눈을 들어 파란 하늘을 보자. 하늘 어디에도 “여기는 물리학의 영역이니 물리학자가 아닌 다른 사람들은 출입금지”라는 푯말이 세워진 경계는 없다. 똑 같은 파란 하늘을 보아도 인문학자가 묻는 질문은 사회과학자의 질문과 다르다. 인문학, 사회과학, 그리고 자연과학이라는 구분은 하늘에는 없다. 우리 사회에서 벌어지는 일들도 마찬가지로 경계가 없는 것이 아닐까. 인문학과 사회과학이 각각 독특한눈으로 사회를 보듯이, 물리학자도 사회를 본다. 좀 별다르게 말이다. 오늘강연에서는 사회현상을 물리학자가 어떤 눈으로 보는지를 보여주고자 한다.

과학기술사를 소개하다 보면 특정 인물을 중심으로 풀어 나가게 되기 쉽다. 특히 한국 과학기술사를 이야기할 때에는 몇몇 과학 위인, 또는 과학 ”영웅"의 이야기를 나열하는 데 머무르고 한국 과학기술사의 큰 흐름은 다루지 못한 채 지나가는 경우가 많다. 이와 같은 과학기술사 서술은 이 분야를 처음 접하는 대중의 흥미를 돋궈 독자로 끌어 들이는 데에는 유용할 수 있으나 결과적으로는 한국 과학기술사에 대한 균형잡힌 시각을 형성하는 것을 저해할 우려가 있다. 역사는 단순히 개인의 업적 기록을 모아 놓은 것이 아니라 사회의 큰 변화를 설명하는 종합적 분석이기 때문이다. 이 발표에서는 소수의 영웅 중심으로 과학기술사를 인식하는 것의 문제점은 무엇인지, 그럼에도 불구하고 계속해서 그와 같은 인식이 살아남고 복제되는 까닭은 무엇인지를 분석해 보고자 한다. 그리고 전통시대와 근현대의 유명한 과학기술 인물이 어떻게 그려지고 있는지 몇 가지 사례를 분석함으로써, 어떤 점들이 개선되어야 하며 바람직한 개선의 방향은 어떤 것인지 함께 고민해 보고자 한다.

The COSMIC Data Analysis and Archival Center (CDAAC) at the University Corporation for Atmospheric research has processed space based GNSS radio occultation, ionospheric, and other remote sensing data for nearly two decades. The CDAAC is undergoing significant development in preparation for operational data processing of the COSMIC-2 constellatio (Constellation Observing System for Meteorology, Ionosphere, and Climate). Key enhancements include geographically separated data management, processing, and archive systems, end-to-end GNSS (GPS+GLONASS) capabilities, upgraded GNSS ground infrastructure, and low latency processing and product generation. This presentation gives an overview of major enhancements, current development status, and expected milestones to launch. We also review the status of existing radio occultation missions, including COSMIC-1, Kompsat-5 (Korea Multi-Purpose Satellite), MetOp (Meteorological Operational Satellite Program of Europe), and other missions of opportunity. Finally, we discuss a project to deploy new terrestrial GNSS receivers to collect measurements and navigation data in support of radio occultation processing.

최근 십수년 간 인터넷과 디지털 기기를 포함한 IT기술의 발전으로 인해 매일 생산되는 데이터의 양이 급속하게 증가하였다. 특히 스마트폰 기술의 발전과 보급으로 인해 페이스북, 유투브 등의 소셜 미디어 사이트에는 매일 엄청난 양의 사용자 제작 컨텐츠들이 등록되고 있다. 국내의 네이버, 카카오 등 대형 포털 서비스에도 뉴스, 음악, 동영상 등의 기존 컨텐츠 데이터뿐 아니라 블로그, 카페를 포함한 다양한 사용자 제작 컨텐츠들이 폭발적으로 증가하고 있다. 이러한 컨텐츠 빅데이터는 사용자 로그와 더불어 부가가치를 창출을 위한 새로운 서비스 개발의 중요한 자원이 될 수 있다. 그러나 데이터의 양이 너무 많을 뿐 아니라 대부분이 비정형적이며 형태도 텍스트, 이미지, 음성 등으로 매우 다양하여 단순한 통계모델 기반의 패턴 마이닝으로는 한계가 존재한다. 네이버 랩스에서는 수년전부터 기계학습을 이용한 빅데이터 패턴 분석 및 응용 연구 및 이에 기반한 서비스 개발을 수행해왔으며, 특히 최근에는 딥러닝을 이용하여 음성인식, 기계번역, 이미지인식, 온라인 쇼핑, 추천 등의 분야에서 괄목할 만한 성능 개선 및 서비스 적용을 진행하였다. 본 강연에서는 기계학습의 역사와 개념에 대하여 간략하게 소개하고 특히 최근 수년간 기계학습 분야의 패러다임으로 자리잡았으며 알파고로 인해 더욱 유명해진 딥러닝에 대하여 소개한다. 그리고 네이버 랩스에서의 기계학습 특히 딥러닝을 이용한 빅데이터 분석 및 이를 응용한 서비스 사례들을 공유한다.

이번 발표는 최근에 필자가 발표한 [유라시아 역사 기행]을 소개하고, 나아가서 한국과의 관련성에 대한 다양한 사회적 현상에 대한 대담을 가질 예정이다. 한국에서는 유라시아의 고고학과 역사에 대한 관심이 높아지는 배경에는 ‘한민족의 기원’이라는 전통적인 인식이 깔려있다. 이러한 인식은 사실 일제강점기때 일본학자들에 의해 형성된 것으로, 이후 별다른 검증이 없이 최근에도 다양하게 표출되고 있다. 다년간 시베리아, 중국 북방, 몽골, 중앙아시아 등을 조사한 강연자는 실물 고고학자료를 통하여 막연한 기원지라는 인식에서 벗어나서 유라시아 고대사의 세계사적 의미를 살펴본다. 막연한 ‘유라시아 기원설’ 또는 ‘한민족 자생설’을 모두 지양하고 한반도의 사람들이 어떻게 주변지역과 교류하였고, 그를 통해 한국의 고대사가 형성되었는지를 보고자 한다. 이러한 필자의 노력은 궁극적으로 단순하게 한국 민족의 기원규명이라는 오래된 물음에 대한 합리적인 대안으로 한반도 고대문화 형성에 대한 유라시아적 의의를 밝히고자 한다.

NASA has made a significant progress in Mars missions since my last visit to KASI in June 2015. In this talk, I will discuss what NASA has accomplished last one year and how much NASA is ready for human missions to Mars. As a proposer of NASA human landing site on the surface of Mars, I will go over the criteria that NASA uses to determine or finalize the human landing site using my proposed site Gale Crater as an example. I will close my talk by examining the impact of NASA Mars missions on science, technology, engineering, STEM education, and economy as well as the significance of human presence on Mars to our future generations.

TBA

Variations in solar activity and its fluctuating irradiance have been invoked as drivers of the Earth's space environment and its climate. Although, such variations and fluctuations have been followed for decades, partly even centuries, a number of important and basic questions surrounding them remain unanswered, or controversial. This also leads to significant uncertainties in the role played by the Sun in, e.g., driving climate change. In this talk I provide an overview of our present knowledge and understanding of solar variability, covering both, commonly accepted and some of the more controversial aspects.

Quasar winds are thought to be an important feedback mechanism for transporting energy and momentum from the central engine surrounding the black hole to the host galaxy. Observational evidence of these winds can be found in Broad (>2000 km/s) Absorption Lines (BALs) from C IV, Mg II, O VI, etc. The origin of the quasar winds seems to be in close relation with their X-ray emission, which is coming from the vicinities (a few times the Schwarzschild radius) of the central black hole. Additionally, the dynamics and structure of the BAL winds can be traced in the UV-rest frame of these quasars. Therefore, in order to understand the origin and evolution of the quasar winds it is fundamental to study them using a multiwavelength approach. In this talk, I will describe different multiwavelength studies of BAL quasars, with the objective of describing the origin, structure, and dynamics of their powerful winds.

Supernova research keeps playing a major role in advancing our understanding of the universe in various ways as exemplified by the phase “seeding the elements and measuring the universe.” The hitherto results from the inaugurating KMTNet Supernova Program, which exploits the unique 24-hour continuous sky coverage of the KMTNet system, look promising for various types of research, including detecting infant supernovae of uttermost interests, new types of rapid optical transients, various variable objects, and extragalactic objects of low surface brightness. I will present interim results from the KMTNet Supernova Program alongside the visible-infrared integral-field spectrograph proposed for the WFIRST for supernova research in collaboration between the University of Toronto and Honeywell Aerospace for Canadian Space Agency and NASA.

One of the most intriguing and challenging quests of current astrophysics is to understand the physical conditions and processes that give rise to the formation of relativistic jets in AGN, production of high-energy particles, and emission of gamma-rays. Of particular interest is the question of how accretion onto super-massive black holes (SMBHs) generates such high-powered directed outflows. A combination of high-resolution very long baseline interferometry (VLBI) images with broadband flux variability measurements is a unique way to probe the emission mechanisms at the bases of jets. Our analysis of gamma-ray flux variability observed by Fermi-Large Area Telescope (LAT) along with the parsec-scale jet kinematics suggests that the gamma-ray emission has a significant correlation with the mm-VLBI core flux and the local orientation of the jet flow. In this talk, I will provide a brief overview of our current knowledge on high-energy emission from blazars. At the end of my talk, I will briefly highlight open questions and particularly promising avenues for progress.

The National Optical Astronomy Observatory (NOAO) is the USA national center for ground-based optical-infrared (OIR) astronomy. It is a Federally Funded Research and Development Center (FFRDC) sponsored by the National Science Foundation and managed by the Association of Universities for Research in Astronomy (AURA). The NOAO mission is to enable discovery for the research community-at-large through open access to world-class facilities, capabilities, services, and data products. NOAO is deploying a new suite of research capabilities including new instruments, data products, and data services. Looking further in the future, NOAO will have major roles in Large Synoptic Survey Telescope (LSST) operations and community research support, and seeks similar roles in the Giant Magellan Telescope (GMT) and/or Thirty Meter Telescope (TMT) facilities as federal funding permits. In parallel to these research enabling activities, NOAO maintains an active program in public education, outreach, and engagement. This talk introduces NOAO and its current activities, presents recent research highlights, and summarizes current strategic initiatives that look towards 2030 and beyond.

The talk will review the largest Russian telescopes – the optical 6-m telescope and the Ratan 600 radio telescope with a ring-type 600 m aperture. Observational methods available to operate at these telescopes, as well as new instrumental studies for these methods – new CCD cameras, spectrographs for the 6-, 1-m telescopes and new radiometric systems for RATAN 600 will be discussed. The most important newest observational results obtained with these telescopes will also be touched in the talk.

Using the Jansky Very Large Array in recent years, Jun-Hui Zhao (CfA), Miller Goss (NRAO) and I have produced a 6-cm continuum map of the bright Sgr A complex that reveals far more detail than has previously been possible.  In this talk, I will describe the unanticipated results from this work, including a large population of new nonthermal filaments, and several magnetically-organized but highly distorted nonthermal filamentary stuctures that suggest the action of collimated outflows from the Galactic black hole, Sgr A*.   There is considerable evidence in both the radio map and a recent XMM X-ray survey that feedback from the Galactic black hole has a strong effect on the central tens of parsecs of the Galaxy, particularly in a direction perpendicular to the Galactic plane.  I’ll also describe new insights into the Sgr A East supernova remnant that appears to subsume Sgr A* within its volume, and shows a runaway neutron star that is the suspected remnant of the explosion.

It was only two decades ago that the reaction to the idea of measuring shape distortions of galaxies by gravitation lensing for reliably constraining cosmological parameters turned from skepticism to enthusiasm. Today, the technique called weak-lensing is routinely used to study dark matter distribution in galaxy clusters, average mass profiles of galaxies, and the large scale structures in the universe. The next decade will be the most exciting era when we to collect accurate cosmic shear data from billions of galaxy shapes. I will provide detailed introduction to gravitational lensing while highlighting some of the key milestones in the field. Ambitious future multi-billion dollar projects such as LSST, EUCLID, and WFIRST will be discussed. I will emphasize that in order to achieve their proclaimed scientific goals, substantial amounts of concerted efforts are required to overcome systematics. Finally, I will present my most recent results obtained from colliding galaxy clusters, which are often dubbed as "cosmic particle accelerators".

Giant molecular clouds tend to join together in a larger structure called molecular cloud complex (MCC). In one way, MCC has an important role in linking the physical properties of Milky Way structures to those of other galaxies. In another way, it serves as the nest of massive star formation event. In this talk, I will discuss recent results from high-angular resolution and high sensitivity observations of Galactic MCCs in both of aspects of connecting to other galaxies and to massive star formation. The framework of connecting to other galaxies is based on the mutual scaling relations between mass, size, velocity dispersion and star formation rate. Whereas, for massive star formation, it is based on the influence of the large scale structure on star formation.

Discovery of billion solar mass quasars at high redshift poses a challenge for modeling the initial seed black hole formation and subsequent growth history. Thus, radiation-hydrodynamic simulation for estimating growth rate of seed black holes in the range 10^2-10^5 solar mass is critical to test suggested scenarios. In this talk, I will discuss how gas accretion onto black holes is regulated by radiative feedback emphasizing the role of thermal and radiation pressure. Given the difficulty of seed black hole growth due to radiative feedback, I will present our most recent work where we show that stellar bulge component can enhance the gas accretion onto black holes when the bulge exceeds the critical mass of ~10^6 solar mass. Our results imply that heavy seed black holes (> 10^5 solar mass) that may form via direct collapse can grow efficiently coupling to the host galaxies whereas light seeds (< 10^2 solar mass) are not able to grow coevally with the host galaxies due to radiative feedback. I will also present Bondi-Hoyle type simulations with radiative feedback to show how dramatically radiative feedback changes the classical understanding of accretion onto black holes in supersonic motion.

Most of the observable matter in the Universe is in the plasma state and there must be a wide range of research topics in plasma astrophysics. Nonetheless plasma astrophysics had remained as relatively a small and less focused branch of astronomy. Only recently a variety of research opportunities in plasma astrophysics are opening up, as will be introduced in this talk. Let me with a brief review of on-going efforts to build facilities for experimental plasma astrophysics in the United States and with phase diagrams for magnetic reconnection in astrophysical systems. In the main part I will discuss specific fundamental issues such as (i) efficiency of magnetic reconnection, (ii) onset of instability, (iii) cross-scale coupling and (iv) particle acceleration, as far as time permits. For each topic, selective results of laboratory experiments will be shown first and then followed by those of solar observations where complex magnetic structure is visible in detail. This presentation is based on workshops on plasma astrophysics held in Princeton Plasma Physics Laboratory and solar research carried out in New Jersey Institute of Technology.

The gravitational waves were detected directly for the first time on September 14 at 18:51 (Korean Standard Time) by twin LIGO detectors located at Livingston, Louisiana and Hanford, Washington nearly simultaneously. This signal was initially noticed by the detection software within 3 minutes of the arrival, but final confirmation was made only after long and careful investigation of the noise characteristics, shape of the signal and possible influence of the environment.  We finally concluded that the detected waves were produced during the last fraction of second of the inspiral and merger of a binary system composed of two black holes of about 39 and 26 Msun each, located at about 1.3 billion light years. During this process, huge amount of energy corresponding to approximately 3 Msun in the form of gravitational waves has been radiated away, leaving a single black hole of about 62 solar mass behind. In this talk, I will briefly describe the nature of the nature of gravitational waves, the principle of the LIGO detectors and their sensitivities, and how actual detection was made. Then I will close my talk by commenting on the prospect of the gravitational wave astronomy brought by this detection.

After 25 years of intensive efforts, microlensing is beginning to gain international recognition as a powerful method to probe planetary demographics. Due to the vision of Cheongho Han more than a decade ago, the Korea Microlensing Telescope Network has completed its commissioning year just at this moment. I explain how KMTNet is the first variability survey specifically optimized for microlensing. I discuss the power of the microlensing technique by its concrete accomplishments, and then discuss the KMTNet strategy to build on these accomplishments over the next five years. Finally, I discuss why KMTNet is the best complement to space-based microlensing studies, both present and future.

Abstract: Clumpiness of intergalactic medium in sub-Mpc scales can boost the recombination rate significantly, thereby affecting the growth of HII bubbles during the Epoch of Reionization (EoR). In this study, we use high-resolution hydrodynamic simulation with radiative-transfer to assess clumpiness of ionized gas in sub-Mpc scales to provide a sub-grid preion for unresolved clumping factor for large-scale EoR simulations. Compared to previous studies, we extend the mass resolution well below 10^8 M_sun to take into account the structures that can form in pre-ionized medium with T10) clumping factor for ionized gas and hugely boosts the recombination rate until they are mostly disrupted by hydrodynamic feedback after ~10 Myr. When our sample volume gets ionized at z_i with a blackbody radiation with the intensity J_21, the integrated recombination from the structures is N^add_rec = 0.32* (J_21)^0.12 [(1+z_i)/11]^-1.7 per H atom on top of what is expected from homogenous distribution of the gas. In models that most the volume ionized near the end of reionization, this can add significantly (N^add_rec ~> 0.5) to the ionizing photon budget to achieve the reionization.

Most young, low-mass stars are surrounded by accretion disks. The increasing number of planets detected around main-sequence stars strongly suggests that planets will form in many, if not all, disks. A broad goal is to connect the properties and evolution of disks with the formation and diversity of planetary systems. Millimeter-wavelength interferometric observations play a central role in these studies by probing the bulk of the gas and dust in disks. In this talk, I present recent results to measure the structure, grain growth, and temporal evolution of disks with an emphasis on ALMA, CARMA, and VLA observations. I will also highlight future directions with ALMA.

유럽연합은 유럽의 글로벌 경쟁력 확보를 목표로 Innovation Union 및 Europe 2020 주요 계획(Flagship Initiative)을 실현하기 위한 연구지원 프로그램(Horizon2020 )을 운영하고 있다. Horizon2020 은 2014년부터 2020년까지 총 7년동안 약 800억유로 (약 110조원)를 투자하는 세계 최대 연구지원 프로그램으로, 역내 금융 위기를 극복하고 일자리를 창출해 지속적인 경제성장을 도모하면서 유럽이 직면한 사회적 현안을 해결하고, 지속적인 성장을 도모한다. 크게 세가지 주요 사업(과학의 우수성, 산업 리더쉽, 사회적 난제)으로 구성되어 있으며, 특히 국제협력 확대, 산업계의 참여 도모, 참여자 중심의 프로그램 운영 등의 특징을 가지고 있다. 유럽집행위원회(European Commission)는 매 2년마다 중점 추진사업별 국제공동연구, 인력교류 및 산업혁신 관련 공고를 발표하고 있으며, 2016-2017년도 Horizon2020 SPACE 분야는 크게 여섯가지 영역으로 구분, 지원된다. (1) Satellite Navigation (Galileo & EGNOS applications and infrastructure), (2) Earth Observation (Earth Observation applications and services), (3) Competitiveness of the European Space sector, (4) Space Surveillance and Tracking support framework, (5) SME Instrument and Fast Track to Innovation, (6) Other Action 한국측 연구자는 EU Horizon2020 대부분의 과제에 참여할 수 있으나, EU 에서 별도의 연구 예산을 지원하지 않는다. 따라서 미래부와 산업부에서는 Horizon2020 과제에 참여가 확정된 한국측 연구자에게 별도의 매칭펀드를 제공하고 있다. (인력교류 과제 연간 50백만원 내외, 공동연구 과제 연간 150~500백만원 내외)

I will talk about astrophysical compact objects g on various properties of neutron stars. A neutron star (NS) is a remnant of stellar collapse (supernova) and is supported against gravity by neutron degeneracy pressure predicted by Pauli's exclusion principle. Since the first discovery in 1967, many more NSs are discovered, and our understanding of theoretical/observational properties of NSs have improved significantly, yet there are still a lot of issues to address. In this talk, I will review fundamental physics in NSs and recent progress in observational and theoretical works.

BOMBOLO is a new multi-band visitor instrument for the SOAR 4m Telescope. It is a three-arm imager covering the near-UV and optical wavelengths through an optimized set of broad and narrow band filters. The three arms work simultaneously and independently, providing synchronized imaging capability for a variety of astronomical events. BOMBOLO is an exemplary case of science exploration feeding technology development in Chile. The instrument is at the Conceptual Design stage, having been approved by the SOAR Board of Directors as a visitor instrument in 2012 and having been granted full funding from CONICYT, the Chilean State Agency of Research, in 2013. The Design Phase has begun and will be completed in the early 2016, followed by a construction phase in 2016, with expected Commissioning in 2017.

The S-class MESSIER satellite has been designed to explore the extremely low surface brightness universe at UV and optical wavelengths. The two driving science cases target the mildly- and highly non-linear regimes of structure formation to test two key predictions of the LCDM scenario: (1) the detection of the putative large number of galaxy satellites, and (2) the identification of the filaments of the cosmic web. The satellite will drift scan the entire sky in 8 bands covering the 200-900 nm range to reach the unprecedented surface brightness levels of 33 mag/arcsec$^2$ in the optical and 37 mag/arcsec$^2$ in the UV. Many important science cases will result as free by-products and will be discussed in some detail, such as the luminosity function of galaxies, the contribution and role of intracluster light, the cosmological background radiation at UV and optical wavelengths, the warm molecular hydrogen content of galaxies at z=0.25, the chemical enrichment of the interstellar medium through mass loss of red giant stars and the accurate measure of the BAO scale at z=0.7. It will provide the first space-based reference UV-optical photometric catalogue of the entire sky, and synergies with GAIA and EUCLID will also be discussed.

We present a CMB map reconstructed from both WMAP and Planck datasets. Using recent statistical tools based on sparsity, we show that the Galactic barrier can be broken down, so that we can have a full sky high quality CMB map, for the first time. In addition, as a result of our novel approach, this high quality map is free of any significant thermal Sunyaev-Zel’Dovich effect contamination. Then, we revisit the different large-scale CMB anomalies considered as violations of its statistical isotropy or Gaussianity. Finally, we present a reconstruction of the primordial power spectrum from Planck data.

Formation and evolution of low HI mass galaxies are affected by environment and by the photoionisation feedback from the UV background after end of reionization. We study the physical processes of low HI mass galaxy formation which are imprinted on the distribution of neutral hydrogen in the Universe using the hierarchical galaxy formation model, GALFORM. We calculate the sensitivity of correlation functions to the HI mass threshold at redshifts $0 \le z \le 0.5$. Parameterizing clustering as $\xi(z)=(r/r_{0})^{-\gamma}$, we find that low HI mass galaxies increase the clustering amplitude $r_{0}$ and slope $\gamma$ in HI selected galaxy samples. This is opposite to expectations from optical galaxy surveys. We show the HI mass function for different host dark matter halo masses and types (central or satellite) to interpret the clustering of HI galaxies. We also show the contribution of low HI mass galaxies to 21cm intensity mapping. We find that semi-analytic modelling of intensity mapping requires a dark matter halo mass resolution of $<$10$^{10}{\rm h}^{-1}$M$_{\odot}$ in order to correctly predict 21cm brightness temperature fluctuations.

Understanding the cosmic growth of supermassive black hole (BH) population and coevolution with their host galaxies is now one of the essential ingredients for a complete picture of galaxy formation and evolution. This talk will show you the results of the related two observational research projects. (1) To directly map the BH-galaxy coevolution, we investigate the cosmic evolution of the BH mass-bulge luminosity scaling relationship using a sample of 52 AGNs at z~0.36 and z~0.57. By employing multi-component spectral and structural decomposition methods to the obtained high-quality Keck spectra and high-resolution HST images, BH masses and bulge luminosities are measured uniformly and consistently. Using Monte Carlo simulations to take into account selection effects, we find the observational evidence that BH growth precedes that of the host galaxies. This indicates that black holes grow first and then the host galaxies follow up in the framework of the BH-galaxy coevolution. (2) To probe the high-redshift BH population and scaling relations, measuring BH masses accurately is the first crucial step. The rest-frame UV CIV broad emission line is usually used for BH mass estimates in high-redshift AGNs (i.e.2