HI Intensity mapping using the Green Bank Telescope
Christopher J. Anderson1, Tzu-Ching Chang2, Xuelei Chen3,4, Apratim Ganguly5, Miranda Jarvis6, Cheng-Yu Kuo7,2, Yi-Chao Li3, Yu-Wei Liao2*, Hsiu-Hsien Lin8, Kiyoshi Masui9, Maura McLaughlin10, Ue-Li Pen11,12, Jeffrey B. Peterson8, Alexander Roman8, Jonathan Sievers13, Peter T. Timbie1, Tabitha Voytek13, Jaswant K. Yadav14
1Department of Physics, University of Wisconsin, Madison, WI, USA
2Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan
3National Astronomical Observatories, Chinese Academy of Science, Beijing, China
4Center of High Energy Physics, Peking University, Beijing, China
5Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics, and Computer Science, University of KwaZulu-Natal, Durban, South Africa
6Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON, Canada
7Department of Physics, National Sun Yat-Sen University, Kaohsiung City, Taiwan
8Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
9Department of Physics and Astronomy, University of British Columbia, Vancouver, BC, Canada
10Department of Physics and Astronomy, West Virginia University, Morgantown WV, USA
11Canadian Institute for Theoretical Astrophysics, Canadian Institute for Theoretical Astrophysics, Toronto, ON, Canada
12Perimeter Institute, Perimeter Institute, Waterloo, Canada
13Astrophysics and Cosmology Research Unit, School of Chemistry and Physics, University of KwaZulu-Natal, Durban, South Africa
14Indian Institute of Science Education and Research Mohali, Knowledge City, Nagar, Manauli, India
* presenting author:Yu-Wei Liao, email:ywliao@asiaa.sinica.edu.tw
The cosmic large scale structure of neutral Hydrogen can be probed through intensity mapping of 21 cm emission. We are using Green Bank Telescope to observe redshifted 21 cm emission lines at frequency 700~900 MHz, corresponding to 0.6 < z < 1.0. We will give an overview of our HI intensity mapping project. The recent results, including HI power spectrum and Fast Radio Bursts, will be also presented. On the other hand, the Galactic Synchrotron Emission Foreground, which is obtained while observing HI emission, can be used to probe Galactic magnetic field distributions through Rotation Measure synthesis. We will also present this part.

Keywords: Cosmology, Large Scale Structure , Galactic, Intensity Mapping