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Titlebook: Low Frequency Radio Observations of Galaxy Clusters and Groups; Thérèse Cantwell Book 2018 Springer Nature Switzerland AG 2018 Galaxy Clus

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發(fā)表于 2025-3-21 20:02:20 | 只看該作者 |倒序?yàn)g覽 |閱讀模式
書(shū)目名稱(chēng)Low Frequency Radio Observations of Galaxy Clusters and Groups
編輯Thérèse Cantwell
視頻videohttp://file.papertrans.cn/589/588780/588780.mp4
概述Nominated as an outstanding Ph.D thesis by the University of Manchester, Manchester, UK.Reports on the discovery of a new radio halo.Presents the first detection of polarisation in NGC 6251 at low fre
叢書(shū)名稱(chēng)Springer Theses
圖書(shū)封面Titlebook: Low Frequency Radio Observations of Galaxy Clusters and Groups;  Thérèse Cantwell Book 2018 Springer Nature Switzerland AG 2018 Galaxy Clus
描述.This book uses new data from the very low radio frequency telescope LOFAR to analyse the magnetic structure in the giant radio galaxy NGC6251. This analysis reveals that the magnetic field strength in the locality of this giant radio galaxy is an order of magnitude lower than in other comparable systems. Due to the observational limitations associated with capturing such huge astrophysical structures, giant radio galaxies are historically a poorly sampled population of objects; however, their preferential placement in the more rarefied regions of the cosmic web makes them a uniquely important probe of large-scale structures. In particular, the polarisation of the radio emissions from giant radio galaxies is one of the few tools available to us that can be used to measure magnetic fields in regions where the strength of those fields is a key differentiator for competing models of the origin of cosmic magnetism. Low frequency polarisation data are crucial for detailed analyses of magnetic structure, but they are also the most challenging type of observational data to work with. This book presents a beautifully coupled description of the technical and scientific analysis required to
出版日期Book 2018
關(guān)鍵詞Galaxy Clusters; Radio Halo; Radio Galaxies; NGC 6251; LOFAR low frequency radio telescope; Low Frequency
版次1
doihttps://doi.org/10.1007/978-3-319-97976-2
isbn_softcover978-3-030-07430-2
isbn_ebook978-3-319-97976-2Series ISSN 2190-5053 Series E-ISSN 2190-5061
issn_series 2190-5053
copyrightSpringer Nature Switzerland AG 2018
The information of publication is updating

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發(fā)表于 2025-3-21 21:25:18 | 只看該作者
LOFAR HBA Observations of NGC 6251,.). The images presented in this chapter are the highest sensitivity and resolution images of NGC 6251 at these frequencies to date. I will also present the first detailed spectral index maps of the source at such low frequencies.
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e spatial reference frame for mental spatial representations. But landmarks are not a fundamental category in current geographic information modelling. For example, among Kuhn’s list of . [36] one finds . and . as separate concepts, which appears to be incompatible with our cognitively motivated vie
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Thérèse Cantwelltions, but are quite unaffordable in moving towards a higher level of development. In this paper, we set a goal to identify existing barriers of knowledge spillovers in small and medium-sized cities and their subsequent localization. We thus indicated the urban environment quality, the financial cap
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Thérèse Cantwellheoretical biology, he considered it the “age d’or de la biologie” (Bataillon 1953, p. 384). He himself, the discoverer of traumatic parthenogenesis in the frog (1910) and an expert in the theory of fertilization, had made a substantial contribution to the image of biology in those years, owing to h
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LOFAR HBA Observations of NGC 6251, giant radio galaxy with a borderline FRI/FRII morphology. The main jet and lobe aregma centre brightened like an FRI however there is a hot spot or ‘warm spot’ in the lobe suggestive of an FRII. In contrast the counter jet and lobe are edge brightened with another hot spot in the southern lobe. The
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發(fā)表于 2025-3-23 05:50:16 | 只看該作者
Techniques and Data Calibration,The resolution of a radio telescope is determined by the equation ., where . is the observing wavelength and . is the diameter of the dish. Increasing the resolution of single dish radio astronomy requires the construction of larger and larger dishes, which quickly becomes both impractical and expensive.
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