1 spectroscopic survey of lamost yongheng zhao (national astronomical observatories of china) on...
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Spectroscopic survey of LAMOST
Yongheng Zhao(National Astronomical Observatories of China)
On behalf of the LAMOST operation team
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Outline
LAMOST Spectroscopic Survey of LAMOST Spectra & stellar parameters LAMOST Sciences Summary
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Structure of LAMOST
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1997-2008: Construction2009 – 2011: Commissioning Oct. 2011 – June 2012: Pilot surveySep. 2012 – June 2017: Regular survey
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Commissioning stage
June 2009 – Sep. 2011 2/3 slit (R=1800) Progress in fiber positioning Realistic survey limiting magnitude: r = 17.8
Scientific test observations M31 area
Planetary nebulae Kinematics + populations Quasars beyond
Quasars Metal-poor stars
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Spectra of stars
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Emission line galaxy
r=19.90 z=0.06
Emission line galaxy
r=19.90 z=0.09
Quasar
r=19.14 z=2.40
K3 star
r=19.40
WD star
r=18.18
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LAMOST Survey
Pilot Survey 2011.10-2012.6
PDR: 2012.8
Regular survey 1st year: 2012.9-2013.6
DR1 (2013.9) 2nd year: 2013.9-2014.6
DR2 (2014.12) 3rd year: 2014.9-2015.6
1st year
2nd year
pilot
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Spectral data
PDR(1 yrs)
DR1(2 yrs)
DR2(3 yrs)
Spectra 717,660 2,204,860 4,158,038
stars 648,820 1,944,406 3,796,583
galaxies 2,723 12,082 37,849
quasars 621 5,017 9,495
Stars (S/N>10) 547,868 1,721,796 3,231,240
AFGK parameters 373,481 1,085,404 2,165,200
1 M spectra / year
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Stellar parameters (2,165,200 spectra in DR2)
Exceeding the total number of currently known database;
Largest stellar parameter catalogue so far
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LAMOST光谱巡天进展
Footprint of 455 million spectra of SNRs > 10 collected by 2015.06
单位(万)
观测截止日期 总光谱数 恒星光谱数 SNR > 10恒星光谱数 有参数恒星光谱数 发布 /释放日期
DR0 20120617 92 82 61 39 2012.08/2012.08
DR1 20130603 220 194 180 106 2013.09/2015.03
DR2 20140603 414 378 322 221 2014.12/2016.07
DR3 20150602 574 520 455 296 2015.12/2017.07
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质量控制
光谱数 达标率( SNRs > 10)
先导巡天( 2011—2012 ) 573,227 48.4%常规巡天第一年( 2012—2013 ) 1,243,478 62.7%常规巡天第二年( 2013—2014 ) 1,326,700 72.4%常规巡天第三年( 2014—2015 ) 1,304,925 71.8%
常规巡天第一年( 2012—2013) 常规巡天第二年( 2013—2014) 常规巡天第 3年( 2014—2015)
反银心方向巡天B、M 面板观测源和达标源星等分布比较
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2D pipeline: sky subtraction
Comparison with SDSS:
•Better in red band for same S/N
760 and 860 nm where large number of sky emission lines
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Flux calibration: spectral accuracy
Green solid line: median Green dashed lines: std.dev Red solid lines: examples
Comparisons of multi-observations as well as with photometry show the final SEDs have an accuracy better than 12%.
Xiang et al. 2014a, to be submitted
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Comparison of LAMOST and SDSS spectra
Low-extinction regions High-extinction regions
Black: LAMOST Red: SDSS DR7
Our approach of flux calibration yields better, more realistic SEDs than SDSS for high extinction fields.
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Comparison with external data: Teff, log g, [Fe/H]
Teff, log g and [Fe/H] are accurate to ~ 150 K, ~ 0.25 dex, 0.15 dex for FGK stars, respectively.
The results of SDSS DR9 are systematically −105 K, 0.24 dex, 0.12 dex lower.
Xiang et al. 2014b, to be submitted
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Comparison with external data: radial velocities
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Scientific papers
48 scientific papers published 38 under processing
Papers with LAMOST data
Papers with SDSS spectral data
PDR DR1
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Scientific results
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White dwarf mass function & birth rate
Rebassa Mansergas et al. in prep.
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Binary fraction in field FGK stars
Yuan et al., to be submittedGao et al., 2014 ApJ Letter
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Based on 66,647 thin disk FGK dwarfs (4200 < Teff < 6800 K, 3.8 < log g < 5.0, e < 0.15) within 600 pc of the Sun.
The largest sample hitherto confirms that VΘ~12km/s. Results from different sub-populations suggest that the local disk is well relaxed
The Local Standard of Rest
Huang et al., 2014a to be submitted
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23Carlin et al., 2013, ApJL
Bulk motions of disk stars
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Metallicity Gradients of the Galaxy
The outer disc shows both radial & vertical metallicity gradients. The radial gradient flattens at |Z| > 1.1 kpc, and so does radial gradient at R > 10 kpc Xiang et al. 2014c, Gong et al. 2014, to be submitted
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Collaboration with Kepler project
62,381 spectra observed 32,462 Kepler stars
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LAMOST Sciences Proposed
Extra-galactic spectroscopic surveyn Galaxy & QSO redshift survey
Stellar spectroscopic survey n Structure of the Galaxy & stellar physics
Cross identification of multi-waveband survey
Present (2/3 slits : R = 500 1800) Galactic survey
Structure & evolution of the Galaxy QSO & galaxy Cross identification of multi-waveband survey
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Spectroscopic surveys
Project aper. FoV fibers spectra timeline
2dF 3.9m 2o 400 250,000 G 1997-2002
6dF 1.2m 6o 150 136,304 S 2002-2004
RAVE 1.2m 6o 150 574,630 S 2006-2013
SDSS-I/II 2.5m 3o 640 1,270,000 G 2000-2008
SDSS-III 2.5m 3o 640 2,000,000 G 2008-2014
LAMOST 4m 5o 4000 5,000,000 S 2012-2017
DESI 3.9m 3o 5000 24,500,000 G 2018 ? -
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Galactic survey ( 2012-2017)
The Milky Way is the only grand-design barred spiral (disk) galaxy that the individual stars can be resolved and studied multi-dimensionally ( 6D phase space + chemical composition).
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SDSS 、 LAMOST & Gaia
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Stellar halo profile
Xu et al. in prep.
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Local dark matter density
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Stellar kinematics
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Scientific goals of the galactic survey
The survey will deliver classification, Vr, Teff, log g, [Fe/H], [α/Fe] for ~5 millions of stars. A magnitude-limited and (statistically) complete sample of ~3 M stars Distributed in a contiguous area Sampling a significant volume of the thin/thick disks and halo
With GAIA data, yield a unique dataset to Study the stellar populations, chemical composition, kinematics and
structure of the thin/thick disks and halo Identify tidal streams & debris of disrupted dwarfs and clusters Probe the gravitational potential and dark matter distribution Map the interstellar extinction as a function of distance Search for rare objects (e.g. stars of peculiar chemical composition or of
hyper-velocities) Ultimately advance our understanding of the assemblage history of the
Milky Way, and of galaxies in general and their regularity and diversity.
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Data policy of LAMOST
Internal release Chinese astronomers International collaborators (with Chinese groups)
DR1 (2013.09) : 1.8 M spectra / 1.0 M parameters DR2 (2014.12): 3.0 M spectra / 2.1 M parameters DR3 (2015.12): 4.5 M spectra / 3.0 M parameters
Public release ( after 1.5 yrs) DR1 (2015.03) : 1.8 M spectra / 1.0 M parameters DR2 (2016.06): 3.0 M spectra / 2.1 M parameters
Collaboration on LAMOST Sciences
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Thank You!