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A Spectroscopic View on Cosmic PAH Emission.
Acc Chem Res
April 2021
Leiden Observatory, Leiden University, Leiden, The Netherlands.
ConspectusPolycyclic aromatic hydrocarbon molecules (PAHs) are ubiquitously present at high abundances in the Universe. They are detected through their infrared (IR) fluorescence UV pumped by nearby massive stars. Hence, their infrared emission is used to determine the star formation rate in galaxies, one of the key indicators for understanding the evolution of galaxies.
View Article and Find Full Text PDFDigging Deeper: Observing Primordial Gravitational Waves below the Binary-Black-Hole-Produced Stochastic Background.
Phys Rev Lett
April 2017
LIGO, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA.
The merger rate of black hole binaries inferred from the detections in the first Advanced LIGO science run implies that a stochastic background produced by a cosmological population of mergers will likely mask the primordial gravitational wave background. Here we demonstrate that the next generation of ground-based detectors, such as the Einstein Telescope and Cosmic Explorer, will be able to observe binary black hole mergers throughout the Universe with sufficient efficiency that the confusion background can potentially be subtracted to observe the primordial background at the level of Ω_{GW}≃10^{-13} after 5 years of observation.
View Article and Find Full Text PDFThe universe that surrounds us is vast, and we are so very small. When we reflect on the vastness of the universe, our humdrum cosmic location, and the inevitable future demise of humanity, our lives can seem utterly insignificant. Many philosophers assume that such worries about our significance reflect a banal metaethical confusion.
View Article and Find Full Text PDFLorentz transformation of blackbody radiation.
Phys Rev E Stat Nonlin Soft Matter Phys
October 2013
Department of Physics, University of Michigan, Ann Arbor, Michigan 48109-1040, USA.
We present a simple calculation of the Lorentz transformation of the spectral distribution of blackbody radiation at temperature T. Here we emphasize that T is the temperature in the blackbody rest frame and does not change. We thus avoid the confused and confusing question of how temperature transforms.
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