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Cosmology and HI Intensity Mapping /

Podczerwinski, John,

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Cosmology and HI Intensity Mapping /

紀錄類型:	書目-電子資源 : Monograph/item
正題名/作者:	Cosmology and HI Intensity Mapping // John Podczerwinski.
作者:	Podczerwinski, John,
面頁冊數:	1 electronic resource (230 pages)
附註:	Source: Dissertations Abstracts International, Volume: 86-03, Section: B.
Contained By:	Dissertations Abstracts International86-03B.
標題:	Astrophysics. -
電子資源:	https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=31562476
ISBN:	9798384426059

Cosmology and HI Intensity Mapping /
Podczerwinski, John,

Cosmology and HI Intensity Mapping /John Podczerwinski. - 1 electronic resource (230 pages)

Source: Dissertations Abstracts International, Volume: 86-03, Section: B.

This thesis is focused on HI intensity mapping, a proposed method for making three dimensional surveys of the universe. I begin by reviewing basic cosmological theory and common observational techniques such as galaxy surveys and observations of the cosmic microwave background (CMB). I then provide motivation for the use of HI intensity mapping along with a description of how such measurements are performed. I describe my research work, which was focused on developing instrumentation and analysis techniques for HI intensity mapping in the post reionization era of the universe (\uD835\uDC67 < 6). A key goal of such observations is to monitor the baryon acoustic oscillations over a wide range of redshifts, providing information about the evolution of dark energy. My work focused mainly on the design of an ultra-wideband antenna and the development of foreground cleaning techniques. For the antenna project, I created an ultra-wideband design that was optimized with intensity mapping systematic effects in mind. This involved the use of a Vivaldi feed with optimized profile and a deep dish with and an elliptical collar. I also investigated the use of absorbing materials on the feed antenna, which helped mitigate systematic effects but resulted in significantly lower sensitivity. The final antenna design achieved satisfactory levels of spectral smoothness, impedance matching and sensitivity to the 21 cm hydrogen line. In simulations, I found that my design efforts helped reduce coupling between neighboring antenna elements, though not to the level desired. For the foreground cleaning projects, I investigated the use of Karhunen-Loeve transforms in both map-space and visibility space. My project was the first to incorporate a KL transform in map space. This work, however, did not seem to provide a substantial improvement over other available methods. I then conclude by discussing ideas on the future of HI intensity mapping.

English

ISBN: 9798384426059Subjects--Topical Terms:

535904
Astrophysics.
Subjects--Index Terms:

HI intensity mapping

Cosmology and HI Intensity Mapping /
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520 $a This thesis is focused on HI intensity mapping, a proposed method for making three dimensional surveys of the universe. I begin by reviewing basic cosmological theory and common observational techniques such as galaxy surveys and observations of the cosmic microwave background (CMB). I then provide motivation for the use of HI intensity mapping along with a description of how such measurements are performed. I describe my research work, which was focused on developing instrumentation and analysis techniques for HI intensity mapping in the post reionization era of the universe (\uD835\uDC67 < 6). A key goal of such observations is to monitor the baryon acoustic oscillations over a wide range of redshifts, providing information about the evolution of dark energy. My work focused mainly on the design of an ultra-wideband antenna and the development of foreground cleaning techniques. For the antenna project, I created an ultra-wideband design that was optimized with intensity mapping systematic effects in mind. This involved the use of a Vivaldi feed with optimized profile and a deep dish with and an elliptical collar. I also investigated the use of absorbing materials on the feed antenna, which helped mitigate systematic effects but resulted in significantly lower sensitivity. The final antenna design achieved satisfactory levels of spectral smoothness, impedance matching and sensitivity to the 21 cm hydrogen line. In simulations, I found that my design efforts helped reduce coupling between neighboring antenna elements, though not to the level desired. For the foreground cleaning projects, I investigated the use of Karhunen-Loeve transforms in both map-space and visibility space. My project was the first to incorporate a KL transform in map space. This work, however, did not seem to provide a substantial improvement over other available methods. I then conclude by discussing ideas on the future of HI intensity mapping.
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650 4 $a Astrophysics. $3 535904
650 4 $a Physics. $3 516296
650 4 $a Astronomy. $3 517668
650 4 $a Theoretical physics. $3 2144760
653 $a HI intensity mapping
653 $a Cosmic microwave background
653 $a Galaxy surveys
653 $a Spectral smoothness
653 $a Ultra-wideband
690 $a 0596
690 $a 0606
690 $a 0605
690 $a 0753
710 2 $a The University of Wisconsin - Madison. $b Physics. $e degree granting institution. $3 3816229
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790 $a 0262
791 $a Ph.D.
792 $a 2024
856 4 0 $u https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=31562476