1. Introduction to the modern observational cosmology 03.03.2011 Introduction/Overview

2. Observational cosmology: what can we observe? Electromagnetic waves  Radio, submillimeter, IR, optical, UV, X, gamma Particles  Neutrinos, cosmic rays Gravitational waves?.....

3. Observational cosmology: where can we observe? From Earth (radio & optical: almost everywhere; close IR, sub-mm: some high places like Atakama desert)‏ From satellites (microwaves, IR, UV, X, gamma)‏

4. Observational cosmology: what kind of objects do we observe? galaxies  individual  surveys Clusters of galaxies CMBR IGM AGNs Lensing effects Transient phenomena:  GRBs  SNIa

5. Cosmic Microwave Background Radiation Temperature maps Polarisation maps 5-year WMAP data Measurements:  Temperature fluctuations (2.7 K +/- 10^(-5))‏  Power spectrum  Photon polarization

6. Galaxies: individual Many types of galaxies in a local and distant Universe Investigating individual galaxies we can understand their evolution, the relation between their properties and their position in the LSS and so on

7. Galaxies: individual An example of a “cosmologically interesting” local galaxy: NGC 1705 Low-metallicity local irregular dwarf galaxy with a recent outburst of star formation: a model of the first galaxies?

8. Galaxies: surveys Angular (only positions on the sky)‏ 3-dimensional (with a redshift measurement) Different wavelengths Sky looks differently in different wavelengths + identification problems

9. Galaxies: local surveys In optical: local: 2dFGRS: spectra for 245 591 objects (mainly galaxies) in 1500 square degrees

10. Galaxies: local surveys In optical: local: SDSS 230 million celestial objects detected in 8,400 square degrees of imaging and spectra of 930,000 galaxies, 120,000 quasars, and 225,000 stars.

11. Galaxies: local surveys In total, the local Universe in ~2 billion light year radius is pretty well known in the optical light More than 1M galaxies LSS “special” objects (quasars, satellites of Milky Way)‏

12. Galaxies: deep imaging surveys CFHTLS:

13. Galaxies: deep imaging surveys Hubble Ultra Deep Field: 10 000 galaxies in 11 square arc minutes

14. Galaxies: deep redshift surveys DEEP2, VVDS, zCOSMOS In total ~a few tens of thousands of galaxies at z>0.5

15. Galaxies: next generation of deep redshift surveys VIPERS >100 000 galaxies at z~1 at 24 square degrees Statistical counterpart of SDSS or 2dF but at z~1 Volume (comoving) ~ 5 x 10 7 h -3 Mpc 3

16. Galaxies: dedicated surveys to search for particular objects If we want to increase the chance that our survey contains “interesting” (e.g. EROs) objects, we make a preselection, most often based on color-color diagrams

17. Galaxies: surveys in other wavelengths (IR)‏ IR: IRAS, 2MASS, Spitzer, AKARI... 350 000 objects, many of them still not identified! Low resolution: 30”-2'

18. Galaxies: surveys in other wavelengths (UV)‏ GALEX: all-sky map in FUV and NUV Unlike in IR, almost every UV source has an optical counterpart Also a poor resolution (Credit: Mark Seibert, OCIW)‏

19. Surveys: basic tools For all the objects:  Redshifts: how to measure and recognize  Colors/morphological types/sizes  Luminosities: apparent and absolute  Stellar masses... Statistics:  Number/magnitude counts (how many objects brighter than...)  Luminosity function  Angular/spatial distribution  Correlation function(s) ...

20. Clusters of galaxies The largest gravitationally bound structures in the Universe Their distribution is “the closest” to the primordial matter distribution Observed in X-rays, because they are filled with hot intergalactic gas (10 – 100 mln K)‏ Often with a massive central elliptical galaxy

21. Virgo: the closest massive cluster of galaxies in optical light and X-rays (1 Mpc)‏ Credit: Ray White, University of AlabamaRay White

22. Intergalactic medium Diffuse intergalactic gas in clusters (in some cases of a mass ~ mass of stars in galaxies)‏ Between clusters: Ly-alpha absorption systems A powerful tool to study  Metal production and feedback processes in the history of galaxy formation  Thermal and ionization history of the Universe during and after the epoch of reionisation

23. Lensing An effect of the change of the direction of photons in the gravitational field, due to the bending of the spacetime (relativistic effect)  Strong (multiple images of the same object, typically a quasar or an “Einstein ring”)‏  Weak (distorted images of objects e.g. behind a rich cluster)‏  Microlensing (change of luminosity, in case of lensing on small objects like planets or small stars)‏ Gravitational lensing is used to “map” mass distribution in galaxy clusters

24. Cosmological lensing: An example of lensing on a rich galaxy cluster – fragments of Einstein rings, distorted images...

25. Transient sources: SN Ia Thought to be white dwarfs from binary systems which collected too much matter from a companion through accretion processes and exceeded the Chandrasekhar mass All ~ of the same mass -> the same absolute luminosity -> standard candles Visible until z~1.3-1.4 Supernova Cosmology Project, Supernova Legacy Survey (SNLS)‏

26. Transient sources: SN Ia Hubble diagram from SN Ia led to “rediscovery” of the cosmological constant

27. Transient sources: GRBs Short (from a few ms to several minutes) and very energetic events, occurring ~ 1/day in the sky In 1997 connected with an optical outburst in a distant galaxy and thus finally proved to be of an extragalactic origin