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Enabling Fainter Astronomical Observ...

Hart, Murdock.

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Enabling Fainter Astronomical Observations through Sky Subtraction and Instrumental Performance.

Record Type:	Electronic resources : Monograph/item
Title/Author:	Enabling Fainter Astronomical Observations through Sky Subtraction and Instrumental Performance./
Author:	Hart, Murdock.
Published:	Ann Arbor : ProQuest Dissertations & Theses, : 2018,
Description:	261 p.
Notes:	Source: Dissertations Abstracts International, Volume: 80-10, Section: B.
Contained By:	Dissertations Abstracts International80-10B.
Subject:	Astronomy. -
Online resource:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=13890076
ISBN:	9781392067895

Enabling Fainter Astronomical Observations through Sky Subtraction and Instrumental Performance.
Hart, Murdock.

Enabling Fainter Astronomical Observations through Sky Subtraction and Instrumental Performance. - Ann Arbor : ProQuest Dissertations & Theses, 2018 - 261 p.

Source: Dissertations Abstracts International, Volume: 80-10, Section: B.

Thesis (Ph.D.)--The Johns Hopkins University, 2018.

This item must not be sold to any third party vendors.

The Prime Focus Spectrograph (PFS) is an massively multiplexed fiber fed instrument which will work in the visible to the near infrared (NIR). PFS has three primary science goals in cosmology, extragalactic astronomy, and galactic archeology. For PFS to succeed it will be necessary to subtract the sky background to a precision which has not been achieved before, and to achieve a high instrumental throughput. This thesis begins with an examination of astronomical spectra, and in particular the atmospheric airglow background. The types of sky subtraction errors will be examined, and a method for removing sky subtraction errors is implemented. A deeper analysis of atmospheric airglow is performed using astronomical sky spectra, and its temporal behavior is quantified on multiple time scales. The last part of this thesis will detail the infrastructure to assemble and characterize the charge coupled devices (CCD) and the complimentary metal oxide semi-conductor (CMOS) devices for PFS. I have been able to align the CCD focal plane arrays (FPA) such that their deviation from flatness is less than one half of the given instrumental tolerance. The characterization of these devices has shown that they meet instrumental performance requirements. The vast majority of visible and near infrared astronomical instruments built today and in the near future will leverage the high efficiency and low noise performance of CCDs and CMOS devices to enable science in new parameter spaces.

ISBN: 9781392067895Subjects--Topical Terms:

517668
Astronomy.

Enabling Fainter Astronomical Observations through Sky Subtraction and Instrumental Performance.
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100 1 $a Hart, Murdock. $3 3437977
245 1 0 $a Enabling Fainter Astronomical Observations through Sky Subtraction and Instrumental Performance.
260 1 $a Ann Arbor : $b ProQuest Dissertations & Theses, $c 2018
300 $a 261 p.
500 $a Source: Dissertations Abstracts International, Volume: 80-10, Section: B.
500 $a Publisher info.: Dissertation/Thesis.
500 $a Advisor: McCandliss, Stephan.
502 $a Thesis (Ph.D.)--The Johns Hopkins University, 2018.
506 $a This item must not be sold to any third party vendors.
506 $a This item must not be added to any third party search indexes.
520 $a The Prime Focus Spectrograph (PFS) is an massively multiplexed fiber fed instrument which will work in the visible to the near infrared (NIR). PFS has three primary science goals in cosmology, extragalactic astronomy, and galactic archeology. For PFS to succeed it will be necessary to subtract the sky background to a precision which has not been achieved before, and to achieve a high instrumental throughput. This thesis begins with an examination of astronomical spectra, and in particular the atmospheric airglow background. The types of sky subtraction errors will be examined, and a method for removing sky subtraction errors is implemented. A deeper analysis of atmospheric airglow is performed using astronomical sky spectra, and its temporal behavior is quantified on multiple time scales. The last part of this thesis will detail the infrastructure to assemble and characterize the charge coupled devices (CCD) and the complimentary metal oxide semi-conductor (CMOS) devices for PFS. I have been able to align the CCD focal plane arrays (FPA) such that their deviation from flatness is less than one half of the given instrumental tolerance. The characterization of these devices has shown that they meet instrumental performance requirements. The vast majority of visible and near infrared astronomical instruments built today and in the near future will leverage the high efficiency and low noise performance of CCDs and CMOS devices to enable science in new parameter spaces.
590 $a School code: 0098.
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710 2 $a The Johns Hopkins University. $b Physics and Astronomy. $3 3437978
773 0 $t Dissertations Abstracts International $g 80-10B.
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