![]() ![]() ![]() We need to correct the stellar velocity dispersion for the instrumental resolution.ĭisp_inst=mrdfits(file,'STELLAR_SIGMACORR',/silent) First we need to read in the raw stellar velocities.ĭisp_raw=mrdfits(file,'STELLAR_SIGMA',/silent) In this section we will plot the stellar velocity dispersion. You cannot reduce the uncertainty on the measured velocity by averaging the velocities of several lines together. Image_plot,ha_flux,x,y replot with the new color tableĪn important note regarding gas velocity fields: The velocities of the emission lines are tied together, so for example, the velocity of the -5007 line is the same as the Hα line, as are the uncertainties. If you have not already downloaded this file, see this tutorial for help with downloading MaNGA data.įile= to 35. For this tutorial, we'll use the maps file for MaNGA object (plate-ifu) 7443-12703 with the MAPS-HYB10-GAU-MILESHC type map. It assumes you're using IDL and have the IDL Astronomy User's Library, the Coyote Graphics Library, and image_plot.pro from the ppxf package. The goal of this introductory tutorial will be to show you the basics of loading and visualizing MaNGA DAP products. However, we highly recommend you consider using Marvin, a python package designed specifically for downloading, visualizing, and analyzing MaNGA data. ![]() Disclaimer: This tutorial teaches you how to look at the DAP output files using the software IDL. ![]()
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