• 천문학회보
• /
• 제36권1호
• /
• pp.43.2-43.2
• /
• 2011

목성 극지방의 분광 관측 자료에는 $H_3+$, $H_2$, 탄화수소 분자들($CH_4,C_2H_2,C_2H_6$)이 방출선의 형태로 나타난다. 이 분자선들은 2 ~ 3 mm에서는 대부분 관측이 이루어졌지만, 7.8 mm 파장대에서는 탄화수소 분자들 중에서 $CH_4$가 hotspot 형태로 관측이 되었다. 본 연구에서는 마우나케아 천문대의 NASA IRTF (InfraRed Telescope Facility) 망원경 중에 중적외선 고분산 분광기 TEXES (Texas Echelon Cross Echelle Spectrograph)를 설치하여 $CH_4$와 함께 처음 발견된 $C_2H_2$의 특성을 분석하였다. 텍사스 주립대학에서 개발한 TEXES는 5 ~ 25 mm의 관측 파장대에서 저분산(R~3,000), 중 분산(R~15,000), 고분산(R~100,000)으로 관측할 수 있다 (Lacy et al., 2002). 본 연구에 사용된 자료는 2009년 5월 29일에 관측되었으며, 파장대는 7.8 mm 이다.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
• /
• 한국우주과학회 2010년도 한국우주과학회보 제19권1호
• /
• pp.32.2-32.2
• /
• 2010

보현산 천문대 1.8-m 망원경과 고분산 에셀 분광기 BOES(BOao Echelle Spectrograph)를 이용해 관측한 다년간의 공생별 관측자료 중 AG Draconis와 EG Andromedae의 방출선들을 분석하여 그 분광학적 특성을 밝혀내고자 한다. 수소 Balmer 계열 방출선들과 He I $\lambda5875{\AA}$, He I $\lambda6678{\AA}$, He I $\lambda7065{\AA}$, He II $\lambda4686{\AA}$, O VI $\lambda6030{\AA}$, O VI $\lambda7088{\AA}$ 방출선들의 단 장기 변화와 특징을 살펴보며, 그 방출선들 간의 비교를 통해 두 공생별의 특성 변화에 대해 알아본다.

• 천문학회보
• /
• 제43권2호
• /
• pp.51.1-51.1
• /
• 2018

Based on the DOAO/eShels observations, we have derived radial velocity curves of the three Algol-type spectroscopic binary systems : Algol, ${\beta}$ Aur, and ${\varepsilon}$ Per. The radial velocity amplitudes of the primary and the secondary (K1 and K2) were consistent within a few % of the values from the previous studies. Mass ratios between the two stars that constitutes each system ranges ~1 to ~10. In addition to the orbital elements derived, we discuss about the spectroscopic ability of the DOAO/eShels instrument.

• 천문학회보
• /
• 제43권2호
• /
• pp.47.2-47.2
• /
• 2018

The umbral oscillations of velocity are commonly observed in the chromosphere of a sunspot. Their sources are considered to be either the external p-mode driving or the internal excitation by magnetoconvection. Even though the possibility of the p-mode driving has been often considered, the internal excitation has been rarely investigated. We report the observational evidence for the internal excitation obtained by analyzing velocity oscillations in the temperature minimum region of a sunspot umbra. The velocity oscillations in the temperature minimum region were determined from Fe I $5435{\AA}$ line data taken by the Fast Imaging Solar Spectrograph (FISS) of the 1.6 m Goode solar Telescope (GST) at the Big Bear Solar Observatory. As a result, we discovered 4 events of oscillations which appear to be internally excited. We analyze their characteristics and relation to photospheric features. Based on these results, we estimate the contribution of the internal excitation for umbral oscillations and discuss their importance.

• 천문학회보
• /
• 제43권2호
• /
• pp.58.3-59
• /
• 2018

We investigate velocity oscillations in a solar quiet region by using the spectral data of the $H{\alpha}$ and Ca II $8542{\AA}$ lines. The data were acquired by the Fast Imaging Solar Spectrograph installed at the 1.6 m Goode Solar Telescope of Big Bear Solar Observatory. According to Chae & Litvinenko (2018)'s theoretical work, there is a correlation between dominant period of the oscillations and the temperature of the temperature minimum region in a non-isothermal atmosphere. In our study, we measure the temporal variations of the intensity and the line of sight Doppler velocity, and find out the relations between the intensity and dominant period of the oscillations. In addition, we investigate oscillations in a few distinct regions and discuss regional characteristics of the oscillations.

• 천문학회보
• /
• 제43권2호
• /
• pp.44.1-44.1
• /
• 2018

Since its installation on March 27th, 2018, the SAO 1-m telescope has been operating for about 5 months. We report first results of these observations in this presentation. Sample images were taken with a $4096{\times}4096$ CCD camera (Field of view of ${\sim}21{\times}21arcmin^2$) and their characteristics such as seeing value, and limiting magnitudes are presented. The best seeing value is 0.85 arcsecond on July $16^{th}$, 2018. We find that the 5 sigma detection limit is about 20 magnitude AB in B, V, R, I bands with about 10-20 min exposures. We will also briefly introduce the spectrum of a faint transient taken with the spectrograph also installed on the SAO 1-m telescope.

• 천문학회보
• /
• 제43권2호
• /
• pp.58.1-58.1
• /
• 2018

In the solar atmosphere, below the region of temperature minimum, temperature decreases with height and above it, temperature increases with height. Therefore the inference of temperature minimum is a basis of the study about the solar atmosphere and heating problem. The temperature of the temperature minimum region can be inferred from acoustic cutoff frequency. According to a recent study the acoustic cutoff frequency is related to the peak frequency of the power spectrum the chromospheric three-minute velocity oscillations. Using this relationship, we infer the temperature of temperature minimum. The three minute velocity oscillation and its power spectrum are obtained for a pore observed with the Fast Imaging Solar Spectrograph (FISS) $H{\alpha}$ band. We present the inferred temperature and compare it with the temperature of Maltby model. We also investigate the effect of the inclination of magnetic field on the temperature minimum.

• 천문학회보
• /
• 제44권1호
• /
• pp.68.1-68.1
• /
• 2019

Using IPHAS $H{\alpha}$ data, we found bright $H{\alpha}$ regions inside the elongated $^{13}CO$ cavity around a Herbig star, MWC 1080. To investigate the ionized hydrogen regions and the molecular cavity, we perform near-IR high-resolution spectroscopic of hydrogen Brackett lines and molecular hydrogen lines by Immersion GRating INfrared Spectrograph (IGRINS) observations. We detected broad Brackett line series and sharp molecular lines with various velocity components. We present three ionized hydrogen regions (near MWC 1080A, MWC 1080E, and CO boundary) with different line widths, central radial velocities, and line ratios. We also show two spatially-separate $Br{\gamma}$ ${\lambda}2.1662{\mu}m$ peaks near MWC 1080A. To reveal a 3D structure of the cavity around MWC 1080, we try to use the detected sharp molecular lines.

• 천문학회보
• /
• 제43권2호
• /
• pp.60-60
• /
• 2018

It has been known that XZ CMi is a near-contact binary composed of a hotter and more massive main-sequence primary star close to its Roche-lobe and a Roche-lobe filling giant/subgiant secondary star. There still exist, however, many discordant matters among the previous investigators: diverse mass ratios and temperatures ranging from 0.38 to 0.83 and from 7,000 K to 8,876 K, respectively. In order to make a contribution to the two confusions we conducted spectroscopic and photometric observations. A total of 34 high-resolution spectra were obtained during 4 nights from 2010 and 2018 with the Bohyunsan Optical Echelle Spectrograph (BOES) at the Bohyunsan Optical Astronomy Observatory (BOAO). In parallel, BVRI multi-band photometric observations were carried out 5 nights in 2010 at Sobaeksan Optical Astronomy Observatory (SOAO). In this presentation, we present physical parameters of XZ CMi through the simultaneous analyses of new double-lined radial velocity curves and new light curves. We will also briefly discuss the evolutionary status of the system.

• 천문학회보
• /
• 제44권2호
• /
• pp.35.2-35.2
• /
• 2019

The next decade will see great advances in ground-based spectroscopic observing capabilities: facilities that are under development today will have larger collecting areas and greater spectroscopic multiplexing capabilities than ever before, and are sure to revolutionize the scientific productivity of our field. In this talk I will review the status of two of these next-generation facilities, the Giant Magellan Telescope's wide-field multiobject optical spectrograph, GMACS, and the Maunakea Spectroscopic Explorer project, a massively multiplexed spectroscopic facility currently under development in Hawaii that features an 11.25m diameter primary mirror which feeds 4,332 fibers and a suite of low- and high-resolution spectrographs. These two projects are scientifically quite complementary and both present exciting instrument development opportunities over the next few years.