Cosmology and Astroparticle Physics
|Date :||From 2012-09-03 To 2012-09-28|
|Advisory committee :|
|Local coordinators :||Xiaojun Bi, Rong-Gen Cai ,Liang Gao, Kaixuan Ni, Hu Zhan (contact person),Peng-Jie Zhang, Yu-Feng Zhou|
|International coordinators :||Rachel Bean,Gary Bernstein,Miao Li(contact person),Eric Linder, Xinmin Zhang|
Advisory Panel: Andreas Albrecht, Robert Brandenberger, Scott Dodelson, Carlos Frenk, and Leszek Roszkowski (chair)
The field of cosmology experienced an extraordinary development recently. Observations of type Ia supernova luminosity distances, the large-scale structure, and the cosmic microwave background have placed tight constraints on the concordance cosmological model and established the paradigm of an accelerating universe with most of its contents in the dark sector: 23% in dark matter and 73% in dark energy. It is widely believed that a breakthrough of the dark sector theories will come from the intersection between cosmology and particle physics and that it may well lead to a revolution in our understanding of fundamental physics.
Since the original proposal of dark matter by F. Zwicky nearly 80 years ago, there have been tremendous advances in particle theories of dark matter as well as laboratory and satellite experiments for detecting and potentially producing dark matter particles. The most definitive evidence so far is still from astronomical observations, but there is also tantalizing evidence for direct detection of dark matter particles from CDMS-II and CoGeNT. With a number of other direct and indirect detection experiments (e.g., XENON, X-MASS, AMS-02, Fermi, etc.) and the powerful LHC running in full capacity, we might be able to gain new insights about dark matter in the next few years.
Astronomical observations over the last decade or so led to yet another puzzle: the accelerated cosmic expansion. A widely discussed mechanism is that dark energy, a smooth inert component of the universe, drives the acceleration with its strong negative pressure. Like dark matter, dark energy is thought to be connected to fundamental physics, maybe at even more profound level. However, unlike dark matter, whose gravitational effect is detected in objects as small as galaxies, dark energy does not appear to have appreciable effects on scales much smaller than the Hubble radius. Hence, one can only measure its properties indirectly by observing its effects on the cosmic distance scale and the growth of large-scale structures as functions of redshift.
Laboratory and astrophysical search for dark matter particles and astronomical surveys for studying the nature of dark energy will (continue to) be a major theme of cosmology and astroparticle physics research in the coming decade. Indeed, a number of projects will be running in 2012 (e.g., AMS-02, CDMS, Fermi, LAMOST, LHC, QUIET, PanSTARRS, Planck, PolarBear, Sloan-III, XENON, X-MASS), some will become just online (e.g., DES), and several next-generation surveys are preparing very hard for a start in the next few years (e.g., BigBOSS, Dome A Optical/NIR Survey Telescope, Euclid, LSST, & WFIRST). New projects are also being developed in China to further our fundamental understanding of the universe.
This program is aimed to bring in new ideas and seed new collaborations by providing a venue for interactions between cosmologists and particle physicists, between experimentalists/observers and theorists, and between experts and new comers. We will cover a number of topics related to dark matter, dark energy, and relevant experiments. During the program, we will also host an International Conference on Particle Physics and Cosmology, which will greatly enhance this program. The rough schedule is as follows.
week 1 (Sept. 3--7): astroparticle physics (with an emphasis on dark matter)
week 2 (Sept. 10--14): COSMO-12 conference (separate registration required)
week 3 (Sept. 17--21): the early universe, large-scale structure, simulations, & dark energy
week 4 (Sept. 24--28): cosmological probes & future surveys
Link to COSMO-12: http://lss.bao.ac.cn/cosmo12/