'Neutral hydrogen' diaporamas de présentation

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1.09k views • 82 slides

C.17 The Milky Way

C.17 The Milky Way. When we try to pick out anything by itself, we find that it is tied to everything else in the universe. John Muir (1838-1914). For comparison of the following slides, the distance from the Sun to Neptune is 8.44 light hours or .000963 light years.

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21cm Lines and Dark Ages

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Galaxies and Cosmology

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The Milky Way Galaxy

The Milky Way Galaxy. The Milky Way Galaxy. Panoramic View. We now know that our Milky Way is a highly flattened system of stars, about 25,000pc across, with the sun about 2/3 of the way from the center. . Studies of Galactic Structure.

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PHYS 1830 Lecture 9:

PHYS 1830 Lecture 9:. HI gas shell in our Milky Way Galaxy. (J. English, J. Stil, & R. Taylor for VGPS.). Previous Class: Optical Telescopes Resolution, Light Gathering Power, Surface Brightness This Class: Radio Images Radio Telescopes Radio Continuum emission

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Lecture 30:

Lecture 30:. The Milky Way. topics:. structure of our Galaxy components of our Galaxy (stars and gas) how we observe different components. Our Galaxy. Edge-on View. The structure of our Galaxy.

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Probing dark matter clustering using the Lyman- ? forest

Probing dark matter clustering using the Lyman- ? forest. Pat McDonald (CITA) COSMO06, Sep. 28, 2006.

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A GPU Implementation of Extragalactic Radio Source Detection A CUDA Approach

A GPU Implementation of Extragalactic Radio Source Detection A CUDA Approach. Gary Resnick Scott Badenhorst Department of Computer Science University of Cape Town 17 March, 2010. Overview. Introduction Approach Plan Outcomes. Radio Astronomy. A radio image of the sky .

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ASKAP Continuum S urveys of Local Galaxies

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H I in galaxies from z = 0.002 to z = 0.2

H I in galaxies from z = 0.002 to z = 0.2. Thijs van der Hulst Kapteyn Astronomical Institute University of Groningen. Kapteyn astronomical institute. Open Questions. When and how quickly did the gas settle in the dark matter potential wells

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Lecture 19 The Interstellar Medium

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Supporting material for Lecture 3: Gamma-Ray Bursts and their counterparts Light extinction:

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PART 1 CLUES TO THE FORMATION AND EVOLUTION OF THE MILKY WAY

PART 1 CLUES TO THE FORMATION AND EVOLUTION OF THE MILKY WAY. This scenario is based upon observations of the motions , ages , metalicities of stars as a function of their locations in the galaxy. There are very clear trends in these observables .

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Edge Neutral Density (ENDD) Diagnostic Overview

Edge Neutral Density (ENDD) Diagnostic Overview. Patrick Ross. Monday, March19, 2007. Monday Physics Meeting. Beam Power Loss Scan with Varied Edge Neutral Density in TRANSP. Shot 120442. 10 12 cm -3.

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Radio Astronomy And The Spiral Structure Of The Milky Way

Radio Astronomy And The Spiral Structure Of The Milky Way. Jess Broderick Supervisor: Dr George Warr. Outline. Overview of the spiral arm structure of the Milky Way. Using radio astronomy to detect the spiral structure. The Spiral Arm Structure Of The Milky Way.

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HI and Molecules

HI and Molecules. 0. Observing Neutral Hydrogen: The 21-cm (radio) line. Forbidden hyperfine-structure transition: A = 2.95x10 -15 s -1. Equal magnetic fields repel => Higher energy. Opposite magnetic fields attract => Lower energy. Magnetic field due to proton spin. 21 cm line.

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The UW Observational Cosmology Group

The UW Observational Cosmology Group. The CMB and the Early Universe.

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