'Distance modulus' presentation slideshows

Parallax

1.17k views • 81 slides

Stellar Properties Distance trig parallax d(pc) = 1/p (arcsec)

Stellar Properties Distance trig parallax d(pc) = 1/p (arcsec) Velocity (V space ) 2 = (V rad ) 2 + (V tan ) 2 Brightness mag = -2.5 log (flux) + constant; L Temperature B-V; spectral class Mass spectroscopic binary; K, P, i Radius eclipsing spectroscopic binary.

865 views • 63 slides

Galactic Structure and Dynamics

390 views • 39 slides

Galactic Structure and Dynamics

414 views • 39 slides

5. Stellar populations 6. Galactic (open) clusters

5. Stellar populations 6. Galactic (open) clusters. The Pleiades open cluster. Stellar populations The concept of stellar populations was introduced by Walter Baade (German-American astronomer in California) in 1944 from observations of the spiral galaxy M31 in Andromeda.

307 views • 30 slides

Vela X-1: Flares & Off States

460 views • 25 slides

The HR Diagram

The HR Diagram. Astronomy 315 Professor Lee Carkner Lecture 8. Flux and Luminosity. How bright a star looks (W/m 2 ) How bright the star is (W) We measure the flux, but we want to know the luminosity. Inverse Square Law. What determines how bright a star looks?

480 views • 24 slides

Various Techniques for Measuring Astronomical Distances

Various Techniques for Measuring Astronomical Distances. Alex Blanton. Introduction. A very common tool for knowing the distance to a star is the distance modulus. Through knowing of the Galaxies motion, a celestial body can be determined by calculating its galactic position.

410 views • 23 slides

1B11 Foundations of Astronomy Cosmic distance scale

1B11 Foundations of Astronomy Cosmic distance scale. Liz Puchnarewicz emp@mssl.ucl.ac.uk www.ucl.ac.uk/webct www.mssl.ucl.ac.uk/. 1B11 Cosmic distance scale. Why is it so important to establish a cosmic distance scale?

410 views • 21 slides

Constraining Accelerating Cosmologies with Distance Measures

327 views • 21 slides

Meaning of deceleration parameter

Meaning of deceleration parameter. q 0 tells you if the Universe is accelerating in its global expansion rate, or decelerating. Flat, matter dominated q0=1/2 Empty Universe q0=0 Flat, radiation dominated q0=1 Flat, Cosmological Constant dominated q0=-1. flat model.

242 views • 21 slides

Class 4 : Basic properties of stars

354 views • 20 slides

S . Nesseris Department of Physics University of Ioannina

Constraints on Dark Energy Models from the Legacy and Gold SnIa Datasets. S . Nesseris Department of Physics University of Ioannina. Main points of talk. Accelerating Expansion of the Universe and the SN Ia

331 views • 20 slides

The sdss galaxies at redshift 0.1

The sdss galaxies at redshift 0.1. What can we learn from the luminosity function a nd color studies?. OUTline. Scientific Questions SDSS Basic Information My Data Set Methods of Analysis Introduction to theory Practically how is it performed? Results and Conclusions.

266 views • 18 slides

East Asia VLBI Workshop (Seoul, 2009 Mar 18-20) Kurayama, Tomoharu (KVN/KASI) *1

Period-Luminosity Relation of Mira-Variables Revealed from VLBI --- Parallax Measurement Results around 500-Day Period with VLBA. East Asia VLBI Workshop (Seoul, 2009 Mar 18-20) Kurayama, Tomoharu (KVN/KASI) *1 Matsui, Makoto (Kagoshima Univ.) *1 Kagoshima Univ. from 2009 April.

283 views • 16 slides

The RR Lyrae of w Centauri: a theoretical route (progress report)

229 views • 16 slides

Constraining Dark Energy from SNIa CMB BAO Observations

Constraining Dark Energy from SNIa CMB BAO Observations. Chien-Wen Chen. Distance Measures. Comoving distance Luminosity distance Angular diameter distance Comoving volume. http://www.astro.ufl.edu/~guzman/ast7939/projects/project01.html.

228 views • 8 slides