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Your search keyword '"Menanteau, Felipe"' showing total 23 results
Start Over Author "Menanteau, Felipe" Topic fos: physical sciences
23 results on '"Menanteau, Felipe"'

1. 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

2. 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

3. Paper 1: The JWST PEARLS View of the El Gordo Galaxy Cluster and of the Structure It Magnifies

Author

Frye, Brenda L., Pascale, Massimo, Foo, Nicholas, Leimbach, Reagen, Garuda, Nikhil, Robles, Paulina Soto, Summers, Jake, Diaz, Carlos, Kamieneski, Patrick, Furtak, Lukas, Cohen, Seth, Diego, Jose, Beauchesne, Benjamin, Windhorst, Rogier, Willner, Steve, Koekemoer, Anton M., Zitrin, Adi, Caminha, Gabriel, Caputi, Karina, Coe, Dan, Conselice, Christopher J., Dai, Liang, Dole, Herve, Driver, Simon, Grogin, Norman, Harrington, Kevin, Jansen, Rolf A., Kneib, Jean-Paul, Lehnert, Matt, Lowenthal, James, Marshall, Madeline A., Menanteau, Felipe, Pampleiga, Belen Alcalde, Pirzkal, Nor, Polletta, Mari, Richard, Johan, Robotham, Aaron, Ryan, Russell E., Rutkowski, Michael J., Sifon, Christobal, Tompkins, Scott, Wang, Daniel, Yan, Haojing, and Yun, Min S.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

The massive galaxy cluster El Gordo (z=0.87) imprints multitudes of gravitationally lensed arcs onto James Webb Space Telescope (JWST) Near-Infrared Camera (NIRCam) images. Eight bands of NIRCam imaging were obtained in the ``Prime Extragalactic Areas for Reionization and Lensing Science'' (``PEARLS'') program. PSF-matched photometry across Hubble Space Telescope (HST) and NIRCam filters supplies new photometric redshifts. A new light-traces-mass lens model based on 56 image multiplicities identifies the two mass peaks and yields a mass estimate within 500 kpc of ~(7.0 +/- 0.30) x 10^14 Msun. A search for substructure in the 140 cluster members with spectroscopic redshifts confirms the two main mass components. The southeastern mass peak that contains the BCG is more tightly bound than the northwestern one. The virial mass within 1.7 Mpc is (5.1 +/- 0.60) x 10^14 Msun, lower than the lensing mass. A significant transverse velocity component could mean the virial mass is underestimated. We contribute one new member to the previously known z=4.32 galaxy group. Intrinsic (delensed) positions of the five secure group members span a physical extent of ~60 kpc. Thirteen additional candidates selected by spectroscopic/photometric constraints are small and faint with a mean intrinsic luminosity ~2.2 mag fainter than L*. NIRCam imaging admits a fairly wide range of brightnesses and morphologies for the group members, suggesting a more diverse galaxy population in this galaxy overdensity., 24 pages, accepted by ApJ

Published
2023

4. The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth

Author

Qu, Frank J., Sherwin, Blake D., Madhavacheril, Mathew S., Han, Dongwon, Crowley, Kevin T., 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, Carron, Julien, Challinor, Anthony, Chesmore, Grace E., Cho, Hsiao-mei, Choi, Steve K., Clark, Susan E., Rosado, Rodrigo Córdova, Cothard, Nicholas F., Coughlin, Kevin, Coulton, William, 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, Gluscevic, Vera, Golec, Joseph E., Guan, Yilun, Halpern, Mark, 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, Li, Yaqiong, Limon, Michele, Lokken, Martine, Louis, Thibaut, Lungu, Marius, MacCrann, Niall, 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present new measurements of cosmic microwave background (CMB) lensing over $9400$ sq. deg. of the sky. These lensing measurements are derived from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) CMB dataset, which consists of five seasons of ACT CMB temperature and polarization observations. We determine the amplitude of the CMB lensing power spectrum at $2.3\%$ precision ($43\sigma$ significance) using a novel pipeline that minimizes sensitivity to foregrounds and to noise properties. To ensure our results are robust, we analyze an extensive set of null tests, consistency tests, and systematic error estimates and employ a blinded analysis framework. The baseline spectrum is well fit by a lensing amplitude of $A_{\mathrm{lens}}=1.013\pm0.023$ relative to the Planck 2018 CMB power spectra best-fit $\Lambda$CDM model and $A_{\mathrm{lens}}=1.005\pm0.023$ relative to the $\text{ACT DR4} + \text{WMAP}$ best-fit model. From our lensing power spectrum measurement, we derive constraints on the parameter combination $S^{\mathrm{CMBL}}_8 \equiv \sigma_8 \left({\Omega_m}/{0.3}\right)^{0.25}$ of $S^{\mathrm{CMBL}}_8= 0.818\pm0.022$ from ACT DR6 CMB lensing alone and $S^{\mathrm{CMBL}}_8= 0.813\pm0.018$ when combining ACT DR6 and Planck NPIPE CMB lensing power spectra. These results are in excellent agreement with $\Lambda$CDM model constraints from Planck or $\text{ACT DR4} + \text{WMAP}$ CMB power spectrum measurements. Our lensing measurements from redshifts $z\sim0.5$--$5$ are thus fully consistent with $\Lambda$CDM structure growth predictions based on CMB anisotropies probing primarily $z\sim1100$. We find no evidence for a suppression of the amplitude of cosmic structure at low redshifts, Comment: 45+21 pages, 50 figures. Prepared for submission to ApJ. Also see companion papers Madhavacheril et al and MacCrann et al

Published
2023
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5. 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

6. 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
Full Text
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7. Constraints on dark matter to dark radiation conversion in the late universe with DES-Y1 and external data

Author

Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnès, Weaverdyck, Noah, Alves, Otavio Alonso, Leonard, C. Danielle, MacCrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ross, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, James, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Pereira, Maria Elidaiana da Silva, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klaus, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Malagón, Andrés Plazas, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, To, Chun-Hao, Varga, Tamas Norbert, Weller, Jochen, Wilkinson, Reese, UAM. Departamento de Física Teórica, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, Instituto Nacional de Ciência e Tecnologia (Brasil), 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), DES, University of Michigan, Duke University, California Institute of Technology, Universidade Estadual Paulista (UNESP), Newcastle Unviersity, Ohio State University, University of Chicago, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), University of Manchester, Stanford University, University College London, Universidade de Lisboa, University of Edinburgh, Perimeter Institute for Theoretical Physics, Observatoire de Sauverny, Carnegie Mellon University, University of Wisconsin-Madison, 382 Via Pueblo Mall, Menlo Park, University of Pennsylvania, Medioambientales y Tecnológicas (CIEMAT), Brookhaven National Laboratory, NSF's National Optical-Infrared Astronomy Research Laboratory, Universidade de São Paulo (USP), LIneA, Fermi National Accelerator Laboratory, Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University of Sussex, Instituto de Astrofisica de Canarias, Dpto. Astrofísica, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Queensland, University of Arizona, University of Oslo, Santa Cruz Institute for Particle Physics, Ludwig-Maximilians-Universität, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universität München, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Cambridge, Peyton Hall, University of Southampton, Oak Ridge National Laboratory, University of Portsmouth, Chen, Angela, Huterer, Dragan, Lee, Sujeong, Ferté, Agnè, Weaverdyck, Noah, Alonso Alves, Otavio, Leonard, C. Danielle, Maccrann, Niall, Raveri, Marco, Porredon, Anna, Di Valentino, Eleonora, Muir, Jessica, Lemos, Pablo, Liddle, Andrew, Blazek, Jonathan, Campos, Andresa, Cawthon, Ro, Choi, Ami, Dodelson, Scott, Elvin-Poole, Jack, Gruen, Daniel, Ross, Ashley, Secco, Lucas F., Sevilla, Ignacio, Sheldon, Erin, Troxel, Michael A., Zuntz, Joe, Abbott, Tim, Aguena, Michel, Allam, Sahar, Annis, Jame, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Bridle, Sarah, Brooks, David, Carnero Rosell, Aurelio, Carrasco Kind, Matia, Carretero, Jorge, Costanzi, Matteo, Crocce, Martin, da Costa, Luiz, Elidaiana da Silva Pereira, Maria, Davis, Tamara, Doel, Peter, Eifler, Tim, Ferrero, Ismael, Fosalba, Pablo, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David, Gruendl, Robert, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel, Hollowood, Devon L., Honscheid, Klau, Hoyle, Ben, James, David, Jarvis, Mike, Kuehn, Kyler, Lahav, Ofer, Maia, Marcio, Marshall, Jennifer, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Palmese, Antonella, Paz-Chinchon, Francisco, Plazas Malagón, André, Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Suchyta, Eric, Tarle, Gregory, Thomas, Daniel, Chun-Hao, To, Varga, Tamas Norbert, Weller, Jochen, and Wilkinson, Reese

Subjects
matter: power spectrum, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, power spectrum, 01 natural sciences, Cosmology, hubble constant, High Energy Physics - Phenomenology (hep-ph), Scale Structure, cosmological model: parameter space, Power Spectrum, Dark energy, Astrophysics - Cosmology and Nongalactic Astrophysic, Large-scale structure of the Universe, 010303 astronomy & astrophysics, media_common, Physics, Energy, massive neutrinos, Hubble Constant, tension, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology, halo-model, statistics, dark energy: density, Dark radiation, symbols, Halo-Model, energy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, galaxy formation, Evolution of the Universe, symbols.namesake, scale structure, 0103 physical sciences, supernova, Galaxy formation and evolution, Self-Interactions, Massive Neutrinos, STFC, Sdss, 010308 nuclear & particles physics, RCUK, resolution, Física, self-interactions, inconsistent, Universe, cosmic background radiation: temperature, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Galaxy Formation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, Hubble's law
Abstract

Chen, A., et al. DES Collaboration, We study a phenomenological class of models where dark matter converts to dark radiation in the low redshift epoch. This class of models, dubbed DMDR, characterizes the evolution of comoving dark-matter density with two extra parameters, and may be able to help alleviate the observed discrepancies between early and late-time probes of the Universe. We investigate how the conversion affects key cosmological observables such as the cosmic microwave background (CMB) temperature and matter power spectra. Combining 3x2pt data from Year 1 of the Dark Energy Survey, Planck-2018 CMB temperature and polarization data, supernovae (SN) Type Ia data from Pantheon, and baryon acoustic oscillation (BAO) data from BOSS DR12, MGS and 6dFGS, we place new constraints on the amount of dark matter that has converted to dark radiation and the rate of this conversion. The fraction of the dark matter that has converted since the beginning of the Universe in units of the current amount of dark matter, ζ, is constrained at 68% confidence level to be, he DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under Grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants Agreement No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2).

Published
2021
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8. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author

Adhikari, Susmita, Shin, Tae-hyeon, Jain, Bhuvnesh, Hilton, Matt, Baxter, Eric, Chang, Chihway, Wechsler, Risa H., Battaglia, Nick, Bond, J. Richard, Bocquet, Sebastian, DeRose, Joseph, Choi, Steve K., Devlin, Mark, Dunkley, Jo, Evrard, August E., Ferraro, Simone, Hill, J. Colin, Hughes, John P., Gallardo, Patricio A., Lokken, Martine, MacInnis, Amanda, McMahon, Jeffrey, Madhavacheril, Mathew S., Nati, Frederico, Newburgh, Laura B., Niemack, Michael D., Page, Lyman A., Palmese, Antonella, Partridge, Bruce, Rozo, Eduardo, Rykoff, Eli, Salatino, Maria, Schillaci, Alessandro, Sehgal, Neelima, Sif��n, Crist��bal, To, Chun-Hao, Wollack, Ed, Wu, Hao-Yi, Xu, Zhilei, Aguena, Michel, Allam, Sahar, Amon, Alexandra, Annis, James, Avila, Santiago, Bacon, David, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L., Rosell, Aurelio C., Kind, Matias Carrasco, Carretero, Jorge, Castander, Francisco Javier, Choi, Ami, Costanzi, Matteo, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Diehl, Thomas H., Doel, Peter, Everett, Spencer, Ferrero, Ismael, Fert��, Agn��s, Flaugher, Brenna, Fosalba, Pablo, Frieman, Josh, Garc��a-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia, Gutierrez, Gaston, Hartley, Will G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, David J., Jeltema, Tesla, Kuehn, Kyler, Kuropatkin, Nikolay, Lahav, Ofer, Lima, Marcos, Maia, Marcio A. G., Marshall, Jennifer L., Martini, Paul, Melchior, Peter, Menanteau, Felipe, Miquel, Ramon, Morgan, Robert, Ogando, Ricardo L. C., Paz-Chinch��n, Francisco, Malag��n, Andr��s Plazas, Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Varga, Tamas N., Wilkinson, Reese D., Zhang, Yuanyuan, Austermann, Jason E., Beall, James A., Becker, Daniel T., Denison, Edward V., Duff, Shannon M., Hilton, Gene C., Hubmayr, Johannes, Ullom, Joel N., Van Lanen, Jeff, Vale, Leila R., Collaboration, DES, Collaboration, ACT, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari, S., Shin, T. -H., Jain, B., Hilton, M., Baxter, E., Chang, C., Wechsler, R. H., Battaglia, N., Bond, J. R., Bocquet, S., Choi, S. K., Derose, J., Devlin, M., Dunkley, J., Evrard, A. E., Ferraro, S., Hill, J. C., Hughes, J. P., Gallardo, P. A., Lokken, M., Macinnis, A., Madhavacheril, M. S., Mcmahon, J., Nati, F., Newburgh, L. B., Niemack, M. D., Page, L. A., Palmese, A., Partridge, B., Rozo, E., Rykoff, E., Salatino, M., Schillaci, A., Sehgal, N., Sifon, C., C. -H., To, Wollack, E., H. -Y., Wu, Xu, Z., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. C., Kind, M. C., Carretero, J., Castander, F. J., Choi, A., Costanzi, M., Da Costa, L. N., Vicente, J. D., Desai, S., Diehl, T. H., Doel, P., Everett, S., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., L. C. Ogando R., Paz-Chinchon, F., Malagon, A. P., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., E. C. Swanson M., Varga, T. N., Wilkinson, R. D., Zhang, Y., Austermann, J. E., Beall, J. A., Becker, D. T., Denison, E. V., Duff, S. M., Hilton, G. C., Hubmayr, J., Ullom, J. N., Lanen, J. V., and Vale, L. R.

Subjects
Galaxy dark matter halos, 010308 nuclear & particles physics, FOS: Physical sciences, Cold dark matter, Astronomy and Astrophysics, Galaxy clusters, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, SZ effect, Galaxy cluster, Surveys, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Galaxy evolution, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Galaxy kinematics
Abstract

Adhikari, S., et al. (DES and ACT Collaboration), We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr., The DES Data Management System is supported by the NSF under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Unionʼs Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2)

Published
2021

9. Finding quadruply imaged quasars with machine learning. I. Methods

Author

Akhazhanov, A., More, A., Amini, A., Hazlett, C., Treu, T., Birrer, S., Shajib, A., Liao, K., Lemon, C., Agnello, A., Nord, B., Aguena, Michel, Allam, Sahar, Andrade-Oliveira, Felipe, Annis, J., Brooks, D., Buckley-Geer, E., Burke, David L., Carnero Rosell, Aurelio, Carrasco Kind, Matias, Carretero, J., Choi, A., Conselice, Christopher J., Costanzi, M., da Costa, L. N., Pereira, M.E.S., De Vicente, J., Desai, S., Dietrich, J.P., Doel, P., Everett, S., Ferrero, Ismael, Finley, D.A., Flaugher, Brenna, Frieman, Josh, García-Bellido, Juan, Gerdes, David W., Gruen, D., Gruendl, Robert A., Gschwend, J., Gutierrez, G., Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klaus, James, D.J., Kim, A.G., Kuehn, K., Kuropatkin, Nikolay, Lahav, Ofer, Lima, M., Lin, H., Maia, Marcio A. G., March, M., Menanteau, Felipe, Miquel, R., Morgan, R., Palmese, Antonella, Paz-Chinchón, Francisco, Pieres, A., Plazas Malagón, Andrés A., Sanchez, E., Scarpine, Vic, Serrano, S., Sevilla-Noarbe, Ignacio, Smith, M., Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Tarlé, Gregory, To, C., Varga, Tamas Norbert, Weller, Jochen, A Akhazhanov, A., More, A., Amini, A., Hazlett, C., Treu, T., Birrer, S., Shajib, A., Liao, K., Lemon, C., Agnello, A., Nord, B., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., Conselice, C., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Finley, D. A., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kim, A. G., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lin, H., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Plazas Malagón, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Varga, T. N., Weller, J., UAM. Departamento de Física Teórica, Department of Energy (US), National Science Foundation (US), Ministerio de Educación y Ciencia (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Generalitat de Catalunya, European Research Council, Science and Technology Facilities Council (UK), and Ministerio de Economía y Competitividad (España)

Subjects
methods: statistical, model, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Survey [astronomical data bases], candidates, Física, gravitational lensing: strong, FOS: Physical sciences, ESTATÍSTICA, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Strong [gravitational lensing], Astronomical Data Bases: Catalogs, Space and Planetary Science, astronomical data bases: surveys, strong gravitational lenses, Statistical [methods], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: et al., Strongly lensed quadruply imaged quasars (quads) are extraordinary objects. They are very rare in the sky and yet they provide unique information about a wide range of topics, including the expansion history and the composition of the Universe, the distribution of stars and dark matter in galaxies, the host galaxies of quasars, and the stellar initial mass function. Finding them in astronomical images is a classic ‘needle in a haystack’ problem, as they are outnumbered by other (contaminant) sources by many orders of magnitude. To solve this problem, we develop state-of-the-art deep learning methods and train them on realistic simulated quads based on real images of galaxies taken from the Dark Energy Survey, with realistic source and deflector models, including the chromatic effects of microlensing. The performance of the best methods on a mixture of simulated and real objects is excellent, yielding area under the receiver operating curve in the range of 0.86–0.89. Recall is close to 100 per cent down to total magnitude i ∼ 21 indicating high completeness, while precision declines from 85 per cent to 70 per cent in the range i ∼ 17–21. The methods are extremely fast: training on 2 million samples takes 20 h on a GPU machine, and 108 multiband cut-outs can be evaluated per GPU-hour. The speed and performance of the method pave the way to apply it to large samples of astronomical sources, bypassing the need for photometric pre-selection that is likely to be a major cause of incompleteness in current samples of known quads., TT acknowledges support from the National Science Foundation through grant NSF-AST-1906976, from NASA through grants HST-GO-15320and HST-GO-15652, and from the Packard Foundation through a Packard Research Fellowship. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Published
2021
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10. The Curious Case of PHL 293B: A Long-Lived Transient in a Metal-Poor Blue Compact Dwarf Galaxy

Author

Burke, Colin J., Baldassare, Vivienne F., Liu, Xin, Foley, Ryan J., Shen, Yue, Palmese, Antonella, Guo, Hengxiao, Herner, Kenneth, Abbott, Tim M. C., Aguena, Michel, Allam, Sahar, Avila, Santiago, Bertin, Emmanuel, Brooks, David, Rosell, Aurelio Carnero, Kind, Matias Carrasco, Carretero, Jorge, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Doel, Peter, Eifler, Tim F., Everett, Spencer, Frieman, Josh, Garcia-Bellido, Juan, Gaztanaga, Enrique, Gruen, Daniel, Gruendl, Robert A., Gschwend, Julia, Gutierrez, Gaston, Hollowood, Devon L., Honscheid, Klaus, James, David J., Krause, Elisabeth, Kuehn, Kyler, Maia, Marcio A. G., Menanteau, Felipe, Miquel, Ramon, Paz-Chinchon, Francisco, Plazas, Andres A., Sanchez, Eusebio, Santiago, Basilio, Scarpine, Vic, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Soares-Santos, Marcelle, Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Douglas L., Varga, Tamas Norbert, Walker, Alistair R., Collaboration, DES, National Aeronautics and Space Administration (US), Department of Energy (US), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, 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), and DES

Subjects
Active galactic nucleus, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Dwarf galaxy, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

arXiv:2002.12369v2 DES Collaboration: et al., We report on small-amplitude optical variability and recent dissipation of the unusually persistent broad emission lines in the blue compact dwarf galaxy PHL 293B. The galaxy's unusual spectral features (P Cygni-like profiles with ~800 km s−1 blueshifted absorption lines) have resulted in conflicting interpretations of the nature of this source in the literature. However, analysis of new Gemini spectroscopy reveals the broad emission has begun to fade after being persistent for over a decade prior. Precise difference imaging light curves constructed with the Sloan Digital Sky Survey and the Dark Energy Survey reveal small-amplitude optical variability of ~0.1 mag in the g band offset by 100 ± 21 pc from the brightest pixel of the host. The light curve is well-described by an active galactic nuclei (AGN)-like damped random walk process. However, we conclude that the origin of the optical variability and spectral features of PHL 293B is due to a long-lived stellar transient, likely a Type IIn supernova or nonterminal outburst, mimicking long-term AGN-like variability. This work highlights the challenges of discriminating between scenarios in such extreme environments, relevant to searches for AGNs in dwarf galaxies. This is the second long-lived transient discovered in a blue compact dwarf, after SDSS1133. Our result implies such long-lived stellar transients may be more common in metal-deficient galaxies. Systematic searches for low-level variability in dwarf galaxies will be possible with the upcoming Legacy Survey of Space and Time at the Vera C. Rubin Observatory., Support for V.F.B. was provided by the National Aeronautics and Space Administration through Einstein Postdoctoral Fellowship Award Number PF7-180161 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant 465376/2014-2).

Published
2020
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11. 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

12. High Confidence Optical Confirmations Among the High Signal-to-Noise Planck Cluster Candidates

Author

Boada, Steven, Hughes, John P., Menanteau, Felipe, Doze, Peter, Barrientos, L. Felipe, and Infante, L.

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

We report on newly identified galaxy clusters from the high signal-to-noise ($>5$-$��$) end of the second all-sky \textit{Planck} Sunyaev-Zel'dovich (SZ) catalog (PSZ2). The clusters are identified in deep, optical imaging from the Kitt Peak National Observatory 4m Mayall telescope taken between 2014 and 2017. Here we focus on the highest richness systems, and identify galaxy clusters through a combination of the maxBCG algorithm and visual image inspection. Galaxy clusters are considered to be confirmed if they are both rich and spatially coincident ($\lesssim 6'$) with the reported PSZ2 position. Of the 85 fields containing unconfirmed PSZ2 candidates observed, we find 15 (17.6% of the observed sample) corresponding galaxy clusters ($ 0.13 < z < 0.78$), 12 of which are previously unrecognized as counterparts. To explain this low identification fraction, we consider three possible scenarios: that clusters are (1) mostly at low-z, (2) mostly at high-z, or (3) located in fields with high object density. None of these scenarios alone can account for the low purity of rich galaxy clusters among the high signal-to-noise PSZ2 unconfirmed candidates., 14 pages, 8 Figures, Accepted by ApJ

Published
2018
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13. The Atacama Cosmology Telescope: CMB Polarization at $200

Author

Naess, Sigurd, Hasselfield, Matthew, McMahon, Jeff, Niemack, Michael D., Addison, Graeme E., Ade, Peter A. R., Allison, Rupert, Amiri, Mandana, Battaglia, Nick, Beall, James A., de Bernardis, Francesco, Bond, J Richard, Britton, Joe, Calabrese, Erminia, Cho, Hsiao-mei, Coughlin, Kevin, Crichton, Devin, Das, Sudeep, Datta, Rahul, Devlin, Mark J., Dicker, Simon R., Dunkley, Joanna, D��nner, Rolando, Fowler, Joseph W., Fox, Anna E., Gallardo, Patricio, Grace, Emily, Gralla, Megan, Hajian, Amir, Halpern, Mark, Henderson, Shawn, Hill, J. Colin, Hilton, Gene C., Hilton, Matt, Hincks, Adam D., Hlozek, Ren��e, Ho, Patty, Hubmayr, Johannes, Huffenberger, Kevin M., Hughes, John P., Infante, Leopoldo, Irwin, Kent, Jackson, Rebecca, Kasanda, Simon Muya, Klein, Jeff, Koopman, Brian, Kosowsky, Arthur, Li, Dale, Louis, Thibaut, Lungu, Marius, Madhavacheril, Mathew, Marriage, Tobias A., Maurin, Lo��c, Menanteau, Felipe, Moodley, Kavilan, Munson, Charles, Newburgh, Laura, Nibarger, John, Nolta, Michael R., Page, Lyman A., Pappas, Christine, Partridge, Bruce, Rojas, Felipe, Schmitt, Benjamin, Sehgal, Neelima, Sherwin, Blake D., Sievers, Jon, Simon, Sara, Spergel, David N., Staggs, Suzanne T., Switzer, Eric R., Thornton, Robert, Trac, Hy, Tucker, Carole, Uehara, Masao, Van Engelen, Alexander, Ward, Jon, and Wollack, Edward J.

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
Abstract

We report on measurements of the cosmic microwave background (CMB) and celestial polarization at 146 GHz made with the Atacama Cosmology Telescope Polarimeter (ACTPol) in its first three months of observing. Four regions of sky covering a total of 270 square degrees were mapped with an angular resolution of $1.3'$. The map noise levels in the four regions are between 11 and 17 $��$K-arcmin. We present TT, TE, EE, TB, EB, and BB power spectra from three of these regions. The observed E-mode polarization power spectrum, displaying six acoustic peaks in the range $200, 16 pages, 15 figures, 5 tables

Published
2014
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14. 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

15. 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

16. 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

17. Southern Cosmology Survey II: Massive Optically-Selected Clusters from 70 square degrees of the SZE Common Survey Area

Author

Menanteau, Felipe, Hughes, John P., Barrientos, L. Felipe, Deshpande, Amruta J., Hilton, Matt, Infante, Leopoldo, Jimenez, Raul, Kosowsky, Arthur, Moodley, Kavilan, Spergel, David, and Verde, Licia

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

We present a catalog of 105 rich and massive ($M>3\times10^{14}M_{\sun}$) optically-selected clusters of galaxies extracted from 70 square-degrees of public archival griz imaging from the Blanco 4-m telescope acquired over 45 nights between 2005 and 2007. We use the clusters' optically-derived properties to estimate photometric redshifts, optical luminosities, richness, and masses. We complement the optical measurements with archival XMM-Newton and ROSAT X-ray data which provide additional luminosity and mass constraints on a modest fraction of the cluster sample. Two of our clusters show clear evidence for central lensing arcs; one of these has a spectacular large-diameter, nearly-complete Einstein Ring surrounding the brightest cluster galaxy. A strong motivation for this study is to identify the massive clusters that are expected to display prominent signals from the Sunyaev-Zeldovich Effect (SZE) and therefore be detected in the wide-area mm-band surveys being conducted by both the Atacama Cosmology Telescope and the South Pole Telescope. The optical sample presented here will be useful for verifying new SZE cluster candidates from these surveys, for testing the cluster selection function, and for stacking analyzes of the SZE data., 13 pages, 7 Figures. Accepted for publication to ApJSS. Full resolution plots and additional material available at http://peumo.rutgers.edu/~felipe/e-prints/

Published
2010

18. First lensing measurements of SZ-discovered clusters

Author

McInnes, Rachel N., Menanteau, Felipe, Heavens, Alan F., Hughes, John P., Jimenez, Raul, Massey, Richard, Simon, Patrick, and Taylor, Andy N.

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 present the first lensing mass measurements of Sunyaev-Zel'dovich (SZ) selected clusters. Using optical imaging from the Southern Cosmology Survey (SCS), we present weak lensing masses for three clusters selected by their SZ emission in the South Pole Telescope survey (SPT). We confirm that the SZ selection procedure is successful in detecting mass concentrations. We also study the weak lensing signals from 38 optically-selected clusters in ~8 square degrees of the SCS survey. We fit Navarro, Frenk and White (NFW) profiles and find that the SZ clusters have amongst the largest masses, as high as 5x10^14 Msun. Using the best fit masses for all the clusters, we analytically calculate the expected SZ integrated Y parameter, which we find to be consistent with the SPT observations., Comment: Minor changes to match accepted version, 5 pages, 3 figures

Published
2009
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19. Improving Photometric Redshifts using GALEX Observations for the SDSS Stripe 82 and the Next Generation of SZ Cluster Surveys

Author

Niemack, Michael D., Jimenez, Raul, Verde, Licia, Menanteau, Felipe, Panter, Ben, and Spergel, David

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Four large-area Sunyaev-Zeldovich (SZ) experiments -- APEX-SZ, SPT, ACT, and Planck -- promise to detect clusters of galaxies through the distortion of Cosmic Microwave Background photons by hot (> 10^6 K) cluster gas (the SZ effect) over thousands of square degrees. A large observational follow-up effort to obtain redshifts for these SZ-detected clusters is under way. Given the large area covered by these surveys, most of the redshifts will be obtained via the photometric redshift (photo-z) technique. Here we demonstrate, in an application using ~3000 SDSS stripe 82 galaxies with r, Comment: 10 pages, 8 figures

Published
2008

20. The Morphological Demographics of galaxies in the ACS Hubble Ultra Deep Parallel Fields

Author

Menanteau, Felipe, Ford, Holland C., Motta, Veronica, Benitez, Narciso, Martel, Andre R., Blakeslee, John P., and Infante, Leopoldo

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

We present a morphological analysis of distant field galaxies using the deep ACS images from the public parallel NICMOS observations of the Hubble Ultra Deep Field obtained in the F435W (B), F606W (V), F775W (i) and F850LP (z) filters. We morphologically segregate galaxies using a combination of visual classification and objective machine based selection. We use the Asymmetry (A) and Central Concentration (C) parameters to characterize galaxies up to z_AB, 7 pages, 6 figures. Accepted for publication in the Astronomical Journal. Full resolution paper at: http://acs.pha.jhu.edu/~felipe/e-prints/

Published
2005
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21. The Nature of Blue Cores in Spheroids: a Possible Connection with AGN and Star Formation

Author

Menanteau, Felipe, Martel, Andre R., Tozzi, Paolo, Frye, Brenda, Ford, Holland C., Infante, Leopoldo, Benitez, Narciso, Galaz, Gaspar, Coe, Daniel, Illingworth, Garth D., Hartig, George F., and Clampin, Marc

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We investigate the physical nature of blue cores in early-type galaxies through the first multi-wavelength analysis of a serendipitously discovered field blue-nucleated spheroid in the background of the deep ACS/WFC griz multicolor observations of the cluster Abell 1689. The resolved g-r, r-i and i-z color maps reveal a prominent blue core identifying this galaxy as a ``typical'' case study, exhibiting variations of 0.5-1.0 mag in color between the center and the outer regions, opposite to the expectations of reddened metallicity induced gradients in passively evolved ellipticals. From a Magellan-Clay spectrum we secure the galaxy redshift at $z=0.624$. We find a strong X-ray source coincident with the spheroid galaxy. Spectral features and a high X-ray luminosity indicate the presence of an AGN in the galaxy. However, a comparison of the X-ray luminosity to a sample derived from the Chandra Deep Field South displays Lx to be comparable to Type I/QSO galaxies while the optical flux is consistent with a normal star-forming galaxy. We conclude that the galaxy's non-thermal component dominates at high-energy wavelengths while we associate the spheroid blue light with the stellar spectrum of normal star-forming galaxies. We argue about a probable association between the presence of blue cores in spheroids and AGN activity., Accepted for publication in the Astrophysical Journal. 6 pages, 3 figures. Full resolution images available at http://acs.pha.jhu.edu/~felipe/e-prints

Published
2004

22. Dark Energy Survey Identification of A Low-Mass Active Galactic Nucleus at Redshift 0.823 from Optical Variability

Author

Daniel Gruen, S. Everett, Marcos Lima, Colin J. Burke, K. Honscheid, Kyler Kuehn, A. Roodman, Luiz N. da Costa, D. W. Gerdes, David J. Brooks, M. Costanzi, Brad E. Tucker, Ricardo L. C. Ogando, A. K. Romer, Devon L. Hollowood, C. Lidman, E. J. Sanchez, Daniela Carollo, Peter Doel, Yu-Ching Chen, Michel Aguena, Aurelio Carnero Rosell, Emmanuel Bertin, E. Suchyta, Enrique Gaztanaga, N. E. Sommer, Juan Garcia-Bellido, Michael Schubnell, Samuel Hinton, G. Gutierrez, V. Scarpine, Eric Morganson, Juan de Vicente, Molly E. C. Swanson, Marcelle Soares-Santos, T. N. Varga, S. Allam, Robert A. Gruendl, Santiago Serrano, F. Paz-Chinchón, Anais Möller, Xin Liu, Kedar A. Phadke, Tim Eifler, Santiago Avila, A. A. Plazas, Ramon Miquel, Marcio A. G. Maia, J. Gschwend, Felipe Menanteau, Kaiwen Zhang, Matias Carrasco Kind, David J. James, Gregory Tarle, Hengxiao Guo, Shantanu Desai, Yue Shen, Mathew Smith, Antonella Palmese, 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 de Physique de Clermont (LPC), Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), DES, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Guo, Hengxiao, Burke, Colin J., Liu, Xin, Phadke, Kedar A., Zhang, Kaiwen, Chen, Yu-Ching, Gruendl, Robert A., Lidman, Christopher, Shen, Yue, Morganson, Eric, Aguena, Michel, Allam, Sahar, Avila, Santiago, Bertin, Emmanuel, Brooks, David, Rosell, Aurelio Carnero, Carollo, Daniela, Kind, Matias Carrasco, Costanzi, Matteo, da Costa, Luiz N., De Vicente, Juan, Desai, Shantanu, Doel, Peter, Eifler, Tim F., Everett, Spencer, García-Bellido, Juan, Gaztanaga, Enrique, Gerdes, David W., Gruen, Daniel, Gschwend, Julia, Gutierrez, Gaston, Hinton, Samuel R., Hollowood, Devon L., Honscheid, Klau, James, David J., Kuehn, Kyler, Lima, Marco, Maia, Marcio A. G., Menanteau, Felipe, Miquel, Ramon, Möller, Anai, Ogando, Ricardo L. C., Palmese, Antonella, Paz-Chinchón, Francisco, Plazas, Andrés A., Romer, Anita K., Roodman, Aaron, Sanchez, Eusebio, Scarpine, Vic, Schubnell, Michael, Serrano, Santiago, Smith, Mathew, Soares-Santos, Marcelle, Sommer, Natalia E., Suchyta, Eric, Swanson, Molly E. C., Tarle, Gregory, Tucker, Brad E., and Varga, Tamas N. (DES Collaboration)

Subjects
Active galactic nucleus, Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies: active, nuclei [galaxies], FOS: Physical sciences, active, [galaxies], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, surveys, galaxies: high-redshift, galaxies: nuclei, quasars: general, 01 natural sciences, Luminosity, 0103 physical sciences, survey, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, Supermassive black hole, general [quasars], 010308 nuclear & particles physics, Astronomy and Astrophysics, Quasar, black hole physic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies]
Abstract

We report the identification of a low-mass AGN, DES J0218$-$0430, in a redshift $z = 0.823$ galaxy in the Dark Energy Survey (DES) Supernova field. We select DES J0218$-$0430 as an AGN candidate by characterizing its long-term optical variability alone based on DES optical broad-band light curves spanning over 6 years. An archival optical spectrum from the fourth phase of the Sloan Digital Sky Survey shows both broad Mg II and broad H$\beta$ lines, confirming its nature as a broad-line AGN. Archival XMM-Newton X-ray observations suggest an intrinsic hard X-ray luminosity of $L_{{\rm 2-12\,keV}}\sim7.6\pm0.4\times10^{43}$ erg s$^{-1}$, which exceeds those of the most X-ray luminous starburst galaxies, in support of an AGN driving the optical variability. Based on the broad H$\beta$ from SDSS spectrum, we estimate a virial BH mass of $M_{\bullet}\approx10^{6.43}$-$10^{6.72}M_{\odot}$ (with the error denoting 1$\sigma$ statistical uncertainties only), consistent with the estimation from OzDES, making it the lowest mass AGN with redshift $>$ 0.4 detected in optical. We estimate the host galaxy stellar mass to be $M_{\ast}\sim10^{10.5\pm0.3}M_{\odot}$ based on modeling the multi-wavelength spectral energy distribution. DES J0218$-$0430 extends the $M_{\bullet}$-$M_{\ast}$ relation observed in luminous AGNs at $z\sim1$ to masses lower than being probed by previous work. Our work demonstrates the feasibility of using optical variability to identify low-mass AGNs at higher redshift in deeper synoptic surveys with direct implications for the upcoming Legacy Survey of Space and Time at Vera C. Rubin Observatory., Comment: 13 pages, 8 figures, 1 table, accepted to MNRAS

Published
2020
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23. Candidate periodically variable quasars from the Dark Energy Survey and the Sloan Digital Sky Survey

Author

J. Carretero, Tamara M. Davis, Matias Carrasco Kind, Samuel Hinton, M. March, S. Everett, Timothy M. C. Abbott, E. Suchyta, G. Gutierrez, H. Thomas Diehl, Luiz N. da Costa, Juan Garcia-Bellido, Marcos Lima, Yu-Ching Chen, Antonella Palmese, Xin Liu, Aurelio Carnero Rosell, Alistair R. Walker, M. Costanzi, Sunayana Bhargava, Jennifer L. Marshall, Brad E. Tucker, Kaiwen Zhang, David J. James, Michel Aguena, Ramon Miquel, Wei-Ting Liao, A. A. Plazas, A. Miguel Holgado, Felipe Menanteau, C. Lidman, Geraint F. Lewis, B. Flaugher, Gregory Tarle, Nikolay Kuropatkin, Michael Schubnell, Karl Glazebrook, Peter Doel, David J. Brooks, Hengxiao Guo, Enrique Gaztanaga, Emmanuel Bertin, Santiago Avila, Shantanu Desai, Devon L. Hollowood, Marcio A. G. Maia, Mathew Smith, D. L. Burke, Yue Shen, S. Allam, Robert A. Gruendl, E. J. Sanchez, F. Paz-Chinchón, Daniel Gruen, Daniela Carollo, Alex G. Kim, Santiago Serrano, Molly E. C. Swanson, Eric Morganson, Juan de Vicente, I. Sevilla-Noarbe, T. N. Varga, Joshua A. Frieman, Douglas Friedel, Kyler Kuehn, 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), DES, National Science Foundation (US), European Commission, European Research Council, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Chen, Yu-Ching, Liu, Xin, Liao, Wei-Ting, Holgado, A Miguel, Guo, Hengxiao, Gruendl, Robert A, Morganson, Eric, Shen, Yue, Zhang, Kaiwen, Abbott, Tim M C, Aguena, Michel, Allam, Sahar, Avila, Santiago, Bertin, Emmanuel, Bhargava, Sunayana, Brooks, David, Burke, David L, Rosell, Aurelio Carnero, Carollo, Daniela, Kind, Matias Carrasco, Carretero, Jorge, Costanzi, Matteo, da Costa, Luiz N, Davis, Tamara M, De Vicente, Juan, Desai, Shantanu, Diehl, H Thoma, Doel, Peter, Everett, Spencer, Flaugher, Brenna, Friedel, Dougla, Frieman, Joshua, García-Bellido, Juan, Gaztanaga, Enrique, Glazebrook, Karl, Gruen, Daniel, Gutierrez, Gaston, Hinton, Samuel R, Hollowood, Devon L, James, David J, Kim, Alex G, Kuehn, Kyler, Kuropatkin, Nikolay, Lewis, Geraint F, Lidman, Christopher, Lima, Marco, Maia, Marcio A G, March, Marisa, Marshall, Jennifer L, Menanteau, Felipe, Miquel, Ramon, Palmese, Antonella, Paz-Chinchón, Francisco, Plazas, Andrés A, Sanchez, Eusebio, Schubnell, Michael, Serrano, Santiago, Sevilla-Noarbe, Ignacio, Smith, Mathew, Suchyta, Eric, Swanson, Molly E C, Tarle, Gregory, Tucker, Brad E, Varga, Tamas Norbert, and Walker, Alistair R

Subjects
Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, galaxies: active, nuclei [galaxies], FOS: Physical sciences, Astrophysics, Data_CODINGANDINFORMATIONTHEORY, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, surveys, galaxies: high-redshift, quasars: general, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, survey, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, ONDAS GRAVITACIONAIS, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Supermassive black hole, general [quasars], 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Quasar, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Light curve, black hole physic, Redshift, Supernova, 13. Climate action, Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies], Astronomical and Space Sciences
Abstract

DES Collaboration: et al., Periodically variable quasars have been suggested as close binary supermassive black holes. We present a systematic search for periodic light curves in 625 spectroscopically confirmed quasars with a median redshift of 1.8 in a 4.6 deg2 overlapping region of the Dark Energy Survey Supernova (DES-SN) fields and the Sloan Digital Sky Survey Stripe 82 (SDSS-S82). Our sample has a unique 20-yr long multicolour (griz) light curve enabled by combining DES-SN Y6 observations with archival SDSS-S82 data. The deep imaging allows us to search for periodic light curves in less luminous quasars (down to r ∼23.5 mag) powered by less massive black holes (with masses ≳ 108.5M⊙) at high redshift for the first time. We find five candidates with significant (at >99.74 per cent single-frequency significance in at least two bands with a global p-value of ∼7 × 10−4–3 × 10−3 accounting for the look-elsewhere effect) periodicity with observed periods of ∼3–5 yr (i.e. 1–2 yr in rest frame) having ∼4–6 cycles spanned by the observations. If all five candidates are periodically variable quasars, this translates into a detection rate of ∼0.8+0.5−0.3 per cent or ∼1.1+0.7−0.5 quasar per deg2. Our detection rate is 4–80 times larger than those found by previous searches using shallower surveys over larger areas. This discrepancy is likely caused by differences in the quasar populations probed and the survey data qualities. We discuss implications on the future direct detection of low-frequency gravitational waves. Continued photometric monitoring will further assess the robustness and characteristics of these candidate periodic quasars to determine their physical origins., The DES data management system is supported by the National Science Foundation under grants AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grants 240672, 291329, and 306478.

Published
2020
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