Publications of the Astronomical Society of Japan最新文献_第7页

KAgoshima Galactic Object survey with Nobeyama 45 m telescope by Mapping in Ammonia lines (KAGONMA): Discovery of parsec-scale CO depletion in the Canis Major star-forming region 利用野边山 45 米望远镜通过氨线测绘（KAGONMA）进行鹿儿岛星系天体巡天：发现大犬座恒星形成区的等秒尺度CO耗竭

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-12-07 DOI: 10.1093/pasj/psad080

Yushi Hirata, Takeru Murase, Junya Nishi, Yoshito Shimajiri, Toshihiro Omodaka, Makoto Nakano, Kazuyoshi Sunada, Takumi Ito, Toshihiro Handa

{"title":"KAgoshima Galactic Object survey with Nobeyama 45 m telescope by Mapping in Ammonia lines (KAGONMA): Discovery of parsec-scale CO depletion in the Canis Major star-forming region","authors":"Yushi Hirata, Takeru Murase, Junya Nishi, Yoshito Shimajiri, Toshihiro Omodaka, Makoto Nakano, Kazuyoshi Sunada, Takumi Ito, Toshihiro Handa","doi":"10.1093/pasj/psad080","DOIUrl":"https://doi.org/10.1093/pasj/psad080","url":null,"abstract":"In observational studies of infrared dark clouds, the number of detections of CO freeze-out on to dust grains (CO depletion) at the pc scale is extremely limited, and the conditions for its occurrence are, therefore, still unknown. We report a new object where pc-scale CO depletion is expected. As part of the Kagoshima Galactic Object survey with Nobeyama 45 m telescope by Mapping in Ammonia lines (KAGONMA), we have made mapping observations of NH3 inversion transition lines towards the star-forming region associated with Canis Major OB1, including IRAS 07077−1026, IRAS 07081−1028, and PGCC G224.28−0.82. By comparing the spatial distributions of NH3 (1,1) and C18O (J = 1–0), an intensity anti-correlation was found in IRAS 07077−1026 and IRAS 07081−1028 on the ∼1 pc scale. Furthermore, we obtained a lower abundance of C18O at least in IRAS 07077−1026 than in the other parts of the star-forming region. After examining high-density gas dissipation, photodissociation, and CO depletion, we concluded that the intensity anti-correlation in IRAS 07077−1026 is due to CO depletion. On the other hand, in the vicinity of the center of PGCC G224.28−0.82, the emission line intensities of both NH3 (1,1) and C18O (J = 1–0) were strongly detected, although the gas temperature and density were similar to IRAS 07077−1026. This indicates that there are situations where C18O (J = 1–0) cannot trace dense gas on the pc scale and implies that the conditional differences in which C18O (J = 1–0) can and cannot trace dense gas are unclear.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":2.3,"publicationDate":"2023-12-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138556306","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

Magnetic activity variability of nearby bright Sun-like stars by 4 yr intensive Hα line monitoring 用4年密集的α谱线监测邻近明亮类太阳恒星的磁活动变化

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-12-04 DOI: 10.1093/pasj/psad077

Sanghee Lee, Yuta Notsu, Bun’ei Sato

{"title":"Magnetic activity variability of nearby bright Sun-like stars by 4 yr intensive Hα line monitoring","authors":"Sanghee Lee, Yuta Notsu, Bun’ei Sato","doi":"10.1093/pasj/psad077","DOIUrl":"https://doi.org/10.1093/pasj/psad077","url":null,"abstract":"We report intensive monitoring of the activity variability in the Hα line for 10 Sun-like stars using the 1.88 m reflector at Okayama Branch Office, Subaru Telescope, during the last four years (2019–2022). Our aim was to investigate features of the stellar magnetic activity behavior. We correlated the Hα line variability of each star with the stellar activity levels derived from the Ca ii H&K line, suggesting its efficiency as a magnetic activity indicator. In analyzing the Hα line variation, we observed that some stars exhibited linear or quadratic trends during the observation period. Among several G- and K-type stars expected to have co-existing activity cycles, we confirmed the 2.9 yr short cycle of ϵ Eri (K2V) from the Hα observations. Additionally, we established upper limits on the Hα variability of β Com (G0V) and κ1 Cet (G5V) concerning their expected shorter cycles. We also detected the possibility of short-term activity cycles in two F-type stars, β Vir (F9V; ∼530 d) and α CMi (F5IV-V; ∼130 d). The cycle in α CMi was observed in only one season of our 4 yr observations, suggesting the temporal absence of the cycle period. However, for stars with planets, we did not observe significant magnetic activity variability likely associated with the planetary orbital period. It is speculated that the impact of Hα variability on radial velocity (RV) measurements may vary with spectral type.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":2.3,"publicationDate":"2023-12-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138507863","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

Sulfur isotopes toward the extended envelope of Sagittarius B2 in the Galactic Center 银河系中心人马座B2扩展包层的硫同位素

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-12-04 DOI: 10.1093/pasj/psad078

Qingxu Li, Juan Li, Siqi Zheng, Junzhi Wang, Feng Gao, Yajun Wu

引用次数: 0

HINOTORI I: The nature of rejuvenation galaxies HINOTORI:星系复兴的本质

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-11-28 DOI: 10.1093/pasj/psad076

Takumi S Tanaka, Kazuhiro Shimasaku, Sandro Tacchella, Makoto Ando, Kei Ito, Hassen M Yesuf, Suin Matsui

{"title":"HINOTORI I: The nature of rejuvenation galaxies","authors":"Takumi S Tanaka, Kazuhiro Shimasaku, Sandro Tacchella, Makoto Ando, Kei Ito, Hassen M Yesuf, Suin Matsui","doi":"10.1093/pasj/psad076","DOIUrl":"https://doi.org/10.1093/pasj/psad076","url":null,"abstract":"We present the HINOTORI (Star Formation History Investigation To Find Rejuvenation) project to reveal the nature of rejuvenation galaxies (RGs), which are galaxies that restarted their star formation after being quiescent. As the first step of HINOTORI, we construct the largest RG sample with 1071 sources. We select these RGs from 8857 MaNGA (Mapping Nearby Galaxies at APO) survey galaxies by reconstructing their star formation histories with the Prospector spectral energy distribution fitting code. Both optical spectral data and UV to IR photometric data are used for the fitting. Using mock data, we confirm that our method can detect weak rejuvenation events that form only about $0.1$% of the total stellar mass with high completeness. The RGs account for ${sim}10$% of the whole sample, and rejuvenation events contribute on average only about $0.1$% of the total stellar mass in those galaxies but $17$% of the cosmic star formation rate density today. Our RGs have a similar mass distribution to quiescent galaxies (QGs). However, the morphology of the RGs is more disk-like than QGs, suggesting that rejuvenation may occur selectively in disk-like QGs. Our results also suggest the possibility of multiple-time rejuvenation events in a single galaxy. Further spatially resolved analyses of integral field unit data and radio observations and comparisons to simulations are needed to identify the mechanism and the role of rejuvenation in galaxy evolution.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":2.3,"publicationDate":"2023-11-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138507877","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

12CO and 13CO observation of the low-metallicity dwarf galaxy DDO 154 低金属丰度矮星系DDO 154的12CO和13CO观测

IF 2.3 4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-11-17 DOI: 10.1093/pasj/psad074

Shinya Komugi, Miku Inaba, Tetsuo Shindou

引用次数: 0

The soft X-ray background with Suzaku. II. Supervirial temperature bubbles? Suzaku的软x射线背景。2常温气泡?

4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-11-14 DOI: 10.1093/pasj/psad073

Hayato Sugiyama, Masaki Ueda, Kotaro Fukushima, Shogo B Kobayashi, Noriko Y Yamasaki, Kosuke Sato, Kyoko Matsushita

{"title":"The soft X-ray background with Suzaku. II. Supervirial temperature bubbles?","authors":"Hayato Sugiyama, Masaki Ueda, Kotaro Fukushima, Shogo B Kobayashi, Noriko Y Yamasaki, Kosuke Sato, Kyoko Matsushita","doi":"10.1093/pasj/psad073","DOIUrl":"https://doi.org/10.1093/pasj/psad073","url":null,"abstract":"Abstract Observations of the hot X-ray emitting interstellar medium in the Milky Way are important for studying the stellar feedback and for understanding the formation and evolution of galaxies. We present measurements of the soft X-ray background emission for 130 Suzaku observations at 75° &lt; l &lt; 285° and |b| &gt; 15°. With the standard soft X-ray background model consisting of the local hot bubble and of the Milky Way halo, residual structures remain at 0.7–1 keV in the spectra of some regions. Adding a collisional-ionization-equilibrium component with a temperature of ∼0.8 keV, much higher than the virial temperature of the Milky Way, significantly reduces the derived C-statistic for 56 out of 130 observations. The emission measure of the 0.8 keV component varies by more than an order of magnitude: assuming the solar abundance, the median value is $3 times 10^{-4}, rm {cm^{-6} pc}$ and the 16th–84th percentile range is $(1!-!8) times 10^{-4}, rm {cm^{-6} pc}$. Regions toward the Orion–Eridanus superbubble, having a large cavity extending from the Ori OB1 association, have the highest emission measures of the 0.8 keV component. While the scatter is large, the emission measures tend to be higher toward lower galactic latitudes. We discuss possible biases caused by the solar wind charge exchange, stars, and background groups. The 0.8 keV component is probably heated by supernovae in the Milky Way disk, possibly related to Galactic fountains.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-11-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134991480","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

On the influence of shock–cloud interactions on the nonthermal X-ray emission from the supernova remnant RCW 86 激波-云相互作用对超新星遗迹rcw86非热x射线辐射的影响

4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-11-07 DOI: 10.1093/pasj/psad075

Aya Bamba, Hidetoshi Sano, Ryo Yamazaki, Jacco Vink

{"title":"On the influence of shock–cloud interactions on the nonthermal X-ray emission from the supernova remnant RCW 86","authors":"Aya Bamba, Hidetoshi Sano, Ryo Yamazaki, Jacco Vink","doi":"10.1093/pasj/psad075","DOIUrl":"https://doi.org/10.1093/pasj/psad075","url":null,"abstract":"Abstract The effect of the surrounding environment of supernova remnant shocks on nonthermal X-rays from accelerated electrons, with or without interacting dense material, is an open issue. We conduct spatially resolved X-ray spectroscopy of the shock–cloud interacting region of RCW 86 with XMM–Newton. It is found that bright soft X-ray filaments surround the dense cloud, observed with 12CO and H i emission lines. These filaments are brighter in thermal X-ray emission, and fainter and possibly softer in synchrotron X-rays, compared to those without interaction. Our results show that the shock decelerates due to the interaction with clouds, which results in an enhancement of thermal X-ray emission. This could possibly also explain the softer X-ray synchrotron component, because it implies that those shocks that move through a low-density environment, and therefore decelerate much less, can be more efficient accelerators. This is similar to SN 1006 and Tycho, and is in contrast to RX J1713.7−3946. This difference among remnants may be due to the clumpiness of dense material interacting with the shock, which should be examined in future observations.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-11-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135540768","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

Gamma-ray emission in the Seyfert galaxy NGC 4151: Investigating the role of jet and coronal activities 塞弗特星系ngc4151的伽马射线发射:研究喷流和日冕活动的作用

4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-10-30 DOI: 10.1093/pasj/psad072

Yoshiyuki Inoue, Dmitry Khangulyan

引用次数: 0

Seimei/KOOLS-IFU mapping of the gas and dust distributions in Galactic PNe: Unveiling the origin and evolution of the Galactic halo PN H4-1 PNe星系气体和尘埃分布的晴明/KOOLS-IFU地图:揭示星系晕PN H4-1的起源和演化

4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-10-27 DOI: 10.1093/pasj/psad069

Masaaki Otsuka, Toshiya Ueta, Akito Tajitsu

{"title":"Seimei/KOOLS-IFU mapping of the gas and dust distributions in Galactic PNe: Unveiling the origin and evolution of the Galactic halo PN H4-1","authors":"Masaaki Otsuka, Toshiya Ueta, Akito Tajitsu","doi":"10.1093/pasj/psad069","DOIUrl":"https://doi.org/10.1093/pasj/psad069","url":null,"abstract":"Abstract H4-1 is a planetary nebula (PN) located in the Galactic halo, and is notably carbon-rich and one of the most metal-deficient PNe in the Milky Way. To unveil its progenitor evolution through accurate measurement of the gas mass, we conducted a comprehensive investigation of H4-1, using the newly obtained Seimei/KOOLS-IFU spectra and multiwavelength spectro-photometry data. The emission-line images generated from the KOOLS-IFU data cube successfully resolve the ellipsoidal nebula and the equatorial flattened disk that are frequently seen in bipolar PNe evolved from massive progenitors. By a fully data-driven method, we directly derived the seven elemental abundances, the gas-to-dust mass ratio, and the gas and dust masses based on our own distance scale. By comparing the observed quantities with both the photoionization model and the binary nucleosynthesis model, we conclude that the progenitors of initial masses of 1.87 M$_{odot }$ and 0.82 M$_{odot }$ are second-generation stars formed ∼4 Gyr after the Big Bang that have undergone mass transfers and a binary merger, and have ultimately evolved into a PN showing unique chemical abundances. Our binary model successfully reproduces the observed abundances and also explains the evolutionary time scale of H4-1.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136262217","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

Magnetic-field structure of the Crab pulsar wind nebula revealed with IXPE 用IXPE揭示的蟹状星云脉冲星风星云的磁场结构

4区物理与天体物理

Publications of the Astronomical Society of Japan Pub Date : 2023-10-27 DOI: 10.1093/pasj/psad070

Tsunefumi Mizuno, Hiroshi Ohno, Eri Watanabe, Niccolò Bucciantini, Shuichi Gunji, Sinpei Shibata, Patrick Slane, Martin C Weisskopf

{"title":"Magnetic-field structure of the Crab pulsar wind nebula revealed with IXPE","authors":"Tsunefumi Mizuno, Hiroshi Ohno, Eri Watanabe, Niccolò Bucciantini, Shuichi Gunji, Sinpei Shibata, Patrick Slane, Martin C Weisskopf","doi":"10.1093/pasj/psad070","DOIUrl":"https://doi.org/10.1093/pasj/psad070","url":null,"abstract":"Abstract We report a detailed study of the magnetic-field structure of the Crab pulsar wind nebula, using the X-ray polarization data in 2–8 keV obtained with the Imaging X-ray Polarimetry Explorer. Contamination of the data for the nebula region by the pulsar emission was removed through application of a stringent pulsation phase cut, extracting a phase range of 0.7–1.0 only. We found that the electric-field vector polarization angle (PA) was about 130○ from north to east with a polarization degree (PD) of about 25% at the pulsar position, indicating that the direction of the toroidal magnetic field is perpendicular to the pulsar spin axis in the region close to the termination shock. The PA gradually deviated from the angle as an increasing function of the distance from the pulsar. There was a region of low PD to the west of the X-ray torus. Although such a region is expected to be located at the torus edge, where geometrical depolarization due to a steep spatial variation of the PA is expected, the observed low-PD region positionally deviated from the edge. We found that the region of low PD positionally coincided with a dense filament seen in the optical band, and conjecture that the low-PD region may be produced through deflection of the pulsar wind. By comparing the values of the PD at the pulsar position between the data and a model, in which toroidal and turbulent magnetic fields were considered, we estimated the fractional energy of the turbulent magnetic field to be about 2$/$3 of the total. We also evaluated the potential polarization of the northern jet in the nebula and derived the PD and PA to be about 30% and 120○, respectively.","PeriodicalId":20733,"journal":{"name":"Publications of the Astronomical Society of Japan","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2023-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136316799","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