• 천문학회보
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• 제46권2호
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• pp.35.1-35.1
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• 2021

Variability in young stellar objects (YSOs) can be caused by various time-dependent phenomena associated with star formation, including accretion rates, geometric changes in the circumstellar disks, stochastic hydromagnetic interactions between stellar surfaces and inner disk edges, reconnections within the stellar magnetosphere, and hot/cold spots on stellar surfaces. Among these YSO variability phenomena, bursts of accretion, which are the most remarkable variability, usually occur sporadically, making it challenging to catch the bursting moments observationally. However, the burst accretion process significantly affects the chemical conditions of the disk and envelope of a YSO, which can be used as a prominent tracer of episodic accretion. I will introduce our ensemble studies of YSO variability at mid-IR and submillimeter and also cover the ALMA observations of several YSOs in the burst accretion phase, especially in the view of chemistry.

• 전자공학회논문지SC
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• 제42권1호
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• pp.39-45
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• 2005

본 논문은 밀리미터파를 이용한 무혈혈당측정기 개발의 기초연구로서, 높은 유전손실을 지닌 유전체의 반사 유전특성 측정법을 제시하고, 이에 의해 10～90 GHz의 밀리미터파 대역에서 글루코오스 농도에 따른 글루코오스 수용액 및 글루코오스 -0.9% NaCl 용액의 유전특성 변화를 조사하였다. 제시된 측정법은 측정 유전제의 앞단에 평행평면판을 배치하여 측정 주파수대역 내에서 전력반사계수가 최소가 되는 최소반사조건이 형성되도록 하고, 이 조건에서 측정된 최소 전력반사계수와 주파수로부터 측정 유전체의 유전특성을 결정할 수 있는 방법이다. 순수의 유전특성에 대한 측정 결과들은 제시된 측정법의 타당성을 입증하였다. 또한 10～90 GHz 대역에서 글루코오스 농도 변화에 따른 글루코오스 용액 및 글루코오스 -0.9% NaCl 용액들의 유전특성 변화에 대한 실험을 통해, 타 대역에 비해 30～45 GHz 범위에서 글루코오스 농도 변화에 의한 각 용액들의 유전특성의 변화가 최대임을 알 수 있었다. 이를 통해 본 측정법에서 전력반사계수와 주파수의 측정 정밀도가 각각 ±0.1 dB와 ±0.01 GHz일 경우, 대략 3 mole/L 정도의 분해능으로 용액 내 글루코오스 농도 변화를 측정할 수 있음을 보였다.

• 천문학논총
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• 제27권4호
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• pp.357-360
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• 2012

This paper presents $H{\alpha}$ emission line detections for four galaxies at z > 3.5 made with AKARI as part of the FUHYU mission program. These are the highest-redshift $H{\alpha}$ detections to date in star-forming galaxies. AKARI's unique near-infrared spectroscopic capability has made these detections possible. For two of these galaxies, this represents the first evidence of their redshifts and confirms their physical association with a companion radio galaxy. The star formation rates (SFRs) estimated from the $H{\alpha}$ lines under-predict the SFRs estimated from their far-infrared luminosities by a factor of ~ 2 - 3. We have also detected broad $H{\alpha}$ components in the two radio galaxies which indicate the presence of quasars.

• 천문학회보
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• 제40권2호
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• pp.31.3-32
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• 2015

We present the physical properties of star forming regions in IC 10 obtained from Korea VLBI Network (KVN) 22GHz, the Submillimeter Array (SMA) CO, Very Large Array (VLA) HI 21cm, optical (U, B, V and H-alpha), and Spitzer infrared observations. IC 10 is a nearby (~0.7Mpc) irregular blue compact dwarf (BCD) galaxy which is likely to be experiencing an intense and recent burst of star formation. This nearby infant system showing high star formation rate but low metallicity (<20% of that of the Sun) provides critical environment of interstellar medium (ISM) under which current galactic star formation models are challenged. To make quantitative analysis of the ISM in the galaxy, we apply 2D cross-correlation technique to the multi-wavelength data for the first time. By cross-correlating different tracers of star formation, dust and gas phases in IC 10 in a two dimensional way, we discuss the gas properties and star formation history of the galaxy.

• 천문학회보
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• 제41권2호
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• pp.66.2-66.2
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• 2016

KASI and NAOJ are making collaborating efforts to implement faster mapping capability into the new 275-500 GHz Atacama Submillimeter Telescope Experiment focal plane array (FPA). Feed horn antenna is one of critical parts of the FPA. Required fractional bandwidth is almost 60 % while that of traditional conical horn is less than 50 %. Therefore, to achieve this wideband performance, we adopted a horn of which the corrugation depths have a longitudinal profile. A profiled horn has features not only of wide bandwidth but also of shorter length compared to a linear-tapered corrugated horn, and lower cost fabrication with less error can be feasible. In our design process the flare region is represented by a cubic splined curve with several parameters. Parameters of the flare region and each dimension of the throat region are optimized by a differential evolution algorithm to keep >20 dB return loss and >30 dB maximum cross-polarization level over the operation bandwidth. To evaluate RF performance of the horn generated by the optimizer, we used a commercial mode matching software, WASP-NET. Also, Gaussian beam (GB) masks to far fields were applied to give better GB behavior over frequencies. The optimized design shows >23 dB return loss and >33 dB maximum cross-polarization level over the whole band. Gaussicity of the horn is over 96.6 %. The length of the horn is 12.5 mm which is just 57 % of the ALMA band 8 feed horn (21.96 mm).

• 천문학회보
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• 제42권2호
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• pp.73.2-73.2
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• 2017

고적색편이의 $Ly{\alpha}$ 방출은하($Ly{\alpha}$ emitter; LAE)는 UV 연속복사에 비해 강한 $Ly{\alpha}$ 방출선을 내는 천체로서 매우 젊고, 낮은 금속함량을 가진 원시은하이다. LAE의 강한 $Ly{\alpha}$ 방출선은 먼지가 매우 적기 때문에 소광이 거의 없이 은하에서 탈출하거나, 먼지의 국지적인 분포 때문에 나타나는 것으로 추정된다. 그러나 기존 전파관측 시설의 낮은 감도 때문에 LAE의 먼지성분은 잘 알려져 있지 않다. 우리는 Atacama Large Millimeter/Submillimeter Array (ALMA)에 의해 우연히 관측된 LAE을 찾아 먼지연속복사를 직접적으로 검출하는 시도를 해 보았다. COSMOS와 ECDFS 영역에서 발견된 약 954개의 LAE 중에서 총 38개가 ALMA로 관측된 영역에 우연히 위치한다는 것을 발견하였고, 이 중 18개의 LAE에 대해 ALMA 관측영상을 모두 더하는 방법(image stacking)을 이용하여, LAE에서 방출되는 먼지연속복사의 상한선을 결정하였다: S(0.50-0.67mm) < $63.2{\mu}Jy$, S(0.21-0.38mm) < $46.7{\mu}Jy$. 본 연구에서는 비록 직접적인 검출에는 실패하였으나, 주어진 LAE 샘플에 대한 ALMA archive 검색, 원자료 다운로드, 영상 만들기, 이미지 합침 과정을 자동화하는 Python 파이프라인을 완성하였다. 이 자동화된 과정을 이용하면, 앞으로 ALMA archive가 늘어남에 따라 감도가 높아진 실험을 쉽게 반복할 수 있을 것으로 기대된다.

• 천문학회보
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• 제42권1호
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• pp.55.3-55.3
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• 2017

The L1641 cloud in Orion is an active site of star formation. We mapped a square region of 60 arcmin by 60 arcmin in the continuum emission from 0.89 mm to 2.0 mm wavelength using MUSIC mounted on the Caltech Submillimeter Observatory 10.4 m telescope. Eight sources were detected in at least two wavelength bands, and all the detected emission comes from thermal dust continuum radiation of dense cloud cores. Their spectral energy distributions were characterized. The dust emissivity spectral index is beta = 1.3 on average, within the range of typical cores in nearby star-forming regions. Two cores, V380 Ori NE and HH 34 MMS, have unusually low emissivity index of beta = 0.3. These cores may contain millimeter-sized dust grains, which suggests that the lifetime of some dense cores can be much longer than the free-fall timescale.

• 천문학회보
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• 제44권1호
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• pp.59.2-59.2
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• 2019

Event Horizon Telescope (EHT) aims to resolve the innermost region to the super massive black hole (SMBH) with its extremely high angular resolution (~20-25 uas) and enhanced sensitivity (down to 1-10 mJy) in concert with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.3 mm wavelength. This has a great importance as the first observational probe of the black hole shadow which has been theoretically predicted as a ring-like emission affected by the general relativistic effect under a strong gravitational field of SMBH. During the 2017 April 5-11, four nights of EHT observing campaign were carried out towards its primary targets, M87 and $SgrA{\ast}$. To robustly ensure the data processing, independent pipelines for various radio data calibration softwares (e.g., AIPS, HOPS, CASA) have been developed and cross-compared each other. The EHT has also been developing newer interferometric imaging techniques (e.g., eht-imaging-library, SMILI, dynamical imaging), as well as using an established method (CLEAN). With these, the EHT has designed various strategies which will be adopted for convincing imaging results. In this talk, I review how the robustness of EHT data processing and imaging will be validated so that the results can be ensured against well known uncertainties or biases in the interferometric data calibration and imaging.

• 천문학회보
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• 제44권1호
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• pp.35.3-35.3
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• 2019

Blazars are a subclass of active galactic nuclei (AGNs) with relativistic jets aligned with our line of sight. The jet physics is yet to be understood, but can be studied with blazar variability (e.g., flares). The highly variable blazar 3C 279 has shown a general decline of its radio flux density since 2013, but the flux density has been increasing since 2017. To better understand physical properties of 3C 279 related with the flux variations, we analyze multi-frequency new radio data obtained with Korean VLBI Network (KVN), as well as archival data from Owens Valley Radio Observatory (OVRO) and Submillimeter Array (SMA). We measure the radio spectral variability and infer the relativistic jet properties of 3C 279. The high-cadence OVRO and SMA observations are used to construct detailed light curves of the source, and KVN data supplement the spectral coverage and allow us to locate the spectral break frequencies precisely. In this talk, we present our analysis results and interpret them using a blazar jet model.

• 대한임베디드공학회논문지
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• 제17권1호
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• pp.25-32
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• 2022

IR-UWB radar has been regarded as the most promising technology for non-contact respiration and heartbeat monitoring because of its ability of detecting slight motion even in submillimeter range. Measuring heart rate is most challenging since the chest movement by heartbeat is quite subtle and easily interfered with by a random body motion or background noise. Additionally, periodic sampling can be limited by the performance of computer that handles the radar signals. In this paper, we deploy Lomb-Scargle periodogram method that estimates heart rate even with irregularly sampled data and uneven signal amplitude. Lomb-Scargle periodogram is known as a method for finding periodicity in irregularly-sampled and noisy data set. We also implement a motion detection scheme in order to make the heart rate estimation pause when a random motion is detected. Our scheme is implemented using Novelda's X4M03 radar development kit and its corresponding drivers and Python packages. Experimental results show that the estimation with Lomb-Scargle periodogram yield more accurate heart rate than the method of measuring peak-to-peak distance.