| Authors : | Navin Chaurasiya1, Surhud More1,2, Shogo Ishikawa3, Shogo Masaki4,5, Daichi Kashino5,6,7, Teppei Okumura2,8 |
| Authors Affiliation: | 1 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411007, India
2 Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5, Kashiwanoha, 2778583, JP
3 Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan
4 National Institute of Technology, Suzuka College, Suzuka, Mie 510-0294, Japan
5 Department of Physics, Nagoya University, Nagoya, Aichi 464-8601, Japan
6 Institute for Advanced Research, Nagoya University, Nagoya, Aichi 464-8601, Japan
7 Division of Science, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
8 Academia Sinica Institute of Astronomy and Astrophysics, AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C |
| Abstract : | In the paradigm of hierarchical structure formation, galaxies are thought to form and evolve inside a potential well environment of 'collisionless' and 'only gravitationally interacting' form of matter; the dark matter halos. These dark halos have formed at the peaks of initial density fluctuations due to gravitational instability and as observations have revealed, are the sites of most of the galaxy formation and evolution. Quantifying the presence of these dark structures of halos by using available galaxy surveys itself is an important and challenging task. This information can then be used to find out the connection between the galaxy and its host halo properties.
In our work, we estimate the masses of dark matter halos which host the photometric galaxies from HSC survey (the lens galaxies) by using the 'weak gravitational lensing' phenomenon. Weak lensing being purely gravitational phenomena, directly and fully probes the total matter content responsible for lensing of the background source galaxies. Our analysis reveals insights into the 'stellar mass - halo mass' (SMHM) relation and its evolution as a function of redshift within 0.3-0.8 and stellar masses. Additionally, we compare the SMHM relations obtained separately by weak lensing and clustering of the same galaxy dataset as the constraint. This comparison provides an angle to the well-known disagreement between individual studies of clustering and lensing.
This work also demonstrates the potential of wide photometric surveys, such as HSC survey, in putting observational constraints on galaxy-halo connections through statistical studies like galaxy-galaxy lensing and clustering. |
