Chemical tagging with. Ricardo Schiavon
|
|
- Wilfred Pierce
- 7 years ago
- Views:
Transcription
1 Chemical tagging with Ricardo Schiavon Stellar Populations Newton Meeting São Paulo, November 30, 2015
2 Chemical tagging with Discovery of a new stellar population in the Galactic bulge
3 Astrophysics Research Institute Liverpool John Moores University (LJMU) 23 staff! 8 postdocs! Cosmology! Galaxy formation/evolution! Star formation! Stellar astrophysics! Time domain 29 grad students Theory! Observations! Instrumentation! Public Outreach
4 Outline 1. Multiple populations in globular clusters! 2. APOGEE! 3. Discovery of nitrogen rich stars in the bulge field! 4. Possible scenarios
5 Piotto et al GCs as single stellar populations
6 GCs as multiple stellar populations Multiple populations identified in the color magnitude diagrams of MW globular clusters High precision photometry and combination of UV and optical filters required Piotto et al. 2015
7 GCs as multiple stellar populations Abundances of C and N in GC stars vary and are anti-correlated Known for 30+ years Other anti-correlations also present, including Na-O, Mg-Al Carretta et al. 2005
8 GCs as multiple stellar populations Secondary populations dominate the mass in GCs today SP/PP ~ 2 Secondary! pop Primary! pop Carretta et al. 2005
9 Features of GC multiple pops Renzini et al GC specificity Ubiquity Variety SP Predominance Discreteness Chemical diversity in light elements No SNe enrichment (in most GCs) Mass budget problem Carretta et al. 2005
10 Features of GC multiple pops Renzini et al GC specificity! Ubiquity Variety SP Predominance Discreteness Chemical diversity in light elements No SNe enrichment (in most GCs) Mass budget problem Carretta et al. 2005
11 Scenarios 1. A history of SF and chemical evolution. Possible nucleosynthetic sources: Supermassive stars (10 4 MSun) Fast rotating massive stars Massive interacting binaries AGB stars 2. Early disk accretion None of the models accounts for the data!
12 The mass budget problem Today: SP/PP ~ 2 For any reasonable IMF, there weren t enough PP stars to generate the observed mass in enriched elements All models invoke a much larger mass in PP stars in the past Past: SP/PP ~ Secondary! pop Primary! pop Carretta et al. 2005
13 Weak chemical tagging Martell & Grebel (2010), Carretta et al. (2010): CN-strong stars in the halo field (see also Lind et al. 2015)! Up to 17% of halo mass originated in GCs! Gratton et al. (2012): Essentially all the halo made from GC dissolution! Key difference is assumption of SP/PP Carollo et al. (2013)
14 Apache Point Observatory Galactic Evolution Experiment
15 APOGEE: an infrared, high resolution spectroscopic survey of the stellar populations of the Galaxy! BOSS: will measure the cosmic distance scale via clustering in the large-scale galaxy distribution and the Lyman-α forest! SEGUE-2: will map the structure, kinematics, and chemical evolution of the outer Milky Way disk and halo! MARVELS: will probe the population of giant planets via radial velocity monitoring of 11,000 stars
16 APOGEE at a Glance Bright time SDSS-III survey, 2011.Q2 to 2014.Q2 300 fiber, R 22,500, cryogenic spectrograph, 7 deg 2 FOV H-band: nm (A H /A V ~ 1/6) Typical S/N = H=12.2 for 3-hr integration RV uncertainty spec < 500 m/s in 3 hr Actual < 100 m/s in 1hr 0.1 dex precision abundances for 15 chemical elements (including C, N, O, Fe, other α, odd-z, possibly neutron-capture) MASS-selected [(J-K) > 0.5] predominantly giant stars, probing all Galactic populations
17 Why APOGEE makes a difference High resolution * Near Infrared * 10 5 giant stars
18 Why APOGEE makes a difference High (enough) resolution * Near Infrared * 10 5 giant stars
19 APOGEE Field Plan
20 Target Selection Main sample is selected from 2MASS (J-K)0 0.5, 7 < H < 13.8 => giants (RGB, AGB, RC) are 80% of the sample Open and globular clusters targeted for science and calibration purposes Ancillary science programs cover a variety of science targets (young Galactic clusters, M dwarfs, M31 GCs in integrated light) For details, see Zasowski et al. (2013)
21 Spatial Coverage - DR12 Bulge Disk
22 APOGEE Spectral Analysis Example: spectral fits around CO lines For details, see Holtzman et al. (2015), García Pérez et al. (2015), Majewski et al. (2015)
23 Performance Survey quality spectra for ~ 150,000 stars (50% over initial goal) RV precision of 100 m/s, exceeding original requirement. Accuracy 1 km/s Abundances pipeline (ASPCAP) delivers precision of 100 K in Teff, 0.15 dex in log g, dex in [Fe/H], and 0.03 dex in [α/fe] Pipeline delivers abundances of 15 elements with 0.1 dex precision, 0.2 dex accuracy (in most cases). Issues with a few elements. Work in progress. Look out for DR13!! Data available publicly as part of Data Release 12 (DR12) since January 2015.
24 Slide from Gail Zasowski Science Working Group Chair: Jo Bovy (IAS) Text
25 C and N abundances in the bulge A population of stars with high N and an N-C anticorrelation was identified in the bulge
26 C and N abundances in the bulge They occupy the same locus as GC stars in this diagnostic plot
27 Al vs N correlation These N-rich stars also occupy the same locus as GC stars in [Al/Fe] vs [N/Fe] space!!!!
28 Al vs N correlation A correlation between the abundances of N and Al is also found, both in the bulge and in the GC sample!!!!
29 Hypothesis These stars are secondary populations from globular clusters, which got somehow lost to the field 1. What fraction of the bulge/inner halo is contributed by dissolved GCs? 2. How much mass is there in dissolved vs existing GCs? In order to answer those questions, we need to know what the ratio SP/PP was in the dissolved GCs
30 SP/PP Ratio To answer these questions, we need to know the value of the SP/PP ratio in dissolved GCs. 1. Today: SP/PP ~ 2 2. Models require: SP/PP ~ in the past
31 However, our observations only identify the analogs of so called secondary populations SP/PP ratio
32 SP/PP ratio S However, our observations only identify the analogs of so called secondary populations S
33 SP/PP ratio The primary populations are indistinguishable from field stars of same [Fe/H]! We have to assume a SP/PP ratio P S S P
34 Minimum mass in dissolved GCs Assuming SP/PP has always been as observed in GCs today: ~ 2/1 Assuming same ratio for bulge field, one gets: M ~ 1.5% of M Bulge ~ M Sun M ~ 17% of M Inner Halo (within 2 kpc) M ~ 5-10 x M GC system
35 Metallicity distributions Bulge Field N-rich stars Galactic GCs
36 Metallicity Distributions 1. Bulge field and N-rich MDF are DIFFERENT: hard to build the bulge from GCs (not surprising)
37 Metallicity distributions Bulge Field N-rich stars Galactic GCs
38 Metallicity Distributions 1. Bulge field and N-rich MDF are DIFFERENT: hard to build the bulge from GCs (not surprising) 2. Bulge field vs N-rich MDF at [Fe/H] < -1: primary population in GCs was at most ~90% of total stellar mass in the past
39 Metallicity distributions Bulge Field N-rich stars Galactic GCs
40 Metallicity Distributions 1. Bulge field and N-rich MDF are DIFFERENT: hard to build the bulge from GCs (not surprising) 2. Bulge field vs N-rich MDF at [Fe/H] < -1: primary population in GCs was at most ~90% of total stellar mass in the past 3. GCs and N-rich MDFs are DIFFERENT: contribution from tidal evaporation of existing GCs to N-rich population is negligible. If these stars ever lived in GCs, they were completely destroyed
41 Summary Assuming GC origin Newly discovered population, with GC chemistry, homogeneously distributed across the bulge At least 5-10 times more mass in destroyed than existing globular clusters Mass in primary populations cannot have been larger than ~90% of the total GC mass. It was probably less than that Cannot build bulge (or halo?) from GCs New population results from destruction of a large population of early GCs
42 But what if these stars were never associated with GCs to begin with?
43 Features of GC multiple pops Renzini et al GC specificity Ubiquity Variety SP Predominance Discreteness Chemical diversity in light elements No SNe enrichment (in most GCs) Mass budget problem Carretta et al. 2005
44 Features of GC multiple pops Renzini et al GC specificity! Ubiquity Variety SP Predominance Discreteness Chemical diversity in light elements No SNe enrichment (in most GCs) Mass budget problem Carretta et al. 2005
45 But what if these stars were never associated with GCs to begin with? N-rich stars were first found in GCs. Doesn t mean they necessarily can only form there GCs and N-rich MDFs don t match, suggesting different origin If N-rich stars can be generated outside GCs, no need to devise complicated destruction mechanisms But mass budget problem persists
46 Summary We have discovered a population of stars in the bulge that look chemically like those found in GCs Spatial distribution indistinguishable from the rest of the bulge If they come from GCs, then a very large population of early GCs were completely destroyed In that scenario, a very small fraction of the bulge mass was contributed by GC dissolution (few %). If in halo, about 20% of stellar mass in inner halo comes from GC dissolution. Our results point to a worsening of the mass budget problem. There may not be a genetic link between PP and SP.
Class #14/15 14/16 October 2008
Class #14/15 14/16 October 2008 Thursday, Oct 23 in class You ll be given equations and constants Bring a calculator, paper Closed book/notes Topics Stellar evolution/hr-diagram/manipulate the IMF ISM
More informationFaber-Jackson relation: Fundamental Plane: Faber-Jackson Relation
Faber-Jackson relation: Faber-Jackson Relation In 1976, Faber & Jackson found that: Roughly, L! " 4 More luminous galaxies have deeper potentials Can show that this follows from the Virial Theorem Why
More information165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
More informationIndiana University Science with the WIYN One Degree Imager
Indiana University Science with the WIYN One Degree Imager Katherine Rhode (Indiana University, WIYN SAC member) Indiana University Department of Astronomy Nine faculty members, plus active emeritus faculty
More informationTop 10 Discoveries by ESO Telescopes
Top 10 Discoveries by ESO Telescopes European Southern Observatory reaching new heights in astronomy Exploring the Universe from the Atacama Desert, in Chile since 1964 ESO is the most productive astronomical
More informationThe Gaia Archive. Center Forum, Heidelberg, June 10-11, 2013. Stefan Jordan. The Gaia Archive, COSADIE Astronomical Data
The Gaia Archive Astronomisches Rechen-Institut am Zentrum für Astronomie der Universität Heidelberg http://www.stefan-jordan.de 1 2 Gaia 2013-2018 and beyond Progress with Gaia 3 HIPPARCOS Gaia accuracy
More informationThe Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy
Carnegie Observatories Astrophysics Series, Vol. 4: Origin and Evolution of the Elements, 2003 ed. A. McWilliam and M. Rauch (Pasadena: Carnegie Observatories, http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html)
More informationPopulations and Components of the Milky Way
Chapter 2 Populations and Components of the Milky Way Our perspective from within the Milky Way gives us an opportunity to study a disk galaxy in detail. At the same time, it s not always easy to relate
More informationEllipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0
Elliptical galaxies: Ellipticals Old view (ellipticals are boring, simple systems)! Ellipticals contain no gas & dust! Ellipticals are composed of old stars! Ellipticals formed in a monolithic collapse,
More informationNew results on HE 0107 5240 and future surveys for metal-poor stars
New results on HE 0107 5240 and future surveys for metal-poor stars Norbert Christlieb Department of Astronomy and Space Physics, Uppsala University HE 0107 5240 [Fe I/H] NLTE = 5.3 The most heavy-element
More informationObserving the Universe
Observing the Universe Stars & Galaxies Telescopes Any questions for next Monday? Light Doppler effect Doppler shift Doppler shift Spectra Doppler effect Spectra Stars Star and planet formation Sun Low-mass
More informationDepartment of Astronomy Tel: (734) 615-6141 311 West Hall, 1085 S. University Ave. Fax: (734) 763-6317
University of Michigan Email: dnidever@umich.edu Department of Astronomy Tel: (734) 615-6141 311 West Hall, 1085 S. University Ave. Fax: (734) 763-6317 Ann Arbor, MI, 48109 http://dept.astro.lsa.umich.edu/~dnidever
More informationSDSS-III Project Execution Plan. Version 1.1 February 5, 2009
SDSS-III Project Execution Plan Version 1.1 February 5, 2009 1 This is version 1.1 of the Project Execution Plan for SDSS-III, submitted to the National Science Foundation on February 6, 2009. This document
More informationThis work was done in collaboration with the Centre de Données astronomiques de Strasbourg (CDS) and in particular with F. X. Pineau.
Chapter 5 Database and website This work was done in collaboration with the Centre de Données astronomiques de Strasbourg (CDS) and in particular with F. X. Pineau. 5.1 Introduction The X-shooter Spectral
More informationIntermediate-Mass Black Holes (IMBHs) in Globular Clusters? HST Proper Motion Constraints. Roeland van der Marel
Intermediate-Mass Black Holes (IMBHs) in Globular Clusters? HST Proper Motion Constraints Roeland van der Marel Why Study IMBHs in Globular Clusters (GCs)? IMBHs: IMBHs can probe a new BH mass range, between
More informationCAUP s Astronomical Instrumentation and Surveys
CAUP s Astronomical Instrumentation and Surveys CENTRO DE ASTROFÍSICA DA UNIVERSIDADE DO PORTO www.astro.up.pt Sérgio A. G. Sousa Team presentation sousasag@astro.up.pt CAUP's Astronomical Instrumentation
More informationMagellanic Cloud planetary nebulae as probes of stellar evolution and populations. Letizia Stanghellini
Magellanic Cloud planetary nebulae as probes of stellar evolution and populations Letizia Stanghellini Planetary nebulae beyond the Milky Way - May 19-21, 2004 1 Magellanic Cloud PNe The known distances,
More informationSoftware challenges in the implementation of large surveys: the case of J-PAS
Software challenges in the implementation of large surveys: the case of J-PAS 1/21 Paulo Penteado - IAG/USP pp.penteado@gmail.com http://www.ppenteado.net/ast/pp_lsst_201204.pdf (K. Taylor) (A. Fernández-Soto)
More informationThe Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC
The Hidden Lives of Galaxies Jim Lochner, USRA & NASA/GSFC What is a Galaxy? Solar System Distance from Earth to Sun = 93,000,000 miles = 8 light-minutes Size of Solar System = 5.5 light-hours What is
More informationUsing Photometric Data to Derive an HR Diagram for a Star Cluster
Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and
More informationLow-Mass X-Ray Binary Models for Ellipticals NGC3379 and NGC4278
Low-Mass X-Ray Binary Models for Ellipticals NGC3379 and NGC4278 Tassos Fragos with V. Kalogera, K. Belczynski, G. Fabbiano et al. Department of Physics and Astronomy Northwestern University MODEST 7b
More informationChapter 15.3 Galaxy Evolution
Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You
More informationIn studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
More information(Long-Baseline) Interferometric Measurements of Binary Stars
(Long-Baseline) Interferometric Measurements of Binary Stars A. Boden MSC/Caltech & GSU C. Hummel USNO/ESO G. Torres & D. Latham CfA H. McAlister CHARA/GSU Outline Introduction: Why study binary stars
More informationSKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT THE HERTZSPRUNG RUSSELL DIAGRAM
PROJECT 4 THE HERTZSPRUNG RUSSELL DIGRM Objective: The aim is to measure accurately the B and V magnitudes of several stars in the cluster, and plot them on a Colour Magnitude Diagram. The students will
More informationPlanets beyond the solar system
Planets beyond the solar system Review of our solar system Why search How to search Eclipses Motion of parent star Doppler Effect Extrasolar planet discoveries A star is 5 parsecs away, what is its parallax?
More informationAstro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
More informationFRONT-LINE RECURRENT NOVA SCIENCE REQUIRES CENTURY OLD DATA
FRONT-LINE RECURRENT NOVA SCIENCE REQUIRES CENTURY OLD DATA Bradley E. Schaefer (Louisiana State University) What stars create Type Ia Supernova? Now a big-money question. Recurrent novae (RN) are a likely
More informationPrinciples of Operation for SDSS- III
ASTROPHYSICAL RESEARCH CONSORTIUM Principles of Operation for SDSS- III VERSION: 11/06/2009 1 Introduction The Sloan Digital Sky Survey III (hereafter SDSS- III) as currently envisaged is a six- year program
More informationOrigins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
More informationAdaptive Optics (AO) TMT Partner Institutions Collaborating Institution Acknowledgements
THIRTY METER TELESCOPE The past century of astronomy research has yielded remarkable insights into the nature and origin of the Universe. This scientific advancement has been fueled by progressively larger
More informationHow To Set Up A Rov-Dfd (Rov Zero Point) Du)
DU640 Radial Velocity Zero-Point Software Requirement Specifications prepared by: approved by: reference: issue: 4 revision: 1 date: 28-03-2008 status: Issued G. Jasniewicz, F. Crifo, D. Hestroffer, A.
More informationGalaxy Survey data analysis using SDSS-III as an example
Galaxy Survey data analysis using SDSS-III as an example Will Percival (University of Portsmouth) showing work by the BOSS galaxy clustering working group" Cosmology from Spectroscopic Galaxy Surveys"
More informationEinstein Rings: Nature s Gravitational Lenses
National Aeronautics and Space Administration Einstein Rings: Nature s Gravitational Lenses Leonidas Moustakas and Adam Bolton Taken from: Hubble 2006 Science Year in Review The full contents of this book
More informationLecture 6: distribution of stars in. elliptical galaxies
Lecture 6: distribution of stars in topics: elliptical galaxies examples of elliptical galaxies different classes of ellipticals equation for distribution of light actual distributions and more complex
More informationand the VO-Science Francisco Jiménez Esteban Suffolk University
The Spanish-VO and the VO-Science Francisco Jiménez Esteban CAB / SVO (INTA-CSIC) Suffolk University The Spanish-VO (SVO) IVOA was created in June 2002 with the mission to facilitate the international
More informationClassroom Exercise ASTR 390 Selected Topics in Astronomy: Astrobiology A Hertzsprung-Russell Potpourri
Classroom Exercise ASTR 390 Selected Topics in Astronomy: Astrobiology A Hertzsprung-Russell Potpourri Purpose: 1) To understand the H-R Diagram; 2) To understand how the H-R Diagram can be used to follow
More informationTowards the Detection and Characterization of Smaller Transiting Planets
Towards the Detection and Characterization of Smaller Transiting Planets David W. Latham 27 July 2007 Kepler MISSION CONCEPT Kepler Mission is optimized for finding habitable planets ( 10 to 0.5 M )
More informationThe Birth and Assembly of Galaxies: the Relationship Between Science Capabilities and Telescope Aperture
The Birth and Assembly of Galaxies: the Relationship Between Science Capabilities and Telescope Aperture Betsy Barton Center for Cosmology University of California, Irvine Grateful acknowledgements to:
More informationThe facts we know today will be the same tomorrow but today s theories may tomorrow be obsolete.
The Scale of the Universe Some Introductory Material and Pretty Pictures The facts we know today will be the same tomorrow but today s theories may tomorrow be obsolete. A scientific theory is regarded
More informationA short history of telescopes and astronomy: Galileo to the TMT
A short history of telescopes and astronomy: Galileo to the TMT Telescopes in the last 400 years Galileo 1608 Hans Lippershey applied for a patent for seeing things far away as if they were nearby 1609
More informationThe Star Formation Histories of Disk and E/S0 Galaxies from Resolved Stars
The Star Formation Histories of Disk and E/S0 Galaxies from Resolved Stars Knut A.G. Olsen National Optical Astronomy Observatory kolsen@noao.edu Phone: (520)-318-8555 Co-authors: Aaron J. Romanowsky (UCO/Lick)
More informationThe formation and evolution of massive galaxies: A major theoretical challenge
The formation and evolution of massive galaxies: A major theoretical challenge Thorsten Naab Max-Planck-Institute for Astrophysics L. Oser, M. Hilz, P. Johansson, J. P. Ostriker Tähtitieteilijäpäivät Haikko,
More informationElliptical Galaxies. Virgo Cluster: distance 15Mpc
Elliptical Galaxies Virgo Cluster: distance 15Mpc Elliptical Galaxies Elliptical galaxies are thought to be the simplest of all types of galaxies. Yet, detailed analysis shows that they are much more complicated
More informationClass 2 Solar System Characteristics Formation Exosolar Planets
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
More informationScience Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
More informationThe Size & Shape of the Galaxy
name The Size & Shape of the Galaxy The whole lab consists of plotting two graphs. What s the catch? Aha visualizing and understanding what you have plotted of course! Form the Earth Science Picture of
More informationFirst Discoveries. Asteroids
First Discoveries The Sloan Digital Sky Survey began operating on June 8, 1998. Since that time, SDSS scientists have been hard at work analyzing data and drawing conclusions. This page describes seven
More informationThe Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun
The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun P.C. Frisch and A.J. Hanson Department of Astronomy and Astrophysics University of Chicago and Computer Science
More informationSDSS-III: Massive Spectroscopic Surveys of the Distant Universe, the Milky Way Galaxy, and Extra-Solar Planetary Systems 1.
SDSS-III: Massive Spectroscopic Surveys of the Distant Universe, the Milky Way Galaxy, and Extra-Solar Planetary Systems 1 January 8, 2008 1 Abstracted from a proposal to the National Science Foundation,
More informationWhat is the Sloan Digital Sky Survey?
What is the Sloan Digital Sky Survey? Simply put, the Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining
More informationUndergraduate Studies Department of Astronomy
WIYN 3.5-meter Telescope at Kitt Peak near Tucson, AZ Undergraduate Studies Department of Astronomy January 2014 Astronomy at Indiana University General Information The Astronomy Department at Indiana
More informationDIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION
1 DIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION Daniel S. Orton email: dsorton1@gmail.com Abstract: There are many longstanding
More informationThe CGM around Dwarf Galaxies
The CGM around Dwarf Galaxies Rongmon Bordoloi STScI + the COS-Halos Team What is the CGM? Shen et al. 212 jectedcolumndensityinacubeof5(proper)kpc Diffuse gas, including metals and dust, o2en on extending
More informationAstronomy & Physics Resources for Middle & High School Teachers
Astronomy & Physics Resources for Middle & High School Teachers Gillian Wilson http://www.faculty.ucr.edu/~gillianw/k12 A cosmologist is.... an astronomer who studies the formation and evolution of the
More informationStar Clusters and Stellar Dynamics
Ay 20 Fall 2004 Star Clusters and Stellar Dynamics (This file has a bunch of pictures deleted, in order to save space) Stellar Dynamics Gravity is generally the only important force in astrophysical systems
More informationEvolution of Close Binary Systems
Evolution of Close Binary Systems Before going on to the evolution of massive stars and supernovae II, we ll think about the evolution of close binary systems. There are many multiple star systems in the
More informationData Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
More informationElliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies
Elliptical Galaxies Houjun Mo April 19, 2004 Basic properties of elliptical galaxies Formation of elliptical galaxies Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses:
More informationS0 galaxy NGC 2787. Marcella Carollo, HST.
S0 galaxy NGC 2787. Marcella Carollo, HST. Dust lane in NGC 5128. Marina Rejkuba, ESO. Peculiar E galaxy NGC 1316. Paul Goudfrooij, HST. Dust-lane E galaxy NGC 5266. Carnegie Atlas of Galaxies. 1994ApJ...43
More informationA Universe of Galaxies
A Universe of Galaxies Today s Lecture: Other Galaxies (Chapter 16, pages 366-397) Types of Galaxies Habitats of Galaxies Dark Matter Other Galaxies Originally called spiral nebulae because of their shape.
More informationElliptical Galaxies. Old view: ellipticals are boring, simple systems
Eliptical Galaxies Elliptical Galaxies Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals formed in a monolithic collapse,
More informationData Mining Challenges and Opportunities in Astronomy
Data Mining Challenges and Opportunities in Astronomy S. G. Djorgovski (Caltech) With special thanks to R. Brunner, A. Szalay, A. Mahabal, et al. The Punchline: Astronomy has become an immensely datarich
More informationA Preliminary Summary of The VLA Sky Survey
A Preliminary Summary of The VLA Sky Survey Eric J. Murphy and Stefi Baum (On behalf of the entire Science Survey Group) 1 Executive Summary After months of critical deliberation, the Survey Science Group
More informationModeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
More informationStar Clusters. Star Clusters E NCYCLOPEDIA OF A STRONOMY AND A STROPHYSICS
Star Clusters Even a small telescope shows obvious local concentrations of stars scattered around the sky. These star clusters are not chance juxtapositions of unrelated stars. They are, instead, physically
More informationDebris disks at high resolution. Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge
Debris disks at high resolution Mark Wyatt Rachel Smith Institute of Astronomy, Cambridge Debris disk overview Debris disks are remnants of planet formation, planetesimals which failed to grow into planets;
More informationHighlights from the VLA/ANGST Survey
Highlights from the VLA/ANGST Survey Evan Skillman U. Minnesota Gas in Galaxies 2011: From Cosmic Web to Molecular Clouds Kloster Seeon, Germany 16/06/2011 VLA/ANGST The ANGST HST Treasury Project allowed
More informationThe Milky Way Galaxy is Heading for a Major Cosmic Collision
The Milky Way Galaxy is Heading for a Major Cosmic Collision Roeland van der Marel (STScI) [based on work with a team of collaborators reported in the Astrophysical Journal July 2012] Hubble Science Briefing
More informationExplorations of the Outer Solar System. B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics
Explorations of the Outer Solar System B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics The Known Solar System How big is the solar system? a tidal R 0 M Sun M Galaxy 1/3 200,000AU How big is
More informationSolar Ast ro p h y s ics
Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3
More informationPISGAH ASTRONOMICAL RESEARCH INSTITUTE AND ASTRONOMICAL PHOTOGRAPHIC DATA ARCHIVE. www.pari.edu
PISGAH ASTRONOMICAL RESEARCH INSTITUTE AND ASTRONOMICAL PHOTOGRAPHIC DATA ARCHIVE www.pari.edu PARI 200ac (80ha) campus 6.2mi (10km) of roads 12 buildings 100,000 ft2 (9290 m2) Extensive Internet Infrastructure
More informationWelcome to Class 4: Our Solar System (and a bit of cosmology at the start) Remember: sit only in the first 10 rows of the room
Welcome to Class 4: Our Solar System (and a bit of cosmology at the start) Remember: sit only in the first 10 rows of the room What is the difference between dark ENERGY and dark MATTER? Is Earth unique,
More information1.1 A Modern View of the Universe" Our goals for learning: What is our place in the universe?"
Chapter 1 Our Place in the Universe 1.1 A Modern View of the Universe What is our place in the universe? What is our place in the universe? How did we come to be? How can we know what the universe was
More informationJ-PAS: low-resolution (R 50) spectroscopy over 8000 deg 2
J-PAS: low-resolution (R 50) spectroscopy over 8000 deg 2 C. López-Sanjuan J. Cenarro, L. A. Díaz-García, J. Varela, K. Viironen, & the J-PAS team Centro de Estudio de Física del Cosmos de Aragón 10th
More information3D MODEL ATMOSPHERES OF THE SUN AND LATE-TYPE STARS. Remo Collet Australian National University
3D MODEL ATMOSPHERES OF THE SUN AND LATE-TYPE STARS Remo Collet Australian National University STELLAR SPECTRA Stellar spectra carry the information about the physical properties and compositions of stars
More informationThe Main Point. Lecture #34: Solar System Origin II. Chemical Condensation ( Lewis ) Model. How did the solar system form? Reading: Chapter 8.
Lecture #34: Solar System Origin II How did the solar system form? Chemical Condensation ("Lewis") Model. Formation of the Terrestrial Planets. Formation of the Giant Planets. Planetary Evolution. Reading:
More informationCurriculum Vitae et Studiorum Elena Pancino November 2013
Curriculum Vitae et Studiorum Elena Pancino November 2013 Name: Elena Surname: Pancino Place of Birth: Venice, Italy Date of Birth: 10 june 1968 Address: INAF Osservatorio Astronomico di Bologna, via Ranzani
More informationNITROGEN-TO-OXYGEN RATIO As a solid tool to ascertain the chemical evolution of star-forming galaxies
NITROGEN-TO-OXYGEN RATIO As a solid tool to ascertain the chemical evolution of star-forming galaxies Enrique Pérez Montero Instituto de Astrofísica de Andalucía - CSIC (Granada) Proyecto ESTALLIDOS DE
More informationModeling the Expanding Universe
H9 Modeling the Expanding Universe Activity H9 Grade Level: 8 12 Source: This activity is produced by the Universe Forum at NASA s Office of Space Science, along with their Structure and Evolution of the
More informationFollow-up Observations of SPY White Dwarf + M-Dwarf Binaries
15 th European Workshop on White Dwarfs ASP Conference Series, Vol. 372, 2007 R. Napiwotzki and M. R. Burleigh Follow-up Observations of SPY White Dwarf + M-Dwarf Binaries P. F. L. Maxted Astrophysics
More informationarxiv:1207.3646v1 [cs.ce] 16 Jul 2012
jcis@epacis.org OGCOSMO: An auxiliary tool for the study of the Universe within hierarchical scenario of structure formation arxiv:1207.3646v1 [cs.ce] 16 Jul 2012 Eduardo S. Pereira 1, Oswaldo D. Miranda
More informationThe orbit of Halley s Comet
The orbit of Halley s Comet Given this information Orbital period = 76 yrs Aphelion distance = 35.3 AU Observed comet in 1682 and predicted return 1758 Questions: How close does HC approach the Sun? What
More informationJINA AT UNIVERSITY OF CHICAGO
Jim Truran Astronomy and Astrophysics Enrico Fermi Institute ASC Center for Astrophysical Thermonuclear Flashes University of Chicago JINA Advisory Committee Meeting University of Notre Dame April 30,
More informationDelayed mergers: The contribution of ellipticals, globular clusters, and protoclusters to the LIGO detection rate
Delayed mergers: The contribution of ellipticals, globular clusters, and protoclusters to the LIGO detection rate Aug 16, 2005 Richard O Shaughnessy (with O Leary, Fregeau, Kalogera, Rasio, Ivanova, Belczynski)
More informationThe Evolution of GMCs in Global Galaxy Simulations
The Evolution of GMCs in Global Galaxy Simulations image from Britton Smith Elizabeth Tasker (CITA NF @ McMaster) Jonathan Tan (U. Florida) Simulation properties We use the AMR code, Enzo, to model a 3D
More informationExtra-solar massive planets with small semi-major axes?
Monografías de la Real Academia de Ciencias de Zaragoza. 25: 115 120, (2004). Extra-solar massive planets with small semi-major axes? S. Fernández, D. Giuliodori and M. A. Nicotra Observatorio Astronómico.
More informationCarbon stars in the Local Group
Carbon stars in the Local Group Martin Groenewegen groen@ster.kuleuven.ac.be Instituut voor Sterrenkunde - K.U.Leuven Torun October 2002 p.1/42 Overview Late-type stars How to find them? Inventory / Status
More informationHIGHLIGHTS OF RECENT RESULTS FROM THE VERITAS GAMMA-RAY OBSERVATORY TAUP-2015 TORINO. Lucy Fortson. VERITAS Collaboration. Fortson, TAUP 2015, Torino
HIGHLIGHTS OF RECENT RESULTS FROM THE VERITAS GAMMA-RAY OBSERVATORY TAUP-2015 TORINO Lucy Fortson forlucy the VERITAS Collaboration Fortson, TAUP 2015, Torino 1 499 PMTs 3.5o field of view 0.15o spacing
More informationName Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
More informationThis paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
More informationSYLLABUS FORM WESTCHESTER COMMUNITY COLLEGE Valhalla, NY l0595. l. Course #:PHYSC 151 2. NAME OF ORIGINATOR /REVISOR: PAUL ROBINSON
SYLLABUS FORM WESTCHESTER COMMUNITY COLLEGE Valhalla, NY l0595 l. Course #:PHYSC 151 2. NAME OF ORIGINATOR /REVISOR: PAUL ROBINSON NAME OF COURSE: ASTRONOMY 3. CURRENT DATE: OCTOBER 26, 2011. Please indicate
More informationGAIA Science and Mission
GAIA Science and Mission Nicholas Walton Institute of Astronomy The University of Cambridge p1 Outline Gaia high level science drivers Example science objectives Gaia mission overview Gaia data analysis
More informationUNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
More informationGalactic Bulge 5.0 Earthquake Study - radius of Population
1 The cluster Terzan 5 as a remnant of a primordial building block of the Galactic bulge F.R. Ferraro 1, E. Dalessandro 1, A. Mucciarelli 1, G.Beccari 2, M. R. Rich 3, L. Origlia 4, B. Lanzoni 1, R. T.
More informationStellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
More informationSSO Transmission Grating Spectrograph (TGS) User s Guide
SSO Transmission Grating Spectrograph (TGS) User s Guide The Rigel TGS User s Guide available online explains how a transmission grating spectrograph (TGS) works and how efficient they are. Please refer
More informationcircular motion & gravitation physics 111N
circular motion & gravitation physics 111N uniform circular motion an object moving around a circle at a constant rate must have an acceleration always perpendicular to the velocity (else the speed would
More informationProbability of detecting compact binary coalescence with enhanced LIGO
Probability of detecting compact binary coalescence with enhanced LIGO Richard O Shaughnessy [V. Kalogera, K. Belczynski] GWDAW-12, December 13, 2007 Will we see a merger soon? Available predictions Isolated
More informationVisualization of Large Multi-Dimensional Datasets
***TITLE*** ASP Conference Series, Vol. ***VOLUME***, ***PUBLICATION YEAR*** ***EDITORS*** Visualization of Large Multi-Dimensional Datasets Joel Welling Department of Statistics, Carnegie Mellon University,
More information