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3. The Atacama Cosmology Telescope: High-resolution component-separated maps across one-third of the sky

Author

Coulton, William R., Madhavacheril, Mathew S., Duivenvoorden, Adriaan J., Hill, J. Colin, Abril-Cabezas, Irene, Ade, Peter A. R., Aiola, Simone, Alford, Tommy, Amiri, Mandana, Amodeo, Stefania, An, Rui, Atkins, Zachary, Austermann, Jason E., Battaglia, Nicholas, Battistelli, Elia Stefano, Beall, James A., Bean, Rachel, Beringue, Benjamin, Bhandarkar, Tanay, Biermann, Emily, Bolliet, Boris, Bond, J Richard, Cai, Hongbo, Calabrese, Erminia, Calafut, Victoria, Capalbo, Valentina, Carrero, Felipe, Chesmore, Grace E., Cho, Hsiao-mei, Choi, Steve K., Clark, Susan E., Rosado, Rodrigo Córdova, Cothard, Nicholas F., Coughlin, Kevin, Crowley, Kevin T., Devlin, Mark J., Dicker, Simon, Doze, Peter, Duell, Cody J., Duff, Shannon M., Dunkley, Jo, Dünner, Rolando, Fanfani, Valentina, Fankhanel, Max, Farren, Gerrit, Ferraro, Simone, Freundt, Rodrigo, Fuzia, Brittany, Gallardo, Patricio A., Garrido, Xavier, Givans, Jahmour, Gluscevic, Vera, Golec, Joseph E., Guan, Yilun, Halpern, Mark, Han, Dongwon, Hasselfield, Matthew, Healy, Erin, Henderson, Shawn, Hensley, Brandon, Hervías-Caimapo, Carlos, Hilton, Gene C., Hilton, Matt, Hincks, Adam D., Hložek, Renée, Ho, Shuay-Pwu Patty, Huber, Zachary B., Hubmayr, Johannes, Huffenberger, Kevin M., Hughes, John P., Irwin, Kent, Isopi, Giovanni, Jense, Hidde T., Keller, Ben, Kim, Joshua, Knowles, Kenda, Koopman, Brian J., Kosowsky, Arthur, Kramer, Darby, Kusiak, Aleksandra, La Posta, Adrien, Lakey, Victoria, Lee, Eunseong, Li, Zack, Li, Yaqiong, Limon, Michele, Lokken, Martine, Louis, Thibaut, Lungu, Marius, MacCrann, Niall, MacInnis, Amanda, Maldonado, Diego, Maldonado, Felipe, Mallaby-Kay, Maya, Marques, Gabriela A., van Marrewijk, Joshiwa, McCarthy, Fiona, McMahon, Jeff, Mehta, Yogesh, Menanteau, Felipe, Moodley, Kavilan, Morris, Thomas W., Mroczkowski, Tony, Naess, Sigurd, Namikawa, Toshiya, Nati, Federico, Newburgh, Laura, Nicola, Andrina, Niemack, Michael D., Nolta, Michael R., Orlowski-Scherer, John, Page, Lyman A., Pandey, Shivam, Partridge, Bruce, Prince, Heather, Puddu, Roberto, Qu, Frank J., Radiconi, Federico, Robertson, Naomi, Rojas, Felipe, Sakuma, Tai, Salatino, Maria, Schaan, Emmanuel, Schmitt, Benjamin L., Sehgal, Neelima, Shaikh, Shabbir, Sherwin, Blake D., Sierra, Carlos, Sievers, Jon, Sifón, Cristóbal, Simon, Sara, Sonka, Rita, Spergel, David N., Staggs, Suzanne T., Storer, Emilie, Switzer, Eric R., Tampier, Niklas, Thornton, Robert, Trac, Hy, Treu, Jesse, Tucker, Carole, Ullom, Joel, Vale, Leila R., Van Engelen, Alexander, Van Lanen, Jeff, Vargas, Cristian, Vavagiakis, Eve M., Wagoner, Kasey, Wang, Yuhan, Wenzl, Lukas, Wollack, Edward J., Xu, Zhilei, Zago, Fernando, and Zheng, Kaiwen

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

Observations of the millimeter sky contain valuable information on a number of signals, including the blackbody cosmic microwave background (CMB), Galactic emissions, and the Compton-$y$ distortion due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Extracting new insight into cosmological and astrophysical questions often requires combining multi-wavelength observations to spectrally isolate one component. In this work, we present a new arcminute-resolution Compton-$y$ map, which traces out the line-of-sight-integrated electron pressure, as well as maps of the CMB in intensity and E-mode polarization, across a third of the sky (around 13,000 sq.~deg.). We produce these through a joint analysis of data from the Atacama Cosmology Telescope (ACT) Data Release 4 and 6 at frequencies of roughly 93, 148, and 225 GHz, together with data from the \textit{Planck} satellite at frequencies between 30 GHz and 545 GHz. We present detailed verification of an internal linear combination pipeline implemented in a needlet frame that allows us to efficiently suppress Galactic contamination and account for spatial variations in the ACT instrument noise. These maps provide a significant advance, in noise levels and resolution, over the existing \textit{Planck} component-separated maps and will enable a host of science goals including studies of cluster and galaxy astrophysics, inferences of the cosmic velocity field, primordial non-Gaussianity searches, and gravitational lensing reconstruction of the CMB., The Compton-y map and associated products will be made publicly available upon publication of the paper. The CMB T and E mode maps will be made available when the DR6 maps are made public

Published
2023

4. The Atacama Cosmology Telescope: Mitigating the impact of extragalactic foregrounds for the DR6 CMB lensing analysis

Author

MacCrann, Niall, Sherwin, Blake D., Qu, Frank J., Namikawa, Toshiya, Madhavacheril, Mathew S., Abril-Cabezas, Irene, An, Rui, Austermann, Jason E., Battaglia, Nicholas, Battistelli, Elia S., Beall, James A., Bolliet, Boris, Bond, J. Richard, Cai, Hongbo, Calabrese, Erminia, Coulton, William R., Darwish, Omar, Duff, Shannon M., Duivenvoorden, Adriaan J., Dunkley, Jo, Farren, Gerrit S., Ferraro, Simone, Golec, Joseph E., Guan, Yilun, Han, Dongwon, Hervías-Caimapo, Carlos, Hill, J. Colin, Hilton, Matt, Hložek, Renée, Hubmayr, Johannes, Kim, Joshua, Li, Zack, Kosowsky, Arthur, Louis, Thibaut, McMahon, Jeff, Marques, Gabriela A., Moodley, Kavilan, Naess, Sigurd, Niemack, Michael D., Page, Lyman, Partridge, Bruce, Schaan, Emmanuel, Sehgal, Neelima, Sifón, Cristóbal, Wollack, Edward J., Salatino, Maria, Ullom, Joel N., Van Lanen, Jeff, Van Engelen, Alexander, and Wenz, Lukas

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

We investigate the impact and mitigation of extragalactic foregrounds for the CMB lensing power spectrum analysis of Atacama Cosmology Telescope (ACT) data release 6 (DR6) data. Two independent microwave sky simulations are used to test a range of mitigation strategies. We demonstrate that finding and then subtracting point sources, finding and then subtracting models of clusters, and using a profile bias-hardened lensing estimator, together reduce the fractional biases to well below statistical uncertainties, with the inferred lensing amplitude, $A_{\mathrm{lens}}$, biased by less than $0.2\sigma$. We also show that another method where a model for the cosmic infrared background (CIB) contribution is deprojected and high frequency data from Planck is included has similar performance. Other frequency-cleaned options do not perform as well, incurring either a large noise cost, or resulting in biased recovery of the lensing spectrum. In addition to these simulation-based tests, we also present null tests performed on the ACT DR6 data which test for sensitivity of our lensing spectrum estimation to differences in foreground levels between the two ACT frequencies used, while nulling the CMB lensing signal. These tests pass whether the nulling is performed at the map or bandpower level. The CIB-deprojected measurement performed on the DR6 data is consistent with our baseline measurement, implying contamination from the CIB is unlikely to significantly bias the DR6 lensing spectrum. This collection of tests gives confidence that the ACT DR6 lensing measurements and cosmological constraints presented in companion papers to this work are robust to extragalactic foregrounds., Comment: Companion paper to Qu et al and Madhavacheril et al

Published
2023

5. The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters

Author

Madhavacheril, Mathew S., Qu, Frank J., Sherwin, Blake D., MacCrann, Niall, Li, Yaqiong, Abril-Cabezas, Irene, Ade, Peter A. R., Aiola, Simone, Alford, Tommy, Amiri, Mandana, Amodeo, Stefania, An, Rui, Atkins, Zachary, Austermann, Jason E., Battaglia, Nicholas, Battistelli, Elia Stefano, Beall, James A., Bean, Rachel, Beringue, Benjamin, Bhandarkar, Tanay, Biermann, Emily, Bolliet, Boris, Bond, J Richard, Cai, Hongbo, Calabrese, Erminia, Calafut, Victoria, Capalbo, Valentina, Carrero, Felipe, Challinor, Anthony, Chesmore, Grace E., Cho, Hsiao-mei, Choi, Steve K., Clark, Susan E., Rosado, Rodrigo Córdova, Cothard, Nicholas F., Coughlin, Kevin, Coulton, William, Crowley, Kevin T., Dalal, Roohi, Darwish, Omar, Devlin, Mark J., Dicker, Simon, Doze, Peter, Duell, Cody J., Duff, Shannon M., Duivenvoorden, Adriaan J., Dunkley, Jo, Dünner, Rolando, Fanfani, Valentina, Fankhanel, Max, Farren, Gerrit, Ferraro, Simone, Freundt, Rodrigo, Fuzia, Brittany, Gallardo, Patricio A., Garrido, Xavier, Givans, Jahmour, Gluscevic, Vera, Golec, Joseph E., Guan, Yilun, Hall, Kirsten R., Halpern, Mark, Han, Dongwon, Harrison, Ian, Hasselfield, Matthew, Healy, Erin, Henderson, Shawn, Hensley, Brandon, Hervías-Caimapo, Carlos, Hill, J. Colin, Hilton, Gene C., Hilton, Matt, Hincks, Adam D., Hložek, Renée, Ho, Shuay-Pwu Patty, Huber, Zachary B., Hubmayr, Johannes, Huffenberger, Kevin M., Hughes, John P., Irwin, Kent, Isopi, Giovanni, Jense, Hidde T., Keller, Ben, Kim, Joshua, Knowles, Kenda, Koopman, Brian J., Kosowsky, Arthur, Kramer, Darby, Kusiak, Aleksandra, La Posta, Adrien, Lague, Alex, Lakey, Victoria, Lee, Eunseong, Li, Zack, Limon, Michele, Lokken, Martine, Louis, Thibaut, Lungu, Marius, MacInnis, Amanda, Maldonado, Diego, Maldonado, Felipe, Mallaby-Kay, Maya, Marques, Gabriela A., McMahon, Jeff, Mehta, Yogesh, Menanteau, Felipe, Moodley, Kavilan, Morris, Thomas W., Mroczkowski, Tony, Naess, Sigurd, Namikawa, Toshiya, Nati, Federico, Newburgh, Laura, Nicola, Andrina, Niemack, Michael D., Nolta, Michael R., Orlowski-Scherer, John, Page, Lyman A., Pandey, Shivam, Partridge, Bruce, Prince, Heather, Puddu, Roberto, Radiconi, Federico, Robertson, Naomi, Rojas, Felipe, Sakuma, Tai, Salatino, Maria, Schaan, Emmanuel, Schmitt, Benjamin L., Sehgal, Neelima, Shaikh, Shabbir, Sierra, Carlos, Sievers, Jon, Sifón, Cristóbal, Simon, Sara, Sonka, Rita, Spergel, David N., Staggs, Suzanne T., Storer, Emilie, Switzer, Eric R., Tampier, Niklas, Thornton, Robert, Trac, Hy, Treu, Jesse, Tucker, Carole, Ulluom, Joel, Vale, Leila R., Van Engelen, Alexander, Van Lanen, Jeff, van Marrewijk, Joshiwa, Vargas, Cristian, Vavagiakis, Eve M., Wagoner, Kasey, Wang, Yuhan, Wenzl, Lukas, Wollack, Edward J., Xu, Zhilei, Zago, Fernando, and Zhang, Kaiwen

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

We present cosmological constraints from a gravitational lensing mass map covering 9400 sq. deg. reconstructed from CMB measurements made by the Atacama Cosmology Telescope (ACT) from 2017 to 2021. In combination with BAO measurements (from SDSS and 6dF), we obtain the amplitude of matter fluctuations $\sigma_8 = 0.819 \pm 0.015$ at 1.8% precision, $S_8\equiv\sigma_8({\Omega_{\rm m}}/0.3)^{0.5}=0.840\pm0.028$ and the Hubble constant $H_0= (68.3 \pm 1.1)\, \text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1}$ at 1.6% precision. A joint constraint with CMB lensing measured by the Planck satellite yields even more precise values: $\sigma_8 = 0.812 \pm 0.013$, $S_8\equiv\sigma_8({\Omega_{\rm m}}/0.3)^{0.5}=0.831\pm0.023$ and $H_0= (68.1 \pm 1.0)\, \text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1}$. These measurements agree well with $\Lambda$CDM-model extrapolations from the CMB anisotropies measured by Planck. To compare these constraints to those from the KiDS, DES, and HSC galaxy surveys, we revisit those data sets with a uniform set of assumptions, and find $S_8$ from all three surveys are lower than that from ACT+Planck lensing by varying levels ranging from 1.7-2.1$\sigma$. These results motivate further measurements and comparison, not just between the CMB anisotropies and galaxy lensing, but also between CMB lensing probing $z\sim 0.5-5$ on mostly-linear scales and galaxy lensing at $z\sim 0.5$ on smaller scales. We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $\Lambda$CDM, limiting the sum of the neutrino masses to $\sum m_{\nu} < 0.12$ eV (95% c.l.), for example. Our results provide independent confirmation that the universe is spatially flat, conforms with general relativity, and is described remarkably well by the $\Lambda$CDM model, while paving a promising path for neutrino physics with gravitational lensing from upcoming ground-based CMB surveys., Comment: 30 pages, 16 figures, prepared for submission to ApJ. Cosmological likelihood data is here: https://lambda.gsfc.nasa.gov/product/act/actadv_prod_table.html ; likelihood software is here: https://github.com/ACTCollaboration/act_dr6_lenslike . Also see companion papers Qu et al and MacCrann et al. Mass maps will be released when papers are published

Published
2023

6. The Atacama Cosmology Telescope: Systematic Transient Search of 3-Day Maps

Author

Li, Yaqiong, Biermann, Emily, Naess, Sigurd, Aiola, Simone, An, Rui, Battaglia, Nicholas, Bhandarkar, Tanay, Calabrese, Erminia, Choi, Steve K., Crowley, Kevin T., Devlin, Mark, Duell, Cody J., Duff, Shannon M., Dunkley, Jo, Dunner, Rolando, Gallardo, Patricio A., Guan, Yilun, Hervias-Caimapo, Carlos, Hincks, Adam D., Hubmayr, Johannes, Huffenberger, Kevin M., Hughes, John P., Kosowsky, Arthur, Louis, Thibaut, Mallaby-Kay, Maya, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman, Sifon, Cristobal, Salatino, Maria, Staggs, Suzanne T., Vargas, Cristian, Vavagiakis, Eve M., Wang, Yuhan, and Wollack, Edward J.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

We conduct a systematic search for transients in three years of data (2017-2019) from the Atacama Cosmology Telescope (ACT). ACT covers 40 percent of the sky at three bands spanning from 77 GHz to 277 GHz. Analysis of 3-day mean-subtracted sky maps, which were match-filtered for point sources, yielded 29 transients detections. Eight of these transients are due to known asteroids, and three others were previously published. Four of these events occur in areas of with poor noise models and thus we cannot be confident they are real transients. We are left with 14 new transient events occurring at 11 unique locations. All of these events are associated with either rotationally variable stars or cool stars. Ten events have flat or falling spectra indicating radiation from synchrotron emission. One event has a rising spectrum indicating a different engine for the flare.

Published
2023

7. Astro2020 APC White Paper Project: The Simons Observatory

Author

Abitbol, Maximilian H, Adachi, Shunsuke, Ade, Peter, Aguirre, James, Ahmed, Zeeshan, Aiola, Simone, Ali, Aamir, Alonso, David, Alvarez, Marcelo A, Arnold, Kam, Ashton, Peter, Atkins, Zachary, Austermann, Jason, Awan, Humna, Baccigalupi, Carlo, Baildon, Taylor, Lizancos, Anton Baleato, Barron, Darcy, Battaglia, Nick, Battye, Richard, Baxter, Eric, Bazarko, Andrew, Beall, James A, Bean, Rachel, Beck, Dominic, Beckman, Shawn, Beringue, Benjamin, Bhandarkar, Tanay, Bhimani, Sanah, Bianchini, Federico, Boada, Steven, Boettger, David, Bolliet, Boris, Bond, J. Richard, Borrill, Julian, Brown, Michael L, Bruno, Sarah Marie, Bryan, Sean, Calabrese, Erminia, Calafut, Victoria, Calisse, Paolo, Carron, Julien, Carl, Fred. M, Cayuso, Juan, Challinor, Anthony, Chesmore, Grace, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Clark, Susan, Clarke, Philip, Contaldi, Carlo, Coppi, Gabriele, Cothard, Nicholas F, Coughlin, Kevin, Coulton, Will, Crichton, Devin, Crowley, Kevin D, Crowley, Kevin T, Cukierman, Ari, D’Ewart, John M, D¨unner, Rolando, Haan, Tijmen de, Devlin, Mark, Dicker, Simon, Dober, Bradley, Duell, Cody J, Duff, Shannon, Duivenvoorden, Adri, Dunkley, Jo, Bouhargani, Hamza El, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Fergusson, James, Ferraro, Simone, Flux`a, Pedro, Freese, Katherine, Frisch, Josef C, Frolov, Andrei, Fuller, George, Galitzki, Nicholas, Gallardo, Patricio A, Ghersi, Jose Tomas Galvez, Gao, Jiansong, Gawiser, Eric, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Golec, Joseph, Gordon, Sam, Gralla, Megan, Green, Daniel, Grigorian, Arpi, Groh, John, Groppi, Chris, Guan, Yilun, Gudmundsson, Jon E, Halpern, Mark, Han, Dongwon, Hargrave, Peter, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hattori, Makoto, Haynes, Victor, Hazumi, Masashi, Healy, Erin, Henderson, Shawn W, Hensley, Brandon, Hervias-Caimapo, Carlos, Hill, Charles A, Hill, J. Colin, Hilton, Gene, Hilton, Matt, Hincks, Adam D, Hinshaw, Gary, Hlozek, Renee, Ho, Shirley, Ho, Shuay-Pwu Patty, Hoang, Thuong D, Hoh, Jonathan, Hotinli, Selim C, Huang, Zhiqi, Hubmayr, Johannes, Huffenberger, Kevin, Hughes, John P, Ijjas, Anna, Ikape, Margaret, Irwin, Kent, Jaffe, Andrew H, Jain, Bhuvnesh, Jeong, Oliver, Johnson, Matthew, Kaneko, Daisuke, Karpel, Ethan D, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kiuchi, Kenji, Klein, Jeff, Knowles, Kenda, Kofman, Anna, Koopman, Brian, Kosowsky, Arthur, Krachmalnicoff, Nicoletta, Kusaka, Akito, LaPlante, Phil, Lashner, Jacob, Lee, Adrian, Lee, Eunseong, Lewis, Antony, Li, Yaqiong, Li, Zack, Limon, Michele, Linder, Eric, Liu, Jia, Lopez-Caraballo, Carlos, Louis, Thibaut, Lungu, Marius, Madhavacheril, Mathew, Mak, Daisy, Maldonado, Felipe, Mani, Hamdi, Mates, Ben, Matsuda, Frederick, Maurin, Loıc, Mauskopf, Phil, May, Andrew, McCallum, Nialh, McCarrick, Heather, McKenney, Chris, McMahon, Jeff, Meerburg, P. Daniel, Mertens, James, Meyers, Joel, Miller, Amber, Mirmelstein, Mark, Moodley, Kavilan, Moore, Jenna, Munchmeyer, Moritz, Munson, Charles, Murata, Masaaki, Naess, Sigurd, Namikawa, Toshiya, Nati, Federico, Navaroli, Martin, Newburgh, Laura, Nguyen, Ho Nam, Nicola, Andrina, Niemack, Mike, Nishino, Haruki, Nishinomiya, Yume, Orlowski-Scherer, John, Pagano, Luca, Partridge, Bruce, Perrotta, Francesca, Phakathi, Phumlani, Piccirillo, Lucio, Pierpaoli, Elena, Pisano, Giampaolo, Poletti, Davide, Puddu, Roberto, Puglisi, Giuseppe, Raum, Chris, Reichardt, Christian L, Remazeilles, Mathieu, Rephaeli, Yoel, Riechers, Dominik, Rojas, Felipe, Rotti, Aditya, Roy, Anirban, Sadeh, Sharon, Sakurai, Yuki, Salatino, Maria, Rao, Mayuri Sathyanarayana, Saunders, Lauren, Schaan, Emmanuel, Schmittfull, Marcel, Sehgal, Neelima, Seibert, Joseph, Seljak, Uros, Shellard, Paul, Sherwin, Blake, Shimon, Meir, Sierra, Carlos, Sievers, Jonathan, Sifon, Cristobal, Sikhosana, Precious, Silva-Feaver, Maximiliano, Simon, Sara M, Sinclair, Adrian, Smith, Kendrick, Sohn, Wuhyun, Sonka, Rita, Spergel, David, Spisak, Jacob, Staggs, Suzanne T, Stein, George, Stevens, Jason R, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Takakura, Satoru, Teply, Grant, Thomas, Daniel B, Thorne, Ben, Thornton, Robert, Trac, Hy, Treu, Jesse, Tsai, Calvin, Tucker, Carole, Ullom, Joel, Vagnozzi, Sunny, Engelen, Alexander van, Lanen, Jeff Van, Winkle, Daniel D. Van, Vavagiakis, Eve M, Verg`es, Clara, Vissers, Michael, Wagoner, Kasey, Walker, Samantha, Wang, Yuhan, Ward, Jon, Westbrook, Ben, Whitehorn, Nathan, Williams, Jason, Williams, Joel, Wollack, Edward, Xu, Zhilei, Yasini, Siavash, Young, Edward, Yu, Byeonghee, Yu, Cyndia, Zago, Fernando, Zannoni, Mario, Zhang, Hezi, Zheng, Kaiwen, Zhu, Ningfeng, and Zonca, Andrea

Subjects
Astrophysics
Abstract

The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form (‘SO-Nominal’) consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating (“Stage 3”) experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4. Construction of SO-Nominal is fully funded, and operations and data analysis are funded for part of the planned five-year observations. We will seek federal funding to complete the observations and analysis of SO-Nominal, at the $25M level. The SO has a low risk and cost efficient upgrade path – the 6 m LAT can accommodate almost twice the baseline number of detectors and the SATs can be duplicated at low cost. We will seek funding at the $75M level for an expansion of the SO (‘SO-Enhanced’) that fills the remaining focal plane in the LAT, adds three SATs, and extends operations by five years, substantially improving our science return. By this time SO may be operating as part of the larger CMB-S4 project. This white paper summarizes and extends material presented in, which describes the science goals of SO-Nominal, and which describe the instrument design.

Published
2019

8. CMB-S4 Decadal Survey APC White Paper

Author

Abazajian, Kevork, Addison, Graeme, Adshead, Peter, Ahmed, Zeeshan, Allen, Steven W, Alonso, David, Alvarez, Marcelo, Anderson, Adam, Arnold, Kam S, Baccigalupi, Carlo, Bailey, Kathy, Barkats, Denis, Barron, Darcy, Barry, Peter S, Bartlett, James G, Thakur, Ritoban Basu, Battaglia, Nicholas, Baxter, Eric, Bean, Rachel, Bebek, Chris, Bender, Amy N, Benson, Bradford A, Berger, Edo, Bhimani, Sanah, Bischoff, Colin A, Bleem, Lindsey, Bocquet, Sebastian, Boddy, Kimberly, Bonato, Matteo, Bond, J. Richard, Borrill, Julian, Bouchet, Francois R, Brown, Michael L, Bryan, Sean, Burkhart, Blakesley, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E, Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L, Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Crawford, Thomas M, Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, Haan, Tijmen de, Zotti, Gianfranco de, Delabrouille, Jacques, Demarteau, Marcel, Devlin, Mark, Valentino, Eleonora Di, Dobbs, Matt, Duff, Shannon, Duivenvoorden, Adriaan, Dvorkin, Cora, Edwards, William, Eimer, Joseph, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P, Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A, Frolov, Andrei, Galitzki, Nicholas, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gilchriese, Murdock, Gluscevic, Vera, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Victor, Gudmundsson, Jon E, Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W, Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Henning, Jason W, Hill, J. Colin, Hlozek, Renee, Holder, Gil, Holzapfel, William, Hubmayr, Johannes, Huffenberger, Kevin M, Huffer, Michael, Hui, Howard, Irwin, Kent, Johnson, Bradley R, Johnstone, Doug, Jones, William C, Karkare, Kirit, Katayama, Nobuhiko, Kerby, James, Kernovsky, Sarah, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Kosowsky, Arthur, Kovac, John, Kovetz, Ely D, Kuhlmann, Steve, Kuo, Chao-lin, Kurita, Nadine, Kusaka, Akito, Lahteenmaki, Anne, Lawrence, Charles R, Lee, Adrian T, Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Madhavacheril, Mathew S, Mantz, Adam, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, Meerburg, P. Daniel, Melin, Jean-Baptiste, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Mroczkowski, Tony, Mukherjee, Suvodip, Munchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Negrello, Mattia, Newburgh, Laura, Niemack, Michael D, Nishino, Haruki, Nordby, Martin, Novosad, Valentine, O’Connor, Paul, Obied, Georges, Padin, Stephen, Pandey, Shivam, Partridge, Bruce, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Rajagopalan, Srini, Raveri, Marco, Reichanadter, Mark, Reichardt, Christian L, Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A, Roy, Anirban, Ruhl, John, Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel M, Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sheehy, Christopher, Sherwin, Blake D, Shirokoff, Erik, Simon, Sara M, Slosar, Anze, Somerville, Rachel, Staggs, Suzanne T, Stark, Antony, Stompor, Radek, Story, Kyle T, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P, Thompson, Keith, Timbie, Peter, Tomasi, Maurizio, Treu, Jesse I, Tristram, Matthieu, Tucker, Gregory, Umilta, Caterina, Engelen, Alexander van, Vieira, Joaquin D, Vieregg, Abigail G, Vogelsberger, Mark, Wang, Gensheng, Watson, Scott, White, Martin, Whitehorn, Nathan, Wollack, Edward J, Wu, W. L. Kimmy, Xu, Zhilei, Yasini, Siavash, Yeck, James, Yoon, Ki Won, Young, Edward, and Zonca, Andrea

Subjects
Astrophysics
Abstract

CMB-S4 is envisioned to be the ultimate ground-based cosmic microwave background experiment, crossing critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. The CMB-S4 science case is spectacular: the search for primordial gravitational waves as predicted from inflation and the imprint of relic particles including neutrinos, unique insights into dark energy and tests of gravity on large scales, elucidating the role of baryonic feedback on galaxy formation and evolution, opening up a window on the transient Universe at millimeter wavelengths, and even the exploration of the outer Solar System. The CMB-S4 sensitivity to primordial gravitational waves will probe physics at the highest energy scales and cross a major theoretically motivated threshold in constraints on inflation. The CMB-S4 search for new light relic particles will shed light on the early Universe 10,000 times farther back than current experiments can reach. Finally, the CMB-S4 Legacy Survey covering 70% of the sky with unprecedented sensitivity and angular resolution from centimeter- to millimeter-wave observing bands will have a profound and lasting impact on Astronomy and Astrophysics and provide a powerful complement to surveys at other wavelengths, such as LSST and WFIRST, and others yet to be imagined. We emphasize that these critical thresholds cannot be reached without the level of community and agency investment and commitment required by CMB-S4. In particular, the CMB-S4 science goals are out of the reach of any projected precursor experiment by a significant margin.

Published
2019

9. Report of the Topical Group on Cosmic Frontier 5 Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before for Snowmass 2021

Author

Chang, Clarence L., Newburgh, Laura, Shoemaker, Deirdre, Ballmer, Stefan W., Green, Daniel, Hlozek, Renee, Huffenberger, Kevin M., Karkare, Kirit S., Liu, Adrian, Mandic, Vuk, Mcmahon, Jeff, and Benjamin Wallisch

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

This report summarizes the envisioned research activities as gathered from the Snowmass 2021 CF5 working group concerning Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before. The scientific goals are to study inflation and to search for new physics through precision measurements of relic radiation from the early universe. The envisioned research activities for this decade (2025-35) are constructing and operating major facilities and developing critical enabling capabilities. The major facilities for this decade are the CMB-S4 project, a new Stage-V spectroscopic survey facility, and existing gravitational wave observatories. Enabling capabilities include aligning and investing in theory, computation and model building, and investing in new technologies needed for early universe studies in the following decade (2035+)., contribution to Snowmass 2021

Published
2022

10. BECAUSE ART: Commentary, Critique & Conversation

Author

McMahon, Jeff

Subjects
Literature/writing, Women's issues/gender studies
Abstract

BECAUSE ART Commentary, Critique & Conversation by John R. Killacky Onion River Press. 252 pages, $20. THIS IS a collection of 56 pieces, written for 39 publications, including this one, [...]

Published
2022

11. The Primordial Inflation Polarization Explorer (PIPER): Current Status and Performance of the First Flight

Author

Pawlyk, Samuel, Ade, Peter A. R, Benford, Dominic, Bennett, Charles L, Chuss, David T, Datta, Rahul, Dotson, Jessie L, Eimer, Joseph R, Fixsen, Dale J, Gandilo, Natalie N, Essinger-Hileman, Thomas, Halpern, Mark, Hilton, Gene, Hinshaw, Gary F, Irwin, Kent, Jhabvala, Christine, Kimball, Mark, Kogut, Alan, Lowe, Luke, McMahon, Jeff J, Miller, Timothy M, Mirel, Paul, Moseley, S. Harvey, Rodriguez, Samelys, Sharp, Elmer III, Shirron, Peter, Staguhn, Johannes G, Sullivan, Dan F, Switzer, Eric R, Taraschi, Peter, Tucker, Carole E, Walts, Alexander, and Wollack, Edward J

Subjects
Optics
Abstract

The Primordial Inflation Polarization ExploreR (PIPER) is a balloon-borne instrument optimized to measure the polarization of the CMB at large angular scales. It will map 85% of the sky over a series of conventional balloon flights from the Northern and Southern hemispheres, measuring the B-mode polarization power spectrumover a range of multipoles from 2-300 covering both the reionization bump and the recombination peak, with sensitivity to measure the tensor-to-scalar ratio down to r = 0.007. PIPER will observe in four frequency bands centered at 200, 270, 350, and 600 GHz to characterize dust foregrounds. The instrument has background-limited sensitivity provided by fully cryogenic (1.7 K) optics focusing the sky signal onto kilo-pixel arrays of time-domain multiplexed Transition-Edge Sensor (TES) bolometers held at 100 mK. Polarization sensitivity and systematiccontrol are provided by front-end Variable-delay Polarization Modulators (VPMs). PIPER had its engineering flight in October 2017 from Fort Sumner, New Mexico. This papers outlines the major components in the PIPER system discussing the conceptual design as well as specific choices made for PIPER. We also report on the results of the engineering flight, looking at the functionality of the payload systems, particularly VPM, as well as pointing out areas of improvement.

Published
2018
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12. 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

13. PICO - the Probe of Inflation and Cosmic Origins

Author

Sutin, Brian M, Alvarez, Marcelo, Battaglia, Nicholas, Bock, Jamie, Borrill, Julian, Chuss, David T, Cooperrider, Joelle, Crill, Brendan, Delabrouille, Jacques, Delvin, 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, and Bonato, Matteo

Published
2018

14. The Atacama Cosmology Telescope: The Persistence of Neutrino Self-Interaction in Cosmological Measurements

Author

Kreisch, Christina D., Park, Minsu, Calabrese, Erminia, Cyr-Racine, Francis-Yan, An, Rui, Bond, J. Richard, Dore, Olivier, Dunkley, Jo, Gallardo, Patricio, Gluscevic, Vera, Hill, J. Colin, Hincks, Adam D., Madhavacheril, Mathew S., McMahon, Jeff, Moodley, Kavilan, Morris, Thomas W., Nati, Federico, Page, Lyman A., Partridge, Bruce, Salatino, Maria, Sifon, Cristobal, Spergel, David N., Vargas, Cristian, and Wollack, Edward J.

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

We use data from the Atacama Cosmology Telescope (ACT) DR4 to search for the presence of neutrino self-interaction in the cosmic microwave background. Consistent with prior works, the posterior distributions we find are bimodal, with one mode consistent with $\Lambda$CDM and one where neutrinos strongly self-interact. By combining ACT data with large-scale information from WMAP, we find that a delayed onset of neutrino free streaming caused by significantly strong neutrino self-interaction is compatible with these data at the $2-3\sigma$ level. As seen in the past, the preference shifts to $\Lambda$CDM with the inclusion of Planck data. We determine that the preference for strong neutrino self-interaction is largely driven by angular scales corresponding to $700 \lesssim \ell \lesssim 1000$ in the ACT E-mode polarization data. This region is expected to be key to discriminate between neutrino self-interacting modes and will soon be probed with more sensitive data., Comment: added additional references, 9+10 pages, 4+8 figures

Published
2022

15. BFORE: The B-mode Foreground Experiment

Author

Niemack, Michael D., Ade, Peter, de Bernardis, Francesco, Boulanger, Francois, Bryan, Sean, Devlin, Mark, Dunkley, Joanna, Eales, Steve, Gomez, Haley, Groppi, Chris, Henderson, Shawn, Hillbrand, Seth, Hubmayr, Johannes, Mauskopf, Philip, McMahon, Jeff, Miville-Deschênes, Marc-Antoine, Pascale, Enzo, Pisano, Giampaolo, Novak, Giles, Scott, Douglas, Soler, Juan, and Tucker, Carole

Published
2016
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16. Two-Season Atacama Cosmology Telescope Polarimeter Lensing Power Spectrum

Author

Shewin, Blake D, van Engelen, Alexander, Sehgal, Neelima, Madhavacheril, Mathew, Addison, Graeme E, Aiola, Simone, Allison, Rupert, Battaglia, Nicholas, Becker, Daniel T, Beall, James A, Bond, J. Richard, Calabrese, Ermini, Datta, Rahul, Devlin, Mark J, Dunner, Rolando, Dunkley, Joanna, Fox, Anna E, Gallardo, Patricio, Halpern, Mark, Hasselfield, Matthew, Henderson, Shawn, Hill, J. Colin, Hilton, Gene C, Hubmayr, Johannes, Hughes, John P, Hincks, Adam D, Hlozek, Renee, Huffenberger, Kevin M, Koopman, Brian, Kosowsky, Arthur, Louis, Thibaut, Maurin, Loic, McMahon, Jeff, Moodley, Kavilan, Naess, Sigurd, Nati, Federico, Newburgh, Laura, Niemack, Michael D, Page, Lyman A, Sievers, Jonathan, Spergel, David N, Staggs, Suzanne T, Thornton, Robert J, Van Lanen, Jeff, Vavagiakis, Eve, and Wollack, Edward J

Subjects
Astrophysics
Abstract

We report a measurement of the power spectrum of cosmic microwave background (CMB) lensing from two seasons of Atacama Cosmology Telescope polarimeter (ACTPol) CMB data. The CMB lensing power spectrum is extracted from both temperature and polarization data using quadratic estimators. We obtain results that are consistent with the expectation from the best-fit Planck CDM model over a range of multipoles L 80-2100, with an amplitude of lensing A(sub lens) = 1.06 +/- 0.15 stat +/- 0.06 sys relative to Planck. Our measurement of the CMB lensing power spectrum gives sigma 8 omega m(sup 0.25) = 0.643 +/- 0.054; including baryon acoustic oscillation scale data, we constrain the amplitude of density fluctuations to be sigma 8 = 0.831 +/- 0.053. We also update constraints on the neutrino mass sum. We verify our lensing measurement with a number of null tests and systematic checks, finding no evidence of significant systematic errors. This measurement relies on a small fraction of the ACTPol data already taken; more precise lensing results can therefore be expected from the full ACTPol data set.

Published
2017
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17. The Atacama Cosmology Telescope: Two-Season ACTPol Spectra and Parameters

Author

Louis, Thibaut, Grace, Emily, Hasselfield, Matthew, Lungu, Marius, Maurin, Loic, Addison, Graeme E, Adem Peter A. R, Aiola, Simone, Allison, Rupert, Amiri, Mandana, Angile, Elio, Battaglia, Nicholas, Beall, James A, De Bernardis, Francesco, Bond, J. Richard, Britton, Joe, Calabrese, Erminia, Cho, Hsiao-mei, Choi, Steve K, Coughlin, Kevin, Crichton, Devin, Crowley, Kevin, Datta, Rahul, Devlin, Mark J, Dicker, Simon R, Dunkley, Joanna, Dunner, Rolando, Ferraro, Simone, Fox, Anna E, Gallardo, Patricio, Gralla, Megan, Halpern, Mark, Henderson, Shawn, Hill, J. Colin, Hilton, Gene C, Hilton, Matt, Hincks, Adam D, Hlozek, Renee, Ho, S. P. Patty, Huang, Zhiqi, Hubmayr, Johannes, Huffenberger, Kevin M, Hughes, John P, Infante, Leopoldo, Irwin, Kent, Kasanda, Simon Muya, Klein, Jeff, Koopman, Brian, Kosowsky, Arthur, Li, Dale, Madhavacheril, Mathew, Marriage, Tobias A, McMahon, Jeff, Menanteau, Felipe, Moodley, Kavilan, Munson, Charles, Naess, Sigurd, Nati, Federico, Newburgh, Laura, Nibarger, John, Niemack, Michael D, Nolta, Michael R, Nunez, Carolina, Pappas, Christine, Partridge, Bruce, Rojas, Felipe, Schaan, Emmanuel, Schmitt, Benjamin L, Sehgal, Neelima, Sherwin, Blake D, Sievers, Jon, Simon, Sara, Spergel, David N, Staggs, Suzanne T, Switzer, Eric R, Thornton, Robert, Trac, Hy, Treu, Jesse, Tucker, Carole, Van Engelen, Alexander, Ward, Jonathan T, and Wollack, Edward J

Subjects
Astrophysics, Statistics And Probability
Abstract

We present the temperature and polarization angular power spectra measuredby the Atacama Cosmology Telescope Polarimeter (ACTPol). We analyze night-time datacollected during 2013-14 using two detector arrays at 149 GHz, from 548 deg(exp. 2) of sky onthe celestial equator. We use these spectra, and the spectra measured with the MBAC camera on ACT from 2008-10, in combination with Planck and WMAP data to estimate cosmological parameters from the temperature, polarization, and temperature-polarization cross-correlations. We find the new ACTPol data to be consistent with the CDM model. The ACTPol temperature-polarization cross-spectrum now provides stronger constraints on multiple parameters than the ACTPol temperature spectrum, including the baryon density, the acoustic peak angular scale, and the derived Hubble constant. The new ACTPol dataprovide information on damping tail parameters. The joint uncertainty on the number of neutrino species and the primordial helium fraction is reduced by 20% when adding ACTPol to Planck temperature data alone.

Published
2017
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19. Ideas in Motion: A Teaching Artist Uses Dance to Confront Stereotypes.

Author

McMahon, Jeff

Abstract

Examines the ways a teaching artist, a dancer, uses movement as the point from which he and students gain a new perspective. The critical thinking that results from student responses to dance often gives voice to stereotypes that block students' broader vision and acceptance of diversity. (SLD)

Published
1996

20. The Design and Characterization of Wideband Spline-profiled Feedhorns for Advanced Actpol

Author

Simon, Sara M, Austermann, Jason, Beall, James A, Choi, Steve K, Coughlin, Kevin P, Duff, Shannon M, Gallardo, Patricio A, Henderson, Shawn W, Hills, Felicity B, Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Josaitis, Alec, Koopman, Brian J, McMahon, Jeff J, Nati, Federico, Newburgh, Laura, Niemack, Michael D, Salatino, Maria, Schillaci, Alessandro, and Wollack, Edward J

Subjects
Instrumentation And Photography, Astrophysics
Abstract

Advanced ACTPol (AdvACT) is an upgraded camera for the Atacama Cosmology Telescope (ACT) that will measure the cosmic microwave background in temperature and polarization over a wide range of angular scales and five frequency bands from 28-230 GHz. AdvACT will employ four arrays of feedhorn-coupled, polarization- sensitive multichroic detectors. To accommodate the higher pixel packing densities necessary to achieve Ad- vACTs sensitivity goals, we have developed and optimized wideband spline-profiled feedhorns for the AdvACT multichroic arrays that maximize coupling efficiency while carefully controlling polarization systematics. We present the design, fabrication, and testing of wideband spline-profiled feedhorns for the multichroic arrays of AdvACT.

Published
2016
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21. Optical Modeling and Polarization Calibration for CMB Measurements with Actpol and Advanced Actpol

Author

Koopman, Brian, Austermann, Jason, Cho, Hsiao-Mei, Coughlin, Kevin P, Duff, Shannon M, Gallardo, Patricio A, Hasselfield, Matthew, Henderson, Shawn W, Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Irwin, Kent D, Li, Dale, McMahon, Jeff, Nati, Federico, Niemack, Michael D, Newburgh, Laura, Page, Lyman A, Salatino, Maria, Schillaci, Alessandro, Schmitt, Benjamin L, Simon, Sara M, Vavagiakis, Eva M, Ward, Jonathan T, and Wollack, Edward J

Subjects
Astrophysics
Abstract

The Atacama Cosmology Telescope Polarimeter (ACTPol) is a polarization sensitive upgrade to the Atacama Cosmology Telescope, located at an elevation of 5190 m on Cerro Toco in Chile. ACTPol uses transition edge sensor bolometers coupled to orthomode transducers to measure both the temperature and polarization of the Cosmic Microwave Background (CMB). Calibration of the detector angles is a critical step in producing polarization maps of the CMB. Polarization angle offsets in the detector calibration can cause leakage in polarization from E to B modes and induce a spurious signal in the EB and TB cross correlations, which eliminates our ability to measure potential cosmological sources of EB and TB signals, such as cosmic birefringence. We calibrate the ACTPol detector angles by ray tracing the designed detector angle through the entire optical chain to determine the projection of each detector angle on the sky. The distribution of calibrated detector polarization angles are consistent with a global offset angle from zero when compared to the EB-nulling offset angle, the angle required to null the EB cross-correlation power spectrum. We present the optical modeling process. The detector angles can be cross checked through observations of known polarized sources, whether this be a galactic source or a laboratory reference standard. To cross check the ACTPol detector angles, we use a thin film polarization grid placed in front of the receiver of the telescope, between the receiver and the secondary reflector. Making use of a rapidly rotating half-wave plate (HWP) mount we spin the polarizing grid at a constant speed, polarizing and rotating the incoming atmospheric signal. The resulting sinusoidal signal is used to determine the detector angles. The optical modeling calibration was shown to be consistent with a global offset angle of zero when compared to EB nulling in the first ACTPol results and will continue to be a part of our calibration implementation. The first array of detectors for Advanced ACTPol, the next generation upgrade to ACTPol, will be deployed in 2016.We plan to continue using both techniques and compare them to astrophysical source measurements for the Advanced ACTPol polarization calibration.

Published
2016
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22. Constraining CMB temperature evolution with Sunyaev-Zel'dovich galaxy clusters from the Atacama Cosmology Telescope

Author

Li, Yunyang, Hincks, Adam D., Amodeo, Stefania, Battistelli, Elia S., Bond, J. Richard, Calabrese, Erminia, Choi, Steve K., Devlin, Mark J., Dunkley, Jo, Ferraro, Simone, Gluscevic, Vera, Guan, Yilun, Halpern, Mark, Hilton, Matt, Hlozek, Renee, Marriage, Tobias A., McMahon, Jeff, Moodley, Kavilan, Naess, Sigurd, Nati, Federico, Niemack, Michael D., Orlowski-Scherer, John, Page, Lyman, Partridge, Bruce, Salatino, Maria, Schaan, Emmanuel, Schillaci, Alessandro, Sehgal, Neelima, Sifon, Cristobal, Staggs, Suzanne T., van Engelen, Alexander, Wollack, Edward J., and Xu, Zhilei

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Sunyaev-Zel'dovich (SZ) effect introduces a specific distortion of the blackbody spectrum of the cosmic microwave background (CMB) radiation when it scatters off hot gas in clusters of galaxies. The frequency dependence of the distortion is only independent of the cluster redshift when the evolution of the CMB radiation is adiabatic. Using 370 clusters within the redshift range $0.07\lesssim z\lesssim1.4$ from the largest SZ-selected cluster sample to date from the Atacama Cosmology Telescope, we provide new constraints on the deviation of CMB temperature evolution from the standard model $\alpha=0.017^{+0.029}_{-0.032}$, where $T(z)=T_0(1+z)^{1-\alpha}$. This result is consistent with no deviation from the standard adiabatic model. Combining it with previous, independent datasets we obtain a joint constraint of $\alpha=-0.001\pm0.012$. Attributing deviation from adiabaticity to the decay of dark energy, this result constrains its effective equation of state $w_\mathrm{eff}=-0.998^{+0.008}_{-0.010}$.

Published
2021

24. The Simons Observatory: metamaterial microwave absorber and its cryogenic applications

Author

Xu, Zhilei, Chesmore, Grace E., Adachi, Shunsuke, Ali, Aamir M., Bazarko, Andrew, Coppi, Gabriele, Devlin, Mark, Devlin, Tom, Dicker, Simon R., Gallardo, Patricio A., Golec, Joseph E., Gudmundsson, Jon E., Harrington, Kathleen, Hattori, Makoto, Kofman, Anna, Kiuchi, Kenji, Kusaka, Akito, Limon, Michele, Matsuda, Frederick, McMahon, Jeff, Nati, Federico, Niemack, Michael D., Sutariya, Shreya, Suzuki, Aritoki, Teply, Grant P., Thornton, Robert J., Wollack, Edward J., Zannoni, Mario, Zhu, Ningfeng, Xu, Z, Chesmore, G, Adachi, S, Ali, A, Bazarko, A, Coppi, G, Devlin, M, Devlin, T, Dicker, S, Gallardo, P, Golec, J, Gudmundsson, J, Harrington, K, Hattori, M, Kofman, A, Kiuchi, K, Kusaka, A, Limon, M, Matsuda, F, Mcmahon, J, Nati, F, Niemack, M, Suzuki, A, Teply, G, Thornton, R, Wollack, E, Zannoni, M, and Zhu, N

Subjects
Materials science, FOS: Physical sciences, Physics::Optics, Dielectric, engineering.material, 01 natural sciences, CMB, Cryogenics, polarization, metamaterial, telescope, 010309 optics, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, Coating, 0103 physical sciences, Electrical and Electronic Engineering, Absorption (electromagnetic radiation), Engineering (miscellaneous), Instrumentation and Methods for Astrophysics (astro-ph.IM), Stray light, business.industry, Metamaterial, Refraction, Atomic and Molecular Physics, and Optics, Molding (decorative), engineering, business, Astrophysics - Instrumentation and Methods for Astrophysics, Microwave
Abstract

Controlling stray light at millimeter wavelengths requires special optical design and selection of absorptive materials that should be compatible with cryogenic operating environments. While a wide selection of absorptive materials exists, these typically exhibit high indices of refraction and reflect/scatter a significant fraction of light before absorption. For many lower index materials such as commercial microwave absorbers, their applications in cryogenic environments are challenging. In this paper, we present a new tool to control stray light: metamaterial microwave absorber tiles. These tiles comprise an outer metamaterial layer that approximates a lossy gradient index anti-reflection coating. They are fabricated via injection molding commercially available carbon-loaded polyurethane (25\% by mass). The injection molding technology enables mass production at low cost. The design of these tiles is presented, along with thermal tests to 1 K. Room temperature optical measurements verify their control of reflectance to less than 1\% up to 65$\circ$ angles of incidence, and control of wide angle scattering below 0.01\%. The dielectric properties of the bulk carbon-loaded material used in the tiles is also measured at different temperatures, confirming that the material maintains similar dielectric properties down to 3 K., 10 pages, 11 figures, published in Applied Optics, selected as "Editor's pick"

Published
2021

27. The Primordial Inflation Polarization Explorer (PIPER)

Author

Lazear, Justin Scott, Ade, Peter A, Benford, Dominic J, Bennett, Charles L, Chuss, David T, Dotson, Jessie L, Eimer, Joseph R, Fixsen, Dale J, Halpern, Mark, Hinderks, James, Hinshaw, Gary F, Irwin, Kent, Jhabvala, Christine, Johnson, Bradley, Kogut, Alan, Lowe, Luke, McMahon, Jeff J, Miller, Timothy M, Mirel, Paul, Moseley, S. Harvey, Rodriguez, Samelys, Staguhn, Johannes G, Switzer, Eric R, Tucker, Carole E, Weston, Amy, and Wollack, Edward

Subjects
Astrophysics
Abstract

The Primordial Inflation Polarization ExploreR (Piper) is a balloon-borne cosmic microwave background (CMB) polarimeter designed to search for evidence of inflation by measuring the large-angular scale CMB polarization signal. Bicep2 recently reported a detection of B-mode power corresponding to the tensor-to-scalar ratio r = 0.2 on approximately 2 degree scales. If the Bicep2 signal is caused by inflationary gravitational waves (IGWs), then there should be a corresponding increase in B-mode power on angular scales larger than 18 degrees. Piper is currently the only suborbital instrument capable of fully testing and extending the Bicep2 results by measuring the B-mode power spectrum on angular scales theta θ = approximately 0.6 deg to 90 deg, covering both the reionization bump and recombination peak, with sensitivity to measure the tensor-to-scalar ratio down to r = 0.007, and four frequency bands to distinguish foregrounds. Piper will accomplish this by mapping 85% of the sky in four frequency bands (200, 270, 350, 600 GHz) over a series of 8 conventional balloon flights from the northern and southern hemispheres. The instrument has background-limited sensitivity provided by fully cryogenic (1.5 K) optics focusing the sky signal onto four 32×40-pixel arrays of time-domain multiplexed Transition-Edge Sensor (TES) bolometers held at 140 milli-Kelvin. Polarization sensitivity and systematic control are provided by front-end Variabledelay Polarization Modulators (VPMs), which rapidly modulate only the polarized sky signal at 3 Hz and allow Piper to instantaneously measure the full Stokes vector (I,Q,U,0V) for each pointing. We describe the Piper instrument and progress towards its first flight.

Published
2014
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28. 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

29. Observations of compact sources in galaxy clusters using MUSTANG2.

Author

Dicker, Simon R, Battistelli, Elia S, Bhandarkar, Tanay, Devlin, Mark J, Duff, Shannon M, Hilton, Gene, Hilton, Matt, Hincks, Adam D, Hubmayr, Johannes, Huffenberger, Kevin, Hughes, John P, Di Mascolo, Luca, Mason, Brian S, Mates, J A B, McMahon, Jeff, Mroczkowski, Tony, Naess, Sigurd, Orlowski-Scherer, John, Partridge, Bruce, and Radiconi, Federico

Subjects
GALAXY clusters, SUNYAEV-Zel'dovich effect, MATCHED filters, COSMIC background radiation, ACTINIC flux, ANGULAR distance
Abstract

Compact sources can cause scatter in the scaling relationships between the amplitude of the thermal Sunyaev–Zel'dovich Effect (tSZE) in galaxy clusters and cluster mass. Estimates of the importance of this scatter vary – largely due to limited data on sources in clusters at the frequencies at which tSZE cluster surveys operate. In this paper, we present 90 GHz compact source measurements from a sample of 30 clusters observed using the MUSTANG2 instrument on the Green Bank Telescope. We present simulations of how a source's flux density, spectral index, and angular separation from the cluster's centre affect the measured tSZE in clusters detected by the Atacama Cosmology Telescope (ACT). By comparing the MUSTANG2 measurements with these simulations we calibrate an empirical relationship between 1.4 GHz flux densities from radio surveys and source contamination in ACT tSZE measurements. We find 3 per cent of the ACT clusters have more than a 20 per cent decrease in Compton- y but another 3 per cent have a 10 per cent increase in the Compton- y due to the matched filters used to find clusters. As sources affect the measured tSZE signal and hence the likelihood that a cluster will be detected, testing the level of source contamination in the tSZE signal using a tSZE-selected catalogue is inherently biased. We confirm this by comparing the ACT tSZE catalogue with optically and X-ray-selected cluster catalogues. There is a strong case for a large, high-resolution survey of clusters to better characterize their source population. [ABSTRACT FROM AUTHOR]

Published
2021
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30. CMB-S4 Science Case, Reference Design, and Project Plan

Author

Abazajian, Kevork, Addison, Graeme, Adshead, Peter, Ahmed, Zeeshan, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Anderson, Adam, Arnold, Kam S., Baccigalupi, Carlo, Bailey, Kathy, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Baxter, Eric, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Berger, Edo, Bhimani, Sanah, Bischoff, Colin A., Bleem, Lindsey, Bocquet, Sebastian, Boddy, Kimberly, Bonato, Matteo, Bond, J. Richard, Borrill, Julian, Bouchet, Fran��ois R., Brown, Michael L., Bryan, Sean, Burkhart, Blakesley, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, de Zotti, Gianfranco, Delabrouille, Jacques, Demarteau, Marcel, Devlin, Mark, Di Valentino, Eleonora, Dobbs, Matt, Duff, Shannon, Duivenvoorden, Adriaan, Dvorkin, Cora, Edwards, William, Eimer, Joseph, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gilchriese, Murdock, Gluscevic, Vera, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Victor, Gudmundsson, Jon E., Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Henning, Jason W., Hill, J. Colin, Hlozek, Ren��e, Holder, Gil, Holzapfel, William, Hubmayr, Johannes, Huffenberger, Kevin M., Huffer, Michael, Hui, Howard, Irwin, Kent, Johnson, Bradley R., Johnstone, Doug, Jones, William C., Karkare, Kirit, Katayama, Nobuhiko, Kerby, James, Kernovsky, Sarah, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kurita, Nadine, Kusaka, Akito, Lahteenmaki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Madhavacheril, Mathew S., Mantz, Adam, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, McQuinn, Matthew, Meerburg, P. Daniel, Melin, Jean-Baptiste, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Mroczkowski, Tony, Mukherjee, Suvodip, M��nchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Negrello, Mattia, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nordby, Martin, Novosad, Valentine, O'Connor, Paul, Obied, Georges, Padin, Stephen, Pandey, Shivam, Partridge, Bruce, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Rajagopalan, Srini, Raveri, Marco, Reichanadter, Mark, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John, Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sheehy, Christopher, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Somerville, Rachel, Spergel, David, Staggs, Suzanne T., Stark, Antony, Stompor, Radek, Story, Kyle T., Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Timbie, Peter, Tomasi, Maurizio, Treu, Jesse I., Tristram, Matthieu, Tucker, Gregory, Umilt��, Caterina, van Engelen, Alexander, Vieira, Joaquin D., Vieregg, Abigail G., Vogelsberger, Mark, Wang, Gensheng, Watson, Scott, White, Martin, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yasini, Siavash, Yeck, James, Yoon, Ki Won, Young, Edward, 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut Lagrange de Paris, Université Paris Descartes - Paris 5 (UPD5), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU), 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), 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), Sorbonne Universités, 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
[PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics of Galaxies (astro-ph.GA), [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We present the science case, reference design, and project plan for the Stage-4 ground-based cosmic microwave background experiment CMB-S4., Comment: 287 pages, 82 figures

Published
2019

31. 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

32. 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

33. 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

34. CMB-S4

Author

Carlstrom, John, Abazajian, Kevork, Addison, Graeme, Adshead, Peter, Ahmed, Zeeshan, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Anderson, Adam, Arnold, Kam S., Baccigalupi, Carlo, Schaan, Emmanuel, Schillaci, Alessandro, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sheehy, Christopher, Sherwin, Blake D., Shirokoff, Erik, Bean, Rachel, Hložek, Renee, Simon, Sara M., Slosar, Anze, Somerville, Rachel, Staggs, Suzanne T., Stark, Antony, Stompor, Radek, Story, Kyle T., Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Holder, Gil, Bebek, Chris, Teply, Grant P., Thompson, Keith, Timbie, Peter, Tomasi, Maurizio, Treu, Jesse I., Tristram, Matthieu, Tucker, Gregory, Umilta, Caterina, van Engelen, Alexander, Holzapfel, William, Vieira, Joaquin D., Bender, Amy N., Vieregg, Abigail G., Vogelsberger, Mark, Wang, Gensheng, Watson, Scott, White, Martin, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Hubmayr, Johannes, Xu, Zhilei, Yasini, Siavash, Benson, Bradford A., Yeck, James, Yoon, Ki Won, Young, Edward, Zonca, Andrea, Berger, Edo, Bhimani, Sanah, Bischoff, Colin A., Huffenberger, Kevin M., Bleem, Lindsey, Bocquet, Sebastian, Boddy, Kimberly, BONATO, MATTEO, Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brown, Michael L., Bryan, Sean, Burkhart, Blakesley, Huffer, Michael, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Hui, Howard, Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, DE ZOTTI, Gianfranco, Delabrouille, Jacques, Irwin, Kent, Demarteau, Marcel, Devlin, Mark, Di Valentino, Eleonora, Dobbs, Matt, Duff, Shannon, Duivenvoorden, Adriaan, Dvorkin, Cora, Edwards, William, Eimer, Joseph, Errard, Josquin, Johnson, Bradley R., Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Johnstone, Doug, Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gilchriese, Murdock, Gluscevic, Vera, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Victor, Bailey, Kathy, Gudmundsson, Jon E., Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Jones, William C., Heitmann, Katrin, Henderson, Shawn, Henning, Jason W., Hill, J. Colin, Karkare, Kirit, Katayama, Nobuhiko, Kerby, James, Kernovsky, Sarah, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Kosowsky, Arthur, Kovac, John, Barkats, Denis, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kurita, Nadine, Kusaka, Akito, Lahteenmaki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Barron, Darcy, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Madhavacheril, Mathew S., Mantz, Adam, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, Meerburg, P. Daniel, Melin, JeanBaptiste, Barry, Peter S., Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Mroczkowski, Tony, Mukherjee, Suvodip, Munchmeyer, Moritz, Nagai, Daisuke, Nagy, Johanna, Namikawa, Toshiya, Bartlett, James G., Nati, Federico, Natoli, Tyler, Negrello, Mattia, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nordby, Martin, Novosad, Valentine, O'Connor, Paul, Obied, Georges, Basu Thakur, Ritoban, Padin, Stephen, Pandey, Shivam, Partridge, Bruce, Pierpaoli, Elena, Pogosian, Levon, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Battaglia, Nicholas, Rajagopalan, Srini, Raveri, Marco, Reichanadter, Mark, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John, Salatino, Maria, Baxter, Eric, and Saliwanchik, Benjamin

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract

We describe the stage 4 cosmic microwave background ground-based experiment CMB-S4.

Published
2019

35. 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

36. Reflectometry Measurements of the Loss Tangent in Silicon at Millimeter Wavelengths

Author

Chesmore, Grace E., Mroczkowski, Tony, McMahon, Jeff, Sutariya, Shreya, Josaitis, Alec, and Jensen, Leif

Subjects
Physics::Instrumentation and Detectors, FOS: Physical sciences, Physics::Optics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

We report here on measurements of the reflectivity and loss tangent measured in the W-band (80-125 GHz) and D-band (125-180 GHz) in two samples of float zone silicon with intrinsic stoichiometry - one irradiated by neutrons, which increases the resistivity by introducing crystalline defects, and the other unperturbed. We find a loss tangent $\tan(\delta)$ of 2.8e-4 and 1.5e-5 for neutron-irradiated silicon and intrinsic silicon, respectively, both with an index of refraction of 3.41. The results demonstrate the applicability of silicon as a warm optical component in millimeter-wave receivers. For our measurements, we use a coherent reflectometer to measure the Fabry-Perot interference fringes of the reflected signal from dielectric slabs. The depth of the reflection nulls provides a sensitive measurement of dielectric losses. We describe the test setup which can also characterize scattering and transmission, and can provide detailed characterization of millimeter wave materials., Comment: 6 pages, proceedings from the 8th ESA Workshop on Millimetre-Wave Technology and Applications (https://atpi.eventsair.com/QuickEventWebsitePortal/millimetre-wave/mm-wave)

Published
2018

37. In Situ Performance of the Low Frequency Array for Advanced ACTPol.

Author

Li, Yaqiong, Austermann, Jason E., Beall, James A., Bruno, Sarah Marie, Choi, Steve K., Cothard, Nicholas F., Crowley, Kevin T., Duff, Shannon M., Ho, Shuay-Pwu Patty, Golec, Joseph E., Hilton, Gene C., Hasselfield, Matthew, Hubmayr, Johannes, Koopman, Brian J., Lungu, Marius, McMahon, Jeff, Niemack, Michael D., Page, Lyman A., Salatino, Maria, and Simon, Sara M.

Subjects
SYNCHROTRON radiation, COSMIC background radiation, PHYSICAL cosmology, BOLOMETERS, POLARISCOPE
Abstract

The AdvancedAtacama Cosmology Telescope Polarimeter (AdvACT) is an upgrade for the Atacama Cosmology Telescope using Transition Edge Sensor (TES) detector arrays to measure cosmic microwave background (CMB) temperature and polarization anisotropies in multiple frequencies. The low frequency (LF) array was deployed early 2020. It consists of 292 TES bolometers observing in two bands centered at 27 GHz and 39 GHz. At these frequencies, it is sensitive to synchrotron radiation from our galaxy as well as to the CMB, and complements the AdvACT arrays operating at 90, 150 and 230 GHz. We present the initial LF array on-site characterization, including the time constant, optical efficiency and array sensitivity. [ABSTRACT FROM AUTHOR]

Published
2021
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38. Cold optical design for the Large Aperture Simons Observatory telescope

Author

Spyromilio, Jason, Marshall, Heather K., Gilmozzi, Roberto, Vavagiakis, Eve M., Ullom, Joel N., Thornton, Robert, Staggs, Suzanne T., Simon, Sara M., Salatino, Maria, Piccirillo, Lucio, Orlowski-Scherer, John L., Niemack, Michael D., Ho, Shuay-Pwu P., Galitzki, Nicholas, Devlin, Mark J., Coppi, Gabriele, Ashton, Peter, Ali, Aamir, Mauskopf, Phillip, Gudmudsson, Jon E., Gallardo, Patricio A., Zhu, Ningfeng, Xu, Zhilei, Wollack, Edward J., McMahon, Jeff, Matsuda, Frederick, Limon, Michele, Lee, Adrian T., Keating, Brian, Hubmayr, Johannes, Hill, Charles A., Dicker, Simon R., AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Dicker, S, Gallardo, P, Gudmudsson, J, Mauskopf, P, Ali, A, Ashton, P, Coppi, G, Devlin, M, Galitzki, N, Ho, S, Hill, C, Hubmayr, J, Keating, B, Lee, A, Limon, M, Matsuda, F, Mcmahon, J, Niemack, M, Orlowski-Scherer, J, Piccirillo, L, Salatino, M, Simon, S, Staggs, S, Thornton, R, Ullom, J, Vavagiakis, E, Wollack, E, Xu, Z, Zhu, N, 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), 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
Cryostat, Simons Observatory, Crossed Dragone, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, 010309 optics, Telescope, Optics, law, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, Reimaging optical design, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Large aperture, submillimeter telescopes, millimeter wave, Polarization (waves), Refracting telescope, Extremely high frequency, silicon lense, cryogenic optical design, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

International audience; The Simons Observatory will consist of a single large (6 m diameter) telescope and a number of smaller (∼0.5 m diameter) refracting telescopes designed to measure the polarization of the Cosmic Microwave Background to unprecedented accuracy. The large aperture telescope is the same design as the CCAT-prime telescope, a modified Crossed Dragone design with a field-of-view of over 7.8 degrees diameter at 90 GHz. This paper presents an overview of the cold reimaging optics for this telescope and what drove our choice of 350–400 mm diameter silicon lenses in a 2.4 m cryostat over other possibilities. We will also consider the future expandability of this design to CMB Stage-4 and beyond.

Published
2018

39. BFORE: a CMB balloon payload to measure reionization, neutrino mass, and cosmic Inflation (Conference Presentation)

Author

Bryan, Sean, Ade, Peter, Bond, J. Richard, Boulanger, François, Devlin, Mark, Doyle, Simon, Filippini, Jeffrey, Fissell, Laura, Groppi, Christopher, Holder, Gilbert, Hubmayr, Johannes, Mauskopf, Philip, McMahon, Jeff, Nagy, Johanna, Netterfield, C. Barth, Niemack, Michael, Novak, Giles, Pascale, Enzo, Pisano, Giampaolo, Ruhl, John, Scott, Douglas, Soler, Juan, Tucker, Carole, Vieira, Joaquin, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
tes detectors, cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation, neutrinos, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, frequency: high, microwaves, B-mode, cryogenics, ionization, optical, electronics: readout, reionization, carbon: fibre, helium: liquid, galaxy, tau, neutrino: mass, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, ballooning, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], microwave squid
Abstract

International audience; BFORE is a NASA high-altitude ultra-long-duration balloon mission to map the cosmic microwave background (CMB) across half the sky during a 28-day mid-latitude flight launched from Wanaka, New Zealand. With the unique access to large angular scales and high frequencies provided by the balloon platform, BFORE will significantly improve measurements of the optical depth to reionization tau, breaking parameter degeneracies needed to detect neutrino mass with the CMB. The mission will hunt for the inflationary gravitational wave B-mode signal at both large angular scales and degree scales, detecting or setting an upper limit on each at the r~0.01 level. The balloon platform allows BFORE to map Galactic dust foregrounds at frequencies where they dominate, in order to robustly separate them from CMB signals measured by BFORE, in addition to complementing data from ground-based telescopes. The BFORE payload will use technologies proven in flight from Spider and Blast, such as a carbon fiber gondola, long hold time liquid helium cryostat, and pointing system. The mission will be the first near-space use of TES multichroic detectors (150/217 GHz and 280/353 GHz bands) using highly-multiplexed mSQUID microwave readout. This system enables a longer flight by reducing the cryogenic heat load on the liquid helium cryostat, simplifies system integration to increase reliability, and reduces the payload weight by using less electrical power in the readout electronics. The flight will raise the technical readiness level of these technologies. BFORE has been selected for partial funding by NASA, which is enabling us to further develop and optimize the detector multiplexing and readout technologies.

Published
2018

40. The Primordial Inflation Polarization Explorer (PIPER)

Author

Gandilo, Natalie, Peter Ade, Benford, Dominic, Bennett, Charles, Chuss, David, Datta, Rahul, Dotson, Jessie, Essinger-Hileman, Thomas, Fixsen, Dale, Halpern, Mark, Hilton, Gene, Hinshaw, Gary, Irwin, Kent, Jhabvala, Christine, Kimball, Mark, Kogut, Al, Lowe, Luke, Mcmahon, Jeff, Miller, Timothy, Mirel, Paul, Moseley, Samuel Harvey, Pawlyk, Samuel, Rodriguez, Samelys, Sharp, Elmer, Shirron, Peter, Staguhn, Johannes G., Sullivan, Dan, Switzer, Eric, Taraschi, Peter, Tucker, Carole, Walts, Alexander, and Wollack, Edward

Subjects
Physics, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), 01 natural sciences, law.invention, 010309 optics, Telescope, law, Sky, 0103 physical sciences, Time domain, 010306 general physics, Adiabatic process, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Reionization, Circular polarization, Astrophysics::Galaxy Astrophysics, QB, media_common
Abstract

The Primordial Inflation Polarization ExploreR (PIPER) is a balloon-borne telescope designed to measure the polarization of the Cosmic Microwave Background on large angular scales. PIPER will map 85% of the sky at 200, 270, 350, and 600 GHz over a series of 8 conventional balloon flights from the northern and southern hemispheres. The first science flight will use two 32x40 arrays of backshort-under-grid transition edge sensors, multiplexed in the time domain, and maintained at 100 mK by a Continuous Adiabatic Demagnetization Refrigerator. Front-end cryogenic Variable-delay Polarization Modulators provide systematic control by rotating linear to circular polarization at 3 Hz. Twin telescopes allow PIPER to measure Stokes I, Q, U, and V simultaneously. The telescope is maintained at 1.5 K in an LHe bucket dewar. Cold optics and the lack of a warm window permit sensitivity at the sky-background limit. The ultimate science target is a limit on the tensor-to-scalar ratio of r ~ 0.007, from the reionization bump to l ~ 300. PIPER's first flight will be from the Northern hemisphere, and overlap with the CLASS survey at lower frequencies. We describe the current status of the PIPER instrument., 8 pages, 6 figures. To be published in Proceedings of SPIE Volume 9914. Presented at SPIE Astronomical Telescopes + Instrumentation 2016, conference 9914

Published
2016

42. Designs for next generation CMB survey strategies from Chile.

Author

Stevens, Jason R., Goeckner-Wald, Neil, Reijo Keskitalo, McCallum, Nialh, Ali, Aamir, Borrill, Julian, Brown, Michael L., Yuji Chinone, Gallardo, Patricio A., Akito Kusaka, Lee, Adrian T., McMahon, Jeff, Niemack, Michael D., Page, Lyman, Puglisi, Giuseppe, Salatino, Maria, Mak, Suet Ying D., Teply, Grant, Thomas, Daniel B., and Vavagiakis, Eve M.

Published
2018
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43. Development of Calibration Strategies for the Simons Observatory.

Author

Bryan, Sean A., Simon, Sara M., Gerbino, Martina, Teply, Grant, Ali, Aamir, Yuji Chinone, Crowley, Kevin, Fabbian, Giulio, Gallardo, Patricio A., Goeckner-Wald, Neil, Keating, Brian, Koopman, Brian, Akito Kusaka, Matsuda, Frederick, Mauskopf, Philip, McMahon, Jeff, Nati, Federico, Puglisi, Giuseppe, Reichardt, Christian L., and Salatino, Maria

Published
2018
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45. Feedhorn development and scalability for Simons Observatory and beyond.

Author

Simon, Sara M., Golec, Joseph E., Ali, Aamir, Austermann, Jason, Beall, James A., Bruno, Sarah Marie M., Choi, Steve K., Crowley, Kevin T., Dicker, Simon, Dober, Bradley, Duff, Shannon M., Healy, Erin, Hill, Charles A., Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Yaqiong Li, Lungu, Marius, McMahon, Jeff, Orlowski-Scherer, John, and Salatino, Maria

Published
2018
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46. Simons Observatory large aperture receiver simulation overview.

Author

Orlowski-Scherer, John L., Ningfeng Zhu, Zhilei Xu, Ali, Aamir, Arnold, Kam S., Ashton, Peter C., Coppi, Gabriele, Devlin, Mark, Dicker, Simon, Galitzki, Nicholas, Gallardo, Patricio A., Keating, Brian, Lee, Adrian T., Limon, Michele, Lungu, Marius, May, Andrew, McMahon, Jeff, Niemack, Michael D., Piccirillo, Lucio, and Puglisi, Giuseppe

Published
2018
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48. Performance of the Advanced ACTPol Low Frequency Array.

Author

Yaqiong Li, Austermann, Jason E., Beall, James A., Bruno, Sarah Marie, Choi, Steve K., Cothard, Nicholas F., Crowley, Kevin T., Duff, Shannon M., Gallardo, Patricio A., Henderson, Shawn W., Ho, Shuay-Pwu Patty, Hubmayr, Johannes, Koopman, Brian J., McMahon, Jeff J., Niemack, Michael D., Salatino, Maria, Simon, Sara M., Staggs, Suzanne T., Stevens, Jason R., and Ullom, Joel N.

Published
2018
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49. Clans of the Southern Wild

Author

McMahon, Jeff

Subjects
Black Sheep Boy: A Novel in Stories (Novel) -- Pousson, Martin -- Book reviews, Books -- Book reviews, Literature/writing, Women's issues/gender studies
Abstract

Black Sheep Boy: A Novel in Stories by Martin Pousson Rare Bird Books. 208 pages, $22. MARTIN POUSSON knows Cajun Acadiana, which he probed in his 2002 novel No Place, [...]

Published
2016

50. The Man Who Loved Birds

Author

McMahon, Jeff

Subjects
The Man Who Loved Birds (Novel) -- Johnson, Fenton -- Book reviews, Literature/writing, Women's issues/gender studies
Abstract

The Man Who Loved Birds Fenton Johnson Univ. Press of Kentucky. 328 pages, $24.95 Brother Flavian, after seventeen years in a Kentucky monastery--which he entered to escape the draft--wanders into [...]

Published
2016

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