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547 results on '"Hill, V"'

1. SpectroTranslator: a deep-neural network algorithm to homogenize spectroscopic parameters

Author: Thomas, G. F., Battaglia, G., Gran, F., Fernandez-Alvar, E., Tsantaki, M., Pancino, E., Hill, V., Kordopatis, G., Gallart, C., Turchi, A., Masseron, T., Thomas, G. F., Battaglia, G., Gran, F., Fernandez-Alvar, E., Tsantaki, M., Pancino, E., Hill, V., Kordopatis, G., Gallart, C., Turchi, A., and Masseron, T.
Abstract: The emergence of large spectroscopic surveys requires homogenising on the same scale the quantities they measure in order to increase their scientific legacy. We developed the SpectroTranslator, a data-driven deep neural network algorithm that can convert spectroscopic parameters from the base of one survey to another. The algorithm also includes a method to estimate the importance that the various parameters play in the conversion from base A to B. As a showcase, we apply the algorithm to transform effective temperature, surface gravity, metallicity, [Mg/Fe] and los velocity from the base of GALAH into the APOGEE base. We demonstrate the efficiency of the SpectroTranslator algorithm to translate the spectroscopic parameters from one base to another using parameters directly by the survey teams, and are able to achieve a similar performance than previous works that have performed a similar type of conversion but using the full spectrum rather than the spectroscopic parameters, allowing to reduce the computational time, and to use the output of pipelines optimized for each survey. By combining the transformed GALAH catalogue with the APOGEE catalogue, we study the distribution of [Fe/H] and [Mg/Fe] across the Galaxy, and we find that the median distribution of both quantities present a vertical asymmetry at large radii. We attribute it to the recent perturbations generated by the passage of a dwarf galaxy across the disc or by the infall of the Large Magellanic Cloud. Although several aspects still need to be refined, in particular how to deal in an optimal manner with regions of the parameter space meagrely populated by stars in the training sample, the SpectroTranslator already shows its capability and promises to play a crucial role in standardizing various spectroscopic surveys onto a unified basis., Comment: 27 pages. Submitted to A&A. Webpage related to the paper: https://research.iac.es/proyecto/spectrotranslator
Published: 2024

2. Chronology of our Galaxy from Gaia Colour-Magnitude Diagram-fitting (ChronoGal). I. The formation and evolution of the thin disk from the Gaia Catalogue of Nearby Stars

Author: Gallart, C., Surot, F., Cassisi, S., Fernández-Alvar, E., Mirabal, D., Rivero, A., Ruiz-Lara, T., Santos-Torres, J., Aznar-Menargues, G., Battaglia, G., Queiroz, A. B., Monelli, M., Vasiliev, E., Chiappini, C., Helmi, A., Hill, V., Massari, D., Thomas, G. F., Gallart, C., Surot, F., Cassisi, S., Fernández-Alvar, E., Mirabal, D., Rivero, A., Ruiz-Lara, T., Santos-Torres, J., Aznar-Menargues, G., Battaglia, G., Queiroz, A. B., Monelli, M., Vasiliev, E., Chiappini, C., Helmi, A., Hill, V., Massari, D., and Thomas, G. F.
Abstract: The current major challenge to reconstruct the chronology of the Milky Way (MW) is the difficulty to derive precise stellar ages. CMD-fitting offers an alternative to individual age determinations to derive the star formation history (SFH). We present CMDft.Gaia and use it to analyse the CMD of the Gaia Catalogue of Nearby Stars (GCNS), which contains a census of the stars within 100 pc of the Sun. The result is an unprecedented detailed view of the evolution of the MW disk. The bulk of star formation started 11-10.5 Gyr ago at [Fe/H]~solar and continued with a slightly decreasing metallicity trend until 6 Gyr ago. Between 6-4 Gyr ago, a break in the age-metallicity distribution is observed, with 3 stellar populations with distinct metallicities (sub-solar, solar, and super-solar), possibly indicating some dramatic event in the Galaxy. Star formation resumed 4 Gyr ago with a bursty behaviour, metallicity near solar and higher average SFR. The derived metallicity distribution closely matches precise spectroscopic data, which also show stellar populations deviating from solar metallicity. Interestingly, our results reveal the presence of intermediate-age populations with both a metallicity typical of the thick disk and supersolar metallicity. Our many tests indicate that, with high precision Gaia photometric and distance data, CMDft.Gaia can achieve a precision ~10% and an accuracy better than 6% in the dating of even old stellar populations. The comparison with independent spectroscopic data shows that metallicity distributions are determined with high precision, without imposing a-priory metallicity information. This opens the door to obtaining detailed and robust information on the evolution of the stellar populations of the MW over cosmic time. As an example we provide an unprecedented detailed view of the age and metallicity distributions of the stars within 100 pc of the Sun., Comment: 35 pages, 30 figures; to be published in A&A; revised version after minor referee comments
Published: 2024

3. 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

4. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

5. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

6. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

7. Critical Appraisal of Artificial Intelligence-Enabled Imaging Tools Using the Levels of Evidence System.

Author: Pham, N, Pham, N, Hill, V, Rauschecker, A, Lui, Y, Niogi, S, Fillipi, C, Zaharchuk, G, Wintermark, M, Chang, Peter, Pham, N, Pham, N, Hill, V, Rauschecker, A, Lui, Y, Niogi, S, Fillipi, C, Zaharchuk, G, Wintermark, M, and Chang, Peter
Abstract: Clinical adoption of an artificial intelligence-enabled imaging tool requires critical appraisal of its life cycle from development to implementation by using a systematic, standardized, and objective approach that can verify both its technical and clinical efficacy. Toward this concerted effort, the ASFNR/ASNR Artificial Intelligence Workshop Technology Working Group is proposing a hierarchal evaluation system based on the quality, type, and amount of scientific evidence that the artificial intelligence-enabled tool can demonstrate for each component of its life cycle. The current proposal is modeled after the levels of evidence in medicine, with the uppermost level of the hierarchy showing the strongest evidence for potential impact on patient care and health care outcomes. The intended goal of establishing an evidence-based evaluation system is to encourage transparency, foster an understanding of the creation of artificial intelligence tools and the artificial intelligence decision-making process, and to report the relevant data on the efficacy of artificial intelligence tools that are developed. The proposed system is an essential step in working toward a more formalized, clinically validated, and regulated framework for the safe and effective deployment of artificial intelligence imaging applications that will be used in clinical practice.
Published: 2023

8. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

9. The Gaia-ESO Survey: Homogenisation of stellar parameters and elemental abundances

Author: Universidad de Alicante. Departamento de Física Aplicada, Hourihane, A., François, P., Worley, C.C., Magrini, L., Gonneau, A., Casey, A.R., Gilmore, Gerard, Randich, Sofia, Sacco, G.G., Recio-Blanco, A., Korn, A., Allende Prieto, C., Smiljanic, R., Blomme, Ronny, Bragaglia, A., Walton, N., Van Eck, S., Bensby, T., Lanzafame, A.C., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, Alex, Montes, David, Feuillet, D.K., Tautvaišienė, G., Guiglion, G., Tabernero, Hugo M., González Hernández, J.I., Gebran, M., Van der Swaelmen, M., Mikolaitis, Š., Daflon, Simone, Merle, T., Morel, Thierry, Lewis, J., González Solares, E.A., Murphy, D.N.A., Jeffries, R., Jackson, R.J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez Esteban, Francisco M., Mahy, Laurent, Gutiérrez Albarrán, M.L., Berlanas, Sara R., Santos, W., Morbidelli, L., Spina, L., Minkevičiūtė, R., Universidad de Alicante. Departamento de Física Aplicada, Hourihane, A., François, P., Worley, C.C., Magrini, L., Gonneau, A., Casey, A.R., Gilmore, Gerard, Randich, Sofia, Sacco, G.G., Recio-Blanco, A., Korn, A., Allende Prieto, C., Smiljanic, R., Blomme, Ronny, Bragaglia, A., Walton, N., Van Eck, S., Bensby, T., Lanzafame, A.C., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, Alex, Montes, David, Feuillet, D.K., Tautvaišienė, G., Guiglion, G., Tabernero, Hugo M., González Hernández, J.I., Gebran, M., Van der Swaelmen, M., Mikolaitis, Š., Daflon, Simone, Merle, T., Morel, Thierry, Lewis, J., González Solares, E.A., Murphy, D.N.A., Jeffries, R., Jackson, R.J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez Esteban, Francisco M., Mahy, Laurent, Gutiérrez Albarrán, M.L., Berlanas, Sara R., Santos, W., Morbidelli, L., Spina, L., and Minkevičiūtė, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted ≳105 stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (Teff ~ 30 000–52 000 K) all the way to K-M (≳3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023

10. The Gaia-ESO Survey : Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, Andreas, Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisiene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., van der Swaelmen, M., Mikolaitis, S., Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that targeted greater than or similar to 10(5) stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its final public release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O (T-eff similar to 30 000-52 000 K) all the way to K-M (greater than or similar to 3500 K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different types. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products, such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, for example, activity and accretion indicators in young stars and membership probability in star clusters for more than 114 000 stars. The spectral analysis is coordinated by a number of working groups (WGs) within the survey, each specialised in one or more of the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all survey results are placed on a common scale in order to arrive at a single set of recommended results for use by all survey collaborators. We also present some general quality and consistency checks performed on the entirety of the survey results.
Published: 2023
Full Text: View/download PDF

11. The Gaia-ESO Survey:Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., François, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-blanco, A., Korn, A. J., Allende Prieto, C., Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaišienė, G., Guiglion, G., Tabernero, H. M., González Hernández, J. I., Gebran, M., Van Der Swaelmen, M., Mikolaitis, Š., Daflon, S., Merle, T., Morel, T., Lewis, J. R., González Solares, E. A., Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofré, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez-esteban, F., Mahy, L., Gutiérrez Albarrán, M. L., Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkevičiūtė, R., Hourihane, A., François, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-blanco, A., Korn, A. J., Allende Prieto, C., Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaišienė, G., Guiglion, G., Tabernero, H. M., González Hernández, J. I., Gebran, M., Van Der Swaelmen, M., Mikolaitis, Š., Daflon, S., Merle, T., Morel, T., Lewis, J. R., González Solares, E. A., Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofré, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez-esteban, F., Mahy, L., Gutiérrez Albarrán, M. L., Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkevičiūtė, R.
Published: 2023

12. The treasure behind the haystack: MUSE analysis of five recently discovered globular clusters

Author: Gran, F., Kordopatis, G., Zoccali, M., Hill, V., Saviane, I., Navarrete, C., Rojas-Arriagada, A., Carballo-Bello, J., Hartke, J., Valenti, E., Ramos, R. Contreras, De Leo, M., Fabbro, S., Gran, F., Kordopatis, G., Zoccali, M., Hill, V., Saviane, I., Navarrete, C., Rojas-Arriagada, A., Carballo-Bello, J., Hartke, J., Valenti, E., Ramos, R. Contreras, De Leo, M., and Fabbro, S.
Abstract: After the second data release of Gaia, the number of new globular cluster candidates has increased importantly. However, most of them need to be properly characterised, both spectroscopically and photometrically, by means of radial velocities, metallicities, and deeper photometric observations. Our goal is to provide an independent confirmation of the cluster nature of Gran 4, a recently discovered globular cluster, with follow-up spectroscopic observations. The derived radial velocity for individual stars, coupled with proper motions, allows us to isolate cluster members from field stars, while the analysis of their spectra allows us to derive metallicities. By including in the analysis the recently confirmed clusters Gran 1, 2, 3, and 5, we aim to completely characterise the sample presented in Gran et al. 2022. Using Gaia DR3 and VVV catalogue data and MUSE@VLT observations, we performed a selection of cluster members based on their proper motions, radial velocities and their position in colour-magnitude diagrams. Furthermore, full spectral synthesis was performed on the cluster members, extracting surface parameters and metallicity from MUSE spectra. Finally, a completeness estimation was performed on the total globular cluster population of the Milky Way. We confirm the nature of Gran 4, a newly discovered globular cluster behind the Galactic bulge, with a mean radial velocity of ${\rm RV} = -265.28 \pm 3.92$ km s$^{-1}$ and a mean metallicity of ${\rm [Fe/H] = -1.72 \pm 0.32}$ dex. Additionally, independent measurements of the metallicities were derived for Gran 1, 2, 3, and 5. We also revise the observational lower mass limit for a globular cluster to survive in the bulge/disk environment. We estimate that $\sim 12-26$ globular clusters have still to be discovered on the other side of the Galaxy (i.e., behind the bulge/bar/disk), up to 20 kpc., Comment: 8 pages, 5 figures, appendix: 5 tables and 1 figure. Accepted for publication for A&A
Published: 2023

13. 1D non-LTE corrections for chemical abundance analyses of very metal-poor stars

Author: Mashonkina, L., Pakhomov, Yu., Sitnova, T., Smogorzhevskii, A., Jablonka, P., Hill, V., Mashonkina, L., Pakhomov, Yu., Sitnova, T., Smogorzhevskii, A., Jablonka, P., and Hill, V.
Abstract: Detailed chemical abundances of very metal-poor (VMP, [Fe/H] < -2) stars are important for better understanding the First Stars, early star formation and chemical enrichment of galaxies. Big on-going and coming high-resolution spectroscopic surveys provide a wealth of material that needs to be carefully analysed. For VMP stars, their elemental abundances should be derived based on the non-local thermodynamic equilibrium (non-LTE = NLTE) line formation because low metal abundances and low electron number density in the atmosphere produce the physical conditions favorable for the departures from LTE. The galactic archaeology research requires homogeneous determinations of chemical abundances. For this purpose, we present grids of the 1D-NLTE abundance corrections for the Na I, Mg I, Ca I, Ca II, Ti II, Fe I, Zn I, Zn II, Sr II, and Ba II lines, which are used in the galactic archaeology research. The range of atmospheric parameters represents VMP stars on various evolutionary stages and covers effective temperatures from 4000 to 6500~K, surface gravities from log g = 0.5 to log g = 5.0, and metallicities $-5.0 \le$ [Fe/H] $\le -2.0$. The data is publicly available, and we provide the tools for interpolating in the grids online., Comment: 11 pages, 10 figures, 3 tables, revised version after the referee's positive report, MNRAS
Published: 2023
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14. Reanalysis of neutron-capture elements in the benchmark r-rich star CS 31082-001

Author: Ernandes, H., Castro, M. J., Barbuy, B., Spite, M., Hill, V., Castilho, B., Evans, C. J., Ernandes, H., Castro, M. J., Barbuy, B., Spite, M., Hill, V., Castilho, B., and Evans, C. J.
Abstract: We revisit the abundances of neutron-capture elements in the metal-poor ([Fe/H]=-2.9) r-process-rich halo star CS 31082-001. Partly motivated by the development of the new near-ultraviolet Cassegrain U-band Efficient Spectrograph for the Very Large Telescope, we compiled an expanded line list for heavy elements over the range 3000-4000 {\AA}, including hyperfine structure for several elements. Combining archival near-ultraviolet spectra of CS 31082-001 from the Hubble Space Telescope and the Very Large Telescope, we investigate the abundances and nucleosynthesis of 35 heavy elements (Ge, Sr, Y, Zr, Nb, Mo, Ru, Rh, Pd, Ag, Cd, Sn, Ba, La, Ce, Pr, Nd, Sm, Eu, Gd, Tb, Dy, Ho, Er, Tm, Yb, Lu, Hf, Os, Ir, Pt, Pb, Bi, Th, and U). Our analysis includes the first abundance estimates for tin, holmium, and ytterbium from these data, and the first for lutetium from ground-based data, enabling a more complete view of the abundance pattern of this important reference star. In general, the r-process dominated elements are as enhanced as those in the Sun, particularly for elements with Z $\ge$ 56 (Ba and heavier). However, the abundances for the lighter elements in our sample, from Ge to Sn (31 $\le$ Z $\le$ 50), do not scale with the solar abundance pattern. Moreover, the Ge abundance is deficient relative to solar, indicating that it is dominantly an iron-peak rather than neutron-capture element. Our results (or upper limits) on Sn, Pt, Au, Pb and Bi all pose further questions, prompting further study on the origin and evolution of the known r-rich and actinide-rich, metal-poor stars.
Published: 2023
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15. The Gaia-ESO Survey: homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, A. J., Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A, Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., Van der Swaelmen, M., Mikolaitis, Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkeviciute, R., Hourihane, A., Francois, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-Blanco, A., Korn, A. J., Prieto, C. Allende, Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A, Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaisene, G., Guiglion, G., Tabernero, H. M., Hernandez, J. I. Gonzalez, Gebran, M., Van der Swaelmen, M., Mikolaitis, Daflon, S., Merle, T., Morel, T., Lewis, J. R., Solares, E. A. Gonzalez, Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofre, P., Zaggia, S., Drazdauskas, A., Stonkute, E., Marfil, E., Jimenez-Esteban, F., Mahy, L., Albarran, M. L. Gutierrez, Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkeviciute, R.
Abstract: The Gaia-ESO Survey is a public spectroscopic survey that has targeted $\gtrsim10^5$ stars covering all major components of the Milky Way from the end of 2011 to 2018, delivering its public final release in May 2022. Unlike other spectroscopic surveys, Gaia-ESO is the only survey that observed stars across all spectral types with dedicated, specialised analyses: from O ($T_\mathrm{eff} \sim 30,000-52,000$~K) all the way to K-M ($\gtrsim$3,500~K). The physics throughout these stellar regimes varies significantly, which has previously prohibited any detailed comparisons between stars of significantly different type. In the final data release (internal data release 6) of the Gaia-ESO Survey, we provide the final database containing a large number of products such as radial velocities, stellar parameters and elemental abundances, rotational velocity, and also, e.g., activity and accretion indicators in young stars and membership probability in star clusters for more than 114,000 stars. The spectral analysis is coordinated by a number of Working Groups (WGs) within the Survey, which specialise in the various stellar samples. Common targets are analysed across WGs to allow for comparisons (and calibrations) amongst instrumental setups and spectral types. Here we describe the procedures employed to ensure all Survey results are placed on a common scale to arrive at a single set of recommended results for all Survey collaborators to use. We also present some general quality and consistency checks performed over all Survey results., Comment: A&A accepted, minor revision, 36 pages, 38 figures
Published: 2023
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16. 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

17. Extremely metal-poor stars in the Fornax and Carina dwarf spheroidal galaxies

Author: Lucchesi, R., Jablonka, P., Skúladóttir, Á., Lardo, C., Mashonkina, L., Primas, F., Venn, K., Hill, V., Minniti, D., Lucchesi, R., Jablonka, P., Skúladóttir, Á., Lardo, C., Mashonkina, L., Primas, F., Venn, K., Hill, V., and Minniti, D.
Abstract: We present our analysis of VLT/UVES and X-shooter observations of six very metal-poor stars, including four stars at around [Fe/H]=-3 in the Fornax and Carina dwarf spheroidal galaxies (dSph). Until now, this metallicity range in these two galaxies was either hardly or not yet investigated. The chemical abundances of 25 elements are presented, based on 1D/LTE model atmospheres. We discuss the different elemental groups, and find that alpha- and iron-peak elements in these two systems are generally in good agreement with the Milky Way halo at the same metallicity. Our analysis reveals that none of the six stars we studied exhibit carbon enhancement, which is noteworthy given the prevalence of carbon-enhanced metal-poor (CEMP-no; no Ba enhancement) stars in the Galaxy at similarly low metallicities. Our compilation of literature data shows that the fraction of CEMP-no stars in dSphs is significantly lower than in the Milky Way, and than in ultra faint dwarf galaxies. Furthermore, we report the discovery of the lowest metallicity, [Fe/H]=-2.92, r-process rich (r-I) star in a dSph galaxy. This star, fnx_06_019, has [Eu/Fe]=+0.8, and also shows enhancement of La, Nd, and Dy, [X/Fe]>+0.5. Our new data in Carina and Fornax help to populate the extremely low metallicity range in dSph galaxies, and add onto the evidence of a low fraction of CEMP-no stars in these systems., Comment: 18 pages, 15 figures, submitted to A&A
Published: 2023

18. The Gaia-ESO Survey:Homogenisation of stellar parameters and elemental abundances

Author: Hourihane, A., François, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-blanco, A., Korn, A. J., Allende Prieto, C., Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaišienė, G., Guiglion, G., Tabernero, H. M., González Hernández, J. I., Gebran, M., Van Der Swaelmen, M., Mikolaitis, Š., Daflon, S., Merle, T., Morel, T., Lewis, J. R., González Solares, E. A., Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofré, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez-esteban, F., Mahy, L., Gutiérrez Albarrán, M. L., Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., Minkevičiūtė, R., Hourihane, A., François, P., Worley, C. C., Magrini, L., Gonneau, A., Casey, A. R., Gilmore, G., Randich, S., Sacco, G. G., Recio-blanco, A., Korn, A. J., Allende Prieto, C., Smiljanic, R., Blomme, R., Bragaglia, A., Walton, N. A., Van Eck, S., Bensby, T., Lanzafame, A., Frasca, A., Franciosini, E., Damiani, F., Lind, K., Bergemann, M., Bonifacio, P., Hill, V., Lobel, A., Montes, D., Feuillet, D. K., Tautvaišienė, G., Guiglion, G., Tabernero, H. M., González Hernández, J. I., Gebran, M., Van Der Swaelmen, M., Mikolaitis, Š., Daflon, S., Merle, T., Morel, T., Lewis, J. R., González Solares, E. A., Murphy, D. N. A., Jeffries, R. D., Jackson, R. J., Feltzing, S., Prusti, T., Carraro, G., Biazzo, K., Prisinzano, L., Jofré, P., Zaggia, S., Drazdauskas, A., Stonkuté, E., Marfil, E., Jiménez-esteban, F., Mahy, L., Gutiérrez Albarrán, M. L., Berlanas, S. R., Santos, W., Morbidelli, L., Spina, L., and Minkevičiūtė, R.
Published: 2023

19. Be, V and Cu in the halo star CS 31082-001 from near-UV spectroscopy

Author: Ernandes, H., Barbuy, B., Friaça, A., Hill, V., Spite, 2 M., Spite, F., Castilho, B. V., Evans, C. J., Ernandes, H., Barbuy, B., Friaça, A., Hill, V., Spite, 2 M., Spite, F., Castilho, B. V., and Evans, C. J.
Abstract: The 'First Stars' programme revealed the metal-poor halo star CS 31082-001 to be r-process and actinide rich, including the first measurement of a uranium abundance for an old star. To better characterise and understand such rare objects, we present the first abundance estimates of three elements (Be, V, Cu) for CS 31082-001 from analysis of its near-ultraviolet spectrum. Beryllium is rarely measured in giant stars, and we confirm that its abundance in this star is low due to the rather cool effective temperature that causes destruction of both Be and Li in its atmosphere. Vanadium and copper are iron-peak elements that are starting to be used as chemical-tagging indicators to investigate the origin of stellar populations. We find V and Cu abundances for CS 31082-001 that are comparable to other metal-poor stars, and present new chemical evolution models to investigate our results. In the case of V, extra nucleosynthesis due to interaction of neutrinos with matter is included in the models to be able to reproduce the measured abundance. Given the availability of high-quality spectroscopy of CS 31082-001, we also explore other atomic lines in the near-ultraviolet as a template for future studies of metal-poor stars with the planned CUBES instrument in development for the Very Large Telescope.
Published: 2022
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20. A stellar stream remnant of a globular cluster below the metallicity floor

Author: Martin, N. F., Venn, K. A., Aguado, D. S., Starkenburg, E., González Hernández, J. I., Ibata, R. A., Bonifacio, P., Caffau, E., Sestito, F., Arentsen, A., Allende Prieto, C., Carlberg, R. G., Fabbro, S., Fouesneau, M., Hill, V., Jablonka, P., Kordopatis, G., Lardo, C., Malhan, Khyati, Mashonkina, L. I., McConnachie, A. W., Navarro, J. F., Sánchez-Janssen, R., Thomas, G. F., Yuan, Z., Mucciarelli, A., Martin, N. F., Venn, K. A., Aguado, D. S., Starkenburg, E., González Hernández, J. I., Ibata, R. A., Bonifacio, P., Caffau, E., Sestito, F., Arentsen, A., Allende Prieto, C., Carlberg, R. G., Fabbro, S., Fouesneau, M., Hill, V., Jablonka, P., Kordopatis, G., Lardo, C., Malhan, Khyati, Mashonkina, L. I., McConnachie, A. W., Navarro, J. F., Sánchez-Janssen, R., Thomas, G. F., Yuan, Z., and Mucciarelli, A.
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 Universe1. Although a few hundred stars with metal content below 1,000th of the solar iron content are known in the Galaxy2–4, none of them inhabit globular clusters, some of the oldest known stellar structures. These show metal content of at least approximately 0.2% of the solar metallicity ([Fe / H] ≳ − 2.7). This metallicity floor appears universal5,6, and it has been proposed that protogalaxies that merged into the galaxies we observe today were simply not massive enough to form clusters that survived to the present day7. Here we report observations of a stellar stream, C-19, whose metallicity is less than 0.05% of the solar metallicity ([Fe/H]=−3.38±0.06(statistical)±0.20(systematic)). 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 is 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.
Published: 2022
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21. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
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22. The Gaia-ESO Public Spectroscopic Survey : Implementation, data products, open cluster survey, science, and legacy

Author: Randich, S., Gilmore, G., Magrini, L., Sacco, G. G., Jackson, R. J., Jeffries, R. D., Worley, C. C., Hourihane, A., Gonneau, A., Vazquez, C. Viscasillas, Franciosini, E., Lewis, J. R., Alfaro, E. J., Allende Prieto, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., Francois, P., Irwin, M. J., Koposov, S. E., Korn, Andreas, Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bayo, A., Bergemann, M., Biazzo, K., Carraro, G., Casey, A. R., Damiani, F., Frasca, A., Heiter, Ulrike, Hill, V, Jofre, P., de Laverny, P., Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Zaggia, S., Adibekyan, V, Bonito, R., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Maiz Apellaniz, J., Montes, D., Morel, T., Soubiran, C., Spina, L., Tabernero, H. M., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N. J., Abbas, U., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Friel, E. D., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Hatzidimitriou, D., Held, E. , V, Jimenez-Esteban, F., Jonsson, H., Jordi, C., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Paunzen, E., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spagna, A., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Vink, J. S., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Walton, N. A., Randich, S., Gilmore, G., Magrini, L., Sacco, G. G., Jackson, R. J., Jeffries, R. D., Worley, C. C., Hourihane, A., Gonneau, A., Vazquez, C. Viscasillas, Franciosini, E., Lewis, J. R., Alfaro, E. J., Allende Prieto, C., Bensby, T., Blomme, R., Bragaglia, A., Flaccomio, E., Francois, P., Irwin, M. J., Koposov, S. E., Korn, Andreas, Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bayo, A., Bergemann, M., Biazzo, K., Carraro, G., Casey, A. R., Damiani, F., Frasca, A., Heiter, Ulrike, Hill, V, Jofre, P., de Laverny, P., Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Zaggia, S., Adibekyan, V, Bonito, R., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Maiz Apellaniz, J., Montes, D., Morel, T., Soubiran, C., Spina, L., Tabernero, H. M., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N. J., Abbas, U., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Friel, E. D., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Hatzidimitriou, D., Held, E. , V, Jimenez-Esteban, F., Jonsson, H., Jordi, C., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Paunzen, E., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spagna, A., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Vink, J. S., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., and Walton, N. A.
Abstract: Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by t
Published: 2022
Full Text: View/download PDF

23. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

24. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

25. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

26. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

27. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jönsson, Henrik, Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. , I, Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
Full Text: View/download PDF

28. The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy

Author: Universidad de Alicante. Departamento de Física Aplicada, Randich, Sofia, Gilmore, Gerard, Magrini, L., Sacco, G.G., Jackson, R.J., Jeffries, R., Worley, C.C., Hourihane, A., Gonneau, A., Viscasillas Vázquez, C., Franciosini, E., Sbordone, L., Sousa, S.G., Zaggia, S., Adibekyan, V.Zh., Bonito, R., Caffau, E., Daflon, Simone, Feuillet, D.K., Drazdauskas, A., Gebran, M., Lagarde, N., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Maíz Apellániz, Jesús, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Evans, N.W., Mahy, Laurent, Soubiran, C., Spina, L., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N.J., Abbas, U., Mapelli, M., Famaey, B., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Berlanas, Sara R., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Marfil, E., Casagrande, L., Franchini, M., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Frémat, Y., Friel, E., Fu, X., Martell, S.L., Geisler, Douglas, Lewis, J., Gerhard, Ortwin, González Solares, E.A., Grebel, E.K., Gutiérrez Albarran, M.L., Hatzidimitriou, D., Held, E.V., Jiménez Esteban, Francisco M., Jönsson, H., Messina, S., Jordi, C., Khachaturyants, T., Alfaro, Emilio J., Kordopatis, G., Kos, J., Miglio, A., Minchev, I., Allende Prieto, C., Moitinho, A., Negueruela, Ignacio, Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Bensby, T., Prusti, T., Palouš, J., Paunzen, E., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Rix, H.-W., Blomme, Ronny, Seabroke, G.M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, Jorick S., Vallenari, A., Wright, N., Bragaglia, A., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Walton, N., Flaccomio, E., François, P., Irwin, M., Bayo, A., Koposov, S., Korn, A., Lanzafame, A.C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Bergemann, M., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Biazzo, K., Carraro, G., Casey, A.R., Damiani, F., Delgado-Mena, E., Frasca, A., Heiter, U., Hill, V., Jofre, P., Laverny, P. de, Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Di Marcantonio, P., Morbidelli, L., Prisinzano, L., Universidad de Alicante. Departamento de Física Aplicada, Randich, Sofia, Gilmore, Gerard, Magrini, L., Sacco, G.G., Jackson, R.J., Jeffries, R., Worley, C.C., Hourihane, A., Gonneau, A., Viscasillas Vázquez, C., Franciosini, E., Sbordone, L., Sousa, S.G., Zaggia, S., Adibekyan, V.Zh., Bonito, R., Caffau, E., Daflon, Simone, Feuillet, D.K., Drazdauskas, A., Gebran, M., Lagarde, N., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Maíz Apellániz, Jesús, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Evans, N.W., Mahy, Laurent, Soubiran, C., Spina, L., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N.J., Abbas, U., Mapelli, M., Famaey, B., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Berlanas, Sara R., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Marfil, E., Casagrande, L., Franchini, M., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Frémat, Y., Friel, E., Fu, X., Martell, S.L., Geisler, Douglas, Lewis, J., Gerhard, Ortwin, González Solares, E.A., Grebel, E.K., Gutiérrez Albarran, M.L., Hatzidimitriou, D., Held, E.V., Jiménez Esteban, Francisco M., Jönsson, H., Messina, S., Jordi, C., Khachaturyants, T., Alfaro, Emilio J., Kordopatis, G., Kos, J., Miglio, A., Minchev, I., Allende Prieto, C., Moitinho, A., Negueruela, Ignacio, Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Bensby, T., Prusti, T., Palouš, J., Paunzen, E., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Rix, H.-W., Blomme, Ronny, Seabroke, G.M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, Jorick S., Vallenari, A., Wright, N., Bragaglia, A., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Walton, N., Flaccomio, E., François, P., Irwin, M., Bayo, A., Koposov, S., Korn, A., Lanzafame, A.C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Bergemann, M., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Biazzo, K., Carraro, G., Casey, A.R., Damiani, F., Delgado-Mena, E., Frasca, A., Heiter, U., Hill, V., Jofre, P., Laverny, P. de, Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Di Marcantonio, P., Morbidelli, L., and Prisinzano, L.
Abstract: Context. In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey, the only one performed on a 8m class telescope, was designed to target 100 000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. Aims. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. Methods. We made use of the information recorded and archived in the observing blocks; during the observing runs; in a number of relevant documents; in the spectra and master catalogue of spectra; in the parameters delivered by the analysis nodes and the working groups; in the final catalogue; and in the science papers. Based on these sources, we critically analyse and discuss the output and products of the Survey, including science highlights. We also determined the average metallicities of the open clusters observed as science targets and of a sample of clusters whose spectra were retrieved from the ESO archive. Results. The Gaia-ESO Survey has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110 000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by t
Published: 2022

29. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author: Universidad de Alicante. Departamento de Física Aplicada, Gilmore, Gerard, Randich, Sofia, Worley, C.C., Hourihane, A., Gonneau, A., Sacco, G.G., Lewis, J., Magrini, L., François, P., Jeffries, R., Koposov, S., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Delgado-Mena, E., Bragaglia, A., Di Marcantonio, P., Drazdauskas, A., Evans, N.W., Famaey, B., Franchini, M., Frémat, Y., Fu, X., Geisler, Douglas, Gerhard, Ortwin, González Solares, E.A., Alfaro, Emilio J., Grebel, E.K., Gutiérrez Albarrán, M.L., Jiménez Esteban, Francisco M., Jönsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H.-G., Mahy, Laurent, Allende Prieto, C., Mapelli, M., Marfil, E., Martell, S.L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Blomme, Ronny, Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Palouš, J., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Korn, A., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G.M., Spina, L., Steinmetz, M., Stonkuté, E., Sutorius, E., Lanzafame, A.C., Thévenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E., Vink, Jorick S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E.V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R.J., Maíz Apellániz, Jesús, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Vallenari, A., Bergemann, M., Casey, A.R., Laverny, P. de, Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S.G., Adibekyan, V.Zh., Caffau, E., Daflon, Simone, Feuillet, D.K., Gebran, M., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Ruchti, G., Soubiran, C., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Viscasillas Vázquez, C., Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N., Zaggia, S., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Bellazzini, M., Berlanas, Sara R., Universidad de Alicante. Departamento de Física Aplicada, Gilmore, Gerard, Randich, Sofia, Worley, C.C., Hourihane, A., Gonneau, A., Sacco, G.G., Lewis, J., Magrini, L., François, P., Jeffries, R., Koposov, S., Binks, A.S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R.S., D'Orazi, V., Dantas, M.L.L., Debattista, V.P., Delgado-Mena, E., Bragaglia, A., Di Marcantonio, P., Drazdauskas, A., Evans, N.W., Famaey, B., Franchini, M., Frémat, Y., Fu, X., Geisler, Douglas, Gerhard, Ortwin, González Solares, E.A., Alfaro, Emilio J., Grebel, E.K., Gutiérrez Albarrán, M.L., Jiménez Esteban, Francisco M., Jönsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H.-G., Mahy, Laurent, Allende Prieto, C., Mapelli, M., Marfil, E., Martell, S.L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M.J.P.F.G., Morossi, C., Blomme, Ronny, Mowlavi, N., Mucciarelli, A., Murphy, D.N.A., Nardetto, N., Ortolani, S., Paletou, F., Palouš, J., Pickering, J.C., Quirrenbach, A., Re Fiorentin, P., Korn, A., Read, J.I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G.M., Spina, L., Steinmetz, M., Stonkuté, E., Sutorius, E., Lanzafame, A.C., Thévenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R.F.G., Zoccali, M., Zorec, J., Zucker, D.B., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E., Vink, Jorick S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E.V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R.J., Maíz Apellániz, Jesús, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A., Micela, G., Negueruela, Ignacio, Prusti, T., Rix, H.-W., Vallenari, A., Bergemann, M., Casey, A.R., Laverny, P. de, Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S.G., Adibekyan, V.Zh., Caffau, E., Daflon, Simone, Feuillet, D.K., Gebran, M., González Hernández, J.I., Guiglion, G., Herrero, Artemio, Lobel, Alex, Merle, T., Mikolaitis, Š., Montes, David, Morel, Thierry, Ruchti, G., Soubiran, C., Tabernero, Hugo M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Viscasillas Vázquez, C., Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N., Zaggia, S., Aguirre Børsen-Koch, V., Alves, J., Balaguer-Nunez, L., Barklem, P.S., Barrado, D., Bellazzini, M., and Berlanas, Sara R.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022

30. The Gaia-ESO Public Spectroscopic Survey: Motivation, implementation, GIRAFFE data processing, analysis, and final data products

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Prieto, C. Allende, Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Apellaniz, J. Maiz, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I., Prusti, T., Rix, H. -W., Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Hernandez, J. I. Gonzalez, Guiglion, G., Herrero, A., Lobel, A., Merle, T., Mikolaitis, S., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V., Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Albarran, M. L. Gutierrez, Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H. -G., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Prieto, C. Allende, Blomme, R., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. V., Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Apellaniz, J. Maiz, Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I., Prusti, T., Rix, H. -W., Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V., Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Hernandez, J. I. Gonzalez, Guiglion, G., Herrero, A., Lobel, A., Merle, T., Mikolaitis, S., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, B., Heiter, U., Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, P. S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V., Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Albarran, M. L. Gutierrez, Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H. -G., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100,000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper (arXiv:2206.02901) introduces the survey results. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. The Gaia-ESO Survey obtained 202,000 spectra of 115,000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022., Comment: 38 pages. A&A in press
Published: 2022
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31. The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy

Author: Randich, S., Gilmore, G., Magrini, L., Sacco, G. G., Jackson, R. J., Jeffries, R. D., Worley, C. C., Hourihane, A., Gonneau, A., Vàzquez, C. Viscasillas, Franciosini, E., Lewis, J. R., Alfaro, E. J., Prieto, C. Allende, Blomme, T. Bensby R., Bragaglia, A., Flaccomio, E., François, P., Irwin, M. J., Koposov, S. E., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I., Prusti, T., Rix, H. -W., Vallenari, A., Bayo, A., Bergemann, M., Biazzo, K., Carraro, G., Casey, A. R., Damiani, F., Frasca, A., Heiter, U., Hill, V., Jofré, P., de Laverny, P., Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Zaggia, S., Adibekyan, V., Bonito, R., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Hernández, J. I. González, Guiglion, G., Herrero, A., Lobel, A., Apellániz, J. Maíz, Merle, T., Mikolaitis, S., Montes, D., Morel, T., Soubiran, C., Spina, L., Tabernero, H. M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N. J., Abbas, U., Børsen-Koch, V. Aguirre, Alves, J., Balaguer-Núnez, L., Barklem, P. S., Barrado, D., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo--Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V., Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Frémat, Y., Friel, E. D., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. González, Grebel, E. K., Albarrán, M. L. Gutiérrez, Hatzidimitriou, D., Held, E. V., Jiménez-Esteban, F., Jönsson, H., Jordi, C., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palouus, J., Paunzen, E., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, J. S., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Walton, N. A., Randich, S., Gilmore, G., Magrini, L., Sacco, G. G., Jackson, R. J., Jeffries, R. D., Worley, C. C., Hourihane, A., Gonneau, A., Vàzquez, C. Viscasillas, Franciosini, E., Lewis, J. R., Alfaro, E. J., Prieto, C. Allende, Blomme, T. Bensby R., Bragaglia, A., Flaccomio, E., François, P., Irwin, M. J., Koposov, S. E., Korn, A. J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I., Prusti, T., Rix, H. -W., Vallenari, A., Bayo, A., Bergemann, M., Biazzo, K., Carraro, G., Casey, A. R., Damiani, F., Frasca, A., Heiter, U., Hill, V., Jofré, P., de Laverny, P., Lind, K., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Morbidelli, L., Prisinzano, L., Sbordone, L., Sousa, S. G., Zaggia, S., Adibekyan, V., Bonito, R., Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Hernández, J. I. González, Guiglion, G., Herrero, A., Lobel, A., Apellániz, J. Maíz, Merle, T., Mikolaitis, S., Montes, D., Morel, T., Soubiran, C., Spina, L., Tabernero, H. M., Tautvaišienė, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Wright, N. J., Abbas, U., Børsen-Koch, V. Aguirre, Alves, J., Balaguer-Núnez, L., Barklem, P. S., Barrado, D., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo--Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V., Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Frémat, Y., Friel, E. D., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. González, Grebel, E. K., Albarrán, M. L. Gutiérrez, Hatzidimitriou, D., Held, E. V., Jiménez-Esteban, F., Jönsson, H., Jordi, C., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I., Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palouus, J., Paunzen, E., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spagna, A., Steinmetz, M., Stonkuté, E., Sutorius, E., Thévenin, F., Tosi, M., Tsantaki, M., Vink, J. S., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., and Walton, N. A.
Abstract: In the last 15 years different ground-based spectroscopic surveys have been started (and completed) with the general aim of delivering stellar parameters and elemental abundances for large samples of Galactic stars, complementing Gaia astrometry. Among those surveys, the Gaia-ESO Public Spectroscopic Survey (GES), the only one performed on a 8m class telescope, was designed to target 100,000 stars using FLAMES on the ESO VLT (both Giraffe and UVES spectrographs), covering all the Milky Way populations, with a special focus on open star clusters. This article provides an overview of the survey implementation (observations, data quality, analysis and its success, data products, and releases), of the open cluster survey, of the science results and potential, and of the survey legacy. A companion article (Gilmore et al.) reviews the overall survey motivation, strategy, Giraffe pipeline data reduction, organisation, and workflow. The GES has determined homogeneous good-quality radial velocities and stellar parameters for a large fraction of its more than 110,000 unique target stars. Elemental abundances were derived for up to 31 elements for targets observed with UVES. Lithium abundances are delivered for about 1/3 of the sample. The analysis and homogenisation strategies have proven to be successful; several science topics have been addressed by the Gaia-ESO consortium and the community, with many highlight results achieved. The final catalogue has been released through the ESO archive at the end of May 2022, including the complete set of advanced data products. In addition to these results, the Gaia-ESO Survey will leave a very important legacy, for several aspects and for many years to come., Comment: Accepted for publication in Astronomy and Astrophysics. 30 pages, 30 figures, 4 tables
Published: 2022
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32. Be, V and Cu in the halo star CS 31082-001 from near-UV spectroscopy

Author: Ernandes, H., Barbuy, B., Friaça, A., Hill, V., Spite, 2 M., Spite, F., Castilho, B. V., Evans, C. J., Ernandes, H., Barbuy, B., Friaça, A., Hill, V., Spite, 2 M., Spite, F., Castilho, B. V., and Evans, C. J.
Abstract: The 'First Stars' programme revealed the metal-poor halo star CS 31082-001 to be r-process and actinide rich, including the first measurement of a uranium abundance for an old star. To better characterise and understand such rare objects, we present the first abundance estimates of three elements (Be, V, Cu) for CS 31082-001 from analysis of its near-ultraviolet spectrum. Beryllium is rarely measured in giant stars, and we confirm that its abundance in this star is low due to the rather cool effective temperature that causes destruction of both Be and Li in its atmosphere. Vanadium and copper are iron-peak elements that are starting to be used as chemical-tagging indicators to investigate the origin of stellar populations. We find V and Cu abundances for CS 31082-001 that are comparable to other metal-poor stars, and present new chemical evolution models to investigate our results. In the case of V, extra nucleosynthesis due to interaction of neutrinos with matter is included in the models to be able to reproduce the measured abundance. Given the availability of high-quality spectroscopy of CS 31082-001, we also explore other atomic lines in the near-ultraviolet as a template for future studies of metal-poor stars with the planned CUBES instrument in development for the Very Large Telescope.
Published: 2022
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33. The Gaia-ESO Public Spectroscopic Survey : Motivation, implementation, GIRAFFE data processing, analysis, and final data products star

Author: Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., Zucker, D. B., Gilmore, G., Randich, S., Worley, C. C., Hourihane, A., Gonneau, A., Sacco, G. G., Lewis, J. R., Magrini, L., Francois, P., Jeffries, R. D., Koposov, S. E., Bragaglia, A., Alfaro, E. J., Allende Prieto, C., Blomme, R., Korn, Andreas J., Lanzafame, A. C., Pancino, E., Recio-Blanco, A., Smiljanic, R., Van Eck, S., Zwitter, T., Bensby, T., Flaccomio, E., Irwin, M. J., Franciosini, E., Morbidelli, L., Damiani, F., Bonito, R., Friel, E. D., Vink, J. S., Prisinzano, L., Abbas, U., Hatzidimitriou, D., Held, E. , V, Jordi, C., Paunzen, E., Spagna, A., Jackson, R. J., Maiz Apellaniz, J., Asplund, M., Bonifacio, P., Feltzing, S., Binney, J., Drew, J., Ferguson, A. M. N., Micela, G., Negueruela, I, Prusti, T., Rix, H-W, Vallenari, A., Bergemann, M., Casey, A. R., de Laverny, P., Frasca, A., Hill, V, Lind, K., Sbordone, L., Sousa, S. G., Adibekyan, V, Caffau, E., Daflon, S., Feuillet, D. K., Gebran, M., Gonzalez Hernandez, J. , I, Guiglion, G., Herrero, A., Lobel, A., Montes, D., Morel, T., Ruchti, G., Soubiran, C., Tabernero, H. M., Tautvaisiene, G., Traven, G., Valentini, M., Van der Swaelmen, M., Villanova, S., Vazquez, C. Viscasillas, Bayo, A., Biazzo, K., Carraro, G., Edvardsson, Bengt, Heiter, Ulrike, Jofre, P., Marconi, G., Martayan, C., Masseron, T., Monaco, L., Walton, N. A., Zaggia, S., Borsen-Koch, V. Aguirre, Alves, J., Balaguer-Nunez, L., Barklem, Paul S., Barrado, D., Bellazzini, M., Berlanas, S. R., Binks, A. S., Bressan, A., Capuzzo-Dolcetta, R., Casagrande, L., Casamiquela, L., Collins, R. S., D'Orazi, V, Dantas, M. L. L., Debattista, V. P., Delgado-Mena, E., Di Marcantonio, P., Drazdauskas, A., Evans, N. W., Famaey, B., Franchini, M., Fremat, Y., Fu, X., Geisler, D., Gerhard, O., Solares, E. A. Gonzalez, Grebel, E. K., Gutierrez Albarran, M. L., Jimenez-Esteban, F., Jonsson, H., Khachaturyants, T., Kordopatis, G., Kos, J., Lagarde, N., Ludwig, H-G, Mahy, L., Mapelli, M., Marfil, E., Martell, S. L., Messina, S., Miglio, A., Minchev, I, Moitinho, A., Montalban, J., Monteiro, M. J. P. F. G., Morossi, C., Mowlavi, N., Mucciarelli, A., Murphy, D. N. A., Nardetto, N., Ortolani, S., Paletou, F., Palous, J., Pickering, J. C., Quirrenbach, A., Fiorentin, P. Re, Read, J. I., Romano, D., Ryde, N., Sanna, N., Santos, W., Seabroke, G. M., Spina, L., Steinmetz, M., Stonkute, E., Sutorius, E., Thevenin, F., Tosi, M., Tsantaki, M., Wright, N., Wyse, R. F. G., Zoccali, M., Zorec, J., and Zucker, D. B.
Abstract: Context. The Gaia-ESO Public Spectroscopic Survey is an ambitious project designed to obtain astrophysical parameters and elemental abundances for 100 000 stars, including large representative samples of the stellar populations in the Galaxy, and a well-defined sample of 60 (plus 20 archive) open clusters. We provide internally consistent results calibrated on benchmark stars and star clusters, extending across a very wide range of abundances and ages. This provides a legacy data set of intrinsic value, and equally a large wide-ranging dataset that is of value for the homogenisation of other and future stellar surveys and Gaia's astrophysical parameters. Aims. This article provides an overview of the survey methodology, the scientific aims, and the implementation, including a description of the data processing for the GIRAFFE spectra. A companion paper introduces the survey results. Methods. Gaia-ESO aspires to quantify both random and systematic contributions to measurement uncertainties. Thus, all available spectroscopic analysis techniques are utilised, each spectrum being analysed by up to several different analysis pipelines, with considerable effort being made to homogenise and calibrate the resulting parameters. We describe here the sequence of activities up to delivery of processed data products to the ESO Science Archive Facility for open use. Results. The Gaia-ESO Survey obtained 202 000 spectra of 115 000 stars using 340 allocated VLT nights between December 2011 and January 2018 from GIRAFFE and UVES. Conclusions. The full consistently reduced final data set of spectra was released through the ESO Science Archive Facility in late 2020, with the full astrophysical parameters sets following in 2022. A companion article reviews the survey implementation, scientific highlights, the open cluster survey, and data products.
Published: 2022
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34. The Pristine survey -- XV. A CFHT ESPaDOnS view on the Milky Way halo and disc populations

Author: Lucchesi, R., Lardo, C., Jablonka, P., Sestito, F., Mashonkina, L., Arentsen, A., Suter, W., Venn, K., Martin, N., Starkenburg, E., Aguado, D., Hill, V., Kordopatis, G., Navarro, J. F., Hernández, J. I. González, Malhan, K., Yuan, Z., Lucchesi, R., Lardo, C., Jablonka, P., Sestito, F., Mashonkina, L., Arentsen, A., Suter, W., Venn, K., Martin, N., Starkenburg, E., Aguado, D., Hill, V., Kordopatis, G., Navarro, J. F., Hernández, J. I. González, Malhan, K., and Yuan, Z.
Abstract: We present a one-dimensional, local thermodynamic equilibrium (1D-LTE) homogeneous analysis of 132 stars observed at high-resolution with ESPaDOnS. This represents the largest sample observed at high resolution (R$\sim$40,000) from the Pristine survey. This sample is based on the first version of the Pristine catalog and covers the full range of metallicities from [Fe/H]$\sim -3$ to $\sim +0.25$, with nearly half of our sample (58 stars) composed of very metal-poor stars ([Fe/H] $\le$ $-$2). This wide range of metallicities provides the opportunity of a new detailed study of the Milky Way stellar population. Because it includes both dwarf and giant stars, it also enables the analysis of any potential bias induced by the Pristine selection process. Based on Gaia EDR3, the orbital analysis of this Pristine$-$Espadons sample shows that it is composed of 65 halo stars and 67 disc stars. After a general assessment of the sample chemical properties with the $\alpha$-elements Mg and Ca, we focus on the abundance of carbon and the neutron capture elements Ba and Sr. While most of our very metal-poor subsample is carbon normal, we also find that 14 stars out of the 38 stars with [Fe/H] $\leq$ $-$2 and measured carbon abundances turn out to be carbon enhanced metal-poor (CEMP) stars. We show that these CEMP stars are nearly exclusively (i.e. 12 stars out of 14) in the regime of low luminosity, unevolved, dwarf stars, which we interpret as the consequence of bias of the Pristine filter against C-rich giants. Among the very metal-poor (VMP) stars, we identify 2 CEMP stars with no enhancement in neutron-capture process elements (CEMP-no) and another one enriched in s-process element (CEMP-s). Finally, one VMP star is found with a very low [Sr/Fe] abundance ratio for its metallicity, as expected if it had been accreted from an ultra-faint dwarf galaxy., Comment: 18 pages, 11 figures, Accepted for publication in MNRAS
Published: 2021
Full Text: View/download PDF

35. The Pristine survey XIV: chemical analysis of two ultra-metal-poor stars

Author: Lardo, C., Mashonkina, L., Jablonka, P., Bonifacio, P., Caffau, E., Aguado, D. S., Hernández, J. I. González, Sestito, F., Kielty, C. L., Venn, K. A., Hill, V., Starkenburg, E., Martin, N. F., Sitnova, T., Arentsen, A., Carlberg, R. G., Navarro, J. F., Kordopatis, G., Lardo, C., Mashonkina, L., Jablonka, P., Bonifacio, P., Caffau, E., Aguado, D. S., Hernández, J. I. González, Sestito, F., Kielty, C. L., Venn, K. A., Hill, V., Starkenburg, E., Martin, N. F., Sitnova, T., Arentsen, A., Carlberg, R. G., Navarro, J. F., and Kordopatis, G.
Abstract: Elemental abundances of the most metal-poor stars reflect the conditions in the early Galaxy and the properties of the first stars. We present a spectroscopic follow-up of two ultra metal-poor stars ([Fe/H]<-4.0) identified by the survey {\em Pristine}: Pristine 221.8781+9.7844 and Pristine 237.8588+12.5660 (hereafter Pr 221 and Pr 237, respectively). Combining data with earlier observations, we find a radial velocity of -149.25 $\pm$ 0.27 and -3.18 $\pm$ 0.19 km/s for Pr 221 and Pr 237, respectively, with no evidence of variability between 2018 and 2020. From a one-dimensional (1D) local thermodynamic equilibrium (LTE) analysis, we measure [Fe/H]$_{\rm LTE}$=-4.79 $\pm$ 0.14 for Pr 221 and [Fe/H]$_{\rm LTE}$=-4.22 $\pm$ 0.12 for Pr 237, in good agreement with previous studies. Abundances of Li, Na, Mg, Al, Si, Ca, Ti, Fe, and Sr were derived based on the non-LTE (NLTE) line formation calculations. When NLTE effects are included, we measure slightly higher metallicities: [Fe/H]$_{\rm NLTE}$=-4.40 $\pm$ 0.13 and [Fe/H]$_{\rm NLTE}$=-3.93 $\pm$ 0.12, for Pr 221 and Pr 237, respectively. Analysis of the G-band yields [C/Fe]$_{\rm 1D-LTE} \leq$ +2.3 and [C/Fe]$_{\rm 1D-LTE} \leq$ +2.0 for Pr 221 and Pr 237. Both stars belong to the low-carbon band. Upper limits on nitrogen abundances are also derived. Abundances for other elements exhibit good agreement with those of stars with similar parameters. Finally, to get insight into the properties of their progenitors, we compare NLTE abundances to theoretical yields of zero-metallicity supernovae. This suggests that the supernovae progenitors had masses ranging from 10.6 to 14.4 M$_{\odot}$ and low-energy explosions with 0.3-1.2 $\times$ 10$^{51}$ erg., Comment: 17 pages, 11 figures, accepted for publication in MNRAS
Published: 2021
Full Text: View/download PDF

36. Tracking the international spread of SARS-CoV-2 lineages B.1.1.7 and B.1.351/501Y-V2 with grinch.

Author: O'Toole, Á, Hill, V, Pybus, OG, Watts, A, Bogoch, II, Khan, K, Messina, JP, COVID-19 Genomics UK (COG-UK) consortium, Network for Genomic Surveillance in South Africa (NGS-SA), Brazil-UK CADDE Genomic Network, Tegally, H, Lessells, RR, Giandhari, J, Pillay, S, Tumedi, KA, Nyepetsi, G, Kebabonye, M, Matsheka, M, Mine, M, Tokajian, S, Hassan, H, Salloum, T, Merhi, G, Koweyes, J, Geoghegan, JL, de Ligt, J, Ren, X, Storey, M, Freed, NE, Pattabiraman, C, Prasad, P, Desai, AS, Vasanthapuram, R, Schulz, TF, Steinbrück, L, Stadler, T, Swiss Viollier Sequencing Consortium, Parisi, A, Bianco, A, García de Viedma, D, Buenestado-Serrano, S, Borges, V, Isidro, J, Duarte, S, Gomes, JP, Zuckerman, NS, Mandelboim, M, Mor, O, Seemann, T, Arnott, A, Draper, J, Gall, M, Rawlinson, W, Deveson, I, Schlebusch, S, McMahon, J, Leong, L, Lim, CK, Chironna, M, Loconsole, D, Bal, A, Josset, L, Holmes, E, St George, K, Lasek-Nesselquist, E, Sikkema, RS, Oude Munnink, B, Koopmans, M, Brytting, M, Sudha Rani, V, Pavani, S, Smura, T, Heim, A, Kurkela, S, Umair, M, Salman, M, Bartolini, B, Rueca, M, Drosten, C, Wolff, T, Silander, O, Eggink, D, Reusken, C, Vennema, H, Park, A, Carrington, C, Sahadeo, N, Carr, M, Gonzalez, G, SEARCH Alliance San Diego, National Virus Reference Laboratory, SeqCOVID-Spain, Danish Covid-19 Genome Consortium (DCGC), Communicable Diseases Genomic Network (CDGN), Dutch National SARS-CoV-2 surveillance program, Division of Emerging Infectious Diseases (KDCA), de Oliveira, T, Faria, N, Rambaut, A, Kraemer, MUG, O'Toole, Á, Hill, V, Pybus, OG, Watts, A, Bogoch, II, Khan, K, Messina, JP, COVID-19 Genomics UK (COG-UK) consortium, Network for Genomic Surveillance in South Africa (NGS-SA), Brazil-UK CADDE Genomic Network, Tegally, H, Lessells, RR, Giandhari, J, Pillay, S, Tumedi, KA, Nyepetsi, G, Kebabonye, M, Matsheka, M, Mine, M, Tokajian, S, Hassan, H, Salloum, T, Merhi, G, Koweyes, J, Geoghegan, JL, de Ligt, J, Ren, X, Storey, M, Freed, NE, Pattabiraman, C, Prasad, P, Desai, AS, Vasanthapuram, R, Schulz, TF, Steinbrück, L, Stadler, T, Swiss Viollier Sequencing Consortium, Parisi, A, Bianco, A, García de Viedma, D, Buenestado-Serrano, S, Borges, V, Isidro, J, Duarte, S, Gomes, JP, Zuckerman, NS, Mandelboim, M, Mor, O, Seemann, T, Arnott, A, Draper, J, Gall, M, Rawlinson, W, Deveson, I, Schlebusch, S, McMahon, J, Leong, L, Lim, CK, Chironna, M, Loconsole, D, Bal, A, Josset, L, Holmes, E, St George, K, Lasek-Nesselquist, E, Sikkema, RS, Oude Munnink, B, Koopmans, M, Brytting, M, Sudha Rani, V, Pavani, S, Smura, T, Heim, A, Kurkela, S, Umair, M, Salman, M, Bartolini, B, Rueca, M, Drosten, C, Wolff, T, Silander, O, Eggink, D, Reusken, C, Vennema, H, Park, A, Carrington, C, Sahadeo, N, Carr, M, Gonzalez, G, SEARCH Alliance San Diego, National Virus Reference Laboratory, SeqCOVID-Spain, Danish Covid-19 Genome Consortium (DCGC), Communicable Diseases Genomic Network (CDGN), Dutch National SARS-CoV-2 surveillance program, Division of Emerging Infectious Diseases (KDCA), de Oliveira, T, Faria, N, Rambaut, A, and Kraemer, MUG
Abstract: Late in 2020, two genetically-distinct clusters of severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2) with mutations of biological concern were reported, one in the United Kingdom and one in South Africa. Using a combination of data from routine surveillance, genomic sequencing and international travel we track the international dispersal of lineages B.1.1.7 and B.1.351 (variant 501Y-V2). We account for potential biases in genomic surveillance efforts by including passenger volumes from location of where the lineage was first reported, London and South Africa respectively. Using the software tool grinch (global report investigating novel coronavirus haplotypes), we track the international spread of lineages of concern with automated daily reports, Further, we have built a custom tracking website (cov-lineages.org/global_report.html) which hosts this daily report and will continue to include novel SARS-CoV-2 lineages of concern as they are detected.
Published: 2021

37. Tracking the international spread of SARS-CoV-2 lineages B.1.1.7 and B.1.351/501Y-V2 with grinch.

Author: O'Toole, Á, Hill, V, Pybus, OG, Watts, A, Bogoch, II, Khan, K, Messina, JP, COVID-19 Genomics UK (COG-UK) consortium, Network for Genomic Surveillance in South Africa (NGS-SA), Brazil-UK CADDE Genomic Network, Tegally, H, Lessells, RR, Giandhari, J, Pillay, S, Tumedi, KA, Nyepetsi, G, Kebabonye, M, Matsheka, M, Mine, M, Tokajian, S, Hassan, H, Salloum, T, Merhi, G, Koweyes, J, Geoghegan, JL, de Ligt, J, Ren, X, Storey, M, Freed, NE, Pattabiraman, C, Prasad, P, Desai, AS, Vasanthapuram, R, Schulz, TF, Steinbrück, L, Stadler, T, Swiss Viollier Sequencing Consortium, Parisi, A, Bianco, A, García de Viedma, D, Buenestado-Serrano, S, Borges, V, Isidro, J, Duarte, S, Gomes, JP, Zuckerman, NS, Mandelboim, M, Mor, O, Seemann, T, Arnott, A, Draper, J, Gall, M, Rawlinson, W, Deveson, I, Schlebusch, S, McMahon, J, Leong, L, Lim, CK, Chironna, M, Loconsole, D, Bal, A, Josset, L, Holmes, E, St George, K, Lasek-Nesselquist, E, Sikkema, RS, Oude Munnink, B, Koopmans, M, Brytting, M, Sudha Rani, V, Pavani, S, Smura, T, Heim, A, Kurkela, S, Umair, M, Salman, M, Bartolini, B, Rueca, M, Drosten, C, Wolff, T, Silander, O, Eggink, D, Reusken, C, Vennema, H, Park, A, Carrington, C, Sahadeo, N, Carr, M, Gonzalez, G, SEARCH Alliance San Diego, National Virus Reference Laboratory, SeqCOVID-Spain, Danish Covid-19 Genome Consortium (DCGC), Communicable Diseases Genomic Network (CDGN), Dutch National SARS-CoV-2 surveillance program, Division of Emerging Infectious Diseases (KDCA), de Oliveira, T, Faria, N, Rambaut, A, Kraemer, MUG, O'Toole, Á, Hill, V, Pybus, OG, Watts, A, Bogoch, II, Khan, K, Messina, JP, COVID-19 Genomics UK (COG-UK) consortium, Network for Genomic Surveillance in South Africa (NGS-SA), Brazil-UK CADDE Genomic Network, Tegally, H, Lessells, RR, Giandhari, J, Pillay, S, Tumedi, KA, Nyepetsi, G, Kebabonye, M, Matsheka, M, Mine, M, Tokajian, S, Hassan, H, Salloum, T, Merhi, G, Koweyes, J, Geoghegan, JL, de Ligt, J, Ren, X, Storey, M, Freed, NE, Pattabiraman, C, Prasad, P, Desai, AS, Vasanthapuram, R, Schulz, TF, Steinbrück, L, Stadler, T, Swiss Viollier Sequencing Consortium, Parisi, A, Bianco, A, García de Viedma, D, Buenestado-Serrano, S, Borges, V, Isidro, J, Duarte, S, Gomes, JP, Zuckerman, NS, Mandelboim, M, Mor, O, Seemann, T, Arnott, A, Draper, J, Gall, M, Rawlinson, W, Deveson, I, Schlebusch, S, McMahon, J, Leong, L, Lim, CK, Chironna, M, Loconsole, D, Bal, A, Josset, L, Holmes, E, St George, K, Lasek-Nesselquist, E, Sikkema, RS, Oude Munnink, B, Koopmans, M, Brytting, M, Sudha Rani, V, Pavani, S, Smura, T, Heim, A, Kurkela, S, Umair, M, Salman, M, Bartolini, B, Rueca, M, Drosten, C, Wolff, T, Silander, O, Eggink, D, Reusken, C, Vennema, H, Park, A, Carrington, C, Sahadeo, N, Carr, M, Gonzalez, G, SEARCH Alliance San Diego, National Virus Reference Laboratory, SeqCOVID-Spain, Danish Covid-19 Genome Consortium (DCGC), Communicable Diseases Genomic Network (CDGN), Dutch National SARS-CoV-2 surveillance program, Division of Emerging Infectious Diseases (KDCA), de Oliveira, T, Faria, N, Rambaut, A, and Kraemer, MUG
Abstract: Late in 2020, two genetically-distinct clusters of severe acute respiratory syndrome coronavirus 2 (SARS-CoV-2) with mutations of biological concern were reported, one in the United Kingdom and one in South Africa. Using a combination of data from routine surveillance, genomic sequencing and international travel we track the international dispersal of lineages B.1.1.7 and B.1.351 (variant 501Y-V2). We account for potential biases in genomic surveillance efforts by including passenger volumes from location of where the lineage was first reported, London and South Africa respectively. Using the software tool grinch (global report investigating novel coronavirus haplotypes), we track the international spread of lineages of concern with automated daily reports, Further, we have built a custom tracking website (cov-lineages.org/global_report.html) which hosts this daily report and will continue to include novel SARS-CoV-2 lineages of concern as they are detected.
Published: 2021

38. The Pristine survey -- XV. A CFHT ESPaDOnS view on the Milky Way halo and disc populations

Author: Lucchesi, R., Lardo, C., Jablonka, P., Sestito, F., Mashonkina, L., Arentsen, A., Suter, W., Venn, K., Martin, N., Starkenburg, E., Aguado, D., Hill, V., Kordopatis, G., Navarro, J. F., Hernández, J. I. González, Malhan, K., Yuan, Z., Lucchesi, R., Lardo, C., Jablonka, P., Sestito, F., Mashonkina, L., Arentsen, A., Suter, W., Venn, K., Martin, N., Starkenburg, E., Aguado, D., Hill, V., Kordopatis, G., Navarro, J. F., Hernández, J. I. González, Malhan, K., and Yuan, Z.
Abstract: We present a one-dimensional, local thermodynamic equilibrium (1D-LTE) homogeneous analysis of 132 stars observed at high-resolution with ESPaDOnS. This represents the largest sample observed at high resolution (R$\sim$40,000) from the Pristine survey. This sample is based on the first version of the Pristine catalog and covers the full range of metallicities from [Fe/H]$\sim -3$ to $\sim +0.25$, with nearly half of our sample (58 stars) composed of very metal-poor stars ([Fe/H] $\le$ $-$2). This wide range of metallicities provides the opportunity of a new detailed study of the Milky Way stellar population. Because it includes both dwarf and giant stars, it also enables the analysis of any potential bias induced by the Pristine selection process. Based on Gaia EDR3, the orbital analysis of this Pristine$-$Espadons sample shows that it is composed of 65 halo stars and 67 disc stars. After a general assessment of the sample chemical properties with the $\alpha$-elements Mg and Ca, we focus on the abundance of carbon and the neutron capture elements Ba and Sr. While most of our very metal-poor subsample is carbon normal, we also find that 14 stars out of the 38 stars with [Fe/H] $\leq$ $-$2 and measured carbon abundances turn out to be carbon enhanced metal-poor (CEMP) stars. We show that these CEMP stars are nearly exclusively (i.e. 12 stars out of 14) in the regime of low luminosity, unevolved, dwarf stars, which we interpret as the consequence of bias of the Pristine filter against C-rich giants. Among the very metal-poor (VMP) stars, we identify 2 CEMP stars with no enhancement in neutron-capture process elements (CEMP-no) and another one enriched in s-process element (CEMP-s). Finally, one VMP star is found with a very low [Sr/Fe] abundance ratio for its metallicity, as expected if it had been accreted from an ultra-faint dwarf galaxy., Comment: 18 pages, 11 figures, Accepted for publication in MNRAS
Published: 2021
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39. The Pristine survey XIV: chemical analysis of two ultra-metal-poor stars

Author: Lardo, C., Mashonkina, L., Jablonka, P., Bonifacio, P., Caffau, E., Aguado, D. S., Hernández, J. I. González, Sestito, F., Kielty, C. L., Venn, K. A., Hill, V., Starkenburg, E., Martin, N. F., Sitnova, T., Arentsen, A., Carlberg, R. G., Navarro, J. F., Kordopatis, G., Lardo, C., Mashonkina, L., Jablonka, P., Bonifacio, P., Caffau, E., Aguado, D. S., Hernández, J. I. González, Sestito, F., Kielty, C. L., Venn, K. A., Hill, V., Starkenburg, E., Martin, N. F., Sitnova, T., Arentsen, A., Carlberg, R. G., Navarro, J. F., and Kordopatis, G.
Abstract: Elemental abundances of the most metal-poor stars reflect the conditions in the early Galaxy and the properties of the first stars. We present a spectroscopic follow-up of two ultra metal-poor stars ([Fe/H]<-4.0) identified by the survey {\em Pristine}: Pristine 221.8781+9.7844 and Pristine 237.8588+12.5660 (hereafter Pr 221 and Pr 237, respectively). Combining data with earlier observations, we find a radial velocity of -149.25 $\pm$ 0.27 and -3.18 $\pm$ 0.19 km/s for Pr 221 and Pr 237, respectively, with no evidence of variability between 2018 and 2020. From a one-dimensional (1D) local thermodynamic equilibrium (LTE) analysis, we measure [Fe/H]$_{\rm LTE}$=-4.79 $\pm$ 0.14 for Pr 221 and [Fe/H]$_{\rm LTE}$=-4.22 $\pm$ 0.12 for Pr 237, in good agreement with previous studies. Abundances of Li, Na, Mg, Al, Si, Ca, Ti, Fe, and Sr were derived based on the non-LTE (NLTE) line formation calculations. When NLTE effects are included, we measure slightly higher metallicities: [Fe/H]$_{\rm NLTE}$=-4.40 $\pm$ 0.13 and [Fe/H]$_{\rm NLTE}$=-3.93 $\pm$ 0.12, for Pr 221 and Pr 237, respectively. Analysis of the G-band yields [C/Fe]$_{\rm 1D-LTE} \leq$ +2.3 and [C/Fe]$_{\rm 1D-LTE} \leq$ +2.0 for Pr 221 and Pr 237. Both stars belong to the low-carbon band. Upper limits on nitrogen abundances are also derived. Abundances for other elements exhibit good agreement with those of stars with similar parameters. Finally, to get insight into the properties of their progenitors, we compare NLTE abundances to theoretical yields of zero-metallicity supernovae. This suggests that the supernovae progenitors had masses ranging from 10.6 to 14.4 M$_{\odot}$ and low-energy explosions with 0.3-1.2 $\times$ 10$^{51}$ erg., Comment: 17 pages, 11 figures, accepted for publication in MNRAS
Published: 2021
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40. Personality development in adolescence and young adulthood

Author: Zeigler-Hill, V, Shackelford, T K, Zeigler-Hill, V ( V ), Shackelford, T K ( T K ), Klimstra, Theo A, Borghuis, Jeroen; https://orcid.org/0000-0002-2702-5203, Bleidorn, Wiebke; https://orcid.org/0000-0003-3795-8143, Zeigler-Hill, V, Shackelford, T K, Zeigler-Hill, V ( V ), Shackelford, T K ( T K ), Klimstra, Theo A, Borghuis, Jeroen; https://orcid.org/0000-0002-2702-5203, and Bleidorn, Wiebke; https://orcid.org/0000-0003-3795-8143
Published: 2018

41. The Pristine Inner Galaxy Survey (PIGS) I : tracing the kinematics of metal-poor stars in the Galactic bulge

Author: Arentsen, A., Starkenburg, E., Martin, N. F., Hill, V., Ibata, R., Kunder, A., Schultheis, M., Venn, K. A., Zucker, D. B., Aguado, D., Carlberg, R., González Hernández, J., Lardo, C., Longeard, N., Malhan, Khyati, Navarro, J. F., Sánchez-Janssen, R., Sestito, F., Thomas, G., Youakim, K., Lewis, G. F., Simpson, J. D., Wan, Z., Arentsen, A., Starkenburg, E., Martin, N. F., Hill, V., Ibata, R., Kunder, A., Schultheis, M., Venn, K. A., Zucker, D. B., Aguado, D., Carlberg, R., González Hernández, J., Lardo, C., Longeard, N., Malhan, Khyati, Navarro, J. F., Sánchez-Janssen, R., Sestito, F., Thomas, G., Youakim, K., Lewis, G. F., Simpson, J. D., and Wan, Z.
Abstract: Our Galaxy is known to contain a central boxy/peanut-shaped bulge, yet the importance of a classical, pressure-supported component within the central part of the Milky Way is still being debated. It should be most visible at low metallicity, a regime that has not yet been studied in detail. Using metallicity-sensitive narrow-band photometry, the Pristine Inner Galaxy Survey (PIGS) has collected a large sample of metal-poor ([Fe/H] < -1.0) stars in the inner Galaxy to address this open question. We use PIGS to trace the metal-poor inner Galaxy kinematics as function of metallicity for the first time. We find that the rotational signal decreases with decreasing [Fe/H], until it becomes negligible for the most metal-poor stars. Additionally, the velocity dispersion increases with decreasing metallicity for -3.0 < [Fe/II] < -0.5, with a gradient of -44 +/- 41un s(-1)dex(-1). These observations may signal a transition between Galactic components of different metallicities and kinematics, a different mapping on to the boxy/peanut-shaped bulge for former disc stars of different metallicities and/or the secular dynamical and gravitational influence of the bar on the pressure-supported component. Our results provide strong constraints on models that attempt to explain the properties of the inner Galaxy.
Published: 2020
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42. The Pristine Inner Galaxy Survey (PIGS) I: Tracing the kinematics of metal-poor stars in the Galactic bulge

Author: Arentsen, A, Starkenburg, E, Martin, NF, Hill, V, Ibata, R, Kunder, A, Schultheis, M, Venn, KA, Zucker, DB, Aguado, D, Carlberg, R, González Hernández, JI, Lardo, C, Longeard, N, Malhan, K, Navarro, JF, Sánchez-Janssen, R, Sestito, F, Thomas, G, Youakim, K, Lewis, GF, Simpson, JD, Wan, Z, Arentsen, A, Starkenburg, E, Martin, NF, Hill, V, Ibata, R, Kunder, A, Schultheis, M, Venn, KA, Zucker, DB, Aguado, D, Carlberg, R, González Hernández, JI, Lardo, C, Longeard, N, Malhan, K, Navarro, JF, Sánchez-Janssen, R, Sestito, F, Thomas, G, Youakim, K, Lewis, GF, Simpson, JD, and Wan, Z
Abstract: Our Galaxy is known to contain a central boxy/peanut-shaped bulge, yet the importance of a classical, pressure-supported component within the central part of the Milky Way is still being debated. It should be most visible at low metallicity, a regime that has not yet been studied in detail. Using metallicity-sensitive narrow-band photometry, the Pristine Inner Galaxy Survey (PIGS) has collected a large sample of metal-poor ([Fe/H]<-1.0$) stars in the inner Galaxy to address this open question. We use PIGS to trace the metal-poor inner Galaxy kinematics as function of metallicity for the first time. We find that the rotational signal decreases with decreasing [Fe/H], until it becomes negligible for the most metal-poor stars. Additionally, the velocity dispersion increases with decreasing metallicity for $-3.0<[Fe/H]<-0.5, with a gradient of-44 ± 4 km s-1 dex-1. These observations may signal a transition between Galactic components of different metallicities and kinematics, a different mapping on to the boxy/peanut-shaped bulge for former disc stars of different metallicities and/or the secular dynamical and gravitational influence of the bar on the pressure-supported component. Our results provide strong constraints on models that attempt to explain the properties of the inner Galaxy.
Published: 2020

43. Post-discharge hospital-associated venous thromboembolism.

Author: Bennett A., Wang H., Chee W.J., Hill V., Powell B., Chunilal S., Yuen H.L., Lim M.S., Scheinkestel C., Bennett A., Wang H., Chee W.J., Hill V., Powell B., Chunilal S., Yuen H.L., Lim M.S., and Scheinkestel C.
Abstract: Background: Hospital-associated venous thromboembolism (HA-VTE) morbidity and mortality has potentially been underestimated to date. Our centre is a tertiary, multi-campus health service which manages 265,000 admissions a year. Our VTE committee, comprising haematologists and other physicians, quality service representatives and pharmacists, routinely audits inpatient VTE (IP-VTE) for potential preventability against VTE prophylaxis guidelines. Over the study period, 81 IP-VTE were reviewed with 23% deemed potentially preventable however post-discharge VTE (PD-VTE) is not routinely captured. This is where VTE, presumably because of the index admission, is diagnosed after discharge, leading to re-admission. Aim(s): To compare the incidence of PD-VTE against IP-VTE and review PD-VTE characteristics, adherence to VTE prophylaxis guidelines and potential preventability. Method(s): A retrospective audit of ICD-10 Australian Modification discharge coding for lower limb deep vein thrombosis (LLDVT) and pulmonary embolism (PE) in adults between January 2018 and May 2019 at Monash Health. Cases were filtered for criteria such as presence of new, objectively confirmed, symptomatic VTE within 90 days of an index admission greater than 48 hours (Figure 1). Our VTE committee reviewed all eligible cases. Result(s): 948 encounters had VTE discharge coding. Of these, 891 were excluded with 57 eligible patients (Figure 1 and Table 1). Median age was 71 years (range, 26 to 92) and 32% with active cancer. Most index admissions were medical (61%) with a median of 19 days between admissions (range 2-86). VTE prophylaxis during the index admission was concordant with guidelines in 51%. Non-adherence included delayed prescription (5%), interruptions (23%), none (14%) and inadequate prescriptions (e.g. inappropriately dose-reduced enoxaparin 7%). Overall, VTE prophylaxis adherence was 68% with 35% VTE events deemed potentially preventable. There were no deaths from PD-VTE. Conclusion(s): O
Published: 2020

44. Cobalt and copper abundances in 56 Galactic bulge red giants

Author: Ernandes, H., Barbuy, B., Friaça, A., Hill, V., Zoccali, M., Minniti, D., Renzini, A., Ortolani, S., Ernandes, H., Barbuy, B., Friaça, A., Hill, V., Zoccali, M., Minniti, D., Renzini, A., and Ortolani, S.
Abstract: The Milky Way bulge is an important tracer of the early formation and chemical enrichment of the Galaxy. The abundances of different iron-peak elements in field bulge stars can give information on the nucleosynthesis processes that took place in the earliest supernovae. Cobalt (Z=27) and copper (Z=29) are particularly interesting.We aim to identify the nucleosynthesis processes responsible for the formation of the iron-peak elements Co and Cu. Methods. We derived abundances of the iron-peak elements cobalt and copper in 56 bulge giants, 13 of which were red clump stars. High-resolution spectra were obtained using FLAMES-UVES at the ESO Very Large Telescope by our group in 2000-2002, which appears to be the highest quality sample of high-resolution data on bulge red giants obtained in the literature to date. Over the years we have derived the abundances of C, N, O, Na, Al, Mg; the iron-group elements Mn and Zn; and neutron-capture elements. In the present work we derive abundances of the iron-peak elements cobalt and copper. We also compute chemodynamical evolution models to interpret the observed behaviour of these elements as a function of iron. The sample stars show mean values of [Co/Fe]~0.0 at all metallicities, and [Cu/Fe]~0.0 for [Fe/H]>-0.8 and decreasing towards lower metallicities with a behaviour of a secondary element. We conclude that [Co/Fe] varies in lockstep with [Fe/H], which indicates that it should be produced in the alpha-rich freezeout mechanism in massive stars. Instead [Cu/Fe] follows the behaviour of a secondary element towards lower metallicities, indicating its production in the weak s-process nucleosynthesis in He-burning and later stages. The chemodynamical models presented here confirm the behaviour of these two elements (i.e. [Co/Fe] vs. [Fe/H]~constant and [Cu/Fe] decreasing with decreasing metallicities)., Comment: Accepted to Astronomy & Astrophysics
Published: 2020
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45. The Pristine survey VIII: The metallicity distribution function of the Milky Way halo down to the extremely metal-poor regime

Author: Youakim, K., Starkenburg, E., Martin, N. F., Matijevic, G., Aguado, D. S., Prieto, C. Allende, Arentsen, A., Bonifacio, P., Carlberg, R. G., Hernández, J. I. González, Hill, V., Kordopatis, G., Lardo, C., Navarro, J. F., Jablonka, P., Janssen, R. Sánchez, Sestito, F., Thomas, G. F., Youakim, K., Starkenburg, E., Martin, N. F., Matijevic, G., Aguado, D. S., Prieto, C. Allende, Arentsen, A., Bonifacio, P., Carlberg, R. G., Hernández, J. I. González, Hill, V., Kordopatis, G., Lardo, C., Navarro, J. F., Jablonka, P., Janssen, R. Sánchez, Sestito, F., and Thomas, G. F.
Abstract: The Pristine survey uses narrow-band photometry to derive precise metallicities down to the extremely metal-poor regime ([Fe/H] < -3), and currently consists of over 4 million FGK-type stars over a sky area of $\sim 2~500\, \mathrm{deg}^2$. We focus our analysis on a subsample of $\sim 80~000$ main sequence turnoff stars with heliocentric distances between 6 and 20 kpc, which we take to be a representative sample of the inner halo. The resulting metallicity distribution function (MDF) has a peak at [Fe/H] = -1.6, and a slope of $\Delta$(LogN)/$\Delta[Fe/H] = 1.0 \pm 0.1$ in the metallicity range of -3.4 < [Fe/H] < -2.5. This agrees well with a simple closed-box chemical enrichment model in this range, but is shallower than previous spectroscopic MDFs presented in the literature, suggesting that there may be a larger proportion of metal-poor stars in the inner halo than previously reported. We identify the Monoceros/TriAnd/ACS/EBS/A13 structure in metallicity space in a low latitude field in the anticenter direction, and also discuss the possibility that the inner halo is dominated by a single, large merger event, but cannot strongly support or refute this idea with the current data. Finally, based on the MDF of field stars, we estimate the number of expected metal-poor globular clusters in the Milky Way halo to be 5.4 for [Fe/H] < -2.5 and 1.5 for [Fe/H] < -3, suggesting that the lack of low metallicity globular clusters in the Milky Way is not due simply to statistical undersampling., Comment: 17 pages, 12 figures, 5 tables, accepted for publication in MNRAS
Published: 2020
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46. Homogeneity in the early chemical evolution of the Sextans dwarf Spheroidal galaxy

Author: Lucchesi, R., Lardo, C., Primas, F., Jablonka, P., North, P., Battaglia, G., Starkenburg, E., Hill, V., Irwin, M., Francois, P., Shetrone, M., Tolstoy, E., Venn, K., Lucchesi, R., Lardo, C., Primas, F., Jablonka, P., North, P., Battaglia, G., Starkenburg, E., Hill, V., Irwin, M., Francois, P., Shetrone, M., Tolstoy, E., and Venn, K.
Abstract: We present the high-resolution spectroscopic analysis of two new extremely metal-poor stars (EMPS) candidates in the dwarf spheroidal galaxy Sextans. These targets were pre-selected from medium resolution spectra centered around the Ca II triplet in the near-infrared and followed-up at higher resolution with VLT/UVES. We confirm their low metallicities with [Fe/H]=-2.95 and [Fe/H]=-3.01, placing them among the most metal-poor stars known in Sextans. The abundances of 18 elements, including C, Na, the alpha-elements, Fe-peak, and neutron capture elements, are determined. In particular, we present the first measurements of Zn in a classical dwarf at extremely low metallicity. There has been previous hints of a large scatter in the abundance ratios of the Sextans stellar population around [Fe/H] -3 when compared to other galaxies. We took the opportunity of this work to re-analyse the full sample of EMPS and find a Milky-Way -like plateau and a normal dispersion at fixed metallicity., Comment: Accepted for publication in A&A. 14 pages, 10 figures
Published: 2020
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47. Post-discharge hospital-associated venous thromboembolism.

Author: Bennett A., Wang H., Chee W.J., Hill V., Powell B., Chunilal S., Yuen H.L., Lim M.S., Scheinkestel C., Bennett A., Wang H., Chee W.J., Hill V., Powell B., Chunilal S., Yuen H.L., Lim M.S., and Scheinkestel C.
Abstract: Background: Hospital-associated venous thromboembolism (HA-VTE) morbidity and mortality has potentially been underestimated to date. Our centre is a tertiary, multi-campus health service which manages 265,000 admissions a year. Our VTE committee, comprising haematologists and other physicians, quality service representatives and pharmacists, routinely audits inpatient VTE (IP-VTE) for potential preventability against VTE prophylaxis guidelines. Over the study period, 81 IP-VTE were reviewed with 23% deemed potentially preventable however post-discharge VTE (PD-VTE) is not routinely captured. This is where VTE, presumably because of the index admission, is diagnosed after discharge, leading to re-admission. Aim(s): To compare the incidence of PD-VTE against IP-VTE and review PD-VTE characteristics, adherence to VTE prophylaxis guidelines and potential preventability. Method(s): A retrospective audit of ICD-10 Australian Modification discharge coding for lower limb deep vein thrombosis (LLDVT) and pulmonary embolism (PE) in adults between January 2018 and May 2019 at Monash Health. Cases were filtered for criteria such as presence of new, objectively confirmed, symptomatic VTE within 90 days of an index admission greater than 48 hours (Figure 1). Our VTE committee reviewed all eligible cases. Result(s): 948 encounters had VTE discharge coding. Of these, 891 were excluded with 57 eligible patients (Figure 1 and Table 1). Median age was 71 years (range, 26 to 92) and 32% with active cancer. Most index admissions were medical (61%) with a median of 19 days between admissions (range 2-86). VTE prophylaxis during the index admission was concordant with guidelines in 51%. Non-adherence included delayed prescription (5%), interruptions (23%), none (14%) and inadequate prescriptions (e.g. inappropriately dose-reduced enoxaparin 7%). Overall, VTE prophylaxis adherence was 68% with 35% VTE events deemed potentially preventable. There were no deaths from PD-VTE. Conclusion(s): O
Published: 2020

48. Personality Processes

Author: Zeigler-Hill, Virgil, Shackelford, Todd K, Zeigler-Hill, V ( Virgil ), Shackelford, T K ( Todd K ), Lindner, Stefanie, Aschwanden, Damaris; https://orcid.org/0000-0002-0899-624X, Allemand, Mathias; https://orcid.org/0000-0002-1978-2044, Zeigler-Hill, Virgil, Shackelford, Todd K, Zeigler-Hill, V ( Virgil ), Shackelford, T K ( Todd K ), Lindner, Stefanie, Aschwanden, Damaris; https://orcid.org/0000-0002-0899-624X, and Allemand, Mathias; https://orcid.org/0000-0002-1978-2044
Published: 2020

49. Developmental changes in personality traits

Author: Zeigler-Hill, Virgil, Shackelford, Todd K, Zeigler-Hill, V ( Virgil ), Shackelford, T K ( Todd K ), Gerl, Chantal Simone, Stieger, Mirjam Nadine; https://orcid.org/0000-0002-9426-6445, Allemand, Mathias; https://orcid.org/0000-0002-1978-2044, Zeigler-Hill, Virgil, Shackelford, Todd K, Zeigler-Hill, V ( Virgil ), Shackelford, T K ( Todd K ), Gerl, Chantal Simone, Stieger, Mirjam Nadine; https://orcid.org/0000-0002-9426-6445, and Allemand, Mathias; https://orcid.org/0000-0002-1978-2044
Published: 2020

50. Scar Model

Author: Zeigler-Hill, Virgil, Shackelford, Todd K, Zeigler-Hill, V ( Virgil ), Shackelford, T K ( Todd K ), Allemand, Mathias; https://orcid.org/0000-0002-1978-2044, Grünenfelder-Steiger, Andrea E, Flückiger, Christoph; https://orcid.org/0000-0003-3058-5815, Zeigler-Hill, Virgil, Shackelford, Todd K, Zeigler-Hill, V ( Virgil ), Shackelford, T K ( Todd K ), Allemand, Mathias; https://orcid.org/0000-0002-1978-2044, Grünenfelder-Steiger, Andrea E, and Flückiger, Christoph; https://orcid.org/0000-0003-3058-5815
Published: 2020

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