http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
DETECTION LEVEL ENHANCEMENTS OF GRAVITATIONAL MICROLENSING EVENTS FROM LIGHT CURVES: THE SIMULATIONS
IBRAHIM, ICHSAN,MALASAN, HAKIM L.,DJAMAL, MITRA,KUNJAYA, CHATIEF,JELANI, ANTON TIMUR,PUTRI, GERHANA PUANNANDRA The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
Microlensing can be seen as a version of strong gravitation lensing where the separation angle of the image formed by light deflection by a massive object is too small to be seen by a ground based optical telescope. As a result, what can be observed is the change in light intensity as function of time; the light curve. Conventionally, the intensity of the source is expressed in magnitudes, which uses a logarithmic function of the apparent flux, known as the Pogson formulae. In this work, we compare the magnitudes from the Pogson formulae with magnitudes from the Asinh formulae (Lupton et al. 1999). We found for small fluxes, Asinh magnitudes give smaller deviations, about 0.01 magnitudes smalller than Pogson magnitudes. This result is expected to give significant improvement in detection level of microlensing light curves.
EXPANSION VELOCITY AND SPECTROSCOPIC CLASSIFICATION OF NOVA DELPHINI 2013
AZALIAH, RHISA,MALASAN, HAKIM L.,HAANS, GABRIELA K.,AKHYAR, SAEFUL The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
Low resolution spectra of Nova Delphini 2013 (V339 Del) in the optical range have been obtained at Bosscha Observatory, Indonesia during its maximum light (V = 4.3). Spectra were observed from August 16 to 27, 2013. The GAO-ITB RTS 20.3 cm telescope, and SBIG DSS-7 spectrograph and SBIG ST-7 XE as the detector have been employed throughout the observations. The spectra show P-Cygni profiles in Balmer, NaI'D' and Fe II lines, from which we determined shell expansion velocities of $1421.66{\pm}39.18km/s$, $1227.54{\pm}21.57km/s$ and 1402.86 km/s, respectively. Our spectroscopic observations followed the spectral evolution of V339 Del from the pre-maximum phase to early Orion phase. The characteristics of the nova Delphini 2013 resembles those of Fe II-type novae.
THE NEED OF DISTANCE LEARNING FOR ASTRONOMY DEVELOPMENT IN INDONESIA
YAMANI, AVIVAH,MALASAN, HAKIM L. The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
Astronomy is a popular topic for the public in term of astronomical phenomenon such as occultations, solar and lunar eclipses or meteor showers. In term of education, astronomy also is popular as one of the world Science Olympiads. Social media, as the new trend in communicating and connecting people, plays a significant role in increasing the size of the astronomy community. Beyond IYA 2009, more and more astronomy activities have been done in many places in Indonesia. New astronomy communities have been formed in several cities and public engagement is also high in social media especially on Facebook and Twitter. In this paper, we will discuss the lesson learned from astronomy outreach achievements in Indonesia and the need for citizen science projects as a distance learning tool for the public as part of astronomy development in Indonesia. We argue and propose that this project will be also important up to a regional scope.
THE BIMA PROJECT: O-C DIAGRAMS OF ECLIPSING BINARY SYSTEMS
HAANS, G.K.,RAMADHAN, D.G.,AKHYAR, S.,AZALIAH, R.,SUHERLI, J.,IRAWATI, P.,SAROTSAKULCHAI, T.,ARIFIN, Z.M.,RICHICHI, A.,MALASAN, H.L.,SOONTHORNTHUM, B. The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
The Eclipsing Binaries Minima (BIMA) Monitoring Project is a CCD-based photometric observational program initiated by Bosscha Observatory - Lembang, Indonesia in June 2012. Since December 2012 the National Astronomical Research Institute of Thailand (NARIT) has joined the BIMA Project as the main partner. This project aims to build an open-database of eclipsing binary minima and to establish the orbital period of each system and its variations. The project is conducted on the basis of multisite monitoring observations of eclipsing binaries with magnitudes less than 19 mag. Differential photometry methods have been applied throughout the observations. Data reduction was performed using IRAF. The observations were carried out in BVRI bands using three different small telescopes situated in Indonesia, Thailand, and Chile. Computer programs have been developed for calculating the time of minima. To date, more than 140 eclipsing binaries have been observed. From them 71 minima have been determined. We present and discuss the O-C diagrams for some eclipsing binary systems.