Cosmology with Fermi -LAT Alberto Domnguez Universidad Complutense - - PowerPoint PPT Presentation

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Cosmology with Fermi -LAT Alberto Domnguez Universidad Complutense - - PowerPoint PPT Presentation

Dec 16, 2023 364 likes •809 views

Cosmology with Fermi -LAT Alberto Domnguez Universidad Complutense de Madrid M. Ajello, K. Helgason, J. Finke, A. Desai, V. Paliya and also R. Wojtak, F. Prada, L. Marcotulli, D. Hartmann Fermi -LAT Collaboration, 2018, Science, 362, 1031

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Alberto Domínguez

Universidad Complutense de Madrid

  • M. Ajello, K. Helgason, J. Finke, A. Desai, V. Paliya

and also R. Wojtak, F. Prada, L. Marcotulli, D. Hartmann

Domínguez, Primack, Bell Scientific American, June 2015

Cosmology with Fermi-LAT

Fermi-LAT Collaboration, 2018, Science, 362, 1031 Desai et al., 2019, ApJL, 874, 7 Domínguez et al., 2019, arXiv:1903.12097 TAUP – Toyama, Japan - September 9-13, 2019

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Galaxy Evolution and Cosmology Galaxy Evolution and Cosmology Ω Ωb

b baryons

baryons Ω ΩΛ

Λ dark energy

Ω ΩD

D

dark matter Ω Ωm

m = Ω

= Ωb

b + Ω

+ ΩD

D

Ω Ωm

m + Ω

+ ΩΛ

Λ= 1

= 1

Scientific American, June 2015

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Cooray 2016 Artistic representation

  • f a binary system

Artistic representation

  • f a blazar

Orion Nebula (birth place of stars) Crab Nebula

Cosmic Diffuse Extragalactic Backgrounds Cosmic Diffuse Extragalactic Backgrounds

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Extragalactic Background Light (Local) Extragalactic Background Light (Local)

z = 0

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Extragalactic Background Light (Evolution) Extragalactic Background Light (Evolution)

Strong divergence

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Ilustration: Nina McCurdy & Joel Primack

Gamma-ray Attenuation Gamma-ray Attenuation

Telescopes: Fermi-LAT and Imaging Atmospheric Cherenkov Telescopes (IACTs) Pair-production interaction Extragalactic source: e.g. Blazar

Blazars: AGNs emitting at all wavelength with energetic jets pointing towards us. Reverse of most known electron-positron annhilation process

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Ilustration: Nina McCurdy & Joel Primack

EBL photon density evolution

Gamma-ray Attenuation Gamma-ray Attenuation

distance cross section

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Gamma-ray Telescopes Gamma-ray Telescopes

Fermi-LAT

VERITAS, Arizona (USA) MAGIC, La Palma (Spain) H.E.S.S., Namibia

All-sky, Energy range 100 MeV – 100 GeV IACTs Small field of view, High sensitivity, Energy range 100 GeV – 10s TeV

CTA North, La Palma (Spain)

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NASA’s Fermi Gamma-Ray Space Telescope NASA’s Fermi Gamma-Ray Space Telescope

  • 1. Tracking system:
  • convert an incident gamma-ray to an electron-positron pair
  • reconstruct the gamma-ray direction from the tracks of the pair
  • 2. Calorimeter:
  • measure the photon energy
  • 3. Anti-coincidence detector:
  • limit the cosmic-ray background
  • Wide fjeld of view (2.4 sr

, 20% of the sky)

  • Large efgective area (~0.9 m2

above 1 GeV)

  • Low dead time (~27 μs*

s )

Launch June 11, 2008 Celebrating 10th year Anniversary

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Optical Depths from Gamma-ray Data Optical Depths from Gamma-ray Data

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Optical Depths from Gamma-ray Data Optical Depths from Gamma-ray Data

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Optical Depths from Gamma-ray Data Optical Depths from Gamma-ray Data

From detection (2012) to characterization (Now) 4 billion years

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Cosmic Gamma-Ray Horizon Cosmic Gamma-Ray Horizon

See also Fazio & Stecker 1970, Domínguez et al. 2013

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Galaxy Luminosity Densities and EBL Galaxy Luminosity Densities and EBL

Luminosity density evolution as sum

  • f log-normal distributions that can

evolve independently

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Galaxy Luminosity Densities and EBL Galaxy Luminosity Densities and EBL

First EBL determination at z>0

z = 0

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Cosmic Star Formation Rate Cosmic Star Formation Rate

UV (0.16 microns) to SFR: (1) Initial Mass Function (2) Average Galaxy Extinction

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Optical Depths from Gamma-ray Data Optical Depths from Gamma-ray Data

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Extragalactic Background Light from Gamma Rays Extragalactic Background Light from Gamma Rays

Local Extragalactic Background Light

(also see works by the MAGIC, VERITAS, and H.E.S.S. Collaborations)

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Tension on H Tension on H0

0 Measurements

Measurements

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Ilustration: Nina McCurdy & Joel Primack

EBL photon density evolution

Gamma-ray Attenuation Gamma-ray Attenuation

See Domínguez & Prada 13, Biteau & Williams 15

distance cross section

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Measuring H Measuring H0

0 with Gamma-ray Attenuation

with Gamma-ray Attenuation

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Tension on H Tension on H0

0 Measurements

Measurements

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Measuring H Measuring H0

0 and

and Ω Ωm

mwith Gamma-ray Attenuation

with Gamma-ray Attenuation

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Take Home Messages Take Home Messages

1.- Very significant detection and characterization of the EBL attenuation up to z~3. 2.- Complete derivation so far of the local EBL and its evolution over redshift from Fermi-LAT and Cherenkov data. 3.- Derived Cosmic Star formation Rate Density up to z~5 unbiased from different galaxy survey incompleteness. 4.- Cosmological measurement of H0 and Ωm from our independent technique.

Gamma-ray astronomy has matured enough to provide useful measurements in galaxy evolution and cosmology

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Backup Backup

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Measuring the Extragalactic Background Light Measuring the Extragalactic Background Light

DIRBE imaged the sky in 10 photometric bands from 1.25 to 240 microns with a beam size of 0.7x0.7 sq. degrees

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Measuring the Extragalactic Background Light Measuring the Extragalactic Background Light

EBL is an order of magnitude lower than foregrounds and subject to large systematic uncertainties, e.g. Gorjian+ 00

Zodiacal light, visible under the right conditions: typically after the sunset in Spring and right before sunrise in Autumn EBL

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Measuring the Extragalactic Background Light Measuring the Extragalactic Background Light

  • ptical

M31 view from the UV to the far-IR, Credit: NASA & ESA UV near-IR mid-IR far-IR Stars + AGNs Dust + AGNs

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Measuring the Extragalactic Background Light Measuring the Extragalactic Background Light

Number counts in the Hubble Deep Field, e.g. Madau & Pozzetti, 2000

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Measuring the Extragalactic Background Light Measuring the Extragalactic Background Light

  • ptical

M31 view from the UV to the far-IR, Credit: NASA & ESA UV near-IR mid-IR far-IR

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Measuring the Extragalactic Background Light Measuring the Extragalactic Background Light

Theoretical Observational Direct galaxy

  • bservations

Indirect observations (e.g. Kneiske+ 10; Finke+ 10; Khaire+ 14)

Over redshift

(e.g. Domínguez+ 11; Helgason+ 12; Stecker+ 16)

Local

(e.g. Stecker+ 06; Franceschini+ 08)

Theoretical

(e.g. Gilmore+ 12; Inoue+ 13)

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Gamma-ray Cherenkov Telescopes (IACTs) Gamma-ray Cherenkov Telescopes (IACTs)

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Gamma-ray Cherenkov Telescopes (IACTs) Gamma-ray Cherenkov Telescopes (IACTs)

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Gamma-ray Cherenkov Telescopes (IACTs) Gamma-ray Cherenkov Telescopes (IACTs)

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The Gamma-Ray Sky The Gamma-Ray Sky

2000 2018

Fermi-LAT All-Sky Map Above 1 GeV

2000

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Gamma-ray Gamma-ray Fermi-LAT Catalogs Fermi-LAT Catalogs

3FGL 1FHL 2FHL 3FHL 4 years (P7Rep), 3033 sources 3 years (P7), 514 sources 6.7 years (P8), 360 sources 7 years (P8), 1556 sources 8 years (P8), 5065 sources 4FGL

0.1 1 100 1 10 1000

GeV

3FGL 1FHL 4 years (P7Rep), 3033 sources 3 years (P7), 514 sources 6.7 years (P8), 360 sources

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Blazars Blazars

Boston University - Cosmovision

Emission described by homogeneous synchrotron/synchrotron-self Compton model.

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Cosmology Dependence on the Optical Depth Cosmology Dependence on the Optical Depth

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Comparison with other Methodologies Comparison with other Methodologies

Combination of techniques is important to control systematics

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EBL models: Finke+ 10 EBL models: Finke+ 10

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EBL models: Domínguez+ 11 EBL models: Domínguez+ 11

Total: 5986 galaxies

EGS field 0.7 sq. deg.

SED fitting

Galaxy luminosity function rest-frame K-band, Cirasuolo+ 10

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Re-ionization of the Universe Re-ionization of the Universe

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Re-ionization of the Universe Re-ionization of the Universe

Constraints from gamma-ray attenuation