CWRU PAT Coffee Agenda

Tuesdays 10:30 - 11:30 | Fridays 11:30 - 12:30

+1 Gravitational-Wave Lunar Observatory for Cosmology.

bump   cxt282 +1

+1 Resilience of long modes in cosmological observables.

cxt282 +1

+1 From AdS to dS Exchanges: Spectral Representation, Mellin Amplitudes and Crossing.

lxj154 +1

Showing votes from 2020-07-17 12:30 to 2020-07-21 11:30 | Next meeting is Friday Aug 22nd, 11:30 am.

users

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astro-ph.CO

  • Gravitational-Wave Lunar Observatory for Cosmology.- [PDF] - [Article]

    Karan Jani, Abraham Loeb
     

    Several large-scale experimental facilities and space-missions are being suggested to probe the universe across the gravitational-wave (GW) spectrum. Here we propose Gravitational-wave Lunar Observatory for Cosmology (GLOC) - the first concept design in the NASA Artemis era for a GW observatory on the Moon. We find that a lunar-based observatory is ideal for probing GW frequencies in the range between deci-Hz to 5 Hz, an astrophysically rich regime that is very challenging for both Earth- and space-based detectors. GLOC can survey $\gtrsim 70\%$ of the observable volume of our universe without significant background contamination. Its unprecedented sensitivity would trace the Hubble expansion rate up to redshift $z \sim 3$ and test General Relativity and $\Lambda$CDM cosmology up to $z\sim 100$.

  • Resilience of long modes in cosmological observables.- [PDF] - [Article]

    Sabino Matarrese, Luigi Pilo, Rocco Rollo
     

    By a careful implementation of gauge transformations involving long-wavelength modes, we show that a variety of effects involving squeezed bispectrum configurations, for which one Fourier mode is much shorter than the other two, cannot be gauged away, except for the unphysical exactly infinite-wavelength ($k=0$) limit. Our result applies, in particular, to the Maldacena consistency relation for single-field inflation, yielding a local non-Gaussianity strength $f_{\rm NL}^{\rm local} = - (5/12)(n_S-1)$ (with $n_S$ the primordial spectral index of scalar perturbations), and to the $f_{\rm NL}^{\rm GR} = -5/3$ term, appearing in the dark matter bispectrum and in the halo bias, as a consequence of the general relativistic non-linear evolution of matter perturbations. Such effects are therefore physical and observable in principle by future high-sensitivity experiments.

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