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<big><big>[[The 9th C-MaNGA workshop, SHAO, June 21-22, 2018]]</big></big>

= Abstract Submission =

Provide the requested information if you are going to give a talk at the meeting. Please follow the same format as the example (keep the example on the top and don't delete it!).


=== Example ===

* Title: A summary of the MaNGA science projects at Tsinghua
:Speaker: Cheng Li
:Abstract: I will summarize the ongoing MaNGA projects at Tsinghua.

'''Please submit your abstract before Jun. 15, 2019.'''

=== Submitted Abstracts ===

* Title: Environmental dependence of star-formation quenching in low-z galaxies
:Speaker: Cheng Li
:Abstract: I will present a new analysis of the environment of MaNGA galaxies, examining the correlation of star formation cessation in MaNGA galaxies as indicated by D4000, EW(Halpha) and EW(Hdelta_A) with their environment. For environment we consider the central/satellite division, the local density and the host dark matter halo mass. I will show that central and satellite galaxies show different quenching status even when stellar mass and halo mass are limited to a narrow range.


* Title: Galaxies with debris of merger in MaNGA
:Speaker: Songlin Li
:Abstract: We crossmatch the galaxies in MaNGA MPL-8 with the Legacy Survey, which provides both g and r band images about one magnitude deeper than those in SDSS. We find 550 galaxies with debris of merger(tidal tails, shells, asymmetric halo or distorted feature with companions). In this sample, we find overall higher star formation rate(SFR) and higher stellar mass comparing with whole MaNGA sample. Moreover, there is a higher possibility for those galaxies with gas-stellar rotating misalignment to contain those debris of merger, while we don't see significant differences of the possibility between co-rotation and counter-rotation. This result corroborates the influence of merger on gas-stellar misalignment and supports the gas precession scenario, a scenario that external misaligned gas could precess to either co-rotation or counter-rotation with in situ stellar due to gravitational dynamical settling.  


* Title: Where does the star formation in galaxies peak?
:Speaker: Shiyin Shen
:Abstract: We develop a new algorithm to identify the HII regions on the Ha maps of MaNGA galaxies. We will take the advantages of the large MaNGA galaxy sample and explore the statistical properties of these HII regions.


* Title: Kinematic Field of Ionized Gas in Galaxy Pairs
:Speaker: Shuai Feng
:Abstract: We explore the kinematic field of ionized gas for galaxy pairs. We find the fraction of non-circular components of the kinematic field increase with decreasing projected separation. For the galaxy pair with a higher fraction of non-circular components, their SFR is significant enhanced than the control sample. While for the other galaxy pair (lower fraction of non-circular components), their SFR shows little enhancement.


* The stellar mass-metallicity relation of pair galaxies
: Speaker: Zhai Sai
: Abstarct: We utilize Mapping Nearby Galaxies at Apache Point Observatory integral field spectroscopy of star-forming region of 5592 galaxies to study the relation between stellar mass and gas-phase metallicity. We stack the spectra from 1 effective radius(Re) to 1.5Re ofper galaxyand obtain emissionlines by fittingwith Penalized Pixel-Fitting(pPXF).  We derive gas phase abundances using indicators that make use of photoionization models-KD02 or combine the empirical and theoretical models-Do2. Stellar masses are derived by spectral energy distribution(SED) fitting from GSWLC. We find that the galaxy with larger stellar mass contains more metal. All the pairs in the sample are selected by using two classification criteria. The separation are required to be r<60 kpc (or 150 kpc), the velocity separation are required to be Δv < 500 km/s (or 1000 km/s).  Comparing with randomly selected isolated galaxies, no clear evidence shows that the Circumgalactic medium effects the metallicity distribution of pair galaxies.

* The internal orbital structures of early-type galaxies and its dependence with environment
: Speaker: Ling Zhu
: Abstarct: We apply orbital superposition Schwarzschild method to 149 ETGs in the mass range of 109.86 1011.61M⊙ selected from the integral-field survey Mapping Nearby Galaxies with APO (MaNGA). These galaxies are classified to be 105 central and 44 satellite galaxies based on the group catalog from Yang et al. (2007). We find that low-mass galaxies with log(M∗/M⊙) < 10.9 have an average dark matter fraction of ∼ 0.2 within one effective radii Re, tend to be oblate-like, and are dominated by minor-axis rotations. High-mass galaxies with log(M∗/M⊙) > 10.9 have an average dark matter fraction of ∼ 0.4 within one effective radii Re, tend to be prolate-like, and are dominated by major-axis rotations and random motions. The change of internal structures within Re are dominated by the total stellar mass of the galaxies, and there is no difference between centrals and satellites with control of stellar mass. However, the galaxies more triaxial or with higher hot orbit fractions do have more close neighbors with $rp < 30$ kpc.