Search

Your search keyword '"Chen Xingang"' showing total 17 results
Start Over Author "Chen Xingang" Topic astrophysics::cosmology and extragalactic astrophysics
17 results on '"Chen Xingang"'

1. Early-Universe-Physics Insensitive and Uncalibrated Cosmic Standards: Constraints on $��_{\rm{m}}$ and Implications for the Hubble Tension

Author

Lin, Weikang, Chen, Xingang, and Mack, Katherine J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

To further shed light on whether pre-recombination models can resolve the Hubble tension, we explore constraints on the cosmic background evolution that are insensitive to early-universe physics. The analysis of the cosmic microwave background (CMB) anisotropy has been thought to highly rely on early-universe physics. However, we show that the fact that the sound horizon at recombination being close to that at the end of the drag epoch is insensitive to early-universe physics. This allows us to link the absolute sizes of the two horizons and treat them as free parameters. Jointly, the CMB peak angular size, Baryon Acoustic Oscillations (BAO), and Type Ia supernovae can be used as "early-universe-physics insensitive and uncalibrated cosmic standards", which measure the cosmic history from recombination to today. They can set strong and robust constraints on the post-recombination cosmic background, especially the matter density parameter with $��_{\rm{m}}=0.302\pm0.008$ ($68\%$ C.L.) assuming a flat $��$CDM after recombination. When we combine these with other non-local observations, we obtain several constraints on $H_0$ with significantly reduced sensitivity to early-universe physics. These are all more consistent with the Planck 2018 result than the local measurement results such as those based on Cepheids. This suggests a tension between the post-recombination, but non-local, observations and the local measurements which cannot be resolved by modifying pre-recombination early universe physics., Results updated with stellar-age constraints; conclusion unchanged. Accepted for publication in ApJ

Published
2021
Full Text
View/download PDF

2. Astro2020 Science White Paper: Primordial Non-Gaussianity

Author

Meerburg, P. Daniel, Green, Daniel, Abidi, Muntazir, Amin, Mustafa A., Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Ávila, Santiago, Baccigalupi, Carlo, Baldauf, Tobias, Ballardini, Mario, Bandura, Kevin, Bartolo, Nicola, Battaglia, Nicholas, Baumann, Daniel, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Bischoff, Colin, Blazek, Jonathan, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Burgess, Cliff, Byrnes, Christian, Calabrese, Erminia, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chen, Xingang, Yeche, Christophe, Cooray, Asantha, Coulton, William, Crawford, Thomas, Chisari, Elisa, Cyr-Racine, Francis-Yan, d'Amico, Guido, de Bernardis, Paolo, de La Macorra, Axel, Dore, Olivier, Duivenvoorden, Adri, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fasiello, Matteo, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, Friedrich, Oliver, Garcia-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Goon, Garrett, Gorski, Krzysztof M., Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hawken, Adam J., Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Huterer, Dragan, Kamionkowski, Marc, Karkare, Kirit S., Keeley, Ryan E., Kinney, William, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Madhavacheril, Mathew, Maldacena, Juan, Marsh, M. C. David, Masui, Kiyoshi, Matarrese, Sabino, Mcallister, Liam, Mcmahon, Jeff, Mcquinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, Dizgah, Azadeh Moradinezhad, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Naselsky, Pavel, Nati, Federico, Nicolis, Alberto, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Pajer, Enrico, Padmanabhan, Hamsa, Palma, Gonzalo A., Peiris, Hiranya V., Percival, Will J., Piacentni, Francesco, Pimentel, Guilherme L., Pogosian, Levon, Prescod-Weinstein, Chanda, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Stompor, Radek, Raveri, Marco, Remazeilles, Mathieu, Rocha, Gracca, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shan, Huanyuan, Shandera, Sarah, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Slosar, Anže, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tomasi, Maurizio, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Uhlemann, Cora, Umiltà, Caterina, van Engelen, Alexander, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wandelt, Benjamin, Wang, Yi, Watson, Scott, Wise, Mark, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Yasini, Siavash, Young, Sam, Yutong, Duan, Zaldarriaga, Matias, Zemcov, Michael, Zhao, Gong-Bo, Zheng, Yi, Zhu, Ningfeng, University of Cambridge [UK] (CAM), University of California [San Diego] (UC San Diego), University of California (UC), Universidad Autónoma de Madrid (UAM), Institute of Cosmology and Gravitation [Portsmouth] (ICG), University of Portsmouth, Ecole Polytechnique Fédérale de Lausanne (EPFL), Canadian Institute for Theoretical Astrophysics (CITA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Argonne National Laboratory [Lemont] (ANL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, Facultad de Ingeniería [Buenos Aires] (FIUBA), Universidad de Buenos Aires [Buenos Aires] (UBA), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), National Oceanography Centre [Southampton] (NOC), University of Southampton, Johns Hopkins University (JHU), Korea Astronomy and Space Science Institute (KASI), ICRA and Physics Department, Columbia University [New York], Dipartimento di Fisica 'G. Galilei', Università degli Studi di Padova = University of Padua (Unipd), Kavli Institute for Cosmological Physics [Chicago] (KICP), University of Chicago, School of Physics and Astronomy [Nottingham], University of Nottingham, UK (UON), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Waterloo [Waterloo], University of New Hampshire (UNH), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Catania (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Manchester [Manchester], Brookhaven National Laboratory [Upton, NY] (BNL), UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY)-U.S. Department of Energy [Washington] (DOE), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre for Theoretical Cosmology, Institute for Advanced Study Princeton, School of physics and astronomy, Rochester Institute of Technology, University of California, Universidad Autonoma de Madrid (UAM), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Universidad Nacional Autónoma de México (UNAM), Okayama University, Universita degli Studi di Padova, Smithsonian Institution-Harvard University [Cambridge], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), U.S. Department of Energy [Washington] (DOE)-UT-Battelle, LLC-Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), and Universidad Nacional Autónoma de México - UNAM (MEXICO)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

5 pages + references; Submitted to the Astro2020 call for science white papers. This version: fixed author list; International audience; Our current understanding of the Universe is established through the pristine measurements of structure in the cosmic microwave background (CMB) and the distribution and shapes of galaxies tracing the large scale structure (LSS) of the Universe. One key ingredient that underlies cosmological observables is that the field that sources the observed structure is assumed to be initially Gaussian with high precision. Nevertheless, a minimal deviation from Gaussianityis perhaps the most robust theoretical prediction of models that explain the observed Universe; itis necessarily present even in the simplest scenarios. In addition, most inflationary models produce far higher levels of non-Gaussianity. Since non-Gaussianity directly probes the dynamics in the early Universe, a detection would present a monumental discovery in cosmology, providing clues about physics at energy scales as high as the GUT scale.

Published
2019

3. Inflation and Dark Energy from spectroscopy at $z > 2$

Author

Ferraro, Simone, Wilson, Michael J, Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Blanc, Guillermo A, Blazek, Jonathan, Bolton, Adam S, Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T, Cai, Zheng, Castander, Francisco J, Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jonás, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Yèche, Christophe, Cohn, JD, Coulton, William, Courtois, Helene, Croft, Rupert AC, Cyr-Racine, Francis-Yan, D'Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Doré, Olivier, Douglass, Kelly A, Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G, Font-Ribera, Andreu, Foreman, Simon, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Green, Daniel, Guy, Julien, Hahn, ChangHoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J, Hernández-Aguayo, César, Hložek, Renée, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E, Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A, Kovetz, Ely D, Krause, Elisabeth, Krolewski, Alex, L'Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Lukić, Zarija, Macorra, Axel de la, Plazas, Andrés A, Marshall, Jennifer L, Martini, Paul, Masui, Kiyoshi, McDonald, Patrick, Meerburg, P Daniel, Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D, Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A, Niz, Gustavo, and Padmanabhan, Hamsa

Subjects
astro-ph.GA, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

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.

Published
2019

4. Inflation and Dark Energy from spectroscopy at z > 2

Author

Ferraro, Simone, Wilson, Michael J., Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, Jos�� Luis, Beutler, Florian, Biagetti, Matteo, Blanc, Guillermo A., Blazek, Jonathan, Bolton, Adam S., Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T., Cai, Zheng, Castander, Francisco J, Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jon��s, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Y��che, Christophe, Cohn, J. D., Coulton, William, Courtois, Helene, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D'Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Dor��, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, Garc��a-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Green, Daniel, Guy, Julien, Hahn, ChangHoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J., Hern��ndez-Aguayo, C��sar, Hlo��ek, Ren��e, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E., Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A., Kovetz, Ely D., Krause, Elisabeth, Krolewski, Alex, L'Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Luki��, Zarija, de la Macorra, Axel, Plazas, Andr��s A., Marshall, Jennifer L., Martini, Paul, Masui, Kiyoshi, McDonald, Patrick, Meerburg, P. Daniel, Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niz, Gustavo, Padmanabhan, Hamsa, Palunas, Povilas, Percival, Will J., Piacentini, Francesco, Pieri, Matthew M., Piro, Anthony L., Prakash, Abhishek, Rhodes, Jason, Ross, Ashley J., Rossi, Graziano, Rudie, Gwen C., Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Simon, Joshua D., Simon, Sara, Slepian, Zachary, Slosar, An��e, Sridhar, Srivatsan, Stebbins, Albert, Escoffier, Stephanie, Switzer, Eric R., Tarl��, Gregory, Trodden, Mark, Uhlemann, Cora, Uren��a-L��pez, L. Arturo, Di Valentino, Eleonora, Vargas-Maga��a, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Hong-Ming

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), astro-ph.GA, astro-ph.CO, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

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 $��(f_{NL}^{\rm local})$ 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., Science white paper submitted to the Astro2020 Decadal Survey

Published
2019

5. Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

Author

Green, Daniel, Amin, Mustafa A, Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N, Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Bond, J Richard, Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E, Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D'Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, Engelen, Alexander van, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos AG, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A, Górski, Krzysztof M, Grin, Daniel, Grohs, Evan, Gudmundsson, Jon E, Hanany, Shaul, Handley, Will, Hill, J Colin, Hirata, Christopher M, Hložek, Renée, Holder, Gilbert, Horiuchi, Shunsaku, Huterer, Dragan, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E, Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M, Kovetz, Ely D, L'Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Lin, Tongyan, Loverde, Marilena, Madhavacheril, Mathew, Masui, Kiyoshi, McMahon, Jeff, McQuinn, Matthew, Meerburg, P Daniel, Mirbabayi, Mehrdad, Motloch, Pavel, Mukherjee, Suvodip, Munõz, Julian B, Nagy, Johanna, Newburgh, Laura, Niemack, Michael D, Nomerotski, Andrei, Page, Lyman, Piacentni, Francesco, Pierpaoli, Elena, Pogosian, Levon, and Pryke, Clement

Subjects
High Energy Physics::Phenomenology, astro-ph.CO, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic microwave background (CMB), the large-scale structure, and the primordial light element abundances, and are important in determining the initial conditions of the universe. We argue that future cosmological observations, in particular improved maps of the CMB on small angular scales, can be orders of magnitude more sensitive for probing the thermal history of the early universe than current experiments. These observations offer a unique and broad discovery space for new physics in the dark sector and beyond, even when its effects would not be visible in terrestrial experiments or in astrophysical environments. A detection of an excess light relic abundance would be a clear indication of new physics and would provide the first direct information about the universe between the times of reheating and neutrino decoupling one second later.

Published
2019

6. Dark Matter Science in the Era of LSST

Author

Bechtol, Keith, Drlica-Wagner, Alex, Abazajian, Kevork N., Abidi, Muntazir, Adhikari, Susmita, Ali-Haïmoud, Yacine, Annis, James, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Baccigalupi, Carlo, Banerjee, Arka, Banik, Nilanjan, Bennett, Charles, Beutler, Florian, Bird, Simeon, Birrer, Simon, Biswas, Rahul, Biviano, Andrea, Blazek, Jonathan, Boddy, Kimberly K., Bonaca, Ana, Borrill, Julian, Bose, Sownak, Bovy, Jo, Frye, Brenda, Brooks, Alyson M., Buckley, Matthew R., Buckley-Geer, Elizabeth, Bulbul, Esra, Burchat, Patricia R., Burgess, Cliff, Calore, Francesca, Caputo, Regina, Castorina, Emanuele, Chang, Chihway, Chapline, George, Charles, Eric, Chen, Xingang, Clowe, Douglas, Cohen-Tanugi, Johann, Comparat, Johan, Croft, Rupert Ac, Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, William A., Macorra, Axel La, Valentino, Eleonora Di, Rivero, Ana Díaz, Digel, Seth, Dodelson, Scott, Doré, Olivier, Dvorkin, Cora, Eckner, Christopher, Ellison, John, Erkal, Denis, Farahi, Arya, Fassnacht, Christopher D., Ferreira, Pedro G., Flaugher, Brenna, Foreman, Simon, Friedrich, Oliver, Frieman, Joshua, García-Bellido, Juan, Gawiser, Eric, Gerbino, Martina, Maurizio Giannotti, Gill, Mandeep Ss, Gluscevic, Vera, Golovich, Nathan, Gontcho, Satya Gontcho A., González-Morales, Alma X., Grin, Daniel, Gruen, Daniel, Hearin, Andrew P., Hendel, David, Hezaveh, Yashar D., Hirata, Christopher M., Hložek, Renee, Horiuchi, Shunsaku, Jain, Bhuvnesh, Jee, M. James, Jeltema, Tesla E., Kamionkowski, Marc, Kaplinghat, Manoj, Keeley, Ryan E., Keeton, Charles R., Khatri, Rishi, Koposov, Sergey E., Koushiappas, Savvas M., Kovetz, Ely D., Lahav, Ofer, Lam, Casey, Lee, Chien-Hsiu, Li, Ting S., Liguori, Michele, Lin, Tongyan, Lisanti, Mariangela, Loverde, Marilena, Lu, Jessica R., Mandelbaum, Rachel, Mao, Yao-Yuan, Mcdermott, Samuel D., Mcnanna, Mitch, Medford, Michael, Meerburg, P. Daniel, Meyer, Manuel, Mirbabayi, Mehrdad, Mishra-Sharma, Siddharth, Marc, Moniez, More, Surhud, Moustakas, John, Muñoz, Julian B., Murgia, Simona, Myers, Adam D., Nadler, Ethan O., Necib, Lina, Newburgh, Laura, Newman, Jeffrey A., Nord, Brian, Nourbakhsh, Erfan, Nuss, Eric, O Connor, Paul, Pace, Andrew B., Padmanabhan, Hamsa, Palmese, Antonella, Peiris, Hiranya V., Peter, Annika Hg, Piacentni, Francesco, Piacentini, Francesco, Plazas, Andrés, Polin, Daniel A., Prakash, Abhishek, Prescod-Weinstein, Chanda, Read, Justin I., Ritz, Steven, Robertson, Brant E., Rose, Benjamin, Rosenfeld, Rogerio, Rossi, Graziano, Samushia, Lado, Sánchez, Javier, Sánchez-Conde, Miguel A., Schaan, Emmanuel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Shipp, Nora, Simon, Joshua D., Simon, Sara, Slatyer, Tracy R., Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Straniero, Oscar, Strigari, Louis E., Tait, Tim Mp, Tollerud, Erik, Troxel, Ma, Tyson, J. Anthony, Uhlemann, Cora, Urenña-López, L. Arturo, Verma, Aprajita, Vilalta, Ricardo, Walter, Christopher W., Wang, Mei-Yu, Watson, Scott, Wechsler, Risa H., Wittman, David, Xu, Weishuang, Yanny, Brian, Young, Sam, Yu, Hai-Bo, Zaharijas, Gabrijela, Zentner, Andrew R., Zuntz, Joe, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and HEP, INSPIRE

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 01 natural sciences, Standard Model, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Particle mass, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, hep-ex, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, 13. Climate action, Fundamental physics, astro-ph.CO, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Experiment, dark matter: parameter space, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Astrophysical observations currently provide the only robust, empirical measurements of dark matter. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space. This white paper summarizes astrophysical observations that can constrain the fundamental physics of dark matter in the era of LSST. We describe how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we highlight theoretical work and experimental/observational facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter., 11 pages, 2 figures, Science Whitepaper for Astro 2020, more information at https://lsstdarkmatter.github.io

Published
2019

7. Scratches from the Past: Inflationary Archaeology through Features in the Power Spectrum of Primordial Fluctuations

Author

Slosar, Anze, Abazajian, Kevork N., Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Amin, Mustafa A., Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bleem, Lindsey, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Byrnes, Christian T., Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cohn, J. D., Cooray, Asantha, Cyr-Racine, Francis-Yan, Demarteau, Marcel, Doré, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Ellison, John, Essinger-Hileman, Tom, Fabbian, Giulio, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, A., Górski, Krzysztof M., Green, Daniel, Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hill, J. Colin, Hložek, Renée, Horiuchi, Shunsaku, Huterer, Dragan, Ishak, Mustapha, Johnson, Bradley, Kamionkowski, Marc, Karkare, Kirit S., Keeley, Ryan E., Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Kazuya Koyama, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Martini, Paul, Masui, Kiyoshi, Mcallister, Liam, Mcmahon, Jeff, Daniel Meerburg, P., Meyers, Joel, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Newburgh, Laura, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Palma, Gonzalo A., Penna-Lima, Mariana, Percival, Will J., Piacentini, Francesco, Pierpaoli, Elena, Pogosian, Levon, Prakash, Abhishek, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Starkman, Glenn, Suzuki, Aritoki, Switzer, Eric R., Basu Thakur, Ritoban, Timbie, Peter, Tolley, Andrew J., Tristram, Matthieu, Trodden, Mark, Umiltà, Caterina, Di Valentino, Eleonora, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wang, Yi, Watson, Scott, Whitehorn, Nathan, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Xu, Zhilei, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zhu, Ningfeng, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, fluctuation: primordial, FOS: Physical sciences, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, inflation: model, power spectrum: primordial, inflation: nonminimal, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], astro-ph.CO, structure, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Inflation may provide unique insight into the physics at the highest available energy scales that cannot be replicated in any realistic terrestrial experiment. Features in the primordial power spectrum are generically predicted in a wide class of models of inflation and its alternatives, and are observationally one of the most overlooked channels for finding evidence for non-minimal inflationary models. Constraints from observations of the cosmic microwave background cover the widest range of feature frequencies, but the most sensitive constraints will come from future large-scale structure surveys that can measure the largest number of linear and quasi-linear modes., Comment: 5 pages + references, 1 figure; science white paper submitted to the Astro2020 decadal survey

Published
2019

8. Inflation and Dark Energy from Spectroscopy at $z > 2$

Author

Ferraro, Simone, Wilson, Michael J., Abidi, Muntazir, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Baccigalupi, Carlo, Bandura, Kevin, Battaglia, Nicholas, Bavdhankar, Chetan, Bernal, Joséluis, Beutler, Florian, Matteo Biagetti, Blanc, Guillermo A., Blazek, Jonathan, Bolton, Adam S., Borrill, Julian, Frye, Brenda, Buckley-Geer, Elizabeth, Bull, Philip, Burgess, Cliff, Byrnes, Christian T., Cai, Zheng, Castander, Francisco J., Castorina, Emanuele, Chang, Tzu-Ching, Chaves-Montero, Jonás, Chen, Shi-Fan, Chen, Xingang, Balland, Christophe, Yèche, Christophe, Cohn, J. D., Coulton, William, Courtois, Helene, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D Amico, Guido, Dawson, Kyle, Delabrouille, Jacques, Dey, Arjun, Doré, Olivier, Douglass, Kelly A., Yutong, Duan, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Fan, Xiaohui, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, Satya Gontcho A., Green, Daniel, Guy, Julien, Hahn, Changhoon, Hanany, Shaul, Handley, Will, Hathi, Nimish, Hawken, Adam J., Hernández-Aguayo, César, Hložek, Renée, Huterer, Dragan, Ishak, Mustapha, Kamionkowski, Marc, Karagiannis, Dionysios, Keeley, Ryan E., Kehoe, Robert, Khatri, Rishi, Kim, Alex, Kneib, Jean-Paul, Kollmeier, Juna A., Kovetz, Ely D., Krause, Elisabeth, Krolewski, Alex, L Huillier, Benjamin, Landriau, Martin, Levi, Michael, Liguori, Michele, Linder, Eric, Lukić, Zarija, La Macorra, Axel, Plazas, Andrés A., Marshall, Jennifer L., Martini, Paul, Masui, Kiyoshi, Mcdonald, Patrick, Daniel Meerburg, P., Meyers, Joel, Mirbabayi, Mehrdad, Moustakas, John, Myers, Adam D., Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niz, Gustavo, Padmanabhan, Hamsa, Palunas, Povilas, Percival, Will J., Piacentini, Francesco, Pieri, Matthew M., Piro, Anthony L., Prakash, Abhishek, Rhodes, Jason, Ross, Ashley J., Rossi, Graziano, Rudie, Gwen C., Samushia, Lado, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Simon, Joshua D., Simon, Sara, Slepian, Zachary, Slosar, Anže, Sridhar, Srivatsan, Stebbins, Albert, Escoffier, Stephanie, Switzer, Eric R., Tarlé, Gregory, Trodden, Mark, Uhlemann, Cora, Arturo Urenña-López, L., Di Valentino, Eleonora, Vargas-Magaña, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, Zhu, Hong-Ming, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
cosmological model, non-Gaussianity, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxy, expansion: acceleration, inflation, dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, boundary condition, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

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., Comment: Science white paper submitted to the Astro2020 Decadal Survey

Published
2019

9. Primordial Non-Gaussianity

Author

Meerburg, P. Daniel, Green, Daniel, Abidi, Muntazir, Amin, Mustafa A., Adshead, Peter, Ahmed, Zeeshan, Alonso, David, Ansarinejad, Behzad, Armstrong, Robert, Avila, Santiago, Baccigalupi, Carlo, Baldauf, Tobias, Ballardini, Mario, Bandura, Kevin, Bartolo, Nicola, Battaglia, Nicholas, Baumann, Daniel, Bavdhankar, Chetan, Bernal, José Luis, Beutler, Florian, Biagetti, Matteo, Bischoff, Colin, Blazek, Jonathan, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Bull, Philip, Burgess, Cliff, Byrnes, Christian, Calabrese, Erminia, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonás, Chen, Xingang, Yèche, Christophe, Cooray, Asantha, Coulton, William, Crawford, Thomas, Chisari, Elisa, Cyr-Racine, Francis-Yan, D Amico, Guido, Bernardis, Paolo, La Macorra, Axel, Doré, Olivier, Duivenvoorden, Adri, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fasiello, Matteo, Ferraro, Simone, Flauger, Raphael, Font-Ribera, Andreu, Foreman, Simon, Friedrich, Oliver, García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Goon, Garrett, Górski, Krzysztof M., Gudmundsson, Jon E., Gupta, Nikhel, Hanany, Shaul, Handley, Will, Hawken, Adam J., Hill, J. Colin, Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Huterer, Dragan, Kamionkowski, Marc, Kirit Karkare, Keeley, Ryan E., Kinney, William, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, L Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Loverde, Marilena, Madhavacheril, Mathew, Maldacena, Juan, Marsh, M. C. David, Masui, Kiyoshi, Matarrese, Sabino, Mcallister, Liam, Mcmahon, Jeff, Mcquinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, Moradinezhad Dizgah, Azadeh, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Naselsky, Pavel, Nati, Federico, Newburgh, Nicolis, Alberto, Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, Page, Lyman, Pajer, Enrico, Padmanabhan, Hamsa, Palma, Gonzalo A., Peiris, Hiranya V., Percival, Will J., Piacentni, Francesco, Pimentel, Guilherme L., Pogosian, Levon, Prescod-Weinstein, Chanda, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Stompor, Radek, Raveri, Marco, Remazeilles, Mathieu, Rocha, Graça, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Sasaki, Misao, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shan, Huanyuan, Shandera, Sarah, Sherwin, Blake D., Silverstein, Eva, Simon, Sara, Slosar, Anze, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tomasi, Maurizio, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Uhlemann, Cora, Umiltà, Caterina, Engelen, Alexander, Vargas-Magaña, M., Vieregg, Abigail, Wallisch, Benjamin, Wands, David, Wandelt, Benjamin, Wang, Yi, Watson, Scott, Wise, Mark, Wu, W. L. K., Xianyu, Zhong-Zhi, Xu, Weishuang, Yasini, Siavash, Young, Sam, Yutong, Duan, Zaldarriaga, Matias, Zemcov, Michael, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Ningfeng

Subjects
High Energy Physics - Theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Theory (hep-th), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Our current understanding of the Universe is established through the pristine measurements of structure in the cosmic microwave background (CMB) and the distribution and shapes of galaxies tracing the large scale structure (LSS) of the Universe. One key ingredient that underlies cosmological observables is that the field that sources the observed structure is assumed to be initially Gaussian with high precision. Nevertheless, a minimal deviation from Gaussianityis perhaps the most robust theoretical prediction of models that explain the observed Universe; itis necessarily present even in the simplest scenarios. In addition, most inflationary models produce far higher levels of non-Gaussianity. Since non-Gaussianity directly probes the dynamics in the early Universe, a detection would present a monumental discovery in cosmology, providing clues about physics at energy scales as high as the GUT scale., Comment: 5 pages + references; Submitted to the Astro2020 call for science white papers. This version: fixed author list

Published
2019
Full Text
View/download PDF

10. Anomalous High Energy Dependence in Inflationary Density Perturbations

Author

Chen, Xingang and Wang, Yi

Subjects
High Energy Physics - Theory, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the contribution of spectator massive scalar fields to the inflationary density perturbations through the universal gravitational coupling. We find that such contribution has several remarkable properties: it does not decrease as the mass of the spectator field increases; it has a significant size and cannot be turned off by any adjustable parameters; and it applies to all massive scalars existed during inflation, making the overall effect unexpectedly large. As a result, the primordial density perturbations are anomalously sensitive to the high energy physics., 4 pages

Published
2012

11. CMBPol Mission Concept Study: Probing Inflation with CMB Polarization

Author

Baumann, Daniel, Jackson, Mark G., Adshead, Peter, Amblard, Alexandre, Ashoorioon, Amjad, Bartolo, Nicola, Bean, Rachel, Beltran, Maria, de Bernardis, Francesco, Bird, Simeon, Chen, Xingang, Chung, Daniel J. H., Colombo, Loris, Cooray, Asantha, Creminelli, Paolo, Dodelson, Scott, Dunkley, Joanna, Dvorkin, Cora, Easther, Richard, Finelli, Fabio, Flauger, Raphael, Hertzberg, Mark, Jones-Smith, Katherine, Kachru, Shamit, Kadota, Kenji, Khoury, Justin, Kinney, William H., Komatsu, Eiichiro, Krauss, Lawrence M., Lesgourgues, Julien, Liddle, Andrew, Liguori, Michele, Lim, Eugene, Linde, Andrei, Matarrese, Sabino, Mathur, Harsh, McAllister, Liam, Melchiorri, Alessandro, Nicolis, Alberto, Pagano, Luca, Peiris, Hiranya V., Peloso, Marco, Pogosian, Levon, Pierpaoli, Elena, Riotto, Antonio, Seljak, Uros, Senatore, Leonardo, Shandera, Sarah, Silverstein, Eva, Smith, Tristan, Vaudrevange, Pascal, Verde, Licia, Wandelt, Ben, Wands, David, Watson, Scott, Wyman, Mark, Yadav, Amit, Valkenburg, Wessel, and Zaldarriaga, Matias

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), Astrophysics (astro-ph), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

We summarize the utility of precise cosmic microwave background (CMB) polarization measurements as probes of the physics of inflation. We focus on the prospects for using CMB measurements to differentiate various inflationary mechanisms. In particular, a detection of primordial B-mode polarization would demonstrate that inflation occurred at a very high energy scale, and that the inflaton traversed a super-Planckian distance in field space. We explain how such a detection or constraint would illuminate aspects of physics at the Planck scale. Moreover, CMB measurements can constrain the scale-dependence and non-Gaussianity of the primordial fluctuations and limit the possibility of a significant isocurvature contribution. Each such limit provides crucial information on the underlying inflationary dynamics. Finally, we quantify these considerations by presenting forecasts for the sensitivities of a future satellite experiment to the inflationary parameters., 107 pages, 14 figures, 17 tables; Inflation Working Group contribution to the CMBPol Mission Concept Study; v2: typos fixed and references added

Published
2008

12. Probing Inflation with CMB Polarization

Author

Baumann, Daniel, Jackson, Mark G., Adshead, Peter, Amblard, Alexandre, Ashoorioon, Amjad, Bartolo, Nicola, Bean, Rachel, Beltran, Maria, Bernardis, Francesco, Bird, Simeon, Chen, Xingang, Chung, Daniel J. H., Colombo, Loris, Cooray, Asantha, Creminelli, Paolo, Scott Dodelson, Dunkley, Joanna, Dvorkin, Cora, Easther, Richard, Finelli, Fabio, Flauger, Raphael, Hertzberg, Mark P., Jones-Smith, Katherine, Kachru, Shamit, Kadota, Kenji, Khoury, Justin, Kinney, William H., Komatsu, Eiichiro, Krauss, Lawrence M., Lesgourgues, Julien, Liddle, Andrew, Liguori, Michele, Lim, Eugene, Linde, Andrei, Matarrese, Sabino, Mathur, Harsh, Mcallister, Liam, Melchiorri, Alessandro, Nicolis, Alberto, Pagano, Luca, Peiris, Hiranya V., Peloso, Marco, Pogosian, Levon, Pierpaoli, Elena, Riotto, Antonio, Seljak, Uros, Senatore, Leonardo, Shandera, Sarah, Silverstein, Eva, Smith, Tristan, Vaudrevange, Pascal, Verde, Licia, Wandelt, Ben, Wands, David, Watson, Scott, Wyman, Mark, Yadav, Amit, Valkenburg, Wessel, Zaldarriaga, Matias, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and Malaval, Virginie

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; We summarize the utility of precise cosmic microwave background (CMB)polarization measurements as probes of the physics of inflation. We focus onthe prospects for using CMB measurements to differentiate various inflationarymechanisms. In particular, a detection of primordial B-mode polarization woulddemonstrate that inflation occurred at a very high energy scale, and that theinflaton traversed a super-Planckian distance in field space. We explain howsuch a detection or constraint would illuminate aspects of physics at thePlanck scale. Moreover, CMB measurements can constrain the scale-dependence andnon-Gaussianity of the primordial fluctuations and limit the possibility of asignificant isocurvature contribution. Each such limit provides crucialinformation on the underlying inflationary dynamics. Finally, we quantify theseconsiderations by presenting forecasts for the sensitivities of a futuresatellite experiment to the inflationary parameters.

Published
2008

13. Inflationary trispectrum for models with large non-Gaussianities

Author

Chen, Xingang, Huang, Min-xin, and Shiu, Gary

Subjects
High Energy Physics - Theory, Physics, Inflation (cosmology), Nuclear and High Energy Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Inflaton, Astrophysics, 01 natural sciences, Cosmology, High Energy Physics - Phenomenology, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), Classical mechanics, High Energy Physics - Theory (hep-th), 0103 physical sciences, C++ string handling, Inflationary epoch, Statistical physics, Trispectrum, Quantum field theory, 010303 astronomy & astrophysics, Bispectrum
Abstract

We compute the leading order contribution to the four-point function of the primordial curvature perturbation in a class of single field models where the inflationary Lagrangian is a general function of the inflaton and its first derivative. This class of models includes string motivated inflationary models such as DBI inflation. We find that the trispectrum for some range of parameters could potentially be observed in future experiments. Moreover, the trispectrum can distinguish DBI inflation from other inflation models with large non-Gaussianities which typically have a similar bispectrum. We also derive a set of consistency conditions for n-point functions of the primordial curvature perturbation in single field inflation, generalizing Maldacena's result for 3-point functions., v2: 5 pages, journal version. v3, v4: formulae for the momentum dependence of trispectrum corrected, main conclusions remain unchanged, this version supersedes the journal version. v5: minor revision with an added reference

Published
2006
Full Text
View/download PDF

14. Running Non-Gaussianities in DBI Inflation

Author

Chen, Xingang

Subjects
High Energy Physics - Theory, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

We study the non-Gaussianity in the simplest infrared (IR) model of the DBI inflation. We show that the non-Gaussianity in such a model is compatible with the current observational bound, and is within the sensitivity of future experiments. We also discuss the scale dependence of the non-Gaussianity. In the DBI inflation, such a feature can be used as a probe to the properties of the background geometry of the extra dimensions or internal space., 17 pages; v3, a numerical correction in f_NL, references added, PRD version

Published
2005

15. The Origin of the Universe as Revealed Through the Polarization of the Cosmic Microwave Background

Author

Dodelson, Scott, Easther, Richard, Hanany, Shaul, Mcallister, Liam, Meyer, Stephan, Page, Lyman, Ade, Peter, Amblard, Alexandre, Ashoorioon, Amjad, Baccigalupi, Carlo, Balbi, Amedeo, Bartlett, James, Bartolo, Nicola, Baumann, Daniel, Beltran, Maria, Benford, Dominic, Birkinshaw, Mark, Bock, Jamie, Bond, Dick, Borrill, Julian, Bouchet, Francois, Bridges, Michael, Bunn, Emory, Calabrese, Erminia, Cantalupo, Christopher, Caramete, Ana, Carbone, Carmelita, Carroll, Sean, Chatterjee, Suchetana, Chen, Xingang, Church, Sarah, Chuss, David, Contaldi, Carlo R., Cooray, Asantha R., Creminelli, Paolo, Das, Sudeep, Bernardis, Francesco, Bernardis, Paolo, Delabrouille, Jacques, Desert, F. Xavier, Devlin, Mark J., Dickinson, Clive, Dicker, Simon, Dipirro, Michael, Dobbs, Matt A., Dore, Olivier, Dotson, Jessie, Dunkley, Joanna, Dvorkin, Cora, Eriksen, H. K., Falvella, Maria Cristina, Finley, Dave, Finkbeiner, Douglas P., Fixsen, Dale, Flauger, Raphael, Fosalba, Pablo, Fowler, Joseph W., Galli, Silvia, Gates, Evalyn I., Gear, Walter, Giraud-Heraud, Yannick, Gorski, Krzysztof, Greene, Brian, Gruppuso, Alessandro, Gundersen, Joshua, Halpern, Mark, Hamilton, Jean-Christophe, Hazumi, Masashi, Hernandez-Monteagudo, Carlos, Hertzberg, Mark, Hinshaw, Gary, Hirata, Christopher, Hivon, Eric, Holman, Richard, Holmes, Warren, Hu, Wayne, Hubmayr, Johannes, Huffenberger, Kevin, Hui, Howard, Hui, Lam, Irwin, Kent, Jackson, Mark, Jaffe, Andrew H., Johnson, Bradley, Johnson, Dean, Jones, William, Kachru, Shamit, Kadota, Kenji, Kaplan, Jean, Kaplinghat, Manoj, Keating, Brian G., Keskitalo, Reijo, Khoury, Justin, Kinney, William H., Kisner, Theodore, Knox, Lloyd, Kodama, Hideo, Kogut, Alan, Komatsu, Eiichiro, Kosowsky, Arthur, Kovac, John, Krauss, Lawrence M., Kurki-Suonio, Hannu, Lamarre, Jean-Michel, Landau, Susana Judith, Lawrence, Charles, Leach, Samuel M., Leblond, Louis, Lee, Adrian, Leitch, Erik, Leonardi, Rodrigo, Lesgourgues, Julien, Liddle, Andrew R., Lim, Eugene A., Limon, Michele, Loverde, Marilena, Lubin, Philip, Lunghi, Enrico, Lykken, Joseph D., Mactavish, Carolyn, Magalhaes, Antonio, Maino, Davide, Martin, Victoria, Sabino Matarrese, Mather, John C., Mathur, Harsh, Matsumura, Tomotake, Meerburg, Pieter, Melchiorri, Alessandro, Mersini-Houghton, Laura, Miller, Amber, Milligan, Michael, Moodley, Kavilan, Neimack, Michael, Nguyen, Hogan, Nicolis, Alberto, O Dwyer, Ian, Olinto, Angela, Pagano, Luca, Pajer, Enrico, Partridge, Bruce, Pearson, Timothy, Peiris, Hiranya V., Peloso, Marco, Piacentini, Francesco, Piat, Michel, Piccirillo, Lucio, Pierpaoli, Elena, Pietrobon, Davide, Pisano, Giampaolo, Pogosian, Levon, Pogosyan, Dmitri, Ponthieu, Nicolas, Popa, Lucia, Pryke, Clement, Raeth, Christoph, Ray, Subharthi, Reichardt, Christian, Ricciardi, Sara, Richards, Paul, Riotto, Antonio, Rocha, Graca, Ruhl, John, Rusholme, Benjamin, Scherrer, Robert, Scoccola, Claudia, Scott, Douglas, Sealfon, Carolyn, Sefusatti, Emiliano, Sehgal, Neelima, Seiffert, Michael, Senatore, Leonardo, Serra, Paolo, Shandera, Sarah E., Shimon, Meir, Shirron, Peter, Sievers, Jonathan, Silk, Joseph I., Sigurdson, Kris, Silverberg, Robert F., Silverstein, Eva, Staggs, Suzanne, Starkman, Glenn D., Stebbins, Albert, Stivoli, Federico, Stompor, Radek, Sugiyama, Naoshi, Swetz, Daniel, Tartari, Andrea, Tegmark, Max, Timbie, Peter, Titov, Maxim P., Tristram, Matthieu, Trodden, Mark, Tucker, Gregory, Urrestilla, Jon, Veneziani, Marcella, Verde, Licia, Vieira, Joaquin, Walker, Terry, Wands, David, Watson, Scott, Weinberg, Steven, Weiss, Rainer, Wandelt, Benjamin, Winstein, Bruce D., Wollack, Edward, Wyman, Mark, Yadav, Amit, Yoon, Ki Won, Zahn, Olivier, Zaldarriaga, Matias, Zemcov, Michael, Zwart, Jonathan, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, APC - Astrophysique des Hautes Energies (APC - AHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Bartlett, James, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, and Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)

Subjects
[SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

Modern cosmology has sharpened questions posed for millennia about the origin of our cosmic habitat. The age-old questions have been transformed into two pressing issues primed for attack in the coming decade: How did the Universe begin? and What physical laws govern the Universe at the highest energies? The clearest window onto these questions is the pattern of polarization in the Cosmic Microwave Background (CMB), which is uniquely sensitive to primordial gravity waves. A detection of the special pattern produced by gravity waves would be not only an unprecedented discovery, but also a direct probe of physics at the earliest observable instants of our Universe. Experiments which map CMB polarization over the coming decade will lead us on our first steps towards answering these age-old questions.

16. Inflation: Theory and Observations

Author

Achúcarro, Ana, Biagetti, Matteo, Matteo Braglia, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Xingang, Coulton, William, Flauger, Raphael, Fumagalli, Jacopo, Ivanov, Mikhail M., Lee, Hayden, Maleknejad, Azadeh, Meerburg, P. Daniel, Dizgah, Azadeh Moradinezhad, Palma, Gonzalo A., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Wallisch, Benjamin, Wandelt, Benjamin D., Witkowski, Lukas T., and Wu, W. L. Kimmy

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), hep-th, FOS: Physical sciences, hep-ph, Astrophysics::Cosmology and Extragalactic Astrophysics, High Energy Physics - Phenomenology, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Theory (hep-th), astro-ph.CO, Particle Physics - Theory, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle Physics - Phenomenology
Abstract

Cosmic inflation provides a window to the highest energy densities accessible in nature, far beyond those achievable in any realistic terrestrial experiment. Theoretical insights into the inflationary era and its observational probes may therefore shed unique light on the physical laws underlying our universe. This white paper describes our current theoretical understanding of the inflationary era, with a focus on the statistical properties of primordial fluctuations. In particular, we survey observational targets for three important signatures of inflation: primordial gravitational waves, primordial non-Gaussianity and primordial features. With the requisite advancements in analysis techniques, the tremendous increase in the raw sensitivities of upcoming and planned surveys will translate to leaps in our understanding of the inflationary paradigm and could open new frontiers for cosmology and particle physics. The combination of future theoretical and observational developments therefore offer the potential for a dramatic discovery about the nature of cosmic acceleration in the very early universe and physics on the smallest scales., Contribution to Snowmass 2021; 103 pages, 8 figures, 378 endorsers; v2: minor changes

17. Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

Author

Green, Daniel, Amin, Mustafa A., Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N., Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Richard Bond, J., Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, Engelen, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos A. G., García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho A Gontcho, Satya, Górski, Krzysztof M., Grin, Daniel, Grohs, Evan, Gudmundsson, Jon E., Hanany, Shaul, Handley, Will, Colin Hill, J., Hirata, Christopher M., Hložek, Renée, Holder, Gilbert, Horiuchi, Shunsaku, Huterer, Dragan, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E., Khatri, Rishi, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., L Huillier, Benjamin, Lahav, Ofer, Lattanzi, Massimiliano, Lee, Hayden, Liguori, Michele, Lin, Tongyan, Loverde, Marilena, Madhavacheril, Mathew, Masui, Kiyoshi, Mcmahon, Jeff, Mcquinn, Matthew, Daniel Meerburg, P., Mirbabayi, Mehrdad, Motloch, Pavel, Mukherjee, Suvodip, Munõz, Julian B., Nagy, Johanna, Newburgh, Laura, Niemack, Michael D., Nomerotski, Andrei, Page, Lyman, Piacentni, Francesco, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rose, Benjamin, Rossi, Graziano, Ruhl, John, Schaan, Emmanuel, Schubnell, Michael, Schutz, Katelin, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Sherwin, Blake D., Simon, Sara, Slosar, Anže, Staggs, Suzanne, Albert Stebbins, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Umiltà, Caterina, Di Valentino, Eleonora, Vargas-Magaña, M., Vieregg, Abigail, Watson, Scott, Weiler, Thomas, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Xu, Zhilei, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zhu, Ningfeng, Zuntz, Joe, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and HEP, INSPIRE

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), long-lived, gravitation: effect, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, High Energy Physics - Phenomenology (hep-ph), time: reheating, relic density, new physics, High Energy Physics::Phenomenology, photon, gravitational radiation, hep-ph, neutrino: sterile, boundary condition, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics - Phenomenology, gravitational radiation: emission, axion, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], astro-ph.CO, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], neutrino: decoupling, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic microwave background (CMB), the large-scale structure, and the primordial light element abundances, and are important in determining the initial conditions of the universe. We argue that future cosmological observations, in particular improved maps of the CMB on small angular scales, can be orders of magnitude more sensitive for probing the thermal history of the early universe than current experiments. These observations offer a unique and broad discovery space for new physics in the dark sector and beyond, even when its effects would not be visible in terrestrial experiments or in astrophysical environments. A detection of an excess light relic abundance would be a clear indication of new physics and would provide the first direct information about the universe between the times of reheating and neutrino decoupling one second later., 5 pages + references; 1 figure; science white paper submitted to the Astro2020 decadal survey

Catalog

Books, media, physical & digital resources
See catalog results