interpreting high resolution sunyaev-zel’dovich effect observations with mustang charles romero...
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Interpreting High Resolution Sunyaev-Zel’dovich Effect
Observations with MUSTANG
Charles RomeroUniversity of Virginia, National Radio Astronomy Observatory
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• Jack Sayers (Caltech)• Nicole Czakon (Sinica)• Phil Korngut (JPL/Caltech)
Collaborators• Brian Mason (NRAO)• Simon Dicker (UPenn)• Alex Young (MIT-LL)• Mark Devlin (UPenn)• Erik Reese (Moorpark)• Tony Mroczkowski (NRL)• Jon Seivers (KwaZulu-Natal)• Craig Sarazin (U Virginia)• Tracy Clarke (NRL)• Sunil Golwala (Caltech)
Credit: NASA
Key: Graduate Student, Postdoc, Faculty
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Outline of Talk
• Galaxy Clusters– Why study them?
• SZ Observations– Substructure & Bulk ICM
• Fitted pressure profiles• Future work & conclusions
Uchicago, adapted from L. Van Sproyboeck
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Cluster Mass Cosmology
Growth of structure
Springel+ 200508 January 2014 AAS Disertation Talk
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Cosmological Parameter Constraints
Sehgal+ 2011
Without scatter in scaling relation With scatter in scaling relation
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SZ surveys and scaling relations
Marriage+ 2011
Czakon+ 2014
Credit: M. Markevitch
Y-M scaling relation
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This Study: CLASH clusters
• 20 X-ray selected• 5 lensing selected• Multi-wavelength!
Postman+ 2012 708 January 2014 AAS Disertation Talk Charles Romero
Outline of Talk
• Galaxy Clusters– Why study them?
• SZ Observations– Substructure & Bulk ICM
• Fitted pressure profiles• Future work & conclusions
Uchicago, adapted from L. Van Sproyboeck
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MUSTANG’s view of CLASH (+1)
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Studying the ICM: Radio (SZ)
Credit: Ned Wright
Sunyaev Zel’dovich Effect
ΔI ∝ Pe
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MUSTANG
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MUSTANG + GBT• The Green Bank Telescope
– Off-axis Gregorian design– 290 MHz to 100 GHz– 240 μm surface RMS– 90 GHz effective area : 2500 m2
– 90 GHz beam size : 9" FWHM – 2” pointing accuracy
• MUSTANG– 64 absorber coupled TESs– 42” FOV– 400 μJy/beam in 3’ x 3’ per hour– Cold reimaging optics
• The science– Star Forming regions– Sunyaev-Zel’dovich Effect (SZE)
100 m
1 pixel
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Data Processing: MUSTANG
Filter out scales > FOV
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MUSTANG results
Korngut+ 2011
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Mason+ 2010
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MUSTANG results, cont.MACS 0717
Mroczkowski+ 2012
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MUSTANG Beam
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Point Source Removal
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Outline of Talk
• Galaxy Clusters– Why study them?
• SZ Observations– Substructure & Bulk ICM
• Fitted pressure profiles• Future work & conclusions
Uchicago, adapted from L. Van Sproyboeck
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Bolocam + MUSTANG
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Bolocam (on the CSO)8’ FOV 58” FWHM at 2.1mm (140 GHz)
Bolocam Beam
MUSTANG Beam
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Pressure Profiles
• Previous studies have constrained these over their samples of clusters– Nagai 2007, Arnaud 2010, Planck 2012, and
Sayers 2013
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MACS 1206 (sequential fit)
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Young et al. 2014 (arXiv:1411.0317)
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MACS 0647 (sequential fit)
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Young et al. 2014 (arXiv:1411.0317)
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MACS 0647 (simultaneous fit!)
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Romero et al. 2015 (arXiv: 1501.00187)
Bolo
cam
onl
yBo
loca
m +
MU
STAN
G
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Abell 1835
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Romero et al. 2015 (arXiv: 1501.00187)
Bolo
cam
onl
yBo
loca
m +
MU
STAN
G
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Comparison of profile sets
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MACS 0647Abell 1835
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Constraints over all clusters
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Subdivided
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Cool cores clearly have steeper core pressure profiles
Comparing Pressure Profiles
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Our sample shows more dispersion at large radii.
Arnaud+ 2010
SZ + X-ray• SZ is directly proportional to Pe
• X-ray emissivity is proportional ne2 T1/2
– X-ray constrains ne well
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• Constrain Te = Pe(SZ) / ne(X)
• Constrain elongation along LOS (ε = [Pe(x)/ Pe(SZ)]2 ) • Constrain helium sedimentation
Helium Sedimentation: Models
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• Proposed as early as Gilfanov+ 1984
• Potential sedimentation calculated by Chuzhoy+ 2004, Peng & Nagai 2009
• Some constraints from Markevitch 2007
• Bulbul+ 2011 investigated impact on scaling relations
• Need high resolution SZ to do this! (scales < 0.1 * R500)
• R500 ~ 2-4 arcmin
Helium Sedimentation: Fitting I
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• Must account for a global offset in pressure between SZ and X-ray
• Offset could be due to elongation along the LOS.
Abell 1835 MACS 1311
Helium Sedimentation: Fitting II
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• Rescaled Pe(SZ) can now be compared to Pe(X)
• Fit model ratios to data.
Deriving Electron Temperatures
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Abell 1835 MACS 1311
Blue = ACCEPT (Cavagnolo+ 2009)Red = ACCEPT2 (Baldi+ current work )Green = This work
Separate from cluster geometry (elongation) and He sedimentation modeling.
Outline of Talk
• Galaxy Clusters– Why study them?
• SZ Observations– Substructure & Bulk ICM
• Fitted pressure profiles• Future work & conclusions
Uchicago, adapted from L. Van Sproyboeck
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Future Work: MUSTANG-1.5Dicker et al. 2014
• 64 dual polarization feeds• 75 – 105 GHz bandpass• Antenna +Feedhorn coupled
TES bolometers.• 9” beam 2.5’ field of view on
GBT(9” and 45” for MUSTANG)
• ~40 times faster mapping speeds
• On the telescope now!
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Fall 2015: MUSTANG-1.5
• 64 detectors populated
• Several proposals for this fall– PIs: Dicker, Gilbank,
Romero, Edge, Crichton
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Conclusions
• MUSTANG sees substructure and compact sources in many clusters– Substructure can reveal dynamics of the cluster
• Point sources can easily be dealt with.• The addition of MUSTANG data to Bolocam
does increase ability to constraint γ.• MUSTANG-1.5 will do significantly better.
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Future Work: NIKA-2
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Appendix
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Comparing Confidence intervals based on assumed centroid.
Y-M scaling relation
• http://arxiv.org/abs/1501.00317– Liang Yu, Kaylea Nelson, and Daisuke Nagai– Also 340.03D talk yesterday
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Abell 1835A10 α and β
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MACS 0647A10 α and β
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Correlation Matrix
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Winter/Spring 2015: MUSTANG-1.5
• 64 detectors populated
• Several proposals for the spring
• PIs: Dicker, Gilbank, Romero, Edge, Crichton
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Observing strategies
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FOV
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Abell 2146->Two shocks->Cold front
currently being observed by MUSTANG
Chandra X-ray image -- Russell et al. (2010)
Abell 2146
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Galaxy Clusters
Credit: NASA
Vacca+ 2011
Optical
X-ray
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