[Speaker1]<\/p>\n\n\n\n
Takafumi Tsukui,
\nSOKENDAI 3rd year (D1),
\n(Supervisor: Satoru Iguchi, Hiroshi Nagai, Yuichi Matsuda) <\/p>\n\n\n\n
[Title1]<\/p>\n\n\n\n
Galactic Dynamics and Dark Matter Profile of NGC1380 with ALMA and VLT\/MUSE.<\/p>\n\n\n\n
[Abstract1]<\/p>\n\n\n\n
ALMA\u2019s high resolution and high sensitivity images enable us to\nobtain kinematics of molecular gas in the center of early-type galaxies (~1kpc)\ncomplementarily to the stellar dynamics obtained with optical IFU instrument.\nThe cold molecular gas dynamics is a powerful tracer of mass distribution of\ngalaxies because the velocity dispersion is low(~10km\/s) and the simple\nrotational model is applicable. To understand the interaction between dark\nmatter and baryonic matter in the galaxy evolution history, it is fundamental\nto measure dark matter distribution in galaxies. However, it is difficult to\nderive the dark matter profile in the central region of early-type galaxies\nbecause of the lack of neutral hydrogen gas in early-type galaxies and the\ndegeneracy between dynamical stellar M\/L and dark matter distribution. To\nresolve this difficulty, we conducted a combined analysis of ALMA cold\nmolecular gas kinematics data and MUSE stellar kinematics data of early-type\nfast rotator galaxy NGC1380. Our strategy is to measure BH mass and stellar\nmass well in the central region (~radius of 6\u201d, 500pc) with the cold gas\nkinematics. Then we derive dark matter profile with the stellar kinematics\nwhich is available in a wide field of view(~radius of 120\u2019\u2019, 10kpc) with the help\nof information of the central cold gas modeling. Dynamical measurement of\nstellar M\/L and BH mass is conducted with ALMA high angular resolution data\n(0.24\u201d\u00d70.18\u201d ~ 21pc\u00d716pc where BH sphere of influence of the resulted BH mass\nis 0.37\u201d~ 33pc). Simple gas rotational disk model reproduce observed data cube\nwell. The obtained BH mass of 3.38\u00d710^8^{+0.30}_{-0.24} solar masses is close\nto the estimated value of 3.9\u00d710^8 solar masses from the empirical M – sigma\nrelation. With Jeans Anisotropic Models (JAM; Cappellari 2008) of stellar\nkinematics, we found that the substantial dark matter halo needs to exist to\nmaintain flat velocity profile at large radius. However, the mass model\nobtained with ALMA cold gas modeling cannot reproduce the central high-velocity\ndispersion peak in the stellar kinematics data (~10\u201d 900pc ), which may\nindicate several possibilities including the steep M\/L variation and hidden\nnon-axisymmetric bar structure. We obtained dark matter profile by using\ninformation from the central gas rotational disk model as a prior knowledge\nwith Bayesian inference. The obtained central slope of the dark matter was\ngamma=0.45^{+0.11}_{-0.10} which is lower than 1.0 NFW profile predict. <\/p>\n\n\n\n
<\/p>\n\n\n\n
[Speaker2]<\/p>\n\n\n\n
Shishido, Takaharu,
\nSOKENDAI 3rd year (D1),
\n(Supervisor:Takayuki tomaru, Yoichi Aso, Ryutaro Takahashi)<\/p>\n\n\n\n
[Title2]<\/p>\n\n\n\n
A study of the sapphire suspension fiber\nfor cryogenic gravitational wave detector KAGRA<\/p>\n\n\n\n
<\/p>\n","protected":false},"excerpt":{"rendered":"
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