Outline: Part II. The end of the dark ages. Structure formation. Merging cold dark matter halos. First stars z t Univ Myr.

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Outline: Part I Outline: Part II The end of the dark ages Dark ages First stars z 20 30 t Univ 100 200 Myr First

detect light sources up to z 11 Merging cold dark matter halos Structure formation Minihalos First stars (in

1 Outline: Part I Outline: Part II The end of the dark ages Dark ages First stars z t Univ Myr First galaxies z t Univ Myr Current observational limit: HST and 8 10 m telescopes on the ground can detect light sources up to z 11 Merging cold dark matter halos Structure formation Minihalos First stars (in minihalos) First galaxy Formation of a ~10 12 M solar dark matter halo Simulation runs from z 12 to 0 (t Univ 0.25 to 13.7 Gyr) 1

Population I, II and III Star formation in dark matter

the Milky Way disk Population II: Metal poor stars

Population III: (Almost) Metal free stars Example:

with gas inside The gas cools by radiating photons and

high redshifts Lack of efficient coolants Population

shaky) The first ones are expected in minihalos prior

Feedback Only a few stars (maybe just one) per minihalo

2 Population I, II and III Star formation in dark matter halos Population I: Metal rich stars Example: Stars in the Milky Way disk Population II: Metal poor stars Example: Stars in the Stellar halo of the Milky Way Population III: (Almost) Metal free stars Example: Stars forming in minihalos at z 20 Dark matter halo with gas inside The gas cools by radiating photons and contracts Star formation Problem: Low metallicity at high redshifts Lack of efficient coolants Population III stars These stars will be very massive, hot and short lived. Mass range Msolar (but predictions still shaky) The first ones are expected in minihalos prior to the formation of the first galaxies. Feedback Only a few stars (maybe just one) per minihalo Intermission: The first stars(?) Normal star hydrogen bomb Dark matter annihilation Dark matter Photon Annihilation Dark matter Neutrino Electron 2

Dark stars Dark star properties WIMP annihilation in centre of CDM

annihilation rather than hydrogen fusion Conventional Pop III stars

dark stars Teff 4000 50000 K Cooler! M 10 2 10 7 Msolar More massive?

?? Problem: Still no consensus on likely masses or life times of dark

The Sun The Sun Vanilla population III star Supermassive dark star

matter halo Star formation inside and outside the first galaxies Star

Object qualifies as a galaxy Simulation runs from z 40 to 11 (t Univ

3 Dark stars Dark star properties WIMP annihilation in centre of CDM halo Gas cools and falls into the centre Star fueled by WIMP annihilation rather than hydrogen fusion Conventional Pop III stars Teff K M Msolar Lifetime yr Pop III dark stars Teff K Cooler! M Msolar More massive??? Lifetime yr More long lived??? Problem: Still no consensus on likely masses or life times of dark stars The sizes of primordial stars I The sizes of primordial stars II The Sun The Sun Vanilla population III star Supermassive dark star Formation of the first galaxies Formation of a 10 7 M solar dark matter halo Star formation inside and outside the first galaxies Star formation in minihalos Minihalo mergers and further star formation Object qualifies as a galaxy Simulation runs from z 40 to 11 (t Univ 65 to 430 Myr) z 23 t Univ 145 Myr z 18 t Univ 215 Myr z 11 t Univ 430 Myr Greif et al. 08 Gas density shapshots Greif et al. 08 3

4 A galaxy is born (at z 10) Reionization Intergalactic medium Ionized Neutral CMBR (Planck) z reion 8 Ly absorption in quasars z reion >6 Reionized Greif et al. 08 What caused reionization? Intermission: Name the telescope! Population III stars in minihalos? High redshift galaxies? Accreting black holes? Decay of exotic particles? Popular scenario Intermission: Name the telescope! Intermission: Name the telescope! 4

How to find and study highredshift galaxies

observations The Hubble Extreme Deep Field

seconds) Cluster lensing observations 2.

Example of one of the most distant galaxy

5 How to find and study highredshift galaxies Imaging strategies Deep field style observations The Hubble Extreme Deep Field Total exposure time: 23 days (2 million seconds) Cluster lensing observations 2.3 arcmin 2 arcmin The Hubble Extreme Deep Field Example of one of the most distant galaxy candidates so far 2.4 arcsec x 2.4 arcsec Bouwens et al. (2010) z 10 candidate Cluster lensing I Cluster lensing II Log 10 magnification Galaxy cluster at z 0.5 Magnification map 5

Pros and Cons of Cluster Lensing Magnification µ = 10 Intermission: Why are redshift records important?

Bottom line: Lensed survey fields can be superior for sources that are very faint, not too rare and not too highly clustered

Emission lines No emission lines Young galaxy Old galaxy The UV/optical spectra of galaxies Absorbed by the neutral interstellar

6 Pros and Cons of Cluster Lensing Magnification µ = 10 Intermission: Why are redshift records important? Observer µ = 1 Galaxy cluster + Background sources appear brighter by a factor µ The volume probed becomes smaller by a factor µ Bottom line: Lensed survey fields can be superior for sources that are very faint, not too rare and not too highly clustered Selecting high z galaxy candidates Two techniques: Dropout selection Lyman alpha surveys The UV/optical spectra of galaxies I Emission lines No emission lines Young galaxy Old galaxy The UV/optical spectra of galaxies Absorbed by the neutral interstellar medium within the galaxy Lyman break (912 Å) Lyman H Drop out techniques: Lyman Break Galaxies z=0 912 Å Lyman break UB V z>2.5 B V normal U: extremely faint U B V 6

Drop out techniques: Lyman Break Galaxies Reionization epoch galaxies At even higher z, neutral gas in the IGM start to absorb everything shortward of

5) Intermission: Which of these drop out candidates is likely to have the highest redshift?

images (covering continuum and line) required for survey of redshift range (z0.

7 Drop out techniques: Lyman Break Galaxies Reionization epoch galaxies At even higher z, neutral gas in the IGM start to absorb everything shortward of Ly (rest =1216 Å) Lyman H U B V Drop out techniques: z>6 objects Eventually, the break shifts into the near IR. Example: z band dropout (z 6.5) Intermission: Which of these drop out candidates is likely to have the highest redshift? A B z Y J H C z Y J H D Optical Near IR z Y J H z Y J H Lyman alpha surveys Potentially the brightest line in rest frame UV/optical Two narrowband images (covering continuum and line) required for survey of redshift range (z0.1) Sharp drop (absorption in neutral IGM) Lyman line Narrowband filter profiles Problem I: Lyman notoriously difficult to predict Ly Ly resonant line random walk through neutral interstellar medium Many Ly photons destroyed by dust before emerging Ly flux ranges from low to very high Lyman at z=7 7

Problem II: Lyman largely absorbed in the neutral intergalactic medium at z>6 Photometric redshifts Fraction of Ly photons reaching the observer Hayes et al.

template spectrum (good match) New telescope for high z studies: ALMA Atacama Large Millimeter/ submillimeter Array (ALMA): An array of seventy 12 m antennas operating @ 200

continuum flux drops slowly with z (if no source evolution).

8 Problem II: Lyman largely absorbed in the neutral intergalactic medium at z>6 Photometric redshifts Fraction of Ly photons reaching the observer Hayes et al. 11 Abrupt drop Ly not good way to find z>6 galaxies (but may be good way to probe reionization) z=0 template spectrum (bad match) Measured photometrical data points Redshifted template spectrum (good match) New telescope for high z studies: ALMA Atacama Large Millimeter/ submillimeter Array (ALMA): An array of seventy 12 m antennas m (sub mm) Can be used to search for dust emission and emission lines like 158 mand m (rest frame) from z>6 galaxies ALMA receivers De Breuck 05 Dust continuum flux drops slowly with z (if no source evolution). Future prospects: JWST James Webb Space Telescope The first light machine To be launched by NASA / ESA / CSA in m mirror m Useful for: Galaxies up to z 15 Pop III supernovae Why infrared? Optical z = 1 JWST NIRCam wavelength range z = 6 z = 10 Zackrisson et al. (2001) model 8

9 Future prospects: E ELT 39 m European Extremely Large Telescope (E ELT) estimated to be completed in

The First Galaxies. Erik Zackrisson. Department of Astronomy Stockholm University

The First Galaxies. Erik Zackrisson. Department of Astronomy Stockholm University The First Galaxies Erik Zackrisson Department of Astronomy Stockholm University Outline The first galaxies what, when, why? What s so special about them? Why are they important for cosmology? How can we