COMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES
|
|
|
- Rafe Sullivan
- 8 years ago
- Views:
Transcription
1 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
2 INTRODUCTION : OBJECTS : warm and dense molecular clouds in the nuclei of 20 nearby galaxies with different morphological types (D < 10 Mpc) targets for ALMA and Herschel GOALS : 1) describe the physical properties of these objects localize the GMCs in these nuclei correlations morphological types - cooling rates? prediction of emission lines for more distant objects 2) understand the links existing between dust and gas cooling rates HOW : Observations of C and CO lines in mm-submm windows (υ= GHz) with CSO (Hawaii, USA) and IRAM-PdB (FRANCE) for the first time C( 3 P 2-3 P 1 ) (υ=809 GHz) high-j CO lines observed : 12 CO(6-5), (7-6) (υ=691 GHz, 806 GHz) LVG (radiative transfer calculations) and PDR (photodissociation regionsthermal balance) models to derive the physical properties
3 GALAXIES SAMPLE : Properties : - accessibles from the northern hemisphere - bright in the low-j CO lines, e.g., 12 CO(1-0) and 12 CO(2-1) - ~20 nearby galaxies with different morphological types: normal spiral galaxies: IC 342, M 51, NGC 6946 irregular star forming galaxies: Henize 2-10, IC 10 starburst galaxies: M 82, M 83, NGC 253 interacting galaxies: NGC 6090, IRAS , the Antennae ULIRGs: Markarian 231, Arp 220 LINER: NGC 4736, NGC 3079
4 E. Bayet OBSERVED LINES : CO = good tracer of H2 molecular masses C linked with PDRs (mostly in the first layers) Study of the variation of C over CO density ratio N(C)/ N(CO) in the molecular cloud Clouds are ruled by: heating - photoelectric effects on grains - collisionnal deexcitation of H2 cooling (condensation of clouds = star formation) - neutral layer (Av < 5): CII, OI - molecular layer (Av > 5) : CO & C From Hollenbach & T ielens (1999) CO lines refer to transitions between two rotationnal levels C lines refer to transitions between two electronical levels
5 MODELS : LVG ( Large Velocity Gradient ) : radiative transfer calculations with one standard spherical component + T k and gas density considered as constant 4 input parameters : N(CO)/FWHM,, n(h 2 ), T k and abundance ratio 12 CO/ CO C ( 13 CO used for discriminating solutions) O PDR or «photodissociation regions» : 2 input parameters : radiation field and n(h) + gaseous phase abundances, etc Intensities of each CO lines are computed up to 12 CO(15-14) and we computed intensities of C lines C( 3 P 1-3 P 0 ) & C( 3 P 2-3 P 1 ) Comparison with observations Physical properties of the ISM derived!! From Hollenbach & T ielens (1999)
6 RESULTS : example (IC 342) of CO cooling curve Observations of the 13 CO(6-5), 12 CO(8-7) and up will be very useful to discriminate models solutions ALMA & Herschel!! 2 LVG models needed to reproduce cold and warm molecular gas
7 E. Bayet CO cooling curves : He 2-10, M 83 & Cloverleaf QSO : peak position 12CO(7-6) and up IC 10, NGC 253, NGC 4038, NGC 6946 & Overlap : peak position 12CO(6-5) IC 342 and Center of Milky Way : peak position 12CO(5-4) and below CO(5-4) to CO(7-6) = major coolants C(3P2-3P1) = major coolant CO cooling rate > C cooling rate Similarities in the CO cooling curves mean similarities in the physical properties, morphological types Grey full points are derived from PDR models
8 E. Bayet Comparison between differents tracers : 1) Morphologic Larger dispersion in dust cooling than in radiation field and density PDR / TOTAL (CII) Dust cooling Dust cooling Cooling efficiency (CO / FIR & C/ FIR) Density (CII / OI) Radiation field (CII / C) (neutral and molecular gas + dust) Dust cooling Contribution of the CII from PDR more important in NGC 6946 CO cooling rate more efficient than C cooling rate IC 10 clearly differs from others Heating efficiency
9 Comparison between differents tracers : 1) Morphologic (bis) (neutral and molecular gas + dust) * CO(1-0) known as tracer of star formation * Total CO cooling rates computed from 1-0 to lines (PDR) also good tracer Dust cooling
10 E. Bayet Comparison between differents tracers : 2) Coolants (neutral and molecular gas + dust) Correlations between CII, C and CO cooling rates CII cooling rate > OI cooling rate Starburst galaxies (NGC 253, M 83) have the highest CII, OI, C & CO cooling rates and highest FIR flux Merger and irregular galaxies have the lowest rates
11 PERSPECTIVES : MERCI! Finish the analysis of these figures and quantify precisely the links existing between o morphological type of nuclei & lines which contribute the most to the CO and C cooling rates o different coolant species (relation between neutral, molecular gas and dust) o cooling and heating processes in the GMCs Complete these results with the other galaxies from our sample: LVG and PDR models should be applied (already published paper in A&A: The submillimeter C and CO lines in Henize 2-10 and NGC 253 and paper in preparation for the other sources) Other works in progress: - Localize the GMCs in IC 10 nucleus from high resolution IRAM-Plateau De Bure observations and compare CO with ISO data (LW2 et LW3 at 7 and 15 µm) - Collaboration at the Leiden Observatory (F. Israel) concerning models: plan to use a combined XDR-PDR models in development My PhD work shall be included in the future large programs performed by ALMA, the Herschel satellite with the HIFI, PACS and SPIRE instruments and the Spitzer Space Satellite with the IRAC camera and the IRS spectrometer.
12
13 OBSERVED LINES : CO & C : several lines which emit: Hollenbach & T ielens (1999) CO(1-0), 12 CO(2-1), 12 CO(3-2), 12 CO(4-3) 13 CO(1-0), 13 CO(2-1)... C( 3 P 1-3 P 0 ), C( 3 P 2-3 P 1 ) CO lines : transitions between two rotationnal levels ex: CO(3-2) transition from level J = 3 to J = 2 C lines : transitions between two electronical levels ex: C( 3 P 1-3 P 0 ) transitions from level 3 P 1 to 3 P 0 CII & OI emission lines from literature (ISO, KAO ) Observations and study of high-j CO lines ( 12 CO(6-5) et (7-6)) = signature of warm and dense molecular gas (n(h 2 ) ~10 4 cm -3, T k ~ K)
14
HerCULES Herschel Comprehensive (U)LIRG Emission Survey
HerCULES Herschel Comprehensive (U)LIRG Emission Survey Paul van der Werf Leiden Observatory ESAC December 17, 2008 Credits! Data processing: Trevor Fulton Kate Isaak Adam Rykala Modeling: Rowin Meijerink
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:
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
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
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
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 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
Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies. João Alves, University of Vienna
Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies João Alves, University of Vienna Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies With: Charles
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,
arxiv:1010.0788v1 [astro-ph.co] 5 Oct 2010
![arxiv:1010.0788v1 [astro-ph.co] 5 Oct 2010](/thumbs/40/21178799.jpg "arxiv:1010.0788v1 [astro-ph.co] 5 Oct 2010")
Astronomy & Astrophysics manuscript no. ms c ESO 2010 October 6, 2010 Star Formation in Extreme Environments: The Effects of Cosmic Rays and Mechanical Heating. R. Meijerink 1, M. Spaans 2, A.F. Loenen
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;
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
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
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
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
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/
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
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,
8 Radiative Cooling and Heating
8 Radiative Cooling and Heating Reading: Katz et al. 1996, ApJ Supp, 105, 19, section 3 Thoul & Weinberg, 1995, ApJ, 442, 480 Optional reading: Thoul & Weinberg, 1996, ApJ, 465, 608 Weinberg et al., 1997,
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
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
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
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
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,
Pdr Reflection of the FUV radiation field
Properties of the Molecular Gas in Low Metallicity Environments Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch Naturwissenschaftlichen Fakultät der Rheinischen Friedrich Wilhelms
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)
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
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
Heating & Cooling in the Interstellar Medium
Section 7 Heating & Cooling in the Interstellar Medium 7.1 Heating In general terms, we can imagine two categories of heating processes in the diuse ISM: 1 large-scale (mechanical, e.g., cloud-cloud collisions),
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:
The effect of violent star formation on the state of the molecular gas in M 82
A&A 365, 571 587 (2001) DOI: 10.1051/0004-6361:20000145 c ESO 2001 Astronomy & Astrophysics The effect of violent star formation on the state of the molecular gas in M 82 A. Weiß 1,N.Neininger 1,S.Hüttemeister
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
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
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
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,
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
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
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
Observations of DCO + : Tracing the abundance of CO and N 2 in prestellar. cores. Laurent Pagani LERMA, UMR8112 du CNRS, Observatoire de Paris
Observations of DCO + : Laurent Pagani LERMA, UMR8112 du CNRS, Observatoire de Paris Tracing the abundance of CO and N 2 in prestellar L183 - Spitzer/IRAC4-8 µm cores with the contribution of A. Bourgoin
Herschel far- infrared surveys of nearby galaxy clusters Jon Davies and the HeViCS team. Scan maps at: 100μm 160μm 250μm 350μm 500μm
Herschel far- infrared surveys of nearby galaxy clusters Jon Davies and the HeViCS team Scan maps at: 100μm 160μm 250μm 350μm 500μm HeViCS consor-um Members Davies, J. I.; Baes, M.; Bendo, G. J.; Bianchi,
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:
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"
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
Seasonal & Daily Temperatures. Seasons & Sun's Distance. Solstice & Equinox. Seasons & Solar Intensity
Seasonal & Daily Temperatures Seasons & Sun's Distance The role of Earth's tilt, revolution, & rotation in causing spatial, seasonal, & daily temperature variations Please read Chapter 3 in Ahrens Figure
Atmospheric Stability & Cloud Development
Atmospheric Stability & Cloud Development Stable situations a small change is resisted and the system returns to its previous state Neutral situations a small change is neither resisted nor enlarged Unstable
How Do Galeries Form?
8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-1 8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-2 Galaxy Formation Leading questions for today How do
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
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:
How To Understand The Origin Of Star Formation
Resultados Concurso Apex 2013-B Propuesta: 2013B-05 Investigador Principal: Mónica Rubio, Universidad de Chile Título: Dust, Molecules, and Star Formation at Low Metallicity Resumen: Dust affects the cooling
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
1. Introduction 2. The H 2 Molecule 3. The CO Molecule 4. Summary. 1. Introduction
Lecture 19. The H 2 and CO Molecules 1. Introduction 2. The H 2 Molecule 3. The CO Molecule 4. Summary References Stahler & Palla, The Formation of Stars, Secs. 5.2-3 Shull & Beckwith, ARAA 20 163 1982
Changing Clouds in a Changing Climate: Anthropogenic Influences
Changing Clouds in a Changing Climate: Anthropogenic Influences Joel Norris Assistant Professor of Climate and Atmospheric Sciences Scripps Institution of Oceanography Global mean radiative forcing of
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
UNIT 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
7613-1 - Page 1. Weather Unit Exam Pre-Test Questions
Weather Unit Exam Pre-Test Questions 7613-1 - Page 1 Name: 1) Equal quantities of water are placed in four uncovered containers with different shapes and left on a table at room temperature. From which
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;
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
5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
National Aeronautics and Space Administration. Teacher s. Science Background. GalaxY Q&As
National Aeronautics and Space Administration Science Background Teacher s GalaxY Q&As 1. What is a galaxy? A galaxy is an enormous collection of a few million to several trillion stars, gas, and dust
New Discoveries in Galaxies across Cosmic Time through Advances in Laboratory Astrophysics. Submitted by the
New Discoveries in Galaxies across Cosmic Time through Advances in Laboratory Astrophysics Submitted by the American Astronomical Society Working Group on Laboratory Astrophysics http://www.aas.org/labastro/
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
TRANSITING EXOPLANETS
TRANSITING EXOPLANETS Introduction 11 Chapter 1 Our Solar System from afar 13 Introduction 13 1.1 Direct imaging 20 1.1.1 Coronagraphy 24 1.1.2 Angular difference imaging 25 1.2 Astrometry 26 1.3 Radial
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
8.5 Comparing Canadian Climates (Lab)
These 3 climate graphs and tables of data show average temperatures and precipitation for each month in Victoria, Winnipeg and Whitehorse: Figure 1.1 Month J F M A M J J A S O N D Year Precipitation 139
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
Chapter 6 Atmospheric Aerosol and Cloud Processes Spring 2015 Cloud Physics Initiation and development of cloud droplets Special interest: Explain how droplet formation results in rain in approximately
Solar System science with the IRAM interferometer. Recent Solar System science with the IRAM Plateau de Bure interferometer
Recent Solar System science with the IRAM Plateau de Bure interferometer J. Boissier (Institut de radioastronomie millimétrique) Contact: boissier@iram.fr Outline Planet moons Io Titan Planets Mars Comets
How To Understand The Physics Of Electromagnetic Radiation
Ay 122 - Fall 2004 Electromagnetic Radiation And Its Interactions With Matter (This version has many of the figures missing, in order to keep the pdf file reasonably small) Radiation Processes: An Overview
How does snow melt? Principles of snow melt. Energy balance. GEO4430 snow hydrology 21.03.2006. Energy flux onto a unit surface:
Principles of snow melt How does snow melt? We need energy to melt snow/ ice. GEO443 snow hydrology 21.3.26 E = m L h we s K = ρ h = w w we f E ρ L L f f Thomas V. Schuler t.v.schuler@geo.uio.no E energy
Intermediate-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
Light as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
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,
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
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
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
TOPIC 5 (cont.) RADIATION LAWS - Part 2
TOPIC 5 (cont.) RADIATION LAWS - Part 2 Quick review ELECTROMAGNETIC SPECTRUM Our focus in this class is on: UV VIS lr = micrometers (aka microns) = nanometers (also commonly used) Q1. The first thing
AGN-driven winds and ionized clouds moving along the jet in PKS 0521-365
GH 2015: Forming and Fueling Supermassive Black Hole Seeds July 6-24, 2015, Tonantzintla, Puebla AGN-driven winds and ionized clouds moving along the jet in PKS 0521-365 Eric Faustino Jiménez-Andrade ericja@inaoep.mx
FIRST CO J =6Y5 AND J =4Y3 DETECTIONS IN LOCAL ULIRGs: THE DENSE GAS IN MARKARIAN 231 AND ITS COOLING BUDGET
The Astrophysical Journal, 668:815Y825, 2007 October 20 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. A FIRST CO J =6Y5 AND J =4Y3 DETECTIONS IN LOCAL ULIRGs: THE DENSE
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
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
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
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,
Titan: The Solar System s Abiotic Petroleum Factory
Titan: The Solar System s Abiotic Petroleum Factory J. Hunter Waite, Ph.D. Institute Scientist Space Science & Engineering Division Southwest Research Institute Titan: The Solar System s Abiotic Petroleum
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
Solar Nebula Theory. Basic properties of the Solar System that need to be explained:
Solar Nebula Theory Basic properties of the Solar System that need to be explained: 1. All planets orbit the Sun in the same direction as the Sun s rotation 2. All planetary orbits are confined to the
Solar Flux and Flux Density. Lecture 3: Global Energy Cycle. Solar Energy Incident On the Earth. Solar Flux Density Reaching Earth
Lecture 3: Global Energy Cycle Solar Flux and Flux Density Planetary energy balance Greenhouse Effect Vertical energy balance Latitudinal energy balance Seasonal and diurnal cycles Solar Luminosity (L)
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
F321 THE STRUCTURE OF ATOMS. ATOMS Atoms consist of a number of fundamental particles, the most important are... in the nucleus of an atom
Atomic Structure F32 TE STRUCTURE OF ATOMS ATOMS Atoms consist of a number of fundamental particles, the most important are... Mass / kg Charge / C Relative mass Relative Charge PROTON NEUTRON ELECTRON
Proceedings of the NATIONAL ACADEMY OF SCIENCES
Proceedings of the NATIONAL ACADEMY OF SCIENCES Volume 55 * Number 1 * January 15, 1966 DYNAMICS OF SPHERICAL GALAXIES, II* BY PHILIP M. CAMPBELL LAWRENCE RADIATION LABORATORY, LIVERMORE, CALIFORNIA Communicated
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
Calibration of Dallas sensors
Calibration of Dallas sensors Mariusz Sapinski INFN Sezione di Roma1 Roma, Italy (April 2006) 1. Objectives The goal of this work is to perform a calibration of Dallas sensors. Nine Dallas sensors are
RESULTS FROM A SIMPLE INFRARED CLOUD DETECTOR
RESULTS FROM A SIMPLE INFRARED CLOUD DETECTOR A. Maghrabi 1 and R. Clay 2 1 Institute of Astronomical and Geophysical Research, King Abdulaziz City For Science and Technology, P.O. Box 6086 Riyadh 11442,
MCQ - ENERGY and CLIMATE
1 MCQ - ENERGY and CLIMATE 1. The volume of a given mass of water at a temperature of T 1 is V 1. The volume increases to V 2 at temperature T 2. The coefficient of volume expansion of water may be calculated
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
Astro 301/ Fall 2005 (48310) Introduction to Astronomy
Astro 301/ Fall 2005 (48310) Introduction to Astronomy Instructor: Professor Shardha Jogee TAs: David Fisher, Donghui Jeong, and Miranda Nordhaus Lecture 22 = Tu Nov 15 Lecture 23 = Th Nov 17 http://www.as.utexas.edu/~sj/a301-fa05/
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
Clouds. Ulrike Lohmann Department of Physics and Atmospheric Science, Dalhousie University, Halifax, N. S., Canada
Clouds Ulrike Lohmann Department of Physics and Atmospheric Science, Dalhousie University, Halifax, N. S., Canada Outline of this Lecture Overview of clouds Warm cloud formation Precipitation formation
Fog and Cloud Development. Bows and Flows of Angel Hair
Fog and Cloud Development Bows and Flows of Angel Hair 1 Ch. 5: Condensation Achieving Saturation Evaporation Cooling of Air Adiabatic and Diabatic Processes Lapse Rates Condensation Condensation Nuclei
Correlation of the Mass Spectrometric Analysis of Heat-Treated Glutaraldehyde Preparations to Their 235nm / 280 nm UV Absorbance Ratio
an ABC Laboratories white paper Correlation of the Mass Spectrometric Analysis of Heat-Treated Glutaraldehyde Preparations to Their 235nm / 280 nm UV Absorbance Ratio A. Sen, R. Dunphy, L. Rosik Analytical