Do we know all the Milky Way Globular Clusters? Dirk Froebrich
|
|
- Buck O’Brien’
- 5 years ago
- Views:
Transcription
1 Do we know all the Milky Way Globular Clusters? Dirk Froebrich
2 People 1) Candidates from the FSR Cluster Sample A. Scholz H. Meusinger C.J. Davis C.L. Raftery 2) Candidates from the GPS and Mercer list A. Longmore R. Kurtev T. Macarone P.W. Lucas V.D. Ivanov D. Minniti J. Borissova R. de Grijs
3 Known Galactic Globular Clusters 158 kown (pre FSR catalogue or 2007) Harris (1996, 2003) lists 150, + Glimpse-C01 (Kobulnicky et al. 2005), GC Whiting1 (Carraro et al. 2005), SDSS J SDSS J (Willman et al. 2005), AL3 (Ortolani et al. 2006), GC SEGUE1 (Belokurov et al. 2007), Koposov1 Koposov2 (Koposov et al. 2007)
4 Whybother? apparent difference in numbers of MW Globular Clusters compared to e.g. the Andromeda galaxy true or selection effect? study the formation and evolution of the Galaxy some GlCls are from captured dwarf galaxies probe the structure of the Galaxy
5 The FSR Cluster Sample
6 The FSR Cluster Sample Zone of Avoidance High extinction and star density low density contrast between cluster and background distant clusters are obscured by dust 10±3 GlCl are missing within 3kpc from the Galactic Center and near the Galactic Plane (Z<0.5kpc) (Ivanov et al. 2005) Froebrich et al. (2007)
7 The FSR Cluster Sample JHK star density maps 14400square degrees each 3.5 resolution 20 pixels 0.5GigaPixel images 120hours computing time on 16node double processor Beowulf-type cluster Froebrich et al. (2007)
8 The FSR Cluster Sample Search for local enhancements in JHK star density maps use SExtractor (Bertin & Arnouts 1996) 4σ above local (10 x5 ) noise and >11square arcmin + manual search cloud edges and spikes of bright stars rejected fainter objects with cluster like appearance added every cluster must be detected in H and (J or K) 2iterations between two people for validation! Froebrich et al. (2007)
9 The FSR Cluster Sample 1788 cluster candidates detected 782 automatically, 1006 manually ratio of auto/manu constant along Galactic Plane SIMBAD cross referencing: 86 known GlCl (out of 93 with d<17kpc in this area) 681 known OpCl 1021 new cluster candidates ~500 real new clusters
10 Classification King (1962) radial density profile Automatic fit at local completeness limit, excluding regions with source confusion (dense cluster centers) Manual verification of validity via majority decision Froebrich et al. (2007)
11 Classification P Op/Gl = N Op/Gl / (N Op + N Gl ) for each plot and cluster plot i Froebrich et al. (2007) /(681/86)
12 Classification new GlCl (85%) OpCl (95%) Froebrich et al. (2007)
13 Classification of Star Clusters C1716 Log(R N )= Glimpse C01 Log(R N )=-0.851
14 Classification of Star Clusters C1735 Log(R N )= Glimpse C01 Log(R N )=-0.851
15 The FSR Cluster Sample Froebrich et al. (2007)
16 The Mercer Cluster Sample 92 new clusters identified in GLIMPSE data Automatic detection based on Bayesian information criterion 59 detected only 6 of these detected in 2MASS automatically 24 show clustering visually 33 objects found by visual inspection of images Mercer et al. (2005)
17 FSR 1735 Froebrich et al. (2007b/2008b)
18 FSR 1735 ESO NTT
19 Fore/Background decontamination Stars in cells in J, (J-H) and (J-K) space in cluster and control field are counted and stars are randomly removed according to statistics (Bonatto & Bica 2007). Cells vary in size according to stellar density. Typically they are ΔJ=0.5mag, Δ(J-H)=0.2mag and Δ(J-K)=0.2mag.
20 Isochrone Fitting Froebrich et al. (2008b) Age>8Gyrs Ak=0.7mag d=7.0kpc [M/H]=-0.7
21 FSR 1716 Froebrich et al. (2008b)
22 FSR 1716 ESO NTT
23 Isochrone Fitting Froebrich et al. (2008b) Age>2Gyrs Ak=0.57mag d=7kpc [M/H]=-0.7±0.4
24 FSR 0584 Classified as probable Globular Cluster by Bica et al. (2007) based on 2MASS and proper motions
25 FSR0584 Bica et al. 2007, A&A, 472, 483 FSR0584 Log(R N )= Based on JHK data and proper motions, its most probably a GlCl. Projected onto W3 cloud. The closest known GlCl! d=1.4kpc A V = mag R core = pc R tid = pc
26 FSR 1767 Classified as Globular Cluster by Bonatto et al. (2007) based on 2MASS and proper motions but Froebrich et al. (2008b)
27 FSR 1767 ESO NTT
28 Fore/Background decontamination
29 Isochrone Fitting Bonatto et al. (2007) Age=10Gyrs Ak=0.62mag d=1.5kpc [M/H]=-1.3
30 Isochrone Fitting Froebrich et al. (2008b) Age=1.25Gyrs Ak=0.4mag d=8.5kpc [M/H]=+0.0
31 Mercer 3 Kurtev et al. (2008)
32 Mercer 3 ESO NTT Kurtev et al. (2008)
33 Mercer 3 Kurtev et al. (2008), A&A, accepted or Strader & Kobulnicky (2008) subm. on astro-ph two days later... Kurtev et al. (2008) Age=??? Ak=2.7mag d=4.6kpc [Fe/H]=-0.33
34 Mercer 5 from Mercer et al. (2005), but independently found in UKIDSS quality control Longmore et al. (2009) in prep.
35 Mercer 5 ESO NTT +UKIDSS
36 Mercer5 Longmore et al. (2009) [Fe/H]=-0.94±0.16
37 Mercer5 Longmore et al. (2009) Age=??? Ak=1.1±0.1mag d=5-6kpc [Fe/H]=-0.94
38 Known Galactic Globular Clusters ? kown 150 in Harris (1996, 2003) + Glimpse-C01 (Kobulnicky et al. 2005), GC Whiting1 (Carraro et al. 2005), SDSS J /J (Willman et al. 2005), AL3 (Ortolani et al. 2006), GC SEGUE1 (Belokurov et al. 2007), Koposov1/2 (Koposov et al. 2007), FSR1735 (Froebrich et al. 2007b/2008b), FSR1767 (Bonatto et al. 2007), FSR0584? (Bica et al. 2007), FSR0190? (Froebrich et al. 2008c), FSR1716 (Froebrich et al. 2008b), Mercer3 (Kurtev et al. 2008), Mercer5 (Longmore et al. 2009)
39 Properties of new GlCls some part of the missing population within ~3kpc from the Galactic Centre (e.g. FSR1735, Mercer3, Mercer5)
40 Properties of new GlCls some part of the missing population within ~3kpc from the Galactic Centre (e.g. FSR1735, Mercer3, Mercer5) metallicities within [M/H] = at lower end of luminosity distribution Palomar GlCls
41 Do we know all the Milky Way Globular Clusters? Probably not, but: Further objects of the known cluster candidates from the FSR, Mercer and future GPS list might be classified as GlCl. There are no more obvious, overlooked objects in 2MASS and Glimpse. The lower end of the luminosity function is still incomplete.
42 Conclusions We have identified 1021 new star cluster candidates with b <20 in star density maps (40-50% contamination rate). Follow up observations/analyses have so far revealt 3 new galactic GlCl candidates from the FSR list (plus a number of old OpCl). At least deep NIR imaging is required to verify their nature. 2MASS alone is insufficient in some cases (e.g. FSR1767)! The Mercer list of clusters also revealt 2 GlCls so far. More, probably Palomar Type GlCls, are likely to be found amongst the FSR, Mercer, and GPS lists.
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 informationDeciphering the origin of globular clusters near the Galactic bulge + more. Masashi Chiba (Tohoku University)
Deciphering the origin of globular clusters near the Galactic bulge + more Masashi Chiba (Tohoku University) ULTIMATE-Subaru in Galactic Archaeology Resolved stars provide important information on galaxy
More informationarxiv: v1 [astro-ph.ga] 11 Dec 2010
Astronomy & Astrophysics manuscript no. Minniti c ESO 2013 October 31, 2013 Discovery of VVV CL001. A Low-Mass Globular Cluster Next to UKS 1 in the Direction of the Galactic Bulge D. Minniti 1, M. Hempel
More informationWhat 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 informationarxiv: v1 [astro-ph] 10 May 2007
A Pair of Boötes: A New Milky Way Satellite S. M. Walsh 1, H. Jerjen 1, B. Willman 2 arxiv:0705.1378v1 [astro-ph] 10 May 2007 ABSTRACT As part of preparations for a southern sky search for faint Milky
More informationarxiv: v1 [astro-ph.ga] 24 Jun 2014
Astronomy& Astrophysics manuscript no. hlc_arxiv c ESO 2018 September 26, 2018 Global survey of star clusters in the Milky Way III. 139 new open clusters at high Galactic latitudes S. Schmeja 1, N. V.
More informationMilky 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 informationStellar Stream map of the Milky Way Halo : Application of STREAMFINDER onto ESA/Gaia DR2
Stellar Stream map of the Milky Way Halo : Application of STREAMFINDER onto ESA/Gaia DR2 w/ Rodrigo A. Ibata and Nicolas F. Martin @kmalhan07 Khyati Malhan PhD Student Supervisor: Dr. Rodrigo Ibata Stellar
More informationAL 3 (BH 261): a new globular cluster in the Galaxy
AL 3 (BH 261): a new globular cluster in the Galaxy S. Ortolani 1,2,3 and E. Bica4 arxiv:astro-ph/0606718v1 29 Jun 2006 and B. Barbuy5 ABSTRACT AL 3 (BH 261), previously classified as a faint open cluster
More informationMilky 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 informationarxiv: v4 [astro-ph] 18 Jun 2008
Chinese Journal of Astronomy and Astrophysics manuscript no. (L A TEX: chjaa.tex; printed on April 18, 2017; 6:18) Chin. J. Astron. Astrophys. Vol. 8 (2008), No. 3, 362 Received 2007 May 31; accepted 2008
More informationarxiv: v1 [astro-ph] 5 Dec 2007
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 25 October 201 (MN LATEX style file v2.2) Probing FSR star cluster candidates in bulge/disk directions with 2MASS colour-magnitude diagrams arxiv:012.062v1
More informationA galaxy is a self-gravitating system composed of an interstellar medium, stars, and dark matter.
Chapter 1 Introduction 1.1 What is a Galaxy? It s surprisingly difficult to answer the question what is a galaxy? Many astronomers seem content to say I know one when I see one. But one possible definition
More informationSpiral Structure. m ( Ω Ω gp ) = n κ. Closed orbits in non-inertial frames can explain the spiral pattern
Spiral Structure In the mid-1960s Lin and Shu proposed that the spiral structure is caused by long-lived quasistatic density waves The density would be higher by about 10% to 20% Stars, dust and gas clouds
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 informationA populous intermediate-age open cluster and evidence of an embedded cluster among the FSR globular cluster candidates
Mon. Not. R. Astron. Soc. 34, 1733 1740 (200) doi:./j.65-266.200.1263.x A populous intermediate-age open cluster and evidence of an embedded cluster among the FSR globular cluster candidates E. Bica and
More informationASTR 200 : Lecture 22 Structure of our Galaxy
ASTR 200 : Lecture 22 Structure of our Galaxy 1 The 'Milky Way' is known to all cultures on Earth (perhaps, unfortunately, except for recent city-bound dwellers) 2 Fish Eye Lens of visible hemisphere (but
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 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 informationThe Structural Properties of Milky Way Dwarf Galaxies. Ricardo Muñoz (Universidad de Chile) Collaborators:
The Structural Properties of Milky Way Dwarf Galaxies Ricardo Muñoz (Universidad de Chile) Milky Way inner 100 kpc Collaborators: Marla Geha (Yale) Patrick Côté (HIA/DAO) Peter Stetson (HIA/DAO) Josh Simon
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 informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa Instituto de astrofisica de Canarias Gran Telescopio Canarias The idea for this study sparked from the desire of
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 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 informationarxiv: v1 [astro-ph.ga] 3 Mar 2014
CCD BVRI and 2MASS Photometry of the Poorly Studied Open Cluster NGC 6631 arxiv:1403.0546v1 [astro-ph.ga] 3 Mar 2014 Tadross, A. L. a, Bendary, R. a, Priya, H. b, Essam, A. a, Osman, A. a a National Research
More informationView of the Galaxy from within. Lecture 12: Galaxies. Comparison to an external disk galaxy. Where do we lie in our Galaxy?
Lecture 12: Galaxies View of the Galaxy from within The Milky Way galaxy Rotation curves and dark matter External galaxies and the Hubble classification scheme Plotting the sky brightness in galactic coordinates,
More informationarxiv: v1 [astro-ph.sr] 30 Dec 2017
Research in Astron. Astrophys. Vol.0 (200x) No.0, 000 000 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Key words: open clusters and associations: general
More information(a) B-V 6 V. (b) B-V
721 TOWARDS AN IMPROVED MODEL OF THE GALAXY Johan Holmberg 1, Chris Flynn 2, Lennart Lindegren 1 1 Lund Observatory, Box 43, SE-22100 Lund, Sweden 2 Tuorla Observatory, Vaisalantie 20, FI-21500 Piikkio,
More informationMulti-wavelength analysis of Hickson Compact Groups of Galaxies.
Multi-wavelength analysis of Hickson Compact Groups of Galaxies. Thodoris Bitsakis Department of Physics, University of Crete Paper: Bitsakis T., Charmandaris V., da Cunha E., Diaz-Santos T., Le Floc h
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 informationThom 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 informationDark Matter Dominated Objects. Louie Strigari Stanford
Dark Matter Dominated Objects Louie Strigari Stanford Milky Way Circa 2009 Satellite Year Discovered LMC 1519 SMC 1519 Sculptor 1937 Fornax 1938 Leo II 1950 Leo I 1950 Ursa Minor 1954 Draco 1954 Carina
More informationarxiv: v1 [astro-ph.ga] 11 Nov 2016
Mon. Not. R. Astron. Soc. 000, (06) Printed April 08 (MN LATEX style file v.) Properties of Star Clusters III: Analysis of 3 FSR Clusters using UKIDSS-GPS and VISTA-VVV arxiv:6.0373v [astro-ph.ga] Nov
More informationFirst results from the Stockholm VIMOS Supernova Survey
First results from the Stockholm VIMOS Supernova Survey - Detection efficiencies and photometric accuracy in supernova surveys Outline The Stockholm VIMOS Supernova Survey, SVISS. First results from the
More informationDwarf galaxies vs. globular clusters: An observer s perspective
Dwarf galaxies vs. globular clusters: An observer s perspective Jay Strader (Michigan St) with Beth Willman (Haverford) A globular cluster A galaxy Galaxy, Defined A galaxy is a gravitationally bound collection
More informationNear-infrared photometry and spectroscopy of the low Galactic latitude globular cluster 2MASS-GC 03
Advance Access publication 2016 July 13 doi:10.1093/mnras/stw1674 Near-infrared photometry and spectroscopy of the low Galactic latitude globular cluster 2MASS-GC 03 Julio A. Carballo-Bello, 1,2,3 S. Ramírez
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 informationBayesian Mass Estimates of the Milky Way: incorporating incomplete data
Bayesian Mass Estimates of the Milky Way: incorporating incomplete data Gwendolyn Eadie, PhD Candidate Dr. William Harris (McMaster), Dr. Lawrence Widrow (Queen's) AstroStat Seminar - March 23, 2015 Measuring
More informationLaboratory: Milky Way
Department of Physics and Geology Laboratory: Milky Way Astronomy 1402 Equipment Needed Quantity Equipment Needed Quantity Milky Way galaxy Model 1 Ruler 1 1.1 Our Milky Way Part 1: Background Milky Way
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 informationThe Mass of the Milky Way Using Globular Cluster Kinematics
The Mass of the Milky Way Using Globular Cluster Kinematics Gwendolyn Eadie, PhD Candidate PhD Supervisor: William Harris Collaborators: Aaron Springford (Stats, Queen s Univ.) Postgraduate Scholarships-Doctoral
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 informationChapter 25: Galaxy Clusters and the Structure of the Universe
Chapter 25: Galaxy Clusters and the Structure of the Universe Distribution of galaxies Evolution of galaxies Study of distant galaxies Distance derived from redshift Hubble s constant age of the Universe:
More informationStellar populations in the Milky Way halo
Stellar populations in the Milky Way halo Paula Jofre Pfeil Max Planck Institute for Astrophysics (Achim Weiss, Ben Panter, Camilla Hansen) Introduction Todayʼs Universe Scenario: Dark matter haloes connected
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 informationUsing ground based data as a precursor for Gaia-based proper motions of satellites
Using ground based data as a precursor for Gaia-based proper motions of satellites 102 Streams T. K. Fritz, N. Kallivayalil, J. Bovy, S.Linden, P. Zivick, R. Beaton, M. Lokken, T. Sohn, D. Angell, M. Boylan-Kolchin,
More informationGlobular Clusters in relation to the VPOS of the Milky Way
Globular Clusters in relation to the VPOS of the Milky Way Marcel S. Pawlowski marcel.pawlowski@case.edu Collaborators: Australia: Duncan Forbes, Helmut Jerjen Austria: Gerhard Hensler, Sylvia Plöckinger
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 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 informationTHE 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 informationTHE GALAXY. Spitzer Space Telescope Images & Spectra: 3µm - 170µm
THE GALAXY Composite infrared colour image of Galactic Centre region taken at 1.25, 2.2 and 3.5 microns with COBE/DIRBE instrument (NASA/GSFC). GALAXY: A conglomeration of stars, gas + dust Topics: Star
More informationA New Analysis in the Field of the Open Cluster Collinder 223
Chin. J. Astron. Astrophys. Vol. 4 (2004), No. 1, 67 74 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics A New Analysis in the Field of the Open Cluster
More informationLocal Group cosmology with ngcfht
Local Group cosmology with ngcfht Nicolas Martin (Strasbourg Observatory & MPIA, Heidelberg) Cosmology on galaxy scales the new frontier observed halo kpc Large scale cosmology is now largely understood
More informationThe Milky Way Galaxy
1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure
More informationJINA 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 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 informationarxiv: v1 [astro-ph.ga] 6 Feb 2018
MNRAS 000, 1 (0000) Preprint 7 February Compiled using MNRAS LATEX style file v3.0 Near-infrared study of new embedded clusters in the Carina complex R. A. P. Oliveira 1, E. Bica 1, and C. Bonatto 1 1
More informationTHE INVISIBLES: A DETECTION ALGORITHM TO TRACE THE FAINTEST MILKY WAY SATELLITES
Draft version July 22, 2008 Preprint typeset using L A TEX style emulateapj v. 08/13/06 THE INVISIBLES: A DETECTION ALGORITHM TO TRACE THE FAINTEST MILKY WAY SATELLITES S. M. Walsh 1, B. Willman 2, H.
More informationOptical and Near- Infrared Photometric Study of NGC 6724
Research in Astron. Astrophys. Vol.0 (201x) No.0, 000 000 http://www.raa-journal.org http://www.iop.org/journals/raa Research in Astronomy and Astrophysics Optical and Near- Infrared Photometric Study
More informationHigh quality seeing V, I and Gunn z imaging of Terzan 4: a blue horizontal branch bulge globular cluster
Astron. Astrophys. 319, 850 854 (1997) ASTRONOMY AND ASTROPHYSICS High quality seeing V, I and Gunn z imaging of Terzan 4: a blue horizontal branch bulge globular cluster S. Ortolani 1, B. Barbuy 2, and
More informationLecture 30. The Galactic Center
Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is
More informationThe Milky Way Galaxy. Sun you are here. This is what our Galaxy would look like if we were looking at it from another galaxy.
The Milky Way Galaxy Sun you are here. This is what our Galaxy would look like if we were looking at it from another galaxy. Examples of three Milky-Way like Galaxies 1. Roughly 100,000 light years across
More informationDark Matter: Observational Constraints
Dark Matter: Observational Constraints Properties of Dark Matter: What is it? And what isn t it? Leo Blitz UC Berkeley Stanford July 31, 2007 How much is there? WMAP results Rotation curves of Galaxies
More informationToday in Astronomy 142: the Milky Way
Today in Astronomy 142: the Milky Way The shape of the Galaxy Stellar populations and motions Stars as a gas: Scale height, velocities and the mass per area of the disk Missing mass in the Solar neighborhood
More informationThe Universe o. Galaxies. The Universe of. Galaxies. Ajit Kembhavi IUCAA
Hello! The Universe of Galaxies The Universe o Galaxies Ajit Kembhavi IUCAA Galaxies: Stars: ~10 11 Mass: ~10 11 M Sun Contain stars, gas and dust, possibly a supermassive black hole at the centre. Much
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 informationarxiv: v1 [astro-ph.ga] 24 Jan 2019
Mon. Not. R. Astron. Soc. 000, 1?? (0000) Printed 25 January 2019 (MN LATEX style file v2.2) Three candidate globular clusters discovered in the Galactic bulge arxiv:1901.08574v1 [astro-ph.ga] 24 Jan 2019
More informationAstronomy 422! Lecture 7: The Milky Way Galaxy III!
Astronomy 422 Lecture 7: The Milky Way Galaxy III Key concepts: The supermassive black hole at the center of the Milky Way Radio and X-ray sources Announcements: Test next Tuesday, February 16 Chapters
More informationThe Milky Way Galaxy. sun. Examples of three Milky-Way like Galaxies
The Milky Way Galaxy sun This is what our Galaxy would look like if we were looking at it from another galaxy. Examples of three Milky-Way like Galaxies 1. Roughly 100,000 light years across 2. Roughly
More informationThe Brown Dwarfs of our Milky Way
The Brown Dwarfs of our Milky Way Benne W. Holwerda (University of Louisville) Isabel van Vledder, Dieuwertje van der Vlucht, Rychard Bouwens, Matthew Kenworthy, Nor Pirzkal Russ Ryan benne.holwerda@gmail.com
More informationChapter 23 The Milky Way Galaxy Pearson Education, Inc.
Chapter 23 The Milky Way Galaxy The Milky Way is our own galaxy viewed from the inside. It is a vast collection of more than 200 billion stars, planets, nebulae, clusters, dust and gas. Our own sun and
More informationAnalyzing Spiral Galaxies Observed in Near-Infrared
Analyzing Spiral Galaxies Observed in Near-Infrared Preben Grosbøl European Southern Observatory Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany Abstract A sample of 54 spiral galaxies was observed
More informationThe 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 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 informationNEW STAR CLUSTERS DISCOVERED IN THE GLIMPSE SURVEY
The Astrophysical Journal, 635:560 569, 2005 December 10 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. NEW STAR CLUSTERS DISCOVERED IN THE GLIMPSE SURVEY E. P. Mercer,
More informationThe Milky Way. Finding the Center. Milky Way Composite Photo. Finding the Center. Milky Way : A band of and a. Milky Way
The Milky Way Milky Way : A band of and a The band of light we see is really 100 billion stars Milky Way probably looks like Andromeda. Milky Way Composite Photo Milky Way Before the 1920 s, astronomers
More informationGalactic Bulge Science
Galactic Bulge Science Ken Freeman Australian National University ngcfht meeting Hilo, Mar 27-29 2013 NGC 5746 1 The Galactic bulge was long thought to be a merger product. We now know that boxy bulges
More informationChapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
More informationHOPS + MALT90 + HiGAL
HOPS + MALT90 + HiGAL Probing star formation on a Galactic scale through mm molecular line and far-ir Galactic plane surveys Steve Longmore (ESO ALMA Fellow) John Bally, Leonardo Testi, Jill Rathborne,
More informationLuminosity Function of Faint Globular Clusters in M87
SLAC-PUB-11959 astro-ph/0607238 July 2006 Luminosity Function of Faint Globular Clusters in M87 Christopher Z. Waters and Stephen E. Zepf Department of Physics and Astronomy, Michigan State University,
More informationMulti-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida
Multi-wavelength Surveys for AGN & AGN Variability Vicki Sarajedini University of Florida What are Active Galactic Nuclei (AGN)? Galaxies with a source of non-stellar emission arising in the nucleus (excessive
More informationAddendum: GLIMPSE Validation Report
August 18, 2004 Addendum: GLIMPSE Validation Report The GLIMPSE Team 1. Motivation In our Validation Report of Jan. 30, 2004, we produced reliability calculations and discussed photometric accuracy estimates
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 informationThe Geometry of Sagittarius Stream from PS1 3π RR Lyrae
The Geometry of Sagittarius Stream from PS1 3π RR Lyrae Nina Hernitschek, Caltech collaborators: Hans-Walter Rix, Branimir Sesar, Judith Cohen Swinburne-Caltech Workshop: Galaxies and their Halos, Sept.
More informationASTR 1120 General Astronomy: Stars & Galaxies
ASTR 1120 General Astronomy: Stars & Galaxies!NNOUNCEMENTS HOMEWORK #6 DUE TODAY, by 5pm HOMEWORK #7 DUE Nov. 10, by 5pm Dark matter halo for galaxies Dark matter extends beyond visible part of the galaxy
More informationThe Milky Way. Mass of the Galaxy, Part 2. Mass of the Galaxy, Part 1. Phys1403 Stars and Galaxies Instructor: Dr. Goderya
Foundations Chapter of Astronomy 15 13e Our Milky Way Seeds Phys1403 Stars and Galaxies Instructor: Dr. Goderya Selected Topics in Chapter 15 A view our Milky Way? The Size of our Milky Way The Mass of
More informationQuantifying Secular Evolution Through Structural Decomposition
Quantifying Secular Evolution Through Structural Decomposition University of St Andrews / ICRAR (UWA) o How do structures form? bulge disk bar pseudo-bulge disk bulge??? o Are ellipticals and bulges essentially
More informationThe nature of the star clusters ESO 93 SC08 and ESO 452 SC11
ASTRONOMY & ASTROPHYSICS APRIL II 1999, PAGE 363 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 136, 363 372 (1999) The nature of the star clusters ESO 93 SC08 and ESO 452 SC11 E. Bica 1, S. Ortolani
More informationASTR 1120 General Astronomy: Stars & Galaxies
ASTR 1120 General Astronomy: Stars & Galaxies!NNOUNCEMENTS HOMEWORK #6 DUE TODAY, by 5pm HOMEWORK #7 DUE Nov. 10, by 5pm Dark matter halo for galaxies REVIEW Dark matter extends beyond visible part of
More informationarxiv: v1 [astro-ph.co] 28 Oct 2009
Mon. Not. R. Astron. Soc., 1 17 (29) Printed 28 October 29 (MN LATEX style file v2.2) The M31 globular cluster system: ugriz and K-band photometry and structural parameters arxiv:91.5475v1 [astro-ph.co]
More informationA CCD BV I color-magnitude study of the metal-rich globular cluster NGC 5927,
ASTRONOMY & ASTROPHYSICS OCTOBER II 1996, PAGE 191 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 119, 191-197 (1996) A CCD BV I color-magnitude study of the metal-rich globular cluster NGC 5927, N.
More informationHalo 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 informationStellar Dynamics and Structure of Galaxies
Stellar Dynamics and Structure of Galaxies. Spherically symmetric objects Vasily Belokurov vasily@ast.cam.ac.uk Institute of Astronomy Lent Term 2016 1 / 21 Outline I 1 2 Globular of galaxies 2 / 21 Why
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 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 informationNew 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 informationResolved Starburst Clusters Near & Far
Resolved Starburst Clusters Near & Far Andrea Stolte I. Physikalisches Institut Universität zu Köln E-ELT Science May 2009 ESO Garching 1 Resolved Starburst Clusters Near & Far 1. Outstanding questions
More informationarxiv: v1 [astro-ph.ga] 9 Sep 2017
MNRAS, 8 () Preprint September 7 Compiled using MNRAS LATEX style file v. The Outer Envelopes of Globular Clusters. II. NGC 8, NGC 8 and NGC 6 P. B. Kuzma, G. S. Da Costa, A. D. Mackey Research School
More informationAS1001:Extra-Galactic Astronomy. Lecture 3: Galaxy Fundamentals
AS1001:Extra-Galactic Astronomy Lecture 3: Galaxy Fundamentals Galaxy Fundamentals How many stars are in a galaxy? How did galaxies form? How many galaxies are there? How far apart are they? How are they
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 information