STAR CLUSTERS Lecture 1 Introduction Nora Ltzgendorf (ESA) I ts a - - PowerPoint PPT Presentation

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STAR CLUSTERS Lecture 1 Introduction Nora Ltzgendorf (ESA) I ts a - - PowerPoint PPT Presentation

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STAR CLUSTERS Lecture 1 Introduction Nora Ltzgendorf (ESA) I ts a school, so ? ? ? ? ? ? ? ? ? ASK QUESTIONS!!! If you dont understand the content If you dont understand the language TAKE NOTES This

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STAR CLUSTERS Lecture 1 Introduction

Nora Lützgendorf (ESA)

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Nora Lützgendorf, KAS16 / 49

➡ ASK QUESTIONS!!!

2

Its a school, so…

? ?

? ? ?

? ? ? ?

➡ If you don’t understand the content… ➡ If you don’t understand the language…

➡ TAKE NOTES

➡ This is the most text on a slide you will see ;)

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Nora Lützgendorf, KAS16 / 49

1.Career 2.Introduction

  • a. What is a star cluster?
  • b. What kind of clusters do we know?
  • c. Where do we find them?
  • d. Characteristics

3

Outline

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Nora Lützgendorf, KAS16 / 49

1.Career 2.Introduction

  • a. What is a star cluster?
  • b. What kind of clusters do we know?
  • c. Where do we find them?
  • d. Characteristics

4

Outline

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Current Position

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JWST/NIRSpec Instrument and Calibration Scientist

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European Space Agency

technology telecom m unications hum an spaceflight earth observation launchers navigation

  • perations

space science exploration

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James Webb Space Telescope

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FACTS

WHAT: Infrared space telescope WHERE: Lagrange Point 2 WHEN: October 2018 MIRROR: 6.5 m

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James Webb Space Telescope

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James Webb Space Telescope

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Current Position

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LAUNCH SEGMENT OBSERVATORY SEGMENT GROUND SEGMENT

Payload adapter Launcher (Ariane 5) Launch site services Science and operation center (STScI) 15 ESA staff members Common systems (deep space network) Provided by NASA Provided by ESA Provided by CSA Spacecraft (bus, sunshield…) Telescope Payload module (ISIM) and instruments NIRCam NIRSpec FGS/NIRISS MIRI

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NIRSpec

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Fixed Slit Spectroscopy Multi Object Spectroscopy Integral Field Spectroscopy

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Tasks

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BEFORE LAUNCH (2018)

  • 80% duties, 20% science
  • assist in calibration campaigns

(like Cryo Vacuum Tests at NASA)

  • reduce and analyze data from these

campaigns

  • create calibration files for the instruments (flat-

fields, darks, …)

  • assist in GTO observation preparations

AFTER LAUNCH

  • 50% duties, 50% science
  • commissioning (final calibration and science

verification of the instrument)

  • user support (help astronomers to observe

with the instrument)

  • calibration monitoring (degrading of

hardware, change in instrument…)

  • …

Making sure the instrument is usable for doing Astronomy Making sure astronomers use the instrument most efficiently

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How did I get here?

MUNICH, D (2005-2013)

2005 - 2010: Diplom (Physics), LMU 2010 - 2013: PhD (Astrophysics), LMU/ESO

LEIDEN, NL (2013-2015)

2013 – 2015: Research Fellow, ESA

LEIPZIG, D (1985-2004)

1996 – 2004: High-School

BALTIMORE, US (since 2015)

since 2015: JWST Instrument Scientist, ESA

Nora Lützgendorf, KAS16 / 49

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Nora Lützgendorf, KAS16 / 49

1.Career 2.Introduction

  • a. What is a star cluster?
  • b. What kind of clusters do we know?
  • c. Where do we find them?
  • d. Characteristics

13

Outline

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“The Milky Way is nothing else but a mass of innumerable stars planted together in clusters”

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Introduction

  • Galileo Galilei (1610)
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Introduction

  • Lada & Lada (2003)

“Most stars form in clusters”

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Star Cluster

Collection of stars roughly born at the same time Collection of stars that are gravitationally bound

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Excursion: Color-magnitude diagram

L/M L/MV T/(V-I)

HOT COLD

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Color-magnitude diagram

Video can be found here: http://hubblesite.org/newscenter/archive/releases/2010/28

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L/M L/MV T/(V-I)

HOT COLD

1) Main Sequence Star

H+He

2) Red Giant

He H+He

4) Asymptotic Giant

C+O He H+He

3) Horizontal Branch Star

H+He He

5) White Dwarf

C+O

Excursion: Color-magnitude diagram

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Marcia Rieke

Excursion: Color-magnitude diagram

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Marcia Rieke

Excursion: Color-magnitude diagram

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Marcia Rieke

Excursion: Color-magnitude diagram

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Marcia Rieke

Excursion: Color-magnitude diagram

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Marcia Rieke

Excursion: Color-magnitude diagram

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Types of clusters

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

N stars

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Environment

OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

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Types of clusters

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Association Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

N stars

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OB Associations

  • 20 - 500 pc
  • 0.1 stars/pc
  • gravitationally unbound
  • 12 within 650 pc

70 pc 300 pc SMC - NGC 346 M33 - NGC 604

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Star Cluster

Collection of stars roughly born at the same time Collection of stars that are gravitationally bound

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Types of clusters

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

N stars

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Embedded clusters

  • 1 - 10 pc
  • 100 - 1000 stars/pc3
  • age < 5 Myr
  • may or may not be bound
  • still gas in / around the cluster

➡ High extinction

1 1 2 3 4 H-K 1 1 2 3 4 J-H

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Embedded clusters

Nora Lützgendorf, KAS16 / 49

Video can be found here: https://www.youtube.com/watch?v=JcqlTOrijtk

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Types of clusters

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

N stars

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Open clusters

  • core radii ~ 2pc
  • mass ~ 100 - 1000 MSUN
  • age: between 3 Myr and a few Gyr
  • no gas left
  • gravitationally bound

NGC 3603 Arches NGC 3766 NGC 4755

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Open clusters - Observations

  • ~ 2000 identified

➡ 1e5 within the Galaxy! (extinction)

Globular Clusters Open Clusters

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Types of clusters

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

N stars

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  • 1-30 pc
  • mass ~ 104 - 106 MSUN
  • gravitationally bound
  • age: 10 - 12 Gyr

➡ oldest objects in the universe!

Globular Clusters

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  • 1-30 pc
  • mass ~ 104 - 106 MSUN
  • gravitationally bound
  • age: 10 - 12 Gyr

➡ oldest objects in the universe!

Globular Clusters

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Globular Clusters - Are dense

SUN ALPHA CENTAURI DENSITY ~103 1/pc3

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PAST:

  • All stars formed at the same time
  • All stars have the same chemical composition

TODAY: (see Lecture 2)

Omega Centauri, Bellini et al., 2011

Globular Clusters - Not what expected

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Always around galaxies Milky Way Andromeda M87

~200 GCs ~500 GCs ~15 000 GCs

Globular Clusters - Live in Galaxies

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Number of Globular Clusters in a galaxy divided by the galaxy’s luminosity:

  • Formation efficiency of Globular Clusters relative to field stars
  • Depends on galaxy type (higher in ellipticals)

37

SN = NGC/LG

Georgiev et al., 2010

Globular Clusters - Specific Frequency

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Blue Globular Clusters

  • metal-poor
  • galaxy halo
  • larger

Red Globular Clusters

  • metal-rich
  • bulge/disk
  • smaller

BLUE RED

Globular Clusters - Bimodality

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Young Massive Clusters

  • Young cluster populations forming today
  • Maybe forming Globular Clusters???
  • Formation Environments:

Galaxy Mergers Spiral Galaxies Starbursting Dwarfs

High Star Formation

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Types of clusters

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

N stars

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Nuclear Clusters

  • 1-30 pc
  • mass ~ 105 - 108 MSUN
  • age: multiple epochs of

star formation

  • centers of galaxies
  • gravitational bound
  • co-existing with black hole
  • densest objects in the

universe

Seth et al., 2006

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SUN ALPHA CENTAURI ALPHA CENTAURI DENSITY ~106 1/pc3 DENSITY ~106 1/pc3

Nuclear Clusters - Are super dense

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Seth et al., 2010

NGC 404

Nuclear Clusters - Host black holes

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Nuclear Clusters - Formation

1.) Globular Cluster infall 2.) Gas accretion, star formation

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Nuclear Clusters - Formation

1.) Globular Cluster infall 2.) Gas accretion, star formation

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Nuclear Clusters - Multiple populations

Sgr/M54

Siegel et al., 2007

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Nuclear Clusters - Peculiar kinematics

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Nuclear Clusters - In our Galaxy

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Nuclear Clusters - In our Galaxy

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Nuclear Clusters - In our Galaxy

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Summary

  • 1. Star Clusters:

➡ Collection of stars roughly born at the same time (sometimes gravitationally bound)

100 -1000 1e5-1e7 1e6-1e8 1e4-1e5 1e4-1e6 OB Associations Embedded Clusters Open Clusters Globular Clusters Nuclear Clusters

  • in the disk
  • gravitationally

unbound

  • in the disk
  • still gas left
  • in the disk
  • gravitationally

bound

  • in the halo/

bulge

  • oldest objects

in the universe

  • at the center
  • f the galaxy
  • densest
  • bjects in the

universe