ifu observations of the high-z universe constraints on feedback from deep field observations with...
TRANSCRIPT
![Page 1: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/1.jpg)
IFU observations of the high-z UniverseConstraints on feedback from deep field observations with
SAURON and VIMOS
Joris Gerssen
![Page 2: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/2.jpg)
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.
![Page 3: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/3.jpg)
• 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
![Page 4: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/4.jpg)
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:
![Page 5: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/5.jpg)
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
– ...
![Page 6: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/6.jpg)
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)
![Page 7: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/7.jpg)
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)
![Page 8: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/8.jpg)
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
![Page 9: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/9.jpg)
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
![Page 10: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/10.jpg)
SSA22a
SAURON observations: overview
SSA22b HB89 1738+350
![Page 11: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/11.jpg)
SSA22b (z = 3.09) Wilman, Gerssen, Bower, Morris, Bacon, de Zeeuw & Davies (Nature, 14 July 2005)
VolView rendering
![Page 12: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/12.jpg)
Ly- distribution
1.0 arcsec = 7.6 kpc
![Page 13: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/13.jpg)
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
![Page 14: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/14.jpg)
Model cartoon
![Page 15: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/15.jpg)
SSA22b results
• Assuming shock velocities of several 100 km/s
• Shell travels ~100 kpc in a few 108yr• Shell can cool to ~104 K in this time
– Implied by the Voigt profile b parameter– Required to be in photoionization equilibrium
• Implied shell mass of 1011 M
• Kinetic energy of the shell ~1058 erg• About 1060 erg available (IMF)• Superwind model provides a consistent, and
energetically feasible description
![Page 16: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/16.jpg)
![Page 17: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/17.jpg)
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)
![Page 18: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/18.jpg)
SINFONI observations of SSA22b
Foerster Schreiber et al.
Constrain the stellar properties
Link them to the superwind
Scheduled for P77 (B)
![Page 19: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/19.jpg)
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
![Page 20: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/20.jpg)
Mean IGM transmission
Adelberger et al. 2003
Adelberger et al. 2005
z ~ 3 z ~ 2.5
![Page 21: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/21.jpg)
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
![Page 22: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/22.jpg)
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
![Page 23: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/23.jpg)
VIMOS 'QSO2'
z = 3.92, Texp = 9 hoursLR mode
![Page 24: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/24.jpg)
Search by eye for candidatesNeed to identify/apply an automated procedure
![Page 25: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/25.jpg)
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)
![Page 26: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/26.jpg)
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
![Page 27: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/27.jpg)
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)
![Page 28: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/28.jpg)
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
![Page 29: IFU observations of the high-z Universe Constraints on feedback from deep field observations with SAURON and VIMOS Joris Gerssen](https://reader034.vdocuments.us/reader034/viewer/2022051517/56649ea75503460f94ba9771/html5/thumbnails/29.jpg)
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