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NEWS Feature Using Galaxies to Shed Light on the Dark World Premier International Research Center Initiative 世界トップレベル研究拠点プログラム Kavli Institute for the Physics and Mathematics of the Universe カブリ数物連携宇宙研究機構 UI I AS The University of Tokyo Institutes for Advanced Study 東京大学国際高等研究所 Feature Using Galaxies to Shed Light on the Dark Universe NEWS Interview with Rashid Sunyaev No. 29 March 2015 Kavli IPMU NEWS CONTENTS English Japanese 3 Director’s Corner Hitoshi Murayama 31 Director’s Corner 村山 斉 Hitoshi Murayama at Work 近況 4 Feature 32 Feature Using Galaxies to Shed Light on the Dark Universe 暗黒宇宙の解明に銀河を利用する Surhud More スルド・モレ 10 Interview with Rashid Sunyaev 38 Interview ラシッド・スニヤエフ教授に聞く 16 Our Team Yasunori Nomura 43 Our Team 野村 泰紀 Edwin L. Turner エドウィン・ターナー 18 Workshop Report 45 Workshop Report String Theory in Greater Tokyo String Theory in Greater Tokyo Charles Melby-Thompson （大東京圏における超弦理論研究会） René Meyer チャールズ・メルビー -トンプソン レネ・マイヤー 19 Workshop Report 46 Workshop Report The 6th Open Meeting of the Hyper-Kamiokande 第6回ハイパーカミオカンデ計画オープンミーティング Project Mark Hartz マーク・ハーツ 20 Workshop Report 47 Workshop Report Workshop on“ Getting a Grip on Galactic Girths” Kavli IPMUフォーカスウィーク研究会「銀河のサイズを理解する」 Kevin Bundy ケビン・バンディ 21 Workshop Report 48 Workshop Report Key Aspects in Exploring Road to Unication Key Aspects in Exploring Road to Unication (KAERU Conference) (KAERU Conference) Shinya Kanemura 兼村晋哉 22 Workshop Report 49 Workshop Report MadGraph5 aMC@NLO Femto Workshop MadGraph5 aMC@NLO Femto Workshop Kentarou Mawatari 馬渡健太郎 23 News 50 News 30 Matter Effects on Neutrino Oscillations 52 ニュートリノ振動の物質効果 Michael Smy マイケル・スミ Surhud More is an Assistant Professor at the Kavli IPMU. He graduated from the Indian Institute of Technology Bombay in May 2005. He received his Ph.D (Dr. rer.nat) from the Max Planck Institute for Astronomy in July 2009. He became a MPIA Postdoctoral Researcher at the Max Planck Institute for Astronomy in July 2009, and the Kavli Institute for Cosmological Physics Fellow at the University of Chicago in November 2009. He then became a Postdoctoral Fellow at the Kavli IPMU in September 2012. Since 2014, he has been Kavli IPMU Assistant Professor. スルド・モレ：Kavli IPMU 助教。2005年5月にインド工科大 学ボンベイ校卒業。2009年7月にマックス・プランク天文学 研究所より博士の学位を取得。2009年7月にマックス・プラ ンク天文学研究所博士研究員、同年11月にシカゴ大学カブリ 宇宙物理学研究所フェロー。2012年9月にKavli IPMU博士研究 員、2014年3月よりIPMU助教。 Director’s Corner Director of Kavli IPMU Hitoshi Murayama at Work Hitoshi Murayama January 13: Lecture at Yamanashi Eiwa Junior and Senior High School. (Photos: Courtesy of Yamanashi Eiwa Junior and Senior High School) March 25 and 26: Opening address (left) and a talk (right) entitled“, Life after Higgs: New SUSY Breaking and New Dark Matter,” at the Conference on“ Key Aspects in Exploring Road to Unication (KAERU Conference),” held at the Kavli IPMU. Director’s Corner March 26: With high school students, a lecturer, and teaching assistants at the“ Spring Science Camp 2015: A challenge to Unravel the Mystery of the Universe through Astronomy, March 26: With administrative ofcers who are leaving the Physics and Mathematics,” held at the Kavli IPMU. Kavli IPMU. 3 FEATURE Kavli IPMU Assistant Professor Surhud More Research Area： Astrophysics and Cosmology Using Galaxies to Shed Light on the Dark Universe questions lie at the interface between particle 1. The Dark Universe physics and cosmology and are at the prime The grandeur of the night sky has bedazzled focus of ongoing research. The Kavli IPMU is mankind from time immemorial. Human curiosity undertaking a multi-pronged approach to attack has lead us on a quest to understand fundamental these problems by astrophysical observations and questions about the nature of the Universe, its laboratory experiments, which can be used to build origin and its fate. Astrophysical observations a theoretical understanding of these mysterious remain at the front and center in this quest. They components of nature. have continued to unravel a number of dark mysteries that the Universe holds in store for us. 2. The Early Universe and the Birth of The most puzzling of the many astrophysical Galaxies discoveries so far, has been the existence of In the simplest concordance cosmological model, dark matter and dark energy. Dark energy is the early Universe started very hot and dense. It an omnipresent, nonclumpy form of energy underwent a rapid phase of ination where the tiny (traditionally attributed to the vacuum), while uctuations of a quantum eld were stretched to dark matter is composed of slow-moving matter cosmologically large scales. These uctuations were particles, which do not interact electromagnetically. imprinted onto the density eld of dark matter These two components dominate (accounting particles. The uctuations in dark matter grew by for nearly 95%) the energy density budget of the the action of gravity and led to the formation of cosmos over that of ordinary matter which we have structure in the Universe. explored and mastered very successfully so far with The growth of these uctuations can be studied laboratory experiments (such as those carried out with the help of computer simulations. This topic with particle accelerators like the Large Hadron has been previously covered in the Kavli IPMU Collider, LHC). News (see feature article by Naoki Yoshida in the What is the nature of dark matter and dark September 2014 edition). The statistics of the dark energy, what are their properties, and how do they matter distribution on the largest scales is governed relate to ordinary matter? Do these components by a number of important cosmological parameters, truly exist, or are they a result of an incomplete such as the amount of matter in the Universe, the theory of gravity on cosmological scales? These amplitude of initial density uctuations. Mapping 4 Kavli IPMU News No. 29 March 2015 Big Bang The Universe Gravity + Gas physics Galaxies Figure 1. Cosmic ination results in a nearly homogeneous Universe, seeded with tiny primordial uctuations. These tiny uctuations are imprinted onto the matter distribution. A snapshot of these uctuations about 380000 years after the big bang can be observed by looking at the cosmic microwave background radiation (see feature article by David Spergel in IPMU News No. 10, June 2010). The dark matter uctuations grow to form a cosmic web structure which forms the backbone of structure in the Universe. Complex astrophysical processes then result in the formation and evolution of galaxies. Intelligent life can arise in such galaxies which can then observe the Universe and unravel its history. out the growth of these uctuations with time is dark matter attract more baryons towards them. important to understand the temporal behavior of The baryons undergo a series of complex dark matter and dark energy. But since dark matter astrophysical processes (such as radiative cooling, does not emit light, it is hard to detect. Fortunately, star formation and feedback) and eventually form we have galaxies which emit lots of light and can galaxies such as our own galaxy, the Milky Way. be detected out to large distances. How are these On the largest scales, the galaxy distribution Feature galaxies then related to the dark matter? is expected to trace the dark matter distribution Dark matter particles clump together to form just due to gravity: wherever there is a lot of dark gravitationally bound objects (we will call them matter, we expect more and brighter galaxies to dark matter halos). These clumps come in a variety form. Galaxies can therefore be used to probe of shapes and sizes, there are numerous small the structure of the dark matter distribution, ones, but the big ones are relatively rare. Baryons and its growth in time, thereby improving our (primarily primordial gas clouds) are attracted understanding of the nature of dark matter and towards the center of the gravitational potential dark energy. of these dark matter halos. Places which are rich in 5 Figure 2. The expected distribution of galaxies (left) and the corresponding distribution of dark matter (right) today in the concordance cosmological model. The dark matter distribution was obtained by running large computer simulations. Semi-analytical recipes for the physics of the galaxy formation and evolution were implemented to predict the distribution of galaxies in the dark matter structure. The galaxy distribution traces the dark matter distribution on large scales. Observations of galaxies at different cosmic epochs can be used to study the growth rate of structure in dark matter. Measurements of the growth of structure can help us understand the nature of dark matter and dark energy. the mass of the halos of these galaxies can then 3. The Clustering of Dark Matter Halos yield cosmological constraints. Since galaxies live in dark matter halos, it is important to understand how halos are related to the dark matter distribution. Dark matter halos 4. Galaxy Observables form at the peaks of the density distribution. Most 4.1 Galaxy Clustering massive halos form at the rare, large scale peaks of Astronomers all over the world are carrying out the density eld. The distribution of such massive large galaxy surveys to map the distribution of halos is highly clustered compared to the low mass galaxies on large scales. One of the prime examples halos. This behavior is qualitatively similar to that of is the Sloan digital sky survey (SDSS), which has the highest mountain peaks that we nd on earth. recently concluded its third incarnation (SDSS-III). The chance of nding a mountain peak at close They obtain accurate positions of galaxies in the proximity to another one is very high (all mountain plane of the sky via imaging data, as well as along peaks with height greater than 7200m are located the radial line-of-sight using the shift of galaxy in the region of the Himalayas). Therefore one gets spectral lines towards the red side of the spectrum a biased view of the dark matter distribution by just (redshift).
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