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2. Kidney and Cardiovascular Effects of Canagliflozin According to Age and Sex: A Post Hoc Analysis of the CREDENCE Randomized Clinical Trial

Author

Perkovic, Vlado, Mahaffey, Kenneth W., Agarwal, Rajiv, Bakris, George, Brenner, Barry M., Cannon, Christopher P., Charytan, David M., de Zeeuw, Dick, Greene, Tom, Jardine, Meg J., Heerspink, Hiddo J.L., Levin, Adeera, Meininger, Gary, Neal, Bruce, Pollock, Carol, Wheeler, David C., Zhang, Hong, Zinman, Bernard, Jardine, Meg, Li, Nicole, Kolesnyk, Inna, Aizenberg, Diego, Pecoits-Filho, Roberto, Cherney, David, Obrador, Gregorio, Chertow, Glenn, Chang, Tara, Hawley, Carmel, Ji, Linong, Wada, Takashi, Jha, Vivekanand, Lim, Soo Kun, Lim-Abrahan, Mary Anne, Santos, Florence, Chae, Dong-Wan, Hwang, Shang-Jyh, Vazelov, Evgueniy, Rychlík, Ivan, Hadjadj, Samy, Krane, Vera, Rosivall, László, De Nicola, Luca, Dreval, Alexander, Nowicki, Michał, Schiller, Adalbert, Distiller, Larry, Górriz, Jose L., Kolesnyk, Mykola, David, Wheeler, C., Guerrero, Rodolfo Andres Ahuad, Albisu, Juan Pablo, Alvarisqueta, Andres, Bartolacci, Ines, Berli, Mario Alberto, Bordonava, Anselmo, Calella, Pedro, Cantero, Maria Cecilia, Cartasegna, Luis Rodolfo, Cercos, Esteban, Coloma, Gabriela Cecilia, Colombo, Hugo, Commendatore, Victor, Cuadrado, Jesus, Cuneo, Carlos Alberto, Cusumano, Ana Maria, Douthat, Walter Guillermo, Dran, Ricardo Dario, Farias, Eduardo, Fernandez, Maria Florencia, Finkelstein, Hernan, Fragale, Guillermo, Fretes, Jose Osvaldo, Garcia, Nestor Horacio, Gastaldi, Anibal, Gelersztein, Elizabeth, Glenny, Jorge Archibaldo, Gonzalez, Joaquin Pablo, Colaso, Patricia del Carmen Gonzalez, Goycoa, Claudia, Greloni, Gustavo Cristian, Guinsburg, Adrian, Hermida, Sonia, Juncos, Luis Isaias, Klyver, Maria Isabel, Kraft, Florencia, Krynski, Fernando, Lanchiotti, Paulina Virginia, Leon de la Fuente, Ricardo Alfonso, Marchetta, Nora, Mele, Pablo, Nicolai, Silvia, Novoa, Pablo Antonio, Orio, Silvia Ines, Otreras, Fabian, Oviedo, Alejandra, Raffaele, Pablo, Resk, Jorge Hector, Rista, Lucas, Papini, Nelson Rodriguez, Sala, Jorgelina, Santos, Juan Carlos, Schiavi, Lilia Beatriz, Sessa, Horacio, Casabella, Tomas Smith, Ulla, Maria Rosa, Valdez, Maria, Vallejos, Augusto, Villarino, Adriana, Visco, Virginia Esther, Wassermann, Alfredo, Zaidman, Cesar Javier, Cheung, Ngai Wah, Droste, Carolyn, Fraser, Ian, Johnson, David, Mah, Peak Mann, Nicholls, Kathy, Packham, David, Proietto, Joseph, Roberts, Anthony, Roger, Simon, Tsang, Venessa, Raduan, Roberto Abrão, Costa, Fernando Augusto Alves da, Amodeo, Celso, Turatti, Luiz Alberto Andreotti, Bregman, Rachel, Sanches, Fernanda Cristina Camelo, Canani, Luis Henrique, Chacra, Antônio Roberto, Borges, João Lindolfo Cunha, Vêncio, Sérgio Alberto Cunha, Franco, Roberto Jorge da Silva, d’Avila, Domingos, Portes, Evandro de Souza, de Souza, Pedro, Deboni, Luciane Mônica, Fraige Filho, Fadlo, Neto, Bruno Geloneze, Gomes, Marcus, Kohara, Suely Keiko, Keitel, Elizete, Saraiva, Jose Francisco Kerr, Lisboa, Hugo Roberto Kurtz, Contieri, Fabiana Loss de Carvalho, Milagres, Rosângela, Junior, Renan Montenegro, de Brito, Claudia Moreira, Hissa, Miguel Nasser, Sabbag, Ângela Regina Nazario, Noronha, Irene, Panarotto, Daniel, Filho, Roberto Pecoits, Pereira, Márcio Antônio, Saporito, Wladmir, Scotton, Antonio Scafuto, Schuch, Tiago, de Almeida, Roberto Simões, Ramos, Cássio Slompo, Felício, João Soares, Thomé, Fernando, Hachmann, Jean Carlo Tibes, Yamada, Sérgio, Hayashida, Cesar Yoiti, Petry, Tarissa Beatrice Zanata, Zanella, Maria Teresa, Andreeva, Viktoria, Angelova, Angelina, Dimitrov, Stefan, Genadieva, Veselka, Genova-Hristova, Gabriela, Hristozov, Kiril, Kamenov, Zdravko, Koundurdjiev, Atanas, Lozanov, Lachezar, Margaritov, Viktor, Nonchev, Boyan, Rangelov, Rangel, Shinkov, Alexander, Temelkova, Margarita, Velichkova, Ekaterina, Yakov, Andrian, Aggarwal, Naresh, Aronson, Ronnie, Bajaj, Harpreet, Chouinard, Guy, Conway, James, Cournoyer, Serge, DaRoza, Gerald, De Serres, Sacha, Dubé, François, Goldenberg, Ronald, Gupta, Anil, Gupta, Milan, Henein, Sam, Khandwala, Hasnain, Leiter, Lawrence, Madore, François, McMahon, Alan, Muirhead, Norman, Pichette, Vincent, Rabasa-Lhoret, Remi, Steele, Andrew, Tangri, Navdeep, Torshizi, Ali, Woo, Vincent, Zalunardo, Nadia, Montenegro, María Alicia Fernández, Gonzalo Godoy Jorquera, Juan, Fariña, Marcelo Medina, Gajardo, Victor Saavedra, Vejar, Margarita, Chen, Nan, Chen, Qinkai, Gan, Shenglian, Kong, Yaozhong, Li, Detian, Li, Wenge, Li, Xuemei, Lin, Hongli, Liu, Jian, Lu, Weiping, Mao, Hong, Ren, Yan, Song, Weihong, Sun, Jiao, Sun, Lin, Tu, Ping, Wang, Guixia, Yang, Jinkui, Yin, Aiping, Yu, Xueqing, Zhao, Minghui, Zheng, Hongguang, Mendoza, Jose Luis Accini, Arcos, Edgar, Avendano, Jorge, Diaz Ruiz, Jorge Ernesto Andres, Ortiz, Luis Hernando Garcia, Gonzalez, Alexander, Triana, Eric Hernandez, Higuera, Juan Diego, Malaver, Natalia, de Salazar, Dora Inés Molina, Rosero, Ricardo, Alexandra Terront Lozano, Monica, Cometa, Luis Valderrama, Valenzuela, Alex, Vargas Alonso, Ruben Dario, Villegas, Ivan, Yupanqui, Hernan, Bartaskova, Dagmar, Barton, Petr, Belobradkova, Jana, Dohnalova, Lenka, Drasnar, Tomas, Ferkl, Richard, Halciakova, Katarina, Klokocnikova, Vera, Kovar, Richard, Lastuvka, Jiri, Lukac, Martin, Pesickova, Satu, Peterka, Karel, Pumprla, Jiri, Rychlik, Ivan, Saudek, Frantisek, Tesar, Vladimir, Valis, Martin, Weiner, Pavel, Zemek, Stanislav, Alamartine, Eric, Borot, Sophie, Cariou, Bertrand, Dussol, Bertrand, Fauvel, Jean-Pierre, Gourdy, Pierre, Klein, Alexandre, Le Meur, Yannick, Penfornis, Alfred, Roussel, Ronan, Saulnier, Pierre-Jean, Thervet, Eric, Zaoui, Philippe, Burst, Volker, Faghih, Markus, Faulmann, Grit, Haller, Hermann, Jerwan-Keim, Reinhold, Maxeiner, Stephan, Paschen, Björn, Plassmann, Georg, Rose, Ludger, Gonzalez Orellana, Ronaldo Arturo, Haase, Franklin Paul, Moreira Diaz, Juan Pablo, Ramirez Roca, Luis Alberto, Sánchez Arenales, Jose Antonio, Sanchez Polo, José Vicente, Juarez, Erick Turcios, Csecsei, Gyongyi, Csiky, Botond, Danos, Peter, Deak, Laszlo, Dudas, Mihaly, Harcsa, Eleonora, Keltai, Katalin, Keresztesi, Sandor, Kiss, Krisztian, Konyves, Laszlo, Major, Lajos, Mileder, Margit, Molnar, Marta, Mucsi, Janos, Oroszlan, Tamas, Ory, Ivan, Paragh, Gyorgy, Peterfai, Eva, Petro, Gizella, Revesz, Katalin, Takacs, Robert, Vangel, Sandor, Vasas, Szilard, Zsom, Marianna, Abraham, Oomman, Bhushan, Raju Sree, Deepak, Dewan, Edwin, Fernando M., Gopalakrishnan, Natarajan, Gracious, Noble, Hansraj, Alva, Jain, Dinesh, Keshavamurthy, C.B., Khullar, Dinesh, Manisha, Sahay, Peringat, Jayameena, Prasad, Narayan, Satyanarayana, Rao K., Sreedhar, Reddy, Sreelatha, Melemadathil, Sudhakar, Bhimavarapu, Chandra Vyasam, Ramesh, Bonadonna, Riccardo, Castellino, Pietro, Ceriello, Antonio, Chiovato, Luca, De Cosmo, Salvatore, Derosa, Giuseppe, Di Carlo, Alberto, Di Cianni, Graziano, Frascà, Giovanni, Fuiano, Giorgio, Gambaro, Giovanni, Garibotto, Giacomo, Giorda, Carlo, Malberti, Fabio, Mandreoli, Marcora, Mannucci, Edoardo, Orsi, Emanuela, Piatti, Piermarco, Santoro, Domenico, Sasso, Ferdinando Carlo, Serviddio, Gaetano, Stella, Andrea, Trevisan, Roberto, Veronelli, Anna Maria, Zanoli, Luca, Akiyama, Hitoshi, Aoki, Hiromi, Asano, Akimichi, Iitsuka, Tadashi, Kajiyama, Shizuo, Kashine, Susumu, Kawada, Toshio, Kodera, Takamoto, Kono, Hiroshi, Koyama, Kazunori, Kumeda, Yasuro, Miyauchi, Shozo, Mizuyama, Kazuyuki, Niiya, Tetsuji, Oishi, Hiroko, Ota, Satoshi, Sakakibara, Terue, Takai, Masahiko, Tomonaga, Osamu, Tsujimoto, Mitsuru, Wakasugi, Masakiyo, Wakida, Yasushi, Watanabe, Takayuki, Yamada, Masayo, Yanagida, Kazuhiro, Yanase, Toshihiko, Yumita, Wataru, Gaupsiene, Egle, Kozloviene, Dalia, Navickas, Antanas, Urbanaviciene, Egle, Abdul Ghani, Rohana, Kadir, Khalid Abdul, Ali, Norsiah, Che Yusof, Mohd Daud, Gan, Chye Lee, Ismail, Mastura, Kong, Wei Yen, Lam, Swee Win, Lee, Li Yuan, Loh, Chek Loong, Manocha, Anita Bhajan, Ng, Kee Sing, Ahmad, Nik Nur Fatnoon Nik, Ratnasingam, Vanassa, Shudim, Saiful Shahrizal Bin, Vengadasalam, Paranthaman, Abraira Munoz, Luis David, Salazar, Melchor Alpizar, Cruz, Juan Baas, Soto, Mario Burgos, Ramos, Jose Chevaile, Wong, Alfredo Chew, Correa Rotter, Jose Ricardo, Escalante, Tonatiu Diaz, Enriquez Sosa, Favio Edmundo, Lozano, Fernando Flores, Flota Cervera, Luis Fernando, Baron, Paul Frenk, Ballesteros, Cecilia Garcia, Gomez Rangel, Jose David, Herrera Jimenez, Luis Enrique, Irizar Santana, Sergio Saul, Flores, Fernando Jimenez, Molina, Hugo Laviada, Luna Ceballos, Rosa Isela, del Campo Blanco, Belia Martin, Franco, Guadalupe Morales, Moreno Loza, Oscar Tarsicio, Rocha, Cynthia Mustieles, Vera, Gregorio Obrador, Castellanos, Ricardo Orozco, Calcaneo, Juan Peralta, Reyes Rosano, Miguel Angel, Pattzi, Hiromi Rodriguez, Guzman, Juan Rosas, Rucker Joerg, Isabel Erika, Saavedra Sanchez, Sandra Berenice, Sanchez Mijangos, Jose Hector, Sanson, Pablo Serrano, Tamayo y Orozco, Juan Alfredo, Chavez, Eloisa Tellez, Cepeda, Alejandro Valdes, Carrillo, Luis Venegas, Mesa, Juan Villagordoa, Escobedo, Rolando Zamarripa, Baker, John, Noonan, Paul, Scott, Russell, Walker, Robert, Watson, Edward, Williams, Michael, Young, Simon, Abejuela, Zaynab, Agra, Jeimeen, Aquitania, Grace, Caringal, Clodoaido, Comia, Rhea Severina, Santos, Lalaine Delos, Gomez, Olivert, Jimeno, Cecilia, Tan, Gerry, Tolentino, Marsha, Yao, Christy, Yap, Yvette Ethel, Lallaine Ygpuara, Ma. Dovie, Bijata-Bronisz, Renata, Hotlos, Lucyna, Januszewicz, Andrzej, Kaczmarek, Barbara, Kaminska, Anna, Lazuka, Lech, Madej, Andrzej, Mazur, Stanislaw, Mlodawska-Choluj, Dorota, Nowicki, Michal, Orlowska-Kowalik, Grazyna, Popenda, Grazyna, Rewerska, Barbara, Sowinski, Dariusz, Angelescu, Liliana Monica, Anghel, Veronica, Avram, Rodica-Ioana, Busegeanu, Mihaela-Magdalena, Cif, Adriana, Cosma, Dana, Crisan, Carmen, Demian, Luiza Despina, Ferariu, Ioana Emilia, Halmagyi, Ildiko, Hancu, Nicolae, Munteanu, Mircea, Negru, Doru, Onaca, Adriana Gabriela, Petrica, Ligia, Popa, Amorin Remus, Ranetti, Aurelian-Emil, Serafinceanu, Cristian, Toarba, Cristina, Agafyina, Alina, Barbarash, Olga, Barysheva, Olga, Chizhov, Daniil, Dobronravov, Vladimir, Glinkina, Irina, Grineva, Elena, Khirmanov, Vladimir, Kolmakova, Elena, Koroleva, Tatiana, Kvitkova, Liudmila, Marasaev, Viacheslav, Mkrtumyan, Ashot, Morugova, Tatiana, Nagibovich, Galina, Nagibovich, Oleg, Nedogoda, Sergei, Osipova, Irina, Raskina, Tatiana, Samoylova, Yulia, Sazonova, Olga, Shamkhalova, Minara, Shutemova, Elena, Shwartz, Yuriy, Uriasyev, Oleg, Vorobyev, Sergey, Zateyshchikova, Anna, Zateyshshikov, Dmitry, Zykova, Tatyana, Antic, Slobodan, Djordjevic, Miodrag, Kendereski, Aleksandra, Lalic, Katarina, Lalic, Nebojsa, Popovic-Radinovic, Vesna, Babikova, Jana, Benusova, Olga, Buganova, Ingrid, Culak, Jan, Dzupina, Andrej, Dzuponova, Jana, Fulop, Peter, Ilavska, Adriana, Martinka, Emil, Ochodnicka, Zuzana, Pella, Daniel, Smatanova, Iveta, Ahmed, Fayzal, Badat, Aysha, Breedt, Johannes, Distiller, Lawrence, Govender, Vimladhevi, Govender, Ravendran, Joshi, Mukesh, Jurgens, Jaco, Latiff, Gulam, Lombard, Landman, Mookadam, Mohamed, Ngcakani, Nomangesi, Nortje, Hendrik, Oosthuizen, Helena, Pillay-Ramaya, Larisha, Prozesky, Hans, Reddy, Jeevren, Rheeder, Paul, Seeber, Mary, Cho, Young Min, Jeong, In-Kyung, Kim, Sin Gon, Kim, Yeong Hoon, Kwon, Hyuk-Sang, Kwon, Min Jeong, Lee, Byung-Wan, Lee, JungEun, Lee, Moon-Kyu, Nam, Moon-Suk, Oh, Kook-Hwan, Park, Cheol- Young, Park, Sun-Hee, Yoon, Kun Ho, Garcia, Pere Alvarez, Mercadal, Luis Asmarats, Barrios, Clara, Castro, Fernando Cereto, Guldris, Secundino Cigarran, Lopez, Marta Dominguez, Egido de los Rios, Jesus, Fresnedo, Gema Fernandez, Serrano, Antonio Galan, Garcia, Isabel, Gonzalez Martinez, Francisco Javier, Jodar Gimeno, Jose Esteban, Mendoza, Manuel Lopez, Marin, Tamara Malek, Portillo, Cristobal Morales, Munar Vila, Maria Antonia, Torres, Manuel Muñoz, Iglesias, Javier Nieto, Perez, Jonay Pantoja, Vera, Merce Perez, Portoles Perez, Jose M., Quesada Simón, María Angustias, Canonge, Rafael Simo, Gonzalez, Alfonso Soto, Riera, Manel Terns, Tinahones Madueno, Francisco Jose, Plaza, Mercedes Velo, Chang, Chwen-Tzuei, Chuang, Lee-Ming, Hsia, Te-Lin, Hsieh, Chang-Hsun, Lin, Chih-Ching, Lu, Yung- Chuan, Sheu, Wayne H-H, Barna, Olga, Bilyk, Svitlana D., Botsyurko, Volodymyr, Dudar, Iryna, Fushtey, Ivan, Godlevska, Olga, Golovchenko, Oleksandr, Gyrina, Olga, Kazmirchuk, Anatoliy, Komisarenko, Iuliia, Korzh, Oleksii, Kravchun, Nonna, Legun, Oleg, Mankovskyy, Borys, Martynyuk, Liliya, Mostovoy, Yuriy, Pashkovska, Nataliia, Pererva, Larysa, Pertseva, Tetyana, Samoylov, Oleksandr, Smirnov, Ivan, Svyshchenko, Yevgeniya, Tomashkevych, Halyna, Topchii, Ivan, Tryshchuk, Nadiya, Tseluyko, Vira, Vizir, Vadym, Vlasenko, Maryna, Zlova, Tetiana, Zub, Liliia, Abusnana, Salah, Railey, Mohamed, Abouglila, Kamal, Ainsworth, Paul, Ali, Zishan, Arutchelvam, Vijayaraman, Barnard, Maria, Bellary, Srikanth, Davies, Emyr, Davies, Mark, Davies, Simon, Dawson, Alison, El Kossi, Mohsen, English, Patrick, Fraser, Donald, Gnudi, Luigi, Gunstone, Anthony, Hall, Timothy, Hanif, Wasim, Jackson, Alan, Johnson, Andrew, Joseph, Franklin, Krishnan, Singhan, Kumwenda, Mick, MacDougall, Iain, Nixon, Paul, O'Hare, Joseph, Philip, Sam, Ramtoola, Shenaz, Saxena, Manish, Sennik, Davesh, Simon, Godwin, Singh, Baldev, Stephens, Jeffrey, Strzelecka, Anna, Symonds, Rehan, Turner, Wayne, Wahba, Mona, Wakeling, John, Wheeler, David, Winocour, Peter, Abdallah, Joseph, Abdullah, Raied, Abramowitz, Matthew, Acosta, Idalia, Aiello, Joseph, Akright, Laura, Akyea-Djamson, Ayim, Alappan, Rajendran, Alicic, Radica, Al-Karadsheh, Amer, Allison, Dale Crawford, Arauz-Pacheco, Carlos, Arfeen, Shahabul, Arif, Ahmed, Arvind, Moogali, Atray, Naveen, Awad, Ahmed, Barnhill, Peggy, Barranco, Elizabeth, Barrera, Carlos, Beacom, Matthew, Behara, Venkata, Belo, Diogo, Bentley-Lewis, Rhonda, Berenguer, Ramon, Bermudez, Lidia, Bernardo, Marializa, Biscoveanu, Mihaela, Bowman-Stroud, Cynthia, Brandon, Donald, Brusco, Osvaldo, Busch, Robert, Canaan, Yamil, Chilito, Alicia, Christensen, Tom, Christiano, Cynthia, Christofides, Elena, Chuateco, Caroucel, Cohen, Kenneth, Cohen, Robert, Cohen-Stein, Debbie, Cook, Charles, Coyne, Daniel, Daboul, Nizar, Darwish, Riad, Daswani, Adarsh, Deck, Kenneth, Desouza, Cyrus, Dev, Devasmita, Dhillon, Monika, Dua, Sohan, Eder, Frank, Elosegui, Ana Maria, El-Shahawy, Mohamed, Ervin, John, Esquenazi, Alberto, Evans, John, Fishbane, Steven, Frias, Juan, Galindo-Ramos, Eugenia, Galphin, Claude, Ghazi, Adline, Gonzalez, Enrique, Gorson, David, Gowda, Anupama, Greco, Barbara, Grubb, Stephen, Gulati, Rakesh, Hammoud, Jamal, Handelsman, Stuart, Hartman, Israel, Hershon, Kenneth, Hiser, Daniel, Hon, George, Jacob, Radu, Jaime, Maria, Jamal, Aamir, Kaupke, Charles, Keightley, Gerald, Kern, Elizabeth, Khanna, Rakhi, Khitan, Zeid, Kim, Sun, Kopyt, Nelson, Kovesdy, Csaba, Krishna, Gopal, Kropp, Jeffrey (Jay), Kumar, Amrendra, Kumar, Jayant, Kumar, Neil, Kusnir, Jorge, Lane, Wendy, Lawrence, Mary, Lehrner, Lawrence, Lentz, John, Levinson, Dennis, Lewis, Derek, Liss, Kenneth, Maddux, Andreas, Maheshwari, Hiralal, Mandayam, Sreedhar, Marar, Isam, Mehta, Bhasker, Middleton, John, Mordujovich, Jorge, Moreda, Ramon, Moustafa, Moustafa, Trenche, Samuel Mujica, Narayanan, Mohanram, Narvarte, Javier, Nassar, Tareq, Newman, George, Nichol, Brian, Nicol, Philip, Nisnisan, Josier, Nossuli, A. Kaldun, Obialo, Chamberlain, Olelewe, Sarah, Oliver, Michael, O'Shaughnessy, Andrew, Padron, John, Pankhaniya, Rohit, Parker, Reginald, Patel, Devesh, Patel, Gnyandev, Patel, Nina, Pavon, Humberto, Perez, Armando, Perez, Carlos, Perlman, Alan, Pettis, Karlton, Pharr, Walter, Phillips, Andrea, Purighalla, Raman, Quesada-Suarez, Luis, Ranjan, Rajiv, Rastogi, Sanjeev, Reddy, Jakkidi, Rendell, Marc, Rich, Lisa, Robinson, Michael, Rodriguez, Hector, Rosas, Sylvia, Saba, Fadi, Sankaram, Rallabhandi, Sarin, Ravi, Schreiman, Robert, Scott, David, Sekkarie, Mohamed, Sensenbrenner, John, Shakeel, Muhammad, Shanik, Michael, Shaw, Sylvia, Smith, Stephen, Solomon, Richard, Sprague, Amy, Spry, Leslie, Suchinda, Pusadee, Sultan, Senan, Surampudi, Prasanth, Sussman, Sherry, Tan, Anjanette, Terrelonge, Antonio, Thompson, Michael, Trespalacios, Fernando, Trippe, Bruce, Trueba, Pilar, Twahirwa, Marcel, Updegrove, John, Van Buren, Peter, Vannorsdall, Mark, Varghese, Freemu, Velasquez-Mieyer, Pedro, Ventrapragada, Sailaja, Vukotic, Goga, Wadud, Khurram, Warren, Mark, Watson, Henry, Watts, Ronald, Weiner, Daniel, Welker, James, Welsh, Jean, Williams, Shelley, Zaniewski-Singh, Michelle, Yi, Tae Won, Smyth, Brendan, Di Tanna, Gian Luca, Arnott, Clare, Cardoza, Kathryn, and Kang, Amy

Published
2023
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3. A dark matter profile to model diverse feedback-induced core sizes of ACDM haloes

Author

Lazar, A, Bullock, JS, Boylan-Kolchin, M, Chan, TK, Hopkins, PF, Graus, AS, Wetzel, A, El-Badry, K, Wheeler, C, Straight, MC, Keres, D, Faucher-Giguère, CA, Fitts, A, and Garrison-Kimmel, S

Subjects
galaxies: evolution, galaxies: formation, dark matter, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We analyse the cold dark matter density profiles of 54 galaxy haloes simulated with Feedback In Realistic Environments (FIRE)-2 galaxy formation physics, each resolved within 0.5 per cent of the halo virial radius. These haloes contain galaxies with masses that range from ultrafaint dwarfs (M* ~ 104.5M) to the largest spirals (M* ˜ 1011M) and have density profiles that are both cored and cuspy. We characterize our results using a new, analytic density profile that extends the standard two-parameter Einasto form to allow for a pronounced constant density core in the resolved innermost radius. With one additional core-radius parameter, rc, this three-parameter core-Einasto profile is able to characterize our feedback-impacted dark matter haloes more accurately than other three-parameter profiles proposed in the literature. To enable comparisons with observations, we provide fitting functions for rc and other profile parameters as a function of both M* and M/Mhalo. In agreement with past studies, we find that dark matter core formation is most efficient at the characteristic stellar-to-halo mass ratio M/Mhalo ˜5 × 10-3, or M* ˜ 109 M, with cores that are roughly the size of the galaxy half-light radius, rc ˜ 15kpc. Furthermore, we find no evidence for core formation at radii > 100 pc in galaxies with M*/Mhalo < 5 × 10-4 or M*-106M. For Milky Way-size galaxies, baryonic contraction often makes haloes significantly more concentrated and dense at the stellar half-light radius than DMO runs. However, even at the Milky Way scale, FIRE-2 galaxy formation still produces small dark matter cores of ˜ 0.5-2 kpc in size. Recent evidence for a ~2 kpc core in the Milky Way's dark matter halo is consistent with this expectation.

Published
2020

4. Be it therefore resolved: Cosmological simulations of dwarf galaxies with 30 solar mass resolution

Author

Wheeler, C, Hopkins, PF, Pace, AB, Garrison-Kimmel, S, Boylan-Kolchin, M, Wetzel, A, Bullock, JS, Kereš, D, Faucher-Giguère, CA, and Quataert, E

Subjects
galaxies: dwarf, galaxies: formation, galaxies: kinematics and dynamics, Local Group, galaxies: star formation, astro-ph.GA, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We study a suite of extremely high-resolution cosmological Feedback in Realistic Environments simulations of dwarf galaxies (Mhalo ≲ 1010 M☉), run to z = 0 with 30 M☉ resolution, sufficient (for the first time) to resolve the internal structure of individual supernovae remnants within the cooling radius. Every halo with Mhalo ≳ 108.6 M☉ is populated by a resolved stellar galaxy, suggesting very low-mass dwarfs may be ubiquitous in the field. Our ultra-faint dwarfs (UFDs; M∗ < 105 M☉) have their star formation (SF) truncated early (z ≳ 2), likely by reionization, while classical dwarfs (M∗ > 105 M☉) continue forming stars to z < 0.5. The systems have bursty star formation histories, forming most of their stars in periods of elevated SF strongly clustered in both space and time. This allows our dwarf with M∗/Mhalo > 10−4 to form a dark matter core >200 pc, while lower mass UFDs exhibit cusps down to ≲100 pc, as expected from energetic arguments. Our dwarfs with M∗ > 104 M☉ have half-mass radii (R1/2) in agreement with Local Group (LG) dwarfs (dynamical mass versus R1/2 and stellar rotation also resemble observations). The lowest mass UFDs are below surface brightness limits of current surveys but are potentially visible in next-generation surveys (e.g. LSST). The stellar metallicities are lower than in LG dwarfs; this may reflect pre-enrichment of the LG by the massive hosts or Pop-III stars. Consistency with lower resolution studies implies that our simulations are numerically robust (for a given physical model).

Published
2019

5. Nebular Spectroscopy of the `Blue Bump' Type Ia Supernova 2017cbv

Author

Sand, D. J., Graham, M. L., Botyánszki, J., Hiramatsu, D., McCully, C., Valenti, S., Hosseinzadeh, G., Howell, D. A., Burke, J., Cartier, R., Diamond, T., Hsiao, E. Y., Jha, S. W., Kasen, D., Kumar, S., Marion, G. H., Suntzeff, N., Tartaglia, L., Wheeler, C., and Wyatt, S.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present nebular phase optical and near-infrared spectroscopy of the Type Ia supernova (SN) 2017cbv. The early light curves of SN~2017cbv showed a prominent blue bump in the $U$, $B$ and $g$ bands lasting for $\sim$5 d. One interpretation of the early light curve was that the excess blue light was due to shocking of the SN ejecta against a nondegenerate companion star -- a signature of the single degenerate scenario. If this is the correct interpretation, the interaction between the SN ejecta and the companion star could result in significant H$\alpha$ (or helium) emission at late times, possibly along with other species, depending on the companion star and its orbital separation. A search for H$\alpha$ emission in our +302 d spectrum yields a nondetection, with a $L_{H\alpha}$$<$8.0$\times$10$^{35}$ erg/s (given an assumed distance of $D$=12.3 Mpc), which we have verified by implanting simulated H$\alpha$ emission into our data. We make a quantitative comparison to models of swept-up material stripped from a nondegenerate companion star, and limit the mass of hydrogen that might remain undetected to $M_{\rm H} < 1 \times 10^{-4}$ $\rm M_{\odot}$. A similar analysis of helium star related lines yields a $M_{\rm He} < 5 \times 10^{-4}$ $\rm M_{\odot}$. Taken at face value, these results argue against a nondegenerate H or He-rich companion in Roche lobe overflow as the progenitor of SN 2017cbv. Alternatively, there could be weaknesses in the envelope-stripping and radiative transfer models necessary to interpret the strong H and He flux limits., Comment: 11 pages, 3 figures, 2 tables. ApJ accepted

Published
2018
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6. Star formation histories of dwarf galaxies in the FIRE simulations: Dependence on mass and Local Group environment

Author

Garrison-Kimmel, S, Wetzel, A, Hopkins, PF, Sanderson, R, El-Badry, K, Graus, A, Chan, TK, Feldmann, R, Boylan-Kolchin, M, Hayward, CC, Bullock, JS, Fitts, A, Samuel, J, Wheeler, C, Kereš, D, and Faucher-Giguère, CA

Subjects
galaxies: dwarf, galaxies: formation, Local Group, cosmology: theory, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We study star formation histories (SFHs) of 500 dwarf galaxies (stellar mass M∗ = 105–109 M) from FIRE-2 cosmological zoom-in simulations. We compare dwarfs around individual Milky Way (MW)-mass galaxies, dwarfs in Local Group (LG)-like environments, and true field (i.e. isolated) dwarf galaxies. We reproduce observed trends wherein higher mass dwarfs quench later (if at all), regardless of environment. We also identify differences between the environments, both in terms of ‘satellite versus central’ and ‘LG versus individual MW versus isolated dwarf central.’ Around the individual MW-mass hosts, we recover the result expected from environmental quenching: central galaxies in the ‘near field’ have more extended SFHs than their satellite counterparts, with the former more closely resemble isolated (true field) dwarfs (though near-field centrals are still somewhat earlier forming). However, this difference is muted in the LG-like environments, where both near-field centrals and satellites have similar SFHs, which resemble satellites of single MW-mass hosts. This distinction is strongest for M∗ = 106–107 M but exists at other masses. Our results suggest that the paired halo nature of the LG may regulate star formation in dwarf galaxies even beyond the virial radii of the MW and Andromeda. Caution is needed when comparing zoom-in simulations targeting isolated dwarf galaxies against observed dwarf galaxies in the LG.

Published
2019

7. FIRE-2 simulations: Physics versus numerics in galaxy formation

Author

Hopkins, PF, Wetzel, A, Kereš, D, Faucher-Giguère, CA, Quataert, E, Boylan-Kolchin, M, Murray, N, Hayward, CC, Garrison-Kimmel, S, Hummels, C, Feldmann, R, Torrey, P, Ma, X, Anglés-Alcázar, D, Su, KY, Orr, M, Schmitz, D, Escala, I, Sanderson, R, Grudić, MY, Hafen, Z, Kim, JH, Fitts, A, Bullock, JS, Wheeler, C, Chan, TK, Elbert, OD, and Narayanan, D

Subjects
methods: numerical, stars: formation, galaxies: active, galaxies: evolution, galaxies: formation, cosmology: theory, astro-ph.GA, astro-ph.CO, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

The Feedback In Realistic Environments (FIRE) project explores feedback in cosmological galaxy formation simulations. Previous FIRE simulations used an identical source code ('FIRE-1') for consistency. Motivated by the development of more accurate numerics - including hydrodynamic solvers, gravitational softening, and supernova coupling algorithms - and exploration of new physics (e.g. magnetic fields), we introduce 'FIRE-2', an updated numerical implementation of FIRE physics for the GIZMO code. We run a suite of simulations and compare against FIRE-1: overall, FIRE-2 improvements do not qualitatively change galaxy-scale properties. We pursue an extensive study of numerics versus physics. Details of the star formation algorithm, cooling physics, and chemistry have weak effects provided that we include metal-line cooling and star formation occurs at higher-than-mean densities. We present new resolution criteria for high-resolution galaxy simulations. Most galaxy-scale properties are robust to numerics we test, provided: (1) Toomre masses are resolved; (2) feedback coupling ensures conservation, and (3) individual supernovae are time-resolved. Stellar masses and profiles are most robust to resolution, followed by metal abundances and morphologies, followed by properties of winds and circum-galactic media. Central (~kpc) mass concentrations in massive (> L*) galaxies are sensitive to numerics (via trapping/recycling of winds in hot haloes). Multiple feedback mechanisms play key roles: supernovae regulate stellar masses/winds; stellar mass-loss fuels late star formation; radiative feedback suppresses accretion on to dwarfs and instantaneous star formation in discs. We provide all initial conditions and numerical algorithms used.

Published
2018

8. No assembly required: Mergers are mostly irrelevant for the growth of low-mass dwarf galaxies

Author

Fitts, A, Boylan-Kolchin, M, Bullock, JS, Weisz, DR, El-Badry, K, Wheeler, C, Faucher-Giguère, CA, Quataert, E, Hopkins, PF, Kereš, D, Wetzel, A, and Hayward, CC

Subjects
galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: star formation, galaxies: structure dark matter, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We investigate the merger histories of isolated dwarf galaxies based on a suite of 15 highresolution cosmological zoom-in simulations, all with masses of Mhalo ≈ 1010M⊙ (and M* ~ 105 - 107M⊙) at z= 0, from the Feedback in Realistic Environments project. The stellar populations of these dwarf galaxies at z= 0 are formed essentially entirely 'in situ': over 90 per cent of the stellar mass is formed in the main progenitor in all but two cases, and all 15 of the galaxies have > 70 per cent of their stellar mass formed in situ. Virtually all galaxy mergers occur prior to z~ 3, meaning that accreted stellar populations are ancient. On average, our simulated dwarfs undergo five galaxy mergers in their lifetimes, with typical pre-merger galaxy mass ratios that are less than 1:10. This merger frequency is generally comparable to what has been found in dissipationless simulations when coupled with abundance matching. Two of the simulated dwarfs have a luminous satellite companion at z= 0. These ultra-faint dwarfs lie at or below current detectability thresholds but are intriguing targets for nextgeneration facilities. The small contribution of accreted stars makes it extremely difficult to discern the effects of mergers in the vast majority of dwarfs either photometrically or using resolved-star colour-magnitude diagrams (CMDs). The important implication for near-field cosmology is that star formation histories (SFHs) of comparably massive galaxies derived from resolved CMDs should trace the build-up of stellar mass in one main system across cosmic time as opposed to reflecting the contributions of many individual SFHs of merged dwarfs.

Published
2018

9. Modelling chemical abundance distributions for dwarf galaxies in the Local Group: The impact of turbulent metal diffusion

Author

Escala, I, Wetzel, A, Kirby, EN, Hopkins, PF, Ma, X, Wheeler, C, Kereš, D, Faucher-Giguère, CA, and Quataert, E

Subjects
diffusion, methods: numerical, galaxies: abundances, galaxies: dwarf, Local Group, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We investigate stellar metallicity distribution functions (MDFs), including Fe and a-element abundances, in dwarf galaxies from the Feedback in Realistic Environment (FIRE) project. We examine both isolated dwarf galaxies and those that are satellites of a MilkyWay-mass galaxy. In particular, we study the effects of including a sub-grid turbulent model for the diffusion of metals in gas. Simulations that include diffusion have narrower MDFs and abundance ratio distributions, because diffusion drives individual gas and star particles towards the average metallicity. This effect provides significantly better agreement with observed abundance distributions in dwarf galaxies in the Local Group, including small intrinsic scatter in [α/Fe] versus [Fe/H] of ≲0.1 dex. This small intrinsic scatter arises in our simulations because the interstellar medium in dwarf galaxies is well mixed at nearly all cosmic times, such that stars that form at a given time have similar abundances to ≲0.1 dex. Thus, most of the scatter in abundances at z = 0 arises from redshift evolution and not from instantaneous scatter in the ISM. We find similar MDF widths and intrinsic scatter for satellite and isolated dwarf galaxies, which suggests that environmental effects play a minor role compared with internal chemical evolution in our simulations. Overall, with the inclusion of metal diffusion, our simulations reproduce abundance distribution widths of observed low-mass galaxies, enabling detailed studies of chemical evolution in galaxy formation.

Published
2018

11. FIRE in the field: Simulating the threshold of galaxy formation

Author

Fitts, A, Boylan-Kolchin, M, Elbert, OD, Bullock, JS, Hopkins, PF, Oñorbe, J, Wetzel, A, Wheeler, C, Faucher-Giguère, CA, Kereš, D, Skillman, ED, and Weisz, DR

Subjects
galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: star formation, galaxies: structure, dark matter, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We present a suite of 15 cosmological zoom-in simulations of isolated dark matter haloes, all with masses of Mhalo ≈ 1010M⊙ at z = 0, in order to understand the relationship among halo assembly, galaxy formation and feedback's effects on the central density structure in dwarf galaxies. These simulations are part of the Feedback in Realistic Environments (FIRE) project and are performed at extremely high resolution (mbaryon = 500M⊙, mdm = 2500M⊙). The resultant galaxies have stellar masses that are consistent with rough abundance matching estimates, coinciding with the faintest galaxies that can be seen beyond the virial radius of the Milky Way (M*/M⊙ ≈ 105 - 107). This non-negligible spread in stellar mass at z = 0 in haloes within a narrow range of virial masses is strongly correlated with central halo density or maximum circular velocity Vmax, both of which are tightly linked to halo formation time. Much of this dependence of M* on a second parameter (beyond Mhalo) is a direct consequence of the Mhalo ~ 1010M⊙ mass scale coinciding with the threshold for strong reionization suppression: the densest, earliest-forming haloes remain above the UV-suppression scale throughout their histories while late-forming systems fall below the UV-suppression scale over longer periods and form fewer stars as a result. In fact, the latest-forming, lowest-concentration halo in our suite fails to form any stars. Haloes that form galaxies with M ≳ 2 × 106 M⊙ have reduced central densities relative to dark-matter-only simulations, and the radial extent of the density modifications is well-approximated by the galaxy half-mass radius r1/2. Lower-mass galaxies do not modify their host dark matter haloes at the mass scale studied here. This apparent stellar mass threshold of M ≈ 2 × 106-2 × 10-4 Mhalo is broadly consistent with previous work and provides a testable prediction of FIRE feedback models in Λcold dark matter.

Published
2017

14. Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples

Author

Betoule, M., Kessler, R., Guy, J., Mosher, J., Hardin, D., Biswas, R., Astier, P., El-Hage, P., Konig, M., Kuhlmann, S., Marriner, J., Pain, R., Regnault, N., Balland, C., Bassett, B. A., Brown, P. J., Campbell, H., Carlberg, R. G., Cellier-Holzem, F., Cinabro, D., Conley, A., D'Andrea, C. B., DePoy, D. L., Doi, M., Ellis, R. S., Fabbro, S., Filippenko, A. V., Foley, R. J., Frieman, J. A., Fouchez, D., Galbany, L., Goobar, A., Gupta, R. R., Hill, G. J., Hlozek, R., Hogan, C. J., Hook, I. M., Howell, D. A., Jha, S. W., Guillou, L. Le, Leloudas, G., Lidman, C., Marshall, J. L., Möller, A., Mourão, A. M., Neveu, J., Nichol, R., Olmstead, M. D., Palanque-Delabrouille, N., Perlmutter, S., Prieto, J. L., Pritchet, C. J., Richmond, M., Riess, A. G., Ruhlmann-Kleider, V., Sako, M., Schahmaneche, K., Schneider, D. P., Smith, M., Sollerman, J., Sullivan, M., Walton, N. A., and Wheeler, C. J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present cosmological constraints from a joint analysis of type Ia supernova (SN Ia) observations obtained by the SDSS-II and SNLS collaborations. The data set includes several low-redshift samples (z<0.1), all 3 seasons from the SDSS-II (0.05 < z < 0.4), and 3 years from SNLS (0.2

Published
2014
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16. The mass dependence of satellite quenching in Milky Way-like haloes

Author

Phillips, JI, Wheeler, C, Cooper, MC, Boylan-Kolchin, M, Bullock, JS, and Tollerud, E

Subjects
galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: star formation, galaxies: statistics, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

Using the Sloan Digital Sky Survey, we examine the quenching of satellite galaxies around isolated Milky Way-like hosts in the local Universe. We find that the efficiency of satellite quenching around isolated galaxies is low and roughly constant over two orders of magnitude in satellite stellar mass (M* = 108.5-1010.5M), with only ~20 per cent of systems quenched as a result of environmental processes. While largely independent of satellite stellar mass, satellite quenching does exhibit clear dependence on the properties of the host. We show that satellites of passive hosts are substantially more likely to be quenched than those of star-forming hosts, and we present evidence that more massive haloes quench their satellites more efficiently. These results extend trends seen previously in more massive host haloes and for higher satellite masses. Taken together, it appears that galaxies with stellar masses larger than about 108M are uniformly resistant to environmental quenching, with the relative harshness of the host environment likely serving as the primary driver of satellite quenching. At lower stellarmasses (

Published
2015

17. Sweating the small stuff: Simulating dwarf galaxies, ultra-faint dwarf galaxies, and their own tiny satellites

Author

Wheeler, C, Oñorbe, J, Bullock, JS, Boylan-Kolchin, M, Elbert, OD, Shea Garrison-Kimmel, M, Hopkins, PF, and Kereš, D

Subjects
galaxies: dwarf, galaxies: groups: general, Local Group, galaxies: star formation, astro-ph.GA, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

We present Feedback in Realistic Environment (FIRE)/GIZMO hydrodynamic zoom-in simulations of isolated dark matter haloes, two each at the mass of classical dwarf galaxies (Mvir ≃ 1010 M o˙) and ultra-faint galaxies (Mvir ≃ 109 M o˙), and with two feedback implementations. The resulting central galaxies lie on an extrapolated abundance matching relation from M* ≃ 106 to 104 M o˙ without a break. Every host is filled with subhaloes, many of which form stars. Each of our dwarfs with M* ≃ 106 M o˙ has 1-2 well-resolved satellites with M* = 3-200 × 103 M o˙. Even our isolated ultra-faint galaxies have star-forming subhaloes. If this is representative, dwarf galaxies throughout the Universe should commonly host tiny satellite galaxies of their own. We combine our results with the Exploring the Local Volume in Simulations (ELVIS) simulations to show that targeting ~50 kpc regions around nearby isolated dwarfs could increase the chances of discovering ultra-faint galaxies by ~35 per cent compared to random pointings, and specifically identify the region around the Phoenix dwarf galaxy as a good potential target. The well-resolved ultra-faint galaxies in our simulations (M* ≃ 3-30 × 103 M o˙) form within Mpeak ≃ 0.5-3 × 109 M o˙ haloes. Each has a uniformly ancient stellar population (>10 Gyr) owing to reionization-related quenching. More massive systems, in contrast, all have late-time star formation. Our results suggest that Mhalo ≃ 5 × 109 M o˙ is a probable dividing line between haloes hosting reionization 'fossils' and those hosting dwarfs that can continue to form stars in isolation after reionization.

Published
2015

18. The surprising inefficiency of dwarf satellite quenching

Author

Wheeler, C, Phillips, JI, Cooper, MC, Boylan-Kolchin, M, and Bullock, JS

Subjects
galaxies: dwarf, galaxies: evolution, galaxies: formation, galaxies: star formation, astro-ph.GA, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We study dwarf satellite galaxy quenching using observations from the Geha et al. NASASloan Atlas/SDSS catalogue together with {n-ary logical and} cold dark matter cosmological simulations to facilitate selection and interpretation. We show that fewer than 30 per cent of dwarfs (M* ≃ 108.5-9.5M⊙) identified as satellites within massive host haloes (Mhost ≃ 1012.5-14M⊙) are quenched, in spite of the expectation from simulations that half of them should have been accreted more than 6 Gyr ago. We conclude that whatever the action triggering environmental quenching of dwarf satellites, the process must be highly inefficient. We investigate a series of simple, one-parameter quenching models in order to understand what is required to explain the low quenched fraction and conclude that either the quenching time-scale is very long (>9.5Gyr, a 'slow starvation' scenario) or that the environmental trigger is not well matched to accretion within the virial volume. We discuss these results in light of the fact that most of the low-mass dwarf satellites in the Local Group are quenched, a seeming contradiction that could point to a characteristic mass scale for satellite quenching. © 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2014

19. Comparative Analysis of Tumor Microbiome, Molecular Profile and Immune Cell Abundance by HPV Status in Head and Neck Cancers and Their Impact on Survival

Author

Upadhyay, R., primary, Dhakal, A., additional, Karivedu, V., additional, Wheeler, C., additional, Hoyd, R., additional, Bhateja, P., additional, Bonomi, M., additional, Valentin, S., additional, Gamez, M.E., additional, Konieczkowski, D.J., additional, Baliga, S., additional, Grecula, J.C., additional, Blakaj, D.M., additional, Gogineni, E., additional, Mitchell, D.L., additional, Denko, N., additional, Jhawar, S.R., additional, and Spakowicz, D., additional

Published
2023
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22. A dichotomy in satellite quenching around L* galaxies

Author

Phillips, JI, Wheeler, C, Boylan-Kolchin, M, Bullock, JS, Cooper, MC, and Tollerud, EJ

Subjects
galaxies: dwarf, galaxies: evolution, cosmology: observations, astro-ph.CO, Astronomy & Astrophysics, Astronomical and Space Sciences
Abstract

We examine the star formation properties of bright (~0.1 L*) satellites around isolated ~L* hosts in the local Universe using spectroscopically confirmed systems in the Sloan Digital Sky Survey Data Release 7. Our selection method is carefully designed with the aid of Nbody simulations to avoid groups and clusters. We find that satellites are significantly more likely to be quenched than a stellarmass-matched sample of isolated galaxies. Remarkably, this quenching occurs only for satellites of hosts that are themselves quenched: while star formation is unaffected in the satellites of star-forming hosts, satellites around quiescent hosts are more than twice as likely to be quenched than stellar-mass-matched field samples. One implication of this is that whatever shuts down star formation in isolated, passive L* galaxies also play at least an indirect role in quenching star formation in their bright satellites. The previously reported tendency for 'galactic conformity' in colour/morphology may be a by-product of this host-specific quenching dichotomy. The Sérsic indices of quenched satellites are statistically identical to those of field galaxies with the same specific star formation rates, suggesting that environmental and secular quenching give rise to the same morphological structure. By studying the distribution of pairwise velocities between the hosts and satellites, we find dynamical evidence that passive host galaxies reside in dark matter haloes that are~45 per cent more massive than those of star-forming host galaxies of the same stellar mass.We emphasize that even around passive hosts, the mere fact that galaxies become satellites does not typically result in star formation quenching: we find that only ~30 per cent of ~0.1L* galaxies that fall in from the field are quenched around passive hosts, compared with ~0 per cent around star-forming hosts. © 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.

Published
2013

23. Broadband Observations of the Afterglow of GRB 000926: Observing the Effect of Inverse Compton Scattering and Evidence for a High-Density Environment

Author

Harrison, F. A., Yost, S. A., Sari, R., Berger, E., Holtzmann, T. J. Galama J., Axelrod, T., Bloom, J. S., Chevalier, R., Costa, E., Diercks, A., Djorgovski, S. G., Frail, D. A., Frontera, F., Hurley, K., Kulkarni, S. R., McCarthy, P., Piro, L., Pooley, G. G., Price, P. A., Reichart, D., Shepard, G. R. Ricker D., Schmidt, B., Walter, F., and Wheeler, C.

Subjects
Astrophysics
Abstract

GRB 000926 has one of the best-studied afterglows to-date, with multiple X-ray observations, as well as extensive multi-frequency optical and radio coverage. Broadband afterglow observations, spanning from X-ray to radio frequencies, provide a probe of the density structure of the circumburst medium, as well as of the ejecta energetics, geometry, and the physical parameters of the relativistic blastwave resulting from the explosion. We present an analysis of {\em Chandra X-ray Observatory} observations of this event, along with {\em Hubble Space Telescope} and radio monitoring. We combine these data with ground-based optical and IR observations and fit the synthesized afterglow lightcurve using models where collimated ejecta expand into a surrounding medium. We find that we can explain the broadband lightcurve with reasonable physical parameters only if the cooling is dominated by inverse Compton scattering. Excess X-ray emission in the broadband spectrum indicates that we are directly observing a contribution from inverse Compton scattering. It is the first time this has been observed in a GRB afterglow, and it implies that the GRB exploded in a reasonably dense (n~30 cm^{-3}) medium, consistent with a diffuse interstellar cloud environment., Comment: 16 pages, 5 figures Accepted for publication in the Astrophysical Journal

Published
2001

24. Explosion Diagnostics of Type Ia Supernovae from Early Infrared Spectra

Author

Wheeler, C. J., Hoeflich, P., Harkness, R., and Spyromillio, J.

Subjects
Astrophysics
Abstract

Models of infrared spectra of Type Ia supernovae around maximum light are presented. The underlying dynamic models are delayed detonation explosions in Chandrasekhar mass carbon/oxygen white dwarfs. In combination with the radiative transport codes employed here, these models provide plausible fits to the optical spectra of "normal" Type Ia supernova. Two independent radiative transport codes are used, one that assumes LTE and one that computes non-LTE excitations and ionization. The models are compared with infrared data available in the literature. The independent codes give a reasonable representation of the data and provide physical explanations for their origin independent of the detailed assumptions of the radiative transfer. The infrared gives an especially powerful diagnostic of the dynamic model because with strongly variable line blanketing opacity it probes different depths within the exploded white dwarf at the same epoch. The velocity of the transition zone between explosive oxygen and carbon burning can be directly determined. The velocity at which the burning to nickel stops can also be probed. These velocities are very sensitive to the explosion physics., Comment: 19 pages, LaTeX, aas2pp4.sty, ApJ

Published
1997

32. Surface pressure measurements on a free-flying cone at mach 7 using pressure sensitive paint

Author

Wheeler, C, Hyslop, A, Vieira, J, Le Page, L, Quinn, MK, Chowdhury, N, and Doherty, L

Abstract

Experiments have been conducted for the first time to investigate the use of binary pressure sensitive paint (PSP) on a free-flying aerodynamic model in the Oxford High Density Tunnel at Mach 7. The model was a 7° half angle cone with a 1.25 mm nose radius and overall length of 250 mm. A binary PSP consisting of a RuDPP3 pressure luminophore and Fluorescein reference luminophore was applied to the model. The model movement and response of the paint were tracked throughout the flight using high-speed videography. The model also featured an on-board inertial measurement unit, thereby providing simultaneous measurement of the aerodynamic forces and surface pressure distribution. The measured surface pressure was compared with analytical and numerical predictions and found to be ≈3kPa higher than expected.

Published
2022

33. Association of Tumor Microbiome and Hypoxia Expression Signatures in Different Anatomic Subsites of Head and Neck Cancer

Author

Dhakal, A., primary, Upadhyay, R., additional, Karivedu, V., additional, Hoyd, R., additional, Wheeler, C., additional, Gamez, M.E., additional, Valentin, S., additional, Vanputten, M., additional, Bhateja, P., additional, Bonomi, M., additional, Konieczkowski, D.J., additional, Baliga, S., additional, Mitchell, D.L., additional, Grecula, J.C., additional, Blakaj, D.M., additional, Jhawar, S.R., additional, and Spakowicz, D., additional

Published
2022
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34. Vaginal Microbiome as a Biomarker of Vaginal Health and Patient-Reported Outcomes in Women Receiving Pelvic Radiation

Author

Quick, A.M., primary, Diaz Pardo, D.A., additional, Miller, E.D., additional, Arnett, A.L.H., additional, Pitter, K.L., additional, Kim, J., additional, Flora, L., additional, Williams, N., additional, Hoyd, R., additional, Wheeler, C., additional, Mo, X., additional, Chambers, L., additional, Spakowicz, D., additional, and Arthur, E., additional

Published
2022
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35. Resiliency among Older Adults Receiving Lung Cancer Treatment (ROAR-LCT, NCT04229381): The feasibility of a novel supportive care intervention with collection of longitudinal gut microbiome specimens and activity tracking during the COVID-19 Pandemic

Author

Presley, C., primary, Grogan, M., additional, Hoyd, R., additional, Compston, A., additional, Hock, K., additional, Knauss, B., additional, Redder, E., additional, Arrato, N., additional, Lo, S., additional, Benedict, J., additional, Janse, S., additional, Hayes, S., additional, Williams, N., additional, Wheeler, C., additional, Carbone, D., additional, Paskett, E., additional, Andersen, B., additional, and Spakowicz, D., additional

Published
2022
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38. EP03.01-014 Results From the BEWELL Study: Black Raspberry Nectar for the Prevention of Lung Cancer (NCT04267874)

Author

BIttoni, M., primary, Bibi, A., additional, Wheeler, C., additional, Williams, N., additional, Hoyd, R., additional, Heitman, K., additional, Webb, M., additional, Grainger, E., additional, Riedl, K., additional, Tabung, F., additional, Vodovotz, Y., additional, Carbone, D., additional, Clinton, S., additional, and Spakowicz, D., additional

Published
2022
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42. In-flight performance of the BLAST-TNG Kinetic Inductance Detector arrays and Readout Electronics

Author

Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., Williams P., Sinclair, A, Gordon, S, Ade, P, Ashton, P, Cho, H, Coppi, G, Corso, A, Devlin, M, Dicker, S, Dober, B, Fissel, L, Galitzky, N, Gao, J, Groppi, C, Hilton, G, Hubmayr, J, Irwin, K, Klein, J, Li, D, Lourie, N, Lowe, I, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pascale, E, Pisano, G, Soler, J, Tucker, C, Underhil, M, Vissers, M, Wheeler, C, Williams, P, Sinclair A., Gordon S. B., Ade P., Ashton P., Cho H. -M., Coppi G., Corso A., Devlin M., Dicker S., Dober B., Fissel L., Galitzky N., Gao J., Groppi C., Hilton G. C., Hubmayr J., Irwin K., Klein J., Li D., Lourie N., Lowe I., Mani H., Mauskopf P. D., McKenney C., Nati F., Novak G., Pascale E., Pisano G., Soler J., Tucker C., Underhil M., Vissers M., Wheeler C., and Williams P.

Published
2020

43. Characterization, deployment, and in-flight performance of the BLAST-TNG cryogenic receiver

Author

Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., Williams P. A., Zmuidzinas J.,Gao J.-R., Lowe, I, Ade, P, Ashton, P, Austermann, J, Coppi, G, Cox, E, Devlin, M, Dober, B, Fanfani, V, Fissel, L, Galitzki, N, Gao, J, Gordon, S, Groppi, C, Hilton, G, Hubmayr, J, Klein, J, Li, D, Lourie, N, Mani, H, Mauskopf, P, Mckenney, C, Nati, F, Novak, G, Pisano, G, Romualdez, J, Soler, J, Sinclair, A, Tucker, C, Ullom, J, Vissers, M, Wheeler, C, Williams, P, Lowe I., Ade P. A. R., Ashton P. C., Austermann J. E., Coppi G., Cox E. G., Devlin M. J., Dober B. J., Fanfani V., Fissel L. M., Galitzki N., Gao J., Gordon S., Groppi C. E., Hilton G. C., Hubmayr J., Klein J., Li D., Lourie N. P., Mani H., Mauskopf P., McKenney C., Nati F., Novak G., Pisano G., Romualdez J., Soler J. D., Sinclair A., Tucker C., Ullom J., Vissers M., Wheeler C., and Williams P. A.

Abstract

The Next Generation Balloon-borne Large Aperture Submillimeter Telescope (BLAST-TNG) is a submillimeter polarimeter designed to map interstellar dust and galactic foregrounds at 250, 350, and 500 microns during a 24-day Antarctic flight. The BLAST-TNG detector arrays are comprised of 918, 469, and 272 MKID pixels, respectively. The pixels are formed from two orthogonally oriented, crossed, linear-polarization sensitive MKID antennae. The arrays are cooled to sub 300 mK temperatures and stabilized via a closed cycle 3He sorption fridge in combination with a 4He vacuum pot. The detectors are read out through a combination of the second-generation Reconfigurable Open Architecture Computing Hardware (ROACH2) and custom RF electronics designed for BLAST-TNG. The firmware and software designed to readout and characterize these detectors was built from scratch by the BLAST team around these detectors, and has been adapted for use by other MKID instruments such as TolTEC and OLIMPO.1 We present an overview of these systems as well as in-depth methodology of the ground-based characterization and the measured in-flight performance.

Published
2020

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