'Mnras' presentation slideshows

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An upper limit to the masses of stars

An upper limit to the masses of stars. Donald F. Figer STScI Collaborators: Sungsoo Kim (KHU) Paco Najarro (CSIC) Rolf Kudritzki (UH) Mark Morris (UCLA) Mike Rich (UCLA). Arches Cluster Illustration. Outline. Introduction to the problem Observations Analysis Violators? Conclusions.

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Subtleties in Foreground Subtraction

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Observational constraints and cosmological parameters

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What do we learn from the recent cosmic-ray positron measurements?

What do we learn from the recent cosmic-ray positron measurements?. K. Blum*, B. Katz*, E. Waxman Weizmann Institute *currently at IAS, Princeton. arXiv:0907.1686 [MNRAS 405, 1458] arXiv:1305.1324. PAMELA 09.

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Scintillation in Extragalactic Radio Sources

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A first look at the UKIDSS data

A first look at the UKIDSS data. Steve Warren UKIDSS Survey Scientist with Steve Weatherley (Deteca Ltd), Paul Hewett (Cambridge). UKIDSS design First data Survey timetable Summary. 1. UKIDSS design. 4x2048x2048 Hawaii II arrays 0.4 arcsec pixels 0.21 sq.degs / exposure

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Observing Orbital Motion in Strongly Curved Spacetime

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Shinpei Shibata ?? ??? Yamagata Univ. ???? Department of Phys ????

IAUS291 ? Beijing 24 Aug 2012. The Structure of the Pulsar Magnetosphere via Particle Simulation with GRAPE. Shinpei Shibata ?? ??? Yamagata Univ. ???? Department of Phys ????. Collaborators T. Wada (NAOJ) S. Yuki (Yamagata U.) M. Umizaki (Yamagata U.).

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by George Doschek

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Methanol maser polarization in W3(OH)

Methanol maser polarization in W3(OH). Lisa Harvey-Smith Collaborators: Vlemmings, Cohen, Soria-Ruiz Joint Institute for VLBI in Europe. Overview. Formation of massive stars Support against cloud collapse -Turbulence -Magnetic support Maser polarization theory -Zeeman splitting

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Acknowledgements

Introduction .

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[Fe II ] 1.64 m m

Robert Sharp and Stuart Ryder AAO Johan Knapen U. Hertfordshire Lisa Mazzuca GSFC Ian Parry U. Cambridge. Pa b 1.28 m m. [Fe II ] 1.64 m m.

78 views • 1 slides