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510 results on '"HAYDEN, BRIAN"'

1. Traditional Corporate Group Economics in Southeast Asia: An Ethnographic Study with Archaeological Implications

Author: Hayden, Brian
Published: 2013
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2. The James Webb Space Telescope Mission

Author: Gardner, Jonathan P., Mather, John C., Abbott, Randy, Abell, James S., Abernathy, Mark, Abney, Faith E., Abraham, John G., Abraham, Roberto, Abul-Huda, Yasin M., Acton, Scott, Adams, Cynthia K., Adams, Evan, Adler, David S., Adriaensen, Maarten, Aguilar, Jonathan Albert, Ahmed, Mansoor, Ahmed, Nasif S., Ahmed, Tanjira, Albat, Rüdeger, Albert, Loïc, Alberts, Stacey, Aldridge, David, Allen, Mary Marsha, Allen, Shaune S., Altenburg, Martin, Altunc, Serhat, Alvarez, Jose Lorenzo, Álvarez-Márquez, Javier, de Oliveira, Catarina Alves, Ambrose, Leslie L., Anandakrishnan, Satya M., Andersen, Gregory C., Anderson, Harry James, Anderson, Jay, Anderson, Kristen, Anderson, Sara M., Aprea, Julio, Archer, Benita J., Arenberg, Jonathan W., Argyriou, Ioannis, Arribas, Santiago, Artigau, Étienne, Arvai, Amanda Rose, Atcheson, Paul, Atkinson, Charles B., Averbukh, Jesse, Aymergen, Cagatay, Bacinski, John J., Baggett, Wayne E., Bagnasco, Giorgio, Baker, Lynn L., Balzano, Vicki Ann, Banks, Kimberly A., Baran, David A., Barker, Elizabeth A., Barrett, Larry K., Barringer, Bruce O., Barto, Allison, Bast, William, Baudoz, Pierre, Baum, Stefi, Beatty, Thomas G., Beaulieu, Mathilde, Bechtold, Kathryn, Beck, Tracy, Beddard, Megan M., Beichman, Charles, Bellagama, Larry, Bely, Pierre, Berger, Timothy W., Bergeron, Louis E., Darveau-Bernier, Antoine, Bertch, Maria D., Beskow, Charlotte, Betz, Laura E., Biagetti, Carl P., Birkmann, Stephan, Bjorklund, Kurt F., Blackwood, James D., Blazek, Ronald Paul, Blossfeld, Stephen, Bluth, Marcel, Boccaletti, Anthony, Boegner Jr., Martin E., Bohlin, Ralph C., Boia, John Joseph, Böker, Torsten, Bonaventura, N., Bond, Nicholas A., Bosley, Kari Ann, Boucarut, Rene A., Bouchet, Patrice, Bouwman, Jeroen, Bower, Gary, Bowers, Ariel S., Bowers, Charles W., Boyce, Leslye A., Boyer, Christine T., Boyer, Martha L., Boyer, Michael, Boyer, Robert, Bradley, Larry D., Brady, Gregory R., Brandl, Bernhard R., Brannen, Judith L., Breda, David, Bremmer, Harold G., Brennan, David, Bresnahan, Pamela A., Bright, Stacey N., Broiles, Brian J., Bromenschenkel, Asa, Brooks, Brian H., Brooks, Keira J., Brown, Bob, Brown, Bruce, Brown, Thomas M., Bruce, Barry W., Bryson, Jonathan G., Bujanda, Edwin D., Bullock, Blake M., Bunker, A. J., Bureo, Rafael, Burt, Irving J., Bush, James Aaron, Bushouse, Howard A., Bussman, Marie C., Cabaud, Olivier, Cale, Steven, Calhoon, Charles D., Calvani, Humberto, Canipe, Alicia M., Caputo, Francis M., Cara, Mihai, Carey, Larkin, Case, Michael Eli, Cesari, Thaddeus, Cetorelli, Lee D., Chance, Don R., Chandler, Lynn, Chaney, Dave, Chapman, George N., Charlot, S., Chayer, Pierre, Cheezum, Jeffrey I., Chen, Bin, Chen, Christine H., Cherinka, Brian, Chichester, Sarah C., Chilton, Zachary S., Chittiraibalan, Dharini, Clampin, Mark, Clark, Charles R., Clark, Kerry W., Clark, Stephanie M., Claybrooks, Edward E., Cleveland, Keith A., Cohen, Andrew L., Cohen, Lester M., Colón, Knicole D., Coleman, Benee L., Colina, Luis, Comber, Brian J., Comeau, Thomas M., Comer, Thomas, Reis, Alain Conde, Connolly, Dennis C., Conroy, Kyle E., Contos, Adam R., Contreras, James, Cook, Neil J., Cooper, James L., Cooper, Rachel Aviva, Correia, Michael F., Correnti, Matteo, Cossou, Christophe, Costanza, Brian F., Coulais, Alain, Cox, Colin R., Coyle, Ray T., Cracraft, Misty M., Noriega-Crespo, Alberto, Crew, Keith A., Curtis, Gary J., Cusveller, Bianca, Maciel, Cleyciane Da Costa, Dailey, Christopher T., Daugeron, Frédéric, Davidson, Greg S., Davies, James E., Davis, Katherine Anne, Davis, Michael S., Day, Ratna, de Chambure, Daniel, de Jong, Pauline, De Marchi, Guido, Dean, Bruce H., Decker, John E., Delisa, Amy S., Dell, Lawrence C., Dellagatta, Gail, Dembinska, Franciszka, Demosthenes, Sandor, Dencheva, Nadezhda M., Deneu, Philippe, DePriest, William W., Deschenes, Jeremy, Dethienne, Nathalie, Detre, Örs Hunor, Diaz, Rosa Izela, Dicken, Daniel, DiFelice, Audrey S., Dillman, Matthew, Disharoon, Maureen O., van Dishoeck, Ewine F., Dixon, William V., Doggett, Jesse B., Dominguez, Keisha L., Donaldson, Thomas S., Doria-Warner, Cristina M., Santos, Tony Dos, Doty, Heather, Douglas Jr., Robert E., Doyon, René, Dressler, Alan, Driggers, Jennifer, Driggers, Phillip A., Dunn, Jamie L., DuPrie, Kimberly C., Dupuis, Jean, Durning, John, Dutta, Sanghamitra B., Earl, Nicholas M., Eccleston, Paul, Ecobichon, Pascal, Egami, Eiichi, Ehrenwinkler, Ralf, Eisenhamer, Jonathan D., Eisenhower, Michael, Eisenstein, Daniel J., Hamel, Zaky El, Elie, Michelle L., Elliott, James, Elliott, Kyle Wesley, Engesser, Michael, Espinoza, Néstor, Etienne, Odessa, Etxaluze, Mireya, Evans, Leah, Fabreguettes, Luce, Falcolini, Massimo, Falini, Patrick R., Fatig, Curtis, Feeney, Matthew, Feinberg, Lee D., Fels, Raymond, Ferdous, Nazma, Ferguson, Henry C., Ferrarese, Laura, Ferreira, Marie-Héléne, Ferruit, Pierre, Ferry, Malcolm, Filippazzo, Joseph Charles, Firre, Daniel, Fix, Mees, Flagey, Nicolas, Flanagan, Kathryn A., Fleming, Scott W., Florian, Michael, Flynn, James R., Foiadelli, Luca, Fontaine, Mark R., Fontanella, Erin Marie, Forshay, Peter Randolph, Fortner, Elizabeth A., Fox, Ori D., Framarini, Alexandro P., Francisco, John I., Franck, Randy, Franx, Marijn, Franz, David E., Friedman, Scott D., Friend, Katheryn E., Frost, James R., Fu, Henry, Fullerton, Alexander W., Gaillard, Lionel, Galkin, Sergey, Gallagher, Ben, Galyer, Anthony D., Marín, Macarena García, Gardner, Lisa E., Garland, Dennis, Garrett, Bruce Albert, Gasman, Danny, Gáspár, András, Gastaud, René, Gaudreau, Daniel, Gauthier, Peter Timothy, Geers, Vincent, Geithner, Paul H., Gennaro, Mario, Gerber, John, Gereau, John C., Giampaoli, Robert, Giardino, Giovanna, Gibbons, Paul C., Gilbert, Karolina, Gilman, Larry, Girard, Julien H., Giuliano, Mark E., Gkountis, Konstantinos, Glasse, Alistair, Glassmire, Kirk Zachary, Glauser, Adrian Michael, Glazer, Stuart D., Goldberg, Joshua, Golimowski, David A., Gonzaga, Shireen P., Gordon, Karl D., Gordon, Shawn J., Goudfrooij, Paul, Gough, Michael J., Graham, Adrian J., Grau, Christopher M., Green, Joel David, Greene, Gretchen R., Greene, Thomas P., Greenfield, Perry E., Greenhouse, Matthew A., Greve, Thomas R., Greville, Edgar M., Grimaldi, Stefano, Groe, Frank E., Groebner, Andrew, Grumm, David M., Grundy, Timothy, Güdel, Manuel, Guillard, Pierre, Guldalian, John, Gunn, Christopher A., Gurule, Anthony, Gutman, Irvin Meyer, Guy, Paul D., Guyot, Benjamin, Hack, Warren J., Haderlein, Peter, Hagan, James B., Hagedorn, Andria, Hainline, Kevin, Haley, Craig, Hami, Maryam, Hamilton, Forrest Clifford, Hammann, Jeffrey, Hammel, Heidi B., Hanley, Christopher J., Hansen, Carl August, Hardy, Bruce, Harnisch, Bernd, Harr, Michael Hunter, Harris, Pamela, Hart, Jessica Ann, Hartig, George F., Hasan, Hashima, Hashim, Kathleen Marie, Hashimoto, Ryan, Haskins, Sujee J., Hawkins, Robert Edward, Hayden, Brian, Hayden, William L., Healy, Mike, Hecht, Karen, Heeg, Vince J., Hejal, Reem, Helm, Kristopher A., Hengemihle, Nicholas J., Henning, Thomas, Henry, Alaina, Henry, Ronald L., Henshaw, Katherine, Hernandez, Scarlin, Herrington, Donald C., Heske, Astrid, Hesman, Brigette Emily, Hickey, David L., Hilbert, Bryan N., Hines, Dean C., Hinz, Michael R., Hirsch, Michael, Hitcho, Robert S., Hodapp, Klaus, Hodge, Philip E., Hoffman, Melissa, Holfeltz, Sherie T., Holler, Bryan Jason, Hoppa, Jennifer Rose, Horner, Scott, Howard, Joseph M., Howard, Richard J., Huber, Jean M., Hunkeler, Joseph S., Hunter, Alexander, Hunter, David Gavin, Hurd, Spencer W., Hurst, Brendan J., Hutchings, John B., Hylan, Jason E., Ignat, Luminita Ilinca, Illingworth, Garth, Irish, Sandra M., Isaacs III, John C., Jackson Jr., Wallace C., Jaffe, Daniel T., Jahic, Jasmin, Jahromi, Amir, Jakobsen, Peter, James, Bryan, James, John C., James, LeAndrea Rae, Jamieson, William Brian, Jandra, Raymond D., Jayawardhana, Ray, Jedrzejewski, Robert, Jeffers, Basil S., Jensen, Peter, Joanne, Egges, Johns, Alan T., Johnson, Carl A., Johnson, Eric L., Johnson, Patricia, Johnson, Phillip Stephen, Johnson, Thomas K., Johnson, Timothy W., Johnstone, Doug, Jollet, Delphine, Jones, Danny P., Jones, Gregory S., Jones, Olivia C., Jones, Ronald A., Jones, Vicki, Jordan, Ian J., Jordan, Margaret E., Jue, Reginald, Jurkowski, Mark H., Justis, Grant, Justtanont, Kay, Kaleida, Catherine C., Kalirai, Jason S., Kalmanson, Phillip Cabrales, Kaltenegger, Lisa, Kammerer, Jens, Kan, Samuel K., Kanarek, Graham Childs, Kao, Shaw-Hong, Karakla, Diane M., Karl, Hermann, Kassin, Susan A., Kauffman, David D., Kavanagh, Patrick, Kelley, Leigh L., Kelly, Douglas M., Kendrew, Sarah, Kennedy, Herbert V., Kenny, Deborah A., Keski-Kuha, Ritva A., Keyes, Charles D., Khan, Ali, Kidwell, Richard C., Kimble, Randy A., King, James S., King, Richard C., Kinzel, Wayne M., Kirk, Jeffrey R., Kirkpatrick, Marc E., Klaassen, Pamela, Klingemann, Lana, Klintworth, Paul U., Knapp, Bryan Adam, Knight, Scott, Knollenberg, Perry J., Knutsen, Daniel Mark, Koehler, Robert, Koekemoer, Anton M., Kofler, Earl T., Kontson, Vicki L., Kovacs, Aiden Rose, Kozhurina-Platais, Vera, Krause, Oliver, Kriss, Gerard A., Krist, John, Kristoffersen, Monica R., Krogel, Claudia, Krueger, Anthony P., Kulp, Bernard A., Kumari, Nimisha, Kwan, Sandy W., Kyprianou, Mark, Labador, Aurora Gadiano, Labiano, Álvaro, Lafrenière, David, Lagage, Pierre-Olivier, Laidler, Victoria G., Laine, Benoit, Laird, Simon, Lajoie, Charles-Philippe, Lallo, Matthew D., Lam, May Yen, LaMassa, Stephanie Marie, Lambros, Scott D., Lampenfield, Richard Joseph, Lander, Matthew Ed, Langston, James Hutton, Larson, Kirsten, Larson, Melora, LaVerghetta, Robert Joseph, Law, David R., Lawrence, Jon F., Lee, David W., Lee, Janice, Lee, Yat-Ning Paul, Leisenring, Jarron, Leveille, Michael Dunlap, Levenson, Nancy A., Levi, Joshua S., Levine, Marie B., Lewis, Dan, Lewis, Jake, Lewis, Nikole, Libralato, Mattia, Lidon, Norbert, Liebrecht, Paula Louisa, Lightsey, Paul, Lilly, Simon, Lim, Frederick C., Lim, Pey Lian, Ling, Sai-Kwong, Link, Lisa J., Link, Miranda Nicole, Lipinski, Jamie L., Liu, XiaoLi, Lo, Amy S., Lobmeyer, Lynette, Logue, Ryan M., Long, Chris A., Long, Douglas R., Long, Ilana D., Long, Knox S., López-Caniego, Marcos, Lotz, Jennifer M., Love-Pruitt, Jennifer M., Lubskiy, Michael, Luers, Edward B., Luetgens, Robert A., Luevano, Annetta J., Lui, Sarah Marie G. Flores, Lund III, James M., Lundquist, Ray A., Lunine, Jonathan, Lützgendorf, Nora, Lynch, Richard J., MacDonald, Alex J., MacDonald, Kenneth, Macias, Matthew J., Macklis, Keith I., Maghami, Peiman, Maharaja, Rishabh Y., Maiolino, Roberto, Makrygiannis, Konstantinos G., Malla, Sunita Giri, Malumuth, Eliot M., Manjavacas, Elena, Marini, Andrea, Marrione, Amanda, Marston, Anthony, Martel, André R, Martin, Didier, Martin, Peter G., Martinez, Kristin L., Maschmann, Marc, Masci, Gregory L., Masetti, Margaret E., Maszkiewicz, Michael, Matthews, Gary, Matuskey, Jacob E., McBrayer, Glen A., McCarthy, Donald W., McCaughrean, Mark J., McClare, Leslie A., McClare, Michael D., McCloskey, John C., McClurg, Taylore D., McCoy, Martin, McElwain, Michael W., McGregor, Roy D., McGuffey, Douglas B., McKay, Andrew G., McKenzie, William K., McLean, Brian, McMaster, Matthew, McNeil, Warren, De Meester, Wim, Mehalick, Kimberly L., Meixner, Margaret, Meléndez, Marcio, Menzel, Michael P., Menzel, Michael T., Merz, Matthew, Mesterharm, David D., Meyer, Michael R., Meyett, Michele L., Meza, Luis E., Midwinter, Calvin, Milam, Stefanie N., Miller, Jay Todd, Miller, William C., Miskey, Cherie L., Misselt, Karl, Mitchell, Eileen P., Mohan, Martin, Montoya, Emily E., Moran, Michael J., Morishita, Takahiro, Moro-Martín, Amaya, Morrison, Debra L., Morrison, Jane, Morse, Ernie C., Moschos, Michael, Moseley, S. H., Mosier, Gary E., Mosner, Peter, Mountain, Matt, Muckenthaler, Jason S., Mueller, Donald G., Mueller, Migo, Muhiem, Daniella, Mühlmann, Prisca, Mullally, Susan Elizabeth, Mullen, Stephanie M., Munger, Alan J, Murphy, Jess, Murray, Katherine T., Muzerolle, James C., Mycroft, Matthew, Myers, Andrew, Myers, Carey R., Myers, Fred Richard R., Myers, Richard, Myrick, Kaila, Nagle IV, Adrian F., Nayak, Omnarayani, Naylor, Bret, Neff, Susan G., Nelan, Edmund P., Nella, John, Nguyen, Duy Tuong, Nguyen, Michael N., Nickson, Bryony, Nidhiry, John Joseph, Niedner, Malcolm B., Nieto-Santisteban, Maria, Nikolov, Nikolay K., Nishisaka, Mary Ann, Nota, Antonella, O'Mara, Robyn C., Oboryshko, Michael, O'Brien, Marcus B., Ochs, William R., Offenberg, Joel D., Ogle, Patrick Michael, Ohl, Raymond G., Olmsted, Joseph Hamden, Osborne, Shannon Barbara, O'Shaughnessy, Brian Patrick, Östlin, Göran, O'Sullivan, Brian, Otor, O. Justin, Ottens, Richard, Ouellette, Nathalie N. -Q., Outlaw, Daria J., Owens, Beverly A., Pacifici, Camilla, Page, James Christophe, Paranilam, James G., Park, Sang, Parrish, Keith A., Paschal, Laura, Patapis, Polychronis, Patel, Jignasha, Patrick, Keith, Pattishall Jr., Robert A., Paul, Douglas William, Paul, Shirley J., Pauly, Tyler Andrew, Pavlovsky, Cheryl M., Peña-Guerrero, Maria, Pedder, Andrew H., Peek, Matthew Weldon, Pelham, Patricia A., Penanen, Konstantin, Perriello, Beth A., Perrin, Marshall D., Perrine, Richard F., Perrygo, Chuck, Peslier, Muriel, Petach, Michael, Peterson, Karla A., Pfarr, Tom, Pierson, James M., Pietraszkiewicz, Martin, Pilchen, Guy, Pipher, Judy L., Pirzkal, Norbert, Pitman, Joseph T., Player, Danielle M., Plesha, Rachel, Plitzke, Anja, Pohner, John A., Poletis, Karyn Konstantin, Pollizzi, Joseph A., Polster, Ethan, Pontius, James T., Pontoppidan, Klaus, Porges, Susana C., Potter, Gregg D., Prescott, Stephen, Proffitt, Charles R., Pueyo, Laurent, Neira, Irma Aracely Quispe, Radich, Armando, Rager, Reiko T., Rameau, Julien, Ramey, Deborah D., Alarcon, Rafael Ramos, Rampini, Riccardo, Rapp, Robert, Rashford, Robert A., Rauscher, Bernard J., Ravindranath, Swara, Rawle, Timothy, Rawlings, Tynika N., Ray, Tom, Regan, Michael W., Rehm, Brian, Rehm, Kenneth D., Reid, Neill, Reis, Carl A., Renk, Florian, Reoch, Tom B., Ressler, Michael, Rest, Armin W., Reynolds, Paul J., Richon, Joel G., Richon, Karen V., Ridgaway, Michael, Riedel, Adric Richard, Rieke, George H., Rieke, Marcia, Rifelli, Richard E., Rigby, Jane R., Riggs, Catherine S., Ringel, Nancy J., Ritchie, Christine E., Rix, Hans-Walter, Robberto, Massimo, Robinson, Michael S., Robinson, Orion, Rock, Frank W., Rodriguez, David R., del Pino, Bruno Rodríguez, Roellig, Thomas, Rohrbach, Scott O., Roman, Anthony J., Romelfanger, Frederick J., Romo Jr., Felipe P., Rosales, Jose J., Rose, Perry, Roteliuk, Anthony F., Roth, Marc N., Rothwell, Braden Quinn, Rouzaud, Sylvain, Rowe, Jason, Rowlands, Neil, Roy, Arpita, Royer, Pierre, Rui, Chunlei, Rumler, Peter, Rumpl, William, Russ, Melissa L., Ryan, Michael B., Ryan, Richard M., Saad, Karl, Sabata, Modhumita, Sabatino, Rick, Sabbi, Elena, Sabelhaus, Phillip A., Sabia, Stephen, Sahu, Kailash C., Saif, Babak N., Salvignol, Jean-Christophe, Samara-Ratna, Piyal, Samuelson, Bridget S., Sanders, Felicia A., Sappington, Bradley, Sargent, B. A., Sauer, Arne, Savadkin, Bruce J., Sawicki, Marcin, Schappell, Tina M., Scheffer, Caroline, Scheithauer, Silvia, Scherer, Ron, Schiff, Conrad, Schlawin, Everett, Schmeitzky, Olivier, Schmitz, Tyler S., Schmude, Donald J., Schneider, Analyn, Schreiber, Jürgen, Schroeven-Deceuninck, Hilde, Schultz, John J., Schwab, Ryan, Schwartz, Curtis H., Scoccimarro, Dario, Scott, John F., Scott, Michelle B., Seaton, Bonita L., Seely, Bruce S., Seery, Bernard, Seidleck, Mark, Sembach, Kenneth, Shanahan, Clare Elizabeth, Shaughnessy, Bryan, Shaw, Richard A., Shay, Christopher Michael, Sheehan, Even, Sheth, Kartik, Shih, Hsin-Yi, Shivaei, Irene, Siegel, Noah, Sienkiewicz, Matthew G., Simmons, Debra D., Simon, Bernard P., Sirianni, Marco, Sivaramakrishnan, Anand, Slade, Jeffrey E., Sloan, G. C., Slocum, Christine E., Slowinski, Steven E., Smith, Corbett T., Smith, Eric P., Smith, Erin C., Smith, Koby, Smith, Robert, Smith, Stephanie J., Smolik, John L., Soderblom, David R., Sohn, Sangmo Tony, Sokol, Jeff, Sonneborn, George, Sontag, Christopher D., Sooy, Peter R., Soummer, Remi, Southwood, Dana M., Spain, Kay, Sparmo, Joseph, Speer, David T., Spencer, Richard, Sprofera, Joseph D., Stallcup, Scott S., Stanley, Marcia K., Stansberry, John A., Stark, Christopher C., Starr, Carl W., Stassi, Diane Y., Steck, Jane A., Steeley, Christine D., Stephens, Matthew A., Stephenson, Ralph J., Stewart, Alphonso C., Stiavelli, Massimo, Stockman Jr., Hervey, Strada, Paolo, Straughn, Amber N., Streetman, Scott, Strickland, David Kendal, Strobele, Jingping F., Stuhlinger, Martin, Stys, Jeffrey Edward, Such, Miguel, Sukhatme, Kalyani, Sullivan, Joseph F., Sullivan, Pamela C., Sumner, Sandra M., Sun, Fengwu, Sunnquist, Benjamin Dale, Swade, Daryl Allen, Swam, Michael S., Swenton, Diane F., Swoish, Robby A., Litten, Oi In Tam, Tamas, Laszlo, Tao, Andrew, Taylor, David K., Taylor, Joanna M., Plate, Maurice te, Van Tea, Mason, Teague, Kelly K., Telfer, Randal C., Temim, Tea, Texter, Scott C., Thatte, Deepashri G., Thompson, Christopher Lee, Thompson, Linda M., Thomson, Shaun R., Thronson, Harley, Tierney, C. M., Tikkanen, Tuomo, Tinnin, Lee, Tippet, William Thomas, Todd, Connor William, Tran, Hien D., Trauger, John, Trejo, Edwin Gregorio, Truong, Justin Hoang Vinh, Tsukamoto, Christine L., Tufail, Yasir, Tumlinson, Jason, Tustain, Samuel, Tyra, Harrison, Ubeda, Leonardo, Underwood, Kelli, Uzzo, Michael A., Vaclavik, Steven, Valenduc, Frida, Valenti, Jeff A., Van Campen, Julie, van de Wetering, Inge, Van Der Marel, Roeland P., van Haarlem, Remy, Vandenbussche, Bart, Vanterpool, Dona D., Vernoy, Michael R., Costas, Maria Begoña Vila, Volk, Kevin, Voorzaat, Piet, Voyton, Mark F., Vydra, Ekaterina, Waddy, Darryl J., Waelkens, Christoffel, Wahlgren, Glenn Michael, Walker Jr., Frederick E., Wander, Michel, Warfield, Christine K., Warner, Gerald, Wasiak, Francis C., Wasiak, Matthew F., Wehner, James, Weiler, Kevin R., Weilert, Mark, Weiss, Stanley B., Wells, Martyn, Welty, Alan D., Wheate, Lauren, Wheeler, Thomas P., White, Christy L., Whitehouse, Paul, Whiteleather, Jennifer Margaret, Whitman, William Russell, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris J., Willoughby, Scott P., Wilson, Andrew, Wilson, Debra, Wilson, Donna V., Windhorst, Rogier, Wislowski, Emily Christine, Wolfe, David J., Wolfe, Michael A., Wolff, Schuyler, Wondel, Amancio, Woo, Cindy, Woods, Robert T., Worden, Elaine, Workman, William, Wright, Gillian S., Wu, Carl, Wu, Chi-Rai, Wun, Dakin D., Wymer, Kristen B., Yadetie, Thomas, Yan, Isabelle C., Yang, Keith C., Yates, Kayla L., Yeager, Christopher R., Yerger, Ethan John, Young, Erick T., Young, Gary, Yu, Gene, Yu, Susan, Zak, Dean S., Zeidler, Peter, Zepp, Robert, Zhou, Julia, Zincke, Christian A., Zonak, Stephanie, and Zondag, Elisabeth
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 years, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit., Comment: Accepted by PASP for the special issue on The James Webb Space Telescope Overview, 29 pages, 4 figures
Published: 2023
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3. The Science Performance of JWST as Characterized in Commissioning

Author: Rigby, Jane, Perrin, Marshall, McElwain, Michael, Kimble, Randy, Friedman, Scott, Lallo, Matt, Doyon, René, Feinberg, Lee, Ferruit, Pierre, Glasse, Alistair, Rieke, Marcia, Rieke, George, Wright, Gillian, Willott, Chris, Colon, Knicole, Milam, Stefanie, Neff, Susan, Stark, Christopher, Valenti, Jeff, Abell, Jim, Abney, Faith, Abul-Huda, Yasin, Acton, D. Scott, Adams, Evan, Adler, David, Aguilar, Jonathan, Ahmed, Nasif, Albert, Loïc, Alberts, Stacey, Aldridge, David, Allen, Marsha, Altenburg, Martin, Marquez, Javier Alvarez, de Oliveira, Catarina Alves, Andersen, Greg, Anderson, Harry, Anderson, Sara, Argyriou, Ioannis, Armstrong, Amber, Arribas, Santiago, Artigau, Etienne, Arvai, Amanda, Atkinson, Charles, Bacon, Gregory, Bair, Thomas, Banks, Kimberly, Barrientes, Jaclyn, Barringer, Bruce, Bartosik, Peter, Bast, William, Baudoz, Pierre, Beatty, Thomas, Bechtold, Katie, Beck, Tracy, Bergeron, Eddie, Bergkoetter, Matthew, Bhatawdekar, Rachana, Birkmann, Stephan, Blazek, Ronald, Blome, Claire, Boccaletti, Anthony, Boeker, Torsten, Boia, John, Bonaventura, Nina, Bond, Nicholas, Bosley, Kari, Boucarut, Ray, Bourque, Matthew, Bouwman, Jeroen, Bower, Gary, Bowers, Charles, Boyer, Martha, Bradley, Larry, Brady, Greg, Braun, Hannah, Breda, David, Bresnahan, Pamela, Bright, Stacey, Britt, Christopher, Bromenschenkel, Asa, Brooks, Brian, Brooks, Keira, Brown, Bob, Brown, Matthew, Brown, Patricia, Bunker, Andy, Burger, Matthew, Bushouse, Howard, Cale, Steven, Cameron, Alex, Cameron, Peter, Canipe, Alicia, Caplinger, James, Caputo, Francis, Cara, Mihai, Carey, Larkin, Carniani, Stefano, Carrasquilla, Maria, Carruthers, Margaret, Case, Michael, Catherine, Riggs, Chance, Don, Chapman, George, Charlot, Stéphane, Charlow, Brian, Chayer, Pierre, Chen, Bin, Cherinka, Brian, Chichester, Sarah, Chilton, Zack, Chonis, Taylor, Clampin, Mark, Clark, Charles, Clark, Kerry, Coe, Dan, Coleman, Benee, Comber, Brian, Comeau, Tom, Connolly, Dennis, Cooper, James, Cooper, Rachel, Coppock, Eric, Correnti, Matteo, Cossou, Christophe, Coulais, Alain, Coyle, Laura, Cracraft, Misty, Curti, Mirko, Cuturic, Steven, Davis, Katherine, Davis, Michael, Dean, Bruce, DeLisa, Amy, deMeester, Wim, Dencheva, Nadia, Dencheva, Nadezhda, DePasquale, Joseph, Deschenes, Jeremy, Detre, Örs Hunor, Diaz, Rosa, Dicken, Dan, DiFelice, Audrey, Dillman, Matthew, Dixon, William, Doggett, Jesse, Donaldson, Tom, Douglas, Rob, DuPrie, Kimberly, Dupuis, Jean, Durning, John, Easmin, Nilufar, Eck, Weston, Edeani, Chinwe, Egami, Eiichi, Ehrenwinkler, Ralf, Eisenhamer, Jonathan, Eisenhower, Michael, Elie, Michelle, Elliott, James, Elliott, Kyle, Ellis, Tracy, Engesser, Michael, Espinoza, Nestor, Etienne, Odessa, Etxaluze, Mireya, Falini, Patrick, Feeney, Matthew, Ferry, Malcolm, Filippazzo, Joseph, Fincham, Brian, Fix, Mees, Flagey, Nicolas, Florian, Michael, Flynn, Jim, Fontanella, Erin, Ford, Terrance, Forshay, Peter, Fox, Ori, Franz, David, Fu, Henry, Fullerton, Alexander, Galkin, Sergey, Galyer, Anthony, Marin, Macarena Garcia, Gardner, Jonathan, Gardner, Lisa, Garland, Dennis, Garrett, Bruce, Gasman, Danny, Gaspar, Andras, Gaudreau, Daniel, Gauthier, Peter, Geers, Vincent, Geithner, Paul, Gennaro, Mario, Giardino, Giovanna, Girard, Julien, Giuliano, Mark, Glassmire, Kirk, Glauser, Adrian, Glazer, Stuart, Godfrey, John, Golimowski, David, Gollnitz, David, Gong, Fan, Gonzaga, Shireen, Gordon, Michael, Gordon, Karl, Goudfrooij, Paul, Greene, Thomas, Greenhouse, Matthew, Grimaldi, Stefano, Groebner, Andrew, Grundy, Timothy, Guillard, Pierre, Gutman, Irvin, Ha, Kong Q., Haderlein, Peter, Hagedorn, Andria, Hainline, Kevin, Haley, Craig, Hami, Maryam, Hamilton, Forrest, Hammel, Heidi, Hansen, Carl, Harkins, Tom, Harr, Michael, Hart, Jessica, Hart, Quyen, Hartig, George, Hashimoto, Ryan, Haskins, Sujee, Hathaway, William, Havey, Keith, Hayden, Brian, Hecht, Karen, Heller-Boyer, Chris, Henriques, Caroline, Henry, Alaina, Hermann, Karl, Hernandez, Scarlin, Hesman, Brigette, Hicks, Brian, Hilbert, Bryan, Hines, Dean, Hoffman, Melissa, Holfeltz, Sherie, Holler, Bryan J., Hoppa, Jennifer, Hott, Kyle, Howard, Joseph, Howard, Rick, Hunter, Alexander, Hunter, David, Hurst, Brendan, Husemann, Bernd, Hustak, Leah, Ignat, Luminita Ilinca, Illingworth, Garth, Irish, Sandra, Jackson, Wallace, Jahromi, Amir, Jakobsen, Peter, James, LeAndrea, James, Bryan, Januszewski, William, Jenkins, Ann, Jirdeh, Hussein, Johnson, Phillip, Johnson, Timothy, Jones, Vicki, Jones, Ron, Jones, Danny, Jones, Olivia, Jordan, Ian, Jordan, Margaret, Jurczyk, Sarah, Jurling, Alden, Kaleida, Catherine, Kalmanson, Phillip, Kammerer, Jens, Kang, Huijo, Kao, Shaw-Hong, Karakla, Diane, Kavanagh, Patrick, Kelly, Doug, Kendrew, Sarah, Kennedy, Herbert, Kenny, Deborah, Keski-kuha, Ritva, Keyes, Charles, Kidwell, Richard, Kinzel, Wayne, Kirk, Jeff, Kirkpatrick, Mark, Kirshenblat, Danielle, Klaassen, Pamela, Knapp, Bryan, Knight, J. Scott, Knollenberg, Perry, Koehler, Robert, Koekemoer, Anton, Kovacs, Aiden, Kulp, Trey, Kumari, Nimisha, Kyprianou, Mark, La Massa, Stephanie, Labador, Aurora, Ortega, Alvaro Labiano, Lagage, Pierre-Olivier, Lajoie, Charles-Phillipe, Lallo, Matthew, Lam, May, Lamb, Tracy, Lambros, Scott, Lampenfield, Richard, Langston, James, Larson, Kirsten, Law, David, Lawrence, Jon, Lee, David, Leisenring, Jarron, Lepo, Kelly, Leveille, Michael, Levenson, Nancy, Levine, Marie, Levy, Zena, Lewis, Dan, Lewis, Hannah, Libralato, Mattia, Lightsey, Paul, Link, Miranda, Liu, Lily, Lo, Amy, Lockwood, Alexandra, Logue, Ryan, Long, Chris, Long, Douglas, Loomis, Charles, Lopez-Caniego, Marcos, Alvarez, Jose Lorenzo, Love-Pruitt, Jennifer, Lucy, Adrian, Luetzgendorf, Nora, Maghami, Peiman, Maiolino, Roberto, Major, Melissa, Malla, Sunita, Malumuth, Eliot, Manjavacas, Elena, Mannfolk, Crystal, Marrione, Amanda, Marston, Anthony, Martel, André, Maschmann, Marc, Masci, Gregory, Masciarelli, Michaela, Maszkiewicz, Michael, Mather, John, McKenzie, Kenny, McLean, Brian, McMaster, Matthew, Melbourne, Katie, Meléndez, Marcio, Menzel, Michael, Merz, Kaiya, Meyett, Michele, Meza, Luis, Miskey, Cherie, Misselt, Karl, Moller, Christopher, Morrison, Jane, Morse, Ernie, Moseley, Harvey, Mosier, Gary, Mountain, Matt, Mueckay, Julio, Mueller, Michael, Mullally, Susan, Murphy, Jess, Murray, Katherine, Murray, Claire, Mustelier, David, Muzerolle, James, Mycroft, Matthew, Myers, Richard, Myrick, Kaila, Nanavati, Shashvat, Nance, Elizabeth, Nayak, Omnarayani, Naylor, Bret, Nelan, Edmund, Nickson, Bryony, Nielson, Alethea, Nieto-Santisteban, Maria, Nikolov, Nikolay, Noriega-Crespo, Alberto, O'Shaughnessy, Brian, O'Sullivan, Brian, Ochs, William, Ogle, Patrick, Oleszczuk, Brenda, Olmsted, Joseph, Osborne, Shannon, Ottens, Richard, Owens, Beverly, Pacifici, Camilla, Pagan, Alyssa, Page, James, Park, Sang, Parrish, Keith, Patapis, Polychronis, Paul, Lee, Pauly, Tyler, Pavlovsky, Cheryl, Pedder, Andrew, Peek, Matthew, Pena-Guerrero, Maria, Pennanen, Konstantin, Perez, Yesenia, Perna, Michele, Perriello, Beth, Phillips, Kevin, Pietraszkiewicz, Martin, Pinaud, Jean-Paul, Pirzkal, Norbert, Pitman, Joseph, Piwowar, Aidan, Platais, Vera, Player, Danielle, Plesha, Rachel, Pollizi, Joe, Polster, Ethan, Pontoppidan, Klaus, Porterfield, Blair, Proffitt, Charles, Pueyo, Laurent, Pulliam, Christine, Quirt, Brian, Neira, Irma Quispe, Alarcon, Rafael Ramos, Ramsay, Leah, Rapp, Greg, Rapp, Robert, Rauscher, Bernard, Ravindranath, Swara, Rawle, Timothy, Regan, Michael, Reichard, Timothy A., Reis, Carl, Ressler, Michael E., Rest, Armin, Reynolds, Paul, Rhue, Timothy, Richon, Karen, Rickman, Emily, Ridgaway, Michael, Ritchie, Christine, Rix, Hans-Walter, Robberto, Massimo, Robinson, Gregory, Robinson, Michael, Robinson, Orion, Rock, Frank, Rodriguez, David, Del Pino, Bruno Rodriguez, Roellig, Thomas, Rohrbach, Scott, Roman, Anthony, Romelfanger, Fred, Rose, Perry, Roteliuk, Anthony, Roth, Marc, Rothwell, Braden, Rowlands, Neil, Roy, Arpita, Royer, Pierre, Royle, Patricia, Rui, Chunlei, Rumler, Peter, Runnels, Joel, Russ, Melissa, Rustamkulov, Zafar, Ryden, Grant, Ryer, Holly, Sabata, Modhumita, Sabatke, Derek, Sabbi, Elena, Samuelson, Bridget, Sapp, Benjamin, Sappington, Bradley, Sargent, B., Sauer, Arne, Scheithauer, Silvia, Schlawin, Everett, Schlitz, Joseph, Schmitz, Tyler, Schneider, Analyn, Schreiber, Jürgen, Schulze, Vonessa, Schwab, Ryan, Scott, John, Sembach, Kenneth, Shanahan, Clare, Shaughnessy, Bryan, Shaw, Richard, Shawger, Nanci, Shay, Christopher, Sheehan, Evan, Shen, Sharon, Sherman, Allan, Shiao, Bernard, Shih, Hsin-Yi, Shivaei, Irene, Sienkiewicz, Matthew, Sing, David, Sirianni, Marco, Sivaramakrishnan, Anand, Skipper, Joy, Sloan, Gregory, Slocum, Christine, Slowinski, Steven, Smith, Erin, Smith, Eric, Smith, Denise, Smith, Corbett, Snyder, Gregory, Soh, Warren, Sohn, Tony, Soto, Christian, Spencer, Richard, Stallcup, Scott, Stansberry, John, Starr, Carl, Starr, Elysia, Stewart, Alphonso, Stiavelli, Massimo, Straughn, Amber, Strickland, David, Stys, Jeff, Summers, Francis, Sun, Fengwu, Sunnquist, Ben, Swade, Daryl, Swam, Michael, Swaters, Robert, Swoish, Robby, Taylor, Joanna M., Taylor, Rolanda, Plate, Maurice Te, Tea, Mason, Teague, Kelly, Telfer, Randal, Temim, Tea, Thatte, Deepashri, Thompson, Christopher, Thompson, Linda, Thomson, Shaun, Tikkanen, Tuomo, Tippet, William, Todd, Connor, Toolan, Sharon, Tran, Hien, Trejo, Edwin, Truong, Justin, Tsukamoto, Chris, Tustain, Samuel, Tyra, Harrison, Ubeda, Leonardo, Underwood, Kelli, Uzzo, Michael, Van Campen, Julie, Vandal, Thomas, Vandenbussche, Bart, Vila, Begoña, Volk, Kevin, Wahlgren, Glenn, Waldman, Mark, Walker, Chanda, Wander, Michel, Warfield, Christine, Warner, Gerald, Wasiak, Matthew, Watkins, Mitchell, Weaver, Andrew, Weilert, Mark, Weiser, Nick, Weiss, Ben, Weissman, Sarah, Welty, Alan, West, Garrett, Wheate, Lauren, Wheatley, Elizabeth, Wheeler, Thomas, White, Rick, Whiteaker, Kevin, Whitehouse, Paul, Whiteleather, Jennifer, Whitman, William, Williams, Christina, Willmer, Christopher, Willoughby, Scott, Wilson, Andrew, Wirth, Gregory, Wislowski, Emily, Wolf, Erin, Wolfe, David, Wolff, Schuyler, Workman, Bill, Wright, Ray, Wu, Carl, Wu, Rai, Wymer, Kristen, Yates, Kayla, Yeager, Christopher, Yeates, Jared, Yerger, Ethan, Yoon, Jinmi, Young, Alice, Yu, Susan, Zak, Dean, Zeidler, Peter, Zhou, Julia, Zielinski, Thomas, Zincke, Cristian, and Zonak, Stephanie
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: This paper characterizes the actual science performance of the James Webb Space Telescope (JWST), as determined from the six month commissioning period. We summarize the performance of the spacecraft, telescope, science instruments, and ground system, with an emphasis on differences from pre-launch expectations. Commissioning has made clear that JWST is fully capable of achieving the discoveries for which it was built. Moreover, almost across the board, the science performance of JWST is better than expected; in most cases, JWST will go deeper faster than expected. The telescope and instrument suite have demonstrated the sensitivity, stability, image quality, and spectral range that are necessary to transform our understanding of the cosmos through observations spanning from near-earth asteroids to the most distant galaxies., Comment: 5th version as accepted to PASP; 31 pages, 18 figures; https://iopscience.iop.org/article/10.1088/1538-3873/acb293
Published: 2022
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4. An Assessment of the In-Situ Growth of the Intracluster Light in the High Redshift Galaxy Cluster SpARCS1049+56

Author: Barfety, Capucine, Valin, Félix-Antoine, Webb, Tracy M. A., Yun, Min, Shipley, Heath, Boone, Kyle, Hayden, Brian, Hlavacek-Larrondo, Julie, Muzzin, Adam, Noble, Allison G., Perlmutter, Saul, Rhea, Carter, Wilson, Gillian, and Yee, H. K. C
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The formation of the stellar mass within galaxy cluster cores is a poorly understood process. It features the complicated physics of cooling flows, AGN feedback, star formation and more. Here, we study the growth of the stellar mass in the vicinity of the Brightest Cluster Galaxy (BCG) in a z = 1.7 cluster, SpARCS1049+56. We synthesize a reanalysis of existing HST imaging, a previously published measurement of the star formation rate, and the results of new radio molecular gas spectroscopy. These analyses represent the past, present and future star formation respectively within this system. We show that a large amount of stellar mass -- between $(2.2 \pm 0.5) \times 10^{10} \: M_\odot$ and $(6.6 \pm 1.2) \times 10^{10}\: M_\odot$ depending on the data processing -- exists in a long and clumpy tail-like structure that lies roughly 12 kpc off the BCG. Spatially coincident with this stellar mass is a similarly massive reservoir ($(1.0 \pm 0.7) \times 10^{11} \: M_\odot$) of molecular gas that we suggest is the fuel for the immense star formation rate of $860 \pm 130 \: M_\odot$/yr, as measured by infrared observations. Hlavacek-Larrondo et al. 2021 surmised that massive, runaway cooling of the hot intracluster X-ray gas was feeding this star formation, a process that had not been observed before at high-redshift. We conclude, based on the amount of fuel and current stars, that this event may be rare in the lifetime of a cluster, producing roughly 15 to 21% of the Intracluster Light (ICL) mass in one go, though perhaps a common event for all galaxy clusters., Comment: 11 pages, 5 figures. Submitted to ApJ. Addressed referee report
Published: 2022
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5. The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries

Author: Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andy, Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C., Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Bohringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildenrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M. James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E., Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, Wechsler, Risa, and Project, The Supernova Cosmology
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The See Change survey was designed to make $z>1$ cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope spanning the redshift range $z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at $z\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this proved to be a highly efficient use of HST for SN observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star-formation rates. We find that the resulting number of SNe Ia per orbit is a factor of $\sim 8$ higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel features include fully blinded SN searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 magnitudes of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host-galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper., Comment: ApJ preprint
Published: 2021
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6. The H$\alpha$ star formation main sequence in cluster and field galaxies at $z\sim1.6$

Author: Nantais, Julie, Wilson, Gillian, Muzzin, Adam, Old, Lyndsay J., Demarco, Ricardo, Cerulo, Pierluigi, Balogh, Michael, Rudnick, Gregory, Chan, Jeffrey, Cooper, M. C., Forrest, Ben, Hayden, Brian, Lidman, Chris, Noble, Allison, Perlmutter, Saul, Rhea, Carter, Surace, Jason, van der Burg, Remco, and van Kampen, Eelco
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We calculate H$\alpha$-based star formation rates and determine the star formation rate-stellar mass relation for members of three SpARCS clusters at $z \sim 1.6$ and serendipitously identified field galaxies at similar redshifts to the clusters. We find similar star formation rates in cluster and field galaxies throughout our range of stellar masses. The results are comparable to those seen in other clusters at similar redshifts, and consistent with our previous photometric evidence for little quenching activity in clusters. One possible explanation for our results is that galaxies in our $z \sim 1.6$ clusters have been accreted too recently to show signs of environmental quenching. It is also possible that the clusters are not yet dynamically mature enough to produce important environmental quenching effects shown to be important at low redshift, such as ram pressure stripping or harassment., Comment: 10 pages, 5 figures, accepted for publication in MNRAS
Published: 2020
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7. The Morphology-Density relationship in 1<z<2 clusters

Author: Sazonova, Elizaveta, Alatalo, Katherine, Lotz, Jennifer, Rowlands, Kate, Snyder, Gregory F., Boone, Kyle, Brodwin, Mark, Hayden, Brian, Lanz, Lauranne, Perlmutter, Saul, and Rodriguez-Gomez, Vicente
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The morphology-density relationship states that dense cosmic environments such as galaxy clusters have an overabundance of quiescent elliptical galaxies, but it is unclear at which redshift this relationship is first established. We study the morphology of 4 clusters with $1.2
Published: 2020
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8. The HST See Change Program. I. Survey Design, Pipeline, and Supernova Discoveries* *Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, under programs 13677, 14327.

Author: Hayden, Brian, Rubin, David, Boone, Kyle, Aldering, Greg, Nordin, Jakob, Brodwin, Mark, Deustua, Susana, Dixon, Sam, Fagrelius, Parker, Fruchter, Andy, Eisenhardt, Peter, Gonzalez, Anthony, Gupta, Ravi, Hook, Isobel, Lidman, Chris, Luther, Kyle, Muzzin, Adam, Raha, Zachary, Ruiz-Lapuente, Pilar, Saunders, Clare, Sofiatti, Caroline, Stanford, Adam, Suzuki, Nao, Webb, Tracy, Williams, Steven C, Wilson, Gillian, Yen, Mike, Amanullah, Rahman, Barbary, Kyle, Böhringer, Hans, Chappell, Greta, Cunha, Carlos, Currie, Miles, Fassbender, Rene, Gladders, Michael, Goobar, Ariel, Hildebrandt, Hendrik, Hoekstra, Henk, Huang, Xiaosheng, Huterer, Dragan, Jee, M James, Kim, Alex, Kowalski, Marek, Linder, Eric, Meyers, Joshua E, Pain, Reynald, Perlmutter, Saul, Richard, Johan, Rosati, Piero, Rozo, Eduardo, Rykoff, Eli, Santos, Joana, Spadafora, Anthony, Stern, Daniel, and Wechsler, Risa
Subjects: astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: The See Change survey was designed to make z > 1 cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope (HST) spanning the redshift range z = 1.13-1.75, discovering 57 likely transients and 27 likely SNe Ia at z ∼ 0.8-2.3. As in similar previous surveys, this proved to be a highly efficient use of HST for supernova observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star formation rates. We find that the resulting number of SNe Ia per orbit is a factor of ∼8 higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and supernova discoveries. Novel features include fully blinded supernova searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 mag of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper.
Published: 2021

9. Mercury and amino acid content relations in northern pike (Esox lucius) in subarctic lakes along a climate-productivity gradient

Author: Kozak, Natalia, Kahilainen, Kimmo K., Pakkanen, Hannu K., Hayden, Brian, Østbye, Kjartan, and Taipale, Sami J.
Published: 2023
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10. The Growth of Brightest Cluster Galaxies and Intracluster Light Over the Past Ten Billion Years

Author: DeMaio, Tahlia, Gonzalez, Anthony H., Zabludoff, Ann, Zaritsky, Dennis, Aldering, Greg, Brodwin, Mark, Connor, Thomas, Donahue, Megan, Hayden, Brian, Mulchaey, John S., Perlmutter, Saul, and Stanford, S. A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We constrain the evolution of the brightest cluster galaxy plus intracluster light (BCG+ICL) using an ensemble of 42 galaxy groups and clusters that span redshifts of z = 0.05-1.75 and masses of $M_{500,c}=2\times10^{13}-10^{15}$ M$_\odot$ Specifically, we measure the relationship between the BCG+ICL stellar mass $M_\star$ and $M_{500,c}$ at projected radii 10 < r < 100 kpc for three different epochs. At intermediate redshift (z = 0.40), where we have the best data, we find $M_\star\propto M_{500,c}^{0.48\pm0.06}$. Fixing the exponent of this power law for all redshifts, we constrain the normalization of this relation to be $2.08\pm0.21$ times higher at z = 0.40 than at high redshift (z = 1.55). We find no change in the relation from intermediate to low redshift (z = 0.10). In other words, for fixed $M_{500,c}$, $M_\star$ at 10 < r < 100 kpc increases from z = 1.55 to z = 0.40 and not significantly thereafter. Theoretical models predict that the physical mass growth of the cluster from z = 1.5 to z = 0 within $r_{500,c}$ is a factor of 1.4, excluding evolution due to definition of $r_{500,c}$. We find that $M_\star$ within the central 100 kpc increases by a factor of 3.8 over the same period. Thus, the growth of $M_\star$ in this central region is more than a factor of two greater than the physical mass growth of the cluster as a whole. Furthermore, the concentration of the BCG+ICL stellar mass, defined by the ratio of stellar mass within 10 kpc to the total stellar mass within 100 kpc, decreases with increasing $M_{500,c}$ at all redshift. We interpret this result as evidence for inside-out growth of the BCG+ICL over the past ten Gyrs, with stellar mass assembly occuring at larger radii at later times., Comment: Accepted to MNRAS, 9 pages, 6 figures
Published: 2019
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11. Precise Mass Determination of SPT-CL J2106-5844, the Most Massive Cluster at z>1

Author: Kim, Jinhyub, Jee, M. James, Perlmutter, Saul, Hayden, Brian, Rubin, David, Huang, Xiaosheng, Aldering, Greg, and Ko, Jongwan
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present a detailed high-resolution weak-lensing (WL) study of SPT-CL J2106-5844 at z=1.132, claimed to be the most massive system discovered at z > 1 in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. Based on the deep imaging data from the Advanced Camera for Surveys and Wide Field Camera 3 on-board the Hubble Space Telescope, we find that the cluster mass distribution is asymmetric, composed of a main clump and a subclump ~640 kpc west thereof. The central clump is further resolved into two smaller northwestern and southeastern substructures separated by ~150 kpc. We show that this rather complex mass distribution is more consistent with the cluster galaxy distribution than a unimodal distribution as previously presented. The northwestern substructure coincides with the BCG and X-ray peak while the southeastern one agrees with the location of the number density peak. These morphological features and the comparison with the X-ray emission suggest that the cluster might be a merging system. We estimate the virial mass of the cluster to be $M_{200c} = (10.4^{+3.3}_{-3.0}\pm1.0)~\times~10^{14}~M_{\odot}$, where the second error bar is the systematic uncertainty. Our result confirms that the cluster SPT-CL J2106-5844 is indeed the most massive cluster at z>1 known to date. We demonstrate the robustness of this mass estimate by performing a number of tests with different assumptions on the centroids, mass-concentration relations, and sample variance., Comment: 17 pages, 12 figures, 2 tables; Resubmission to ApJ after first referee revision
Published: 2019
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12. The Massive and Distant Clusters of WISE Survey VI: Stellar Mass Fractions of a Sample of High-Redshift Infrared-selected Clusters

Author: Decker, Bandon, Brodwin, Mark, Abdulla, Zubair, Gonzalez, Anthony H., Marrone, Daniel P., O'Donnell, Christine, Stanford, S. A., Wylezalek, Dominika, Carlstrom, John E., Eisenhardt, Peter R. M., Mantz, Adam, Mo, Wenli, Moravec, Emily, Stern, Daniel, Aldering, Greg, Ashby, Matthew L. N., Boone, Kyle, Hayden, Brian, Gupta, Nikhel, and McDonald, Michael A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present measurements of the stellar mass fractions ($f_\star$) for a sample of high-redshift ($0.93 \le z \le 1.32$) infrared-selected galaxy clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) and compare them to the stellar mass fractions of Sunyaev-Zel'dovich (SZ) effect-selected clusters in a similar mass and redshift range from the South Pole Telescope (SPT)-SZ Survey. We do not find a significant difference in mean $f_\star$ between the two selection methods, though we do find an unexpectedly large range in $f_\star$ for the SZ-selected clusters. In addition, we measure the luminosity function of the MaDCoWS clusters and find $m^*= 19.41\pm0.07$, similar to other studies of clusters at or near our redshift range. Finally, we present SZ detections and masses for seven MaDCoWS clusters and new spectroscopic redshifts for five MaDCoWS clusters. One of these new clusters, MOO J1521+0452 at $z=1.31$, is the most distant MaDCoWS cluster confirmed to date., Comment: Accepted to ApJ
Published: 2019
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13. The Massive and Distant Clusters of WISE Survey. I: Survey Overview and a Catalog of >2000 Galaxy Clusters at z~1

Author: Gonzalez, Anthony H., Gettings, Daniel P., Brodwin, Mark, Eisenhardt, Peter R. M., Stanford, S. Adam, Wylezalek, Dominika, Decker, Bandon, Marrone, Daniel P., Moravec, Emily, O'Donnell, Christine, Stalder, Brian, Stern, Daniel, Abdulla, Zubair, Brown, Gillen, Carlstrom, John, Chambers, Kenneth C., Hayden, Brian, Lin, Yen-Ting, Magnier, Eugene, Masci, Frank, Mantz, Adam B., McDonald, Michael, Mo, Wenli, Perlmutter, Saul, Wright, Edward L., and Zeimann, Gregory R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present the Massive and Distant Clusters of WISE Survey (MaDCoWS), a search for galaxy clusters at 0.7-30 degrees) and the remainder of the southern extragalactic sky at Dec<-30 degrees for which shallower optical data from SuperCOSMOS Sky Survey are available. In this paper we describe the search algorithm, characterize the sample, and present the first MaDCoWS data release -- catalogs of the 2433 highest amplitude detections in the WISE--Pan-STARRS region and the 250 highest amplitude detections in the WISE--SuperCOSMOS region. A total of 1723 of the detections from the WISE--Pan-STARRS sample have also been observed with the Spitzer Space Telescope, providing photometric redshifts and richnesses, and an additional 64 detections within the WISE--SuperCOSMOS region also have photometric redshifts and richnesses. Spectroscopic redshifts for 38 MaDCoWS clusters with IRAC photometry demonstrate that the photometric redshifts have an uncertainty of $\sigma_z/(1+z)\sim0.036$. Combining the richness measurements with Sunyaev-Zel'dovich observations of MaDCoWS clusters, we also present a preliminary mass-richness relation that can be used to infer the approximate mass distribution of the full sample. The estimated median mass for the WISE--Pan-STARRS catalog is $M_{500}=1.6^{+0.7}_{-0.8}\times10^{14} \mathrm{M}_\odot$, with the Sunyaev-Zel'dovich data confirming that we detect clusters with masses up to $M_{500}\sim5\times10^{14} \mathrm{M}_\odot$ $(M_{200}\sim10^{15} \mathrm{M}_\odot)$., Comment: 26 pages, 17 figures, submitted to The Astrophysical Journal Supplement Series. Machine readable versions of tables 3-6 are included with the source files in the arXiv submission
Published: 2018
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14. SN Ia Standardization on the Rise: Evidence for the Cosmological Importance of Pre-Maximum Measurements

Author: Hayden, Brian, Rubin, David, and Strovink, Mark
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present SALT2X, an extension of the SALT2 model for SN Ia supernova light curves. SALT2X separates the light-curve-shape parameter x1 into an x1r and x1f for the rise and fall portions of the light curve. Using the Joint Lightcurve Analysis (JLA) SN sample, we assess the importance of the rising and falling portions of the light curve for cosmological standardization using a modified version of the Unified Nonlinear Inference for Type Ia cosmologY (UNITY) framework. We find strong evidence that x1r has a stronger correlation with peak magnitude than x1f. We see evidence that standardizing on the rise affects the color standardization relation, and reduces the size of the host-galaxy standardization and the unexplained ("intrinsic") luminosity dispersion. Since SNe Ia generally rise more quickly than they decline, a faster observing cadence in future surveys will be necessary to maximize the gain from this work, and to continue to explore the impacts of decoupling the rising and falling portions of SN Ia light curves., Comment: Updated to match refereed version
Published: 2018
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15. Type Ia Supernova Distances at z > 1.5 from the Hubble Space Telescope Multi-Cycle Treasury Programs: The Early Expansion Rate

Author: Riess, Adam G., Rodney, Steven A., Scolnic, Daniel M., Shafer, Daniel L., Strolger, Louis-Gregory, Ferguson, Henry C., Postman, Marc, Graur, Or, Maoz, Dan, Jha, Saurabh W., Mobasher, Bahram, Casertano, Stefano, Hayden, Brian, Molino, Alberto, Hjorth, Jens, Garnavich, Peter M., Jones, David O., Kirshner, Robert P., Koekemoer, Anton M., Grogin, Norman A., Brammer, Gabriel, Hemmati, Shoubaneh, Dickinson, Mark, Challis, Peter M., Wolff, Schuyler, Clubb, Kelsey I., Filippenko, Alexei V., Nayyeri, Hooshang, Vivian, U, Koo, David C., Faber, Sandra M., Kocevski, Dale, Bradley, Larry, and Coe, Dan
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an analysis of 15 Type Ia supernovae (SNe Ia) at redshift z > 1 (9 at 1.5 < z < 2.3) recently discovered in the CANDELS and CLASH Multi-Cycle Treasury programs using WFC3 on the Hubble Space Telescope. We combine these SNe Ia with a new compilation of 1050 SNe Ia, jointly calibrated and corrected for simulated survey biases to produce accurate distance measurements. We present unbiased constraints on the expansion rate at six redshifts in the range 0.07 < z < 1.5 based only on this combined SN Ia sample. The added leverage of our new sample at z > 1.5 leads to a factor of ~3 improvement in the determination of the expansion rate at z = 1.5, reducing its uncertainty to ~20%, a measurement of H(z=1.5)/H0=2.67 (+0.83,-0.52). We then demonstrate that these six measurements alone provide a nearly identical characterization of dark energy as the full SN sample, making them an efficient compression of the SN Ia data. The new sample of SNe Ia at z > 1 usefully distinguishes between alternative cosmological models and unmodeled evolution of the SN Ia distance indicators, placing empirical limits on the latter. Finally, employing a realistic simulation of a potential WFIRST SN survey observing strategy, we forecast optimistic future constraints on the expansion rate from SNe Ia., Comment: 14 pages, 5 figures, 7 tables; submitted to ApJ
Published: 2017
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16. The Discovery of a Gravitationally Lensed Supernova Ia at Redshift 2.22

Author: Rubin, David, Hayden, Brian, Huang, Xiaosheng, Aldering, Greg, Amanullah, Rahman, Barbary, Kyle, Boone, Kyle, Brodwin, Mark, Deustua, Susana E., Dixon, Sam, Eisenhardt, Peter, Fruchter, Andrew S., Gonzalez, Anthony H., Goobar, Ariel, Gupta, Ravi R., Hook, Isobel, Jee, M. James, Kim, Alex G., Kowalski, Marek, Lidman, Chris E., Linder, Eric, Luther, Kyle, Nordin, Jakob, Pain, Reynald, Perlmutter, Saul, Raha, Zachary, Rigault, Mickael, Ruiz-Lapuente, Pilar, Saunders, Clare M., Sofiatti, Caroline, Spadafora, Anthony L., Stanford, S. Adam, Stern, Daniel, Suzuki, Nao, and Williams, Steven C.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the discovery and measurements of a gravitationally lensed supernova (SN) behind the galaxy cluster MOO J1014+0038. Based on multi-band Hubble Space Telescope and Very Large Telescope (VLT) photometry of the supernova, and VLT spectroscopy of the host galaxy, we find a 97.5% probability that this SN is a SN Ia, and a 2.5% chance of a CC SN. Our typing algorithm combines the shape and color of the light curve with the expected rates of each SN type in the host galaxy. With a redshift of 2.2216, this is the highest redshift SN Ia discovered with a spectroscopic host-galaxy redshift. A further distinguishing feature is that the lensing cluster, at redshift 1.23, is the most distant to date to have an amplified SN. The SN lies in the middle of the color and light-curve shape distributions found at lower redshift, disfavoring strong evolution to z = 2.22. We estimate an amplification due to gravitational lensing of 2.8+0.6-0.5 (1.10 +- 0.23 mag)---compatible with the value estimated from the weak-lensing-derived mass and the mass-concentration relation from LambdaCDM simulations---making it the most amplified SN Ia discovered behind a galaxy cluster., Comment: Accepted for publication in ApJ
Published: 2017
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17. Eddington-Limited Accretion in z~2 WISE-selected Hot, Dust-Obscured Galaxies

Author: Wu, Jingwen, Jun, Hyunsung D., Assef, Roberto J., Tsai, Chao-Wei, Wright, Edward L., Eisenhardt, Peter R. M., Blain, Andrew, Stern, Daniel, Díaz-Santos, Tanio, Denney, Kelly D., Hayden, Brian T., Perlmutter, Saul, Aldering, Greg, Boone, Kyle, and Fagrelius, Parker
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Hot, Dust-Obscured Galaxies, or "Hot DOGs", are a rare, dusty, hyperluminous galaxy population discovered by the WISE mission. Predominantly at redshifts 2-3, they include the most luminous known galaxies in the universe. Their high luminosities likely come from accretion onto highly obscured super massive black holes (SMBHs). We have conducted a pilot survey to measure the SMBH masses of five z~2 Hot DOGs via broad H_alpha emission lines, using Keck/MOSFIRE and Gemini/FLAMINGOS-2. We detect broad H_alpha emission in all five Hot DOGs. We find substantial corresponding SMBH masses for these Hot DOGs (~ 10^{9} M_sun), and their derived Eddington ratios are close to unity. These z~2 Hot DOGs are the most luminous AGNs at given BH masses, suggesting they are accreting at the maximum rates for their BHs. A similar property is found for known z~6 quasars. Our results are consistent with scenarios in which Hot DOGs represent a transitional, high-accretion phase between obscured and unobscured quasars. Hot DOGs may mark a special evolutionary stage before the red quasar and optical quasar phases, and they may be present at other cosmic epochs., Comment: 15 pages, 9 figures. Accepted by ApJ
Published: 2017
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18. Design, development, and implementation of IsoBank: A centralized repository for isotopic data.

Author: Shipley, Oliver N., Dabrowski, Anna J., Bowen, Gabriel J., Hayden, Brian, Pauli, Jonathan N., Jordan, Christopher, Anderson, Lesleigh, Bailey, Adriana, Bataille, Clement P., Cicero, Carla, Close, Hilary G., Cook, Craig, Cook, Joseph A., Desai, Ankur R., Evaristo, Jaivime, Filley, Tim R., France, Christine A. M., Jackson, Andrew L., Kim, Sora Lee, and Kopf, Sebastian
Subjects: DATA libraries, STABLE isotopes, DATABASES, DATABASE design, RESEARCH personnel, VIRTUAL communities
Abstract: Stable isotope data have made pivotal contributions to nearly every discipline of the physical and natural sciences. As the generation and application of stable isotope data continues to grow exponentially, so does the need for a unifying data repository to improve accessibility and promote collaborative engagement. This paper provides an overview of the design, development, and implementation of IsoBank (www.isobank.org), a community-driven initiative to create an open-access repository for stable isotope data implemented online in 2021. A central goal of IsoBank is to provide a web-accessible database supporting interdisciplinary stable isotope research and educational opportunities. To achieve this goal, we convened a multi-disciplinary group of over 40 analytical experts, stable isotope researchers, database managers, and web developers to collaboratively design the database. This paper outlines the main features of IsoBank and provides a focused description of the core metadata structure. We present plans for future database and tool development and engagement across the scientific community. These efforts will help facilitate interdisciplinary collaboration among the many users of stable isotopic data while also offering useful data resources and standardization of metadata reporting across eco-geoinformatics landscapes. [ABSTRACT FROM AUTHOR]
Published: 2024
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19. Frozen out: unanswered questions about winter biology

Author: Sutton, Alex O., Studd, Emily K., Fernandes, Timothy, Bates, Amanda E., Bramburger, Andrew J., Cooke, Steven J., Hayden, Brian, Henry, Hugh A.L., Humphries, Murray M., Martin, Rosemary, McMeans, Bailey, Moise, Eric, O'Sullivan, Antoin M., Sharma, Sapna, and Templer, Pamela H.
Subjects: Ecosystems -- Environmental aspects, Climatic changes -- Environmental aspects, Winter -- Environmental aspects, Environmental issues
Abstract: Winter conditions impose dramatic constraints on temperate, boreal, and polar ecosystems, and shape the abiotic and biotic interactions underpinning these systems. At high latitudes, winter can last longer than the growing season and may have a disproportionately large impact on organisms and ecosystems. Even so, our understanding of the ecological implications of winter is often lacking. Indeed, even what exactly defines winter is currently unclear, and boundaries that delineate this season are blurred across marine, freshwater, and terrestrial realms and fields of biology. Here, we discuss the complexity of defining winter, and highlight the importance of maintaining the capacity to test hypotheses across seasons, realms, and domains of life. We then outline questions drawn from diverse fields of research that address current gaps in our understanding of winter ecology and how winter influences multiple levels of biological organization, from individuals to ecosystems. Finally, we highlight the potential consequences of changes to both the length and severity of winter due to climate change, and discuss the role winter may play in mediating ecosystem function in the future. Key words: climate change, communities, ecosystems, individuals, populations. Les conditions hivernales imposent des contraintes dramatiques aux ecosystemes temperes, boreaux et polaires, et elles faconnent les interactions abiotiques et biotiques qui soutiennent ces systemes. Aux hautes latitudes, l'hiver peut durer plus longtemps que la saison de croissance et il peut avoir un impact disproportionne sur les organismes et les ecosystemes. Malgre cela, notre comprehension des implications ecologiques de l'hiver est souvent insuffisante. En effet, meme ce qui definitexactementl'hiver n'est pas clair actuellement et les frontieres qui delimitent cette saison sont floues a travers les domaines marins, d'eau douce et terrestres et les champs de la biologie. Les auteurs discutent ici de la complexite de definir l'hiver et soulignent l'importance de maintenir la capacite de tester des hypotheses a travers les saisons, les roy-aumes et les domaines de la vie. Ils presentent ensuite des questions tirees de divers domaines de recherche qui visent a combler les lacunes actuelles dans notre comprehension de l'ecologie hivernale et de la facon dont l'hiver influence de multiples niveaux d'organisation biologique, des individus aux ecosystemes. Enfin, ils soulignent les consequences potentielles des changements de la duree et de la rigueur de l'hiver dus aux changements climatiques et discutent du role que l'hiver pourrait jouer dans la mediation de la fonction des ecosystemes dans le futur. [Traduit par la Redaction] Mots-cles: changements climatiques, communautes, ecosystemes, individus, populations., Introduction Ecologists have traditionally regarded winter as a dormant time of year; a time when most organisms actively or passively depress their metabolism or seek out warmer climates until spring [...]
Published: 2021
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20. Eddington-limited Accretion in z ∼ 2 WISE-selected Hot, Dust-obscured Galaxies

Author: Wu, Jingwen, Jun, Hyunsung D, Assef, Roberto J, Tsai, Chao-Wei, Wright, Edward L, Eisenhardt, Peter RM, Blain, Andrew, Stern, Daniel, Díaz-Santos, Tanio, Denney, Kelly D, Hayden, Brian T, Perlmutter, Saul, Aldering, Greg, Boone, Kyle, and Fagrelius, Parker
Subjects: galaxies: evolution, galaxies: high-redshift, galaxies: ISM, infrared: galaxies, quasars: supermassive black holes, astro-ph.GA, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract: Hot, dust-obscured galaxies, or "Hot DOGs," are a rare, dusty, hyperluminous galaxy population discovered by the WISE mission. Predominantly at redshifts 2-3, they include the most luminous known galaxies in the universe. Their high luminosities likely come from accretion onto highly obscured supermassive black holes (SMBHs). We have conducted a pilot survey to measure the SMBH masses of five z ∼ 2 Hot DOGs via broad Hα emission lines, using Keck/MOSFIRE and Gemini/FLAMINGOS-2. We detect broad Hα emission in all five Hot DOGs. We find substantial corresponding SMBH masses for these Hot DOGs (∼ 109 M⊙), and their derived Eddington ratios are close to unity. These z ∼ 2 Hot DOGs are the most luminous active galactic nuclei for their BH masses, suggesting that they are accreting at the maximum rates for their BHs. A similar property is found for known z ∼ 6 quasars. Our results are consistent with scenarios in which Hot DOGs represent a transitional, high-accretion phase between obscured and unobscured quasars. Hot DOGs may mark a special evolutionary stage before the red quasar and optical quasar phases, and they may be present at other cosmic epochs.
Published: 2018

21. Is the expansion of the universe accelerating? All signs point to yes

Author: Rubin, David and Hayden, Brian
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The accelerating expansion of the universe is one of the most profound discoveries in modern cosmology, pointing to a universe in which 70% of the mass-energy density has an unknown form spread uniformly across the universe. This result has been well established using a combination of cosmological probes (e.g., Planck Collaboration et al. 2016), resulting in a "standard model" of modern cosmology that is a combination of a cosmological constant with cold dark matter and baryons. The first compelling evidence for the acceleration came in the late 1990's, when two independent teams studying type Ia supernovae discovered that distant SNe Ia were dimmer than expected. The combined analysis of modern cosmology experiments, including SNe Ia, the Hubble constant, baryon acoustic oscillations, and the cosmic microwave background has now measured the contributions of matter and the cosmological constant to the energy density of the universe to better than 0.01, providing a secure measurement of acceleration. A recent study (Tr{\o}st Nielsen et al. 2015) has claimed that the evidence for acceleration from SNe Ia is "marginal." Here we demonstrate errors in that analysis which reduce the acceleration significance from SNe Ia, and further demonstrate that conservative constraints on the curvature or matter density of the universe increase the significance even more. Analyzing the Joint Light-curve Analysis supernova sample, we find 4.2{\sigma} evidence for acceleration with SNe Ia alone, and 11.2{\sigma} in a flat universe. With our improved supernova analysis and by not rejecting all other cosmological constraints, we find that acceleration is quite secure., Comment: Accepted for publication. New cosmological models and new figures
Published: 2016
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22. The Massive and Distant Clusters of WISE Survey: MOO J1142+1527, A 10$^{15}$ M$_\odot$ Galaxy Cluster at z=1.19

Author: Gonzalez, Anthony H., Decker, Bandon, Brodwin, Mark, Eisenhardt, Peter R. M., Marrone, Daniel P., Stanford, S. A., Stern, Daniel, Wylezalek, Dominika, Aldering, Greg, Abdulla, Zubair, Boone, Kyle, Carlstrom, John, Fagrelius, Parker, Gettings, Daniel P., Greer, Christopher H., Hayden, Brian, Leitch, Erik M., Lin, Yen-Ting, Mantz, Adam B., Muchovej, Stephen, Perlmutter, Saul, and Zeimann, Gregory R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present confirmation of the cluster MOO J1142+1527, a massive galaxy cluster discovered as part of the Massive and Distant Clusters of WISE Survey. The cluster is confirmed to lie at $z=1.19$, and using the Combined Array for Research in Millimeter-wave Astronomy we robustly detect the Sunyaev-Zel'dovich (SZ) decrement at 13.2$\sigma$. The SZ data imply a mass of $\mathrm{M}_{200m}=(1.1\pm0.2)\times10^{15}$ $\mathrm{M}_\odot$, making MOO J1142+1527 the most massive galaxy cluster known at $z>1.15$ and the second most massive cluster known at $z>1$. For a standard $\Lambda$CDM cosmology it is further expected to be one of the $\sim 5$ most massive clusters expected to exist at $z\ge1.19$ over the entire sky. Our ongoing Spitzer program targeting $\sim1750$ additional candidate clusters will identify comparably rich galaxy clusters over the full extragalactic sky., Comment: Submitted to ApJ Letters, 6 pages, 4 figures
Published: 2015
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23. An Extreme Starburst in Close Proximity to the Central Galaxy of a Rich Galaxy Cluster at z=1.7

Author: Webb, Tracy, Noble, Allison, DeGroot, Andrew, Wilson, Gillian, Muzzin, Adam, Bonaventura, Nina, Cooper, Mike, Delahaye, Anna, Foltz, Ryan, Lidman, Chris, Surace, Jason, Yee, H. K. C, Chapman, Scott, Dunne, Loretta, Geach, James, Hayden, Brian, Hildebrandt, Hendrik, Huang, Jiasheng, Pope, Alexandra, Smith, Matthew W. L., Perlmutter, Saul, and Tudorica, Alex
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have discovered an optically rich galaxy cluster at z=1.7089 with star formation occurring in close proximity to the central galaxy. The system, SpARCS104922.6+564032.5, was detected within the Spitzer Adaptation of the red-sequence Cluster Survey, (SpARCS), and confirmed through Keck-MOSFIRE spectroscopy. The rest-frame optical richness of Ngal(500kpc) = 30+/-8 implies a total halo mass, within 500kpc, of ~3.8+/-1.2 x 10^14 Msun, comparable to other clusters at or above this redshift. There is a wealth of ancillary data available, including Canada-France-Hawaii Telescope optical, UKIRT-K, Spitzer-IRAC/MIPS, and Herschel-SPIRE. This work adds submillimeter imaging with the SCUBA2 camera on the James Clerk Maxwell Telescope and near-infrared imaging with the Hubble Space Telescope (HST). The mid/far-infrared (M/FIR) data detect an Ultra-luminous Infrared Galaxy spatially coincident with the central galaxy, with LIR = 6.2+/-0.9 x 10^12 Lsun. The detection of polycyclic aromatic hydrocarbons (PAHs) at z=1.7 in a Spitzer-IRS spectrum of the source implies the FIR luminosity is dominated by star formation (an Active Galactic Nucleus contribution of 20%) with a rate of ~860+/-30 Msun/yr. The optical source corresponding to the IR emission is likely a chain of of > 10 individual clumps arranged as "beads on a string" over a linear scale of 66 kpc. Its morphology and proximity to the Brightest Cluster Galaxy imply a gas-rich interaction at the center of the cluster triggered the star formation. This system indicates that wet mergers may be an important process in forming the stellar mass of BCGs at early times., Comment: 11 pages, 5 figures, accepted for publication in the Astrophysical Journal
Published: 2015
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24. Two Type Ia Supernovae at Redshift ~2 : Improved Classification and Redshift Determination with Medium-band Infrared Imaging

Author: Rodney, Steven A., Riess, Adam G., Scolnic, Daniel M., Jones, David O., Hemmati, Shoubaneh, Molino, Alberto, McCully, Curtis, Mobasher, Bahram, Strolger, Louis-Gregory, Graur, Or, Hayden, Brian, and Casertano, Stefano
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: We present two supernovae (SNe) discovered with the Hubble Space Telescope (HST) in the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS), an HST multi-cycle treasury program. We classify both objects as Type Ia SNe and find redshifts of z = 1.80+-0.02 and 2.26 +0.02 -0.10, the latter of which is the highest redshift Type Ia SN yet seen. Using light curve fitting we determine luminosity distances and find that both objects are consistent with a standard Lambda-CDM cosmological model. These SNe were observed using the HST Wide Field Camera 3 infrared detector (WFC3-IR), with imaging in both wide- and medium-band filters. We demonstrate that the classification and redshift estimates are significantly improved by the inclusion of single-epoch medium-band observations. This medium-band imaging approximates a very low resolution spectrum (lambda/delta lambda ~ 100) which can isolate broad spectral absorption features that differentiate Type Ia SNe from their most common core collapse cousins. This medium-band method is also insensitive to dust extinction and (unlike grism spectroscopy) it is not affected by contamination from the SN host galaxy or other nearby sources. As such, it can provide a more efficient - though less precise - alternative to IR spectroscopy for high-z SNe., Comment: This version corrects errors in values reported in the text for x1, c, and mB for both Type Ia SNe (erratum accepted to AJ). This error was only in the text, and did not affect any figures or conclusions
Published: 2015
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25. UNITY: Confronting Supernova Cosmology's Statistical and Systematic Uncertainties in a Unified Bayesian Framework

Author: Rubin, David, Aldering, Greg, Barbary, Kyle, Boone, Kyle, Chappell, Greta, Currie, Miles, Deustua, Susana, Fagrelius, Parker, Fruchter, Andrew, Hayden, Brian, Lidman, Chris, Nordin, Jakob, Perlmutter, Saul, Saunders, Clare, and Sofiatti, Caroline
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: While recent supernova cosmology research has benefited from improved measurements, current analysis approaches are not statistically optimal and will prove insufficient for future surveys. This paper discusses the limitations of current supernova cosmological analyses in treating outliers, selection effects, shape- and color-standardization relations, unexplained dispersion, and heterogeneous observations. We present a new Bayesian framework, called UNITY (Unified Nonlinear Inference for Type-Ia cosmologY), that incorporates significant improvements in our ability to confront these effects. We apply the framework to real supernova observations and demonstrate smaller statistical and systematic uncertainties. We verify earlier results that SNe Ia require nonlinear shape and color standardizations, but we now include these nonlinear relations in a statistically well-justified way. This analysis was primarily performed blinded, in that the basic framework was first validated on simulated data before transitioning to real data. We also discuss possible extensions of the method., Comment: Minor fix in PGM
Published: 2015
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26. Growth of amorphous, anatase and rutile phase TiO2 thin films on Pt/TiO2/SiO2/Si (SSTOP) substrate for resistive random access memory (ReRAM) device application

Author: Alsaiari, Mabkhoot A., Alhemiary, Nabil A., Umar, Ahmad, and Hayden, Brian E.
Published: 2020
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27. Type Ia Supernova Rate Measurements to Redshift 2.5 from CANDELS : Searching for Prompt Explosions in the Early Universe

Author: Rodney, Steven A., Riess, Adam G., Strolger, Louis-Gregory, Dahlen, Tomas, Graur, Or, Casertano, Stefano, Dickinson, Mark E., Ferguson, Henry C., Garnavich, Peter, Hayden, Brian, Jha, Saurabh W., Jones, David O., Kirshner, Robert P., Koekemoer, Anton M., McCully, Curtis, Mobasher, Bahram, Patel, Brandon, Weiner, Benjamin J., Cenko, S. Bradley, Clubb, Kelsey I., Cooper, Michael, Filippenko, Alexei V., Frederiksen, Teddy F., Hjorth, Jens, Leibundgut, Bruno, Matheson, Thomas, Nayyeri, Hooshang, Penner, Kyle, Trump, Jonathan, Silverman, Jeffrey M., U, Vivian, Bostroem, K. Azalee, Challis, Peter, Rajan, Abhijith, Wolff, Schuyler, Faber, S. M., Grogin, Norman A., and Kocevski, Dale
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of ~0.25 deg^2 with ~900 HST orbits spread across 5 fields over 3 years. Within these survey images we discovered 65 supernovae (SN) of all types, out to z~2.5. We classify ~24 of these as Type Ia SN (SN Ia) based on host-galaxy redshifts and SN photometry (supplemented by grism spectroscopy of 6 SN). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z=2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SN that exploded when the universe was only ~3 Gyr old and near the peak of the cosmic star-formation history. This gives the CANDELS high-redshift sample unique leverage for evaluating the fraction of SN Ia that explode promptly after formation (<500 Myr). Combining the CANDELS rates with all available SN Ia rate measurements in the literature we find that this prompt SN Ia fraction is fP=0.53 +0.09 -0.10 (stat) +0.10 -0.26 (sys), consistent with a delay time distribution that follows a simple t^{-1} power law for all times t>40 Myr. However, a mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH, we find a low rate of SN Ia at z>1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only ~20% of all SN Ia explosions -- though further analysis and larger samples will be needed to examine that suggestion., Comment: 20 pages + 10-page appendix, 12 figures + 5 in appendix; Accepted to AJ ; latest version includes updates to discussion and figures, responding to referee and others
Published: 2014
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28. The Data Release of the Sloan Digital Sky Survey-II Supernova Survey

Author: Sako, Masao, Bassett, Bruce, Becker, Andrew C., Brown, Peter J., Campbell, Heather, Cane, Rachel, Cinabro, David, D'Andrea, Chris B., Dawson, Kyle S., DeJongh, Fritz, Depoy, Darren L., Dilday, Ben, Doi, Mamoru, Filippenko, Alexei V., Fischer, John A., Foley, Ryan J., Frieman, Joshua A., Galbany, Lluis, Garnavich, Peter M., Goobar, Ariel, Gupta, Ravi R., Hill, Gary J., Hayden, Brian T., Hlozek, Renee, Holtzman, Jon A., Hopp, Ulrich, Jha, Saurabh W., Kessler, Richard, Kollatschny, Wolfram, Leloudas, Giorgos, Marriner, John, Marshall, Jennifer L., Miquel, Ramon, Morokuma, Tomoki, Mosher, Jennifer, Nichol, Robert C., Nordin, Jakob, Olmstead, Matthew D., Ostman, Linda, Prieto, Jose L., Richmond, Michael, Romani, Roger W., Sollerman, Jesper, Stritzinger, Max, Schneider, Donald P., Smith, Mathew, Wheeler, J. Craig, Yasuda, Naoki, and Zheng, Chen
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper describes the data release of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey conducted between 2005 and 2007. Light curves, spectra, classifications, and ancillary data are presented for 10,258 variable and transient sources discovered through repeat ugriz imaging of SDSS Stripe 82, a 300 deg2 area along the celestial equator. This data release is comprised of all transient sources brighter than r~22.5 mag with no history of variability prior to 2004. Dedicated spectroscopic observations were performed on a subset of 889 transients, as well as spectra for thousands of transient host galaxies using the SDSS-III BOSS spectrographs. Photometric classifications are provided for the candidates with good multi-color light curves that were not observed spectroscopically. From these observations, 4607 transients are either spectroscopically confirmed, or likely to be, supernovae, making this the largest sample of supernova candidates ever compiled. We present a new method for SN host-galaxy identification and derive host-galaxy properties including stellar masses, star-formation rates, and the average stellar population ages from our SDSS multi-band photometry. We derive SALT2 distance moduli for a total of 1443 SN Ia with spectroscopic redshifts as well as photometric redshifts for a further 677 purely-photometric SN Ia candidates. Using the spectroscopically confirmed subset of the three-year SDSS-II SN Ia sample and assuming a flat Lambda-CDM cosmology, we determine Omega_M = 0.315 +/- 0.093 (statistical error only) and detect a non-zero cosmological constant at 5.7 sigmas., Comment: Submitted to ApJS. Full catalogs and datafiles are available here: http://sdssdp62.fnal.gov/sdsssn/DataRelease/index.html
Published: 2014
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29. AN EXTREME STARBURST IN THE CORE OF A RICH GALAXY CLUSTER AT z = 1.7

Author: Webb, Tracy, Noble, Allison, DeGroot, Andrew, Wilson, Gillian, Muzzin, Adam, Bonaventura, Nina, Cooper, Mike, Delahaye, Anna, Foltz, Ryan, Lidman, Chris, Surace, Jason, Yee, HKC, Chapman, Scott, Dunne, Loretta, Geach, James, Hayden, Brian, Hildebrandt, Hendrik, Huang, Jiasheng, Pope, Alexandra, Smith, Matthew WL, Perlmutter, Saul, and Tudorica, Alex
Subjects: Space Sciences, Physical Sciences, galaxies: clusters: general, galaxies: evolution, galaxies: interactions, galaxies: starburst, astro-ph.GA, astro-ph.CO, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We have discovered an optically rich galaxy cluster at z = 1.7089 with star formation occurring in close proximity to the central galaxy. The system, SpARCS104922.6+564032.5, was detected within the Spitzer Adaptation of the red-sequence Cluster Survey, and confirmed through Keck-MOSFIRE spectroscopy. The rest-frame optical richness of Ngal (500 kpc) = 30 8 implies a total halo mass, within 500 kpc, of ∼3.8 1.2 1014 Mo, comparable to other clusters at or above this redshift. There is a wealth of ancillary data available, including Canada-France-Hawaii Telescope optical, UKIRT-K, Spitzer-IRAC/MIPS, and Herschel-SPIRE. This work adds submillimeter imaging with the SCUBA2 camera on the James Clerk Maxwell Telescope and near-infrared imaging with the Hubble Space Telescope. The mid/far-infrared (M/FIR) data detect an Ultra-luminous Infrared Galaxy spatially coincident with the central galaxy, with LIR = 6.2 0.9 1012 Lo. The detection of polycyclic aromatic hydrocarbons at z = 1.7 in a Spitzer-IRS spectrum of the source implies the FIR luminosity is dominated by star formation (an Active Galactic Nucleus contribution of 20%) with a rate of ∼860 130 Mo yr-1. The optical source corresponding to the IR emission is likely a chain of >10 individual clumps arranged as "beads on a string" over a linear scale of 66 kpc. Its morphology and proximity to the Brightest Cluster Galaxy (BCG) imply a gas-rich interaction at the center of the cluster triggered the star formation. This system indicates that wet mergers may be an important process in forming the stellar mass of BCGs at early times.
Published: 2015

30. The Discovery of the Most Distant Known Type Ia Supernova at Redshift 1.914

Author: Jones, David O., Rodney, Steven A., Riess, Adam G., Mobasher, Bahram, Dahlen, Tomas, McCully, Curtis, Frederiksen, Teddy F., Casertano, Stefano, Hjorth, Jens, Keeton, Charles R., Koekemoer, Anton, Strolger, Louis-Gregory, Wiklind, Tommy G., Challis, Peter, Graur, Or, Hayden, Brian, Patel, Brandon, Weiner, Benjamin J., Filippenko, Alexei V., Garnavich, Peter, Jha, Saurabh W., Kirshner, Robert P., Ferguson, Henry C., Grogin, Norman A., and Kocevski, Dale
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the discovery of a Type Ia supernova (SN) at redshift $z = 1.914$ from the CANDELS multi-cycle treasury program on the \textit{Hubble Space Telescope (HST)}. This SN was discovered in the infrared using the Wide-Field Camera 3, and it is the highest-redshift Type Ia SN yet observed. We classify this object as a SN\,Ia by comparing its light curve and spectrum with those of a large sample of Type Ia and core-collapse supernovae (SNe). Its apparent magnitude is consistent with that expected from the $\Lambda$CDM concordance cosmology. We discuss the use of spectral evidence for classification of $z > 1.5$ SNe\,Ia using {\it HST} grism simulations, finding that spectral data alone can frequently rule out SNe\,II, but distinguishing between SNe\,Ia and SNe\,Ib/c can require prohibitively long exposures. In such cases, a quantitative analysis of the light curve may be necessary for classification. Our photometric and spectroscopic classification methods can aid the determination of SN rates and cosmological parameters from the full high-redshift CANDELS SN sample., Comment: 10 pages, 5 figures; accepted for publication in ApJ; minor changes
Published: 2013
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31. The Fundamental Metallicity Relation Reduces Type Ia SN Hubble Residuals More Than Host Mass Alone

Author: Hayden, Brian T., Gupta, Ravi R., Garnavich, Peter M., Mannucci, Filippo, Nichol, Robert C., and Sako, Masao
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Type Ia Supernova Hubble residuals have been shown to correlate with host galaxy mass, imposing a major obstacle for their use in measuring dark energy properties. Here, we calibrate the fundamental metallicity relation (FMR) of Mannucci et al. (2010) for host mass and star formation rates measured from broad-band colors alone. We apply the FMR to the large number of hosts from the SDSS-II sample of Gupta et al. (2011) and find that the scatter in the Hubble residuals is significantly reduced when compared with using only stellar mass (or the mass-metallicity relation) as a fit parameter. Our calibration of the FMR is restricted to only star-forming galaxies and in the Hubble residual calculation we include only hosts with log(SFR) > -2. Our results strongly suggest that metallicity is the underlying source of the correlation between Hubble residuals and host galaxy mass. Since the FMR is nearly constant between z = 2 and the present, use of the FMR along with light curve width and color should provide a robust distance measurement method that minimizes systematic errors., Comment: 14 pages, 14 figures, submitted response to ApJ referee comments on Dec 6, 2012
Published: 2012
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32. The fabrication of graphene-reinforced Al-based nanocomposites using high-pressure torsion

Author: Huang, Yi, Bazarnik, Piotr, Wan, Diqing, Luo, Dan, Pereira, Pedro Henrique R., Lewandowska, Malgorzata, Yao, Jin, Hayden, Brian E., and Langdon, Terence G.
Published: 2019
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33. The particle size dependence of CO oxidation on model planar titania supported gold catalysts measured by parallel thermographic imaging

Author: Emmanuel, Jovine, Hayden, Brian E., and Saleh-Subaie, Jaffar
Published: 2019
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34. A Type Ia Supernova at Redshift 1.55 in Hubble Space Telescope Infrared Observations from CANDELS

Author: Rodney, Steven A., Riess, Adam G., Dahlen, Tomas, Strolger, Louis-Gregory, Ferguson, Henry C., Hjorth, Jens, Frederiksen, Teddy F., Weiner, Benjamin J., Mobasher, Bahram, Casertano, Stefano, Jones, David O., Challis, Peter, Faber, S. M., Filippenko, Alexei V., Garnavich, Peter, Graur, Or, Grogin, Norman A., Hayden, Brian, Jha, Saurabh W., Kirshner, Robert P., Kocevski, Dale, Koekemoer, Anton, McCully, Curtis, Patel, Brandon, Rajan, Abhijith, and Scarlata, Claudia
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the discovery of a Type Ia supernova (SNIa) at redshift z=1.55 with the infrared detector of the Wide Field Camera 3 (WFC3-IR) on the Hubble Space Telescope (HST). This object was discovered in CANDELS imaging data of the Hubble Ultra Deep Field, and followed as part of the CANDELS+CLASH Supernova project, comprising the SN search components from those two HST multi-cycle treasury programs. This is the highest redshift SNIa with direct spectroscopic evidence for classification. It is also the first SN Ia at z>1 found and followed in the infrared, providing a full light curve in rest-frame optical bands. The classification and redshift are securely defined from a combination of multi-band and multi-epoch photometry of the SN, ground-based spectroscopy of the host galaxy, and WFC3-IR grism spectroscopy of both the SN and host. This object is the first of a projected sample at z>1.5 that will be discovered by the CANDELS and CLASH programs. The full CANDELS+CLASH SN Ia sample will enable unique tests for evolutionary effects that could arise due to differences in SN Ia progenitor systems as a function of redshift. This high-z sample will also allow measurement of the SN Ia rate out to z~2, providing a complementary constraint on SN Ia progenitor models., Comment: 10 pages, 6 figures, accepted for publication in ApJ
Published: 2012
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35. Single or Double Degenerate Progenitors? Searching for Shock Emission in the SDSS-II Type Ia Supernovae

Author: Hayden, Brian T., Garnavich, Peter M., Kasen, Daniel, Dilday, Benjamin, Frieman, Joshua A., Jha, Saurabh W., Lampeitl, Hubert, Nichol, Robert C., Sako, Masao, Schneider, Donald P., Smith, Mathew, Sollerman, Jesper, and Wheeler, J. Craig
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: From the set of nearly 500 spectroscopically confirmed type~Ia supernovae and around 10,000 unconfirmed candidates from SDSS-II, we select a subset of 108 confirmed SNe Ia with well-observed early-time light curves to search for signatures from shock interaction of the supernova with a companion star. No evidence for shock emission is seen; however, the cadence and photometric noise could hide a weak shock signal. We simulate shocked light curves using SN Ia templates and a simple, Gaussian shock model to emulate the noise properties of the SDSS-II sample and estimate the detectability of the shock interaction signal as a function of shock amplitude, shock width, and shock fraction. We find no direct evidence for shock interaction in the rest-frame $B$-band, but place an upper limit on the shock amplitude at 9% of supernova peak flux ($M_B > -16.6$ mag). If the single degenerate channel dominates type~Ia progenitors, this result constrains the companion stars to be less than about 6 $M_{\odot}$ on the main sequence, and strongly disfavors red giant companions., Comment: 28 pages, 3 figures
Published: 2010
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36. The Rise and Fall of Type Ia Supernova Light Curves in the SDSS-II Supernova Survey

Author: Hayden, Brian T., Garnavich, Peter M., Kessler, Richard, Frieman, Joshua A., Jha, Saurabh W., Cinabro, David, Dilday, Benjamin, Kasen, Daniel, Marriner, John, Nichol, Robert C., Riess, Adam G., Sako, Masao, Schneider, Donald P., Smith, Mathew, Sollerman, Jesper, and Bassett, Bruce
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We analyze the rise and fall times of type Ia supernova (SN Ia) light curves discovered by the SDSS-II Supernova Survey. From a set of 391 light curves k-corrected to the rest frame B and V bands, we find a smaller dispersion in the rising portion of the light curve compared to the decline. This is in qualitative agreement with computer models which predict that variations in radioactive nickel yield have less impact on the rise than on the spread of the decline rates. The differences we find in the rise and fall properties suggest that a single 'stretch' correction to the light curve phase does not properly model the range of SN Ia light curve shapes. We select a subset of 105 light curves well-observed in both rise and fall portions of the light curves and develop a '2-stretch' fit algorithm which estimates the rise and fall times independently. We find the average time from explosion to B-band peak brightness is 17.38 +/- 0.17 days. Our average rise time is shorter than the 19.5 days found in previous studies; this reflects both the different light curve template used and the application of the 2-stretch algorithm. We find that slow declining events tend to have fast rise times, but that the distribution of rise minus fall time is broad and single-peaked. This distribution is in contrast to the bimodality in this parameter that was first suggested by Strovink (2007) from an analysis of a small set of local SNe Ia. We divide the SDSS-II sample in half based on the rise minus fall value, tr-tf <= 2 days and tr-tf>2 days, to search for differences in their host galaxy properties and Hubble residuals; we find no difference in host galaxy properties or Hubble residuals in our sample., Comment: 42 pages, 15 figures, accepted to ApJ for publication in March 2010, v711 issue
Published: 2010
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37. TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE

Author: Rodney, Steven A, Riess, Adam G, Strolger, Louis-Gregory, Dahlen, Tomas, Graur, Or, Casertano, Stefano, Dickinson, Mark E, Ferguson, Henry C, Garnavich, Peter, Hayden, Brian, Jha, Saurabh W, Jones, David O, Kirshner, Robert P, Koekemoer, Anton M, McCully, Curtis, Mobasher, Bahram, Patel, Brandon, Weiner, Benjamin J, Cenko, S Bradley, Clubb, Kelsey I, Cooper, Michael, Filippenko, Alexei V, Frederiksen, Teddy F, Hjorth, Jens, Leibundgut, Bruno, Matheson, Thomas, Nayyeri, Hooshang, Penner, Kyle, Trump, Jonathan, Silverman, Jeffrey M, Vivian, U, Bostroem, K Azalee, Challis, Peter, Rajan, Abhijith, Wolff, Schuyler, Faber, SM, Grogin, Norman A, and Kocevski, Dale
Subjects: infrared: general, supernovae: general, surveys, astro-ph.CO, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of ∼0.25 deg2 with ∼900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z ∼ 2.5. We classify ∼24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z = 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only ∼3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation ( 40 Myr. However, mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH (Cluster Lensing And Supernova Survey with Hubble), we find a low rate of SNe Ia at z > 1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only 20% of all SN Ia explosions - though further analysis and larger samples will be needed to examine that suggestion. © 2014. The American Astronomical Society. All rights reserved.
Published: 2014

38. Why we need a centralized repository for isotopic data

Author: Pauli, Jonathan N., Newsome, Seth D., Cook, Joseph A., Harrod, Chris, Steffan, Shawn A., Baker, Christopher J. O., Ben-David, Merav, Bloom, David, Bowen, Gabriel J., Cerling, Thure E., Cicero, Carla, Cook, Craig, Dohm, Michelle, Dharampal, Prarthana S., Graves, Gary, Gropp, Robert, Hobson, Keith A., Jordan, Chris, MacFadden, Bruce, Birch, Suzanne Pilaar, Poelen, Jorrit, Ratnasingham, Sujeevan, Russell, Laura, Stricker, Craig A., Uhen, Mark D., Yarnes, Christopher T., and Hayden, Brian
Published: 2017

39. Were Luxury Foods the First Domesticates? Ethnoarchaeological Perspectives from Southeast Asia

Author: Hayden, Brian
Published: 2003

40. Cultural Collapses in the Northwest: A Reply to Ian Kuijt

Author: Hayden, Brian and Ryder, June
Published: 2003
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41. Observations on the Prehistoric Social and Economic Structure of the North American Plateau

Author: Hayden, Brian
Published: 1997

42. The Plateau Interaction Sphere and Late Prehistoric Cultural Complexity

Author: Hayden, Brian and Schulting, Rick
Published: 1997
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43. The World's Longest-Lived Corporate Group: Lithic Analysis Reveals Prehistoric Social Organization near Lillooet, British Columbia

Author: Hayden, Brian, Bakewell, Edward, and Gargett, Rob
Published: 1996
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44. Roadmap on chalcogenide photonics

Author: Gholipour, Behrad, primary, Elliott, Stephen R, additional, Müller, Maximilian J, additional, Wuttig, Matthias, additional, Hewak, Daniel W, additional, Hayden, Brian E, additional, Li, Yifei, additional, Jo, Seong Soon, additional, Jaramillo, Rafael, additional, Simpson, Robert E, additional, Tominaga, Junji, additional, Cui, Yihao, additional, Mandal, Avik, additional, Eggleton, Benjamin J, additional, Rochette, Martin, additional, Rezaei, Mohsen, additional, Alamgir, Imtiaz, additional, Shamim, Hosne Mobarok, additional, Kormokar, Robi, additional, Anjum, Arslan, additional, Zeweldi, Gebrehiwot Tesfay, additional, Karnik, Tushar Sanjay, additional, Hu, Juejun, additional, Kasap, Safa O, additional, Belev, George, additional, and Reznik, Alla, additional
Published: 2023
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45. Foragers or « Feasters ? » Inequalities in the Upper Palaeolithic

Author: Hayden, Brian
Subjects: Paléolithique supérieur, inequality, chasseurs/cueilleurs, transegalitarian societies, General Engineering, Upper Paleolithic, inégalité, prestige items, hunter/gatherers, sociétés transégalitaires, objets de prestige
Abstract: Over the last half century, the dominant view in European archaeology has been that Upper Paleolithic societies were highly mobile egalitarian groups. While this model may be accurate for resource poor areas, it is increasingly evident that in some rich refugia like the Dordogne and Charente, more complex societies existed that exhibited transegalitarian types of characteristics including socioeconomic inequalities. Ethnographically, it is in the context of transegalitarian types of societies that unique features occur such as rich burials, prestige items, feasting, complex astronomical observations, elaborate numbering systems, rituals in deep caves, and other special features of the French Southwest Upper Paleolithic. Indeed, due to the socioeconomic dynamics involved, these features make the most sense as part of transegalitarian societies, whereas both the dynamics and these features are rare or are completely lacking among ethnographic egalitarian foragers. This paper re-assesses the status of Upper Paleolithic hunter/gatherers from the transegalitarian perspective. It focuses particular attention on the role and importance of prestige items making the important distinction between communal ritual prestige items and individual status prestige items. Ten other key features are discussed briefly that indicate the existence of complex hunter/gatherers in the Upper Paleolithic. Depuis un demi-siècle, le point de vue dominant de l’archéologie européenne est de considérer que les groupes humains du Paléolithique supérieur vivaient dans des sociétés égalitaires très mobiles. Bien que ce modèle puisse être exact pour les régions pauvres en ressources, il apparaît probable que dans certains refuges riches en ressources comme en Dordogne et en Charente, des sociétés de type transégalitaire marquées par des inégalités socio-économiques aient existé.D'un point de vue ethnographique, c'est préférentiellement dans ce type de dynamique socio-économique que naissent les sépultures, les objets de prestige, les festins, les observations astronomiques complexes, les systèmes de numérotation élaborés, les rituels dans les grottes profondes, autant d’aspects que l’on rencontre dans le Paléolithique supérieur du Sud-Ouest français et qui n’existent pas, ou de manière erratique, parmi les nomades égalitaires.Cet article se propose de réévaluer le statut des chasseurs-cueilleurs du Paléolithique supérieur dans une perspective sociale transégalitaire. Il porte une attention particulière au rôle et à l'importance des objets de prestige en établissant une distinction entre les objets de prestige destinés aux rituels communautaires et ceux qui ont pour vocation de marquer le rang élevé des individus. Dix autres caractéristiques clés sont brièvement abordées qui plaident pour l'existence de sociétés complexes de chasseurs-cueilleurs au Paléolithique supérieur.
Published: 2021

46. Parallel evolution of profundal Arctic charr morphs in two contrasting fish communities

Author: Knudsen, Rune, Amundsen, Per-Arne, Eloranta, Antti P., Hayden, Brian, Siwertsson, Anna, and Klemetsen, Anders
Published: 2016
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47. A specialised cannibalistic Arctic charr morph in the piscivore guild of a subarctic lake

Author: Knudsen, Rune, Gjelland, Karl Øystein, Eloranta, Antti P., Hayden, Brian, Siwertsson, Anna, Amundsen, Per-Arne, and Klemetsen, Anders
Published: 2016
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48. Lake morphometry and resource polymorphism determine niche segregation between cool- and cold-water-adapted fish

Author: Hayden, Brian, Harrod, Chris, and Kahilainen, Kimmo K.
Published: 2014

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