The Inner Milky Way Structure with VVV. Marina Rejkuba ESO, Germany
|
|
- Leslie Jordan
- 5 years ago
- Views:
Transcription
1 The Inner Milky Way Structure with VVV Marina Rejkuba ESO, Germany
2 Overview Red Clump stars as distance indicators Dependence on age and metallicity Tracing the bar with RC stars in VVV Inner bar flafening and the bar orientagon The structure behind the bar Based on work published in: Gonzalez, O., et al., 2011, A&A 534, A3 Gonzalez, O., et al., 2011, A&A LeF 534, L14
3 V Catelan 2009 B- V
4 our four target galaxies. The relatively large number of clump stars found in our four fields in Fornax (see Table lowed us to derive their mean K-band magnitudes indially for each field in this galaxy. We did this by selecting stars with K-band magnitudes in the range from 18.3 to mag and J!K colors in the range from 0.3 to 0.85 mag function (1) to the histograms of the K and J magnitudes of red clump stars from the combined data are displayed in Figure 2. The corresponding results of hki = & and hji = & were finally adopted as the mean K- and J-band apparent magnitudes of red clump stars in the Fornax dwarf galaxy. Red Clump in nearby galaxies in near- IR Gonzalez et al.: bulge reddening maps and metallicity gradients VVV Gle b278 3 Fig. 2. J,H and Ks magnitudes differences between VVV catalogs and 2MASS for stars. Dashed horizontal lines show the mean difference between both catalogs in the range denoted by the solid vertical lines Gonzalez t atile l. 2b Fig. 3. Final observed (J-Ks,Ks) CMD forethe once calibrated and completed with 2MASS photometry. range 13>Kvvv >12 for all three bands were used as zero points to be applied to the magnitudes in the VVV catalogs in order to obtain photometry fully consistent with 2MASS. The Data magpietrzynski, ieren UFornax. dalski 2have 003 g. 1. K, J!K near-infrared color-magnitude diagrams for the LMC, G SMC, Carina,& and been combined from the different fields nitude range used for the calibration is based on the fact that ved in each galaxy (see Table 1). 2MASS photometry is very accurate for our purpose down to a magnitude of K2mass 13 and therefore this range ensures that
5 Distance determinagon: recipe 1. ExGncGon correcgon select the reddening law Nishiyama et al. 2009: A K = * [(J- Ks) 0 (J- Ks)] Mean intrinsic color for RC in Baade s Window (J- Ks) 0 = Make a luminosity funcgon and fit it with a 2 nd order polynomial (underlying RGB) + a Gaussian (RC) N(K s0 ) = a + bk s0 + ck 2 s 0 + N RC σ RC 2π exp 3. The peak of the Gaussian is the m(rc) 4. Distance modulus: (m M) 0,target = m RC Κ M RC Κ A Κ [ (K RC s0 K s0 ) 2 2σ 2 RC The results of the Gaussian fits for each RC are lis M Κ RC RC zero point ΔM Κ RC populagon correcgon with respect to populagon used to establish the zero point M λ RC ]
6 Red Clump magnitude variagon as a funcgon of longitude at b=+1, - 1 deg Stars are closer to us at posigve longitude Tile b313 l=-9.3 Tile b317 l=-3.4 Tile b341 l=-9.3 Tile b345 l=-3.4 Tile b320 l=+1.0 Tile b348 l=+1.0 Tile b322 l=+3.9 Tile b350 l=+3.9 Tile b326 l=+9.7 Tile b354 l=+9.7 Gonzalez et al. 2011, A&A LeF
7 K- band RC magnitude Alves 2000; Alves et al MASS & CIO + Hipparcos (Solar Neighb.) Grocholski & Sarajedini 2002 WIYN Open clusters Pietrzynski et al LMC, SMC, Fornax, Carina (Araucaria project) Salaris & Girardi 2002 populagon effects (theoregcal) Percival & Salaris 2003 populagon effects (empirical + models) Laney et al SAAO + Hipparcos (Solar Neighbourhood) Oscar s Bulge metallicity map Percival & Salaris 2003 b l M K = (solar metallicity, 10 Gyr old isochrone: Pietrinferni et al. 2004)
8 From RC distances to structure Gonzalez et al. 2011, A&A LeF
9 Inner bar flafening Model: MarGnez- Valpuesta & Gerhard 2011 Gerhard & MarGnez- Valpuesta 2012
10 And below the plane At b=- 5, ~750 pc below the plane the bar flafens much less Gerhard & MarGnez- Valpuesta 2012 Gonzalez et al. 2012, submifed
11 K=14 Second clump Tile b313 l=-9.3 Tile b341 l=-9.3 Tile b317 l=-3.4 Tile b345 l=-3.4 Tile b320 l=+1.0 Tile b348 l=+1.0 Tile b322 l=+3.9 Tile b350 l=+3.9 Tile b326 l=+9.7 Tile b354 l=+9.7 Y (kpc) K= kpc 3 kpc 2 kpc 1 kpc K=13 K=12.5 K=12 K=11 X (kpc) K=11.5
12 SGll some head scratching l=+10 l= Tile: b255 l = 8, b=- 6.5 Second clump ~2.5 kpc behind the bar and ~ 1kpc below the plane! l=+1 l= Ks l=- 4 l= Residual Ks
13 Summary VVV depth and resolugon provides ideal dataset for inner Bulge structure studies RC, eclipsing binaries, RR Lyr à tracing different components? Complexity: patchy exgncgon (BEAM calculator) Mix of populagons bar/bulge, thin disk and spiral arms, thick disk? Comparison with models
The Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way
Figure 70.01 The Milky Way Wide-angle photo of the Milky Way Overview: Number of Stars Mass Shape Size Age Sun s location First ideas about MW structure Figure 70.03 Shapely (~1900): The system of globular
More informationarxiv: v1 [astro-ph.ga] 5 Oct 2011
Astronomy & Astrophysics manuscript no. vvv2 accepted leng ref c ESO 2013 April 29, 2013 The inner Galactic bar traced by the VVV survey O. A. Gonzalez 1, M. Rejkuba 1, D. Minniti 2,3,4, M. Zoccali 2,
More informationStudying the Milky Way with pulsating stars
Studying the Milky Way with pulsating stars ( 東京大学 ) Noriyuki Matsunaga (The University of Tokyo) The first C-rich Miras found in the bulge All the AGB stars confirmed in the bulge were O-rich. C-rich
More informationSpatial 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 informationTHE 2MASS COLOR-MAGNITUDE DIAGRAM OF THE GLOBULAR CLUSTER LYNG8Å7 1
The Astronomical Journal, 1281228 1232, 2004 September # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 2MASS COLOR-MAGNITUDE DIAGRAM OF THE GLOBULAR CLUSTER LYNG8Å7
More informationSTELLAR PHOTOMETRY IN THE LOCAL GROUP DWARF GALAXY CETUS
STELLAR PHOTOMETRY IN THE LOCAL GROUP DWARF GALAXY CETUS Tutor: Marina Rejkuba Introduction Nataliya Kovalenko Data reduction and PSF photometry Maria Morales Aperture photometry Loredana Spezzi Results
More informationTechniques for measuring astronomical distances generally come in two variates, absolute and relative.
Chapter 6 Distances 6.1 Preliminaries Techniques for measuring astronomical distances generally come in two variates, absolute and relative. Absolute distance measurements involve objects possibly unique
More informationW. Gieren ABSTRACT. of project number 69.D Based on observations obtained with the NTT telescope at the European Southern Observatory as part
The ARAUCARIA project: Deep near-infrared survey of nearby galaxies. I. The distance to the Large Magellanic Cloud from -band photometry of red clump stars 1 G. Pietrzyński Universidad de Concepción, Departamento
More informationReddening map of the Large Magellanic Cloud bar region. A. Subramaniam
A&A 430, 421 426 (2005) DOI: 10.1051/0004-6361:20041279 c ESO 2005 Astronomy & Astrophysics Reddening map of the Large Magellanic Cloud bar region A. Subramaniam Indian Institute of Astrophysics, II Block,
More informationSMASHing the LMC. Yumi Choi. Montana State University/University of Arizona. Collaborator
SMASHing the LMC Montana State University/University of Arizona Collaborator David Nidever, Knut Olsen, Gurtina Besla, Robert Blum, Dennis Zaritsky, Roeland van der Marel, Eric Bell, Carme Gallart, Maria-Rosa
More informationPopulation synthesis models
Population synthesis models From stellar evolution models to synthetic populations in the Milky Way Léo Girardi OAPadova INAF Italy LIneA Rio de Janeiro Brazil GAIA/ITN School, Tenerife, Sep 2013 Léo Girardi
More informationBuilding 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 informationRecent Researches concerning Semi-Regular Variables
Recent Researches concerning Semi-Regular Variables I.S. Glass (SAAO) ASSA Symposium, Durban 2008 Distances in the Universe - the distance ladder a summary Trig parallaxes only direct method Variable stars
More informationTHE 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 informationMulti-wavelength study of the Milky Way Galaxy
29 th ASI Meeting ASI Conference Series, 2011, Vol. 3, pp 79 83 Edited by Pushpa Khare & C. H. Ishwara-Chandra Multi-wavelength study of the Milky Way Galaxy Shashikiran Ganesh Physical Research Laboratory,
More informationUniversity of Naples Federico II, Academic Year Istituzioni di Astrofisica, read by prof. Massimo Capaccioli. Lecture 16
University of Naples Federico II, Academic Year 2011-2012 Istituzioni di Astrofisica, read by prof. Massimo Capaccioli Lecture 16 Stellar populations Walter Baade (1893-1960) Learning outcomes The student
More informationUsing the HR Diagram to Measure the Star Formation Histories of Galaxies. Tammy Smecker-Hane University of California, Irvine
Using the HR Diagram to Measure the Star Formation Histories of Galaxies Tammy Smecker-Hane University of California, Irvine tsmecker@uci.edu Irvine, California 1 Outline 1. Stellar Evolution Hertzsprung-Russell
More informationThe 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 informationTaurus stars membership in the Pleiades open cluster
Taurus stars membership in the Pleiades open cluster Tadross, A. L., Hanna, M. A., Awadalla, N. S. National Research Institute of Astronomy & Geophysics, NRIAG, 11421 Helwan, Cairo, Egypt ABSTRACT In this
More informationSurface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationClassical Methods for Determining Stellar Masses, Temperatures, and Radii
Classical Methods for Determining Stellar Masses, Temperatures, and Radii Willie Torres Harvard-Smithsonian Center for Astrophysics 2010 Sagan Exoplanet Summer Workshop 1 Outline Basic properties of stars
More informationAstr 5465 Feb. 5, 2018 Kinematics of Nearby Stars
Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Properties of Nearby Stars Most in orbit with the Sun around Galactic Center Stellar Kinematics Reveal Groups of Stars with Common Space Motion (Moving
More informationDwarf spheroidal satellites of M31: Variable stars and stellar populations
Dwarf spheroidal satellites of M31: Variable stars and stellar populations Felice Cusano INAF-Osservatorio Astronomico di Bologna LBT Team Italy collaborators: Gisella Clementini, Alessia Garofalo, Michele
More informationLecture Five: The Milky Way: Structure
Lecture Five: The Milky Way: Structure The Celestial Sphere http://www.astro.rug.nl/~etolstoy/pog14 We use equatorial coordinates to determine the positions of stars in the sky. A stars declination (like
More informationThe Star Clusters of the Magellanic Clouds
The Dance of Stars MODEST-14 The Star Clusters of the Magellanic Clouds Eva K. Grebel Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Star Clusters in the Magellanic Clouds!
More informationUNIVERSITY OF SOUTHAMPTON
UNIVERSITY OF SOUTHAMPTON PHYS2013W1 SEMESTER 1 EXAMINATION 2012/13 GALAXIES Duration: 120 MINS Answer all questions in Section A and two and only two questions in Section B. Section A carries 1/3 of the
More informationThe structure of the Milky Way s bar outside the bulge
doi:10.1093/mnras/stv745 The structure of the Milky Way s bar outside the bulge Christopher Wegg, Ortwin Gerhard and Matthieu Portail Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse,
More informationThe chemical evolution of the Galactic Bulge seen through micro-lensing events
The chemical evolution of the Galactic Bulge seen through micro-lensing events Sofia Feltzing Lund Observatory Main collaborators: Martin Asplund (MPA),Thomas Bensby (Lund), Andy Gold (Ohio), Jennifer
More informationSpectroscopy of Blue Supergiants in the Disks of Spiral Galaxies: Metallicities and Distances. Rolf Kudritzki
Spectroscopy of Blue Supergiants in the Disks of Spiral Galaxies: Metallicities and Distances Rolf Kudritzki ΛCDM-universe metallicity of galaxies depends on their mass Extragalactic stellar astronomy
More informationAn Extended View of the Pulsating Stars in the Carina Dwarf Spheroidal Galaxy
Kathy Vivas (CIDA, Venezuela) & Mario Mateo (University of Michigan, USA) ESO/G. Bono & CTIO An Extended View of the Pulsating Stars in the Carina Dwarf Spheroidal Galaxy CMD from Monelli et al (2003)
More informationZoccali 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 informationOptical photometry of the old Open Cluster Ruprecht 6 and the Galactic Metallicity Gradient
Optical photometry of the old Open Cluster Ruprecht 6 and the Galactic Metallicity Gradient Gye Ryong Mountain (845 m) Dong Hak Buddist Temple (near KASI) Sang Chul KIM Korea Astronomy and Space Science
More informationHubble sequence galaxy classification scheme, originally based on appearance, but correlates with other properties as well.
Normal Galaxies (Ch. 24) Here we will cover topics in Ch. 24 up to 24.4, but then skip 24.4, 24.5. The sections we are skipping are all about processes that occur in the centers of galaxies, so I d like
More informationChapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
More informationThe Milky Way Part 3 Stellar kinematics. Physics of Galaxies 2011 part 8
The Milky Way Part 3 Stellar kinematics Physics of Galaxies 2011 part 8 1 Stellar motions in the MW disk Let s continue with the rotation of the Galaxy, this time from the point of view of the stars First,
More informationThe Milky Way Part 2 Stellar kinematics. Physics of Galaxies 2012 part 7
The Milky Way Part 2 Stellar kinematics Physics of Galaxies 2012 part 7 1 Stellar motions in the MW disk Let s look at the rotation of the Galactic disk First, we need to introduce the concept of the Local
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationA Reinvestigation of the Physical Properties of Pismis 3 based on 2MASS Photometry
Chin. J. Astron. Astrophys. Vol. 8 (2008), No. 3, 362 368 (http://www.chjaa.org) Chinese Journal of Astronomy and Astrophysics A Reinvestigation of the Physical Properties of Pismis 3 based on 2MASS Photometry
More informationThe Color-Magnitude Diagram for local stars from Hipparcos. Red Giant Branch (RGB) Red clump. Absolute Magnitude Main Sequence. White dwarfs.
The Color-Magnitude Diagram for local stars from Hipparcos Absolute Magnitude Main Sequence Red clump Red Giant Branch (RGB) White dwarfs Kovalevsky 1998 Color Lebreton 2001 The Hipparcos H-R Diagram of
More informationThe Great Debate: The Size of the Universe (1920)
The Great Debate: The Size of the Universe (1920) Heber Curtis Our Galaxy is rather small, with Sun near the center. 30,000 LY diameter. Universe composed of many separate galaxies Spiral nebulae = island
More informationA wide-field view of the Phoenix transition type dwarf galaxy (Battaglia et al., MNRAS accepted, airxv/ )
A wide-field view of the Phoenix transition type dwarf galaxy (Battaglia et al., MNRAS accepted, airxv/1205.2704) Giuseppina Battaglia INAF Astronomical Observatory of Bologna With thanks to M.Rejkuba,
More informationObserving Miras as tracers of the inner part of the Milky Way
Observing Miras as tracers of the inner part of the Milky Way ( 東京大学 ) Noriyuki Matsunaga (The University of Tokyo) Outline Introduction Miras as tracers of the Milky Way Case study 1 Miras in the bulge
More informationSUPPLEMENTARY INFORMATION
1. Identification of classical Cepheids: We identified three classical Cepheids amongst the 45 short-period variables discovered. Our sample includes classical Cepheids, type II Cepheids, eclipsing binaries
More informationM31 Color Mag Diagram Brown et al 592:L17-L20!
The physical origin of the form of the IMF is not well understood Use the stellar mass-luminosity relation and present day stellar luminosity function together with a model of how the star formation rate
More informationAge Dating A SSP. Quick quiz: please write down a 3 sentence explanation of why these plots look like they do.
Color is only a weak function of age after ~3Gyrs (for a given metallicity) (See MBW pg 473) But there is a strong change in M/L V and weak change in M/L K Age Dating A SSP Quick quiz: please write down
More informationGaia Revue des Exigences préliminaires 1
Gaia Revue des Exigences préliminaires 1 Global top questions 1. Which stars form and have been formed where? - Star formation history of the inner disk - Location and number of spiral arms - Extent of
More informationTHE GALACTIC BULGE AS SEEN BY GAIA
143 THE GALACTIC BULGE AS SEEN BY GAIA C. Reylé 1, A.C. Robin 1, M. Schultheis 1, S. Picaud 2 1 Observatoire de Besançon, CNRS UMR 6091, BP 1615, 25010 Besançon cedex, France 2 IAG/USP Departamento de
More informationStellar Population Synthesis: The Role of Adaptive Optics
Stellar Population Synthesis: The Role of Adaptive Optics Jason Melbourne (Caltech) Nearby (2.5 Mpc) Dwarf Irregular Galaxy KKH 98 HST F475W (Blue), HST F814W (Green), Keck AO K-band (red) Melbourne et
More informationNormal Galaxies ASTR 2120 Sarazin
Normal Galaxies ASTR 2120 Sarazin Test #2 Monday, April 8, 11-11:50 am ASTR 265 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other materials or any person
More informationData Reduction with NIRI. Knut Olsen and Andrew Stephens Gemini Data Workshop Tucson, AZ July 21, 2010
Data Reduction with NIRI Knut Olsen and Andrew Stephens Gemini Data Workshop Tucson, AZ July 21, 2010 Near InfraRed Imager and Spectrometer Built by UH/IfA Science data since 2002 Primary reference: Hodapp
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationThe Milky Way Formation Timescale
Mem. S.A.It. Vol. 75, 13 c SAIt 2004 Memorie della The Milky Way Formation Timescale A. Aparicio 1,2, A. Rosenberg 2, G. Piotto 3, I. Saviane 4 and A. Recio-Blanco 3 1 Departamento de Astrofisica, Universidad
More informationThe 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 informationGalaxies. Lecture Topics. Lecture 23. Discovering Galaxies. Galaxy properties. Local Group. History Cepheid variable stars. Classifying galaxies
Galaxies Lecture 23 APOD: NGC 3628 (The Hamburger Galaxy) 1 Lecture Topics Discovering Galaxies History Cepheid variable stars Galaxy properties Classifying galaxies Local Group 2 23-1 Discovering Galaxies
More informationarxiv: v1 [astro-ph.ga] 1 Apr 2013
First identification and absolute magnitudes of the red clump stars in the Solar neighbourhood for WISE arxiv:1304.0435v1 [astro-ph.ga] 1 Apr 2013 E. Yaz Gökce a,, S. Bilir a, N. D. Öztürkmena, Ş. Duran
More informationPractice Problem!! Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.
Practice Problem Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.05 cm -3 (a) estimate the minimum mass that could collapse, (b) what is the
More informationThe Milky Way Galaxy and Interstellar Medium
The Milky Way Galaxy and Interstellar Medium Shape of the Milky Way Uniform distribution of stars in a band across the sky lead Thomas Wright, Immanuel Kant, and William Herschel in the 18th century to
More informationSimple Stellar Populations
Stellar Objects: Simple Stellar Populations 1 Simple Stellar Populations 1 Theoretical isochrones Update date: December 14, 2010 Simple Stellar Population consists of stars born at the same time and having
More informationModelling the Milky Way bar
Modelling the Milky Way bar Shude Mao Tsinghua University/NAOC June 25, 2015@IPMU Collaborators: Yougang Wang, Richard Long, Juntai Shen, Liang Cao, Outline! Observed properties of barred galaxies " The
More informationReview of the Bulge Stellar Population And Comparison to the Nuclear Bulge
Review of the Bulge Stellar Population And Comparison to the Nuclear Bulge David M. Nataf, Australian National University 22 July, 2016 IAU Symposium 322, 'The Multi- Messenger Astrophysics of the Galactic
More informationAstronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION CHAPTER 14 The Milky Way Galaxy Lecture Presentation 14.0 the Milky Way galaxy How do we know the Milky Way exists? We can see it even though
More information2MASS observations of spectroscopically identified extragalactic C stars
2MASS observations of spectroscopically identified extragalactic C stars Serge Demers and Mathieu Dallaire Département de Physique Université de Montréal, Montreal, Qc H3C 3J7, Canada and Paolo Battinelli
More informationDISTANCES TO POPULOUS CLUSTERS IN THE LARGE MAGELLANIC CLOUD VIA THE K-BAND LUMINOSITY OF THE RED CLUMP
The Astronomical Journal, 134:680Y693, 2007 August # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. DISTANCES TO POPULOUS CLUSTERS IN THE LARGE MAGELLANIC CLOUD VIA THE
More informationChapter 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 informationExploring 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 informationDust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.
More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column
More informationChapter 8: Simple Stellar Populations
Chapter 8: Simple Stellar Populations Simple Stellar Population consists of stars born at the same time and having the same initial element composition. Stars of different masses follow different evolutionary
More informationLuminosity Functions of Planetary Nebulae & Globular Clusters. By Azmain Nisak ASTR 8400
Luminosity Functions of Planetary Nebulae & Globular Clusters By Azmain Nisak ASTR 8400 Calculating Distance! m = apparent magnitude! M = absolute magnitude! r = distance in pc GLOBULAR CLUSTERS AS DISTANCE
More informationarxiv:astro-ph/ v1 22 Mar 2000
K-Band Calibration of the Red Clump Luminosity David R. Alves Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218 Email: alves@stsci.edu arxiv:astro-ph/0003329v1 22 Mar 2000 ABSTRACT
More informationarxiv: v1 [astro-ph.ga] 16 May 2011
The Edge of the Milky Way Stellar Disk Revealed Using Clump Giant Stars as Distance Indicators arxiv:1105.3151v1 [astro-ph.ga] 16 May 2011 D. Minniti 1,2,3, R. K. Saito 1, J. Alonso-García 1, P. W. Lucas
More informationAstronomy 330 Lecture 7 24 Sep 2010
Astronomy 330 Lecture 7 24 Sep 2010 Outline Review Counts: A(m), Euclidean slope, Olbers paradox Stellar Luminosity Function: Φ(M,S) Structure of the Milky Way: disk, bulge, halo Milky Way kinematics Rotation
More informationOUR DUSTY MILKY WAY: CONSTRAINING THE DUST DISTRIBUTION IN THE DISK OF OUR GALAXY
OUR DUSTY MILKY WAY: CONSTRAINING THE DUST DISTRIBUTION IN THE DISK OF OUR GALAXY Gail Zasowski 1 Advisor: Steven R. Majewski 1 1 Department of Astronomy, University of Virginia, Charlottesville, VA, 22904
More informationUniversita degli Studi di Padova Facoltà di Scienze MM.FF.NN.
Universita degli Studi di Padova Facoltà di Scienze MM.FF.NN. Dipartimento di Astronomia Scuola di Dottorato in Astronomia A R C S : T H E A S I A G O R E D C L U M P S P E C T R O S C O P I C S U R V
More informationThe 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 informationStellar Evolution & issues related to the post Turn-Off evolution
Stellar Evolution & issues related to the post Turn-Off evolution Santi Cassisi INAF - Astronomical Observatory of Teramo, Italy The point of view of Population Synthesis users What do they want? Magnitudes
More information6. Detached eclipsing binaries
Rolf Kudritzki SS 2015 6. Detached eclipsing binaries 50% of all stars live in binary systems and some of them are eclipsing 1 Rolf Kudritzki SS 2015 classification of binary systems by geometry of equipotential
More informationLecture 27 Galaxy Types and the Distance Ladder December 3, 2018
Lecture 27 Galaxy Types and the Distance Ladder December 3, 2018 1 2 Early Observations Some galaxies had been observed before 1900 s. Distances were not known. Some looked like faint spirals. Originally
More informationIntro to SQL. Two components. Data Definition Language (DDL): create table, etc. Data Manipulation Language (DML):
Intro to SQL Two components Data Definition Language (DDL): create table, etc. Data Manipulation Language (DML): select, insert, delete, update, etc. The basic SELECT statement: Select From Where A1, A2,...AN
More informationAbundance 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 informationProper motion measurements as indicators of binarity in open clusters. E. Bica and C. Bonatto
A&A 431, 43 51 (25) DOI:.51/4-6361:24223 c ESO 25 Astronomy & Astrophysics Proper motion measurements as indicators of binarity in open clusters E. Bica and C. Bonatto Universidade Federal do Rio Grande
More informationSurface Photometry Quantitative description of galaxy morphology. Hubble Sequence Qualitative description of galaxy morphology
Hubble Sequence Qualitative description of galaxy morphology Surface Photometry Quantitative description of galaxy morphology Galaxy structure contains clues about galaxy formation and evolution Point
More informationAS1001: Galaxies and Cosmology
AS1001: Galaxies and Cosmology Keith Horne kdh1@st-and.ac.uk http://www-star.st-and.ac.uk/~kdh1/eg/eg.html Text: Kutner Astronomy:A Physical Perspective Chapters 17-21 Cosmology Today Blah Title Current
More informationEvolution of Galaxies: IMF SFR - SFH
Evolution of Galaxies: IMF SFR - SFH J.Köppen joachim.koppen@astro.unistra.fr http://astro.u-strasbg.fr/~koppen/jkhome.html Galactic (Chemical) Evolution is driven by stars which burn hydrogen on the Main
More informationTristan Cantat-Gaudin
Open Clusters in the Milky Way with Gaia ICCUB Winter Meeting 1-2 Feb 2018, Barcelona Tristan Cantat-Gaudin Carme Jordi, Antonella Vallenari, Laia Casamiquela, and Gaia people in Barcelona and around the
More informationStellar Populations in the Local Group
Stellar Populations in the Local Group Recall what we ve learned from the Milky Way: Age and metallicity tend to be correlated: older -> lower heavy element content younger -> greater heavy element content
More informationClicker Question: Clicker Question: Clicker Question: Clicker Question: What is the remnant left over from a Type Ia (carbon detonation) supernova:
Test 3 results D C Grades posted in cabinet and Grades posted on-line B A F If you are not properly registered then come see me for your grade What is the ultimate origin of the elements heavier than helium
More informationA photometric study of the intermediate age open cluster King 5
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 06 (03.11.1; 16.06.1; 19.06.1; 19.37.1; 19.53.1; 19.63.1) ASTRONOMY AND ASTROPHYSICS A photometric study of the intermediate
More informationMeasuring the distances, masses and radii of neutron stars
Measuring the distances, masses and radii of neutron stars Tolga Güver, Feryal Özel, Antonio Cabrera-Lavers, Patricia Wroblewski, Larry Camarota, Dimitrios Psaltis University of Arizona 1 Distances, Masses,
More information2016 Bogotá, Colombia
ADELA PRODUCTS: 2016 Bogotá, Colombia Movies The VVV Survey Extension: RRLyrae, Cepheids and more Dante Minniti The VVV Science Team Dante Minniti VVV Latest Results 1. RR Lyrae in the Bulge-Halo Transition
More informationThe Milky Way & Galaxies
The Milky Way & Galaxies The Milky Way Appears as a milky band of light across the sky A small telescope reveals that it is composed of many stars (Galileo again!) Our knowledge of the Milky Way comes
More informationGalaxies The Hubble Sequence Different Types of Galaxies 4 broad Morphological Types created by Edwin Hubble Galaxies come is a variety of shapes and
Galaxies The Hubble Sequence Different Types of Galaxies 4 broad Morphological Types created by Edwin Hubble Galaxies come is a variety of shapes and sizes Edwin Hubble classified the galaxies into four
More informationThe Physics of the Interstellar Medium
The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,
More informationGalaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).
Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution
More informationEinführung in die Astronomie II
Einführung in die Astronomie II Teil 12 Peter Hauschildt yeti@hs.uni-hamburg.de Hamburger Sternwarte Gojenbergsweg 112 21029 Hamburg 13. September 2017 1 / 77 Overview part 12 The Galaxy Historical Overview
More informationGalaxies -- Introduction. Classification -- Feb 13, 2014
Galaxies -- Introduction Classification -- Feb 13, 2014 Why Begin with Classification? The Hubble system forms the basic vocabulary of the subject. The sequence of galaxy types reflects an underlying physical
More informationDistance Measuring Techniques and The Milky Way Galaxy
Distance Measuring Techniques and The Milky Way Galaxy Measuring distances to stars is one of the biggest challenges in Astronomy. If we had some standard candle, some star with a known luminosity, then
More informationThe magnitude system. ASTR320 Wednesday January 30, 2019
The magnitude system ASTR320 Wednesday January 30, 2019 What we measure: apparent brightness How bright a star appears to be in the sky depends on: How bright it actually is Luminosity and its distance
More informationTesting the COBE/IRAS All-Sky Reddening Map Using the Galactic Globular Clusters
Testing the COBE/IRAS All-Sky Reddening Map Using the Galactic Globular Clusters K. Z. Stanek 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS20, Cambridge, MA 02138 e-mail: kstanek@cfa.harvard.edu
More informationLecture Three: Stellar Populations. Stellar Properties: Stellar Populations = Stars in Galaxies. What defines luminous properties of galaxies
Lecture Three: ~2% of galaxy mass in stellar light Stellar Populations What defines luminous properties of galaxies face-on edge-on https://www.astro.rug.nl/~etolstoy/pog16/ 18 th April 2016 Sparke & Gallagher,
More information