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Label Transfer from APOGEE to LAMOST: Precise Stellar Parameters for 450,000 LAMOST Giants

Ho, Anna Y. Q. and Ness, Melissa K. and Hogg, David W. and Rix, Hans-Walter and Liu, Chao and Yang, Fan and Zhang, Yong and Hou, Yonghui and Wang, Yuefei (2017) Label Transfer from APOGEE to LAMOST: Precise Stellar Parameters for 450,000 LAMOST Giants. Astrophysical Journal, 836 (5). pp. 1-15. ISSN 0004-637X.

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In this era of large-scale spectroscopic stellar surveys, measurements of stellar attributes (“labels,” i.e., parameters and abundances) must be made precise and consistent across surveys. Here, we demonstrate that this can be achieved by a data-driven approach to spectral modeling. With The Cannon, we transfer information from the APOGEE survey to determine precise T_(eff), log g, [Fe/H], and [α/M] from the spectra of 450,000 LAMOST giants. The Cannon fits a predictive model for LAMOST spectra using 9952 stars observed in common between the two surveys, taking five labels from APOGEE DR12 as ground truth T_(eff), log g, [Fe/H], [α/M], and K-band extinction A_k. The model is then used to infer T_(eff) , log g, [Fe/H], and [α/M] for 454,180 giants, 20% of the LAMOST DR2 stellar sample. These are the first [α/M] values for the full set of LAMOST giants, and the largest catalog of [α/M] for giant stars to date. Furthermore, these labels are by construction on the APOGEE label scale; for spectra with S/N > 50, cross-validation of the model yields typical uncertainties of 70 K in T_(eff), 0.1 in log g, 0.1 in [Fe/H], and 0.04 in [α/M], values comparable to the broadly stated, conservative APOGEE DR12 uncertainties. Thus, by using “label transfer” to tie low-resolution (LAMOST R ≈ 1800) spectra to the label scale of a much higher-resolution (APOGEE R ≈ 22,500) survey, we substantially reduce the inconsistencies between labels measured by the individual survey pipelines. This demonstrates that label transfer with The Cannon can successfully bring different surveys onto the same physical scale.

Item Type:Article
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URLURL TypeDescription Paper ItemCode used to produce results
Ho, Anna Y. Q.0000-0002-9017-3567
Ness, Melissa K.0000-0001-5082-6693
Hogg, David W.0000-0003-2866-9403
Rix, Hans-Walter0000-0003-4996-9069
Liu, Chao0000-0001-7049-493X
Alternate Title:Survey Cross-Calibration with The Cannon: APOGEE-scale Stellar Labels from LAMOST Spectra
Additional Information:© 2017 the American Astronomical Society. Received 2016 January 30; accepted 2016 December 16; published 2017 February 3. It is a pleasure to thank Jo Bovy (U. Toronto), Andy Casey (IoA Cambridge), Morgan Fouesneau (MPIA), Evan Kirby (Caltech), Branimir Sesar (MPIA), and Yuan-Sen Ting (Harvard) for valuable discussions and assistance. A.Y.Q.H. is grateful to the community at the MPIA for their support and hospitality during the period in which most of this work was performed. The authors would like to thank two anonymous referees for their detailed and constructive feedback, which greatly improved the strength and clarity of the paper. A.Y.Q.H. was supported by a Fulbright grant through the German-American Fulbright Commission and a National Science Foundation Graduate Research Fellowship under grant No. DGE1144469. M.K.N. and H.W.R. have received funding for this research from the European Research Council under the European Union’s Seventh Framework Programme (FP 7) ERC Grant Agreement n. [321035]. D.W.H. was partially supported by the NSF (grant IIS-1124794), NASA (grant NNX08AJ48G), and the Moore-Sloan Data Science Environment at NYU. C.L. acknowledges the Strategic Priority Research Program “The Emergence of Cosmological Structures” of the Chinese Academy of Sciences, grant No. XDB09000000, the National Key Basic Research Program of China 2014CB845700, and the National Natural Science Foundation of China (NSFC) grants No. 11373032 and 11333003. Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. Facilities: Sloan (APOGEE spectrograph), LAMOST. Note added in revision. After the completion and submission of our paper, Li et al. (2016) also demonstrated that [α/M] can be realiably measured from LAMOST spectra. They developed a technique for this measurement using template matching and an extension of the LAMOST Stellar Pipeline. The code used to produce the results described in this paper was written in Python and is available online in an open-source repository: An archival copy has been preserved with Zenodo (Ho et al. 2016).
Funding AgencyGrant Number
German-American Fulbright CommissionUNSPECIFIED
NSF Graduate Research FellowshipDGE-1144469
European Research Council (ERC)321035
New York University (NYU)UNSPECIFIED
Chinese Academy of SciencesXDB09000000
National Key Basic Research Program of China2014CB845700
National Natural Science Foundation of China11373032
National Natural Science Foundation of China11333003
Subject Keywords:Catalogs; methods: data analysis; methods: statistical; stars: abundances; stars: fundamental parameters; techniques: spectroscopic
Issue or Number:5
Record Number:CaltechAUTHORS:20161121-085144811
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72190
Deposited By: Melissa Ray
Deposited On:21 Nov 2016 19:15
Last Modified:03 Oct 2019 16:15

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