Gravitational Lensing

Slides:



Advertisements
Similar presentations
The Formation of Galactic Disks By H. J. Mo, Shude Mao and Simon D. M. White (1998) Presented by Mike Berry.
Advertisements

1 st Doha International Astronomy Conference, Feb 2013 Complying with Tully–Fisher Y Sobouti Institute for Advanced Studies in Basic Sciences – Zanjan.
Introduction to Astrophysics Lecture 14: Galaxies NGC1232.
Week 10 Dark Matter Reading: Dark Matter: 16.1, 16.5d (4 pages)
By: Avishai Dekel and Joseph Silk Presented By: Luke Hovey.
DARK MATTER IN GALAXIES
When Galaxies Collide. It is not uncommon for galaxies to gravitationally interact with each other, and even collide!
Session: MGAT9 – Self-Gravitating Systems SPHERICALLY SYMMETRIC RELATIVISTIC STELLAR CLUSTERS WITH ANISOTROPIC MOMENTUM DISTRIBUTION Marco MERAFINA Department.
Clusters & Super Clusters Large Scale Structure Chapter 22.
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2.
The Distribution of DM in Galaxies Paolo Salucci (SISSA) TeVPa Paris,2010.
Stellar Kinematics Astronomy 315 Professor Lee Carkner Lecture 17.
1 Announcements Reading for next class: Chapters 22.6, 23 Cosmos Assignment 4, Due Wednesday, April 21, Angel Quiz Monday, April 26 Quiz 3 & Review, chapters.
Chapter 23: Our Galaxy Our location in the galaxy Structure of the galaxy Dark matter Spiral arm formation Our own supermassive black hole.
First Results from an HST/ACS Snapshot Survey of Intermediate Redshift, Intermediate X-ray Luminosity Clusters of Galaxies: Early Type Galaxies and Weak.
Constraining Galactic Halos with the SZ-effect
Chapter 14: The Milky Way Galaxy The scenario for the formation of galaxies is very reminiscent of the formation process for solar systems. Giant cloud.
9B The Milky Way Our Galactic Home. 9B 9B Goals Structure of our Galaxy. Its size and shape. How do stars and things move through it? Mass and Dark Matter.
Galaxies Chapter Twenty-Six. Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to.
A1143 Quiz 4 Distribution of Grades: No Curve. Milky Way: Bright Band Across Sky (Resolved by Galileo)
Christopher | Vlad | David | Nino SUPERMASSIVE BLACK HOLES.
Survey Science Group Workshop 박명구, 한두환 ( 경북대 )
1 Gravitational lensing and neutrinos Why not look where natural lenses exist? Proposal of an additional candidate list in point source search: 1. Motivation.
Chapter 15 Galaxies What do you think? Do galaxies all have spiral arms? Are most of the stars in a spiral galaxy in its arms? Are galaxies isolated.
Galaxy Characteristics Surface Brightness Alternative to Luminosity I(R) = Flux/area = erg/s/cm 2 /arcsec 2 I(0) – center flux I(R) = at radius R Define.
Weak Lensing 3 Tom Kitching. Introduction Scope of the lecture Power Spectra of weak lensing Statistics.
Copyright © 2010 Pearson Education, Inc. Galaxies Unit 10.
Feedback & Large Surveys Harry Ferguson (STScI). Feedback Behroozi Halo quenching Quasar mode AGN Radio Mode AGN (SNe) SNe Satellites: Ram pressure,
Σπειροειδείς γαλαξίες
The differential Tully-Fisher relation for spiral galaxies Irina Yegorova SISSA, Trieste, Italy.
The formation of galactic disks An overview of Mo Mao & White 1998 MNRAS
Unit 6 Galaxies *Basic Galaxy Info. *Types of Galaxies -Characteristics of The Milky Way (Spiral Galaxies) *Red Shift & Hubble’s Law.
Chapter 25 Galaxies and Dark Matter Dark Matter in the Universe We use the rotation speeds of galaxies to measure their mass:
Lecture 18 : Weighing the Universe, and the need for dark matter Recap – Constraints on the baryon density parameter  B The importance of measuring the.
Possible Evidence of Thermodynamic Activity in Dark Matter Haloes.
Correlations of Mass Distributions between Dark Matter and Visible Matter Yuriy Mishchenko and Chueng-Ryong Ji NC State University Raleigh, NC KIAS-APCTP-DMRC.
How did the universe begin?. How do we know? Doppler Shift Lower pitched, longer wavelength Higher pitched, shorter wavelength.
Cosmic shear and intrinsic alignments Rachel Mandelbaum April 2, 2007 Collaborators: Christopher Hirata (IAS), Mustapha Ishak (UT Dallas), Uros Seljak.
Rotation curves and spiral arms in galaxies - observations and theory
The dark side of the Universe: dark energy and dark matter Harutyun Khachatryan Center for Cosmology and Astrophysics.
Galactic structure and star counts Du cuihua BATC meeting, NAOC.
Title Galaxy Structure and Dark Matter Michael Merrifield University of Nottingham.
Copyright © 2010 Pearson Education, Inc. Chapter 14 The Milky Way Galaxy Lecture Outline.
Copyright © 2010 Pearson Education, Inc. Chapter 16 Galaxies and Dark Matter Lecture Outline.
Universe Tenth Edition Chapter 23 Galaxies Roger Freedman Robert Geller William Kaufmann III.
Astronomy 1020 Stellar Astronomy Spring_2016 Day-38.
Bayesian analysis of joint strong gravitational lensing and dynamic galactic mass in SLACS: evidence of line-of-sight contamination Antonio C. C. Guimarães.
© 2017 Pearson Education, Inc.
How fast would a galaxy 2,000 megaparsecs away be moving with respect to us, according to Hubble’s Law? Hint: H0 = 70 km/s/Mpc 1,400 km/s 14,000 km/s 140,000.
WEIGHING THE UNIVERSE Neta A. Bahcall Princeton University.
ASTR 1020 – April 11 . Final Problem Set Due Today
Lecture 18 : Weighing the Universe, and the need for dark matter
Speaker: Bingxiao Xu Peking University
SMP: Supermassive Black Holes Faber-Jackson vs. Tully-Fisher
Scaling laws for dark halos of galaxies
PHYS 1443 – Section 003 Lecture #15
AY202a Galaxies & Dynamics Lecture 3: Galaxy Characteristics
The Milky Way Our Galactic Home.
Chapter 14 Spiral Galaxy.
Galaxies.
Spring 2002 Lecture #15 Dr. Jaehoon Yu Mid-term Results
The scenario for the formation of galaxies is very reminiscent of the formation process for solar systems. Giant cloud of gas and dust, shrinks under its.
Surface Brightness Profile - NGC 3379 (giant elliptical)
Strong lensing constraints on modified gravity models
Dark matter and anomalous gas in the spiral galaxy NGC 4559
“Violent Relaxation” of Star Cluster
Galaxies.
Potential - density pairs
The scenario for the formation of galaxies is very reminiscent of the formation process for solar systems. Giant cloud of gas and dust, shrinks under its.
PHYS 1443 – Section 003 Lecture #15
Presentation transcript:

Gravitational Lensing ASTC22. Lectures L21 Gravitational Lensing SMP on Lensing (continued L20:) Are these two empirical laws similar? The same? Isothermal spheres Isothermal distribution functions Isothermal singular sphere Isothermal non-singular sphere Conclusions for the magnitude of dynamical friction in dark halos: the reason for efficient mergers Rotation and flattening of elliptical galaxies: only a weak connection

Tully-Fisher relationship, a correlation between the luminosity and rotation for disk galaxies Log Vc -2.5 log L

Faber-Jackson relationship: Luminosity ~ sigma^4 applies to ellipticals Tully-Fisher relationship Luminosity ~ (Vc)^3.85 applies to disk galaxies but the two are almost identical: both the disks and the ellipticals are immersed in the same type of dark halos which determines the maximum Vc via potential well depth.

(sorry, that’s my teenage daughter)

Good for modeling flat-Vc galaxies in dark halos

...so this is one major reason why mergers of galactic systems are so rapid (a few to a few dozen periods)

One more empirical correlation: between rotation and flattening of ellipticals, which can be understood based on stellar dynamics Fastest rotation according to theory But remember: theory gives the upper envelope only. Most ellipticals are NOT supported or flattened by rotation. They simply are not relaxed; flattening comes from initial conditions, including geometry of encounter.