奥村 真一郎

プラネタリーディフェンス活動において，地球に衝突する可能性のある，いわゆる地球接近天体を発見することがまずは必要である．そのような候補が見つかった場合に，見失ってしまわないように速やかに追加の位置測定観測を行い軌道を定めることが重要である．また，衝突の回避や衝突時の被害を小さくする検討のための情報として地球接近天体の素性を調べる物理的な観測も必要とされる．本稿ではプラネタリーディフェンスに向けた活動に関連して，美星スペースガードセンターでの観測活動，JAXAで開発した高速画像処理技術（重ね合わせ法），東京大学木曽観測所のトモエゴゼンカメラ，すばる望遠鏡の観測データから太陽系小天体を発見・報告できるウェブアプリケーションCOIASなど，国内における地球接近天体の観測活動について紹介する．

Abstract We studied the optical variability of 241 BL Lacertae (BL Lacs) and 83 flat-spectrum radio quasars (FSRQs) from the 4LAC catalog using data from the Tomo-e Gozen Northern Sky Transient Survey, with ∼50 epochs per blazar on average. We excluded blazars whose optical variability may be underestimated due to the influence of their host galaxy based on their optical luminosity (L _O ). FSRQs with γ-ray photon index greater than 2.6 exhibit very low optical variability, and their distribution of standard deviation of repeated photometry is significantly different from that of the other FSRQs (Kolmogorov–Smirnov test p-value equal to 5 × 10⁻⁶). Among a sample of blazars at any particular cosmological epoch, those with lower γ-ray luminosity (L _γ ) tend to have lower optical variability, and those FSRQs with a γ-ray photon index greater than 2.6 tend to have low L _γ . We also measured the structure function of optical variability and found that the amplitude of the structure function for FSRQs is higher than previously measured and higher than that of BL Lacs at multiple time lags. Additionally, the amplitude of the structure function of FSRQs with high γ-ray photon index is significantly lower than that of FSRQs with low γ-ray photon index. The structure function of FSRQs of high γ-ray photon index shows a characteristic timescale of more than 10 days, which may be the variability timescale of the accretion disk. In summary, we infer that the optical component of FSRQs with high γ-ray photon index may be dominated by the accretion disk.

ABSTRACT We present photometric, spectroscopic, and polarimetric observations of the intermediate-luminosity Type IIP supernova (SN) 2021gmj from 1 to 386 d after the explosion. The peak absolute V-band magnitude of SN 2021gmj is −15.5 mag, which is fainter than that of normal Type IIP SNe. The spectral evolution of SN 2021gmj resembles that of other sub-luminous SNe: The optical spectra show narrow P-Cygni profiles, indicating a low expansion velocity. We estimate the progenitor mass to be about 12 $\rm {\rm M}_{\odot}$ from the nebular spectrum and the 56Ni mass to be about 0.02 $\rm {\rm M}_{\odot}$ from the bolometric light curve. We also derive the explosion energy to be about 3 × 1050 erg by comparing numerical light-curve models with the observed light curves. Polarization in the plateau phase is not very large, suggesting nearly spherical outer envelope. The early photometric observations capture the rapid rise of the light curve, which is likely due to the interaction with a circumstellar material (CSM). The broad emission feature formed by highly ionized lines on top of a blue continuum in the earliest spectrum gives further indication of the CSM at the vicinity of the progenitor. Our work suggests that a relatively low-mass progenitor of an intermediate-luminosity Type IIP SN can also experience an enhanced mass-loss just before the explosion, as suggested for normal Type IIP SNe.

ABSTRACT The population of optical transients evolving within a time-scale of a few hours or a day (so-called fast optical transients, FOTs) has recently been debated extensively. In particular, our understanding of extragalactic FOTs and their rates is limited. We present a search for extragalactic FOTs with the Tomo-e Gozen high-cadence survey. Using the data taken from 2019 August to 2022 June, we obtain 113 FOT candidates. Through light curve analysis and cross-matching with other survey data, we find that most of these candidates are in fact supernovae, variable quasars, and Galactic dwarf novae that were partially observed around their peak brightness. We find no promising candidate of extragalactic FOTs. From this non-detection, we obtain upper limits on the event rate of extragalactic FOTs as a function of their time-scale. For a very luminous event (absolute magnitude M < −26 mag), we obtain the upper limits of 4.4 × 10−9 Mpc−3 yr−1 for a time-scale of 4 h, and 7.4 × 10−10 Mpc−3 yr−1 for a time-scale of 1 d. Thanks to our wide (although shallow) surveying strategy, our data are less affected by the cosmological effects, and thus, give one of the more stringent limits to the event rate of intrinsically luminous transients with a time-scale of <1 d.

Abstract We report on a one-second-cadence wide-field survey for M-dwarf flares using the Tomo-e Gozen camera mounted on the Kiso Schmidt telescope. We detect 22 flares from M3–M5 dwarfs with a rise time of 5 s ≲ trise ≲ 100 s and an amplitude of 0.5 ≲ ΔF/F⋆ ≲ 20. The flare light-curves mostly show steeper rises and shallower decays than those obtained from the Kepler one-minute cadence data and tend to have flat peak structures. Assuming a blackbody spectrum with a temperature of 9000–15000 K, the peak luminosities and energies are estimated to be 1029 erg s−1 ≲ Lpeak ≲ 1031 erg s−1 and 1031 erg ≲ Eflare ≲ 1034 erg, which constitutes the bright end of fast optical flares for M dwarfs. We confirm that more than $90\%$ of the host stars of the detected flares are magnetically active based on their Hα-emission-line intensities obtained by LAMOST. An estimated occurrence rate of detected flares is ∼0.7 per day per active star, indicating they are common in magnetically active M dwarfs. We argue that the flare light-curves can be explained by the chromospheric compression model: the rise time is broadly consistent with the Alfvén transit time of a magnetic loop with a length scale of lloop ∼ 104 km and a field strength of 1000 gauss, while the decay time is likely determined by the radiative cooling of the compressed chromosphere down near to the photosphere with a temperature of ≳ 10000 K. These flares from M dwarfs could be a major contamination source for a future search of fast optical transients of unknown types.

Hayabusa2 is the Japanese Asteroid Return Mission and targeted the carbonaceous asteroid Ryugu, conducted by the Japan Aerospace Exploration Agency (JAXA). The goal of this mission was to conduct proximity operations including remote sensing observations, material sampling, and a Small Carry-On Impact experiment, as well as sample analyses. As of September 2020, the spacecraft is on the way back to Earth with samples from Ryugu with no critical issues after the successful departure in November 2019. Here, we propose an extended mission in which the spacecraft will rendezvous with a small asteroid with ~30 m - ~40 m in diameter that is rotating at a spin period of ~10 min after an additional ~10-year cruise phase. We introduce that two scenarios are suitable for the extended mission. In the first scenario, the spacecraft will perform swing-by maneuvers at Venus once and Earth twice to arrive at asteroid 2001 AV43. In the second scenario, it will perform swing-by maneuvers at Earth twice to reach asteroid 1998 KY26. In both scenarios, the mission will continue until the early 2030s. JAXA recently released the decision that the spacecraft will rendezvous with 1998 KY26. This paper focuses on our scientific assessments of the two scenarios but leaves the decision process to go to 1998 KY26 for future reports. Rendezvous operations will be planned to detail the physical properties and surrounding environments of the target, one of the smallest elements of small planetary bodies. By achieving the planned operations, the mission will provide critical hints on the violent histories of collisions and accumulations of small bodies in the solar system. Furthermore, the established scientific knowledge and techniques will advance key technologies for planetary defense....

スペースガードとは,地球へ接近する太陽系小天体(Near Earth Object=NEO)の発見,衝突回避の研究を行う活動である. 1990年頃より, NEOの早期発見と軌道導出を行うスペースガード観測が世界各地で行われており,現在では1万を超えるNEOが発見されている.美星スペースガードセンターは国内唯一のスペースガード観測に特化した施設であり, NEOを始めとする太陽系小天体の発見,追観測,科学観測を行っている.本稿では,スペースガード観測の現状と,美星スペースガードセンターで行われている実際の観測,さらに将来の展望について紹介する.

Sulfur dioxide (SO₂) absorbs ultraviolet (UV) radiation, and airborne spectrometers can measure its spatial distribution using backscattered solar light. A new algorithm was developed to estimate the SO₂ vertical column amount. This algorithm is based on the Differential Optical Absorption Spectroscopy (DOAS) technique and the radiative transfer calculation. Aircraft-borne measurements using a ultraviolet spectrometer, the Airborne-OPUS, were performed above Miyake-jima (34^°N, 139.5^°E) in January 2002. The amount of SO₂ estimated by the Airborne-OPUS was validated using SO₂ mixing ratios measured simultaneously by an onboard air-sampling sensor during the spiral-down flight above and inside volcanic plumes. The results suggested that the above algorithm is capable of quantifying the column amount of volcanic SO₂.

We have developed an air-borne ultraviolet remote sensor, named "Airborne-OPUS." It is a nadir-looking hyper spectral imaging spectrograph, with 1100 spectral channels and 330 spatial channels. It covers the wavelength range of 190-455 nm with 0.34 nm sampling step and covers 15 degrees field of view. All main components of the sensor are composed of commercially available products : a Jobin-Yvon spectrograph as a disperser, a PixelVision 1100&times;330 CCD camera as a detector, and a ready-made single lens as its front-end optics. For the data calibration, we examined the basic parameters and the performance characteristics of the detector, such as read noise, dark current, linearity, and pixel-response uniformity.<BR>After two-demonstration flights using the Gulfstream-II aircraft, the performances of Airborne-OPUS, such as spectral resolution, signal-to-noise ratio, have been evaluated. In the flights around Miyake-jima and Sakura-jima volcanoes, the absorption structure of SO₂ was detected in the observed spectra, using the DOAS technique. The vertical column amount of SO₂ was derived from each data, and its horizontal distribution was revealed. The sensitivity of the sensor was also examined, and we discussed its application to the detection of urban pollutions.