necessary for testing the method of the Sersic index (ns) calculation in the statmorph program. To find such bimodality, we use B-V color index from VIPERS database. To perform the error analysis of morphological parameters, we simulated galaxy images with a random background of different magnitudes and estimated the errors as the dispersion of the parameters. We also found asymptotic values of errors of morphological parameters by increasing the numbers of mock images. To analyse the possible variation of each morphological parameter during the convolution of close galactic images, we have simulated them to research. As a result of this investigation, we have analysed the dependence of every morphological parameter from CAS and Gini-M$_{20}$ statistics, from the distance between galactic centers.The differences between our results for VIPERS and Gini-M$_{20}$ distribution for PanStarrs galaxies at z 0.5 which corresponds to VIPERS sample. Also we concluded that galaxy mergers were more frequent in the early Universe

X-ray galaxies selected from HyperLEDA database

We cross-matched the 4XMM-DR10 catalog with the HyperLEDA database and obtained a new sample of galaxies that contain X-ray sources. Excluding duplicate observations and false matches, we present a total of 7759 galaxies with X-ray sources. In the current work, we present general properties of the sample: namely the distribution in equatorial coordinates, radial velocity distribution, morphological type, and X-ray fluxes. The sample includes morphological classification for 5241 galaxies with X-ray emission, almost half of which, 42% are elliptical (E, E-S0). Most galaxies in the sample have nuclear X-ray emission (6313 or 81%), and the remaining 1443 (19%) present X-ray emission from the host galaxy. This sample can be used for future deep studies of multi-wavelengths properties of the galaxies with X-ray emission