Watching the Interstellar Medium Move. Alyssa A. Goodman Harvard University

Size: px
Start display at page:

Download "Watching the Interstellar Medium Move. Alyssa A. Goodman Harvard University"

Transcription

1 Watching the Interstellar Medium Move Alyssa A. Goodman Harvard University

2 Bart Bok and the Dark Nebulae They are no good, and only a damn fool would be bothered by such a thing. A sensible person does not get involved with the dark nebulae but steers to the clear parts in between. --Pieter van Rhijn, Bok s Thesis Advisor (commenting on Bok s book, The Distribution of Stars in Space, in 1937)

3 Taurus Dark Cloud Complex Optical Image

4 3 pc Taurus Dark Cloud Complex 100 µm ISSA image

5 Taurus: Star Counting 6 Arce & Goodman Star counting 4 A V [mag] Declination [deg, 1950]

6 Taurus: Star Counting, Color Excess of Stars 6 Arce & Goodman Star counting Stars with spectral classification 4 A V [mag] Declination [deg, 1950]

7 Taurus: All Methods of Measuring Extinction 6 Schlegel, Finkbeiner & Davis 1998 Arce & Goodman COBE+ISSA Star counting Stars with spectral classification ISSA in star pixel ISSA (cut width average) Average color excess A V [mag] Declination [deg, 1950]

8 Bart Bok in 1955 With the increased angular resolution to be provided by paraboloid antennas now under construction, and with continued emphasis on the improvement of electronic equipment, 21 cm research promises to provide increasingly useful information on the cloud structure of the interstellar medium. By continuing our efforts to blend optical and radio studies of the interstellar medium into one whole, we have real hope of greatly advancing our knowledge of the interstellar medium in years to come. --Bart Bok, AJ, 60, p. 148.

9 Adding a Third Dimension Spectral Line Observations Loss of 1 dimension Mountain Range No loss of information

10 Dense Cores/ Bok Globules MHD Waves Turbulence Outflows Infall H II Regions SNR Thermal Motions

11 Watching the ISM Move W3: Massive Star-Forming Region velocity information explains magnetic field geometry & star formation Ursa Major: High-Latitude Cloud velocity analysis shows dripping & impact Dense Cores velocity dimension reveals coherence Spectral Correlation Function should lead to better simulations & more

12 W3 13 CO Integrated Intensity Dust Thermal Emission 13 CO Channel Maps -39to-31km/sec -49 to -41 km/sec 4% polarizati on Kannappan & Goodman 1998; Dowell 1998

13 The Origin and Evolution of High-Latitude Clouds Ursa Major HLC Complex Pound & Goodman 1997

14 High-latitude Clouds High-latitude = very nearby (D UMAJ ~100 pc) ~No star formation 1 Energy distribution very different than starforming regions High Latitude Cloud 2 Gravitational << Magnetic n Kinetic Star-Forming Cloud 3 Gravitational n Magnetic n Kinetic (1) Magnani et al. 1996; (2) Myers, Goodman, Güsten & Heiles 1995; (3) Myers & Goodman 1988

15 The Velocity Field in Ursa Major H I CO Pound & Goodman 1997

16 Hat Creek H I Data v and v LSR Gradients Latitude [deg] v Longitude [deg] v LSR

17 In General... v tan v rad y Line width primarily tangential...in Ursa Major v z,obs implication: v tan >> v rad z θ ω Line width primarily radial z θ ω Line width primarily radial v z,obs implication: v tan << v rad Line width primarily tangential -y

18 Confirmation: Position Velocity Diagrams for H I and CO CO H I Position Along Filament 1 CO Blueshifted w.r.t. H I in both filaments, in arc-like pattern Position Along Filament 2

19 y v z,rot v z,rot 2 1 v z,exp z v z,exp 3 4 Observed in Ursa Major v z,obs Red CO blueshifted w.r.t H I Shell Blue

20

21 Implications of Ursa Major Study Many HLC s may be related to supershell structures; some shells harder to identify than NCP Loop. (Commonly observed) velocity offsets between atomic and molecular gas may be due to impacts, followed by conservation of momentum. Use this as a clue in other cases.

22 Dense Cores/Bok Globules MHD Waves Turbulence Outflows Gravitation H II Regions SNR Thermal Motions

23 Bok and his Globules In recent years several authors have drawn attention to the possibility of the formation of stars from condensations in the interstellar medium (Spitzer 1941; Whipple 1946). --Bok & Reilly 1947, ApJ, 105, 255, opening paragraph

24 Bok and his Globules The globules are interesting objects Every one of them merits further careful study with the largest available reflecting telescopes. --Bok & Reilly 1947, ApJ, 105, 255, closing paragraph

25 1990: Bart Bok Was Correct!

26 Rotation Motions Of, In and Around Dense Cloud Cores β~0.04; enough to matter but not to fragment Velocity Coherence Cores as Islands of Calm in a Turbulent Sea Bulk motion Infall: see Ho, Lada, Keto, Myers, Williams, Wilner, Zhang... Outflow: see Arce, Lada, Raymond...

27 Coherent Cores: Islands of Calm in a Turbulent Sea "Rolling Waves" by KanO Tsunenobu The Idemitsu Museum of Arts.

28 Hint #1: Independent Core Rotation Goodman, Benson, Fuller & Myers 1993

29 Hint #2: Constant Line Width in Cores?

30 Types of Line width-size Relations Ensemble of Clouds Type 1: Larson s Law Non-thermal Line Width Tracer 1 Tracer 2 Tracer 3 Tracer 4 Tracer 5 v~r 0.5 FWHM of Various Tracers Shown Observed Size Gives overall state of ISM~magnetic virial equilibrium. See Larson 1981; Myers & Goodman 1988 for examples.

31 Types of Line width-size Relations Type 3: Single Cloud Observed in Multiple Tracers Non-thermal Line Width Observed Size Gives pressure structure of an individual cloud. See Fuller & Myers 1992.

32 Types of Line width-size Relations Type 3: Single Cloud Observed in Multiple Tracers Non-thermal Line Width Density Observed Size

33 Types of Line width-size Relations Type 4: Single Cloud Observed in a Single Tracer Non-thermal Line Width Type 4 Type 4 Observed Size Gives information on power spectrum of velocity fluctuations. See Barranco & Goodman 1998; Goodman, Barranco, Heyer & Wilner 1998.

34 An Example of the (Original) Evidence for Coherence Type 4 Line width- Size Relations "Radius" from Peak [parsecs] "Radius" from Peak [parsecs] TMC-1C, NH 3 (1, 1) v NT =(0.20±0.02)T A -0.11±0.07 v NT [km s -1 ] 5 4 v NT [km s -1 ] TMC-1C, OH 1667 MHz v NT =(0.64±0.05)T A -0.7± T A [K] T A [K] v NT = (1.0 ± 0.2)R 0.27± 0.08 v NT = (0.30 ± 0.09)R 0.12 ±0.08

35 The (Newer) Evidence for Coherence IRAM 30-m C 17 O (1-0) IRAM 30-m C 18 O (2-1) IRAM 30-m C 34 S (2-1) v [km s -1 ] 5 4 v [km s -1 ] 5 4 v [km s -1 ] 5 4 v [km s -1 ] TA [K] 1 FCRAO C 17 O (1-0) 3 Type 4 slope 2 4x10 appears to TA [K] 1 decrease with 9 8 FCRAO C 18 O (1-0) density, 7 as predicted. 6 5 v [km s -1 ] 4 v [km s -1 ] TA [K] FCRAO C 34 S (2-1) x TA [K] TA [K] 0.1 2x TA [K] "Radius" from Peak [pc] "Radius" from Peak [pc] TMC-1C, NH 3 (1, 1) -0.11±0.07 v NT =(0.20±0.02)T A 3 "Radius" from Peak [pc] 6 6 v NT [km s -1 ] 5 4 v NT [km s -1 ] 5 4 v NT [km s -1 ] 3 TMC-1C, OH 1667 MHz -0.7±0.2 v NT =(0.64±0.05)T A T A [K] T A [K] T A [K]

36 Coherent Dense Core ~0.1 pc (in Taurus) "Velocity Coherent" Core "Chaff"...

37 Coherence in Spatial Distribution of Stars R 10 0 o 8 Surface Density of Stellar Companions (Taurus) Size [pc] log Σ c (θ) [stars/sq. deg] 6 4 Coherent Turbulent σ NT [km s -1 ] 2 Parameterized Line Width-Size Relation log θ [deg] Goodman et al Larson 1995; see also Gomez et al. 1993; Simon 1997

38 The Cause of Coherence? Most likely suspect: Loss of magnetic support due to reduced ionization fraction in core. (Scale gives clues.) Interesting question raised: What causes residual non-thermal line width? 3D MHD simulation of Ostriker, Gammie & Stone (in prep.) No ambipolar diffusion yet...

39 Learning More from Too Much Data Product (S/N)*N pixels *N channels N channels S/N N pixels N channels, S/N in 1 hour, N pixels Year

40 The Spectral Correlation Function Figure from Falgarone et al Simulation

41 Goals of SCF Project Develop a sharp tool for statistical analysis of ISM, using as much data of a data cube as possible Compare information from this tool with other tools (e.g CLUMPFIND, GAUSSCLUMPS, ACF, Wavelets), applied to same cubes Use best suite of tools to compare real & simulated ISM Adjust simulations to match, understanding physical inputs

42 How the SCF Works Measures similarity of neighboring spectra within a specified beam size lag & scaling adjustable signal-to-noise equalized See: Rosolowsky, Goodman, Wilner & Williams 1998.

43 A Real Molecular Cloud IRAM Key Project Data

44 Initial Comparisons using the SCF L1512 (Real Cloud) Matching? Turbulence Simulation IRAM Key Project Data Falgarone et al. 1994

45 Initial Comparisons using the SCF L1512 (Real Cloud) Better? MHD Simulation IRAM Key Project Data Gammie, Ostriker & Stone 1998

46 Goals of SCF Project Develop a sharp tool for statistical analysis of ISM, using as much data of a data cube as possible Compare information from this tool with other tools (e.g CLUMPFIND, GAUSSCLUMPS, ACF, Wavelets), applied to same cubes Use best suite of tools to compare real & simulated ISM Adjust simulations to match, understanding physical inputs

47 Watching the ISM Move W3: Massive Star-Forming Region velocity information explains field geometry & star formation Ursa Major: High-Latitude Cloud velocity analysis shows dripping & impact Dense Cores velocity dimension reveals coherence Spectral Correlation Function should lead to better simulations & more

48 Extra slides follow...

49 Optical View of W3 Region

50 Go no further than A V ~1.3 mag P R [%] Arce et al A V [mag] 3 4 Magnetic Fields Background to Cold Dark Cloud Background to General ISM

51 Star and Planet Formation "Cores" and Outflows Giant Molecular Clouds Solar System Formation Jets and Disks

52 The Velocity Field in Ursa Major Pound & Goodman 1997

Where, Exactly, do Stars Form? (and how can SOFIA help with the answer)

Where, Exactly, do Stars Form? (and how can SOFIA help with the answer) Where, Exactly, do Stars Form? (and how can SOFIA help with the answer) Alyssa A. Goodman Harvard University Astronomy Department photo credit: Alves, Lada & Lada On a galactic scale Star Formation=Column

More information

Numerical Simulations of the ISM: What Good are They?

Numerical Simulations of the ISM: What Good are They? Numerical Simulations of the ISM: What Good are They? Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics Principal Collaborators Héctor Arce, CfA Javier Ballesteros-Paredes, AMNH Sungeun Kim,

More information

Lecture 26 Clouds, Clumps and Cores. Review of Molecular Clouds

Lecture 26 Clouds, Clumps and Cores. Review of Molecular Clouds Lecture 26 Clouds, Clumps and Cores 1. Review of Dense Gas Observations 2. Atomic Hydrogen and GMCs 3. Formation of Molecular Clouds 4. Internal Structure 5. Observing Cores 6. Preliminary Comments on

More information

Theory of star formation

Theory of star formation Theory of star formation Monday 8th 17.15 18.00 Molecular clouds and star formation: Introduction Tuesday 9th 13.15 14.00 Molecular clouds: structure, physics, and chemistry 16.00 16.45 Cloud cores: statistics

More information

Lecture 23 Internal Structure of Molecular Clouds

Lecture 23 Internal Structure of Molecular Clouds Lecture 23 Internal Structure of Molecular Clouds 1. Location of the Molecular Gas 2. The Atomic Hydrogen Content 3. Formation of Clouds 4. Clouds, Clumps and Cores 5. Observing Molecular Cloud Cores References

More information

Statistical Analyses of Data Cubes

Statistical Analyses of Data Cubes Statistical Analyses of Data Cubes Erik Rosolowsky University of British Columbia, Okanagan Campus FCRAO survey of Taurus 1. Whence datacubes 2. Things that I m not going to talk about 3. Analyses from

More information

Magnetic Fields & Turbulence: Observations. Mark Heyer University of Massachusetts

Magnetic Fields & Turbulence: Observations. Mark Heyer University of Massachusetts Magnetic Fields & Turbulence: Observations Mark Heyer University of Massachusetts Protostellar/Cluster Cores Alves etal 2 Tafalla etal 2006 Decoupled Cores Lombardi etal 2006 Goodman etal 1998 SIZE SIZE

More information

Notes: Most of the material presented in this chapter is taken from Stahler and Palla (2004), Chap. 3. v r c, (3.1) ! obs

Notes: Most of the material presented in this chapter is taken from Stahler and Palla (2004), Chap. 3. v r c, (3.1) ! obs Chapter 3. Molecular Clouds Notes: Most of the material presented in this chapter is taken from Stahler and Palla 2004), Chap. 3. 3.1 Definitions and Preliminaries We mainly covered in Chapter 2 the Galactic

More information

PROJECT SUMMARY. clumps

PROJECT SUMMARY. clumps PROJECT SUMMARY This project will offer quantitative new measures of how the material between the stars, known as the Interstellar Medium, or ISM is distributed. Recently, it has become technically feasible

More information

igure 4 of McMullin et al McMullin et al Testi & Sargent 1998 Figure 1 of Testi & Sargent 1998:

igure 4 of McMullin et al McMullin et al Testi & Sargent 1998 Figure 1 of Testi & Sargent 1998: igure 4 of McMullin et al. 1994. Figure 1 of Testi & Sargent 1998: McMullin et al. 1994 BIMA with (only!) three elements Eight configurationsàcoverage of 2 kλ to 30 kλ Naturally wtd. Beam of 11" x 6" (for

More information

Astronomy 1 Fall 2016

Astronomy 1 Fall 2016 Astronomy 1 Fall 2016 Lecture11; November 1, 2016 Previously on Astro-1 Introduction to stars Measuring distances Inverse square law: luminosity vs brightness Colors and spectral types, the H-R diagram

More information

Centimeter Wave Star Formation Studies in the Galaxy from Radio Sky Surveys

Centimeter Wave Star Formation Studies in the Galaxy from Radio Sky Surveys Centimeter Wave Star Formation Studies in the Galaxy from Radio Sky Surveys W. J. Welch Radio Astronomy Laboratory, Depts of EECS and Astronomy University of California Berkeley, CA 94720 Tel: (510) 643-6543

More information

Lec 22 Physical Properties of Molecular Clouds

Lec 22 Physical Properties of Molecular Clouds Lec 22 Physical Properties of Molecular Clouds 1. Giant Molecular Clouds 2. Orion s Clouds 3. Correlations of Observed Properties 4. The X-Factor References Origins of Stars & Planetary Systems eds. Lada

More information

The Birth Of Stars. How do stars form from the interstellar medium Where does star formation take place How do we induce star formation

The Birth Of Stars. How do stars form from the interstellar medium Where does star formation take place How do we induce star formation Goals: The Birth Of Stars How do stars form from the interstellar medium Where does star formation take place How do we induce star formation Interstellar Medium Gas and dust between stars is the interstellar

More information

Lecture 2: Molecular Clouds: Galactic Context and Observational Tracers. Corona Australis molecular cloud: Andrew Oreshko

Lecture 2: Molecular Clouds: Galactic Context and Observational Tracers. Corona Australis molecular cloud: Andrew Oreshko Lecture 2: Molecular Clouds: Galactic Context and Observational Tracers Corona Australis molecular cloud: Andrew Oreshko Classification of Young Stellar Objects (YSOs) Spectral Index Hartmann: Accretion

More information

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Aim Review the characteristics of regions of ionized gas within young massive star forming regions. Will focus the discussion

More information

STARLESS CORES. Mario Tafalla. (Observatorio Astronómico Nacional, Spain)

STARLESS CORES. Mario Tafalla. (Observatorio Astronómico Nacional, Spain) STARLESS CORES Mario Tafalla (Observatorio Astronómico Nacional, Spain) Outline: 1. Internal Structure a. Introduction b. How to characterize the internal strcuture of starless cores c. L1498 & L1517B:

More information

II- Molecular clouds

II- Molecular clouds 2. II- Molecular clouds 3. Introduction 4. Observations of MC Pierre Hily-Blant (Master2) The ISM 2012-2013 218 / 290 3. Introduction 3. Introduction Pierre Hily-Blant (Master2) The ISM 2012-2013 219 /

More information

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)?

Clicker Question: Clicker Question: What is the expected lifetime for a G2 star (one just like our Sun)? How Long do Stars Live (as Main Sequence Stars)? A star on Main Sequence has fusion of H to He in its core. How fast depends on mass of H available and rate of fusion. Mass of H in core depends on mass

More information

Topics for Today s Class

Topics for Today s Class Foundations of Astronomy 13e Seeds Chapter 11 Formation of Stars and Structure of Stars Topics for Today s Class 1. Making Stars from the Interstellar Medium 2. Evidence of Star Formation: The Orion Nebula

More information

Atoms and Star Formation

Atoms and Star Formation Atoms and Star Formation What are the characteristics of an atom? Atoms have a nucleus of protons and neutrons about which electrons orbit. neutrons protons electrons 0 charge +1 charge 1 charge 1.67 x

More information

Gas 1: Molecular clouds

Gas 1: Molecular clouds Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,

More information

Star Formation. Stellar Birth

Star Formation. Stellar Birth Star Formation Lecture 12 Stellar Birth Since stars don t live forever, then they must be born somewhere and at some time in the past. How does this happen? And when stars are born, so are planets! 1 Molecular

More information

Stellar evolution Part I of III Star formation

Stellar evolution Part I of III Star formation Stellar evolution Part I of III Star formation The interstellar medium (ISM) The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful

More information

Reflections on Modern Work Simulated Zeeman Measurements and Magnetic Equilibrium in Molecular Clouds

Reflections on Modern Work Simulated Zeeman Measurements and Magnetic Equilibrium in Molecular Clouds Reflections on Modern Work Simulated Zeeman Measurements and Magnetic Equilibrium in Molecular Clouds Paolo Padoan University of California, San Diego ICREA - University of Barcelona (Spring 2010) Collaborators:

More information

Astr 2310 Thurs. March 23, 2017 Today s Topics

Astr 2310 Thurs. March 23, 2017 Today s Topics Astr 2310 Thurs. March 23, 2017 Today s Topics Chapter 16: The Interstellar Medium and Star Formation Interstellar Dust and Dark Nebulae Interstellar Dust Dark Nebulae Interstellar Reddening Interstellar

More information

Energy. mosquito lands on your arm = 1 erg. Firecracker = 5 x 10 9 ergs. 1 stick of dynamite = 2 x ergs. 1 ton of TNT = 4 x ergs

Energy. mosquito lands on your arm = 1 erg. Firecracker = 5 x 10 9 ergs. 1 stick of dynamite = 2 x ergs. 1 ton of TNT = 4 x ergs Energy mosquito lands on your arm = 1 erg Firecracker = 5 x 10 9 ergs 1 stick of dynamite = 2 x 10 13 ergs 1 ton of TNT = 4 x 10 16 ergs 1 atomic bomb = 1 x 10 21 ergs Magnitude 8 earthquake = 1 x 10 26

More information

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc.

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc. Chapter 16 Lecture The Cosmic Perspective Seventh Edition Star Birth 2014 Pearson Education, Inc. Star Birth The dust and gas between the star in our galaxy is referred to as the Interstellar medium (ISM).

More information

Collapse of magnetized dense cores. Is there a fragmentation crisis?

Collapse of magnetized dense cores. Is there a fragmentation crisis? Collapse of magnetized dense cores Is there a fragmentation crisis? Patrick Hennebelle (ENS-Observatoire de Paris) Collaborators: Benoît Commerçon, Andréa Ciardi, Sébastien Fromang, Romain Teyssier, Philippe

More information

The Physics of the Interstellar Medium

The Physics of the Interstellar Medium The Physics of the Interstellar Medium Ulrike Heiter Contact: 471 5970 ulrike@astro.uu.se www.astro.uu.se Matter between stars Average distance between stars in solar neighbourhood: 1 pc = 3 x 1013 km,

More information

The formation of super-stellar clusters

The formation of super-stellar clusters The formation of super-stellar clusters François Boulanger Institut d Astrophysique Spatiale Cynthia Herrera, Edith Falgarone, Pierre Guillard, Nicole Nesvadba, Guillaume Pineau des Forets Outline How

More information

AST4930: Star and Planet Formation. Syllabus. AST4930: Star and Planet Formation, Spring 2014

AST4930: Star and Planet Formation. Syllabus. AST4930: Star and Planet Formation, Spring 2014 AST4930: Star and Planet Formation Lecture 1: Overview Assoc. Prof. Jonathan C. Tan jt@astro.ufl.edu Bryant 302 Syllabus AST4930: Star and Planet Formation, Spring 2014 Assoc. Prof. Jonathan C. Tan (jt

More information

Halo Gas Velocities Using Multi-slit Spectroscopy

Halo Gas Velocities Using Multi-slit Spectroscopy Halo Gas Velocities Using Multi-slit Spectroscopy Cat Wu Thesis Proposal, Fall 2009 Astronomy Department New Mexico State University Outline Diffuse ionized gas; galaxy halos Origin of halo galactic fountain

More information

Molecular clouds (see review in astro-ph/990382) (also CO [12.1,12.2])

Molecular clouds (see review in astro-ph/990382) (also CO [12.1,12.2]) Molecular clouds (see review in astro-ph/990382) (also CO [12.1,12.2]) Massive interstellar gas clouds Up to ~10 5 M 100 s of LY in diameter. Giant Molecular Clouds (GMCs) defined to be M > 10 4 M High

More information

THE GALAXY. Spitzer Space Telescope Images & Spectra: 3µm - 170µm

THE GALAXY. Spitzer Space Telescope Images & Spectra: 3µm - 170µm THE GALAXY Composite infrared colour image of Galactic Centre region taken at 1.25, 2.2 and 3.5 microns with COBE/DIRBE instrument (NASA/GSFC). GALAXY: A conglomeration of stars, gas + dust Topics: Star

More information

Journal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al.

Journal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al. Journal Club Presentation on The BIMA Survey of Nearby Galaxies. I. The Radial Distribution of CO Emission in Spiral Galaxies by Regan et al. ApJ, 561:218-237, 2001 Nov 1 1 Fun With Acronyms BIMA Berkely

More information

RAMPS: The Radio Ammonia Mid-Plane Survey. James Jackson Institute for Astrophysical Research Boston University

RAMPS: The Radio Ammonia Mid-Plane Survey. James Jackson Institute for Astrophysical Research Boston University RAMPS: The Radio Ammonia Mid-Plane Survey James Jackson Institute for Astrophysical Research Boston University High Frequency Workshop, Green Bank, 21 September 2015 Collaborators (partial list) Taylor

More information

A Tale of Star and Planet Formation. Lynne Hillenbrand Caltech

A Tale of Star and Planet Formation. Lynne Hillenbrand Caltech A Tale of Star and Planet Formation Lynne Hillenbrand Caltech Vermeer s The Astronomer (1688) Mauna Kea (last week) photos by: Sarah Anderson and Bill Bates Context: Our Sun The Sun is a completely average

More information

Philamentary Structure and Velocity Gradients in the Orion A Cloud

Philamentary Structure and Velocity Gradients in the Orion A Cloud Red: CO from Mini survey Orion B Philamentary Structure and Velocity Gradients in the Orion A Cloud Spitzer Orion Cloud Survey: 10 sq. degrees in Orion A and Orion B mapped between 2004-2009 Orion A Green

More information

The Interstellar Medium (ch. 18)

The Interstellar Medium (ch. 18) The Interstellar Medium (ch. 18) The interstellar medium (ISM) is all the gas (and about 1% dust) that fills our Galaxy and others. It is the raw material from which stars form, and into which stars eject

More information

7. Dust Grains & Interstellar Extinction. James R. Graham University of California, Berkeley

7. Dust Grains & Interstellar Extinction. James R. Graham University of California, Berkeley 7. Dust Grains & Interstellar Extinction James R. Graham University of California, Berkeley Visual Extinction Presence of interstellar gas or nebulae has a long history Existence of absorbing interstellar

More information

Astrofysikaliska Dynamiska Processer

Astrofysikaliska Dynamiska Processer Astrofysikaliska Dynamiska Processer VT 2008 Susanne Höfner hoefner@astro.uu.se Aims of this Course - understanding the role and nature of dynamical processes in astrophysical contexts and how to study

More information

ASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium:

ASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium: ASTR2050 Spring 2005 Lecture 10am 29 March 2005 Please turn in your homework now! In this class we will discuss the Interstellar Medium: Introduction: Dust and Gas Extinction and Reddening Physics of Dust

More information

Chapter 11 The Formation and Structure of Stars

Chapter 11 The Formation and Structure of Stars Chapter 11 The Formation and Structure of Stars Guidepost The last chapter introduced you to the gas and dust between the stars that are raw material for new stars. Here you will begin putting together

More information

Lecture 19 CO Observations of Molecular Clouds

Lecture 19 CO Observations of Molecular Clouds Lecture 9 CO Observations of Molecular Clouds. CO Surveys 2. Nearby molecular clouds 3. Antenna temperature and radiative transfer 4. Determining cloud conditions from CO References Tielens, Ch. 0 Myers,

More information

Galactic dust in the Herschel and Planck era. François Boulanger Institut d Astrophysique Spatiale

Galactic dust in the Herschel and Planck era. François Boulanger Institut d Astrophysique Spatiale Galactic dust in the Herschel and Planck era François Boulanger Institut d Astrophysique Spatiale Motivation Dust emission Dust models Dust life cycle Planck early results Dust polarisation Outline Dust

More information

- Strong extinction due to dust

- Strong extinction due to dust The Galactic Centre - Strong extinction due to dust At optical wavelemgth the absorption is almost total Information from the 21 line, IR and radio 10 Region between and cm 14 10 22 1 arcsec at the distance

More information

Chapter 10 The Interstellar Medium

Chapter 10 The Interstellar Medium Chapter 10 The Interstellar Medium Guidepost You have begun your study of the sun and other stars, but now it is time to study the thin gas and dust that drifts through space between the stars. This chapter

More information

Lecture 22 Stability of Molecular Clouds

Lecture 22 Stability of Molecular Clouds Lecture 22 Stability of Molecular Clouds 1. Stability of Cloud Cores 2. Collapse and Fragmentation of Clouds 3. Applying the Virial Theorem References Myers, Physical Conditions in Molecular Clouds in

More information

Energy Sources of the Far IR Emission of M33

Energy Sources of the Far IR Emission of M33 Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also

More information

The Universe o. Galaxies. The Universe of. Galaxies. Ajit Kembhavi IUCAA

The Universe o. Galaxies. The Universe of. Galaxies. Ajit Kembhavi IUCAA Hello! The Universe of Galaxies The Universe o Galaxies Ajit Kembhavi IUCAA Galaxies: Stars: ~10 11 Mass: ~10 11 M Sun Contain stars, gas and dust, possibly a supermassive black hole at the centre. Much

More information

SMA observations of Magnetic fields in Star Forming Regions. Josep Miquel Girart Institut de Ciències de l Espai (CSIC-IEEC)

SMA observations of Magnetic fields in Star Forming Regions. Josep Miquel Girart Institut de Ciències de l Espai (CSIC-IEEC) SMA observations of Magnetic fields in Star Forming Regions Josep Miquel Girart Institut de Ciències de l Espai (CSIC-IEEC) SMA Community Day, July 11, 2011 Simultaneous process of infall and outflow"

More information

Star Formation Taste Tests. Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics & Initiative for Innovative Computing at Harvard

Star Formation Taste Tests. Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics & Initiative for Innovative Computing at Harvard Star Formation Taste Tests Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics & Initiative for Innovative Computing at Harvard Taste Tests? Taste Tests? We frame this project by analogy. How

More information

Mass loss from stars

Mass loss from stars Mass loss from stars Can significantly affect a star s evolution, since the mass is such a critical parameter (e.g., L ~ M 4 ) Material ejected into interstellar medium (ISM) may be nuclear-processed:

More information

Chapter 15 Star Birth. Star-Forming Clouds. Stars form in dark clouds of dusty gas in interstellar space

Chapter 15 Star Birth. Star-Forming Clouds. Stars form in dark clouds of dusty gas in interstellar space Chapter 15 Star Birth Star-Forming Clouds Stars form in dark clouds of dusty gas in interstellar space The gas between the stars is called the interstellar medium Visible light (Hubble Space Telescope)

More information

Interstellar Medium: H2

Interstellar Medium: H2 Interstellar Medium: H2 Gas in molecular clouds Composition: H2 + traces of other molecules (CO, NH3, H2O, HC13N...) Very low ionization fraction (cosmic rays) (HCO+, N2H+,...) Molecules with several isotopologues

More information

Magnetic fields and massive star formation. Qizhou Zhang Harvard-Smithsonian Center for Astrophysics

Magnetic fields and massive star formation. Qizhou Zhang Harvard-Smithsonian Center for Astrophysics Magnetic fields and massive star formation Qizhou Zhang Harvard-Smithsonian Center for Astrophysics Role of Magnetic Field in Star Formation Cloud scale: formation/support magnetic or turbulent? Clump

More information

The Milky Way - Chapter 23

The Milky Way - Chapter 23 The Milky Way - Chapter 23 The Milky Way Galaxy A galaxy: huge collection of stars (10 7-10 13 ) and interstellar matter (gas & dust). Held together by gravity. Much bigger than any star cluster we have

More information

Interstellar Dust and Gas

Interstellar Dust and Gas Interstellar Dust and Gas In 1783 William Herschel began a survey of the heavens using an 18 ¾ inch reflector of his own construction. His goal was to discover new star clusters, nebulae, and double stars.

More information

THE INTERSTELLAR MEDIUM

THE INTERSTELLAR MEDIUM THE INTERSTELLAR MEDIUM An IR view of dust clouds In particular, light from polycyclic aromatic hydrocarbons (PAH s) Little bit of carbon out there, forms hydrocarbons like car exhaust Associated with

More information

Chapter 9. The Formation and Structure of Stars

Chapter 9. The Formation and Structure of Stars Chapter 9 The Formation and Structure of Stars The Interstellar Medium (ISM) The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful

More information

PART 3 Galaxies. Gas, Stars and stellar motion in the Milky Way

PART 3 Galaxies. Gas, Stars and stellar motion in the Milky Way PART 3 Galaxies Gas, Stars and stellar motion in the Milky Way The Interstellar Medium The Sombrero Galaxy Space is far from empty! Clouds of cold gas Clouds of dust In a galaxy, gravity pulls the dust

More information

INTRODUCTION TO SPACE

INTRODUCTION TO SPACE INTRODUCTION TO SPACE 25.3.2019 The Galaxy II: Stars: Classification and evolution Various types of stars Interstellar matter: dust, gas Dark matter ELEC-E4530 Radio astronomy: the Sun, pulsars, microquasars,

More information

INITIAL CONDITIONS. Paola Caselli. School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES. Protoplanetary disks

INITIAL CONDITIONS. Paola Caselli. School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES. Protoplanetary disks Paola Caselli School of Physics and Astronomy FACULTY OF MATHEMATICS & PHYSICAL SCIENCES Protoplanetary disks INITIAL CONDITIONS Boley 2009 Quiescent molecular clouds High-mass star forming regions Pre-stellar

More information

18. Stellar Birth. Initiation of Star Formation. The Orion Nebula: A Close-Up View. Interstellar Gas & Dust in Our Galaxy

18. Stellar Birth. Initiation of Star Formation. The Orion Nebula: A Close-Up View. Interstellar Gas & Dust in Our Galaxy 18. Stellar Birth Star observations & theories aid understanding Interstellar gas & dust in our galaxy Protostars form in cold, dark nebulae Protostars evolve into main-sequence stars Protostars both gain

More information

Pressure equilibrium. The diffuse cold (100 K), warm ( K) and hot components (10 6 K) are in rough pressure equilibrium

Pressure equilibrium. The diffuse cold (100 K), warm ( K) and hot components (10 6 K) are in rough pressure equilibrium Chapter 7 Planet formation The observations indicate that planets form in circumstellar disks around young stars. Therefore, planet formation is strongly linked to the star formation process which we describe

More information

Interstellar Medium and Star Birth

Interstellar Medium and Star Birth Interstellar Medium and Star Birth Interstellar dust Lagoon nebula: dust + gas Interstellar Dust Extinction and scattering responsible for localized patches of darkness (dark clouds), as well as widespread

More information

Recall what you know about the Big Bang.

Recall what you know about the Big Bang. What is this? Recall what you know about the Big Bang. Most of the normal matter in the universe is made of what elements? Where do we find most of this normal matter? Interstellar medium (ISM) The universe

More information

Infrared Dark Clouds seen by Herschel and ALMA

Infrared Dark Clouds seen by Herschel and ALMA Infrared Dark Clouds seen by Herschel and ALMA Ke Wang ESO Fellow www.eso.org/~kwang Collaborators: Qizhou Zhang, Xing (Walker) Lu, Izaskun Jimenez-Serra 1 IR-dark clouds: shadows in infrared sky Image

More information

Nearby Universe: Rapporteur

Nearby Universe: Rapporteur Nearby Universe: Rapporteur Margaret Meixner (STScI) SAGE: Tracing the Lifecycle of Baryonic Matter: Intermediate mass stars High mass stars credit: http://hea-www.cfa.harvard.edu/champ/education/public/icons/

More information

5) What spectral type of star that is still around formed longest ago? 5) A) F B) A C) M D) K E) O

5) What spectral type of star that is still around formed longest ago? 5) A) F B) A C) M D) K E) O HW2 Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) The polarization of light passing though the dust grains shows that: 1) A) the dust grains

More information

Astronomy across the spectrum: telescopes and where we put them. Martha Haynes Exploring Early Galaxies with the CCAT June 28, 2012

Astronomy across the spectrum: telescopes and where we put them. Martha Haynes Exploring Early Galaxies with the CCAT June 28, 2012 Astronomy across the spectrum: telescopes and where we put them Martha Haynes Exploring Early Galaxies with the CCAT June 28, 2012 CCAT: 25 meter submm telescope CCAT Site on C. Chajnantor Me, at 18,400

More information

Measurement of Galactic Rotation Curve

Measurement of Galactic Rotation Curve Measurement of Galactic Rotation Curve Objective: The 21-cm line produced by neutral hydrogen in interstellar space provides radio astronomers with a very useful probe for studying the differential rotation

More information

Star Formation in GMCs: Lessons from Herschel Observations of the Aquila Complex

Star Formation in GMCs: Lessons from Herschel Observations of the Aquila Complex Herschel PACS/SPIRE map of Aquila (Gould Belt survey) ORISTARS erc project Lab. AIM, Paris-Saclay, France Ph. André, A. Men'shchikov, N. Schneider, S. Bontemps, D. Arzoumanian, N. Peretto, P. Didelon,

More information

Stellar Birth. Stellar Formation. A. Interstellar Clouds. 1b. What is the stuff. Astrophysics: Stellar Evolution. A. Interstellar Clouds (Nebulae)

Stellar Birth. Stellar Formation. A. Interstellar Clouds. 1b. What is the stuff. Astrophysics: Stellar Evolution. A. Interstellar Clouds (Nebulae) Astrophysics: Stellar Evolution 1 Stellar Birth Stellar Formation A. Interstellar Clouds (Nebulae) B. Protostellar Clouds 2 C. Protostars Dr. Bill Pezzaglia Updated: 10/02/2006 A. Interstellar Clouds 1.

More information

Interstellar Dust and Gas

Interstellar Dust and Gas Interstellar Dust and Gas In 1783 William Herschel began a survey of the heavens using an 18 ¾ inch reflector of his own construction. His goal was to discover new star clusters, nebulae, and double stars.

More information

Cinthya Herrera (NAOJ)

Cinthya Herrera (NAOJ) Cinthya Herrera (NAOJ) ASTE/ALMA Development Workshop 2014, June 18th, 2014 Galaxies interactions... Key in hierarchical model of galaxy formation and evolution (e.g., Kauffmann et al. 1993) Most massive

More information

6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and

6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and 6-1 6. Interstellar Medium 6.1 Nebulae Emission nebulae are diffuse patches of emission surrounding hot O and early B-type stars. Gas is ionized and heated by radiation from the parent stars. In size,

More information

The Formation of Star Clusters

The Formation of Star Clusters The Formation of Star Clusters Orion Nebula Cluster (JHK) - McCaughrean Jonathan Tan University of Florida & KITP In collaboration with: Brent Buckalew (ERAU), Michael Butler (UF u-grad), Jayce Dowell

More information

Chapter 16: Star Birth

Chapter 16: Star Birth Chapter 16 Lecture Chapter 16: Star Birth Star Birth 16.1 Stellar Nurseries Our goals for learning: Where do stars form? Why do stars form? Where do stars form? Star-Forming Clouds Stars form in dark clouds

More information

THE NATURE OF THE DENSE CORE POPULATION IN THE PIPE NEBULA: A SURVEY OF NH 3, CCS, AND HC 5 N MOLECULAR LINE EMISSION

THE NATURE OF THE DENSE CORE POPULATION IN THE PIPE NEBULA: A SURVEY OF NH 3, CCS, AND HC 5 N MOLECULAR LINE EMISSION The Astrophysical Journal Supplement Series, 174:396Y425, 2008 February # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE NATURE OF THE DENSE CORE POPULATION IN THE

More information

Astrophysical Quantities

Astrophysical Quantities Astr 8300 Resources Web page: http://www.astro.gsu.edu/~crenshaw/astr8300.html Electronic papers: http://adsabs.harvard.edu/abstract_service.html (ApJ, AJ, MNRAS, A&A, PASP, ARAA, etc.) General astronomy-type

More information

Where do Stars Form?

Where do Stars Form? Where do Stars Form? Coldest spots in the galaxy: T ~ 10 K Composition: Mainly molecular hydrogen 1% dust EGGs = Evaporating Gaseous Globules ftp://ftp.hq.nasa.gov/pub/pao/pressrel/1995/95-190.txt Slide

More information

Ay 1 Midterm. Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA

Ay 1 Midterm. Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA Ay 1 Midterm Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA You have THREE HOURS to complete the exam, but it is about two hours long. The

More information

Galactic Supershells and GSH Vanessa A. Moss Parkes 50th Symposium 3rd November

Galactic Supershells and GSH Vanessa A. Moss Parkes 50th Symposium 3rd November Galactic Supershells and GSH 006-15+7 Vanessa A. Moss Parkes 50th Symposium 3rd November 2011 1 Contents Early history of supershells Discovery Early interpretation Surveys of supershells Northern hemisphere

More information

NRAO Instruments Provide Unique Windows On Star Formation

NRAO Instruments Provide Unique Windows On Star Formation NRAO Instruments Provide Unique Windows On Star Formation Crystal Brogan North American ALMA Science Center Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank

More information

Diffuse Interstellar Medium

Diffuse Interstellar Medium Diffuse Interstellar Medium Basics, velocity widths H I 21-cm radiation (emission) Interstellar absorption lines Radiative transfer Resolved Lines, column densities Unresolved lines, curve of growth Abundances,

More information

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc.

Chapter 16 Lecture. The Cosmic Perspective Seventh Edition. Star Birth Pearson Education, Inc. Chapter 16 Lecture The Cosmic Perspective Seventh Edition Star Birth Star Birth 16.1 Stellar Nurseries Our goals for learning: Where do stars form? Why do stars form? Where do stars form? Star-Forming

More information

Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2

Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2 Next Generation Very Large Array Working Group 2 HI in M74: Walter+ 08 CO in M51: Schinnerer+ 13 Continuum in M82: Marvil & Owen Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of

More information

Unscrambling the Egg. Yvonne Pendleton NASA Ames Research Center. JWST Workshop Nov. 14, 2017

Unscrambling the Egg. Yvonne Pendleton NASA Ames Research Center. JWST Workshop Nov. 14, 2017 Unscrambling the Egg Yvonne Pendleton NASA Ames Research Center JWST Workshop Nov. 14, 2017 From interstellar dust to new stars and planets Comparisons between material forming new planetary systems and

More information

Lecture 26 Low-Mass Young Stellar Objects

Lecture 26 Low-Mass Young Stellar Objects Lecture 26 Low-Mass Young Stellar Objects 1. Nearby Star Formation 2. General Properties of Young Stars 3. T Tauri Stars 4. Herbig Ae/Be Stars References Adams, Lizano & Shu ARAA 25 231987 Lada OSPS 1999

More information

Collapse of Massive Cloud Cores

Collapse of Massive Cloud Cores Collapse of Massive Cloud Cores Robi Banerjee ITA, University of Heidelberg Based on 3D MHD, AMR* Simulations * Adaptive Mesh Refinement Collapse of Hydrostatic Cores Cloud formation by TI Slowly rotating

More information

ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE

ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE Snežana Stanimirović, October 6, 2014 1. Introduction This project has two goals: we want to measure the Milky Way (or Galactic) rotation curve by

More information

Survey of Astrophysics A110

Survey of Astrophysics A110 Goals: Galaxies To determine the types and distributions of galaxies? How do we measure the mass of galaxies and what comprises this mass? How do we measure distances to galaxies and what does this tell

More information

Physics and chemistry of the interstellar medium. Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro

Physics and chemistry of the interstellar medium. Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro Physics and chemistry of the interstellar medium Lecturers: Simon Glover, Rowan Smith Tutor: Raquel Chicharro This course consists of three components: Lectures Exercises Seminar [Wed., 2-4] [Thu., 4-5]

More information

HI clouds near the Galactic Center:

HI clouds near the Galactic Center: PHISCC 217 February 7th, Pune HI clouds near the Galactic Center: Possible tracers for a Milky-Way nuclear wind? Enrico Di Teodoro Research School of Astronomy and Astrophysics Australian National University

More information

The Effects of Radiative Transfer on Low-Mass Star Formation

The Effects of Radiative Transfer on Low-Mass Star Formation The Effects of Radiative Transfer on Low-Mass Star Formation Stella Offner NSF Fellow, ITC Dense Cores in Dark Clouds Oct 23 2009 Collaborators: Chris McKee (UC Berkeley), Richard Klein (UC Berkeley; LLNL),

More information

Star-Forming Clouds. Stars form in dark clouds of dusty gas in interstellar space. The gas between the stars is called the interstellar medium.

Star-Forming Clouds. Stars form in dark clouds of dusty gas in interstellar space. The gas between the stars is called the interstellar medium. Star Birth Chapter 16 Lecture 16.1 Stellar Nurseries The Cosmic Perspective Our goals for learning: Where do stars form? Why do stars form? Seventh Edition Star Birth Where do stars form? Star-Forming

More information

Cooling Limits for the

Cooling Limits for the Cooling Limits for the Page et al. 2004 Youngest Neutron Stars Cooling from the Youngest NSs SNR Zone NSs younger than ~50 kyr offer strong constraints on rapid cooling - the associated physical processes

More information

Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars

Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Properties of Nearby Stars Most in orbit with the Sun around Galactic Center Stellar Kinematics Reveal Groups of Stars with Common Space Motion (Moving

More information