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1. Notes on the Music: A social data infrastructure for music annotation

Author: Weigl, David, Goebl, Werner, Baker, David J., Crawford, Tim, Zubani, Federico, Gkiokas, Aggelos, Gutierrez, Nicolas F., Porter, Alastair, Santos, Patricia, Weigl, David, Goebl, Werner, Baker, David J., Crawford, Tim, Zubani, Federico, Gkiokas, Aggelos, Gutierrez, Nicolas F., Porter, Alastair, and Santos, Patricia
Abstract: Beside transmitting musical meaning from composer to reader, symbolic music notation affords the dynamic addition of layers of information by annotation. This allows music scores to serve as rudimentary communication frameworks. Music encodings bring these affordances into the digital realm; though annotations may be represented as digital pen-strokes upon a score image, they must be captured using machine-interpretable semantics to fully benefit from this transformation. This is challenging, as annotators’ requirements are heterogeneous, varying both across different types of user (e.g., musician, scholar) and within these groups, depending on the specific use-case. A hypothetical all-encompassing tool catering to every conceivable annotation type, even if it were possible to build, would vastly complicate user interaction. This additional complexity would significantly increase cognitive load and impair usability, particularly in dynamic real-time usage contexts, e.g., live annotation during music rehearsal or performance. To address this challenge, we present a social data infrastructure that facilitates the creation of use-case specific annotation toolkits. Its components include a selectable-score module that supports customisable click-and-drag selection of score elements (e.g., notes, measures, directives); the Web Annotations data model, extended to support the creation of custom, Web-addressable annotation types supporting the specification and (re-)use of annotation palettes; and the Music Encoding and Linked Data (MELD) Javascript client library, used to build interfaces that map annotation types to rendering and interaction handlers. We have extended MELD to support the Solid platform for social Linked Data, allowing annotations to be privately stored in user-controlled Personal Online Datastores (Pods), or selectively shared or published. To demonstrate the feasibility of our proposed approach, we present annotation interfaces employing the outlined inf
Published: 2024

2. FAIR Interconnection and Enrichment of Public-Domain Music Resources on the Web

Author: Weigl, David, Goebl, Werner, Crawford, Tim, Gkiokas, Aggelos, Gómez, Emilia, Gutierrez, Nicolas F., Liem, Cynthia C. S., Santos, Patricia, Weigl, David, Goebl, Werner, Crawford, Tim, Gkiokas, Aggelos, Gómez, Emilia, Gutierrez, Nicolas F., Liem, Cynthia C. S., and Santos, Patricia
Abstract: Vast amounts of publicly licensed classical music resources are housed within many different repositories on the Web encompassing richly diverse facets of information—including bibliographical and biographical data, digitized images of music notation, music score encodings, audiovisual performance recordings, derived feature data, scholarly commentaries, and listener reactions. While these varied perspectives ought to contribute to greater holistic understanding of the music objects under consideration, in practice, such repositories are typically minimally connected. The TROMPA project aims to improve this situation by interconnecting and enriching public-domain music repositories. This is achieved, on the one hand, by the application of automated, cutting-edge Music Information Retrieval techniques, and on the other, by the development of contribution mechanisms enabling users to integrate their expertise. Information within established repositories is interrelated with data generated by the project within a data infrastructure whose design is guided by the FAIR principles of data management and stewardship: making music information Findable, Accessible, Interoperable, and Reusable. We provide an overview of challenges of description, identification, representation, contribution, and reliability toward applying the FAIR principles to music information, and outline TROMPA's implementational approach to overcoming these challenges. This approach applies a graph-based data infrastructure to interrelate information hosted in different repositories on the Web within a unifying data model (a 'knowledge graph'). Connections are generated across different representations of music content beyond the catalogue level, for instance connecting note elements within score encodings to corresponding moments in performance time-lines. Contributions of user data are supported via privacy-first mechanisms that retain control of such data with the contributing user. Provenance inform
Published: 2024

3. The wide-field, multiplexed, spectroscopic facility WEAVE : Survey design, overview, and simulated implementation

Author: Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, Zurita, Cristina, Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, and Zurita, Cristina
Abstract: WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959nm at R similar to 5000, or two shorter ranges at . After summarizing the design and implementation of WEAVE and its data systems, we present the organization, science drivers, and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for similar to 3 million stars and detailed abundances for similar to 1.5 million brighter field and open-cluster stars; (ii) survey similar to 0.4 million Galactic-plane OBA stars, young stellar objects, and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey similar to 400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionized gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in field galaxies at 0.3 less than or similar to z less than or similar to 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; and (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.
Published: 2024
Full Text: View/download PDF

4. The wide-field, multiplexed, spectroscopic facility WEAVE : Survey design, overview, and simulated implementation

Author: Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, Zurita, Cristina, Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, and Zurita, Cristina
Abstract: WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959nm at R similar to 5000, or two shorter ranges at . After summarizing the design and implementation of WEAVE and its data systems, we present the organization, science drivers, and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for similar to 3 million stars and detailed abundances for similar to 1.5 million brighter field and open-cluster stars; (ii) survey similar to 0.4 million Galactic-plane OBA stars, young stellar objects, and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey similar to 400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionized gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in field galaxies at 0.3 less than or similar to z less than or similar to 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; and (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.
Published: 2024
Full Text: View/download PDF

5. The wide-field, multiplexed, spectroscopic facility WEAVE : Survey design, overview, and simulated implementation

Author: Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, Zurita, Cristina, Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, and Zurita, Cristina
Abstract: WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959nm at R similar to 5000, or two shorter ranges at . After summarizing the design and implementation of WEAVE and its data systems, we present the organization, science drivers, and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for similar to 3 million stars and detailed abundances for similar to 1.5 million brighter field and open-cluster stars; (ii) survey similar to 0.4 million Galactic-plane OBA stars, young stellar objects, and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey similar to 400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionized gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in field galaxies at 0.3 less than or similar to z less than or similar to 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; and (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.
Published: 2024
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6. Improving Uncertainty-Error Correspondence in Deep Bayesian Medical Image Segmentation

Author: MS Radiotherapie, Cancer, Mody, Prerak, Chaves-de-Plaza, Nicolas F., Rao, Chinmay, Astrenidou, Eleftheria, de Ridder, Mischa, Hoekstra, Nienke, Hildebrandt, Klaus, Staring, Marius, MS Radiotherapie, Cancer, Mody, Prerak, Chaves-de-Plaza, Nicolas F., Rao, Chinmay, Astrenidou, Eleftheria, de Ridder, Mischa, Hoekstra, Nienke, Hildebrandt, Klaus, and Staring, Marius
Published: 2024

7. The wide-field, multiplexed, spectroscopic facility WEAVE : Survey design, overview, and simulated implementation

Author: Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, Zurita, Cristina, Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcon-Barroso, Jesus, Gaensicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragon-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Dominguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Farina, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Mendez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguio, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Perez, Isabel, Perez-Rafols, Ignasi, Pico, Sergio, Raddi, Roberto, Romero-Gomez, Merce, Royer, Frederic, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Allende Prieto, Carlos, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Nunez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Dominguez-Gomez, Jesus, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferre-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, Garcia-Benito, Ruben, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Gonzalez Delgado, Rosa M., Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I., Larsen, Sren S., Lemasle, Bertrand, Lewis, Ian J., Lhome, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Maiz Apellaniz, Jesus, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escude, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sebastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Roettgering, Huub J. A., Rubino-Martin, Jose Alberto, Sabater, Jose, San Juan, Jose, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simon-Diaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, and Zurita, Cristina
Abstract: WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366-959nm at R similar to 5000, or two shorter ranges at . After summarizing the design and implementation of WEAVE and its data systems, we present the organization, science drivers, and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for similar to 3 million stars and detailed abundances for similar to 1.5 million brighter field and open-cluster stars; (ii) survey similar to 0.4 million Galactic-plane OBA stars, young stellar objects, and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey similar to 400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionized gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in field galaxies at 0.3 less than or similar to z less than or similar to 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; and (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.
Published: 2024
Full Text: View/download PDF

8. MusE GAs FLOw and Wind (MEGAFLOW) XI. Scaling relations between outflows and host galaxy properties

Author: Schroetter, Ilane, Bouché, Nicolas F., Zabl, Johannes, Wendt, Martin, Cherrey, Maxime, Langan, Ivanna, Schaye, Joop, Contini, Thierry, Schroetter, Ilane, Bouché, Nicolas F., Zabl, Johannes, Wendt, Martin, Cherrey, Maxime, Langan, Ivanna, Schaye, Joop, and Contini, Thierry
Abstract: Absorption line spectroscopy using background quasars can provide strong constraints on galactic outflows. In this paper, we investigate possible scaling relations between outflow properties, namely outflow velocity \Vout, the mass ejection rate $\dot M_{\rm out}$, and the mass loading factor $\eta$ and the host galaxy properties, such as star formation rate (SFR), SFR surface density, redshift, and stellar mass using galactic outflows probed by background quasars from MEGAFLOW and other surveys. We find that $V_{\rm out}$ ($\eta$) is (anti-)correlated with SFR and SFR surface density. We extend the formalism of momentum-driven outflows of Heckman et al. to show that it applies not only to down the barrel studies but also to winds probed by background quasars, suggesting a possible universal wind formalism. Under this formalism, we find a clear distinction between ``strong'' and ``weak'' outflows where ``strong'' outflows seem to have tighter correlations with galaxy properties (SFR or galaxy stellar mass) than ``weak'' outflows., Comment: 13 pages, 9 figures, accepted for publication in A&A
Published: 2024

9. The Effect of Cosmic Rays on the Observational Properties of the CGM

Author: DeFelippis, Daniel, Bournaud, Frédéric, Bouché, Nicolas F., Tollet, Edouard, Farcy, Marion, Rey, Maxime, Rosdahl, Joakim, Blaizot, Jérémy, DeFelippis, Daniel, Bournaud, Frédéric, Bouché, Nicolas F., Tollet, Edouard, Farcy, Marion, Rey, Maxime, Rosdahl, Joakim, and Blaizot, Jérémy
Abstract: The circumgalactic medium (CGM) contains information on the cumulative effect of galactic outflows over time, generally thought to be caused by feedback from star formation and active galactic nuclei. Observations of such outflows via absorption in CGM gas of quasar sightlines show a significant amount of cold ($\lesssim 10^4 \; \rm{K}$) gas which cosmological simulations struggle to reproduce. Here, we use the adaptive mesh refinement hydrodynamical code RAMSES to investigate the effect of cosmic rays (CR) on the cold gas content of the CGM using three zoom realizations of a $z=1$ star-forming galaxy with supernova mechanical feedback: one with no CR feedback (referred to as no-CR), one with a medium CR diffusion coefficient $\kappa = 10^{28} \; \rm{cm^{2}\; s^{-1}}$ (CR$-\kappa_{\rm med}$), and one with a high rate of diffusion of $\kappa = 3\times10^{29} \; \rm{cm^{2}\; s^{-1}}$ (CR$-\kappa_{\rm high}$). We find that, for CR$-\kappa_{\rm med}$, the effects of CRs are largely confined to the galaxy itself as CRs do not extend far into the CGM. However, for CR$-\kappa_{\rm high}$, the CGM temperature is lowered and the amount of outflowing gas is boosted. Our CR simulations fall short of the observed Mg II covering fraction, a tracer of gas at temperatures $\lesssim 10^4 \; \rm{K}$, but the CR$-\kappa_{\rm high}$ simulation is more in agreement with covering fractions of C IV and O VI, which trace higher temperature gas., Comment: Accepted to MNRAS. 14 pages, 10 figures
Published: 2024
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10. The Wide-field Spectroscopic Telescope (WST) Science White Paper

Author: Mainieri, Vincenzo, Anderson, Richard I., Brinchmann, Jarle, Cimatti, Andrea, Ellis, Richard S., Hill, Vanessa, Kneib, Jean-Paul, McLeod, Anna F., Opitom, Cyrielle, Roth, Martin M., Sanchez-Saez, Paula, Smiljanic, Rodolfo, Tolstoy, Eline, Bacon, Roland, Randich, Sofia, Adamo, Angela, Annibali, Francesca, Arevalo, Patricia, Audard, Marc, Barsanti, Stefania, Battaglia, Giuseppina, Aran, Amelia M. Bayo, Belfiore, Francesco, Bellazzini, Michele, Bellini, Emilio, Beltran, Maria Teresa, Berni, Leda, Bianchi, Simone, Biazzo, Katia, Bisero, Sofia, Bisogni, Susanna, Bland-Hawthorn, Joss, Blondin, Stephane, Bodensteiner, Julia, Boffin, Henri M. J., Bonito, Rosaria, Bono, Giuseppe, Bouche, Nicolas F., Bowman, Dominic, Braga, Vittorio F., Bragaglia, Angela, Branchesi, Marica, Brucalassi, Anna, Bryant, Julia J., Bryson, Ian, Busa, Innocenza, Camera, Stefano, Carbone, Carmelita, Casali, Giada, Casali, Mark, Casasola, Viviana, Castro, Norberto, Catelan, Marcio, Cavallo, Lorenzo, Chiappini, Cristina, Cioni, Maria-Rosa, Colless, Matthew, Colzi, Laura, Contarini, Sofia, Couch, Warrick, D'Ammando, Filippo, D., William d'Assignies, D'Orazi, Valentina, da Silva, Ronaldo, Dainotti, Maria Giovanna, Damiani, Francesco, Danielski, Camilla, De Cia, Annalisa, de Jong, Roelof S., Dhawan, Suhail, Dierickx, Philippe, Driver, Simon P., Dupletsa, Ulyana, Escoffier, Stephanie, Escorza, Ana, Fabrizio, Michele, Fiorentino, Giuliana, Fontana, Adriano, Fontani, Francesco, Sanchez, Daniel Forero, Franois, Patrick, Galindo-Guil, Francisco Jose, Gallazzi, Anna Rita, Galli, Daniele, Garcia, Miriam, Garcia-Rojas, Jorge, Garilli, Bianca, Grand, Robert, Guarcello, Mario Giuseppe, Hazra, Nandini, Helmi, Amina, Herrero, Artemio, Iglesias, Daniela, Ilic, Dragana, Irsic, Vid, Ivanov, Valentin D., Izzo, Luca, Jablonka, Pascale, Joachimi, Benjamin, Kakkad, Darshan, Kamann, Sebastian, Koposov, Sergey, Kordopatis, Georges, Kovacevic, Andjelka B., Kraljic, Katarina, Kuncarayakti, Hanindyo, Kwon, Yuna, La Forgia, Fiorangela, Lahav, Ofer, Laigle, Clotilde, Lazzarin, Monica, Leaman, Ryan, Leclercq, Floriane, Lee, Khee-Gan, Lee, David, Lehnert, Matt D., Lira, Paulina, Loffredo, Eleonora, Lucatello, Sara, Magrini, Laura, Maguire, Kate, Mahler, Guillaume, Majidi, Fatemeh Zahra, Malavasi, Nicola, Mannucci, Filippo, Marconi, Marcella, Martin, Nicolas, Marulli, Federico, Massari, Davide, Matsuno, Tadafumi, Mattheee, Jorryt, McGee, Sean, Merc, Jaroslav, Merle, Thibault, Miglio, Andrea, Migliorini, Alessandra, Minchev, Ivan, Minniti, Dante, Miret-Roig, Nuria, Ibero, Ana Monreal, Montano, Federico, Montet, Ben T., Moresco, Michele, Moretti, Chiara, Moscardini, Lauro, Moya, Andres, Mueller, Oliver, Nanayakkara, Themiya, Nicholl, Matt, Nordlander, Thomas, Onori, Francesca, Padovani, Marco, Pala, Anna Francesca, Panda, Swayamtrupta, Pandey-Pommier, Mamta, Pasquini, Luca, Pawlak, Michal, Pessi, Priscila J., Pisani, Alice, Popovic, Lukav C., Prisinzano, Loredana, Raddi, Roberto, Rainer, Monica, Rebassa-Mansergas, Alberto, Richard, Johan, Rigault, Mickael, Rocher, Antoine, Romano, Donatella, Rosati, Piero, Sacco, Germano, Sanchez-Janssen, Ruben, Sander, Andreas A. C., Sanders, Jason L., Sargent, Mark, Sarpa, Elena, Schimd, Carlo, Schipani, Pietro, Sefusatti, Emiliano, Smith, Graham P., Spina, Lorenzo, Steinmetz, Matthias, Tacchella, Sandro, Tautvaisiene, Grazina, Theissen, Christopher, Thomas, Guillaume, Ting, Yuan-Sen, Travouillon, Tony, Tresse, Laurence, Trivedi, Oem, Tsantaki, Maria, Tsedrik, Maria, Urrutia, Tanya, Valenti, Elena, Van der Swaelmen, Mathieu, Van Eck, Sophie, Verdiani, Francesco, Verdier, Aurelien, Vergani, Susanna Diana, Verhamme, Anne, Vernet, Joel, Verza, Giovanni, Viel, Matteo, Vielzeuf, Pauline, Vietri, Giustina, Vink, Jorick S., Vazquez, Carlos Viscasillas, Wang, Hai-Feng, Weilbacher, Peter M., Wendt, Martin, Wright, Nicholas, Ye, Quanzhi, Yeche, Christophe, Yu, Jiaxi, Zafar, Tayyaba, Zibetti, Stefano, Ziegler, Bodo, Zinchenko, Igor, Mainieri, Vincenzo, Anderson, Richard I., Brinchmann, Jarle, Cimatti, Andrea, Ellis, Richard S., Hill, Vanessa, Kneib, Jean-Paul, McLeod, Anna F., Opitom, Cyrielle, Roth, Martin M., Sanchez-Saez, Paula, Smiljanic, Rodolfo, Tolstoy, Eline, Bacon, Roland, Randich, Sofia, Adamo, Angela, Annibali, Francesca, Arevalo, Patricia, Audard, Marc, Barsanti, Stefania, Battaglia, Giuseppina, Aran, Amelia M. Bayo, Belfiore, Francesco, Bellazzini, Michele, Bellini, Emilio, Beltran, Maria Teresa, Berni, Leda, Bianchi, Simone, Biazzo, Katia, Bisero, Sofia, Bisogni, Susanna, Bland-Hawthorn, Joss, Blondin, Stephane, Bodensteiner, Julia, Boffin, Henri M. J., Bonito, Rosaria, Bono, Giuseppe, Bouche, Nicolas F., Bowman, Dominic, Braga, Vittorio F., Bragaglia, Angela, Branchesi, Marica, Brucalassi, Anna, Bryant, Julia J., Bryson, Ian, Busa, Innocenza, Camera, Stefano, Carbone, Carmelita, Casali, Giada, Casali, Mark, Casasola, Viviana, Castro, Norberto, Catelan, Marcio, Cavallo, Lorenzo, Chiappini, Cristina, Cioni, Maria-Rosa, Colless, Matthew, Colzi, Laura, Contarini, Sofia, Couch, Warrick, D'Ammando, Filippo, D., William d'Assignies, D'Orazi, Valentina, da Silva, Ronaldo, Dainotti, Maria Giovanna, Damiani, Francesco, Danielski, Camilla, De Cia, Annalisa, de Jong, Roelof S., Dhawan, Suhail, Dierickx, Philippe, Driver, Simon P., Dupletsa, Ulyana, Escoffier, Stephanie, Escorza, Ana, Fabrizio, Michele, Fiorentino, Giuliana, Fontana, Adriano, Fontani, Francesco, Sanchez, Daniel Forero, Franois, Patrick, Galindo-Guil, Francisco Jose, Gallazzi, Anna Rita, Galli, Daniele, Garcia, Miriam, Garcia-Rojas, Jorge, Garilli, Bianca, Grand, Robert, Guarcello, Mario Giuseppe, Hazra, Nandini, Helmi, Amina, Herrero, Artemio, Iglesias, Daniela, Ilic, Dragana, Irsic, Vid, Ivanov, Valentin D., Izzo, Luca, Jablonka, Pascale, Joachimi, Benjamin, Kakkad, Darshan, Kamann, Sebastian, Koposov, Sergey, Kordopatis, Georges, Kovacevic, Andjelka B., Kraljic, Katarina, Kuncarayakti, Hanindyo, Kwon, Yuna, La Forgia, Fiorangela, Lahav, Ofer, Laigle, Clotilde, Lazzarin, Monica, Leaman, Ryan, Leclercq, Floriane, Lee, Khee-Gan, Lee, David, Lehnert, Matt D., Lira, Paulina, Loffredo, Eleonora, Lucatello, Sara, Magrini, Laura, Maguire, Kate, Mahler, Guillaume, Majidi, Fatemeh Zahra, Malavasi, Nicola, Mannucci, Filippo, Marconi, Marcella, Martin, Nicolas, Marulli, Federico, Massari, Davide, Matsuno, Tadafumi, Mattheee, Jorryt, McGee, Sean, Merc, Jaroslav, Merle, Thibault, Miglio, Andrea, Migliorini, Alessandra, Minchev, Ivan, Minniti, Dante, Miret-Roig, Nuria, Ibero, Ana Monreal, Montano, Federico, Montet, Ben T., Moresco, Michele, Moretti, Chiara, Moscardini, Lauro, Moya, Andres, Mueller, Oliver, Nanayakkara, Themiya, Nicholl, Matt, Nordlander, Thomas, Onori, Francesca, Padovani, Marco, Pala, Anna Francesca, Panda, Swayamtrupta, Pandey-Pommier, Mamta, Pasquini, Luca, Pawlak, Michal, Pessi, Priscila J., Pisani, Alice, Popovic, Lukav C., Prisinzano, Loredana, Raddi, Roberto, Rainer, Monica, Rebassa-Mansergas, Alberto, Richard, Johan, Rigault, Mickael, Rocher, Antoine, Romano, Donatella, Rosati, Piero, Sacco, Germano, Sanchez-Janssen, Ruben, Sander, Andreas A. C., Sanders, Jason L., Sargent, Mark, Sarpa, Elena, Schimd, Carlo, Schipani, Pietro, Sefusatti, Emiliano, Smith, Graham P., Spina, Lorenzo, Steinmetz, Matthias, Tacchella, Sandro, Tautvaisiene, Grazina, Theissen, Christopher, Thomas, Guillaume, Ting, Yuan-Sen, Travouillon, Tony, Tresse, Laurence, Trivedi, Oem, Tsantaki, Maria, Tsedrik, Maria, Urrutia, Tanya, Valenti, Elena, Van der Swaelmen, Mathieu, Van Eck, Sophie, Verdiani, Francesco, Verdier, Aurelien, Vergani, Susanna Diana, Verhamme, Anne, Vernet, Joel, Verza, Giovanni, Viel, Matteo, Vielzeuf, Pauline, Vietri, Giustina, Vink, Jorick S., Vazquez, Carlos Viscasillas, Wang, Hai-Feng, Weilbacher, Peter M., Wendt, Martin, Wright, Nicholas, Ye, Quanzhi, Yeche, Christophe, Yu, Jiaxi, Zafar, Tayyaba, Zibetti, Stefano, Ziegler, Bodo, and Zinchenko, Igor
Abstract: The Wide-field Spectroscopic Telescope (WST) is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys. This white paper summarises the initial concept as well as the corresponding science cases. WST will feature simultaneous operation of a large field-of-view (3 sq. degree), a high multiplex (20,000) multi-object spectrograph (MOS) and a giant 3x3 sq. arcmin integral field spectrograph (IFS). In scientific capability these requirements place WST far ahead of existing and planned facilities. Given the current investment in deep imaging surveys and noting the diagnostic power of spectroscopy, WST will fill a crucial gap in astronomical capability and work synergistically with future ground and space-based facilities. This white paper shows that WST can address outstanding scientific questions in the areas of cosmology; galaxy assembly, evolution, and enrichment, including our own Milky Way; origin of stars and planets; time domain and multi-messenger astrophysics. WST's uniquely rich dataset will deliver unforeseen discoveries in many of these areas. The WST Science Team (already including more than 500 scientists worldwide) is open to the all astronomical community. To register in the WST Science Team please visit https://www.wstelescope.com/for-scientists/participate, Comment: 194 pages, 66 figures. Comments are welcome (wstelescope@gmail.com)
Published: 2024

11. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Author: Jin, S, Trager, S, Dalton, G, Aguerri, J, Drew, J, Falcón-Barroso, J, Gänsicke, B, Hill, V, Iovino, A, Pieri, M, Poggianti, B, Smith, D, Vallenari, A, Abrams, D, Aguado, D, Antoja, T, Aragón-Salamanca, A, Ascasibar, Y, Babusiaux, C, Balcells, M, Barrena, R, Battaglia, G, Belokurov, V, Bensby, T, Bonifacio, P, Bragaglia, A, Carrasco, E, Carrera, R, Cornwell, D, Domínguez-Palmero, L, Duncan, K, Famaey, B, Fari na, C, Gonzalez, O, Guest, S, Hatch, N, Hess, K, Hoskin, M, Irwin, M, Knapen, J, Koposov, S, Kuchner, U, Laigle, C, Lewis, J, Longhetti, M, Lucatello, S, Méndez-Abreu, J, Mercurio, A, Molaeinezhad, A, Monguió, M, Morrison, S, Murphy, D, de Arriba, L, Pérez, I, Pérez-Ràfols, I, Picó, S, Raddi, R, Romero-Gómez, M, Royer, F, Siebert, A, Seabroke, G, Som, D, Terrett, D, Thomas, G, Wesson, R, Worley, C, Alfaro, E, Prieto, C, Alonso-Santiago, J, Amos, N, Ashley, R, Balaguer-Nú nez, L, Balbinot, E, Bellazzini, M, Benn, C, Berlanas, S, Bernard, E, Best, P, Bettoni, D, Bianco, A, Bishop, G, Blomqvist, M, Boeche, C, Bolzonella, M, Bonoli, S, Bosma, A, Britavskiy, N, Busarello, G, Caffau, E, Cantat-Gaudin, T, Castro-Ginard, A, Couto, G, Carbajo-Hijarrubia, J, Carter, D, Casamiquela, L, Conrado, A, Corcho-Caballero, P, Costantin, L, Deason, A, de Burgos, A, De Grandi, S, Di Matteo, P, Domínguez-Gómez, J, Dorda, R, Drake, A, Dutta, R, Erkal, D, Feltzing, S, Ferré-Mateu, A, Feuillet, D, Figueras, F, Fossati, M, Franciosini, E, Frasca, A, Fumagalli, M, Gallazzi, A, García-Benito, R, Fusillo, N, Gebran, M, Gilbert, J, Gledhill, T, Delgado, R, Greimel, R, Guarcello, M, Guerra, J, Gullieuszik, M, Haines, C, Hardcastle, M, Harris, A, Haywood, M, Helmi, A, Hernandez, N, Herrero, A, Hughes, S, Irsic, V, Jablonka, P, Jarvis, M, Jordi, C, Kondapally, R, Kordopatis, G, Krogager, J, Barbera, F, Lam, M, Larsen, S, Lemasle, B, Lewis, I, Lhomé, E, Lind, K, Lodi, M, Longobardi, A, Lonoce, I, Magrini, L, Apellániz, J, Marchal, O, Marco, A, Martin, N, Matsuno, T, Maurogordato, S, Merluzzi, P, Miralda-Escudé, J, Molinari, E, Monari, G, Morelli, L, Mottram, C, Naylor, T, Negueruela, I, Onorbe, J, Pancino, E, Peirani, S, Peletier, R, Pozzetti, L, Rainer, M, Ramos, P, Read, S, Rossi, E, Röttgering, H, Rubi no-Martín, J, Montes, J, Juan, J, Sanna, N, Schallig, E, Schiavon, R, Schultheis, M, Serra, P, Shimwell, T, Simón-Díaz, S, Smith, R, Sordo, R, Sorini, D, Soubiran, C, Starkenburg, E, Steele, I, Stott, J, Stuik, R, Tolstoy, E, Tortora, C, Tsantaki, M, Van der Swaelmen, M, van Weeren, R, Vergani, D, Verheijen, M, Verro, K, Vink, J, Vioque, M, Walcher, C, Walton, N, Wegg, C, Weijmans, A, Williams, W, Wilson, A, Wright, N, Xylakis-Dornbusch, T, Youakim, K, Zibetti, S, Zurita, C, Jin, Shoko, Trager, Scott C, Dalton, Gavin B, Aguerri, J Alfonso L, Drew, J E, Falcón-Barroso, Jesús, Gänsicke, Boris T, Hill, Vanessa, Iovino, Angela, Pieri, Matthew M, Poggianti, Bianca M, Smith, D J B, Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S, Antoja, Teresa, Aragón-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J, Domínguez-Palmero, Lilian, Duncan, Kenneth J, Famaey, Benoit, Fari na, Cecilia, Gonzalez, Oscar A, Guest, Steve, Hatch, Nina A, Hess, Kelley M, Hoskin, Matthew J, Irwin, Mike, Knapen, Johan H, Koposov, Sergey E, Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Méndez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguió, Maria, Morrison, Sean, Murphy, David N A, de Arriba, Luis Peralta, Pérez, Isabel, Pérez-Ràfols, Ignasi, Picó, Sergio, Raddi, Roberto, Romero-Gómez, Mercè, Royer, Frédéric, Siebert, Arnaud, Seabroke, George M, Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C Clare, Alfaro, Emilio J, Prieto, Carlos Allende, Alonso-Santiago, Javier, Amos, Nicholas J, Ashley, Richard P, Balaguer-Nú nez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R, Berlanas, Sara R, Bernard, Edouard J, Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M, Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Domínguez-Gómez, Jesús, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferré-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, García-Benito, Rubén, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T M, Delgado, Rosa M González, Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P, Hardcastle, Martin J, Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J, Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, Barbera, Francesco La, Lam, Man I, Larsen, Søren S, Lemasle, Bertrand, Lewis, Ian J, Lhomé, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Apellániz, Jesús Maíz, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F, Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escudé, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J, Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sébastien, Peletier, Reynier F, Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C, Rossi, Elena Maria, Röttgering, Huub J A, Rubi no-Martín, Jose Alberto, Montes, Jose Sabater, Juan, José San, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P, Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W, Simón-Díaz, Sergio, Smith, Russell J, Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A, Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J, Vergani, Daniela, Verheijen, Marc A W, Verro, Kristiina, Vink, Jorick S, Vioque, Miguel, Walcher, C Jakob, Walton, Nicholas A, Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L, Wilson, Andrew J, Wright, Nicholas J, Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, Zurita, Cristina, Jin, S, Trager, S, Dalton, G, Aguerri, J, Drew, J, Falcón-Barroso, J, Gänsicke, B, Hill, V, Iovino, A, Pieri, M, Poggianti, B, Smith, D, Vallenari, A, Abrams, D, Aguado, D, Antoja, T, Aragón-Salamanca, A, Ascasibar, Y, Babusiaux, C, Balcells, M, Barrena, R, Battaglia, G, Belokurov, V, Bensby, T, Bonifacio, P, Bragaglia, A, Carrasco, E, Carrera, R, Cornwell, D, Domínguez-Palmero, L, Duncan, K, Famaey, B, Fari na, C, Gonzalez, O, Guest, S, Hatch, N, Hess, K, Hoskin, M, Irwin, M, Knapen, J, Koposov, S, Kuchner, U, Laigle, C, Lewis, J, Longhetti, M, Lucatello, S, Méndez-Abreu, J, Mercurio, A, Molaeinezhad, A, Monguió, M, Morrison, S, Murphy, D, de Arriba, L, Pérez, I, Pérez-Ràfols, I, Picó, S, Raddi, R, Romero-Gómez, M, Royer, F, Siebert, A, Seabroke, G, Som, D, Terrett, D, Thomas, G, Wesson, R, Worley, C, Alfaro, E, Prieto, C, Alonso-Santiago, J, Amos, N, Ashley, R, Balaguer-Nú nez, L, Balbinot, E, Bellazzini, M, Benn, C, Berlanas, S, Bernard, E, Best, P, Bettoni, D, Bianco, A, Bishop, G, Blomqvist, M, Boeche, C, Bolzonella, M, Bonoli, S, Bosma, A, Britavskiy, N, Busarello, G, Caffau, E, Cantat-Gaudin, T, Castro-Ginard, A, Couto, G, Carbajo-Hijarrubia, J, Carter, D, Casamiquela, L, Conrado, A, Corcho-Caballero, P, Costantin, L, Deason, A, de Burgos, A, De Grandi, S, Di Matteo, P, Domínguez-Gómez, J, Dorda, R, Drake, A, Dutta, R, Erkal, D, Feltzing, S, Ferré-Mateu, A, Feuillet, D, Figueras, F, Fossati, M, Franciosini, E, Frasca, A, Fumagalli, M, Gallazzi, A, García-Benito, R, Fusillo, N, Gebran, M, Gilbert, J, Gledhill, T, Delgado, R, Greimel, R, Guarcello, M, Guerra, J, Gullieuszik, M, Haines, C, Hardcastle, M, Harris, A, Haywood, M, Helmi, A, Hernandez, N, Herrero, A, Hughes, S, Irsic, V, Jablonka, P, Jarvis, M, Jordi, C, Kondapally, R, Kordopatis, G, Krogager, J, Barbera, F, Lam, M, Larsen, S, Lemasle, B, Lewis, I, Lhomé, E, Lind, K, Lodi, M, Longobardi, A, Lonoce, I, Magrini, L, Apellániz, J, Marchal, O, Marco, A, Martin, N, Matsuno, T, Maurogordato, S, Merluzzi, P, Miralda-Escudé, J, Molinari, E, Monari, G, Morelli, L, Mottram, C, Naylor, T, Negueruela, I, Onorbe, J, Pancino, E, Peirani, S, Peletier, R, Pozzetti, L, Rainer, M, Ramos, P, Read, S, Rossi, E, Röttgering, H, Rubi no-Martín, J, Montes, J, Juan, J, Sanna, N, Schallig, E, Schiavon, R, Schultheis, M, Serra, P, Shimwell, T, Simón-Díaz, S, Smith, R, Sordo, R, Sorini, D, Soubiran, C, Starkenburg, E, Steele, I, Stott, J, Stuik, R, Tolstoy, E, Tortora, C, Tsantaki, M, Van der Swaelmen, M, van Weeren, R, Vergani, D, Verheijen, M, Verro, K, Vink, J, Vioque, M, Walcher, C, Walton, N, Wegg, C, Weijmans, A, Williams, W, Wilson, A, Wright, N, Xylakis-Dornbusch, T, Youakim, K, Zibetti, S, Zurita, C, Jin, Shoko, Trager, Scott C, Dalton, Gavin B, Aguerri, J Alfonso L, Drew, J E, Falcón-Barroso, Jesús, Gänsicke, Boris T, Hill, Vanessa, Iovino, Angela, Pieri, Matthew M, Poggianti, Bianca M, Smith, D J B, Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S, Antoja, Teresa, Aragón-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J, Domínguez-Palmero, Lilian, Duncan, Kenneth J, Famaey, Benoit, Fari na, Cecilia, Gonzalez, Oscar A, Guest, Steve, Hatch, Nina A, Hess, Kelley M, Hoskin, Matthew J, Irwin, Mike, Knapen, Johan H, Koposov, Sergey E, Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Méndez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguió, Maria, Morrison, Sean, Murphy, David N A, de Arriba, Luis Peralta, Pérez, Isabel, Pérez-Ràfols, Ignasi, Picó, Sergio, Raddi, Roberto, Romero-Gómez, Mercè, Royer, Frédéric, Siebert, Arnaud, Seabroke, George M, Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C Clare, Alfaro, Emilio J, Prieto, Carlos Allende, Alonso-Santiago, Javier, Amos, Nicholas J, Ashley, Richard P, Balaguer-Nú nez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R, Berlanas, Sara R, Bernard, Edouard J, Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M, Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Domínguez-Gómez, Jesús, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferré-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossati, Matteo, Franciosini, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, García-Benito, Rubén, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T M, Delgado, Rosa M González, Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P, Hardcastle, Martin J, Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J, Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, Barbera, Francesco La, Lam, Man I, Larsen, Søren S, Lemasle, Bertrand, Lewis, Ian J, Lhomé, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrini, Laura, Apellániz, Jesús Maíz, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F, Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escudé, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J, Naylor, Tim, Negueruela, Ignacio, Onorbe, Jose, Pancino, Elena, Peirani, Sébastien, Peletier, Reynier F, Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C, Rossi, Elena Maria, Röttgering, Huub J A, Rubi no-Martín, Jose Alberto, Montes, Jose Sabater, Juan, José San, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P, Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W, Simón-Díaz, Sergio, Smith, Russell J, Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A, Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J, Vergani, Daniela, Verheijen, Marc A W, Verro, Kristiina, Vink, Jorick S, Vioque, Miguel, Walcher, C Jakob, Walton, Nicholas A, Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L, Wilson, Andrew J, Wright, Nicholas J, Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, and Zurita, Cristina
Abstract: WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, saw first light in late 2022. WEAVE comprises a new 2-deg field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable ‘mini’ integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366–959 nm at R ∼ 5000, or two shorter ranges at R ∼ 20 000. After summarizing the design and implementation of WEAVE and its data systems, we present the organization, science drivers, and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy’s origins by completing Gaia’s phase-space information, providing metallicities to its limiting magnitude for ∼3 million stars and detailed abundances for ∼1.5 million brighter field and open-cluster stars; (ii) survey ∼0.4 million Galactic-plane OBA stars, young stellar objects, and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey ∼400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionized gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in ∼25 000 field galaxies at 0.3 ≲ z ≲ 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; and (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.
Published: 2024

12. EMPRESS. XII. Statistics on the Dynamics and Gas Mass Fraction of Extremely Metal-poor Galaxies

Author: Xu, Yi, Ouchi, Masami, Isobe, Yuki, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, Zhang, Yechi, Xu, Yi, Ouchi, Masami, Isobe, Yuki, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, and Zhang, Yechi
Published: 2024

13. EMPRESS. XII. Statistics on the Dynamics and Gas Mass Fraction of Extremely Metal-poor Galaxies

Author: Xu, Yi, Ouchi, Masami, Isobe, Yuki, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, Zhang, Yechi, Xu, Yi, Ouchi, Masami, Isobe, Yuki, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, and Zhang, Yechi
Published: 2024

14. Accelerating hyperbolic t-SNE

Author: Skrodzki, Martin, van Geffen, Hunter, Chaves-de-Plaza, Nicolas F., Höllt, Thomas, Eisemann, Elmar, Hildebrandt, Klaus, Skrodzki, Martin, van Geffen, Hunter, Chaves-de-Plaza, Nicolas F., Höllt, Thomas, Eisemann, Elmar, and Hildebrandt, Klaus
Abstract: The need to understand the structure of hierarchical or high-dimensional data is present in a variety of fields. Hyperbolic spaces have proven to be an important tool for embedding computations and analysis tasks as their non-linear nature lends itself well to tree or graph data. Subsequently, they have also been used in the visualization of high-dimensional data, where they exhibit increased embedding performance. However, none of the existing dimensionality reduction methods for embedding into hyperbolic spaces scale well with the size of the input data. That is because the embeddings are computed via iterative optimization schemes and the computation cost of every iteration is quadratic in the size of the input. Furthermore, due to the non-linear nature of hyperbolic spaces, Euclidean acceleration structures cannot directly be translated to the hyperbolic setting. This paper introduces the first acceleration structure for hyperbolic embeddings, building upon a polar quadtree. We compare our approach with existing methods and demonstrate that it computes embeddings of similar quality in significantly less time. Implementation and scripts for the experiments can be found at https://graphics.tudelft.nl/accelerating-hyperbolic-tsne.
Published: 2024

15. Optimizing Crop Management with Reinforcement Learning and Imitation Learning

Author: Tao, Ran, Martin, Nicolas F., Zhao, Pan, Harrison, Matthew T., Wu, Jing, Ferreira, Carla, Kalantari, Zahra, Hovakimyan, Naira, Tao, Ran, Martin, Nicolas F., Zhao, Pan, Harrison, Matthew T., Wu, Jing, Ferreira, Carla, Kalantari, Zahra, and Hovakimyan, Naira
Abstract: To increase crop yield while minimizing environmental impact, we present an intelligent crop management system that optimizes nitrogen fertilization and irrigation simultaneously via reinforcement learning (RL), imitation learning (IL), and crop simulations using DSSAT. We first use deep RL to train management policies that require a large number of state variables from the simulator as observations (denoted as full observation). We then invoke IL to train management policies that only need a limited number of variables that are measurable in the real world (denoted as partial observation) by mimicking the actions of the RL-trained policies under full observation. Simulation experiments using maize in Florida demonstrate that our trained policies under both full and partial observations achieve better outcomes than a baseline policy. Most importantly, the IL-trained management policies are directly deployable in the real world as they use readily available information., QC 20231010
Published: 2023

16. Zeolitization of a devitrified high-silica rhyolitic tuff producing dachiardite: A comparison of hydrothermal experiments with the corresponding reaction progress modeling

Author: Knauss, Kevin G, Knauss, Kevin G, Saldi, Giuseppe D, Spycher, Nicolas F, Knauss, Kevin G, Knauss, Kevin G, Saldi, Giuseppe D, and Spycher, Nicolas F
Abstract: We have investigated the hydrothermal alteration of polished wafers of tuff reacted with dilute groundwater at 90 °C, 150 °C and 250 °C for time periods ranging from 2 months to nearly 1 year. The polished rock wafer provided a convenient surface upon which to grow secondary minerals. Reaction product minerals were identified and analyzed at the end of each experiment and, along with the evolving fluid chemistry, were compared to computational results from corresponding reaction progress models. At 250 °C after a few months the run products in the experiment were dominantly the mordenite group zeolite minerals: dachiardite (a Ca-rich variety) and mordenite, itself. At 150 °C after a few months of reaction only minor amounts of clay were produced, but after 1 year of reaction at this temperature both mordenite group zeolites were again present. At this lower temperature the total amount of run products was much smaller. At 90 °C no run products could be seen at all, even after 1 year of reaction. The reaction progress modeling results for reaction products were in good relative agreement with the experimental results. The higher the temperature, and the greater the extent of reaction, the better the fluid phase modeling results agreed with the actual experimental results. At 250 °C the agreement was good for nearly all elements. At 150 °C agreement for pH, SiO2, Na and K were good, but less good for Al, Mg and Ca, especially after short reaction times. At 90 °C agreement for pH, SiO2 and Na was reasonable, but not as good for the other elements, and all modeling results for short reaction times did not match experimental results as well as the longer time results. This study demonstrates that reaction progress modeling provides a powerful tool for predicting hydrothermal rock-water interactions, with results expected to improve, as more and better quality thermodynamic and kinetic data become available and as process-oriented simulators incorporate better and more co
Published: 2023

17. Implementation of Delineation Error Detection Systems in Clinical Practice: Do AI-Supported Optimization and Human Preferences Meet?

Author: Chaves-de-Plaza, Nicolas F. (author) and Chaves-de-Plaza, Nicolas F. (author)
Abstract: Computer Graphics and Visualisation
Published: 2023

18. EMPRESS. IX. Extremely Metal-poor Galaxies are Very Gas-rich Dispersion-dominated Systems:Will the James Webb Space Telescope Witness Gaseous Turbulent High-z Primordial Galaxies?

Author: Isobe, Yuki, Ouchi, Masami, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Xu, Yi, Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, Zhang, Yechi, Isobe, Yuki, Ouchi, Masami, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Xu, Yi, Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, and Zhang, Yechi
Published: 2023

19. Probing the early Milky Way with GHOST spectra of an extremely metal-poor star in the Galactic disk

Author: Dovgal, Anya, Venn, Kim A., Sestito, Federico, Hayes, Christian R., McConnachie, Alan W., Navarro, Julio F., Placco, Vinicius M., Starkenburg, Else, Martin, Nicolas F., Pazder, John S., Chiboucas, Kristin, Deibert, Emily, Gamen, Roberto, Heo, Jeong-Eun, Kalari, Venu M., Martioli, Eder, Xu, Siyi, Diaz, Ruben, Gomez-Jiminez, Manuel, Henderson, David, Prado, Pablo, Quiroz, Carlos, Robertson, J. Gordon, Ruiz-Carmona, Roque, Simpson, Chris, Urrutia, Cristian, Waller, Fletcher, Berg, Trsytyn, Burley, Gregory, Hartman, Zachary, Ireland, Michael, Margheim, Steve, Perez, Gabriel, Thomas-Osip, Joanna, Dovgal, Anya, Venn, Kim A., Sestito, Federico, Hayes, Christian R., McConnachie, Alan W., Navarro, Julio F., Placco, Vinicius M., Starkenburg, Else, Martin, Nicolas F., Pazder, John S., Chiboucas, Kristin, Deibert, Emily, Gamen, Roberto, Heo, Jeong-Eun, Kalari, Venu M., Martioli, Eder, Xu, Siyi, Diaz, Ruben, Gomez-Jiminez, Manuel, Henderson, David, Prado, Pablo, Quiroz, Carlos, Robertson, J. Gordon, Ruiz-Carmona, Roque, Simpson, Chris, Urrutia, Cristian, Waller, Fletcher, Berg, Trsytyn, Burley, Gregory, Hartman, Zachary, Ireland, Michael, Margheim, Steve, Perez, Gabriel, and Thomas-Osip, Joanna
Abstract: Pristine_183.6849+04.8619 (P1836849) is an extremely metal-poor ([Fe/H]$=-3.3\pm0.1$) star on a prograde orbit confined to the Galactic disk. Such stars are rare and may have their origins in protogalactic fragments that formed the early Milky Way, in low mass satellites accreted later, or forming in situ in the Galactic plane. Here we present a chemo-dynamical analysis of the spectral features between $3700-11000$\r{A} from a high-resolution spectrum taken during Science Verification of the new Gemini High-resolution Optical SpecTrograph (GHOST). Spectral features for many chemical elements are analysed (Mg, Al, Si, Ca, Sc, Ti, Cr, Mn, Fe, Ni), and valuable upper limits are determined for others (C, Na, Sr, Ba). This main sequence star exhibits several rare chemical signatures, including (i) extremely low metallicity for a star in the Galactic disk, (ii) very low abundances of the light $\alpha$-elements (Na, Mg, Si) compared to other metal-poor stars, and (iii) unusually large abundances of Cr and Mn, where [Cr, Mn/Fe]$_{\rm NLTE}>+0.5$. A comparison to theoretical yields from supernova models suggests that two low mass Population III objects (one 10 M$_\odot$ supernova and one 17 M$_\odot$ hypernova) can reproduce the abundance pattern well (reduced $\chi^2<1$). When this star is compared to other extremely metal-poor stars on quasi-circular, prograde planar orbits, differences in both chemistry and kinematics imply there is little evidence for a common origin. The unique chemistry of P1836849 is discussed in terms of the earliest stages in the formation of the Milky Way., Comment: 16 pages, 10 figures, 6 tables. Accepted by MNRAS November 22; Revisions include comparisons to more EMP stars, results unchanged
Published: 2023
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20. GHOST Commissioning Science Results II: a very metal-poor star witnessing the early Galactic assembly

Author: Sestito, Federico, Hayes, Christian R., Venn, Kim A., Jensen, Jaclyn, McConnachie, Alan W., Pazder, John, Waller, Fletcher, Arentsen, Anke, Jablonka, Pascale, Martin, Nicolas F., Matsuno, Tadafumi, Navarro, Julio F., Starkenburg, Else, Vitali, Sara, Bassett, John, Berg, Trystyn A. M., Diaz, Ruben, Edgar, Michael L., Firpo, Veronica, Gomez-Jimenez, Manuel, Kalari, Venu, Lambert, Sam, Lawrence, Jon, Robertson, Gordon, Ruiz-Carmona, Roque, Salinas, Ricardo, Sebo, Kim M., Venkatesan, Sudharshan, Sestito, Federico, Hayes, Christian R., Venn, Kim A., Jensen, Jaclyn, McConnachie, Alan W., Pazder, John, Waller, Fletcher, Arentsen, Anke, Jablonka, Pascale, Martin, Nicolas F., Matsuno, Tadafumi, Navarro, Julio F., Starkenburg, Else, Vitali, Sara, Bassett, John, Berg, Trystyn A. M., Diaz, Ruben, Edgar, Michael L., Firpo, Veronica, Gomez-Jimenez, Manuel, Kalari, Venu, Lambert, Sam, Lawrence, Jon, Robertson, Gordon, Ruiz-Carmona, Roque, Salinas, Ricardo, Sebo, Kim M., and Venkatesan, Sudharshan
Abstract: This study focuses on Pristine$\_180956.78$$-$$294759.8$ (hereafter P180956, $[Fe/H] =-1.95\pm0.02$), a star selected from the Pristine Inner Galaxy Survey (PIGS), and followed-up with the recently commissioned Gemini High-resolution Optical SpecTrograph (GHOST) at the Gemini South telescope. The GHOST spectrograph's high efficiency in the blue spectral region ($3700-4800$~\AA) enables the detection of elemental tracers of early supernovae (\eg Al, Mn, Sr, Eu). The star exhibits chemical signatures resembling those found in ultra-faint dwarf systems, characterised by very low abundances of neutron-capture elements (Sr, Ba, Eu), which are uncommon among stars in the Milky Way halo. Our analysis suggests that P180956 bears the chemical imprints of a small number (2 or 4) of low-mass hypernovae ($\sim10-15 M_{\odot}$), which are needed to mostly reproduce the abundance pattern of the light-elements (\eg [Si, Ti/Mg, Ca] $\sim0.6$), and one fast-rotating intermediate-mass supernova ($\sim300\kms$, $\sim80-120 M_{\odot}$), which is the main channel contributing to the high [Sr/Ba] ($\sim +1.2$). The small pericentric ($\sim0.7$ kpc) and apocentric ($\sim13$ kpc) distances and its orbit confined to the plane ($\lesssim 2$ kpc), indicate that this star was likely accreted during the early Galactic assembly phase. Its chemo-dynamical properties suggest that P180956 formed in a system similar to an ultra-faint dwarf galaxy accreted either alone, as one of the low-mass building blocks of the proto-Galaxy, or as a satellite of Gaia-Sausage-Enceladus. The combination of Gemini's large aperture with GHOST's high efficiency and broad spectral coverage makes this new spectrograph one of the leading instruments for near-field cosmology investigations., Comment: Accepted version, minor editing. New figure showing Sr and Ba lines. Section 4.7 revised
Published: 2023

21. Gaia's brightest very metal-poor (VMP) stars: A metallicity catalogue of a thousand VMP stars from Gaia RVS spectra

Author: Viswanathan, Akshara, Starkenburg, Else, Matsuno, Tadafumi, Venn, Kim A., Martin, Nicolas F., Longeard, Nicolas, Ardern-Arentsen, Anke, Carlberg, Raymond G., Fabbro, Sebastien, Kordopatis, Georges, Montelius, Martin, Sestito, Federico, Yuan, Zhen, Viswanathan, Akshara, Starkenburg, Else, Matsuno, Tadafumi, Venn, Kim A., Martin, Nicolas F., Longeard, Nicolas, Ardern-Arentsen, Anke, Carlberg, Raymond G., Fabbro, Sebastien, Kordopatis, Georges, Montelius, Martin, Sestito, Federico, and Yuan, Zhen
Abstract: Context. Gaia DR3 has offered the scientific community a remarkable dataset of approximately one million spectra acquired with the Radial Velocity Spectrometer (RVS) in the Calcium II triplet region, that is well-suited to identify very metal-poor (VMP) stars. However, over 40% of these spectra have no released parameters by Gaia's GSP Spec pipeline in the domain of VMP stars, whereas VMP stars are key tracers of early Galactic evolution. Aims. We aim to provide spectroscopic metallicities for VMP stars using Gaia RVS spectra, thereby producing a catalogue of bright VMP stars distributed over the full sky that can serve as the basis to study early chemical evolution throughout the Galaxy. Methods. We select VMP stars using photometric metallicities from the literature and analyse the Gaia RVS spectra to infer spectroscopic metallicities for these stars. Results. The inferred metallicities agree very well with literature high-resolution metallicities with a median systematic offset of 0.1 dex and standard deviation of $\sim$0.15 dex. The purity of this sample in the VMP regime is $\sim$80% with outliers representing a mere $\sim$3%. Conclusions. We make available an all-sky catalogue of $\sim$1500 stars with reliable spectroscopic metallicities down to [Fe/H]$\sim$-4.0, of which $\sim$1000 are VMP stars. More than 75% of these stars have either no metallicity value in the literature to date or are flagged to be unreliable in their literature metallicity estimates. This catalogue of bright (G<13) VMP stars is three times larger than the current sample of well-studied VMP stars in the literature in this magnitude range, making it ideal for high-resolution spectroscopic follow-up and to study the properties of VMP stars in different parts of our Galaxy., Comment: Submitted to A&A. 11 pages, 4 pages appendix, 5 figures. Catalogue is made available public here: https://astroakshara.github.io/rvs-paper/Gaia-RVS-VMP-catalogue-AV23b-vSep23.csv Feel free to use it to do amazing science with the amazing data Gaia has given us
Published: 2023
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22. The Pristine survey -- XXIII. Data Release 1 and an all-sky metallicity catalogue based on Gaia DR3 BP/RP spectro-photometry

Author: Martin, Nicolas F., Starkenburg, Else, Yuan, Zhen, Fouesneau, Morgan, Arentsen, Anke, De Angeli, Francesca, Gran, Felipe, Montelius, Martin, Andrae, René, Bellazzini, Michele, Montegriffo, Paolo, Esselink, Anna F., Zhang, Hanyuan, Venn, Kim A., Viswanathan, Akshara, Aguado, David S., Battaglia, Giuseppina, Bayer, Manuel, Bonifacio, Piercarlo, Caffau, Elisabetta, Côté, Patrick, Carlberg, Raymond, Fabbro, Sébastien, Alvar, Emma Fernández, Hernández, Jonay I. González, de La Vernhe, Isaure González Rivera, Hill, Vanessa, Ibata, Rodrigo A., Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, McConnachie, Alan W., Navarrete, Camila, Navarro, Julio, Recio-Blanco, Alejandra, Janssen, Rubén Sánchez, Sestito, Federico, Thomas, Guillaume F., Vitali, Sara, Youakim, Kristopher, Martin, Nicolas F., Starkenburg, Else, Yuan, Zhen, Fouesneau, Morgan, Arentsen, Anke, De Angeli, Francesca, Gran, Felipe, Montelius, Martin, Andrae, René, Bellazzini, Michele, Montegriffo, Paolo, Esselink, Anna F., Zhang, Hanyuan, Venn, Kim A., Viswanathan, Akshara, Aguado, David S., Battaglia, Giuseppina, Bayer, Manuel, Bonifacio, Piercarlo, Caffau, Elisabetta, Côté, Patrick, Carlberg, Raymond, Fabbro, Sébastien, Alvar, Emma Fernández, Hernández, Jonay I. González, de La Vernhe, Isaure González Rivera, Hill, Vanessa, Ibata, Rodrigo A., Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, McConnachie, Alan W., Navarrete, Camila, Navarro, Julio, Recio-Blanco, Alejandra, Janssen, Rubén Sánchez, Sestito, Federico, Thomas, Guillaume F., Vitali, Sara, and Youakim, Kristopher
Abstract: We use the spectro-photometric information of ~219 million stars from Gaia's DR3 to calculate synthetic, narrow-band, metallicity-sensitive CaHK magnitudes that mimic the observations of the Pristine survey, a survey of photometric metallicities of Milky Way stars that has been mapping more than 6,500 deg^2 of the northern sky with the CFHT since 2015. These synthetic magnitudes are used for an absolute re-calibration of the deeper Pristine photometry and, combined with broadband Gaia information, synthetic and Pristine CaHK magnitudes are used to estimate photometric metallicities over the whole sky. The resulting metallicity catalogue is accurate down to [Fe/H]~-3.5 and is particularly suited for the exploration of the metal-poor Milky Way ([Fe/H]<-1.0). We make available here the catalogue of synthetic CaHK_syn magnitudes for all stars with BP/RP information in Gaia DR3, as well as an associated catalogue of more than ~30 million photometric metallicities for high S/N FGK stars. This paper further provides the first public DR of the Pristine catalogue in the form of higher quality recalibrated Pristine CaHK magnitudes and photometric metallicities for all stars in common with the BP/RP information in Gaia DR3. We demonstrate that, when available, the much deeper Pristine data greatly enhances the quality of the derived metallicities, in particular at the faint end of the catalogue (G_BP>16). Combined, both catalogues include more than 2 million metal-poor star candidates as well as more than 200,000 and ~8,000 very and extremely metal-poor candidates. Finally, we show that these metallicity catalogues can be used efficiently, among other applications, for Galactic archaeology, to hunt for the most metal-poor stars, and to study how the structure of the Milky Way varies with metallicity, from the flat distribution of disk stars to the spheroid-shaped metal-poor halo. (Shortened), Comment: 30 pages, 24 figures, submitted to A&A. First two authors are co-first author. The CaHK photometry catalogue and the two photometric metallicity catalogues are available, before acceptance, as large compressed csv files at: https://seafile.unistra.fr/d/ee0c0f05719d4368bcbb
Published: 2023

23. Large-scale excess HI absorption around $z\approx4$ galaxies detected in a background galaxy spectrum in the MUSE eXtremely Deep Field

Author: Matthee, Jorryt, Golling, Christopher, Mackenzie, Ruari, Pezzulli, Gabriele, Lilly, Simon, Schaye, Joop, Bacon, Roland, Kusakabe, Haruka, Urrutia, Tanya, Boogaard, Leindert, Brinchmann, Jarle, Maseda, Michael V., Garel, Thibault, Bouché, Nicolas F., Wisotzki, Lutz, Matthee, Jorryt, Golling, Christopher, Mackenzie, Ruari, Pezzulli, Gabriele, Lilly, Simon, Schaye, Joop, Bacon, Roland, Kusakabe, Haruka, Urrutia, Tanya, Boogaard, Leindert, Brinchmann, Jarle, Maseda, Michael V., Garel, Thibault, Bouché, Nicolas F., and Wisotzki, Lutz
Abstract: Observationally mapping the relation between galaxies and the intergalactic medium (IGM) is of key interest for studies of cosmic reionization. Diffuse hydrogen gas has typically been observed in HI Lyman-$\alpha$ (Ly$\alpha$) absorption in the spectra of bright background quasars. However, it is important to extend these measurements to background galaxies as quasars become increasingly rare at high redshift and rarely probe closely separated sight-lines. Here we use deep integral field spectroscopy in the MUSE eXtremely Deep Field to demonstrate the measurement of the Ly$\alpha$ transmission at $z\approx4$ in absorption to a background galaxy at $z=4.77$. The HI transmission is consistent with independent quasar sight-lines at similar redshifts. Exploiting the high number of spectroscopic redshifts of faint galaxies (500 between $z=4.0-4.7$ within a radius of 8 arcmin) that are tracers of the density field, we show that Ly$\alpha$ transmission is inversely correlated with galaxy density, i.e. transparent regions in the Ly$\alpha$ forest mark under-dense regions at $z\approx4$. Due to large-scale clustering, galaxies are surrounded by excess HI absorption over the cosmic mean out to 4 cMpc/h. We also find that redshifts from the peak of the Ly$\alpha$ line are typically offset from the systemic redshift by +170 km/s. This work extends results from $z\approx 2 - 3$ to higher redshifts and demonstrates the power of deep integral field spectroscopy to simultaneously measure the ionization structure of the IGM and the large-scale density field in the early Universe., Comment: Accepted for publication in MNRAS. Main text 10 pages, 9 figures. Key results in Fig 4 (Lya forest transmission in the MXDF field) and Fig 9 (transmission - galaxy distance cross-correlation)
Published: 2023

24. EMPRESS. XII. Statistics on the Dynamics and Gas Mass Fraction of Extremely-Metal Poor Galaxies

Author: Xu, Yi, Ouchi, Masami, Isobe, Yuki, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-Hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, Zhang, Yechi, Xu, Yi, Ouchi, Masami, Isobe, Yuki, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-Hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, and Zhang, Yechi
Abstract: We present demography of the dynamics and gas-mass fraction of 33 extremely metal-poor galaxies (EMPGs) with metallicities of $0.015-0.195~Z_\odot$ and low stellar masses of $10^4-10^8~M_\odot$ in the local universe. We conduct deep optical integral-field spectroscopy (IFS) for the low-mass EMPGs with the medium high resolution ($R=7500$) grism of the 8m-Subaru FOCAS IFU instrument by the EMPRESS 3D survey, and investigate H$\alpha$ emission of the EMPGs. Exploiting the resolution high enough for the low-mass galaxies, we derive gas dynamics with the H$\alpha$ lines by the fitting of 3-dimensional disk models. We obtain an average maximum rotation velocity ($v_\mathrm{rot}$) of $15\pm3~\mathrm{km~s^{-1}}$ and an average intrinsic velocity dispersion ($\sigma_0$) of $27\pm10~\mathrm{km~s^{-1}}$ for 15 spatially resolved EMPGs out of the 33 EMPGs, and find that all of the 15 EMPGs have $v_\mathrm{rot}/\sigma_0<1$ suggesting dispersion dominated systems. There is a clear decreasing trend of $v_\mathrm{rot}/\sigma_0$ with the decreasing stellar mass and metallicity. We derive the gas mass fraction ($f_\mathrm{gas}$) for all of the 33 EMPGs, and find no clear dependence on stellar mass and metallicity. These $v_\mathrm{rot}/\sigma_0$ and $f_\mathrm{gas}$ trends should be compared with young high-$z$ galaxies observed by the forthcoming JWST IFS programs to understand the physical origins of the EMPGs in the local universe., Comment: 18 pages, 9 figures, accepted for publication in ApJ
Published: 2023
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25. The PAndAS View of the Andromeda Satellite System. IV Global properties

Author: Doliva-Dolinsky, Amandine, Martin, Nicolas F., Yuan, Zhen, Savino, Alessandro, Weisz, Daniel R., Ferguson, Annette M. N., Ibata, Rodrigo A., Kim, Stacy Y., Lewis, Geraint F., McConnachie, Alan W., Thomas, Guillaume F., Doliva-Dolinsky, Amandine, Martin, Nicolas F., Yuan, Zhen, Savino, Alessandro, Weisz, Daniel R., Ferguson, Annette M. N., Ibata, Rodrigo A., Kim, Stacy Y., Lewis, Geraint F., McConnachie, Alan W., and Thomas, Guillaume F.
Abstract: We build a statistical framework to infer the global properties of the satellite system of the Andromeda galaxy (M31) from the properties of individual dwarf galaxies located in the Pan-Andromeda Archaelogical Survey (PAndAS) and the previously determined completeness of the survey. Using forward modeling, we infer the slope of the luminosity function of the satellite system, the slope of its spatial density distribution, and the size-luminosity relation followed by the dwarf galaxies. We find that the slope of the luminosity function is $\beta=-1.5\pm0.1$. Combined with the spatial density profile, it implies that, when accounting for survey incompleteness, M31 hosts $92_{-26}^{+19}$ dwarf galaxies with $M_\textrm{V}<-5.5$ and a sky-projected distance from M31 between 30 and 300kpc. We conclude that many faint or distant dwarf galaxies remain to be discovered around Andromeda, especially outside the PAndAS footprint. Finally, we use our model to test if the higher number of satellites situated in the hemisphere facing the Milky Way could be explained simply by the detection limits of dwarf galaxy searches. We rule this out at $>99.9\%$ confidence and conclude that this anisotropy is an intrinsic feature of the M31 satellite system. The statistical framework we present here is a powerful tool to robustly constrain the properties of a satellite system and compare those across hosts, especially considering the upcoming start of the Euclid or Rubin large photometric surveys that are expected to uncover a large number of dwarf galaxies in the Local Volume., Comment: Submitted to ApJ - 12 pages, 6 figures, 2 tables
Published: 2023
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26. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Author: Universidad de Alicante. Departamento de Física Aplicada, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J.E., Falcón-Barroso, Jesús, Gänsicke, B.T., Hill, V., Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Fumagalli, Michele, Boeche, Corrado, Fariña, Cecilia, Gonzalez, Oscar A., Guest, Steve, Bellazzini, M., Drake, Alyssa, Longhetti, Marcella, Herrero, Artemio, Monari, Giacomo, Carrasco, Esperanza, Dutta, Rajeshwari, Deason, Alis, Irwin, M., Sordo, R., Serra, Paolo, Lucatello, Sara, Bolzonella, Micol, Gallazzi, Anna, Peralta de Arriba, Luis, García-Benito, Rubén, Van der Swaelmen, M., Stuik, Remko, Peletier, Reynier F., Hughes, Sarah, de Burgos, Abel, Magrini, L., Ferré-Mateu, Anna, Pérez, Isabel, Carter, David, Haines, Christopher P., Som, Debopam, Lind, K., Hardcastle, Martin J., Raddi, Roberto, Weijmans, Anne-Marie, Vioque, Miguel, Schiavon, Ricardo P., Figueras, Francesca, Irsic, Vid, Bernard, Edouard J., Jablonka, Pascale, Amos, Nicholas J., Lodi, Marcello, Ascasibar, Yago, Abrams, Don Carlos, Best, Philip, Gebran, M., Lam, Man I., Bonoli, Silvia, Larsen, Søren S., Domínguez-Palmero, Lilian, Bragaglia, A., Verro, Kristiina, Longobardi, Alessia, Morelli, Lorenzo, Jarvis, Matt J., Schultheis, Mathias, Feuillet, D.K., Bosma, Albert, Haywood, Misha, Marco, Amparo, Casamiquela, L., Sabater Montes, Jose, Martin, Nicolas F., Sorini, Daniele, Cantat-Gaudin, T., Kuchner, Ulrike, Hoskin, Matthew J., Smith, D.J.B., Jordi, C., Mottram, Christopher J., Fossati, Matteo, Naylor, Tim, Dorda Laforet, Ricardo, San Juan, José, Antoja, Teresa, Vink, Jorick S., Merluzzi, Paola, Franciosini, E., Lewis, Ian J., Ramos, Pau, Gilbert, James, Read, Shaun C., Siebert, Arnaud, Picó, Sergio, Hatch, Nina A., Miralda-Escudé, Jordi, Sanna, N., Tolstoy, Eline, Negueruela, Ignacio, Vallenari, A., Gledhill, T.M., González Delgado, Rosa M., Maurogordato, Sophie, Simón Díaz, Sergio, Helmi, Amina, Wright, N., Méndez-Abreu, Jairo, Smith, Russell J., Babusiaux, Carine, Gullieuszik, Marco, Balbinot, Eduardo, Alonso-Santiago, Javier, Hernandez, Nauzet, Onorbe, Jose, Tortora, Crescenzo, Kondapally, Rohit, Tsantaki, M., Bettoni, Daniela, Pérez-Ràfols, Ignasi, Xylakis-Dornbusch, Theodora, Schallig, Ellen, Hess, Kelley M., Soubiran, C., Kordopatis, G., Röttgering, Huub J.A., Walton, N., Lhomé, Emilie, Wegg, Christopher, La Barbera, Francesco, Carbajo-Hijarrubia, Juan, Caffau, Elisabetta, Alfaro, Emilio J., Starkenburg, Else, Youakim, Kris, Aragón-Salamanca, Alfonso, Zibetti, Stefano, Marchal, Olivier, Erkal, Denis, Domínguez-Gómez, Jesús, Molinari, Emilio, van Weeren, Reinout J., Carrera, Ricardo, Pancino, E., Cornwell, Daniel J., Gentile Fusillo, Nicola, Frasca, A., Britavskiy, Nikolay, Mercurio, Amata, Zurita, Cristina, Allende Prieto, C., Balcells, Marc, Peirani, Sébastien, Williams, Wendy L., Knapen, Johan H., Rubiño-Martín, J.A., Terrett, David, Koposov, S., Rainer, Monica, Harris, Amy, Guerra, Jose, De Grandi, Sabrina, Belokurov, Vasily, Molaeinezhad, Alireza, Steele, Iain A., Monguió, María, Shimwell, Timothy W., Thomas, Guillaume, Busarello, Gianni, Lewis, J., Stott, John, Duncan, Kenneth J., Romero-Gómez, Mercè, Vergani, Daniela, Royer, Frédéric, Lemasle, Bertrand, Krogager, Jens-Kristian, Greimel, Robert, Wesson, Roger, Bianco, Andrea, Morrison, Sean, Di Matteo, Paola, Barrena, R., Verheijen, Marc A.W., Laigle, Clotilde, Ashley, Richard P., Wilson, Andrew J., Conrado, Ana M., Balaguer-Nunez, L., Feltzing, S., Walcher, C. Jakob, Matsuno, Tadafumi, Maíz Apellániz, Jesús, Battaglia, Giuseppina, Murphy, D.N.A., Bishop, Georgia, Bensby, T., Blomqvist, Michael, Aguado, David S., Corcho-Caballero, Pablo, Worley, C.C., Guarcello, Mario Giuseppe, Benn, Chris R., Bonifacio, P., Seabroke, G.M., Castro-Ginard, Alfred, Famaey, Benoit, Couto, Guilherme, Rossi, Elena Maria, Pozzetti, Lucia, Lonoce, Ilaria, Berlanas, Sara R., Costantin, Luca, Universidad de Alicante. Departamento de Física Aplicada, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J.E., Falcón-Barroso, Jesús, Gänsicke, B.T., Hill, V., Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Fumagalli, Michele, Boeche, Corrado, Fariña, Cecilia, Gonzalez, Oscar A., Guest, Steve, Bellazzini, M., Drake, Alyssa, Longhetti, Marcella, Herrero, Artemio, Monari, Giacomo, Carrasco, Esperanza, Dutta, Rajeshwari, Deason, Alis, Irwin, M., Sordo, R., Serra, Paolo, Lucatello, Sara, Bolzonella, Micol, Gallazzi, Anna, Peralta de Arriba, Luis, García-Benito, Rubén, Van der Swaelmen, M., Stuik, Remko, Peletier, Reynier F., Hughes, Sarah, de Burgos, Abel, Magrini, L., Ferré-Mateu, Anna, Pérez, Isabel, Carter, David, Haines, Christopher P., Som, Debopam, Lind, K., Hardcastle, Martin J., Raddi, Roberto, Weijmans, Anne-Marie, Vioque, Miguel, Schiavon, Ricardo P., Figueras, Francesca, Irsic, Vid, Bernard, Edouard J., Jablonka, Pascale, Amos, Nicholas J., Lodi, Marcello, Ascasibar, Yago, Abrams, Don Carlos, Best, Philip, Gebran, M., Lam, Man I., Bonoli, Silvia, Larsen, Søren S., Domínguez-Palmero, Lilian, Bragaglia, A., Verro, Kristiina, Longobardi, Alessia, Morelli, Lorenzo, Jarvis, Matt J., Schultheis, Mathias, Feuillet, D.K., Bosma, Albert, Haywood, Misha, Marco, Amparo, Casamiquela, L., Sabater Montes, Jose, Martin, Nicolas F., Sorini, Daniele, Cantat-Gaudin, T., Kuchner, Ulrike, Hoskin, Matthew J., Smith, D.J.B., Jordi, C., Mottram, Christopher J., Fossati, Matteo, Naylor, Tim, Dorda Laforet, Ricardo, San Juan, José, Antoja, Teresa, Vink, Jorick S., Merluzzi, Paola, Franciosini, E., Lewis, Ian J., Ramos, Pau, Gilbert, James, Read, Shaun C., Siebert, Arnaud, Picó, Sergio, Hatch, Nina A., Miralda-Escudé, Jordi, Sanna, N., Tolstoy, Eline, Negueruela, Ignacio, Vallenari, A., Gledhill, T.M., González Delgado, Rosa M., Maurogordato, Sophie, Simón Díaz, Sergio, Helmi, Amina, Wright, N., Méndez-Abreu, Jairo, Smith, Russell J., Babusiaux, Carine, Gullieuszik, Marco, Balbinot, Eduardo, Alonso-Santiago, Javier, Hernandez, Nauzet, Onorbe, Jose, Tortora, Crescenzo, Kondapally, Rohit, Tsantaki, M., Bettoni, Daniela, Pérez-Ràfols, Ignasi, Xylakis-Dornbusch, Theodora, Schallig, Ellen, Hess, Kelley M., Soubiran, C., Kordopatis, G., Röttgering, Huub J.A., Walton, N., Lhomé, Emilie, Wegg, Christopher, La Barbera, Francesco, Carbajo-Hijarrubia, Juan, Caffau, Elisabetta, Alfaro, Emilio J., Starkenburg, Else, Youakim, Kris, Aragón-Salamanca, Alfonso, Zibetti, Stefano, Marchal, Olivier, Erkal, Denis, Domínguez-Gómez, Jesús, Molinari, Emilio, van Weeren, Reinout J., Carrera, Ricardo, Pancino, E., Cornwell, Daniel J., Gentile Fusillo, Nicola, Frasca, A., Britavskiy, Nikolay, Mercurio, Amata, Zurita, Cristina, Allende Prieto, C., Balcells, Marc, Peirani, Sébastien, Williams, Wendy L., Knapen, Johan H., Rubiño-Martín, J.A., Terrett, David, Koposov, S., Rainer, Monica, Harris, Amy, Guerra, Jose, De Grandi, Sabrina, Belokurov, Vasily, Molaeinezhad, Alireza, Steele, Iain A., Monguió, María, Shimwell, Timothy W., Thomas, Guillaume, Busarello, Gianni, Lewis, J., Stott, John, Duncan, Kenneth J., Romero-Gómez, Mercè, Vergani, Daniela, Royer, Frédéric, Lemasle, Bertrand, Krogager, Jens-Kristian, Greimel, Robert, Wesson, Roger, Bianco, Andrea, Morrison, Sean, Di Matteo, Paola, Barrena, R., Verheijen, Marc A.W., Laigle, Clotilde, Ashley, Richard P., Wilson, Andrew J., Conrado, Ana M., Balaguer-Nunez, L., Feltzing, S., Walcher, C. Jakob, Matsuno, Tadafumi, Maíz Apellániz, Jesús, Battaglia, Giuseppina, Murphy, D.N.A., Bishop, Georgia, Bensby, T., Blomqvist, Michael, Aguado, David S., Corcho-Caballero, Pablo, Worley, C.C., Guarcello, Mario Giuseppe, Benn, Chris R., Bonifacio, P., Seabroke, G.M., Castro-Ginard, Alfred, Famaey, Benoit, Couto, Guilherme, Rossi, Elena Maria, Pozzetti, Lucia, Lonoce, Ilaria, Berlanas, Sara R., and Costantin, Luca
Abstract: WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable ‘mini’ integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366−959 nm at R ∼ 5000, or two shorter ranges at R ∼ 20 000. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy’s origins by completing Gaia’s phase-space information, providing metallicities to its limiting magnitude for ∼3 million stars and detailed abundances for ∼1.5 million brighter field and open-cluster stars; (ii) survey ∼0.4 million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey ∼400 neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in z < 0.5 cluster galaxies; (vi) survey stellar populations and kinematics in ∼25 000 field galaxies at 0.3 ≲ z ≲ 0.7; (vii) study the cosmic evolution of accretion and star formation using >1 million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at z > 2. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator.
Published: 2023

27. Towards a Comprehensive Evaluation of the Environmental and Health Impacts of Shipping Emissions

Author: Mensink, C., Jorba, O., Kukkonen, J., Fridell, E., Jalkanen, J.-P., Moldanova, J., Ntziachristos, L., Grigoriadis, A., Barmpas, F., Tsegas, G., Maragkidou, A., Sofiev, M., Grönholm, T., Majamäki, E., Borken-Kleefeld, J., Sokhi, R. S., Tiwari, P. R., Ozdemir, U. A., Zervakis, V., Krasakopoulou, E., Hassellöv, I.-M., Ytreberg, E., Williams, I., Hudson, M., Zapata-Restrepo, L., Hole, L. R., Aghito, M., Breivik, O., Petrovic, M., Rodriguez-Mozaz, S., Ktoris, A., Neophytou, M., Monteiro, A., Russo, M. A., Oikonomou, F., Arampatzi, P., Gondikas, A., Marcomini, A., Giubilato, E., Calgaro, L., Jaakkola, J. J. K., Kiihamäki, S.-P., Aittamaa, R., Broström, G., Hassellöv, M., Tamminen, J., Nicolas, F., Kaitaranta, J., Granberg, M., Magnusson, K., Mensink, C., Jorba, O., Kukkonen, J., Fridell, E., Jalkanen, J.-P., Moldanova, J., Ntziachristos, L., Grigoriadis, A., Barmpas, F., Tsegas, G., Maragkidou, A., Sofiev, M., Grönholm, T., Majamäki, E., Borken-Kleefeld, J., Sokhi, R. S., Tiwari, P. R., Ozdemir, U. A., Zervakis, V., Krasakopoulou, E., Hassellöv, I.-M., Ytreberg, E., Williams, I., Hudson, M., Zapata-Restrepo, L., Hole, L. R., Aghito, M., Breivik, O., Petrovic, M., Rodriguez-Mozaz, S., Ktoris, A., Neophytou, M., Monteiro, A., Russo, M. A., Oikonomou, F., Arampatzi, P., Gondikas, A., Marcomini, A., Giubilato, E., Calgaro, L., Jaakkola, J. J. K., Kiihamäki, S.-P., Aittamaa, R., Broström, G., Hassellöv, M., Tamminen, J., Nicolas, F., Kaitaranta, J., Granberg, M., and Magnusson, K.
Abstract: We present a new concept for marine research, applied in the EU-funded project EMERGE, “Evaluation, control and Mitigation of the EnviRonmental impacts of shippinG Emissions” (2020–2024; https://emerge-h2020.eu/). For the first time, both the various marine and atmospheric impacts of the shipping sector have been and will be comprehensively analyzed, using a concerted modelling and measurements framework. The experimental part of the project focuses on five European geographical case studies in different ecologically vulnerable regions, and a mobile onboard case study. The EMERGE consortium has also developed a harmonised and integrated modelling framework to assess the combined impacts of shipping emissions, both (i) on the marine ecosystems and (ii) the atmospheric environment. The first results include substantial refinements of a range of models to be applied, especially those for the STEAM and OpenDrift models. In particular, the STEAM (Ship Traffic Emission Assessment Model) model has been extended to allow for the effects of atmospheric and oceanographic factors on the fuel consumption and emissions of the ships. The OpenDrift model has been improved to take into account the partitioning, degradation, and volatilization of pollutants in water. The predicted emission and discharge values have been used as input for both regional scale atmospheric dispersion models, such as WRF-CMAQ (Weather Research and Forecasting—Community Multiscale Air Quality Model) and SILAM (System for Integrated modeLling of Atmospheric composition), and water quality and circulation models, such as OpenDrift (Open source model for the drifting of substances in the ocean) and Delft3D (oceanographic model). The case study regions are Eastern Mediterranean, Northern Adriatic Sea, the Lagoon of Aveiro, the Solent Strait and the Öresund Strait. We have also conducted a substantial part of the experimental campaigns scheduled in the project. The final assessment will include the benefits an
Published: 2023
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28. Towards a Comprehensive Evaluation of the Environmental and Health Impacts of Shipping Emissions

Author: Mensink, C., Jorba, O., Kukkonen, J., Fridell, E., Jalkanen, J.-P., Moldanova, J., Ntziachristos, L., Grigoriadis, A., Barmpas, F., Tsegas, G., Maragkidou, A., Sofiev, M., Grönholm, T., Majamäki, E., Borken-Kleefeld, J., Sokhi, R. S., Tiwari, P. R., Ozdemir, U. A., Zervakis, V., Krasakopoulou, E., Hassellöv, I.-M., Ytreberg, E., Williams, I., Hudson, M., Zapata-Restrepo, L., Hole, L. R., Aghito, M., Breivik, O., Petrovic, M., Rodriguez-Mozaz, S., Ktoris, A., Neophytou, M., Monteiro, A., Russo, M. A., Oikonomou, F., Arampatzi, P., Gondikas, A., Marcomini, A., Giubilato, E., Calgaro, L., Jaakkola, J. J. K., Kiihamäki, S.-P., Aittamaa, R., Broström, G., Hassellöv, M., Tamminen, J., Nicolas, F., Kaitaranta, J., Granberg, M., Magnusson, K., Mensink, C., Jorba, O., Kukkonen, J., Fridell, E., Jalkanen, J.-P., Moldanova, J., Ntziachristos, L., Grigoriadis, A., Barmpas, F., Tsegas, G., Maragkidou, A., Sofiev, M., Grönholm, T., Majamäki, E., Borken-Kleefeld, J., Sokhi, R. S., Tiwari, P. R., Ozdemir, U. A., Zervakis, V., Krasakopoulou, E., Hassellöv, I.-M., Ytreberg, E., Williams, I., Hudson, M., Zapata-Restrepo, L., Hole, L. R., Aghito, M., Breivik, O., Petrovic, M., Rodriguez-Mozaz, S., Ktoris, A., Neophytou, M., Monteiro, A., Russo, M. A., Oikonomou, F., Arampatzi, P., Gondikas, A., Marcomini, A., Giubilato, E., Calgaro, L., Jaakkola, J. J. K., Kiihamäki, S.-P., Aittamaa, R., Broström, G., Hassellöv, M., Tamminen, J., Nicolas, F., Kaitaranta, J., Granberg, M., and Magnusson, K.
Abstract: We present a new concept for marine research, applied in the EU-funded project EMERGE, “Evaluation, control and Mitigation of the EnviRonmental impacts of shippinG Emissions” (2020–2024; https://emerge-h2020.eu/). For the first time, both the various marine and atmospheric impacts of the shipping sector have been and will be comprehensively analyzed, using a concerted modelling and measurements framework. The experimental part of the project focuses on five European geographical case studies in different ecologically vulnerable regions, and a mobile onboard case study. The EMERGE consortium has also developed a harmonised and integrated modelling framework to assess the combined impacts of shipping emissions, both (i) on the marine ecosystems and (ii) the atmospheric environment. The first results include substantial refinements of a range of models to be applied, especially those for the STEAM and OpenDrift models. In particular, the STEAM (Ship Traffic Emission Assessment Model) model has been extended to allow for the effects of atmospheric and oceanographic factors on the fuel consumption and emissions of the ships. The OpenDrift model has been improved to take into account the partitioning, degradation, and volatilization of pollutants in water. The predicted emission and discharge values have been used as input for both regional scale atmospheric dispersion models, such as WRF-CMAQ (Weather Research and Forecasting—Community Multiscale Air Quality Model) and SILAM (System for Integrated modeLling of Atmospheric composition), and water quality and circulation models, such as OpenDrift (Open source model for the drifting of substances in the ocean) and Delft3D (oceanographic model). The case study regions are Eastern Mediterranean, Northern Adriatic Sea, the Lagoon of Aveiro, the Solent Strait and the Öresund Strait. We have also conducted a substantial part of the experimental campaigns scheduled in the project. The final assessment will include the benefits an
Published: 2023
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29. The Pristine survey -- XX: GTC follow-up observations of extremely metal-poor stars identified from Pristine and LAMOST

Author: Arentsen, Anke, Aguado, David S., Sestito, Federico, Hernández, Jonay I. González, Martin, Nicolas F., Starkenburg, Else, Jablonka, Pascale, Yuan, Zhen, Arentsen, Anke, Aguado, David S., Sestito, Federico, Hernández, Jonay I. González, Martin, Nicolas F., Starkenburg, Else, Jablonka, Pascale, and Yuan, Zhen
Abstract: Ultra metal-poor stars ([Fe/H] < -4.0) are very rare, and finding them is a challenging task. Both narrow-band photometry and low-resolution spectroscopy have been useful tools for identifying candidates, and in this work we combine both approaches. We cross-matched metallicity-sensitive photometry from the Pristine survey with the low-resolution spectroscopic LAMOST database, and re-analysed all LAMOST spectra with [Fe/H]_Pristine < -2.5. We find that ~1/3rd of this sample (selected without [Fe/H]_Pristine quality cuts) also have spectroscopic [Fe/H] < -2.5. From this sample, containing many low signal-to-noise (S/N) spectra, we selected eleven stars potentially having [Fe/H] < -4.0 or [Fe/H] < -3.0 with very high carbon abundances, and we performed higher S/N medium-resolution spectroscopic follow-up with OSIRIS on the 10.4m Gran Telescopio Canarias (GTC). We confirm their extremely low metallicities, with a mean of [Fe/H] = -3.4 and the most metal-poor star having [Fe/H]= -3.8. Three of these are clearly carbon-enhanced metal-poor (CEMP) stars with +1.65 < [C/Fe] < +2.45. The two most carbon-rich stars are either among the most metal-poor CEMP-s stars or the most carbon-rich CEMP-no stars known, the third is likely a CEMP-no star. We derived orbital properties for the OSIRIS sample and find that only one of our targets can be confidently associated with known substructures/accretion events, and that three out of four inner halo stars have prograde orbits. Large spectroscopic surveys may contain many hidden extremely and ultra metal-poor stars, and adding additional information from e.g. photometry as in this work can uncover them more efficiently and confidently., Comment: 13 pages, accepted for publication in MNRAS
Published: 2023
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30. Bipolar Outflows out to 10~kpc for Massive Galaxies at Redshift $z\approx 1$

Author: Guo, Yucheng, Bacon, Roland, Bouché, Nicolas F., Wisotzki, Lutz, Schaye, Joop, Blaizot, Jérémy, Verhamme, Anne, Cantalupo, Sebastiano, Boogaard, Leindert A., Brinchmann, Jarle, Cherrey, Maxime, Kusakabe, Haruka, Langan, Ivanna, Leclercq, Floriane, Matthee, Jorryt, Michel-Dansac, Léo, Schroetter, Ilane, Wendt, Martin, Guo, Yucheng, Bacon, Roland, Bouché, Nicolas F., Wisotzki, Lutz, Schaye, Joop, Blaizot, Jérémy, Verhamme, Anne, Cantalupo, Sebastiano, Boogaard, Leindert A., Brinchmann, Jarle, Cherrey, Maxime, Kusakabe, Haruka, Langan, Ivanna, Leclercq, Floriane, Matthee, Jorryt, Michel-Dansac, Léo, Schroetter, Ilane, and Wendt, Martin
Abstract: Galactic outflows are believed to play a critical role in the evolution of galaxies by regulating their mass build-up and star formation. Theoretical models assumes bipolar shapes for the outflows that extends well into the circumgalctic medium (CGM), up to tens of kpc perpendicular to the galaxies. They have been directly observed in the local Universe in several individual galaxies, e.g., around the Milky Way and M82. At higher redshifts, cosmological simulations of galaxy formation predict an increase in the frequency and efficiency of galactic outflows due to the increasing star formation activity. Outflows are responsible for removing potential fuel for star formation from the galaxy, while at the same enriching the CGM and the intergalactic medium. These feedback processes, although incorporated as key elements of cosmological simulations, are still poorly constrained on CGM scales. Here we present an ultra-deep MUSE image of the mean MgII emission surrounding a sample of galaxies at z~1 that strongly suggests the presence of outflowing gas on physical scales of more than 10kpc. We find a strong dependence of the detected signal on the inclination of the central galaxy, with edge-on galaxies clearly showing enhanced MgII emission along the minor axis, while face-on galaxies display much weaker and more isotropic emission. We interpret these findings as supporting the idea that outflows typically have a bipolar cone geometry perpendicular to the galactic disk. We demonstrate that the signal is not dominated by a few outliers. After dividing the galaxy sample in subsamples by mass, the bipolar emission is only detected in galaxies with stellar mass $\mathrm{M_* \gtrsim 10^{9.5} M_\odot}$., Comment: published in Nature. 25 pages, 10 figures
Published: 2023
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31. The Pristine Inner Galaxy Survey (PIGS) VIII: Characterising the orbital properties of the ancient, very metal-poor inner Milky Way

Author: Ardern-Arentsen, Anke, Monari, Giacomo, Queiroz, Anna B. A., Starkenburg, Else, Martin, Nicolas F., Chiappini, Cristina, Aguado, David S., Belokurov, Vasily, Carlberg, Ray, Monty, Stephanie, Myeong, GyuChul, Schultheis, Mathias, Sestito, Federico, Venn, Kim A., Vitali, Sara, Yuan, Zhen, Zhang, Hanyuan, Buder, Sven, Lewis, Geraint F., Oliver, William H., Wan, Zhen, Zucker, Daniel B., Ardern-Arentsen, Anke, Monari, Giacomo, Queiroz, Anna B. A., Starkenburg, Else, Martin, Nicolas F., Chiappini, Cristina, Aguado, David S., Belokurov, Vasily, Carlberg, Ray, Monty, Stephanie, Myeong, GyuChul, Schultheis, Mathias, Sestito, Federico, Venn, Kim A., Vitali, Sara, Yuan, Zhen, Zhang, Hanyuan, Buder, Sven, Lewis, Geraint F., Oliver, William H., Wan, Zhen, and Zucker, Daniel B.
Abstract: The oldest stars in the Milky Way (born in the first few billion years) are expected to have a high density in the inner few kpc, spatially overlapping with the Galactic bulge. We use spectroscopic data from the Pristine Inner Galaxy Survey (PIGS) to study the dynamical properties of ancient, metal-poor inner Galaxy stars. We compute distances using StarHorse, and orbital properties in a barred Galactic potential. With this paper, we release the spectroscopic AAT/PIGS catalogue (13 235 stars). We find that most PIGS stars have orbits typical for a pressure-supported population. The fraction of stars confined to the inner Galaxy decreases with decreasing metallicity, but many very metal-poor stars (VMP, [Fe/H] < -2.0) stay confined (~ 60% stay within 5 kpc). The azimuthal velocity v$_\phi$ also decreases between [Fe/H] = -1.0 and -2.0, but is constant for VMP stars (at ~ 40 km/s). The carbon-enhanced metal-poor (CEMP) stars in PIGS appear to have similar orbital properties compared to normal VMP stars. Our results suggest a possible transition between two spheroidal components - a more metal-rich, more concentrated, faster rotating component, and a more metal-poor, more extended and slower/non-rotating component. We propose that the former may be connected to pre-disc in-situ stars (or those born in large building blocks), whereas the latter may be dominated by contributions from smaller galaxies. This is an exciting era where large metal-poor samples, such as in this work (as well as upcoming surveys, e.g., 4MOST), shed light on the earliest evolution of our Galaxy., Comment: Accepted to MNRAS, new: Figures 4, 8 and 9 and Table 2 - Figure 9 shows two inner halo components
Published: 2023

32. Exploring the impact of a rapidly decelerating bar on transforming bulge orbits into disc-like orbits

Author: Li, Chengdong, Yuan, Zhen, Monari, Giacomo, Martin, Nicolas F., Siebert, Arnaud, Famaey, Benoit, Chiba, Rimpei, Kordopatis, Georges, Ibata, Rodrigo A., Hill, Vanessa, Li, Chengdong, Yuan, Zhen, Monari, Giacomo, Martin, Nicolas F., Siebert, Arnaud, Famaey, Benoit, Chiba, Rimpei, Kordopatis, Georges, Ibata, Rodrigo A., and Hill, Vanessa
Abstract: The most metal-poor tail of the Milky Way ([Fe/H] $\leq$ $-$2.5) contains a population of stars with very prograde planar orbits, which is puzzling in both their origin and evolution. A possible scenario is that they are shepherded by the bar from the inner Galaxy, where many of the old and low-metallicity stars in the Galaxy are located. To investigate this scenario, we use test-particle simulations with an axisymmetric background potential plus a central bar model. The test particles are generated by an extended distribution function (EDF) model based on the observational constraints of bulge stars. According to the simulation results, a bar with constant pattern speed cannot help bring stars from the bulge to the solar vicinity. In contrast, when the model includes a rapidly decelerating bar, some bulge stars can gain rotation and move outwards as they are trapped in the co-rotation regions of the bar. The resulting distribution of shepherded stars heavily depends on the present-day azimuthal angle between the bar and the Sun. The majority of the low-metallicity bulge stars driven outwards are distributed in the fourth quadrant of the Galaxy with respect to the Sun, and about 10$\%$ of them are within 6 kpc from us. Our experiments indicate that the decelerating bar perturbation can be a contributing process to explain part of the most metal-poor stars with prograde planar orbits seen in the Solar neighborhood but is unlikely to be the dominant one., Comment: 12 pages, 11 figures, re-submitted to A&A with revisions
Published: 2023

33. Could very low-metallicity stars with rotation-dominated orbits have been shepherded by the bar?

Author: Yuan, Zhen, Li, Chengdong, Martin, Nicolas F., Monari, Giacomo, Famaey, Benoit, Siebert, Arnaud, Ardern-Arentsen, Anke, Sestito, Federico, Thomas, Guillaume F., Hill, Vanessa, Ibata, Rodrigo A., Kordopatis, Georges, Starkenburg, Else, Viswanathan, Akshara, Yuan, Zhen, Li, Chengdong, Martin, Nicolas F., Monari, Giacomo, Famaey, Benoit, Siebert, Arnaud, Ardern-Arentsen, Anke, Sestito, Federico, Thomas, Guillaume F., Hill, Vanessa, Ibata, Rodrigo A., Kordopatis, Georges, Starkenburg, Else, and Viswanathan, Akshara
Abstract: The most metal-poor stars (e.g. [Fe/H] $\leq-2.5$) are the ancient fossils from the early assembly epoch of our Galaxy, very likely before the formation of the thick disc. Recent studies have shown that a non-negligible fraction of them have prograde planar orbits, which makes their origin a puzzle. It has been suggested that a later-formed rotating bar could have driven these old stars from the inner Galaxy outward, and transformed their orbits to be more rotation-dominated. However, it is not clear if this mechanism can explain these stars as observed in the solar neighborhood. In this paper, we explore the possibility of this scenario by tracing these stars backwards in an axisymmetric Milky Way potential with a bar perturber. We integrate their orbits backward for 6 Gyr under two bar models: one with a constant pattern speed and another one with a decelerating speed. Our experiments show that, under the constantly-rotating bar model, the stars of interest are little affected by the bar and cannot have been shepherded from a spheroidal inner Milky Way to their current orbits. In the extreme case of a rapidly decelerating bar, some of the very metal-poor stars on planar and prograde orbits can be brought from the inner Milky Way, but $\sim90\%$ of them were nevertheless already rotation-dominated ($J_{\phi}$ $\geq$ 1000 km s$^{-1}$ kpc) 6 Gyr ago. The chance of these stars having started with spheroid-like orbits with small rotation ($J_{\phi}$ $\lesssim$ 600 km s$^{-1}$ kpc) is very low ($<$ 3$\%$). We therefore conclude that, within the solar neighborhood, the bar is unlikely to have shepherded a significant fraction of inner Galaxy spheroid stars to produce the overdensity of stars on prograde, planar orbits that is observed today., Comment: submitted to A&A, comments are welcome
Published: 2023

34. EMPRESS. IX. Extremely Metal-poor Galaxies are Very Gas-rich Dispersion-dominated Systems:Will the James Webb Space Telescope Witness Gaseous Turbulent High-z Primordial Galaxies?

Author: Isobe, Yuki, Ouchi, Masami, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Xu, Yi, Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, Zhang, Yechi, Isobe, Yuki, Ouchi, Masami, Nakajima, Kimihiko, Ozaki, Shinobu, Bouché, Nicolas F., Wise, John H., Xu, Yi, Emsellem, Eric, Kusakabe, Haruka, Hattori, Takashi, Nagao, Tohru, Chiaki, Gen, Fukushima, Hajime, Harikane, Yuichi, Hayashi, Kohei, Hirai, Yutaka, Kim, Ji Hoon, Maseda, Michael V., Nagamine, Kentaro, Shibuya, Takatoshi, Sugahara, Yuma, Yajima, Hidenobu, Aoyama, Shohei, Fujimoto, Seiji, Fukushima, Keita, Hatano, Shun, Inoue, Akio K., Ishigaki, Tsuyoshi, Kawasaki, Masahiro, Kojima, Takashi, Komiyama, Yutaka, Koyama, Shuhei, Koyama, Yusei, Lee, Chien-hsiu, Matsumoto, Akinori, Mawatari, Ken, Moriya, Takashi J., Motohara, Kentaro, Murai, Kai, Nishigaki, Moka, Onodera, Masato, Ono, Yoshiaki, Rauch, Michael, Saito, Tomoki, Sasaki, Rin, Suzuki, Akihiro, Takeuchi, Tsutomu T., Umeda, Hiroya, Umemura, Masayuki, Watanabe, Kuria, Yabe, Kiyoto, and Zhang, Yechi
Published: 2023

35. Simulated dataset of corn response to nitrogen over thousands of fields and multiple years in Illinois.

Author: Mandrini, German, Mandrini, German, Archontoulis, Sotirios V, Pittelkow, Cameron M, Mieno, Taro, Martin, Nicolas F, Mandrini, German, Mandrini, German, Archontoulis, Sotirios V, Pittelkow, Cameron M, Mieno, Taro, and Martin, Nicolas F
Abstract: Nitrogen (N) fertilizer recommendations for corn (Zea mays L.) in the US Midwest have been a puzzle for several decades, without agreement among stakeholders for which methodology is the best to balance environmental and economic outcomes. Part of the reason is the lack of long-term data of crop responses to N over multiple fields since trial data is often limited in the number of soils and years it can explore. To overcome this limitation, we designed an analytical platform based on crop simulations run over millions of farming scenarios over extensive geographies. The database was calibrated and validated using data from more than four hundred trials in the region. This dataset can have an important role for research and education in N management, machine leaching, and environmental policy analysis. The calibration and validation procedure provides a framework for future gridded crop model studies. We describe dataset characteristics and provide thorough descriptions of the model setup.
Published: 2022

36. The Pristine survey -- XVII. The C-19 stream is dynamically hot and more extended than previously thought

Author: Yuan, Zhen, Martin, Nicolas F., Ibata, Rodrigo A., Caffau, Elisabetta, Bonifacio, Piercarlo, Mashonkina, Lyudmila I., Errani, Raphaël, Doliva-Dolinsky, Amandine, Starkenburg, Else, Venn, Kim A., Arensten, Anke, Aguado, David S., Bellazzini, Michele, Famaey, Benoit, Fouesneau, Morgan, Hernández, Jonay I. González, Jablonka, Pascale, Lardo, Carmela, Malhan, Khyati, Navarro, Julio F., Janssen, Rubén Sánchez, Sestito, Federico, Thomas, Guillaume F., Viswanathan, Akshara, Vitali, Sara, Yuan, Zhen, Martin, Nicolas F., Ibata, Rodrigo A., Caffau, Elisabetta, Bonifacio, Piercarlo, Mashonkina, Lyudmila I., Errani, Raphaël, Doliva-Dolinsky, Amandine, Starkenburg, Else, Venn, Kim A., Arensten, Anke, Aguado, David S., Bellazzini, Michele, Famaey, Benoit, Fouesneau, Morgan, Hernández, Jonay I. González, Jablonka, Pascale, Lardo, Carmela, Malhan, Khyati, Navarro, Julio F., Janssen, Rubén Sánchez, Sestito, Federico, Thomas, Guillaume F., Viswanathan, Akshara, and Vitali, Sara
Abstract: The C-19 stream is the most metal poor stellar system ever discovered, with a mean metallicity $[Fe/H] = -3.38\pm0.06$. Its low metallicity dispersion ($\sigma_{\rm [Fe/H]}$ $<$ 0.18 at the 95\% confidence level) as well as variations in sodium abundances strongly suggest a globular cluster origin. In this work, we use VLT/UVES spectra of seven C-19 stars to derive more precise velocity measurements for member stars, and to identify two new members with radial velocities and metallicities consistent with the stream's properties. One of these new member stars is located 30 $\deg$ away from the previously identified body of C-19, implying that the stream is significantly more extended than previously known and that more members likely await discovery. In the main part of C-19, we measure a radial velocity dispersion $\sigma_v$ = 6.2$^{+2.0}_{-1.4}$ km s$^{-1}$ from nine members, and a stream width of 0.56$\deg\pm0.08\deg$, equivalent to $\sim$158 pc at a heliocentric distance of 18 kpc. These confirm that C-19 is comparatively hotter, dynamically, than other known globular cluster streams and shares the properties of faint dwarf galaxy streams. On the other hand, the variations in the Na abundances of the three newly observed bright member stars, the variations in Mg and Al for two of them, and the normal Ba abundance of the one star where it can be measured provide further evidence for a globular cluster origin. The tension between the dynamical and chemical properties of C-19 suggests that its progenitor experienced a complex birth environment or disruption history., Comment: 7 pages, 6 figures, submitted to MNRAS. The C-19 member list is published via https://github.com/zyuan-astro/C-19
Published: 2022

37. The MUSE Extremely Deep Field: a first panoramic view of an Mg II emitting intragroup medium

Author: Leclercq, Floriane, Verhamme, Anne, Epinat, Benoit, Simmonds, Charlotte, Matthee, Jorryt, Bouché, Nicolas F., Garel, Thibault, Urrutia, Tanya, Wisotzki, Lutz, Zabl, Johannes, Bacon, Roland, Abril-Melgarejo, Valentina, Boogaard, Leindert, Brinchmann, Jarle, Cantalupo, Sebastiano, Contini, Thierry, Kerutt, Josephine, Kusakabe, Haruka, Maseda, Michael, Michel-Dansac, Léo, Muzahid, Sowgat, Nanayakkara, Themiya, Richard, Johan, Schaye, Joop, Leclercq, Floriane, Verhamme, Anne, Epinat, Benoit, Simmonds, Charlotte, Matthee, Jorryt, Bouché, Nicolas F., Garel, Thibault, Urrutia, Tanya, Wisotzki, Lutz, Zabl, Johannes, Bacon, Roland, Abril-Melgarejo, Valentina, Boogaard, Leindert, Brinchmann, Jarle, Cantalupo, Sebastiano, Contini, Thierry, Kerutt, Josephine, Kusakabe, Haruka, Maseda, Michael, Michel-Dansac, Léo, Muzahid, Sowgat, Nanayakkara, Themiya, Richard, Johan, and Schaye, Joop
Abstract: Using the exquisite MUSE eXtremely Deep Field data, we report the discovery of an MgII emission nebula with an area above a 2$\sigma$ significance level of 1000 proper kpc$^2$, providing the first panoramic view of the spatial distribution of magnesium in the intragroup medium of a low mass group of five star-forming galaxies at z=1.31. The galaxy group members are separated by less than 50 physical kpc in projection and $\approx$120 km/s in velocity space. The most massive galaxy has a stellar mass of 10$^{9.35}$ M$_\odot$ and shows an MgII P-Cygni line profile indicating the presence of an outflow, which is consistent with the spatially resolved spectral analysis showing $\approx+$120 km/s shift of the MgII emission lines with respect to the systemic redshift. The other galaxies are less massive and only show MgII in emission. The detected MgII nebula has a maximal projected extent of $\approx$70 kpc including a low surface brightness (2 $\times$ 10$^{-19}$ erg/s/cm$^{2}$/arcsec$^{2}$) gaseous bridge between two subgroups of galaxies. The presence of absorption features in the spectrum of a background galaxy located at an impact parameter of 19 kpc from the closest galaxy of the group indicates the presence of gas enriched in magnesium even beyond the detected nebula seen in emission, suggesting that we are observing the tip of a larger intragroup medium. The observed MgII velocity gradient suggests an overall rotation of the structure along the major axis of the most massive galaxy. Our MUSE data also reveal extended Fe II* emission in the vicinity of the most massive galaxy, aligned with its minor axis. Extended [OII] emission is found around the galaxy group members and at the location of the MgII bridge. Our results suggest that both tidal stripping effects from galaxy interactions and outflows are enriching the intragroup medium of this system., Comment: Submitted to A&A. Referee's first comments implemented
Published: 2022

38. The Global Dynamical Atlas of the Milky Way mergers: Constraints from Gaia EDR3 based orbits of globular clusters, stellar streams and satellite galaxies

Author: Malhan, Khyati, Ibata, Rodrigo A., Sharma, Sanjib, Famaey, Benoit, Bellazzini, Michele, Carlberg, Raymond G., D'Souza, Richard, Yuan, Zhen, Martin, Nicolas F., Thomas, Guillaume F., Malhan, Khyati, Ibata, Rodrigo A., Sharma, Sanjib, Famaey, Benoit, Bellazzini, Michele, Carlberg, Raymond G., D'Souza, Richard, Yuan, Zhen, Martin, Nicolas F., and Thomas, Guillaume F.
Abstract: The Milky Way halo was predominantly formed by the merging of numerous progenitor galaxies. However, our knowledge of this process is still incomplete, especially in regard to the total number of mergers, their global dynamical properties and their contribution to the stellar population of the Galactic halo. Here, we uncover the Milky Way mergers by detecting groupings of globular clusters, stellar streams and satellite galaxies in action ($\mathbf{J}$) space. While actions fully characterize the orbits, we additionally use the redundant information on their energy ($\textit{E}$) to enhance the contrast between groupings. For this endeavour, we use $\textit{Gaia}$ EDR3 based measurements of $170$ globular clusters, $41$ streams and $46$ satellites to derive their $\mathbf{J}$ and $\textit{E}$. To detect groups, we use the $\texttt{ENLINK}$ software, coupled with a statistical procedure that accounts for the observed phase-space uncertainties of these objects. We detect a total of $N=6$ groups, including the previously known mergers $\textit{Sagittarius}$, $\textit{Cetus}$, $\textit{Gaia-Sausage/Enceladus}$, $\textit{LMS-1/Wukong}$, $\textit{Arjuna/Sequoia/I'itoi}$ and one new merger that we call $\textit{Pontus}$. All of these mergers, together, comprise $62$ objects ($\approx 25\%$ of our sample). We discuss their members, orbital properties and metallicity distributions. We find that the three most metal-poor streams of our Galaxy -- "C-19" ([Fe/H]$=-3.4$ dex), "Sylgr" ([Fe/H]$=-2.9$ dex) and "Phoenix" ([Fe/H]$=-2.7$ dex) -- are associated with $\textit{LMS-1/Wukong}$; showing it to be the most metal-poor merger. The global dynamical atlas of Milky Way mergers that we present here provides a present-day reference for galaxy formation models., Comment: Published in ApJ. Key results in Table 3. The paper contains 38 pages, 17 figures, 4 Tables
Published: 2022
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39. The Pristine survey -- XVI. The metallicity of 26 stellar streams around the Milky Way detected with the STREAMFINDER in Gaia EDR3

Author: Martin, Nicolas F., Ibata, Rodrigo A., Starkenburg, Else, Yuan, Zhen, Malhan, Khyati, Bellazzini, Michele, Viswanathan, Akshara, Aguado, David, Arentsen, Anke, Bonifacio, Piercarlo, Carlberg, Ray, Hernández, Jonay I. González, Hill, Vanessa, Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, McConnachie, Alan W., Navarro, Julio, Sánchez-Janssen, Rubén, Sestito, Federico, Thomas, Guillaume F., Venn, Kim A., Vitali, Sara, Voggel, Karina T., Martin, Nicolas F., Ibata, Rodrigo A., Starkenburg, Else, Yuan, Zhen, Malhan, Khyati, Bellazzini, Michele, Viswanathan, Akshara, Aguado, David, Arentsen, Anke, Bonifacio, Piercarlo, Carlberg, Ray, Hernández, Jonay I. González, Hill, Vanessa, Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, McConnachie, Alan W., Navarro, Julio, Sánchez-Janssen, Rubén, Sestito, Federico, Thomas, Guillaume F., Venn, Kim A., Vitali, Sara, and Voggel, Karina T.
Abstract: We use the photometric metallicities provided by the panoramic Pristine survey to study the veracity and derive the metallicities of the numerous stellar streams found by Ibata et al. (2021) from the application of the STREAMFINDER algorithm to the Gaia EDR3 data. All 26 streams present in Pristine show a clear metallicity distribution function, which provides an independent check of the reality of these structures, supporting the reliability of STREAMFINDER in finding streams and the power of Pristine to measure precise metallicities. We further present 6 candidate structures with coherent phase-space and metallicity signals that are very likely streams. The majority of studied streams are very metal-poor (14 structures with [Fe/H]<-2.0) and include 3 extremely metal-poor systems ([Fe/H]<-3.0; C-11, C-19, and C-20). These streams could be the closest debris of low-luminosity dwarf galaxies or may have originated from globular clusters of significantly lower metallicity than any known current Milky Way globular cluster. Our study shows that the promise of the Gaia data for Galactic Archeology studies can be substantially strengthened by quality photometric metallicities, allowing us to peer back into the earliest epochs of the formation of our Galaxy and its stellar halo constituents., Comment: 25 pages, 29 figures, submitted to MNRAS
Published: 2022

40. A stellar stream remnant of a globular cluster below the metallicity floor

Author: Martin, Nicolas F., Venn, Kim A., Aguado, David S., Starkenburg, Else, Hernández, Jonay I. González, Ibata, Rodrigo A., Bonifacio, Piercarlo, Caffau, Elisabetta, Sestito, Federico, Arentsen, Anke, Prieto, Carlos Allende, Carlberg, Raymond G., Fabbro, Sébastien, Fouesneau, Morgan, Hill, Vanessa, Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, Malhan, Khyati, Mashonkina, Lyudmila I., McConnachie, Alan W., Navarro, Julio F., Janssen, Rubén Sánchez, Thomas, Guillaume F., Yuan, Zhen, Mucciarelli, Alessio, Martin, Nicolas F., Venn, Kim A., Aguado, David S., Starkenburg, Else, Hernández, Jonay I. González, Ibata, Rodrigo A., Bonifacio, Piercarlo, Caffau, Elisabetta, Sestito, Federico, Arentsen, Anke, Prieto, Carlos Allende, Carlberg, Raymond G., Fabbro, Sébastien, Fouesneau, Morgan, Hill, Vanessa, Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, Malhan, Khyati, Mashonkina, Lyudmila I., McConnachie, Alan W., Navarro, Julio F., Janssen, Rubén Sánchez, Thomas, Guillaume F., Yuan, Zhen, and Mucciarelli, Alessio
Abstract: Stellar ejecta gradually enrich the gas out of which subsequent stars form, making the least chemically enriched stellar systems direct fossils of structures formed in the early universe. Although a few hundred stars with metal content below one thousandth of the solar iron content are known in the Galaxy, none of them inhabit globular clusters, some of the oldest known stellar structures. These show metal content of at least ~0.2 percent of the solar metallicity ([Fe/H] > -2.7). This metallicity floor appears universal and it has been proposed that proto-galaxies that merge into the galaxies we observe today were simply not massive enough to form clusters that survived to the present day. Here, we report the discovery of a stellar stream, C-19, whose metallicity is less than 0.05 per cent the solar metallicity ([Fe/H]=-3.38 +/- 0.06 (stat.) +/- 0.20 (syst.)). The low metallicity dispersion and the chemical abundances of the C-19 stars show that this stream is the tidal remnant of the most metal-poor globular cluster ever discovered, and significantly below the purported metallicity floor: clusters with significantly lower metallicities than observed today existed in the past and contributed their stars to the Milky Way halo., Comment: 14 pages, 6 figures, 5 tables. Nature, accepted
Published: 2022
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41. The Pristine survey - XVI. The metallicity of 26 stellar streams around the Milky Way detected with the STREAMFINDER in Gaia EDR3

Author: Martin, Nicolas F., Ibata, Rodrigo A., Starkenburg, Else, Yuan, Zhen, Malhan, Khyati, Bellazzini, Michele, Viswanathan, Akshara, Aguado, David, Arentsen, Anke, Bonifacio, Piercarlo, Carlberg, Ray, González Hernández, Jonay I., Hill, Vanessa, Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, McConnachie, Alan W., Navarro, Julio, Sánchez-Janssen, Rubén, Sestito, Federico, Thomas, Guillaume F., Venn, Kim A., Vitali, Sara, Voggel, Karina T., Martin, Nicolas F., Ibata, Rodrigo A., Starkenburg, Else, Yuan, Zhen, Malhan, Khyati, Bellazzini, Michele, Viswanathan, Akshara, Aguado, David, Arentsen, Anke, Bonifacio, Piercarlo, Carlberg, Ray, González Hernández, Jonay I., Hill, Vanessa, Jablonka, Pascale, Kordopatis, Georges, Lardo, Carmela, McConnachie, Alan W., Navarro, Julio, Sánchez-Janssen, Rubén, Sestito, Federico, Thomas, Guillaume F., Venn, Kim A., Vitali, Sara, and Voggel, Karina T.
Abstract: We use the photometric metallicities provided by the panoramic Pristine survey to study the veracity and derive the metallicities of the numerous stellar streams found by the application of the STREAMFINDER algorithm to the Gaia Early Data Release 3 data. All 26 streams present in Pristine show a clear metallicity distribution function, which provides an independent check of the reality of these structures, supporting the reliability of STREAMFINDER in finding streams and the power of Pristine to measure precise metallicities. We further present six candidate structures with coherent phase-space and metallicity signals that are very likely streams. The majority of studied streams are very metal-poor (14 structures with [Fe/H] < −2.0) and include three systems with [Fe/H] < −2.9 (C-11, C-19, and C-20). These streams could be the closest debris of low-luminosity dwarf galaxies or may have originated from globular clusters of significantly lower metallicity than any known current Milky Way globular cluster. Our study shows that the promise of the Gaia data for Galactic Archeology studies can be substantially strengthened by quality photometric metallicities, allowing us to peer back into the earliest epochs of the formation of our Galaxy and its stellar halo constituents.
Published: 2022
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42. Simulated dataset of corn response to nitrogen over thousands of fields and multiple years in Illinois.

Author: Mandrini, German, Mandrini, German, Archontoulis, Sotirios V, Pittelkow, Cameron M, Mieno, Taro, Martin, Nicolas F, Mandrini, German, Mandrini, German, Archontoulis, Sotirios V, Pittelkow, Cameron M, Mieno, Taro, and Martin, Nicolas F
Abstract: Nitrogen (N) fertilizer recommendations for corn (Zea mays L.) in the US Midwest have been a puzzle for several decades, without agreement among stakeholders for which methodology is the best to balance environmental and economic outcomes. Part of the reason is the lack of long-term data of crop responses to N over multiple fields since trial data is often limited in the number of soils and years it can explore. To overcome this limitation, we designed an analytical platform based on crop simulations run over millions of farming scenarios over extensive geographies. The database was calibrated and validated using data from more than four hundred trials in the region. This dataset can have an important role for research and education in N management, machine leaching, and environmental policy analysis. The calibration and validation procedure provides a framework for future gridded crop model studies. We describe dataset characteristics and provide thorough descriptions of the model setup.
Published: 2022

43. Improving Error Detection in Deep Learning Based Radiotherapy Autocontouring Using Bayesian Uncertainty

Author: Mody, Prerak (author), Chaves-de-Plaza, Nicolas F. (author), Hildebrandt, K.A. (author), Staring, M. (author), Mody, Prerak (author), Chaves-de-Plaza, Nicolas F. (author), Hildebrandt, K.A. (author), and Staring, M. (author)
Abstract: Bayesian Neural Nets (BNN) are increasingly used for robust organ auto-contouring. Uncertainty heatmaps extracted from BNNs have been shown to correspond to inaccurate regions. To help speed up the mandatory quality assessment (QA) of contours in radiotherapy, these heatmaps could be used as stimuli to direct visual attention of clinicians to potential inaccuracies. In practice, this is non-trivial to achieve since many accurate regions also exhibit uncertainty. To influence the output uncertainty of a BNN, we propose a modified accuracy-versus-uncertainty (AvU) metric as an additional objective during model training that penalizes both accurate regions exhibiting uncertainty as well as inaccurate regions exhibiting certainty. For evaluation, we use an uncertainty-ROC curve that can help differentiate between Bayesian models by comparing the probability of uncertainty in inaccurate versus accurate regions. We train and evaluate a FlipOut BNN model on the MICCAI2015 Head and Neck Segmentation challenge dataset and on the DeepMind-TCIA dataset, and observed an increase in the AUC of uncertainty-ROC curves by 5.6% and 5.9%, respectively, when using the AvU objective. The AvU objective primarily reduced false positives regions (uncertain and accurate), drawing less visual attention to these regions, thereby potentially improving the speed of error detection., Green Open Access added to TU Delft Institutional Repository 'You share, we take care!' - Taverne project https://www.openaccess.nl/en/you-share-we-take-care Otherwise as indicated in the copyright section: the publisher is the copyright holder of this work and the author uses the Dutch legislation to make this work public., Computer Graphics and Visualisation, Pattern Recognition and Bioinformatics
Published: 2022
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44. Towards fast human-centred contouring workflows for adaptive external beam radiotherapy

Author: Chaves-de-Plaza, Nicolas F. (author), Mody, P. (author), Hildebrandt, K.A. (author), Staring, M. (author), Astreinidou, Eleftheria (author), de Ridder, Mischa (author), de Ridder, H. (author), van Egmond, R. (author), Chaves-de-Plaza, Nicolas F. (author), Mody, P. (author), Hildebrandt, K.A. (author), Staring, M. (author), Astreinidou, Eleftheria (author), de Ridder, Mischa (author), de Ridder, H. (author), and van Egmond, R. (author)
Abstract: Delineation of tumours and organs-at-risk permits detecting and correcting changes in the patients' anatomy throughout the treatment, making it a core step of adaptive external beam radiotherapy. Although auto-contouring technologies have sped up this process, the time needed to perform the quality assessment of the generated contours remains a bottleneck, taking clinicians between several minutes and an hour to complete. The authors of this article conducted several interviews and an observational study at two treatment centres in the Netherlands to identify challenges and opportunities for speeding up the delineation process in adaptive therapies. The study revealed three contextual variables that influence contouring performance: usable additional information, applicable domain-specific knowledge, and available editing capabilities in contouring software. In practice, clinicians leverage these variables to accelerate contouring in two ways. First, they use domain-specific knowledge and relevant clinical features such as the proximity of the organs-at-risk to the tumour to enable targeted inspection of the delineation. Second, clinicians modulate editing precision depending on the effect they anticipate the edit will have on the patient outcome. By implementing these acceleration strategies in guidelines and contouring tools, developers and workflow builders could increase contouring efficiency and consistency without affecting the patient outcome., Green Open Access added to TU Delft Institutional Repository ‘You share, we take care!’ – Taverne project https://www.openaccess.nl/en/you-share-we-take-care Otherwise as indicated in the copyright section: the publisher is the copyright holder of this work and the author uses the Dutch legislation to make this work public., Computer Graphics and Visualisation, Pattern Recognition and Bioinformatics, Human Information Communication Design
Published: 2022

45. ProtoFold Neighborhood Inspector

Author: Chaves-de-Plaza, Nicolas F., Hildebrandt, Klaus, Vilanova, Anna, Chaves-de-Plaza, Nicolas F., Hildebrandt, Klaus, and Vilanova, Anna
Abstract: Post-translational modifications (PTMs) affecting a protein's residues (amino acids) can disturb its function, leading to illness. Whether or not a PTM is pathogenic depends on its type and the status of neighboring residues. In this paper, we present the ProtoFold Neighborhood Inspector (PFNI), a visualization system for analyzing residues neighborhoods. The main contribution is a visualization idiom, the Residue Constellation (RC), for identifying and comparing three-dimensional neighborhoods based on per-residue features and spatial characteristics. The RC leverages two-dimensional representations of the protein's three-dimensional structure to overcome problems like occlusion, easing the analysis of neighborhoods that often have complicated spatial arrangements. Using the PFNI, we explored proteins' structural PTM data, which allowed us to identify patterns in the distribution and quantity of per-neighborhood PTMs that might be related to their pathogenic status. In the following, we define the tasks that guided the development of the PFNI and describe the data sources we derived and used. Then, we introduce the PFNI and illustrate its usage through an example of an analysis workflow. We conclude by reflecting on preliminary findings obtained while using the tool on the provided data and future directions concerning the development of the PFNI., Comment: Accepted submission for the Bio+MedVis challenge @ IEEE VIS 2022
Published: 2022

46. Optimizing Crop Management with Reinforcement Learning and Imitation Learning

Author: Tao, Ran, Zhao, Pan, Wu, Jing, Martin, Nicolas F., Harrison, Matthew T., Ferreira, Carla, Kalantari, Zahra, Hovakimyan, Naira, Tao, Ran, Zhao, Pan, Wu, Jing, Martin, Nicolas F., Harrison, Matthew T., Ferreira, Carla, Kalantari, Zahra, and Hovakimyan, Naira
Abstract: Crop management, including nitrogen (N) fertilization and irrigation management, has a significant impact on the crop yield, economic profit, and the environment. Although management guidelines exist, it is challenging to find the optimal management practices given a specific planting environment and a crop. Previous work used reinforcement learning (RL) and crop simulators to solve the problem, but the trained policies either have limited performance or are not deployable in the real world. In this paper, we present an intelligent crop management system which optimizes the N fertilization and irrigation simultaneously via RL, imitation learning (IL), and crop simulations using the Decision Support System for Agrotechnology Transfer (DSSAT). We first use deep RL, in particular, deep Q-network, to train management policies that require all state information from the simulator as observations (denoted as full observation). We then invoke IL to train management policies that only need a limited amount of state information that can be readily obtained in the real world (denoted as partial observation) by mimicking the actions of the previously RL-trained policies under full observation. We conduct experiments on a case study using maize in Florida and compare trained policies with a maize management guideline in simulations. Our trained policies under both full and partial observations achieve better outcomes, resulting in a higher profit or a similar profit with a smaller environmental impact. Moreover, the partial-observation management policies are directly deployable in the real world as they use readily available information.
Published: 2022

47. Report on AI-Infused Contouring Workflows for Adaptive Proton Therapy in the Head and Neck

Author: Chaves-de-Plaza, Nicolas F., Mody, Prerak, Hildebrandt, Klaus, Staring, Marius, Astreinidou, Eleftheria, de Ridder, Mischa, de Ridder, Huib, van Egmond, Rene, Chaves-de-Plaza, Nicolas F., Mody, Prerak, Hildebrandt, Klaus, Staring, Marius, Astreinidou, Eleftheria, de Ridder, Mischa, de Ridder, Huib, and van Egmond, Rene
Abstract: Delineation of tumors and organs-at-risk permits detecting and correcting changes in the patients' anatomy throughout the treatment, making it a core step of adaptive proton therapy (APT). Although AI-based auto-contouring technologies have sped up this process, the time needed to perform the quality assessment (QA) of the generated contours remains a bottleneck, taking clinicians between several minutes up to an hour to complete. This paper introduces a fast contouring workflow suitable for time-critical APT, enabling detection of anatomical changes in shorter time frames and with a lower demand of clinical resources. The proposed AI-infused workflow follows two principles uncovered after reviewing the APT literature and conducting several interviews and an observational study in two radiotherapy centers in the Netherlands. First, enable targeted inspection of the generated contours by leveraging AI uncertainty and clinically-relevant features such as the proximity of the organs-at-risk to the tumor. Second, minimize the number of interactions needed to edit faulty delineations with redundancy-aware editing tools that provide the user a sense of predictability and control. We use a proof of concept that we validated with clinicians to demonstrate how current and upcoming AI capabilities support the workflow and how it would fit into clinical practice.
Published: 2022

48. Comparing Bayesian models for organ contouring in head and neck radiotherapy

Author: Mody, Prerak (author), Chaves-de-Plaza, Nicolas F. (author), Hildebrandt, K.A. (author), van Egmond, R. (author), de Ridder, H. (author), Staring, Marius (author), Mody, Prerak (author), Chaves-de-Plaza, Nicolas F. (author), Hildebrandt, K.A. (author), van Egmond, R. (author), de Ridder, H. (author), and Staring, Marius (author)
Abstract: Deep learning models for organ contouring in radiotherapy are poised for clinical usage, but currently, there exist few tools for automated quality assessment (QA) of the predicted contours. Bayesian models and their associated uncertainty, can potentially automate the process of detecting inaccurate predictions. We investigate two Bayesian models for auto-contouring, DropOut and FlipOut, using a quantitative measure – expected calibration error (ECE) and a qualitative measure – region-based accuracy-vs-uncertainty (R-AvU) graphs. It is well understood that a model should have low ECE to be considered trustworthy. However, in a QA context, a model should also have high uncertainty in inaccurate regions and low uncertainty in accurate regions. Such behaviour could direct visual attention of expert users to potentially inaccurate regions, leading to a speed-up in the QA process. Using R-AvU graphs, we qualitatively compare the behaviour of different models in accurate and inaccurate regions. Experiments are conducted on the MICCAI2015 Head and Neck Segmentation Challenge and on the DeepMindTCIA CT dataset using three models: DropOut-DICE, Dropout-CE (Cross Entropy) and FlipOut-CE. Quantitative results show that DropOut-DICE has the highest ECE, while Dropout-CE and FlipOut-CE have the lowest ECE. To better understand the difference between DropOut-CE and FlipOut-CE, we use the R-AvU graph which shows that FlipOut-CE has better uncertainty coverage in inaccurate regions than DropOut-CE. Such a combination of quantitative and qualitative metrics explores a new approach that helps to select which model can be deployed as a QA tool in clinical settings., Computer Graphics and Visualisation, Human Information Communication Design
Published: 2022
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49. Optimizing Nitrogen Management with Deep Reinforcement Learning and Crop Simulations

Author: Wu, Jing, Tao, Ran, Zhao, Pan, Martin, Nicolas F., Hovakimyan, Naira, Wu, Jing, Tao, Ran, Zhao, Pan, Martin, Nicolas F., and Hovakimyan, Naira
Abstract: Nitrogen (N) management is critical to sustain soil fertility and crop production while minimizing the negative environmental impact, but is challenging to optimize. This paper proposes an intelligent N management system using deep reinforcement learning (RL) and crop simulations with Decision Support System for Agrotechnology Transfer (DSSAT). We first formulate the N management problem as an RL problem. We then train management policies with deep Q-network and soft actor-critic algorithms, and the Gym-DSSAT interface that allows for daily interactions between the simulated crop environment and RL agents. According to the experiments on the maize crop in both Iowa and Florida in the US, our RL-trained policies outperform previous empirical methods by achieving higher or similar yield while using less fertilizers
Published: 2022

50. Local Group Dwarf Galaxy Detection Limit in the CSST survey

Author: Qu, Han, Yuan, Zhen, Doliva-Dolinsky, Amandine, Martin, Nicolas F., Kang, Xi, Wei, Chengliang, Li, Guoliang, Luo, Yu, Chang, Jiang, Tsai, Chao-Wei, Fan, Zhou, Ibata, Rodrigo, Qu, Han, Yuan, Zhen, Doliva-Dolinsky, Amandine, Martin, Nicolas F., Kang, Xi, Wei, Chengliang, Li, Guoliang, Luo, Yu, Chang, Jiang, Tsai, Chao-Wei, Fan, Zhou, and Ibata, Rodrigo
Abstract: We predict the dwarf galaxy detection limits for the upcoming Chinese Space Station Telescope (CSST) survey that will cover 17,500 deg$^{2}$ of the sky with a wide field of view of 1.1 deg$^2$. The point-source depth reaches 26.3 mag in the $g$ band and 25.9 mag in the $i$ band. Constructing mock survey data based on the designed photometric bands, we estimate the recovery rate of artificial dwarf galaxies from mock point-source photometric catalogues. The detection of these artificial dwarf galaxies is strongly dependent on their distance, magnitude and size, in agreement with searches in current surveys. We expect CSST to enable the detection of dwarf galaxies with $M_V = -3.0$ and $\mu_{250} = 32.0$ mag/arcsec$^2$ (surface-brightness limit for a system of half-light radius $r_{\rm h}$ = 250 pc at 400 kpc, and $M_V = -4.9$ and $\mu_{250} = 30.5$ mag/arcsec$^2$ around the Andromeda galaxy. Beyond the Local Group, the CSST survey will achieve $M_V = -5.8$, and $\mu_{250}$ = 29.7 mag/arcsec$^2$ in the distance range of 1--2 Mpc, opening up an exciting discovery space for faint field dwarf galaxies. With its optical bands, wide survey footprint, and space resolution, CSST will undoubtedly expand our knowledge of low-mass dwarf galaxies to an unprecedented volume., Comment: 11 pages, 10 figures. Accepted to MNRAS
Published: 2022
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