Interpreting High Resolution Sunyaev-Zel’dovich Effect Observations with MUSTANG Charles Romero University of Virginia, National Radio Astronomy Observatory

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Interpreting High Resolution Sunyaev-Zel’dovich Effect

Observations with MUSTANG

Charles RomeroUniversity of Virginia, National Radio Astronomy Observatory

Charles Romero 2

• 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

08 January 2014 AAS Disertation Talk

Charles Romero 3

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


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





808 January 2014 AAS Disertation Talk Charles Romero

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MUSTANG’s view of CLASH (+1)


Studying the ICM: Radio (SZ)

Credit: Ned Wright

Sunyaev Zel’dovich Effect

ΔI ∝ Pe

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MUSTANG


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


Data Processing: MUSTANG

Filter out scales > FOV


MUSTANG results

Korngut+ 2011

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Mason+ 2010


MUSTANG results, cont.MACS 0717

Mroczkowski+ 2012


MUSTANG Beam


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Point Source Removal


Charles Romero

Outline of Talk






Bolocam + MUSTANG

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Bolocam (on the CSO)8’ FOV 58” FWHM at 2.1mm (140 GHz)

Bolocam Beam

MUSTANG Beam


Pressure Profiles

• Previous studies have constrained these over their samples of clusters– Nagai 2007, Arnaud 2010, Planck 2012, and

Sayers 2013


MACS 1206 (sequential fit)

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Young et al. 2014 (arXiv:1411.0317)


MACS 0647 (sequential fit)

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Young et al. 2014 (arXiv:1411.0317)


MACS 0647 (simultaneous fit!)

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Romero et al. 2015 (arXiv: 1501.00187)

Bolo

cam

onl

yBo

loca

m +

MU

STAN

G


Abell 1835

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Romero et al. 2015 (arXiv: 1501.00187)

Bolo

cam

onl

yBo

loca

m +

MU

STAN

G


Comparison of profile sets

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MACS 0647Abell 1835


Constraints over all clusters

08 January 2014 AAS Disertation Talk Charles Romero 25

Subdivided


Cool cores clearly have steeper core pressure profiles

Comparing Pressure Profiles


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


• Constrain Te = Pe(SZ) / ne(X)

• Constrain elongation along LOS (ε = [Pe(x)/ Pe(SZ)]2 ) • Constrain helium sedimentation

Helium Sedimentation: Models


• 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


• 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


• Rescaled Pe(SZ) can now be compared to Pe(X)

• Fit model ratios to data.

Deriving Electron Temperatures


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






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!


Fall 2015: MUSTANG-1.5

• 64 detectors populated

• Several proposals for this fall– PIs: Dicker, Gilbank,

Romero, Edge, Crichton

04 Sept. 2014 Caltech Lunch Talk Charles Romero 35

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.


Future Work: NIKA-2


Appendix


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


http://arxiv.org/abs/1501.00317

http://arxiv.org/abs/1501.00317

Abell 1835A10 α and β


MACS 0647A10 α and β


Correlation Matrix


Winter/Spring 2015: MUSTANG-1.5

• 64 detectors populated

• Several proposals for the spring

• PIs: Dicker, Gilbank, Romero, Edge, Crichton


Observing strategies

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FOV


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


Documents

Interpreting High Resolution Sunyaev-Zel’dovich Effect Observations with MUSTANG Charles Romero University of Virginia, National Radio Astronomy Observatory