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University of Pennsylvania ScholarlyCommons Publicly Accessible Penn Dissertations Spring 2011 The Multiplexed Squid Tes Array at Ninety Gigahertz (Mustang) Phillip M. Korngut University of Pennsylvania, [email protected] Follow this and additional works at: https://repository.upenn.edu/edissertations Part of the External Galaxies Commons, and the Instrumentation Commons Recommended Citation Korngut, Phillip M., "The Multiplexed Squid Tes Array at Ninety Gigahertz (Mustang)" (2011). Publicly Accessible Penn Dissertations. 317. https://repository.upenn.edu/edissertations/317 This paper is posted at ScholarlyCommons. https://repository.upenn.edu/edissertations/317 For more information, please contact [email protected]. The Multiplexed Squid Tes Array at Ninety Gigahertz (Mustang) Abstract The Multiplexed SQUID/TES Array at Ninety Gigahertz (MUSTANG) is a bolometric continuum imaging camera designed to operate at the Gregorian focus of the 100m Green Bank Telescope (GBT) in Pocahontas county, West Virginia. The combination of the GBT's large collecting area and the 8x8 array of transition edge sensors at the heart of MUSTANG allows for deep imaging at 10'' resolution at 90GHz. The MUSTANG receiver is now a facility instrument of the National Radio Astronomy Observatory available to the general astronomical community. The 3.3mm continuum passband is useful to access a large range of Galactic and extra-Galactic astrophysics. Sources with synchrotron, free-free and thermal blackbody emission can be detected at 3.3mm. Of particular interest is the Sunyaev Zel'dovich effect in clusters of galaxies, which arises from the inverse Compton scattering of CMB photons off hot electrons in the intra-cluster medium. In the MUSTANG band, the effect is observationally manifested as an artificial decrement in power on the sky in the direction of the cluster. There have been many experiments in the past two decades dedicated to measurements of the SZE, however, nearly all of them were accomplished with angular resolution larger than ~1'. The massive primary of the GBT enables measurements of the SZE on 10'' scales. This provides a new technique to map pressure substructure in the plasma atmospheres of merging clusters of galaxies. By analyzing MUSTANG data along side X-ray data, spatially resolved measurements of the temperature, density and pressure of the ICM can be performed which can be used to infer the physics governing major mergers. This thesis details the design, commissioning and operation of the various components which comprise the MUSTANG receiver. This includes the sub-kelvin cryogenic cooling, the time domain multiplexed readout electronics and the array of transition edge sensor bolometers. Laboratory characterization of the detector array is thoroughly described, including the measurements of the transition temperatures, thermal conductance, noise properties and time constants. Bolometric cameras measure celestial radiation as time ordered data. To reliably produce images from traces in the time domain, care must be taken to modulate the signal in an optimized fashion during observations. Once the data are taken, algorithms must be developed to isolate the signal of interest from the foregrounds produced by atmospheric emission. This thesis presents the techniques developed to scan, calibrate, filter and produce images from time ordered data taken with MUSTANG and the GBT. From the Fall of 2006 to the winter of 2010, the MUSTANG receiver was commissioned on the GBT and used for a range of astrophysical measurements. The commissioning process and early science results are given in this thesis. This includes the modifications made ot the instrument which have resulted in dramatically enhanced sensitivity as well as the images produced from bright extended millimeter sources such as high mass star forming regions, active galactic nuclei and supernova remnants. This thesis presents a sample of merging clusters of galaxies imaged through their Sunyaev Zel'dovich signatures at high angular resolution. In the massive cluster RXJ1347, a previously reported pressure enhancement to the south east of the cluster peak was confirmed. This is now interpreted as a parcel of hot shock heated gas (KT~20keV) produced in a recent merger. In the high redshift systems MACS0744 and CL1226, pressure substructure was identified and is believed to be associated with merger activity. Both systems contain peaks in dark matter revealed by gravitational lensing which are not associated with baryonic emission, supportive of a scenario in which an infalling cluster has passed through a main cluster being stripped of its baryons. In MACS0744, the SZE and X-ray morphology is suggestive of a shock wave propagating through the ICM. By fitting the Rankine Hugoniot jump conditions in a simultaneous SZE/X-ray analysis, the likelihood of this interpretation is explored. The system is well described by a mildly supersonic shock wave propagating with a Mach number of ~1.2. Degree Type Dissertation Degree Name Doctor of Philosophy (PhD) Graduate Group Physics & Astronomy First Advisor Mark Devlin Keywords Sunyaev Zeldovich effect, Bolometers, Cosmology, Radio Telescopes Subject Categories External Galaxies | Instrumentation This dissertation is available at ScholarlyCommons: https://repository.upenn.edu/edissertations/317 THE MULTIPLEXED SQUID TES ARRAYAT NINETY GIGAHERTZ (MUSTANG) Phillip M. Korngut A DISSERTATION in Physics and Astronomy Presented to the Faculties of the University of Pennsylvania in Partial Fulfillment of the Requirements for the degree of Doctor of Philosophy 2011 Supervisor of Dissertation: Mark Devlin, Professor, Astrophysics Experiment Graduate Group Chairperson: A. T. Charlie Johnson, Professor, Condensed Matter Experiment Dissertation Committee: Masao Sako, Assistant Professor, Astrophysics Gary Bernstein, Professor, Astrophysics Bhuvnesh Jain, Professor, Astrophysics Theory Josh Klein, Associate Professor, Experimental Particle Physics Acknowledgements Throughout my tenure as a graduate researcher at UPENN, I have had the privilege of getting to work with a wide range of scientists at a variety of institutions. The work presented in this thesis would not have been possible without their help and I am in their debt. My advisor, Mark Devlin, has consistently provided wise and meaningful guidance. His knowledge of the field and keen insight to the way in which things fit into a larger picture have taught me valuable lessons about the process of science. He works harder than anyone else I know, tirelessly proposing to secure funding and look out for the future of those around him. His extensive success in the field is clearly well earned. I am grateful for all the opportunity he has provided me with. It has had profound positive influence on the path my career has taken. Much of my effort in the proverbial trenches at the front lines of MUSTANG research was directly guided by two mentors; Simon Dicker and Brian Mason. My knowledge of data analysis, cryogenics, optics and all aspects of telescope operation is a direct consequence of working with them. They have always been more than willing to work closely with me through the gritty details of the experiment and have proved to be excellent companions through the long months spent at Green Bank. The functionality of MUSTANG would not have been possible without a tremen- dous amount of support from the staff at NRAO. I’ve always had help from the receiver folks like Steve White, Mike Stennes and Dave Woody. The cryo guys, Bob Simon and Kenny Lehman, were always there to troubleshoot helium related issues and to provide any fitting or pipes we needed. Software people like Melinda Mello, Mark Whitehead and Ray Creager have ensured a fantastic control interface and were quick with fixing any ob- scure bug I came across. The GBT operators, Greg Monk, Donna Stricklin and Barry Sharp have provided lots of late night assistance while running observations and I thank them for their attentiveness. ii I have learned a tremendous amount about TES detectors from working with the teams at NASA GSFC and NIST. Dominic Benford, Johannes Staghun, Jay Chervenak, Tali Figueroa, Harvey Moseley, Joel Ullom and Galen O’Neil have taught me the intricacies of detector operation and optimization. I’d also like to thank several senior scientists who have helped me along the way including Masao Sako, Craig Sarazin, Bill Cotton and James Aguirre. Post-docs like Erik Reese and Tony Mroczkowski helped me work through difficult problems. Fellow grad- uate students and staff who worked in the Experimental Cosmology lab such as Marie Rex, Dan Swetz, Chris Semich, Matt Truch, Bob Thornton, Danica Marsden, Elio Angile, Ben Schmidt, Alex Young, Jeff Klein, Fritz Stabeneau, Kim Scott and Roxana Lupu have also made for a pleasant and productive work environment. There is no way I could have made it through classes without the help of my friends and classmates, in particular Ravi Gupta, Jon McDonald, and Jon Fischer. They made working through difficult problem sets feasible and at times, even fun. My parents, Robert and Heidi Korngut, have always encouraged my scientific endeavors and they presented me with the opportunities to pursue them. I am forever grateful for their support. Finally, I would like to thank Rebekah Midberry, for her love and understanding throughout the PhD process. iii ABSTRACT THE MULTIPLEXED SQUID TES ARRAYAT NINETY GIGAHERTZ (MUSTANG) Phillip M. Korngut Mark Devlin The Multiplexed SQUID/TES Array at Ninety Gigahertz (MUSTANG) is a bolometric continuum imaging camera designed to operate at the Gregorian focus of the 100 m Green Bank Telescope (GBT) in Pocahontas county, West Virginia. The combination of the GBT’s large collecting area and the 8 8 array of transition edge sensors at the heart of × MUSTANG allows for deep imaging at 10′′ resolution at 90 GHz. The MUSTANG receiver is now a facility instrument of the National Radio Astronomy Observatory available to the general astronomical community. The 3.3 mm continuum passband is useful to access a large range of Galactic and extra-Galactic astrophysics. Sources with synchrotron, free-free and thermal blackbody emission can be detected at 3.3 mm.
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