Photometric analysis in the Kepler Science Operations Center pipeline
Identifieur interne :
000134 ( PascalFrancis/Curation );
précédent :
000133;
suivant :
000135
Photometric analysis in the Kepler Science Operations Center pipeline
Auteurs : Joseph D. Twicken [
États-Unis] ;
Bruce D. Clarke [
États-Unis] ;
Stephen T. Bryson [
États-Unis] ;
Peter Tenenbaum [
États-Unis] ;
Hayley Wu [
États-Unis] ;
Jon M. Jenkins [
États-Unis] ;
Forrest Girouard [
États-Unis] ;
Todd C. Klaus [
États-Unis]
Source :
-
Proceedings of SPIE, the International Society for Optical Engineering [ 0277-786X ] ; 2010.
RBID : Pascal:11-0004562
Descripteurs français
- Pascal (Inist)
- Processeur pipeline,
Composant logiciel,
Traitement pipeline,
Série temporelle,
Photométrie,
Système sur puce,
Centre gravité,
Nettoyage,
Vol,
Caractéristique temporelle,
Barycentre,
Date,
Archive,
Télescope,
Application spatiale.
- Wicri :
English descriptors
- KwdEn :
- Archive,
Barycenter,
Center of mass,
Cleaning,
Date,
Flight,
Photometry,
Pipeline processing,
Pipeline processor,
Software component,
Space application,
System on a chip,
Telescope,
Time curve,
Time series.
Abstract
We describe the Photometric Analysis (PA) software component and its context in the Kepler Science Operations Center (SOC) Science Processing Pipeline. The primary tasks of this module are to compute the photometric flux and photocenters (centroids) for over 160,000 long cadence (-thirty minute) and 512 short cadence (˜one minute) stellar targets from the calibrated pixels in their respective apertures. We discuss science algorithms for long and short cadence PA: cosmic ray cleaning; background estimation and removal; aperture photometry; and flux-weighted centroiding. We discuss the end-to-end propagation of uncertainties for the science algorithms. Finally, we present examples of photometric apertures, raw flux light curves, and centroid time series from Kepler flight data. PA light curves, centroid time series, and barycentric timestamp corrections are exported to the Multi-mission Archive at Space Telescope [Science Institute] (MAST) and are made available to the general public in accordance with the NASA/Kepler data release policy.
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| A08 | 01 | 1 | ENG | @1 Photometric analysis in the Kepler Science Operations Center pipeline |
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| A12 | 02 | 1 | | @1 BRIDGER (Alan) @9 ed. |
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| A14 | 01 | | | @1 SETI Institute/NASA Ames Research Center, MS 244-30 @2 Moffett Field, CA, 94035-1000 @3 USA @Z 1 aut. @Z 2 aut. @Z 4 aut. @Z 5 aut. @Z 6 aut. |
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| A14 | 02 | | | @1 NASA Ames Research Center, MS 244-30 @2 Moffett Field, CA, 94035-1000 @3 USA @Z 3 aut. |
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| C01 | 01 | | ENG | @0 We describe the Photometric Analysis (PA) software component and its context in the Kepler Science Operations Center (SOC) Science Processing Pipeline. The primary tasks of this module are to compute the photometric flux and photocenters (centroids) for over 160,000 long cadence (-thirty minute) and 512 short cadence (˜one minute) stellar targets from the calibrated pixels in their respective apertures. We discuss science algorithms for long and short cadence PA: cosmic ray cleaning; background estimation and removal; aperture photometry; and flux-weighted centroiding. We discuss the end-to-end propagation of uncertainties for the science algorithms. Finally, we present examples of photometric apertures, raw flux light curves, and centroid time series from Kepler flight data. PA light curves, centroid time series, and barycentric timestamp corrections are exported to the Multi-mission Archive at Space Telescope [Science Institute] (MAST) and are made available to the general public in accordance with the NASA/Kepler data release policy. |
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| C03 | 01 | X | SPA | @0 Procesador oleoducto @5 06 |
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| C03 | 02 | X | FRE | @0 Composant logiciel @5 07 |
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| C03 | 02 | X | ENG | @0 Software component @5 07 |
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| C03 | 02 | X | SPA | @0 Componente logicial @5 07 |
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| C03 | 03 | 3 | FRE | @0 Traitement pipeline @5 08 |
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| C03 | 03 | 3 | ENG | @0 Pipeline processing @5 08 |
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| C03 | 04 | X | FRE | @0 Série temporelle @5 09 |
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| C03 | 04 | X | ENG | @0 Time series @5 09 |
|---|
| C03 | 04 | X | SPA | @0 Serie temporal @5 09 |
|---|
| C03 | 05 | X | FRE | @0 Photométrie @5 18 |
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| C03 | 05 | X | ENG | @0 Photometry @5 18 |
|---|
| C03 | 05 | X | SPA | @0 Fotometría @5 18 |
|---|
| C03 | 06 | X | FRE | @0 Système sur puce @5 19 |
|---|
| C03 | 06 | X | ENG | @0 System on a chip @5 19 |
|---|
| C03 | 06 | X | SPA | @0 Sistema sobre pastilla @5 19 |
|---|
| C03 | 07 | X | FRE | @0 Centre gravité @5 20 |
|---|
| C03 | 07 | X | ENG | @0 Center of mass @5 20 |
|---|
| C03 | 07 | X | SPA | @0 Centro gravitacional @5 20 |
|---|
| C03 | 08 | X | FRE | @0 Nettoyage @5 21 |
|---|
| C03 | 08 | X | ENG | @0 Cleaning @5 21 |
|---|
| C03 | 08 | X | SPA | @0 Limpieza @5 21 |
|---|
| C03 | 09 | X | FRE | @0 Vol @5 22 |
|---|
| C03 | 09 | X | ENG | @0 Flight @5 22 |
|---|
| C03 | 09 | X | SPA | @0 Vuelo @5 22 |
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| C03 | 10 | X | FRE | @0 Caractéristique temporelle @5 23 |
|---|
| C03 | 10 | X | ENG | @0 Time curve @5 23 |
|---|
| C03 | 10 | X | SPA | @0 Característica temporal @5 23 |
|---|
| C03 | 11 | X | FRE | @0 Barycentre @5 24 |
|---|
| C03 | 11 | X | ENG | @0 Barycenter @5 24 |
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| C03 | 11 | X | SPA | @0 Baricentro @5 24 |
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| C03 | 12 | X | FRE | @0 Date @5 25 |
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| C03 | 12 | X | ENG | @0 Date @5 25 |
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| C03 | 12 | X | SPA | @0 Fecha @5 25 |
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| C03 | 13 | X | FRE | @0 Archive @5 26 |
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| C03 | 13 | X | ENG | @0 Archive @5 26 |
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| C03 | 13 | X | SPA | @0 Archivo @5 26 |
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| C03 | 14 | X | FRE | @0 Télescope @5 27 |
|---|
| C03 | 14 | X | ENG | @0 Telescope @5 27 |
|---|
| C03 | 14 | X | SPA | @0 Telescopio @5 27 |
|---|
| C03 | 15 | X | FRE | @0 Application spatiale @5 28 |
|---|
| C03 | 15 | X | ENG | @0 Space application @5 28 |
|---|
| C03 | 15 | X | SPA | @0 Aplicación espacial @5 28 |
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| N21 | | | | @1 003 |
|---|
| N44 | 01 | | | @1 OTO |
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| N82 | | | | @1 OTO |
|---|
|
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| pR |
| A30 | 01 | 1 | ENG | @1 Software and cyberinfrastructure for astronomy @3 San Diego CA USA @4 2010 |
|---|
|
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Le document en format XML
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</affiliation><series><title level="j" type="main">Proceedings of SPIE, the International Society for Optical Engineering</title>
<title level="j" type="abbreviated">Proc. SPIE Int. Soc. Opt. Eng.</title>
<idno type="ISSN">0277-786X</idno>
<imprint><date when="2010">2010</date>
</imprint><seriesStmt><title level="j" type="main">Proceedings of SPIE, the International Society for Optical Engineering</title>
<title level="j" type="abbreviated">Proc. SPIE Int. Soc. Opt. Eng.</title>
<idno type="ISSN">0277-786X</idno>
</seriesStmt><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Archive</term>
<term>Barycenter</term>
<term>Center of mass</term>
<term>Cleaning</term>
<term>Date</term>
<term>Flight</term>
<term>Photometry</term>
<term>Pipeline processing</term>
<term>Pipeline processor</term>
<term>Software component</term>
<term>Space application</term>
<term>System on a chip</term>
<term>Telescope</term>
<term>Time curve</term>
<term>Time series</term>
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<term>Composant logiciel</term>
<term>Traitement pipeline</term>
<term>Série temporelle</term>
<term>Photométrie</term>
<term>Système sur puce</term>
<term>Centre gravité</term>
<term>Nettoyage</term>
<term>Vol</term>
<term>Caractéristique temporelle</term>
<term>Barycentre</term>
<term>Date</term>
<term>Archive</term>
<term>Télescope</term>
<term>Application spatiale</term>
</keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Vol</term>
</keywords><front><div type="abstract" xml:lang="en">We describe the Photometric Analysis (PA) software component and its context in the Kepler Science Operations Center (SOC) Science Processing Pipeline. The primary tasks of this module are to compute the photometric flux and photocenters (centroids) for over 160,000 long cadence (-thirty minute) and 512 short cadence (˜one minute) stellar targets from the calibrated pixels in their respective apertures. We discuss science algorithms for long and short cadence PA: cosmic ray cleaning; background estimation and removal; aperture photometry; and flux-weighted centroiding. We discuss the end-to-end propagation of uncertainties for the science algorithms. Finally, we present examples of photometric apertures, raw flux light curves, and centroid time series from Kepler flight data. PA light curves, centroid time series, and barycentric timestamp corrections are exported to the Multi-mission Archive at Space Telescope [Science Institute] (MAST) and are made available to the general public in accordance with the NASA/Kepler data release policy.</div>
</front><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0277-786X</s0>
</fA01><fA02 i1="01"><s0>PSISDG</s0>
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</fA06><fA08 i1="01" i2="1" l="ENG"><s1>Photometric analysis in the Kepler Science Operations Center pipeline</s1>
</fA08><fA09 i1="01" i2="1" l="ENG"><s1>Software and cyberinfrastructure for astronomy : 27-30 June 2010, San Diego, California, United States</s1>
</fA09><fA11 i1="01" i2="1"><s1>TWICKEN (Joseph D.)</s1>
</fA11><fA11 i1="02" i2="1"><s1>CLARKE (Bruce D.)</s1>
</fA11><fA11 i1="03" i2="1"><s1>BRYSON (Stephen T.)</s1>
</fA11><fA11 i1="04" i2="1"><s1>TENENBAUM (Peter)</s1>
</fA11><fA11 i1="05" i2="1"><s1>WU (Hayley)</s1>
</fA11><fA11 i1="06" i2="1"><s1>JENKINS (Jon M.)</s1>
</fA11><fA11 i1="07" i2="1"><s1>GIROUARD (Forrest)</s1>
</fA11><fA11 i1="08" i2="1"><s1>KLAUS (Todd C.)</s1>
</fA11><fA12 i1="01" i2="1"><s1>RADZIWILL (Nicole M.)</s1>
<s9>ed.</s9>
</fA12><fA12 i1="02" i2="1"><s1>BRIDGER (Alan)</s1>
<s9>ed.</s9>
</fA12><fA14 i1="01"><s1>SETI Institute/NASA Ames Research Center, MS 244-30</s1>
<s2>Moffett Field, CA, 94035-1000</s2>
<s3>USA</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
</fA14><fA14 i1="02"><s1>NASA Ames Research Center, MS 244-30</s1>
<s2>Moffett Field, CA, 94035-1000</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
</fA14><fA14 i1="03"><s1>Orbital Sciences Corporation/NASA Ames Research Center, MS 244-30</s1>
<s2>Moffett Field, CA, 94035-1000</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
</fA14><fA18 i1="01" i2="1"><s1>SPIE</s1>
<s3>USA</s3>
<s9>org-cong.</s9>
</fA18><fA18 i1="02" i2="1"><s1>American Astronomical Society</s1>
<s3>USA</s3>
<s9>org-cong.</s9>
</fA18><fA20><s2>774023.1-774023.12</s2>
</fA20><fA21><s1>2010</s1>
</fA21><fA23 i1="01"><s0>ENG</s0>
</fA23><fA25 i1="01"><s1>SPIE</s1>
<s2>Bellingham, Wash.</s2>
</fA25><fA26 i1="01"><s0>978-0-8194-8230-3</s0>
</fA26><fA26 i1="02"><s0>0-8194-8230-7</s0>
</fA26><fA43 i1="01"><s1>INIST</s1>
<s2>21760</s2>
<s5>354000174702880690</s5>
</fA43><fA44><s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44><fA45><s0>19 ref.</s0>
</fA45><fA47 i1="01" i2="1"><s0>11-0004562</s0>
</fA47><fA60><s1>P</s1>
<s2>C</s2>
</fA60><fA64 i1="01" i2="1"><s0>Proceedings of SPIE, the International Society for Optical Engineering</s0>
</fA64><fA66 i1="01"><s0>USA</s0>
</fA66><fC01 i1="01" l="ENG"><s0>We describe the Photometric Analysis (PA) software component and its context in the Kepler Science Operations Center (SOC) Science Processing Pipeline. The primary tasks of this module are to compute the photometric flux and photocenters (centroids) for over 160,000 long cadence (-thirty minute) and 512 short cadence (˜one minute) stellar targets from the calibrated pixels in their respective apertures. We discuss science algorithms for long and short cadence PA: cosmic ray cleaning; background estimation and removal; aperture photometry; and flux-weighted centroiding. We discuss the end-to-end propagation of uncertainties for the science algorithms. Finally, we present examples of photometric apertures, raw flux light curves, and centroid time series from Kepler flight data. PA light curves, centroid time series, and barycentric timestamp corrections are exported to the Multi-mission Archive at Space Telescope [Science Institute] (MAST) and are made available to the general public in accordance with the NASA/Kepler data release policy.</s0>
</fC01><fC02 i1="01" i2="X"><s0>001D02B09</s0>
</fC02><fC03 i1="01" i2="X" l="FRE"><s0>Processeur pipeline</s0>
<s5>06</s5>
</fC03><fC03 i1="01" i2="X" l="ENG"><s0>Pipeline processor</s0>
<s5>06</s5>
</fC03><fC03 i1="01" i2="X" l="SPA"><s0>Procesador oleoducto</s0>
<s5>06</s5>
</fC03><fC03 i1="02" i2="X" l="FRE"><s0>Composant logiciel</s0>
<s5>07</s5>
</fC03><fC03 i1="02" i2="X" l="ENG"><s0>Software component</s0>
<s5>07</s5>
</fC03><fC03 i1="02" i2="X" l="SPA"><s0>Componente logicial</s0>
<s5>07</s5>
</fC03><fC03 i1="03" i2="3" l="FRE"><s0>Traitement pipeline</s0>
<s5>08</s5>
</fC03><fC03 i1="03" i2="3" l="ENG"><s0>Pipeline processing</s0>
<s5>08</s5>
</fC03><fC03 i1="04" i2="X" l="FRE"><s0>Série temporelle</s0>
<s5>09</s5>
</fC03><fC03 i1="04" i2="X" l="ENG"><s0>Time series</s0>
<s5>09</s5>
</fC03><fC03 i1="04" i2="X" l="SPA"><s0>Serie temporal</s0>
<s5>09</s5>
</fC03><fC03 i1="05" i2="X" l="FRE"><s0>Photométrie</s0>
<s5>18</s5>
</fC03><fC03 i1="05" i2="X" l="ENG"><s0>Photometry</s0>
<s5>18</s5>
</fC03><fC03 i1="05" i2="X" l="SPA"><s0>Fotometría</s0>
<s5>18</s5>
</fC03><fC03 i1="06" i2="X" l="FRE"><s0>Système sur puce</s0>
<s5>19</s5>
</fC03><fC03 i1="06" i2="X" l="ENG"><s0>System on a chip</s0>
<s5>19</s5>
</fC03><fC03 i1="06" i2="X" l="SPA"><s0>Sistema sobre pastilla</s0>
<s5>19</s5>
</fC03><fC03 i1="07" i2="X" l="FRE"><s0>Centre gravité</s0>
<s5>20</s5>
</fC03><fC03 i1="07" i2="X" l="ENG"><s0>Center of mass</s0>
<s5>20</s5>
</fC03><fC03 i1="07" i2="X" l="SPA"><s0>Centro gravitacional</s0>
<s5>20</s5>
</fC03><fC03 i1="08" i2="X" l="FRE"><s0>Nettoyage</s0>
<s5>21</s5>
</fC03><fC03 i1="08" i2="X" l="ENG"><s0>Cleaning</s0>
<s5>21</s5>
</fC03><fC03 i1="08" i2="X" l="SPA"><s0>Limpieza</s0>
<s5>21</s5>
</fC03><fC03 i1="09" i2="X" l="FRE"><s0>Vol</s0>
<s5>22</s5>
</fC03><fC03 i1="09" i2="X" l="ENG"><s0>Flight</s0>
<s5>22</s5>
</fC03><fC03 i1="09" i2="X" l="SPA"><s0>Vuelo</s0>
<s5>22</s5>
</fC03><fC03 i1="10" i2="X" l="FRE"><s0>Caractéristique temporelle</s0>
<s5>23</s5>
</fC03><fC03 i1="10" i2="X" l="ENG"><s0>Time curve</s0>
<s5>23</s5>
</fC03><fC03 i1="10" i2="X" l="SPA"><s0>Característica temporal</s0>
<s5>23</s5>
</fC03><fC03 i1="11" i2="X" l="FRE"><s0>Barycentre</s0>
<s5>24</s5>
</fC03><fC03 i1="11" i2="X" l="ENG"><s0>Barycenter</s0>
<s5>24</s5>
</fC03><fC03 i1="11" i2="X" l="SPA"><s0>Baricentro</s0>
<s5>24</s5>
</fC03><fC03 i1="12" i2="X" l="FRE"><s0>Date</s0>
<s5>25</s5>
</fC03><fC03 i1="12" i2="X" l="ENG"><s0>Date</s0>
<s5>25</s5>
</fC03><fC03 i1="12" i2="X" l="SPA"><s0>Fecha</s0>
<s5>25</s5>
</fC03><fC03 i1="13" i2="X" l="FRE"><s0>Archive</s0>
<s5>26</s5>
</fC03><fC03 i1="13" i2="X" l="ENG"><s0>Archive</s0>
<s5>26</s5>
</fC03><fC03 i1="13" i2="X" l="SPA"><s0>Archivo</s0>
<s5>26</s5>
</fC03><fC03 i1="14" i2="X" l="FRE"><s0>Télescope</s0>
<s5>27</s5>
</fC03><fC03 i1="14" i2="X" l="ENG"><s0>Telescope</s0>
<s5>27</s5>
</fC03><fC03 i1="14" i2="X" l="SPA"><s0>Telescopio</s0>
<s5>27</s5>
</fC03><fC03 i1="15" i2="X" l="FRE"><s0>Application spatiale</s0>
<s5>28</s5>
</fC03><fC03 i1="15" i2="X" l="ENG"><s0>Space application</s0>
<s5>28</s5>
</fC03><fC03 i1="15" i2="X" l="SPA"><s0>Aplicación espacial</s0>
<s5>28</s5>
</fC03><fN21><s1>003</s1>
</fN21><fN44 i1="01"><s1>OTO</s1>
</fN44><fN82><s1>OTO</s1>
</fN82><pR><fA30 i1="01" i2="1" l="ENG"><s1>Software and cyberinfrastructure for astronomy</s1>
<s3>San Diego CA USA</s3>
<s4>2010</s4>
</fA30>
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