1. Interpreting High Resolution Sunyaev-Zel’dovich Effect Observations with MUSTANG Charles Romero University of Virginia, National Radio Astronomy Observatory 1 Brian Mason, Craig Sarazin, Mark Whittle, Mike Skrutskie, and Barry Condron

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) Sara Stanchfield (Upenn) Credit: NASA Key: Graduate Student, Postdoc, Faculty 2 15 July 2015 Dissertation Defense Charles Romero

3. Outline of Talk Galaxy Clusters – Why study them? SZ Observations – Substructure & Bulk ICM Fitted pressure profiles MUSTANG-2 – Science & Hardware Conclusions & future work Uchicago, adapted from L. Van Sproyboeck 3 15 July 2015 Dissertation Defense Charles Romero

4. Galaxy Clusters 80-90% Dark Matter 9-18% ICM Gas – n e ~ 10 -3 to 10 -1 [cm -3 ] – k B T e ~ 5 keV (T e ~ 6 x 10 7 K) 1-2% Galaxies 15 July 2015 Dissertation Defense Charles Romero4 10 14 – 10 15 M ○ R 500 ~ 1 Mpc

5. X-ray cavities Sloshing Radio relics Radio halos Radio phoenixes Shocks Cold fronts 15 July 2015 Dissertation Defense Charles Romero5 Fabian+ 2006, Russell+ 2012, van Weeren+ 2012, Giacintucci+ 2014 ICM Physics

6. Cluster Mass  Cosmology Growth of structure Springel+ 2005 6 15 July 2015 Dissertation Defense Charles Romero

7. SZ surveys and scaling relations 7 Marriage+ 2011 Czakon+ 2014 Credit: M. Markevitch Y-M scaling relation 15 July 2015 Dissertation Defense Charles Romero

8. Cosmological Parameter Constraints Sehgal+ 2011 8 Without scatter in scaling relation With scatter in scaling relation 15 July 2015 Dissertation Defense Charles Romero

9. This Study: CLASH clusters 20 X-ray selected 5 lensing selected Multi-wavelength! 0.18 < z < 0.89 Postman+ 2012 9 15 July 2015 Dissertation Defense Charles Romero

10. Outline of Talk Galaxy Clusters – Why study them? SZ Observations – Substructure & Bulk ICM Fitted pressure profiles MUSTANG-2 – Science & Hardware Conclusions & future work Uchicago, adapted from L. Van Sproyboeck 10 15 July 2015 Dissertation Defense Charles Romero

11. MUSTANG’s view of CLASH (+1) 11 15 July 2015 Dissertation Defense Charles Romero

12. Studying the ICM: Radio (SZ) Credit: Ned Wright Sunyaev Zel’dovich Effect Δ I ∝ P e 12 MUSTANG 15 July 2015 Dissertation Defense Charles Romero

13. MUSTANG + GBT The Green Bank Telescope – Off-axis Gregorian design – 290 MHz to 100 GHz – 240 μm surface RMS – 90 GHz effective area : 2500 m 2 – 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 13 15 July 2015 Dissertation Defense Charles Romero

14. Observing via the SZ effect 15 July 2015 Dissertation Defense Charles Romero14

15. Data Processing: MUSTANG Filter out scales > FOV 15 15 July 2015 Dissertation Defense Charles Romero

16. MUSTANG results Korngut+ 2011 16 Mason+ 2010 15 July 2015 Dissertation Defense Charles Romero

17. MUSTANG results, cont. MACS 0717 Mroczkowski+ 2012 17 15 July 2015 Dissertation Defense Charles Romero

18. MUSTANG Beam 18 15 July 2015 Dissertation Defense Charles Romero

19. Point Source Removal 19 15 July 2015 Dissertation Defense Charles Romero

20. Point source removal (cont.) 15 July 2015 Dissertation Defense Charles Romero20

21. Outline of Talk Galaxy Clusters – Why study them? SZ Observations – Substructure & Bulk ICM Fitted pressure profiles MUSTANG-2 – Science & Hardware Conclusions & future work Uchicago, adapted from L. Van Sproyboeck 21 15 July 2015 Dissertation Defense Charles Romero

22. Bolocam + MUSTANG 22 Bolocam (on the CSO) 8’ FOV 58” FWHM at 2.1mm (140 GHz) Bolocam Beam MUSTANG Beam 15 July 2015 Dissertation Defense Charles Romero

23. Pressure Profiles Previous studies have constrained these parameters over their samples of clusters – Nagai 2007, Arnaud 2010, Planck 2012, and Sayers 2013 23 15 July 2015 Dissertation Defense Charles Romero

24. Linear Joint Fitting 15 July 2015 Dissertation Defense Charles Romero ++ ? 24

25. MACS 1206 (sequential fit) 25 Young et al. 2014 (arXiv:1411.0317) 15 July 2015 Dissertation Defense Charles Romero

26. MACS 0647 (simultaneous fit!) 26 Romero et al. 2015 (arXiv: 1501.00187) Bolocam only Bolocam + MUSTANG 15 July 2015 Dissertation Defense Charles Romero

27. Abell 1835 27 Romero et al. 2015 (arXiv: 1501.00187) Bolocam only Bolocam + MUSTANG 15 July 2015 Dissertation Defense Charles Romero Abell 1835: SZE vs. X-ray

28. Comparison of profile sets 28 MACS 0647 Abell 1835 15 July 2015 Dissertation Defense Charles Romero

29. Constraints over all clusters 15 July 2015 Dissertation Defense 29Charles Romero

30. Subdivided 15 July 2015 Dissertation Defense 30 Cool cores clearly have steeper core pressure profiles Charles Romero

31. Comparing Pressure Profiles 15 July 2015 Dissertation Defense 31 Our sample shows more dispersion at large radii. Arnaud+ 2010 Charles Romero

32. Y-M relation 32Charles Romero 15 July 2015 Dissertation Defense

33. SZ + X-ray SZ is directly proportional to P e X-ray emissivity is proportional n e 2 T 1/2 – X-ray constrains n e well 15 July 2015 Dissertation Defense 33 Constrain T e = P e(SZ) / n e(X) Constrain elongation along LOS (ε = [P e(sz) / P e(X) ] 2 ) Constrain helium sedimentation Charles Romero

34. 15 July 2015 Dissertation Defense Charles Romero34 Separate from cluster geometry (elongation) and He sedimentation modeling. Blue = ACCEPT (Cavagnolo+ 2009) Green = This work Solid line: Vikhlinin model Dotted line: Bulbul model Deriving Electron Temperatures

35. Cluster Geometry 15 July 2015 Dissertation Defense Charles Romero35 b a

36. Cluster Geometry 15 July 2015 Dissertation Defense Charles Romero36 b a

37. Helium Sedimentation: Models 15 July 2015 Dissertation Defense 37 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 * R 500 ) R 500 ~ 4-6 arcmin Charles Romero

38. Helium Sedimentation: Fitting I 15 July 2015 Dissertation Defense 38 Must account for a global offset in pressure between SZ and X-ray Offset could be due to elongation along the LOS. Abell 1835MACS 1311 Charles Romero

39. Helium Sedimentation: Fitting II 15 July 2015 Dissertation Defense 39 Rescaled P e(SZ) can now be compared to P e(X) Fit model ratios to data. Charles Romero

40. Outline of Talk Galaxy Clusters – Why study them? SZ Observations – Substructure & Bulk ICM Fitted pressure profiles MUSTANG-2 – Science & Hardware Conclusions & future work Uchicago, adapted from L. Van Sproyboeck 40 15 July 2015 Dissertation Defense Charles Romero

41. MUSTANG-2 Dicker et al. 2014 223 dual polarization feeds 75 – 105 GHz bandpass Antenna +Feedhorn coupled TES bolometers. 9” beam 4.2’ field of view on GBT (9” and 42” for MUSTANG) >200 times faster mapping speeds 41 15 July 2015 Dissertation Defense Charles Romero

42. MUSTANG-1.5 15 July 2015 Dissertation Defense Charles Romero42 Detector module 64 dual polarization feeds 2.5’ field of view on GBT ~40 times faster mapping speeds First light this past spring

43. Window Determine transmission properties of window materials 15 July 2015 Dissertation Defense Charles Romero43

44. Window Results Total transmission, absorption, and reflection determined. 15 July 2015 Dissertation Defense Charles Romero44

45. Chandra X-ray image Russell et al. (2012) Shocks: Abell 2146

46. Shock Heating

47. Observing Abell 2146 Observed in Winter 2011; >7 hours on source

48. Outline of Talk Galaxy Clusters – Why study them? SZ Observations – Substructure & Bulk ICM Fitted pressure profiles MUSTANG-2 – Science & Hardware Conclusions & future work Uchicago, adapted from L. Van Sproyboeck 48 15 July 2015 Dissertation Defense Charles Romero

49. Conclusions Able to constrain pressure profile – MUSTANG adds ability to constrain γ – Pressure profile shape in agreement with previous gNFW results Addition of X-ray data reveals: – Differences between SZ and X-ray profiles – Geometric, temperature, and other checks. 15 July 2015 Dissertation Defense Charles Romero49

50. Appendix 15 July 2015 Dissertation Defense Charles Romero50

51. Future Work abc 15 July 2015 Dissertation Defense Charles Romero51

52. Centroids 52 15 July 2015 Dissertation Defense Comparing Confidence intervals based on assumed centroid. Charles Romero

53. Future Work: NIKA-2 IRAM 30m with 6.5’ FOV FWHM: 18.0” @ 150 GHz; 13.2” @ 240 GHz 1000 pixels for 150 GHz, 2000 pixels for each linear polarization at 240 GHz 15 July 2015 Dissertation Defense 53 Monfardini+ 2014 Charles Romero

54. X-ray Properties of Clusters 15 July 2015 Dissertation Defense 54 Mantz+ 2010 Charles Romero

55. Ensemble Pressure Profiles 15 July 2015 Dissertation Defense Charles Romero55

56. SZ fits to ACCEPT pressure 15 July 2015 Dissertation Defense 56Charles Romero

57. 15 July 2015 Dissertation Defense Charles Romero57

58. Deriving Electron Temperatures 15 July 2015 Dissertation Defense 58 Abell 1835MACS 1311 Blue = ACCEPT (Cavagnolo+ 2009) Red = ACCEPT2 (Baldi+ current work ) Green = This work Separate from cluster geometry (elongation) and He sedimentation modeling. Charles Romero

59. Abell 1835 A10 α and β 59 15 July 2015 Dissertation Defense Charles Romero

60. MACS 0647 A10 α and β 60 15 July 2015 Dissertation Defense Charles Romero

61. 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. – Combination with X-ray allows for constraints on helium sedimentation or temperature profiles. MUSTANG-1.5 will do significantly better. 61 15 July 2015 Dissertation Defense Charles Romero

62. Beam uncertainties 15 July 2015 Dissertation Defense Charles Romero62

63. Correlation Matrix 63 15 July 2015 Dissertation Defense Charles Romero

64. Winter/Spring 2015: MUSTANG-1.5 64 detectors populated Several proposals for the spring PIs: Dicker, Gilbank, Romero, Edge, Crichton 64 15 July 2015 Dissertation Defense Charles Romero

65. Observing strategies 65 FOV 15 July 2015 Dissertation Defense Charles Romero

66. MACS 0647 (sequential fit) 66 Young et al. 2014 (arXiv:1411.0317) 15 July 2015 Dissertation Defense Charles Romero

67. Galaxy Clusters Credit: NASA Vacca+ 2011 Optical X-ray 67 15 July 2015 Dissertation Defense Charles Romero

68. Observing with MUSTANG ~20 hours per cluster Good weather Calibration every 30 min. OOF  adjust GBT surface 15 July 2015 Dissertation Defense Charles Romero FOV 68

69. Y-M scaling relation http://arxiv.org/abs/1501.00317 – Liang Yu, Kaylea Nelson, and Daisuke Nagai – Also 340.03D talk at AAS 69 15 July 2015 Dissertation Defense Charles Romero