1. IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen

2. Overview Until a decade ago only extreme objects were known in the distant universe Since then photometric redshift surveys and narrow band surveys identified ( at z ~2 to ~4) –Lyman Break Galaxies –Ly-alpha galaxies Observational constraints on galaxy formation and evolution –e.g. morphology, star formation history, luminosty functions, etc.

3. Among the drivers behind this advancement are –The 10m class telescopes and instruments –Hubble Space Telescope –Theoretical understanding of structure formation Integral Field Spectropscopy (IFS) is a recent development with great potential to further galaxy evolution studies

4. Integral Field Spectroscopy Data cube: f(x, y, lambda) - VIMOS - SINFONI - MUSE - SAURON - PMAS - … Field-of-View few (tens) of arcsec Spectral resolution: R ~200 to ~2500 Typical properties:

5. High-redshift science with IFUs (e.g. list of MUSE science drivers) Formation and evolution of galaxies: –High-z Ly-  emitters –Feedback –Luminosity functions (PPAK, VIRUS) –Reionization –...

6. Feedback A longstanding problem in galaxy formation is to understand how gas cools to form galaxies Discrepancy between observed baryon fraction (~8%) and predicted fraction (> 50% ) To solve this “cosmic cooling crisis” the cooling of gas needs to be balanced by the injection of energy (SNe/AGN)

7. Feedback Galactic outflows driven by AGN and/or SNe –Resolve discrepancy between observed and predicted baryon fraction –Terminate star formation –Enrich IGM NGC 6240 (ULIRG) M82 (starburst)

8. IFU Deep Field Observations Deep SAURON & VIMOS observations of blank sky But in practice centered on QSOs/high-z galaxies –observe extended Ly-  halo emission –serendipitous detections

9. SAURON Deep Fields The SAURON IFU is optimized for the study of internal kinematics in early type galaxies DF observations of: SSA22a, SSA22b, HB89 Redshift range 2.9 - 3.3 (4900 - 5400 Angstrom) Texp ~10 hours FoV: 33 x 41 arcsec, R ~ 1500

10. SSA22a SAURON observations: overview SSA22b HB89 1738+350

11. SSA22b (z = 3.09) Wilman, Gerssen, Bower, Morris, Bacon, de Zeeuw & Davies (Nature, 14 July 2005) VolView rendering

12. Ly-  distribution 1.0 arcsec = 7.6 kpc

13. Line profiles Emission lines ~ 1000 km/s wide Emission peaks shift by a few 100 km/s Absorption minima differ by at most a few tens of km/s Ly alpha is resonant scattered, naturally double peaked Yet, absorption by neutral gas is a more straighforward explanation

14. Model cartoon

15. SSA22b results Assuming shock velocities of several 100 km/s Shell travels ~100 kpc in a few 10 8 yr Shell can cool to ~10 4 K in this time – Implied by the Voigt profile b parameter – Required to be in photoionization equilibrium Implied shell mass of 10 11 M  Kinetic energy of the shell ~10 58 erg About 10 60 erg available (IMF) Superwind model provides a consistent, and energetically feasible description

17. Comparison with SSA22a SSA22a –Kinematical structure more irregular –Luminous sub-mm source Suggests that a similar outflow may have just begun Probe a wider range of galaxies: –SCUBA galaxy (observed last year) –Radio galaxy (observed one last week) –LBG (a few hours last week)

18. SINFONI observations of SSA22b Foerster Schreiber et al. Constrain the stellar properties Link them to the superwind Scheduled for P77 (B)

19. Serendipitous emitters The correlation of Ly-alpha emitters with the distribution of intergalactic gas provides another route to observationally constrain feedback Based on Adelberger et al (2003) who find that the mean transmission increases close to a QSO –This result is derived from 3 Ly-  sources only

20. Mean IGM transmission Adelberger et al. 2003 Adelberger et al. 2005 z ~ 3 z ~ 2.5

21. Advantage of IFUs IFUs cover a smaller FOV then narrow band imaging, but –IFUs are better matched to Ly-alpha line width –Do not require spectroscopic follow-up –Directly probe the volume around a central QSO Thus, IFUs should be more efficient than narrow band surveys

22. IFU observations Search the data cube for emitters Use the QSO spectrum to measure the gas distribution –Likely require the UVES spectra Available: –One SAURON data cube –2 of 4 VIMOS IFU data cubes SAURON example: HB89 +1738+350

23. VIMOS 'QSO2' z = 3.92, Texp = 9 hours LR mode

24. Search by eye for candidates Need to identify/apply an automated procedure

25. Detection algorithms Matched kernel search –Many false detections IDL algorithm (van Breukelen & Jarvis 2005) FLEX: X-ray based technique (Braito et al. 2005) ELISE-3D: sextractor based (Foucaud 2005)

26. van Breukelen & Jarvis (MNRAS 2005) Similar data set: –Radio galaxy at z = 2.9 –same instrumental set up –similar exposure time Yet, they find more (14) and brighter Ly-  emitters –Using an automated source finder

27. In progress A direct comparison with the van Breukelen results –Obtained their data from ESO archive –And reduced and analyzed it with our procedures Preliminary results are in reasonably good agreement –‘Our’ data appears somwhat more noisy –Find their emitters and their new type-II quasar (Jarvis et al 2005)

28. Preliminary results Number density of Ly alpha emitters agrees with model predictions (fortuitous) –The VIMOS fields contain 5 - 14 emitters –Models (Deliou 2005) predict 9 in a similar volume IFUs are sensitive to at least a few 10E-18 erg/s/cm2

29. Summary IFUs provide a uniquely powerful way to study the haloes around high redshift proto-galaxies Volumetric data are an efficient way to search for Ly-alpha galaxies –An alternative method to constrain feedback IFUs are a very valuable new tool to study the formation and evolution of galaxies