'Spiral galaxies' presentation slideshows

AY202a Galaxies & Dynamics Lecture 24: Cosmological Distance Ladder

AY202a Galaxies & Dynamics Lecture 24: Cosmological Distance Ladder. The Hubble Constant:. H 0 = *current* expansion rate = (velocity) / (distance) = (km/s) / (Megaparsecs) named after Edwin Hubble who discovered the relation in 1929.

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Chapter 24 Galaxies

589 views • 48 slides

590 views • 46 slides

The Milky Way

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3/24/14 Mass & Weight

3/24/14 Mass & Weight. Warm up questions: Periods 1 & 3 Would you weight more on Earth or on the Moon? What factors do you have to consider when figuring out your weight at these two locations?. 5. 3/24/14 Mass & Weight. Warm up question: Periods 5,6 & 7

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Suzy Collin-Zahn LUTH, Observatoire de Paris Meudon

AGN, MASSIVE BLACK HOLES, ACCRETION. OR. ARE AGN FACTORIES OF HIGH ENERGY PARTICLES AND PHOTONS?. Suzy Collin-Zahn LUTH, Observatoire de Paris Meudon. THE CONTEXT. STRONG AND WEAK ACCRETORS. DICHOTOMY RADIO LOUD / RADIO QUIET OBJECTS AND JETS / WINDS. CONCLUSION. THE CONTEXT.

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Galaxy Types

Galaxy Types. Hubble Tuning Fork. Elliptical. Elliptical. On the left of the diagram are the Elliptical galaxies Elliptical galaxies contain very little gas and dust, and the gas that is present is very hot and diffuse.

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Astro-2: History of the Universe

Astro-2: History of the Universe. Lecture 2; April 6 2006. Previously.. On Astro-2. The goal of cosmology is to understand how the universe formed and evolved. How can we build a theory of the universe valid at all times in every place?

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Stars & Galaxies in Motion

Stars & Galaxies in Motion. Wednesday, October 15 Next Planetarium Show: tonight, 6:30 pm. Newton Says:

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Galaxy Formation

Galaxy Formation. Formation of galaxies in cold dark matter universe. Hubble Galaxy Sequence. Ellipticals (round through oval) Spirals (centrally condensed with arms) Barred Spirals (distinct bar shape with bulge). Shapes of Galaxies. Spirals disk shaped with spiral arms

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Dark Matter

Dark Matter. Evidence for Dark Matter Dark Matter Candidates How to search for DM particles? Recent puzzling observations (PAMELA, ATIC, EGRET). Dark Matter. coma.

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Objectives: 1) To learn about Spirals 2) To learn about Barred Spirals

Goal: To know the different types of galaxies and to understand their differences and similarities. Objectives: 1) To learn about Spirals 2) To learn about Barred Spirals 3) To learn about Elliptical Galaxies 4) To learn about Irregular Galaxies. What type of galaxy is this?.

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tcapreview

tcapreview. by: Adrian Pettigrew. Spiral galaxies.

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Light Years, Important People, Galaxies

Light Years, Important People, Galaxies. 8 th Grade. WHAT IS A GALAXY?. A galaxy is a huge group of single stars , star systems, star clusters, dust , and gas held together by gravity. How big are galaxies?. The largest galaxies have more than a TRILLION stars.

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The Sun

The Sun. IV. The Sun. A. All life on Earth depends on the energy that comes from the star in the center of our solar system. B. Energy produced by the Sun is due to hydrogen atoms fusing together to produce helium atoms. C. The Sun is composed of 3 layers:

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Swift/BAT Hard X-ray Survey

Swift/BAT Hard X-ray Survey. 35'. Preliminary results in Markwardt et al 2005. energy coded color. BAT Instrument Parameters. Energy Range 14 - 195 keV Area 5200 cm 2 (x 50% open fraction) Field of View 2 Steradian, partially coded Background 10,000 ct/s (cosmic diffuse dominated)

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Radio continuum observations of the Sombrero galaxy NGC4594 (M104) and other edge-on spirals

Radio continuum observations of the Sombrero galaxy NGC4594 (M104) and other edge-on spirals. Marita Krause MPIfR, Bonn Michael Dumke ESO, Chile Richard Wielebinski MPIfR, Bonn. Outline

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Galaxies

Galaxies. 18 th century: Charles Messier accidentally discovered many galaxies while searching for comets. He noticed a large number of faint, diffuse patches of light. To avoid confusing them with comets, he assigned them numbers and made a catalog of their positions

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Galaxy Resarch Project

By Yulissa Mendez

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CONCLUSIONS:

The Cosmic Evolution Survey (COSMOS): galaxy morphologies and colors as a function of mass and environment at z=0.7

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