Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies. João Alves, University of Vienna
|
|
|
- Timothy Stanley
- 8 years ago
- Views:
Transcription
1 Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies João Alves, University of Vienna
2 Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies With: Charles Lada, CfA Marco Lombardi, University of Milan Jan Forbrich, University of Vienna Carlos Roman-Zuniga, UNAM Chris Faesi, CfA João Alves, University of Vienna
3 The Star Formation Rate Across Cosmic History What are the physical processes that set the SFR and control galaxy evolution? Bouwens et al. 2010
4 Schmidt s Conjecture: It would seem most probable that the rate of star formation depends on the gas density and we shall assume that the number formed per unit interval of time varies with a power of the gas density... Schmidt (1959) Σ SFR = κ (Σ g ) β [M pc -2 ]
5 Schmidt s Conjecture: It would seem most probable that the rate of star formation depends on the gas density and we shall assume that the number formed per unit interval of time varies with a power of the gas density... Schmidt (1959) Σ SFR = κ (Σ g ) β [M pc -2 ] It is rather tempting to try to estimate the effects of star formation...in galaxies as a whole.
6 Galaxies (z ~ 0)
7 Galaxies (z ~ 0)
8 Galaxies (z ~ 0) Schmidt-Kennicutt Law Σ SFR = A (Σ gas ) 1.6
9 Galaxies (z ~ 0) Schmidt-Kennicutt Law Σ SFR = A (Σ gas ) 1.6
10 Galaxies (z ~ 0) Bigiel et al. 2008
11 Galaxies (z ~ 0) Bigiel et al. 2008
12 Galaxies (z ~ 0) Bigiel et al. 2008
13 Galaxies (z ~ 0) Bigiel et al. 2008
14 Galaxies (z ~ 0) Bigiel et al. 2008
15 Galaxies (z ~ 0) Bigiel et al. 2008
16 Galaxies (z ~ 0) Bigiel et al. 2008
17 Giant Molecular Clouds?
18 Milky Way GMCs
19 Milky Way GMCs SFRs: Direct Counting of YSOs and measured ages.
20 Milky Way GMCs SFRs: Direct Counting of YSOs and measured ages. Masses: Resolved measurements of dust column densities and an asssumed gas-to-dust ratio
21 Dust Column Densities
22 Dust Column Densities Optical
23 Dust Column Densities Optical Near infrared Alves+01
24 Dust Column Densities Optical Near infrared Alves+01
25 Dust Column Densities Optical Near infrared Alves+01 Nielbock+13, Roy+14
26 Local molecular clouds (same size scale) Perseus Pipe Ophiuchus Taurus 10 pc Orion 10 pc Lombardi Alves Lada 06-12
27 Giant Molecular Clouds Does a Schmidt Law exist for MW GMCs?
28 Giant Molecular Clouds
29 Giant Molecular Clouds
30 Giant Molecular Clouds
31 Giant Molecular Clouds A Schmidt Law does NOT exist between GMCs
32 Giant Molecular Clouds M = Σ c R 2 Lombardi et al. 2010
33 Giant Molecular Clouds M = Σ c R 2 Lombardi et al Well known scaling relation of Larson (1981)
34 Giant Molecular Clouds M = Σ c R 2 Lombardi et al Well known scaling relation of Larson (1981) A Schmidt Law does NOT exist between GMCs
35 Giant Molecular Clouds Does a Schmidt Law exist within GMCs?
36 1.0 5 Orion B Mon R2 λ Orion 0.8 LBN LDN 1652 LBN 1017 Galactic Latitude 15 TGU H1523 NGC 2149 NGC 2170 LBN AK (mag) GN LBN 1016 LBN 1019 Orion A IC Galactic Longitude
37 1.0 5 Orion B λ Orion Mon R2 0.8 LBN 1015 LDN 1652 LBN Galactic Latitude AK (mag) NGC 2170 TGU H1523 Mon R2 LBN 933 NGC 2071 NGC GN ri 16 O Galactic Latitude on B NGC NGC 2024 Orion A IC 423 LBN LBN 1019 Orion Nebula 0.2 NGC Orion A 10 pc Galactic Longitude Galactic Longitude
38 12 Mon R2 14 NGC 2071 NGC 2068 Galactic Latitude NGC 2024 Orion B Orion Nebula NGC Orion A 10 pc Galactic Longitude Lombardi et al Planck+Herschel+2MASS
39 12 Mon R2 14 NGC 2071 NGC 2068 Galactic Latitude NGC 2024 Orion B Orion Nebula NGC Orion A 10 pc Galactic Longitude Lombardi et al Planck+Herschel+2MASS
40 12 Mon R2 14 NGC 2071 NGC 2068 Galactic Latitude NGC 2024 Orion B Orion Nebula NGC Orion A 10 pc Galactic Longitude Lombardi et al Planck+Herschel+2MASS
41 12 Mon R2 14 NGC 2071 NGC 2068 Galactic Latitude β = 2 NGC 2024 Orion B Orion Nebula NGC Orion A 10 pc Galactic Longitude Lombardi et al Planck+Herschel+2MASS
42 Schmidt Law in Giant Molecular Clouds California Orion A California Results: Orion A Taurus California Orion B β 2.0 ± ± ± ± 0.2 κ 1.6 ± ± ± ± 0.1 σ 0.03± ± ± ± 0.02 A ± ± ± ±0.14 Herschel
43 Schmidt Law in Giant Molecular Clouds California Orion A California Results: Orion A Taurus California Orion B β 2.0 ± ± ± ± 0.2 κ 1.6 ± ± ± ± 0.1 σ 0.03± ± ± ± 0.02 A ± ± ± ±0.14 Herschel Gutermuth et al. 2011
44 Schmidt Law in Giant Molecular Clouds California Orion A California Results: Orion A Taurus California Orion B β 2.0 ± ± ± ± 0.2 A Schmidt Law Exists within GMCs κ 1.6 ± ± ± ± 0.1 Heidermann et al. 2010, Gutermuth et al. 2011, Lombardi et al. 2013, σ 0.03± ± ± ± 0.02 Lada et al. 2013, Evans et Aal ± ± ± ±0.14 Herschel Gutermuth et al. 2011
45 Giant Molecular Clouds Milky Way GMCs A Schmidt Law within clouds does NOT explain variations in SFRs between clouds.
46 Schmidt Law and Star Formation in GMCs
47 Schmidt Law and Star Formation in GMCs
48 Schmidt Law and Star Formation in GMCs N * (>A K ) = Σ * (>A K ) x S(>A K )
49
50 Surface Area Distribution Function, S(>A K )
51 Cloud structure plays a critical role in determining the SFR in clouds! Surface Area Distribution Function, S(>A K )
52 Scaling Relations for Local GMCs Need to consider integrated quantities
53 Extending the Scaling Relation to Higher Masses and SFRs: the Nearby Galaxy NGC 300
54 Scaling Relations for GMCs: Nearby Galaxies NGC 300 Faesi et al. 2014
55 A Column Density Threshold for Star Formation
56 Column Density Threshold for Star Formation Orion A Herschel: 250 µm Lombardi et al. 2014
57 Column Density Threshold for Star Formation Orion A Herschel: 250 µm Lombardi et al. 2014
58 Column Density Threshold for Star Formation Orion A Herschel: 250 µm 90% of Protostars at A K > 1.0 mag Lombardi et al. 2014
59 Column Density Threshold for Star Formation Orion A Local Dark Cloud Sample Protostars Evans et al. 2014
60 Column Density Threshold for Star Formation Orion A Local Dark Cloud Sample Protostars 90% of Protostars at A K > 1.0 mag Evans et al. 2014
61 Kruijssen Longmore+2013 Column Density Threshold for Star Formation?
62 Star Formation Scaling Law for Local Clouds A linear scaling relation 1 Lada et al A K > Myr The SFR is controlled by the mass or total amount of dense gas contained within molecular clouds SFR = (t gc ) -1 M dense t gc = gas consumption time = 2.2 x 10 7 yrs 1 SFR = 2.5 x 10-5 N(YSOs) M /yr
63 Star Formation Scaling Law for Local Clouds A linear scaling relation 1 The SFR is controlled by the mass or total amount of dense gas contained within molecular clouds t gc = gas consumption time = 2.2 x 10 7 yrs 1 SFR = 2.5 x 10-5 N(YSOs) M /yr
64 Star Formation Scaling Law for Local Clouds A linear scaling relation 1 The SFR is controlled by the mass or total amount of dense gas contained within molecular clouds t gc = gas consumption time = 2.2 x 10 7 yrs 1 SFR = 2.5 x 10-5 N(YSOs) M /yr
65 f = 1.0 f = 0.1 f = 0.01 From GMCs to Galaxies SFR = ( t gc ) -1 M >0.8 The SFR is controlled by the mass of dense gas contained within molecular clouds and entire galaxies. Gao & Solomon 2004
66 f = 1.0 f = 0.1 f = 0.01 From GMCs to Galaxies SFR = ( t gc ) -1 M >0.8 The SFR is controlled by the mass of dense molecular gas within GMCs and galaxies. Gao & Solomon 2004
67 Scaling Relations for Star Formation GMCs Scaling Law from GMCs to Galaxies SFR = ( t gc ) -1 M >A0 Gao & Solomon Wu et al. 2005
68 Scaling Relations for GMCs Star Formation Scaling Law from GMCs to Galaxies SFR = ( t gc ) -1 M >A0 The physical process of star formation in galaxies must be very similar to that in MW GMCs Gao & Solomon Wu et al. 2005
69 f = 1.0 f = 0.1 f = 0.01 Star Formation Scaling Law from GMCs to Galaxies SFR = ( t gc ) -1 M >A0 Gao & Solomon Wu et al. 2005
70 f = 1.0 f = 0.1 f = 0.01 Star Formation Scaling Law from GMCs to Galaxies SFR = ( t gc ) -1 M >A0 Early Universe: z = 2-4 Gao & Solomon Wu et al. 2005
71 f = 1.0 f = 0.1 f = 0.01 The physical process of star formation in distant galaxies and through much of cosmic history must be reasonably the same as it is presently in the nearest molecular clouds. Star Formation Scaling Law from GMCs to Galaxies SFR = ( t gc ) -1 M >A0 Early Universe: z = 2-4 Gao & Solomon Wu et al. 2005
72 Deconstructing the Kennicutt-Schmidt Scaling Relation
73 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 Bigiel et al AJ 136:2846
74 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 Bigiel et al AJ 136:2846 Schruba et al AJ 142;37
75 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 Bigiel et al AJ 136:2846 Schruba et al AJ 142;37
76 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 Bigiel et al AJ 136:2846 Schruba et al AJ 142;37
77 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 HI DILUTION Bigiel et al AJ 136:2846 Schruba et al AJ 142;37
78 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 HI DILUTION Bigiel et al AJ 136:2846 Schruba et al AJ 142;37
79 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 HI DILUTION Bigiel et al AJ 136:2846 Schruba et al AJ 142;37
80 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 4 M pc -2 f mb = 0.1 HI DILUTION Bigiel et al AJ 136:2846
81 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 4 M pc -2 f mb = 0.1 HI DILUTION 8 M pc -2 f mb = 0.2 Bigiel et al AJ 136:2846
82 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 4 M pc -2 f mb = 0.1 HI DILUTION 8 M pc -2 f mb = M pc -2 f mb = 1.0 Bigiel et al AJ 136:2846
83 Deconstructing the Kennicutt-Schmidt Law: Galaxies HI H 2 4 M pc -2 f mb = 0.1 HI DILUTION 8 M pc -2 f mb = 0.2 CLOUD COUNTING 40 M pc -2 f mb = 1.0 Bigiel et al AJ 136:2846
84 Deconstructing the Kennicutt-Schmidt Law: Galaxies Starburst Galaxies: Disks HI H 2 Starbursts 4 M pc -2 f mb = 0.1 HI DILUTION 8 M pc -2 f mb = 0.2 CLOUD COUNTING 40 M pc -2 f mb = 1.0 Bigiel et al. 2008
85 Deconstructing the Kennicutt-Schmidt Law: Galaxies Starburst Galaxies: Disks HI H 2 Starbursts 4 M pc -2 f mb = 0.1 HI DILUTION 8 M pc -2 f mb = 0.2 INCREASED f dense CLOUD COUNTING 40 M pc -2 f mb = 1.0 Bigiel et al. 2008
86 Summary 1. There is no Schmidt Law between GMCs 2. A Schmidt Law does exist within GMCs but it does not provide a complete description of a cloud s star formation activity. 3. The structure of a cloud plays a pivotal role in setting its global SFR and the overall level of its star formation activity. 4. The integrated SFR scales linearly with, and is most reliably traced by, the dense gas mass in a star forming region. 5. The amount of dense gas sets the SFR in systems ranging from individual GMCs to entire galaxies. 6. The Kennicutt-Schmidt law for galaxies is largely the result of unresolved measurements of GMCs and not a result of any underlying physical law of star formation.
87 Conclusion
88 Conclusion The physical process of star formation in distant galaxies and through much of cosmic history may be reasonably the same as it is presently in the nearest molecular clouds.
Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies
Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies With: Marco Lombardi, University of Milan Joao Alves, University of Vienna Jan Forbrich, University of Vienna Carlos Roman-Zuniga,
A Star and Gas Surface Density Correlation within Nearby Molecular Clouds
A Star and Gas Surface Density Correlation within Nearby Molecular Clouds Rob Gutermuth Five College Astronomy Dept. Fellow in Research & Teaching Smith College & UMass Amherst MonR2 Giant Molecular Cloud
The 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
Star Formation in the Large Magellanic Cloud: Tracing an Evolution of Giant Molecular Clouds
Star Formation in the Large Magellanic Cloud: Tracing an Evolution of Giant Molecular Clouds Toshikazu Onishi Osaka Prefecture University Yasuo Fukui; Akiko Kawamura; Norikazu Mizuno; Tetsuhiro Minamidani;
Dinamica del Gas nelle Galassie II. Star formation
Dinamica del Gas nelle Galassie II. Star formation Overview on ISM Molecular clouds: composition and properties. Plasmas Charge neutrality, infinite conductivity; Field freezing; Euler equation with magnetic
IV. Molecular Clouds. 1. Molecular Cloud Spectra
IV. Molecular Clouds Dark structures in the ISM emit molecular lines. Dense gas cools, Metals combine to form molecules, Molecular clouds form. 1. Molecular Cloud Spectra 1 Molecular Lines emerge in absorption:
COMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES
IC 10 Henize 2-10 NGC 253 COMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES E.Bayet: LRA-LERMA-ENS (Paris) Antennae IC 342 M 83 NGC 6946 INTRODUCTION : OBJECTS : warm and dense molecular clouds
Lecture 3 Properties and Evolution of Molecular Clouds. Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11
Lecture 3 Properties and Evolution of Molecular Clouds Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11 From slide from Annie Hughes Review CO t in clouds HI: Atomic Hydrogen http://www.atnf.csiro.au/research/lvmeeting/magsys_pres/
In 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
Modeling 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
NGUYEN LUONG QUANG. Président du jury: J. Le Bourlot Rapporteurs: H. Beuther, T. Moore Examinateurs: I. Bonnell, F. Boulanger, F. Combes, F.
NGUYEN LUONG QUANG Supervisors: Frédérique Motte (CEA Saclay) Marc Sauvage (CEA Saclay) Président du jury: J. Le Bourlot Rapporteurs: H. Beuther, T. Moore Examinateurs: I. Bonnell, F. Boulanger, F. Combes,
Chapter 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
Resultados Concurso Apex 2007
Resultados Concurso Apex 2007 Propuesta: CC-07-03 Investigador Principal: Leonardo Bronfman Título: ATLASGAL: APEX Telescope Large Area Survey of the Galaxy Resumen: The location of the APEX telescope
Class 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
Faber-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
Resultados Concurso Apex 2014-A
Resultados Concurso Apex 2014-A Propuesta: 2014A/04 Investigador Principal: Guido Garay, Universidad de Chila Título: SuperMALT: determining the physical and chemical evolution of high-mass starforming
Adaptive 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
CO isotopologues in the Perseus Molecular Cloud Complex: the X-factor and regional variations
CO isotopologues in the Perseus Molecular Cloud Complex: the X-factor and regional variations Jaime E. Pineda Harvard-Smithsonian Center for Astrophysics, 6 Garden St., MS-1, Cambridge, MA 2138, USA jpineda@cfa.harvard.edu
Observing 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
Populations 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
Probes of Star Formation in the Early Universe
Gamma Ray Bursts Probes of Star Formation in the Early Universe Edward P.J.van den Heuvel Universiteit van Amsterdam &KITP-UCSB KITP, March 17, 2007 Age of the Universe: 13.7 billion years Age of our Milky
Cloud Formation, Evolution and Destruction
Chapter 4 Cloud Formation, Evolution and Destruction We now begin to trace the journey towards a star. How long does this take? The answer is surprisingly short: a good many clouds already contain new
Answers for the Student Worksheet for the Hubble Space Telescope Scavenger Hunt
Instructions: Answers are typed in blue. Answers for the Student Worksheet for the Hubble Space Telescope Scavenger Hunt Crab Nebula What is embedded in the center of the nebula? Neutron star Who first
165 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
Ellipticals. 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,
Highlights 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
Gamma Rays from Molecular Clouds and the Origin of Galactic Cosmic Rays. Stefano Gabici APC, Paris
Gamma Rays from Molecular Clouds and the Origin of Galactic Cosmic Rays Stefano Gabici APC, Paris The Origin of galactic Cosmic Rays Facts: the spectrum is (ALMOST) a single power law -> CR knee at few
The 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
Summary: Four Major Features of our Solar System
Summary: Four Major Features of our Solar System How did the solar system form? According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar
Science 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
Carbon 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
Planck Early Results: New light on Anomalous Microwave Emission from Spinning Dust Grains
Planck Early Results: New light on Anomalous Microwave Emission from Spinning Dust Grains Perseus in the optical Clive Dickinson Jodrell Bank Centre for Astrophysics (University of Manchester) On behalf
How did the Solar System form?
How did the Solar System form? Is our solar system unique? Are there other Earth-like planets, or are we a fluke? Under what conditions can Earth-like planets form? Is life common or rare? Ways to Find
The Messier Objects As A Tool in Teaching Astronomy
The Messier Objects As A Tool in Teaching Astronomy Dr. Jesus Rodrigo F. Torres President, Rizal Technological University Individual Member, International Astronomical Union Chairman, Department of Astronomy,
7. In which part of the electromagnetic spectrum are molecules most easily detected? A. visible light B. radio waves C. X rays D.
1. Most interstellar matter is too cold to be observed optically. Its radiation can be detected in which part of the electromagnetic spectrum? A. gamma ray B. ultraviolet C. infrared D. X ray 2. The space
Direct Detections of Young Stars in Nearby Ellipticals
Direct Detections of Young Stars in Nearby Ellipticals (NRAO Green Bank) Joel N. Bregman (University of Michigan) Click icon to add picture ApJ, in press (arxiv:1205.1066) Red and Dead Conventional wisdom:
Astronomy & Teaching Programs at UCT
Astronomy & Teaching Programs at UCT Prof. Renée C. Kraan-Korteweg Astronomy Department (UCT) Co-Director Astrophysics, Cosmology and Gravity Centre (ACGC) Astronomy Departmental Profile Developments (mostly
YSO Orion Molecular Cloud Aims Of Stahler & Bakk.N.R.T.P.R.T.T.
Protobinaries von Cornelia Weber, Bakk.rer.nat. Overview Motivation Molecular Clouds Young Stellar Objects Multiplicity of YSO Orion Molecular Cloud Aims of my thesis Motivation Binary and Multiple system
Name: João Fernando Alves da Silva Class: 7-4 Number: 10
Name: João Fernando Alves da Silva Class: 7-4 Number: 10 What is the constitution of the Solar System? The Solar System is constituted not only by planets, which have satellites, but also by thousands
Star formation relations across the CO ladder and redshift Thomas R. Greve (University College London)
Star formation relations across the CO ladder and redshift Thomas R. Greve (University College London) DeMoGas: Manolis Xilouris (NOA) Ioanna Leonid (NOA) Padelis Papadopoulos (Cardiff) Paul van der Werf
Resultados Concurso Apex 2008-1
Resultados Concurso Apex 2008-1 Lista 1 Propuestas seleccionadas Propuesta: C-081.F-0015-2008 Investigador Principal: Sophia A. Khan Título: Constraining the nature of submillimetre galaxies: a LABOCA
The Expanding Universe
Stars, Galaxies, Guided Reading and Study This section explains how astronomers think the universe and the solar system formed. Use Target Reading Skills As you read about the evidence that supports the
Initial Highlights from the Gould Belt Survey
Initial Highlights from the Gould Belt Survey Philippe André, CEA/SAp Saclay A.Men shchikov, S.Bontemps, V. Könyves, F. Motte, N. Schneider, P. Didelon, V. Minier, P. Saraceno, D.Ward- Thompson, J. Di
ALMA Overview. Leonardo Testi (European Southern Observatory)
ALMA Overview Leonardo Testi (European Southern Observatory) The ALMA Project Status Timeline towards Early and Full Science Operations Future Developments Atacama Large Millimeter Array At least 50x12m
Elliptical 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:
The 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:
TELESCOPE AS TIME MACHINE
TELESCOPE AS TIME MACHINE Read this article about NASA s latest high-tech space telescope. Then, have fun doing one or both of the word puzzles that use the important words in the article. A TELESCOPE
SUPPLEMENT 2. ESTIMATING THE EPOCHS OF THE GCC AND GA
Crucifying the Earth on the Galactic Cross. upplement 2 1 UPPLEMENT 2. ETIMATING THE EPOCH OF THE GCC AND GA 2.1. OLAR YTEM AND GALACTIC PARAMETER Coordinate ystems. In the Equatorial and al coordinate
Modelling clumpy! galactic disks
Modelling clumpy! galactic disks Simone Bianchi INAF-Osservatorio Astrofisico di Arcetri, Firenze with TRADING! Transfer of RAdiation through Dust IN Galaxies (Bianchi 2008) Radiative Transfer models"
The Birth of the Universe Newcomer Academy High School Visualization One
The Birth of the Universe Newcomer Academy High School Visualization One Chapter Topic Key Points of Discussion Notes & Vocabulary 1 Birth of The Big Bang Theory Activity 4A the How and when did the universe
The 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
RICHARD B. LARSON Yale Astronomy Department, Box 6666, New Haven, CT 06511, U.S.A.
PRESENT-DAY CLUSTER FORMATION RICHARD B. LARSON Yale Astronomy Department, Box 6666, New Haven, CT 06511, U.S.A. ABSTRACT A review is presented of some of the observed features of cluster formation in
Study Guide: Solar System
Study Guide: Solar System 1. How many planets are there in the solar system? 2. What is the correct order of all the planets in the solar system? 3. Where can a comet be located in the solar system? 4.
8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
ASTRONOMY AND ASTROPHYSICS. Deep search for CO emission in the Low Surface Brightness galaxy Malin 1. J. Braine 1, F. Herpin 1,2, and S.J.E.
Astron. Astrophys. 358, 494 498 (2000) Deep search for CO emission in the Low Surface Brightness galaxy Malin 1 ASTRONOMY AND ASTROPHYSICS J. Braine 1, F. Herpin 1,2, and S.J.E. Radford 3 1 Observatoire
Exceptionally massive and bright, the earliest stars changed the course of cosmic history
THE FIRST STARS IN THE UNIVERSE Exceptionally massive and bright, the earliest stars changed the course of cosmic history BY RICHARD B. LARSON AND VOLKER BROMM ILLUSTRATIONS BY DON DIXON We live in a universe
13 Space Photos To Remind You The Universe Is Incredible
13 Space Photos To Remind You The Universe Is Incredible NASA / Via photojournal.jpl.nasa.gov New ultraviolet images from NASA s Galaxy Evolution Explorer shows a speeding star that is leaving an enormous
The 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)
1.1 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
Top 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
The Interstellar Medium Astronomy 216 Spring 2005
The Interstellar Medium Astronomy 216 Spring 2005 Al Glassgold & James Graham University of California, Berkeley The Interstellar Medium/Media (ISM) What is the ISM? Just what it says: The stuff between
The 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
1 A Solar System Is Born
CHAPTER 3 1 A Solar System Is Born SECTION Formation of the Solar System BEFORE YOU READ After you read this section, you should be able to answer these questions: What is a nebula? How did our solar system
Dense gas in ULIRGs. Paul van der Werf. Leiden Observatory. Crete September 15, 2008
Dense gas in ULIRGs Paul van der Werf Leiden Observatory Crete September 15, 2008 Credits Padeli Papadopoulos (Bonn University) Kate Isaak (Cardiff University) Dense gas in ULIRGs 2 Simple people who think
Sound. References: L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol. 2, Gas Dynamics, Chapter 8
References: Sound L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol., Gas Dynamics, Chapter 8 1 Speed of sound The phenomenon of sound waves is one that
Lesson 3: Isothermal Hydrostatic Spheres. B68: a self-gravitating stable cloud. Hydrostatic self-gravitating spheres. P = "kt 2.
Lesson 3: Isothermal Hydrostatic Spheres B68: a self-gravitating stable cloud Bok Globule Relatively isolated, hence not many external disturbances Though not main mode of star formation, their isolation
Nuclear fusion in stars. Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars
Nuclear fusion in stars Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars The origin of structure in the Universe Until the time of formation of protogalaxies,
Activity: Multiwavelength Bingo
ctivity: Multiwavelength background: lmost everything that we know about distant objects in the Universe comes from studying the light that is emitted or reflected by them. The entire range of energies
The 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
FXA 2008. UNIT G485 Module 5 5.5.1 Structure of the Universe. Δλ = v λ c CONTENTS OF THE UNIVERSE. Candidates should be able to :
1 Candidates should be able to : CONTENTS OF THE UNIVERSE Describe the principal contents of the universe, including stars, galaxies and radiation. Describe the solar system in terms of the Sun, planets,
Probability 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
Astro 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,
So What All Is Out There, Anyway?
So What All Is Out There, Anyway? Imagine that, like Alice in Wonderland, you have taken a magic potion that makes you grow bigger and bigger. You get so big that soon you are a giant. You can barely make
A 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.
Lecture 7: Formation of the Solar System
Lecture 7: Formation of the Solar System Dust and debris disk around Fomalhaut, with embedded young planet! Claire Max April 24 th, 2014 Astro 18: Planets and Planetary Systems UC Santa Cruz Solar System
First 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
The Ultimate Messier Object Log PDF
The Ultimate Messier Object Log PDF This special version of The Ultimate Messier Object Log was created in response to all those people who don t have Filemaker, or who don t have the computer skills to
L3: The formation of the Solar System
credit: NASA L3: The formation of the Solar System UCL Certificate of astronomy Dr. Ingo Waldmann A stable home The presence of life forms elsewhere in the Universe requires a stable environment where
Origins 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
!"#"$%&'"((&"(()'*#%&+,-.&-.)&/012 3456&#)((78(&9:7'&-.)&;01&<&=51& >3?!/5&(@:A)%& *%&B:"8C7,(&="''):&
!"#"$%&'"((&"(()'*#%&+,-.&-.)&/012 3456&#)((78(&9:7'&-.)&;01&3?!/5&(@:A)%& *%&B:"8C7,(&="''):& 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78& G& M83 NGC 1365 M100 SABbc M 31 NGC 2997 NGC 1313 5."I,8J&/2/01&5K,)8K)&"8L&>8(-:@')8-"M78&
The Universe Inside of You: Where do the atoms in your body come from?
The Universe Inside of You: Where do the atoms in your body come from? Matthew Mumpower University of Notre Dame Thursday June 27th 2013 Nucleosynthesis nu cle o syn the sis The formation of new atomic
California Standards Grades 9 12 Boardworks 2009 Science Contents Standards Mapping
California Standards Grades 912 Boardworks 2009 Science Contents Standards Mapping Earth Sciences Earth s Place in the Universe 1. Astronomy and planetary exploration reveal the solar system s structure,
Unit 1.7: Earth and Space Science The Structure of the Cosmos
Lesson Summary: This week students will search for evidence provided in passages that lend support about the structure and organization of the Cosmos. Then students will summarize a passage. Materials
What 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
The 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
The 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
Debris 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;
Explorations 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
Lecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula
Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain
Heating & Cooling in Molecular Clouds
Lecture 8: Cloud Stability Heating & Cooling in Molecular Clouds Balance of heating and cooling processes helps to set the temperature in the gas. This then sets the minimum internal pressure in a core
Galaxy Classification and Evolution
name Galaxy Classification and Evolution Galaxy Morphologies In order to study galaxies and their evolution in the universe, it is necessary to categorize them by some method. A classification scheme generally
PISGAH 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
Searching for young proto-planetary disks from ALMA archival data Final presentation
Searching for young proto-planetary disks from ALMA archival data Final presentation Speaker: Pou Ieng Cheong( 張 寶 瑩 ) 1 Supervisor: Shih Ping Lai( 賴 詩 萍 ) 2,3 1 Department of electrophysics, NCTU 2 Department
THE FORMATION OF THE HIGH-VELOCITY CLOUDS OF THE MILKY WAY
THE FORMATION OF THE HIGH-VELOCITY CLOUDS OF THE MILKY WAY Antonino Marasco Kapteyn Astronomical Institute, Groningen In collaboration with: Filippo Fraternali (University of Bologna) Federico Marinacci
STUDY GUIDE: Earth Sun Moon
The Universe is thought to consist of trillions of galaxies. Our galaxy, the Milky Way, has billions of stars. One of those stars is our Sun. Our solar system consists of the Sun at the center, and all
The Origin and Evolution of the Universe
The Origin and Evolution of the Universe 9.7 People have been wondering about the Universe for a long time. They have asked questions such as Where did the Universe come from? How big is it? What will
Week 1-2: Overview of the Universe & the View from the Earth
Week 1-2: Overview of the Universe & the View from the Earth Hassen M. Yesuf (hyesuf@ucsc.edu) September 29, 2011 1 Lecture summary Protein molecules, the building blocks of a living organism, are made
Elliptical 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,
Star 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
THE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk
THE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk 1.INTRODUCTION Late in the nineteenth century, astronomers had tools that revealed a great deal about stars. By that time, advances in telescope