A $\gamma$-ray determination of the Universe's star-formation history

The Fermi-LAT Collaboration,; Ajello, M.; Helgason, K.; Paliya, V.; Finke, J.; Dominguez, A.; Desai, A.

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A $\gamma$-ray determination of the Universe's star-formation history

MPS-Authors

The Fermi-LAT Collaboration,
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

Ajello, M.
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

Helgason, K.
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

Paliya, V.
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

Finke, J.
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

Dominguez, A.
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

Desai, A.
Max Planck Institute for Physics, Max Planck Society and Cooperation Partners;

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引用

The Fermi-LAT Collaboration, Ajello, M., Helgason, K., Paliya, V., Finke, J., Dominguez, A., & Desai, A. (2018). A $\gamma$-ray determination of the Universe's star-formation history. Science Magazine, (362), 1031. Retrieved from https://publications.mppmu.mpg.de/?action=search&mpi=MPP-2018-380.

引用: https://hdl.handle.net/21.11116/0000-0003-F971-5

要旨

The light emitted by all galaxies over the history of the Universe produces the extragalactic background light (EBL) at ultraviolet, optical, and infrared wavelengths. The EBL is a source of opacity for $\gamma$ rays via photon-photon interactions, leaving an imprint in the spectra of distant $\gamma$-ray sources. We measure this attenuation using {739} active galaxies and one gamma-ray burst detected by the {\it Fermi} Large Area Telescope. This allows us to reconstruct the evolution of the EBL and determine the star-formation history of the Universe over 90\% of cosmic time. Our star-formation history is consistent with independent measurements from galaxy surveys, peaking at redshift $z\sim2$. Upper limits of the EBL at the epoch of re-ionization suggest a turnover in the abundance of faint galaxies at $z\sim 6$.