2021, Pinna, Francesca, Neumayer, Nadine, Seth, Anil, Emsellem, Eric, Nguyen, Dieu D., Böker, Torsten, Cappellari, Michele, McDermid, Richard M., Voggel, Karina, Walcher, C. Jakob

We have identified an error in Equations (D3) and (D4) in Appendix D of the published article. These equations result from the combination of Equations (16), (17), and (18) in Harborne et al. (2020). In the published article, the right-hand sides are swapped with each other. The corrected versions of the equations are (Formula Presented). All results shown and discussed in the published article were obtained using the correct version of the equations and do not need any modifications.

2019, Aguado, D. S., Ahumada, Romina, Almeida, Andrés, Anderson, Scott F., Andrews, Brett H., Anguiano, Borja, Ortíz, Erik Aquino, Aragón-Salamanca, Alfonso, Argudo-Fernández, Maria, Aubert, Marie, Avila-Reese, Vladimir, Seong Hwang, Ho, Ibarra-Medel, Héctor J., Eduardo Jimenez Angel, Camilo, Johnson, Jennifer, Jones, Amy, Jönsson, Henrik, Kinemuchi, Karen, Kollmeier, Juna, Krawczyk, Coleman, Kreckel, Kathryn, Badenes, Carles, Kruk, Sandor, Lacerna, Ivan, Lan, Ting-Wen, Lane, Richard R., Law, David R., Lee, Young-Bae, Li, Cheng, Lian, Jianhui, Lin, Lihwai, Lin, Yen-Ting, Barboza Rembold, Sandro, Lintott, Chris, Long, Dan, Longa-Peña, Penélope, Ted Mackereth, J., de la Macorra, Axel, Majewski, Steven R., Malanushenko, Olena, Manchado, Arturo, Maraston, Claudia, Mariappan, Vivek, Barger, Kat, Marinelli, Mariarosa, Marques-Chaves, Rui, Masseron, Thomas, Masters, Karen L., McDermid, Richard M., Medina Peña, Nicolás, Meneses-Goytia, Sofia, Merloni, Andrea, Merrifield, Michael, Meszaros, Szabolcs, Barrera-Ballesteros, Jorge, Minniti, Dante, Minsley, Rebecca, Muna, Demitri, Myers, Adam D., Nair, Preethi, Correa do Nascimento, Janaina, Newman, Jeffrey A., Nitschelm, Christian, Olmstead, Matthew D, Oravetz, Audrey, Bates, Dominic, Oravetz, Daniel, Ortega Minakata, René A., Pace, Zach, Padilla, Nelson, Palicio, Pedro A., Pan, Kaike, Pan, Hsi-An, Parikh, Taniya, Parker, James, Peirani, Sebastien, Bautista, Julian, Penny, Samantha, Percival, Will J., Perez-Fournon, Ismael, Peterken, Thomas, Pinsonneault, Marc H., Prakash, Abhishek, Raddick, M. Jordan, Raichoor, Anand, Riffel, Rogemar A., Riffel, Rogério, Beaton, Rachael L., Rix, Hans-Walter, Robin, Annie C., Roman-Lopes, Alexandre, Rose, Benjamin, Ross, Ashley J., Rossi, Graziano, Rowlands, Kate, Rubin, Kate H. R., Sánchez, Sebastián F., Sánchez-Gallego, José R., Beers, Timothy C., Sayres, Conor, Schaefer, Adam, Schiavon, Ricardo P., Schimoia, Jaderson S., Schlafly, Edward, Schlegel, David, Schneider, Donald P., Schultheis, Mathias, Seo, Hee-Jong, Shamsi, Shoaib J., Belfiore, Francesco, Shao, Zhengyi, Shen, Shiyin, Shetty, Shravan, Simonian, Gregory, Smethurst, Rebecca J., Sobeck, Jennifer, Souter, Barbara J., Spindler, Ashley, Stark, David V., Stassun, Keivan G., Bernardi, Mariangela, Steinmetz, Matthias, Storchi-Bergmann, Thaisa, Stringfellow, Guy S., Suárez, Genaro, Sun, Jing, Taghizadeh-Popp, Manuchehr, Talbot, Michael S., Tayar, Jamie, Thakar, Aniruddha R., Thomas, Daniel, Bershady, Matthew, Tissera, Patricia, Tojeiro, Rita, Troup, Nicholas W., Unda-Sanzana, Eduardo, Valenzuela, Octavio, Vargas-Magaña, Mariana, Antonio Vázquez-Mata, José, Wake, David, Alan Weaver, Benjamin, Weijmans, Anne-Marie, Beutler, Florian, Westfall, Kyle B., Wild, Vivienne, Wilson, John, Woods, Emily, Yan, Renbin, Yang, Meng, Zamora, Olga, Zasowski, Gail, Zhang, Kai, Zheng, Zheng, Bird, Jonathan, Zheng, Zheng, Zhu, Guangtun, Zinn, Joel C., Zou, Hu, Bizyaev, Dmitry, Blanc, Guillermo A., Blanton, Michael R., Blomqvist, Michael, Bolton, Adam S., Boquien, Médéric, Borissova, Jura, Bovy, Jo, Nielsen Brandt, William, Brinkmann, Jonathan, Brownstein, Joel R., Bundy, Kevin, Burgasser, Adam, Byler, Nell, Cano Diaz, Mariana, Cappellari, Michele, Carrera, Ricardo, Cervantes Sodi, Bernardo, Chen, Yanping, Cherinka, Brian, Doohyun Choi, Peter, Chung, Haeun, Coffey, Damien, Comerford, Julia M., Comparat, Johan, Covey, Kevin, da Silva Ilha, Gabriele, da Costa, Luiz, Sophia Dai, Yu, Damke, Guillermo, Darling, Jeremy, Davies, Roger, Dawson, Kyle, de Sainte Agathe, Victoria, Deconto Machado, Alice, Del Moro, Agnese, De Lee, Nathan, Diamond-Stanic, Aleksandar M., Domínguez Sánchez, Helena, Donor, John, Drory, Niv, du Mas des Bourboux, Hélion, Duckworth, Chris, Dwelly, Tom, Ebelke, Garrett, Emsellem, Eric, Escoffier, Stephanie, Fernández-Trincado, José G., Feuillet, Diane, Fischer, Johanna-Laina, Fleming, Scott W., Fraser-McKelvie, Amelia, Freischlad, Gordon, Frinchaboy, Peter M., Fu, Hai, Galbany, Lluís, Garcia-Dias, Rafael, García-Hernández, D. A., Alberto Garma Oehmichen, Luis, Antonio Geimba Maia, Marcio, Gil-Marín, Héctor, Grabowski, Kathleen, Gu, Meng, Guo, Hong, Ha, Jaewon, Harrington, Emily, Hasselquist, Sten, Hayes, Christian R., Hearty, Fred, Hernandez Toledo, Hector, Hicks, Harry, Hogg, David W., Holley-Bockelmann, Kelly, Holtzman, Jon A., Hsieh, Bau-Ching, Hunt, Jason A. S.

Twenty years have passed since first light for the Sloan Digital Sky Survey (SDSS). Here, we release data taken by the fourth phase of SDSS (SDSS-IV) across its first three years of operation (2014 July–2017 July). This is the third data release for SDSS-IV, and the 15th from SDSS (Data Release Fifteen; DR15). New data come from MaNGA—we release 4824 data cubes, as well as the first stellar spectra in the MaNGA Stellar Library (MaStar), the first set of survey-supported analysis products (e.g., stellar and gas kinematics, emission-line and other maps) from the MaNGA Data Analysis Pipeline, and a new data visualization and access tool we call "Marvin." The next data release, DR16, will include new data from both APOGEE-2 and eBOSS; those surveys release no new data here, but we document updates and corrections to their data processing pipelines. The release is cumulative; it also includes the most recent reductions and calibrations of all data taken by SDSS since first light. In this paper, we describe the location and format of the data and tools and cite technical references describing how it was obtained and processed. The SDSS website (www.sdss.org) has also been updated, providing links to data downloads, tutorials, and examples of data use. Although SDSS-IV will continue to collect astronomical data until 2020, and will be followed by SDSS-V (2020–2025), we end this paper by describing plans to ensure the sustainability of the SDSS data archive for many years beyond the collection of data.

2022, Williams, Thomas G., Sun, Jiayi, Barnes, Ashley T., Schinnerer, Eva, Henshaw, Jonathan D., Meidt, Sharon E., Querejeta, Miguel, Watkins, Elizabeth J., Bigiel, Frank, Blanc, Guillermo A., Boquien, Médéric, Cao, Yixian, Chevance, Mélanie, Egorov, Oleg V., Emsellem, Eric, Glover, Simon C. O., Grasha, Kathryn, Hassani, Hamid, Jeffreson, Sarah, Jiménez-Donaire, María J., Kim, Jaeyeon, Klessen, Ralf S., Kreckel, Kathryn, Kruijssen, J. M. Diederik, Larson, Kirsten L., Leroy, Adam K., Liu, Daizhong, Pessa, Ismael, Pety, Jérôme, Pinna, Francesca, Rosolowsky, Erik, Sandstrom, Karin M., Smith, Rowan, Sormani, Mattia C., Stuber, Sophia, Thilker, David A., Whitmore, Bradley C.

We combine JWST observations with Atacama Large Millimeter/submillimeter Array CO and Very Large Telescope MUSE Hα data to examine off-spiral arm star formation in the face-on, grand-design spiral galaxy NGC 628. We focus on the northern spiral arm, around a galactocentric radius of 3-4 kpc, and study two spurs. These form an interesting contrast, as one is CO-rich and one CO-poor, and they have a maximum azimuthal offset in MIRI 21 μm and MUSE Hα of around 40° (CO-rich) and 55° (CO-poor) from the spiral arm. The star formation rate is higher in the regions of the spurs near spiral arms, but the star formation efficiency appears relatively constant. Given the spiral pattern speed and rotation curve of this galaxy and assuming material exiting the arms undergoes purely circular motion, these offsets would be reached in 100-150 Myr, significantly longer than the 21 μm and Hα star formation timescales (both < 10 Myr). The invariance of the star formation efficiency in the spurs versus the spiral arms indicates massive star formation is not only triggered in spiral arms, and cannot simply occur in the arms and then drift away from the wave pattern. These early JWST results show that in situ star formation likely occurs in the spurs, and that the observed young stars are not simply the “leftovers” of stellar birth in the spiral arms. The excellent physical resolution and sensitivity that JWST can attain in nearby galaxies will well resolve individual star-forming regions and help us to better understand the earliest phases of star formation.