CyberinfraV1, PascalFrancis, Corpus, bibRecord, 000080

Selecting Pixels for Kepler Downlink

Identifieur interne : 000080 ( PascalFrancis/Corpus ); précédent : 000079; suivant : 000081

Selecting Pixels for Kepler Downlink

Auteurs : Stephen T. Bryson ; Jon M. Jenkins ; Todd C. Klaus ; Miles T. Cote ; Elisa V. Quintana ; Jennifer R. Hall ; Khadeejah Ibrahim ; Hema Chandrasekaran ; Douglas A. Caldwell ; Jeffrey E. Van Cleve ; Michael R. Haas

Source :

Proceedings of SPIE, the International Society for Optical Engineering [ 0277-786X ] ; 2010.

RBID : Pascal:11-0006805

Descripteurs français

Pascal (Inist)
- Largeur bande, Spationef, Brillance, Rapport signal bruit.

English descriptors

KwdEn :
- Bandwidth, Brightness, Signal to noise ratio, Spacecraft.

Abstract

The Kepler mission monitors ˜ 165, 000 stellar targets using 42 2200 x 1024 pixel CCDs. Onboard storage and bandwidth constraints prevent the storage and downlink of all 96 million pixels per 30-minute cadence, so the Kepler spacecraft downlinks a specified collection of pixels for each target. These pixels are selected by considering the object brightness, background and the signal-to-noise in each pixel, and maximizing the signal-to-noise ratio of the target. This paper describes pixel selection, creation of spacecraft apertures that efficiently capture selected pixels, and aperture assignment to a target. Engineering apertures, short-cadence targets and custom-specified shapes are discussed.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A02	`01`			`@0 PSISDG`
A03		`1`		`@0 Proc. SPIE Int. Soc. Opt. Eng.`
A05				`@2 7740`
A06				`@3 p. 2`
A08	`01`	`1`	`ENG`	`@1 Selecting Pixels for Kepler Downlink`
A09	`01`	`1`	`ENG`	`@1 Software and cyberinfrastructure for astronomy : 27-30 June 2010, San Diego, California, United States`
A11	`01`	`1`		`@1 BRYSON (Stephen T.)`
A11	`02`	`1`		`@1 JENKINS (Jon M.)`
A11	`03`	`1`		`@1 KLAUS (Todd C.)`
A11	`04`	`1`		`@1 COTE (Miles T.)`
A11	`05`	`1`		`@1 QUINTANA (Elisa V.)`
A11	`06`	`1`		`@1 HALL (Jennifer R.)`
A11	`07`	`1`		`@1 IBRAHIM (Khadeejah)`
A11	`08`	`1`		`@1 CHANDRASEKARAN (Hema)`
A11	`09`	`1`		`@1 CALDWELL (Douglas A.)`
A11	`10`	`1`		`@1 VAN CLEVE (Jeffrey E.)`
A11	`11`	`1`		`@1 HAAS (Michael R.)`
A12	`01`	`1`		`@1 RADZIWILL (Nicole M.) @9 ed.`
A12	`02`	`1`		`@1 BRIDGER (Alan) @9 ed.`
A14	`01`			`@1 NASA Ames Research Center, M/S 244-30 @2 Moffett Field, CA 94305 @3 USA @Z 1 aut. @Z 4 aut. @Z 11 aut.`
A14	`02`			`@1 SETI Institute/NASA Ames Research Center, M/S 244-30 @2 Moffett Field, CA 94305 @3 USA @Z 2 aut. @Z 5 aut. @Z 9 aut. @Z 10 aut.`
A14	`03`			`@1 Orbital Sciences Corporation/NASA Ames Research Center, M/S 244-30 @2 Moffett Field, CA 94305 @3 USA @Z 3 aut. @Z 6 aut. @Z 7 aut.`
A14	`04`			`@1 Lawrence Livermore National Laboratory, P.O. Box 808, L-478 @2 Livermore, CA-94551 @3 USA @Z 8 aut.`
A18	`01`	`1`		`@1 SPIE @3 USA @9 org-cong.`
A18	`02`	`1`		`@1 American Astronomical Society @3 USA @9 org-cong.`
A20				`@2 77401D.1-77401D.12`
A21				`@1 2010`
A23	`01`			`@0 ENG`
A25	`01`			`@1 SPIE @2 Bellingham, Wash.`
A26	`01`			`@0 978-0-8194-8230-3`
A26	`02`			`@0 0-8194-8230-7`
A43	`01`			`@1 INIST @2 21760 @5 354000174702880460`
A44				`@0 0000 @1 © 2011 INIST-CNRS. All rights reserved.`
A45				`@0 13 ref.`
A47	`01`	`1`		`@0 11-0006805`
A60				`@1 P @2 C`
A61				`@0 A`
A64	`01`	`1`		`@0 Proceedings of SPIE, the International Society for Optical Engineering`
A66	`01`			`@0 USA`
C01	`01`		`ENG`	@0 The Kepler mission monitors ˜ 165, 000 stellar targets using 42 2200 x 1024 pixel CCDs. Onboard storage and bandwidth constraints prevent the storage and downlink of all 96 million pixels per 30-minute cadence, so the Kepler spacecraft downlinks a specified collection of pixels for each target. These pixels are selected by considering the object brightness, background and the signal-to-noise in each pixel, and maximizing the signal-to-noise ratio of the target. This paper describes pixel selection, creation of spacecraft apertures that efficiently capture selected pixels, and aperture assignment to a target. Engineering apertures, short-cadence targets and custom-specified shapes are discussed.
C02	`01`	`X`		`@0 001D02C03`
C03	`01`	`X`	`FRE`	`@0 Largeur bande @5 06`
C03	`01`	`X`	`ENG`	`@0 Bandwidth @5 06`
C03	`01`	`X`	`SPA`	`@0 Anchura banda @5 06`
C03	`02`	`X`	`FRE`	`@0 Spationef @5 18`
C03	`02`	`X`	`ENG`	`@0 Spacecraft @5 18`
C03	`02`	`X`	`SPA`	`@0 Vehículo espacial @5 18`
C03	`03`	`X`	`FRE`	`@0 Brillance @5 19`
C03	`03`	`X`	`ENG`	`@0 Brightness @5 19`
C03	`03`	`X`	`SPA`	`@0 Brillantez @5 19`
C03	`04`	`X`	`FRE`	`@0 Rapport signal bruit @5 23`
C03	`04`	`X`	`ENG`	`@0 Signal to noise ratio @5 23`
C03	`04`	`X`	`SPA`	`@0 Relación señal ruido @5 23`
N21				`@1 003`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

A30	`01`	`1`	`ENG`	`@1 Software and cyberinfrastructure for astronomy @3 San Diego CA USA @4 2010`

Format Inist (serveur)

NO :	PASCAL 11-0006805 INIST
ET :	Selecting Pixels for Kepler Downlink
AU :	BRYSON (Stephen T.); JENKINS (Jon M.); KLAUS (Todd C.); COTE (Miles T.); QUINTANA (Elisa V.); HALL (Jennifer R.); IBRAHIM (Khadeejah); CHANDRASEKARAN (Hema); CALDWELL (Douglas A.); VAN CLEVE (Jeffrey E.); HAAS (Michael R.); RADZIWILL (Nicole M.); BRIDGER (Alan)
AF :	NASA Ames Research Center, M/S 244-30/Moffett Field, CA 94305/Etats-Unis (1 aut., 4 aut., 11 aut.); SETI Institute/NASA Ames Research Center, M/S 244-30/Moffett Field, CA 94305/Etats-Unis (2 aut., 5 aut., 9 aut., 10 aut.); Orbital Sciences Corporation/NASA Ames Research Center, M/S 244-30/Moffett Field, CA 94305/Etats-Unis (3 aut., 6 aut., 7 aut.); Lawrence Livermore National Laboratory, P.O. Box 808, L-478/Livermore, CA-94551/Etats-Unis (8 aut.)
DT :	Publication en série; Congrès; Niveau analytique
SO :	Proceedings of SPIE, the International Society for Optical Engineering; ISSN 0277-786X; Coden PSISDG; Etats-Unis; Da. 2010; Vol. 7740; No. p. 2; 77401D.1-77401D.12; Bibl. 13 ref.
LA :	Anglais
EA :	The Kepler mission monitors ˜ 165, 000 stellar targets using 42 2200 x 1024 pixel CCDs. Onboard storage and bandwidth constraints prevent the storage and downlink of all 96 million pixels per 30-minute cadence, so the Kepler spacecraft downlinks a specified collection of pixels for each target. These pixels are selected by considering the object brightness, background and the signal-to-noise in each pixel, and maximizing the signal-to-noise ratio of the target. This paper describes pixel selection, creation of spacecraft apertures that efficiently capture selected pixels, and aperture assignment to a target. Engineering apertures, short-cadence targets and custom-specified shapes are discussed.
CC :	001D02C03
FD :	Largeur bande; Spationef; Brillance; Rapport signal bruit
ED :	Bandwidth; Spacecraft; Brightness; Signal to noise ratio
SD :	Anchura banda; Vehículo espacial; Brillantez; Relación señal ruido
LO :	INIST-21760.354000174702880460
ID :	11-0006805

Links to Exploration step

Pascal:11-0006805

Le document en format XML

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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Bandwidth</term>
<term>Brightness</term>
<term>Signal to noise ratio</term>
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</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Largeur bande</term>
<term>Spationef</term>
<term>Brillance</term>
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<front><div type="abstract" xml:lang="en">The Kepler mission monitors ˜ 165, 000 stellar targets using 42 2200 x 1024 pixel CCDs. Onboard storage and bandwidth constraints prevent the storage and downlink of all 96 million pixels per 30-minute cadence, so the Kepler spacecraft downlinks a specified collection of pixels for each target. These pixels are selected by considering the object brightness, background and the signal-to-noise in each pixel, and maximizing the signal-to-noise ratio of the target. This paper describes pixel selection, creation of spacecraft apertures that efficiently capture selected pixels, and aperture assignment to a target. Engineering apertures, short-cadence targets and custom-specified shapes are discussed.</div>
</front>
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<fA08 i1="01" i2="1" l="ENG"><s1>Selecting Pixels for Kepler Downlink</s1>
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<fA11 i1="01" i2="1"><s1>BRYSON (Stephen T.)</s1>
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<fA11 i1="02" i2="1"><s1>JENKINS (Jon M.)</s1>
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<fA11 i1="03" i2="1"><s1>KLAUS (Todd C.)</s1>
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<fA11 i1="04" i2="1"><s1>COTE (Miles T.)</s1>
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<fA11 i1="05" i2="1"><s1>QUINTANA (Elisa V.)</s1>
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<fA11 i1="06" i2="1"><s1>HALL (Jennifer R.)</s1>
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<fA11 i1="07" i2="1"><s1>IBRAHIM (Khadeejah)</s1>
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<fA11 i1="08" i2="1"><s1>CHANDRASEKARAN (Hema)</s1>
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<fA11 i1="09" i2="1"><s1>CALDWELL (Douglas A.)</s1>
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<fA11 i1="10" i2="1"><s1>VAN CLEVE (Jeffrey E.)</s1>
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<server><NO>PASCAL 11-0006805 INIST</NO>
<ET>Selecting Pixels for Kepler Downlink</ET>
<AU>BRYSON (Stephen T.); JENKINS (Jon M.); KLAUS (Todd C.); COTE (Miles T.); QUINTANA (Elisa V.); HALL (Jennifer R.); IBRAHIM (Khadeejah); CHANDRASEKARAN (Hema); CALDWELL (Douglas A.); VAN CLEVE (Jeffrey E.); HAAS (Michael R.); RADZIWILL (Nicole M.); BRIDGER (Alan)</AU>
<AF>NASA Ames Research Center, M/S 244-30/Moffett Field, CA 94305/Etats-Unis (1 aut., 4 aut., 11 aut.); SETI Institute/NASA Ames Research Center, M/S 244-30/Moffett Field, CA 94305/Etats-Unis (2 aut., 5 aut., 9 aut., 10 aut.); Orbital Sciences Corporation/NASA Ames Research Center, M/S 244-30/Moffett Field, CA 94305/Etats-Unis (3 aut., 6 aut., 7 aut.); Lawrence Livermore National Laboratory, P.O. Box 808, L-478/Livermore, CA-94551/Etats-Unis (8 aut.)</AF>
<DT>Publication en série; Congrès; Niveau analytique</DT>
<SO>Proceedings of SPIE, the International Society for Optical Engineering; ISSN 0277-786X; Coden PSISDG; Etats-Unis; Da. 2010; Vol. 7740; No. p. 2; 77401D.1-77401D.12; Bibl. 13 ref.</SO>
<LA>Anglais</LA>
<EA>The Kepler mission monitors ˜ 165, 000 stellar targets using 42 2200 x 1024 pixel CCDs. Onboard storage and bandwidth constraints prevent the storage and downlink of all 96 million pixels per 30-minute cadence, so the Kepler spacecraft downlinks a specified collection of pixels for each target. These pixels are selected by considering the object brightness, background and the signal-to-noise in each pixel, and maximizing the signal-to-noise ratio of the target. This paper describes pixel selection, creation of spacecraft apertures that efficiently capture selected pixels, and aperture assignment to a target. Engineering apertures, short-cadence targets and custom-specified shapes are discussed.</EA>
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Selecting Pixels for Kepler Downlink

Selecting Pixels for Kepler Downlink

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