Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by...

17
Introduction to Cosmology Lecture 9 2001:WMAP (NASA) 2009: Planck (ESA) 1998: BOOMERanG (Caltech/Rome) 1989: COBE (NASA)

Transcript of Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by...

Page 1: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

Introduction to CosmologyLecture 9

2001:WMAP (NASA)2009: Planck (ESA)

1998: BOOMERanG (Caltech/Rome)1989: COBE (NASA)

Page 2: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 3: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 4: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 5: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

H atom

Page 6: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 7: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 8: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

Robert Dicke Jim Peebles

Page 9: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

George Gamow

Page 10: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

2001:WMAP (NASA)2009: Planck (ESA)

1998: BOOMERanG (Caltech/Rome)1989: COBE (NASA)

Page 11: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

δT

T(θ,φ) =

T (θ,φ)− �T ��T �

Page 12: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 13: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

δT

T(θ,φ) =

T (θ,φ)− �T ��T �

Page 14: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 15: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 16: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably
Page 17: Introduction to Cosmology Lecture 9pettini/Intro... · The Cosmic Microwave Background as seen by Planck and WMAP WMAP Planck . 100 10 100 10 150 10 -200 10 105 inflation probably

Spettrofotometria - Docenti Unifem.docente.unife.it/francesco.bernardi/materiale-didattico... · h costante di Planck= 6.63x10-34 Joule ... Esistono quindi vari tipi di radiazione

Spettrofotometria - Docenti Unifem.docente.unife.it/francesco.bernardi/materiale-didattico... · h costante di Planck= 6.63x10-34 Joule ... Esistono quindi vari tipi di radiazione

Anastasia Fialkov - Max Planck Society · Anastasia Fialkov Tel Aviv University MPIK 29.10.2012 Credit: WMAP team Based on: AF, Itzhaki, Kovetz(JCAP 2010) Rathaus,AF, Itzhaki(JCAP

Anastasia Fialkov - Max Planck Society · Anastasia Fialkov Tel Aviv University MPIK 29.10.2012 Credit: WMAP team Based on: AF, Itzhaki, Kovetz(JCAP 2010) Rathaus,AF, Itzhaki(JCAP

Planck E A Radiacao Do Corpo Negro

Planck E A Radiacao Do Corpo Negro

[eV] - neutrino.pd.infn.itneutrino.pd.infn.it/lezioni/Corso2004/MisureDirette.pdf · Dopo gli ultimi dati di WMAP (astro-ph/0302209). i m i < 0. 25 eV (95%CL) k (h Mpc ... E’ necessario

[eV] - neutrino.pd.infn.itneutrino.pd.infn.it/lezioni/Corso2004/MisureDirette.pdf · Dopo gli ultimi dati di WMAP (astro-ph/0302209). i m i < 0. 25 eV (95%CL) k (h Mpc ... E’ necessario

Subir Sarkarh2 ≈ 0.018 → BBN √ ⇒ baryon fraction in clusters ~10% √ SDSS (note that Σ m ν ≈ 1.5 eV … well above ‘WMAP bound’) The small-scale power would be excessive

Subir Sarkarh2 ≈ 0.018 → BBN √ ⇒ baryon fraction in clusters ~10% √ SDSS (note that Σ m ν ≈ 1.5 eV … well above ‘WMAP bound’) The small-scale power would be excessive

NASA/WMAP Science μ Team€¦ · causes the count loss due to timewalk of the ASDs. All hits must be considered even when they do not coincide in a clock interval. ①All hits ②Coincident

NASA/WMAP Science μ Team€¦ · causes the count loss due to timewalk of the ASDs. All hits must be considered even when they do not coincide in a clock interval. ①All hits ②Coincident

Planck evidence for a closed Universe and a possible ... · the evidence for a closed universe from Planck, showing that positive curvature naturally explains the anomalous lensing

Planck evidence for a closed Universe and a possible ... · the evidence for a closed universe from Planck, showing that positive curvature naturally explains the anomalous lensing

Julian Heeck 24.9 - Max Planck Society · The Big Bang Theory Julian Heeck Implications of In ation on Particle Physics 1/26

Julian Heeck 24.9 - Max Planck Society · The Big Bang Theory Julian Heeck Implications of In ation on Particle Physics 1/26

SINVAL FERNANDES DE SOUSA - repositorio.ufu.br · τ Tempo de vida de emissão h Constante de Planck (6,62 x 10-34 m2 kg s-1) ν Frequência da radiação OLEDs Diodos orgânicos

SINVAL FERNANDES DE SOUSA - repositorio.ufu.br · τ Tempo de vida de emissão h Constante de Planck (6,62 x 10-34 m2 kg s-1) ν Frequência da radiação OLEDs Diodos orgânicos

Planck Report on the status of the mission Carlo Baccigalupi, SISSA.

Planck Report on the status of the mission Carlo Baccigalupi, SISSA.

AGASA Masahiro Teshima Max-Planck-Institut für Physik, München, Germany for AGASA collaboration.

AGASA Masahiro Teshima Max-Planck-Institut für Physik, München, Germany for AGASA collaboration.

1 Geometry of pure states - Max Planck Societyissqui05/ZRAUM1A.pdf · 1.5 Mandelstam-Tam-inequality We see from (8) that cosfi • jh ˆ0;ˆ1ij (10) Therefore, we have the following

1 Geometry of pure states - Max Planck Societyissqui05/ZRAUM1A.pdf · 1.5 Mandelstam-Tam-inequality We see from (8) that cosfi • jh ˆ0;ˆ1ij (10) Therefore, we have the following

The Alpha Magnetic Spectrometer (AMS) Experimentcyclo.mit.edu/AMITS/MIT.Student/MIT-Student-Presentation.pdf · KKKK MMMM FFFF EEE HHHH Shaded region allowed by WMAP, etc. AMS is

The Alpha Magnetic Spectrometer (AMS) Experimentcyclo.mit.edu/AMITS/MIT.Student/MIT-Student-Presentation.pdf · KKKK MMMM FFFF EEE HHHH Shaded region allowed by WMAP, etc. AMS is

Planck-Weltraumteleskop Vortrag von Veronika Neuhauser und Peter Hausegger.

Planck-Weltraumteleskop Vortrag von Veronika Neuhauser und Peter Hausegger.

Thirty Years Ago!. At the Max Planck CdTe Resonant Brillouin Scattering.

Thirty Years Ago!. At the Max Planck CdTe Resonant Brillouin Scattering.

TheUsesofReflectionPositivity - ETH Z · TheUsesofReflectionPositivity Erhard Seiler Max-Planck-Institut fur¨ Physik, Munchen¨ (Werner-Heisenberg-Institut) Schrader memorial,

TheUsesofReflectionPositivity - ETH Z · TheUsesofReflectionPositivity Erhard Seiler Max-Planck-Institut fur¨ Physik, Munchen¨ (Werner-Heisenberg-Institut) Schrader memorial,

Wlodek Bednarek - Max Planck Society

Wlodek Bednarek - Max Planck Society

AGASA Results Masahiro Teshima Max-Planck-Institut für Physik, München, Germany for AGASA collaboration.

AGASA Results Masahiro Teshima Max-Planck-Institut für Physik, München, Germany for AGASA collaboration.

Constraining Inert Dark Matter by R and WMAP data · 2019. 11. 10. · Constraining Inert Dark Matter by R and WMAP data Maria Krawczyk, Dorota Soko lowska, Pawe l Swaczyna, Bogumi

Constraining Inert Dark Matter by R and WMAP data · 2019. 11. 10. · Constraining Inert Dark Matter by R and WMAP data Maria Krawczyk, Dorota Soko lowska, Pawe l Swaczyna, Bogumi

PARAMERI COSMOLOGICI DETERMINAZIONE DI Ω m E Ω Λ DA SN 1A & WMAP Marco Nardini Cosmologia Osservativa anno accademico 2004-2005.

PARAMERI COSMOLOGICI DETERMINAZIONE DI Ω m E Ω Λ DA SN 1A & WMAP Marco Nardini Cosmologia Osservativa anno accademico 2004-2005.