science briefing may 3, 2018 birth of stars, dr. solange
TRANSCRIPT
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Birth of Stars,
Near and Far
Dr. Solange Ramírez (Caltech/IPAC)
Dr. Steven Finkelstein (University of Texas at Austin)
Dr. Bryan Méndez (University of California, Berkeley)
Facilitator: Dr. Emma Marcucci (STScI)
Science Briefing
May 3, 2018
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Lagoon Nebula
Zoom and Pan: http://hubblesite.org/video/1031/news_release/2018-21
Image Credit: NASA/ESA/STScI
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Additional Resources
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http://nasawavelength.org/list/2146Hubble’s 28th Anniversary
Lagoon Nebula: Stellar Nursery
Lagoon Nebula Images
Lagoon Nebula Videos
Celebrity Video:
Think Tank: A Star is Born
Images / Lithos and Activities:
NGC 2174: Monkey Head Nebula and Star Formation Activity
Stellar Spire in the Eagle Nebula
Star Birth: Cool Cosmos
Milky Way: Cool Cosmos
Additional Nearby Star Formation resources
Progressive Star Formation in the Magellanic Clouds
Hubble Survey Unlocks Clues to Star Birth in Neighboring Galaxy
Firestorm of Star Birth in Galaxy M33
http://nasawavelength.org/list/2142Additional list curated by Dr. Bryan Méndez:
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Outline of this Science Briefing
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1. Solange Ramírez (Caltech/IPAC)
Nearby Star Formation: Understanding Star Formation in the Milky Way
2. Steven Finkelstein (University of Texas at Austin)
Distant Star Formation: Star Formation in the Early Universe
3. Bryan Méndez (University of California, Berkeley)
Highlight of Resources to Engage Audiences
4. Discussion / Questions
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Star Formation in the Milky Way
Solange V. Ramirez(Caltech/IPAC)
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Where do stars form ?
• Molecular clouds are part of the Interstellar Medium
• Star formation starts with the collapse of a molecular cloud, due to gravity
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Visible and Infrared Light
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Infrared light has the ability to “see” through opaque molecular clouds
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How do stars form ?
• More material will be accreted until the collapse is stopped
• The material of the disk will form planets
• The cores will form a proto-star and a disk
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Star Forming Core
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Cores are hidden in the visible, they are cold, and
they emit most of their light in the infrared
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Star Forming Outflow
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Outflows appear as a core collapses
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Protostar
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Outflow dissipates
Disk is present
Star starts to ignite
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Star with Disk
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Star light has been blocked in these images, revealing a debris disk
Planets may be formed from the material from the debris disk
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How is the collapse stopped ?
• Gravity goes inwards
• A star is born when it starts radiating
• Radiation pressure goes outwards
• The equilibrium between gravity and pressure stops the collapse
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What makes a star shine ?
NUCLEAR FUSION
1H + 1H 1He + Radiation (light)
The core of the star is hot enough to become a natural nuclear reactor !
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Where do stars form ?
• The collapse may be inhomogeneous and form filamentary structures
• Cores of material will evolve to form stars
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Where do stars form ?
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Stars can form in groups!
The Orion Nebula is a giant stellar nursery, where thousands of stars are being born.
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The Milky Way: our Galaxy
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The Milky Way is a spiral galaxy
This is a scientifically based artist concept of the Milky Way
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Most star forming clouds are in Spiral Arms in the Milky Way
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Star formation in external galaxies: 30 Dor in the LMC
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S T A R F O R M A T I O N I N
T H E E A R L Y U N I V E R S E
S T E V E N F I N K E L S T E I NT H E U N I V E R S I T Y O F T E X A S A T A U S T I N
N A S A ’ S U N I V E R S E O F L E A R N I N G M A Y 3 R D , 2 0 1 8
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W H A T I S A G A L A X Y ?
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G A L A X I E S I N T H E E A R L Y U N I V E R S E
L O O K V E R Y D I F F E R E N T
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U N D E R S T A N D I N G T H I S P R O C E S S I S O N E
O F T H E M A I N G O A L S O F M Y R E S E A R C H
???
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D E T E C T I N G S T A R - F O R M A T I O N
• When new stars form, they form at all masses, distributed according to the “initial
mass function”, which observations show produces many more low-mass stars
than high-mass stars.
• However, high-mass stars are so much brighter than low-mass stars that they
outshine them.
• They also have very short lifetimes, so if you see UV emission from a massive
star, it means it has just formed, and you have discovered ongoing star-
formation activity.
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G A L A X I E S W H I C H A R E F O R M I N G S T A R S H A V E
S P E C T R A L I K E H I G H - M A S S S T A R S
UltravioletOptical
Infrared
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T H E A N D R O M E D A G A L A X Y
Ultraviolet
Optical
Infrared
M A S S I V E ,
N E W L Y F O R M E D
S T A R S
L O W E R - M A S S ,
O L D E R S T A R S
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T O S E E T H I S I N T H E D I S T A N T U N I V E R S E , T H E E X P A N D I N G
U N I V E R S E M E A N S T H A T W E H A V E T O L O O K I N T H E
O P T I C A L ( A N D E V E N T U A L L Y , I N T H E N E A R - I N F R A R E D )
E D W I N H U B B L E
( 1 8 8 9 - 1 9 5 3 )
Redshift
(z)
Ultraviolet
Wavelength
(nm)
Time since
Big Bang(billions of
years)
0 150 13.8
1 300 6
2 450 3
4 750 1.5
6 1050 0.9
8 1350 0.7
10 1650 0.5
12 1950 0.3
Hu
bb
le’s
Wh
eelh
ou
se
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E V O L U T I O N O F S T A R F O R M A T I O N W I T H
C O S M I C T I M E
• This plot shows the evolution of the “cosmic star-formation rate density”.
This is the amount of star-formation, per unit volume, measured in solar
masses per year - it can be thought of as how many stars of a mass like the
Sun form per year.
• As you can imagine, this requires some of the deepest imaging imaginable - this
plot comes from a paper by Piero Madau using the original Hubble Deep Field.
Madau 1996
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M O V I N G T O H I G H E R R E D S H I F T W I T H H U B B L E
• New deep fields, first the Hubble Ultra Deep field, done with
the newer visible-light Advanced Camera for Surveys, then
the near-infrared version, done with the Wide-Field Camera
3, allowed these studies to be pushed to z ~ 10.
Finkelstein 201629
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B R E A K I N G T H E R E D S H I F T 1 0 B A R R I E R
• To move to even higher redshift requires a telescope
which is sensitive to even redder wavelengths than
Hubble, which is one of the primary science drivers for the
James Webb Space Telescope.
Redshift
(z)
Ultraviolet
Wavelength
(nm)
Time since
Big Bang(billions of
years)
2 450 3
4 750 1.5
6 1050 0.9
8 1350 0.7
10 1650 0.5
12 1950 0.35
15 2400 0.25
Hu
bb
le’s
Wh
eelh
ou
se
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C O N C L U S I O N S
• We can trace star-formation activity by looking for ultraviolet
emission from bright, high-mass stars. They are short lived, so
their presence indicates ongoing star formation.
• To observe this in the distant universe, we must observe redshifted
ultraviolet emission, which exists in the optical for modest redshifts,
and in the infrared for the most distant galaxies known.
• Through these observations, we have found that star-formation
activity rose at a slow-but-steady level from early times, peaking
around 10 billion years into the past. This activity has since been
decreasing at a fast clip, such that the star-formation rate density
today is similar to that at a time when the universe was less than
one billion years old.
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Star FormationEducational Resources
Dr. Bryan Mendez, UC Berkeley@bryanjmendez
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NASA Wavelength
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Images: NASA Website
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Images: HUBBLESITE
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Images: AstroPix
36@bryanjmendez
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Images: WISE
37@bryanjmendez
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Images: OWN
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Observe
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Elaborate
40@bryanjmendez
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Elaborate
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ASTC partnership
A Professional Development opportunity –
How to Use NASA Resources;
future funding resources available
• Seven webinars were held in 2018, with these goals:o Improve familiarity of NASA Astrophysics resources and ways to use themo Increase knowledge of NASA Astrophysics-related conceptso Utilize real NASA datao Interact with NASA Subject Matter Experts
• Webinars are archived for viewing in the NASA’s Universe of Learning Community of Practice space, http://community.astc.org/communities/community-home?CommunityKey=1255165e-7b78-4791-8fcf-3eccfc52500b
As a follow-on to this webinar series, there will be an opportunity to apply for $2,500 mini-fund resources to be competitively awarded to selected institutions, in order to implement or facilitate programming, produce exhibits, etc., using Universe of Learning resources.
Applications open May 9, 2018 and are due June 4, 2018.
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To ensure we meet the needs of the education community (you!), NASA’s UoL is committed to performing regular evaluations, to determine the effectiveness of Professional Learning opportunities like the Science Briefings.
If you prefer not to participate in the evaluation process, you can opt out by contactingKay Ferrari <[email protected]>.
This product is based upon work supported by NASA under award number NNX16AC65A to the Space Telescope Science Institute, working in partnership with Caltech/IPAC, Jet Propulsion Laboratory, Smithsonian Astrophysical Observatory, and Sonoma State University. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Aeronautics and Space Administration.
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