Technosignature, previously known as SETI(search for extraterrestrial intelligence), is the scientic evidence of past or present extraterrestrial civilizations. Since NRAO's Project Ozma was performed in 1960, most of the noticeable technosignature searches have been done by radio telescopes, hoping to find strong and narrow bandwidth signals that cannot be explained by known natural processes. Recently, the Breakthrough Listen project has opened a new opportunity for technosignature by utilizing both optical telescopes, radio telescopes, and next-generation radio telescope arrays. In this review, mainly based on NASA Technosignatures Workshop (2018), we review the current trends of technosignature surveys, as well as other possible methods for detecting technosignature. Also, we suggest what the Korean community could contribute the technosignature research, including the new SETI project with Korea VLBI Network (KVN).

Since the farside of the moon is a place to avoid arti cial radio frequency interference (RFI) created byhuman civilization, it is a most suitable place for searching technosignature, which are signs of technolog-ical civilization in the universe, in the radio band. The RFI is a factor that makes the study of searchingtechnosignature quite complicated because it is di cult to distinguish between technological signals pro-duced by human and extraterrestrial civilizations. In this paper, we review why the farside of the moon isthe best place to detect technosignature and also introduce radio observatories on the farside of the moonthat have been proposed in radio astronomy. The SETI (Search for Extraterrestrial Intelligence) projecton the farside of the moon is expected to be one of the main candidates for international collaborationresearch topics on lunar surface observatory.

기술경영학은 1960년대 미국 공공연구기관의 체계적 연구관리(R&D) 필요성과 영국 고등교육기관의 관련 학술지 창간 등에 의해 태동된 후 현재는 전 세계 809개 이상, 국내 19개 이상의 기관에서 연구와 교육활동을 수행할 정도로 크게 확산되었다. 특히, 한국에서는 2007년부터 산업부를 중심으로 지속적으로 정부예산을 투입해 단기간 내에 양적·질적으로 대학원 수준의 기술경영 인력양성 체계가 자리 잡게 되었다. 한국의 기술경영학 교육과정은 현장중심형 교육과정 운영, 교육기관 간 표준화와 동형화, 인접학문과의 친연성 등에 있어 해외의 기관과는 다른 경로와 차별성을 보인다. 본 연구에서는 한국의 기술경영학 교과과정을 체계적으로 분석함으로써 그 정체성과 차별성을 확인한다. 이를 위해 본 연구에서는 기술경영학의 주요 교재 11종(한국어 3종, 영어 8종)을 분석하여 기술경영학의 교과과정의 주요 내용을 7개 주제영역으로 구분하고 인접학문과의 차별성, 기술경영학의 정의적 특성에 관해 논하였다. 다음으로는 기술경영 대학원과정을 운영하는 한국의 9개 대학원 교과과정을 7개 주제영역에 투사하였다. 분석결과, 한국의 대학원 교과과정은 기업에서의 기술경영의 운영 측면, 산업별/기술별 기술경영, 산학연계 프로젝트/ 세미나에 62.5%의 교과목이 배정되어 있었다. 즉, 한국적 기술경영 교육과정은 지역산업에서 필요로 하는 중간관리자급의 기술경영 실행인재의 양성을 주요 목표로 하고 있다고 볼 수 있다. 본 연구는 기술경영 교과과정의 분석 토대 위에 한국의 산업발전단계를 고려한 향후 기술경영학 교육의 발전방향을 시사점으로 도출하였다. 즉, 기술과 혁신의 개념과 특성에 대한 이론, 기업 기술경영의 운영만이 아니라 전략적 측면, 기술경영의 경제사회적 맥락에 대한 교육과정이 보강될 필요가 있다는 점을 제시한다.

The main goal of the Korean VLBI Network Calibrator Survey (KVNCS) is to expand the VLBI calibrators catalog for KVN, KaVA(KVN and VERA Array), EAVN(East-Asian VLBINetwork), and other extended regions. The secondKVNCS (KVNCS2) aimed to detect VLBI fringes of new candidates for calibrators in the K band. Out of the 1533 sources whose single-dish flux density in the K band was measured with KVN telescopes (Lee et al. 2017), 556 sources were observed with KVN in the K band. KVNCS2 confirmed the detection of VLBI fringes of 424 calibrator candidates over a single baseline. All detected sources had a high Signal-to-Noise Ratio (SNR) of >25. Finally, KVNCS2 confirmed 347 new candidates as VLBI calibrators in the K band, resulting in a 5% increase in the sky coverage compared to previous studies. The spatial distribution was quasi-uniform across the observable region (Dec. > −32.5◦). In addition, the possibility as calibrator candidates for the detected sources was checked, using an analysis of the flux-flux relationship. Ultimately, the KVNCS catalog will not only become the VLBI calibrator list but is also useful as a database of compact radio sources for astronomical studies.

In this paper, we describe the first multi-frequency synthesis observations of blazar 0059+581 made with the Radioastron spaceground interferometer in conjunction with the Korean VLBI Network (KVN), Medicina and Torun ground telescopes. We conducted these observations to assess the spaceground interferometer multi-frequency mode capability for the first time.

The Crab nebula is widely used as a polarization angle calibrator for single-dish radio observations because of its brightness, high degree of linear polarization, and well-known polarization angle over a wide frequency range. However, the Crab nebula cannot be directly used as a polarization angle calibrator for single-dish observations with the Korean VLBI Network (KVN), because the beam size of the telescopes is smaller than the size of the nebula. To determine the polarization angle of the Crab nebula as seen by KVN, we use 3C 286, a compact polarized extragalactic radio source whose polarization angle is well-known, as a reference target. We observed both the Crab nebula and 3C 286 with the KVN from 2017 to 2021 and find that the polarization angles at the total intensity peak of the Crab nebula (equatorial coordinates (J2000) R.A. = 05h34m32.3804s and Dec = 22◦00′44.0982′′) are 154.2◦ ±0.3◦, 151.0◦ ±0.2◦, 150.0◦ ±1.0◦, and 151.3◦ ±1.1◦ at 22, 43, 86, and 94 GHz, respectively. We also find that the polarization angles at the pulsar position (RA = 05h34m31.971s and Dec = 22◦00′52.06′′) are 154.4◦ ±0.4◦, 150.7◦ ±0.4◦, and 149.0◦ ± 1.0◦ for the KVN at 22, 43, and 86 GHz. At 129 GHz, we suggest to use the values 149.0◦ ± 1.6◦ at the total intensity peak and 150.2◦ ± 2.0◦ at the pulsar position obtained with the Institute for Radio Astronomy in the Millimeter Range (IRAM) 30-meter Telescope. Based on our study, both positions within the Crab nebula can be used as polarization angle calibrators for the KVN single-dish observations.

During the course of analysing both single-dish and very long baseline interferometry (VLBI) data obtained from the Korean VLBI Network (KVN), we found a systematic oset between ux density measurements from dierent antennas. We were able to attribute a majority of the systematic osets to changes in the \a priori" antenna gains, which were found to have varied up to 10 percent at 22 GHz and up to 30 percent at 43 GHz. Using historical calibrator observations, we present a revised set of gains that may be applied to KVN data taken from 2015 August to 2019 January. Application of the revised gains to the KVN results in a consistency of correlated ux density measurements between the three baselines of approximately ve percent. We found that images from the recalibrated data typically have a 50 percent higher dynamic range, with some cases showing an increase of dynamic range of up to a factor of three.

공공조달에 대한 산업정책과 혁신정책 관점의 중요성이 최근 부각되고 있다. 특히, 공공조달이 중소기업의 성장과 혁신에 직접 영향을 끼치는지에 대한 논의와 연구가 있 어 왔다. 이러한 연구의 연장선상에서, 본 연구는 공공조달에 참여하는 기업의 특성 중 기업 의 연령이 성장에 대한 공공조달의 효과를 조절하는지를 분석한다. 분석 자료는 2006년부터 2017년까지 조달청 우수제품으로 지정된 약 1,247개 기업의 재무적 성과와 공공조달 매출 성 과를 연계하여 구축하였다. 패널회귀모형을 통해 분석한 결과, 공공조달 참여 정도가 큰 기 업일수록 높은 성장률을 보였을 뿐만 아니라, 이 관계는 젊은 기업일수록 더 강하게 나타났 다. 이 결과는 공공조달의 효과에 대한 기존 학술적 논의에 기여할 뿐만 아니라 공공조달 정 책 수립에 있어서도 의의를 가진다.

The KVN(Korean VLBI Network)-style simultaneous multi-frequency receiving mode is demonstrated to be promising for mm-VLBI observations. Recently, other Very long baseline interferometry (VLBI) facilities all over the globe start to implement compatible optics systems. Simultaneous dual/multi-frequency VLBI observations at mm wavelengths with international baselines are thus possible. In this paper, we present the results from the first successful simultaneous 22/43 GHz dualfrequency observation with KaVA(KVN and VERA array), including images and astrometric results. Our analysis shows that the newly implemented simultaneous receiving system has brought a significant extension of the coherence time of the 43 GHz visibility phases along the international baselines. The astrometric results obtained with KaVA are consistent with those obtained with the independent analysis of the KVN data. Our results thus confirm the good performance of the simultaneous receiving systems for the non-KVN stations. Future simultaneous observations with more global stations bring even higher sensitivity and micro-arcsecond level astrometric measurements of the targets.