Inflation and Dark Energy from spectroscopy at $z > 2$. (arXiv:1903.09208v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_M/0/1/0/all/0/1">Michael J. Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abidi_M/0/1/0/all/0/1">Muntazir Abidi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_D/0/1/0/all/0/1">David Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansarinejad_B/0/1/0/all/0/1">Behzad Ansarinejad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Armstrong_R/0/1/0/all/0/1">Robert Armstrong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asorey_J/0/1/0/all/0/1">Jacobo Asorey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avelino_A/0/1/0/all/0/1">Arturo Avelino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baccigalupi_C/0/1/0/all/0/1">Carlo Baccigalupi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bandura_K/0/1/0/all/0/1">Kevin Bandura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nicholas Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bavdhankar_C/0/1/0/all/0/1">Chetan Bavdhankar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernal_J/0/1/0/all/0/1">José Luis Bernal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beutler_F/0/1/0/all/0/1">Florian Beutler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biagetti_M/0/1/0/all/0/1">Matteo Biagetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanc_G/0/1/0/all/0/1">Guillermo A. Blanc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blazek_J/0/1/0/all/0/1">Jonathan Blazek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolton_A/0/1/0/all/0/1">Adam S. Bolton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borrill_J/0/1/0/all/0/1">Julian Borrill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frye_B/0/1/0/all/0/1">Brenda Frye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_Geer_E/0/1/0/all/0/1">Elizabeth Buckley-Geer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bull_P/0/1/0/all/0/1">Philip Bull</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgess_C/0/1/0/all/0/1">Cliff Burgess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Byrnes_C/0/1/0/all/0/1">Christian T. Byrnes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_Z/0/1/0/all/0/1">Zheng Cai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castander_F/0/1/0/all/0/1">Francisco J Castander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castorina_E/0/1/0/all/0/1">Emanuele Castorina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_T/0/1/0/all/0/1">Tzu-Ching Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaves_Montero_J/0/1/0/all/0/1">Jonás Chaves-Montero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_S/0/1/0/all/0/1">Shi-Fan Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_X/0/1/0/all/0/1">Xingang Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balland_C/0/1/0/all/0/1">Christophe Balland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yeche_C/0/1/0/all/0/1">Christophe Yèche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cohn_J/0/1/0/all/0/1">J.D. Cohn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coulton_W/0/1/0/all/0/1">William Coulton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Courtois_H/0/1/0/all/0/1">Helene Courtois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Croft_R/0/1/0/all/0/1">Rupert A. C. Croft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cyr_Racine_F/0/1/0/all/0/1">Francis-Yan Cyr-Racine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAmico_G/0/1/0/all/0/1">Guido D'Amico</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_K/0/1/0/all/0/1">Kyle Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delabrouille_J/0/1/0/all/0/1">Jacques Delabrouille</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dey_A/0/1/0/all/0/1">Arjun Dey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dore_O/0/1/0/all/0/1">Olivier Doré</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Douglass_K/0/1/0/all/0/1">Kelly A. Douglass</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yutong_D/0/1/0/all/0/1">Duan Yutong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dvorkin_C/0/1/0/all/0/1">Cora Dvorkin</a>, et al. (97 additional authors not shown)
The expansion of the Universe is understood to have accelerated during two
epochs: in its very first moments during a period of Inflation and much more
recently, at $z < 1$, when Dark Energy is hypothesized to drive cosmic
acceleration. The undiscovered mechanisms behind these two epochs represent
some of the most important open problems in fundamental physics. The large
cosmological volume at $2 < z < 5$, together with the ability to efficiently
target high-$z$ galaxies with known techniques, enables large gains in the
study of Inflation and Dark Energy. A future spectroscopic survey can test the
Gaussianity of the initial conditions up to a factor of ~50 better than our
current bounds, crossing the crucial theoretical threshold of
$sigma(f_{NL}^{rm local})$ of order unity that separates single field and
multi-field models. Simultaneously, it can measure the fraction of Dark Energy
at the percent level up to $z = 5$, thus serving as an unprecedented test of
the standard model and opening up a tremendous discovery space.
The expansion of the Universe is understood to have accelerated during two
epochs: in its very first moments during a period of Inflation and much more
recently, at $z < 1$, when Dark Energy is hypothesized to drive cosmic
acceleration. The undiscovered mechanisms behind these two epochs represent
some of the most important open problems in fundamental physics. The large
cosmological volume at $2 < z < 5$, together with the ability to efficiently
target high-$z$ galaxies with known techniques, enables large gains in the
study of Inflation and Dark Energy. A future spectroscopic survey can test the
Gaussianity of the initial conditions up to a factor of ~50 better than our
current bounds, crossing the crucial theoretical threshold of
$sigma(f_{NL}^{rm local})$ of order unity that separates single field and
multi-field models. Simultaneously, it can measure the fraction of Dark Energy
at the percent level up to $z = 5$, thus serving as an unprecedented test of
the standard model and opening up a tremendous discovery space.
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