Modelling the Milky Way – I. Method and first results fitting the thick disc and halo with DES-Y3 data,Monthly Notices of the Royal Astronomical Society

当前位置： X-MOL 学术 › Mon. Not. R. Astron. Soc. › 论文详情

Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)

Modelling the Milky Way – I. Method and first results fitting the thick disc and halo with DES-Y3 data
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2020-07-09 , DOI: 10.1093/mnras/staa1980
A Pieres _{1,

2} , L Girardi _{1,

3} , E Balbinot ₄ , B Santiago _{1,

5} , L N da Costa _{1,

2} , A Carnero Rosell _{1,

6} , A B Pace ₇ , K Bechtol ₈ , M A T Groenewegen ₉ , A Drlica-Wagner _{10,

11} , T S Li _{10,

11} , M A G Maia _{1,

2} , R L C Ogando _{1,

2} , M dal Ponte _{1,

5} , H T Diehl ₁₀ , A Amara ₁₂ , S Avila ₁₃ , E Bertin _{14,

15} , D Brooks ₁₆ , D L Burke _{17,

18} , M Carrasco Kind _{19,

20} , J Carretero ₂₁ , J De Vicente ₆ , S Desai ₂₂ , T F Eifler _{23,

24} , B Flaugher ₁₀ , P Fosalba _{25,

26} , J Frieman _{10,

11} , J García-Bellido ₁₃ , E Gaztanaga _{25,

26} , D W Gerdes _{27,

28} , D Gruen _{17,

18,

29} , R A Gruendl _{19,

20} , J Gschwend _{1,

2} , G Gutierrez ₁₀ , D L Hollowood ₃₀ , K Honscheid _{31,

32} , D J James ₃₃ , K Kuehn ₃₄ , N Kuropatkin ₁₀ , J L Marshall ₇ , R Miquel _{21,

35} , A A Plazas ₃₆ , E Sanchez ₆ , S Serrano _{25,

26} , I Sevilla-Noarbe ₆ , E Sheldon ₃₇ , M Smith ₃₈ , M Soares-Santos ₃₉ , F Sobreira _{1,

40} , E Suchyta ₄₁ , M E C Swanson ₂₀ , G Tarle ₂₈ , D Thomas ₄₂ , V Vikram ₄₃ , A R Walker ₄₄

Affiliation

Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil
Observatório Nacional, Rua Gal. José Cristino 77, Rio de Janeiro, RJ - 20921-400, Brazil
Osservatorio Astronomico di Padova, INAF, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy
Kapteyn Astronomical Institute, University of Groningen, Landleven 12, NL-9747 AD Groningen, the Netherlands
Instituto de Física, UFRGS, Caixa Postal 15051, Porto Alegre, RS - 91501-970, Brazil
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA
LSST 933 North Cherry Avenue, Tucson, AZ 85721, USA
Koninklijke Sterrenwacht van België, Ringlaan 3, B-1180 Brussels, Belgium
Fermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USA
Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA
Department of Physics, ETH Zurich, Wolfgang-Pauli-Strasse 16, CH-8093 Zurich, Switzerland
Instituto de Fisica Teorica UAM/CSIC, Universidad Autonoma de Madrid, E-28049 Madrid, Spain
CNRS, UMR 7095, Institut d’Astrophysique de Paris, F-75014 Paris, France
Sorbonne Universités, UPMC Univ Paris 06, UMR 7095, Institut d’Astrophysique de Paris, F-75014 Paris, France
Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
Kavli Institute for Particle Astrophysics & Cosmology, PO Box 2450, Stanford University, Stanford, CA 94305, USA
SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
Department of Astronomy, University of Illinois at Urbana-Champaign, 1002 W. Green Street, Urbana, IL 61801, USA
National Centre for Supercomputing Applications, 1205 West Clark St., Urbana, IL 61801, USA
Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, E-08193 Bellaterra (Barcelona), Spain
Department of Physics, IIT Hyderabad, Kandi, Telangana 502285, India
Department of Astronomy/Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA
Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain
Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain
Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA
Department of Physics, University of Michigan, Ann Arbor, MI 48109, USA
Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305, USA
Santa Cruz Institute for Particle Physics, Santa Cruz, CA 95064, USA
Center for Cosmology and Astro-Particle Physics, The Ohio State University, Columbus, OH 43210, USA
Department of Physics, The Ohio State University, Columbus, OH 43210, USA
Harvard-Smithsonian Centre for Astrophysics, Cambridge, MA 02138, USA
Australian Astronomical Optics, Macquarie University, North Ryde, NSW 2113, Australia
Institució Catalana de Recerca i Estudis Avançats, E-08010 Barcelona, Spain
Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, NJ 08544, USA
Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA
School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK
Physics Department, Brandeis University, 415 South Street, Waltham, MA 02453, USA
Instituto de Física Gleb Wataghin, Universidade Estadual de Campinas, 13083-859 Campinas, SP, Brazil
Computer Science and Mathematics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831, USA
Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK
Argonne National Laboratory, 9700 South Cass Avenue, Lemont, IL 60439, USA
Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile

We present MWFitting, a method to fit the stellar components of the Galaxy by comparing Hess Diagrams (HDs) from TRILEGAL models to real data. We apply MWFitting to photometric data from the first three years of the Dark Energy Survey (DES). After removing regions containing known resolved stellar systems such as globular clusters, dwarf galaxies, nearby galaxies, the Large Magellanic Cloud and the Sagittarius Stream, our main sample spans a total area of $\sim$2,300 deg$^2$ distributed across the DES footprint. We further explore a smaller subset ($\sim$ 1,300 deg$^2$) that excludes all regions with known stellar streams and stellar overdensities. Validation tests on synthetic data possessing similar properties to the DES data show that the method is able to recover input parameters with a precision better than 3\%. Based on the best-fit models, we create simulated stellar catalogues covering the whole DES footprint down to $g = 24$ magnitude. Comparisons of data and simulations provide evidence for a break in the power law index describing the stellar density of the Milky Way (MW) halo. Several previously discovered stellar over-densities are recovered in the residual stellar density map, showing the reliability of MWFitting in determining the Galactic components. Simulations made with the best-fitting parameters are a promising way to predict MW star counts for surveys such as LSST and Euclid.

中文翻译：

银河系建模——I. 用 DES-Y3 数据拟合厚圆盘和光晕的方法和初步结果

我们提出了 MWFitting，这是一种通过将来自 TRILEGAL 模型的赫斯图 (HD) 与真实数据进行比较来拟合银河系恒星成分的方法。我们将 MWFitting 应用于暗能量调查 (DES) 前三年的光度数据。在去除了包含已知解析恒星系统的区域后，例如球状星团、矮星系、附近星系、大麦哲伦星云和人马座流，我们的主要样本跨越 DES 足迹的总面积为 $\sim$2,300 deg$^2$ . 我们进一步探索了一个较小的子集（$\sim$ 1,300 deg$^2$），它排除了所有已知恒星流和恒星密度过高的区域。对具有与 DES 数据相似特性的合成数据的验证测试表明，该方法能够以优于 3\% 的精度恢复输入参数。基于最佳拟合模型，我们创建了涵盖整个 DES 足迹的模拟恒星目录，低至 $g = 24$ 星等。数据和模拟的比较为描述银河系 (MW) 晕恒星密度的幂律指数的突破提供了证据。在残余恒星密度图中恢复了几个先前发现的恒星超密度，显示了 MWFitting 在确定银河成分方面的可靠性。使用最佳拟合参数进行的模拟是预测 LSST 和 Euclid 等调查的 MW 恒星数量的有前途的方法。在残余恒星密度图中恢复了几个先前发现的恒星超密度，显示了 MWFitting 在确定银河成分方面的可靠性。使用最佳拟合参数进行的模拟是预测 LSST 和 Euclid 等调查的 MW 恒星数量的有前途的方法。在残余恒星密度图中恢复了几个先前发现的恒星超密度，显示了 MWFitting 在确定银河成分方面的可靠性。使用最佳拟合参数进行的模拟是预测 LSST 和 Euclid 等调查的 MW 恒星数量的有前途的方法。

更新日期：2020-07-09

点击分享查看原文

点击收藏

公开下载

阅读更多本刊最新论文本刊介绍/投稿指南11