'Hubble constant' diaporamas de présentation

Chapter 18 Our Expanding Universe

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How Do You Make a Universe?

How Do You Make a Universe?. Geary Albright Saturday Morning Physics March 3, 2012. The history of the Universe can be summed up like this: Hydrogen is a light, odorless, colorless gas, that if given enough time, turns into people.

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Cosmology

Cosmology. Cosmology- the study of the origin, present, and future of the universe. http://www.damtp.cam.ac.uk/user/gr/public/bb_cosmo.html. Einstein and Gravity.

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Tools We Will Need on our Journey through the Universe

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03/000

Australian Government Geoscience Australia. Cosmologic astrometry. Yonsei University, Seoul 1 8 October 2010. 03/000. Geoscience Australia. 18 October 2010. The concept. ?. ?. B. B = 10000 km , ? = 0.03 cos? sec. Geoscience Australia. 18 October 2010.

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The Accelerating Universe

The Accelerating Universe. Megan Donahue Michigan State University. The Accelerating Universe. What is the evidence that the Universe is not only expanding, but accelerating? What is dark energy? What does an accelerating Universe imply?. Edwin Hubble (1889-1953).

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Chapter 26 Cosmology

Chapter 26 Cosmology. Units of Chapter 26. 26.1 The Universe on the Largest Scales 26.2 The Expanding Universe 26.3 The Fate of the Cosmos 26.4 The Geometry of Space Curved Space 26.5 Will the Universe Expand Forever? Einstein and the Cosmological Constant.

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Expansion of the Universe, Ch. 26, 52

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Physics 133: Extragalactic Astronomy and Cosmology

Physics 133: Extragalactic Astronomy and Cosmology. Lecture 9; February 10 2014. Previously:. Measuring kinematics of the universe determines cosmological parameters. Proper distance depends on redshift via the Hubble constant, to first order

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P 7 20 Questions

P 7 20 Questions. Traffic Light Quiz. Rules. Everyone should reveal their answer at the same time Count down: 3, 2, 1, show!. 1. The parallax angle of a star is. twice the angle moved against the background of distant stars in 6 months

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ASTR 1102-002 2008 Fall Semester

ASTR 1102-002 2008 Fall Semester. Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture21]. Chapter 24 : Galaxies and Chapter 26: Cosmology. Individual Galaxies. Location in Space Coordinate (angular) position on the sky Distance from Earth

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ASTR 1102-002 2008 Fall Semester

ASTR 1102-002 2008 Fall Semester. Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture21]. Chapter 24 : Galaxies and Chapter 26: Cosmology. Individual Galaxies. Location in Space Coordinate (angular) position on the sky Distance from Earth

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Dark Energy and the Hubble Constant

Dark Energy and the Hubble Constant. Jim Condon. What is dark energy (DE)? How does an accurate ( ? < 3%) local measurement of the Hubble constant H 0 plus CMB data constrain DE? How can astrometry determine H 0 ? Bonus: accurate SMBH masses The Megamaser Cosmology Project

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Expansion of the Universe

Expansion of the Universe. Alexandra Higareda DeMaris Wilson. Introduction. Albert Einstein's General Theory of Relativity "the greatest blunder of my life" Enter Hubble. Expansion of the Universe

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Measuring the Hubble Constant

Measuring the Hubble Constant. The Scale of the Universe I: The Solar System. Pluto is 5.913 billion km (39.53 AU) from the Sun. The Oort cloud extends much further than this: out to around 100,000 AU or about 2 ly . The next closest star, Alpha Centauri, is 4.2ly away. 1ly=9.46 x 10 12 km.

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The Curvature of Space

The Curvature of Space. The Isotropic and Homogeneous Universe. What does curved space look like?. The Expansion of the Universe. The Doppler Effect. Galaxy Spectra are Redshifted. Edwin Hubble (1889-1953). Hubble Diagram (1929). V = H r H ~ 500 km/s / Mpc (first measurement!).

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Optical Spectrum of a Galaxy

Optical Spectrum of a Galaxy. H a. Recession velocity = 14387 km / s z = 0.0479. Flux. H b. [O III]. Vesto Slipher. Redshifted Spectra. Edwin Hubble. The Original Hubble Law. Modern-Day Hubble Law. Today our best value for the Hubble constant is 70 +/- 5 km / s / Mpc.

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ABSTRACT:

Infrared Studies of Type Ia Supernovae. M. Verdugo O. (PUC), K. Krisciunas (CTIO/OCIW), N. B. Suntzeff (CTIO), M. M. Phillips (OCIW), P. Candia (CTIO). ABSTRACT:

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