HI4PI: a full-sky H i survey based on EBHIS and GASS
N. Ben BekhtiArgelander-Institut fr Astronomie (AIfA), University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyL. FlöerArgelander-Institut für Astronomie (AIfA), University of Bonn, Auf dem Hügel 71, 53121 Bonn, GermanyReinhard KellerMax-Planck-Institut fr Radioastronomie (MPIfR), Auf dem Hgel 69, 53121 Bonn, GermanyJ. KerpArgelander-Institut fr Astronomie (AIfA), University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyDaniel LenzArgelander-Institut fr Astronomie (AIfA), University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyB. WinkelArgelander-Institut fr Astronomie (AIfA), University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyJeremy BailinDepartment of Physics and Astronomy, University of Alabama, PO Box 870324, Tuscaloosa, AL, 35487-0324, USAM. R. CalabrettaCSIRO Astronomy and Space Science, PO Box 76, Epping, NSW 1710, AustraliaL. DedesArgelander-Institut fr Astronomie (AIfA), University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyH. Alyson FordSteward Observatory, University of Arizona, Tucson, AZ 85721, USAB. K. GibsonE. A. Milne Centre for Astrophysics, University of Hull, Hull, HU6 7RX, UKU. HaudTartu Observatory, 61602 Travere, Tartumaa, EstoniaSteven JanowieckiInternational Centre for Radio Astronomy Research (ICRAR), University of Western Australia, 35 Stirling Highway, Crawley, WA 6009, AustraliaP. M. W. KalberlaArgelander-Institut fr Astronomie (AIfA), University of Bonn, Auf dem Hgel 71, 53121 Bonn, GermanyF. J. LockmanNational Radio Astronomy Observatory, PO Box 2, Green Bank, WV, 24944, USAN. M. McClure‐GriffithsCSIRO Astronomy and Space Science, PO Box 76, Epping, NSW 1710, AustraliaT. MurphySydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, AustraliaH. NakanishiGraduate School of Science and Engineering, Kagoshima university, 1-21-35 Korimoto, 890-0065 Kagoshima, JapanD. J. PisanoDepartment of Physics and Astronomy, West Virginia University, PO Box 6315, Morgantown, WV 26506, USAL. Staveley‐SmithARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia
2016en
ABI
Аннотация
Context. Measurement of the Galactic neutral atomic hydrogen (H i) column density, N H i , and brightness temperatures, T B , is of high scientific value for a broad range of astrophysical disciplines. In the past two decades, one of the most-used legacy H i datasets has been the Leiden/Argentine/Bonn Survey (LAB).
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