Publications of the Astronomical Society of Japan最新文献_第5页

Synthesized modeling and active disturbance rejection control for the Leighton Chajnantor Telescope 用于莱顿-恰南托尔望远镜的合成建模和主动干扰抑制控制系统

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-02-13 DOI: 10.1093/pasj/psad087

Weirui Chen, Yiwei Yao, Zheng Wang

{"title":"Synthesized modeling and active disturbance rejection control for the Leighton Chajnantor Telescope","authors":"Weirui Chen, Yiwei Yao, Zheng Wang","doi":"10.1093/pasj/psad087","DOIUrl":"https://doi.org/10.1093/pasj/psad087","url":null,"abstract":"The Caltech Submillimeter Observatory telescope was completely disassembled in 2023 October and will be shipped from Hawaii, USA to the new site at Chajnantor Plateau, Chile in 2024, where it is expected to be refurbished and renamed the Leighton Chajnantor Telescope (LCT). Since the much stronger wind load at the new site will provide a great challenge for LCT’s realization of a higher pointing and tracking accuracy, an active disturbance rejection controller (ADRC) is designed for LCT’s pointing control system. Due to the unavailability of LCT during its relocation process, it is necessary to develop a testbed to verify the performance of ADRC by constructing a synthesized simulation model of LCT’s pointing control system, including a mechanical dynamics model of the antenna, an analog circuit model of the motor drive system, a mathematical model of the direct current motors and the reducers, and a wind disturbance model. On the testbed, ADRC undergoes simulations to verify its capability to eliminate the negative impact of strong wind disturbance on LCT’s pointing control performance. The simulation results show that ADRC can bring benefits in improving LCT’s pointing and tracking accuracy when facing strong wind disturbance.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"1 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-02-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139754303","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Hitomi HXT deconvolution imaging of the Crab Nebula dazzled by the Crab pulsar 蟹状星云被蟹脉冲星眩晕时的 Hitomi HXT 去卷积成像

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-02-09 DOI: 10.1093/pasj/psae008

Mikio Morii, Yoshitomo Maeda, Hisamitsu Awaki, Kouichi Hagino, Manabu Ishida, Koji Mori

引用次数: 0

Detection of the neutral iron line from the supernova remnant W 49 B with Suzaku 用 "铃作 "探测超新星残余物 W 49 B 的中性铁线

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-02-08 DOI: 10.1093/pasj/psae006

Nari Suzuki, Shigeo Yamauchi, Kumiko K Nobukawa, Masayoshi Nobukawa, Satoru Katsuda

引用次数: 0

Census for the rest-frame optical and UV morphologies of galaxies at z = 4–10: First phase of inside-out galaxy formation z = 4-10 时星系静帧光学和紫外形态的普查：由内向外星系形成的第一阶段

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-02-07 DOI: 10.1093/pasj/psae004

Yoshiaki Ono, Yuichi Harikane, Masami Ouchi, Kimihiko Nakajima, Yuki Isobe, Takatoshi Shibuya, Minami Nakane, Hiroya Umeda, Yi Xu, Yechi Zhang

{"title":"Census for the rest-frame optical and UV morphologies of galaxies at z = 4–10: First phase of inside-out galaxy formation","authors":"Yoshiaki Ono, Yuichi Harikane, Masami Ouchi, Kimihiko Nakajima, Yuki Isobe, Takatoshi Shibuya, Minami Nakane, Hiroya Umeda, Yi Xu, Yechi Zhang","doi":"10.1093/pasj/psae004","DOIUrl":"https://doi.org/10.1093/pasj/psae004","url":null,"abstract":"We present the rest-frame optical and UV surface brightness (SB) profiles for 149 galaxies with Mopt &lt; −19.4 mag at z = 4–10 (29 of which are spectroscopically confirmed with JWST NIRSpec), securing high signal-to-noise ratios of 10–135 with deep JWST NIRCam 1–$5, mu$m images obtained by the CEERS survey. We derive morphologies of our high-z galaxies, carefully evaluating the systematics of SB profile measurements with Monte Carlo simulations as well as the impacts of a) AGNs, b) multiple clumps including galaxy mergers, c) spatial resolution differences with previous HST studies, and d) strong emission lines, e.g., Hα and [O iii], on optical morphologies with medium-band F410M images. Conducting Sérsic profile fitting for our high-z galaxy SBs with GALFIT, we obtain effective radius ranges for optical re,opt and UV re,UV wavelengths of re, opt = 0.05–1.6 kpc and re,UV = 0.03–1.7 kpc that are consistent with previous results within large scatters in the size–luminosity relations. However, we find that the effective radius ratio, re,opt$/$re,UV, is almost unity, $1.01^{+0.35}_{-0.22}$, over z = 4–10 with no signatures of past inside-out star formation such as found at z ∼ 0–2. There are no spatial offsets exceeding 3σ between the optical and UV morphology centers in cases of no mergers, indicative of major star-forming activity only being found near mass centers of galaxies at z ≳ 4 probably experiencing the first phase of inside-out galaxy formation.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"26 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-02-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139754513","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The Milky Way tomography with Subaru Hyper Suprime-Cam. I. Halo substructures 利用 Subaru Hyper Suprime-Cam 进行的银河层析成像。I. 光环子结构

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-01-31 DOI: 10.1093/pasj/psae003

Yoshihisa Suzuki, Masashi Chiba, Yutaka Komiyama, Kohei Hayashi, Masayuki Tanaka, Tetsuya Fukushima, Scott G Carlsten, Akira Tokiwa, Tian Qiu, Masahiro Takada

{"title":"The Milky Way tomography with Subaru Hyper Suprime-Cam. I. Halo substructures","authors":"Yoshihisa Suzuki, Masashi Chiba, Yutaka Komiyama, Kohei Hayashi, Masayuki Tanaka, Tetsuya Fukushima, Scott G Carlsten, Akira Tokiwa, Tian Qiu, Masahiro Takada","doi":"10.1093/pasj/psae003","DOIUrl":"https://doi.org/10.1093/pasj/psae003","url":null,"abstract":"We analyze the photometric data in the Wide layer of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) over ∼1200 deg2 to uncover new halo substructures beyond the distance, D⊙ ∼ 30 kpc, from the Sun. For this purpose, we develop an isochrone filter for an old, metal-poor stellar system to extract the faint main-sequence stars at a range of distances. With this method, we detect not only the previously discovered substructures such as the Orphan Stream, but also a new overdensity toward Boötes at about D⊙ ∼ 60 kpc and a new stream-like feature toward Pisces at around D⊙ ∼ 60 kpc. It has been suggested that a small-scale overdensity exists in this direction of Pisces (the so-called Pisces Overdensity), but our results show that the overdensity is widely spread with a tidally elongated feature. Combining our results with the ongoing Hyper Suprime-Cam narrow-band survey and the near-future spectroscopic survey with Prime Focus Spectrograph (PFS) will allow us to place strong constraints on the origin of these halo substructures.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"5 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-01-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139658868","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

GALAXY CRUISE: Spiral and ring classifications for bright galaxies at z = 0.01–0.3 银河巡航：z = 0.01-0.3 明亮星系的螺旋和环状分类

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-01-29 DOI: 10.1093/pasj/psae002

Rhythm Shimakawa, Masayuki Tanaka, Kei Ito, Makoto Ando

{"title":"GALAXY CRUISE: Spiral and ring classifications for bright galaxies at z = 0.01–0.3","authors":"Rhythm Shimakawa, Masayuki Tanaka, Kei Ito, Makoto Ando","doi":"10.1093/pasj/psae002","DOIUrl":"https://doi.org/10.1093/pasj/psae002","url":null,"abstract":"This paper presents a morphology classification catalog of spiral and ring features of 59854 magnitude-limited galaxies (r &lt; 17.8 mag, and additional 628005 subsamples down to r = 20 mag) at z = 0.01–0.3 based on the Third Public Data Release of the Hyper Suprime-Cam Subaru Strategic Program. We employ two deep-learning classifiers to determine the spiral and ring structures separately based on GALAXY CRUISE Data Release 1, which is dedicated to Hyper Suprime-Cam data. The number of spiral and ring galaxies contain 31864 and 8808 sources, respectively, which constitute 53% and 15% of the sample. A notable result of this study is the construction of a large sample of ring galaxies utilizing high-quality imaging data delivered by the Subaru Hyper Suprime-Cam. However, the accurate identification of ring galaxies remains difficult at a limited seeing resolution. Additionally, we confirm that most spiral galaxies are located on the star-forming main sequence, whereas ring galaxies preferentially reside in the green valley at stellar masses of 1010.5–1011 solar mass. Furthermore, decreasing fractions of spiral and ring galaxies are observed toward the centers of the galaxy clusters. The obtained morphology catalog is publicly available on the GALAXY CRUISE website.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"280 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-01-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139586989","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Multiwavelength observation of an active M-dwarf star EV Lacertae and its stellar flare accompanied by a delayed prominence eruption 多波长观测活动M矮星EV Lacertae及其恒星耀斑，伴有延迟的突出喷发

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-01-29 DOI: 10.1093/pasj/psae001

Shun Inoue, Teruaki Enoto, Kosuke Namekata, Yuta Notsu, Satoshi Honda, Hiroyuki Maehara, Jiale Zhang, Hong-Peng Lu, Hiroyuki Uchida, Takeshi Go Tsuru, Daisaku Nogami, Kazunari Shibata

{"title":"Multiwavelength observation of an active M-dwarf star EV Lacertae and its stellar flare accompanied by a delayed prominence eruption","authors":"Shun Inoue, Teruaki Enoto, Kosuke Namekata, Yuta Notsu, Satoshi Honda, Hiroyuki Maehara, Jiale Zhang, Hong-Peng Lu, Hiroyuki Uchida, Takeshi Go Tsuru, Daisaku Nogami, Kazunari Shibata","doi":"10.1093/pasj/psae001","DOIUrl":"https://doi.org/10.1093/pasj/psae001","url":null,"abstract":"We conducted four-night multiwavelength observations of an active M-dwarf star EV Lacertae on 2022 October 24–27 with simultaneous coverage of soft X-rays (NICER; 0.2–12 keV, Swift XRT; 0.2–10 keV), near-ultraviolet (Swift UVOT/UVW2; 1600–3500 Å), optical photometry (TESS; 6000–10000 Å), and optical spectroscopy (Nayuta/MALLS; 6350–6800 Å). During the campaign, we detected a flare starting at 12:28 UTC on October 25 with a white-light bolometric energy of 3.4 × 1032 erg. At about 1 h after this flare peak, our Hα spectrum showed a blueshifted excess component at a corresponding velocity of ∼100 km s−1. This may indicate that the prominence erupted with a 1 h delay of the flare peak. Furthermore, the simultaneous 20 s cadence near-ultraviolet (NUV) and white-light curves show gradual and rapid brightening behaviors during the rising phase at this flare. The ratio of flux in NUV to white light at the gradual brightening was ∼0.49, which may suggest that the temperature of the blackbody is low (&lt;9000 K) or the maximum energy flux of a non-thermal electron beam is less than 5 × 1011 erg cm−2 s−1. Our simultaneous observations of the NUV and white-light flare raise the issue of a simple estimation of UV flux from optical continuum data by using a blackbody model.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"17 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-01-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139586900","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Trigonometric parallax and proper motion of Sagittarius A* measured by VERA using the new broad-band back-end system OCTAVE-DAS VERA 利用新的宽带后端系统 OCTAVE-DAS 测量的人马座 A* 的三角视差和适当运动

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-01-27 DOI: 10.1093/pasj/psad088

Tomoaki Oyama, Takumi Nagayama, Aya Yamauchi, Daisuke Sakai, Hiroshi Imai, Mareki Honma, Yu Asakura, Kazuhiro Hada, Yoshiaki Hagiwara, Tomoya Hirota, Takaaki Jike, Yusuke Kono, Syunsaku Suzuki, Hideyuki Kobayashi, Noriyuki Kawaguchi

{"title":"Trigonometric parallax and proper motion of Sagittarius A* measured by VERA using the new broad-band back-end system OCTAVE-DAS","authors":"Tomoaki Oyama, Takumi Nagayama, Aya Yamauchi, Daisuke Sakai, Hiroshi Imai, Mareki Honma, Yu Asakura, Kazuhiro Hada, Yoshiaki Hagiwara, Tomoya Hirota, Takaaki Jike, Yusuke Kono, Syunsaku Suzuki, Hideyuki Kobayashi, Noriyuki Kawaguchi","doi":"10.1093/pasj/psad088","DOIUrl":"https://doi.org/10.1093/pasj/psad088","url":null,"abstract":"We successfully measured the trigonometric parallax of Sagittarius A* (Sgr A*) to be 117 ± 17 micro-arcseconds ($, mu mbox{as}$) using the VLBI Exploration of Radio Astrometry (VERA) with the newly developed broad-band signal-processing system named “OCTAVE-DAS.” The measured parallax corresponds to a Galactocentric distance at the Sun of $R_0 = 8.5^{+1.5}_{-1.1}:$kpc. By combining the astrometric results with VERA and the Very Long Baseline Array (VLBA) over a monitoring period of 25 yr, the proper motion of Sgr A* is obtained to be (μα, μδ) = (−3.133 ± 0.003, −5.575 ± 0.005) mas yr−1 in equatorial coordinates, corresponding to (μl, μb) = (−6.391 ± 0.005, −0.230 ± 0.004) mas yr−1 in Galactic coordinates. This gives an angular orbital velocity of the Sun of Ω⊙ = 30.30 ± 0.02 km s−1 kpc−1. We find upper limits to the core wander, Δθ &lt; 0.20 mas (1.6 au), peculiar motion, Δμ &lt; 0.10 mas yr−1 (3.7 km s−1), and acceleration, a &lt; 2.6 $, mu mbox{as} :$yr−2 (0.10 km s−1 yr−1) for Sgr A*. Thus, we obtained upper mass limits of $approx 3 times 10^{4}, M_{odot }$ and $approx 3 times 10^{3}, M_{odot }$ for the supposed intermediate-mass black holes at 0.1 and 0.01 pc from the Galactic center, respectively.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"174 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139586870","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Absolute properties of the oscillating eclipsing Algol XZ Ursae Majoris 大熊座摆动食星XZ的绝对特性

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-01-25 DOI: 10.1093/pasj/psad085

Jae Woo Lee, Kyeongsoo Hong, Hye-Young Kim, Marek Wolf, Jang-Ho Park, Pakakaew Rittipruk

{"title":"Absolute properties of the oscillating eclipsing Algol XZ Ursae Majoris","authors":"Jae Woo Lee, Kyeongsoo Hong, Hye-Young Kim, Marek Wolf, Jang-Ho Park, Pakakaew Rittipruk","doi":"10.1093/pasj/psad085","DOIUrl":"https://doi.org/10.1093/pasj/psad085","url":null,"abstract":"It is known from archival TESS data that the semi-detached Algol system XZ Ursae Majoris (UMa) is one of the candidate binary stars exhibiting short-period oscillations. We secured new high-resolution spectroscopic observations for the program target to better understand its binary and pulsation properties. From the echelle spectra, the radial velocities (RVs) of the eclipsing pair were derived, and the atmosphere parameters of the primary component were measured to be vAsin i = 80 ± 7 km s−1, Teff, A = 7940 ± 120 K, and [M/H] = −0.15 ± 0.20. The combined solution of our double-lined RVs and the TESS data provides robust physical parameters for XZ UMa with mass and radius measurement precision of better than 2%. The outside-eclipse residuals from a mean light curve in the 0.002 phase bin were used for multifrequency analyses, and we extracted 32 significant frequencies (22 in &lt;5.0 d−1 and 10 in 39–52 d−1). The low frequencies may be mostly aliasing sidelobes, while six of the high frequencies may be pulsation signals arising from the detached primary located inside the δ Sct domain. Their periods, pulsation constants, and pulsational–orbital-period ratios indicate that the mass-accreting primary star is a δ Sct pulsator and, hence, XZ UMa is an oscillating eclipsing Algol.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"37 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-01-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139586868","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Survivability of amorphous ice in comets depends on the latent heat of crystallization of impure water ice 彗星中无定形冰的生存能力取决于不纯水冰的结晶潜热

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2024-01-22 DOI: 10.1093/pasj/psad086

Sota Arakawa, Shigeru Wakita

{"title":"Survivability of amorphous ice in comets depends on the latent heat of crystallization of impure water ice","authors":"Sota Arakawa, Shigeru Wakita","doi":"10.1093/pasj/psad086","DOIUrl":"https://doi.org/10.1093/pasj/psad086","url":null,"abstract":"Comets are believed to have amorphous rather than crystalline ice at the epoch of their accretion. Cometary ice contains some impurities that govern the latent heat of ice crystallization, Lcry. However, it is still controversial whether the crystallization process is exothermic or endothermic. In this study, we perform one-dimensional simulations of the thermal evolution of kilometer-sized comets and investigate the effect of the latent heat. We find that the depth at which amorphous ice can survive significantly depends on the latent heat of ice crystallization. Assuming the cometary radius of 2 km, the depth of the amorphous ice mantle is approximately 100 m when the latent heat is positive (i.e., the exothermic case with Lcry = +9 × 104 J kg−1). In contrast, when we consider the impure ice representing the endothermic case with Lcry = −9 × 104 J kg−1, the depth of the amorphous ice mantle could exceed 1 km. Although our numerical results indicate that these depths depend on the size and the accretion age of comets, the depth in a comet with the negative latent heat is a few to several times larger than in the positive case for a given comet size. This work suggests that the spatial distribution of the ice crystallinity in a comet nucleus depends on the latent heat, which can be different from the previous estimates assuming pure water ice.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":"16 1","pages":""},"PeriodicalIF":2.3,"publicationDate":"2024-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139552707","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0