Modelling clumpy! galactic disks

Save this PDF as:
 WORD  PNG  TXT  JPG

Size: px
Start display at page:

Download "Modelling clumpy! galactic disks"

Transcription

1 Modelling clumpy! galactic disks Simone Bianchi INAF-Osservatorio Astrofisico di Arcetri, Firenze with TRADING! Transfer of RAdiation through Dust IN Galaxies (Bianchi 2008)

2 Radiative Transfer models" for a spiral (disk) galaxy Smooth exponential stellar disk + spheroidal bulge i = 90 i = 85 + smooth exponential dust disk MC model for dust extinction" Bianchi, Ferrara & Giovanardi (1996)

3 Real galaxies vs models" (Kylafis & Bahcall 1984; Xilouris et al. 1997,1998,1999; " Baes et al. 2010; de Looze et al. 2012; De Geyter et al. 2013) V band NGC other objects Bianchi (2007) model K band model

4 From dust absorption to dust emission NGC 6946 (Bianchi et al. 2000) Stellar SED Absorbed energy -> Temperature map -> Dust emission Dust emission SED Dust emission is typically 30% of the Bolometric Luminosity (Popescu & Tuffs 2002; Davies et al. 2012) high τ V is needed for the energy balance Energy balance problem confirmed in may spirals (Popescu et al. 2000; Baes et al. 2010; de Looze et al 2012)

5 Clumping of dust: a solution? (Bianchi et al. 1999; Misiriotis & Bianchi 2002) I obs / I o (V Band) Clumpy disks are more transparent Clumps as MW molecular clouds A grid is required! 75% of dust in clumps What if the heating source is within a cloud? Homogeneous Radial Profile of an Edge-On Disk (τ V =2)

6 TRADING features Continuum RT in a dusty medium Monte Carlo code An adaptive grid for dust Stellar emission from diffuse/point-like sources of different spectra Thermal & stochastic dust emission from a distribution of grain sizes and material (Draine & Li 2007) Dust self-absorption.

7 RT and the Monte Carlo Method (details on Steinacker, Baes & Gordon 2013) The path of a phothon through dust Emission from stars Extinction: scattering or absorption? Out of dust: observed Several images

8 RT and the Monte Carlo Method (details on Steinacker, Baes & Gordon 2013) The path of a phothon through dust Extinction: scattering and absorption! Optimizations Photon weights Forced Scattering (Cashwell & Everett 1959) Peeling-off (Yusef-Zadeh et al. 1984) Continuous Absorption (Lucy 1999)

9 RT and the Monte Carlo Method (details on Steinacker, Baes & Gordon 2013) Emission from dust Local ISRF J λ = W λ /(4π κ λ ) j λ Dust Emission Coefficient Thermal & Stochastic heating Absorbed energy Mean absorption coefficient Dust self absorption (iteratively) l.o.s. integration Scheme similar to other MCs (DIRTY, Misselt et al. 2001; SKIRT, Baes et al. 2011)

10 TRADING: an adaptive grid " for a clumpy medium 3-D Tree structure: a regular Octree Finer grid on a denser (more opaque) spot Clumps of different size Resolution within the clump Neighbour cells found with the bookkeeping method (as defined by Saft et al. 2013) GMC: D 100 pc Disk: D 20 kpc

11 Model of an NGC891-like galaxy! seen at i=86 (Bianchi 2008) B, V, R B, V, R 70µm, 160µm, 850µm

12 Modelling NGC891! Bianchi 2008; Bianchi & Xilouris 2011 Is the model consistent with optical-nir images? Galaxy parameters from optical fits of Xilouris et al. (1999) Add enough dust to match thermal SED Model in K-band 2-MASS Ks-band Is the model consistent with FIR/submm maps? Herschel-SPIRE

13 Modelling NGC4244! Holwerda et al SPIRE SPIRE 250 & 500um Galaxy parameters from optical fits of MacLachlan et al. (2012) SDSS-r & IRAC 3.6um

14 The ISRF around NGC891! Bocchio et al Optical SED at R=12 kpc for z=0, 2, 5, 10, 15, 20 kpc compared to the LISRF (Mathis et al. 1983) Strength of the ISRF on a galactic meridian plane. Red contours refer to an ISRF 10, 1 and 0.1x the LISRF.

15 The dust model TRADING works with a distribution of grain sizes and materials Draine & Li (2007) model 4 materials and a total of 50 grains Thermal emission for a 0.01 μm Stochastic emission for smaller grains Method of Guhathakurta & Draine (1989) N=80 temperature bins

16 Not only disks! Optical: dust extinction FIR: dust emission

17 The spectral energy distribution of z 6 quasars: the case of SDSS J Schneider et al, submitted

18 Ivezic et al Checking the code Pascucci et al. 2004

19 Galactic disk geometry Benchmarking TRADING with SKIRT (+ DIRTY & CRT not shown) TRADING τ 1µm =1 τ 1µm = TRADING - SKIRT

20 TRADING features Continuum RT in a dusty medium Monte Carlo code An adaptive grid for dust Stellar emission from diffuse/point-like sources of different spectra Thermal & stochastic dust emission from a distribution of grain sizes and material (Draine & Li 2007) Dust self-absorption.

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 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,

More information

Modeling Galaxy Formation

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

More information

The Evolution of GMCs in Global Galaxy Simulations

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

More information

Faber-Jackson relation: Fundamental Plane: Faber-Jackson Relation

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

More information

IV. Molecular Clouds. 1. Molecular Cloud Spectra

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:

More information

Ellipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0

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,

More information

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.

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

More information

MCRT: L6. Initial weight of packet: W = L / N MC At each interaction multiply weight by probability of scattering: W = a W

MCRT: L6. Initial weight of packet: W = L / N MC At each interaction multiply weight by probability of scattering: W = a W MCRT: L6 Variance reduction techniques improve signal-to-noise of simulation using same number of MC packets Examples of where MCRT is inefficient optically thin (need lots of photons) Weights keep packet

More information

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 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;

More information

Resultados Concurso Apex 2007

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

More information

Astronomy. Astrophysics. HERschel Observations of Edge-on Spirals (HEROES) I. Far-infrared morphology and dust mass determination

Astronomy. Astrophysics. HERschel Observations of Edge-on Spirals (HEROES) I. Far-infrared morphology and dust mass determination A&A 556, A54 (213) DOI: 1.151/4-6361/2122733 c ESO 213 Astronomy & Astrophysics HERschel Observations of Edge-on Spirals (HEROES) I. Far-infrared morphology and dust mass determination J. Verstappen 1,

More information

Chapter 19 Star Formation

Chapter 19 Star Formation Chapter 19 Star Formation 19.1 Star-Forming Regions Units of Chapter 19 Competition in Star Formation 19.2 The Formation of Stars Like the Sun 19.3 Stars of Other Masses 19.4 Observations of Cloud Fragments

More information

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 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/

More information

Let s consider a homogeneous medium characterized by the extinction coefficient β ext, single scattering albedo ω 0 and phase function P(µ, µ').

Let s consider a homogeneous medium characterized by the extinction coefficient β ext, single scattering albedo ω 0 and phase function P(µ, µ'). Lecture 22. Methods for solving the radiative transfer equation with multiple scattering. Part 4: Monte Carlo method. Radiative transfer methods for inhomogeneous ouds. Objectives: 1. Monte Carlo method.

More information

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. 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,

More information

Chapter 15.3 Galaxy Evolution

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

More information

Class #14/15 14/16 October 2008

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 information

Milky Way & Hubble Law

Milky Way & Hubble Law Milky Way & Hubble Law Astronomy 1 Elementary Astronomy LA Mission College Spring F2015 Quotes & Cartoon of the Day Happy Thanksgiving! Announcements 3rd midterm 12/3 I will drop the lowest midterm grade

More information

8.1 Radio Emission from Solar System objects

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

More information

Using the Amazon Compute Cloud to Analyze Large Data Sets

Using the Amazon Compute Cloud to Analyze Large Data Sets Using the Amazon Compute Cloud to Analyze Large Data Sets The Panchromatic Hubble Andromeda Treasury Benjamin F. Williams University of Washington Movie by Anil Seth Ben Williams March 11, 2015 Hubble

More information

Chapter 5 Light and Matter: Reading Messages from the Cosmos

Chapter 5 Light and Matter: Reading Messages from the Cosmos Chapter 5 Light and Matter: Reading Messages from the Cosmos Messages Interactions of Light and Matter The interactions determine everything we see, including what we observe in the Universe. What is light?

More information

Rough subdivision. Characteristic values for E s (Schneider 2006). Elliptical galaxies. Elliptical galaxies

Rough subdivision. Characteristic values for E s (Schneider 2006). Elliptical galaxies. Elliptical galaxies Rough subdivision Normal ellipticals. Giant ellipticals (ge s), intermediate luminosity (E s), and compact ellipticals (ce s), covering a range of luminosities from M B 23 m to M B 15 m. Dwarf ellipticals

More information

Powerful Molecular Outflows in Nearby Active Galaxies

Powerful Molecular Outflows in Nearby Active Galaxies Powerful Molecular Outflows in Nearby Active Galaxies S. Veilleux (U. Maryland) NGC 253 12CO 1-0 (ALMA Cycle 0) M 82 H2 2.12 µm η = dm/dt / SFR ~1 kpc H2: SV, Rupke, & Swaters (2009) CO: Walter, Weiss,

More information

The Interstellar Medium Astronomy 216 Spring 2005

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

More information

2 Absorbing Solar Energy

2 Absorbing Solar Energy 2 Absorbing Solar Energy 2.1 Air Mass and the Solar Spectrum Now that we have introduced the solar cell, it is time to introduce the source of the energy the sun. The sun has many properties that could

More information

Origins of the Cosmos Summer 2016. Pre-course assessment

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

More information

Heating & Cooling in Molecular Clouds

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

More information

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 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

More information

COMPARISON OF GAS AND DUST COOLING RATES IN NEARBY GALAXIES

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

More information

S0 galaxy NGC 2787. Marcella Carollo, HST.

S0 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 information

Observing the Universe

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

More information

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. 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

Solar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation

Solar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation Outline MAE 493R/593V- Renewable Energy Devices Solar Energy Electromagnetic wave Solar spectrum Solar global radiation Solar thermal energy Solar thermal collectors Solar thermal power plants Photovoltaics

More information

Protobinaries. von Cornelia Weber, Bakk.rer.nat. Donnerstag, 23. Mai 13

Protobinaries. von Cornelia Weber, Bakk.rer.nat. Donnerstag, 23. Mai 13 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

More information

165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars

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

More information

Using Photometric Data to Derive an HR Diagram for a Star Cluster

Using 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 information

Measuring Optical and Thermal Properties of High Temperature Receivers

Measuring Optical and Thermal Properties of High Temperature Receivers www.dlr.de Folie 1 Measuring Optical and Thermal Properties of High Temperature Receivers Johannes Pernpeintner, Thomas Fend 4 th SFERA Summerschool, May 15-16, 2013, Burg Hornberg www.dlr.de Folie 2 Part

More information

Part III. PhD course originally developed by René Liseau Updated to Master level course by Alexis Brandeker

Part III. PhD course originally developed by René Liseau Updated to Master level course by Alexis Brandeker Part III Early stages in stellar tll evolution PhD ii ll d l db R éli PhD course originally developed by René Liseau Updated to Master level course by Alexis Brandeker Part III Early stages in stellar

More information

Resultados Concurso Apex 2014-A

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

More information

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) 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

More information

Exploring Multiwavelength AGN Variability with Swift Archival Data

Exploring Multiwavelength AGN Variability with Swift Archival Data Exploring Multiwavelength AGN Variability with Swift Archival Data, a Caryl Gronwall, b Dirk Grupe, c Dan Vanden Berk d and Jian Wu e a Spectral Sciences Inc., 4 Fourth Ave., Burlington MA 01803, USA b

More information

Solar Ast ro p h y s ics

Solar 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 information

Astro 130, Fall 2011, Homework, Chapter 17, Due Sep 29, 2011 Name: Date:

Astro 130, Fall 2011, Homework, Chapter 17, Due Sep 29, 2011 Name: Date: Astro 130, Fall 2011, Homework, Chapter 17, Due Sep 29, 2011 Name: Date: 1. If stellar parallax can be measured to a precision of about 0.01 arcsec using telescopes on Earth to observe stars, to what distance

More information

Invisible Galaxies. University of Nebraska, October Beth Willman (Haverford College)

Invisible Galaxies. University of Nebraska, October Beth Willman (Haverford College) Invisible Galaxies University of Nebraska, October 2013 Beth Willman (Haverford College) Invisible Galaxies Finding and studying invisible galaxies The connection with dark matter Contributions of Haverford

More information

Dinamica del Gas nelle Galassie II. Star formation

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

More information

7. In which part of the electromagnetic spectrum are molecules most easily detected? A. visible light B. radio waves C. X rays D.

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

More information

Starbursts In Ultraluminous Infrared Galaxies - Fueling And Properties

Starbursts In Ultraluminous Infrared Galaxies - Fueling And Properties Starbursts In Ultraluminous Infrared Galaxies - Fueling And Properties Paul P. van der Werf Leiden Observatory, P.O. Box 9513, NL 2300 RA Leiden, The Netherlands arxiv:astro-ph/0101185v1 11 Jan 2001 Abstract.

More information

Resultados Concurso Apex 2013-B

Resultados Concurso Apex 2013-B 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

More information

Populations and Components of the Milky Way

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

More information

Detection and characterisation of the first Planck high-z candidates

Detection and characterisation of the first Planck high-z candidates Detection and characterisation of the first Planck high-z candidates Inés Flores-Cacho (IRAP - CNRS/Université de Toulouse) on behalf of the Planck Collaboration Acknowledgements The scientific results

More information

Improved predictive modeling of white LEDs with accurate luminescence simulation and practical inputs

Improved predictive modeling of white LEDs with accurate luminescence simulation and practical inputs Improved predictive modeling of white LEDs with accurate luminescence simulation and practical inputs TracePro Opto-Mechanical Design Software s Fluorescence Property Utility TracePro s Fluorescence Property

More information

The Unique, Optically-Dominated Quasar Jet of PKS 1421-490

The Unique, Optically-Dominated Quasar Jet of PKS 1421-490 The Unique, Optically-Dominated Quasar Jet of PKS 1421-490 J.M. Gelbord & H.L. Marshall (MIT) D.M. Worrall & M. Birkinshaw (U. Bristol) J.E.J. Lovell, R. Ojha, L. Godfrey & D.L. Jauncey (CSIRO) D.A. Schwartz

More information

Light. Light. Overview. In-class activity. What are waves? In this section: PSC 203. What is it? Your thoughts?

Light. Light. Overview. In-class activity. What are waves? In this section: PSC 203. What is it? Your thoughts? Light PSC 203 Overview In this section: What is light? What is the EM Spectrum? How is light created? What can we learn from light? In-class activity Discuss your answers in groups of 2 Think of as many

More information

Giant Molecular Clouds

Giant Molecular Clouds Giant Molecular Clouds http://www.astro.ncu.edu.tw/irlab/projects/project.htm Galactic Open Clusters Galactic Structure GMCs The Solar System and its Place in the Galaxy In Encyclopedia of the Solar System

More information

Ay 122 - Fall 2004 Electromagnetic Radiation And Its Interactions With Matter

Ay 122 - Fall 2004 Electromagnetic Radiation And Its Interactions With Matter 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

More information

From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation?

From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation? From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation? From lowest energy to highest energy, which of the following correctly

More information

Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies

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,

More information

Elliptical Galaxies. Old view: ellipticals are boring, simple systems

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,

More information

Corso di Fisica Te T cnica Ambientale Solar Radiation

Corso di Fisica Te T cnica Ambientale Solar Radiation Solar Radiation Solar radiation i The Sun The Sun is the primary natural energy source for our planet. It has a diameter D = 1.39x10 6 km and a mass M = 1.989x10 30 kg and it is constituted by 1/3 of He

More information

THE NATURE OF INFRARED EMISSION IN THE LOCAL GROUP DWARF GALAXY NGC 6822 AS REVEALED BY SPITZER

THE NATURE OF INFRARED EMISSION IN THE LOCAL GROUP DWARF GALAXY NGC 6822 AS REVEALED BY SPITZER The Astrophysical Journal, 652:1170Y1187, 2006 December 1 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE NATURE OF INFRARED EMISSION IN THE LOCAL GROUP DWARF GALAXY

More information

The CGM around Dwarf Galaxies

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

More information

Ultraluminous ellipticals revealed from IR SEDs (PEGASE.3)

Ultraluminous ellipticals revealed from IR SEDs (PEGASE.3) Ultraluminous ellipticals revealed from IR SEDs (PEGASE.3) B. Rocca-Volmerange, Institut d Astrophysique de Paris Université Paris-Sud With the collaboration of N. Seymour, V. de Lapparent, M. Fioc Modeling

More information

Treasure Hunt. Lecture 2 How does Light Interact with the Environment? EMR Principles and Properties. EMR and Remote Sensing

Treasure Hunt. Lecture 2 How does Light Interact with the Environment? EMR Principles and Properties. EMR and Remote Sensing Lecture 2 How does Light Interact with the Environment? Treasure Hunt Find and scan all 11 QR codes Choose one to watch / read in detail Post the key points as a reaction to http://www.scoop.it/t/env202-502-w2

More information

Name Class Date. spectrum. White is not a color, but is a combination of all colors. Black is not a color; it is the absence of all light.

Name Class Date. spectrum. White is not a color, but is a combination of all colors. Black is not a color; it is the absence of all light. Exercises 28.1 The Spectrum (pages 555 556) 1. Isaac Newton was the first person to do a systematic study of color. 2. Circle the letter of each statement that is true about Newton s study of color. a.

More information

arxiv:astro-ph/0108367v1 22 Aug 2001

arxiv:astro-ph/0108367v1 22 Aug 2001 RE-SUBMITTED TO APJ: 22 AUGUST 2001 Preprint typeset using L A TEX style emulateapj v. 26/01/00 THE EFFECTS OF DUST IN SIMPLE ENVIRONMENTS: LARGE MAGELLANIC CLOUD H II REGIONS ERIC F. BELL, KARL D. GORDON,

More information

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 João Alves, University of Vienna Schmidt s Conjecture and Star Formation in Giant Molecular Clouds and Galaxies With: Charles

More information

Electromagnetic Radiation (EMR) and Remote Sensing

Electromagnetic Radiation (EMR) and Remote Sensing Electromagnetic Radiation (EMR) and Remote Sensing 1 Atmosphere Anything missing in between? Electromagnetic Radiation (EMR) is radiated by atomic particles at the source (the Sun), propagates through

More information

Overview. What is EMR? Electromagnetic Radiation (EMR) LA502 Special Studies Remote Sensing

Overview. What is EMR? Electromagnetic Radiation (EMR) LA502 Special Studies Remote Sensing LA502 Special Studies Remote Sensing Electromagnetic Radiation (EMR) Dr. Ragab Khalil Department of Landscape Architecture Faculty of Environmental Design King AbdulAziz University Room 103 Overview What

More information

12-3. Spherical groups of millions of stars found in the Milky Way are called: a) novas b) globular clusters X c) open clusters d) galactic clusters

12-3. Spherical groups of millions of stars found in the Milky Way are called: a) novas b) globular clusters X c) open clusters d) galactic clusters Chapter 12 Quiz, Nov. 28, 2012, Astro 162, Section 4 12-1. Where in our Galaxy has a supermassive (or galactic) black hole been observed? a) at the outer edge of the nuclear bulge b) in the nucleus X c)

More information

3D 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 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 information

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 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 information

Total radiative heating/cooling rates.

Total radiative heating/cooling rates. Lecture. Total radiative heating/cooling rates. Objectives:. Solar heating rates.. Total radiative heating/cooling rates in a cloudy atmosphere.. Total radiative heating/cooling rates in different aerosol-laden

More information

Cosmic Dust in an Expanding Universe?

Cosmic Dust in an Expanding Universe? Planck energy - E - ev Cosmic Dust in an Expanding Universe? QED Radiations, Discovery Bay, Hong Kong, China nanoqed@gmail.com Copyright 2016 Horizon Research Publishing All rights reserved. Abstract Dust

More information

Arjen van der Wel -- MPIA, Heidelberg

Arjen van der Wel -- MPIA, Heidelberg THE PATH FROM COMPACT Z = 2 GALAXY TO GIANT ELLIPTICAL Arjen van der Wel -- MPIA, Heidelberg with the 3D-HST and CANDELS teams THE PATH FROM COMPACT Z = 2 GALAXY TO GIANT ELLIPTICAL The size-mass relation

More information

A Star and Gas Surface Density Correlation within Nearby Molecular Clouds

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

More information

Transition between atomic and molecular hydrogen in the Galaxy: vertical variation of the molecular fraction

Transition between atomic and molecular hydrogen in the Galaxy: vertical variation of the molecular fraction Astron. Astrophys. 319, 1 6 (1997) ASTRONOMY AND ASTROPHYSICS Transition between atomic and molecular hydrogen in the Galaxy: vertical variation of the molecular fraction K. Imamura and Y. Sofue Institute

More information

arxiv:astro-ph/9601169v1 30 Jan 1996

arxiv:astro-ph/9601169v1 30 Jan 1996 THE DISTRIBUTION OF DUST AND GAS IN ELLIPTICAL GALAXIES arxiv:astro-ph/9601169v1 30 Jan 1996 PAUL GOUDFROOIJ European Southern Observatory Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany Abstract.

More information

Class 2 Solar System Characteristics Formation Exosolar Planets

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

More information

The obscured circumnuclear region of the outflow galaxy NGC 3079

The obscured circumnuclear region of the outflow galaxy NGC 3079 Astron. Astrophys. 336, 433 444 (1998) ASTRONOMY AND ASTROPHYSICS The obscured circumnuclear region of the outflow galaxy NGC 3079 F.P. Israel 1, P.P. van der Werf 1, T.G. Hawarden 2, and C. Aspin 2,3

More information

The Size & Shape of the Galaxy

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

More information

Magellanic 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 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 information

Biomedical Optics Theory

Biomedical Optics Theory Introduction Biomedical Optics Theory Diffuse reflectance spectroscopy (DRS) and Laser Doppler Flowmetry (LDF) are booth optical techniques that can quantify a number of microcirculatory parameters. Prof

More information

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 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,

More information

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 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

More information

Convec,on, cloud and radia,on

Convec,on, cloud and radia,on Convec,on, cloud and radia,on Convection redistributes the thermal energy yielding (globally-averaged), a mean lapse rate of ~ -6.5 o C/km. Radiative processes tend to produce a more negative temperature

More information

Elliptical Galaxies. Galaxies and Their Properties, Part II: Fine Structure in E-Galaxies: A Signature of Recent Merging

Elliptical Galaxies. Galaxies and Their Properties, Part II: Fine Structure in E-Galaxies: A Signature of Recent Merging Elliptical Galaxies Ay 21 - Lecture 12 Galaxies and Their Properties, Part II: Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals

More information

VARIANCE REDUCTION TECHNIQUES FOR IMPLICIT MONTE CARLO SIMULATIONS

VARIANCE REDUCTION TECHNIQUES FOR IMPLICIT MONTE CARLO SIMULATIONS VARIANCE REDUCTION TECHNIQUES FOR IMPLICIT MONTE CARLO SIMULATIONS An Undergraduate Research Scholars Thesis by JACOB TAYLOR LANDMAN Submitted to Honors and Undergraduate Research Texas A&M University

More information

FIRST LIGHT IN THE UNIVERSE

FIRST LIGHT IN THE UNIVERSE FIRST LIGHT IN THE UNIVERSE Richard Ellis, Caltech 1. Role of Observations in Cosmology & Galaxy Formation 2. Galaxies & the Hubble Sequence 3. Cosmic Star Formation Histories 4. Stellar Mass Assembly

More information

lecture 10. The Milky Way s Interstellar Medium Birgitta Nordström, Copenhagen, & Gerhard Hensler, Vienna

lecture 10. The Milky Way s Interstellar Medium Birgitta Nordström, Copenhagen, & Gerhard Hensler, Vienna IX. The Milky Way gas distribution lecture 10. The Milky Way s Interstellar Medium Birgitta Nordström, Copenhagen, & Gerhard Hensler, Vienna 1 2 1 1. HI Gas HI is observed by the 21cm hyperfine-structure

More information

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 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 information

where h = 6.62 10-34 J s

where h = 6.62 10-34 J s Electromagnetic Spectrum: Refer to Figure 12.1 Molecular Spectroscopy: Absorption of electromagnetic radiation: The absorptions and emissions of electromagnetic radiation are related molecular-level phenomena

More information

Finding High Quality Young Star Candidates in Ceph C using X-ray, Optical, and IR data

Finding High Quality Young Star Candidates in Ceph C using X-ray, Optical, and IR data Finding High Quality Young Star Candidates in Ceph C using X-ray, Optical, and IR data Mentor Teacher: Laura Orr, Ukiah School, Ukiah, OR Alexandra Miller, Milken Community Schools, Los Angeles, CA Milton

More information

Galaxy Classification and Evolution

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

More information

Galaxy Formation. Leading questions for today How do visible galaxies form inside halos? Why do galaxies/halos merge so easily?

Galaxy Formation. Leading questions for today How do visible galaxies form inside halos? Why do galaxies/halos merge so easily? 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

More information

Brief ideas for a long discussion

Brief ideas for a long discussion Brief ideas for a long discussion 1. Disk formation/survival in mergers 2. Bulgeless galaxies 3. Global z~2 to z~0 evolution 4. Interface between Cold flows / Disks / Outflows 5. Emergence of a bimodality

More information

A Preliminary Summary of The VLA Sky Survey

A 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 information

8001782 Owner s Manual

8001782 Owner s Manual 8001782 Digital Infrared Thermometer Owner s Manual Introduction This instrument is a portable, easy to use compact-size digital thermometer with laser sighting designed for one hand operation. The meter

More information

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 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 information

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 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

More information

The First Stars and Evolution of the Early Universe Seattle July 3 7 2006. Raffaella Schneider. INAF/OAArcetri

The First Stars and Evolution of the Early Universe Seattle July 3 7 2006. Raffaella Schneider. INAF/OAArcetri The First Stars and Evolution of the Early Universe Seattle July 3 7 2006 Star Formation with the First Dust Raffaella Schneider INAF/OAArcetri Collaborators Simone Bianchi INAF/ Benedetta Ciardi MPA Andrea

More information