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We analyse the integral-field spectroscopy data for the $\approx10,000$ galaxies in final data release of the MaNGA survey. We identify 188 galaxies for which the emission lines cannot be described by single Gaussian components. These galaxies can be classified into (1) 38 galaxies with broad $H\alpha$ and [OIII] $\lambda$5007 lines, (2) 101 galaxies with broad $H\alpha$ lines but no broad [OIII] $\lambda$5007 lines, and (3) 49 galaxies with double-peaked narrow emission lines. Most of the broad line galaxies are classified as Active Galactic Nuclei (AGN) from their line ratios. The catalogue helps us further understand the AGN-galaxy coevolution through the stellar population of broad-line region host galaxies and the relation between broad lines' properties and the host galaxies' dynamical properties. The stellar population properties (including mass, age and metallicity) of broad-line host galaxies suggest there is no significant difference between narrow-line Seyfert-2 galaxies and Type-1 AGN with broad $H\alpha$ lines. We use the broad-$H\alpha$ line width and luminosity to estimate masses of black hole in these galaxies, and test the $M_{BH}-\sigma_{e}$ relation in Type-1 AGN host galaxies. Furthermore we find three dual AGN candidates supported by radio images from the VLA FIRST survey. This sample may be useful for further studies on AGN activities and feedback processes., Comment: 20 pages, 17 figures, LaTeX. Submitted to MNRAS

We present the measurement of total and stellar/dark matter decomposed mass density profile around a sample of galaxy groups and clusters with dynamical masses derived from integral-field stellar kinematics from the MaNGA survey in Paper~I and weak lensing derived from the DECaLS imaging survey. Combining the two data sets enables accurate measurement of the radial density distribution from several kpc to Mpc scales. Intriguingly, we find that the excess surface density derived from stellar kinematics in the inner region cannot be explained by simply adding an NFW dark matter halo extrapolated from lensing measurement at a larger scale to a stellar mass component derived from the NASA-Sloan Atlas (NSA) catalog. We find that a good fit to both data sets requires a stellar mass normalization about 3 times higher than that derived from the NSA catalog, which would require an unrealistically too-heavy initial mass function for stellar mass estimation. If we keep the stellar mass normalization to that of the NSA catalog but allow a varying inner dark matter density profile, we obtain an asymptotic slope of $\gamma_{\rm gnfw}$= $1.82_{-0.25}^{+0.15}$, $\gamma_{\rm gnfw}$= $1.48_{-0.41}^{+0.20}$ for the group bin and the cluster bin respectively, significantly steeper than the NFW case. We also compare the total mass inner density slopes with those from Illustris-TNG300 and find that the values from the simulation are lower than the observation by at least $3\sigma$ level., Comment: 12 pages, 9 figures, was submitted to MNRAS

We present dynamical scaling relations, combined with the stellar population properties, for a subsample of about 6000 nearby galaxies with the most reliable dynamical models extracted from the full MaNGA sample of 10K galaxies. We show that the inclination-corrected mass plane (MP) for both early-type galaxies (ETGs) and late-type galaxies (LTGs), which links dynamical mass, projected half-light radius $R_{\rm e}$, and the second stellar velocity moment $\sigma_{\rm e}$ within $R_{\rm e}$, satisfies the virial theorem and is even tighter than the uncorrected one. We find a clear parabolic relation between $\lg(M/L)(, Comment: 21 pages, 16 figures, 1 table, Submitted to MNRAS

We analyze the global stellar population, radial gradients and non-parametric star formation history of $\sim 10$K galaxies from the MaNGA Survey final data release 17 (DR17), based on stellar population synthesis and full-spectrum fitting, and relate them with dynamical properties of galaxies. We confirm that stellar population correlates with stellar velocity dispersion $\sigma_{\rm e}$ better than with stellar mass $M_{\ast}$, but also find that younger galaxies are more metal-poor at fixed $\sigma_{\rm e}$. Stellar age, metallicity, and mass-to-light ratio $M_{\ast}/L$ all decrease with galaxy rotation, while radial gradients become more negative (i.e., younger, more metal-poor, and lower $M_{\ast}/L$ in the outskirts). The trend between metallicity gradients and rotation reverses for slow rotators, which stand out for their more negative metallicity gradients than faster-rotating galaxies. We highlight a population of massive disk galaxies on the green valley, on the $(\sigma_{\rm e},\rm Age)$ plane, that show steep negative age and metallicity gradients, consistent with their old central bulges surrounded by young star-forming disks and metal-poor gas accretion. Galaxies with high $\sigma_{\rm e}$, steep total mass-density slope, low dark matter fraction, high $M_{\ast}/L$, and high metallicity have the highest star-formation rate at earlier times, and are currently quenched. We discover a population of low-mass star-forming galaxies with low rotation but physically distinct from the massive slow rotators. A catalogue of the population properties is provided publicly., Comment: 23 pages, 18 figures, 1 table. Submitted to MNRAS. The catalogue will become available at https://manga-dynpop.github.io/ once the paper is published by MNRAS

Galaxy properties are known to correlate most tightly with the galaxy effective stellar velocity dispersion $��_{\rm e}$. Here we look for {\em additional} trends at fixed $��_{\rm e}$ using 1339 galaxies ($M_\ast \gtrsim 6\times10^9$ M$_\odot$) with different morphologies in the MaNGA (DR14) sample with integral-field spectroscopy data. We focus on the gradients ($��_{\rm rms} \equiv ��(R_{\rm e}/4)/��_{\rm e}$) of the stellar root-mean-square velocity ($V_{\rm rms} \equiv \sqrt{V^2 + ��^2}$), which we show traces the total mass density gradient $��_{\rm tot}$ derived from dynamical models and, more weakly, the bulge fraction. We confirm that $��_{\rm rms}$ increases with $��_{\rm e}$, age and metallicity. We additionally find that these correlations still exist at fixed $��_{\rm e}$, where galaxies with larger $��_{\rm rms}$ are found to be older and more metal-rich. It means that mass density gradients contain information of the stellar population which is not fully accounted for by $��_{\rm e}$. This result puts an extra constraint on our understanding of galaxy quenching. We compare our results with galaxies in the IllustrisTNG hydrodynamical simulations and find that, at fixed $��_{\rm e}$, similar trends exist with age, the bulge fraction, and the total mass density slope but, unlike observations, no correlation with metallicity can be detected in the simulations., 8 pages, 6 figures; Accepted for publication in MNRAS

Atrial natriuretic peptide (ANP), a small peptide consisting of 28 amino acids, has been applied in clinical treatment for heart failure, but it can encounter proteolytic degradation during its expression in host cells. Therefore, it is usually reported that ANP was expressed as a part of fusion protein. The aim of our study was to use an overexpression system to express the fusion protein REF-ANP and to optimize a purification method. First, Escherichia coli DH5alpha was transformed with constructed expression vector containing two tandem copies of ref-anp gene and the fusion protein REF-ANP was overexpressed in shaking flask culture. Subsequently, the inclusion bodies were purified with reverse phase chromatography and pooled fractions were lyophilized. After this step, REF-ANP can be solubilized under native conditions without urea. After cleavage reaction, the sample was subjected to size exclusion chromatography and then rANP was polished with reverse phase chromatography. The final purity of rANP was more than 98% and the recovery of rANP per liter of shaking flask culture was more than 3mg. Such methods as mass spectrometry, capillary isoelectrofocusing analysis, and N-terminal amino acid sequence were used to identify rANP. The capillary isoelectrofocusing analysis showed that the pI of ANP was about pH 9.7. In this study, an efficient refolding and purification process should make scaling-up procedures easier and more successful than earlier reports. Moreover, it is possible that the refolding and purification method along with the overexpression system described in this article may offer new ideas on optimizing expression and purification of other kinds of short peptides.