24 results on '"Staggs, Suzanne"'
Search Results
2. Report of the Dark Energy Task Force
- Author
-
Albrecht, Andreas, Bernstein, Gary, Cahn, Robert, Freedman, Wendy L., Hewitt, Jacqueline, Hu, Wayne, Huth, John, Kamionkowski, Marc, Kolb, Edward W., Knox, Lloyd, Mather, John C., Staggs, Suzanne, and Suntzeff, Nicholas B.
- Subjects
Astrophysics - Abstract
Dark energy appears to be the dominant component of the physical Universe, yet there is no persuasive theoretical explanation for its existence or magnitude. The acceleration of the Universe is, along with dark matter, the observed phenomenon that most directly demonstrates that our theories of fundamental particles and gravity are either incorrect or incomplete. Most experts believe that nothing short of a revolution in our understanding of fundamental physics will be required to achieve a full understanding of the cosmic acceleration. For these reasons, the nature of dark energy ranks among the very most compelling of all outstanding problems in physical science. These circumstances demand an ambitious observational program to determine the dark energy properties as well as possible., Comment: The Dark Energy Task Force (DETF) was established by the Astronomy and Astrophysics Advisory Committee (AAAC) and the High Energy Physics Advisory Panel (HEPAP) as a joint sub-committee to advise the Department of Energy, the National Aeronautics and Space Administration, and the National Science Foundation on future dark energy research
- Published
- 2006
3. First attempt at measuring the CMB cross-polarization
- Author
-
de Oliveira-Costa, Angelica, Tegmark, Max, Zaldarriaga, Matias, Barkats, Denis, Gundersen, Josh O., Hedman, Matt M., Staggs, Suzanne T., and Winstein, Bruce
- Subjects
Astrophysics - Abstract
We compute upper limits on CMB cross-polarization by cross-correlating the PIQUE and Saskatoon experiments. We also discuss theoretical and practical issues relevant to measuring cross-polarization and illustrate them with simulations of the upcoming BOOMERanG 2002 experiment. We present a method that separates all six polarization power spectra (TT, EE, BB, TE, TB, EB) without any other "leakage" than the familiar EE-BB mixing caused by incomplete sky coverage. Since E and B get mixed, one might expect leakage between TE and TB, between EE and EB and between BB and EB - our method eliminates this by preserving the parity symmetry under which TB and EB are odd and the other four power spectra are even., Comment: Polarization movies can be found at http://www.hep.upenn.edu/~angelica/polarization.html
- Published
- 2002
- Full Text
- View/download PDF
4. Astro2020 APC White Paper Project: The Simons Observatory
- Author
-
Abitbol, Maximilian H, Adachi, Shunsuke, Ade, Peter, Aguirre, James, Ahmed, Zeeshan, Aiola, Simone, Ali, Aamir, Alonso, David, Alvarez, Marcelo A, Arnold, Kam, Ashton, Peter, Atkins, Zachary, Austermann, Jason, Awan, Humna, Baccigalupi, Carlo, Baildon, Taylor, Lizancos, Anton Baleato, Barron, Darcy, Battaglia, Nick, Battye, Richard, Baxter, Eric, Bazarko, Andrew, Beall, James A, Bean, Rachel, Beck, Dominic, Beckman, Shawn, Beringue, Benjamin, Bhandarkar, Tanay, Bhimani, Sanah, Bianchini, Federico, Boada, Steven, Boettger, David, Bolliet, Boris, Bond, J. Richard, Borrill, Julian, Brown, Michael L, Bruno, Sarah Marie, Bryan, Sean, Calabrese, Erminia, Calafut, Victoria, Calisse, Paolo, Carron, Julien, Carl, Fred. M, Cayuso, Juan, Challinor, Anthony, Chesmore, Grace, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Clark, Susan, Clarke, Philip, Contaldi, Carlo, Coppi, Gabriele, Cothard, Nicholas F, Coughlin, Kevin, Coulton, Will, Crichton, Devin, Crowley, Kevin D, Crowley, Kevin T, Cukierman, Ari, D’Ewart, John M, D¨unner, Rolando, Haan, Tijmen de, Devlin, Mark, Dicker, Simon, Dober, Bradley, Duell, Cody J, Duff, Shannon, Duivenvoorden, Adri, Dunkley, Jo, Bouhargani, Hamza El, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Fergusson, James, Ferraro, Simone, Flux`a, Pedro, Freese, Katherine, Frisch, Josef C, Frolov, Andrei, Fuller, George, Galitzki, Nicholas, Gallardo, Patricio A, Ghersi, Jose Tomas Galvez, Gao, Jiansong, Gawiser, Eric, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Golec, Joseph, Gordon, Sam, Gralla, Megan, Green, Daniel, Grigorian, Arpi, Groh, John, Groppi, Chris, Guan, Yilun, Gudmundsson, Jon E, Halpern, Mark, Han, Dongwon, Hargrave, Peter, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hattori, Makoto, Haynes, Victor, Hazumi, Masashi, Healy, Erin, Henderson, Shawn W, Hensley, Brandon, Hervias-Caimapo, Carlos, Hill, Charles A, Hill, J. Colin, Hilton, Gene, Hilton, Matt, Hincks, Adam D, Hinshaw, Gary, Hlozek, Renee, Ho, Shirley, Ho, Shuay-Pwu Patty, Hoang, Thuong D, Hoh, Jonathan, Hotinli, Selim C, Huang, Zhiqi, Hubmayr, Johannes, Huffenberger, Kevin, Hughes, John P, Ijjas, Anna, Ikape, Margaret, Irwin, Kent, Jaffe, Andrew H, Jain, Bhuvnesh, Jeong, Oliver, Johnson, Matthew, Kaneko, Daisuke, Karpel, Ethan D, Katayama, Nobuhiko, Keating, Brian, Keskitalo, Reijo, Kisner, Theodore, Kiuchi, Kenji, Klein, Jeff, Knowles, Kenda, Kofman, Anna, Koopman, Brian, Kosowsky, Arthur, Krachmalnicoff, Nicoletta, Kusaka, Akito, LaPlante, Phil, Lashner, Jacob, Lee, Adrian, Lee, Eunseong, Lewis, Antony, Li, Yaqiong, Li, Zack, Limon, Michele, Linder, Eric, Liu, Jia, Lopez-Caraballo, Carlos, Louis, Thibaut, Lungu, Marius, Madhavacheril, Mathew, Mak, Daisy, Maldonado, Felipe, Mani, Hamdi, Mates, Ben, Matsuda, Frederick, Maurin, Loıc, Mauskopf, Phil, May, Andrew, McCallum, Nialh, McCarrick, Heather, McKenney, Chris, McMahon, Jeff, Meerburg, P. Daniel, Mertens, James, Meyers, Joel, Miller, Amber, Mirmelstein, Mark, Moodley, Kavilan, Moore, Jenna, Munchmeyer, Moritz, Munson, Charles, Murata, Masaaki, Naess, Sigurd, Namikawa, Toshiya, Nati, Federico, Navaroli, Martin, Newburgh, Laura, Nguyen, Ho Nam, Nicola, Andrina, Niemack, Mike, Nishino, Haruki, Nishinomiya, Yume, Orlowski-Scherer, John, Pagano, Luca, Partridge, Bruce, Perrotta, Francesca, Phakathi, Phumlani, Piccirillo, Lucio, Pierpaoli, Elena, Pisano, Giampaolo, Poletti, Davide, Puddu, Roberto, Puglisi, Giuseppe, Raum, Chris, Reichardt, Christian L, Remazeilles, Mathieu, Rephaeli, Yoel, Riechers, Dominik, Rojas, Felipe, Rotti, Aditya, Roy, Anirban, Sadeh, Sharon, Sakurai, Yuki, Salatino, Maria, Rao, Mayuri Sathyanarayana, Saunders, Lauren, Schaan, Emmanuel, Schmittfull, Marcel, Sehgal, Neelima, Seibert, Joseph, Seljak, Uros, Shellard, Paul, Sherwin, Blake, Shimon, Meir, Sierra, Carlos, Sievers, Jonathan, Sifon, Cristobal, Sikhosana, Precious, Silva-Feaver, Maximiliano, Simon, Sara M, Sinclair, Adrian, Smith, Kendrick, Sohn, Wuhyun, Sonka, Rita, Spergel, David, Spisak, Jacob, Staggs, Suzanne T, Stein, George, Stevens, Jason R, Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Takakura, Satoru, Teply, Grant, Thomas, Daniel B, Thorne, Ben, Thornton, Robert, Trac, Hy, Treu, Jesse, Tsai, Calvin, Tucker, Carole, Ullom, Joel, Vagnozzi, Sunny, Engelen, Alexander van, Lanen, Jeff Van, Winkle, Daniel D. Van, Vavagiakis, Eve M, Verg`es, Clara, Vissers, Michael, Wagoner, Kasey, Walker, Samantha, Wang, Yuhan, Ward, Jon, Westbrook, Ben, Whitehorn, Nathan, Williams, Jason, Williams, Joel, Wollack, Edward, Xu, Zhilei, Yasini, Siavash, Young, Edward, Yu, Byeonghee, Yu, Cyndia, Zago, Fernando, Zannoni, Mario, Zhang, Hezi, Zheng, Kaiwen, Zhu, Ningfeng, and Zonca, Andrea
- Subjects
Astrophysics - Abstract
The Simons Observatory (SO) is a ground-based cosmic microwave background (CMB) experiment sited on Cerro Toco in the Atacama Desert in Chile that promises to provide breakthrough discoveries in fundamental physics, cosmology, and astrophysics. Supported by the Simons Foundation, the Heising-Simons Foundation, and with contributions from collaborating institutions, SO will see first light in 2021 and start a five year survey in 2022. SO has 287 collaborators from 12 countries and 53 institutions, including 85 students and 90 postdocs. The SO experiment in its currently funded form (‘SO-Nominal’) consists of three 0.4 m Small Aperture Telescopes (SATs) and one 6 m Large Aperture Telescope (LAT). Optimized for minimizing systematic errors in polarization measurements at large angular scales, the SATs will perform a deep, degree-scale survey of 10% of the sky to search for the signature of primordial gravitational waves. The LAT will survey 40% of the sky with arc-minute resolution. These observations will measure (or limit) the sum of neutrino masses, search for light relics, measure the early behavior of Dark Energy, and refine our understanding of the intergalactic medium, clusters and the role of feedback in galaxy formation. With up to ten times the sensitivity and five times the angular resolution of the Planck satellite, and roughly an order of magnitude increase in mapping speed over currently operating (“Stage 3”) experiments, SO will measure the CMB temperature and polarization fluctuations to exquisite precision in six frequency bands from 27 to 280 GHz. SO will rapidly advance CMB science while informing the design of future observatories such as CMB-S4. Construction of SO-Nominal is fully funded, and operations and data analysis are funded for part of the planned five-year observations. We will seek federal funding to complete the observations and analysis of SO-Nominal, at the $25M level. The SO has a low risk and cost efficient upgrade path – the 6 m LAT can accommodate almost twice the baseline number of detectors and the SATs can be duplicated at low cost. We will seek funding at the $75M level for an expansion of the SO (‘SO-Enhanced’) that fills the remaining focal plane in the LAT, adds three SATs, and extends operations by five years, substantially improving our science return. By this time SO may be operating as part of the larger CMB-S4 project. This white paper summarizes and extends material presented in, which describes the science goals of SO-Nominal, and which describe the instrument design.
- Published
- 2019
5. 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
6. Two-Season Atacama Cosmology Telescope Polarimeter Lensing Power Spectrum
- Author
-
Shewin, Blake D, van Engelen, Alexander, Sehgal, Neelima, Madhavacheril, Mathew, Addison, Graeme E, Aiola, Simone, Allison, Rupert, Battaglia, Nicholas, Becker, Daniel T, Beall, James A, Bond, J. Richard, Calabrese, Ermini, Datta, Rahul, Devlin, Mark J, Dunner, Rolando, Dunkley, Joanna, Fox, Anna E, Gallardo, Patricio, Halpern, Mark, Hasselfield, Matthew, Henderson, Shawn, Hill, J. Colin, Hilton, Gene C, Hubmayr, Johannes, Hughes, John P, Hincks, Adam D, Hlozek, Renee, Huffenberger, Kevin M, Koopman, Brian, Kosowsky, Arthur, Louis, Thibaut, Maurin, Loic, McMahon, Jeff, Moodley, Kavilan, Naess, Sigurd, Nati, Federico, Newburgh, Laura, Niemack, Michael D, Page, Lyman A, Sievers, Jonathan, Spergel, David N, Staggs, Suzanne T, Thornton, Robert J, Van Lanen, Jeff, Vavagiakis, Eve, and Wollack, Edward J
- Subjects
Astrophysics - Abstract
We report a measurement of the power spectrum of cosmic microwave background (CMB) lensing from two seasons of Atacama Cosmology Telescope polarimeter (ACTPol) CMB data. The CMB lensing power spectrum is extracted from both temperature and polarization data using quadratic estimators. We obtain results that are consistent with the expectation from the best-fit Planck CDM model over a range of multipoles L 80-2100, with an amplitude of lensing A(sub lens) = 1.06 +/- 0.15 stat +/- 0.06 sys relative to Planck. Our measurement of the CMB lensing power spectrum gives sigma 8 omega m(sup 0.25) = 0.643 +/- 0.054; including baryon acoustic oscillation scale data, we constrain the amplitude of density fluctuations to be sigma 8 = 0.831 +/- 0.053. We also update constraints on the neutrino mass sum. We verify our lensing measurement with a number of null tests and systematic checks, finding no evidence of significant systematic errors. This measurement relies on a small fraction of the ACTPol data already taken; more precise lensing results can therefore be expected from the full ACTPol data set.
- Published
- 2017
- Full Text
- View/download PDF
7. 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
- Full Text
- View/download PDF
8. 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
- Full Text
- View/download PDF
9. AlMn Transition Edge Sensors for Advanced ACTPol
- Author
-
Li, Dale, Austermann, Jason E, Beall, James A, Tucker, Daniel T, Duff, Shannon M, Gallardo, Patricio A, Henderson, Shawn W, Hilton, Gene C, Ho, Shuay-Pwu, Hubmayr, Johannes, Koopman, Brian J, McMahon, Jeffrey J, Nati, Federico, Niemack, Michael D, Pappas, Christine G, Salatino, Maria, Schmitt, Benjamin L, Simon, Sara M, Staggs, Suzanne T, Van Lanen, Jeff, Ward, Jonathan T, and Wollack, Edward J
- Subjects
Astrophysics - Abstract
Advanced ACTPol (Adv ACT) will use an array of multichroic polarization sensitive AIMn transition edge sensor (TES) bolometers read out through time-division multiplexing. Aluminum doped with a low concentration of manganese can be deposited to a bulk film thickness for a more reliable superconducting critical temperature uniformity compared to thin bilayers. To build the TES, the AlMn alloy is deposited, over Nb wiring, to a specific thickness to set the TES normal resistance. The doping concentration of manganese coarsely defines the TES critical temperature, while a fine tuning is achieved by heating the deposited film to a specific temperature. The TES island is connected to the thermal bath via four silicon-nitride membranes, where their geometry defines the thermal conductance to the temperature of the bath. Lastly, the TES heat capacity is increased by addition of PdAu electrically connected to the AlMn film. Designs and performance characteristics of these AlMn TESs are presented for use in AdvACT.
- Published
- 2016
- Full Text
- View/download PDF
10. Evidence for the Thermal Sunyaev Zeldovich Effect Associated with Quasar Feedback
- Author
-
Crichton, Devin, Gralla, Megan B, Hall, Kirsten, Marriage, Tobias A, Zakamska, Nadia L, Battaglia, Nick, Bond, J. Richard, Devlin, Mark J, Hill, J. Colin, Hilton, Matt, Hincks, Adam D, Huffenberger, Kevin M, Hughes, John P, Kosowsky, Arthur, Moodley, Kavilan, Niemack, Michael D, Page, Lyman A, Partridge, Bruce, Sievers, Jonathan L, Sifon, Cristobal, Staggs, Suzanne T, Viero, Marco P, and Wollack, Edward J
- Subjects
Astrophysics - Abstract
Using a radio-quiet subsample of the Sloan Digital Sky Survey spectroscopic quasar catalogue, spanning redshifts 0.5-3.5, we derive the mean millimetre and far-infrared quasar spectral energy distributions (SEDs) via a stacking analysis of Atacama Cosmology Telescope and Herschel-Spectral and Photometric Imaging REceiver data. We constrain the form of the far-infrared emission and find 3 sigma-4 sigma evidence for the thermal Sunyaev-Zel'dovich (SZ) effect, characteristic of a hot ionized gas component with thermal energy (6.2 plus or minus 1.7) × 10 (exp 60) erg. This amount of thermal energy is greater than expected assuming only hot gas in virial equilibrium with the dark matter haloes of (1-5) × 10(exp 12) h(exp −1) solar mass that these systems are expected to occupy, though the highest quasar mass estimates found in the literature could explain a large fraction of this energy. Our measurements are consistent with quasars depositing up to (14.5 +/- 3.3)tau (sub 8)(exp -1) per cent of their radiative energy into their circumgalactic environment if their typical period of quasar activity is tau(sub 8) x 108 yr. For high quasar host masses, approximately 10(exp 13) h(exp −1) solar mass, this percentage will be reduced. Furthermore, the uncertainty on this percentage is only statistical and additional systematic uncertainties enter at the 40 per cent level. The SEDs are dust dominated in all bands and we consider various models for dust emission. While sufficiently complex dust models can obviate the SZ effect, the SZ interpretation remains favoured at the 3 sigma-4 sigma level for most models.
- Published
- 2016
- Full Text
- View/download PDF
11. 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
- Full Text
- View/download PDF
12. The Atacama Cosmology Telescope: Dusty Star-Forming Galaxies and Active Galactic Nuclei in the Southern Survey
- Author
-
Marsden, Danica, Gralla, Megan, Marriage, Tobias A, Switzer, Eric R, Partridge, Bruce, Massardi, Marcella, Morales, Gustavo, Addison, Graeme, Bond, J. Richard, Crighton, Devin, Das, Sudeep, Devlin, Mark, Dunner, Rolando, Hajian, Amir, Hilton, Matt, Hincks, Adam, Hughes, John P, Irwin, Kent, Kosowsky, Arthur, Menanteau, Felipe, Moodley, Kavilan, Niemack, Michael, Page, Lyman, Reese, Erik D, Schmitt, Benjamin, Sehgal, Neelima, Sievers, Johnathan, Staggs, Suzanne, Swetz, Daniel, Thornton, Robert, and Wollack, Edward
- Subjects
Astronomy ,Astrophysics - Abstract
We present a catalogue of 191 extragalactic sources detected by the Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern survey. Flux densities span 14 -1700 mJy, and we use source spectral indices derived using ACT-only data to divide our sources into two subpopulations: 167 radio galaxies powered by central active galactic nuclei (AGN) and 24 dusty star-forming galaxies (DSFGs). We cross-identify 97 per cent of our sources (166 of the AGN and 19 of the DSFGs) with those in currently available catalogues. When combined with flux densities from the Australia Telescope 20 GHz survey and follow-up observations with the Australia Telescope Compact Array, the synchrotron-dominated population is seen to exhibit a steepening of the slope of the spectral energy distribution from 20 to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated source population has a median spectral index, A(sub 148-218), of 3.7 (+0.62 or −0.86), and includes both local galaxies and sources with redshift around 6. Dusty sources with no counterpart in existing catalogues likely belong to a recently discovered subpopulation of DSFGs lensed by foreground galaxies or galaxy groups.
- Published
- 2014
- Full Text
- View/download PDF
13. 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
- Full Text
- View/download PDF
14. The Atacama Cosmology Telescope: Beam Measurements and the Microwave Brightness Temperatures of Uranus and Saturn
- Author
-
Hasselfield, Matthew, Moodley, Kavilan, Bond, J. Richard, Das, Sudeep, Devlin, Mark J, Dunkley, Joanna, Dunner, Rolando, Fowler, Joseph W, Gallardo, Patricio, Gralla, Megan B, Hajian, Amir, Halpern, Mark, Hincks, Adam D, Marriage, Tobias A, Marsden, Danica, Niemack, Michael D, Nolta, Michael R, Page, Lyman A, Partridge, Bruce, Schmitt, Benjamin L, Sehgal, Neelima, Sievers, Jon, Staggs, Suzanne T, Swetz, Daniel S, Switzer, Eric R, and Wollack, Edward J
- Subjects
Astrophysics - Abstract
We describe the measurement of the beam profiles and window functions for the Atacama Cosmology Telescope (ACT), which operated from 2007 to 2010 with kilopixel bolometer arrays centered at 148, 218, and 277 GHz. Maps of Saturn are used to measure the beam shape in each array and for each season of observations. Radial profiles are transformed to Fourier space in a way that preserves the spatial correlations in the beam uncertainty to derive window functions relevant for angular power spectrum analysis. Several corrections are applied to the resulting beam transforms, including an empirical correction measured from the final cosmic microwave background (CMB) survey maps to account for the effects of mild pointing variation and alignment errors. Observations of Uranus made regularly throughout each observing season are used to measure the effects of atmospheric opacity and to monitor deviations in telescope focus over the season. Using the WMAP-based calibration of the ACT maps to the CMB blackbody, we obtain precise measurements of the brightness temperatures of the Uranus and Saturn disks at effective frequencies of 149 and 219 GHz. For Uranus we obtain thermodynamic brightness temperatures T(149/U) = 106.7 +/- 2.2 K and T(219/U) = 100.1 +/- 3.1 K. For Saturn, we model the effects of the ring opacity and emission using a simple model and obtain resulting (unobscured) disk temperatures of T(149/S) = 137.3 +/- 3.2 K and T(219/S) = 137.3 +/- 4.7 K.
- Published
- 2013
- Full Text
- View/download PDF
15. 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
- Full Text
- View/download PDF
16. Power-Law Template for Infrared Point-Source Clustering
- Author
-
Addison, Graeme E, Dunkley, Joanna, Hajian, Amir, Viero, Marco, Bond, J. Richard, Das, Sudeep, Devlin, Mark J, Halpern, Mark, Hincks, Adam D, Hlozek, Renee, Marriage, Tobias A, Moodley, Kavilan, Page, Lyman A, Reese, Erik D, Scott, Douglas, Spergel, David N, Staggs, Suzanne T, and Wollack, Edward
- Subjects
Astrophysics - Abstract
We perform a combined fit to angular power spectra of unresolved infrared (IR) point sources from the Planck satellite (at 217, 353, 545, and 857 GHz, over angular scales 100 approx < l approx < 2200), the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST; 250, 350, and 500 micron; 1000 approx < l approx < 9000), and from correlating BLAST and Atacama Cosmology Telescope (ACT; 148 and 218 GHz) maps. We find that the clustered power over the range of angular scales and frequencies considered is well fitted by a simple power law of the form C(sup clust)(sub l) varies as l (sub −n) with n = 1.25 +/- 0.06. While the IR sources are understood to lie at a range of redshifts, with a variety of dust properties, we find that the frequency dependence of the clustering power can be described by the square of a modified blackbody, ν(sup Beta)B(ν, T(sub eff) ), with a single emissivity index Beta = 2.20 +/- 0.07 and effective temperature T(sub eff) = 9.7 K. Our predictions for the clustering amplitude are consistent with existing ACT and South Pole Telescope results at around 150 and 220 GHz, as is our prediction for the effective dust spectral index, which we find to be alpha(sub 150-220) = 3.68 +/- 0.07 between 150 and 220 GHz. Our constraints on the clustering shape and frequency dependence can be used to model the IR clustering as a contaminant in cosmic microwave background anisotropy measurements. The combined Planck and BLAST data also rule out a linear bias clustering model.
- Published
- 2012
- Full Text
- View/download PDF
17. The Atacama Cosmology Telescope: ACT-CL J0102-4915 'EL GORDO', A Massive Merging Cluster at Redshift 0.87
- Author
-
Menanteau, Felipe, Hughes, John P, Sifon, Cristobal, Hilton, Matt, Gonzalez, Jorge, Infante, Leopoldo, Barrientos, L. Felipe, Baker, Andrew J, Bond, John R, Das, Sudeep, Devlin, Mark J, Dunkley, Joanna, Hajian, Amir, Hincks, Adam D, Kosowsky, Arthur, Marsden, Danica, Marriage, Tobias A, Moodley, Kavilan, Niemack, Michael D, Nolta, Michael R, Page, Lyman A, Reese, Erik D, Sehgal, Neelima, Seivers, Jon, Spergel, David N, Staggs, Suzanne T, and Wollack, Edward
- Subjects
Astronomy ,Astrophysics - Abstract
We present a detailed analysis from new multi-wavelength observations of the exceptional galaxy cluster ACT-CL J0102−4915, likely the most massive, hottest, most X-ray luminous and brightest Sunyaev-Zel'dovich (SZ) effect cluster known at redshifts greater than 0.6. The Atacama Cosmology Telescope (ACT) collaboration discovered ACT-CL J0102−4915 as the most significant Sunyaev-Zeldovich (SZ) decrement in a sky survey area of 755 square degrees. Our VLT/FORS2 spectra of 89 member galaxies yield a cluster redshift, z = 0.870, and velocity dispersion, sigma(sub gal) = 1321+/-106 km s−1. Our Chandra observations reveal a hot and X-ray luminous system with an integrated temperature of T(sub X) = 14.5+/-1.0 keV and 0.5-2.0 keV band luminosity of L(sub X) = (2.19+/-0.11)×10(sup 45) h(sup −2)(sub 70) erg s−1. We obtain several statistically consistent cluster mass estimates; using empirical mass scaling relations with velocity dispersion, X-ray Y(sub X), and integrated SZ distortion, we estimate a cluster mass of M(sub 200a) = (2.16+/-0.32)×1015 h(sup −1)(sub 70) solar mass. We constrain the stellar content of the cluster to be less than 1% of the total mass, using Spitzer IRAC and optical imaging. The Chandra and VLT/FORS2 optical data also reveal that ACT-CL J0102−4915 is undergoing a major merger between components with a mass ratio of approximately 2 to 1. The X-ray data show significant temperature variations from a low of 6.6+/-0.7 keV at the merging low-entropy, high-metallicity, cool core to a high of 22+/-6 keV. We also see a wake in the X-ray surface brightness and deprojected gas density caused by the passage of one cluster through the other. Archival radio data at 843 MHz reveal diffuse radio emission that, if associated with the cluster, indicates the presence of an intense double radio relic, hosted by the highest redshift cluster yet. ACT-CL J0102−4915 is possibly a high-redshift analog of the famous Bullet Cluster. Such a massive cluster at this redshift is rare, although consistent with the standard ΛCDM cosmology in the lower part of its allowed mass range. Massive, highredshift mergers like ACT-CL J0102−4915 are unlikely to be reproduced in the current generation of numerical N-body cosmological simulations.
- Published
- 2012
18. Power-Law Template for IR Point Source Clustering
- Author
-
Addison, Graeme E, Dunkley, Joanna, Hajian, Amir, Viero, Marco, Bond, J. Richard, Das, Sudeep, Devlin, Mark, Halpern, Mark, Hincks, Adam, Hlozek, Renee, Marriage, Tobias A, Moodley, Kavilan, Page, Lyman A, Reese, Erik D, Scott, Douglass, Spergel, David N, Staggs,Suzanne T, and Wollack, Edward
- Subjects
Astrophysics - Abstract
We perform a combined fit to angular power spectra of unresolved infrared (IR) point sources from the Planck satellite (at 217,353,545 and 857 GHz, over angular scales 100 < I < 2200), the Balloonborne Large-Aperture Submillimeter Telescope (BLAST; 250, 350 and 500 microns; 1000 < I < 9000), and from correlating BLAST and Atacama Cosmology Telescope (ACT; 148 and 218 GHz) maps. We find that the clustered power over the range of angular scales and frequencies considered is well fit by a simple power law of the form C_l\propto I(sup -n) with n = 1.25 +/- 0.06. While the IR sources are understood to lie at a range of redshifts, with a variety of dust properties, we find that the frequency dependence of the clustering power can be described by the square of a modified blackbody, nu(sup beta) B(nu,T_eff), with a single emissivity index beta = 2.20 +/- 0.07 and effective temperature T_eff= 9.7 K. Our predictions for the clustering amplitude are consistent with existing ACT and South Pole Telescope results at around 150 and 220 GHz, as is our prediction for the effective dust spectral index, which we find to be alpha_150-220 = 3.68 +/- 0.07 between 150 and 220 GHz. Our constraints on the clustering shape and frequency dependence can be used to model the IR clustering as a contaminant in Cosmic Microwave Background anisotropy measurements. The combined Planck and BLAST data also rule out a linear bias clustering model.
- Published
- 2011
19. 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
20. Atacama Cosmology Telescope: Combined kinematic and thermal Sunyaev-Zel’dovich measurements from BOSS CMASS and LOWZ halos
- Author
-
Schaan, Emmanuel, Ferraro, Simone, Amodeo, Stefania, Battaglia, Nick, Aiola, Simone, Austermann, Jason E., Beall, James A., Bean, Rachel, Becker, Daniel T., Bond, Richard J., Calabrese, Erminia, Calafut, Victoria, Choi, Steve K., Denison, Edward V., Devlin, Mark J., Duff, Shannon M., Duivenvoorden, Adriaan J., Dunkley, Jo, Dünner, Rolando, Gallardo, Patricio A., Guan, Yilun, Han, Dongwon, Hill, J. Colin, Hilton, Gene C., Hilton, Matt, Hložek, Renée, Hubmayr, Johannes, Huffenberger, Kevin M., Hughes, John P., Koopman, Brian J., MacInnis, Amanda, McMahon, Jeff, Madhavacheril, Mathew S., Moodley, Kavilan, Mroczkowski, Tony, Naess, Sigurd, Nati, Federico, Newburgh, Laura B., Niemack, Michael D., Page, Lyman A., Partridge, Bruce, Salatino, Maria, Sehgal, Neelima, Schillaci, Alessandro, Sifón, Cristóbal, Smith, Kendrick M., Spergel, David N., Staggs, Suzanne, Storer, Emilie R., Trac, Hy, Page, A., Ullom, Joel N., Van Lanen, Jeff, R. Vale, Leila, van Engelen, Alexander, Vargas Magaña, Mariana, M. Vavagiakis, Eve, Wollack, Edward J., Xu, Zhilei, Schaan, E, Ferraro, S, Amodeo, S, Battaglia, N, Aiola, S, Austermann, J, Beall, J, Bean, R, Becker, D, Bond, R, Calabrese, E, Calafut, V, Choi, S, Denison, E, Devlin, M, Duff, S, Duivenvoorden, A, Dunkley, J, Dunner, R, Gallardo, P, Guan, Y, Han, D, Hill, J, Hilton, G, Hilton, M, Hlozek, R, Hubmayr, J, Huffenberger, K, Hughes, J, Koopman, B, Macinnis, A, Mcmahon, J, Madhavacheril, M, Moodley, K, Mroczkowski, T, Naess, S, Nati, F, Newburgh, L, Niemack, M, Page, L, Partridge, B, Salatino, M, Sehgal, N, Schillaci, A, Sifon, C, Smith, K, Spergel, D, Staggs, S, Storer, E, Trac, H, Ullom, J, Van Lanen, J, Vale, L, Van Engelen, A, Magana, M, Vavagiakis, E, Wollack, E, and Xu, Z
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,astro-ph.GA ,Cosmic microwave background ,FOS: Physical sciences ,High resolution ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,CMB ,01 natural sciences ,Atomic ,symbols.namesake ,Particle and Plasma Physics ,0103 physical sciences ,Nuclear ,Planck ,010306 general physics ,Astrophysics::Galaxy Astrophysics ,Physics ,Quantum Physics ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Molecular ,Astrophysics - Astrophysics of Galaxies ,Nuclear & Particles Physics ,Redshift ,Galaxy ,13. Climate action ,Astrophysics of Galaxies (astro-ph.GA) ,Atacama Cosmology Telescope ,symbols ,astro-ph.CO ,Halo ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The scattering of cosmic microwave background (CMB) photons off the free-electron gas in galaxies and clusters leaves detectable imprints on high resolution CMB maps: the thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ respectively). We use combined microwave maps from the Atacama Cosmology Telescope (ACT) DR5 and Planck in combination with the CMASS and LOWZ galaxy catalogs from the Baryon Oscillation Spectroscopic Survey (BOSS DR10 and DR12), to study the gas associated with these galaxy groups. Using individual reconstructed velocities, we perform a stacking analysis and reject the no-kSZ hypothesis at 6.5$\sigma$, the highest significance to date. This directly translates into a measurement of the electron number density profile, and thus of the gas density profile. Despite the limited signal to noise, the measurement shows at high significance that the gas density profile is more extended than the dark matter density profile, for any reasonable baryon abundance (formally $>90\sigma$ for the cosmic baryon abundance). We simultaneously measure the tSZ signal, i.e. the electron thermal pressure profile of the same CMASS objects, and reject the no-tSZ hypothesis at 10$\sigma$. We combine tSZ and kSZ measurements to estimate the electron temperature to 20% precision in several aperture bins, and find it comparable to the virial temperature. In a companion paper, we analyze these measurements to constrain the gas thermodynamics and the properties of feedback inside galaxy groups. We present the corresponding LOWZ measurements in this paper, ruling out a null kSZ (tSZ) signal at 2.9 (13.9)$\sigma$, and leave their interpretation to future work. Our stacking software ThumbStack is publicly available at https://github.com/EmmanuelSchaan/ThumbStack and directly applicable to future Simons Observatory and CMB-S4 data., Comment: Accepted in Physical Review D, Editors' Suggestion
- Full Text
- View/download PDF
21. The Simons Observatory: science goals and forecasts
- Author
-
Ade, Peter, Aguirre, James, Ahmed, Zeeshan, Aiola, Simone, Ali, Aamir, Alonso, David, Alvarez, Marcelo A., Arnold, Kam, Ashton, Peter, Austermann, Jason, Awan, Humna, Baccigalupi, Carlo, Baildon, Taylor, Barron, Darcy, Battaglia, Nick, Battye, Richard, Baxter, Eric, Bazarko, Andrew, Beall, James A., Bean, Rachel, Beck, Dominic, Beckman, Shawn, Beringue, Benjamin, Bianchini, Federico, Boada, Steven, Boettger, David, Richard Bond, J., Borrill, Julian, Brown, Michael L., Bruno, Sarah Marie, Bryan, Sean, Calabrese, Erminia, Calafut, Victoria, Calisse, Paolo, Carron, Julien, Challinor, Anthony, Chesmore, Grace, Chinone, Yuji, Chluba, Jens, Cho, Hsiao-Mei Sherry, Choi, Steve, Coppi, Gabriele, Cothard, Nicholas F., Coughlin, Kevin, Crichton, Devin, Crowley, Kevin D., Crowley, Kevin T., Cukierman, Ari, D`Ewart, Mitch, Dünner, Rolando, de Haan, Tijmen, Devlin, Mark, Dicker, Simon, DIDIER, JOY, Dobbs, Matt, Dober, Bradley, Duell, Cody, Duff, Shannon, Duivenvoorden, Adri, Dunkley, Jo, Dusatko, John, Errard, Josquin, Fabbian, Giulio, Feeney, Stephen, Ferraro, Simone, Fluxà, Pedro, Freese, Katherine, Frisch, Josef, Frolov, Andrei, Fuller, George, Fuzia, Brittany, Galitzki, Nicholas, Gallardo, Patricio A., Galvez Ghersi, Jose Tomas, Gao, Jiansong, Gawiser, Eric, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Golec, Joseph, Gordon, Sam, Gralla, Megan, Green, Daniel, Grigorian, Arpi, Groh, John, Groppi, Chris, Guan, Yilun, Gudmundsson, Jon E., Han, Dongwon, Hargrave, Peter, Hasegawa, Masaya, Hasselfield, Matthew, Hattori, Makoto, Haynes, Victor, Hazumi, Masashi, He, Yizhou, Healy, Erin, Henderson, Shawn, Hervias-Caimapo, Carlos, Hill, Charles A., Colin Hill, J., HILTON, GENE, Hilton, Matt, Hincks, Adam D., Hinshaw, Gary, Hložek, Renée, Ho, Shirley, Ho, Shuay-Pwu Patty, Howe, Logan, Huang, Zhiqi, Hubmayr, Johannes, Huffenberger, Kevin, Hughes, John P., Ijjas, Anna, Ikape, Margaret, Irwin, Kent, Jaffe, Andrew H., Jain, Bhuvnesh, Jeong, Oliver, Kaneko, Daisuke, Karpel, Ethan, Katayama, Nobuhiko, Keating, Brian, Kernasovski, Sarah, Keskitalo, Reijo, Kisner, Theodore, Kiuchi, Kenji, Klein, Jeff, Knowles, Kenda, Koopman, Brian, Kosowsky, Arthur, Krachmalnicoff, Nicoletta, Kuenstner, Stephen, Kuo, Chao-Lin, Kusaka, Akito, Lashner, Jacob, Lee, Adrian, Lee, Eunseong, Leon, David, Leung, Jason S.-Y., Lewis, Antony, Li, Yaqiong, Li, Zack, Limon, Michele, Linder, Eric, Lopez-Caraballo, Carlos, Louis, Thibaut, Lowry, Lindsay, Lungu, Marius, Madhavacheril, Mathew, Mak, Daisy, Maldonado, Felipe, Mani, Hamdi, Mates, Ben, Matsuda, Frederick, Maurin, Loïc, Mauskopf, Phil, May, Andrew, McCallum, Nialh, McKenney, Chris, McMahon, Jeff, Daniel Meerburg, P., Meyers, Joel, Miller, Amber, Mirmelstein, Mark, Moodley, Kavilan, Munchmeyer, Moritz, Munson, Charles, Naess, Sigurd, Nati, Federico, Navaroli, Martin, Newburgh, Laura, Nguyen, Ho Nam, Niemack, Mike, Nishino, Haruki, Orlowski-Scherer, John, Page, Lyman, Partridge, Bruce, Peloton, Julien, Perrotta, Francesca, Piccirillo, Lucio, Pisano, Giampaolo, Poletti, Davide, Puddu, Roberto, Puglisi, Giuseppe, Raum, Chris, Reichardt, Christian L., Remazeilles, Mathieu, Rephaeli, Yoel, Riechers, Dominik, Rojas, Felipe, Roy, Anirban, Sadeh, Sharon, Sakurai, Yuki, Salatino, Maria, Rao, Mayuri Sathyanarayana, Schaan, Emmanuel, Schmittfull, Marcel, Sehgal, Neelima, Seibert, Joseph, Seljak, Uros, Sherwin, Blake, Shimon, Meir, Sierra, Carlos, Sievers, Jonathan, Sikhosana, Precious, Silva-Feaver, Max, Simon, Sara M., Sinclair, Adrian, Siritanasak, Praween, Smith, Kendrick, Smith, Steve, Spergel, David, Staggs, Suzanne, Stein, George, Stevens, Jason R., Stompor, Radek, Suzuki, Aritoki, Tajima, Osamu, Takakura, Satoru, Teply, Grant, Thomas, Daniel B., Thorne, Ben, Thornton, Robert, Trac, Hy, Tsai, Calvin, Tucker, Carole, Ullom, Joel, Vagnozzi, Sunny, van Engelen, Alexander, Van Lanen, Jeff, van Winkle, Dan, Vavagiakis, Eve M., Vergès, Clara, Vissers, Michael, Wagoner, Kasey, Walker, Samantha, Ward, Jon, WESTBROOK, BEN, Whitehorn, Nathan, Williams, Jason, Williams, Joel, Wollack, Edward J., Xu, Zhilei, Ye, Jiani, Yu, Byeonghee, Yu, Cyndria, Zago, Fernando, Zhang, Hezi, Zhu, Ningfeng, 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 spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Simons Observatory, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), ANR-17-CE31-0022,BxB,Champs B interstellaires et modes B de l'inflation(2017), Ade, P, Aguirre, J, Ahmed, Z, Aiola, S, Ali, A, Alonso, D, Alvarez, M, Arnold, K, Ashton, P, Austermann, J, Awan, H, Baccigalupi, C, Baildon, T, Barron, D, Battaglia, N, Battye, R, Baxter, E, Bazarko, A, Beall, J, Bean, R, Beck, D, Beckman, S, Beringue, B, Bianchini, F, Boada, S, Boettger, D, Bond, J, Borrill, J, Brown, M, Bruno, S, Bryan, S, Calabrese, E, Calafut, V, Calisse, P, Carron, J, Challinor, A, Chesmore, G, Chinone, Y, Chluba, J, Cho, H, Choi, S, Coppi, G, Cothard, N, Coughlin, K, Crichton, D, Crowley, K, Cukierman, A, D'Ewart, J, Dünner, R, de Haan, T, Devlin, M, Dicker, S, Didier, J, Dobbs, M, Dober, B, Duell, C, Duff, S, Duivenvoorden, A, Dunkley, J, Dusatko, J, Errard, J, Fabbian, G, Feeney, S, Ferraro, S, Fluxà, P, Freese, K, Frisch, J, Frolov, A, Fuller, G, Fuzia, B, Galitzki, N, Gallardo, P, Ghersi, J, Gao, J, Gawiser, E, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Golec, J, Gordon, S, Gralla, M, Green, D, Grigorian, A, Groh, J, Groppi, C, Guan, Y, Gudmundsson, J, Han, D, Hargrave, P, Hasegawa, M, Hasselfield, M, Hattori, M, Haynes, V, Hazumi, M, He, Y, Healy, E, Henderson, S, Hervias-Caimapo, C, Hill, C, Hill, J, Hilton, G, Hilton, M, Hincks, A, Hinshaw, G, Hložek, R, Ho, S, Howe, L, Huang, Z, Hubmayr, J, Huffenberger, K, Hughes, J, Ijjas, A, Ikape, M, Irwin, K, Jaffe, A, Jain, B, Jeong, O, Kaneko, D, Karpel, E, Katayama, N, Keating, B, Kernasovskiy, S, Keskitalo, R, Kisner, T, Kiuchi, K, Klein, J, Knowles, K, Koopman, B, Kosowsky, A, Krachmalnicoff, N, Kuenstner, S, Kuo, C, Kusaka, A, Lashner, J, Lee, A, Lee, E, Leon, D, Leung, J, Lewis, A, Li, Y, Li, Z, Limon, M, Linder, E, Lopez-Caraballo, C, Louis, T, Lowry, L, Lungu, M, Madhavacheril, M, Mak, D, Maldonado, F, Mani, H, Mates, B, Matsuda, F, Maurin, L, Mauskopf, P, May, A, Mccallum, N, Mckenney, C, Mcmahon, J, Meerburg, P, Meyers, J, Miller, A, Mirmelstein, M, Moodley, K, Munchmeyer, M, Munson, C, Naess, S, Nati, F, Navaroli, M, Newburgh, L, Nguyen, H, Niemack, M, Nishino, H, Orlowski-Scherer, J, Page, L, Partridge, B, Peloton, J, Perrotta, F, Piccirillo, L, Pisano, G, Poletti, D, Puddu, R, Puglisi, G, Raum, C, Reichardt, C, Remazeilles, M, Rephaeli, Y, Riechers, D, Rojas, F, Roy, A, Sadeh, S, Sakurai, Y, Salatino, M, Rao, M, Schaan, E, Schmittfull, M, Sehgal, N, Seibert, J, Seljak, U, Sherwin, B, Shimon, M, Sierra, C, Sievers, J, Sikhosana, P, Silva-Feaver, M, Simon, S, Sinclair, A, Siritanasak, P, Smith, K, Smith, S, Spergel, D, Staggs, S, Stein, G, Stevens, J, Stompor, R, Suzuki, A, Tajima, O, Takakura, S, Teply, G, Thomas, D, Thorne, B, Thornton, R, Trac, H, Tsai, C, Tucker, C, Ullom, J, Vagnozzi, S, Engelen, A, Lanen, J, Winkle, D, Vavagiakis, E, Vergès, C, Vissers, M, Wagoner, K, Walker, S, Ward, J, Westbrook, B, Whitehorn, N, Williams, J, Wollack, E, Xu, Z, Yu, B, Yu, C, Zago, F, Zhang, H, Zhu, N, 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 High-Energy Frontier
- Subjects
CMBR polarisation ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,media_common.quotation_subject ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,7. Clean energy ,law.invention ,Telescope ,symbols.namesake ,Settore FIS/05 - Astronomia e Astrofisica ,Observatory ,law ,0103 physical sciences ,CMBR experiments ,Cosmological parameters from CMBR ,Astronomy and Astrophysics ,Planck ,Reionization ,QC ,Astrophysics::Galaxy Astrophysics ,media_common ,Physics ,010308 nuclear & particles physics ,Settore FIS/05 ,Astrophysics::Instrumentation and Methods for Astrophysics ,cosmological parameters from CMBR ,Nuclear & Particles Physics ,Atomic, Molecular, Nuclear, Particle and Plasma Physics ,Gravitational lens ,13. Climate action ,Sky ,symbols ,astro-ph.CO ,Neutrino ,Cosmology and Nongalactic Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astronomical and Space Sciences ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The Simons Observatory (SO) is a new cosmic microwave background experiment being built on Cerro Toco in Chile, due to begin observations in the early 2020s. We describe the scientific goals of the experiment, motivate the design, and forecast its performance. SO will measure the temperature and polarization anisotropy of the cosmic microwave background in six frequency bands: 27, 39, 93, 145, 225 and 280 GHz. The initial configuration of SO will have three small-aperture 0.5-m telescopes (SATs) and one large-aperture 6-m telescope (LAT), with a total of 60,000 cryogenic bolometers. Our key science goals are to characterize the primordial perturbations, measure the number of relativistic species and the mass of neutrinos, test for deviations from a cosmological constant, improve our understanding of galaxy evolution, and constrain the duration of reionization. The SATs will target the largest angular scales observable from Chile, mapping ~10% of the sky to a white noise level of 2 $\mu$K-arcmin in combined 93 and 145 GHz bands, to measure the primordial tensor-to-scalar ratio, $r$, at a target level of $\sigma(r)=0.003$. The LAT will map ~40% of the sky at arcminute angular resolution to an expected white noise level of 6 $\mu$K-arcmin in combined 93 and 145 GHz bands, overlapping with the majority of the LSST sky region and partially with DESI. With up to an order of magnitude lower polarization noise than maps from the Planck satellite, the high-resolution sky maps will constrain cosmological parameters derived from the damping tail, gravitational lensing of the microwave background, the primordial bispectrum, and the thermal and kinematic Sunyaev-Zel'dovich effects, and will aid in delensing the large-angle polarization signal to measure the tensor-to-scalar ratio. The survey will also provide a legacy catalog of 16,000 galaxy clusters and more than 20,000 extragalactic sources., Comment: This paper presents an overview of the Simons Observatory science goals, details about the instrument will be presented in a companion paper. The author contribution to this paper is available at https://simonsobservatory.org/publications.php (Abstract abridged) -- matching version published in JCAP
- Full Text
- View/download PDF
22. Evidence for the kinematic Sunyaev-Zel’dovich effect with the Atacama Cosmology Telescope and velocity reconstruction from the Baryon Oscillation Spectroscopic Survey
- Author
-
Simone Aiola, Mathew S. Madhavacheril, Benjamin L. Schmitt, Matthew Hasselfield, Neelima Sehgal, J. Colin Hill, Loïc Maurin, Kent D. Irwin, Suzanne T. Staggs, Edward J. Wollack, Kavilan Moodley, M. Lungu, Michael D. Niemack, Bruce Partridge, Laura Newburgh, J. Richard Bond, Brian J. Koopman, Jeff McMahon, Jonathan Sievers, Dale Li, Francesco De Bernardis, Hsiao-Mei Cho, David N. Spergel, Sigurd Naess, Thibaut Louis, Adam D. Hincks, Mariana Vargas-Magaña, Arthur Kosowsky, Shawn W. Henderson, Christine G. Pappas, Erminia Calabrese, Lyman A. Page, John P. Hughes, Emmanuel Schaan, Johannes Hubmayr, Simone Ferraro, Mark J. Devlin, Patricio A. Gallardo, Nicholas Battaglia, Federico Nati, Shirley Ho, Blake D. Sherwin, Joanna Dunkley, Alexander van Engelen, Renée Hlozek, Kendrick M. Smith, Schaan, E, Ferraro, S, Vargas-Magaña, M, Smith Kendrick, M, Ho, S, Aiola, S, Battaglia, N, Bond J., R, De Bernardis, F, Calabrese, E, Cho, H, Devlin Mark, J, Dunkley, J, Gallardo Patricio, A, Hasselfield, M, Henderson, S, Hill J., C, Hincks Adam, D, Hlozek, R, Hubmayr, J, Hughes John, P, Irwin Kent, D, Koopman, B, Kosowsky, A, Li, D, Louis, T, Lungu, M, Madhavacheril, M, Maurin, L, Mcmahon Jeffrey, J, Moodley, K, Naess, S, Nati, F, Newburgh, L, Niemack Michael, D, Page Lyman, A, Pappas Christine, G, Partridge, B, Schmitt Benjamin, L, Sehgal, N, Sherwin Blake, D, Sievers Jonathan, L, Spergel David, N, Staggs Suzanne, T, Van Engelen, A, and Wollack Edward, J
- Subjects
Nuclear and High Energy Physics ,Active galactic nucleus ,Dark matter ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Sunyaev–Zel'dovich effect ,01 natural sciences ,Atomic ,Galaxy groups and clusters ,Particle and Plasma Physics ,0103 physical sciences ,Nuclear ,010303 astronomy & astrophysics ,QC ,Astrophysics::Galaxy Astrophysics ,Physics ,Quantum Physics ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Molecular ,Nuclear & Particles Physics ,Redshift ,Galaxy ,Baryon ,Atacama Cosmology Telescope ,astro-ph.CO ,Astronomical and Space Sciences - Abstract
Author(s): Schaan, E; Ferraro, S; Vargas-Magana, M; Smith, KM; Ho, S; Aiola, S; Battaglia, N; Bond, JR; De Bernardis, F; Calabrese, E; Cho, HM; Devlin, MJ; Dunkley, J; Gallardo, PA; Hasselfield, M; Henderson, S; Hill, JC; Hincks, AD; Hlozek, R; Hubmayr, J; Hughes, JP; Irwin, KD; Koopman, B; Kosowsky, A; Li, D; Louis, T; Lungu, M; Madhavacheril, M; Maurin, L; McMahon, JJ; Moodley, K; Naess, S; Nati, F; Newburgh, L; Niemack, MD; Page, LA; Pappas, CG; Partridge, B; Schmitt, BL; Sehgal, N; Sherwin, BD; Sievers, JL; Spergel, DN; Staggs, ST; Van Engelen, A; Wollack, EJ | Abstract: We use microwave temperature maps from two seasons of data from the Atacama Cosmology Telescope at 146 GHz, together with the "Constant Mass" CMASS galaxy sample from the Baryon Oscillation Spectroscopic Survey to measure the kinematic Sunyaev-Zel'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 microwave temperature at the location of each halo, weighted by the corresponding reconstructed velocity. We vary the size of the aperture photometry filter used, thus probing the free electron profile of these halos from within the virial radius out to three virial radii, on the scales relevant for investigating the missing baryons problem. The resulting best fit kSZ model is preferred over the no-kSZ hypothesis at 3.3 and 2.9σ for two independent velocity reconstruction methods, using 25,537 galaxies over 660 square degrees. The data suggest that the baryon profile is shallower than the dark matter in the inner regions of the halos probed here, potentially due to energy injection from active galactic nucleus or supernovae. Thus, by constraining the gas profile on a wide range of scales, this technique will be useful for understanding the role of feedback in galaxy groups and clusters. The effect of foregrounds that are uncorrelated with the galaxy velocities is expected to be well below our signal, and residual thermal Sunyaev-Zel'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.
- Published
- 2016
23. THE ATACAMA COSMOLOGY TELESCOPE: LENSING OF CMB TEMPERATURE AND POLARIZATION DERIVED FROM COSMIC INFRARED BACKGROUND CROSS-CORRELATION
- Author
-
Alexander van Engelen, Blake D. Sherwin, Neelima Sehgal, Graeme E. Addison, Rupert Allison, Nick Battaglia, Francesco de Bernardis, J. Richard Bond, Erminia Calabrese, Kevin Coughlin, Devin Crichton, Rahul Datta, Mark J. Devlin, Joanna Dunkley, Rolando Dünner, Patricio Gallardo, Emily Grace, Megan Gralla, Amir Hajian, Matthew Hasselfield, Shawn Henderson, J. Colin Hill, Matt Hilton, Adam D. Hincks, Renée Hlozek, Kevin M. Huffenberger, John P. Hughes, Brian Koopman, Arthur Kosowsky, Thibaut Louis, Marius Lungu, Mathew Madhavacheril, Loïc Maurin, Jeff McMahon, Kavilan Moodley, Charles Munson, Sigurd Naess, Federico Nati, Laura Newburgh, Michael D. Niemack, Michael R. Nolta, Lyman A. Page, Christine Pappas, Bruce Partridge, Benjamin L. Schmitt, Jonathan L. Sievers, Sara Simon, David N. Spergel, Suzanne T. Staggs, Eric R. Switzer, Jonathan T. Ward, Edward J. Wollack, Engelen Alexander, V, Sherwin Blake, D, Sehgal, N, Addison Graeme, E, Allison, R, Battaglia, N, Bernardis Francesco, D, Bond J., R, Calabrese, E, Coughlin, K, Crichton, D, Datta, R, Devlin Mark, J, Dunkley, J, Dünner, R, Gallardo, P, Grace, E, Gralla, M, Hajian, A, Hasselfield, M, Henderson, S, Hill J., C, Hilton, M, Hincks Adam, D, Hlozek, R, Huffenberger Kevin, M, Hughes John, P, Koopman, B, Kosowsky, A, Louis, T, Lungu, M, Madhavacheril, M, Maurin, L, Mcmahon, J, Moodley, K, Munson, C, Naess, S, Nati, F, Newburgh, L, Niemack Michael, D, Nolta Michael, R, Page Lyman, A, Pappas, C, Partridge, B, Schmitt Benjamin, L, Sievers Jonathan, L, Simon, S, Spergel David, N, Staggs Suzanne, T, Switzer Eric, R, Ward Jonathan, T, and Wollack Edward, J
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Cosmic microwave background ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,cosmic background radiation ,symbols.namesake ,General Relativity and Quantum Cosmology ,Cosmic infrared background ,Planck ,cosmology: observations ,infrared: diffuse background ,large-scale structure of universe ,Astronomy and Astrophysics ,Space and Planetary Science ,Astrophysics::Galaxy Astrophysics ,Physics ,cosmology: observation ,Cross-correlation ,Astrophysics::Instrumentation and Methods for Astrophysics ,Polarization (waves) ,Amplitude ,Gravitational lens ,13. Climate action ,Atacama Cosmology Telescope ,symbols ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present a measurement of the gravitational lensing of the Cosmic Microwave Background (CMB) temperature and polarization fields obtained by cross-correlating the reconstructed convergence signal from the first season of ACTPol data at 146 GHz with Cosmic Infrared Background (CIB) fluctuations measured using the Planck satellite. Using an overlap area of 206 square degrees, we detect gravitational lensing of the CMB polarization by large-scale structure at a statistical significance of 4.5 sigma. Combining both CMB temperature and polarization data gives a lensing detection at 9.1 sigma significance. A B-mode polarization lensing signal is present with a significance of 3.2 sigma. We also present the first measurement of CMB lensing--CIB correlation at small scales corresponding to l > 2000. Null tests and systematic checks show that our results are not significantly biased by astrophysical or instrumental systematic effects, including Galactic dust. Fitting our measurements to the best-fit lensing-CIB cross power spectrum measured in Planck data, scaled by an amplitude A, gives A=1.02 +0.12/-0.18 (stat.) +/-0.06(syst.), consistent with the Planck results., Submitted to ApJ
- Published
- 2015
24. Evidence of lensing of the cosmic microwave background by dark matter halos
- Author
-
Rolando Dünner, Edward J. Wollack, Sigurd Naess, Federico Nati, Adam D. Hincks, Nick Battaglia, Kavilan Moodley, Rahul Datta, Benjamin L. Schmitt, J. Colin Hill, Devin Crichton, Lyman A. Page, Mark J. Devlin, M. Lungu, Robert Thornton, Suzanne T. Staggs, Blake D. Sherwin, Matthew Hasselfield, Arthur Kosowsky, Erminia Calabrese, Laura Newburgh, Michael D. Niemack, Jonathan T. Ward, Bruce Partridge, Mathew S. Madhavacheril, J. Richard Bond, Jerod Caligiuri, Jeff McMahon, Kevin Coughlin, Charles Munson, David N. Spergel, Rupert Allison, Neelima Sehgal, Amir Hajian, Matt Hilton, Alexander van Engelen, Emily Grace, Thibaut Louis, John P. Hughes, Joanna Dunkley, Jon Sievers, Kevin Fogarty, Renée Hlozek, Madhavacheril, M, Sehgal, N, Allison, R, Battaglia, N, Bond J., R, Calabrese, E, Caligiuri, J, Coughlin, K, Crichton, D, Datta, R, Devlin Mark, J, Dunkley, J, Dünner, R, Fogarty, K, Grace, E, Hajian, A, Hasselfield, M, Hill J., C, Hilton, M, Hincks Adam, D, Hlozek, R, Hughes John, P, Kosowsky, A, Louis, T, Lungu, M, Mcmahon, J, Moodley, K, Munson, C, Naess, S, Nati, F, Newburgh, L, Niemack Michael, D, Page Lyman, A, Partridge, B, Schmitt, B, Sherwin Blake, D, Sievers, J, Spergel David, N, Staggs Suzanne, T, Thornton, R, Van Engelen, A, Ward Jonathan, T, and Wollack Edward, J
- Subjects
Physics ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Hot dark matter ,Strong gravitational lensing ,Cosmic microwave background ,Dark matter ,Scalar field dark matter ,Astrophysics::Instrumentation and Methods for Astrophysics ,General Physics and Astronomy ,Astronomy ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Dark matter halo ,Physics and Astronomy (all) ,Physics::Space Physics ,Astrophysics::Solar and Stellar Astrophysics ,Weak gravitational lensing ,Dark fluid ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present evidence of the gravitational lensing of the cosmic microwave background by $10^{13}$ solar mass dark matter halos. Lensing convergence maps from the Atacama Cosmology Telescope Polarimeter (ACTPol) are stacked at the positions of around 12,000 optically-selected CMASS galaxies from the SDSS-III/BOSS survey. The mean lensing signal is consistent with simulated dark matter halo profiles, and is favored over a null signal at 3.2 sigma significance. This result demonstrates the potential of microwave background lensing to probe the dark matter distribution in galaxy group and galaxy cluster halos., 9 pages, 3 figures, accepted by PRL, author list corrected
- Published
- 2015
Catalog
Discovery Service for Jio Institute Digital Library
For full access to our library's resources, please sign in.