Measuring stellar populations, dust attenuation and ionized gas at kpc scales in 10,010 nearby galaxies using the integral field spectroscopy from MaNGA

As one of the three major experiments of the fourth-generation Sloan Digital Sky Survey (SDSS-IV), the Mapping Nearby Galaxies at Apatch Point Observatory (MaNGA) survey has obtained high-quality integral field spectroscopy (IFS) with a resolution of 1~2 kpc for 10010 galaxies in the local Universe during its six-year operation from July 2014 through August 2020. It is crucial to reliably measure the physical properties of the different components in each spectrum before one can use the data for any scientific study. In the past years we have made lots of efforts to develop a novel technique of full spectral fitting, which estimates a model-independent dust attenuation curve from each spectrum, thus allowing us to break the degeneracy between dust attenuation and stellar population properties when fitting the spectrum with stellar population synthesis models. We have applied our technique to the final data release of MaNGA, and obtained measurements of stellar population properties and emission line parameters, as well as the kinematics and dust attenuation of both stellar and ionized gas components. We describe our technique and the content and format of our data products in the article "Measuring stellar populations, dust attenuation and ionized gas at kpc scales in 10,010 nearby galaxies using the integral field spectroscopy from MaNGA" published in the journal Chinese Physics B.For a given galaxy, all the data products are stored in a single fts-format file, contained separately in 35 data extensions. Extension 0 has no data but some information about the observation in the header. Extension 1 is signal-to-noise of the spectra. Extension 2 is the normalization coefficients of the spectra. Extension 3 is stellar velocity and extension 4 is error of stellar velocity. Extension 5 is stellar velocity dispersion and extension 6 is error of stellar velocity dispersion. Extension 7 is weights of simple stellar populations used in the spectral fitting. Extension 8 is color excess of stellar continuum and extension 9 is error of color excess. Extension 10 is degree of freedom in the fitting and extension 11 is chi-square of the fitting. Extension 12 is stellar mass. Extension 13 and 17 are light-weighted stellar age in logarithm with different definitions. Extension 14 and 18 are light-weighted stellar metallicity with different definitions. Extension 15 and 19 are mass-weighted stellar age in logarithm with different definitions. Extension 16 and 20 are mass-weighted stellar metallicity with different definitions. Extension 21 is weights of eigenspectral used in the spectral fitting. Extension 22 is coefficients to produce relative dust attenuation curve. Extension 23 is best-fit wavelength center of emission lines and extension 24 is its error. Extension 25 is best-fit dispersion of emission lines and extension 26 is its error. Extension 27 is flux of emission lines and extension 28 is its error. Extension 29 is equivalent width of emission lines and extension 30 is its error. Extension 31 is 4000 angstrom break and extension 32 is its error. Extension 33 is equivalent width of Hdelta absorption and extension 34 is its error.