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1. Fingerprints of a Non-Inflationary Universe from Massive Fields

Author: Quintin, Jerome, Chen, Xingang, Ebadi, Reza, Quintin, Jerome, Chen, Xingang, and Ebadi, Reza
Abstract: We construct explicit models of classical primordial standard clocks in an alternative to inflation, namely the slowly contracting ekpyrotic scenario. We study the phenomenology of massive spectator fields added to a state-of-the-art ekpyrotic model, with coupling functions that allow for these heavy fields to be classically excited while the background is slowly contracting. We perform numerical computations of the corrections to the scalar primordial power spectrum and compare with analytical estimates. Our full numerical results reveal so-called clock signals, sharp feature signals, as well as signals that link the two together. The models are found to predict oscillatory features that are resolutely different from what is calculated in inflation, and thus, such features represent unique fingerprints of a slowly contracting universe. This confirms the capability of primordial standard clocks to model-independently discriminate among very early universe scenarios., Comment: 70 pages, 22 figures
Published: 2024

2. New inflationary probes of axion dark matter

Author: Chen, Xingang, Fan, JiJi, Li, Lingfeng, Chen, Xingang, Fan, JiJi, and Li, Lingfeng
Abstract: If a light axion is present during inflation and becomes part of dark matter afterwards, its quantum fluctuations contribute to dark matter isocurvature. In this article, we introduce a whole new suite of cosmological observables for axion isocurvature, which could help test the presence of axions, as well as its coupling to the inflaton and other heavy spectator fields during inflation such as the radial mode of the Peccei-Quinn field. They include correlated clock signals in the curvature and isocurvature spectra, and mixed cosmological-collider non-Gaussianities involving both curvature and isocurvature fluctuations with shapes and running unconstrained by the current data analyses. Taking into account of the existing strong constraints on axion isocurvature fluctuations from the CMB, these novel signals could still be sizable and potentially observable. In some models, the signals, if observed, could even help us significantly narrow down the range of the inflationary Hubble scale, a crucial parameter difficult to be determined in general, independent of the tensor mode., Comment: 45 pages, 15 figures, updated according to the version published in JHEP
Published: 2023

3. ABO Blood Group and the Risk and Prognosis of Lymphoma

Author: Qin,Ling, Gao,Dongli, Wang,Qian, Zheng,Xuewei, Wang,Jingjing, Chen,Xingang, Fu,Dongliao, Ma,Haodi, Tan,Junjia, Yin,Qinan, Qin,Ling, Gao,Dongli, Wang,Qian, Zheng,Xuewei, Wang,Jingjing, Chen,Xingang, Fu,Dongliao, Ma,Haodi, Tan,Junjia, and Yin,Qinan
Abstract: Ling Qin,1 Dongli Gao,1 Qian Wang,1 Xuewei Zheng,2 Jingjing Wang,2 Xingang Chen,2 Dongliao Fu,2 Haodi Ma,2 Junjia Tan,3 Qinan Yin2 1The First Affiliated Hospital, and College of Clinical Medicine of Henan University of Science and Technology, Luoyang, Peopleâs Republic of China; 2Laboratory for Precision Medicine, School of Medical Technology and Engineering, Henan University of Science and Technology, Luoyang, Peopleâs Republic of China; 3Section for Statistical Analysis and Data Collection, Luoyang Branch, Bank of China, Luoyang, Peopleâs Republic of ChinaCorrespondence: Qinan Yin, School of Medical Technology and Engineering, Henan University of Science and Technology, No. 263 Kaiyuan Avenue, Luoyang, 471000, Peopleâs Republic of China, Tel +86-13939928711, Email qinanyin@haust.edu.cnAbstract: ABO blood group antigens exhibit alternative phenotypes and genetically derived structures that are located on the red cell surface. The role of ABO blood group in cancer biology has been intensely reported by several studies, and it is now widely recognized that ABO antigens are associated with the risk and prognosis of several types of tumors, namely gastric cancer and pancreatic cancer. However, there have been contentious limited issues with the association between the ABO blood group and lymphoma. In this narrative review, based on literature data, we discuss the role of ABO blood group in the risk and prognosis of lymphoma and summarize the current knowledge of the underlying pathogenic mechanisms of the association. The possible association of ABO blood group with racial disparities and pathological classification in lymphoma patients is also discussed.Keywords: ABO blood group, lymphoma, survival, disease susceptibility, race
Published: 2023

4. Cosmology of Single Species Hidden Dark Matter

Author: Lin, Weikang, Chen, Xingang, Ganjoo, Himanish, Hou, Liqiang, Mack, Katherine J., Lin, Weikang, Chen, Xingang, Ganjoo, Himanish, Hou, Liqiang, and Mack, Katherine J.
Abstract: Cosmology and astrophysics provide various ways to study the properties of dark matter even if they have negligible non-gravitational interactions with the Standard Model particles and remain hidden. We study a type of hidden dark matter model in which the dark matter is completely decoupled from the Standard Model sector except gravitationally, and consists of a single species with a conserved comoving particle number. This category of hidden dark matter includes models that act as warm dark matter but is more general. In particular, in addition to having an independent temperature from the Standard Model sector, it includes cases in which dark matter is in its own thermal equilibrium or is free-streaming, obeys fermionic or bosonic statistics, and processes a chemical potential that controls the particle occupation number. While the usual parameterization using the free-streaming scale or the particle mass no longer applies, we show that all cases can be well approximated by a set of functions parameterized by only one parameter as long as the chemical potential is nonpositive: the characteristic scale factor at the time of the relativistic-to-nonrelativistic transition. We study the constraints from Big Bang Nucleosynthesis, the cosmic microwave background, the Lyman-$\alpha$ forest, and the smallest halo mass. We show that the most significant phenomenological impact is the suppression of the small-scale matter power spectrum -- a typical feature when the dark matter has a velocity dispersion or pressure at early times. So far, small dark matter halos provide the strongest constraint, limiting the transition scale factor to be no larger than $\sim1.4\times10^{-4}$ times the scale factor at matter-radiation equality., Comment: 24 pages, 3 tables, 8 figures, comments welcome
Published: 2023

5. New inflationary probes of axion dark matter

Author: Chen, Xingang, Fan, JiJi, Li, Lingfeng, Chen, Xingang, Fan, JiJi, and Li, Lingfeng
Abstract: If a light axion is present during inflation and becomes part of dark matter afterwards, its quantum fluctuations contribute to dark matter isocurvature. In this article, we introduce a whole new suite of cosmological observables for axion isocurvature, which could help test the presence of axions, as well as its coupling to the inflaton and other heavy spectator fields during inflation such as the radial mode of the Peccei-Quinn field. They include correlated clock signals in the curvature and isocurvature spectra, and mixed cosmological-collider non-Gaussianities involving both curvature and isocurvature fluctuations with shapes and running unconstrained by the current data. Taking into account of the existing strong constraints on axion isocurvature fluctuations from the CMB, these novel signals could still be sizable and potentially observable. In some models, the signals, if observed, could even help us significantly narrow down the range of the inflationary Hubble scale, a crucial parameter difficult to be determined in general, independent of the tensor mode., Comment: 44 pages, 15 figures
Published: 2023

6. Cosmology of Single Species Hidden Dark Matter

Author: Lin, Weikang, Chen, Xingang, Ganjoo, Himanish, Hou, Liqiang, Mack, Katherine J., Lin, Weikang, Chen, Xingang, Ganjoo, Himanish, Hou, Liqiang, and Mack, Katherine J.
Abstract: Cosmology and astrophysics provide various ways to study the properties of dark matter even if they have negligible non-gravitational interactions with the Standard Model particles and remain hidden. We study a type of hidden dark matter model in which the dark matter is completely decoupled from the Standard Model sector except gravitationally, and consists of a single species with a conserved comoving particle number. This category of hidden dark matter includes models that act as warm dark matter but is more general. In particular, in addition to having an independent temperature from the Standard Model sector, it includes cases in which dark matter is in its own thermal equilibrium or is free-streaming, obeys fermionic or bosonic statistics, and processes a chemical potential that controls the particle occupation number. While the usual parameterization using the free-streaming scale or the particle mass no longer applies, we show that all cases can be well approximated by a set of functions parameterized by only one parameter as long as the chemical potential is nonpositive: the characteristic scale factor at the time of the relativistic-to-nonrelativistic transition. We study the constraints from Big Bang Nucleosynthesis, the cosmic microwave background, the Lyman-$\alpha$ forest, and the smallest halo mass. We show that the most significant phenomenological impact is the suppression of the small-scale matter power spectrum -- a typical feature when the dark matter has a velocity dispersion or pressure at early times. So far, small dark matter halos provide the strongest constraint, limiting the transition scale factor to be no larger than $\sim1.4\times10^{-4}$ times the scale factor at matter-radiation equality., Comment: 24 pages, 3 tables, 8 figures, comments welcome
Published: 2023

7. New inflationary probes of axion dark matter

Author: Chen, Xingang, Fan, JiJi, Li, Lingfeng, Chen, Xingang, Fan, JiJi, and Li, Lingfeng
Abstract: If a light axion is present during inflation and becomes part of dark matter afterwards, its quantum fluctuations contribute to dark matter isocurvature. In this article, we introduce a whole new suite of cosmological observables for axion isocurvature, which could help test the presence of axions, as well as its coupling to the inflaton and other heavy spectator fields during inflation such as the radial mode of the Peccei-Quinn field. They include correlated clock signals in the curvature and isocurvature spectra, and mixed cosmological-collider non-Gaussianities involving both curvature and isocurvature fluctuations with shapes and running unconstrained by the current data. Taking into account of the existing strong constraints on axion isocurvature fluctuations from the CMB, these novel signals could still be sizable and potentially observable. In some models, the signals, if observed, could even help us significantly narrow down the range of the inflationary Hubble scale, a crucial parameter difficult to be determined in general, independent of the tensor mode., Comment: 44 pages, 15 figures
Published: 2023

8. Inflation: Theory and Observations

Author: Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, 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., Wu, W. L. Kimmy, Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, 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
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., Comment: Contribution to Snowmass 2021; 103 pages, 8 figures, 378 endorsers; v2: minor changes
Published: 2022

9. Inflation: Theory and Observations

Author: Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, Cabass, Giovanni, Castorina, Emanuele, Caldwell, Robert, Chen, Xingang, Coulton, William, Flauger, Raphael, Fumagalli, Jacopo, Ivanov, Mikhail M., Lee, Hayden, Maleknejad, Azadeh, Meerburg, P. Daniel, Dizgah, Azadeh Moradinezhad, Palma, Gonzalo A., Renaux-Petel, Sébastien, Pimentel, Guilherme L., Wallisch, Benjamin, Wandelt, Benjamin D., Witkowski, Lukas T., Wu, W. L. Kimmy, Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, Cabass, Giovanni, Castorina, Emanuele, Caldwell, Robert, Chen, Xingang, Coulton, William, Flauger, Raphael, Fumagalli, Jacopo, Ivanov, Mikhail M., Lee, Hayden, Maleknejad, Azadeh, Meerburg, P. Daniel, Dizgah, Azadeh Moradinezhad, Palma, Gonzalo A., Renaux-Petel, Sébastien, Pimentel, Guilherme L., Wallisch, Benjamin, Wandelt, Benjamin D., Witkowski, Lukas T., and Wu, W. L. Kimmy
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., Comment: Contribution to Snowmass 2021; 99 pages, 7 figures, 362 endorsers
Published: 2022

10. Classical Cosmological Collider Physics and Primordial Features

Author: Chen, Xingang, Ebadi, Reza, Kumar, Soubhik, Chen, Xingang, Ebadi, Reza, and Kumar, Soubhik
Abstract: Features in the inflationary landscape can inject extra energies to inflation models and produce on-shell particles with masses much larger than the Hubble scale of inflation. This possibility extends the energy reach of the program of cosmological collider physics, in which signals associated with these particles are generically Boltzmann-suppressed. We study the mechanisms of this classical cosmological collider in two categories of primordial features. In the first category, the primordial feature is classical oscillation, which includes the case of coherent oscillation of a massive field and the case of oscillatory features in the inflationary potential. The second category includes any sharp feature in the inflation model. All these classical features can excite unsuppressed quantum modes of other heavy fields which leave observational signatures in primordial non-Gaussianities, including the information about the particle spectra of these heavy degrees of freedom., Comment: 47 pages, 14 figures
Published: 2022

11. Inflation: Theory and Observations

Author: Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, Cabass, Giovanni, Castorina, Emanuele, Caldwell, Robert, Chen, Xingang, Coulton, William, Flauger, Raphael, Fumagalli, Jacopo, Ivanov, Mikhail M., Lee, Hayden, Maleknejad, Azadeh, Meerburg, P. Daniel, Dizgah, Azadeh Moradinezhad, Palma, Gonzalo A., Renaux-Petel, Sébastien, Pimentel, Guilherme L., Wallisch, Benjamin, Wandelt, Benjamin D., Witkowski, Lukas T., Wu, W. L. Kimmy, Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, Cabass, Giovanni, Castorina, Emanuele, Caldwell, Robert, Chen, Xingang, Coulton, William, Flauger, Raphael, Fumagalli, Jacopo, Ivanov, Mikhail M., Lee, Hayden, Maleknejad, Azadeh, Meerburg, P. Daniel, Dizgah, Azadeh Moradinezhad, Palma, Gonzalo A., Renaux-Petel, Sébastien, Pimentel, Guilherme L., Wallisch, Benjamin, Wandelt, Benjamin D., Witkowski, Lukas T., and Wu, W. L. Kimmy
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., Comment: Contribution to Snowmass 2021; 99 pages, 7 figures, 362 endorsers
Published: 2022

12. Inflation: Theory and Observations

Author: Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, 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., Wu, W. L. Kimmy, Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, 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
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., Comment: Contribution to Snowmass 2021; 103 pages, 8 figures, 378 endorsers; v2: minor changes
Published: 2022

13. Snowmass Theory Frontier: Astrophysics and Cosmology

Author: Green, Daniel, Ruderman, Joshua T., Safdi, Benjamin R., Shelton, Jessie, Achúcarro, Ana, Adshead, Peter, Akrami, Yashar, Baryakhtar, Masha, Baumann, Daniel, Berlin, Asher, Blinov, Nikita, Boddy, Kimberly K., Buschmann, Malte, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Thomas Y., Chen, Xingang, Coulton, William, Croon, Djuna, Cui, Yanou, Curtin, David, Cyr-Racine, Francis-Yan, Dessert, Christopher, Dienes, Keith R., Draper, Patrick, Du, Peizhi, Ellis, Sebastian A. R., Essig, Rouven, Flauger, Raphael, Fong, Chee Sheng, Foster, Joshua W., Fumagalli, Jacopo, Harigaya, Keisuke, Horiuchi, Shunsaku, Ivanov, Mikhail M., Kahn, Yonatan, Knapen, Simon, Leane, Rebecca K., Lee, Hayden, Lentz, Erik W., Lewandowski, Matthew, Lisanti, Mariangela, Long, Andrew J., Loverde, Marilena, Maleknejad, Azadeh, McAllister, Liam, McDermott, Samuel D., McGehee, Robert, Meerburg, P. Daniel, Meyers, Joel, Dizgah, Azadeh Moradinezhad, Münchmeyer, Moritz, Outmezguine, Nadav Joseph, Pajer, Enrico, Palma, Gonzalo A., Parikh, Aditya, Park, Jong-Chul, Peter, Annika H. G., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Rodd, Nicholas L., Shakya, Bibhushan, Shiu, Gary, Silverstein, Eva, Simonovic, Marko, Singh, Rajeev, Sleight, Charlotte, Takhistov, Volodymyr, Tanedo, Philip, Taronna, Massimo, Thomas, Brooks, Toro, Natalia, Tsai, Yu-Dai, Vitagliano, Edoardo, Vogelsberger, Mark, Wallisch, Benjamin, Wandelt, Benjamin D., Wechsler, Risa H., Weniger, Christoph, Wu, W. L. Kimmy, Xu, Weishuang Linda, Yamada, Masaki, Yu, Hai-Bo, Zhang, Zhengkang, Zhong, Yi-Ming, Zurek, Kathryn, Green, Daniel, Ruderman, Joshua T., Safdi, Benjamin R., Shelton, Jessie, Achúcarro, Ana, Adshead, Peter, Akrami, Yashar, Baryakhtar, Masha, Baumann, Daniel, Berlin, Asher, Blinov, Nikita, Boddy, Kimberly K., Buschmann, Malte, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Thomas Y., Chen, Xingang, Coulton, William, Croon, Djuna, Cui, Yanou, Curtin, David, Cyr-Racine, Francis-Yan, Dessert, Christopher, Dienes, Keith R., Draper, Patrick, Du, Peizhi, Ellis, Sebastian A. R., Essig, Rouven, Flauger, Raphael, Fong, Chee Sheng, Foster, Joshua W., Fumagalli, Jacopo, Harigaya, Keisuke, Horiuchi, Shunsaku, Ivanov, Mikhail M., Kahn, Yonatan, Knapen, Simon, Leane, Rebecca K., Lee, Hayden, Lentz, Erik W., Lewandowski, Matthew, Lisanti, Mariangela, Long, Andrew J., Loverde, Marilena, Maleknejad, Azadeh, McAllister, Liam, McDermott, Samuel D., McGehee, Robert, Meerburg, P. Daniel, Meyers, Joel, Dizgah, Azadeh Moradinezhad, Münchmeyer, Moritz, Outmezguine, Nadav Joseph, Pajer, Enrico, Palma, Gonzalo A., Parikh, Aditya, Park, Jong-Chul, Peter, Annika H. G., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Rodd, Nicholas L., Shakya, Bibhushan, Shiu, Gary, Silverstein, Eva, Simonovic, Marko, Singh, Rajeev, Sleight, Charlotte, Takhistov, Volodymyr, Tanedo, Philip, Taronna, Massimo, Thomas, Brooks, Toro, Natalia, Tsai, Yu-Dai, Vitagliano, Edoardo, Vogelsberger, Mark, Wallisch, Benjamin, Wandelt, Benjamin D., Wechsler, Risa H., Weniger, Christoph, Wu, W. L. Kimmy, Xu, Weishuang Linda, Yamada, Masaki, Yu, Hai-Bo, Zhang, Zhengkang, Zhong, Yi-Ming, and Zurek, Kathryn
Abstract: We summarize progress made in theoretical astrophysics and cosmology over the past decade and areas of interest for the coming decade. This Report is prepared as the TF09 "Astrophysics and Cosmology" topical group summary for the Theory Frontier as part of the Snowmass 2021 process., Comment: 57 pages
Published: 2022

14. Classical Cosmological Collider Physics and Primordial Features

Author: Chen, Xingang, Ebadi, Reza, Kumar, Soubhik, Chen, Xingang, Ebadi, Reza, and Kumar, Soubhik
Abstract: Features in the inflationary landscape can inject extra energies to inflation models and produce on-shell particles with masses much larger than the Hubble scale of inflation. This possibility extends the energy reach of the program of cosmological collider physics, in which signals associated with these particles are generically Boltzmann-suppressed. We study the mechanisms of this classical cosmological collider in two categories of primordial features. In the first category, the primordial feature is classical oscillation, which includes the case of coherent oscillation of a massive field and the case of oscillatory features in the inflationary potential. The second category includes any sharp feature in the inflation model. All these classical features can excite unsuppressed quantum modes of other heavy fields which leave observational signatures in primordial non-Gaussianities, including the information about the particle spectra of these heavy degrees of freedom., Comment: 49 pages, 14 figures. Changes in v2: clarifications added. Matches the version published in JCAP
Published: 2022
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15. Questions on calculation of primordial power spectrum with large spikes: the resonance model case

Author: Inomata, Keisuke, Braglia, Matteo, Chen, Xingang, Renaux-Petel, Sébastien, Inomata, Keisuke, Braglia, Matteo, Chen, Xingang, and Renaux-Petel, Sébastien
Abstract: Inflationary models predicting a scale-dependent large amplification of the density perturbations have recently attracted a lot of attention because the amplified perturbations can seed a sizable amount of primordial black holes (PBHs) and stochastic background of gravitational waves (GWs). While the power spectra in these models are computed based on the linear equation of motion, it is not obvious whether loop corrections are negligible when such a large amplification occurs during inflation. In this paper, as a first step to discuss the loop corrections in such models, we use the in-in formalism and calculate the one-loop scalar power spectrum numerically and analytically in an illustrative model where the density perturbations are resonantly amplified due to oscillatory features in the inflaton potential. Our calculation is technically new in that the amplified perturbations are numerically taken into account in the in-in formalism for the first time. In arriving at our analytical estimates, we highlight the role that the Wronskian condition of perturbations, automatically satisfied in our model, plays in obtaining the correct estimates. We also discuss the necessary conditions for subdominant loop corrections in this model. We find that, for the typical parameter space leading to the $\mathcal O(10^7)$ amplification of the power spectrum required for a sufficient PBH production, the one-loop power spectrum dominates over the tree-level one, indicating the breakdown of the perturbation theory., Comment: 42 pages, 14 figures, v3: An error in the equation of the two-vertex contribution corrected. Accordingly, the splitting of the two-vertex contribution changed and Appendix B added. The final one-loop power spectrum becomes smaller than the previous results, whereas the main conclusion (the typical oscillatory models lead to dominant loop power spectra) is unchanged
Published: 2022
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16. Snowmass Theory Frontier: Astrophysics and Cosmology

Author: Green, Daniel, Ruderman, Joshua T., Safdi, Benjamin R., Shelton, Jessie, Achúcarro, Ana, Adshead, Peter, Akrami, Yashar, Baryakhtar, Masha, Baumann, Daniel, Berlin, Asher, Blinov, Nikita, Boddy, Kimberly K., Buschmann, Malte, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Thomas Y., Chen, Xingang, Coulton, William, Croon, Djuna, Cui, Yanou, Curtin, David, Cyr-Racine, Francis-Yan, Dessert, Christopher, Dienes, Keith R., Draper, Patrick, Du, Peizhi, Ellis, Sebastian A. R., Essig, Rouven, Flauger, Raphael, Fong, Chee Sheng, Foster, Joshua W., Fumagalli, Jacopo, Harigaya, Keisuke, Horiuchi, Shunsaku, Ivanov, Mikhail M., Kahn, Yonatan, Knapen, Simon, Leane, Rebecca K., Lee, Hayden, Lentz, Erik W., Lewandowski, Matthew, Lisanti, Mariangela, Long, Andrew J., Loverde, Marilena, Maleknejad, Azadeh, McAllister, Liam, McDermott, Samuel D., McGehee, Robert, Meerburg, P. Daniel, Meyers, Joel, Dizgah, Azadeh Moradinezhad, Münchmeyer, Moritz, Outmezguine, Nadav Joseph, Pajer, Enrico, Palma, Gonzalo A., Parikh, Aditya, Park, Jong-Chul, Peter, Annika H. G., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Rodd, Nicholas L., Shakya, Bibhushan, Shiu, Gary, Silverstein, Eva, Simonovic, Marko, Singh, Rajeev, Sleight, Charlotte, Takhistov, Volodymyr, Tanedo, Philip, Taronna, Massimo, Thomas, Brooks, Toro, Natalia, Tsai, Yu-Dai, Vitagliano, Edoardo, Vogelsberger, Mark, Wallisch, Benjamin, Wandelt, Benjamin D., Wechsler, Risa H., Weniger, Christoph, Wu, W. L. Kimmy, Xu, Weishuang Linda, Yamada, Masaki, Yu, Hai-Bo, Zhang, Zhengkang, Zhong, Yi-Ming, Zurek, Kathryn, Green, Daniel, Ruderman, Joshua T., Safdi, Benjamin R., Shelton, Jessie, Achúcarro, Ana, Adshead, Peter, Akrami, Yashar, Baryakhtar, Masha, Baumann, Daniel, Berlin, Asher, Blinov, Nikita, Boddy, Kimberly K., Buschmann, Malte, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Thomas Y., Chen, Xingang, Coulton, William, Croon, Djuna, Cui, Yanou, Curtin, David, Cyr-Racine, Francis-Yan, Dessert, Christopher, Dienes, Keith R., Draper, Patrick, Du, Peizhi, Ellis, Sebastian A. R., Essig, Rouven, Flauger, Raphael, Fong, Chee Sheng, Foster, Joshua W., Fumagalli, Jacopo, Harigaya, Keisuke, Horiuchi, Shunsaku, Ivanov, Mikhail M., Kahn, Yonatan, Knapen, Simon, Leane, Rebecca K., Lee, Hayden, Lentz, Erik W., Lewandowski, Matthew, Lisanti, Mariangela, Long, Andrew J., Loverde, Marilena, Maleknejad, Azadeh, McAllister, Liam, McDermott, Samuel D., McGehee, Robert, Meerburg, P. Daniel, Meyers, Joel, Dizgah, Azadeh Moradinezhad, Münchmeyer, Moritz, Outmezguine, Nadav Joseph, Pajer, Enrico, Palma, Gonzalo A., Parikh, Aditya, Park, Jong-Chul, Peter, Annika H. G., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Rodd, Nicholas L., Shakya, Bibhushan, Shiu, Gary, Silverstein, Eva, Simonovic, Marko, Singh, Rajeev, Sleight, Charlotte, Takhistov, Volodymyr, Tanedo, Philip, Taronna, Massimo, Thomas, Brooks, Toro, Natalia, Tsai, Yu-Dai, Vitagliano, Edoardo, Vogelsberger, Mark, Wallisch, Benjamin, Wandelt, Benjamin D., Wechsler, Risa H., Weniger, Christoph, Wu, W. L. Kimmy, Xu, Weishuang Linda, Yamada, Masaki, Yu, Hai-Bo, Zhang, Zhengkang, Zhong, Yi-Ming, and Zurek, Kathryn
Abstract: We summarize progress made in theoretical astrophysics and cosmology over the past decade and areas of interest for the coming decade. This Report is prepared as the TF09 "Astrophysics and Cosmology" topical group summary for the Theory Frontier as part of the Snowmass 2021 process., Comment: 57 pages
Published: 2022

17. Questions on calculation of primordial power spectrum with large spikes: the resonance model case

Author: Inomata, Keisuke, Braglia, Matteo, Chen, Xingang, Renaux-Petel, Sébastien, Inomata, Keisuke, Braglia, Matteo, Chen, Xingang, and Renaux-Petel, Sébastien
Abstract: Inflationary models predicting a scale-dependent large amplification of the density perturbations have recently attracted a lot of attention because the amplified perturbations can seed a sizable amount of primordial black holes (PBHs) and stochastic background of gravitational waves (GWs). While the power spectra in these models are computed based on the linear equation of motion, it is not obvious whether loop corrections are negligible when such a large amplification occurs during inflation. In this paper, as a first step to discuss the loop corrections in such models, we use the in-in formalism and calculate the one-loop scalar power spectrum numerically and analytically in an illustrative model where the density perturbations are resonantly amplified due to oscillatory features in the inflaton potential. Our calculation is technically new in that the amplified perturbations are numerically taken into account in the in-in formalism for the first time. In arriving at our analytical estimates, we highlight the role that the Wronskian condition of perturbations, automatically satisfied in our model, plays in obtaining the correct estimates. We also discuss the necessary conditions for subdominant loop corrections in this model. We find that, for the typical parameter space leading to the $\mathcal O(10^7)$ amplification of the power spectrum required for a sufficient PBH production, the one-loop power spectrum dominates over the tree-level one, indicating the breakdown of the perturbation theory., Comment: 42 pages, 14 figures, v3: An error in the equation of the two-vertex contribution corrected. Accordingly, the splitting of the two-vertex contribution changed and Appendix B added. The final one-loop power spectrum becomes smaller than the previous results, whereas the main conclusion (the typical oscillatory models lead to dominant loop power spectra) is unchanged
Published: 2022
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18. Back to the features: assessing the discriminating power of future CMB missions on inflationary models

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Pinol, Lucas, Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, and Pinol, Lucas
Abstract: Future Cosmic Microwave Background (CMB) experiments will deliver extremely accurate measurements of the E-modes pattern of the CMB polarization field. Given the sharpness of the E-modes transfer functions, such surveys make for a powerful detector of high-frequency signals from primordial features that may be lurking in current data sets. With a handful of toy models that increase the fit to the latest Planck data, but are of marginal statistical significance, we use a state-of-the-art forecast pipeline to illustrate the promising prospects to test primordial features in the next decade. Not only will future experiments allow us to detect such features in data, but they will also be able to discriminate between models and narrow down the physical mechanism originating them with high statistical significance. On the other hand, if the anomalies in the currently measured CMB spectra are just statistical fluctuations, all the current feature best fit candidates will be ruled out. Either way, our results show that primordial features are a clear target of forthcoming CMB surveys beyond the detection of tensor modes., Comment: 36 pages, 15 figures; v2 matches version published in JCAP
Published: 2022
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19. Snowmass Theory Frontier: Astrophysics and Cosmology

Author: Green, Daniel, Ruderman, Joshua T., Safdi, Benjamin R., Shelton, Jessie, Achúcarro, Ana, Adshead, Peter, Akrami, Yashar, Baryakhtar, Masha, Baumann, Daniel, Berlin, Asher, Blinov, Nikita, Boddy, Kimberly K., Buschmann, Malte, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Thomas Y., Chen, Xingang, Coulton, William, Croon, Djuna, Cui, Yanou, Curtin, David, Cyr-Racine, Francis-Yan, Dessert, Christopher, Dienes, Keith R., Draper, Patrick, Du, Peizhi, Ellis, Sebastian A. R., Essig, Rouven, Flauger, Raphael, Fong, Chee Sheng, Foster, Joshua W., Fumagalli, Jacopo, Harigaya, Keisuke, Horiuchi, Shunsaku, Ivanov, Mikhail M., Kahn, Yonatan, Knapen, Simon, Leane, Rebecca K., Lee, Hayden, Lentz, Erik W., Lewandowski, Matthew, Lisanti, Mariangela, Long, Andrew J., Loverde, Marilena, Maleknejad, Azadeh, McAllister, Liam, McDermott, Samuel D., McGehee, Robert, Meerburg, P. Daniel, Meyers, Joel, Dizgah, Azadeh Moradinezhad, Münchmeyer, Moritz, Outmezguine, Nadav Joseph, Pajer, Enrico, Palma, Gonzalo A., Parikh, Aditya, Park, Jong-Chul, Peter, Annika H. G., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Rodd, Nicholas L., Shakya, Bibhushan, Shiu, Gary, Silverstein, Eva, Simonovic, Marko, Singh, Rajeev, Sleight, Charlotte, Takhistov, Volodymyr, Tanedo, Philip, Taronna, Massimo, Thomas, Brooks, Toro, Natalia, Tsai, Yu-Dai, Vitagliano, Edoardo, Vogelsberger, Mark, Wallisch, Benjamin, Wandelt, Benjamin D., Wechsler, Risa H., Weniger, Christoph, Wu, W. L. Kimmy, Xu, Weishuang Linda, Yamada, Masaki, Yu, Hai-Bo, Zhang, Zhengkang, Zhong, Yi-Ming, Zurek, Kathryn, Green, Daniel, Ruderman, Joshua T., Safdi, Benjamin R., Shelton, Jessie, Achúcarro, Ana, Adshead, Peter, Akrami, Yashar, Baryakhtar, Masha, Baumann, Daniel, Berlin, Asher, Blinov, Nikita, Boddy, Kimberly K., Buschmann, Malte, Cabass, Giovanni, Caldwell, Robert, Castorina, Emanuele, Chen, Thomas Y., Chen, Xingang, Coulton, William, Croon, Djuna, Cui, Yanou, Curtin, David, Cyr-Racine, Francis-Yan, Dessert, Christopher, Dienes, Keith R., Draper, Patrick, Du, Peizhi, Ellis, Sebastian A. R., Essig, Rouven, Flauger, Raphael, Fong, Chee Sheng, Foster, Joshua W., Fumagalli, Jacopo, Harigaya, Keisuke, Horiuchi, Shunsaku, Ivanov, Mikhail M., Kahn, Yonatan, Knapen, Simon, Leane, Rebecca K., Lee, Hayden, Lentz, Erik W., Lewandowski, Matthew, Lisanti, Mariangela, Long, Andrew J., Loverde, Marilena, Maleknejad, Azadeh, McAllister, Liam, McDermott, Samuel D., McGehee, Robert, Meerburg, P. Daniel, Meyers, Joel, Dizgah, Azadeh Moradinezhad, Münchmeyer, Moritz, Outmezguine, Nadav Joseph, Pajer, Enrico, Palma, Gonzalo A., Parikh, Aditya, Park, Jong-Chul, Peter, Annika H. G., Pimentel, Guilherme L., Renaux-Petel, Sébastien, Rodd, Nicholas L., Shakya, Bibhushan, Shiu, Gary, Silverstein, Eva, Simonovic, Marko, Singh, Rajeev, Sleight, Charlotte, Takhistov, Volodymyr, Tanedo, Philip, Taronna, Massimo, Thomas, Brooks, Toro, Natalia, Tsai, Yu-Dai, Vitagliano, Edoardo, Vogelsberger, Mark, Wallisch, Benjamin, Wandelt, Benjamin D., Wechsler, Risa H., Weniger, Christoph, Wu, W. L. Kimmy, Xu, Weishuang Linda, Yamada, Masaki, Yu, Hai-Bo, Zhang, Zhengkang, Zhong, Yi-Ming, and Zurek, Kathryn
Abstract: We summarize progress made in theoretical astrophysics and cosmology over the past decade and areas of interest for the coming decade. This Report is prepared as the TF09 "Astrophysics and Cosmology" topical group summary for the Theory Frontier as part of the Snowmass 2021 process., Comment: 57 pages
Published: 2022

20. Classical Cosmological Collider Physics and Primordial Features

Author: Chen, Xingang, Ebadi, Reza, Kumar, Soubhik, Chen, Xingang, Ebadi, Reza, and Kumar, Soubhik
Abstract: Features in the inflationary landscape can inject extra energies to inflation models and produce on-shell particles with masses much larger than the Hubble scale of inflation. This possibility extends the energy reach of the program of cosmological collider physics, in which signals associated with these particles are generically Boltzmann-suppressed. We study the mechanisms of this classical cosmological collider in two categories of primordial features. In the first category, the primordial feature is classical oscillation, which includes the case of coherent oscillation of a massive field and the case of oscillatory features in the inflationary potential. The second category includes any sharp feature in the inflation model. All these classical features can excite unsuppressed quantum modes of other heavy fields which leave observational signatures in primordial non-Gaussianities, including the information about the particle spectra of these heavy degrees of freedom., Comment: 49 pages, 14 figures. Changes in v2: clarifications added. Matches the version published in JCAP
Published: 2022
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21. Inflation: Theory and Observations

Author: Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, 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., Wu, W. L. Kimmy, Achúcarro, Ana, Biagetti, Matteo, Braglia, Matteo, 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
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., Comment: Contribution to Snowmass 2021; 103 pages, 8 figures, 378 endorsers; v2: minor changes
Published: 2022

22. Primordial Standard Clock Models and CMB Residual Anomalies

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: The residuals of the power spectra of WMAP and Planck's cosmic microwave background (CMB) anisotropies data are known to exhibit a few interesting anomalies at different scales with marginal statistical significance. Combining bottom-up and top-down model-building approaches and using a pipeline that efficiently compares model predictions with data, we construct a model of primordial standard clock that is able to link and address the anomalies at both the large and small scales. This model, and its variant, provide some of the best fits to the feature anomalies in CMB. According to Bayes evidences, these models are currently statistically indistinguishable from the Standard Model. We show that the difference between them will soon become statistically significant with various higher quality data on the CMB polarization. We demonstrate that such a model-building and data-analyses process may be used to uncover a portion of detailed evolutionary history of our universe during its primordial epoch., Comment: 39 pages, 25 figures; v2: version published by PRD
Published: 2021
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23. Early-Universe-Physics Insensitive and Uncalibrated Cosmic Standards: Constraints on $\Omega_{\rm{m}}$ and Implications for the Hubble Tension

Author: Lin, Weikang, Chen, Xingang, Mack, Katherine J., Lin, Weikang, Chen, Xingang, and Mack, Katherine J.
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 $\Omega_{\rm{m}}=0.302\pm0.008$ ($68\%$ C.L.) assuming a flat $\Lambda$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., Comment: Results updated with stellar-age constraints; conclusion unchanged. Accepted for publication in ApJ
Published: 2021
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24. Comparing multi-field primordial feature models with the Planck data

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: In this paper, we use a complete model of classical primordial standard clocks as an example to develop a methodology of directly comparing numerical predictions from complicated multi-field feature models with the Planck data, including the Planck 2018 Plik unbinned likelihood and the statistically most powerful CamSpec 2020 likelihood for temperature and polarization data. As this two-field inflationary model offers a plethora of primordial feature spectra that represent combinations of sharp and resonance feature signals non-trivially distributed over extended cosmological scales, its data comparison has not been satisfactorily addressed by previous attempts using analytical templates. The method of this paper, consisting of numerical prediction, effective parameter construction and nested sampling data comparison, allows us to efficiently explore every possible spectra from the model. We classify the resulting feature candidates in three different frequency ranges. We use the Bayesian evidences to assess the statistical significance of the candidates over the baseline model, taking into account the effect of additional parameters and the look-elsewhere effect. Although none of the candidates is statistically significant, the methodology of this paper can be used to facilitate the future model-building and data-screening process of primordial features, and the candidates can be subjected to further tests with data from the upcoming cosmic microwave background polarization observations and galaxy surveys., Comment: v1: 37 pages, 19 figures and 3 tables; v2: references added, accepted for publication in JCAP
Published: 2021
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25. Primordial Standard Clock Models and CMB Residual Anomalies

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: The residuals of the power spectra of WMAP and Planck's cosmic microwave background (CMB) anisotropies data are known to exhibit a few interesting anomalies at different scales with marginal statistical significance. Combining bottom-up and top-down model-building approaches and using a pipeline that efficiently compares model predictions with data, we construct a model of primordial standard clock that is able to link and address the anomalies at both the large and small scales. This model, and its variant, provide some of the best fits to the feature anomalies in CMB. According to Bayes evidences, these models are currently statistically indistinguishable from the Standard Model. We show that the difference between them will soon become statistically significant with various higher quality data on the CMB polarization. We demonstrate that such a model-building and data-analyses process may be used to uncover a portion of detailed evolutionary history of our universe during its primordial epoch., Comment: 35 pages, 22 figures
Published: 2021

26. Primordial Standard Clock Models and CMB Residual Anomalies

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: The residuals of the power spectra of WMAP and Planck's cosmic microwave background (CMB) anisotropies data are known to exhibit a few interesting anomalies at different scales with marginal statistical significance. Combining bottom-up and top-down model-building approaches and using a pipeline that efficiently compares model predictions with data, we construct a model of primordial standard clock that is able to link and address the anomalies at both the large and small scales. This model, and its variant, provide some of the best fits to the feature anomalies in CMB. According to Bayes evidences, these models are currently statistically indistinguishable from the Standard Model. We show that the difference between them will soon become statistically significant with various higher quality data on the CMB polarization. We demonstrate that such a model-building and data-analyses process may be used to uncover a portion of detailed evolutionary history of our universe during its primordial epoch., Comment: 39 pages, 25 figures; v2: version published by PRD
Published: 2021
Full Text: View/download PDF

27. Primordial Standard Clock Models and CMB Residual Anomalies

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: The residuals of the power spectra of WMAP and Planck's cosmic microwave background (CMB) anisotropies data are known to exhibit a few interesting anomalies at different scales with marginal statistical significance. Combining bottom-up and top-down model-building approaches and using a pipeline that efficiently compares model predictions with data, we construct a model of primordial standard clock that is able to link and address the anomalies at both the large and small scales. This model, and its variant, provide some of the best fits to the feature anomalies in CMB. According to Bayes evidences, these models are currently statistically indistinguishable from the Standard Model. We show that the difference between them will soon become statistically significant with various higher quality data on the CMB polarization. We demonstrate that such a model-building and data-analyses process may be used to uncover a portion of detailed evolutionary history of our universe during its primordial epoch., Comment: 39 pages, 25 figures; v2: version published by PRD
Published: 2021
Full Text: View/download PDF

28. Uncovering the History of Cosmic Inflation from Anomalies in Cosmic Microwave Background Spectra

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: We propose an inflationary primordial feature model that can explain both the large and small-scale anomalies in the currently measured cosmic microwave background (CMB) anisotropy spectra, revealing a clip of adventurous history of the Universe during its primordial epoch. Although the model is currently statistically indistinguishable from the Standard Model, we show that future observations such as the Simons Observatory and LiteBIRD will complement each other in distinguishing the model differences due to their accurate E-mode polarization measurements, and the PICO mission, if funded, can put stringent constraints on all characteristic properties. The model predicts a signal of classical primordial standard clock, which can also be used to distinguish the inflation and alternative scenarios in a model-independent fashion., Comment: v1: 8 pages, 4 figures; v2: consistent with the companion paper 2108.10110, main results are unaffected; v3: improved forecast analysis, version accepted by EPJC
Published: 2021
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29. Uncovering the History of Cosmic Inflation from Anomalies in Cosmic Microwave Background Spectra

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: We propose an inflationary primordial feature model that can explain both the large and small-scale anomalies in the currently measured cosmic microwave background (CMB) anisotropy spectra, revealing a clip of adventurous history of the Universe during its primordial epoch. Although the model is currently statistically indistinguishable from the Standard Model, we show that future observations such as the Simons Observatory and LiteBIRD will complement each other in distinguishing the model differences due to their accurate E-mode polarization measurements, and the PICO mission, if funded, can put stringent constraints on all characteristic properties. The model predicts a signal of classical primordial standard clock, which can also be used to distinguish the inflation and alternative scenarios in a model-independent fashion., Comment: v1: 8 pages, 4 figures; v2: consistent with the companion paper 2108.10110, main results are unaffected; v3: improved forecast analysis, version accepted by EPJC
Published: 2021
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30. Comparing multi-field primordial feature models with the Planck data

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: In this paper, we use a complete model of classical primordial standard clocks as an example to develop a methodology of directly comparing numerical predictions from complicated multi-field feature models with the Planck data, including the Planck 2018 Plik unbinned likelihood and the statistically most powerful CamSpec 2020 likelihood for temperature and polarization data. As this two-field inflationary model offers a plethora of primordial feature spectra that represent combinations of sharp and resonance feature signals non-trivially distributed over extended cosmological scales, its data comparison has not been satisfactorily addressed by previous attempts using analytical templates. The method of this paper, consisting of numerical prediction, effective parameter construction and nested sampling data comparison, allows us to efficiently explore every possible spectra from the model. We classify the resulting feature candidates in three different frequency ranges. We use the Bayesian evidences to assess the statistical significance of the candidates over the baseline model, taking into account the effect of additional parameters and the look-elsewhere effect. Although none of the candidates is statistically significant, the methodology of this paper can be used to facilitate the future model-building and data-screening process of primordial features, and the candidates can be subjected to further tests with data from the upcoming cosmic microwave background polarization observations and galaxy surveys., Comment: v1: 37 pages, 19 figures and 3 tables; v2: references added, accepted for publication in JCAP
Published: 2021
Full Text: View/download PDF

31. Primordial Standard Clock Models and CMB Residual Anomalies

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: The residuals of the power spectra of WMAP and Planck's cosmic microwave background (CMB) anisotropies data are known to exhibit a few interesting anomalies at different scales with marginal statistical significance. Combining bottom-up and top-down model-building approaches and using a pipeline that efficiently compares model predictions with data, we construct a model of primordial standard clock that is able to link and address the anomalies at both the large and small scales. This model, and its variant, provide some of the best fits to the feature anomalies in CMB. According to Bayes evidences, these models are currently statistically indistinguishable from the Standard Model. We show that the difference between them will soon become statistically significant with various higher quality data on the CMB polarization. We demonstrate that such a model-building and data-analyses process may be used to uncover a portion of detailed evolutionary history of our universe during its primordial epoch., Comment: 39 pages, 25 figures; v2: version published by PRD
Published: 2021
Full Text: View/download PDF

32. Uncovering the History of Cosmic Inflation from Anomalies in Cosmic Microwave Background Spectra

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: We propose an inflationary primordial feature model that can explain both the large and small-scale anomalies in the currently measured cosmic microwave background (CMB) anisotropy spectra, revealing a clip of adventurous history of the Universe during its primordial epoch. Although the model is currently statistically indistinguishable from the Standard Model, we show that future observations such as the Simons Observatory and LiteBIRD will complement each other in distinguishing the model differences due to their accurate E-mode polarization measurements, and the PICO mission, if funded, can put stringent constraints on all characteristic properties. The model predicts a signal of classical primordial standard clock, which can also be used to distinguish the inflation and alternative scenarios in a model-independent fashion., Comment: v1: 8 pages, 4 figures; v2: consistent with the companion paper 2108.10110, main results are unaffected; v3: improved forecast analysis, version accepted by EPJC
Published: 2021
Full Text: View/download PDF

33. Comparing multi-field primordial feature models with the Planck data

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: In this paper, we use a complete model of classical primordial standard clocks as an example to develop a methodology of directly comparing numerical predictions from complicated multi-field feature models with the Planck data, including the Planck 2018 Plik unbinned likelihood and the statistically most powerful CamSpec 2020 likelihood for temperature and polarization data. As this two-field inflationary model offers a plethora of primordial feature spectra that represent combinations of sharp and resonance feature signals non-trivially distributed over extended cosmological scales, its data comparison has not been satisfactorily addressed by previous attempts using analytical templates. The method of this paper, consisting of numerical prediction, effective parameter construction and nested sampling data comparison, allows us to efficiently explore every possible spectra from the model. We classify the resulting feature candidates in three different frequency ranges. We use the Bayesian evidences to assess the statistical significance of the candidates over the baseline model, taking into account the effect of additional parameters and the look-elsewhere effect. Although none of the candidates is statistically significant, the methodology of this paper can be used to facilitate the future model-building and data-screening process of primordial features, and the candidates can be subjected to further tests with data from the upcoming cosmic microwave background polarization observations and galaxy surveys., Comment: v1: 37 pages, 19 figures and 3 tables; v2: references added, accepted for publication in JCAP
Published: 2021
Full Text: View/download PDF

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

Author: Lin, Weikang, Chen, Xingang, Mack, Katherine J., Lin, Weikang, Chen, Xingang, and Mack, Katherine J.
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 $\Omega_{\rm{m}}=0.302\pm0.008$ ($68\%$ C.L.) assuming a flat $\Lambda$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., Comment: Results updated with stellar-age constraints; conclusion unchanged. Accepted for publication in ApJ
Published: 2021
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35. Planck residuals anomaly as a fingerprint of alternative scenarios to inflation

Author: Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, Loeb, Abraham, Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, and Loeb, Abraham
Abstract: Planck's residuals of the CMB temperature power spectrum present a curious oscillatory shape that resembles an extra smoothing effect of lensing and is the source of the lensing anomaly. The smoothing effect of lensing to the CMB temperature power spectrum is, to some extent, degenerate with oscillatory modulations of the primordial power spectrum, in particular if the frequency is close to that of the acoustic peaks. We consider the possibility that the lensing anomaly reported by the latest Planck 2018 results may be hinting at an oscillatory modulation generated by a massive scalar field during an alternative scenario to inflation or by a sharp feature during inflation. We use the full TTTEEE+low E CMB likelihood from Planck to derive constraints on these two types of models. We obtain that in both cases the $A_L$ anomaly is mildly reduced to slightly less than $2\sigma$, to be compared with the $2.8\sigma$ deviation from $A_L=1$ in $\Lambda$CDM. Although the oscillatory features are not able to satisfactorily ease the lensing anomaly, we find that the oscillatory modulation generated during an alternative scenario alone, i.e. with $A_L=1$, presents the lowest value of $\chi^2$, with $\Delta\chi^2=-13$ compared to $\Lambda$CDM. Furthermore, the Akaike Information Criterion suggests that such an oscillation constitutes an attractive candidate since it has a value $\Delta{\rm AIC}=-5$ with respect to $\Lambda$CDM, comparable to the $A_L$ parameter. We also obtain that the equation of state parameter in the alternative scenario is given at $1\sigma$ by $w=0.13\pm0.17$. Interestingly, the matter bounce and radiation bounce scenarios are compatible with our results. We discuss how these models of oscillatory features can be tested with future observations., Comment: revised version
Published: 2020
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36. Planck residuals anomaly as a fingerprint of alternative scenarios to inflation

Author: Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, Loeb, Abraham, Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, and Loeb, Abraham
Abstract: Planck's residuals of the CMB temperature power spectrum present a curious oscillatory shape that resembles an extra smoothing effect of lensing and is the source of the lensing anomaly. The smoothing effect of lensing to the CMB temperature power spectrum is, to some extent, degenerate with oscillatory modulations of the primordial power spectrum, in particular if the frequency is close to that of the acoustic peaks. We consider the possibility that the lensing anomaly reported by the latest Planck 2018 results may be hinting at an oscillatory modulation generated by a massive scalar field during an alternative scenario to inflation or by a sharp feature during inflation. We use the full TTTEEE+low E CMB likelihood from Planck to derive constraints on these two types of models. We obtain that in both cases the $A_L$ anomaly is mildly reduced to slightly less than $2\sigma$, to be compared with the $2.8\sigma$ deviation from $A_L=1$ in $\Lambda$CDM. Although the oscillatory features are not able to satisfactorily ease the lensing anomaly, we find that the oscillatory modulation generated during an alternative scenario alone, i.e. with $A_L=1$, presents the lowest value of $\chi^2$, with $\Delta\chi^2=-13$ compared to $\Lambda$CDM. Furthermore, the Akaike Information Criterion suggests that such an oscillation constitutes an attractive candidate since it has a value $\Delta{\rm AIC}=-5$ with respect to $\Lambda$CDM, comparable to the $A_L$ parameter. We also obtain that the equation of state parameter in the alternative scenario is given at $1\sigma$ by $w=0.13\pm0.17$. Interestingly, the matter bounce and radiation bounce scenarios are compatible with our results. We discuss how these models of oscillatory features can be tested with future observations., Comment: revised version
Published: 2020
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37. Planck residuals anomaly as a fingerprint of alternative scenarios to inflation

Author: Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, Loeb, Abraham, Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, and Loeb, Abraham
Abstract: Planck's residuals of the CMB temperature power spectrum present a curious oscillatory shape that resembles an extra smoothing effect of lensing and is the source of the lensing anomaly. The smoothing effect of lensing to the CMB temperature power spectrum is, to some extent, degenerate with oscillatory modulations of the primordial power spectrum, in particular if the frequency is close to that of the acoustic peaks. We consider the possibility that the lensing anomaly reported by the latest Planck 2018 results may be hinting at an oscillatory modulation generated by a massive scalar field during an alternative scenario to inflation or by a sharp feature during inflation. We use the full TTTEEE+low E CMB likelihood from Planck to derive constraints on these two types of models. We obtain that in both cases the $A_L$ anomaly is mildly reduced to slightly less than $2\sigma$, to be compared with the $2.8\sigma$ deviation from $A_L=1$ in $\Lambda$CDM. Although the oscillatory features are not able to satisfactorily ease the lensing anomaly, we find that the oscillatory modulation generated during an alternative scenario alone, i.e. with $A_L=1$, presents the lowest value of $\chi^2$, with $\Delta\chi^2=-13$ compared to $\Lambda$CDM. Furthermore, the Akaike Information Criterion suggests that such an oscillation constitutes an attractive candidate since it has a value $\Delta{\rm AIC}=-5$ with respect to $\Lambda$CDM, comparable to the $A_L$ parameter. We also obtain that the equation of state parameter in the alternative scenario is given at $1\sigma$ by $w=0.13\pm0.17$. Interestingly, the matter bounce and radiation bounce scenarios are compatible with our results. We discuss how these models of oscillatory features can be tested with future observations., Comment: revised version
Published: 2020
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38. Probing Primordial Features with the Stochastic Gravitational Wave Background

Author: Braglia, Matteo, Chen, Xingang, Hazra, Dhiraj Kumar, Braglia, Matteo, Chen, Xingang, and Hazra, Dhiraj Kumar
Abstract: The stochastic gravitational wave background (SGWB) offers a new opportunity to observe signals of primordial features from inflationary models. We study their detectability with future space-based gravitational waves experiments, focusing our analysis on the frequency range of the LISA mission. We compute gravitational wave spectra from primordial features by exploring the parameter space of a two-field inflation model capable of generating different classes of features. Fine-tuning in scales and amplitudes is necessary for these signals to fall in the observational windows. Once they show up, several classes of frequency-dependent oscillatory signals, characteristic of different underlying inflationary physics, may be distinguished and the SGWB provides a window on dynamics of the primordial universe independent of cosmic microwave background and large-scale structure. To connect with future experimental data, we discuss two approaches of how the results may be applied to data analyses. First, we discuss the possibility of reconstructing the signal with LISA, which requires a high signal-to-noise ratio. The second more sensitive approach is to apply templates representing the spectra as estimators. For the latter purpose, we derive templates that can accurately capture the spectral features of several classes of feature signals and compare them with the SGWB produced by other physical mechanisms., Comment: 34 pages, 15 figures; v2 references added, typos corrected, accepted for publication in JCAP
Published: 2020
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39. Planck residuals anomaly as a fingerprint of alternative scenarios to inflation

Author: Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, Loeb, Abraham, Domènech, Guillem, Chen, Xingang, Kamionkowski, Marc, and Loeb, Abraham
Abstract: Planck's residuals of the CMB temperature power spectrum present a curious oscillatory shape that resembles an extra smoothing effect of lensing and is the source of the lensing anomaly. The smoothing effect of lensing to the CMB temperature power spectrum is, to some extent, degenerate with oscillatory modulations of the primordial power spectrum, in particular if the frequency is close to that of the acoustic peaks. We consider the possibility that the lensing anomaly reported by the latest Planck 2018 results may be hinting at an oscillatory modulation generated by a massive scalar field during an alternative scenario to inflation or by a sharp feature during inflation. We use the full TTTEEE+low E CMB likelihood from Planck to derive constraints on these two types of models. We obtain that in both cases the $A_L$ anomaly is mildly reduced to slightly less than $2\sigma$, to be compared with the $2.8\sigma$ deviation from $A_L=1$ in $\Lambda$CDM. Although the oscillatory features are not able to satisfactorily ease the lensing anomaly, we find that the oscillatory modulation generated during an alternative scenario alone, i.e. with $A_L=1$, presents the lowest value of $\chi^2$, with $\Delta\chi^2=-13$ compared to $\Lambda$CDM. Furthermore, the Akaike Information Criterion suggests that such an oscillation constitutes an attractive candidate since it has a value $\Delta{\rm AIC}=-5$ with respect to $\Lambda$CDM, comparable to the $A_L$ parameter. We also obtain that the equation of state parameter in the alternative scenario is given at $1\sigma$ by $w=0.13\pm0.17$. Interestingly, the matter bounce and radiation bounce scenarios are compatible with our results. We discuss how these models of oscillatory features can be tested with future observations., Comment: revised version
Published: 2020
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40. 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, 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, 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, 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, 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, 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, Umilta, 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, 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, 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, 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, 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, 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, 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, Umilta, 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, and Zhu, Ningfeng
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

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

Author: Slosar, Anže, Chen, Xingang, Dvorkin, Cora, Green, Daniel, Meerburg, P. Daniel, Silverstein, Eva, Wallisch, Benjamin, Slosar, Anže, Chen, Xingang, Dvorkin, Cora, Green, Daniel, Meerburg, P. Daniel, Silverstein, Eva, and Wallisch, Benjamin
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

42. Dark Matter Science in the Era of LSST

Author: Bechtol, Keith, 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 de 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, Giannotti, Maurizio, 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, Bechtol, Keith, 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 de 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, Giannotti, Maurizio, 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, and Lisanti, Mariangela
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.
Published: 2019

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

Author: Ferraro, Simone, 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, Padmanabhan, Hamsa, Ferraro, Simone, 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
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

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

Author: Green, Daniel, 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, Pryke, Clement, Green, Daniel, 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
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

45. 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, 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, 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, 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, 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, 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, Umilta, 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, 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, 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, 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, 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, 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, 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, Umilta, 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, and Zhu, Ningfeng
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

46. 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, 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, 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, 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, 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, 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, Umilta, 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, 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, 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, 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, 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, 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, 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, Umilta, 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, and Zhu, Ningfeng
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

47. 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, 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, de la Macorra, Axel, 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, 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, Urenña-López, L. Arturo, Di Valentino, Eleonora, Vargas-Magaña, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, Zhu, Hong-Ming, 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, 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, de la Macorra, Axel, 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, 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, Urenña-López, L. Arturo, Di Valentino, Eleonora, Vargas-Magaña, M., Wang, Yi, Watson, Scott, White, Martin, Xu, Weishuang, Yu, Byeonghee, Zhao, Gong-Bo, Zheng, Yi, and Zhu, Hong-Ming
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

48. 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 A. C., Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D'Amico, Guido, Davis, Tamara M, Dawson, William A., de la Macorra, Axel, Di Valentino, Eleonora, 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, Giannotti, Maurizio, Gill, Mandeep S. S., 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 H. G., 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 M. P., Tollerud, Erik, Troxel, M. A., 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, 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 A. C., Cuoco, Alessandro, Cyr-Racine, Francis-Yan, D'Amico, Guido, Davis, Tamara M, Dawson, William A., de la Macorra, Axel, Di Valentino, Eleonora, 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, Giannotti, Maurizio, Gill, Mandeep S. S., 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 H. G., 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 M. P., Tollerud, Erik, Troxel, M. A., 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., and Zuntz, Joe
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., Comment: 11 pages, 2 figures, Science Whitepaper for Astro 2020, more information at https://lsstdarkmatter.github.io
Published: 2019

49. Dark Matter Science in the Era of LSST

Author: Bechtol, Keith, 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 de 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, Giannotti, Maurizio, 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, Bechtol, Keith, 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 de 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, Giannotti, Maurizio, 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, and Lisanti, Mariangela
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.
Published: 2019

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

Author: Green, Daniel, 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, Pryke, Clement, Green, Daniel, 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
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

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