Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope
The South Pole Telescope is a 10m millimeter-wavelength telescope for finding galaxy clusters via the thermal Sunyaev-Zel'dovich (tSZ) effect. This thesis is divided into two parts. The first part describes the development of the kilopixel SPT-SZ receiver and the frequency-domain multiplexor (f...
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eScholarship, University of California
2010
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Online Access: | https://escholarship.org/uc/item/1m21q7w6 |
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ftcdlib:oai:escholarship.org/ark:/13030/qt1m21q7w6 |
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openpolar |
institution |
Open Polar |
collection |
University of California: eScholarship |
op_collection_id |
ftcdlib |
language |
English |
topic |
Physics Cosmic Microwave Background Large-Scale Structure Millimeter Wave Instrumentation Superconducting Quantum Interference Devices |
spellingShingle |
Physics Cosmic Microwave Background Large-Scale Structure Millimeter Wave Instrumentation Superconducting Quantum Interference Devices Lueker, Martin Van Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope |
topic_facet |
Physics Cosmic Microwave Background Large-Scale Structure Millimeter Wave Instrumentation Superconducting Quantum Interference Devices |
description |
The South Pole Telescope is a 10m millimeter-wavelength telescope for finding galaxy clusters via the thermal Sunyaev-Zel'dovich (tSZ) effect. This thesis is divided into two parts. The first part describes the development of the kilopixel SPT-SZ receiver and the frequency-domain multiplexor (fMUX). The second part describes the first SPT power spectrum measurement and the first detection of the tSZ power spectrum. The SPT-SZ focal plane consists of 960 spiderweb coupled transition-edge sensors. Due to strong electro-thermal feedback, these devices have good sensitivity and linearity, though risk spontaneous oscillations. Adding heat capacity to these devices can ensure stability, so long as the loopgain, $\mathcal{L}$, is less than $G_\textrm{int}/G_0$, the ratio between the thermal conductances linking the TES to the heat capacity and linking the heat capacity to the bath. I describe as experimental technique for measuring the internal thermal structure of these devices, allowing for rapid sensor evaluation. The fMUX readout system reduces wiring complexity in this receiver by AC-biasing each sensor at a unique frequency and sending signals from multiple bolometers along one pair of wires. The Series SQUID Arrays (SSAs) used to read changes in bolometer current are notably non-linear and extremely sensititve to ambient magnetic fields. The SSAs are housed in compact magnetic shielding modules which reduces their effective area to 80 $\textrm{m}\Phi_0/\textrm{gauss}$. The SSA are fedback with a flux-locked loop to improve their linearity and dynamic range, and decrease their input reactance. The FLL is bandwidth of 1 MHz with a measured loopgain of 10. In the current implementation, this bandwidth is limited between the SQUID input coil and other reactances, which I study in Chapter \ref{chap:fllstab}.In the second part of the thesis I present power spectrum measurements for the first 100~deg$^2$ field observed by the SPT. On angular scales where the primary CMB anisotropy is dominant, $\ell \lesssim 3000$, the SPT power spectrum is consistent with the standard $\Lambda$CDM cosmology. On smaller scales, we see strong evidence for a point source contribution, consisteThe South Pole Telescope is a 10m millimeter-wavelength telescope for finding galaxy clusters via the thermal Sunyaev-Zel'dovich (tSZ) effect. This thesis is divided into two parts. The first part describes the development of the kilopixel SPT-SZ receiver and the frequency-domain multiplexor (fMUX). The second part describes the first SPT power spectrum measurement and the first detection of the tSZ power spectrum. The SPT-SZ focal plane consists of 960 spiderweb coupled transition-edge sensors. Due to strong electro-thermal feedback, these devices have good sensitivity and linearity, though risk spontaneous oscillations. Adding heat capacity to these devices can ensure stability, so long as the loopgain, $\mathcal{L}$, is less than $G_\textrm{int}/G_0$, the ratio between the thermal conductances linking the TES to the heat capacity and linking the heat capacity to the bath. I describe as experimental technique for measuring the internal thermal structure of these devices, allowing for rapid sensor evaluation. The fMUX readout system reduces wiring complexity in this receiver by AC-biasing each sensor at a unique frequency and sending signals from multiple bolometers along one pair of wires. The Series SQUID Arrays (SSAs) used to read changes in bolometer current are notably non-linear and extremely sensititve to ambient magnetic fields. The SSAs are housed in compact magnetic shielding modules which reduces their effective area to 80 $\textrm{m}\Phi_0/\textrm{gauss}$. The SSA are fedback with a flux-locked loop to improve their linearity and dynamic range, and decrease their input reactance. The FLL is bandwidth of 1 MHz with a measured loopgain of 10. In the current implementation, this bandwidth is limited between the SQUID input coil and other reactances, which I study in Chapter \ref{chap:fllstab}.In the second part of the thesis I present power spectrum measurements for the first 100~deg$^2$ field observed by the SPT. On angular scales where the primary CMB anisotropy is dominant, $\ell \lesssim 3000$, the SPT power spectrum is consistent with the standard $\Lambda$CDM cosmology. On smaller scales, we see strong evidence for a point source contribution, consistent with a population of dusty, star-forming galaxies. I combine the 150 and 220$\,$GHz data to remove the majority of the point source power, and use the point source subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at $2.6\,\sigma$. At $\ell=3000$, the SZ power in the subtracted bandpowers is $4.2\,$$\pm$$\,1.5\, \mu\rm{K}^2$, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. t with a population of dusty, star-forming galaxies. I combine the 150 and 220$\,$GHz data to remove the majority of the point source power, and use the point source subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at $2.6\,\sigma$. At $\ell=3000$, the SZ power in the subtracted bandpowers is $4.2\,$$\pm$$\,1.5\, \mu\rm{K}^2$, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. |
author2 |
Holzapfel, William L |
format |
Other/Unknown Material |
author |
Lueker, Martin Van |
author_facet |
Lueker, Martin Van |
author_sort |
Lueker, Martin Van |
title |
Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope |
title_short |
Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope |
title_full |
Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope |
title_fullStr |
Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope |
title_full_unstemmed |
Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope |
title_sort |
measurements of secodary cosmic microwave background anisotropies with the south pole telescope |
publisher |
eScholarship, University of California |
publishDate |
2010 |
url |
https://escholarship.org/uc/item/1m21q7w6 |
long_lat |
ENVELOPE(-62.983,-62.983,-64.300,-64.300) |
geographic |
Lambda South Pole |
geographic_facet |
Lambda South Pole |
genre |
South pole |
genre_facet |
South pole |
op_relation |
qt1m21q7w6 https://escholarship.org/uc/item/1m21q7w6 |
op_rights |
public |
_version_ |
1766202457106415616 |
spelling |
ftcdlib:oai:escholarship.org/ark:/13030/qt1m21q7w6 2023-05-15T18:23:02+02:00 Measurements of Secodary Cosmic Microwave Background Anisotropies with the South Pole Telescope Lueker, Martin Van Holzapfel, William L 2010-01-01 application/pdf https://escholarship.org/uc/item/1m21q7w6 en eng eScholarship, University of California qt1m21q7w6 https://escholarship.org/uc/item/1m21q7w6 public Physics Cosmic Microwave Background Large-Scale Structure Millimeter Wave Instrumentation Superconducting Quantum Interference Devices etd 2010 ftcdlib 2020-06-06T07:56:52Z The South Pole Telescope is a 10m millimeter-wavelength telescope for finding galaxy clusters via the thermal Sunyaev-Zel'dovich (tSZ) effect. This thesis is divided into two parts. The first part describes the development of the kilopixel SPT-SZ receiver and the frequency-domain multiplexor (fMUX). The second part describes the first SPT power spectrum measurement and the first detection of the tSZ power spectrum. The SPT-SZ focal plane consists of 960 spiderweb coupled transition-edge sensors. Due to strong electro-thermal feedback, these devices have good sensitivity and linearity, though risk spontaneous oscillations. Adding heat capacity to these devices can ensure stability, so long as the loopgain, $\mathcal{L}$, is less than $G_\textrm{int}/G_0$, the ratio between the thermal conductances linking the TES to the heat capacity and linking the heat capacity to the bath. I describe as experimental technique for measuring the internal thermal structure of these devices, allowing for rapid sensor evaluation. The fMUX readout system reduces wiring complexity in this receiver by AC-biasing each sensor at a unique frequency and sending signals from multiple bolometers along one pair of wires. The Series SQUID Arrays (SSAs) used to read changes in bolometer current are notably non-linear and extremely sensititve to ambient magnetic fields. The SSAs are housed in compact magnetic shielding modules which reduces their effective area to 80 $\textrm{m}\Phi_0/\textrm{gauss}$. The SSA are fedback with a flux-locked loop to improve their linearity and dynamic range, and decrease their input reactance. The FLL is bandwidth of 1 MHz with a measured loopgain of 10. In the current implementation, this bandwidth is limited between the SQUID input coil and other reactances, which I study in Chapter \ref{chap:fllstab}.In the second part of the thesis I present power spectrum measurements for the first 100~deg$^2$ field observed by the SPT. On angular scales where the primary CMB anisotropy is dominant, $\ell \lesssim 3000$, the SPT power spectrum is consistent with the standard $\Lambda$CDM cosmology. On smaller scales, we see strong evidence for a point source contribution, consisteThe South Pole Telescope is a 10m millimeter-wavelength telescope for finding galaxy clusters via the thermal Sunyaev-Zel'dovich (tSZ) effect. This thesis is divided into two parts. The first part describes the development of the kilopixel SPT-SZ receiver and the frequency-domain multiplexor (fMUX). The second part describes the first SPT power spectrum measurement and the first detection of the tSZ power spectrum. The SPT-SZ focal plane consists of 960 spiderweb coupled transition-edge sensors. Due to strong electro-thermal feedback, these devices have good sensitivity and linearity, though risk spontaneous oscillations. Adding heat capacity to these devices can ensure stability, so long as the loopgain, $\mathcal{L}$, is less than $G_\textrm{int}/G_0$, the ratio between the thermal conductances linking the TES to the heat capacity and linking the heat capacity to the bath. I describe as experimental technique for measuring the internal thermal structure of these devices, allowing for rapid sensor evaluation. The fMUX readout system reduces wiring complexity in this receiver by AC-biasing each sensor at a unique frequency and sending signals from multiple bolometers along one pair of wires. The Series SQUID Arrays (SSAs) used to read changes in bolometer current are notably non-linear and extremely sensititve to ambient magnetic fields. The SSAs are housed in compact magnetic shielding modules which reduces their effective area to 80 $\textrm{m}\Phi_0/\textrm{gauss}$. The SSA are fedback with a flux-locked loop to improve their linearity and dynamic range, and decrease their input reactance. The FLL is bandwidth of 1 MHz with a measured loopgain of 10. In the current implementation, this bandwidth is limited between the SQUID input coil and other reactances, which I study in Chapter \ref{chap:fllstab}.In the second part of the thesis I present power spectrum measurements for the first 100~deg$^2$ field observed by the SPT. On angular scales where the primary CMB anisotropy is dominant, $\ell \lesssim 3000$, the SPT power spectrum is consistent with the standard $\Lambda$CDM cosmology. On smaller scales, we see strong evidence for a point source contribution, consistent with a population of dusty, star-forming galaxies. I combine the 150 and 220$\,$GHz data to remove the majority of the point source power, and use the point source subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at $2.6\,\sigma$. At $\ell=3000$, the SZ power in the subtracted bandpowers is $4.2\,$$\pm$$\,1.5\, \mu\rm{K}^2$, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. t with a population of dusty, star-forming galaxies. I combine the 150 and 220$\,$GHz data to remove the majority of the point source power, and use the point source subtracted spectrum to detect Sunyaev-Zel'dovich (SZ) power at $2.6\,\sigma$. At $\ell=3000$, the SZ power in the subtracted bandpowers is $4.2\,$$\pm$$\,1.5\, \mu\rm{K}^2$, which is significantly lower than the power predicted by a fiducial model using WMAP5 cosmological parameters. Other/Unknown Material South pole University of California: eScholarship Lambda ENVELOPE(-62.983,-62.983,-64.300,-64.300) South Pole |