the age of the universe - amazon s3 · into a type ia supernova . credit: nasa, esa, and a. riess...
TRANSCRIPT
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THE AGE OF THE UNIVERSE
CAROLIN CRAWFORD
GRESHAM PROFESSOR OF ASTRONOMY
NASA/ESA/Hubble Heritage
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NASA/NOAA/GSFC/Suomi NPP/VIIRS/Norman Kuring
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Linda Bruce
Lord Kelvin
1824 - 1907
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Daughter material
Parent material
time
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Arthur Holmes
1890 - 1945
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NASA
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Clair Patterson
1922-1995
F. Antonucci, M. Angelini, & F. Tagliani, ADARA Astrobrallo
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NASA/ESA/Hubble Heritage
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Alan Friedman (Averted Imagination)
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Chris Hetlage
cosmological constant
LeMaitre Friedmann
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Edwin Hubble
1889 - 1953
2
d π 4
Luminosity Flux
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combined measurements of
distances to and
velocities of
the ‘spiral nebulae’
all galaxies are receding
Stephen Leshin
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Stephen Leshin
Hubble’s Law
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uniform expansion of space
Galaxy twice as far away has moved twice as far/as fast
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– the universe is expanding
– it was smaller in the past
Big Bang !
Russell Croman
A galaxy a distance d away
moving away from us at velocity v
has taken a time of ~ d/v to travel to that point
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NASA
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NASA/ESA/Reiss (STScI/JHU)
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NASA. ESA, Hubble Heritage (STScI/AURA)
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NASA. ESA, Hubble Heritage (STScI/AURA)
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Martin Pugh
• Luminosity of a star depends on its mass
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Martin Pugh
• Luminosity of a star depends on its mass
• Age of a star depends on its mass
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Martin Pugh
• Luminosity of a star depends on its mass
• Age of a star depends on its mass
Faintest ►lowest-mass ► oldest stars
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Martin Pugh
73 km s-1 per Megaparsec
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NASA/ESA/ Rigby, Sharon, Gladders & Wuyts
“matter tells space how to curve,
and space tells matter how to move”
Wheeler
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Cre
NASA/WMAP science team
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Cre
NASA/WMAP science team
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recollapsing
Universe
present
past
future
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recollapsing
Universe
open
Universe
present
past
future
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recollapsing
Universe
open
Universe
present
past
future
critical
Universe
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an important cosmological parameter...
density parameter of the Universe
Ω = / c
where c is the critical density of matter needed to close the
Universe
if Ω > 1 closed Universe
universe will eventually stop expanding, then collapse
If Ω < 1 open Universe
the universe expands forever
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recollapsing
Universe
open
Universe
present
past
future
Ω<1 Ω>1 Ω=1
critical
Universe
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–200μK +400μK
The cosmic microwave background
NASA/WMAP science team
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NASA/WMAP science team
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NASA/WMAP science team
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recollapsing
Universe
open
Universe
present
past
future
Ω<1 Ω>1 Ω=1
critical
Universe
size of CMB
fluctuations shows
we live in a
flat (‘critical’)
universe
all the
matter + radiation
in the Universe is
only 25% of what is
required
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Baryonic mass of cluster is determined from the
amount of light radiated – at all wavelengths
Total gravitating mass of cluster (including dark
matter) obtained through many methods (X-rays,
galaxy motions, gravitational lensing)
NASA/ESA/J Richard & JP Kneib
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Dean Rowe
the observed baryonic fraction
fb = baryonic mass / total mass
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Observations
of nearby
clusters
show fb~0.12
fb
Radius in cluster
Allen et al
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Observations of clusters of galaxies tell us the ratio of
ordinary mass / total (dark+ordinary) mass ~ 0.12
calculations of primordial synthesis fix how much
ordinary matter was created in the Big Bang
so we know the total amount of matter in the
Universe
Palomar-Quest Survey Team
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baryon fraction should be the same all across the Universe
change reference cosmology used to derive these
observables until the fraction of baryonic mass is
the same for all clusters
Allen et al
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Supernova type 1a
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Sun-like
star
expands to
red giant
sheds outer
layers
cools and
contracts to
white dwarf
...but if it can
accrete mass from
a binary partner
once over 1.4 Msun
it will suddenly explode
into a type Ia supernova
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Sun-like
star
expands to
red giant
sheds outer
layers
cools and
contracts to
white dwarf
...but if it can
accrete mass from
a binary partner
once over 1.4 Msun
it will suddenly explode
into a type Ia supernova
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Credit: NASA, ESA, and A. Riess (STScI)
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Rela
tiv
e brig
htness
Brighter supernovae
fade more
slowly…
Kim et al 1997
Days after peak brightness
Supernova
explosion
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velocity
dis
tance
distant supernovae are:
dimmer and so
further away
than expected
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distance expected
distance measured
v
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The supernova results show that:
• the expansion of the Universe is speeding up
• this acceleration started about 6 billion years ago
– the Universe is younger than we thought
– gravity does not control the Universe
Johannes Schedler (Panther Observatory)
Perlmutter Schmidt Riess
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All matter (+radiation) accounts for only
¼ of the mass-energy density of the Universe
The other ¾ must take the form of energy
we call this ‘dark energy’...
...and this ‘dark energy’ is responsible for the
accelerated expansion of the Universe
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Dark energy
75%
Visible matter
5%
Dark matter
20%
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The attractive force of gravity
is a property of matter
accelerating
Universe
The repulsive force of dark energy
is a property of space
Thus as the universe expands,
dark energy
begins to dominate over gravity
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recollapsing
Universe
open
Universe
present
past
future
Ω<1 Ω>1 Ω=1
critical
Universe
accelerating
Universe
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The cosmological
constant
What is the dark energy?
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The cosmological
constant
What is the dark energy?
The vacuum
energy of
space
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The cosmological
constant
What is the dark energy?
The vacuum
energy of
space
Quintessence
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NASA/CXC/M.Weiss
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Hubble HUDF team
13.772±0.059 billion years
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EXOPLANETS…
…AND HOW TO FIND THEM
WED 6TH
MARCH 1PM