Serveur d'exploration Cyberinfrastructure

Attention, ce site est en cours de développement !
Attention, site généré par des moyens informatiques à partir de corpus bruts.
Les informations ne sont donc pas validées.

Calibration of LAMOST Spectral Analysis

Identifieur interne : 000146 ( PascalFrancis/Checkpoint ); précédent : 000145; suivant : 000147

Calibration of LAMOST Spectral Analysis

Auteurs : F. F. Wang [République populaire de Chine] ; A. L. Luo [République populaire de Chine] ; Y. H. Zhao [République populaire de Chine]

Source :

RBID : Pascal:11-0070247

Descripteurs français

English descriptors

Abstract

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) started its test observation in the past year (2009). The spectroscopic reduction and analysis software is avalible for the determination of spectral classifications, redshifts and the fundamental stellar atmospheric parameters (effective temperature, surface gravity, and metallicity). The analysis results show some systematic errors that need to be calibrated. We will present the results of these calibrations in this paper. Comparing with known objects observed by the Sloan Digital Sky Survey (SDSS), we can calibrate the redshifts of LAMOST galaxy spectra. Results from external spectral analysis software, the Sloan Extension for Galactic Exploration and Understanding (SEGUE) Stellar Parameter Pipeline (SSPP), will be applied to check the accuracy of the radial velocity (RV) measurement. Meanwhile, the atmospheric parameters of LAMOST stellar spectra are compared with known objects for calibrating our spectral analysis.


Affiliations:


Links toward previous steps (curation, corpus...)


Links to Exploration step

Pascal:11-0070247

Le document en format XML

<record>
<TEI>
<teiHeader>
<fileDesc>
<titleStmt>
<title xml:lang="en" level="a">Calibration of LAMOST Spectral Analysis</title>
<author>
<name sortKey="Wang, F F" sort="Wang, F F" uniqKey="Wang F" first="F. F." last="Wang">F. F. Wang</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Chaoyang District, Beijing, 100012</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Beijing, 100012</wicri:noRegion>
</affiliation>
</author>
<author>
<name sortKey="Luo, A L" sort="Luo, A L" uniqKey="Luo A" first="A. L." last="Luo">A. L. Luo</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Chaoyang District, Beijing, 100012</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Beijing, 100012</wicri:noRegion>
</affiliation>
</author>
<author>
<name sortKey="Zhao, Y H" sort="Zhao, Y H" uniqKey="Zhao Y" first="Y. H." last="Zhao">Y. H. Zhao</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Chaoyang District, Beijing, 100012</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Beijing, 100012</wicri:noRegion>
</affiliation>
</author>
</titleStmt>
<publicationStmt>
<idno type="wicri:source">INIST</idno>
<idno type="inist">11-0070247</idno>
<date when="2010">2010</date>
<idno type="stanalyst">PASCAL 11-0070247 INIST</idno>
<idno type="RBID">Pascal:11-0070247</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">000046</idno>
<idno type="wicri:Area/PascalFrancis/Curation">000199</idno>
<idno type="wicri:Area/PascalFrancis/Checkpoint">000146</idno>
</publicationStmt>
<sourceDesc>
<biblStruct>
<analytic>
<title xml:lang="en" level="a">Calibration of LAMOST Spectral Analysis</title>
<author>
<name sortKey="Wang, F F" sort="Wang, F F" uniqKey="Wang F" first="F. F." last="Wang">F. F. Wang</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Chaoyang District, Beijing, 100012</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Beijing, 100012</wicri:noRegion>
</affiliation>
</author>
<author>
<name sortKey="Luo, A L" sort="Luo, A L" uniqKey="Luo A" first="A. L." last="Luo">A. L. Luo</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Chaoyang District, Beijing, 100012</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Beijing, 100012</wicri:noRegion>
</affiliation>
</author>
<author>
<name sortKey="Zhao, Y H" sort="Zhao, Y H" uniqKey="Zhao Y" first="Y. H." last="Zhao">Y. H. Zhao</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Chaoyang District, Beijing, 100012</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
<country>République populaire de Chine</country>
<wicri:noRegion>Beijing, 100012</wicri:noRegion>
</affiliation>
</author>
</analytic>
<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>
</series>
</biblStruct>
</sourceDesc>
<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>
</fileDesc>
<profileDesc>
<textClass>
<keywords scheme="KwdEn" xml:lang="en">
<term>Astrophysics</term>
<term>Bias</term>
<term>Calibration</term>
<term>Classification</term>
<term>Cosmology</term>
<term>Gravity</term>
<term>Meteorology</term>
<term>Milky Way</term>
<term>Pipeline processor</term>
<term>Pipelines</term>
<term>Spectral analysis</term>
<term>Surface temperature</term>
<term>Velocity measurement</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr">
<term>Classification</term>
<term>Cosmologie</term>
<term>Processeur pipeline</term>
<term>Astrophysique</term>
<term>Météorologie</term>
<term>Température superficielle</term>
<term>Gravité</term>
<term>Voie lactée</term>
<term>Etalonnage</term>
<term>Analyse spectrale</term>
<term>Erreur systématique</term>
<term>Pipeline</term>
<term>Mesure vitesse</term>
</keywords>
<keywords scheme="Wicri" type="topic" xml:lang="fr">
<term>Classification</term>
<term>Cosmologie</term>
<term>Météorologie</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front>
<div type="abstract" xml:lang="en">The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) started its test observation in the past year (2009). The spectroscopic reduction and analysis software is avalible for the determination of spectral classifications, redshifts and the fundamental stellar atmospheric parameters (effective temperature, surface gravity, and metallicity). The analysis results show some systematic errors that need to be calibrated. We will present the results of these calibrations in this paper. Comparing with known objects observed by the Sloan Digital Sky Survey (SDSS), we can calibrate the redshifts of LAMOST galaxy spectra. Results from external spectral analysis software, the Sloan Extension for Galactic Exploration and Understanding (SEGUE) Stellar Parameter Pipeline (SSPP), will be applied to check the accuracy of the radial velocity (RV) measurement. Meanwhile, the atmospheric parameters of LAMOST stellar spectra are compared with known objects for calibrating our spectral analysis.</div>
</front>
</TEI>
<inist>
<standard h6="B">
<pA>
<fA01 i1="01" i2="1">
<s0>0277-786X</s0>
</fA01>
<fA02 i1="01">
<s0>PSISDG</s0>
</fA02>
<fA03 i2="1">
<s0>Proc. SPIE Int. Soc. Opt. Eng.</s0>
</fA03>
<fA05>
<s2>7740</s2>
</fA05>
<fA06>
<s3>p. 2</s3>
</fA06>
<fA08 i1="01" i2="1" l="ENG">
<s1>Calibration of LAMOST Spectral Analysis</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>WANG (F. F.)</s1>
</fA11>
<fA11 i1="02" i2="1">
<s1>LUO (A. L.)</s1>
</fA11>
<fA11 i1="03" i2="1">
<s1>ZHAO (Y. H.)</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>National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road</s1>
<s2>Chaoyang District, Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</fA14>
<fA14 i1="02">
<s1>Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences</s1>
<s2>Beijing, 100012</s2>
<s3>CHN</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 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>774031.1-774031.9</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>354000174702880990</s5>
</fA43>
<fA44>
<s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45>
<s0>12 ref.</s0>
</fA45>
<fA47 i1="01" i2="1">
<s0>11-0070247</s0>
</fA47>
<fA60>
<s1>P</s1>
<s2>C</s2>
</fA60>
<fA61>
<s0>A</s0>
</fA61>
<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>The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) started its test observation in the past year (2009). The spectroscopic reduction and analysis software is avalible for the determination of spectral classifications, redshifts and the fundamental stellar atmospheric parameters (effective temperature, surface gravity, and metallicity). The analysis results show some systematic errors that need to be calibrated. We will present the results of these calibrations in this paper. Comparing with known objects observed by the Sloan Digital Sky Survey (SDSS), we can calibrate the redshifts of LAMOST galaxy spectra. Results from external spectral analysis software, the Sloan Extension for Galactic Exploration and Understanding (SEGUE) Stellar Parameter Pipeline (SSPP), will be applied to check the accuracy of the radial velocity (RV) measurement. Meanwhile, the atmospheric parameters of LAMOST stellar spectra are compared with known objects for calibrating our spectral analysis.</s0>
</fC01>
<fC02 i1="01" i2="3">
<s0>001E03A55C</s0>
</fC02>
<fC02 i1="02" i2="3">
<s0>001E03A75M</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE">
<s0>Classification</s0>
<s5>06</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG">
<s0>Classification</s0>
<s5>06</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE">
<s0>Cosmologie</s0>
<s5>07</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG">
<s0>Cosmology</s0>
<s5>07</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE">
<s0>Processeur pipeline</s0>
<s5>08</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG">
<s0>Pipeline processor</s0>
<s5>08</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA">
<s0>Procesador oleoducto</s0>
<s5>08</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE">
<s0>Astrophysique</s0>
<s5>18</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG">
<s0>Astrophysics</s0>
<s5>18</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE">
<s0>Météorologie</s0>
<s5>19</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG">
<s0>Meteorology</s0>
<s5>19</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE">
<s0>Température superficielle</s0>
<s5>20</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG">
<s0>Surface temperature</s0>
<s5>20</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA">
<s0>Temperatura superficial</s0>
<s5>20</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE">
<s0>Gravité</s0>
<s5>21</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG">
<s0>Gravity</s0>
<s5>21</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE">
<s0>Voie lactée</s0>
<s5>22</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG">
<s0>Milky Way</s0>
<s5>22</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE">
<s0>Etalonnage</s0>
<s5>23</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG">
<s0>Calibration</s0>
<s5>23</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE">
<s0>Analyse spectrale</s0>
<s5>24</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG">
<s0>Spectral analysis</s0>
<s5>24</s5>
</fC03>
<fC03 i1="11" i2="X" l="FRE">
<s0>Erreur systématique</s0>
<s5>25</s5>
</fC03>
<fC03 i1="11" i2="X" l="ENG">
<s0>Bias</s0>
<s5>25</s5>
</fC03>
<fC03 i1="11" i2="X" l="SPA">
<s0>Error sistemático</s0>
<s5>25</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE">
<s0>Pipeline</s0>
<s5>26</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG">
<s0>Pipelines</s0>
<s5>26</s5>
</fC03>
<fC03 i1="13" i2="3" l="FRE">
<s0>Mesure vitesse</s0>
<s5>27</s5>
</fC03>
<fC03 i1="13" i2="3" l="ENG">
<s0>Velocity measurement</s0>
<s5>27</s5>
</fC03>
<fN21>
<s1>045</s1>
</fN21>
<fN44 i1="01">
<s1>OTO</s1>
</fN44>
<fN82>
<s1>OTO</s1>
</fN82>
</pA>
<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>
</pR>
</standard>
</inist>
<affiliations>
<list>
<country>
<li>République populaire de Chine</li>
</country>
</list>
<tree>
<country name="République populaire de Chine">
<noRegion>
<name sortKey="Wang, F F" sort="Wang, F F" uniqKey="Wang F" first="F. F." last="Wang">F. F. Wang</name>
</noRegion>
<name sortKey="Luo, A L" sort="Luo, A L" uniqKey="Luo A" first="A. L." last="Luo">A. L. Luo</name>
<name sortKey="Luo, A L" sort="Luo, A L" uniqKey="Luo A" first="A. L." last="Luo">A. L. Luo</name>
<name sortKey="Wang, F F" sort="Wang, F F" uniqKey="Wang F" first="F. F." last="Wang">F. F. Wang</name>
<name sortKey="Zhao, Y H" sort="Zhao, Y H" uniqKey="Zhao Y" first="Y. H." last="Zhao">Y. H. Zhao</name>
<name sortKey="Zhao, Y H" sort="Zhao, Y H" uniqKey="Zhao Y" first="Y. H." last="Zhao">Y. H. Zhao</name>
</country>
</tree>
</affiliations>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Ticri/CIDE/explor/CyberinfraV1/Data/PascalFrancis/Checkpoint
HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 000146 | SxmlIndent | more

Ou

HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Checkpoint/biblio.hfd -nk 000146 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Ticri/CIDE
   |area=    CyberinfraV1
   |flux=    PascalFrancis
   |étape=   Checkpoint
   |type=    RBID
   |clé=     Pascal:11-0070247
   |texte=   Calibration of LAMOST Spectral Analysis
}}

Wicri

This area was generated with Dilib version V0.6.25.
Data generation: Thu Oct 27 09:30:58 2016. Site generation: Sun Mar 10 23:08:40 2024