dark matter and dark energy: the evidence · 2018. 10. 17. · dark matter and dark energy: the...

Dark matter and dark energy: the evidence 1933 Fritz Zwicky provides the first evidence for the existence of dark matter by studying the Coma galaxy cluster. First hint of dark matter F. Zwicky (P.D. [WC]) V. Rubin (Carnegie Instit. Washington) 1970s Vera Rubin’s team gathers convincing evidence for dark matter in galaxies by studying their rotational motion. Further evidence 1998-1999 The Supernova Cosmology Project and the High-Z Supernova Search Team, led by Saul Perlmutter, Brian Schmidt and Adam Riess, measure the accelerated expansion of the universe (2011 Nobel Prize). Dark energy discovery a) B. Schmidt (M. Pössel) b) S. Perlmutter (H. Motzkau, [CC]) c) A. Riess (H. Motzkau, [CC]) a c b 06 2009-2013 The Planck Satellite measures with amazing accuracy the cosmic microwave background radiation, confirming the existence of dark matter and dark energy. Accurate measurement Illustration of Planck spacecraft (ESA/AOES Medialab) While dark matter attracts visible matter and enhances the formation of galaxies, dark energy has the opposite effect due to its repulsive nature. The distribution of galaxies and their motion within clusters are also affected by dark matter. Clustering Fornax Cluster (ESO/J. Emerson/VISTA. Ackn.: Cambridge Astronomical Survey Unit) By looking at how fast gas and stars move in and around galaxies, we can estimate their mass. Curiously, this mass is much larger than we can explain by the visible matter. Since the missing mass does not emit or absorb light, we call it dark matter. Dark matter is believed to be distributed in giant clouds, called halos, around galaxies. These clouds are roughly ten times larger and more massive than the observed galaxy. Observation of galaxies M83 Galaxy (ESO) At the end of their life, massive stars undergo a gigantic explosion called a “supernova”. As shown above, the brightness of such explosions is comparable with that of galaxies. By measuring their luminosity, it was found that supernovae are moving away from us in an accelerated way. This was the first observational evidence that the universe is in an accelerated expansion which requires some unknown form of energy, called dark energy. Supernovae Supernova 1994D in galaxy NGC 4526 (NASA/ESA, The Hubble Key Project Team and The High-Z Supernova Search Team) Light bending Quasar and galaxy gravitationally lensed by galaxy cluster SDSS J1004+4112 (ESA, NASA, K. Sharon (Tel Aviv U.) and E. Ofek (Caltech)) The way light rays bend depends on both the amount and the distribution of visible and dark matter. In the picture above, a galaxy cluster distorts the light coming from galaxies and quasars that are even further away, changing their shape and size and even creating multiple images of the same object. Three images of the same galaxy Four images of the same quasar

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Dark matter and dark energy:the evidence

1933 Fritz Zwicky provides

the first evidence for the existence of dark matter by studying the Coma galaxy cluster.

First hint of dark matter

F. Zwicky (P.D. [WC])

V. Rubin (Carnegie Instit. Washington)

1970

s Vera Rubin’s team gathers convincing evidence for dark matter in galaxies bystudying their rotationalmotion.

Further evidence

1998

-199

9 The Supernova Cosmology Project and the High-Z Supernova Search Team, led by Saul Perlmutter, Brian Schmidt and Adam Riess, measure the accelerated expansion of theuniverse (2011 Nobel Prize).

Dark energy discovery

a) B. Schmidt (M. Pössel)b) S. Perlmutter (H. Motzkau, [CC])

c) A. Riess (H. Motzkau, [CC])

a cb

2009

-201

3 The Planck Satellite measures with amazing accuracy the cosmicmicrowave background radiation, confirming the existence of dark matter and dark energy.

Accurate measurement

Illustration of Planck spacecraft (ESA/AOES Medialab)

While dark matter attracts visible matter and enhances the formation ofgalaxies, dark energy has the opposite effect due to its repulsive nature.

The distribution of galaxies and theirmotion within clusters are also affectedby dark matter.

Clustering

Fornax Cluster (ESO/J. Emerson/VISTA. Ackn.: Cambridge Astronomical Survey Unit)

By looking at how fast gas and starsmove in and around galaxies, we canestimate their mass. Curiously, thismass is much larger than we can explain by the visible matter.

Since the missing mass does not emitor absorb light, we call it dark matter.Dark matter is believed to be distributedin giant clouds, called halos, aroundgalaxies. These clouds are roughly tentimes larger and more massive thanthe observed galaxy.

Observation of galaxies

M83 Galaxy (ESO)

At the end of their life, massive starsundergo a gigantic explosion called a “supernova”. As shown above, thebrightness of such explosions iscomparable with that of galaxies.

By measuring their luminosity, it wasfound that supernovae are movingaway from us in an accelerated way.

This was the first observationalevidence that the universe is in anaccelerated expansion which requiressome unknown form of energy, calleddark energy.

Supernovae

Supernova 1994D in galaxy NGC 4526 (NASA/ESA, The Hubble Key Project Team and The High-Z Supernova Search Team)

Light bending

Quasar and galaxy gravitationally lensed by galaxy cluster SDSS J1004+4112 (ESA, NASA, K. Sharon (Tel Aviv U.) and E. Ofek (Caltech))

The way light rays bend depends onboth the amount and the distribution ofvisible and dark matter.

In the picture above, a galaxy clusterdistorts the light coming from galaxiesand quasars that are even further away, changing their shape and size and even creating multiple images of the same object.

Three images of the same galaxyFour images of the same quasar

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