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Lyman Break Galaxies as Markers for Large Scale Structure at z=5. Elizabeth Stanway University of Bristol With Malcolm Bremer, Luke Davies, Matt Lehnert, Mark Birkinshaw, Chris Carilli, Alain Omont. The ESO Remote Galaxy Survey. Targets the 10 EDisCS Survey cluster fields (VRIJK) - PowerPoint PPT Presentation
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Elizabeth Stanway - Obergurgl, December 2009
Lyman Break Galaxies as Markers for Large Scale
Structure at z=5
Elizabeth StanwayUniversity of Bristol
With Malcolm Bremer, Luke Davies, Matt Lehnert, Mark Birkinshaw, Chris Carilli, Alain Omont
Elizabeth Stanway - Obergurgl, December 2009
The ESO Remote Galaxy Survey
VRI image of CL1037-1243
• Targets the 10 EDisCS Survey cluster fields (VRIJK)
• Adds Z band imaging and 100hrs of spectroscopy
• Also Spitzer/IRAC photometry
• 20 VLT/FORS2 Slitmasks
• Targets R-drops with R-I>1.3, IAB<26.3, z~5
• R~660, ~6500-10000Å
(Douglas et al, 2009, 2010)
Elizabeth Stanway - Obergurgl, December 2009
• Better than 80% spectroscopic completeness for dropout candidates
• Reasonable S/N on continuum
• 68 Confirmed Redshifts at 4.4<z<6.4 including:
• 35 Lyman- emission lines
• 33 redshifts determined from Lyman breaks (18 class A, 13 B)
The ESO Remote Galaxy Survey
Elizabeth Stanway - Obergurgl, December 2009
Tip of an Iceberg?
• These structures may extend beyond the limits of the imaging fields
• One of the fields shows evidence for spatial as well as redshift clustering
• Redshift precision is better than 0.002
• The redshift spikes are not in skyline-free wavelength regions
500 kpc
Examples of Lyman Break galaxy spectra in the z=5.00 field
Overdensities at z=5.00 and z=5.15
Elizabeth Stanway - Obergurgl, December 2009
Moving to Longer Wavelengths
High Redshift Galaxies at Millimetre Wavelengths
• At z=5, 850m is close to the dust emission peak (i.e. negative K-correction starting to break down in sub-mm)
• Molecular gas is traced at all redshifts by CO emission
• The fundamental rotational transition of CO is at 115.271 GHz
• CO(1-0) at z=5 is in the 12mm/K band
• CO(2-1) emission at z=5 and CO(3-2) at z=8 are both in the 7mm/Ka band
• CO(5-2) emission at z=5 is in the 3mm band
Also - [CII] is a promising emission line, particularly in low metallicity systems, and can be observed in the 1mm band at z=5-6
Elizabeth Stanway - Obergurgl, December 2009
Cool Gas at High Redshift
• Pilot test– Single pointing at
ATCA– 24 hours at 12mm– 44 hours at 7mm– Bandwidth
z~0.03 (240 MHz)
•Limiting Sensitivity– 0.11 mJy/Beam at 12mm, 0.10 mJy/Beam at 7mm (in 30 km/s)
•Angular Resolution–16x10’’ at 12mm, 7x5’’ at 7mm
Elizabeth Stanway - Obergurgl, December 2009
Cool Gas at High Redshift
(Stanway et al, 2008)
Elizabeth Stanway - Obergurgl, December 2009
Cool Gas at High Redshift
• No detection from LBGs in field
=> MH2<2x109 Msun
BUT• Strong line emission
from optically-faint source at 37.64GHz
• Likely CO(2-1) at z=5.1245±0.0001
MH2=2x1010 Msun
Elizabeth Stanway - Obergurgl, December 2009
Confirming the Line
• Reobserved at the NRAO Green Bank Telescope in May 2009
• Observations shallower than planned
• Source redetected at 3
• Flux and velocity width consistent with ATCA values
Elizabeth Stanway - Obergurgl, December 2009
LABOCA Observations
• APEX/Laboca Observations• 11hrs, June-July 2009, Image r.m.s. = 2.8 mJy• No significant detections of CO Emitter source• No detections of LBGs in field
Intensity Coverage
5 arcmin
Elizabeth Stanway - Obergurgl, December 2009
Dust Limits on Cluster LBGs
• Laboca image covers 4x4 arcmin2 at 90% depth
• Can obtain a limit on the dust mass for spectroscopically confirmed z=5 Galaxies in this field
• Mstars ~ few x 109 M
in these sources
• MH2 < few x 109 M
(2), based on CO line non-detection
• Mdust < few x 108 M
(2 limit) at reasonable temperatures
Elizabeth Stanway - Obergurgl, December 2009
Dust Limits on the CO Source
• Mdust < 5 x 108 M
(2 limit) at 30K from LABOCA
• Mdust < 2 x 108 M
(2 limit) at 30K from MAMBO
• 1.2mm and 850m limits consistent except at high temperatures (T≈100K)
Mgas/Mdust > 100
Elizabeth Stanway - Obergurgl, December 2009
MAMBO Observations
• IRAM 30m MAMBO Observations in April 2009 (4hr)
• S1mm = -0.278 ± 0.438 mJy
• Implies L’CO/LFIR ratio more akin to lower redshift star-forming galaxies than ULIRGs/SMGs/QSO hosts
Figures modified from Solomon & vanden Bout (2005)
Elizabeth Stanway - Obergurgl, December 2009
Constraints on the SED
• SED rules out gas-to-dust ratios typically seen in ULIRGs and QSO hosts at high z.
• More like local star-forming galaxies - Normal not exceptional SF galaxy.
• ALMA will be able to do this work trivially
Elizabeth Stanway - Obergurgl, December 2009
Constraints on the SED
• SED rules out gas-to-dust ratios typically seen in ULIRGs and QSO hosts at high z.
• More like local star-forming galaxies - Normal not exceptional SF galaxy.
• ALMA will be able to do this work trivially
Elizabeth Stanway - Obergurgl, December 2009
Our 2009 ATCA Survey
• Targeted second LBG over-density covering 3 times as much area at 37Ghz and 2 GHz bandwidth
• Encompasses 7 LBGs in z~0.1 range (around z~4.95), and 1 other z=5.2 source.
• Observed each pointing for 2 nights using the ATCA with two 2GHz IFs and 1MHz resolution (at 37GHz).
• Redshift coverage of ~4.23-5.34 at 19GHz and ~4.81-5.44 at 37GHz.
• RMS limits ~0.2mJy/beam at 19GHz
~0.3mJy/beam at 37GHz
(in 1 MHz channels)
Elizabeth Stanway - Obergurgl, December 2009
Preliminary Results
• 6 Possible detections within the ATCA primary beams.
• Three detected at 19GHz and three at 37GHz.
• One has possible 19 and 37GHz detection.
• 3 would fall within the redshift of the over-density.
• Two are closely separated in redshift at z~4.6.
• Gas masses (H2) ~ 3-6 x109M for 37GHz detection and ~ 3-6 x1010M
for 19GHz detections.
• FWHM ~50-120kms-1. Comparable to previous detection.
Elizabeth Stanway - Obergurgl, December 2009
• z=4.92
• 3x109 Msun in H2
• May be detected in two CO transitions
• Peak flux 0.4 mJy
• v = 50 km/s
Preliminary Results
Elizabeth Stanway - Obergurgl, December 2009
Limits on LBGs in the Field
• All LBGs are not detected at 19GHz or 37GHz.
• Image R.M.S. Noise ~ 0.16mJy/beam (at CO(1-0) line)
~ 0.37mJy/beam (at CO(2-1) line)
• Gives 2 detection limit ~ LCO< 2.8x1010 K kms-1 pc2
~ LCO< 1.7x1010 K kms-1 pc2
For an unresolved 200 kms-1 emission line at the redshifts of the galaxies.
Can constrain molecular gas in LBGs in the field to:
M(H2)<2.2x1010 M (2, CO(1-0))
M(H2)<1.4x1010 M (2, CO(2-1))
Total observed mass in stellar component and H2 ~1.3x1011 M in 33.8Mpc3
Elizabeth Stanway - Obergurgl, December 2009
Conclusions
• Lyman Break Galaxies clearly mark out underlying structure at very high redshifts
• Regions overdense in LBGs are perfect for follow-up at over wavelengths
• Molecular Gas may contribute a substantial fraction of the the baryon mass at z=5
• CO emission lines are currently the most accessible probe of this
• Searches for dust and gas dominated galaxies at high z are possible with current instrumentation with several promising candidates already identified
• ALMA will enable more complete surveys of the baryon distribution in high z large scale structure
Elizabeth Stanway - Obergurgl, December 2009
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