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1. The Atacama Cosmology Telescope: reionization kSZ trispectrum methodology and limits.

Author

MacCrann, Niall, Qu, Frank J, Namikawa, Toshiya, Bolliet, Boris, Cai, Hongbo, Calabrese, Erminia, Choi, Steve K, Coulton, William, Darwish, Omar, Ferraro, Simone, Guan, Yilun, Hill, J Colin, Hilton, Matt, Hložek, Renée, Kramer, Darby, Madhavacheril, Mathew S, Moodley, Kavilan, Sehgal, Neelima, Sherwin, Blake D, and Sifón, Cristóbal

Subjects
LARGE scale structure (Astronomy), POWER spectra, AGE of stars, MIDDLE Ages, PHYSICAL cosmology, COSMIC background radiation
Abstract

Patchy reionization generates kinematic Sunyaev–Zel'dovich (kSZ) anisotropies in the cosmic microwave background (CMB). Large-scale velocity perturbations along the line of sight modulate the small-scale kSZ power spectrum, leading to a trispectrum (or four-point function) in the CMB that depends on the physics of reionization. We investigate the challenges in detecting this trispectrum and use tools developed for CMB lensing, such as realization-dependent bias subtraction and cross-correlation based estimators, to counter uncertainties in the instrumental noise and assumed CMB power spectrum. We also find that both lensing and extragalactic foregrounds can impart larger trispectrum contributions than the reionization kSZ signal. We present a range of mitigation methods for both of these sources of contamination, validated on microwave-sky simulations. We use ACT DR6 and Planck data to calculate an upper limit on the reionization kSZ trispectrum from a measurement dominated by foregrounds. The upper limit is about 50 times the signal predicted from recent simulations. [ABSTRACT FROM AUTHOR]

Published
2024
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2. Impact of Galactic dust non-Gaussianity on searches for B-modes from inflation.

Author

Abril-Cabezas, Irene, Hervías-Caimapo, Carlos, von Hausegger, Sebastian, Sherwin, Blake D, and Alonso, David

Subjects
DUST, COVARIANCE matrices, COSMIC background radiation, RANDOM fields
Abstract

A key challenge in the search for primordial B -modes is the presence of polarized Galactic foregrounds, especially thermal dust emission. Power-spectrum-based analysis methods generally assume the foregrounds to be Gaussian random fields when constructing a likelihood and computing the covariance matrix. In this paper, we investigate how non-Gaussianity in the dust field instead affects CMB and foreground parameter inference in the context of inflationary B -mode searches, capturing this effect via modifications to the dust power-spectrum covariance matrix. For upcoming experiments such as the Simons Observatory, we find no dependence of the tensor-to-scalar ratio uncertainty |$\sigma (r)$| on the degree of dust non-Gaussianity or the nature of the dust covariance matrix. We provide an explanation of this result, noting that when frequency decorrelation is negligible, dust in mid-frequency channels is cleaned using high-frequency data in a way that is independent of the spatial statistics of dust. We show that our results hold also for non-zero levels of frequency decorrelation that are compatible with existing data. We find, however, that neglecting the impact of dust non-Gaussianity in the covariance matrix can lead to inaccuracies in goodness-of-fit metrics. Care must thus be taken when using such metrics to test B -mode spectra and models, although we show that any such problems can be mitigated by using only cleaned spectrum combinations when computing goodness-of-fit statistics. [ABSTRACT FROM AUTHOR]

Published
2024
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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. A new probe of inflationary gravitational waves: cross-correlations of lensed primary CMB B-modes with large-scale structure

Author

Namikawa, Toshiya and Sherwin, Blake D.

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

We propose a new probe of inflationary gravitational waves (IGWs): the cross-correlation of the lensing of inflationary $B$-mode polarization with a large-scale structure (LSS) tracer, which can also be a CMB lensing map. This is equivalent to measuring a three-point function of two CMB $B$-modes and an LSS tracer. We forecast expected $1\,\sigma$ constraints on the tensor-to-scalar ratio, $r$, albeit with a simplistic foreground treatment, and find constraints of $\sigma_r \simeq 7 \times 10^{-3}$ from the correlation of CMB-S4-Deep $B$-mode lensing and LSST galaxies, $\sigma_r \simeq 5 \times 10^{-3}$ from the correlation of CMB-S4-Deep $B$-mode lensing and CMB-S4-Deep CMB lensing, and $\sigma_r \simeq 10^{-2}$ from the correlation of LiteBIRD $B$-mode lensing and CMB-S4-Wide lensing. Because this probe is inherently non-Gaussian, simple Gaussian foregrounds will not produce any biases to the measurement of $r$. While a detailed investigation of non-Gaussian foreground contamination for different cross-correlations will be essential, this observable has the potential to be a powerful probe of IGWs, complementary to standard methods for constraining $r$., Comment: 7 pages, 1 figure

Published
2023

5. 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

6. 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

7. 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

8. Probing early structure and model-independent neutrino mass with high-redshift CMB lensing mass maps

Author

Qu, Frank J., Sherwin, Blake D., Darwish, Omar, Namikawa, Toshiya, and Madhavacheril, Mathew S.

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

CMB lensing maps probe the mass distribution in projection out to high redshifts, but significant sensitivity to low-redshift structure remains. In this paper we discuss a method to remove the low-redshift contributions from CMB lensing mass maps by subtracting suitably scaled galaxy density maps, nulling the low redshift structure with a model-insensitive procedure that is similar to delensing. This results in a high-$z$-only mass map that can provide a probe of structure growth at uniquely high redshifts: if systematics can be controlled, we forecast that CMB-S4 lensing combined with a Rubin-LSST-like galaxy survey can probe the amplitude of structure at redshifts $z>3.75$ ($z>5$) to within $2.3\%$ ($3.3\%$). We then discuss other example applications of such high-$z$ CMB lensing maps. In standard analyses of CMB lensing, assuming the wrong dark energy model (or wrong model parametrization) can lead to biases in neutrino mass constraints. In contrast, we show with forecasts that a high-$z$ mass map constructed from CMB-S4 lensing and LSST galaxies can provide a nearly model-independent neutrino mass constraint, with only negligible sensitivity to the presence of non-standard dark energy models, irrespective of their parametrization., 19 pages, 11 figures

Published
2022

9. Snowmass 2021 CMB-S4 White Paper

Author

Abazajian, Kevork, Abdulghafour, Arwa, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Ajello, Marco, Akerib, Daniel, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Amiri, Mandana, Anderson, Adam, Ansarinejad, Behzad, Archipley, Melanie, Arnold, Kam S., Ashby, Matt, Aung, Han, Baccigalupi, Carlo, Baker, Carina, Bakshi, Abhishek, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Barton, Paul, Basu Thakur, Ritoban, Battaglia, Nicholas, Beall, Jim, Bean, Rachel, Beck, Dominic, Belkner, Sebastian, Benabed, Karim, Bender, Amy N., Benson, Bradford A., Besuner, Bobby, Bethermin, Matthieu, Bhimani, Sanah, Bianchini, Federico, Biquard, Simon, Birdwell, Ian, Bischoff, Colin A., Bleem, Lindsey, Bocaz, Paulina, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chan, Victor, Chang, Clarence L., Chapman, Scott, Charles, Eric, Chauvin, Eric, Cheng, Cheng, Chesmore, Grace, Cheung, Kolen, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Clancy, Justin, Clark, Susan, Cooray, Asantha, Coppi, Gabriele, Corlett, John, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, Dai, Wei-Ming, Daley, Cail, Dart, Eli, Daues, Gregorg, Haan, Tijmen, Deaconu, Cosmin, Delabrouille, Jacques, Derylo, Greg, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dober, Brad, Doriese, Randy, Duff, Shannon, Dutcher, Daniel, Dvorkin, Cora, Dunner, Rolando, Eftekhari, Tarraneh, Eimer, Joseph, Bouhargani, Hamza El, Elleflot, Tucker, Emerson, Nick, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Fanfani, Valentina, Fasano, Alessandro, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frisch, Josef, Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Giannakopoulos, Christos, Gilchriese, Murdock, Gluscevic, Vera, Goecknerwald, Neil, Goldfinger, David, Green, Daniel, Grimes, Paul, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Guarino, Vic, Gudmundsson, Jon E., Gullett, Ian, Guns, Sam, Habib, Salman, Haller, Gunther, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Hand, Emma, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Herbst, Ryan, Hervias-Caimapo, Carlos, Hill, J. Colin, Hills, Richard, Hivon, Eric, Hlozek, Renee, Ho, Anna, Holder, Gil, Hollister, Matt, Holzapfel, William, Hood, John, Hotinli, Selim, Hryciuk, Alec, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Ibanez, Roberto, Ibitoye, Ayodeji, Ikape, Margaret, Irwin, Kent, Jacobus, Cooper, Jeong, Oliver, Johnson, Bradley R., Johnstone, Doug, Jones, William C., Joseph, John, Jost, Baptiste, Kang, Jae Hwan, Kaplan, Ari, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, King, Cesiley, Kisner, Theodore, Klein, Matthias, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Krolewski, Alex, Kubik, Donna, Kuhlmann, Steve, Kuo, Chao-Lin, Kusaka, Akito, Lahteenmaki, Anne, Lau, Kenny, Lawrence, Charles R., Lee, Adrian T., Legrand, Louis, Leitner, Matthaeus, Leloup, Clement, Lewis, Antony, Li, Dale, Linder, Eric, Liodakis, Ioannis, Liu, Jia, Long, Kevin, Louis, Thibaut, Loverde, Marilena, Lowry, Lindsay, Lu, Chunyu, Lubin, Phil, Ma, Yin-Zhe, Maccarone, Thomas, Madhavacheril, Mathew S., Maldonado, Felipe, Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, May, Jared, Mccarrick, Heather, Mccracken, Ken, Mcmahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Miranda, Vivian, Mitchell, Don, Mohr, Joseph, Moncelsi, Lorenzo, Maria Elena Monzani, Moshed, Magdy, Mroczkowski, Tony, Mukherjee, Suvodip, Munchmeyer, Moritz, Nagai, Daisuke, Nagarajappa, Chandan, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Nerval, Simran, Newburgh, Laura, Nguyen, Hogan, Nichols, Erik, Nicola, Andrina, Niemack, Michael D., Nord, Brian, Norton, Tim, Novosad, Valentine, O Brient, Roger, Omori, Yuuki, Orlando, Giorgio, Osherson, Benjamin, Osten, Rachel, Padin, Stephen, Paine, Scott, Partridge, Bruce, Patil, Sanjaykumar, Petravick, Don, Petroff, Matthew, Pierpaoli, Elena, Pilleux, Mauricio, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Raghunathan, Srinivasan, Rahlin, Alexandra, Raveri, Marco, Reese, Ben, Reichardt, Christian L., Remazeilles, Mathieu, Rizzieri, Arianna, Rocha, Graca, Roe, Natalie A., Rotermund, Kaja, Roy, Anirban, Ruhl, John E., Saba, Joe, Sailer, Noah, Salatino, Maria, Saliwanchik, Benjamin, Sapozhnikov, Leonid, Rao, Mayuri Sathyanarayana, Saunders, Lauren, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Shiu, Corwin, Simon, Sara M., Singari, Baibhav, Slosar, Anze, Spergel, David, St Germaine, Tyler, Staggs, Suzanne T., Stark, Antony A., Starkman, Glenn D., Steinbach, Bryan, Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Tandoi, Chris, Teply, Grant P., Thayer, Gregg, Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Trendafilova, Cynthia, Tristram, Matthieu, Tucker, Carole, Tucker, Gregory, Umilta, Caterina, Engelen, Alexander, Marrewijk, Joshiwa, Vavagiakis, Eve M., Verges, Clara, Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Wang, Guo-Jian, Watson, Scott, Watts, Duncan, Weaver, Chris, Wenzl, Lukas, Westbrook, Ben, White, Martin, Whitehorn, Nathan, Wiedlea, Andrew, Williams, Paul, Wilson, Robert, Winch, Harrison, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yefremenko, Volodymyr G., Yu, Cyndia, Zegeye, David, Zivick, Jeff, 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), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre Pierre Binétruy (CPB), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-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), and CMB-S4

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gr-qc, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), cosmic background radiation, General Relativity and Quantum Cosmology, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), cosmological model: parameter space, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], structure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Particle Physics - Phenomenology, General Relativity and Cosmology, hep-ex, hep-ph, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Particle Physics - Experiment, astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross 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. We provide an overview of the science case, the technical design, and project plan., Comment: Contribution to Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1908.01062, arXiv:1907.04473

Published
2022

10. Cosmic birefringence tomography and calibration independence with reionization signals in the CMB.

Author

Sherwin, Blake D and Namikawa, Toshiya

Subjects
*COSMIC background radiation, *BIREFRINGENCE, *TOMOGRAPHY, *BREWSTER'S angle
Abstract

The search for cosmic polarization rotation or birefringence in the cosmic microwave background (CMB) is well motivated because it can provide powerful constraints on parity-violating new physics, such as axion-like particles. In this paper, we point out that since the CMB polarization is produced at two very different redshifts – it is generated at both reionization and recombination – new parity-violating physics can generically rotate the polarization signals from these different sources by different amounts. We explore two implications of this. First, measurements of CMB birefringence are challenging because the effect is degenerate with a miscalibration of CMB polarization angles; however, by taking the difference of the reionization and recombination birefringence angles (measured from different CMB angular scales), we can obtain a cosmological signal that is immune to instrumental angle miscalibration. Secondly, we note that the combination with other methods for probing birefringence can give tomographic information, constraining the redshift origin of any physics producing birefringence. We forecast that the difference of the reionization and recombination birefringence angles can be competitively determined to within ∼0.05 deg for future CMB satellites such as LiteBIRD. Although much further work is needed, we argue that foreground mitigation for this measurement should be less challenging than for inflationary B -mode searches on similar scales due to larger signals and lower foregrounds. [ABSTRACT FROM AUTHOR]

Published
2023
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11. Restoring cosmological concordance with early dark energy and massive neutrinos?

Author

Reeves, Alexander, Herold, Laura, Vagnozzi, Sunny, Sherwin, Blake D, and Ferreira, Elisa G M

Subjects
NEUTRINOS, COSMIC background radiation, GALAXY clusters, NEUTRINO mass, LARGE scale structure (Astronomy), BAYESIAN analysis
Abstract

The early dark energy (EDE) solution to the Hubble tension comes at the cost of an increased clustering amplitude that has been argued to worsen the fit to galaxy clustering data. We explore whether freeing the total neutrino mass M ν, which can suppress small-scale structure growth, improves EDE's fit to galaxy clustering. Using Planck Cosmic Microwave Background and BOSS galaxy clustering data, a Bayesian analysis shows that freeing M ν does not appreciably increase the inferred EDE fraction f EDE: we find the 95 per cent C.L. upper limits f EDE < 0.092 and |$M_{\nu }\lt 0.15\, {\rm eV}$|⁠. Similarly, in a frequentist profile likelihood setting (where our results support previous findings that prior volume effects are important), we find that the baseline EDE model (with |$M_{\nu }=0.06\, {\rm eV}$|⁠) provides the overall best fit. For instance, compared to baseline EDE, a model with |$M_\nu =0.24\, {\rm eV}$| maintains the same H 0(km/s/Mpc) = (70.08, 70.11, respectively) whilst decreasing S 8 = (0.837, 0.826) to the ΛCDM level, but worsening the fit significantly by Δ χ 2 = 7.5. For the datasets used, these results are driven not by the clustering amplitude, but by background modifications to the late-time expansion rate due to massive neutrinos, which worsen the fit to measurements of the BAO scale. [ABSTRACT FROM AUTHOR]

Published
2023
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12. 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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13. Cosmological Parameters From Pre-Planck CMB Measurements: A 2017 Update

Author

Calabrese, Erminia, Hlolzek, Renee A, Bond, J. Richard, Devlin, Mark J, Dunkley, Joanna, Halpern, Mark, Hincks, Adam D, Irwin, Kent D, Kosowsky, Arthur, Moodley, Kavilan, Newburgh, Laura B, Niemack, Michael D, Page, Lyman A, Sherwin, Blake D, Sievers, Jonathan L, Spergel, David N, Staggs, Suzanne T, and Wollack, Edward J

Subjects
Astrophysics
Abstract

We present cosmological constraints from the combination of the full mission nine-year WMAP release and small-scale temperature data from the pre-Planck Atacama Cosmology Telescope (ACT) and South Pole Telescope (SPT) generation of instruments. This is an update of the analysis presented in Calabrese et al. [Phys. Rev. D 87, 103012 (2013)], and highlights the impact on CDM cosmology of a 0.06 eV massive neutrino which was assumed in the Planck analysis but not in the ACTSPT analyses and a Planck-cleaned measurement of the optical depth to reionization. We show that cosmological constraints are now strong enough that small differences in assumptions about reionization and neutrino mass give systematic differences which are clearly detectable in the data. We recommend that these updated results be used when comparing cosmological constraints from WMAP, ACT and SPT with other surveys or with current and future full-mission Planck cosmology. Cosmological parameter chains are publicly available on the NASAs LAMBDA data archive.

Published
2017
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14. CMB-S4

Author

Collaboration, The CMB-S4, Abazajian, Kevork, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, 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, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, 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, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E., Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Hill, Charles, Hill, J. Colin, Hlozek, Renée, Ho, Shuay-Pwu Patty, Hoang, Thuong, Holder, Gil, Holzapfel, William, Hood, John, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Jones, William C., Kang, Jae Hwan, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kusaka, Akito, Lähteenmäki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Lubin, Phil, Madhavacheril, Mathew S., Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria, Mroczkowski, Tony, Mukherjee, Suvodip, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nord, Brian, Novosad, Valentine, O'Brient, Roger, Padin, Stephen, Palladino, Steven, Partridge, Bruce, Petravick, Don, Pierpaoli, Elena, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Rahlin, Alexandra, Rao, Mayuri Sathyanarayana, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John E., Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony, Starkman, Glenn D., Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vavagiakis, Eve M., Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Watson, Scott, Westbrook, Ben, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yang, H. Y. Eric, Yasini, Siavash, Yefremenko, Volodymyr G., Yoon, Ki Won, Young, Edward, Yu, Cyndia, 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), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-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 de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CMB-S4, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11), Apollo - University of Cambridge Repository, Van Swinderen Institute for Particle Physics and G, Cosmic Frontier, Abazajian, K, Addison, G, Adshead, P, Ahmed, Z, Akerib, D, Ali, A, Allen, S, Alonso, D, Alvarez, M, Amin, M, Anderson, A, Arnold, K, Ashton, P, Baccigalupi, C, Bard, D, Barkats, D, Barron, D, Barry, P, Bartlett, J, Basu Thakur, R, Battaglia, N, Bean, R, Bebek, C, Bender, A, Benson, B, Bianchini, F, Bischoff, C, Bleem, L, Bock, J, Bocquet, S, Boddy, K, Richard Bond, J, Borrill, J, Bouchet, F, Brinckmann, T, Brown, M, Bryan, S, Buza, V, Byrum, K, Hervias Caimapo, C, Calabrese, E, Calafut, V, Caldwell, R, Carlstrom, J, Carron, J, Cecil, T, Challinor, A, Chang, C, Chinone, Y, Sherry Cho, H, Cooray, A, Coulton, W, Crawford, T, Crites, A, Cukierman, A, Cyr-Racine, F, De Haan, T, Delabrouille, J, Devlin, M, Di Valentino, E, Dierickx, M, Dobbs, M, Duff, S, Dvorkin, C, Eimer, J, Elleflot, T, Errard, J, Essinger-Hileman, T, Fabbian, G, Feng, C, Ferraro, S, Filippini, J, Flauger, R, Flaugher, B, Fraisse, A, Frolov, A, Galitzki, N, Gallardo, P, Galli, S, Ganga, K, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Green, D, Grin, D, Grohs, E, Gualtieri, R, Gudmundsson, J, Gullett, I, Gupta, N, Habib, S, Halpern, M, Halverson, N, Hanany, S, Harrington, K, Hasegawa, M, Hasselfield, M, Hazumi, M, Heitmann, K, Henderson, S, Hensley, B, Hill, C, Colin Hill, J, Hlozek, R, Patty Ho, S, Hoang, T, Holder, G, Holzapfel, W, Hood, J, Hubmayr, J, Huffenberger, K, Hui, H, Irwin, K, Jeong, O, Johnson, B, Jones, W, Hwan Kang, J, Karkare, K, Katayama, N, Keskitalo, R, Kisner, T, Knox, L, Koopman, B, Kosowsky, A, Kovac, J, Kovetz, E, Kuhlmann, S, Kuo, C, Kusaka, A, Lahteenmaki, A, Lawrence, C, Lee, A, Lewis, A, Li, D, Linder, E, Loverde, M, Lowitz, A, Lubin, P, Madhavacheril, M, Mantz, A, Marques, G, Matsuda, F, Mauskopf, P, Mccarrick, H, Mcmahon, J, Daniel Meerburg, P, Melin, J, Menanteau, F, Meyers, J, Millea, M, Mohr, J, Moncelsi, L, Monzani, M, Mroczkowski, T, Mukherjee, S, Nagy, J, Namikawa, T, Nati, F, Natoli, T, Newburgh, L, Niemack, M, Nishino, H, Nord, B, Novosad, V, O'Brient, R, Padin, S, Palladino, S, Partridge, B, Petravick, D, Pierpaoli, E, Pogosian, L, Prabhu, K, Pryke, C, Puglisi, G, Racine, B, Rahlin, A, Sathyanarayana Rao, M, Raveri, M, Reichardt, C, Remazeilles, M, Rocha, G, Roe, N, Roy, A, Ruhl, J, Salatino, M, Saliwanchik, B, Schaan, E, Schillaci, A, Schmitt, B, Schmittfull, M, Scott, D, Sehgal, N, Shandera, S, Sherwin, B, Shirokoff, E, Simon, S, Slosar, A, Spergel, D, S, T, Staggs, S, Stark, A, Starkman, G, Stompor, R, Stoughton, C, Suzuki, A, Tajima, O, Teply, G, Thompson, K, Thorne, B, Timbie, P, Tomasi, M, Tristram, M, Tucker, G, Umilta, C, Van Engelen, A, Vavagiakis, E, Vieira, J, Vieregg, A, Wagoner, K, Wallisch, B, Wang, G, Watson, S, Westbrook, B, Whitehorn, N, Wollack, E, Kimmy Wu, W, Xu, Z, Eric Yang, H, Yasini, S, Yefremenko, V, Won Yoon, K, Young, E, Yu, C, Zonca, A, University of California Irvine, Johns Hopkins University, University of Illinois at Urbana-Champaign, SLAC National Accelerator Laboratory, University of California Berkeley, Stanford University, University of Oxford, Rice University, Fermi National Accelerator Laboratory, University of California San Diego, International School for Advanced Studies, Lawrence Berkeley National Laboratory, Harvard University, University of New Mexico, Argonne National Laboratory, Université Paris-Diderot, California Institute of Technology, Cornell University, University of Melbourne, University of Cincinnati, Ludwig Maximilian University of Munich, University of Toronto, UMR7095, Stony Brook University, University of Manchester, Arizona State University, Florida State University, Cardiff University, Dartmouth College, University of Geneva, University of Cambridge, The University of Tokyo, University of Groningen, University of Chicago, University of Pennsylvania, McGill University, National Institute of Standards and Technology, NASA Goddard Space Flight Center, University of Sussex, Princeton University, Simon Fraser University, National Institute for Nuclear Physics, Haverford College, Stockholm University, Case Western Reserve University, University of British Columbia, University of Colorado Boulder, University of Minnesota Twin Cities, University of Michigan, Ann Arbor, Simons Foundation, Columbia University, University of Virginia, University of California Davis, Yale University, University of Pittsburgh, Ben-Gurion University of the Negev, Department of Electronics and Nanoengineering, Jet Propulsion Laboratory, University of California Santa Barbara, Perimeter Institute for Theoretical Physics, Service d'Astrophysique CEA, European Southern Observatory, Washington University St. Louis, University of Milan - Bicocca, University of Southern California, Institute for Advanced Studies, Pennsylvania State University, Brookhaven National Laboratory, Kyoto University, University of Wisconsin-Madison, University of Milano, Université Paris-Saclay, Brown University, Syracuse University, University of California Los Angeles, Aalto-yliopisto, and Aalto University

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology, CMB, Settore FIS/05, Space and Planetary Science, astro-ph.CO, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies and Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CMB-S4---the next-generation ground-based cosmic microwave background (CMB) experiment---is set to significantly advance the sensitivity of CMB measurements and enhance 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. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semi-analytic projection tool, targeted explicitly towards optimizing constraints on the tensor-to-scalar ratio, $r$, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2--3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments given a desired scientific goal. To form a closed-loop process, we couple this semi-analytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for $r > 0.003$ at greater than $5��$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473

Published
2022

15. Density reconstruction from biased tracers and its application to primordial non-Gaussianity

Author

Darwish, Omar, Foreman, Simon, Abidi, Muntazir M., Baldauf, Tobias, Sherwin, Blake D., Meerburg, P. Daniel, and Cosmic Frontier

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, 0103 physical sciences, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 010306 general physics, 01 natural sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Large-scale Fourier modes of the cosmic density field are of great value for learning about cosmology because of their well-understood relationship to fluctuations in the early universe. However, cosmic variance generally limits the statistical precision that can be achieved when constraining model parameters using these modes as measured in galaxy surveys, and moreover, these modes are sometimes inaccessible due to observational systematics or foregrounds. For some applications, both limitations can be circumvented by reconstructing large-scale modes using the correlations they induce between smaller-scale modes of an observed tracer (such as galaxy positions). In this paper, we further develop a formalism for this reconstruction, using a quadratic estimator similar to the one used for lensing of the cosmic microwave background. We incorporate nonlinearities from gravity, nonlinear biasing, and local-type primordial non-Gaussianity, and verify that the estimator gives the expected results when applied to N-body simulations. We then carry out forecasts for several upcoming surveys, demonstrating that, when reconstructed modes are included alongside directly-observed tracer density modes, constraints on local primordial non-Gaussianity are generically tightened by tens of percents compared to standard single-tracer analyses. In certain cases, these improvements arise from cosmic variance cancellation, with reconstructed modes taking the place of modes of a separate tracer, thus enabling an effective "multitracer" approach with single-tracer observations., Comment: 30 pages plus 14 pages appendices, 19 figures

Published
2021

16. First Measurement of the Cross-Correlation of CMB Lensing and Galaxy Lensing

Author

Hand, Nick, Leauthaud, Alexie, Das, Sudeep, Sherwin, Blake D, Addison, Graeme E, Bond, J. Richard, Calabrese, Erminia, Charbonnier, Aldée, Devlin, Mark J, Dunkley, Joanna, Erben, Thomas, Hajian, Amir, Halpern, Mark, Harnois-Déraps, Joachim, Heymans, Catherine, Hildebrandt, Hendrik, Hincks, Adam D, Kneib, Jean-Paul, Kosowsky, Arthur, Makler, Martin, Miller, Lance, Moodley, Kavilan, Moraes, Bruno, Niemack, Michael D, Page, Lyman A, Partridge, Bruce, Sehgal, Neelima, Shan, Huanyuan, Sievers, Jonathan L, Spergel, David N, Staggs, Suzanne T, Switzer, Eric R, Taylor, James E, Waerbeke, Ludovic Van, Welker, Charlotte, and Wollack, Edward J

Subjects
Astrophysics
Abstract

We measure the cross-correlation of cosmic microwave background (CMB) lensing convergence maps derived from Atacama Cosmology Telescope data with galaxy lensing convergence maps as measured by the Canada-France-Hawaii Telescope Stripe 82 Survey. The CMB-galaxy lensing cross power spectrum is measured for the first time with a significance of 4.2σ, which corresponds to a 12% constraint on the amplitude of density fluctuations at redshifts ∼0.9. With upcoming improved lensing data, this novel type of measurement will become a powerful cosmological probe, providing a precise measurement of the mass distribution at intermediate redshifts and serving as a calibrator for systematic biases in weak lensing measurements.

Published
2015
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17. Delensing the CMB with the cosmic infrared background: the impact of foregrounds.

Author

Baleato Lizancos, Antón, Challinor, Anthony, Sherwin, Blake D, and Namikawa, Toshiya

Subjects
COSMIC background radiation, GRAVITATIONAL lenses, DUST, GRAVITATIONAL waves, STATISTICAL errors, POWER spectra
Abstract

The most promising avenue for detecting primordial gravitational waves from cosmic inflation is through measurements of degree-scale cosmic microwave background (CMB) B -mode polarization. This approach must face the challenge posed by gravitational lensing of the CMB, which obscures the signal of interest. Fortunately, the lensing effects can be partially removed by combining high-resolution E -mode measurements with an estimate of the projected matter distribution. For near-future experiments, the best estimate of the latter will arise from co-adding internal reconstructions (derived from the CMB itself) with external tracers such as the cosmic infrared background (CIB). In this work, we characterize how foregrounds impact the delensing procedure when CIB intensity, I , is used as the matter tracer. We find that higher point functions of the CIB and Galactic dust such as 〈 BEI 〉 c and 〈 EIEI 〉 c can, in principle, bias the power spectrum of delensed B -modes. To quantify these, we first estimate the dust residuals in currently available CIB maps and upcoming, foreground-cleaned Simons Observatory CMB data. Then, using non-Gaussian simulations of Galactic dust – extrapolated to the relevant frequencies, assuming the spectral index of polarized dust emission to be fixed at the value determined by Planck – we show that the bias to any primordial signal is small compared to statistical errors for ground-based experiments, but might be significant for space-based experiments probing very large angular scales. However, mitigation techniques based on multifrequency cleaning appear to be very effective. We also show, by means of an analytical model, that the bias arising from the higher point functions of the CIB itself ought to be negligible. [ABSTRACT FROM AUTHOR]

Published
2022
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18. physical origin of dark energy constraints from rubin observatory and CMB-S4 lensing tomography.

Author

Yu, Byeonghee, Ferraro, Simone, Knight, Z Robert, Knox, Lloyd, and Sherwin, Blake D

Subjects
DARK energy, COSMIC background radiation, OBSERVATORIES, FORCE & energy, TOMOGRAPHY, LARGE scale structure (Astronomy)
Abstract

We seek to clarify the origin of constraints on the dark energy equation of state parameter from CMB lensing tomography, that is the combination of galaxy clustering and the cross-correlation of galaxies with CMB lensing in a number of redshift bins. We focus on the analytic understanding of the origin of the constraints. Dark energy information in these data arises from the influence of three primary relationships: distance as a function of redshift (geometry), the amplitude of the power spectrum as a function of redshift (growth), and the power spectrum as a function of wavenumber (shape). We find that the effects from geometry and growth play a significant role and partially cancel each other out, while the shape effect is unimportant. We also show that Dark Energy Task Force figure of merit forecasts from the combination of LSST galaxies and CMB-S4 lensing are comparable to the forecasts from cosmic shear in the absence of the CMB lensing map, thus providing an important independent check. Compared to the forecasts with the LSST galaxies alone, combining CMB lensing and LSST clustering information increases the FoM by roughly a factor of 3–4 in the optimistic scenario where systematics are fully under control. We caution that achieving these forecasts will likely require a full analysis of higher-order biasing, photometric redshift uncertainties, and stringent control of other systematic limitations, which are outside the scope of this work, whose primary purpose is to elucidate the physical origin of the constraints. [ABSTRACT FROM AUTHOR]

Published
2022
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19. The Herschel-SPIRE Legacy Survey (HSLS): the scientific goals of a shallow and wide submillimeter imaging survey with SPIRE

Author

Cooray, Asantha, Eales, Steve, Chapman, Scott, Clements, David L., Dore, Olivier, Farrah, Duncan, Jarvis, Matt J., Kaplinghat, Manoj, Negrello, Mattia, Melchiorri, Alessandro, Peiris, Hiranya, Pope, Alexandra, Santos, Mario G., Serjeant, Stephen, Thompson, Mark, White, Glenn, Amblard, Alexandre, Banerji, Manda, Corasaniti, Pier-Stefano, Das, Sudeep, Bernardis, Francesco, Zotti, Gianfranco, Giannantonio, Tommaso, Gonzalez-Nuevo Gonzalez, Joaquin, Khostovan, Ali Ahmad, Mitchell-Wynne, Ketron, Serra, Paolo, Song, Yong-Seon, Vieira, Joaquin, Wang, Lingyu, Zemcov, Michael, Abdalla, Filipe, Afonso, Jose, Aghanim, Nabila, Andreani, Paola, Aretxaga, Itziar, Auld, Robbie, Baes, Maarten, Baker, Andrew, Barkats, Denis, Belen Barreiro, R., Bartolo, Nicola, Barton, Elizabeth, Barway, Sudhanshu, Stefano Battistelli, Elia, Baugh, Carlton, Beelen, Alexander, Benabed, Karim, Blain, Andrew, Bland-Hawthorn, Joss, Bock, James J., Bond, J. Richard, Borrill, Julian, Borys, Colin, Boselli, Alessandro, Bouchet, Francois R., Bridge, Carrie, Brighenti, Fabrizio, Buat, Veronique, Buote, David, Burgarella, Denis, Bussmann, Robert, Calabrese, Erminia, Cantalupo, Christopher, Carlberg, Raymond, Sofia Carvalho, Carla, Caitlin Casey, Cava, Antonio, Cepa, Jordi, Chapin, Edward, Ram Chary, Ranga, Chen, Xuelei, Colafrancesco, Sergio, Cole, Shaun, Coles, Peter, Conley, Alexander, Conversi, Luca, Cooke, Jeff, Crawford, Steven, Cress, Catherine, Da Cunha, Elisabete, Dalton, Gavin, Danese, Luigi, Dannerbauer, Helmut, Davies, Jonathan, Bernardis, Paolo, Putter, Roland, Devlin, Mark, Diego, Jose M., Dole, Herve, Douspis, Marian, Dunkley, Joanna, Dunlop, James, Dunne, Loretta, Dunner, Rolando, Dye, Simon, Efstathiou, George, Egami, Eiichi, Fang, Taotao, Ferrero, Patrizia, Franceschini, Alberto, Frazer, Christopher C., Frayer, David, Frenk, Carlos, Ganga, Ken, Gavazzi, Raphael, Glenn, Jason, Gong, Yan, Gonzalez-Solares, Eduardo, Griffin, Matt, Guo, Qi, Gurwell, Mark, Hajian, Amir, Halpern, Mark, Hanson, Duncan, Hardcastle, Martin, Hatziminaoglou, Evanthia, Heavens, Alan, Heinis, Sebastien, Herranz, Diego, Hilton, Matt, Ho, Shirley, Holwerda, Benne W., Hopwood, Rosalind, Horner, Jonathan, Huffenberger, Kevin, Hughes, David H., Hughes, John P., Ibar, Edo, Ivison, Rob, Jackson, Neal, Jaffe, Andrew, Jenness, Timothy, Joncas, Gilles, Joudaki, Shahab, Kaviraj, Sugata, Kim, Sam, King, Lindsay, Kisner, Theodore, Knapen, Johan, Kniazev, Alexei, Komatsu, Eiichiro, Koopmans, Leon, Kuo, Chao-Lin, Lacey, Cedric, Lahav, Ofer, Lasenby, Anthony N., Lawrence, Andy, Lee, Myung Gyoon, Leeuw, Lerothodi L., Levenson, Louis R., Lewis, Geraint, Loaring, Nicola, Lopez-Caniego, Marcos, Maddox, Steve, Marriage, Tobias, Marsden, Gaelen, Martinez-Gonzalez, Enrique, Masi, Silvia, Matarrese, Sabino, Mathews, William G., Matsuura, Shuji, Mcmahon, Richard, Mellier, Yannick, Menanteau, Felipe, Michalowski, Michal J., Millea, Marius, Mobasher, Bahram, Mohanty, Subhanjoy, Montier, Ludovic, Moodley, Kavilan, Moriarty-Schieven, Gerald H., Mortier, Angela, Munshi, Dipak, Murphy, Eric, Nandra, Kirpal, Natoli, Paolo, Nguyen, Hien, Oliver, Seb, Omont, Alain, Page, Lyman, Page, Mathew, Paladini, Roberta, Pandolfi, Stefania, Pascale, Enzo, Patanchon, Guillaume, Peacock, John, Pearson, Chris, Perez-Fournon, Ismael, Perez-Gonz, Pablo G., Piacentini, Francesco, Pierpaoli, Elena, Pohlen, Michael, Pointecouteau, Etienne, Polenta, Gianluca, Rawlings, Jason, Reese, Erik D., Rigby, Emma, Rodighiero, Giulia, Romero-Colmenero, Encarni, Roseboom, Isaac, Rowan-Robinson, Michael, Sanchez-Portal, Miguel, Schmidt, Fabian, Schneider, Michael, Schulz, Bernhard, Scott, Douglas, Sedgwick, Chris, Sehgal, Neelima, Seymour, Nick, Sherwin, Blake D., Short, Jo, Shupe, David, Sievers, Jonathan, Skibba, Ramin, Smidt, Joseph, Smith, Anthony, Smith, Daniel J. B., Smith, Matthew W. L., Spergel, David, Staggs, Suzanne, Stevens, Jason, Switzer, Eric, Takagi, Toshinobu, Takeuchi, Tsutomu, Temi, Pasquale, Trichas, Markos, Trigilio, Corrado, Tugwell, Katherine, Umana, Grazia, Vacca, William, Vaccari, Mattia, Vaisanen, Petri, Valtchanov, Ivan, Heyden, Kurt, Werf, Paul P., Kampen, Eelco, Waerbeke, Ludovic, Vegetti, Simona, Veneziani, Marcella, Verde, Licia, Verma, Aprajita, Vielva, Patricio, Viero, Marco P., Vila Vilaro, Baltasar, Wardlow, Julie, Wilson, Grant, Wright, Edward L., Xu, C. Kevin, Yun, Min S., Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A large sub-mm survey with Herschel will enable many exciting science opportunities, especially in an era of wide-field optical and radio surveys and high resolution cosmic microwave background experiments. The Herschel-SPIRE Legacy Survey (HSLS), will lead to imaging data over 4000 sq. degrees at 250, 350, and 500 micron. Major Goals of HSLS are: (a) produce a catalog of 2.5 to 3 million galaxies down to 26, 27 and 33 mJy (50% completeness; 5 sigma confusion noise) at 250, 350 and 500 micron, respectively, in the southern hemisphere (3000 sq. degrees) and in an equatorial strip (1000 sq. degrees), areas which have extensive multi-wavelength coverage and are easily accessible from ALMA. Two thirds of the of the sources are expected to be at z > 1, one third at z > 2 and about a 1000 at z > 5. (b) Remove point source confusion in secondary anisotropy studies with Planck and ground-based CMB data. (c) Find at least 1200 strongly lensed bright sub-mm sources leading to a 2% test of general relativity. (d) Identify 200 proto-cluster regions at z of 2 and perform an unbiased study of the environmental dependence of star formation. (e) Perform an unbiased survey for star formation and dust at high Galactic latitude and make a census of debris disks and dust around AGB stars and white dwarfs., White paper supplement to the proposal submitted by the HSLS science team to ESA for Herschel open-time programs

Published
2020

20. First Measurement of the Cross-Correlation of CMB Lensing and Galaxy Lensing

Author

Hand, Nick, Leauthaud, Alexie, das, Sudeep, Das, Sudeep, Sherwin, Blake D, Addison, Graeme E, Bond, J. Richard, Calabrese, Erminia, Charbonnier, Ald´ee, Devlin, Mark J, Dunkley, Joanna, Erben, Thomas, Hajian, Amir, Halpern, Mark, Harnois-D´eraps, Joachim, Heymans, Catherine, Hildebrandt, Hendrik, Hincks, Adam D, Kneib, Jean-Paul, Kosowsky, Arthur, Makler, Martin, Miller, Lance, Moodley, Kavilan, Moraes, Bruno, Niemack, Michael D, Page, Lyman A, Partridge, Bruce, Sehgal, Neelima, Shan, Huanyuan, Sievers, Jonathan L, Spergel, David N, Staggs, Suzanne T, Switzer, Eric R, Taylor, James E, Waerbeke, Ludovic Van, and Wollack, Edward J

Subjects
Astrophysics
Abstract

We measure the cross-correlation of cosmic microwave background lensing convergence maps derived from Atacama Cosmology Telescope data with galaxy lensing convergence maps as measured by the Canada-France-Hawaii Telescope Stripe 82 Survey. The CMB-galaxy lensing cross power spectrum is measured for the first time with a significance of 3.2σ, which corresponds to a 16% constraint on the amplitude of density fluctuations at redshifts ~ 0.9. With upcoming improved lensing data, this novel type of measurement will become a powerful cosmological probe, providing a precise measurement of the mass distribution at intermediate redshifts and serving as a calibrator for systematic biases in weak lensing measurements.

Published
2013
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21. The Atacama Cosmology Telescope: Cross-Correlation of Cosmic Microwave Background Lensing and Quasars

Author

Sherwin, Blake D, Das, Sudeep, Haijian, Amir, Addison, Graeme, Bond, Richard, Crichton, Devin, Devlin, Mark J, Dunkley, Joanna, Gralla, Megan B, Halpern, Mark, Hill, J. Colin, Hincks, Adam D, Hughes, John P, Huffenberger, Kevin, Hlozek, Renee, Kosowsky, Arthur, Louis, Thibaut, Marriage, Tobias A, Marsden, Danica, Menanteau, Felipe, Moodley, Kavilan, Niemack, Michael D, Page, Lyman A, Reese. Erik D, Sehgal, Neelima, Sievers, Jon, Sifon, Cristobal, Spergel, David N, Staggs, Suzanne T, Switzer, Eric R, and Wollack, Ed

Subjects
Astrophysics
Abstract

We measure the cross-correlation of Atacama cosmology telescope cosmic microwave background (CMB) lensing convergence maps with quasar maps made from the Sloan Digital Sky Survey DR8 SDSS-XDQSO photometric catalog. The CMB lensing quasar cross-power spectrum is detected for the first time at a significance of 3.8 sigma, which directly confirms that the quasar distribution traces the mass distribution at high redshifts z > 1. Our detection passes a number of null tests and systematic checks. Using this cross-power spectrum, we measure the amplitude of the linear quasar bias assuming a template for its redshift dependence, and find the amplitude to be consistent with an earlier measurement from clustering; at redshift z ap 1.4, the peak of the distribution of quasars in our maps, our measurement corresponds to a bias of b = 2.5 +/- 0.6. With the signal-to-noise ratio on CMB lensing measurements likely to improve by an order of magnitude over the next few years, our results demonstrate the potential of CMB lensing crosscorrelations to probe astrophysics at high redshifts.

Published
2012
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22. The Atacama Cosmology Telescope: A Measurement of the Thermal Sunyaev-Zel'dovich Effect Using the Skewness of the CMB Temperature Distribution

Author

Wilson, Michael J, Sherwin, Blake D, Hill, J. Collin, Addison, Graeme, Battaglia, Nick, Bond, J. Richard, Das, Sudeep, Devlin, Mark J, Dunkley, Joanna, Duenner, Rolando, Fowler, Joseph W, Gralla, Megan, B, Hajian, Amir, Halpern, Mark, Hilton, Matt, Hincks, Adam D, Hlozek, Renee, Huffenberger, Kevin, Hughes, John P, Kosowsky, Arthur, Louis, Thibaut, Marriage, Tobias A, Marsden, Danica, Menanteau, Felipe, and Wollack, Ed

Subjects
Astronomy
Abstract

We present a detection of the unnormalized skewness (T(sup ~)(sup 2)(n(circumflex)) induced by the thermal Sunyaev-Zel'dovich (tSZ) effect in filtered Atacama Cosmology Telescope (ACT) 148 GHz cosmic microwave background temperature maps. Contamination due to infrared and radio sources is minimized by template subtraction of resolved sources and by constructing a mask using outlying values in the 218 GHz (tSZ-null) ACT maps. We measure (T(sup ~)(sup 3) (n(circumflex)) = -31 plus or minus 6 micro-K(sup 3) (measurement error only) or plus or minus 14 micro-K(sup 3) (including cosmic variance error) in the filtered ACT data, a 5sigma detection. We show that the skewness is a sensitive probe of sigma(sub 8), and use analytic calculations and tSZ simulations to obtain cosmological constraints from this measurement. From this signal alone we infer a value of sigma(sub 8) = 0.78 sup +0.03 sub -0.04 (68% C.L.) sup +0.05 sub -0.16. Our results demonstrate that measurements of nonGaussianity can be a useful method for characterizing the tSZ effect and extracting the underlying cosmological information.

Published
2012

23. Evidence for Dark Energy from the Cosmic Microwave Background Alone Using the Atacama Cosmology Telescope Lensing Measurements

Author

Sherwin, Blake D, Dunkley, Joanna, Das, Sudeep, Appel, John W, Bond, J. Richard, Carvalho, C. Sofia, Devlin, Mark J, Duenner, Rolando, Essinger-Hileman, Thomas, Fowler, Joesph J, Hajian, Amir, Halpern, Mark, Hasselfield, Matthew, Hincks, Adam D, Hlozek, Renee, Hughes, John P, Irwin, Kent D, Klein, Jeff, Kosowsky, Arthur, Marriage, Tobias A, Marsden, Danica, Moodley, Kavilan, Menanteau, Felipe, Niemack, Michael D, and Wollack, Ed

Subjects
Astronomy
Abstract

For the first time, measurements of the cosmic microwave background radiation (CMB) alone favor cosmologies with w = -1 dark energy over models without dark energy at a 3.2-sigma level. We demonstrate this by combining the CMB lensing deflection power spectrum from the Atacama Cosmology Telescope with temperature and polarization power spectra from the "Wilkinson Microwave Anisotropy Probe. The lensing data break the geometric degeneracy of different cosmological models with similar CMB temperature power spectra. Our CMB-only measurement of the dark energy density Omega(delta) confirms other measurements from supernovae, galaxy clusters and baryon acoustic oscillations, and demonstrates the power of CMB lensing as a new cosmological tool.

Published
2011

24. 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

25. 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

26. 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

27. 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

28. 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

29. 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

30. Towards Neutrino Mass from Cosmology without Optical Depth Information

Author

Yu, Byeonghee, Knight, Robert Z, Sherwin, Blake D., Ferraro, Simone, Knox, Lloyd, and Schmittfull, Marcel

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

With low redshift probes reaching unprecedented precision, uncertainty of the CMB optical depth is expected to be the limiting factor for future cosmological neutrino mass constraints. In this paper, we discuss to what extent combinations of CMB lensing and galaxy surveys measurements at low redshifts $z\sim 0.5-5$ will be able to make competitive neutrino mass measurements without relying on any optical depth constraints. We find that the combination of LSST galaxies and CMB-S4 lensing should be able to achieve constraints on the neutrino mass sum of 25meV without optical depth information, an independent measurement that is competitive with or slightly better than the constraint of 30meV possible with CMB-S4 and present-day optical depth measurements. These constraints originate both in structure growth probed by cross-correlation tomography over a wide redshift range as well as, most importantly, the shape of the galaxy power spectrum measured over a large volume. We caution that possible complications such as higher-order biasing and systematic errors in the analysis of high redshift galaxy clustering are only briefly discussed and may be non-negligible. Nevertheless, our results show that new kinds of high-precision neutrino mass measurements at and beyond the present-day optical depth limit may be possible., 8 pages, 6 figures

Published
2018

31. Determining the Hubble constant without the sound horizon scale: measurements from CMB lensing.

Author

Baxter, Eric J and Sherwin, Blake D

Subjects
*HUBBLE constant, *COSMIC background radiation, *SCALING (Social sciences), *DARK matter, *LARGE scale structure (Astronomy), *HORIZON, *GRAVITATIONAL lenses
Abstract

Measurements of the Hubble constant, H 0, from the cosmic distance ladder are currently in tension with the value inferred from Planck observations of the cosmic microwave background (CMB) and other high-redshift data sets if a flat Λ cold dark matter (ΛCDM) cosmological model is assumed. One of the few promising theoretical resolutions of this tension is to invoke new physics that changes the sound horizon scale in the early Universe; this can bring CMB and baryon acoustic oscillations (BAO) constraints on H 0 into better agreement with local measurements. In this paper, we discuss how a measurement of the Hubble constant can be made from the CMB without using information from the sound horizon scale, r s. In particular, we show how measurements of the CMB lensing power spectrum can place interesting constraints on H 0 when combined with measurements of either supernovae or galaxy weak lensing, which constrain the matter density parameter. The constraints arise from the sensitivity of the CMB lensing power spectrum to the horizon scale at matter–radiation equality (in projection); this scale could have a different dependence on new physics than the sound horizon. From an analysis of current CMB lensing data from Planck and Pantheon supernovae with conservative external priors, we derive an r s-independent constraint of |$H_0 = 73.5\pm 5.3\, {\rm km}\,{\rm s}^{-1}\,{\rm Mpc}^{-1}$|⁠. Forecasts for future CMB surveys indicate that improving constraints beyond an error of |$\sigma (H_0) = 3\, {\rm km}\,{\rm s}^{-1}\,{\rm Mpc}^{-1}$| will be difficult with CMB lensing, although applying similar methods to the galaxy power spectrum may allow for further improvements. [ABSTRACT FROM AUTHOR]

Published
2021
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32. The Atacama Cosmology Telescope: a CMB lensing mass map over 2100 square degrees of sky and its cross-correlation with BOSS-CMASS galaxies.

Author

Darwish, Omar, Madhavacheril, Mathew S, Sherwin, Blake D, Aiola, Simone, Battaglia, Nicholas, Beall, James A, Becker, Daniel T, Bond, J Richard, Calabrese, Erminia, Choi, Steve K, Devlin, Mark J, Dunkley, Jo, Dünner, Rolando, Ferraro, Simone, Fox, Anna E, Gallardo, Patricio A, Guan, Yilun, Halpern, Mark, Han, Dongwon, and Hasselfield, Matthew

Subjects
CROSS correlation, COSMIC background radiation, LARGE scale structure (Astronomy), TELESCOPES, DARK matter
Abstract

We construct cosmic microwave background lensing mass maps using data from the 2014 and 2015 seasons of observations with the Atacama Cosmology Telescope (ACT). These maps cover 2100 square degrees of sky and overlap with a wide variety of optical surveys. The maps are signal dominated on large scales and have fidelity such that their correlation with the cosmic infrared background is clearly visible by eye. We also create lensing maps with thermal Sunyaev−Zel'dovich contamination removed using a novel cleaning procedure that only slightly degrades the lensing signal-to-noise ratio. The cross-spectrum between the cleaned lensing map and the BOSS CMASS galaxy sample is detected at 10σ significance, with an amplitude of A = 1.02 ± 0.10 relative to the Planck best-fitting Lambda cold dark matter cosmological model with fiducial linear galaxy bias. Our measurement lays the foundation for lensing cross-correlation science with current ACT data and beyond. [ABSTRACT FROM AUTHOR]

Published
2021
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33. The Atacama Cosmology Telescope: delensed power spectra and parameters.

Author

Han, Dongwon, Sehgal, Neelima, MacInnis, Amanda, van Engelen, Alexander, Sherwin, Blake D., Madhavacheril, Mathew S., Aiola, Simone, Battaglia, Nicholas, Beall, James A., Becker, Daniel T., Calabrese, Erminia, Choi, Steve K., Darwish, Omar, Denison, Edward V., Devlin, Mark J., Dunkley, Jo, Ferraro, Simone, Fox, Anna E., Hasselfield, Matthew, and Hill, J. Colin

Published
2021
Full Text
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34. CMB-S4 Science Book, First Edition

Author

Abazajian, Kevork N., Adshead, Peter, Ahmed, Zeeshan, Allen, Steven W., Alonso, David, Arnold, Kam S., Baccigalupi, Carlo, Bartlett, James G., Battaglia, Nicholas, Benson, Bradford A., Bischoff, Colin A., Borrill, Julian, Buza, Victor, Calabrese, Erminia, Caldwell, Robert, Carlstrom, John E., Chang, Clarence L., Crawford, Thomas M., Francis-Yan, Cyr-Racine, Francesco, Bernardis, Haan, Tijmen, Di Serego Alighieri, Sperello, Dunkley, Joanna, Dvorkin, Cora, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Fuller, George M., Gluscevic, Vera, Green, Daniel, Grin, Daniel, Grohs, Evan, Henning, Jason W., Colin Hill, J., Hložek, Renée, Holder, Gilbert, Holzapfel, William, Hu, Wayne, Huffenberger, Kevin M., Keskitalo, Reijo, Knox, Lloyd, Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Chao-Lin, Kuo, Kusaka, Akito, Maude Le, Jeune, Lee, Adrian T., Lilley, Marc, Loverde, Marilena, Mathew Madhavacheril, Mantz, Adam, Marsh, David J. E., Jeffrey, Mcmahon, Pieter Daniel, Meerburg, Meyers, Joel, Miller, Amber D., Munoz, Julian B., Nguyen, Ho Nam, Niemack, Michael D., Peloso, Marco, Peloton, Julien, Pogosian, Levon, Pryke, Clement, Raveri, Marco, Reichardt, Christian L., Rocha, Graca, Rotti, Aditya, Schaan, Emmanuel, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Smith, Tristan L., Sorbo, Lorenzo, Starkman, Glenn D., Story, Kyle T., Engelen, Alexander, Vieira, Joaquin D., Watson, Scott, Whitehorn, Nathan, and Wu, W. L. Kimmy

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

This book lays out the scientific goals to be addressed by the next-generation ground-based cosmic microwave background experiment, CMB-S4, envisioned to consist of dedicated telescopes at the South Pole, the high Chilean Atacama plateau and possibly a northern hemisphere site, all equipped with new superconducting cameras. CMB-S4 will dramatically advance cosmological studies by crossing critical thresholds in the search for the B-mode polarization signature of primordial gravitational waves, in the determination of the number and masses of the neutrinos, in the search for evidence of new light relics, in constraining the nature of dark energy, and in testing general relativity on large scales.

Published
2017

35. POLARBEAR constraints on cosmic birefringence and primordial magnetic fields

Author

POLARBEAR Collaboration, Ade, Peter A. R., Arnold, Kam, Atlas, Matt, Baccigalupi, Carlo, Barron, Darcy, Boettger, David, Borrill, Julian, Chapman, Scott, Chinone, Yuji, Cukierman, Ari, Dobbs, Matt, Ducout, Anne, Dunner, Rolando, Elleflot, Tucker, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Feng, Chang, Gilbert, Adam, Goeckner-Wald, Neil, Groh, John, Hall, Grantland, Halverson, Nils W., Hasegawa, Masaya, Hattori, Kaori, Hazumi, Masashi, Hill, Charles, Holzapfel, William L., Hori, Yasuto, Howe, Logan, Inoue, Yuki, Jaehnig, Gregory C., Jaffe, Andrew H., Jeong, Oliver, Katayama, Nobuhiko, Kaufman, Jonathan P., Keating, Brian, Kermish, Zigmund, Keskitalo, Reijo, Kisner, Theodore, Kusaka, Akito, Jeune, Maude Le, Lee, Adrian T., Leitch, Erik M., Leon, David, Li, Yun, Linder, Eric, Lowry, Lindsay, Matsuda, Frederick, Matsumura, Tomotake, Miller, Nathan, Montgomery, Josh, Myers, Michael J., Navaroli, Martin, Nishino, Haruki, Okamura, Takahiro, Paar, Hans, Peloton, Julien, Pogosian, Levon, Poletti, Davide, Puglisi, Giuseppe, Raum, Christopher, Rebeiz, Gabriel, Reichardt, Christian L., Richards, Paul L., Ross, Colin, Rotermund, Kaja M., Schenck, David E., Sherwin, Blake D., Shimon, Meir, Shirley, Ian, Siritanasak, Praween, Smecher, Graeme, Stebor, Nathan, Steinbach, Bryan, Suzuki, Aritoki, Suzuki, Jun-ichi, Tajima, Osamu, Takakura, Satoru, Tikhomirov, Alexei, Tomaru, Takayuki, Whitehorn, Nathan, Wilson, Brandon, Yadav, Amit, Zahn, Alex, Zahn, Oliver, Science and Technology Facilities Council (STFC), Departamento de Astronomía y Astrofísica [Santiago], Pontificia Universidad Católica de Chile (UC), APC - Gravitation (APC-Gravitation), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Atmospheric Science [Laramie], University of Wyoming (UW), Laboratoire Kastler Brossel (LKB (Lhomond)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Catania (INGV), Istituto Nazionale di Geofisica e Vulcanologia, University of California [San Diego] (UC San Diego), University of California (UC), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), University of California, 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)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Ade, P, Arnold, K, Atlas, M, Baccigalupi, C, Barron, D, Boettger, D, Borrill, J, Chapman, S, Chinone, Y, Cukierman, A, Dobbs, M, Ducout, A, Dunner, R, Elleflot, T, Errard, J, Fabbian, G, Feeney, S, Feng, C, Gilbert, A, Goeckner-Wald, N, Groh, J, Hall, G, Halverson, N, Hasegawa, M, Hattori, K, Hazumi, M, Hill, C, Holzapfel, W, Hori, Y, Howe, L, Inoue, Y, Jaehnig, G, Jaffe, A, Jeong, O, Katayama, N, Kaufman, J, Keating, B, Kermish, Z, Keskitalo, R, Kisner, T, Kusaka, A, Le Jeune, M, Lee, A, Leitch, E, Leon, D, Li, Y, Linder, E, Lowry, L, Matsuda, F, Matsumura, T, Miller, N, Montgomery, J, Myers, M, Navaroli, M, Nishino, H, Okamura, T, Paar, H, Peloton, J, Pogosian, L, Poletti, D, Puglisi, G, Raum, C, Rebeiz, G, Reichardt, C, Richards, P, Ross, C, Rotermund, K, Schenck, D, Sherwin, B, Shimon, M, Shirley, I, Siritanasak, P, Smecher, G, Stebor, N, Steinbach, B, Suzuki, A, Suzuki, J, Tajima, O, Takakura, S, Tikhomirov, A, Tomaru, T, Whitehorn, N, Wilson, B, Yadav, A, Zahn, A, Zahn, O, École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmic microwave background, Astrophysics, 7. Clean energy, 01 natural sciences, Atomic, Physics, Particles & Fields, Particle and Plasma Physics, Observational cosmology, B-MODE POLARIZATION, ANISOTROPIES, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, [PHYS]Physics [physics], Physics, Quantum Physics, COSMIC cancer database, TEV BLAZARS, Settore FIS/05, SIGNATURE, SPTPOL DATA, Polarization (waves), Nuclear & Particles Physics, Magnetic field, GRAVITY-WAVES, Physical Sciences, symbols, astro-ph.CO, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Nuclear and High Energy Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, symbols.namesake, 0202 Atomic, Molecular, Nuclear, Particle And Plasma Physics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Faraday effect, LARGE-SCALE STRUCTURE, Nuclear, 100 SQUARE DEGREES, Planck, 0206 Quantum Physics, Background radiation, Science & Technology, 010308 nuclear & particles physics, Molecular, FARADAY-ROTATION, microwave background polarization, large-scale structure, b-mode polarization, 100 square degrees, faraday-rotation, gravity-waves, tev blazars, sptpol data, anisotropies, signature, cosmic microwave background, birefringence, 0201 Astronomical And Space Sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION
Abstract

注記: Polarbear Collaboration 86名 [所属. 宇宙航空研究開発機構宇宙科学研究所 (JAXA)(ISAS) 松村, 知岳], Note: Polarbear Collaboration 86members [Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS) Matsumura, Tomotake], 資料番号: SA1150239000

Published
2015

36. Evidence for the kinematic Sunyaev-Ze\v{l}dovich effect with ACTPol and velocity reconstruction from BOSS

Author

Schaan, Emmanuel, Ferraro, Simone, Vargas-Magaña, Mariana, Smith, Kendrick M., Ho, Shirley, Aiola, Simone, Battaglia, Nicholas, Bond, J. Richard, De Bernardis, Francesco, Calabrese, Erminia, Cho, Hsiao-Mei, Devlin, Mark J., Dunkley, Joanna, Gallardo, Patricio A., Hasselfield, Matthew, Henderson, Shawn, Hill, J. Colin, Hincks, Adam D., Hlozek, Renée, Hubmayr, Johannes, Hughes, John P., Irwin, Kent D., Koopman, Brian, Kosowsky, Arthur, Li, Dale, Louis, Thibaut, Lungu, Marius, Madhavacheril, Mathew, Maurin, Loïc, McMahon, Jeffrey John, Moodley, Kavilan, Naess, Sigurd, Nati, Federico, Newburgh, Laura, Niemack, Michael D., Page, Lyman A., Pappas, Christine G., Partridge, Bruce, Schmitt, Benjamin L., Sehgal, Neelima, Sherwin, Blake D., Sievers, Jonathan L., Spergel, David N., Staggs, Suzanne T., van Engelen, Alexander, and Wollack, Edward J.

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We use microwave temperature maps from two seasons of data from the Atacama Cosmology Telescope (ACTPol) at 146 GHz, together with the Constant Mass CMASS galaxy sample from the Baryon Oscillation Spectroscopic Survey to measure the kinematic Sunyaev-Ze\v{l}dovich (kSZ) effect over the redshift range z = 0.4 - 0.7. We use galaxy positions and the continuity equation to obtain a reconstruction of the line-of-sight velocity field. We stack the cosmic microwave background temperature at the location of each halo, weighted by the corresponding reconstructed velocity. The resulting best fit kSZ model is preferred over the no-kSZ hypothesis at 3.3sigma and 2.9sigma for two independent velocity reconstruction methods, using 25,537 galaxies over 660 square degrees. The effect of foregrounds that are uncorrelated with the galaxy velocities is expected to be well below our signal, and residual thermal Sunyaev-Ze\v{l}dovich contamination is controlled by masking the most massive clusters. Finally, we discuss the systematics involved in converting our measurement of the kSZ amplitude into the mean free electron fraction of the halos in our sample., Comment: 7 pages, 2 figures

Published
2015

37. Reconstructing small-scale lenses from the cosmic microwave background temperature fluctuations.

Author

Horowitz, Benjamin, Ferraro, Simone, and Sherwin, Blake D

Subjects
COSMIC background radiation, MAXIMUM likelihood statistics, MATCHED filters, TEMPERATURE measurements, LENSES, MAGNITUDE (Mathematics)
Abstract

Cosmic microwave background (CMB) lensing is a powerful probe of the matter distribution in the Universe. The standard quadratic estimator, which is typically used to measure the lensing signal, is known to be suboptimal for low-noise polarization data from next-generation experiments. In this paper, we explain why the quadratic estimator will also be suboptimal for measuring lensing on very small scales, even for measurements in temperature where this estimator typically performs well. Though maximum likelihood methods could be implemented to improve performance, we explore a much simpler solution, revisiting a previously proposed method to measure lensing that involves a direct inversion of the background gradient. An important application of this simple formalism is the measurement of cluster masses with CMB lensing. We find that directly applying a gradient inversion matched filter to simulated lensed images of the CMB can tighten constraints on cluster masses compared to the quadratic estimator. While the difference is not relevant for existing surveys, for future surveys it can translate to significant improvements in mass calibration for distant clusters, where galaxy lensing calibration is ineffective due to the lack of enough resolved background galaxies. Improvements can be as large as |${\sim } 50{{\ \rm per\ cent}}$| for a cluster at z  = 2 and a next-generation CMB experiment with 1  |$\mu$| K arcmin noise, and over an order of magnitude for lower noise levels. For future surveys, this simple matched filter or gradient inversion method approaches the performance of maximum likelihood methods, at a fraction of the computational cost. [ABSTRACT FROM AUTHOR]

Published
2019
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38. Cosmological Parameters from Pre-Planck CMB Measurements

Author

Calabrese, Erminia, Hlozek, Ren��e A., Battaglia, Nick, Battistelli, Elia S., Bond, J. Richard, Chluba, Jens, Crichton, Devin, Das, Sudeep, Devlin, Mark J., Dunkley, Joanna, D��nner, Rolando, Farhang, Marzieh, Gralla, Megan B., Hajian, Amir, Halpern, Mark, Hasselfield, Matthew, Hincks, Adam D., Irwin, Kent D., Kosowsky, Arthur, Louis, Thibaut, Marriage, Tobias A., Moodley, Kavilan, Newburgh, Laura, Niemack, Michael D., Nolta, Michael R., Page, Lyman A., Sehgal, Neelima, Sherwin, Blake D., Sievers, Jonathan L., Sif��n, Crist��bal, Spergel, David N., Staggs, Suzanne T., Switzer, Eric R., and Wollack, Edward J.

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

Recent data from the WMAP, ACT and SPT experiments provide precise measurements of the cosmic microwave background temperature power spectrum over a wide range of angular scales. The combination of these observations is well fit by the standard, spatially flat LCDM cosmological model, constraining six free parameters to within a few percent. The scalar spectral index, n_s = 0.9690 +/- 0.0089, is less than unity at the 3.6 sigma level, consistent with simple models of inflation. The damping tail of the power spectrum at high resolution, combined with the amplitude of gravitational lensing measured by ACT and SPT, constrains the effective number of relativistic species to be N_eff = 3.28 +/- 0.40, in agreement with the standard model's three species of light neutrinos., 5 pages, 4 figures

Published
2013

39. Detection and removal of B-mode dust foregrounds with signatures of statistical anisotropy.

Author

Philcox, Oliver H E, Sherwin, Blake D, and van Engelen, Alexander

Subjects
*GRAVITATIONAL waves, *COSMIC background radiation, *DUST, *GALAXIES, *SIMULATION methods & models
Abstract

Searches for inflationary gravitational wave signals in the cosmic microwave background (CMB) B-mode polarization are expected to reach unprecedented power over the next decade. A major difficulty in these ongoing searches is that Galactic foregrounds such as dust can easily mimic inflationary signals. Though, typically, foregrounds are separated from primordial signals using the foregrounds’ different frequency dependence, in this paper we investigate instead the extent to which the Galactic dust B-modes’ statistical anisotropy can be used to distinguish them from inflationary B-modes, building on the work of Kamionkowski and Kovetz (2014). In our work, we extend existing anisotropy estimators and apply them to simulations of polarized dust to forecast their performance for future experiments. Considering the application of this method as a null-test for dust contamination to CMB-S4, we find that we can detect residual dust levels corresponding to r ∼ 0.001 at 2σ, which implies that statistical anisotropy estimators will be a powerful diagnostic for foreground residuals (though our results show some dependence on the dust simulation used). Finally, considering applications beyond a simple null test, we demonstrate how anisotropy statistics can be used to construct an estimate of the dust B-mode map, which could potentially be used to clean the B-mode sky. [ABSTRACT FROM AUTHOR]

Published
2018
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40. The Atacama Cosmology Telescope: Cross-Correlation of CMB Lensing and Quasars

Author

Sherwin, Blake D., Das, Sudeep, Hajian, Amir, Addison, Graeme, Bond, J. Richard, Crichton, Devin, Devlin, Mark J., Dunkley, Joanna, Gralla, Megan B., Halpern, Mark, Hill, J. Colin, Hincks, Adam D., Hughes, John P., Huffenberger, Kevin, Hlozek, Renee, Kosowsky, Arthur, Louis, Thibaut, Marriage, Tobias A., Marsden, Danica, Menanteau, Felipe, Moodley, Kavilan, Niemack, Michael D., Page, Lyman A., Reese, Erik D., Sehgal, Neelima, Sievers, Jon, Sifon, Cristobal, Spergel, David N., Staggs, Suzanne T., Switzer, Eric R., and Wollack, Ed

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We measure the cross-correlation of Atacama Cosmology Telescope CMB lensing convergence maps with quasar maps made from the Sloan Digital Sky Survey DR8 SDSS-XDQSO photometric catalog. The CMB lensing-quasar cross-power spectrum is detected for the first time at a significance of 3.8 sigma, which directly confirms that the quasar distribution traces the mass distribution at high redshifts z>1. Our detection passes a number of null tests and systematic checks. Using this cross-power spectrum, we measure the amplitude of the linear quasar bias assuming a template for its redshift dependence, and find the amplitude to be consistent with an earlier measurement from clustering; at redshift z ~ 1.4, the peak of the distribution of quasars in our maps, our measurement corresponds to a bias of b = 2.5 +/- 0.6. With the signal-to-noise ratio on CMB lensing measurements likely to improve by an order of magnitude over the next few years, our results demonstrate the potential of CMB lensing cross-correlations to probe astrophysics at high redshifts., 7 pages, 5 figures; replaced with version accepted by Phys. Rev. D

Published
2012

41. The Ara OB1a association : Stellar population and star formation history

Author

Marriage, Tobias A., Acquaviva, Viviana, Ade, Peter A. R., Aguirre, Paula, Amiri, Mandana, Appel, John William, Felipe Barrientos, L., Battistelli, Elia S., Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Das, Sudeep, Devlin, Mark J., Dicker, Simon R., Doriese, W. Bertrand, Dunkley, Joanna, Duenner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P., Fowler, Joseph W., Hajian, Amir, Halpern, Mark, Hasselfield, Matthew, Hernandez-Monteagudo, Carlos, Hilton, Gene C., Hilton, Matt, Hincks, Adam D., Hlozek, Renee, Huffenberger, Kevin M., Handel Hughes, David, Hughes, John P., Infante, Leopoldo, Irwin, Kent D., Baptiste Juin, Jean, Kaul, Madhuri, Klein, Jeff, Kosowsky, Arthur, Lau, Judy M., Limon, Michele, Lin, Yen-Ting, Lupton, Robert H., Marsden, Danica, Martocci, Krista, Mauskopf, Phil, Menanteau, Felipe, Moodley, Kavilan, Moseley, Harvey, Netterfield, Calvin B., Niemack, Michael D., Nolta, Michael R., Page, Lyman A., Parker, Lucas, Partridge, Bruce, Quintana, Hernan, Reese, Erik D., Reid, Beth, Sehgal, Neelima, Sherwin, Blake D., Sievers, Jon, Spergel, David N., Staggs, Suzanne T., Swetz, Daniel S., Switzer, Eric R., Thornton, Robert, Trac, Hy, Tucker, Carole, Warne, Ryan, Wilson, Grant, Wollack, Ed, and Zhao, Yue

Subjects
Stellar population, Ciencias Físicas, FOS: Physical sciences, Context (language use), Astrophysics, stars: pre-main sequence, open clusters and associations: individual: NGC 6193, purl.org/becyt/ford/1 [https], Cluster (physics), pre-main sequence [stars], Physics, stars: formation, formation [stars], Star formation, individual: NGC 6193 [open clusters and associations], individual: NGC 6167 [open clusters and associations], Galactic quadrant, open clusters and associations: individual: NGC 6167, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], open clusters and associations: general, Astrophysics - Astrophysics of Galaxies, Interstellar medium, Astronomía, Stars, Star cluster, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), general [open clusters and associations], CIENCIAS NATURALES Y EXACTAS
Abstract

Context. The Ara OB1a association is a nearby complex in the fourth Galactic quadrant where a number of young/embedded star clusters are projected close to more evolved, intermediate age clusters. It is also rich in interstellar matter, and contains evidence of the interplay between massive stars and their surrounding medium, such as the rim HII region NGC 6188. Aims. We provide robust estimates of the fundamental parameters (age and distance) of the two most prominent stellar clusters, NGC 6167 and NGC 6193, that may be used as a basis for studing the star formation history of the region. Methods. The study is based on a photometric optical survey (UBVIHα) of NGC 6167 and NGC 6193 and their nearby field, complemented with data from 2MASS-VVV, UCAC3, and IRAC-Spitzer in this region. Results. We produce a uniform photometric catalogue and estimate more robustly the fundamental parameters of NGC 6167 and NGC 6193, in addition to the IRAS 16375-4854 source. As a consequence, all of them are located at approximately the same distance from the Sun in the Sagittarius-Carina Galactic arm. However, the ages we estimate differ widely: NGC 6167 is found to be an intermediate-age cluster (20-30 Myr), NGC 6193 a very young one (1-5 Myr) with PMS, Hα emitters and class II objects, and the IRAS 16375-4854 source is the youngest of the three containing several YSOs. Conclusions. These results support a picture in which Ara OB1a is a region where star formation has proceeded for several tens of Myr until the present. The difference in the ages of the different stellar groups can be interpreted as a consequence of a triggered star formation process. In the specific case of NGC 6193, we find evidence of possible non-coeval star formation., Instituto de Astrofísica de La Plata, Facultad de Ciencias Astronómicas y Geofísicas

Published
2011

42. The atacama cosmology telescope: sunyaev-zeldovich-selected galaxy clusters at 148 ghz in the 2008 survey

Author

Sehgal, Neelima, Trac, Hy, Acquaviva, Viviana, Ade, Peter A. R., Aguirre, Paula, Amiri, Mandana, Appel, John W., Felipe Barrientos, L., Battistelli, Elia S., Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Das, Sudeep, Devlin, Mark J., Dicker, Simon R., Doriese, W. Bertrand, Dunkley, Joanna, Duenner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P., Fowler, Joseph W., Hajian, Amir, Halpern, Mark, Hasselfield, Matthew, Hernandez-Monteagudo, Carlos, Hilton, Gene C., Hilton, Matt, Hincks, Adam D., Hlozek, Renee, Holtz, David, Huffenberger, Kevin M., Hughes, David H., Hughes, John P., Infante, Leopoldo, Irwin, Kent D., Jones, Andrew, Baptiste Juin, Jean, Klein, Jeff, Kosowsky, Arthur, Lau, Judy M., Limon, Michele, Lin, Yen-Ting, Lupton, Robert H., Marriage, Tobias A., Marsden, Danica, Martocci, Krista, Mauskopf, Phil, Menanteau, Felipe, Moodley, Kavilan, Moseley, Harvey, Netterfield, Calvin B., Niemack, Michael D., Nolta, Michael R., Page, Lyman A., Parker, Lucas, Partridge, Bruce, Reid, Beth, Sherwin, Blake D., Sievers, Jon, Spergel, David N., Staggs, Suzanne T., Swetz, Daniel S., Switzer, Eric R., Thornton, Robert, Tucker, Carole, Warne, Ryan, Wollack, Ed, and Zhao, Yue

Published
2011

43. The Atacama Cosmology Telescope: Calibration with WMAP Using Cross-Correlations

Author

Hajian, Amir, Acquaviva, Viviana, Ade, Peter A. R., Aguirre, Paula, Amiri, Mandana, Appel, John William, Barrientos, L. Felipe, Battistelli, Elia S., Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Das, Sudeep, Devlin, Mark J., Dicker, Simon R., Doriese, W. Bertrand, Dunkley, Joanna, Dunner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P., Fowler, Joseph W., Halpern, Mark, Hasselfield, Matthew, Hernandez-Monteagudo, Carlos, Hilton, Gene C., Hilton, Matt, Hincks, Adam D., Hlozek, Renee, Huffenberger, Kevin M., Hughes, David H., Hughes, John P., Infante, Leopoldo, Irwin, Kent D., Juin, Jean Baptiste, Kaul, Madhuri, Klein, Jeff, Kosowsky, Arthur, Lau, Judy M, Limon, Michele, Lin, Yen-Ting, Lupton, Robert H., Marriage, Tobias A., Marsden, Danica, Mauskopf, Phil, Menanteau, Felipe, Moodley, Kavilan, Moseley, Harvey, Netterfield, Calvin B., Niemack, Michael D., Nolta, Michael R., Page, Lyman A., Parker, Lucas, Partridge, Bruce, Reid, Beth, Sehgal, Neelima, Sherwin, Blake D., Sievers, Jon, Spergel, David N., Staggs, Suzanne T., Swetz, Daniel S., Switzer, Eric R., Thornton, Robert, Trac, Hy, Tucker, Carole, Warne, Ryan, Wollack, Ed, and Zhao, Yue

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation – cosmology: observations – methods: data analysis – methods: statistical, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a new calibration method based on cross-correlations with WMAP and apply it to data from the Atacama Cosmology Telescope (ACT). ACT's observing strategy and map making procedure allows an unbiased reconstruction of the modes in the maps over a wide range of multipoles. By directly matching the ACT maps to WMAP observations in the multipole range of 400 < ell < 1000, we determine the absolute calibration with an uncertainty of 2% in temperature. The precise measurement of the calibration error directly impacts the uncertainties in the cosmological parameters estimated from the ACT power spectra. We also present a combined map based on ACT and WMAP data that has high signal-to-noise over a wide range of multipoles., Submitted to ApJ. This is a companion to Das et al (2010) and Dunkley et al (2010)

Published
2011

44. The Atacama Cosmology Telescope: measuring radio galaxy bias through cross-correlation with lensing.

Author

Allison, Rupert, Lindsay, Sam N., Sherwin, Blake D., de Bernardis, Francesco, Bond, J. Richard, Calabrese, Erminia, Devlin, Mark J., Dunkley, Joanna, Gallardo, Patricio, Henderson, Shawn, Hincks, Adam D., Hlozek, Renée, Jarvis, Matt, Kosowsky, Arthur, Louis, Thibaut, Madhavacheril, Mathew, McMahon, Jeff, Moodley, Kavilan, Naess, Sigurd, and Newburgh, Laura

Subjects
METAPHYSICAL cosmology, TELESCOPE design & construction, RADIO galaxies, STATISTICAL correlation, MICROLENSING (Astrophysics)
Abstract

We correlate the positions of radio galaxies in the FIRST survey with the cosmic microwave background lensing convergence estimated from the Atacama Cosmology Telescope over 470 deg² to determine the bias of these galaxies. We remove optically cross-matched sources below redshift z = 0.2 to preferentially select active galactic nuclei (AGN). We measure the angular cross-power spectrum Clkgl at 4.4σ significance in the multipole range 100 < l < 3000, corresponding to physical scales within ≈2-60 Mpc at an effective redshift zeff = 1.5. Modelling the AGN population with a redshift-dependent bias, the cross-spectrum is well fitted by the Planck best-fitting A cold dark matter cosmological model. Fixing the cosmology and assumed redshift distribution of sources, we fit for the overall bias model normalization, finding b(zeff) = 3.5 ± 0.8 for the full galaxy sample and b(zeff) = 4.0 ± 1.1(3.0 ± 1.1) for sources brighter (fainter) than 2.5 mJy. This measurement characterizes the typical halo mass of radio-loud AGN: we find log(Mhalo/Mʘ) = 13.6+0.3-0.4 [ABSTRACT FROM AUTHOR]

Published
2015
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45. Delensing the CMB with the cosmic infrared background.

Author

Sherwin, Blake D. and Schmittfull, Marcel

Subjects
*COSMIC background radiation, *ASTROPHYSICAL radiation, *PHYSICAL cosmology
Abstract

As confusion with lensing B modes begins to limit experiments that search for primordial B-mode polarization, robust methods for delensing the cosmic microwave background (CMB) polarization sky are becoming increasingly important. We investigate in detail the possibility of delensing the CMB with the cosmic infrared background (CIB), emission from dusty star-forming galaxies that is an excellent tracer of the CMB lensing signal, in order to improve constraints on the tensor-to-scalar ratio r. We find that the maps of the CIB, such as current Planck satellite maps at 545 GHz, can be used to remove more than half of the lensing B-mode power. Calculating optimal combinations of different large-scale-structure tracers for delensing, we find that coadding CIB data and external arcminute-resolution CMB lensing reconstruction can lead to significant additional improvements in delensing performance. We investigate whether measurement uncertainty in the CIB power spectra will degrade the delensing performance if no model of the CIB spectra is assumed, and instead the CIB power spectra are marginalized over, when constraining r. We find that such uncertainty does not significantly affect B-mode surveys smaller than a few thousand degrees. Even for larger surveys it causes only a moderate reduction in CIB delensing performance, especially if the surveys have high (arcminute) resolution, which allows self calibration of the delensing procedure. Though further work on the impact of foreground residuals is required, our overall conclusions for delensing with current CIB data are optimistic: this delensing method can tighten constraints on r by a factor up to≈2.2, and by a factor up to ≈4 when combined with external lensing reconstruction for ≈3 μK-arcmin noise, without requiring the modeling of CIB properties. CIB delensing is thus a promising method for the upcoming generation of CMB polarization surveys. [ABSTRACT FROM AUTHOR]

Published
2015
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46. WISE measurement of the integrated Sachs-Wolfe effect.

Author

Ferrara, Simone, Sherwin, Blake D., and Spergel, David N.

Subjects
*DARK energy, *COSMIC background radiation, *GRAVITATIONAL potential, *DARK matter, *PLANCK'S constant, *FLUCTUATIONS (Physics)
Abstract

The integrated Sachs-Wolfe (ISW) effect measures the decay of the gravitational potential due to cosmic acceleration and is thus a direct probe of dark energy. In some of the earlier studies, the amplitude of the ISW effect was found to be in tension with the predictions of the standard Lambda cold dark matter (ΛCDM) model. We measure the cross power of galaxies and active galactic nuclei (AGN) from the Wide-field Infrared Survey Explorer mission with cosmic microwave background temperature data from WMAP9 in order to provide an independent measurement of the ISW amplitude. Cross-correlations with the recently released Planck lensing potential maps are used to calibrate the bias and contamination fraction of the sources, thus avoiding systematic effects that could be present when using autospectra to measure bias. We find an amplitude of the cross power of A = 1.24±0.47 from the galaxies and A = 0.88±0.74 from the AGN, fully consistent with the ΛCDM prediction of A = 1. The ISW measurement signal-to-noise ratio is 2.7 and 1.2 respectively. Comparing the amplitudes of the Galaxy and AGN cross-correlations, which arise from different redshifts, we find no evidence for redshift evolution in dark energy properties, consistent with a cosmological constant. [ABSTRACT FROM AUTHOR]

Published
2015
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47. Hypervelocity stars from the Andromeda galaxy.

Author

Sherwin, Blake D., Loeb, Abraham, and O'Leary, Ryan M.

Subjects
*ANDROMEDA Galaxy, *MILKY Way, *BLACK holes, *GALACTIC center, *GALACTIC halos
Abstract

Hypervelocity stars (HVSs) discovered in the Milky Way (MW) halo are thought to be ejected from near the massive black hole (MBH) at the Galactic centre. In this paper, we investigate the spatial and velocity distributions of the HVSs which are expected to be similarly produced in the Andromeda galaxy (M31). We consider three different HVS production mechanisms: (i) the disruption of stellar binaries by the galactocentric MBH; (ii) the ejection of stars by an in-spiralling intermediate-mass black hole and (iii) the scattering of stars off a cluster of stellar-mass black holes orbiting around the MBH. While the first two mechanisms would produce large numbers of HVSs in M31, we show that the third mechanism would not be effective in M31. We numerically calculate trajectories of HVSs from M31 within a simple model of the Local Group and hence infer the current distribution of these stars. Gravitational focusing of the HVSs by the MW and the diffuse Local Group medium leads to high densities of low-mass M31 HVSs near the MW. Within the virialized MW halo, we expect there to be of the order of 1000 HVSs for the first mechanism and a few hundred HVSs for the second mechanism; many of these stars should have distinctively large approach velocities . In addition, we predict approximately five hypervelocity red giant branch (RGB) stars within the M31 halo which could be identified observationally. Future MW astrometric surveys or searches for distant giants could thus find HVSs from M31. [ABSTRACT FROM AUTHOR]

Published
2008
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48. Cosmological constraints from moments of the thermal Sunyaev-Zel'dovich effect.

Author

Hill, J. Colin and Sherwin, Blake D.

Subjects
*CONSTRAINTS (Physics), *ASTROPHYSICS, *PHYSICAL cosmology, *GAUSSIAN processes, *GALAXY clusters, *SKEWNESS (Probability theory), *OSCILLATIONS
Abstract

In this paper, we explain how moments of the thermal Sunyaev-Zel'dovich (tSZ) effect can constrain both cosmological parameters and the astrophysics of the intracluster medium. As the tSZ signal is strongly non-Gaussian, higher moments of tSZ maps contain useful information. We first calculate the dependence of the tSZ moments on cosmological parameters, finding that higher moments scale more steeply with °~ and are sourced by more massive galaxy clusters. Taking advantage of the different dependence of the variance and skewness on cosmological and astrophysical parameters, we construct a statistic, ∣1,4, which cancels much of the dependence on cosmology (i.e., σ8) yet remains sensitive to the astrophysics of intracluster gas (in particular, to the gas fraction in low-mass clusters). Constraining the intracluster medium astrophysics using this statistic could break the well-known degeneracy between cosmology and gas physics in tSZ measurements, allowing for tight constraints on cosmological parameters. Although detailed simulations will be needed to fully characterize the accuracy of this technique, we provide a first application to data from the Atacama Cosmology Telescope and the South Pole Telescope. We estimate that a Planck-like full-sky tSZ map could achieve a ≲ 1% constraint on °8 and a 1σ error on the sum of the neutrino masses that is comparable to the existing lower bound from oscillation measurements. [ABSTRACT FROM AUTHOR]

Published
2013
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49. Atacama Cosmology Telescope: A measurement of the thermal Sunyaev-Zel'Fdovich effect using the skewness of the CMB temperature distribution.

Author

Wilson, Michael J., Sherwin, Blake D., Hill, J. Colin, Addison, Graeme, Battaglia, Nick, Bond, J. Richard, Das, Sudeep, Devlin, Mark J., Dunkley, Joanna, Dünner, Rolando, Fowler, Joseph W., Gralla, Megan B., Hajian, Amir, Halpern, Mark, Hilton, Matt, Hincks, Adam D., Hlozek, Renée, Huffenberger, Kevin, Hughes, John R., and Kosowsky, Arthur

Subjects
*METAPHYSICAL cosmology, *TELESCOPES, *TEMPERATURE distribution, *SKEWNESS (Probability theory), *COSMIC background radiation, *RADIO sources (Astronomy)
Abstract

We present a detection of the unnormalized skewness {&Ttilde;³(&ncirc)} induced by the thermal Sunyaev-Zel'dovich (tSZ) effect in filtered Atacama Cosmology Telescope (ACT) 148 GHz cosmic microwave background temperature maps. Contamination due to infrared and radio sources is minimized by template subtraction of resolved sources and by constructing a mask using outlying values in the 218 GHz (tSZnull) ACT maps. We measure {&Ttilde;³(&ncirc)} = -31 ± 6 µ³ (Gaussian statistics assumed) or ±14 µ³ (including non-Gaussian corrections) in the filtered ACT data, a 5σ detection. We show that the skewness is a sensitive probe of σ8, and use analytic calculations and tSZ simulations to obtain cosmological constraints from this measurement. From this signal alone we infer a value of σ8 = 0.79+0.03-0.03 (68% C.L.) +0.06-0.06 (95% C.L.). Our results demonstrate that measurements of non-Gaussianity can be a useful method for characterizing the tSZ effect and extracting the underlying cosmological information. [ABSTRACT FROM AUTHOR]

Published
2012
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50. Shift of the baryon acoustic oscillation scale: A simple physical picture.

Author

Sherwin, Blake D. and Zaldarriaga, Matias

Subjects
*ASTRONOMICAL observations, *BARYONS, *OSCILLATIONS, *COMPUTER simulation, *QUANTUM perturbations, *NONLINEAR theories, *WAVELENGTHS
Abstract

A shift of the baryon acoustic oscillation (BAO) scale to smaller values than predicted by linear theory was observed in simulations. In this paper, we try to provide an intuitive physical understanding of why this shift occurs, explaining in more pedagogical detail earlier perturbation theory calculations. We find that the shift is mainly due to the following physical effect. A measurement of the BAO scale is more sensitive to regions with long-wavelength overdensities than underdensities, because (due to nonlinear growth and bias) these overdense regions contain larger fluctuations and more tracers and hence contribute more to the total correlation function. In overdense regions the BAO scale shrinks because such regions locally behave as positively curved closed universes, and hence a smaller scale than predicted by linear theory is measured in the total correlation function. Other effects which also contribute to the shift are briefly discussed. We provide approximate analytic expressions for the nonlinear shift including a brief discussion of biased tracers and explain why reconstruction should entirely reverse the shift. Our expressions and findings are in agreement with simulation results, and confirm that nonlinear shifts should not be problematic for next-generation BAO measurements. [ABSTRACT FROM AUTHOR]

Published
2012
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