Studying the Milky Way with pulsating stars
|
|
- Richard Lawrence
- 5 years ago
- Views:
Transcription
1 Studying the Milky Way with pulsating stars ( 東京大学 ) Noriyuki Matsunaga (The University of Tokyo)
2 The first C-rich Miras found in the bulge All the AGB stars confirmed in the bulge were O-rich. C-rich Miras among OGLE-III Miras and those in Catchpole+16 Target selection based on (J-Ks) and (9-18) colors Low-resolution spectra from SAAO 74inch/SpUpNIC Boundaries for classification from Ishihara et al. (2011)
3 Distances to the C-rich Miras Relatively large errors remain due to the mix of interstellar and circumstellar extinction. P-W relation with J/Ks is useful to check the approximate positions. 4 Miras (and maybe another) are within the bulge. 3 foreground (including a symbiotic C-rich Mira in Miszalski+13) 4 members 1 background?
4 The origin of C-rich Miras It is unclear how these C-rich Miras were formed. Intermediate-age stars (around Gyr)?? Old objects evolved from stellar mergers?? Accretion from a (merged) dwarf galaxy?? They are tracing a rare stellar population in the bulge. Kinematics and chemical information may help uncover their origin(s). Matsunaga et al. (2017, MNRAS, 469, 4949)
5 Main topics Introduction Pulsating stars as tracers of the Galactic disk New Cepheids revealing the structure of the inner Galaxy and beyond Review of new Cepheids discovered since 2011 Concluding remarks
6 Introduction Pulsating stars as tracers of the Galactic disk
7 Pulsating stars as tracers Type II Cepheid RR Lyr Classical Cepheid Mira Period-luminosity relation Distance Unique evolutionary stage Age Kinematic and Chemical information can be added with follow-up studies. Gautchy & Saio (1995)
8 Ks [mag] As distance indicators Period-Luminosity relations of Cepheids and Miras in the LMC (from Matsunaga et al. 2009, 2011) Classical Cepheid Mira Longer-P Miras Type II Cepheid For Miras, P-L relations are narrow only in the IR (not in the optical) log(period/day)
9 As age indicators Type Initial Mass Age Classical Cepheids 4 10 M Myr Miras 1 6 M 100 Myr 10 Gyr Type II Cepheids ~1 M ~10 Gyr RR Lyrs ~1 M ~10 Gyr log (Age/yr) Myr Myr Period-Age relation of classical Cepheids (Bono et al. 2005) Myr 10Myr log (Period/day) Miras show a loose anticorrelation between age and period (see eg. Feast et al. 2006).
10 Metallicity gradient of Cepheids Higher metallicity towards the inner Galaxy. Cepheids ( Myr) show the most clear and tight metallicity gradient. Genovali et al. (2014, A&A, 566, 37) Genovali et al. (2015, A&A, 580, 17) [Na/Fe] [Fe/H] [Al/Fe] R GC [kpc] [Si/Fe] R GC [kpc]
11 MW Cepheids from classical surveys Distant Cepheids in the Galactic disk are obscured. Very important to extend the sample to a large space. Different locations along each spiral arm, a wider azimuth range, a wider range of Gactrocentric distance GC Sun The distribution of ~500 Cepheids from DDO database: overlaid on the illustration by GLIMPSE project (2008)
12 Cepheids waiting to be found Windmark et al. 2011, A&A, 530, A76 A simple exponential-disc model: f R, z = exp R 3.5kpc sech z z 0 20,000 Cepheids predicted (see ~2,000 new members from OGLE-IV in Udalski 2017, arxiv: ) 9,000 Cepheids may be detected by Gaia. to be detected by Gaia not to be detected by Gaia Sun GC Simulation of Cepheids to be detected by Gaia (Windmark et al. 2011)
13 Cepheids/Miras remain important. Many new to be found by OGLE, VVV, Gaia, LSST... No Gaia parallaxes for a large part of the disk. Cepheids and Miras are bright (especially in the IR) and can be detected across the disk. Gaia s first sky map (2016 Sep)
14 New Cepheids revealing the structure of the inner Galaxy and beyond Review of new Cepheids discovered since 2011
15 IRSF + SIRIUS 1.4-m telescope in Sutherland (SAAO) SIRIUS: FOV: about 7.7 x 7.7 Pixel Scale: /pix, Simultaneous JHK s images. It has been steadily working for over 17 years since 2000, during which 170+ papers were published. 24+ PhD theses (20 in JP, 3 in SA) Manchester, 25 June 2004
16
17 Matsunaga et al. (2011, Nature, 477, 188) 3 Cepheids from IRSF All 3 have P~20 days, aged ~25 Myr. ~0.1 M/yr at ~25 Myr ago
18 Soszynski et al. (2011, AcA, 61, 275) OGLE-III survey 32 classical Cepheids (based on P-W relation, all of them seem located beyond the bulge)
19 5 Cepheids in the disc flare Feast et al. 2014, Nature 509, 342 Based on IRSF photometric data, Estimated distances to 5 OGLE-III Cepheids toward the bulge (Soszynski et al. 2011). The kinematics from SALT spectroscopic data are consistent with the disc rotation. The first stars ever confirmed to be in the disc flare. Other OGLE Cepheids remain to be characterized better. Cepheids identified far from the plane
20 Dekany et al. (2015, ApJL, 799, L12; 2015, ApJL, 812, L29) Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) 37 classical Cepheids from VVV survey
21 Dekany et al. (2015, ApJL, 799, L12; 2015, ApJL, 812, L29) Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) 37 classical Cepheids from VVV survey Matsunaga et al. (2016, MNRAS, 462, 414) 26 Cepheids, from IRSF, in addition to the three in the Nuclear Stellar Disk
22 Conflicting results in 2015/2016 Dekany et al. (2015) and Matsunaga et al. (2016) reported significantly different distributions of Cepheids in the inner part of the Galactic disk. Our work (shallower) Dekany et al. (2015) 29 classical Ceps from IRSF/SIRIUS 37 classical Ceps from VVV 11 Cepheids are common, and μ 0 (ours) are systematically larger than μ 0 (Dekany et al.). Δμ 0 ~0.5 mag
23 Impact of the extinction law Conversion from a color excess to an extinction depends on the extinction law, A Ks /E(H K s ). These works consider the direction of the bulge. A classical value in Cardelli et al. (1989) Label Reference Data A Ks E H K s C89 Cardelli+1989 Mixed 1.82 N06 Nishiyama+2006 IRSF 1.44 N09 Nishiyama MASS 1.61 AG15 Alonso-Garcia+2015 VVV 1.28 M16 Majaess+2016 VVV 1.49
24 A(K s )/E(H-K s ) (and P-W relation) (μ 0, A Ks ) are derived with two-band magnitudes and PLRs. From the extinction law A Ks = A Ks E(H K s ) μ 0 = K s M Ks A Ks H K s (M H M Ks ) observed from PLR unknown Period-Wesenheit relations are also affected by the error in the extinction law. W HKs = K s γ (H K s ) This term doesn t work as a correction of the interstellar extinction unless γ is correct.
25 E H K s = 1. 5~2. 5 for our targets (the color excess can be determined regardless of the extinction law.) A K s E H K s Matsunaga et al. (2016) used the N06 coefficient. = A Ks = 2. 2~3. 6 A K s E H K s Dekany et al. (2015) used the N09 coefficient. = A Ks = 2. 4~4. 0 ~0.3 mag difference
26 4 Cepheids in the NSD One of the young stellar populations found in the NSD. Radial velocities also support the membership. These Cepheids are located at the distance of GC (8.0±0.5 kpc) and give a constraint on A Ks /E H-Ks. l-v diagram for Cepheids compared with CO gas and orbits around the GC 3 Cepheids within 35 pc (projected) of the GC +1 at ~50 pc Matsunaga et al. (2011) Matsunaga et al. (2015)
27 The λ 2 law towards Bulge The distance modulus to the GC (μ 0 =14.5±0.15 mag; Nishiyama+06b) y-axis: Apparent modulus =True modulus + Extinction Bulge red clumps split into many sub-regions give A Ks /E H-Ks =1.44 (Nishiyama+06a) x-axis: Color excess
28 The λ 2 law towards Bulge PLRs in H and Ks can put individual Cepheids on this diagram (without assuming the extinction law or the distance). y-axis: Apparent modulus =True modulus + Extinction 4 NSD Cepheids x-axis: Color excess
29 The λ 2 law towards Bulge The Nishiyama+06 law is consistent with that the 4 Cepheids are at the GC distance. y-axis: Apparent modulus =True modulus + Extinction A Ks /E H-Ks x-axis: Color excess
30 The λ 2 law towards Bulge A Ks /E H-Ks y-axis: Apparent modulus =True modulus + Extinction 25 other Cepheids in our survey x-axis: Color excess
31 The λ 2 law towards Bulge Also, we found no Cepheids on the nearer side. y-axis: Apparent modulus =True modulus + Extinction A Ks /E H-Ks x-axis: Color excess
32 The λ 2 law towards Bulge The extinction law of A(Ks)/E(H Ks)=1.44 is supported for the direction of the bulge. Very few Cepheids are present within ~2.5 kpc of the Galactic Centre except the NSD. Also see the discussion in the proceedings book for 22 nd Pulsation Conference at San Pedro (eds. M. Catelan & W. Gieren) y-axis: Apparent modulus =True modulus + Extinction A Ks /E H-Ks x-axis: Color excess
33 Classical Cepheids in the far side of the disk Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) 4 classical Cepheids in the Nuclear Stellar Disc Lack of classical Cepheids within 2.5 kpc of the GC except 4 in the Nuclear Stellar Disc ( l <2 deg) no simple exp. disc
34 Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) Tanioka et al. (2017, ApJ, 842, 104) 3 Cepheids from IRSF
35 Tanioka et al. (2017, ApJ, 842, 104) Monte-Carlo simulations allows us that two Cepheids rotate slower than the Galactic rotation (V LSR of Cepheids from Subaru/IRCS). Slow (3.1 σ) Large errors in (μ 0, A Ks ) remain by Cepheids considering far behind the the extinction bulge laws in (Soszynski Nishiyama+06 et al. 2012; and Feast Cardelli+89. et al. 2014) μ 0 = Consistent with MW rotation D (T2C) 3D extinction map (Schultheis+14) D (CC) μ 0 = Slow (1.6 σ) μ 0 =
36 Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) New near-ir survey for the northern disk (Yanagisawa-san s talk) OGLE Cepheids (Udalski, 2017, arxiv: )
37 Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) KISOGP survey l= deg ~100 Cepheids OGLE VVV Gaia for the entire range (except obscured region)
38 KISOGP survey l= deg ~100 Cepheids Cepheids far behind the bulge (Soszynski et al. 2012; Feast et al. 2014) New surveys are discovering Cepheids (and other variable stars) spread across the Galactic disk. Spectroscopy will be important to study the disk evolution, and must be efficient for >1000 objects. OGLE VVV Gaia for the entire range (except obscured region)
39 Concluding remarks
40 Concluding remarks A large number of new pulsating stars are expected from large surveys: OGLE, VVV, Gaia, LSST Characterizing the interstellar extinction is an urgent task for mapping the wide area of disk. Gaia s proper motions will be crucial. Talk by Kawata-san and more Spectroscopic follow-up will be crucial. Kinematics and chemical abundances demanded. Near-IR spectroscopic observations are required to observe new ones in the obscured regions. Talks by Ikeda-san and Fukue-san
Observing 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 informationarxiv: v1 [astro-ph.sr] 13 Apr 2018
AKARI color useful for classifying chemical types of Miras Noriyuki Matsunaga 1 1 Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan arxiv:1804.04940v1 [astro-ph.sr]
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 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 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 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 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 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 informationThe 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 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 informationGaia 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 informationTime-series surveys and pulsating stars: The near-infrared perspective
Time-series surveys and pulsating stars: The near-infrared perspective Noriyuki Matsunaga 1, 1 Department of Astronomy, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan Abstract.
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 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 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 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 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 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 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 informationdsph in Local Group July 2014 Vienna
John Menzies SAAO dsph in Local Group Local Group associated with Galaxy, M31, within ~1 Mpc of centre of mass Galaxy has 25 companion dsph M31 has ~ 26 ~ 3 dsph not associated with either, near boundary
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 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 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 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 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 informationThe Inner Milky Way Structure with VVV. Marina Rejkuba ESO, Germany
The Inner Milky Way Structure with VVV Marina Rejkuba ESO, Germany Overview Red Clump stars as distance indicators Dependence on age and metallicity Tracing the bar with RC stars in VVV Inner bar flafening
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 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 informationStellar Populations in the Galaxy
Stellar Populations in the Galaxy Stars are fish in the sea of the galaxy, and like fish they often travel in schools. Star clusters are relatively small groupings, the true schools are stellar populations.
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 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 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 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 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 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 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 informationSummary: Nuclear burning in stars
Summary: Nuclear burning in stars Reaction 4 1 H 4 He 3 4 He 12 C 12 C + 4 He 16 O, Ne, Na, Mg Ne O, Mg O Mg, S Si Fe peak Min. Temp. 10 7 o K 2x10 8 8x10 8 1.5x10 9 2x10 9 3x10 9 Evolution through nuclear
More informationDemographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?
Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen
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 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 informationOutline. 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(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 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 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 informationGalaxies. With a touch of cosmology
Galaxies With a touch of cosmology Types of Galaxies Spiral Elliptical Irregular Spiral Galaxies Spiral Galaxies Disk component where the spiral arms are Interstellar medium Star formation Spheroidal
More informationOur View of the Milky Way. 23. The Milky Way Galaxy
23. The Milky Way Galaxy The Sun s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral
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 informationCharacterization of the exoplanet host stars. Exoplanets Properties of the host stars. Characterization of the exoplanet host stars
Characterization of the exoplanet host stars Exoplanets Properties of the host stars Properties of the host stars of exoplanets are derived from a combination of astrometric, photometric, and spectroscopic
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 informationRelativity and Astrophysics Lecture 15 Terry Herter. RR Lyrae Variables Cepheids Variables Period-Luminosity Relation. A Stellar Properties 2
Stellar Properties Relativity and Astrophysics Lecture 15 Terry Herter Outline Spectroscopic Parallax Masses of Stars Periodic Variable Stars RR Lyrae Variables Cepheids Variables Period-Luminosity Relation
More informationNear infrared high resolution spectroscopy of variable stars G. Bono, Univ. Of Rome ToV + D. Magurno, M. Urbaneja + many others
Near infrared high resolution spectroscopy of variable stars G. Bono, Univ. Of Rome ToV + D. Magurno, M. Urbaneja + many others Near infrared high resolution spectroscopy of variable stars G. Bono, Univ.
More informationChemical evolution of the Galactic disk using Open Clusters
Chemical evolution of the Galactic disk using Open Clusters ICC Winter Meeting Feb 2017 1. Galactic Archaeology Unravel the formation and evolution of the Milky Way (MW) Resolved stars provide a fossil
More informationProbing 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 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 information1.4 Galaxy Light Distributions
26 1.4 Galaxy Light Distributions List of topics Hubble classification scheme see Binney & Merrifield text Galaxy surface brightness profiles (JL 2.3.1, plus additional material) Galaxy luminosity function
More informationLecture 25: The Cosmic Distance Scale Sections 25-1, 26-4 and Box 26-1
Lecture 25: The Cosmic Distance Scale Sections 25-1, 26-4 and Box 26-1 Key Ideas The Distance Problem Geometric Distances Trigonometric Parallaxes Luminosity Distances Standard Candles Spectroscopic Parallaxes
More informationLecture 28: Spiral Galaxies Readings: Section 25-4, 25-5, and 26-3
Lecture 28: Spiral Galaxies Readings: Section 25-4, 25-5, and 26-3 Key Ideas: Disk & Spheroid Components Old Stars in Spheroid Old & Young Stars in Disk Rotation of the Disk: Differential Rotation Pattern
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 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 informationRed giant variables: OGLE II and MACHO
Mem. S.A.It. Vol. 77, 303 c SAIt 2006 Memorie della Red giant variables: OGLE II and MACHO L.L. Kiss 1 and P. Lah 2 1 School of Physics A28, University of Sydney, NSW 2006, Australia, e-mail: laszlo@physics.usyd.edu.au
More informationThe 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 informationThe Milky Way - Chapter 23
The Milky Way - Chapter 23 The Milky Way Galaxy A galaxy: huge collection of stars (10 7-10 13 ) and interstellar matter (gas & dust). Held together by gravity. Much bigger than any star cluster we have
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 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 informationMyung Gyoon Lee. With Ho Seong Hwang (CfA) and Hong Soo Park (NAOJ) (Dept of Physics and Astronomy, Seoul National University)
Myung Gyoon Lee (Dept of Physics and Astronomy, Seoul National University) With Ho Seong Hwang (CfA) and Hong Soo Park (NAOJ) 2013. 10. 22 Dynamics of Disk Galaxies, The 7 th Korean Astrophysics Workshop,
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 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 informationFollowing 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 informationGaia-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 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 informationLecture #21: Plan. Normal Galaxies. Classification Properties Distances
Lecture #21: Plan Normal Galaxies Classification Properties Distances Messier 31 = M31 Early 20 th Century The Great Debate (4/26/1920): Harlow Shapley (Mt Wilson) vs Heber Curtis (Lick Observatory) Smithsonian
More informationA100H Exploring the Universe: Discovering Galaxies. Martin D. Weinberg UMass Astronomy
A100H Exploring the Universe: Discovering Galaxies Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 05, 2016 Read: Chap 19 04/05/16 slide 1 Exam #2 Returned by next class meeting
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 informationPulsating Variable Stars in the MACHO Bulge database: The Semiregular Variables
Pulsating Variable Stars in the MACHO Bulge database: The Semiregular Variables D. Minniti 1, C. Alcock, D. Alves, K. Cook, S. Marshall Lawrence Livermore National Laboratory R. Allsman, T. Axelrod, K.
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 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 informationAST 6336, Interstellar Medium, Spring 2015
AST 6336, Interstellar Medium, Spring 2015 Young stellar clusters (lectures by Nicola Da Rio ndario@ufl.edu) January 2, 4, 2015 Star formation A molecular cloud may become unsupported gas pressure + magnetic
More informationGalaxy evolution through resolved stellar populations: from the Local Group to Coma
Galaxy evolution through resolved stellar populations: from the Local Group to Coma Isabel Pérez Kapteyn Institute & Universidad de Granada Brief summary of the science cases presented at the Local Universe
More informationGALAXIES 626. The Milky Way II. Chemical evolution:
GALAXIES 626 The Milky Way II. Chemical evolution: Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which
More informationThe Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds.
The Milky Way, Hubble Law, the expansion of the Universe and Dark Matter Chapter 14 and 15 The Milky Way Galaxy and the two Magellanic Clouds. Image taken from the European Southern Observatory in Chile
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 informationThe Local Spiral Arm of the Galaxy explained by trapping of stars in the corotation resonance
The Local Spiral Arm of the Galaxy explained by trapping of stars in the corotation resonance Jacques R.D. Lépine,Tatiana A. Michtchenko,Douglas A. Barros, Ronaldo S.S. Vieira University of São Paulo Lund
More informationExam 4 Review EXAM COVERS LECTURES 22-29
Exam 4 Review EXAM COVERS LECTURES 22-29 Theoretically is there a center of the universe? Is there an edge? Do we know where Earth is on this? There is no center to the Universe, What kind of light we
More informationDetermination 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 informationThe 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 informationarxiv: v1 [astro-ph.sr] 12 Jul 2017
Astronomy& Astrophysics manuscript no. popii_cep c ESO 7 July 3, 7 Galactic Bulge Population II Cepheids in the VVV Survey: Period-Luminosity Relations and a Distance to the Galactic Center A. Bhardwaj,,
More informationThe physical properties of galaxies in Universe
The physical properties of galaxies in Universe Iurii Babyk, Dublin Institute for Advanced Studies, Dublin City University, Main Astronomical Observatory of the NAS of Ukraine. Introduction Large-Scale
More information24.1 Hubble s Galaxy Classification
Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble s Law 24.4 XXActive Galactic Nuclei XXRelativistic Redshifts and Look-Back
More informationDistances based on Mira variables. Leonid Georgiv IA UNAM
Distances based on Mira variables. Leonid Georgiv IA UNAM A short story 1999 King et al reported a nova in the galaxy IC 1613. (King et al. 1999, IAUC, 7287) A short story The star were detected on our
More informationAction-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE
IAU Symposium 330 Nice, 27. April 2017 Action-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE Wilma Trick (MPIA, Heidelberg) Hans-Walter Rix (MPIA) Jo Bovy (Uni Toronto) Open Questions
More informationThree classical Cepheid variable stars in the nuclear bulge of the Milky Way
Three classical Cepheid variable stars in the nuclear bulge of the Milky Way Noriyuki Matsunaga 1*, Takahiro Kawadu 2, Shogo Nishiyama 3, Takahiro Nagayama 4, Naoto Kobayashi 1,5, Motohide Tamura 3, Giuseppe
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 informationNormal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Symbolically: E0.E7.. S0..Sa..Sb..Sc..Sd..Irr
Normal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Here we will cover topics in Ch. 24 up to 24.4, but then skip 24.4, 24.5 and proceed to 25.1, 25.2, 25.3. Then, if there is time remaining,
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 informationSTRUCTURE AND DYNAMICS OF GALAXIES
STRUCTURE AND DYNAMICS OF GALAXIES 23. Piet van der Kruit Kapteyn Astronomical Institute University of Groningen, the Netherlands www.astro.rug.nl/ vdkruit Beijing, September 2011 Outline The local Mass
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 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 informationGalaxies. Need a (physically) meaningful way of describing the relevant properties of a galaxy.
Galaxies Aim to understand the characteristics of galaxies, how they have evolved in time, and how they depend on environment (location in space), size, mass, etc. Need a (physically) meaningful way of
More informationGalaxies Guiding Questions
Galaxies Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to galaxies? Do all galaxies have spiral arms, like the Milky Way? How do
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 information