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1. Design and characterization of new 90 GHz detectors for the Cosmology Large Angular Scale Surveyor (CLASS)

Author

Núñez, Carolina, Appel, John W., Bruno, Sarah Marie, Datta, Rahul, Ali, Aamir, Bennett, Charles L., Dahal, Sumit, Couto, Jullianna Denes, Denis, Kevin L., Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Tom, Helson, Kyle, Iuliano, Jeffrey, Marriage, Tobias A., Pérez, Carolina Morales, Valle, Deniz Augusto Nunes, Petroff, Matthew A., Rostem, Karwan, Shi, Rui, Watts, Duncan J., Wollack, Edward J., and Xu, Zhilei

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Cosmology Large Angular Scale Surveyor (CLASS) is a polarization-sensitive telescope array located at an altitude of 5,200 m in the Chilean Atacama Desert. CLASS is designed to measure "E-mode" (even parity) and "B-mode" (odd parity) polarization patterns in the Cosmic Microwave Background (CMB) over large angular scales with the aim of improving our understanding of inflation, reionization, and dark matter. CLASS is currently observing with three telescopes covering four frequency bands: one at 40 GHz (Q); one at 90 GHz (W1); and one dichroic system at 150/220 GHz (G). In these proceedings, we discuss the updated design and in-lab characterization of new 90 GHz detectors. The new detectors include design changes to the transition-edge sensor (TES) bolometer architecture, which aim to improve stability and optical efficiency. We assembled and tested four new detector wafers, to replace four modules of the W1 focal plane. These detectors were installed into the W1 telescope, and will achieve first light in the austral winter of 2022. We present electrothermal parameters and bandpass measurements from in-lab dark and optical testing. From in-lab dark tests, we also measure a median NEP of 12.3 $\mathrm{aW\sqrt{s}}$ across all four wafers about the CLASS signal band, which is below the expected photon NEP of 32 $\mathrm{aW\sqrt{s}}$ from the field. We therefore expect the new detectors to be photon noise limited., Comment: 10 pages, 6 figures, to appear in Proc. SPIE Astronomical Telescopes and Instrumentation 2022

Published
2022

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

Author

Green, Daniel, Amin, Mustafa A., Meyers, Joel, Wallisch, Benjamin, Abazajian, Kevork N., Abidi, Muntazir, Adshead, Peter, Ahmed, Zeeshan, Ansarinejad, Behzad, Armstrong, Robert, Baccigalupi, Carlo, Bandura, Kevin, Barron, Darcy, Battaglia, Nicholas, Baumann, Daniel, Bechtol, Keith, Bennett, Charles, Benson, Bradford, Beutler, Florian, Bischoff, Colin, Bleem, Lindsey, Bond, J. Richard, Borrill, Julian, Buckley-Geer, Elizabeth, Burgess, Cliff, Carlstrom, John E., Castorina, Emanuele, Challinor, Anthony, Chen, Xingang, Cooray, Asantha, Coulton, William, Craig, Nathaniel, Crawford, Thomas, Cyr-Racine, Francis-Yan, D'Amico, Guido, Demarteau, Marcel, Doré, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Ellison, John, van Engelen, Alexander, Escoffier, Stephanie, Essinger-Hileman, Tom, Fabbian, Giulio, Filippini, Jeffrey, Flauger, Raphael, Foreman, Simon, Fuller, George, Garcia, Marcos A. G., García-Bellido, Juan, Gerbino, Martina, Gluscevic, Vera, Gontcho, 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, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rose, Benjamin, Rossi, Graziano, Ruhl, John, Schaan, Emmanuel, Schubnell, Michael, Schutz, Katelin, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Sherwin, Blake D., Simon, Sara, Slosar, Anže, Staggs, Suzanne, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tristram, Matthieu, Trodden, Mark, Tsai, Yu-Dai, Umiltà, Caterina, Di Valentino, Eleonora, Vargas-Magaña, M., Vieregg, Abigail, Watson, Scott, Weiler, Thomas, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Xu, Zhilei, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zhu, Ningfeng, and Zuntz, Joe

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
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., Comment: 5 pages + references; 1 figure; science white paper submitted to the Astro2020 decadal survey

Published
2019

3. 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, and Zhu, Ningfeng

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Theory
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

4. Science from an Ultra-Deep, High-Resolution Millimeter-Wave Survey

Author

Sehgal, Neelima, Nguyen, Ho Nam, Meyers, Joel, Munchmeyer, Moritz, Mroczkowski, Tony, Di Mascolo, Luca, Baxter, Eric, Cyr-Racine, Francis-Yan, Madhavacheril, Mathew, Beringue, Benjamin, Holder, Gil, Nagai, Daisuke, Dicker, Simon, Dvorkin, Cora, Ferraro, Simone, Fuller, George M., Gluscevic, Vera, Han, Dongwon, Jain, Bhuvnesh, Johnson, Bradley, Klaassen, Pamela, Meerburg, Daan, Motloch, Pavel, Spergel, David N., van Engelen, Alexander, Adshead, Peter, Armstrong, Robert, Baccigalupi, Carlo, Barron, Darcy, Basu, Kaustuv, Benson, Bradford, Beutler, Florian, Bond, J. Richard, Borrill, Julian, Calabrese, Erminia, Darwish, Omar, Denny, S. Lucas, Douglass, Kelly A., Essinger-Hileman, Tom, Foreman, Simon, Frayer, David, Gerbino, Martina, Gontcho, Satya Gontcho A, Grohs, Evan B., Gupta, Nikhel, Hill, J. Colin, Hirata, Christopher M., Hotinli, Selim, Johnson, Matthew C., Kamionkowski, Marc, Kovetz, Ely D., Lau, Erwin T., Liguori, Michele, Namikawa, Toshiya, Newburgh, Laura, Partridge, Bruce, Piacentni, Francesco, Rose, Benjamin, Rossi, Graziano, Saliwanchik, Benjamin, Schaan, Emmanuel, Shan, Huanyuan, Simon, Sara, Slosar, Anže, Switzer, Eric R., Trac, Hy, Xu, Weishuang, Zaldarriaga, Matias, and Zemcov, Michael

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology
Abstract

Opening up a new window of millimeter-wave observations that span frequency bands in the range of 30 to 500 GHz, survey half the sky, and are both an order of magnitude deeper (about 0.5 uK-arcmin) and of higher-resolution (about 10 arcseconds) than currently funded surveys would yield an enormous gain in understanding of both fundamental physics and astrophysics. In particular, such a survey would allow for major advances in measuring the distribution of dark matter and gas on small-scales, and yield needed insight on 1.) dark matter particle properties, 2.) the evolution of gas and galaxies, 3.) new light particle species, 4.) the epoch of inflation, and 5.) the census of bodies orbiting in the outer Solar System., Comment: 5 pages + references; Submitted to the Astro2020 call for science white papers

Published
2019

5. PICO: Probe of Inflation and Cosmic Origins

Author

Hanany, Shaul, Alvarez, Marcelo, Artis, Emmanuel, Ashton, Peter, Aumont, Jonathan, Aurlien, Ragnhild, Banerji, Ranajoy, Barreiro, R. Belen, Bartlett, James G., Basak, Soumen, Battaglia, Nick, Bock, Jamie, Boddy, Kimberly K., Bonato, Matteo, Borrill, Julian, Bouchet, François, Boulanger, François, Burkhart, Blakesley, Chluba, Jens, Chuss, David, Clark, Susan E., Cooperrider, Joelle, Crill, Brendan P., De Zotti, Gianfranco, Delabrouille, Jacques, Di Valentino, Eleonora, Didier, Joy, Doré, Olivier, Eriksen, Hans K., Errard, Josquin, Essinger-Hileman, Tom, Feeney, Stephen, Filippini, Jeffrey, Fissel, Laura, Flauger, Raphael, Fuskeland, Unni, Gluscevic, Vera, Gorski, Krzysztof M., Green, Dan, Hensley, Brandon, Herranz, Diego, Hill, J. Colin, Hivon, Eric, Hložek, Renée, Hubmayr, Johannes, Johnson, Bradley R., Jones, William, Jones, Terry, Knox, Lloyd, Kogut, Al, López-Caniego, Marcos, Lawrence, Charles, Lazarian, Alex, Li, Zack, Madhavacheril, Mathew, Melin, Jean-Baptiste, Meyers, Joel, Murray, Calum, Negrello, Mattia, Novak, Giles, O'Brient, Roger, Paine, Christopher, Pearson, Tim, Pogosian, Levon, Pryke, Clem, Puglisi, Giuseppe, Remazeilles, Mathieu, Rocha, Graca, Schmittfull, Marcel, Scott, Douglas, Shirron, Peter, Stephens, Ian, Sutin, Brian, Tomasi, Maurizio, Trangsrud, Amy, van Engelen, Alexander, Vansyngel, Flavien, Wehus, Ingunn K., Wen, Qi, Xu, Siyao, Young, Karl, and Zonca, Andrea

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

The Probe of Inflation and Cosmic Origins (PICO) is an imaging polarimeter that will scan the sky for 5 years in 21 frequency bands spread between 21 and 799 GHz. It will produce full-sky surveys of intensity and polarization with a final combined-map noise level of 0.87 $\mu$K arcmin for the required specifications, equivalent to 3300 Planck missions, and with our current best-estimate would have a noise level of 0.61 $\mu$K arcmin (6400 Planck missions). PICO will either determine the energy scale of inflation by detecting the tensor to scalar ratio at a level $r=5\times 10^{-4}~(5\sigma)$, or will rule out with more than $5\sigma$ all inflation models for which the characteristic scale in the potential is the Planck scale. With LSST's data it could rule out all models of slow-roll inflation. PICO will detect the sum of neutrino masses at $>4\sigma$, constrain the effective number of light particle species with $\Delta N_{\rm eff}<0.06~(2\sigma)$, and elucidate processes affecting the evolution of cosmic structures by measuring the optical depth to reionization with errors limited by cosmic variance and by constraining the evolution of the amplitude of linear fluctuations $\sigma_{8}(z)$ with sub-percent accuracy. Cross-correlating PICO's map of the thermal Sunyaev-Zeldovich effect with LSST's gold sample of galaxies will precisely trace the evolution of thermal pressure with $z$. PICO's maps of the Milky Way will be used to determine the make up of galactic dust and the role of magnetic fields in star formation efficiency. With 21 full sky legacy maps in intensity and polarization, which cannot be obtained in any other way, the mission will enrich many areas of astrophysics. PICO is the only single-platform instrument with the combination of sensitivity, angular resolution, frequency bands, and control of systematic effects that can deliver this compelling, timely, and broad science., Comment: Probe class mission study submitted to NASA and 2020 Decadal Panel. Executive summary: 2.5 pages; Science: 28 pages; Total: 50 pages, 36 figures

Published
2019

6. 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, MC David, Masui, Kiyoshi, Matarrese, Sabino, McAllister, Liam, McMahon, Jeff, McQuinn, Matthew, Meyers, Joel, Mirbabayi, Mehrdad, and Dizgah, Azadeh Moradinezhad

Subjects
astro-ph.CO, hep-th
Abstract

Our current understanding of the Universe is established through the pristinemeasurements of structure in the cosmic microwave background (CMB) and thedistribution and shapes of galaxies tracing the large scale structure (LSS) ofthe Universe. One key ingredient that underlies cosmological observables isthat the field that sources the observed structure is assumed to be initiallyGaussian with high precision. Nevertheless, a minimal deviation fromGaussianityis perhaps the most robust theoretical prediction of models thatexplain the observed Universe; itis necessarily present even in the simplestscenarios. In addition, most inflationary models produce far higher levels ofnon-Gaussianity. Since non-Gaussianity directly probes the dynamics in theearly Universe, a detection would present a monumental discovery in cosmology,providing clues about physics at energy scales as high as the GUT scale.

Published
2019

7. CMB-S4 Technology Book, First Edition

Author

Abitbol, Maximilian H., Ahmed, Zeeshan, Barron, Darcy, Thakur, Ritoban Basu, Bender, Amy N., Benson, Bradford A., Bischoff, Colin A., Bryan, Sean A., Carlstrom, John E., Chang, Clarence L., Chuss, David T., Crowley, Kevin T., Cukierman, Ari, de Haan, Tijmen, Dobbs, Matt, Essinger-Hileman, Tom, Filippini, Jeffrey P., Ganga, Ken, Gudmundsson, Jon E., Halverson, Nils W., Hanany, Shaul, Henderson, Shawn W., Hill, Charles A., Ho, Shuay-Pwu P., Hubmayr, Johannes, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Kernasovskiy, Sarah A., Kovac, John M., Kusaka, Akito, Lee, Adrian T., Maria, Salatino, Mauskopf, Philip, McMahon, Jeff J., Moncelsi, Lorenzo, Nadolski, Andrew W., Nagy, Johanna M., Niemack, Michael D., O'Brient, Roger C., Padin, Stephen, Parshley, Stephen C., Pryke, Clement, Roe, Natalie A., Rostem, Karwan, Ruhl, John, Simon, Sara M., Staggs, Suzanne T., Suzuki, Aritoki, Switzer, Eric R., Tajima, Osamu, Thompson, Keith L., Timbie, Peter, Tucker, Gregory S., Vieira, Joaquin D., Vieregg, Abigail G., Westbrook, Benjamin, Wollack, Edward J., Yoon, Ki Won, Young, Karl S., and Young, Edward Y.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

CMB-S4 is a proposed experiment to map the polarization of the Cosmic Microwave Background (CMB) to nearly the cosmic variance limit for angular scales that are accessible from the ground. The science goals and capabilities of CMB-S4 in illuminating cosmic inflation, measuring the sum of neutrino masses, searching for relativistic relics in the early universe, characterizing dark energy and dark matter, and mapping the matter distribution in the universe have been described in the CMB-S4 Science Book. This Technology Book is a companion volume to the Science Book. The ambitious science goals of CMB-S4, a "Stage-4" experiment, require a step forward in experimental capability from the current Stage=II experiments. To guide this process, we summarize the current state of CMB instrumentation technology, and identify R&D efforts necessary to advance it for use in CMB-S4. The book focuses on technical challenges in four broad areas: Telescope Design; Receiver Optics; Focal-Plane Optical Coupling; and Focal-Plane Sensor and Readout., Comment: 191 pages

Published
2017

8. Silicon-Based Antenna-Coupled Polarization-Sensitive Millimeter-Wave Bolometer Arrays for Cosmic Microwave Background Instruments

Author

Rostem, Karwan, Ali, Aamir, Appel, John W., Bennett, Charles L., Brown, Ari, Chang, Meng-Ping, Chuss, David T., Colazo, Felipe A., Costen, Nick, Denis, Kevin L., Essinger-Hileman, Tom, Hu, Ron, Marriage, Tobias A., Moseley, Samuel H., Stevenson, Thomas R., U-Yen, Kongpop, Wollack, Edward J., and Xu, Zhilei

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe feedhorn-coupled polarization-sensitive detector arrays that utilize monocrystalline silicon as the dielectric substrate material. Monocrystalline silicon has a low-loss tangent and repeatable dielectric constant, characteristics that are critical for realizing efficient and uniform superconducting microwave circuits. An additional advantage of this material is its low specific heat. In a detector pixel, two Transition-Edge Sensor (TES) bolometers are antenna-coupled to in-band radiation via a symmetric planar orthomode transducer (OMT). Each orthogonal linear polarization is coupled to a separate superconducting microstrip transmission line circuit. On-chip filtering is employed to both reject out-of-band radiation from the upper band edge to the gap frequency of the niobium superconductor, and to flexibly define the bandwidth for each TES to meet the requirements of the application. The microwave circuit is compatible with multi-chroic operation. Metalized silicon platelets are used to define the backshort for the waveguide probes. This micro-machined structure is also used to mitigate the coupling of out-of-band radiation to the microwave circuit. At 40 GHz, the detectors have a measured efficiency of 90%. In this paper, we describe the development of the 90 GHz detector arrays that will be demonstrated using the Cosmology Large Angular Scale Surveyor (CLASS) ground-based telescope.

Published
2016
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9. Scalable background-limited polarization-sensitive detectors for mm-wave applications

Author

Rostem, Karwan, Ali, Aamir, Appel, John W., Bennett, Charles L., Chuss, David T., Colazo, Felipe A., Crowe, Erik, Denis, Kevin L., Essinger-Hileman, Tom, Marriage, Tobias A., Moseley, Samuel H., Stevenson, Thomas R., Towner, Deborah W., U-Yen, Kongpop, and Wollack, Edward J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We report on the status and development of polarization-sensitive detectors for millimeter-wave applications. The detectors are fabricated on single-crystal silicon, which functions as a low-loss dielectric substrate for the microwave circuitry as well as the supporting membrane for the Transition-Edge Sensor (TES) bolometers. The orthomode transducer (OMT) is realized as a symmetric structure and on-chip filters are employed to define the detection bandwidth. A hybridized integrated enclosure reduces the high-frequency THz mode set that can couple to the TES bolometers. An implementation of the detector architecture at Q-band achieves 90% efficiency in each polarization. The design is scalable in both frequency coverage, 30-300 GHz, and in number of detectors with uniform characteristics. Hence, the detectors are desirable for ground-based or space-borne instruments that require large arrays of efficient background-limited cryogenic detectors., Comment: 7 pages, 3 figures, Presented at SPIE Astronomical Telescopes and Instrumentation 2014: Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VII. To be published in Proceedings of SPIE Volume 9153

Published
2014
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10. Design and characterization of new 90 GHz detectors for the Cosmology Large Angular Scale Surveyor (CLASS)

Author

Nunez, Carolina, primary, Appel, John W., additional, Bruno, Sarah Marie, additional, Datta, Rahul, additional, Ali, Aamir, additional, Bennett, Charles L., additional, Dahal, Sumit, additional, Denes Couto, Jullianna, additional, Denis, Kevin, additional, Eimer, Joseph, additional, Espinoza, Francisco, additional, Essinger-Hileman, Tom, additional, Helson, Kyle, additional, Iuliano, Jeffrey, additional, Marriage, Tobias, additional, Morales Peréz, Carolina, additional, Nunes Valle, Deniz Augusto, additional, Petroff, Matthew, additional, Rostem, Karwan, additional, Shi, Rui, additional, Watts, Duncan J., additional, Wollack, Edward J., additional, and Xu, Zhilei, additional

Published
2022
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11. Design and characterization of new 90 GHz detectors for the Cosmology Large Angular Scale Surveyor (CLASS)

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Nunez, Carolina, Appel, John W., Bruno, Sarah Marie, Datta, Rahul, Ali, Aamir, Bennett, Charles L., Dahal, Sumit, Denes Couto, Jullianna, Denis, Kevin L., Eimer, Joseph, Espinoza, Francisco, Essinger-Hileman, Tom, Helson, Kyle, Iuliano, Jeffrey, Marriage, Tobias A., Morales Peréz, Carolina, Nunes Valle, Deniz Augusto, Petroff, Matthew A., Rostem, Karwan, Shi, Rui, Watts, Duncan J., Wollack, Edward J., and Xu, Zhilei

Published
2022
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12. CMB-S4 Technology Book, First Edition

Author

Abitbol, Maximilian H., Ahmed, Zeeshan, Barron, Darcy, Thakur, Ritoban Basu, Bender, Amy N., Benson, Bradford A., Bischoff, Colin A., Bryan, Sean A., Carlstrom, John E., Chang, Clarence L., Chuss, David T., Crowley, Kevin T., Cukierman, Ari, de Haan, Tijmen, Dobbs, Matt, Essinger-Hileman, Tom, Filippini, Jeffrey P., Ganga, Ken, Gudmundsson, Jon E., Halverson, Nils W., Hanany, Shaul, Henderson, Shawn W., Hill, Charles A., Ho, Shuay-Pwu P., Hubmayr, Johannes, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Kernasovskiy, Sarah A., Kovac, John M., Kusaka, Akito, Lee, Adrian T., Maria, Salatino, Mauskopf, Philip, McMahon, Jeff J., Moncelsi, Lorenzo, Nadolski, Andrew W., Nagy, Johanna M., Niemack, Michael D., O'Brient, Roger C., Padin, Stephen, Parshley, Stephen C., Pryke, Clement, Roe, Natalie A., Rostem, Karwan, Ruhl, John, Simon, Sara M., Staggs, Suzanne T., Suzuki, Aritoki, Switzer, Eric R., Tajima, Osamu, Thompson, Keith L., Timbie, Peter, Tucker, Gregory S., Vieira, Joaquin D., Vieregg, Abigail G., Westbrook, Benjamin, Wollack, Edward J., Yoon, Ki Won, Young, Karl S., Young, Edward Y., AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CMB-S4, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
detector: technology, Astrophysics::Instrumentation and Methods for Astrophysics, electronics: readout, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), optics, detector: design, activity report
Abstract

CMB-S4 is a proposed experiment to map the polarization of the Cosmic Microwave Background (CMB) to nearly the cosmic variance limit for angular scales that are accessible from the ground. The science goals and capabilities of CMB-S4 in illuminating cosmic inflation, measuring the sum of neutrino masses, searching for relativistic relics in the early universe, characterizing dark energy and dark matter, and mapping the matter distribution in the universe have been described in the CMB-S4 Science Book. This Technology Book is a companion volume to the Science Book. The ambitious science goals of CMB-S4, a "Stage-4" experiment, require a step forward in experimental capability from the current Stage=II experiments. To guide this process, we summarize the current state of CMB instrumentation technology, and identify R&D efforts necessary to advance it for use in CMB-S4. The book focuses on technical challenges in four broad areas: Telescope Design; Receiver Optics; Focal-Plane Optical Coupling; and Focal-Plane Sensor and Readout., 191 pages

Published
2019

13. Astro2020 Science White Paper: Primordial Non-Gaussianity

Author

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

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

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

Published
2019

14. Gravitational probes of ultra-light axions

Author

Grin, Daniel, Amin, Mustafa A., Gluscevic, Vera, Hlǒzek, Renée, Marsh, David J.E., Poulin, Vivian, Prescod-Weinstein, Chanda, Smith, Tristan L., Ahmed, Zeeshan, Armengaud, Eric, Armstrong, Robert, Baccigalupi, Carlo, Baldi, Marco, Banik, Nilanjan, Barkana, Rennan, Barron, Darcy, Baumann, Daniel, Bechtol, Keith, Bischoff, Colin, Bleem, Lindsey, Bond, J. Richard, Borrill, Julian, Broadhurst, Tom, Carlstrom, John, Castorina, Emanuele, Clowe, Douglas, Cyr-Racine, Francis-Yan, Cooray, Asantha, Demarteau, Marcel, D'Amico, Guido, Doré, Oliver, Du, Xiaolong, Dunkley, Joanna, Dvorkin, Cora, Emami, Razieh, Essinger-Hileman, Tom, Ferreira, Pedro G., Flauger, Raphael, Foreman, Simon, Gerbino, Martina, Giblin, Jr John T., González-Morales, Alma, Green, Daniel, Gudmundsson, Jon E., Hanany, Shaul, Hertzberg, Mark, Hernández-Aguayo, César, Hill, J. Colin, Hirata, Christopher M., Hui, Lam, Huterer, Dragan, Iršič, Vid, Kadota, Kenji, Kamionkowski, Marc, Keeley, Ryan E., Kisner, Theodore, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Kobayashi, Takeshi, Lattanzi, Massimiliano, Li, Bohua, Lidz, Adam, Liguori, Michele, Lommen, Andrea, de la Macorra, Axel, Matos, Tonatiuh, Masui, Kiyoshi, McAllister, Liam, McMahon, Jeff, McQuinn, Matthew, Meerburg, P. Daniel, Meyers, Joel, Mirbabayi, Mehrdad, Mukherjee, Suvodip, Muñoz, Julian B., Nagy, Johanna, Niemeyer, Jens, Nomerotski, Andrei, Nori, Matteo, Page, Lyman, Partridge, Bruce, Piacentini, Francesco, Pogosian, Levon, Pradler, Josef, Pryke, Clement, Puglisi, Giuseppe, Raccanelli, Alvise, Raffelt, Georg, Rajendran, Surjeet, Raveri, Marco, Redondo, Javier, Rindler-Daller, Tanja, Saikawa, Ken'ichi, Schive, Hsi-Yu, Schwabe, Bodo, Sehgal, Neelima, Senatore, Leonardo, Shapiro, Paul R., Sherwin, Blake D., Sikivie, Pierre, Simon, Sara, Slosar, Anže, Soda, Jiro, Spergel, David N., Staggs, Suzanne, Stebbins, Albert, Stompor, Radek, Suzuki, Aritoki, Tsai, Yu-Dai, Uhlemann, Cora, Umiltà, Caterina, Ureña-Lopez, L., Di Valentino, Eleonora, Venters, Tonia M., Vieregg, Abigail, Visinelli, Luca, Wallisch, Benjamin, Watson, Scott, Whitehorn, Nathan, Wu, W.L.K., Zaldarriaga, Matias, Zhu, Ningfeng, Laboratoire Univers et Particules de Montpellier (LUPM), and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, interference, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), dark matter: density, Astrophysics::Cosmology and Extragalactic Astrophysics, General Relativity and Quantum Cosmology, microwaves: background, High Energy Physics - Phenomenology (hep-ph), cosmological model: parameter space, structure, string model, Particle Physics - Phenomenology, background: anisotropy, General Relativity and Cosmology, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, strong interaction, hep-ph, suppression, tension, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), gravitation, dark energy: density, axion, hydrogen, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], black hole: mass spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], absorption, Particle Physics - Theory, signature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The axion is a hypothetical, well-motivated dark-matter particle whose existence would explain the lack of charge-parity violation in the strong interaction. In addition to this original motivation, an `axiverse' of ultra-light axions (ULAs) with masses $10^{-33}\,{\rm eV}\lesssim m_{\rm a}\lesssim 10^{-10}\,{\rm eV}$ also emerges from string theory. Depending on the mass, such a ULA contributes to the dark-matter density, or alternatively, behaves like dark energy. At these masses, ULAs' classical wave-like properties are astronomically manifested, potentially mitigating observational tensions within the $\Lambda$CDM paradigm on local-group scales. ULAs also provide signatures on small scales such as suppression of structure, interference patterns and solitons to distinguish them from heavier dark matter candidates. Through their gravitational imprint, ULAs in the presently allowed parameter space furnish a host of observational tests to target in the next decade, altering standard predictions for microwave background anisotropies, galaxy clustering, Lyman-$\alpha$ absorption by neutral hydrogen along quasar sightlines, pulsar timing, and the black-hole mass spectrum., Comment: 5 pages, 1 figure, Astro2020 Decadal Survey science white paper

Published
2019

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

Author

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

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

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

Published
2019

16. PICO: Probe of Inflation and Cosmic Origins

Author

Bennett, Charles, Dodelson, Scott, Page, Lyman, Bartlett, James, Battaglia, Nick, Bock, Jamie, Borrill, Julian, Chuss, David, Crill, Brendan P., Delabrouille, Jacques, Devlin, Mark, Fissel, Laura, Flauger, Raphael, Green, Dan, Hill, J.Colin, Hubmayr, Johannes, Jones, William, Knox, Lloyd, Kogut, Al, Lawrence, Charles, McMahon, Jeff, Pearson, Tim, Pryke, Clem, Schmittfull, Marcel, Trangsrud, Amy, van Engelen, Alexander, Alvarez, Marcelo, Artis, Emmanuel, Ashton, Peter, Aumont, Jonathan, Aurlien, Ragnhild, Banerji, Ranajoy, Belen Barreiro, R., Bartlett, James G., Basak, Soumen, Boddy, Kimberly K., Bonato, Matteo, Bouchet, François, Boulanger, François, Burkhart, Blakesley, Chluba, Jens, Clark, Susan E., Cooperrider, Joelle, De Zotti, Gianfranco, Di Valentino, Eleonora, DIDIER, JOY, Doré, Olivier, Eriksen, Hans K., Errard, Josquin, Essinger-Hileman, Tom, Feeney, Stephen, Filippini, Jeffrey, Fuskeland, Unni, Gluscevic, Vera, Gorski, Krzysztof M., Hanany, Shaul, Hensley, Brandon, Herranz, Diego, Colin Hill, J., Hivon, Eric, Hložek, Renée, Johnson, Bradley R., JONES, TERRY, López-Caniego, Marcos, Lazarian, Alex, Li, Zack, Madhavacheril, Mathew, Melin, Jean-Baptiste, Meyers, Joel, Murray, Calum, Negrello, Mattia, Novak, Giles, O'Brient, Roger, Paine, Christopher, Pogosian, Levon, Puglisi, Giuseppe, Remazeilles, Mathieu, Rocha, Graca, Scott, Douglas, Shirron, Peter, Stephens, Ian, Sutin, Brian, Tomasi, Maurizio, Vansyngel, Flavien, Wehus, Ingunn K., Wen, Qi, Xu, Siyao, Young, Karl, Zonca, Andrea, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), NASA PICO, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
High Energy Physics - Theory, Planck, fluctuation: linear, scalar tensor, costs, magnetic field, cosmic background radiation, power spectrum, thermal, pressure, optical, neutrino: mass, High Energy Astrophysical Phenomena (astro-ph.HE), birefringence, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], photon, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, star: formation, inflation: model, Astrophysics - Solar and Stellar Astrophysics, infrared, Sunyaev-Zel'dovich effect, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, scale: inflation, noise, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter, supernova, ionization, structure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), beam: polarization, inflation: slow-roll approximation, scale: Planck, gravitational radiation, temperature, gold, redshift, sensitivity, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Theory (hep-th), angular resolution, quantum gravity, efficiency, Astrophysics of Galaxies (astro-ph.GA), galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The Probe of Inflation and Cosmic Origins (PICO) is an imaging polarimeter that will scan the sky for 5 years in 21 frequency bands spread between 21 and 799 GHz. It will produce full-sky surveys of intensity and polarization with a final combined-map noise level of 0.87 $\mu$K arcmin for the required specifications, equivalent to 3300 Planck missions, and with our current best-estimate would have a noise level of 0.61 $\mu$K arcmin (6400 Planck missions). PICO will either determine the energy scale of inflation by detecting the tensor to scalar ratio at a level $r=5\times 10^{-4}~(5\sigma)$, or will rule out with more than $5\sigma$ all inflation models for which the characteristic scale in the potential is the Planck scale. With LSST's data it could rule out all models of slow-roll inflation. PICO will detect the sum of neutrino masses at $>4\sigma$, constrain the effective number of light particle species with $\Delta N_{\rm eff}, Comment: Probe class mission study submitted to NASA and 2020 Decadal Panel. Executive summary: 2.5 pages; Science: 28 pages; Total: 50 pages, 36 figures

Published
2019
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17. Silicon-based antenna-coupled polarization-sensitive millimeter-wave bolometer arrays for cosmic microwave background instruments

Author

Rostem, Karwan, additional, Ali, Aamir, additional, Appel, John W., additional, Bennett, Charles L., additional, Brown, Ari, additional, Chang, Meng-Ping, additional, Chuss, David T., additional, Colazo, Felipe A., additional, Costen, Nick, additional, Denis, Kevin L., additional, Essinger-Hileman, Tom, additional, Hu, Ron, additional, Marriage, Tobias A., additional, Moseley, Samuel H., additional, Stevenson, Thomas R., additional, U-Yen, Kongpop, additional, Wollack, Edward J., additional, and Xu, Zhilei, additional

Published
2016
Full Text
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18. Scalable background-limited polarization-sensitive detectors for mm-wave applications

Author

Rostem, Karwan, additional, Ali, Aamir, additional, Appel, John W., additional, Bennett, Charles L., additional, Chuss, David T., additional, Colazo, Felipe A., additional, Crowe, Erik, additional, Denis, Kevin L., additional, Essinger-Hileman, Tom, additional, Marriage, Tobias A., additional, Moseley, Samuel H., additional, Stevenson, Thomas R., additional, Towner, Deborah W., additional, U-Yen, Kongpop, additional, and Wollack, Edward J., additional

Published
2014
Full Text
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19. Silicon-based antenna-coupled polarization-sensitive millimeter-wave bolometer arrays for cosmic microwave background instruments

Author

Holland, Wayne S., Zmuidzinas, Jonas, Rostem, Karwan, Ali, Aamir, Appel, John W., Bennett, Charles L., Brown, Ari, Chang, Meng-Ping, Chuss, David T., Colazo, Felipe A., Costen, Nick, Denis, Kevin L., Essinger-Hileman, Tom, Hu, Ron, Marriage, Tobias A., Moseley, Samuel H., Stevenson, Thomas R., U-Yen, Kongpop, Wollack, Edward J., and Xu, Zhilei

Published
2016
Full Text
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21. Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics

Author

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

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

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

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