We report the discovery of a giant exoplanet in the microlensing event OGLE-2017-BLG-1049, with a planet―host star mass ratio of q = 9.53 ± 0.39 × 10-3 and a caustic crossing feature in Korea Microlensing Telescope Network (KMTNet) observations. The caustic crossing feature yields an angular Einstein radius of θE = 0.52 ± 0.11 mas. However, the microlens parallax is not measured because the time scale of the event, tE ≃ 29 days, is too short. Thus, we perform a Bayesian analysis to estimate physical quantities of the lens system. We find that the lens system has a star with mass Mh = 0.55+0.36 -0.29 M⊙ hosting a giant planet with Mp = 5.53+3.62 -2.87 MJup, at a distance of DL = 5.67+1.11 -1.52 kpc. The projected star{planet separation is aㅗ = 3.92+1.10 -1.32 au. This means that the planet is located beyond the snow line of the host. The relative lens{source proper motion is μrel ~ 7 mas yr-1, thus the lens and source will be separated from each other within 10 years. After this, it will be possible to measure the flux of the host star with 30 meter class telescopes and to determine its mass.

스리랑카는 채소의 주년 생산에 적합한 기후를 갖고 있는 열대국가이다. 열대, 아열대 채소의 재배면적은 전체 농지(105,062 ha)의 약 3%이다. 지난 50년 동안 스리랑카에서 채소 육종에 관한 체계적인 연구가 이루어졌고 채소 부문은 지속적으로 증가하였다. 하지만 채소 육종, 재배 및 가공과 관련된 기술이 선진국에 비해 많이 뒤떨어져 있는 형편이다. 전통 육종법을 통해 개발된 다양한 농업적 형질을 가진 품종이 현재까지 스리랑카의 채소 생산에 이용되고 있지만 생명공학적 방법을 접목한 채소 품종 육종법의 중요성이 점차로 부각되고 있다. 본 논문은 스리랑카에서 중요한 채소 작물인 토마토, 고추류, 콩류, 가지 및 여주의 육종과 품종 현황을 소개하고 향후 스리랑카 육종 전망에 대해 논의하였다.

The purpose of this research is to examine the mediating effect of enterprise competitiveness on the relationship between operational service quality management and customer perception level of freight forwarders’ services in East Coast region of Peninsular Malaysia. Data were collected from 106 customers of freight forwarders through accessible random sampling method. Usable data were analyzed through Partial Least-squares Structural Equation Modeling (PLS-SEM) approach using Smart PLS-SEM software version 3.2.8. The validity of the survey questionnaire was confirmed using content validity, structural validity and expert validity. The results revealed that operational service quality management influences customer perception toward service providers’ services. Meanwhile, enterprise competitive mediates the relationship between operational service quality management and customer perception on service providers’ services. The enterprise competitiveness was found to be a driver for better customer perception on freight forwarder service providers. Besides, it has a strong mediating effect which ultimately effect on both customer perception level of satisfaction and could enhance customer perception on operational service quality management through words of mouth. These findings would therefore offer the freight forwarders’ management teams a new perspective in developing a better operational service quality management strategies and practices with emphasis on enterprise competitiveness. It also demonstrates the significance of enterprise competitiveness in donimating towards consumer perception in service preference and future repurchase intension.

We report a spatial uctuation analysis of the sky brightness in the near-infrared from observations towards the north ecliptic pole (NEP) by AKARI at 2.4 and 3.2 μm. As a follow up study of our previous work on the Monitor eld of AKARI, we used NEP deep survey data, which covered a circular area of about 0.4 square degrees, in order to extend uctuation analysis at angular scales up to 1000". After pre-processing, additional correction procedures were done to correct time varying components and instrumental effects such as MUXbleed. To remove resolved objects, we applied 2α clipping and point spread function (PSF) subtraction. We finally obtained mosaicked images which can be used for the study of various diffuse emissions in the near-infrared sky and found that there are spatial structures in the mosaicked images using a power spectrum analysis.

Currently, the luxury retail market exceeds one trillion dollars in sales (Aroche, 2015) and is proliferated by the use of celebrities as endorsers and luxury brand ambassadors (Buckley, 2015; Okonkwo 2010). The practice of linking celebrities in luxury brand communications dates back to at least the 1800s and while the successful usage of celebrities is widely documented (e.g., Agrawal & Kamakura, 1995), so too are the stories of catastrophes as a result of celebrity transgression, overshadowing or just poor fit. Even without negative publicity or inappropriate behaviours, the use of a celebrity can still present risks to the luxury brand. For example, where unintended meanings associated with the celebrities are transferred to the luxury brand (Walker & Langmeyer, 1992; Till, 1998) or when the popularity of the celebrity (e.g. Angelina Jolie) overshadows the brand (e.g. St John) (Buckley, 2015; Horwell, 2011; Rossiter & Percy, 1987; Till & Busler, 2000). Overshadowing isn’t the only risk luxury brand managers may encounter when utilising a celebrity to endorse their brand. If, for example, consumers don’t see a match between the brand and the celebrity, or if consumers perceive the celebrity as being irrelevant to the brand, or if the celebrity has lost their appeal and connection with consumers then the celebrity presents a risk for the brand image (Choi & Rifon, 2012; Fleck, Korchia & Le Roy, 2012; Till & Busler, 2000). The choice of the ‘wrong’ celebrity can be an extremely costly mistake, with loss of sales and/or damage to the brand equity and image of the luxury brand being the potential outcome (Carrillat, D’Astous & Lasure, 2013; Folse, Burton & Netemeyer, 2013; Halonen-Knight & Hurmerinta, 2010; Thwaites, Lowe, Monkhouse & Barmes, 2012). Risk reducing strategies and due diligence during the selection process is a lengthy, complicated and complex process (Erdogan, Baker & Tagg, 2001). Luxury brand managers have long called for a more systematic and objective criteria by which to evaluate the potential celebrity risk factors (Okonkwo, 2010; Toncar, Reid, & Anderson, 2007); and this paper takes up that call with three contributions to both the literature and to practice. The first contribution concerns risk reduction strategies and extensions to the current thinking on the celebrity construct (for a thorough discussion on the celebrity construct see Gabler, 2001; Goldman, 2011; Rojek, 2001; Turner, 2004). There is a small stream of research that discusses the non-human celebrity as both a risk reducer for celebrity endorsement and also as an extension of the concept of ‘celebrity’ (e.g., Blewitt, 2013; Callcott & Lee, 1995; Folse et al., 2013; Giles, 2013; Rindova, Pollock & Hayward, 2006). This stream of research is novel and emergent and our work adds to this literature by defending our claim that like firms, animals, mythical beings and fictitious humans, events can also be celebrities. Broadening the conceptualisation of celebrity to apply to more than just real people, allows luxury brand managers to reduce costs, and regain some degree of control over the important image and reputational management of the celebrities with whom they wish to be associated The second contribution is the Celebrity Criterion Checklist, which provides luxury brand managers with a simple, systematic and quick way to determine whether someone or something (an entity) is a celebrity or not (given at least 15 years of debate about the contest term of “celebrity”). The Celebrity Criterion Checklist contains five criterion. If a luxury brand manager finds the entity they are considering fulfils all five criteria, then the brand manager be confident that they are a celebrity. The third contribution is the Celebrity Risk Evaluation Matrix (CREM). The Celebrity Risk Evaluation Matrix (CREM), facilitates higher-ordered assessments of the risk/benefit ratio associated with using different types of celebrities in luxury brand communications in a simple visual representation. Since celebrities are dynamic and have an ongoing narrative, celebrities can and do move between these quadrants and movement will depend on their life-cycle, their behavioural choices, their media presence, their authenticity and their relevance to consumers.

Polarbear is a ground-based experiment located in the Atacama desert of northern Chile. The experiment is designed to measure the Cosmic Microwave Background B-mode polarization at several arcminute resolution. The CMB B-mode polarization on degree angular scales is a unique signature of primordial gravitational waves from cosmic in ation and B-mode signal on sub-degree scales is induced by the gravitational lensing from large-scale structure. Science observations began in early 2012 with an array of 1,274 polarization sensitive antenna-couple Transition Edge Sensor (TES) bolometers at 150 GHz. We published the first CMB-only measurement of the B-mode polarization on sub-degree scales induced by gravitational lensing in December 2013 followed by the first measurement of the B-mode power spectrum on those scales in March 2014. In this proceedings, we review the physics of CMB B-modes and then describe the Polarbear experiment, observations, and recent results.

Most of the stars in the Galaxy are in binary systems. Binaries should be possible as the hosting stars of planets. Searching for planetary companions to binaries, especially evolved close binary stars, can provide insight into the formation and the ultimate fate of circumbinary planets and shed light on the late evolution of binary stars. In order to do this, we have chosen some post common envelope binaries including sdB-type eclipsing binaries and detached WD+dM eclipsing binaries as our targets and monitored them for several years. In this paper, we will present some of our new observations and results for three targets, NSVS 07826147, NSVS14256825 and RR Cae.

Due to the lack of an accretion disk in a polar (magnetic cataclysmic variable, MCV), the material transferred from the secondary is directly accreted onto the white dwarf, forming an accretion stream and a hot spot on the white-dwarf component. During the eclipses, different light components can be isolated. Therefore, the monitoring of eclipsing polars could provide valuable information on several modern astrophysical problems, e.g., CVs as planetary hosting stars, mass transfer and mass accretion in CVs, and the magnetic activity of the most rapidly rotating cool dwarfs. In the past five years, we have monitored about 10 eclipsing polars (e.g., DP Leo and HU Aqr) using several 2-m class telescopes and about 100 eclipse profiles were obtained. In this paper, we will introduce the progress of our research group at YNOs. The first direct evidence of variable mass transfer in a CV is obtained and we show that it is the dark-spot activity that causes the mass transfer in CVs. Magnetic activity cycles of the cool secondary were detected and we show that the variable mass transfer is not caused by magnetic activity cycles. These results will shed light on the structure and evolution of close binary stars (e.g., CVs and Algols).

We report a search for fluctuations of the sky brightness toward the North Ecliptic Pole with AKARI, at 2.4, 3.2, and 4.1 μm . The stacked images with a diameter of 10 arcminutes of the AKARI-Monitor Field show a spatial structure on the scale of a few hundred arcseconds. A power spectrum analysis shows that there is a significant excess fluctuation at angular scales larger than 100 arcseconds that cannot be explained by zodiacal light, diffuse Galactic light, shot noise of faint galaxies, or clustering of low-redshift galaxies. These findings indicate that the detected fluctuation could be attributed to the first stars of the universe, i.e., Population III stars.

The international cooperation project CIBER (Cosmic Infrared Background ExpeRiment) is a rocket-borne instrument, of which the scientific goal is to measure the cosmic near-infrared extra-galactic background to search for signatures of primordial galaxy formation. CIBER consists of a wide-field two-color camera, a low-resolution absolute spectrometer, and a high-resolution narrow-band imaging spectrometer. Currently, all the subsystems have been built, and the integration, testing, and calibration of the CIBER system are on process for the scheduled launch in June 2008.