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34 results on '"Gorski, Krzysztof"'

1. Cosmic Microwave Background Recovery: A Graph-Based Bayesian Convolutional Network Approach

Author

Adams, Jadie, Lu, Steven, Gorski, Krzysztof M., Rocha, Graca, and Wagstaff, Kiri L.

Subjects
Computer Science - Machine Learning, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The cosmic microwave background (CMB) is a significant source of knowledge about the origin and evolution of our universe. However, observations of the CMB are contaminated by foreground emissions, obscuring the CMB signal and reducing its efficacy in constraining cosmological parameters. We employ deep learning as a data-driven approach to CMB cleaning from multi-frequency full-sky maps. In particular, we develop a graph-based Bayesian convolutional neural network based on the U-Net architecture that predicts cleaned CMB with pixel-wise uncertainty estimates. We demonstrate the potential of this technique on realistic simulated data based on the Planck mission. We show that our model accurately recovers the cleaned CMB sky map and resulting angular power spectrum while identifying regions of uncertainty. Finally, we discuss the current challenges and the path forward for deploying our model for CMB recovery on real observations., Comment: Published at the Thirty-fifth Annual Conference on Innovative Applications of Artificial Intelligence (IAAI-23). 7 pages, 6 figures

Published
2023

2. Foreground Separation and Constraints on Primordial Gravitational Waves with the PICO Space Mission

Author

Aurlien, Ragnhild, Remazeilles, Mathieu, Belkner, Sebastian, Carron, Julien, Delabrouille, Jacques, Eriksen, Hans Kristian, Flauger, Raphael, Fuskeland, Unni, Galloway, Mathew, Gorski, Krzysztof M., Hanany, Shaul, Hensley, Brandon S., Hill, J. Colin, Lawrence, Charles R., van Engelen, Alexander, and Wehus, Ingunn Kathrine

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

PICO is a concept for a NASA probe-scale mission aiming to detect or constrain the tensor to scalar ratio $r$, a parameter that quantifies the amplitude of inflationary gravity waves. We carry out map-based component separation on simulations with five foreground models and input $r$ values $r_{in}=0$ and $r_{in} = 0.003$. We forecast $r$ determinations using a Gaussian likelihood assuming either no delensing or a residual lensing factor $A_{\rm lens}$ = 27%. By implementing the first full-sky, post component-separation, map-domain delensing, we show that PICO should be able to achieve $A_{\rm lens}$ = 22% - 24%. For four of the five foreground models we find that PICO would be able to set the constraints $r < 1.3 \times 10^{-4} \,\, \mbox{to} \,\, r <2.7 \times 10^{-4}\, (95\%)$ if $r_{in}=0$, the strongest constraints of any foreseeable instrument. For these models, $r=0.003$ is recovered with confidence levels between $18\sigma$ and $27\sigma$. We find weaker, and in some cases significantly biased, upper limits when removing few low or high frequency bands. The fifth model gives a $3\sigma$ detection when $r_{in}=0$ and a $3\sigma$ bias with $r_{in} = 0.003$. However, by correlating $r$ determinations from many small 2.5% sky areas with the mission's 555 GHz data we identify and mitigate the bias. This analysis underscores the importance of large sky coverage. We show that when only low multipoles $\ell \leq 12$ are used, the non-Gaussian shape of the true likelihood gives uncertainties that are on average 30% larger than a Gaussian approximation., Comment: 34 pages, 13 figures, published in JCAP

Published
2022
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3. 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

4. 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

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. PICO - the probe of inflation and cosmic origins

Author

Sutin, Brian, Alvarez, Marcelo, Battaglia, Nicholas, Bock, Jamie, Bonato, Matteo, Borrill, Julian, Chuss, David T., Cooperrider, Joelle, Crill, Brendan, Delabrouille, Jacques, Devlin, Mark, Essinger-Hileman, Thomas, Fissel, Laura, Flauger, Raphael, Gorski, Krzysztof, Green, Daniel, Hanany, Shaul, Hubmayr, Johannes, Johnson, Bradley, Jones, William C., Knox, Lloyd, Kogut, Alan, Lawrence, Charles, McMahon, Jeff, Matsumura, Tomotake, Negrello, Mattia, O'Brient, Roger, Paine, Christopher, Pryke, Clement, Shirron, Peter, Trangsrud, Amy, Wen, Qi, Young, Karl, and de Zotti, Gianfranco

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

The Probe of Inflation and Cosmic Origins (PICO) is a NASA-funded study of a Probe-class mission concept. The top-level science objectives are to probe the physics of the Big Bang by measuring or constraining the energy scale of inflation, probe fundamental physics by measuring the number of light particles in the Universe and the sum of neutrino masses, to measure the reionization history of the Universe, and to understand the mechanisms driving the cosmic star formation history, and the physics of the galactic magnetic field. PICO would have multiple frequency bands between 21 and 799 GHz, and would survey the entire sky, producing maps of the polarization of the cosmic microwave background radiation, of galactic dust, of synchrotron radiation, and of various populations of point sources. Several instrument configurations, optical systems, cooling architectures, and detector and readout technologies have been and continue to be considered in the development of the mission concept. We will present a snapshot of the baseline mission concept currently under development., Comment: 11 pages, 5 Figure, submitted to SPIE, Proceedings of the Conference on Astronomical Telescopes and Instrumentation, 2018

Published
2018

7. 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

9. PICO - the probe of inflation and cosmic origins

Author

Sutin, Brian M, Alvarez, Marcelo, Battaglia, Nicholas, Bock, Jamie, Bonato, Matteo, Borrill, Jullian, Chuss, David T, Cooperrider, Joelle, Crill, Brendan, Delabrouille, Jacques, Devlin, Mark, Essinger-Hileman, Thomas, Fissel, Laura, Flauger, Raphael, Gorski, Krzysztof, Green, Daniel, Hanany, Shaul, Hubmayr, Johannes, Johnson, Bradley, Jones, William C, Knox, Lloyd, Kogut, Alan, Lawrence, Charles, McMahon, Jeff, Matsumura, Tomotake, Negrello, Mattia, O'Brient, Roger, Paine, Christopher, Pryke, Clement, Shirron, Peter, Trangsrud, Amy, Wen, Qi, Young, Karl, and de Zotti, Gianfranco

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, cosmic microwave background, polarization, space mission, bolometers, cryocooling, B-modes, probe-class, astro-ph.IM, astro-ph.CO, Communications engineering, Electronics, sensors and digital hardware, Atomic, molecular and optical physics
Abstract

The Probe of Inflation and Cosmic Origins (PICO) is a NASA-funded study of a Probe-class mission concept. The toplevel science objectives are to probe the physics of the Big Bang by measuring or constraining the energy scale of inflation, probe fundamental physics by measuring the number of light particles in the Universe and the sum of neutrino masses, to measure the reionization history of the Universe, and to understand the mechanisms driving the cosmic star formation history, and the physics of the galactic magnetic field. PICO would have multiple frequency bands between 21 and 799 GHz, and would survey the entire sky, producing maps of the polarization of the cosmic microwave background radiation, of galactic dust, of synchrotron radiation, and of various populations of point sources. Several instrument configurations, optical systems, cooling architectures, and detector and readout technologies have been and continue to be considered in the development of the mission concept. We will present a snapshot of the baseline mission concept currently under development.

Published
2018

10. The interplay of intersystem crossing and internal conversion in quadrupolar tetraarylpyrrolo[3,2-b]pyrroles

Author

Gorski, Krzysztof, Kusy, Damian, Ozaki, Shuhei, Banasiewicz, Marzena, Valiev, Rashid, Sahoo, Smruti Ranjan, Kamada, Kenji, Baryshnikov, Glib, Gryko, Daniel T., Gorski, Krzysztof, Kusy, Damian, Ozaki, Shuhei, Banasiewicz, Marzena, Valiev, Rashid, Sahoo, Smruti Ranjan, Kamada, Kenji, Baryshnikov, Glib, and Gryko, Daniel T.

Abstract

Adding nitro groups to aromatic compounds usually quenches their fluorescence via intersystem crossing (ISC) or internal conversion (IC). Herein, we investigated centrosymmetric 1,4-dihydropyrrolo[3,2-b]pyrroles linked to variously substituted nitro-heteroaryls. A 1,4-orientation of the nitro substituent versus the electron rich 1,4-dihydropyrrolo[3,2-b]pyrrole core invokes a strong fluorescence in non-polar solvents and intense two-photon absorption while a 1,3-orientation of push-pull substituents results in a dramatic hypsochromic shift of absorption, weak, bathochromically shifted emission and weak two-photon absorption. The combined experimental and computational study indicates that the primary responsible factors are: (1) the difference in electron density distribution in the LUMO; (2) the difference in mu 10. IC is a dominant mechanism of non-radiative dissipation of energy in all these dyes but as long as the distribution of electron density within the HOMO and LUMO is delocalized on the 1,4-dihydropyrrolo[3,2-b]pyrrole core as well as on the nitroaromatic moieties its rate is slower than the fluorescence rate in non-polar solvents., Funding Agencies|Foundation for Polish Science (TEAM) [POIR.04.04.00-00-3CF4/16-00]; National Science Centre, Poland [2017/25/Z/ST2/03038]; OPUS [2020/37/B/ST4/00017]; European Union [101007804]; JSPS KAKENHI [21H01887]; Ministry of Education and Science of Ukraine [0121U107533]; Academy of Finland [346369]; Swedish Research Council [2022-06725]; Swedish Research Council [2020-04600]; Olle Engkvists Stiftelse (Sweden) [212-0136]

Published
2024
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18. PICO - the Probe of Inflation and Cosmic Origins

Author

Bonato, Matteo, De Zotti, Gianfranco, Young, Karl, Wen, Qi, Trangsrud, Amy, Shirron, Peter, Pryke, Clement, 'O'Brient, Roger', 'Paine, Christopher, Negrello, Mattia, Matsumura, Tomotake, McMahon, Jeff, Lawrence, Charles, Kogut, Alan, Knox, Lloyd, Jones, William C, Johnson, Bradley, Hubmayr, Johannes, Hanany, Shaul, Green, Daniel, Gorski, Krzysztof, Flauger, Raphael, Fissel, Laura, Essinger-Hileman, Thomas, Delvin, Mark, Delabrouille, Jacques, Crill, Brendan, Cooperrider, Joelle, Chuss, David T, Borrill, Julian, Bock, Jamie, Battaglia, Nicholas, Alvarez, Marcelo, and Sutin, Brian M

Abstract

The Probe of Inflation and Cosmic Origins (PICO) is a NASA-funded study of a Probe-class mission concept. The top-level science objectives are to probe the physics of the Big Bang by measuring or constraining the energy scale of inflation, probe fundamental physics by measuring the number of light particles in the Universe and the sum of neutrino masses, to measure the reionization history of the Universe, and to understand the mechanisms driving the cosmic star formation history, and the physics of the galactic magnetic field. PICO would have multiple frequency bands between 21 and 799 GHz, and would survey the entire sky, producing maps of the polarization of the cosmic microwave background radiation, of galactic dust, of synchrotron radiation, and of various populations of point sources. Several instrument configurations, optical systems, cooling architectures, and detector and readout technologies have been and continue to be considered in the development of the mission concept. We will present a snapshot of the baseline mission concept currently under development.

Published
2018

21. Quadrupolar Dyes Based on Highly Polarized Coumarins

Author

Gorski, Krzysztof, Deperasinska, Irena, Baryshnikov, Glib, V, Ozaki, Shuhei, Kamada, Kenji, Ågren, Hans, Gryko, Daniel T., Gorski, Krzysztof, Deperasinska, Irena, Baryshnikov, Glib, V, Ozaki, Shuhei, Kamada, Kenji, Ågren, Hans, and Gryko, Daniel T.

Abstract

The fluorescence and other photophysical parameters of highly polarized, quadrupolar bis-coumarins possessing an electron-rich pyrrolo[3,2-b]pyrrole bridging unit are highly dependent on the linking position between both chromophores. Delocalization of the LUMO on the entire pi-system results in intense emission and strong two-photon absorption.

Published
2021
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23. 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

24. Dark Energy and Modified Gravity

Author

Slosar, Anže, Abazajian, Kevork N., Ahmed, Zeeshan, Alonso, David, Amin, Mustafa A., Ansarinejad, Behzad, Armstrong, Robert, Asorey, Jacobo, Avelino, Arturo, Avila, Santiago, Baccigalupi, Carlo, Ballardini, Mario, Bandura, Kevin, Battaglia, Nicholas, Bender, Amy N., Bennett, Charles, Benson, Bradford, Beutler, Florian, Bianchini, F., Bilicki, Maciej, Bischoff, Colin, Biviano, Andrea, Blazek, Jonathan, Bleem, Lindsey, Bolton, Adam S., Bond, J. Richard, Borrill, Julian, Bose, Sownak, Boucaud, Alexandre, Bouchet, Francois R., Buckley-Geer, Elizabeth, Bull, Philip, Cai, Zheng, Carlstrom, John E., Castander, Francisco J., Castorina, Emanuele, Challinor, Anthony, Chang, Tzu-Ching, Chaves-Montero, Jonas, Chisari, Nora Elisa, Clowe, Douglas, Comparat, Johan, Cooray, Asantha, Croft, Rupert A. C., Cyr-Racine, Francis-Yan, D Amico, Guido, Davis, Tamara M., Dawson, Kyle, Demarteau, Marcel, Dey, Arjun, Dore, Olivier, Yutong, Duan, Dunkley, Joanna, Dvorkin, Cora, Eggemeier, Alexander, Eisenstein, Daniel, Ellison, John, Engelen, Alexander, Escoffier, Stephanie, Fabbian, Giulio, Ferraro, Simone, Ferreira, Pedro G., Font-Ribera, Andreu, Foreman, Simon, Fosalba, Pablo, Friedrich, Oliver, Garcıa-Bellido, Juan, Gerbino, Martina, Gill, Mandeep S. S., Gluscevic, Vera, Gontcho A Gontcho, Satya, Gorski, Krzysztof M., Gruen, Daniel, Gudmundsson, Jon E., Gupta, Nikhel, Guy, Julien, Hanany, Shaul, Handley, Will, Hernández-Aguayo, César, Hill, J. Colin, Hirata, Christopher M., Hlozek, Renée, Holder, Gilbert, Huterer, Dragan, Ishak, Mustapha, Jeltema, Tesla, Jha, Saurabh W., Cohen-Tanugi, Johann, Johnson, Bradley, Kamionkowski, Marc, Karkare, Kirit S., E Keeley, Ryan, Khatri, Rishi, Kirkby, David, Kisner, Theodore, Kneib, Jean-Paul, Knox, Lloyd, Koushiappas, Savvas M., Kovetz, Ely D., Koyama, Kazuya, Krause, Elisabeth, Benjamin L'Huillier, Lahav, Ofer, Lattanzi, Massimiliano, Leonard, Danielle, Levi, Michael, Liguori, Michele, Linden, Anja, Loverde, Marilena, Lukic, Zarija, La Macorra, Axel, Madhavacheril, Mathew, Plazas, Andres, Spurio Mancini, Alessio, Manera, Marc, Mantz, Adam, Martini, Paul, Masui, Kiyoshi, Mcmahon, Jeff, Meerburg, P. Daniel, Mertens, James, Meyers, Joel, More, Surhud, Motloch, Pavel, Mukherjee, Suvodip, Muñoz, Julian B., Myers, Adam D., Nagy, Johanna, Palanque-Delabrouille, Nathalie, Newburgh, Laura, Newman, Jeffrey A., Niemack, Michael D., Niz, Gustavo, Nomerotski, Andrei, O Connor, Paul, Page, Lyman, Palmese, Antonella, Penna-Lima, Mariana, Percival, Will J., Piacentni, Francesco, Pieri, Matthew M., Pierpaoli, Elena, Pogosian, Levon, Prakash, Abhishek, Pryke, Clement, Puglisi, Giuseppe, Stompor, Radek, Raveri, Marco, Reichardt, Christian L., Rhodes, Jason, Rodney, Steven, Rose, Benjamin, Ross, Ashley J., Rossi, Graziano, Ruhl, John, Saliwanchik, Benjamin, Samushia, Lado, Sanchez, Javier, Sasaki, Misao, Schaan, Emmanuel, Schlegel, David J., Schmittfull, Marcel, Schubnell, Michael, Scott, Douglas, Sehgal, Neelima, Senatore, Leonardo, Seo, Hee-Jong, Shafieloo, Arman, Shan, Huanyuan, Sherwin, Blake D., Shi, Feng, Simon, Sara, Slosar, Anze, Staggs, Suzanne, Starkman, Glenn, Stebbins, Albert, Suzuki, Aritoki, Switzer, Eric R., Timbie, Peter, Tolley, Andrew J., Tristram, Matthieu, Trodden, Mark, Troxel, M. A., Uhlemann, Cora, Umilta, Caterina, Urenna-Lopez, L. Arturo, Di Valentino, Eleonora, Vargas-Magana, M., Vieregg, Abigail, Walter, Christopher W., Wang, Yi, Watson, Scott, White, Martin, Whitehorn, Nathan, Wu, W. L. K., Xu, Weishuang, Yasini, Siavash, Zaldarriaga, Matias, Zhao, Gong-Bo, Zheng, Yi, Zhu, Hong-Ming, Zhu, Ningfeng, Zuntz, Joe, 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), 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), 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), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), HEP, INSPIRE, 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)-Université de Montpellier (UM)-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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, and 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)

Subjects
cosmological model, Hubble constant, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitation: model, FOS: Physical sciences, cosmic background radiation, baryon: oscillation: acoustic, gravitation: lens, statistical analysis, supernova, Sunyaev-Zel'dovich effect, astro-ph.CO, galaxy: cluster, expansion: acceleration, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Despite two decades of tremendous experimental and theoretical progress, the riddle of the accelerated expansion of the Universe remains to be solved. On the experimental side, our understanding of the possibilities and limitations of the major dark energy probes has evolved; here we summarize the major probes and their crucial challenges. On the theoretical side, the taxonomy of explanations for the accelerated expansion rate is better understood, providing clear guidance to the relevant observables. We argue that: i) improving statistical precision and systematic control by taking more data, supporting research efforts to address crucial challenges for each probe, using complementary methods, and relying on cross-correlations is well motivated; ii) blinding of analyses is difficult but ever more important; iii) studies of dark energy and modified gravity are related; and iv) it is crucial that R&D for a vibrant dark energy program in the 2030s be started now by supporting studies and technical R&D that will allow embryonic proposals to mature. Understanding dark energy, arguably the biggest unsolved mystery in both fundamental particle physics and cosmology, will remain one of the focal points of cosmology in the forthcoming decade., 5 pages + references; science white paper submitted to the Astro2020 decadal survey

Published
2019

25. 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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28. PICO - the probe of inflation and cosmic origins

Author

Lystrup, Makenzie, MacEwen, Howard A., Fazio, Giovanni G., Batalha, Natalie, Siegler, Nicholas, Tong, Edward C., Sutin, Brian M., Alvarez, Marcelo, Battaglia, Nicholas, Bock, Jamie, Bonato, Matteo, Borrill, Julian, Chuss, David T., Cooperrider, Joelle, Crill, Brendan, Delabrouille, Jacques, Devlin, Mark, Essinger-Hileman, Thomas, Fissel, Laura, Flauger, Raphael, Gorski, Krzysztof, Green, Daniel, Hanany, Shaul, Hubmayr, Johannes, Johnson, Bradley, Jones, William C., Knox, Lloyd, Kogut, Alan, Lawrence, Charles, McMahon, Jeff, Matsumura, Tomotake, Negrello, Mattia, O'Brient, Roger, Paine, Christopher, Pryke, Clement, Shirron, Peter, Trangsrud, Amy, Wen, Qi, Young, Karl, De Zotti, Gianfranco, Lystrup, Makenzie, MacEwen, Howard A., Fazio, Giovanni G., Batalha, Natalie, Siegler, Nicholas, Tong, Edward C., Sutin, Brian M., Alvarez, Marcelo, Battaglia, Nicholas, Bock, Jamie, Bonato, Matteo, Borrill, Julian, Chuss, David T., Cooperrider, Joelle, Crill, Brendan, Delabrouille, Jacques, Devlin, Mark, Essinger-Hileman, Thomas, Fissel, Laura, Flauger, Raphael, Gorski, Krzysztof, Green, Daniel, Hanany, Shaul, Hubmayr, Johannes, Johnson, Bradley, Jones, William C., Knox, Lloyd, Kogut, Alan, Lawrence, Charles, McMahon, Jeff, Matsumura, Tomotake, Negrello, Mattia, O'Brient, Roger, Paine, Christopher, Pryke, Clement, Shirron, Peter, Trangsrud, Amy, Wen, Qi, Young, Karl, and De Zotti, Gianfranco

Abstract

The Probe of Inflation and Cosmic Origins (PICO) is a NASA-funded study of a Probe-class mission concept. The toplevel science objectives are to probe the physics of the Big Bang by measuring or constraining the energy scale of inflation, probe fundamental physics by measuring the number of light particles in the Universe and the sum of neutrino masses, to measure the reionization history of the Universe, and to understand the mechanisms driving the cosmic star formation history, and the physics of the galactic magnetic field. PICO would have multiple frequency bands between 21 and 799 GHz, and would survey the entire sky, producing maps of the polarization of the cosmic microwave background radiation, of galactic dust, of synchrotron radiation, and of various populations of point sources. Several instrument configurations, optical systems, cooling architectures, and detector and readout technologies have been and continue to be considered in the development of the mission concept. We will present a snapshot of the baseline mission concept currently under development.

Published
2018

29. Population management in integrated care organization in Poland: resource utilization for performing health risk assessment

Author

Guzek, Marika, primary, Szafraniec-Buryło, Sylwia I., additional, Prusaczyk, Artur, additional, Zuk, Pawel, additional, Bukato, Grzegorz, additional, Gronwald, Jacek, additional, Dziegielewski, Michal, additional, Kulaga, Katarzyna, additional, Wiktorzak, Katarzyna, additional, Gorski, Krzysztof, additional, and Kurpas, Donata, additional

Published
2018
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30. Optical design of PICO: a concept for a space mission to probe inflation and cosmic origins

Author

Young, Karl, primary, Alvarez, Marcelo, primary, Fissel, Laura, primary, Green, Daniel, primary, Hubmayr, Johannes, primary, Tan, Xin Zhi, primary, De Zotti, Gianfranco, primary, Wen, Qi, primary, Hanany, Shaul, primary, Borrill, Jullian, primary, Crill, Brendan, primary, Delabrouille, Jacques, primary, Devlin, Mark, primary, Flauger, Raphael, primary, Jones, William, primary, Knox, Lloyd, primary, Kogut, Alan, primary, Lawrence, Charles, primary, McMahon, Jeff, primary, Pryke, Clement, primary, Trangsrud, Amy, primary, Gorski, Krzysztof, primary, Johnson, Bradley, primary, Matsumura, Tomotake, primary, O'Brient, Roger, primary, Hills, Richard, primary, McGuire, James, primary, Bock, Jamie, primary, Battaglia, Nicholas, primary, Chuss, David, primary, and Sutin, Brian M., primary

Published
2018
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31. PICO - the probe of inflation and cosmic origins

Author

Sutin, Brian M., primary, Trangsrud, Amy R., primary, Hanany, Shaul, primary, O'Brient, Roger, primary, Paine, Christopher, primary, Bock, James, primary, Borrill, Jullian, primary, Crill, Brendan, primary, Delabrouille, Jacques, primary, Devlin, Mark, primary, Gorski, Krzysztof, primary, Flauger, Raphael, primary, Jones, William C., primary, Knox, lloyd, primary, Kogut, Alan, primary, Lawrence, Charles, primary, Matsumura, Tomotake, primary, McMahon, Jeff, primary, Pryke, Clement, primary, Johnson, Bradley R., primary, Alvarez, Marcelo, primary, Battaglia, Nicholas, primary, Bonato, Matteo, primary, Chuss, David T., primary, Cooperrider, Joelle, primary, Essinger-Hileman, Thomas, primary, Fissel, Laura, primary, Green, Daniel, primary, Hubmayr, Johannes, primary, Negrello, Mattia, primary, Shirron, Peter, primary, Wen, Qi, primary, Young, Karl, primary, and de Zotti, Gianfranco, primary

Published
2018
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34. Modelling the pulse transformer in SPICE

Author

Godlewska, Malgorzata, Gorecki, Krzysztof, and Gorski, Krzysztof

Abstract

The paper is devoted to modelling pulse transformers in SPICE. It shows the character of the selected models of this element, points out their advantages and disadvantages, and presents the results of experimental verification of the considered models. These models are characterized by varying degrees of complexity - from linearly coupled linear coils to nonlinear electrothermal models. The study was conducted for transformer with ring cores made of a variety of ferromagnetic materials, while exciting the sinusoidal signal of a frequency 100 kHz and different values of load resistance. The transformers operating conditions under which the considered models ensure the acceptable accuracy of calculations are indicated.

Published
2016

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