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51. 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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52. A High-Eccentricity Warm Jupiter Orbiting TOI-4127

Author: Gupta, Arvind F., Jackson, Jonathan M., Hebrard, Guillaume, Lin, Andrea S., Stassun, Keivan G., Dong, Jiayin, Villanueva, Steven, Dragomir, Diana, Mahadevan, Suvrath, Wright, Jason T., Almenara, Jose Manuel, Blake, Cullen H., Boisse, Isabelle, Cortes-Zuleta, Pia, Dalba, Paul A., Diaz, Rodrigo F., Ford, Eric B., Forveille, Thierry, Gagliano, Robert, Halverson, Samuel P., Heidari, Neda, Kanodia, Shubham, Kiefer, Flavien, Latham, David W., McElwain, Michael W., Mireles, Ismael, Pepper, Joshua, Ricker, George R., Robertson, Paul, Roy, Arpita, Schlecker, Martin, Schwab, Christian, Seager, Sara, Shporer, Avi, Stefansson, Gudmundur, Terrien, Ryan C., Ting, Eric B., Winn, Joshua N., and Youngblood, Allison
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the discovery of TOI-4127 b, a transiting, Jupiter-sized exoplanet on a long-period ($P = 56.39879^{+0.00010}_{-0.00010}$ d), high-eccentricity orbit around a late F-type dwarf star. This warm Jupiter was first detected and identified as a promising candidate from a search for single-transit signals in TESS Sector 20 data, and later characterized as a planet following two subsequent transits (TESS Sectors 26 and 53) and follow-up ground-based RV observations with the NEID and SOPHIE spectrographs. We jointly fit the transit and RV data to constrain the physical ($R_p = 1.096^{+0.039}_{-0.032} R_J$, $M_p = 2.30^{+0.11}_{-0.11} M_J$) and orbital parameters of the exoplanet. Given its high orbital eccentricity ($e=0.7471^{+0.0078}_{-0.0086}$), TOI-4127 b is a compelling candidate for studies of warm Jupiter populations and of hot Jupiter formation pathways. We show that the present periastron separation of TOI-4127 b is too large for high-eccentricity tidal migration to circularize its orbit, and that TOI-4127 b is unlikely to be a hot Jupiter progenitor unless it is undergoing angular momentum exchange with an undetected outer companion. Although we find no evidence for an external companion, the available observational data are insufficient to rule out the presence of a perturber that can excite eccentricity oscillations and facilitate tidal migration.
Published: 2023
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53. An extreme test case for planet formation: a close-in Neptune orbiting an ultracool star

Author: Stefansson, Gudmundur, Mahadevan, Suvrath, Miguel, Yamila, Robertson, Paul, Delamer, Megan, Kanodia, Shubham, Cañas, Caleb, Winn, Joshua, Ninan, Joe, Terrien, Ryan, Holcomb, Rae, Ford, Eric, Zawadzki, Brianna, Bowler, Brendan P., Bender, Chad, Cochran, William, Diddams, Scott, Endl, Michael, Fredrick, Connor, Halverson, Samuel, Hearty, Fred, Hill, Gary J., Lin, Andrea, Metcalf, Andrew, Monson, Andrew, Ramsey, Lawrence, Roy, Arpita, Schwab, Christian, Wright, Jason, and Zeimann, Gregory
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: In current theories of planet formation, close-orbiting planets as massive as Neptune are expected to be very rare around low-mass stars. We report the discovery of a Neptune-mass planet orbiting the `ultracool' star LHS 3154, which is nine times less massive than the Sun. The planet's orbital period is 3.7 days and its minimum mass is 13.2 Earth masses, giving it the largest known planet-to-star mass ratio among short-period planets ($<$\,100 days) orbiting ultracool stars. Both the core accretion and gravitational instability theories for planet formation struggle to account for this system. In the core-accretion scenario, in particular, the dust mass of the protoplanetary disk would need to be an order of magnitude higher than typically seen in protoplanetary disk observations of ultracool stars., Comment: Original Manuscript as submitted to Science on Oct 17, 2022. In review
Published: 2023

54. TOI-3984 A b and TOI-5293 A b: two temperate gas giants transiting mid-M dwarfs in wide binary systems

Author: Cañas, Caleb I., Kanodia, Shubham, Libby-Roberts, Jessica, Lin, Andrea S. J., Schutte, Maria, Powers, Luke, Jones, Sinclaire, Monson, Andrew, Wang, Songhu, Stefánsson, Guðmundur, Cochran, William D., Robertson, Paul, Mahadevan, Suvrath, Kowalski, Adam F., Wisniewski, John, Parker, Brock A., Larsen, Alexander, Chapman, Franklin A. L., Kobulnicky, Henry A., Gupta, Arvind F., Everett, Mark E., Penprase, Bryan Edward, Zeimann, Gregory, Beard, Corey, Bender, Chad F., Colón, Knicole D., Diddams, Scott A., Fredrick, Connor, Halverson, Samuel, Ninan, Joe P., Ramsey, Lawrence W., Roy, Arpita, and Schwab, Christian
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs with stellar companions at wide separations. TOI-3984 A ($J=11.93$) is an M4 dwarf hosting a short-period ($4.353326 \pm 0.000005$ days) gas giant ($M_p=0.14\pm0.03~\mathrm{M_{J}}$ and $R_p=0.71\pm0.02~\mathrm{R_{J}}$) with a wide separation white dwarf companion. TOI-5293 A ($J=12.47$) is an M3 dwarf hosting a short-period ($2.930289 \pm 0.000004$ days) gas giant ($M_p=0.54\pm0.07~\mathrm{M_{J}}$ and $R_p=1.06\pm0.04~\mathrm{R_{J}}$) with a wide separation M dwarf companion. We characterize both systems using a combination of ground-based and space-based photometry, speckle imaging, and high-precision radial velocities from the Habitable-zone Planet Finder and NEID spectrographs. TOI-3984 A b ($T_{eq}=563\pm15$ K and $\mathrm{TSM}=138_{-27}^{+29}$) and TOI-5293 A b ($T_{eq}=675_{-30}^{+42}$ K and $\mathrm{TSM}=92\pm14$) are two of the coolest gas giants among the population of hot Jupiter-sized gas planets orbiting M dwarfs and are favorable targets for atmospheric characterization of temperate gas giants and three-dimensional obliquity measurements to probe system architecture and migration scenarios., Comment: Published in AJ, 46 pages, 16 figures, 6 tables, updated to reflect published version. arXiv admin note: substantial text overlap with arXiv:2201.09963
Published: 2023
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55. Dye degradation activity of biogenically synthesized Cu/Fe/Ag trimetallic nanoparticles

Author: Roy Arpita, Kunwar Srijal, Bhusal Utsav, Idris Dahir Sagir, Alghamdi Saad, Chidambaram Kumarappan, Qureshi Absar Ahmed, Qusty Naeem F., Khan Abduljawad Abdulshakor, Kaur Kirtanjot, and Roy Amit
Subjects: trimetallic nanoparticles, green synthesis, antioxidant activity, catalytic dye degradation, Chemistry, QD1-999
Abstract: Over the past few decades, nanotechnology has gained momentum because of its potential to create a safer and healthier living environment using eco-friendly approaches. This study describes a safer, more dependable, and ecologically friendly technique of biologically synthesizing Cu/Fe/Ag trimetallic nanoparticles (NPs) using an aqueous leaf extract of Catharanthus roseus as the reducing and stabilizing agent. The synthesized trimetallic NPs were characterized by scanning electron microscope, Fourier transform infrared, dynamic light scattering, and ultraviolet–visible analysis and were evaluated for their potential applications, which included antioxidant properties and catalytic dye degradation. The result suggests that the antioxidant properties of Cu/Fe/Ag NPs are more significant than those of ascorbic acid, a known antioxidant, at lower doses (10 µg·ml−1) while a higher dose of 1,000 µg·ml−1 gives a 69.81% scavenging activity. The impact of Cu/Fe/Ag trimetallic NPs on the catalytic degradation of hazardous dyes such as phenol red (PR) and eosin yellow (EY) was also studied in this work. For PR and EY, the corresponding percentages of degradation were 76% and 48.6%, respectively.
Published: 2024
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56. The unusual M-dwarf Warm Jupiter TOI-1899~b: Refinement of orbital and planetary parameters

Author: Lin, Andrea S. J., Libby-Roberts, Jessica E., Alvarado-Montes, Jaime A., Cañas, Caleb I., Kanodia, Shubham, Han, Te, Hebb, Leslie, Jensen, Eric L. N., Mahadevan, Suvrath, Powers, Luke C., Swaby, Tera N., Wisniewski, John, Beard, Corey, Bender, Chad F., Blake, Cullen H., Cochran, William D., Diddams, Scott A., Frazier, Robert C., Fredrick, Connor, Gully-Santiago, Michael, Halverson, Samuel, Logsdon, Sarah E., McElwain, Michael W., Morley, Caroline, Ninan, Joe P., Rajagopal, Jayadev, Ramsey, Lawrence W., Robertson, Paul, Roy, Arpita, Schwab, Christian, Stefánsson, Guðmundur, Stevens, Daniel J., Terrien, Ryan C., and Wright, Jason T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: TOI-1899 b is a rare exoplanet, a temperate Warm Jupiter orbiting an M-dwarf, first discovered by Ca\~nas et al. (2020) from a TESS single-transit event. Using new radial velocities (RVs) from the precision RV spectrographs HPF and NEID, along with additional TESS photometry and ground-based transit follow-up, we are able to derive a much more precise orbital period of $P = 29.090312_{-0.000035}^{+0.000036}$ d, along with a radius of $R_p = 0.99 \pm 0.03~R_J$. We have also improved the constraints on planet mass, $M_p = 0.67 \pm 0.04~M_J$, and eccentricity, which is consistent with a circular orbit at 2$\sigma$ ($e = 0.044_{-0.027}^{+0.029}$). TOI-1899 b occupies a unique region of parameter space as the coolest known ($T_{eq} \approx$ 380 K) Jovian-sized transiting planet around an M-dwarf; we show that it has great potential to provide clues regarding the formation and migration mechanisms of these rare gas giants through transmission spectroscopy with JWST as well as studies of tidal evolution., Comment: 28 pages, 15 figures, 3 tables, accepted to AJ
Published: 2023
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57. The Quantitative detection of different types of Hb variants through HPLC Technique: Report of 428 cases in Indian population.

Author: Shrivastava, Abhinav, Mohapatra, S.K., Roy, Arpita, Das, S. N., and Tyagi, Gaurav
Published: 2010

58. NEID Reveals that The Young Warm Neptune TOI-2076 b Has a Low Obliquity

Author: Frazier, Robert C., Stefansson, Gudmundur, Mahadevan, Suvrath, Yee, Samuel W., Canas, Caleb I., Winn, Josh, Luhn, Jacob, Dai, Fei, Doyle, Lauren, Cegla, Heather, Kanodia, Shubham, Robertson, Paul, Wisniewski, John, Bender, Chad, Dong, Jiayin, Gupta, Arvind F., Halverson, Samuel, Hawley, Suzanne, Hebb, Leslie, Holcomb, Rae, Kowalski, Adam, Libby-Roberts, Jessica, Lin, Andrea, McElwain, Michael, Ninan, Joe, Petrovich, Cristobal, Roy, Arpita, Schwab, Christian, Terrien, Ryan, and Wright, Jason
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: TOI-2076 b is a sub-Neptune-sized planet ($R= 2.39 \pm 0.10 {R_\oplus}$) that transits a young ($204 \pm 50 {MYr}$) bright ($V = 9.2$) K-dwarf hosting a system of three transiting planets. Using spectroscopic observations with the NEID spectrograph on the WIYN 3.5 m Telescope, we model the Rossiter-McLaughlin effect of TOI-2076 b, and derive a sky-projected obliquity of $\lambda=-3_{-15}^{+16\:\circ}$. Using the size of the star ($R=0.775 \pm0.015 {R_\odot}$), and the stellar rotation period ($P_{\mathrm{rot}}=7.27\pm0.23$ days), we estimate an obliquity of $\psi=18_{-9}^{+10\:\circ}$ ($\psi < 34^\circ$ at 95\% confidence), demonstrating that TOI-2076 b is on a well-aligned orbit. Simultaneous diffuser-assisted photometry from the 3.5 m Telescope at Apache Point Observatory rules out flares during the transit. TOI-2076 b joins a small but growing sample of young planets in compact multi-planet systems with well-aligned orbits, and is the fourth planet with an age $\lesssim 300$ Myr in a multi-transiting system with an obliquity measurement. The low obliquity of TOI-2076 b and the presence of transit timing variations in the system suggest the TOI-2076 system likely formed via convergent disk migration in an initially well-aligned disk., Comment: Published in ApJL, 11 pages, 4 figures, 3 tables
Published: 2022
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59. Can pre-supernova winds from massive stars enrich the interstellar medium with nitrogen at high redshift?

Author: Roy, Arpita, Krumholz, Mark R., Dopita, Michael A., Sutherland, Ralph S., Kewley, Lisa J., and Heger, Alexander
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Understanding the nucleosynthetic origin of nitrogen and the evolution of the N/O ratio in the interstellar medium is crucial for a comprehensive picture of galaxy chemical evolution at high-redshift because most observational metallicity (O/H) estimates are implicitly dependent on the N/O ratio. The observed N/O at high-redshift shows an overall constancy with O/H, albeit with a large scatter. We show that these heretofore unexplained features can be explained by the pre-supernova wind yields from rotating massive stars (M$\gtrsim 10 \, \mathrm{M}_\odot$, $v/v_{\rm{crit}} \gtrsim 0.4$). Our models naturally produce the observed N/O plateau, as well as the scatter at low O/H. We find the scatter to arise from varying star formation efficiency. However, the models that have supernovae dominated yields produce a poor fit to the observed N/O at low O/H. This peculiar abundance pattern at low O/H suggests that dwarf galaxies are most likely to be devoid of SNe yields and are primarily enriched by pre-supernova wind abundances., Comment: 6 pages, 1 figure, published in Proceedings of the International Astronomical Union No. 366, 2022 titled "The Origin of Outflows in Evolved Stars"
Published: 2022
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60. The impact of carbon and oxygen abundances on the metal-poor initial mass function

Author: Sharda, Piyush, Amarsi, Anish M., Grasha, Kathryn, Krumholz, Mark R., Yong, David, Chiaki, Gen, Roy, Arpita, and Nordlander, Thomas
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Star formation models predict that the metal-poor initial mass function (IMF) can be substantially different from that observed in the metal-rich Milky Way. This changeover occurs because metal-poor gas clouds cool inefficiently due to their lower abundance of metals and dust. However, predictions for the metal-poor IMF to date rely on assuming Solar-scaled abundances, that is, [X/O] = 0 at all [O/H]. There is now growing evidence that elements such as C and O that dominate metal line cooling in the ISM do not follow Solar scaling at low metallicities. In this work, we extend models that predict the variation in the characteristic (or, the peak) IMF mass as a function of metallicity using [C/O] ratios derived from observations of metal-poor Galactic stars and of H II regions in dwarf galaxies. These data show [C/O] < 0 at sub-Solar [O/H], which leads to a substantially different metal-poor IMF in the metallicity range where C I and C II cooling dominate ISM thermodynamics, resulting in an increase in the characteristic mass by a factor as large as 7. An important consequence of this difference is a shift in the location of the transition from a top- to a bottom-heavy IMF upwards by 0.5 $-$ 1 dex in metallicity. Our findings indicate that the IMF is very sensitive to the assumptions around Solar-scaled ISM compositions in metal-poor systems (e.g., dwarf galaxies, the Galactic halo and metal-poor stars) that are a key focus of JWST., Comment: 14 pages, 8 figures. Accepted by MNRAS
Published: 2022
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61. Scope of Nanomaterials in Treating Wastewater Produced by Industries

Author: Gupta, Aaryan, Roy, Arpita, Singh, V. P., Editor-in-Chief, Berndtsson, R., Editorial Board Member, Rodrigues, L. N., Editorial Board Member, Sarma, Arup Kumar, Editorial Board Member, Sherif, M. M., Editorial Board Member, Sivakumar, B., Editorial Board Member, Zhang, Q., Editorial Board Member, Pandit, Soumya, editor, Kumar, Lakhan, editor, Mathuriya, Abhilasha Singh, editor, Jadhav, Dipak Ashok, editor, and Ray, Subhasree, editor
Published: 2024
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62. Quantifying broadband chromatic drifts in Fabry-Perot resonators for exoplanet science

Author: Kreider, Molly Kate, Fredrick, Connor, Diddams, Scott A., Terrien, Ryan C., Mahadevan, Suvrath, Ninan, Joe P., Bender, Chad F., Mitchell, Daniel, Rajagopal, Jayadev, Roy, Arpita, Schwab, Christian, and Wright, Jason T.
Subjects: Physics - Optics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The possibility of an Earth-Sun analog beyond our solar system is one of the most longstanding questions in science. At present, answering this question embodies an extremely difficult measurement problem that requires multiple coordinated advances in astronomical telescopes, fiber optics, precision spectrographs, large format detector arrays, and advanced data processing. Taken together, addressing this challenge will require the measurement and calibration of shifts in stellar spectra at the 10^-10 level over multi-year periods. The potential for such precision has recently been advanced by the introduction of laser frequency combs (LFCs) to the field of precision astronomical spectroscopy. However, the expense, complexity and lack of full spectral coverage of LFCs has limited their widespread use and ultimate impact. To address this issue, we explore simple and robust white-light-illuminated Fabry-Perot (FP) etalons as spectral calibrators for precise radial velocity measurements. We track the frequencies of up to 13,000 etalon modes of the installed FPs from two state-of-the-art astronomical spectrographs. Combining these measurements with modeling, we trace unexpected chromatic variations of the FP modes to sub-picometer changes in the dielectric layers of the broad bandwidth FP mirrors. This yields the determination of the frequencies of the FP modes with precision approaching 10^-11/day, equivalent to a radial velocity (RV) Doppler shift of 3 mm/s/day. These results represent critical progress in precision RV measurements on two fronts: first, they make FP etalons a more powerful stand-alone calibration tool, and second, they demonstrate the capability of LFCs to extend cm/s level RV measurement precision over periods approaching a year. Together, these advances highlight a path to achieving spectroscopic calibration at levels that will be critical for finding earths like our own., Comment: 12 pages, 4 figures
Published: 2022

63. Real-time exposure control and instrument operation with the NEID spectrograph GUI

Author: Gupta, Arvind F., Bender, Chad F., Ninan, Joe P., Logsdon, Sarah E., Kanodia, Shubham, Golub, Eli, Higuera, Jesus, Klusmeyer, Jessica, Halverson, Samuel, Mahadevan, Suvrath, McElwain, Michael W., Schwab, Christian, Stefansson, Gudmundur, Robertson, Paul, Roy, Arpita, Terrien, Ryan C., and Wright, Jason T.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The NEID spectrograph on the WIYN 3.5-m telescope at Kitt Peak has completed its first full year of science operations and is reliably delivering sub-m/s precision radial velocity measurements. The NEID instrument control system uses the TIMS package (Bender et al. 2016), which is a client-server software system built around the twisted python software stack. During science observations, interaction with the NEID spectrograph is handled through a pair of graphical user interfaces (GUIs), written in PyQT, which wrap the underlying instrument control software and provide straightforward and reliable access to the instrument. Here, we detail the design of these interfaces and present an overview of their use for NEID operations. Observers can use the NEID GUIs to set the exposure time, signal-to-noise ratio (SNR) threshold, and other relevant parameters for observations, configure the calibration bench and observing mode, track or edit observation metadata, and monitor the current state of the instrument. These GUIs facilitate automatic spectrograph configuration and target ingestion from the nightly observing queue, which improves operational efficiency and consistency across epochs. By interfacing with the NEID exposure meter, the GUIs also allow observers to monitor the progress of individual exposures and trigger the shutter on user-defined SNR thresholds. In addition, inset plots of the instantaneous and cumulative exposure meter counts as each observation progresses allow for rapid diagnosis of changing observing conditions as well as guiding failure and other emergent issues., Comment: Published in Proceedings of the SPIE Astronomical Telescopes + Instrumentation, 2022; 12 pages
Published: 2022
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64. Detection of p-mode Oscillations in HD 35833 with NEID and TESS

Author: Gupta, Arvind F., Luhn, Jacob K., Wright, Jason T., Mahadevan, Suvrath, Ford, Eric B., Stefansson, Gudmundur, Bender, Chad F., Blake, Cullen H., Halverson, Samuel, Hearty, Fred R., Kanodia, Shubham, Logsdon, Sarah E., McElwain, Michael W., Ninan, Joe P., Robertson, Paul, Roy, Arpita, Schwab, Christian, and Terrien, Ryan C.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude $A_{\rm RV}=1.11\pm0.09$ m s$^{-1}$, photometric amplitude $A_{\rm phot}=6.42\pm0.60$ ppm, frequency of maximum power $\nu_{\rm max} = 595.71\pm17.28$ $\mu$Hz, and mode spacing $\Delta \nu = 36.65\pm0.96$ $\mu$Hz) as well as a non-detection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone, and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times $t<\nu_{\rm max}^{-1}$, and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by $>4\sigma$, hinting at gaps in the underlying physical models., Comment: 19 Pages, 14 Figures, Appendix
Published: 2022
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65. Retrieving C and O Abundance of HR 8799 c by Combining High- and Low-Resolution Data

Author: Wang, Ji, Wang, Jason J., Ruffio, Jean-Baptiste, Blake, Geoffrey A., Mawet, Dimitri, Baker, Ashley, Bartos, Randall, Bond, Charlotte Z., Calvin, Benjamin, Cetre, Sylvain, Delorme, Jacques-Robert, Doppmann, Greg, Echeverri, Daniel, Finnerty, Luke, Fitzgerald, Michael P., Jovanovic, Nemanja, Lopez, Ronald, Martin, Emily C., Morris, Evan, Pezzato, Jacklyn, Ragland, Sam, Ruane, Garreth, Sappey, Ben, Schofield, Tobias, Skemer, Andrew, Venenciano, Taylor, Wallace, J. Kent, Wizinowich, Peter, Xuan, Jerry W., Bryan, Marta L., Roy, Arpita, and Wallack, Nicole L.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: The formation and evolution pathway for the directly-imaged multi-planetary system HR 8799 remains mysterious. Accurate constraints on the chemical composition of the planetary atmosphere(s) are key to solving the mystery. We perform a detailed atmospheric retrieval on HR 8799~c to infer the chemical abundances and abundance ratios using a combination of photometric data along with low- and high-resolution spectroscopic data (R$\sim$20-35,000). We specifically retrieve [C/H], [O/H], and C/O and find them to be 0.55$^{+0.36}_{-0.39}$, 0.47$^{+0.31}_{-0.32}$, and 0.67$^{+0.12}_{-0.15}$ at 68\% confidence. The super-stellar C and O abundances, yet a stellar C/O ratio, reveal a potential formation pathway for HR 8799~c. Planet c, and likely the other gas giant planets in the system, formed early on (likely within $\sim$1 Myr), followed by further atmospheric enrichment in C and O through the accretion of solids beyond the CO iceline. The enrichment either preceded or took place during the early phase of the inward migration to the planet current locations., Comment: 19 pages, 6 figures, 3 tables, accepted to AAS journals
Published: 2022
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66. TOI-5205 b: A Short-period Jovian Planet Transiting a Mid-M Dwarf

Author: Kanodia, Shubham, Mahadevan, Suvrath, Libby-Roberts, Jessica, Stefansson, Gudmundur, Canas, Caleb I., Piette, Anjali A. A., Boss, Alan, Teske, Johanna, Chambers, John, Zeimann, Greg, Monson, Andrew, Robertson, Paul, Ninan, Joe P., Lin, Andrea S. J., Bender, Chad F., Cochran, William D., Diddams, Scott A., Gupta, Arvind F., Halverson, Samuel, Hawley, Suzanne, Kobulnicky, Henry A., Metcalf, Andrew J., Parker, Brock A., Powers, Luke, Ramsey, Lawrence W., Roy, Arpita, Schwab, Christian, Swaby, Tera N., Terrien, Ryan C., and Wisniewski, John
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the discovery of TOI-5205~b, a transiting Jovian planet orbiting a solar metallicity M4V star, which was discovered using Transiting Exoplanet Survey Satellite photometry and then confirmed using a combination of precise radial velocities, ground-based photometry, spectra, and speckle imaging. TOI-5205~b has one of the highest mass ratios for M dwarf planets with a mass ratio of almost 0.3$\%$, as it orbits a host star that is just $0.392 \pm 0.015$ \solmass{}. Its planetary radius is $1.03 \pm 0.03~R_J$, while the mass is $1.08 \pm 0.06~M_J$. Additionally, the large size of the planet orbiting a small star results in a transit depth of $\sim 7\%$, making it one of the deepest transits of a confirmed exoplanet orbiting a main-sequence star. The large transit depth makes TOI-5205~b a compelling target to probe its atmospheric properties, as a means of tracing the potential formation pathways. While there have been radial-velocity-only discoveries of giant planets around mid-M dwarfs, this is the first transiting Jupiter with a mass measurement discovered around such a low-mass host star. The high mass of TOI-5205~b stretches conventional theories of planet formation and disk scaling relations that cannot easily recreate the conditions required to form such planets., Comment: Accepted in AJ. arXiv admin note: text overlap with arXiv:2203.07178
Published: 2022
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67. TESS-Keck Survey XIV: Two giant exoplanets from the Distant Giants Survey

Author: Van Zandt, Judah E., Petigura, Erik A., MacDougall, Mason, Gilbert, Gregory J., Lubin, Jack, Barclay, Thomas, Batalha, Natalie M., Crossfield, Ian J. M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Henze, Christopher E., Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Howell, Steve B., Jenkins, Jon M., Latham, David W., Mayo, Andrew, Mireles, Ismael, Mocnik, Teo, Murphy, Joseph M. Akana, Pidhorodetska, Daria, Polanski, Alex S., Ricker, George R., Rosenthal, Lee J., Rubenzahl, Ryan A., Seager, Sara, Scarsdale, Nicholas, Turtleboom, Emma V., Vanderspek, Roland, and Winn, Joshua N.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the Distant Giants Survey, a three-year radial velocity (RV) campaign to measure P(DG|CS), the conditional occurrence of distant giant planets (DG; M_p ~ 0.3 - 13 M_J, P > 1 year) in systems hosting a close-in small planet (CS; R_p < 10 R_E). For the past two years, we have monitored 47 Sun-like stars hosting small transiting planets detected by TESS. We present the selection criteria used to assemble our sample and report the discovery of two distant giant planets, TOI-1669 b and TOI-1694 c. For TOI-1669 b we find that Msin i = 0.573 +/- 0.074 M_J, P = 502 +/- 16 days, and e < 0.27, while for TOI-1694 c, Msin i = 1.05 +/- 0.05 M_J, P = 389.2 +/- 3.9 days, and e = 0.18 +/- 0.05. We also confirmed the 3.8-day transiting planet TOI-1694 b by measuring a true mass of M = 26.1 +/- 2.2 M_E. We also confirmed the 3.8-day transiting planet TOI-1694 b by measuring a true mass of M = 26.1 +/- 2.2 M_E. At the end of the Distant Giants Survey, we will incorporate TOI-1669 b and TOI-1694 c into our calculation of P(DG|CS), a crucial statistic for understanding the relationship between outer giants and small inner companions.
Published: 2022
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68. Entire function with its linear differential polynomial normally or weakly shares a set and some related topics

Author: Banerjee, Abhijit and Roy, Arpita
Published: 2024
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69. Bio-fabrication of Cu/Fe/Zn nanoparticles and its antioxidant and catalytic activity

Author: Bhusal, Utsav, Roy, Arpita, and Kunwar, Srijal
Published: 2023
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70. GJ 3929: High Precision Photometric and Doppler Characterization of an Exo-Venus and its Hot, Mini-Neptune-mass Companion

Author: Beard, Corey, Robertson, Paul, Kanodia, Shubham, Lubin, Jack, Cañas, Caleb I., Gupta, Arvind F., Holcomb, Rae, Jones, Sinclaire, Libby-Roberts, Jessica E., Lin, Andrea S. J., Mahadevan, Suvrath, Stefánsson, Guðmundur, Bender, Chad F., Blake, Cullen H., Cochran, William D., Endl, Michael, Everett, Mark, Ford, Eric B., Fredrick, Connor, Halverson, Samuel, Hebb, Leslie, Li, Dan, Logsdon, Sarah E., Luhn, Jacob, McElwain, Michael W., Metcalf, Andrew J., Ninan, Joe P., Rajagopal, Jayadev, Roy, Arpita, Schutte, Maria, Schwab, Christian, Terrien, Ryan C., Wisniewski, John, and Wright, Jason T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We detail the follow up and characterization of a transiting exo-Venus identified by TESS, GJ 3929b, (TOI-2013b) and its non-transiting companion planet, GJ 3929c (TOI-2013c). GJ 3929b is an Earth-sized exoplanet in its star's Venus-zone (P$_{b}$ = 2.616272 $\pm$ 0.000005 days; S$_{b}$ = 17.3$^{+0.8}_{-0.7}$ S$_{\oplus}$) orbiting a nearby M dwarf. GJ 3929c is most likely a non-transiting sub-Neptune. Using the new, ultra-precise NEID spectrometer on the WIYN 3.5 m Telescope at Kitt Peak National Observatory, we are able to modify the mass constraints of planet b reported in previous works and consequently improve the significance of the mass measurement to almost 4$\sigma$ confidence (M$_{b}$ = 1.75 $\pm$ 0.45 M$_{\oplus}$). We further adjust the orbital period of planet c from its alias at 14.30 $\pm$ 0.03 days to the likely true period of 15.04 $\pm$ 0.03 days, and adjust its minimum mass to m$\sin i$ = 5.71 $\pm$ 0.92 M$_{\oplus}$. Using the diffuser-assisted ARCTIC imager on the ARC 3.5 m telescope at Apache Point Observatory, in addition to publicly available TESS and LCOGT photometry, we are able to constrain the radius of planet b to R$_{p}$ = 1.09 $\pm$ 0.04 R$_{\oplus}$. GJ 3929b is a top candidate for transmission spectroscopy in its size regime (TSM = 14 $\pm$ 4), and future atmospheric studies of GJ 3929b stand to shed light on the nature of small planets orbiting M dwarfs., Comment: Accepted for publication in ApJ. arXiv admin note: text overlap with arXiv:2204.09063
Published: 2022
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71. Report on Community Cadence Observing to Maximize the Scientific Output of the Keck Planet Finder

Author: Petigura, Erik, Howard, Andrew, Bean, Jacob, Beichman, Charles, Fischer, Debra, Fulton, BJ, Isaacson, Howard, O'Meara, John, Jordan, Carolyn, Huber, Daniel, Robertson, Paul, Roy, Arpita, Teske, Johanna, and Walawender, Josh
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The arrival of the Keck Planet Finder (KPF) in 2022 represents a major advance in the precision radial velocity (PRV) capabilities of the W. M. Keck Observatory. In preparation for KPF science, our committee of PRV experts and WMKO staff studied the current implementation of cadence observing at Keck and other PRV facilities. We find that many of KPF's major science cases are not feasible through Keck's standard allocations of full or half nights to individual PIs. Pooling time among several PIs as is currently done by the California Planet Search (CPS) collaboration with HIRES results in lower quality science results than is possible when KPF is available at higher observational cadence. This strategy also creates barriers to entry, particularly for researchers wishing to lead small proposals. This report makes recommendations for optimizing PRV cadence at Keck subject to the following constraints: preservation of clear boundaries between cadence observations and classically scheduled time; and ensuring fairness and scientific independence of different Keck TACs and different KPF PIs. We recommend establishing a new category of Keck time allocation, "KPF Community Cadence" (KPF-CC). In many ways, KPF-CC will formalize observing strategies provided by CPS, but with higher observational cadence appropriate for KPF science and with universal access to the program for all Keck users. We recommend that KPF-CC time be scheduled classically into blocks as small as a quarter night subject to considerations of bright/dark time, variations in proposal pressure with the seasons, and the needs of non-KPF observing programs. Within KPF-CC time, the Keck Observing Assistants would execute observations generated by a dynamic scheduler. We recommend that Keck staff and a board of PRV experts design and maintain the scheduling software., Comment: 31 pages, 10 figures, prepared for the Keck Science Steering Committee, report delivered on Nov 7, 2021
Published: 2022

72. 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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73. ATOCA: an algorithm to treat order contamination. Application to the NIRISS SOSS mode

Author: Darveau-Bernier, Antoine, Albert, Loïc, Talens, Geert Jan, Lafrenière, David, Radica, Michael, Doyon, René, Cook, Neil J., Rowe, Jason F., Artigau, Étienne, Benneke, Björn, Cowan, Nicolas, Dang, Lisa, Espinoza, Néstor, Johnstone, Doug, Kaltenegger, Lisa, Lim, Olivia, Pelletier, Stefan, Piaulet, Caroline, Roy, Arpita, Roy, Pierre-Alexis, Splinter, Jared, Taylor, Jake, and Turner, Jake D.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: After a successful launch, the James Webb Space Telescope is preparing to undertake one of its principal missions, the characterization of the atmospheres of exoplanets. The Single Object Slitless Spectroscopy (SOSS) mode of the Near Infrared Imager and Slitless Spectrograph (NIRISS) is the only observing mode that has been specifically designed for this objective. It features a wide simultaneous spectral range (0.6--2.8\,\micron) through two spectral diffraction orders. However, due to mechanical constraints, these two orders overlap slightly over a short range, potentially introducing a ``contamination'' signal in the extracted spectrum. We show that for a typical box extraction, this contaminating signal amounts to 1\% or less over the 1.6--2.8\,\micron\ range (order 1), and up to 1\% over the 0.85--0.95\,\micron\ range (order 2). For observations of exoplanet atmospheres (transits, eclipses or phase curves) where only temporal variations in flux matter, the contamination signal typically biases the results by order of 1\% of the planetary atmosphere spectral features strength. To address this problem, we developed the Algorithm to Treat Order ContAmination (ATOCA). By constructing a linear model of each pixel on the detector, treating the underlying incident spectrum as a free variable, ATOCA is able to perform a simultaneous extraction of both orders. We show that, given appropriate estimates of the spatial trace profiles, the throughputs, the wavelength solutions, as well as the spectral resolution kernels for each order, it is possible to obtain an extracted spectrum accurate to within 10\,ppm over the full spectral range., Comment: Submitted to PASP. 22 pages, 12 figures
Published: 2022
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74. APPLESOSS: A Producer of ProfiLEs for SOSS. Application to the NIRISS SOSS Mode

Author: Radica, Michael, Albert, Loïc, Taylor, Jake, Lafrenière, David, Coulombe, Louis-Philippe, Darveau-Bernier, Antoine, Doyon, René, Cook, Neil, Cowan, Nicolas, Espinoza, Néstor, Johnstone, Doug, Kaltenegger, Lisa, Piaulet, Caroline, Roy, Arpita, and Talens, Geert Jan
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The SOSS mode of the NIRISS instrument is poised to be one of the workhorse modes for exoplanet atmosphere observations with the newly launched James Webb Space Telescope. One of the challenges of the SOSS mode, however, is the physical overlap of the first two diffraction orders of the G700XD grism on the detector. Recently, the ATOCA algorithm was developed and implemented as an option in the official JWST pipeline, as a method to extract SOSS spectra by decontaminating the detector -- that is, separating the first and second orders. Here, we present APPLESOSS (A Producer of ProfiLEs for SOSS), which generates the spatial profiles for each diffraction order upon which ATOCA relies. We validate APPLESOSS using simulated SOSS time series observations of WASP-52\,b, and compare it to ATOCA extractions using two other spatial profiles (a best and worst case scenario on-sky), as well as a simple box extraction performed without taking into account the order contamination. We demonstrate that APPLESOSS profiles retain a high degree of fidelity to the true underlying spatial profiles, and therefore yield accurate extracted spectra. We further confirm that the effects of the order contamination for relative measurements (e.g., exoplanet transmission or emission observations) is small -- the transmission spectrum obtained from each of our four tests, including the contaminated box extraction, is consistent at the $\sim$1$\sigma$ level with the atmosphere model input into our noiseless simulations. We further confirm via a retrieval analysis that the atmosphere parameters (metallicity and C/O) obtained from each transmission spectrum are consistent with the true underlying values., Comment: 11 pages, 10 figures. Published in PASP
Published: 2022
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75. The TESS-Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-Mass Outer Companion around TOI-1272

Author: MacDougall, Mason G., Petigura, Erik A., Fetherolf, Tara, Beard, Corey, Lubin, Jack, Angelo, Isabel, Batalha, Natalie M., Behmard, Aida, Blunt, Sarah, Brinkman, Casey, Chontos, Ashley, Crossfield, Ian J. M., Dai, Fei, Dalba, Paul A., Dressing, Courtney, Fulton, Benjamin, Giacalone, Steven, Hill, Michelle L., Howard, Andrew W., Huber, Daniel, Isaacson, Howard, Kane, Stephen R., Kosiarek, Molly, Mayo, Andrew, Mocnik, Teo, Murphy, Joseph M. Akana, Pidhorodetska, Daria, Polanski, Alex, Rice, Malena, Robertson, Paul, Rosenthal, Lee J., Roy, Arpita, Rubenzahl, Ryan A., Scarsdale, Nicholas, Turtelboom, Emma V., Tyler, Dakotah, Van Zandt, Judah, Weiss, Lauren M., Esparza-Borges, Emma, Fukui, Akihiko, Isogai, Keisuke, Kawauchi, Kiyoe, Mori, Mayuko, Murgas, Felipe, Narita, Norio, Nishiumi, Taku, Palle, Enric, Parviainen, Hannu, Watanabe, Noriharu, Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, S., Vanderspek, Roland K., Winn, Joshua N., Bieryla, Allyson, Caldwell, Douglas A., Dragomir, Diana, Fausnaugh, M. M., Mireles, Ismael, and Rodriguez, David R.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of an eccentric hot Neptune and a non-transiting outer planet around TOI-1272. We identified the eccentricity of the inner planet, with an orbital period of 3.3 d and $R_{\rm p,b} = 4.1 \pm 0.2$ $R_\oplus$, based on a mismatch between the observed transit duration and the expected duration for a circular orbit. Using ground-based radial velocity measurements from the HIRES instrument at the Keck Observatory, we measured the mass of TOI-1272b to be $M_{\rm p,b} = 25 \pm 2$ $M_\oplus$. We also confirmed a high eccentricity of $e_b = 0.34 \pm 0.06$, placing TOI-1272b among the most eccentric well-characterized sub-Jovians. We used these RV measurements to also identify a non-transiting outer companion on an 8.7-d orbit with a similar mass of $M_{\rm p,c}$ sin$i= 27 \pm 3$ $M_\oplus$ and $e_c \lesssim 0.35$. Dynamically stable planet-planet interactions have likely allowed TOI-1272b to avoid tidal eccentricity decay despite the short circularization timescale expected for a close-in eccentric Neptune. TOI-1272b also maintains an envelope mass fraction of $f_{\rm env} \approx 11\%$ despite its high equilibrium temperature, implying that it may currently be undergoing photoevaporation. This planet joins a small population of short-period Neptune-like planets within the "Hot Neptune Desert" with a poorly understood formation pathway., Comment: Accepted at The Astronomical Journal; 17 pages, 11 figures
Published: 2022
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76. Retrieving C and O Abundance of HR 8799 c by Combining High- and Low-resolution Data

Author: Wang, Ji, Wang, Jason J, Ruffio, Jean-Baptiste, Blake, Geoffrey A, Mawet, Dimitri, Baker, Ashley, Bartos, Randall, Bond, Charlotte Z, Calvin, Benjamin, Cetre, Sylvain, Delorme, Jacques-Robert, Doppmann, Greg, Echeverri, Daniel, Finnerty, Luke, Fitzgerald, Michael P, Jovanovic, Nemanja, Lopez, Ronald, Martin, Emily C, Morris, Evan, Pezzato, Jacklyn, Ragland, Sam, Ruane, Garreth, Sappey, Ben, Schofield, Tobias, Skemer, Andrew, Venenciano, Taylor, Wallace, J Kent, Wizinowich, Peter, Xuan, Jerry W, Bryan, Marta L, Roy, Arpita, and Wallack, Nicole L
Subjects: Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: The formation and evolution pathway for the directly imaged multiplanetary system HR 8799 remains mysterious. Accurate constraints on the chemical composition of the planetary atmosphere(s) are key to solving the mystery. We perform a detailed atmospheric retrieval on HR 8799 c to infer the chemical abundances and abundance ratios using a combination of photometric data along with low- and high-resolution spectroscopic data (R ∼ 20-35,000). We specifically retrieve [C/H], [O/H], and C/O and find them to be 0.55 − 0.39 + 0.36 , 0.47 − 0.32 + 0.31 , and 0.67 − 0.15 + 0.12 at 68% confidence. The superstellar C and O abundances, yet a stellar C/O ratio, reveal a potential formation pathway for HR 8799 c. Planet c, and likely the other gas giant planets in the system, formed early on (likely within ∼1 Myr), followed by further atmospheric enrichment in C and O through the accretion of solids beyond the CO ice line. The enrichment either preceded or took place during the early phase of the inward migration to the current planet locations.
Published: 2023

77. An effective supramolecular metallohydrogel-based non-volatile memory device for application in logic gate circuit

Author: Roy, Arpita and Ray, Soumya Jyoti
Published: 2024
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78. List of contributors

Author: Abebe, Buzuayehu, primary, Afthoni, Mohammad, additional, Agarwal, Lokesh Kumar, additional, Agarwal, Shikha, additional, Ali, Shafaqat, additional, Ananda Murthy, H.C., additional, Arasu, Ponnusamy Thillai, additional, Asghar, Waleed, additional, Aziz, Humera, additional, Balamurali, Saminathan, additional, Barua, Siddharth, additional, Batool, Muazzama, additional, Chakrabarty, Mithun, additional, Chakraborty, Bhaswati, additional, Chandan Gowda, U., additional, Chandrasekaran, M., additional, Chen, Zhongli, additional, Chikkud, Venkatesh, additional, da Costa Pinto, Geicielly, additional, da Paixão, Bryan, additional, Das, Naren, additional, de Oliveira Lourenço, Vitória, additional, Delgado, Vinicius Marx Silva, additional, Din, Salah Ud, additional, Ekanayake, Sagarika, additional, Farooq, Sana, additional, Gamage, Vinidu, additional, Gazal, Umaima, additional, Geethalakshmi, V., additional, Giridhar Reddy, S., additional, Guin, Mridula, additional, Gunewardene, Siyath, additional, Hamed, Ali, additional, Haq, Tanveer ul, additional, Harini, H.V., additional, Jadhav, Vikram R., additional, Jamshaid, Muhammad Usman, additional, Jayanetti, Sumedha, additional, Joshi, Venkatesh, additional, Kalel, Rahul A., additional, Kalyan, Imon, additional, Kannan, Sadasivam, additional, Kataoka, Ryota, additional, Khobragade, Moni Udhaorao, additional, Kumar, A. Naveen, additional, Kumaravel, A., additional, Kuswandi, Bambang, additional, Mahmood, Ahmad, additional, Manjula, N.G., additional, Mayegowda, Shilpa Borehalli, additional, Mehmood, Mirza Zahid, additional, Michael, Anugrah, additional, Munawar, Anam, additional, Murugan, Arumugam, additional, Nagaraj, Revathi, additional, Nagaswarupa, H.P., additional, Naik, Ramachandra, additional, Nalini, N., additional, Namli, Ayten, additional, Nayak, Ashish Kumar, additional, Neeraja, Ganta, additional, Nishshanka, Upul, additional, Nithin Gowda, B.K., additional, Nithyashree, S., additional, Nouri, Mohamed, additional, Palake, Ashwini, additional, Pasqual, Onali, additional, Priyantha, Namal, additional, Prote, Larissa Cristiane Souza, additional, Rakha, Allah, additional, Rathnayake, Anushka, additional, Rathod, Prakash B., additional, Riaz, Ahsan, additional, Riaz, Umair, additional, Roy, Arpita, additional, Roy, Nishant, additional, Saketha, Y., additional, Santinelli, Bruna, additional, Sathyamoorthi, S., additional, Shad, Naveed A., additional, Silva, Christopher Santos, additional, Singh, Aniket, additional, Singh, Mahendra Pratap, additional, Siva, Vadivel, additional, Soni, Shivani, additional, Srivastava, Noopur, additional, Srivastava, Sarita, additional, Tagad, Chandrakant K., additional, Teli, Pankaj, additional, Teli, Sunita, additional, Thangamani, K.S., additional, Thiripuranathar, Gobika, additional, Tomar, Mahendra Pratap Singh, additional, Tonelli, Fernanda Maria Policarpo, additional, Tonelli, Flávia Cristina Policarpo, additional, and Turgay, Oguz Can, additional
Published: 2024
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79. Preface

Author: Policarpo Tonelli, Fernanda Maria, primary, Roy, Arpita, additional, Ozturk, Munir, additional, and Murthy, H.C. Ananda, additional
Published: 2024
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80. The TESS-Keck Survey. XI. Mass Measurements for Four Transiting sub-Neptunes orbiting K dwarf TOI-1246

Author: Turtelboom, Emma V., Weiss, Lauren M., Dressing, Courtney D., Nowak, Grzegorz, Pallé, Enric, Beard, Corey, Blunt, Sarah, Brinkman, Casey, Chontos, Ashley, Claytor, Zachary R., Dai, Fei, Dalba, Paul A., Giacalone, Steven, Gonzales, Erica, Harada, Caleb K., Hill, Michelle L., Holcomb, Rae, Korth, Judith, Lubin, Jack, Masseron, Thomas, MacDougall, Mason, Mayo, Andrew W., Močnik, Teo, Murphy, Joseph M. Akana, Polanski, Alex S., Rice, Malena, Rubenzahl, Ryan A., Scarsdale, Nicholas, Stassun, Keivan G., Tyler, Dakotah B., Van Zandt, Judah, Crossfield, Ian J. M., Deeg, Hans J., Fulton, Benjamin, Gandolfi, Davide, Howard, Andrew W., Huber, Dan, Isaacson, Howard, Kane, Stephen R., Lam, Kristine W. F., Luque, Rafael, Martín, Eduardo L., Morello, Giuseppe, Orell-Miquel, Jaume, Petigura, Erik A., Robertson, Paul, Roy, Arpita, Van Eylen, Vincent, Baker, David, Belinski, Alexander A., Bieryla, Allyson, Ciardi, David R., Collins, Karen A., Cutting, Neil, Della-Rose, Devin J., Ellingsen, Taylor B., Furlan, E., Gan, Tianjun, Gnilka, Crystal L., Guerra, Pere, Howell, Steve B., Jimenez, Mary, Latham, David W., Larivière, Maude, Lester, Kathryn V., Lillo-Box, Jorge, Luker, Lindy, Mann, Christopher R., Plavchan, Peter P., Safonov, Boris, Skinner, Brett, Strakhov, Ivan A., Wittrock, Justin M., Caldwell, Douglas A., Essack, Zahra, Jenkins, Jon M., Quintana, Elisa V., Ricker, George R., Vanderspek, Roland, Seager, S., and Winn, Joshua N.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Multi-planet systems are valuable arenas for investigating exoplanet architectures and comparing planetary siblings. TOI-1246 is one such system, with a moderately bright K dwarf ($\rm{V=11.6,~K=9.9}$) and four transiting sub-Neptunes identified by TESS with orbital periods of $4.31~\rm{d},~5.90~\rm{d},~18.66~\rm{d}$, and $~37.92~\rm{d}$. We collected 130 radial velocity observations with Keck/HIRES and TNG/HARPS-N to measure planet masses. We refit the 14 sectors of TESS photometry to refine planet radii ($\rm{2.97 \pm 0.06~R_\oplus},\rm{2.47 \pm 0.08~R_\oplus}, \rm{3.46 \pm 0.09~R_\oplus}$, $\rm{3.72 \pm 0.16~R_\oplus}$), and confirm the four planets. We find that TOI-1246 e is substantially more massive than the three inner planets ($\rm{8.1 \pm 1.1 M_\oplus}$, $\rm{8.8 \pm 1.2 M_\oplus}$, $\rm{5.3 \pm 1.7 M_\oplus}$, $\rm{14.8 \pm 2.3 M_\oplus}$). The two outer planets, TOI-1246 d and TOI-1246 e, lie near to the 2:1 resonance ($\rm{P_{e}/P_{d}=2.03}$) and exhibit transit timing variations. TOI-1246 is one of the brightest four-planet systems, making it amenable for continued observations. It is one of only six systems with measured masses and radii for all four transiting planets. The planet densities range from $\rm{0.70 \pm 0.24}$ to $3.21 \pm 0.44 \rm{g/cm^3}$, implying a range of bulk and atmospheric compositions. We also report a fifth planet candidate found in the RV data with a minimum mass of 25.6 $\pm$ 3.6 $\rm{M_\oplus}$. This planet candidate is exterior to TOI-1246 e with a candidate period of 93.8 d, and we discuss the implications if it is confirmed to be planetary in nature., Comment: Accepted at The Astronomical Journal; 33 pages, 10 figures
Published: 2022
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81. TOI-1696 and TOI-2136: Constraining the Masses of Two Mini-Neptunes with HPF

Author: Beard, Corey, Robertson, Paul, Kanodia, Shubham, Libby-Roberts, Jessica, Canas, Caleb I., Gupta, Arvind F., Holcomb, Rae, Jones, Sinclaire, Kobulnicky, Henry A., Lin, Andrea S. J., Lubin, Jack, Maney, Marissa, Parker, Brock A., Stefansson, Gudmundur, Cochran, William D., Endl, Michael, Hebb, Leslie, Mahadevan, Suvrath, Wisniewski, John, Bender, Chad F., Diddams, Scott A., Everett, Mark, Fredrick, Connor, Halverson, Samuel, Hearty, Fred, Metcalf, Andrew J., Monson, Andrew, Ninan, Joe P., Roy, Arpita, Schutte, Maria, Schwab, Christian, and Terrien, Ryan C
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the validation of two planets orbiting M dwarfs, TOI-1696b and TOI-2136b. Both planets are mini-Neptunes orbiting nearby stars, making them promising prospects for atmospheric characterization with the James Webb Space Telescope. We validated the planetary nature of both candidates using high contrast imaging, ground-based photometry, and near-infrared radial velocities. Adaptive Optics images were taken using the ShARCS camera on the 3 m Shane Telescope. Speckle images were taken using the NN-Explore Exoplanet Stellar Speckle Imager on the WIYN 3.5 m telescope. Radii and orbital ephemerides were refined using a combination of TESS, the diffuser-assisted ARCTIC imager on the 3.5m ARC telescope at Apache Point Observatory, and the 0.6 m telescope at Red Buttes Observatory. We obtained radial velocities using the Habitable-Zone Planet Finder on the 10 m Hobby-Eberly Telescope, which enabled us to place upper limits on the masses of both transiting planets. TOI-1696b (P = 2.5 days; R$_{p}$ = 3.24 R$_{\oplus}$; M$_{p}$ $<$ 56.6 M$_{\oplus}$) falls into a sparsely-populated region of parameter space considering its host star's temperature (T$_{\rm{eff}}$ = 3168 K, M4.5), as planets of its size are quite rare around mid to late M dwarfs. On the other hand, TOI-2136b (P = 7.85 days; R$_{p}$ = 2.09 R$_{\oplus}$; M$_{p}$ $<$ 15.0 M$_{\oplus}$) is an excellent candidate for atmospheric follow-up with JWST., Comment: Accepted for Publication in the Astronomical Journal
Published: 2022
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82. Leveraging space-based data from the nearest Solar-type star to better understand stellar activity signatures in radial velocity data

Author: Ervin, Tamar, Halverson, Samuel, Burrows, Abigail, Murphy, Neil, Roy, Arpita, Haywood, Raphaelle D., Rescigno, Federica, Bender, Chad F., Lin, Andrea S. J., Burt, Jennifer, and Mahadevan, Suvrath
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Stellar variability is a key obstacle in reaching the sensitivity required to recover Earth-like exoplanetary signals using the radial velocity (RV) detection method. To explore activity signatures in Sun-like stars, we present SolAster, a publicly-distributed analysis pipeline that allows for comparison of space-based measurements with ground-based disk-integrated RVs. Using high spatial resolution Dopplergrams, magnetograms, and continuum filtergrams from the Helioseismic and Magnetic Imager (HMI) aboard the Solar Dynamics Observatory (SDO), we estimate 'Sun-as-a-star' disk-integrated RVs due to rotationally modulated flux imbalances and convective blueshift suppression, as well as other observables such as unsigned magnetic flux. Comparing these measurements with ground-based RVs from the NEID instrument, which observes the Sun daily using an automated solar telescope, we find a strong relationship between magnetic activity indicators and RV variation, supporting efforts to examine unsigned magnetic flux as a proxy for stellar activity in slowly rotating stars. Detrending against measured unsigned magnetic flux allows us to improve the NEID RV measurements by ~20\% (~50 cm/s in a quadrature sum), yielding an RMS scatter of ~60 cm/s over five months. We also explore correlations between individual and averaged spectral line shapes in the NEID spectra and SDO-derived magnetic activity indicators, motivating future studies of these observables. Finally, applying SolAster to archival planetary transits of Venus and Mercury, we demonstrate the ability to recover small amplitude (< 50 cm/s) RV variations in the SDO data by directly measuring the Rossiter-McLaughlin (RM) signals., Comment: 20 pages, 12 figures
Published: 2022
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83. A close-in puffy Neptune with hidden friends: The enigma of TOI 620

Author: Reefe, Michael A., Luque, Rafael, Gaidos, Eric, Beard, Corey, Plavchan, Peter P., Cointepas, Marion, Cale, Bryson L., Palle, Enric, Parviainen, Hannu, Feliz, Dax L., Eastman, Jason, Stassun, Keivan, Gagné, Jonathan, Jenkins, Jon M., Boyd, Patricia T., Kidwell, Richard C., McDermott, Scott, Collins, Karen A., Fong, William, Guerrero, Natalia, Almenara-Villa, Jose-Manuel, Bean, Jacob, Beichman, Charles A., Berberian, John, Bieryla, Allyson, Bonfils, Xavier, Bouchy, François, Brady, Madison, Bryant, Edward M., Cacciapuoti, Luca, Cañas, Caleb I., Ciardi, David R., Collins, Kevin I., Crossfield, Ian, Dressing, Courtney D., Eigmueller, Philipp, Mufti, Mohammed El, Esparza-Borges, Emma, Fukui, Akihiko, Gao, Peter, Geneser, Claire, Gnilka, Crystal L., Gonzales, Erica, Gupta, Arvind F., Halverson, Sam, Hearty, Fred, Howell, Steve B., Irwin, Jonathan, Kanodia, Shubham, Kasper, David, Kodama, Takanori, Kostov, Veselin, Latham, David W., Lendl, Monika, Lin, Andrea, Livingston, John H., Lubin, Jack, Mahadevan, Suvrath, Matson, Rachel, Matthews, Elisabeth, Murgas, Felipe, Narita, Norio, Newman, Patrick, Ninan, Joe, Osborn, Ares, Quinn, Samuel N., Robertson, Paul, Roy, Arpita, Schlieder, Joshua, Schwab, Christian, Seifahrt, Andreas, Smith, Gareth D., Sohani, Ahmad, Stefánsson, Guðmundur, Stevens, Daniel, Stürmer, Julian, Tanner, Angelle, Terrien, Ryan, Teske, Johanna, Vermilion, David, Wang, Sharon X., Wittrock, Justin, Wright, Jason T., Zechmeister, Mathias, and Zohrabi, Farzaneh
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the validation of a transiting low-density exoplanet orbiting the M2.5 dwarf TOI 620 discovered by the NASA TESS mission. We utilize photometric data from both TESS and ground-based follow-up observations to validate the ephemerides of the 5.09-day transiting signal and vet false positive scenarios. High-contrast imaging data are used to resolve the stellar host and exclude stellar companions at separations $\gtrsim 0.2''$. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with multiple PRV spectrographs to confirm the planetary nature of the transiting exoplanet. We calculate a 5$\sigma$ upper limit of $M_P < 7.1$ M$_\oplus$ and $\rho_P < 0.74$ g cm$^{-3}$, and we identify a non-transiting 17.7-day candidate. We also find evidence for a substellar (1-20 M$_{\rm J}$) companion with a projected separation $\lesssim 20$ au from a combined analysis of Gaia, AO imaging, and RVs. With the discovery of this outer companion, we carry out a detailed exploration of the possibilities that TOI 620 b might instead be a circum-secondary planet or a pair of eclipsing binary stars orbiting the host in a hierarchical triple system. We find, under scrutiny, that we can exclude both of these scenarios from the multi-wavelength transit photometry, thus validating TOI 620 b as a low-density exoplanet transiting the central star in this system. The low density of TOI 620 b makes it one of the most amenable exoplanets for atmospheric characterization, such as with JWST and Ariel, validated or confirmed by the TESS mission to date., Comment: 64 pages, 34 figures, 22 tables. Accepted for publication in the Astronomical Journal
Published: 2022
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84. TOI-3757 b: A low density gas giant orbiting a solar-metallicity M dwarf

Author: Kanodia, Shubham, Libby-Roberts, Jessica, Canas, Caleb I., Ninan, Joe P., Mahadevan, Suvrath, Stefansson, Gudmundur, Lin, Andrea S. J., Jones, Sinclaire, Monson, Andrew, Parker, Brock A., Kobulnicky, Henry A., Swaby, Tera N., Powers, Luke, Beard, Corey, Bender, Chad F., Blake, Cullen H., Cochran, William D., Dong, Jiayin, Diddams, Scott A., Fredrick, Connor, Gupta, Arvind F., Halverson, Samuel, Hearty, Fred, Logsdon, Sarah E., Metcalf, Andrew J., McElwain, Michael W., Morley, Caroline, Rajagopal, Jayadev, Ramsey, Lawrence W., Robertson, Paul, Roy, Arpita, Schwab, Christian, Terrien, Ryan C., Wisniewski, John, and Wright, Jason T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of a new Jovian-sized planet, TOI-3757 b, the lowest density planet orbiting an M dwarf (M0V). It orbits a solar-metallicity M dwarf discovered using TESS photometry and confirmed with precise radial velocities (RV) from HPF and NEID. With a planetary radius of $12.0^{+0.4}_{-0.5}$ $R_{\oplus}$ and mass of $85.3^{+8.8}_{-8.7}$ $M_{\oplus}$, not only does this object add to the small sample of gas giants ($\sim 10$) around M dwarfs, but also, its low density ($\rho =$ $0.27^{+0.05}_{-0.04}$ $\textrm{g~cm}^{-3}$) provides an opportunity to test theories of planet formation. We present two hypotheses to explain its low density; first, we posit that the low metallicity of its stellar host ($\sim$ 0.3 dex lower than the median metallicity of M dwarfs hosting gas giants) could have played a role in the delayed formation of a solid core massive enough to initiate runaway accretion. Second, using the eccentricity estimate of $0.14 \pm 0.06$ we determine it is also plausible for tidal heating to at least partially be responsible for inflating the radius of TOI-3757b b. The low density and large scale height of TOI-3757 b makes it an excellent target for transmission spectroscopy studies of atmospheric escape and composition (TSM $\sim$ 190). We use HPF to perform transmission spectroscopy of TOI-3757 b using the helium 10830 \AA~ line. Doing this, we place an upper limit of 6.9 \% (with 90\% confidence) on the maximum depth of the absorption from the metastable transition of He at $\sim$ 10830 \AA, which can help constraint the atmospheric mass loss rate in this energy limited regime., Comment: AJ. arXiv admin note: text overlap with arXiv:2107.13670
Published: 2022
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85. Retrieving the C and O Abundances of HR 7672~AB: a Solar-Type Primary Star with a Benchmark Brown Dwarf

Author: Wang, Ji, Kolecki, Jared R., Ruffio, Jean-Baptiste, Wang, Jason J., Mawet, Dimitri, Baker, Ashley, Bartos, Randall, Blake, Geoffrey A., Bond, Charlotte Z., Calvin, Benjamin, Cetre, Sylvain, Delorme, Jacques-Robert, Doppmann, Greg, Echeverri, Daniel, Finnerty, Luke, Fitzgerald, Michael P., Jovanovic, Nemanja, Liu, Michael C., Lopez, Ronald, Morris, Evan, Asnodkar, Anusha Pai, Pezzato, Jacklyn, Ragland, Sam, Roy, Arpita, Ruane, Garreth, Sappey, Ben, Schofield, Tobias, Skemer, Andrew, Venenciano, Taylor, Wallace, J. Kent, Wallack, Nicole L., Wizinowich, Peter, and Xuan, Jerry W.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: A benchmark brown dwarf (BD) is a BD whose properties (e.g., mass and chemical composition) are precisely and independently measured. Benchmark BDs are valuable in testing theoretical evolutionary tracks, spectral synthesis, and atmospheric retrievals for sub-stellar objects. Here, we report results of atmospheric retrieval on a synthetic spectrum and a benchmark BD -- HR 7672~B -- with \petit. First, we test the retrieval framework on a synthetic PHOENIX BT-Settl spectrum with a solar composition. We show that the retrieved C and O abundances are consistent with solar values, but the retrieved C/O is overestimated by 0.13-0.18, which is $\sim$4 times higher than the formal error bar. Second, we perform retrieval on HR 7672~B using high spectral resolution data (R=35,000) from the Keck Planet Imager and Characterizer (KPIC) and near infrared photometry. We retrieve [C/H], [O/H], and C/O to be $-0.24\pm0.05$, $-0.19\pm0.04$, and $0.52\pm0.02$. These values are consistent with those of HR 7672~A within 1.5-$\sigma$. As such, HR 7672~B is among only a few benchmark BDs (along with Gl 570~D and HD 3651~B) that have been demonstrated to have consistent elemental abundances with their primary stars. Our work provides a practical procedure of testing and performing atmospheric retrieval, and sheds light on potential systematics of future retrievals using high- and low-resolution data., Comment: 29 pages, 17 figures, 5 tables, resubmitted to AAS journals after first revision
Published: 2022
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86. Sustainable soil management under drought stress through biochar application: Immobilizing arsenic, ameliorating soil quality, and augmenting plant growth

Author: Kumar, Abhishek, Bhattacharya, Tanushree, Shaikh, Wasim Akram, and Roy, Arpita
Published: 2024
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87. Nanocarriers for nutraceutical delivery: A miniaturized revolution in health

Author: Sawant, Rajashri B., Nikam, Sonali P., Roy, Arpita, Kumar, Ashish, Mohammed, Osama A., Sharma, Kuldeep, Rai, Ashutosh Kumar, Roy, Amit, Gaur, Ashish, and Verma, Rajan
Published: 2024
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88. Toxicological and bioremediation profiling of nonessential heavy metals (mercury, chromium, cadmium, aluminium) and their impact on human health: A review

Author: Sable, Harsh, Singh, Vandana, Kumar, Vaishali, Roy, Arpita, Pandit, Soumya, Kaur, Kirtanjot, Rustagi, Sarvesh, and Malik, Sumira
Published: 2024
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89. Comprehensive investigation on fabrication, spectral characterization and biological importance of Co(II) and Ni(II) heteroleptic complexes

Author: Marlin Risana, M., Balasubramaniyan, S., Govindharaju, R., Mohamed Azharudeen, A., Mary Juliet, B., MukilMeenakshi, V., Alsaiari, Ahad Amer, Roy, Arpita, Verma, Rajan, and Sharma, Kuldeep
Published: 2024
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90. Nanocarrier optimization: Encapsulating Hydrastis canadensis in chitosan nanoparticles for enhanced antibacterial and dye degradation performance

Author: Revathi, Sorimuthu, Dey, Nibedita, Thangaleela, Subramanian, Vinayagam, Saranya, Gnanasekaran, Lalitha, Sundaram, Thanigaivel, Malik, Abdul, Khan, Azmat Ali, Roy, Arpita, and Kumar, Ashish
Published: 2024
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91. NEID Rossiter-McLaughlin Measurement of TOI-1268b: A Young Warm Saturn Aligned with Its Cool Host Star

Author: Dong, Jiayin, Huang, Chelsea X., Zhou, George, Dawson, Rebekah I., Stefánsson, Gudmundur K., Bender, Chad F., Blake, Cullen H., Ford, Eric B., Halverson, Samuel, Kanodia, Shubham, Mahadevan, Suvrath, McElwain, Michael W., Ninan, Joe P., Robertson, Paul, Roy, Arpita, Schwab, Christian, Stevens, Daniel J., Terrien, Ryan C., Vanderburg, Andrew, Kraus, Adam L., Douglas, Stephanie, Newton, Elisabeth, Rampalli, Rayna, Krolikowski, Daniel M., Collins, Karen A., Rodriguez, Joseph E., Feliz, Dax L., Srdoc, Gregor, Ziegler, Carl, Barkaoui, Khalid, Pozuelos, Francisco J., Jehin, Emmanuel, Gillon, Michaël, Benkhaldoun, Zouhair, Lewin, Pablo, Forés-Toribio, Raquel, Muñoz, Jose A., McLeod, Kim K., Özyurt, Fiona Powers, Horta, Ferran Grau, Murgas, Felipe, Latham, David W., Quinn, Samuel N., Bieryla, Allyson, Howell, Steve B., Gnilka, Crystal L., Ciardi, David R., Lund, Michael B., Dressing, Courtney D., Giacalone, Steven, Savel, Arjun B., Strakhov, Ivan A., Belinski, Alexander A., Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Torres, Guillermo, and Paegert, Martin
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Close-in gas giants present a surprising range of stellar obliquity, the angle between a planet's orbital axis and its host star's spin axis. It is unclear whether the obliquities reflect the planets' dynamical history (e.g., aligned for in situ formation or disk migration versus misaligned for high-eccentricity tidal migration) or whether other mechanisms (e.g., primordial misalignment or planet-star interactions) are more important in sculpting the obliquity distribution. Here we present the stellar obliquity measurement of TOI-1268 (TIC-142394656, $V_{\rm mag} {\sim} 10.9$), a young K-type dwarf hosting an 8.2-day period, Saturn-sized planet. TOI-1268's lithium abundance and rotation period suggest the system age between the ages of Pleiades cluster (${\sim}120$ Myr) and Praesepe cluster (${\sim}670$ Myr). Using the newly commissioned NEID spectrograph, we constrain the stellar obliquity of TOI-1268 via the Rossiter-McLaughlin (RM) effect from both radial velocity (RV) and Doppler Tomography (DT) signals. The 3$\sigma$ upper bounds of the projected stellar obliquity $|\lambda|$ from both models are below 60$^\circ$. The large host star separation ($a/R_\star {\sim} 17$), combined with the system's young age, makes it unlikely that the planet has realigned its host star. The stellar obliquity measurement of TOI-1268 probes the architecture of a young gas giant beyond the reach of tidal realignment ($a/R_\star {\gtrsim} 10$) and reveals an aligned or slightly misaligned system., Comment: 14 pages, 6 figures, 1 table, accepted for publication in ApJL; see independent work by Subjak et al. for RV follow-up of TOI-1268
Published: 2022
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92. Validation of 13 Hot and Potentially Terrestrial TESS Planets

Author: Giacalone, Steven, Dressing, Courtney D., Hedges, Christina, Kostov, Veselin B., Collins, Karen A., Jensen, Eric L. N., Yahalomi, Daniel A., Bieryla, Allyson, Ciardi, David R., Howell, Steve B., Lillo-Box, Jorge, Barkaoui, Khalid, Winters, Jennifer G., Matthews, Elisabeth, Livingston, John H., Quinn, Samuel N., Safonov, Boris S., Cadieux, Charles, Furlan, E., Crossfield, Ian J. M., Mandell, Avi M., Gilbert, Emily A., Kruse, Ethan, Quintana, Elisa V., Ricker, George R., Seager, S., Winn, Joshua N., Jenkins, Jon M., Adkins, Britt Duffy, Baker, David, Barclay, Thomas, Barrado, David, Batalha, Natalie M., Belinski, Alexander A., Benkhaldoun, Zouhair, Buchhave, Lars A., Cacciapuoti, Luca, Charbonneau, David, Chontos, Ashley, Christiansen, Jessie L., Cloutier, Ryan, Collins, Kevin I., Conti, Dennis M., Cutting, Neil, Dixon, Scott, Doyon, René, Mufti, Mohammed El, Esparza-Borges, Emma, Essack, Zahra, Fukui, Akihiko, Gan, Tianjun, Gary, Kaz, Ghachoui, Mourad, Gillon, Michaël, Girardin, Eric, Glidden, Ana, Gonzales, Erica J., Guerra, Pere, Horch, Elliott P., Helminiak, Krzysztof G., Howard, Andrew W., Huber, Daniel, Irwin, Jonathan M., Isopi, Giovanni, Jehin, Emmanuël, Kagetani, Taiki, Kane, Stephen R., Kawauchi, Kiyoe, Kielkopf, John F., Lewin, Pablo, Luker, Lindy, Lund, Michael B., Mallia, Franco, Mao, Shude, Massey, Bob, Matson, Rachel A., Mireles, Ismael, Mori, Mayuko, Murgas, Felipe, Narita, Norio, O`Dwyer, Tanner, Petigura, Erik A., Polanski, Alex S., Pozuelos, Francisco J., Palle, Enric, Parviainen, Hannu, Plavchan, Peter P., Relles, Howard M., Robertson, Paul, Rose, Mark E., Rowden, Pamela, Roy, Arpita, Savel, Arjun B., Schlieder, Joshua E., Schnaible, Chloe, Schwarz, Richard P., Sefako, Ramotholo, Selezneva, Aleksandra, Skinner, Brett, Stockdale, Chris, Strakhov, Ivan A., Tan, Thiam-Guan, Torres, Guillermo, Tronsgaard, René, Twicken, Joseph D., Vermilion, David, Waite, Ian A., Walter, Bradley, Wang, Gavin, Ziegler, Carl, and Zou, Yujie
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The James Webb Space Telescope (JWST) will be able to probe the atmospheres and surface properties of hot, terrestrial planets via emission spectroscopy. We identify 18 potentially terrestrial planet candidates detected by the Transiting Exoplanet Survey Satellite (TESS) that would make ideal targets for these observations. These planet candidates cover a broad range of planet radii ($R_{\rm p} \sim 0.6 - 2.0 R_\oplus$) and orbit stars of various magnitudes ($K_s = 5.78 - 10.78$, $V = 8.4 - 15.69$) and effective temperatures ($T_{\rm eff }\sim 3000 - 6000$ K). We use ground-based observations collected through the TESS Follow-up Observing Program (TFOP) and two vetting tools -- DAVE and TRICERATOPS -- to assess the reliabilities of these candidates as planets. We validate 13 planets: TOI-206 b, TOI-500 b, TOI-544 b, TOI-833 b, TOI-1075 b, TOI-1411 b, TOI-1442 b, TOI-1693 b, TOI-1860 b, TOI-2260 b, TOI-2411 b, TOI-2427 b, and TOI-2445 b. Seven of these planets (TOI-206 b, TOI-500 b, TOI-1075 b, TOI-1442 b, TOI-2260 b, TOI-2411 b, and TOI-2445 b) are ultra-short-period planets. TOI-1860 is the youngest ($133 \pm 26$ Myr) solar twin with a known planet to date. TOI-2260 is a young ($321 \pm 96$ Myr) G dwarf that is among the most metal-rich ([Fe/H] = $0.22 \pm 0.06$ dex) stars to host an ultra-short-period planet. With an estimated equilibrium temperature of $\sim 2600$ K, TOI-2260 b is also the fourth hottest known planet with $R_{\rm p} < 2 \, R_\oplus$.
Published: 2022
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93. Rotational modulation of spectroscopic Zeeman signatures in low-mass stars

Author: Terrien, Ryan C., Keen, Allison, Oda, Katy, Parts, Winter, Stefánsson, Guðmundur, Mahadevan, Suvrath, Robertson, Paul, Ninan, Joe P., Beard, Corey, Bender, Chad F., Cochran, William D., Cunha, Katia, Diddams, Scott A., Fredrick, Connor, Halverson, Samuel, Hearty, Fred, Ickler, Adam, Kanodia, Shubham, Libby-Roberts, Jessica E., Lubin, Jack, Metcalf, Andrew J., Olsen, Freja, Ramsey, Lawrence W., Roy, Arpita, Schwab, Christian, Smith, Verne V., and Turner, Ben
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Accurate tracers of the stellar magnetic field and rotation are cornerstones for the study of M dwarfs and for reliable detection and characterization of their exoplanetary companions. Such measurements are particularly challenging for old, slowly rotating, fully convective M dwarfs. To explore the use of new activity and rotation tracers, we examined multi-year near-infrared spectroscopic monitoring of two such stars -- GJ 699 (Barnard's Star) and Teegarden's Star -- carried out with Habitable Zone Planet Finder spectrograph. We detected periodic variations in absorption line widths across the stellar spectrum with higher amplitudes towards longer wavelengths. We also detected similar variations in the strength and width of the 12435.67 Angstrom neutral potassium (K I) line, a known tracer of the photospheric magnetic field. Attributing these variations to rotational modulation, we confirm the known $145\pm15$ d rotation period of GJ 699, and measure the rotation period of Teegarden's Star to be $99.6\pm1.4$ d. Based on simulations of the K I line and the wavelength-dependence of the line width signal, we argue that the observed signals are consistent with varying photospheric magnetic fields and the associated Zeeman effect. These results highlight the value of detailed line profile measurements in the near-infrared for diagnosing stellar magnetic field variability. Such measurements may be pivotal for disentangling activity and exoplanet-related signals in spectroscopic monitoring of old, low-mass stars., Comment: Accepted for publication in ApJL
Published: 2022
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94. TOI-3714 b and TOI-3629 b: Two gas giants transiting M dwarfs confirmed with HPF and NEID

Author: Cañas, Caleb I., Kanodia, Shubham, Bender, Chad F., Mahadevan, Suvrath, Stefánsson, Guðmundur, Cochran, William D., Lin, Andrea S. J., Hwang, Hsiang-Chih, Powers, Luke, Monson, Andrew, Green, Elizabeth M., Parker, Brock A., Swaby, Tera N., Kobulnicky, Henry A., Wisniewski, John, Gupta, Arvind F., Everett, Mark E., Jones, Sinclaire, Anjakos, Benjamin, Beard, Corey, Blake, Cullen H., Diddams, Scott A., Dong, Zehao, Fredrick, Connor, Hakemiamjad, Elnaz, Hebb, Leslie, Libby-Roberts, Jessica E., Logsdon, Sarah E., McElwain, Michael W., Metcalf, Andrew J., Ninan, Joe P., Rajagopal, Jayadev, Ramsey, Lawrence W., Robertson, Paul, Roy, Arpita, Ruhle, Jacob, Schwab, Christian, Terrien, Ryan C., and Wright, Jason T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs. TOI-3714 ($V=15.24,~J=11.74$) is an M2 dwarf hosting a hot Jupiter ($M_p=0.70 \pm 0.03~\mathrm{M_J}$ and $R_p=1.01 \pm 0.03~\mathrm{R_J}$) on an orbital period of $2.154849 \pm 0.000001$ days with a resolved white dwarf companion. TOI-3629 ($V=14.63,~J=11.42$) is an M1 dwarf hosting a hot Jupiter ($M_p=0.26 \pm 0.02~\mathrm{M_J}$ and $R_p=0.74 \pm 0.02~\mathrm{R_J}$) on an orbital period of $3.936551_{-0.000006}^{+0.000005}$ days. We characterize each transiting companion using a combination of ground-based and space-based photometry, speckle imaging, and high-precision velocimetry from the Habitable-zone Planet Finder and the NEID spectrographs. With the discovery of these two systems, there are now nine M dwarfs known to host transiting hot Jupiters. Among this population, TOI-3714 b ($T_{eq}=750\pm20$ K and $\mathrm{TSM}=98\pm7$) and TOI-3629 b ($T_{eq}=690\pm20$ K and $\mathrm{TSM}=80\pm9$) are warm gas giants amenable to additional characterization with transmission spectroscopy to probe atmospheric chemistry and, for TOI-3714, obliquity measurements to probe formation scenarios., Comment: 39 pages, 13 figures, 4 tables. Accepted for publication in AJ
Published: 2022
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95. The TESS-Keck Survey. VIII. Confirmation of a Transiting Giant Planet on an Eccentric 261 day Orbit with the Automated Planet Finder Telescope

Author: Dalba, Paul A., Kane, Stephen R., Dragomir, Diana, Villanueva Jr., Steven, Collins, Karen A., Jacobs, Thomas Lee, Lacourse, Daryll M., Gagliano, Robert, Kristiansen, Martti H., Omohundro, Mark, Schwengeler, Hans M., Terentev, Ivan A., Vanderburg, Andrew, Fulton, Benjamin, Isaacson, Howard, Van Zandt, Judah, Howard, Andrew W., Thorngren, Daniel P., Howell, Steve B., Batalha, Natalie M., Chontos, Ashley, Crossfield, Ian J. M., Dressing, Courtney D., Huber, Daniel, Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Brinkman, Casey L., Giacalone, Steven, Hill, Michelle L., Lubin, Jack, Mayo, Andrew W., Močnik, Teo, Murphy, Joseph M. Akana, Polanski, Alex S., Rice, Malena, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Turtelboom, Emma V., Tyler, Dakotah, Benni, Paul, Boyce, Pat, Esposito, Thomas M., Girardin, E., Laloum, Didier, Lewin, Pablo, Mann, Christopher R., Marchis, Franck, Schwarz, Richard P., Srdoc, Gregor, Steuer, Jana, Sivarani, Thirupathi, Unni, Athira, Eisner, Nora L., Fetherolf, Tara, Li, Zhexing, Yao, Xinyu, Pepper, Joshua, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Burke, Christopher J., Eastman, Jason D., Lund, Michael B., Rodriguez, David R., Rowden, Pamela, Ting, Eric B., and Villaseñor, Jesus Noel
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of TOI-2180 b, a 2.8 $M_{\rm J}$ giant planet orbiting a slightly evolved G5 host star. This planet transited only once in Cycle 2 of the primary Transiting Exoplanet Survey Satellite (TESS) mission. Citizen scientists identified the 24 hr single-transit event shortly after the data were released, allowing a Doppler monitoring campaign with the Automated Planet Finder telescope at Lick Observatory to begin promptly. The radial velocity observations refined the orbital period of TOI-2180 b to be 260.8$\pm$0.6 days, revealed an orbital eccentricity of 0.368$\pm$0.007, and discovered long-term acceleration from a more distant massive companion. We conducted ground-based photometry from 14 sites spread around the globe in an attempt to detect another transit. Although we did not make a clear transit detection, the nondetections improved the precision of the orbital period. We predict that TESS will likely detect another transit of TOI-2180 b in Sector 48 of its extended mission. We use giant planet structure models to retrieve the bulk heavy-element content of TOI-2180 b. When considered alongside other giant planets with orbital periods over 100 days, we find tentative evidence that the correlation between planet mass and metal enrichment relative to stellar is dependent on orbital properties. Single-transit discoveries like TOI-2180 b highlight the exciting potential of the TESS mission to find planets with long orbital periods and low irradiation fluxes despite the selection biases associated with the transit method., Comment: Published in AJ
Published: 2022
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96. Evaluation of different phytochemicals from Cannabis sativa against Myelin oligodendrocyte glycoprotein receptor

Author: Roy, Arpita, Gupta, Aaryan, and Verma, Devvret
Published: 2023
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97. Computational study of bioactive compounds from endophytic fungi against SARS-CoV-2

Author: Roy, Arpita, Menon, Tarunya, and Rawat, Janhvi Mishra
Published: 2023
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98. Synthesis of a silica matrix with ZnO nanoparticles for the fabrication of a recyclable photodegradation system to eliminate methylene blue dye

Author: Naik Harshala Sandip, Sah Parvindar Manejar, Dhangade Manali, Lakkakula Jaya, Raut Rajesh Warluji, Roy Arpita, Alghamdi Saad, Qusty Naeem, Alhindi Zain, Kabrah Ahmed, and Rani Anju
Subjects: silica matrix, zno nanoparticles, photocatalytic activity, recoverable matrix, Chemistry, QD1-999
Abstract: In this study, a silica matrix was utilized as a substrate for zinc oxide nanoparticles (ZnO NPs) to enhance their photocatalytic activity for the degradation of methylene blue (MB) dye. The recovery of the prepared material was also investigated. To compare the performance of the prepared material with ZnO NPs and bare silica, various analyses were conducted. ZnO NPs were synthesized via a coprecipitation method and characterized using Fourier-transform infrared spectra and X-ray diffraction (XRD). The XRD results revealed highly crystalline ZnO NPs with an average crystallite size of less than 100 nm. The presence of ZnO on the silica matrix was confirmed using scanning electron microscopy (SEM) and EDX analysis. The prepared ZnO NPs showed enhanced photocatalytic activity for the degradation of MB dye, and reasonable material recovery was also observed. The silica-coated ZnO NPs degraded MB dye by 97% in just 40 min and retained their photocatalytic activity for up to 20 cycles. In comparison, bare silica exhibited effective photodegradation but lost its photodegradation capacity after five cycles. ZnO NPs without silica coating took 5 h to degrade MB dye. The significant accomplishment in this study is the development of novel materials with high recoverability, simple preparation, and efficient photocatalytic activity. In the future, ZnO NPs supported on a silica matrix can be utilized for various applications.
Published: 2023
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99. TOI 560 : Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS and HIRES RVs

Author: Mufti, Mohammed El, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villasenor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Murphy, Joseph M. Akana, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J, Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We validate the presence of a two-planet system orbiting the 0.15--1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, $P = 6.3980661^{+0.0000095}_{-0.0000097}$ days, $e=0.294^{+0.13}_{-0.062}$, $M= 0.94^{+0.31}_{-0.23}M_{Nep}$) initially discovered in the Sector 8 \tess\ mission observations, and a transiting mini-Neptune (TOI 560 c, $P = 18.8805^{+0.0024}_{-0.0011}$ days, $M= 1.32^{+0.29}_{-0.32}M_{Nep}$) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from \tess\, \textit{Spitzer}, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false positive scenarios, and detect the photo-eccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published PFS RVs from Magellan Observatory. We detect the masses of both planets at $> 3-\sigma$ significance. We apply a Gaussian process (GP) model to the \tess\ light curves to place priors on a chromatic radial velocity GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of NIR RVs in mitigating stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multi-planet system with two planets suitable for atmospheric characterization with James Webb Space Telescope (JWST) and other upcoming missions. In particular, it will undergo six transit pairs separated by $<$6 hours before June 2027., Comment: AAS Journals, Accepted for publication
Published: 2021

100. Observing the Sun as a star: Design and early results from the NEID solar feed

Author: Lin, Andrea S. J., Monson, Andrew, Mahadevan, Suvrath, Ninan, Joe P., Halverson, Samuel, Nitroy, Colin, Bender, Chad F., Logsdon, Sarah E., Kanodia, Shubham, Terrien, Ryan C., Roy, Arpita, Luhn, Jacob K., Gupta, Arvind F., Ford, Eric B., Hearty, Fred, Laher, Russ R., Hunting, Emily, McBride, William R., Rivera, Noah Isaac Salazar, Rajagopal, Jayadev, Wolf, Marsha J., Robertson, Paul, Wright, Jason T., Blake, Cullen H., Canas, Caleb I., Lubar, Emily, McElwain, Michael W., Ramsey, Lawrence W., Schwab, Christian, and Stefansson, Gudmundur
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Efforts with extreme-precision radial velocity (EPRV) instruments to detect small-amplitude planets are largely limited, on many timescales, by the effects of stellar variability and instrumental systematics. One avenue for investigating these effects is the use of small solar telescopes which direct disk-integrated sunlight to these EPRV instruments, observing the Sun at high cadence over months or years. We have designed and built a solar feed system to carry out "Sun-as-a-star" observations with NEID, a very high precision Doppler spectrometer recently commissioned at the WIYN 3.5m Telescope at Kitt Peak National Observatory. The NEID solar feed has been taking observations nearly every day since December 2020; data is publicly available at the NASA Exoplanet Science Institute (NExScI) NEID Solar Archive: \url{https://neid.ipac.caltech.edu/search_solar.php}. In this paper, we present the design of the NEID solar feed and explanations behind our design intent. We also present early radial velocity (RV) results which demonstrate NEID's RV stability on the Sun over 4 months of commissioning: 0.66~m/s RMS under good sky conditions and improving to 0.41~m/s RMS under best conditions., Comment: Accepted to AJ
Published: 2021
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