The Large Sky Area Multi- Object Spectroscopic Telescope (LAMOST)

Size: px
Start display at page:

Download "The Large Sky Area Multi- Object Spectroscopic Telescope (LAMOST)"

Transcription

1 The Large Sky Area Multi- Object Spectroscopic Telescope (LAMOST) The Milky Way and its Stars February 25 KITP!! Martin C. Smith Shanghai Astronomical Observatory

2 LAMOST introduction China s largest optical telescope A 4-5m telescope with 4 fibers across a 2 sq deg field of view, at R = 2, Full surveys started in 22, obtaining over M good stellar spectra (S/N > ) each year, current total of over 3M spectra Fields cover halo/disc/anti-centre, with ancillary projects such as LAMOST-Kepler led by Fu & De Cat (~6k good spectra in the Kepler field) Five-year survey, with possibility of higher-resolution (R=5,-,) in future

3 LAMOST introduction China s largest optical telescope A 4-5m telescope with 4 fibers across a 2 sq deg field of view, at R = 2, Full surveys started in 22, obtaining over M good stellar spectra (S/N > ) each year, current total of over 3M spectra Fields cover halo/disc/anti-centre, with ancillary projects such as LAMOST-Kepler led by Fu & De Cat (~6k good spectra in the Kepler field) Five-year survey, with possibility of higher-resolution (R=5,-,) in future

4 B M F 7 57 KEPLER 6 78 Total Plate Spe r LAMOST introduction China s largest optical telescope A 4-5m telescope with 4 fibers across a 2 sq deg field of view, at R = 2, Full surveys started in 22, obtaining over M good stellar spectra (S/N > ) each year, current total of over 3M spectra Fields cover halo/disc/anti-centre, with ancillary projects such as LAMOST-Kepler led by Fu & De Cat (~6k good spectra in the Kepler field) Five-year survey, with possibility of higher-resolution (R=5,-,) in future GAC 69 9 M V EG 4 5 HD 62 2 B M F 95 KEPLER 2 Total

5 Overview of data quality Success rate (S/N > ) around 7%, with a limiting magnitude of r ~ 7, so great synergy with Gaia 2nd Full survey year Regular 2nd year Survey data Very bright plates 9 < V < 4 observed Pipelines in place, with 2.2M FGK stars with parameters from first two years Similar accuracy to SDSS (~.5 dex in [Fe/H], ~.2 dex in log(g), ~K in T eff ) although issues with gravities Various plans to estimate alphas, although not currently implemented r-band magnitude

6 Overview of data quality Success rate (S/N > ) around 7%, with a limiting magnitude of r ~ 7, so great synergy with Gaia Comparison to SDSS (Yue Wu) 2nd Full survey year Regular 2nd year Survey data Very bright plates 9 < V < 4 observed Pipelines in place, with 2.2M FGK stars with parameters from first two years Similar accuracy to SDSS (~.5 dex in [Fe/H], ~.2 dex in log(g), ~K in T eff ) although issues with gravities Various plans to estimate alphas, although not currently implemented r-band magnitude

7 Overview of data quality ( S SVM V R ) -vs l ogg (L M ) log(g)l ogg offset Seism. log(g) offset vs (LAMOST l ogg (Seism. S V R ) - l ogg LM) 28). Second, the other features, e.g., Balmer lines (Wilhelm, Beers & Gray 999), CaII K 2 and H lines (Lee et al. 28) etc., can also be l ogg ( S V R ) - l ogg ( L M ) useful to determine the surface gravity. Morem e d i an l ogg ( S V R ) - l ogg ( L M ).5 over, some algorithms determine the surface gravity together with the effective temperature and metallicity, simultaneously, by comparing Improvements in survey depths and with success rates the full spectra the spectral library (e.g.,.5 Lee et al. 28; Wu et al. 2a). In addition, Comparison SDSSapproaches, (Yue Wu) e.g. the supervised machine to learning Full survey 2ndsupport yearsurvey data st year Regular Survey 2nd year Regular artificial neural networks, vector ma Success rate (S/N > ) around chine etc., have also been used to derive the.5 observed observed Very bright plates 7%, with a limiting magnitude of surface gravity based on the training spectra 9 < V < 4 with known surface gravity values as the tarr ~ 7, so great synergy with Gaia gets (Re Fiorentin et al. 27; Liu et al. 22)..5 The typical accuracy of the surface gravity es Pipelines in place, with 2.2M FGK LAMOST Kepler (Liu et al.spectra, 25) e.g. SDSS timates +for low resolution 2 stars with from first 4 parameters 2 3 (Ahn et al. 24) or LAMOST (Cui et al. 22), l ogg ( S V R ) is about.2-.4 dex (Wilhelm, Beers & Gray log(g) from Seismology two years.5 o ff se t =et.al. 28; 999; Re Fiorentin et al. 27; Lee Fig. 2. The comparison between the SVR and σ =. 3 Wu et al. 24). Similarlogg accuracy to dataset SDSS (the (~.5 the LAMOST for the test black s t d d etool v =. Asteroseismology is a powerful to2derive.5 dots). dex The in red[fe/h], filled circles bars ~.2with dexthe in error log(g), the fundamental parameters, e.g. stellar mass, raare the median values and σ dispersions of the dius, and Teff, for a star (see Brown & Gilliland ~K in Teff) although issues difference of logg at each logg(sv R) bin ; Chaplin & Migio 23). Thanks to the with gravities Kepler (Borucki et al. 2) mission, the Sun like oscillations for tens of thousands of stars Various plans to estimate alphas,.5 (b ) ((ca) ) ( d()b ) although not currently implemented Te ff (LM ) [ Fe /H ] ( L M ).4 r-band magnitude ogt (LM [ Fe /H ] ( L M ) l oggeseismology ( ast ) ) log(g) lfrom ff Fig. 3. for Thethe residual of the as SVR logg, logg(sv dual of the SVR logg, logg(sv R) logg(ast), test dataset functions of the R) lo

8 Science highlights Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) K-giants (Liu et al. 24) Local UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) Repeat observations (per year) Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep) M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) Other science: stellar physics; open clusters; ages & chemo-dynamical studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc)

9 Science highlights Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) K-giants (Liu et al. 24) Local UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) Repeat observations (per year) Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep).8 M-type stars, incl. -3k giants.6 (Zhong et al. in prep; Li et al. in prep) f B.4 Other science: stellar physics; open clusters; ages & chemo-dynamical.2 studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc) SDSS SEGUE LAMOST LEGUE Gao et al. (24) SDSS SEGUE G/F subsample LAMOST LEGUE 7 T eff (K) [Fe/H] 6

10 Science highlights Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) K-giants (Liu et al. 24) Local UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) Repeat observations (per year) Qia et al. (25) Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep) M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) Other science: stellar physics; open clusters; ages & chemo-dynamical studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc)

11 Science highlights Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) K-giants (Liu et al. 24) Zhong et al. (in prep) Local UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep) M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) Other science: stellar physics; open clusters; ages & chemo-dynamical studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc)

12 Science highlights.6.4 Mdwarf Kgiant Li et al. (in prep) Kdwarf Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) K-giants (Liu et al. 24) (J K) Zhong et al. (in prep) Local UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) (W W2).2.2 (W W2).2.2 (W W2) Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep) M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) Other science: stellar physics; open clusters; ages & chemo-dynamical studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc) (J K).5.5 Kgiant Mdwarf Kdwarf (W W2)

13 Science highlights.6.4 Mdwarf Kgiant Li et al. (in prep) Kdwarf Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) K-giants (Liu et al. 24) Local UV-velocity distribution from 5, F/G 8 dwarfs (Xia et al. 25) Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep) 2 dec 6 4 M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) 2 M-giants in WISE Other science: 4 stellar physics; open clusters; ages & chemo-dynamical 6 studies; HVS; dark matter density; chemically 8 peculiar stars (e.g. Am, Li-rich, alpha-poor, 35 3 metal-poor, 25 etc) 2 ra 5 (J K) (J K) Sagittarius stream (W W2).5.5 Zhong et al. (in prep).2.2 (W W2).2.2 (W W2) Kgiant Mdwarf Kdwarf (W W2)

14 2 Science highlights Li et al. (in prep) ~ B (deg).6 Mdwarf.4 Kgiant Kdwarf.2 Binaries (Gao et al. 24) & RR Lyrae (Yang et al. 24) - (J K) Zhong et al. (in prep) K-giants (Liu et al. 24).4 Distance papers (in prep) White dwarfs (Rebassa-Mansergas et al. in prep) M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) Other science: stellar physics; open clusters; ages & chemo-dynamical studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc) ~ B (deg) (W W2).2.2 (W W2).2.2 (W W2).5 Kgiant Mdwarf Kdwarf - -2 (J K) Local UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) Distance (kpc) (W W2)2 ~ Λ (deg).2.3 3

15 Li et al. (in prep) Science highlights 4.2 & RR (Gao et al. 24) [Fe/H]phot [Fe/H]APOGEE Lyrae (Yang et al. 24) 2 K-giants.4 UV-velocity distribution from 5, F/G dwarfs (Xia et al. 25) Distance papers (in prep) (W W2) Other science: stellar physics; open clusters; ages & chemo-dynamical studies; HVS; dark matter density; chemically peculiar stars (e.g. Am, Li-rich, alpha-poor, metal-poor, etc) ~ B (deg).2.2 (W W2).2.2 (W W2).5.5 White dwarfs (Rebassa-Mansergas et al. in prep) M-type stars, incl. -3k giants (Zhong et al. in prep; Li et al. in prep) (W W2) (J K). Λ =8-2 (deg).2 Kdwarf Zhong et al. (in prep) Local Kgiant (Liu et al. 24) Mdwarf Λ =3-7 (deg) - (J K) Binaries.6 Distance (kpc) [Fe/H]APOGEE ~ B (deg) 2 Li et al. (in prep) Kgiant.5 Λ =24-28 (deg) Mdwarf Kdwarf 3 2 Λ =29-33 (deg) [Fe/H]phot. (W W2)2 ~ Λ (deg).2.3 3

16 LAMOST summary Other projects Full survey is making good progress, obtaining over M stars each year to 7th mag Pipelines are relatively robust and continually being improved Large number of spectra for Kepler/K2 fields A lot of great science underway DR will be released internationally in March, including catalogues and spectra (.8M with S/N > ; M FGK star parameters) Hills & hypervelocity stars (Yanqiong Zhang & John Vickers -SHAO, Shanghai) Alphas & ages for LAMOST stars, starting with LAMOST-KEPLER (Emma Small & John Vickers - SHAO, Shanghai; Corrado Boeche - ARI, Heidelberg) Orbital structure of disc & bulge stars from N-body models, currently analysing the APOGEE bulge high-velocity peaks (Matthew Molloy - KIAA, Beijing) Outer-halo substructures using BHBs from deep u-band photometry, including a comprehensive characterisation of the Pisces over-density (Jundan Nie - NAOC, Beijing) Pulsar microlensing (Dai Shi - PKU, Beijing)

17 Discussion points What aspects of the data analysis would you like to see worked on? Alphas are being coming, as I have shown gravities can be calibrated (with caveats), but is there anything else? Future plans for LAMOST? The five year survey will end in Summer 27. What next? The higher-res grating is an option (see below), especially useful if this will provide reliable alpha-element abundances. Or time domain for binaries or variables? Or just keep going, making a complete survey of the disc. This is what they said back in 22 regarding the higher-resolution option: The survey will also include an R = 5-, mode, which will yield two pieces of the spectrum that are 35A wide, one in the red and one in the blue.the blue wavelength coverage is centered around 53A to sample many metal lines,including the prominent Mg b (575A) triplet. The red segment covers the spectral range A, sampling the CaII triplet, Fe I, Ti I, and other lines, which are ideal for measuring the RV and [Fe/H]. This R = 5 mode wavelength coverage and dispersion is similar to that of the RAVE experiment.

JINA Observations, Now and in the Near Future

JINA Observations, Now and in the Near Future JINA Observations, Now and in the Near Future Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics Examples SDSS-I, II, and III

More information

(Present and) Future Surveys for Metal-Poor Stars

(Present and) Future Surveys for Metal-Poor Stars (Present and) Future Surveys for Metal-Poor Stars Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics SDSS 1 Why the Fascination

More information

Outline. c.f. Zhao et al. 2006, ChJA&A, 6, 265. Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey

Outline. c.f. Zhao et al. 2006, ChJA&A, 6, 265. Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey KIAA-CambridgeJoint Workshop on Near-Field Cosmology and Galactic Archeology ZHAO Gang National Astronomical Observatories, Chinese Academy of Sciences Dec 1-5, 2008 Beijing Outline LAMOST stellar spectroscopic

More information

Radial Velocity Surveys. Matthias Steinmetz (AIP)

Radial Velocity Surveys. Matthias Steinmetz (AIP) Radial Velocity Surveys Matthias Steinmetz (AIP) The Galactic case for RV surveys Information on how galaxies form is locked in n the phase-space (position,velocities) Information is locked in stars (abundances)

More information

Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia

Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Chengqun Yang Contents 1 Stellar Halo

More information

Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee

Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee Determination of [α/fe] and its Application to SEGUE F/G Stars Young Sun Lee Research Group Meeting on June 16, 2010 Outline Introduction Why [α/fe]? Determination of [α/fe] Validation of estimate of [α/fe]

More information

Estimating the mass of our Milky Way from the LAMOST Galactic spectroscopic survey

Estimating the mass of our Milky Way from the LAMOST Galactic spectroscopic survey 2 nd LAMOST KEPLER WORKSHOP LAMOST in the era of large spectroscopic surveys July 31-August 3, 2017, @ Brussels Estimating the mass of our Milky Way from the LAMOST Galactic spectroscopic survey Yang Huang

More information

Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles

Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Ling Zhu, Jie Wang Contents 1

More information

Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator)

Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator) Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator) The Gaia-ESO Survey http://www.gaia-eso.eu Public spectroscopic

More information

The Gaia-ESO Spectroscopic Survey. Survey Co-PIs. Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs

The Gaia-ESO Spectroscopic Survey. Survey Co-PIs. Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs The Gaia-ESO Spectroscopic Survey Survey Co-PIs Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs Gaia-ESO survey context and motivations (conclusions and key words of several talks)

More information

Asterseismology and Gaia

Asterseismology and Gaia Asterseismology and Gaia Asteroseismology can deliver accurate stellar radii and masses Huber et al 2017 compare results on distances from Gaia and asteroseismology for 2200 Kepler stars Asteroseismology

More information

arxiv: v1 [astro-ph.ga] 30 Jan 2015

arxiv: v1 [astro-ph.ga] 30 Jan 2015 Title : will be set by the publisher Editors : will be set by the publisher EAS Publications Series, Vol.?, 2018 arxiv:1501.07824v1 [astro-ph.ga] 30 Jan 2015 NEARBY LOW-MASS HYPERVELOCITY STARS Yanqiong

More information

Gaia-LSST Synergy. A. Vallenari. INAF, Padova

Gaia-LSST Synergy. A. Vallenari. INAF, Padova Gaia-LSST Synergy A. Vallenari INAF, Padova The Galaxy view Unveiling the complex history of the MW assembly and internal evolution is still one of the main interest of astrophysics However the specific

More information

SDSS-IV MaStar: a Large, Comprehensive, and High Quality Empirical Stellar Library

SDSS-IV MaStar: a Large, Comprehensive, and High Quality Empirical Stellar Library 3rd International Workshop on Spectral Stellar Libraries ASI Conference Series, 2017, Vol. 14, pp 99 103 Editors: P. Coelho, L. Martins & E. Griffin SDSS-IV MaStar: a Large, Comprehensive, and High Quality

More information

Extremely Metal-Poor Stars

Extremely Metal-Poor Stars ngcfht workshop 2013.3.27-29. Extremely Metal-Poor Stars Wako Aoki National Astronomical Observatory of Japan Extremely Metal-Poor (EMP) Stars Chemical composition of EMP stars Nucleosynthesis of first

More information

Oxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto!

Oxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Oxygen in red giants from near-infrared OH lines: 3D effects and first results from Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Overview! 1. APOGEE: status and prospects! 2. A first look at

More information

Galactic archaeology with the RAdial Velocity Experiment

Galactic archaeology with the RAdial Velocity Experiment Galactic archaeology with the RAdial Velocity Experiment Georges Kordopatis & RAVE collaboration Leibniz-Institute for Astrophysics, Potsdam Multi-Object Spectroscopy in the next decade: Big questions,

More information

Tests of MATISSE on large spectral datasets from the ESO Archive

Tests of MATISSE on large spectral datasets from the ESO Archive Tests of MATISSE on large spectral datasets from the ESO Archive Preparing MATISSE for the ESA Gaia Mission C.C. Worley, P. de Laverny, A. Recio-Blanco, V. Hill, Y. Vernisse, C. Ordenovic and A. Bijaoui

More information

Matthias Steinmetz. 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1

Matthias Steinmetz. 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1 Matthias Steinmetz 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1 The RAVE Survey Spectroscopic high latitude survey of the MW 9 < I < 13 GAIA spectral range and resolution

More information

arxiv: v1 [astro-ph.ga] 19 Jan 2017

arxiv: v1 [astro-ph.ga] 19 Jan 2017 Mon. Not. R. Astron. Soc. 000, 1 22 (2015) Printed 12 March 2018 (MN LATEX style file v2.2) LAMOST Spectroscopic Survey of the Galactic Anticentre (LSS-GAC): the second release of value-added catalogues

More information

New insights into the Sagittarius stream

New insights into the Sagittarius stream New insights into the Sagittarius stream EWASS, Turku July 8th, 213 Martin C. Smith Shanghai Astronomical Observatory http://hubble.shao.ac.cn/~msmith/ Sagittarius dwarf spheroidal(ish) Since its discovery

More information

Introduction to SDSS -instruments, survey strategy, etc

Introduction to SDSS -instruments, survey strategy, etc Introduction to SDSS -instruments, survey strategy, etc (materials from http://www.sdss.org/) Shan Huang 17 February 2010 Survey type Status Imaging and Spectroscopy Basic Facts SDSS-II completed, SDSS-III

More information

Galactic, stellar (and planetary) archaeology with Gaia: The galactic white dwarf population

Galactic, stellar (and planetary) archaeology with Gaia: The galactic white dwarf population Galactic, stellar (and planetary) archaeology with Gaia: The galactic white dwarf population Boris Gänsicke & Roberto Raddi Richard Ashley Jay Farihi Nicola Gentile Fusillo Mark Hollands Paula Izquierdo

More information

WEAVE Galactic Surveys

WEAVE Galactic Surveys WEAVE Galactic Surveys A. Vallenari INAF, Padova On behalf of the Science Team Overview WEAVE Surveys Milky Way Surveys WEAVE Characteristics Project structure Primary Science Surveys There are six primary

More information

Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg"

Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg" Spectroscopy of (cool) giants and supergiants! Maria Bergemann MPIA Heidelberg" Outline! Motivation why do spectroscopy of giant

More information

LAMOST Sky Survey --Site limitations and survey planning

LAMOST Sky Survey --Site limitations and survey planning LAMOST Sky Survey --Site limitations and survey planning Chao Liu, Licai Deng National Astronomical Observatories, CAS Heidi Newberg Rensselaer Polytechnic Institute Overview Site limitations that strictly

More information

Halo Tidal Star Streams with DECAM. Brian Yanny Fermilab. DECam Community Workshop NOAO Tucson Aug

Halo Tidal Star Streams with DECAM. Brian Yanny Fermilab. DECam Community Workshop NOAO Tucson Aug Halo Tidal Star Streams with DECAM Brian Yanny Fermilab DECam Community Workshop NOAO Tucson Aug 19 2011 M31 (Andromeda) Our Local Group neighbors: Spiral galaxies similar to The Milky Way 150 kpc M33

More information

The Apache Point Observatory Galactic Evolution Experiment. Ricardo Schiavon

The Apache Point Observatory Galactic Evolution Experiment. Ricardo Schiavon The Apache Point Observatory Galactic Evolution Experiment Ricardo Schiavon CS20, Boston, August 1st, 2018 Overview paper: Majewski, Schiavon et al. (2017) APOGEE at a Glance Dual hemisphere spectroscopic

More information

Pre-observations and models

Pre-observations and models Pre-observations and models Carine Babusiaux Observatoire de Paris - GEPI GREAT-ITN, IAC, September 2012 The questions 1) Can the observing program tackle the scientific problem? 2) What is the best configuration

More information

Milky Way S&G Ch 2. Milky Way in near 1 IR H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/

Milky Way S&G Ch 2. Milky Way in near 1 IR   H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/ Why study the MW? its "easy" to study: big, bright, close Allows detailed studies of stellar kinematics, stellar evolution. star formation, direct detection of dark matter?? Milky Way S&G Ch 2 Problems

More information

Exploring the Structure of the Milky Way with WFIRST

Exploring the Structure of the Milky Way with WFIRST Exploring the Structure of the Milky Way with WFIRST Heidi Jo Newberg Rensselaer Polytechnic Institute Simulation: Stefan Gottlöber/AIP Image Credit: Heidi Newberg Milky Way Structure we want it all: The

More information

White Dwarf - M Dwarf Binaries. Sloan Digital Sky Survey

White Dwarf - M Dwarf Binaries. Sloan Digital Sky Survey White Dwarf - M Dwarf Binaries from the Sloan Digital Sky Survey René Heller, Axel Schwope, Roy Østensen René Heller Astrophysikalisches Institut Potsdam rheller@aip.de Viña del Mar March 08, 2011 The

More information

Gaia DR2 and/versus RAVE DR5: application for the semi-analytic thin disk model

Gaia DR2 and/versus RAVE DR5: application for the semi-analytic thin disk model Gaia DR2 and/versus RAVE DR5: application for the semi-analytic thin disk model Speaker: Supervisor: Kseniia Sysoliatina (ARI) Prof. Dr. Andreas Just Gaia DR2 workshop Heidelberg, Outline (1) Comparison

More information

arxiv: v1 [astro-ph] 12 Nov 2008

arxiv: v1 [astro-ph] 12 Nov 2008 Self-Organizing Maps. An application to the OGLE data and the Gaia Science Alerts Łukasz Wyrzykowski, and Vasily Belokurov arxiv:0811.1808v1 [astro-ph] 12 Nov 2008 Institute of Astronomy, University of

More information

arxiv: v2 [astro-ph.ga] 14 Apr 2016

arxiv: v2 [astro-ph.ga] 14 Apr 2016 Draft version April 15, 216 Preprint typeset using L A TEX style emulateapj v. 5/2/11 SELECTING M-GIANTS WITH INFRA-RED PHOTOMETRY: DISTANCES, METALLICITIES AND THE SAGITTARIUS STREAM Jing Li 1,2, Martin

More information

Outline. ESA Gaia mission & science objectives. Astrometric & spectroscopic census of all stars in Galaxy to G=20 mag.

Outline. ESA Gaia mission & science objectives. Astrometric & spectroscopic census of all stars in Galaxy to G=20 mag. Atomic Data Requirements for Large Spectroscopic Surveys: ESA Gaia and ESO GES Alex Lobel Royal Observatory of Belgium Outline ESA Gaia mission & science objectives. Astrometric & spectroscopic census

More information

A comparison of stellar atmospheric parameters from the LAMOST and APOGEE datasets

A comparison of stellar atmospheric parameters from the LAMOST and APOGEE datasets RAA 2015 Vol. 15 No. 8, 1125 1136 doi: 10.1088/1674 4527/15/8/003 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics A comparison of stellar atmospheric parameters

More information

Star clusters before and after Gaia Ulrike Heiter

Star clusters before and after Gaia Ulrike Heiter Star clusters before and after Gaia Ulrike Heiter Uppsala University Outline Gaia mission overview Use of stellar clusters for calibration of stellar physical parameters Impact of Gaia data on cluster

More information

Candidate members of the Pal 5, GD-1, Cetus Polar, and Orphan. tidal stellar halo streams from SDSS DR9, LAMOST DR3 and

Candidate members of the Pal 5, GD-1, Cetus Polar, and Orphan. tidal stellar halo streams from SDSS DR9, LAMOST DR3 and Research in Astronomy and Astrophysics manuscript no. (L A TEX: 0222.tex; printed on March 24, 2017; 9:40) Candidate members of the Pal 5, GD-1, Cetus Polar, and Orphan tidal stellar halo streams from

More information

Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations

Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations Diogo Souto Observatório Nacional - ON/MCTI + Katia Cunha Anibal Verne Smith C. Allende Prieto Garcia Hernandez Olga Zamora

More information

The Gaia-ESO Public Spectroscopic Survey a lesson for our community in use of limited telescope access. Gerry Gilmore Sofia Randich Gaia-ESO Co-PIs

The Gaia-ESO Public Spectroscopic Survey a lesson for our community in use of limited telescope access. Gerry Gilmore Sofia Randich Gaia-ESO Co-PIs The Gaia-ESO Public Spectroscopic Survey a lesson for our community in use of limited telescope access Gerry Gilmore Sofia Randich Gaia-ESO Co-PIs 1 We have Gaia! We want more Gaia will provide 60 million

More information

Data-driven models of stars

Data-driven models of stars Data-driven models of stars David W. Hogg Center for Cosmology and Particle Physics, New York University Center for Data Science, New York University Max-Planck-Insitut für Astronomie, Heidelberg 2015

More information

Classical observations of stellar properties

Classical observations of stellar properties Classical observations of stellar properties Luca Casagrande M. Bessell - J. Meléndez - I. Ramírez / M. Asplund R. Schönrich / V. Silva Aguirre Spectroscopy F(l) : lots of info, but also model dependent

More information

Abundance distribution in the Galactic thick disk

Abundance distribution in the Galactic thick disk Abundance distribution in the Galactic thick disk omas Bensby Lund Observatory, Department of Astronomy and eoretical Physics Discovery of thick disks (Burstein 1979, ApJ, 234, 829) Discovery of the Galactic

More information

The Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

The Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution I S I The Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution Yang Huang (LAMOST Fellow, yanghuang@pku.edu.cn) N G U N I V E R P E K T Y 1 8 9 8 Peking University

More information

arxiv: v1 [astro-ph.sr] 8 Oct 2015

arxiv: v1 [astro-ph.sr] 8 Oct 2015 Research in Astron. Astrophys. Vol. X No. XX, http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics arxiv:151.228v1 [astro-ph.sr] 8 Oct 215 Validation of LAMOST

More information

The Gaia Mission. Coryn Bailer-Jones Max Planck Institute for Astronomy Heidelberg, Germany. ISYA 2016, Tehran

The Gaia Mission. Coryn Bailer-Jones Max Planck Institute for Astronomy Heidelberg, Germany. ISYA 2016, Tehran The Gaia Mission Coryn Bailer-Jones Max Planck Institute for Astronomy Heidelberg, Germany ISYA 2016, Tehran What Gaia should ultimately achieve high accuracy positions, parallaxes, proper motions e.g.

More information

Making precise and accurate measurements with data-driven models

Making precise and accurate measurements with data-driven models Making precise and accurate measurements with data-driven models David W. Hogg Center for Cosmology and Particle Physics, Dept. Physics, NYU Center for Data Science, NYU Max-Planck-Insitut für Astronomie,

More information

Following the evolution of the Galactic disc with Open Clusters

Following the evolution of the Galactic disc with Open Clusters Following the evolution of the Galactic disc with Open Clusters Laura Magrini INAF-Osservatorio Astrofisico di Arcetri With Nikos Prantzos and the GES collaboration (in particular Lorenzo Spina, Sofia

More information

12. Physical Parameters from Stellar Spectra. Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances

12. Physical Parameters from Stellar Spectra. Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances 12. Physical Parameters from Stellar Spectra Fundamental effective temperature calibrations Surface gravity indicators Chemical abundances 1 Fundamental Properties of Stars Temperature (T) Radius (R) Chemical

More information

Milky Way Companions. Dave Nero. February 3, UT Astronomy Bag Lunch

Milky Way Companions. Dave Nero. February 3, UT Astronomy Bag Lunch UT Astronomy Bag Lunch February 3, 2008 Outline 1 Background 2 Cats and Dogs, Hair and a Hero 3 Theoretical Evolution of the Galactic Halo Outline Background 1 Background 2 Cats and Dogs, Hair and a Hero

More information

Design Reference Mission. DRM approach

Design Reference Mission. DRM approach Design Reference Mission The Design Reference Mission (DRM) is a set of observing programs which together provide a tool to assist with tradeoff decisions in the design of the E-ELT (examples of observing

More information

SkyMapper and the Southern Sky Survey

SkyMapper and the Southern Sky Survey SkyMapper and the Southern Sky Survey Stefan Keller Mt. Stromlo Observatory Brian Schmidt, Mike Bessell and Patrick Tisserand SkyMapper 1.35m telescope with a 5.7 sq. degree field of view located at Siding

More information

THE QUEST RR LYRAE SURVEY AND HALO SUB-STRUCTURE

THE QUEST RR LYRAE SURVEY AND HALO SUB-STRUCTURE THE QUEST RR LYRAE SURVEY AND HALO SUB-STRUCTURE Kathy Vivas (CIDA, Venezuela), Bob Zinn (Yale U., USA), Sonia Duffau (U. de Chile), Yara Jaffé, Jesús Hernández, Yolimar Subero (CIDA, Venezuela), G. Carraro

More information

The Milky Way Galaxy (ch. 23)

The Milky Way Galaxy (ch. 23) The Milky Way Galaxy (ch. 23) [Exceptions: We won t discuss sec. 23.7 (Galactic Center) much in class, but read it there will probably be a question or a few on it. In following lecture outline, numbers

More information

Automated analysis: SDSS, BOSS, GIRAFFE

Automated analysis: SDSS, BOSS, GIRAFFE Automated analysis: SDSS, BOSS, GIRAFFE Tests with MILES spectra (R~2000) from the INT (Sanchez Blazquez et al. 2006) The same code (FERRE) Fitting data calibrated in flux and continuumnormalized Software

More information

Cecilia Fariña - ING Support Astronomer

Cecilia Fariña - ING Support Astronomer Cecilia Fariña - ING Support Astronomer Introduction: WHT William Herschel Telescope 2 Introduction: WHT WHT located in La Palma, Canary Islands, Spain William Herschel Telescope l 2 3 Introduction: WHT

More information

What is an ultra-faint Galaxy?

What is an ultra-faint Galaxy? What is an ultra-faint Galaxy? UCSB KITP Feb 16 2012 Beth Willman (Haverford College) Large Magellanic Cloud, M V = -18 ~ 1/10 Milky Way luminosity image credit: Yuri Beletsky (ESO) and APOD NGC 205, M

More information

Thorium (Th) Enrichment in the Milky Way Galaxy

Thorium (Th) Enrichment in the Milky Way Galaxy Thorium (Th) Enrichment in the Milky Way Galaxy National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan E-mail: aoki.wako@nao.ac.jp Satoshi Honda Kwasan Observatory, Kyoto

More information

THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy

THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS B. Barbuy IAG - Universidade de São Paulo Outline: Interest of studies on Galactic bulge and globulars Data available on metallicity,, kinematics in field

More information

The cosmic distance scale

The cosmic distance scale The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,

More information

Probing the history of star formation in the Local Group using the galactic fossil record

Probing the history of star formation in the Local Group using the galactic fossil record Probing the history of star formation in the Local Group using the galactic fossil record Brian O Shea (Michigan State University) Collaborators: Tim Beers, Carolyn Peruta, Monica Derris (MSU), Jason Tumlinson

More information

The Accretion History of the Milky Way

The Accretion History of the Milky Way The Accretion History of the Milky Way Julio F. Navarro The Milky Way as seen by COBE Collaborators Mario Abadi Amina Helmi Matthias Steinmetz Ken Ken Freeman Andres Meza The Hierarchical Formation of

More information

How Massive is the Milky Way?

How Massive is the Milky Way? How Massive is the Milky Way? See also: Klypin et al. (2002) Simon s talk Matthias Steinmetz Astrophysical Institute Potsdam Overview Spectroscopic Surveys of the MW Geneva-Copenhagen, SDSS, RAVE Mass

More information

The Three Dimensional Universe, Meudon - October, 2004

The Three Dimensional Universe, Meudon - October, 2004 GAIA : The science machine Scientific objectives and impacts ------- F. Mignard OCA/ Cassiopée 1 Summary Few figures about Gaia Gaia major assets What science with Gaia Few introductory highlights Conclusion

More information

Mario Juric Institute for Advanced Study, Princeton

Mario Juric Institute for Advanced Study, Princeton Mapping Galactic density, metallicity and kinematics. Mario Juric Institute for Advanced Study, Princeton with Zeljko Ivezic, Nick Bond, Branimir Sesar, Robert Lupton and the SDSS Collaboration Dissecting

More information

Mapping the Galactic halo with main-sequence and RR Lyrae stars

Mapping the Galactic halo with main-sequence and RR Lyrae stars EPJ Web of Conferences 19, 02002 (2012) DOI: 10.1051/epjconf/20121902002 C Owned by the authors, published by EDP Sciences, 2012 Mapping the Galactic halo with main-sequence and RR Lyrae stars B. Sesar

More information

The HERMES project. Reconstructing Galaxy Formation. Ken Freeman RSAA, ANU. The metallicity distribution in the Milky Way discs Bologna May 2012

The HERMES project. Reconstructing Galaxy Formation. Ken Freeman RSAA, ANU. The metallicity distribution in the Milky Way discs Bologna May 2012 The HERMES project Reconstructing Galaxy Formation Ken Freeman RSAA, ANU The metallicity distribution in the Milky Way discs Bologna May 2012 HERMES is a new high-resolution fiber-fed multi-object spectrometer

More information

The Pristine survey: An efficient search for extremely metal-poor stars. Kris Youakim. ING Seminar Jan 22, 2018

The Pristine survey: An efficient search for extremely metal-poor stars. Kris Youakim. ING Seminar Jan 22, 2018 The Pristine survey: An efficient search for extremely metal-poor stars Kris Youakim ING Seminar Jan 22, 2018 Credit: NASA / WMAP Science Team Movie First Light Wise, Abel, Kaehler, 2009 Image: Aladin sky

More information

ROSAT Roentgen Satellite. Chandra X-ray Observatory

ROSAT Roentgen Satellite. Chandra X-ray Observatory ROSAT Roentgen Satellite Joint facility: US, Germany, UK Operated 1990 1999 All-sky survey + pointed observations Chandra X-ray Observatory US Mission Operating 1999 present Pointed observations How do

More information

SkyMapper and the Southern Sky Survey

SkyMapper and the Southern Sky Survey and the Southern Sky Survey, Brian Schmidt and Mike Bessell Slide 1 What is? 1.35m telescope with a 5.7 sq. degree field of view To reside at Siding Spring Observatory, NSW To conduct the Southern Sky

More information

Chemical tagging of FGK stars: testing membership to stellar kinematic groups

Chemical tagging of FGK stars: testing membership to stellar kinematic groups Chemical tagging of FGK stars: testing membership to stellar kinematic groups David Montes, Hugo M. Tabernero, Jonay I. González Hernández Dpto. Astrofísica, F. Físicas Universidad Complutense de Madrid,

More information

SkyMapper and EMP stars

SkyMapper and EMP stars SkyMapper and EMP stars Mike Bessell on behalf of the EMP team Research School of Astronomy & Astrophysics Slide 2 The discovery of the ancient star with no Fe lines. SkyMapper 2.3m WiFeS Magellan MIKE

More information

The Chemical/Dynamical Evolution of the Galactic Bulge

The Chemical/Dynamical Evolution of the Galactic Bulge Astro2020 Science White Paper The Chemical/Dynamical Evolution of the Galactic Bulge Thematic Areas: Stars and Stellar Evolution Resolved Stellar Populations and their Environments Galaxy Evolution Principal

More information

VISTA HEMISPHERE SURVEY DATA RELEASE 1

VISTA HEMISPHERE SURVEY DATA RELEASE 1 Release date (will be set by ESO) VISTA HEMISPHERE SURVEY DATA RELEASE 1 PROPOSAL ESO No.: 179.A-2010 PRINCIPAL INVESTIGATOR: Richard McMahon Authors: R. McMahon, M. Banerji, N. Lodieu for the VHS Collaboration

More information

arxiv:astro-ph/ v1 14 Dec 1998

arxiv:astro-ph/ v1 14 Dec 1998 Spectroscopy of red giants of the Sagittarius dwarf galaxy arxiv:astro-ph/9812267v1 14 Dec 1998 G. Marconi Osservatorio Astronomico di Roma P. Bonifacio Osservatorio Astronomico di Trieste L. Pasquini

More information

Combining Gaia DR1, DR2 and Matthias Steinmetz (AIP) a preview on the full Gaia dataset. Matthias Steinmetz (AIP)

Combining Gaia DR1, DR2 and Matthias Steinmetz (AIP) a preview on the full Gaia dataset. Matthias Steinmetz (AIP) Combining Gaia DR, DR and Matthias Steinmetz (AIP) a preview on the full Gaia dataset Matthias Steinmetz (AIP) a t a d h AS t 5 - TG E V & A R ase e l e r Ga lact ic D app y lica nam tion ics s Towards

More information

Automated Classification of HETDEX Spectra. Ted von Hippel (U Texas, Siena, ERAU)

Automated Classification of HETDEX Spectra. Ted von Hippel (U Texas, Siena, ERAU) Automated Classification of HETDEX Spectra Ted von Hippel (U Texas, Siena, ERAU) Penn State HETDEX Meeting May 19-20, 2011 Outline HETDEX with stable instrumentation and lots of data ideally suited to

More information

Gaia News:Counting down to launch A. Vallenari. INAF, Padova Astronomical Observatory on behalf of DPACE

Gaia News:Counting down to launch A. Vallenari. INAF, Padova Astronomical Observatory on behalf of DPACE Gaia News:Counting down to launch A. Vallenari INAF, Padova Astronomical Observatory on behalf of DPACE Outline Gaia Spacecraft status The Gaia sky Gaia open and globular clusters From data to science:

More information

Thom et al. (2008), ApJ

Thom et al. (2008), ApJ Star S674 along the same LOS as Complex C Star S441 along the same LOS as Complex C Thom et al. (2008), ApJ Distances to HVCs From spectroscopy of high Galactic latitude stars at small angular separations

More information

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye

Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!

More information

Milky Way star clusters

Milky Way star clusters Using Γα ια for studying Milky Way star clusters Eugene Vasiliev Institute of Astronomy, Cambridge MODEST-, 26 June Overview of Gaia mission Scanning the entire sky every couple of weeks Astrometry for

More information

Signatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars

Signatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars Signatures of Peculiar Supernova Nucleosynthesis in Extremely α-enhanced Metal-poor Stars Hye-Eun Jang 1, Sung-Chul Yoon 1, Young Sun Lee 2, Ho-Gyu Lee 3, Wonseok Kang 4 and Sang-Gak Lee 1 1 Seoul National

More information

FGK 22µm Excess Stars in LAMOST DR2 Stellar Catalog

FGK 22µm Excess Stars in LAMOST DR2 Stellar Catalog Research in Astron. Astrophys. 2012 Vol. X No. XX, 000 000 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics FGK 22µm Excess Stars in LAMOST DR2 Stellar

More information

Potential Synergies Between MSE and the ELTs A Purely TMT-centric perspective But generally applicable to ALL ELTs

Potential Synergies Between MSE and the ELTs A Purely TMT-centric perspective But generally applicable to ALL ELTs Potential Synergies Between MSE and the ELTs A Purely TMT-centric perspective But generally applicable to ALL ELTs Warren Skidmore, TMT Instrument System Scientist 2 nd May, 2018 IPAC Science Talk 1 TMT

More information

GDR1 photometry. CU5/DPCI team

GDR1 photometry. CU5/DPCI team GDR1 photometry CU5/DPCI team What is, or isn't included GDR1 only provides G mean flux and error Derived mean magnitude, all entries Zero point used is in Vega system Zero point for AB system also available

More information

Probing GCs in the GC region with GLAO

Probing GCs in the GC region with GLAO Probing GCs in the GC region with GLAO Masashi Chiba (Tohoku University) AO beginner! Life is good! Subaru/GLAO in Galactic Archaeology Resolved stars provide important information on galaxy formation

More information

Overview of Dynamical Modeling. Glenn van de Ven

Overview of Dynamical Modeling. Glenn van de Ven Overview of Dynamical Modeling Glenn van de Ven glenn@mpia.de 1 Why dynamical modeling? -- mass total mass stellar systems key is to their evolution compare luminous mass: constrain DM and/or IMF DM radial

More information

WHITE DWARFS FROM LAMOST AND A CANDIDATE DEBRIS DISK AROUND WD FROM SDSS

WHITE DWARFS FROM LAMOST AND A CANDIDATE DEBRIS DISK AROUND WD FROM SDSS WHITE DWARFS FROM LAMOST AND A CANDIDATE DEBRIS DISK AROUND WD FROM SDSS GUO JINCHENG( 郭金承 ) PEKING UNIVERSITY COLLABORATOR:LIUJIFENG(NAOC), ZHANG HUAWEI(PKU), ZHAO JINGKUN(NAOC), WANG ZHONGXIANG(SHAO),LI

More information

Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution

Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution Chap.3 The nature of Galactic components Overview of (old) Galactic components bulge, thick disk, metal-weak halo Globular clusters metallicity & age distribution Satellite galaxies spatial and metallicity

More information

Spatial distribution of stars in the Milky Way

Spatial distribution of stars in the Milky Way Spatial distribution of stars in the Milky Way What kinds of stars are present in the Solar neighborhood, and in what numbers? How are they distributed spatially? How do we know? How can we measure this?

More information

Metal Poor Stars: A Review for Non-Observers. Charli Sakari

Metal Poor Stars: A Review for Non-Observers. Charli Sakari Metal Poor Stars: A Review for Non-Observers Charli Sakari Outline Summary: What we know and have discussed already How should we interpret published stellar abundances? Martin Asplund et al.: NOT observed

More information

The Besançon Galaxy Model development

The Besançon Galaxy Model development The Besançon Galaxy Model development Annie C. Robin and collaborators Institut UTINAM, OSU THETA, Université Bourgogne-Franche-Comté, Besançon, France Outline Population synthesis principles New scheme

More information

Igor Soszyński. Warsaw University Astronomical Observatory

Igor Soszyński. Warsaw University Astronomical Observatory Igor Soszyński Warsaw University Astronomical Observatory SATELLITE vs. GROUND-BASED ASTEROSEISMOLOGY SATELLITE: Outstanding precision! High duty cycle (no aliases) HST MOST Kepler CoRoT Gaia IAU GA 2015,

More information

The M31 Globular Cluster System

The M31 Globular Cluster System The M31 Globular Cluster System How alike are the GC systems of the Milky Way and M31? Jean Brodie UCO/Lick Observatory UCSC 1 GCs trace the star formation and assembly GC formation occurs early Accompanies

More information

Exploring the structure and evolu4on of the Milky Way disk

Exploring the structure and evolu4on of the Milky Way disk Exploring the structure and evolu4on of the Milky Way disk Results from the Gaia-ESO survey and plans for 4MOST Thomas Bensby Dept. of Astronomy and Theore3cal Physics Lund University Sweden Chemistry

More information

Milky Way Satellite Galaxies with DES

Milky Way Satellite Galaxies with DES Milky Way Satellite Galaxies with DES Alex Drlica-Wagner kadrlica@fnal.gov! DES Milky Way Working Group Coordinator! January 11, 2015 Milky Way Satellite Galaxies Segue 1 The Milky Way is surrounded by

More information

Our Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.

Our Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Our Galaxy Our Galaxy We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Early attempts to locate our solar system produced erroneous results.

More information

Chapter 14 The Milky Way Galaxy

Chapter 14 The Milky Way Galaxy Chapter 14 The Milky Way Galaxy Spiral Galaxy M81 - similar to our Milky Way Galaxy Our Parent Galaxy A galaxy is a giant collection of stellar and interstellar matter held together by gravity Billions

More information

Building the cosmic distance scale: from Hipparcos to Gaia

Building the cosmic distance scale: from Hipparcos to Gaia The Fundamental Distance Scale: state of the art and the Gaia perspectives 3-6 May 2011 Building the cosmic distance scale: from Hipparcos to Gaia Catherine TURON and Xavier LURI 1 ESA / ESO-H. Heyer Fundamental

More information