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1. CO radial gradients in the bulge of M31

Author: La Barbera, F., Vazdekis, A., Pasquali, A., Heidt, J., Gargiulo, A., Eftekhari, E., La Barbera, F., Vazdekis, A., Pasquali, A., Heidt, J., Gargiulo, A., and Eftekhari, E.
Abstract: We present new H- and K-band spectroscopy for the bulge of M31, taken with the LUCI spectrograph at the Large Binocular Telescope (LBT). We studied radial trends of CO absorption features (namely, CO1.58, CO1.60, CO1.64, CO1.66, CO1.68, CO2.30, CO2.32, CO2.35) in the bulge of M31, out to a galactocentric distance of 100'' (380pc). We find that most COs do not exhibit a strong radial gradient, despite the strong metallicity gradient inferred from the optical spectral range, except for CO1.64, showing a steep increase in the center. We compared the observed line strengths to predictions of different state-of-the-art stellar population models, including an updated version of EMILES models, which also uses the extended IRTF spectral library. The observed COs are close to models' predictions, but in some models they turn out to be underestimated. We find that the lack of radial gradients is due to the combination of increasing CO strength with metallicity and C abundance, and decreasing CO strength with IMF slope and O abundance. We speculate that the steep gradient of CO1.64 might be due to Na overabundance. Remarkably, we were able to fit, at the same time, optical indices and all the NIR COs except for CO1.68, leaving abundance ratios (i.e., [C/Fe], [O/Fe], and [Mg/Fe]) as free-fitting parameters, imposing age and metallicity constraints from the optical, with no significant contribution from intermediate-age populations. For the majority of the bulge, we find [Mg/Fe]~0.15dex, [O/Fe] larger than [Mg/Fe] (by ~0.1dex), and C abundance consistent with that of Mg. In the central (few arcsec) region, we still find an enhancement of O and Mg, but significantly lower [C/Fe]. We find that the COs' line strengths of the bulge are significantly lower than those of massive galaxies, possibly because of a difference in carbon abundance, as well as, to some extent, total metallicity., Comment: 20 pages, 10 figures, accepted for publication on A&A
Published: 2024

2. 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

3. Stellar metallicity from optical and UV spectral indices: Test case for WEAVE-StePS

Author: Ditrani, F, Longhetti, M, La Barbera, F, Iovino, A, Costantin, L, Zibetti, S, Gallazzi, A, Fossati, M, Angthopo, J, Ascasibar, Y, Poggianti, B, Sanchez-Blazquez, P, Balcells, M, Bianconi, M, Bolzonella, M, Cassara, L, Cucciati, O, Dalton, G, Ferre-Mateu, A, Garcia-Benito, R, Granett, B, Gullieuszik, M, Ikhsanova, A, Jin, S, Knapen, J, Mcgee, S, Mercurio, A, Morelli, L, Moretti, A, Murphy, D, Pizzella, A, Pozzetti, L, Spiniello, C, Tortora, C, Trager, S, Vazdekis, A, Vergani, D, Vulcani, B, Ditrani F. R., Longhetti M., La Barbera F., Iovino A., Costantin L., Zibetti S., Gallazzi A., Fossati M., Angthopo J., Ascasibar Y., Poggianti B., Sanchez-Blazquez P., Balcells M., Bianconi M., Bolzonella M., Cassara L. P., Cucciati O., Dalton G., Ferre-Mateu A., Garcia-Benito R., Granett B., Gullieuszik M., Ikhsanova A., Jin S., Knapen J. H., McGee S., Mercurio A., Morelli L., Moretti A., Murphy D., Pizzella A., Pozzetti L., Spiniello C., Tortora C., Trager S. C., Vazdekis A., Vergani D., Vulcani B., Ditrani, F, Longhetti, M, La Barbera, F, Iovino, A, Costantin, L, Zibetti, S, Gallazzi, A, Fossati, M, Angthopo, J, Ascasibar, Y, Poggianti, B, Sanchez-Blazquez, P, Balcells, M, Bianconi, M, Bolzonella, M, Cassara, L, Cucciati, O, Dalton, G, Ferre-Mateu, A, Garcia-Benito, R, Granett, B, Gullieuszik, M, Ikhsanova, A, Jin, S, Knapen, J, Mcgee, S, Mercurio, A, Morelli, L, Moretti, A, Murphy, D, Pizzella, A, Pozzetti, L, Spiniello, C, Tortora, C, Trager, S, Vazdekis, A, Vergani, D, Vulcani, B, Ditrani F. R., Longhetti M., La Barbera F., Iovino A., Costantin L., Zibetti S., Gallazzi A., Fossati M., Angthopo J., Ascasibar Y., Poggianti B., Sanchez-Blazquez P., Balcells M., Bianconi M., Bolzonella M., Cassara L. P., Cucciati O., Dalton G., Ferre-Mateu A., Garcia-Benito R., Granett B., Gullieuszik M., Ikhsanova A., Jin S., Knapen J. H., McGee S., Mercurio A., Morelli L., Moretti A., Murphy D., Pizzella A., Pozzetti L., Spiniello C., Tortora C., Trager S. C., Vazdekis A., Vergani D., and Vulcani B.
Abstract: Context. The upcoming generation of optical spectrographs on four meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide high-quality spectra for thousands of galaxies. These data will allow us to examine of the stellar population properties at intermediate redshift, an epoch that remains unexplored by large and deep surveys. Aims. We assess our capability to retrieve the mean stellar metallicity in galaxies at different redshifts and signal-to-noise ratios (S/N), while simultaneously exploiting the ultraviolet (UV) and optical rest-frame wavelength coverage. Methods. The work is based on a comprehensive library of spectral templates of stellar populations, covering a wide range of age and metallicity values and built assuming various star formation histories, to cover an observable parameter space with diverse chemical enrichment histories and dust attenuation. We took into account possible observational errors, simulating realistic observations of a large sample of galaxies carried out with WEAVE at the William Herschel Telescope at different redshifts and S/N values. We measured all the available and reliable indices on the simulated spectra and on the comparison library. We then adopted a Bayesian approach to compare the two sets of measurements in order to obtain the probability distribution of stellar metallicity with an accurate estimate of the uncertainties. Results. The analysis of the spectral indices has shown how some mid-UV indices, such as BL3580 and Fe3619, can provide reliable constraints on stellar metallicity, along with optical indicators. The analysis of the mock observations has shown that even at S/N = 10, the metallicity can be derived within 0.3 dex, in particular, for stellar populations older than 2 Gyr. The S/N value plays a crucial role in the uncertainty of the estimated metallicity and so, the differences between S/N = 10 and S/N = 30 are quit
Published: 2023

4. WEAVE-StePS: A stellar population survey using WEAVE at WHT

Author: Iovino, A, Poggianti, B, Mercurio, A, Longhetti, M, Bolzonella, M, Busarello, G, Gullieuszik, M, La Barbera, F, Merluzzi, P, Morelli, L, Tortora, C, Vergani, D, Zibetti, S, Haines, C, Costantin, L, Ditrani, F, Pozzetti, L, Angthopo, J, Balcells, M, Bardelli, S, Benn, C, Bianconi, M, Cassara, L, Corsini, E, Cucciati, O, Dalton, G, Ferre-Mateu, A, Fossati, M, Gallazzi, A, Garcia-Benito, R, Granett, B, Gonzalez Delgado, R, Ikhsanova, A, Iodice, E, Jin, S, Knapen, J, Mcgee, S, Moretti, A, Murphy, D, Peralta De Arriba, L, Pizzella, A, Sanchez-Blazquez, P, Spiniello, C, Talia, M, Trager, S, Vazdekis, A, Vulcani, B, Zucca, E, Iovino A., Poggianti B. M., Mercurio A., Longhetti M., Bolzonella M., Busarello G., Gullieuszik M., La Barbera F., Merluzzi P., Morelli L., Tortora C., Vergani D., Zibetti S., Haines C. P., Costantin L., Ditrani F. R., Pozzetti L., Angthopo J., Balcells M., Bardelli S., Benn C. R., Bianconi M., Cassara L. P., Corsini E. M., Cucciati O., Dalton G., Ferre-Mateu A., Fossati M., Gallazzi A., Garcia-Benito R., Granett B., Gonzalez Delgado R. M., Ikhsanova A., Iodice E., Jin S., Knapen J. H., Mcgee S., Moretti A., Murphy D. N. A., Peralta De Arriba L., Pizzella A., Sanchez-Blazquez P., Spiniello C., Talia M., Trager S. C., Vazdekis A., Vulcani B., Zucca E., Iovino, A, Poggianti, B, Mercurio, A, Longhetti, M, Bolzonella, M, Busarello, G, Gullieuszik, M, La Barbera, F, Merluzzi, P, Morelli, L, Tortora, C, Vergani, D, Zibetti, S, Haines, C, Costantin, L, Ditrani, F, Pozzetti, L, Angthopo, J, Balcells, M, Bardelli, S, Benn, C, Bianconi, M, Cassara, L, Corsini, E, Cucciati, O, Dalton, G, Ferre-Mateu, A, Fossati, M, Gallazzi, A, Garcia-Benito, R, Granett, B, Gonzalez Delgado, R, Ikhsanova, A, Iodice, E, Jin, S, Knapen, J, Mcgee, S, Moretti, A, Murphy, D, Peralta De Arriba, L, Pizzella, A, Sanchez-Blazquez, P, Spiniello, C, Talia, M, Trager, S, Vazdekis, A, Vulcani, B, Zucca, E, Iovino A., Poggianti B. M., Mercurio A., Longhetti M., Bolzonella M., Busarello G., Gullieuszik M., La Barbera F., Merluzzi P., Morelli L., Tortora C., Vergani D., Zibetti S., Haines C. P., Costantin L., Ditrani F. R., Pozzetti L., Angthopo J., Balcells M., Bardelli S., Benn C. R., Bianconi M., Cassara L. P., Corsini E. M., Cucciati O., Dalton G., Ferre-Mateu A., Fossati M., Gallazzi A., Garcia-Benito R., Granett B., Gonzalez Delgado R. M., Ikhsanova A., Iodice E., Jin S., Knapen J. H., Mcgee S., Moretti A., Murphy D. N. A., Peralta De Arriba L., Pizzella A., Sanchez-Blazquez P., Spiniello C., Talia M., Trager S. C., Vazdekis A., Vulcani B., and Zucca E.
Abstract: Context. The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide valuable opportunities for forthcoming galaxy surveys through their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage. Aims. WEAVE is a new wide-field spectroscopic facility mounted on the 4.2 m William Herschel Telescope in La Palma. WEAVE-StePS is one of the five extragalactic surveys that will use WEAVE during its first five years of operations. It will observe galaxies using WEAVE MOS (∼950 fibres distributed across a field of view of ∼3 square degrees on the sky) in low-resolution mode (R ∼ 5000, spanning the wavelength range 3660-9590 Å). Methods. WEAVE-StePS will obtain high-quality spectra (S/N ∼ 10 Å -1 at R ∼ 5000) for a magnitude-limited (IAB = 20.5) sample of ∼25 000 galaxies, the majority selected at z ≥ 0.3. The survey goal is to provide precise spectral measurements in the crucial interval that bridges the gap between LEGA-C and SDSS data. The wide area coverage of ∼25 square degrees will enable us to observe galaxies in a variety of environments. The ancillary data available in each of the observed fields (including X-ray coverage, multi-narrow-band photometry and spectroscopic redshift information) will provide an environmental characterisation for each observed galaxy. Results. This paper presents the science case of WEAVE-StePS, the fields to be observed, the parent catalogues used to define the target sample, and the observing strategy that was chosen after a forecast of the expected performance of the instrument for our typical targets. Conclusions. WEAVE-StePS will go back further in cosmic time than SDSS, extending its reach to encompass more than ∼6 Gyr. This is nearly half of the age of the Universe. The spectral and redshift range covered by WEAVE-StePS will open a new observational window by continuously tracing the evolutionary path of galaxies in the largely unexplored intermediate
Published: 2023

5. INSPIRE: INvestigating Stellar Population In RElics V. A catalogue of ultra-compact massive galaxies outside the local Universe and their degree of relicness

Author: Spiniello, C., D'Ago, G., Coccato, L., Hartke, J., Tortora, C., Ferré-Mateu, A., Pulsoni, C., Cappellari, M., Maksymowicz-Maciata, M., Arnaboldi, M., Bevacqua, D., Gallazzi, A., Hunt, L. K., La Barbera, F., Martín-Navarro, I., Napolitano, N. R., Radovich, M., Saracco, P., Scognamiglio, D., Spavone, M., Zibetti, S., Spiniello, C., D'Ago, G., Coccato, L., Hartke, J., Tortora, C., Ferré-Mateu, A., Pulsoni, C., Cappellari, M., Maksymowicz-Maciata, M., Arnaboldi, M., Bevacqua, D., Gallazzi, A., Hunt, L. K., La Barbera, F., Martín-Navarro, I., Napolitano, N. R., Radovich, M., Saracco, P., Scognamiglio, D., Spavone, M., and Zibetti, S.
Abstract: This paper presents the third data release of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 52 ultra-compact massive galaxies (UCMGs) observed with the X-Shooter spectrograph. We measure integrated stellar velocity dispersion, [Mg/Fe] abundances, ages, and metallicities for all the INSPIRE objects. We thus infer star formation histories and confirm the existence of a degree of relicness (DoR), defined in terms of the fraction of stellar mass formed by $z=2$, the time at which a galaxy has assembled 75\% of its mass, and the final assembly time. Objects with a high DoR assembled their stellar mass at early epochs, while low-DoR objects show a non-negligible fraction of later-formed populations and hence a spread in ages and metallicities. A higher DoR correlates with larger [Mg/Fe], super-solar metallicity, and larger velocity dispersion values. The 52 UMCGs span a large range of DoR from 0.83 to 0.06, with 38 of them having formed more than 75\% of their mass by $z=2$. Of these, nine are extreme relics (DoR$>0.7$), since they formed the totality ($>99\%$) of their stellar mass by redshift $z=2$. The remaining 14 UCMGs cannot be considered relics, as they are characterised by more extended star formation histories. With INSPIRE, we built the first sizeable sample of relics outside the local Universe, up to $z\sim0.4$, increasing the number of confirmed relics by a factor of $>10$, and opening up an important window to explain the mass assembly of massive galaxies in the high-z Universe., Comment: accepted for publication on MNRAS, 20 pages, 15 figures, 3 tables
Published: 2023

6. Stellar metallicity from optical and UV spectral indices: Test case for WEAVE-StePS

Author: Ditrani, F. R., Longhetti, M., La Barbera, F., Iovino, A., Costantin, L., Zibetti, S., Gallazzi, A., Fossati, M., Angthopo, J., Ascasibar, Y., Poggianti, B., Sánchez-Blázquez, P., Balcells, M., Bianconi, M., Bolzonella, M., Cassarà, L. P., Cucciati, O., Dalton, G., Ferré-Mateu, A., García-Benito, R., Granett, B., Gullieuszik, M., Ikhsanova, A., Jin, S., Knapen, J. H., McGee, S., Mercurio, A., Morelli, L., Moretti, A., Murphy, D., Pizzella, A., Pozzetti, L., Spiniello, C., Tortora, C., Trager, S. C., Vazdekis, A., Vergani, D., Vulcani, B., Ditrani, F. R., Longhetti, M., La Barbera, F., Iovino, A., Costantin, L., Zibetti, S., Gallazzi, A., Fossati, M., Angthopo, J., Ascasibar, Y., Poggianti, B., Sánchez-Blázquez, P., Balcells, M., Bianconi, M., Bolzonella, M., Cassarà, L. P., Cucciati, O., Dalton, G., Ferré-Mateu, A., García-Benito, R., Granett, B., Gullieuszik, M., Ikhsanova, A., Jin, S., Knapen, J. H., McGee, S., Mercurio, A., Morelli, L., Moretti, A., Murphy, D., Pizzella, A., Pozzetti, L., Spiniello, C., Tortora, C., Trager, S. C., Vazdekis, A., Vergani, D., and Vulcani, B.
Abstract: The upcoming generation of optical spectrographs on four meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide high-quality spectra for thousands of galaxies. These data will allow us to examine of the stellar population properties at intermediate redshift, an epoch that remains unexplored by large and deep surveys. We assess our capability to retrieve the mean stellar metallicity in galaxies at different redshifts and S/N, while simultaneously exploiting the UV and optical rest-frame wavelength coverage. The work is based on a comprehensive library of spectral templates of stellar populations, covering a wide range of age and metallicity values and built assuming various SFHs. We simulated realistic observations of a large sample of galaxies carried out with WEAVE at the WHT at different redshifts and S/N values. We measured all the reliable indices on the simulated spectra and on the comparison library. We then adopted a Bayesian approach to obtain the probability distribution of stellar metallicity. The analysis of the spectral indices has shown how some mid-UV indices can provide reliable constraints on stellar metallicity, along with optical indicators. The analysis of the mock observations has shown that even at S/N=10, the metallicity can be derived within 0.3 dex, in particular, for stellar populations older than 2 Gyr. Our results are in good agreement with other theoretical and observational works in the literature and show how the UV indicators can be advantageous in constraining metallicities. This is very promising for the upcoming surveys carried out with new, highly multiplexed, large-field spectrographs, such as StePS at the WEAVE and 4MOST, which will provide spectra of thousands of galaxies covering large spectral ranges at relatively high S/N., Comment: 16 pages, 14 figures. Submitted 31/03/2023, Accepted 20/07/2023
Published: 2023
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7. INSPIRE: INvestigating Stellar Population In RElics III. Second data release (DR2): testing the systematics on the stellar velocity dispersion

Author: D'Ago, G., Spiniello, C., Coccato, L., Tortora, C., La Barbera, F., Arnaboldi, M., Bevacqua, D., Ferré-Mateu, A., Gallazzi, A., Hartke, J., Hunt, L. K., Martín-Navarro, I., Napolitano, N. R., Pulsoni, C., Radovich, M., Saracco, P., Scognamiglio, D., Zibetti, S., D'Ago, G., Spiniello, C., Coccato, L., Tortora, C., La Barbera, F., Arnaboldi, M., Bevacqua, D., Ferré-Mateu, A., Gallazzi, A., Hartke, J., Hunt, L. K., Martín-Navarro, I., Napolitano, N. R., Pulsoni, C., Radovich, M., Saracco, P., Scognamiglio, D., and Zibetti, S.
Abstract: This is the second data release (DR2) of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 21 new systems with observations completed before March 2022. For each system, we release four one-dimensional (1D) spectra to the ESO Science Archive, one spectrum for each arm of the X-Shooter spectrograph. In this paper, we focus on the line-of-sight velocity distribution, measuring integrated stellar velocity dispersions from the spectra, and assessing their robustness and the associated uncertainties. For each of the 21 new systems, we systematically investigated the effect of the parameters and set-ups of the full spectral fitting on the stellar velocity dispersion ($\sigma$) measurements. In particular, we tested how $\sigma$ changes when several parameters of the fit as well as the resolution and spectral coverage of the input spectra are varied. We found that the effect that causes the largest systematic uncertainties on $\sigma$ is the wavelength range used for the fit, especially for spectra with a lower signal-to-noise ratio (S/N $\leq$ 30). When using blue wavelengths (UVB arm) one generally underestimates the velocity dispersion (by $\sim$15 km/s). The values obtained from the near-IR (NIR) arm present a larger scatter because the quality of the spectra is lower. We finally compared our results with those in literature, finding a very good agreement overall. Joining results obtained in DR1 with those presented here, INSPIRE contains 40 ultra-compact massive galaxies, corresponding to 75% of the whole survey. By plotting these systems in a stellar mass-velocity dispersion diagram, we identify at least four highly reliable relic candidates among the new systems. Their velocity dispersion is larger than that of normal-sized galaxies of similar stellar mass., Comment: Accepted for publication, and in press on A&A
Published: 2023
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8. Post-anaesthesia pulmonary complications after use of muscle relaxants (POPULAR): a multicentre, prospective observational study

Author: Kirmeier, E, Eriksson, L, Lewald, H, Jonsson Fagerlund, M, Hoeft, A, Hollmann, M, Meistelman, C, Hunter, J, Ulm, K, Blobner, M, Abad Gurumeta, A, Abernethy, C, Abigail, P, Achaibar, K, Adam, E, Afshari, A, Agudelo Montoya, M, Akgun, F, Aletti, G, Alkis, N, Allan, K, Allan, A, Allaouchiche, B, Allcock, C, Almasy, E, Amey, I, Amigoni, M, Andersen, E, Andersson, P, Anipchenko, N, Antunes, P, Armstrong, E, Aslam, T, Aslin, B, Assuncao, J, Ausserer, J, Avvai, M, Awad, N, Ayas Montero, B, Ayuso, M, Azevedo, P, Badarau, V, Badescu, R, Baiardo Redaelli, M, Baird, C, Baird, Y, Baker, T, Balaji, P, Balan, C, Balandin, A, Balescu-Arion, C, Baliuliene, V, Baltasar Isabel, J, Baluch, S, Bandrabur, D, Bankewitz, C, Barber, K, Barbera, F, Barcraft-Barnes, H, Barletti, V, Barnett, G, Baron, K, Barros, A, Barsan, V, Bartlett, P, Batistaki, C, Baumgarten, G, Baytas, V, Beauchamp, N, Becerra Cayetano, I, Bell, S, Bellandi, M, Belletti, A, Belmonte Cuenca, J, Benitez-Cano, A, Beretta, L, Berger, M, Bergmann, N, Bergmark, K, Bermudez Lopez, M, Bernotaite, M, Beurskens, C, Bidd, H, Bifulco, F, Bignami, E, Bilic, A, Bilskiene, D, Bischoff, P, Bishop, L, Bjonness, T, Blaylock, H, Blethyn, K, Blincoe, T, Blokhin, I, Blunt, N, Boer, C, Bois, G, Bonicolini, E, Booth, J, Borecka-Kedzierska, M, Borstnar, K, Borys, M, Boselli, E, Bouvet, L, Bouwman, A, Bowen, L, Bowrey, S, Boxall, L, Bozic, T, Bradley, T, Branco, T, Brazzi, L, Brazzoni, M, Brear, T, Brogly, N, Brohi, F, Broms, J, Bubliauskas, A, Bucolo, G, Buerkle, H, Buggy, D, Buhre, W, Bukauskas, T, Butturini, F, Byttner, A, Cabrera Diaz, I, Calderon, A, Calhau, R, Callejo, A, Cammu, G, Campesato, M, Can, O, Candeias, M, Cantor, A, Carise, E, Carmona, C, Carreteiro, J, Carrieri, C, Carter, A, Casal, M, Casanova, I, Cascella, M, Casero, L, Casiraghi, G, Castelo-Branco, L, Castro Arranz, C, Cernea, D, Cervantes, J, Chandler, B, Charnock, R, Chatzimicali, A, Chinery, E, Chishti, A, Chondhury, P, Christie, E, Christodoudiles, G, Ciardo, S, Cimpeanu, L, Cindea, I, Cinnella, G, Clark, S, Clayton, M, Cocu, S, Collyer, T, Colvin, C, Cope, S, Copeta, F, Copotoiu, S, Correia de Barros, F, Corso, R, Cortegiani, A, Costa, G, Cowton, A, Cox, N, Craig, J, Cricca, V, Cronin, J, Cunha, M, Cuomo, A, Curley, K, Czuczwar, M, Dabrowska, D, Damster, S, Danguy des Deserts, M, Daniliuc, A, Danninger, T, Darwish, I, Dascalu, C, Davies, K, Davies, S, De Boer, H, De Flaviis, A, De Selincourt, G, Deana, C, Debaene, B, Debreceni, G, Dedhia, J, Delgado Garcia, I, Della Rocca, G, Delroy-Buelles, L, Desai, T, Dhillon, P, Di Giacinto, I, Di Mauro, P, Diaz Gomez, T, Dimitrovski, A, Dinic, V, Dirzu, D, Divander, M, Dolinar, J, Domingues, S, Doolan, J, Downes, C, Dragoescu, N, Droc, G, Dum, E, Dumitrescu, A, Duncan, L, Dzurnakova, P, Eberl, S, Edwards, J, Edwards, M, Ekelund, K, Ekengren, P, Elghouty, E, Ellerkmann, R, Ellis, H, Elme, A, Ernst, T, Errando, C, Estenes, S, Ewaldsson, C, Farid, N, Featherstone, J, Febres, D, Fedorov, S, Feggeler, J, Feijten, P, Fellmann, T, Fernandez Candil, J, Fernandez Castineira, A, Fernandez Castineira, J, Fernando, A, Ferrando, C, Ferreira, L, Ferreira, P, Feyling, A, Filipescu, D, Fleischer, A, Floris, L, Foerster, U, Fox, B, Franke, U, Frasca, D, Frey, C, Frost, V, Fullin, G, Fumagalli, J, Furneval, J, Fusari, M, Gallacher, S, Galushka, S, Gambale, G, Gambino, I, Garcia-Perez, M, Garg, S, Garlak, J, Gavranovic, Z, Gavrilov, R, Gaynor, L, Gecaj Gashi, A, Georghiou, M, Gerjevic, B, Gferer, G, Giarratano, A, Gibson, A, Gievski, V, Giles, J, Gillberg, L, Gilowska, K, Gilsanz Rodriguez, F, Gioia, A, Giovannoni, C, Girotra, V, Gkinas, D, Gkiokas, G, Godoroja, D, Goebel, U, Goel, V, Gonzalez, M, Goranovic, T, Gornik-Wlaszczuk, E, Gosavi, S, Gottfridsson, P, Gottschalk, A, Granell, M, Granstrom, A, Grassetto, A, Greenwood, A, Grigoras, I, Grintescu, I, Gritsan, A, Gritsan, G, Grynyuk, A, Guadagnin, G, Guarnieri, M, Guclu, C, Guerrero Diez, M, Gunenc, F, Gunther, U, Gupta, P, Guttenthaler, V, Hack, 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Oduro-Dominah, L, Oldner, A, Oliveira, I, Ologoiu, D, Oloktsidou, I, O'Reilly, R, Orlando, A, Ovezov, A, Ozbilgin, S, Paal, P, Padin Barreiro, L, Palugniok, R, Papaioannou, A, Papapostolou, K, Paranthaman, P, Pardey Bracho, G, Parente, S, Parfeni, A, Pasin, L, Passey, S, Pastor, E, Patch, S, Patil, A, Paunescu, M, Pehboeck, D, Pereira, M, Pereira, C, Perez Caballero, P, Perez Garcia, A, Perez Soto, A, Perez Tejero, G, Perez-Cerda, F, Pesenti, A, Petta, R, Philippe, S, Pickering, D, Pico Veloso, J, Pina, P, Pinho-Oliveira, V, Pinol, S, Pinto, R, Pistidda, L, Pitterle, M, Piwowarczyk, P, Plotnikova, O, Pohl, H, Poldermann, J, Polkovicova, L, Pompei, L, Popescu, M, Popovic, R, Pota, V, Potocnik, M, Potrec, B, Potter, A, Pramod, N, Prchalova, M, Preckel, B, Pugh, R, Pulletz, M, Radoeshki, A, Rafi, A, Ragazzi, R, Raineri Santi, M, Rajamanickam, T, Rajput, Z, Ramachandran, R, Ramasamy, R, Ramessur, S, Rao, R, Rasmussen, A, Rato, A, Razaque, U, Real Navacerrada, M, Reavley, C, Reid, J, 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Smith, N, Smith, T, Smitz, C, Smole, D, Sojcic, N, Soler Pedrola, M, Somanath, S, Sonksen, J, Sorella, M, Sormus, A, Soro, M, Soto, C, Spada, A, Spadaro, S, Spaeth, J, Sparr, H, Spielmann, A, Spindler-Vesel, A, Stamelos, M, Stancombe L, L, Stanculescu, A, Standl, T, Standley, T, Stanek, O, Stanisavljevic, S, Starczewska, M, Stauble, C, Steen, J, Stefan, O, Stell, E, Stera, C, Stevens, M, Stoerckel, M, Stosic, B, Stourac, P, Stroumpoulis, K, Struck, R, Suarez de la Rica, A, Sultanpori, A, Sundara Rajan, R, Suying, O, Svensen, C, Swan, L, Syrogianni, P, Sysiak, J, Szederjesi, J, Taddei, S, Tan Hao, E, Tanou, V, Tarabova, K, Tardaguila Sancho, P, Tarroso, M, Tartaglione, M, Taylor, E, Tbaily, L, Telford, R, Terenzoni, M, Theodoraki, K, Thornley, H, Tiganiuc, L, Toim, H, Tomescu, D, Tommasino, C, Toni, J, Toninelli, A, Toretti, I, Townley, S, Trepenaitis, D, Trethowan, B, Tsaousi, G, Tsiftsi, A, Tudor, A, Turan, G, Turhan, S, Unic-Stojanovic, D, Unterbuchner, C, Unzueta, C, Uranjek, J, Ursic, T, Vaida, S, Valldeperas Ferrer, S, Valldeperas Hernandez, M, Valsamidis, D, Van Beek, R, Van dasselaer, N, Van Der Beek, T, Van Duivenvoorde, Y, van Klei, W, Van Poorter, F, Van Zaane, B, Van Zundert, T, Van Zyl, R, Vargas Munoz, A, Varsani, N, Vasconcelos, P, Vassilakis, G, Vecchiatini, T, Vecera, L, Vercauteren, M, Verdouw, B, Verheyen, V, Verri, M, Vicari Sottosanti, L, Vico, M, Vidal Mitjans, P, Vilardi, A, Vissicchio, D, Vitale, G, Vitkovic, B, Vizcaychipi, M, Voicu, A, Voje, M, Volfova, I, Volta, C, Von Lutterotti, T, von Tiesenhausen, A, Vrecic-Slabe, S, Vukcevic, D, Vukovic, R, Vullo, P, Wade, A, Wallberg, H, Wallden, J, Wallner, J, Walther Sturesson, L, Watson, D, Weber, S, Wegiel Leskiewiq, A, Weller, D, Wensing, C, Werkmann, M, Westberg, H, Wikstrom, E, Williams, B, Wilson, R, Wirth, S, Wittmann, M, Wood, L, Wright, S, Zachoval, C, Zambon, M, Zampieri, S, Zampone, S, Zangrillo, A, Zani, G, Zavackiene, A, Zieglerder, R, Zonneveldt, H, Zsisku, L, Zucker, T, Zukowski, M, Zuleika, M, Zupaneie, D, Kirmeier E., Eriksson L. I., Lewald H., Jonsson Fagerlund M., Hoeft A., Hollmann M., Meistelman C., Hunter J. M., Ulm K., Blobner M., Abad Gurumeta A., Abernethy C., Abigail P., Achaibar K., Adam E., Afshari A., Agudelo Montoya M. E., Akgun F. N., Aletti G., Alkis N., Allan K., Allan A., Allaouchiche B., Allcock C., Almasy E., Amey I., Amigoni M., Andersen E., Andersson P., Anipchenko N., Antunes P., Armstrong E., Aslam T. N., Aslin B., Assuncao J. P., Ausserer J., Avvai M., Awad N., Ayas Montero B., Ayuso M., Azevedo P., Badarau V., Badescu R., Baiardo Redaelli M., Baird C., Baird Y., Baker T., Balaji P., Balan C., Balandin A., Balescu-Arion C., Baliuliene V., Baltasar Isabel J., Baluch S. N., Bandrabur D., Bankewitz C., Barber K., Barbera F., Barcraft-Barnes H., Barletti V., Barnett G., Baron K., Barros A., Barsan V., Bartlett P., Batistaki C., Baumgarten G., Baytas V., Beauchamp N., Becerra Cayetano I. A., Bell S., Bellandi M., Belletti A., Belmonte Cuenca J., Benitez-Cano A., Beretta L., Berger M., Bergmann N., Bergmark K., Bermudez Lopez M., Bernotaite M., Beurskens C., Bidd H., Bifulco F., Bignami E., Bilic A., Bilskiene D., Bischoff P., Bishop L., Bjonness T., Blaylock H., Blethyn K., Blincoe T., Blokhin I., Blunt N., Boer C., Bois G., Bonicolini E., Booth J., Borecka-Kedzierska M., Borstnar K., Borys M., Boselli E., Bouvet L., Bouwman A., Bowen L., Bowrey S., Boxall L., Bozic T., Bradley T., Branco T., Brazzi L., Brazzoni M., Brear T., Brogly N., Brohi F., Broms J., Bubliauskas A., Bucolo G. E., Buerkle H., Buggy D., Buhre W., Bukauskas T., Butturini F., Byttner A., Cabrera Diaz I., Calderon A., Calhau R., Callejo A., Cammu G., Campesato M., Can O. S., Candeias M., Cantor A., Carise E., Carmona C., Carreteiro J., Carrieri C., Carter A., Casal M., Casanova I., Cascella M., Casero L. M., Casiraghi G. M., Castelo-Branco L., Castro Arranz C., Cernea D. D., Cervantes J., Chandler B., Charnock R., Chatzimicali A., Chinery E., Chishti A., Chondhury P., Christie E., Christodoudiles G., Ciardo S., Cimpeanu L., Cindea I., Cinnella G., Clark S., Clayton M., Cocu S., Collyer T., Colvin C., Cope S., Copeta F., Copotoiu S. -M., Correia de Barros F., Corso R. M., Cortegiani A., Costa G., Cowton A., Cox N., Craig J., Cricca V., Cronin J., Cunha M., Cuomo A., Curley K., Czuczwar M., Dabrowska D., Damster S., Danguy des Deserts M., Daniliuc A., Danninger T., Darwish I., Dascalu C., Davies K., Davies S., De Boer H., De Flaviis A., De Selincourt G., Deana C., Debaene B., Debreceni G., Dedhia J., Delgado Garcia I., Della Rocca G., Delroy-Buelles L., Desai T., Dhillon P., Di Giacinto I., Di Mauro P., Diaz Gomez T. V., Dimitrovski A., Dinic V., Dirzu D. -S., Divander M. B., Dolinar J., Domingues S., Doolan J., Downes C., Dragoescu N. A., Droc G., Dum E., Dumitrescu A., Duncan L., Dzurnakova P., Eberl S., Edwards J., Edwards M., Ekelund K., Ekengren P., Elghouty E., Ellerkmann R., Ellis H., Elme A., Ernst T., Errando C. L., Estenes S., Ewaldsson C., Farid N., Featherstone J., Febres D., Fedorov S., Feggeler J., Feijten P., Fellmann T., Fernandez Candil J., Fernandez Castineira A., Fernandez Castineira J., Fernando A., Ferrando C., Ferreira L., Ferreira P., Feyling A., Filipescu D., Fleischer A., Floris L., Foerster U., Fox B., Franke U., Frasca D., Frey C., Frost V., Fullin G., Fumagalli J., Furneval J., Fusari M., Gallacher S., Galushka S., Gambale G., Gambino I., Garcia-Perez M. L., Garg S., Garlak J., Gavranovic Z., Gavrilov R., Gaynor L., Gecaj Gashi A., Georghiou M., Gerjevic B., Gferer G., Giarratano A., Gibson A., Gievski V., Giles J., Gillberg L., Gilowska K., Gilsanz Rodriguez F., Gioia A., Giovannoni C., Girotra V., Gkinas D., Gkiokas G., Godoroja D., Goebel U., Goel V., Gonzalez M., Goranovic T., Gornik-Wlaszczuk E., Gosavi S., Gottfridsson P., Gottschalk A., Granell M., Granstrom A., Grassetto A., Greenwood A., Grigoras I., Grintescu I., Gritsan A., Gritsan G., Grynyuk A., Guadagnin G. M., Guarnieri M., Guclu C., Guerrero Diez M., Gunenc F., Gunther U., Gupta P., Guttenthaler V., Hack Y., Hafisayena A., Hagau N., Haldar J., Hales D., Hanci V., Hanna-Jumma S., Harazim H., Harlet P., Harper D., Harris B., Harvey O., Hashimi M., Hawkins L., Hayes C., Heaton J., Heier T., Helliwell L., Hemmes S., Henderson K., Hermanides J., Hermanns H., Herrera Hueso B., Hestenes S., Hettiarachchi R., Highgate J., Hodgson K., Hoelbling D., Holland J., Horhota L., Hormis A., Hribar R., Hua A., Humphreys S., Humphries R., Humplikova S., Hunt J., Husnain A., Hussein A., Hyams B., Iannuccelli F., Ilette K., Ilyas C., Inan T., India I., Ionitav V., Irwin F., Jain V., Janez B., Jankovic R., Jenkins S., Jenko M., Jimenez R., Jimenez Gomez B., Joachim S., Joelsson-Alm E., John J., Jonikaite L., Jovic M., Jungwirth B., Junke E., Kabakov B., Kadaoui S. -D., Kanski A., Karadag S., Karbonskiene A., Karjagin J., Kasnik D., Katanolli F., Katsika E., Kaufmann K., Keane H., Kelly M., Kent M., Keraitiene G., Khudhur A., Khuenl-Brady K., Kidd L., King S., Kirchgassner K., Klancir T., Klucniks A., Knotzer J., Knowlden P., Koers L., Kompan J., Koneti K. K., Kooij F., Koolen E., Koopman - van Gemert A. W. M. M., Kopp K., Korfiotis D., Korolkov O., Kosinova M., Kostenberger M., Kotzinger O., Kovacevic M., Kranke P., Kranke E., Kraus C., Kraus S., Kubitzek C., Kucharski R., Kucukguclu S., Kudrashou A., Kumar V., Kummen L., Kunit C., Kushakovsky V., Kuvaki B., Kuzmanovska B., Kyttari A., Landoni G., Lau G., Lazarev K., Legett S., Legrottaglie A. M., Leonardi S., Leong M., Lercher H., Leuvrey M., Leva B., Levstek M., Limb J., Lindholm E., Linton F., Liperi C., Lipski F., Lirk P., Lisi A., Liskova K., Lluch Oltra A., Loganathan V., Lombardi S., Lopez E., Lopez Rodriguez M., Lorenzini L., Lowicka M., Lugovoy A., Luippold M., Lumb A., Macas A., Macgregor M., Machado H., Maciariello M., Madeira I., Maitan S., Majewski J., Maldini B., Malewski G., Manfredini L., Manner O., Marchand B., Marcu A., Margalef J., Margarson M., Marinheiro L., Markic A., Markovic Bozic J., Marrazzo F., Martin J., Martin Ayuso M., Martinez E., Martino E. A., Martinson V., Marusic-Gaser K., Mascarenhas C., Mathis C., Matsota P., Mavrommati E., Mazul Sunko B., McCourt K., McGill N., McKee R., Meco B. C., Meier S., Melbourne S., Melbybrathen G., Meli A., Melia A., Melotti R. M., Menga M. R., Mercer P., Merotra S., Mescolini S., Metterlein T., Michalov M., Michlig S., Midgley S., Milic M., Milojevic M., Minana A., Minto G., Mirabella L., Mirea L., Mittelstadt L., Moeglen A., Moise A., Mokini Z., Molin A., Molto L., Monea M. C., Montalto F., Montgomery J., Montgomery C., Montillo G., Moore S., Moore F., Moreira Z., Moreno T., Moreno R., Moret E., Moreton S., Morgan M., Moro Velasco C., Morri D., Moull A., Moura F., Mraz P., Mrozek K., Mukhtar K., Muniyappa S., Murray H., Murthy B. V., Mushambi M., Nadolski M., Nardelli P., Nardin G., Navarro Perez R., Naveiro A., Negri M., Nesek Adam V., Neskovic V., Neuwersch S., Neves M., Nguyen B., Ni Eochagain A., Nicholas C., Nightingale J., Norrie K., Novak-Jankovic V., Novakova A., Novillo M., Numan S., Oduro-Dominah L., Oldner A., Oliveira I., Ologoiu D., Oloktsidou I., O'Reilly R., Orlando A., Ovezov A., Ozbilgin S., Paal P., Padin Barreiro L., Palugniok R., Papaioannou A., Papapostolou K., Paranthaman P., Pardey Bracho G., Parente S., Parfeni A., Pasin L., Passey S., Pastor E., Patch S., Patil A., Paunescu M. -A., Pehboeck D., Pereira M., Pereira C., Perez Caballero P., Perez Garcia A., Perez Soto A., Perez Tejero G., Perez-Cerda F., Pesenti A., Petta R., Philippe S., Pickering D., Pico Veloso J., Pina P., Pinho-Oliveira V., Pinol S., Pinto R., Pistidda L., Pitterle M., Piwowarczyk P., Plotnikova O., Pohl H., Poldermann J., Polkovicova L., Pompei L., Popescu M., Popovic R., Pota V., Potocnik M., Potrec B., Potter A., Pramod N., Prchalova M., Preckel B., Pugh R., Pulletz M., Radoeshki A., Rafi A., Ragazzi R., Raineri Santi M., Rajamanickam T., Rajput Z., Ramachandran R., Ramasamy R., Ramessur S., Rao R., Rasmussen A., Rato A., Razaque U., Real Navacerrada M. I., Reavley C., Reid J., Reschreiter H., Rial E., Ribas Carrasco P., Ribeiro S., Rich N., Richardson L., Rimaitis K., Rimaitis M., Ringvold E. -M., Ripke F., Ristescu I., Ritchie K., Rodenas F., Rodrigues P., Rogers E., Rogerson D., Romagnoli S., Romero E., Rondovic G., Rose B. O., Roth W., Rotter M. -T., Rousseau G., Rudjord A., Rueffert H., Rundgren M., Rupprecht K., Rushton A., Russotto V., Rypulak E., Ryszka M., Sa J., Sa Couto P., Saby S., Sagic J., Saleh O., Sales G., Sanchez Sanchez Y., Sanghera S., Sanli Karip C., Santiveri Papiol F. J., Santos S., Sarno S., Saul D., Saunders D., Savic N., Scalco L., Scanlon D., Schaller S., Schax C., Scheffer G. J., Schening A., Schiavone V., Schmidt-Ehrenberg F., Schmidt-Mutter C., Schonberg C., Schopflin C., Schreiber J. -U., Schultz M., Schurig M., Scott C., Sebestian S., Sehgal S., Sem V., Semenas E., Serafini E., Serchan P., Shields M., Shobha R., Shosholcheva M., Siamansour T., Siddaiah N., Siddiqi K., Sinclair R., Singh P., Singh R., Sinha A., Skinner A., Smee E., Smekalova O., Smith N., Smith T., Smitz C., Smole D., Sojcic N., Soler Pedrola M., Somanath S., Sonksen J., Sorella M. C., Sormus A., Soro M., Soto C., Spada A., Spadaro S., Spaeth J., Sparr H., Spielmann A., Spindler-Vesel A., Stamelos M., Stancombe L L., Stanculescu A., Standl T., Standley T., Stanek O., Stanisavljevic S., Starczewska M., Stauble C., Steen J., Stefan O. M., Stell E., Stera C., Stevens M., Stoerckel M., Stosic B., Stourac P., Stroumpoulis K., Struck R., Suarez de la Rica A., Sultanpori A., Sundara Rajan R., Suying O., Svensen C., Swan L., Syrogianni P., Sysiak J., Szederjesi J., Taddei S., Tan Hao E., Tanou V., Tarabova K., Tardaguila Sancho P., Tarroso M., Tartaglione M., Taylor E., Tbaily L., Telford R., Terenzoni M., Theodoraki K., Thornley H., Tiganiuc L., Toim H., Tomescu D., Tommasino C., Toni J., Toninelli A., Toretti I., Townley S., Trepenaitis D., Trethowan B., Tsaousi G., Tsiftsi A., Tudor A., Turan G., Turhan S. C., Unic-Stojanovic D., Unterbuchner C., Unzueta C., Uranjek J., Ursic T., Vaida S., Valldeperas Ferrer S., Valldeperas Hernandez M. I., Valsamidis D., Van Beek R., Van dasselaer N., Van Der Beek T., Van Duivenvoorde Y., van Klei W. A., Van Poorter F., Van Zaane B., Van Zundert T., Van Zyl R., Vargas Munoz A. M., Varsani N., Vasconcelos P., Vassilakis G., Vecchiatini T., Vecera L., Vercauteren M., Verdouw B., Verheyen V., Verri M., Vicari Sottosanti L. G., Vico M., Vidal Mitjans P., Vilardi A., Vissicchio D., Vitale G., Vitkovic B., Vizcaychipi M. P., Voicu A., Voje M., Volfova I., Volta C. A., Von Lutterotti T., von Tiesenhausen A., Vrecic-Slabe S., Vukcevic D., Vukovic R., Vullo P. A., Wade A., Wallberg H., Wallden J., Wallner J., Walther Sturesson L., Watson D., Weber S., Wegiel Leskiewiq A., Weller D., Wensing C., Werkmann M., Westberg H., Wikstrom E., Williams B., Wilson R., Wirth S., Wittmann M., Wood L., Wright S., Zachoval C., Zambon M., Zampieri S., Zampone S., Zangrillo A., Zani G., Zavackiene A., Zieglerder R., Zonneveldt H., Zsisku L., Zucker T. -P., Zukowski M., Zuleika M., Zupaneie D., Kirmeier, E, Eriksson, L, Lewald, H, Jonsson Fagerlund, M, Hoeft, A, Hollmann, M, Meistelman, C, Hunter, J, Ulm, K, Blobner, M, Abad Gurumeta, A, Abernethy, C, Abigail, P, Achaibar, K, Adam, E, Afshari, A, Agudelo Montoya, M, Akgun, F, Aletti, G, Alkis, N, Allan, K, Allan, A, Allaouchiche, B, Allcock, C, Almasy, E, Amey, I, Amigoni, M, Andersen, E, Andersson, P, Anipchenko, N, Antunes, P, Armstrong, E, Aslam, T, Aslin, B, Assuncao, J, Ausserer, J, Avvai, M, Awad, N, Ayas Montero, B, Ayuso, M, Azevedo, P, Badarau, V, Badescu, R, Baiardo Redaelli, M, Baird, C, Baird, Y, Baker, T, Balaji, P, Balan, C, Balandin, A, Balescu-Arion, C, Baliuliene, V, Baltasar Isabel, J, Baluch, S, Bandrabur, D, Bankewitz, C, Barber, K, Barbera, F, Barcraft-Barnes, H, Barletti, V, Barnett, G, Baron, K, Barros, A, Barsan, V, Bartlett, P, Batistaki, C, Baumgarten, G, Baytas, V, Beauchamp, N, Becerra Cayetano, I, Bell, S, Bellandi, M, Belletti, A, Belmonte Cuenca, J, Benitez-Cano, A, Beretta, L, Berger, M, Bergmann, N, Bergmark, K, Bermudez Lopez, M, Bernotaite, M, Beurskens, C, Bidd, H, Bifulco, F, Bignami, E, Bilic, A, Bilskiene, D, Bischoff, P, Bishop, L, Bjonness, T, Blaylock, H, Blethyn, K, Blincoe, T, Blokhin, I, Blunt, N, Boer, C, Bois, G, Bonicolini, E, Booth, J, Borecka-Kedzierska, M, Borstnar, K, Borys, M, Boselli, E, Bouvet, L, Bouwman, A, Bowen, L, Bowrey, S, Boxall, L, Bozic, T, Bradley, T, Branco, T, Brazzi, L, Brazzoni, M, Brear, T, Brogly, N, Brohi, F, Broms, J, Bubliauskas, A, Bucolo, G, Buerkle, H, Buggy, D, Buhre, W, Bukauskas, T, Butturini, F, Byttner, A, Cabrera Diaz, I, Calderon, A, Calhau, R, Callejo, A, Cammu, G, Campesato, M, Can, O, Candeias, M, Cantor, A, Carise, E, Carmona, C, Carreteiro, J, Carrieri, C, Carter, A, Casal, M, Casanova, I, Cascella, M, Casero, L, Casiraghi, G, Castelo-Branco, L, Castro Arranz, C, Cernea, D, Cervantes, J, Chandler, B, Charnock, R, Chatzimicali, A, Chinery, E, Chishti, A, Chondhury, P, Christie, E, Christodoudiles, G, Ciardo, S, Cimpeanu, L, Cindea, I, Cinnella, G, Clark, S, Clayton, M, Cocu, S, Collyer, T, Colvin, C, Cope, S, Copeta, F, Copotoiu, S, Correia de Barros, F, Corso, R, Cortegiani, A, Costa, G, Cowton, A, Cox, N, Craig, J, Cricca, V, Cronin, J, Cunha, M, Cuomo, A, Curley, K, Czuczwar, M, Dabrowska, D, Damster, S, Danguy des Deserts, M, Daniliuc, A, Danninger, T, Darwish, I, Dascalu, C, Davies, K, Davies, S, De Boer, H, De Flaviis, A, De Selincourt, G, Deana, C, Debaene, B, Debreceni, G, Dedhia, J, Delgado Garcia, I, Della Rocca, G, Delroy-Buelles, L, Desai, T, Dhillon, P, Di Giacinto, I, Di Mauro, P, Diaz Gomez, T, Dimitrovski, A, Dinic, V, Dirzu, D, Divander, M, Dolinar, J, Domingues, S, Doolan, J, Downes, C, Dragoescu, N, Droc, G, Dum, E, Dumitrescu, A, Duncan, L, Dzurnakova, P, Eberl, S, Edwards, J, Edwards, M, Ekelund, K, Ekengren, P, Elghouty, E, Ellerkmann, R, Ellis, H, Elme, A, Ernst, T, Errando, C, Estenes, S, Ewaldsson, C, Farid, N, Featherstone, J, Febres, D, Fedorov, S, Feggeler, J, Feijten, P, Fellmann, T, Fernandez Candil, J, Fernandez Castineira, A, Fernandez Castineira, J, Fernando, A, Ferrando, C, Ferreira, L, Ferreira, P, Feyling, A, Filipescu, D, Fleischer, A, Floris, L, Foerster, U, Fox, B, Franke, U, Frasca, D, Frey, C, Frost, V, Fullin, G, Fumagalli, J, Furneval, J, Fusari, M, Gallacher, S, Galushka, S, Gambale, G, Gambino, I, Garcia-Perez, M, Garg, S, Garlak, J, Gavranovic, Z, Gavrilov, R, Gaynor, L, Gecaj Gashi, A, Georghiou, M, Gerjevic, B, Gferer, G, Giarratano, A, Gibson, A, Gievski, V, Giles, J, Gillberg, L, Gilowska, K, Gilsanz Rodriguez, F, 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R, Jenkins, S, Jenko, M, Jimenez, R, Jimenez Gomez, B, Joachim, S, Joelsson-Alm, E, John, J, Jonikaite, L, Jovic, M, Jungwirth, B, Junke, E, Kabakov, B, Kadaoui, S, Kanski, A, Karadag, S, Karbonskiene, A, Karjagin, J, Kasnik, D, Katanolli, F, Katsika, E, Kaufmann, K, Keane, H, Kelly, M, Kent, M, Keraitiene, G, Khudhur, A, Khuenl-Brady, K, Kidd, L, King, S, Kirchgassner, K, Klancir, T, Klucniks, A, Knotzer, J, Knowlden, P, Koers, L, Kompan, J, Koneti, K, Kooij, F, Koolen, E, Koopman - van Gemert, A, Kopp, K, Korfiotis, D, Korolkov, O, Kosinova, M, Kostenberger, M, Kotzinger, O, Kovacevic, M, Kranke, P, Kranke, E, Kraus, C, Kraus, S, Kubitzek, C, Kucharski, R, Kucukguclu, S, Kudrashou, A, Kumar, V, Kummen, L, Kunit, C, Kushakovsky, V, Kuvaki, B, Kuzmanovska, B, Kyttari, A, Landoni, G, Lau, G, Lazarev, K, Legett, S, Legrottaglie, A, Leonardi, S, Leong, M, Lercher, H, Leuvrey, M, Leva, B, Levstek, M, Limb, J, Lindholm, E, Linton, F, Liperi, C, Lipski, F, Lirk, P, Lisi, A, Liskova, K, Lluch 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A., Bell S., Bellandi M., Belletti A., Belmonte Cuenca J., Benitez-Cano A., Beretta L., Berger M., Bergmann N., Bergmark K., Bermudez Lopez M., Bernotaite M., Beurskens C., Bidd H., Bifulco F., Bignami E., Bilic A., Bilskiene D., Bischoff P., Bishop L., Bjonness T., Blaylock H., Blethyn K., Blincoe T., Blokhin I., Blunt N., Boer C., Bois G., Bonicolini E., Booth J., Borecka-Kedzierska M., Borstnar K., Borys M., Boselli E., Bouvet L., Bouwman A., Bowen L., Bowrey S., Boxall L., Bozic T., Bradley T., Branco T., Brazzi L., Brazzoni M., Brear T., Brogly N., Brohi F., Broms J., Bubliauskas A., Bucolo G. E., Buerkle H., Buggy D., Buhre W., Bukauskas T., Butturini F., Byttner A., Cabrera Diaz I., Calderon A., Calhau R., Callejo A., Cammu G., Campesato M., Can O. S., Candeias M., Cantor A., Carise E., Carmona C., Carreteiro J., Carrieri C., Carter A., Casal M., Casanova I., Cascella M., Casero L. M., Casiraghi G. M., Castelo-Branco L., Castro Arranz C., Cernea D. 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K., Kooij F., Koolen E., Koopman - van Gemert A. W. M. M., Kopp K., Korfiotis D., Korolkov O., Kosinova M., Kostenberger M., Kotzinger O., Kovacevic M., Kranke P., Kranke E., Kraus C., Kraus S., Kubitzek C., Kucharski R., Kucukguclu S., Kudrashou A., Kumar V., Kummen L., Kunit C., Kushakovsky V., Kuvaki B., Kuzmanovska B., Kyttari A., Landoni G., Lau G., Lazarev K., Legett S., Legrottaglie A. M., Leonardi S., Leong M., Lercher H., Leuvrey M., Leva B., Levstek M., Limb J., Lindholm E., Linton F., Liperi C., Lipski F., Lirk P., Lisi A., Liskova K., Lluch Oltra A., Loganathan V., Lombardi S., Lopez E., Lopez Rodriguez M., Lorenzini L., Lowicka M., Lugovoy A., Luippold M., Lumb A., Macas A., Macgregor M., Machado H., Maciariello M., Madeira I., Maitan S., Majewski J., Maldini B., Malewski G., Manfredini L., Manner O., Marchand B., Marcu A., Margalef J., Margarson M., Marinheiro L., Markic A., Markovic Bozic J., Marrazzo F., Martin J., Martin Ayuso M., Martinez E., Martino E. A., Martinson V., Marusic-Gaser K., Mascarenhas C., Mathis C., Matsota P., Mavrommati E., Mazul Sunko B., McCourt K., McGill N., McKee R., Meco B. C., Meier S., Melbourne S., Melbybrathen G., Meli A., Melia A., Melotti R. M., Menga M. R., Mercer P., Merotra S., Mescolini S., Metterlein T., Michalov M., Michlig S., Midgley S., Milic M., Milojevic M., Minana A., Minto G., Mirabella L., Mirea L., Mittelstadt L., Moeglen A., Moise A., Mokini Z., Molin A., Molto L., Monea M. C., Montalto F., Montgomery J., Montgomery C., Montillo G., Moore S., Moore F., Moreira Z., Moreno T., Moreno R., Moret E., Moreton S., Morgan M., Moro Velasco C., Morri D., Moull A., Moura F., Mraz P., Mrozek K., Mukhtar K., Muniyappa S., Murray H., Murthy B. V., Mushambi M., Nadolski M., Nardelli P., Nardin G., Navarro Perez R., Naveiro A., Negri M., Nesek Adam V., Neskovic V., Neuwersch S., Neves M., Nguyen B., Ni Eochagain A., Nicholas C., Nightingale J., Norrie K., Novak-Jankovic V., Novakova A., Novillo M., Numan S., Oduro-Dominah L., Oldner A., Oliveira I., Ologoiu D., Oloktsidou I., O'Reilly R., Orlando A., Ovezov A., Ozbilgin S., Paal P., Padin Barreiro L., Palugniok R., Papaioannou A., Papapostolou K., Paranthaman P., Pardey Bracho G., Parente S., Parfeni A., Pasin L., Passey S., Pastor E., Patch S., Patil A., Paunescu M. -A., Pehboeck D., Pereira M., Pereira C., Perez Caballero P., Perez Garcia A., Perez Soto A., Perez Tejero G., Perez-Cerda F., Pesenti A., Petta R., Philippe S., Pickering D., Pico Veloso J., Pina P., Pinho-Oliveira V., Pinol S., Pinto R., Pistidda L., Pitterle M., Piwowarczyk P., Plotnikova O., Pohl H., Poldermann J., Polkovicova L., Pompei L., Popescu M., Popovic R., Pota V., Potocnik M., Potrec B., Potter A., Pramod N., Prchalova M., Preckel B., Pugh R., Pulletz M., Radoeshki A., Rafi A., Ragazzi R., Raineri Santi M., Rajamanickam T., Rajput Z., Ramachandran R., Ramasamy R., Ramessur S., Rao R., Rasmussen A., Rato A., Razaque U., Real Navacerrada M. I., Reavley C., Reid J., Reschreiter H., Rial E., Ribas Carrasco P., Ribeiro S., Rich N., Richardson L., Rimaitis K., Rimaitis M., Ringvold E. -M., Ripke F., Ristescu I., Ritchie K., Rodenas F., Rodrigues P., Rogers E., Rogerson D., Romagnoli S., Romero E., Rondovic G., Rose B. O., Roth W., Rotter M. -T., Rousseau G., Rudjord A., Rueffert H., Rundgren M., Rupprecht K., Rushton A., Russotto V., Rypulak E., Ryszka M., Sa J., Sa Couto P., Saby S., Sagic J., Saleh O., Sales G., Sanchez Sanchez Y., Sanghera S., Sanli Karip C., Santiveri Papiol F. J., Santos S., Sarno S., Saul D., Saunders D., Savic N., Scalco L., Scanlon D., Schaller S., Schax C., Scheffer G. J., Schening A., Schiavone V., Schmidt-Ehrenberg F., Schmidt-Mutter C., Schonberg C., Schopflin C., Schreiber J. -U., Schultz M., Schurig M., Scott C., Sebestian S., Sehgal S., Sem V., Semenas E., Serafini E., Serchan P., Shields M., Shobha R., Shosholcheva M., Siamansour T., Siddaiah N., Siddiqi K., Sinclair R., Singh P., Singh R., Sinha A., Skinner A., Smee E., Smekalova O., Smith N., Smith T., Smitz C., Smole D., Sojcic N., Soler Pedrola M., Somanath S., Sonksen J., Sorella M. C., Sormus A., Soro M., Soto C., Spada A., Spadaro S., Spaeth J., Sparr H., Spielmann A., Spindler-Vesel A., Stamelos M., Stancombe L L., Stanculescu A., Standl T., Standley T., Stanek O., Stanisavljevic S., Starczewska M., Stauble C., Steen J., Stefan O. M., Stell E., Stera C., Stevens M., Stoerckel M., Stosic B., Stourac P., Stroumpoulis K., Struck R., Suarez de la Rica A., Sultanpori A., Sundara Rajan R., Suying O., Svensen C., Swan L., Syrogianni P., Sysiak J., Szederjesi J., Taddei S., Tan Hao E., Tanou V., Tarabova K., Tardaguila Sancho P., Tarroso M., Tartaglione M., Taylor E., Tbaily L., Telford R., Terenzoni M., Theodoraki K., Thornley H., Tiganiuc L., Toim H., Tomescu D., Tommasino C., Toni J., Toninelli A., Toretti I., Townley S., Trepenaitis D., Trethowan B., Tsaousi G., Tsiftsi A., Tudor A., Turan G., Turhan S. C., Unic-Stojanovic D., Unterbuchner C., Unzueta C., Uranjek J., Ursic T., Vaida S., Valldeperas Ferrer S., Valldeperas Hernandez M. I., Valsamidis D., Van Beek R., Van dasselaer N., Van Der Beek T., Van Duivenvoorde Y., van Klei W. A., Van Poorter F., Van Zaane B., Van Zundert T., Van Zyl R., Vargas Munoz A. M., Varsani N., Vasconcelos P., Vassilakis G., Vecchiatini T., Vecera L., Vercauteren M., Verdouw B., Verheyen V., Verri M., Vicari Sottosanti L. G., Vico M., Vidal Mitjans P., Vilardi A., Vissicchio D., Vitale G., Vitkovic B., Vizcaychipi M. P., Voicu A., Voje M., Volfova I., Volta C. A., Von Lutterotti T., von Tiesenhausen A., Vrecic-Slabe S., Vukcevic D., Vukovic R., Vullo P. A., Wade A., Wallberg H., Wallden J., Wallner J., Walther Sturesson L., Watson D., Weber S., Wegiel Leskiewiq A., Weller D., Wensing C., Werkmann M., Westberg H., Wikstrom E., Williams B., Wilson R., Wirth S., Wittmann M., Wood L., Wright S., Zachoval C., Zambon M., Zampieri S., Zampone S., Zangrillo A., Zani G., Zavackiene A., Zieglerder R., Zonneveldt H., Zsisku L., Zucker T. -P., Zukowski M., Zuleika M., and Zupaneie D.
Abstract: Background: Results from retrospective studies suggest that use of neuromuscular blocking agents during general anaesthesia might be linked to postoperative pulmonary complications. We therefore aimed to assess whether the use of neuromuscular blocking agents is associated with postoperative pulmonary complications. Methods: We did a multicentre, prospective observational cohort study. Patients were recruited from 211 hospitals in 28 European countries. We included patients (aged ≥18 years) who received general anaesthesia for any in-hospital procedure except cardiac surgery. Patient characteristics, surgical and anaesthetic details, and chart review at discharge were prospectively collected over 2 weeks. Additionally, each patient underwent postoperative physical examination within 3 days of surgery to check for adverse pulmonary events. The study outcome was the incidence of postoperative pulmonary complications from the end of surgery up to postoperative day 28. Logistic regression analyses were adjusted for surgical factors and patients' preoperative physical status, providing adjusted odds ratios (ORadj) and adjusted absolute risk reduction (ARRadj). This study is registered with ClinicalTrials.gov, number NCT01865513. Findings: Between June 16, 2014, and April 29, 2015, data from 22 803 patients were collected. The use of neuromuscular blocking agents was associated with an increased incidence of postoperative pulmonary complications in patients who had undergone general anaesthesia (1658 [7·6%] of 21 694); ORadj 1·86, 95% CI 1·53–2·26; ARRadj −4·4%, 95% CI −5·5 to −3·2). Only 2·3% of high-risk surgical patients and those with adverse respiratory profiles were anaesthetised without neuromuscular blocking agents. The use of neuromuscular monitoring (ORadj 1·31, 95% CI 1·15–1·49; ARRadj −2·6%, 95% CI −3·9 to −1·4) and the administration of reversal agents (1·23, 1·07–1·41; −1·9%, −3·2 to −0·7) were not associated with a decreased risk of postoperative pulmonary
Published: 2019

9. GAlaxy Light profile convolutional neural NETworks (GaLNets). I. fast and accurate structural parameters for billion galaxy samples

Author: Li, R., Napolitano, N. R., Roy, N., Tortora, C., La Barbera, F., Sonnenfeld, A., Qiu, C., Liu, S., Li, R., Napolitano, N. R., Roy, N., Tortora, C., La Barbera, F., Sonnenfeld, A., Qiu, C., and Liu, S.
Abstract: Next generation large sky surveys will observe up to billions of galaxies for which basic structural parameters are needed to study their evolution. This is a challenging task that, for ground-based observations, is complicated by seeing limited point-spread function (PSF). To perform a fast and accurate analysis of galaxy surface brightness, we have developed a family of supervised Convolutional Neural Networks (CNN) to derive Sersic profile parameters of galaxies. This work presents the first two Galaxy Light profile convolutional neural Networks (GaLNets) of this family. The first one is trained using galaxy images only (GaLNet-1), and the second is trained with both galaxy images and the local PSF (GaLNet-2). We have compared the results from the GaLNets with structural parameters (total magnitude, effective radius, Sersic index etc.) derived on a set of galaxies from the Kilo-Degree Survey (KiDS) by 2DPHOT, as a representative of "standard" PSF convolved Sersic fitting tools. The comparison shows that GaLNet-2 can reach an accuracy as high as 2DPHOT, while GaLNet-1 performs worse because it misses the information on the local PSF. Both GaLNets are three orders of magnitude faster than standard methods in terms of computational speed. This first application of CNNs to ground-based galaxy surface photometry shows that they are promising tools to perform parametric analyses of very large galaxy samples, like the ones expected from Vera Rubin/LSST surveys. However, the GaLNets can be easily modified for space observations from Euclid and the China Space Station Telescope., Comment: Accepted for publication by APJ
Published: 2021

10. Sei missioni “a prova di futuro”: verso Torino 2030

Author: Barbera, F, Bocco, A, De Rossi, A, Guerzoni, M, Lombardi, P, Mellano, P, Quarta, A, Semi, G, Barbera, F, Bocco, A, De Rossi, A, Guerzoni, M, Lombardi, P, Mellano, P, Quarta, A, and Semi, G
Abstract: Le missioni qui di seguito descritte vanno intese come corsie preferenziali per andare verso gli scenari auspicabili delineati nei capitoli precedenti, così come strumenti per evitare gli scenari wicked. Vanno intese, dunque, come leve per costruire una città “a prova di futuro”.
Published: 2021

11. Ritorno al futuro? Reindustrializzazione manifatturiera smart e green per rilanciare lo sviluppo industriale dell’area metropolitana basato su conoscenza, sostenibilità e occupazione

Author: Barbera, F, Bocco, A, De Rossi, A, Guerzoni, M, Lombardi, P, Mellano, P, Quarta, A, Semi, G, Barbera, F, Bocco, A, De Rossi, A, Guerzoni, M, Lombardi, P, Mellano, P, Quarta, A, and Semi, G
Abstract: Il libro tratta del decennale declino economico della città di Torino e della prodzuione manifatturiera come prima causa. Individa punti di forza e debolezza per il rilancio della città e individua una possibile soluzione in una allaenza tra la manifattura da rilanciare e le nuove tecnologie. Solo in questo modo si può rilanciare lo sviluppo industriale dell’area metropolitana basato su conoscenza, sostenibilità e occupazione.
Published: 2021

12. GAlaxy Light profile convolutional neural NETworks (GaLNets). I. fast and accurate structural parameters for billion galaxy samples

Author: Li, R., Napolitano, N. R., Roy, N., Tortora, C., La Barbera, F., Sonnenfeld, A., Qiu, C., Liu, S., Li, R., Napolitano, N. R., Roy, N., Tortora, C., La Barbera, F., Sonnenfeld, A., Qiu, C., and Liu, S.
Abstract: Next generation large sky surveys will observe up to billions of galaxies for which basic structural parameters are needed to study their evolution. This is a challenging task that, for ground-based observations, is complicated by seeing limited point-spread function (PSF). To perform a fast and accurate analysis of galaxy surface brightness, we have developed a family of supervised Convolutional Neural Networks (CNN) to derive Sersic profile parameters of galaxies. This work presents the first two Galaxy Light profile convolutional neural Networks (GaLNets) of this family. The first one is trained using galaxy images only (GaLNet-1), and the second is trained with both galaxy images and the local PSF (GaLNet-2). We have compared the results from the GaLNets with structural parameters (total magnitude, effective radius, Sersic index etc.) derived on a set of galaxies from the Kilo-Degree Survey (KiDS) by 2DPHOT, as a representative of "standard" PSF convolved Sersic fitting tools. The comparison shows that GaLNet-2 can reach an accuracy as high as 2DPHOT, while GaLNet-1 performs worse because it misses the information on the local PSF. Both GaLNets are three orders of magnitude faster than standard methods in terms of computational speed. This first application of CNNs to ground-based galaxy surface photometry shows that they are promising tools to perform parametric analyses of very large galaxy samples, like the ones expected from Vera Rubin/LSST surveys. However, the GaLNets can be easily modified for space observations from Euclid and the China Space Station Telescope., Comment: Accepted for publication by APJ
Published: 2021
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13. Mild radial variations of the stellar IMF in the bulge of M31

Author: La Barbera, F., Vazdekis, A., Ferreras, I., Pasquali, A., La Barbera, F., Vazdekis, A., Ferreras, I., and Pasquali, A.
Abstract: Using new, homogeneous, long-slit spectroscopy in the wavelength range from ~0.35 to ~1micron, we study radial gradients of optical and near-infrared (NIR) IMF-sensitive features along the major axis of the bulge of M31, out to a galacto-centric distance of ~200'' (~800pc). Based on state-of-the-art stellar population synthesis models with varying Na abundance ratio, we fit a number of spectral indices, from different chemical species (including TiO's, Ca, and Na indices), to constrain the low-mass (<0.5M_Sun) end slope (i.e. the fraction of low-mass stars) of the stellar IMF, as a function of galacto-centric distance. Outside a radial distance of ~10'', we infer an IMF similar to a Milky-Way-like distribution, while at small galacto-centric distances, an IMF radial gradient is detected, with a mildly bottom-heavy IMF in the few inner arcsec. We are able to fit Na features (both NaD and NaI8190), without requiring extremely high Na abundance ratios. [Na/Fe] is ~0.4dex for most of the bulge, rising up to ~0.6dex in the innermost radial bins. Our results imply an overall, luminosity-weighted, IMF and mass-to-light ratio for the M31 bulge, consistent with those for a Milky-Way-like distribution, in contrast to results obtained, in general, for most massive early-type galaxies., Comment: accepted for publication in MNRAS, 22 pages, 16 figures
Published: 2021
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14. INSPIRE: INvestigating Stellar Population In RElics II. First Data Release (DR1)

Author: Spiniello, C., Tortora, C., D'Ago, G., Coccato, L., La Barbera, F., Ferré-Mateu, A., Pulsoni, C., Arnaboldi, M., Gallazzi, A., Hunt, L., Napolitano, N. R., Radovich, M., Scognamiglio, D., Spavone, M., Zibetti, S., Spiniello, C., Tortora, C., D'Ago, G., Coccato, L., La Barbera, F., Ferré-Mateu, A., Pulsoni, C., Arnaboldi, M., Gallazzi, A., Hunt, L., Napolitano, N. R., Radovich, M., Scognamiglio, D., Spavone, M., and Zibetti, S.
Abstract: The INvestigating Stellar Population In RElics is an on-going project targeting 52 ultra-compact massive galaxies at 0.12) through a short and intense star formation burst, that evolved passively and undisturbed until the present-day. Relics provide a unique opportunity to study the mechanisms of star formation at high-z. In this paper, we present the first INSPIRE Data Release, comprising 19 systems with observations completed in 2020. We use the methods already presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For these 19 systems, we obtain an estimate of the stellar velocity dispersion, fitting separately the two UVB and VIS XSH arms at their original resolution. We estimate [Mg/Fe] abundances via line-index strength and mass-weighted integrated stellar ages and metallicities with full spectral fitting on the combined spectrum. Ages are generally old, in agreement with the photometric ones, and metallicities are almost always super-solar, confirming the mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the great majority of the galaxies, as expected. We find that 10 objects have formed more than 75% of their stellar mass (M*) within 3 Gyr from the Big Bang and classify them as relics. Among these, we identify 4 galaxies which had already fully assembled their M* by that time. They are therefore `extreme relics' of the ancient Universe. The INSPIRE DR1 catalogue of 10 known relics to-date augment by a factor of 3.3 the total number of confirmed relics, also enlarging the redshift window. It is therefore the largest publicly available collection. Thanks to the larger number of systems, we can also better quantify the existence of a 'degree of relicness', already hinted at the Pilot Paper., Comment: (Abstract abridged) 21 pages, 12 figures and 5 tables in the main body, plus 3 figure and 1 table in the appendix, accepted for publication on A&A. The associated data are available via the ESO Phase 3 Science Portal
Published: 2021
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15. INSPIRE: INvestigating Stellar Population in RElics: I. Survey presentation and pilot study

Author: Oxford Hintze Centre for Astrophysical Surveys (UK), La Caixa, Bonn-Cologne Graduate School of Physics and Astronomy, Sun Yat-sen University, International Max Planck Research Schools, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Napolitano, N. R., Spavone, M., Scognamiglio, D., Arnaboldi, M., Gallazzi, A., Hunt, L., Moehler, S., Radovich, Milan, Zibetti, Stefano, Oxford Hintze Centre for Astrophysical Surveys (UK), La Caixa, Bonn-Cologne Graduate School of Physics and Astronomy, Sun Yat-sen University, International Max Planck Research Schools, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Napolitano, N. R., Spavone, M., Scognamiglio, D., Arnaboldi, M., Gallazzi, A., Hunt, L., Moehler, S., Radovich, Milan, and Zibetti, Stefano
Abstract: [Context] Massive elliptical galaxies are thought to form through a two-phase process. At early times (z > 2), an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact, and massive (i.e. red nuggets). Then, a time-extended second phase, which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a small fraction of red nuggets survive, without any interaction, massive and compact until today: these are relic galaxies. Since this fraction depends on the processes dominating the size growth, counting relics at low-z is a valuable way of disentangling between different galaxy evolution models. [Aims] In this paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE) Project, which aims to spectroscopically confirm and fully characterise a large number of relics at 0:1z0:5. We focus here on the first results based on a pilot study targeting three systems, representative of the whole sample. [Methods] For these three candidates, we extracted 1D optical spectra over an aperture of r = 0:4000, which comprises 30% of the galaxies’ light, and we obtained the line-of-sight integrated stellar velocity and velocity dispersion. We also inferred the stellar [/Fe] abundance from line-index measurements and mass-weighted age and metallicity from full-spectral fitting with single stellar population models. [Results] Two galaxies have large integrated stellar velocity dispersion values (250 km s), confirming their massive nature. They are populated by stars with super-solar metallicity and [/Fe]. Both objects have formed 80% of their stellar mass within a short (0:5:0 Gyr) initial star formation episode occurred only 1 Gyr after the Big Bang. The third galaxy has a more extendedstar formation history and a lower velocity dispersion. Thus we confirm two out of three candidates as relics. [Conclusions] This paper is the first step towards
Published: 2021

16. INSPIRE: INvestigating stellar population in RElics: II. First data release (DR1)

Author: Oxford Hintze Centre for Astrophysical Surveys (UK), International Max Planck Research Schools, Bonn-Cologne Graduate School of Physics and Astronomy, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Arnaboldi, M., Gallazzi, A., Hunt, L., Napolitano, N. R., Radovich, Milan, Scognamiglio, D., Spavone, M., Zibetti, Stefano, Oxford Hintze Centre for Astrophysical Surveys (UK), International Max Planck Research Schools, Bonn-Cologne Graduate School of Physics and Astronomy, Spiniello, C., Tortora, C., D'Ago, G., Coccato, Lodovico, Barbera, F. la, Ferré-Mateu, Anna, Arnaboldi, M., Gallazzi, A., Hunt, L., Napolitano, N. R., Radovich, Milan, Scognamiglio, D., Spavone, M., and Zibetti, Stefano
Abstract: [Context] The INvestigating Stellar Population In RElics (INSPIRE) is an ongoing project targeting 52 ultra-compact massive galaxies at 0.1 < z < 0.5 with the X-shooter at VLT spectrograph (XSH). These objects are the ideal candidates to be 'relics', massive red nuggets that have formed at high redshift (z > 2) through a short and intense star formation burst, and then have evolved passively and undisturbed until the present day. Relics provide a unique opportunity to study the mechanisms of star formation at high-z. [Aims] INSPIRE is designed to spectroscopically confirm and fully characterise a large sample of relics, computing their number density in the redshift window 0.1 < z < 0.5 for the first time, thus providing a benchmark for cosmological galaxy formation simulations. In this paper, we present the INSPIRE Data Release (DR1), comprising 19 systems with observations completed in 2020. [Methods] We use the methods already presented in the INSPIRE Pilot, but revisiting the 1D spectral extraction. For the 19 systems studied here, we obtain an estimate of the stellar velocity dispersion, fitting the two XSH arms (UVB and VIS) separately at their original spectral resolution to two spectra extracted in different ways. We estimate [Mg/Fe] abundances via line-index strength and mass-weighted integrated stellar ages and metallicities with full spectral fitting on the combined (UVB+VIS) spectrum. [Results] For each system, different estimates of the velocity dispersion always agree within the errors. Spectroscopic ages are very old for 13/19 galaxies, in agreement with the photometric ones, and metallicities are almost always (18/19) super-solar, confirming the mass-metallicity relation. The [Mg/Fe] ratio is also larger than solar for the great majority of the galaxies, as expected. We find that ten objects formed more than 75% of their stellar mass (M∗) within 3 Gyr from the big bang and classify them as relics. Among these, we identify four galaxies that had alrea
Published: 2021

17. On the accretion of a new group of galaxies on to Virgo:I. Internal kinematics of nine in-falling dEs

Author: Bidaran, B. (Bahar), Pasquali, A. (Anna), Lisker, T. (Thorsten), Coccato, L. (Lodovico), Falcón-Barroso, J. (Jesus), van de Ven, G. (Glenn), Peletier, R. (Reynier), Emsellem, E. (Eric), Grebel, E. K. (Eva K.), La Barbera, F. (Francesco), Janz, J. (Joachim), Sybilska, A. (Agnieszka), Vijayaraghavan, R. (Rukmani), Gallagher, J. I. (John, III), Gadotti, D. A. (Dimitri A.), Bidaran, B. (Bahar), Pasquali, A. (Anna), Lisker, T. (Thorsten), Coccato, L. (Lodovico), Falcón-Barroso, J. (Jesus), van de Ven, G. (Glenn), Peletier, R. (Reynier), Emsellem, E. (Eric), Grebel, E. K. (Eva K.), La Barbera, F. (Francesco), Janz, J. (Joachim), Sybilska, A. (Agnieszka), Vijayaraghavan, R. (Rukmani), Gallagher, J. I. (John, III), and Gadotti, D. A. (Dimitri A.)
Abstract: Galaxy environment has been shown to play an important role in transforming late-type, star-forming galaxies to quiescent spheroids. This transformation is expected to be more severe for low-mass galaxies (⁠M < 10¹⁰ M⊙⁠) in dense galaxy groups and clusters, mostly due to the influence of their past host haloes (also known as pre-processing) and their present-day environments. For the first time, in this study, we investigate a sample of nine early-type dwarf galaxies (dEs) that were accreted as a likely bound group on to the Virgo galaxy cluster about 2–3 Gyr ago. Considering this special condition, these nine dEs may provide a test bed for distinguishing between the influence of the Virgo galaxy cluster and the effects of the previous host halo on their current properties. Specifically, we use VLT/MUSE integral-field unit spectra to derive their kinematics and specific angular momentum (λR) profiles. We observe a spread in the λR profiles of our sample dEs, finding that the λR profiles of half of them are as high as those of low-mass field galaxies. The remaining dEs exhibit λR profiles as low as those of Virgo dEs that were likely accreted longer ago. Moreover, we detect nebular emission in one dE with a gas velocity offset suggesting ongoing gas stripping in Virgo. We suggest that the low-λR dEs in our sample were processed by their previous host halo, prior to their infall to Virgo, and that the high-λR dEs may be experiencing ram pressure stripping in Virgo.
Published: 2020

18. Risorse bibliografiche digitali: come affrontarle. Alcuni consigli pratici [How to deal with digital bibliographic resources. Some practical advice]

Author: Pais, I, Barbera, F, Lacqua, F, Pais, I, Barbera, F, and Lacqua, F
Published: 2020

19. INSPIRE: INvestigating Stellar Population In RElics -- I. Survey presentation and pilot program

Author: Spiniello, C., Tortora, C., D'Ago, G., Coccato, L., La Barbera, F., Ferré-Mateu, A., Napolitano, N. R., Spavone, M., Scognamiglio, D., Arnaboldi, M., Gallazzi, A., Hunt, L., Moehler, S., Radovich, M., Zibetti, S., Spiniello, C., Tortora, C., D'Ago, G., Coccato, L., La Barbera, F., Ferré-Mateu, A., Napolitano, N. R., Spavone, M., Scognamiglio, D., Arnaboldi, M., Gallazzi, A., Hunt, L., Moehler, S., Radovich, M., and Zibetti, S.
Abstract: Massive ETGs are thought to form through a two-phase process. At early times, an intense and fast starburst forms blue and disk-dominated galaxies. After quenching, the remaining structures become red, compact and massive, i.e., 'red nuggets'. Then, a time-extended second phase which is dominated by mergers, causes structural evolution and size growth. Given the stochastic nature of mergers, a small fraction of red nuggets survives, without any interaction, massive and compact until today: relic galaxies. Since this fraction depends on the processes dominating the size growth, counting relics at low-z is a valuable way to disentangle between different galaxy evolution models. In this paper, we introduce the INvestigating Stellar Population In RElics (INSPIRE) Project, that aims at spectroscopically confirming and fully characterizing a large number of relics at 0.180 % of their stellar mass within a short (0.5 - 1.0 Gyrs) initial star formation episode occurred only ~1 Gyr after the Big Bang. The third galaxy has a more extended star formation history and a lower velocity dispersion. Thus we confirm two out of three candidates as relics., Comment: 19 pages, 14 figures, accepted for publication in A&A
Published: 2020
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20. Can brachytherapy be properly considered in the clinical practice? Trilogy project: The vision of the AIRO (Italian Association of Radiotherapy and Clinical Oncology) Interventional Radiotherapy study group

Author: Tagliaferri, Luca, Vavassori, Andrea, Lancellotta, V., de Sanctis, V., Barbera, F., Fusco, Vincenzo, Vidali, Cristiana, Fionda, B., Colloca, Giuseppe Ferdinando, Gambacorta, Maria Antonietta, Aristei, Cynthia, Corvo, R., Magrini, S. M., Tagliaferri L. (ORCID:0000-0003-2308-0982), Vavassori A., Fusco V., Vidali C., Colloca G., Gambacorta M. A. (ORCID:0000-0001-5455-8737), Aristei C., Tagliaferri, Luca, Vavassori, Andrea, Lancellotta, V., de Sanctis, V., Barbera, F., Fusco, Vincenzo, Vidali, Cristiana, Fionda, B., Colloca, Giuseppe Ferdinando, Gambacorta, Maria Antonietta, Aristei, Cynthia, Corvo, R., Magrini, S. M., Tagliaferri L. (ORCID:0000-0003-2308-0982), Vavassori A., Fusco V., Vidali C., Colloca G., Gambacorta M. A. (ORCID:0000-0001-5455-8737), and Aristei C.
Abstract: Purpose: Brachytherapy (BT, interventional radiotherapy – IRT) is a kind of radiation therapy, in which the radioactive source is placed nearby or even inside the cancer itself. Even though this kind of radiation therapy appears effective and valuable, BT has been facing a slow but progressive decline over the past decades in Europe, particularly in Italy. Aims of this study were to identify the practical and theoretical reasons why BT is facing a slow decline in Italy, and to define a vision of the Italian Association of Radiotherapy and Clinical Oncology (AIRO) and a strategy about this emerged issues. Material and methods: A programmatic path divided into three steps like a trilogy was launched by AIRO Interventional Radiotherapy study group. The study group performed an initial data collection to highlight both the clinical and the educational topics and problems through specific surveys. After having analyzed the results of the surveys and shared a vision about the emerged issues, a specific strategy was adopted. Results: Four relevant domains were identified and for each ones, a strategy has been discussed and defined. This manuscript shows in detail the individual actions defined (accomplished or in progress). Conclusions: The AIRO vision implies that specific strategic interventions must be carried out in the field of national guidelines, education, research, and communication with patients and colleagues of other specialties in an interdisciplinary setting.
Published: 2020

21. The role of palliative interventional radiotherapy (brachytherapy) in esophageal cancer: An AIRO (Italian Association of Radiotherapy and Clinical Oncology) systematic review focused on dysphagia-free survival

Author: Lancellotta, V., Cellini, Francesco, Fionda, B., De Sanctis, V., Vidali, C., Fusco, Vincenzo, Barbera, F., Gambacorta, Maria Antonietta, Corvo, R., Magrini, S. M., Tagliaferri, Luca, Cellini F. (ORCID:0000-0002-2145-2300), Fusco V., Gambacorta M. A. (ORCID:0000-0001-5455-8737), Tagliaferri L. (ORCID:0000-0003-2308-0982), Lancellotta, V., Cellini, Francesco, Fionda, B., De Sanctis, V., Vidali, C., Fusco, Vincenzo, Barbera, F., Gambacorta, Maria Antonietta, Corvo, R., Magrini, S. M., Tagliaferri, Luca, Cellini F. (ORCID:0000-0002-2145-2300), Fusco V., Gambacorta M. A. (ORCID:0000-0001-5455-8737), and Tagliaferri L. (ORCID:0000-0003-2308-0982)
Abstract: Purpose: The aim of this review was to examine efficacy of palliative interventional radiotherapy (IRT) in esophageal cancer compared with other treatment in terms of dysphagia-free survival (DyFS) and safety. Methods and Material: A systematic research using PubMed, Scopus, and Cochrane library was performed to identify full articles evaluating the efficacy of IRT as palliation in patients with esophageal cancer. ClinicalTrials.gov was searched for ongoing or recently completed trials, and PROSPERO was searched for ongoing or recently completed systematic reviews. We analyzed only clinical study as full text of patients with symptomatic esophageal cancer treated with IRT alone or in combination with other treatment. Conference paper, survey, letter, editorial, book chapter, and review were excluded. Time restriction (1990–2018) as concerns the years of the publication was considered. The primary outcome was the duration of dysphagia relief (DyFS) after brachytherapy vs. other treatment (external-beam radiotherapy, photodynamic therapy, argon plasma coagulation, stent, and laser) during followup. Secondary outcomes included overall survival and adverse event rates. Results: The literature search resulted in 554 articles. Sixty-six articles were assessed via full text for eligibility. Of these, 59 articles were excluded for various reasons, leaving seven randomized studies. The number of evaluated patients was 905 patients, and median age was 70.5 years. In the IRT group, the median DyFS was 99 days, the most relevant G3–G4 toxicity were fistula development and stenosis reported, respectively, in 8.3% and 12.2%; the overall median survival was 175.5 days. Conclusion: In conclusion, we provided evidence-based support that IRT is an effective and safe treatment option; therefore, its underuse is no longer justified.
Published: 2020

22. The Fundamental Plane of cluster spheroidal galaxies at z$\sim1.3$. Evidence for mass-dependent evolution

Author: Saracco, P., Gargiulo, A., La Barbera, F., Annunziatella, M., Marchesini, D., Saracco, P., Gargiulo, A., La Barbera, F., Annunziatella, M., and Marchesini, D.
Abstract: We present spectroscopic observations obtained at the {\it Large Binocular Telescope} in the field of the cluster XLSSJ0223-0436 at $z=1.22$. We confirm 12 spheroids cluster members and determine stellar velocity dispersion for 7 of them. We combine these data with those in the literature for clusters RXJ0848+4453 at $z=1.27$ (8 galaxies) and XMMJ2235-2557 at $z=1.39$ (7 galaxies) to determine the Fundamental Plane of cluster spheroids. We find that the FP at $z\sim1.3$ is offset and { rotated ($\sim3\sigma$)} with respect to the local FP. The offset corresponds to a mean evolution $\Delta$\rm{log}(M$_{dyn}$/L$_B$)=(-0.5$\pm$0.1)$z$. High-redshift galaxies follow a steeper mass-dependent M$_{dyn}$/L$_B$-M$_{dyn}$ relation than local ones. Assuming $\Delta$ log$(M_{dyn}/L_B)$=$\Delta$ log$(M^*/L_B)$, higher-mass galaxies (log(M$_{dyn}$/M$_\odot$)$\geq$11.5) have a higher-formation redshift ($z_f\geq$6.5) than lower-mass ones ($z_f\leq$2 for log(M$_{dyn}$/M$_\odot$$\leq$10)), with a median $z_f\simeq2.5$ for the whole sample. Also, galaxies with higher stellar mass density host stellar populations formed earlier than those in lower density galaxies. At fixed IMF, M$_{dyn}$/M$^*$ varies systematically with mass and mass density. It follows that the evolution of the stellar populations (M$^*/L_B$) accounts for the observed evolution of M$_{dyn}/L_B$ for M$_{dyn}$$>10^{11}$ M$_\odot$ galaxies, while accounts for $\sim$85\% of the evolution at M$_{dyn}$$<10^{11}$ M$_\odot$. We find no evidence in favour of structural evolution of individual galaxies, while we find evidences that spheroids later added to the population account for the observed discrepancy at masses $<10^{11}$ M$_\odot$. [Abridged], Comment: 19 pages (including appendices), 16 figures, 5 tables, accepted for publication in MNRAS
Published: 2019
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23. A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate redshift galaxies with WEAVE

Author: Costantin, L., Iovino, A., Zibetti, S., Longhetti, M., Gallazzi, A., Mercurio, A., Lonoce, I., Balcells, M., Bolzonella, M., Busarello, G., Dalton, G., Ferré-Mateu, A., García-Benito, R., Gargiulo, A., Haines, C., Jin, S., La Barbera, F., McGee, S., Merluzzi, P., Morelli, L., Murphy, D. N. A., de Arriba, L. Peralta, Pizzella, A., Poggianti, B. M., Pozzetti, L., Sánchez-Blázquez, P., Talia, M., Tortora, C., Trager, S. C., Vazdekis, A., Vergani, D., Vulcani, B., Costantin, L., Iovino, A., Zibetti, S., Longhetti, M., Gallazzi, A., Mercurio, A., Lonoce, I., Balcells, M., Bolzonella, M., Busarello, G., Dalton, G., Ferré-Mateu, A., García-Benito, R., Gargiulo, A., Haines, C., Jin, S., La Barbera, F., McGee, S., Merluzzi, P., Morelli, L., Murphy, D. N. A., de Arriba, L. Peralta, Pizzella, A., Poggianti, B. M., Pozzetti, L., Sánchez-Blázquez, P., Talia, M., Tortora, C., Trager, S. C., Vazdekis, A., Vergani, D., and Vulcani, B.
Abstract: The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7. We aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar populations superimposed on the bulk of older ones. We produce spectra of galaxies closely mimicking data from the forthcoming Stellar Populations at intermediate redshifts Survey (StePS), a survey that uses the WEAVE spectrograph on the William Herschel Telescope. First, we assess our ability to reliably measure both ultraviolet and optical spectral indices in galaxies of different spectral types for typically expected signal-to-noise levels. Then, we analyze such mock spectra with a Bayesian approach, deriving the probability density function of r- and u-band light-weighted ages as well as of their difference. We find that the ultraviolet indices significantly narrow the uncertainties in estimating the r- and u-band light-weighted ages and their difference in individual galaxies. These diagnostics, robustly retrievable for large galaxy samples even when observed at moderate signal-to-noise ratios, allow us to identify secondary episodes of star formation up to an age of ~0.1 Gyr for stellar populations older than ~1.5 Gyr, pushing up to an age of ~1 Gyr for stellar populations older than ~5 Gyr. The difference between r-band and u-band light-weighted ages is shown to be a powerful diagnostic to characterize and constrain extended star-formation histories and the presence of young stellar populations on top of older ones. This parameter can be used to explore the interplay between different galaxy star-formation histories and physical parameters such as galaxy mass, size, morphology, and environment., Comment: 18 pages, 20 figures, accepted for publication in A&A
Published: 2019
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24. Chronos: A NIR spectroscopic survey to target the most important phases of galaxy evolution across cosmic time

Author: Ferreras, I., Cropper, M., Sharples, R., Bland-Hawthorn, J., Bruzual, G., Charlot, S., Conselice, C. J., Driver, S., Dunlop, J., Hopkins, A. M., Kaviraj, S., Kitching, T., La Barbera, F., Lahav, O., Pasquali, A., Serjeant, S., Silk, J., Windhorst, R., Ferreras, I., Cropper, M., Sharples, R., Bland-Hawthorn, J., Bruzual, G., Charlot, S., Conselice, C. J., Driver, S., Dunlop, J., Hopkins, A. M., Kaviraj, S., Kitching, T., La Barbera, F., Lahav, O., Pasquali, A., Serjeant, S., Silk, J., and Windhorst, R.
Abstract: (Abridged summary) Responding to ESA's Voyage 2050 call to define the long-term plan for the future space missions that will address the astrophysics science questions during the 2035-2050 cycle, we propose a dedicated, ultra-deep spectroscopic survey in the near infrared (NIR), that will target a mass-limited sample of galaxies during two of the most fundamental epochs of cosmic evolution: the formation of the first galaxies (at z>6; cosmic dawn), and at the peak of galaxy formation activity (between redshift z=1 and 3; cosmic noon). By way of NIR observations, it is possible to study the Lyman-alpha region in the former, and the optical rest-frame in the latter, allowing us to extract fundamental observables such as gas and stellar kinematics, chemical abundances, and ages, providing a unique legacy database covering these two crucial stages of cosmic evolution. A dedicated, space-based facility will overcome the challenges faced by ground-based telescopes, no matter how large the aperture, or the reduced field of view and low multiplex factor of the best space-based instrument in the near future, namely NIRSpec at the JWST. Our project (codename Chronos) aims to produce about 1 million high quality spectra, with a high S/N in the continuum, where information about the underlying stellar populations is encoded., Comment: 24 pages, 14 figures. Submitted to ESA's Voyage 2050 call to shape the future space science programme. arXiv admin note: text overlap with arXiv:1306.6333
Published: 2019

25. IMF radial gradients in most massive early-type galaxies

Author: La Barbera, F., Vazdekis, A., Ferreras, I., Pasquali, A., Prieto, C. Allende, Martín-Navarro, I., Aguado, D. S., de Carvalho, R. R., Rembold, S., Falcón-Barroso, J., van de Ven, G., La Barbera, F., Vazdekis, A., Ferreras, I., Pasquali, A., Prieto, C. Allende, Martín-Navarro, I., Aguado, D. S., de Carvalho, R. R., Rembold, S., Falcón-Barroso, J., and van de Ven, G.
Abstract: Using new long-slit spectroscopy obtained with X-Shooter at ESO-VLT, we study, for the first time, radial gradients of optical and Near-Infrared IMF-sensitive features in a representative sample of galaxies at the very high-mass end of the galaxy population. The sample consists of seven early-type galaxies (ETGs) at $z\sim0.05$, with central velocity dispersion in the range $300<\sigma<350$km/s. Using state-of-art stellar population synthesis models, we fit a number of spectral indices, from different chemical species (including TiO's and Na indices), to constrain the IMF slope (i.e. the fraction of low-mass stars), as a function of galactocentric distance, over a radial range out to $\sim4$kpc. ETGs in our sample show a significant correlation of IMF slope and surface mass density. The bottom-heavy population (i.e. an excess of low-mass stars in the IMF) is confined to central galaxy regions with surface mass density above $\sim 10^{10} M_\odot kpc^{-2}$, or, alternatively, within a characteristic radius of $\sim2$~kpc. Radial distance, in physical units, and surface mass density, are the best correlators to IMF variations, with respect to other dynamical (e.g. velocity dispersion) and stellar population (e.g. metallicity) properties. Our results for the most massive galaxies suggest that there is no single parameter} that fully explains variations in the stellar IMF, but IMF radial profiles at z$\sim$0 rather result from the complex formation and mass accretion history of galaxy inner and outer regions., Comment: 23 pages, 13 figures, accepted for publication in MNRAS
Published: 2019
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26. The SAMI Galaxy Survey: Stellar population radial gradients in early-type galaxies

Author: Ferreras, I., Scott, N., La Barbera, F., Croom, S. M., van de Sande, J., Hopkins, A., Colless, M., Barone, T., d'Eugenio, F., Bland-Hawthorn, J., Brough, S., Bryant, J. J., Konstantopoulos, I. S., Lagos, C., Lawrence, J. S., López-Sánchez, A., Medling, A. M., Owers, M. S., Richards, S. N., Ferreras, I., Scott, N., La Barbera, F., Croom, S. M., van de Sande, J., Hopkins, A., Colless, M., Barone, T., d'Eugenio, F., Bland-Hawthorn, J., Brough, S., Bryant, J. J., Konstantopoulos, I. S., Lagos, C., Lawrence, J. S., López-Sánchez, A., Medling, A. M., Owers, M. S., and Richards, S. N.
Abstract: We study the internal radial gradients of the stellar populations in a sample comprising 522 early-type galaxies (ETGs) from the SAMI (Sydney- AAO Multi-object Integral field spectrograph) Galaxy Survey. We stack the spectra of individual spaxels in radial bins, and derive basic stellar population properties: total metallicity ([Z/H]), [Mg/Fe], [C/Fe] and age. The radial gradient ($\nabla$) and central value of the fits (evaluated at R$_e$/4) are compared against a set of six possible drivers of the trends. We find that velocity dispersion ($\sigma$) - or, equivalently gravitational potential - is the dominant driver of the chemical composition gradients. Surface mass density is also correlated with the trends, especially with stellar age. The decrease of $\nabla$[Mg/Fe] with increasing $\sigma$ is contrasted by a rather shallow dependence of $\nabla$[Z/H] with $\sigma$ (although this radial gradient is overall rather steep). This result, along with a shallow age slope at the massive end, imposes stringent constraints on the progenitors of the populations that contribute to the formation of the outer envelopes of ETGs. The SAMI sample is split between a 'field' sample and a cluster sample. Only weak environment-related differences are found, most notably a stronger dependence of central total metallicity ([Z/H]$_{e4}$) with $\sigma$, along with a marginal trend of $\nabla$[Z/H] to steepen in cluster galaxies, a result that is not followed by [Mg/Fe]. The results presented here serve as constraints on numerical models of the formation and evolution of ETGs., Comment: 14 pages, 9 figures, 3 tables. Submitted to MNRAS
Published: 2019
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27. The Fornax 3D project: a two-dimensional view of the stellar initial mass function in the massive lenticular galaxy FCC 167

Author: Martin-Navarro, I., Lyubenova, M., van de Ven, G., Falcon-Barroso, J., Coccato, L., Corsini, E. M., Gadotti, D. A., Iodice, E., La Barbera, F., McDermid, R. M., Pinna, F., Sarzi, M., Viaene, S., de Zeeuw, P. T., Zhu, L., Martin-Navarro, I., Lyubenova, M., van de Ven, G., Falcon-Barroso, J., Coccato, L., Corsini, E. M., Gadotti, D. A., Iodice, E., La Barbera, F., McDermid, R. M., Pinna, F., Sarzi, M., Viaene, S., de Zeeuw, P. T., and Zhu, L.
Abstract: The stellar initial mass function (IMF) regulates the baryonic cycle within galaxies, and is a key ingredient to translate observations into physical quantities. Although for decades it was assumed to be universal, there is now growing observational evidence showing that the center of massive early-type galaxies host an enhanced population of low-mass stars compared to the expectations from the Milky Way. Moreover, these variations in the IMF have been found to be related to the radial metallicity variations in massive galaxies. We present here a two-dimensional stellar population analysis of the massive lenticular galaxy FCC 167 (NGC 1380) as part of the Fornax3D project. Using a newly developed stellar population fitting scheme, we derive a full two-dimensional IMF map of an early-type galaxy. This two-dimensional analysis allows us go further than a radial analysis, showing how the metallicity changes along a disc-like structure while the IMF follows a distinct, less disky distribution. Thus, our findings indicate that metallicity cannot be the sole driver of the observed radial IMF variations. In addition, a comparison with the orbital decomposition shows suggestive evidence of a coupling between stellar population properties and the internal dynamical structure of FCC 167, where metallicity and IMF maps seem to track the distribution of cold and warm orbits, respectively., Comment: 12 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2019
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28. Age, metallicity and star formation history of spheroidal galaxies in cluster at z~1.2

Author: Saracco, P., La Barbera, F., Gargiulo, A., Mannucci, F., Marchesini, D., Nonino, M., Ciliegi, P., Saracco, P., La Barbera, F., Gargiulo, A., Mannucci, F., Marchesini, D., Nonino, M., and Ciliegi, P.
Abstract: We present the analysis, based on spectra collected at the Large Binocular Telescope, of the stellar populations in seven spheroidal galaxies in the cluster XLSSJ0223 at $z$$\sim$1.22. The aim is to constrain the epoch of their formation and their star formation history. Using absorption line strenghts and full spectral fitting, we derive for the stellar populations of the seven spheroids a median age =2.4$\pm$0.6 Gyr, corresponding to a median formation redshift $<$$z_f$$>$$\sim2.6_{-0.5}^{+0.7}$ (lookback time = 11$_{-1.0}^{+0.6}$ Gyr). We find a significant scatter in age, showing that massive spheroids, at least in our targeted cluster, are not coeval. The median metallicity is [Z/H]=0.09$\pm$0.16, as for early-types in clusters at 0$<$$z$<0.9. This lack of evolution of [Z/H] over the range 0$<$$z$$<$1.3, corresponding to the last 9 billions years, suggests that no significant additional star formation and chemical enrichment are required for cluster spheroids to reach the present-day population. We do not detect significant correlation between age and velocity dispersion $\sigma_e$, or dynamical mass M$_{dyn}$, or effective stellar mass density $\Sigma_e$. On the contrary, the metallicity [Z/H] of the seven spheroids is correlated to their dynamical mass M$_{dyn}$, according to a relation similar to the one for local spheroids. [Z/H] is also anticorrelated to stellar mass density $\Sigma_e$ because of the anticorrelation between M$_{dyn}$ and $\Sigma_e$. Therefore, the basic trends observed in the local universe were already established at $z\sim1.3$, i.e. more massive spheroids are more metal rich, have lower stellar mass density and tend to be older than lower-mass galaxies., Comment: 16 pages, 6 figures, 6 tables, published on MNRAS
Published: 2019
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29. The SAMI Galaxy Survey: Stellar population radial gradients in early-type galaxies

Author: Ferreras, I., Scott, N., La Barbera, F., Croom, S. M., van de Sande, J., Hopkins, A., Colless, M., Barone, T., d'Eugenio, F., Bland-Hawthorn, J., Brough, S., Bryant, J. J., Konstantopoulos, I. S., Lagos, C., Lawrence, J. S., López-Sánchez, A., Medling, A. M., Owers, M. S., Richards, S. N., Ferreras, I., Scott, N., La Barbera, F., Croom, S. M., van de Sande, J., Hopkins, A., Colless, M., Barone, T., d'Eugenio, F., Bland-Hawthorn, J., Brough, S., Bryant, J. J., Konstantopoulos, I. S., Lagos, C., Lawrence, J. S., López-Sánchez, A., Medling, A. M., Owers, M. S., and Richards, S. N.
Abstract: We study the internal radial gradients of the stellar populations in a sample comprising 522 early-type galaxies (ETGs) from the SAMI (Sydney- AAO Multi-object Integral field spectrograph) Galaxy Survey. We stack the spectra of individual spaxels in radial bins, and derive basic stellar population properties: total metallicity ([Z/H]), [Mg/Fe], [C/Fe] and age. The radial gradient ($\nabla$) and central value of the fits (evaluated at R$_e$/4) are compared against a set of six possible drivers of the trends. We find that velocity dispersion ($\sigma$) - or, equivalently gravitational potential - is the dominant driver of the chemical composition gradients. Surface mass density is also correlated with the trends, especially with stellar age. The decrease of $\nabla$[Mg/Fe] with increasing $\sigma$ is contrasted by a rather shallow dependence of $\nabla$[Z/H] with $\sigma$ (although this radial gradient is overall rather steep). This result, along with a shallow age slope at the massive end, imposes stringent constraints on the progenitors of the populations that contribute to the formation of the outer envelopes of ETGs. The SAMI sample is split between a 'field' sample and a cluster sample. Only weak environment-related differences are found, most notably a stronger dependence of central total metallicity ([Z/H]$_{e4}$) with $\sigma$, along with a marginal trend of $\nabla$[Z/H] to steepen in cluster galaxies, a result that is not followed by [Mg/Fe]. The results presented here serve as constraints on numerical models of the formation and evolution of ETGs., Comment: 14 pages, 9 figures, 3 tables. Submitted to MNRAS
Published: 2019
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30. The Fornax 3D project: a two-dimensional view of the stellar initial mass function in the massive lenticular galaxy FCC 167

Author: Martin-Navarro, I., Lyubenova, M., van de Ven, G., Falcon-Barroso, J., Coccato, L., Corsini, E. M., Gadotti, D. A., Iodice, E., La Barbera, F., McDermid, R. M., Pinna, F., Sarzi, M., Viaene, S., de Zeeuw, P. T., Zhu, L., Martin-Navarro, I., Lyubenova, M., van de Ven, G., Falcon-Barroso, J., Coccato, L., Corsini, E. M., Gadotti, D. A., Iodice, E., La Barbera, F., McDermid, R. M., Pinna, F., Sarzi, M., Viaene, S., de Zeeuw, P. T., and Zhu, L.
Abstract: The stellar initial mass function (IMF) regulates the baryonic cycle within galaxies, and is a key ingredient to translate observations into physical quantities. Although for decades it was assumed to be universal, there is now growing observational evidence showing that the center of massive early-type galaxies host an enhanced population of low-mass stars compared to the expectations from the Milky Way. Moreover, these variations in the IMF have been found to be related to the radial metallicity variations in massive galaxies. We present here a two-dimensional stellar population analysis of the massive lenticular galaxy FCC 167 (NGC 1380) as part of the Fornax3D project. Using a newly developed stellar population fitting scheme, we derive a full two-dimensional IMF map of an early-type galaxy. This two-dimensional analysis allows us go further than a radial analysis, showing how the metallicity changes along a disc-like structure while the IMF follows a distinct, less disky distribution. Thus, our findings indicate that metallicity cannot be the sole driver of the observed radial IMF variations. In addition, a comparison with the orbital decomposition shows suggestive evidence of a coupling between stellar population properties and the internal dynamical structure of FCC 167, where metallicity and IMF maps seem to track the distribution of cold and warm orbits, respectively., Comment: 12 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2019
Full Text: View/download PDF

31. Age, metallicity and star formation history of spheroidal galaxies in cluster at z~1.2

Author: Saracco, P., La Barbera, F., Gargiulo, A., Mannucci, F., Marchesini, D., Nonino, M., Ciliegi, P., Saracco, P., La Barbera, F., Gargiulo, A., Mannucci, F., Marchesini, D., Nonino, M., and Ciliegi, P.
Abstract: We present the analysis, based on spectra collected at the Large Binocular Telescope, of the stellar populations in seven spheroidal galaxies in the cluster XLSSJ0223 at $z$$\sim$1.22. The aim is to constrain the epoch of their formation and their star formation history. Using absorption line strenghts and full spectral fitting, we derive for the stellar populations of the seven spheroids a median age =2.4$\pm$0.6 Gyr, corresponding to a median formation redshift $<$$z_f$$>$$\sim2.6_{-0.5}^{+0.7}$ (lookback time = 11$_{-1.0}^{+0.6}$ Gyr). We find a significant scatter in age, showing that massive spheroids, at least in our targeted cluster, are not coeval. The median metallicity is [Z/H]=0.09$\pm$0.16, as for early-types in clusters at 0$<$$z$<0.9. This lack of evolution of [Z/H] over the range 0$<$$z$$<$1.3, corresponding to the last 9 billions years, suggests that no significant additional star formation and chemical enrichment are required for cluster spheroids to reach the present-day population. We do not detect significant correlation between age and velocity dispersion $\sigma_e$, or dynamical mass M$_{dyn}$, or effective stellar mass density $\Sigma_e$. On the contrary, the metallicity [Z/H] of the seven spheroids is correlated to their dynamical mass M$_{dyn}$, according to a relation similar to the one for local spheroids. [Z/H] is also anticorrelated to stellar mass density $\Sigma_e$ because of the anticorrelation between M$_{dyn}$ and $\Sigma_e$. Therefore, the basic trends observed in the local universe were already established at $z\sim1.3$, i.e. more massive spheroids are more metal rich, have lower stellar mass density and tend to be older than lower-mass galaxies., Comment: 16 pages, 6 figures, 6 tables, published on MNRAS
Published: 2019
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32. The Fundamental Plane of cluster spheroidal galaxies at z$\sim1.3$. Evidence for mass-dependent evolution

Author: Saracco, P., Gargiulo, A., La Barbera, F., Annunziatella, M., Marchesini, D., Saracco, P., Gargiulo, A., La Barbera, F., Annunziatella, M., and Marchesini, D.
Abstract: We present spectroscopic observations obtained at the {\it Large Binocular Telescope} in the field of the cluster XLSSJ0223-0436 at $z=1.22$. We confirm 12 spheroids cluster members and determine stellar velocity dispersion for 7 of them. We combine these data with those in the literature for clusters RXJ0848+4453 at $z=1.27$ (8 galaxies) and XMMJ2235-2557 at $z=1.39$ (7 galaxies) to determine the Fundamental Plane of cluster spheroids. We find that the FP at $z\sim1.3$ is offset and { rotated ($\sim3\sigma$)} with respect to the local FP. The offset corresponds to a mean evolution $\Delta$\rm{log}(M$_{dyn}$/L$_B$)=(-0.5$\pm$0.1)$z$. High-redshift galaxies follow a steeper mass-dependent M$_{dyn}$/L$_B$-M$_{dyn}$ relation than local ones. Assuming $\Delta$ log$(M_{dyn}/L_B)$=$\Delta$ log$(M^*/L_B)$, higher-mass galaxies (log(M$_{dyn}$/M$_\odot$)$\geq$11.5) have a higher-formation redshift ($z_f\geq$6.5) than lower-mass ones ($z_f\leq$2 for log(M$_{dyn}$/M$_\odot$$\leq$10)), with a median $z_f\simeq2.5$ for the whole sample. Also, galaxies with higher stellar mass density host stellar populations formed earlier than those in lower density galaxies. At fixed IMF, M$_{dyn}$/M$^*$ varies systematically with mass and mass density. It follows that the evolution of the stellar populations (M$^*/L_B$) accounts for the observed evolution of M$_{dyn}/L_B$ for M$_{dyn}$$>10^{11}$ M$_\odot$ galaxies, while accounts for $\sim$85\% of the evolution at M$_{dyn}$$<10^{11}$ M$_\odot$. We find no evidence in favour of structural evolution of individual galaxies, while we find evidences that spheroids later added to the population account for the observed discrepancy at masses $<10^{11}$ M$_\odot$. [Abridged], Comment: 19 pages (including appendices), 16 figures, 5 tables, accepted for publication in MNRAS
Published: 2019
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33. A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate redshift galaxies with WEAVE

Author: Costantin, L., Iovino, A., Zibetti, S., Longhetti, M., Gallazzi, A., Mercurio, A., Lonoce, I., Balcells, M., Bolzonella, M., Busarello, G., Dalton, G., Ferré-Mateu, A., García-Benito, R., Gargiulo, A., Haines, C., Jin, S., La Barbera, F., McGee, S., Merluzzi, P., Morelli, L., Murphy, D. N. A., de Arriba, L. Peralta, Pizzella, A., Poggianti, B. M., Pozzetti, L., Sánchez-Blázquez, P., Talia, M., Tortora, C., Trager, S. C., Vazdekis, A., Vergani, D., Vulcani, B., Costantin, L., Iovino, A., Zibetti, S., Longhetti, M., Gallazzi, A., Mercurio, A., Lonoce, I., Balcells, M., Bolzonella, M., Busarello, G., Dalton, G., Ferré-Mateu, A., García-Benito, R., Gargiulo, A., Haines, C., Jin, S., La Barbera, F., McGee, S., Merluzzi, P., Morelli, L., Murphy, D. N. A., de Arriba, L. Peralta, Pizzella, A., Poggianti, B. M., Pozzetti, L., Sánchez-Blázquez, P., Talia, M., Tortora, C., Trager, S. C., Vazdekis, A., Vergani, D., and Vulcani, B.
Abstract: The upcoming new generation of optical spectrographs on four-meter-class telescopes will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7. We aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar populations superimposed on the bulk of older ones. We produce spectra of galaxies closely mimicking data from the forthcoming Stellar Populations at intermediate redshifts Survey (StePS), a survey that uses the WEAVE spectrograph on the William Herschel Telescope. First, we assess our ability to reliably measure both ultraviolet and optical spectral indices in galaxies of different spectral types for typically expected signal-to-noise levels. Then, we analyze such mock spectra with a Bayesian approach, deriving the probability density function of r- and u-band light-weighted ages as well as of their difference. We find that the ultraviolet indices significantly narrow the uncertainties in estimating the r- and u-band light-weighted ages and their difference in individual galaxies. These diagnostics, robustly retrievable for large galaxy samples even when observed at moderate signal-to-noise ratios, allow us to identify secondary episodes of star formation up to an age of ~0.1 Gyr for stellar populations older than ~1.5 Gyr, pushing up to an age of ~1 Gyr for stellar populations older than ~5 Gyr. The difference between r-band and u-band light-weighted ages is shown to be a powerful diagnostic to characterize and constrain extended star-formation histories and the presence of young stellar populations on top of older ones. This parameter can be used to explore the interplay between different galaxy star-formation histories and physical parameters such as galaxy mass, size, morphology, and environment., Comment: 18 pages, 20 figures, accepted for publication in A&A
Published: 2019
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34. IMF radial gradients in most massive early-type galaxies

Author: La Barbera, F., Vazdekis, A., Ferreras, I., Pasquali, A., Prieto, C. Allende, Martín-Navarro, I., Aguado, D. S., de Carvalho, R. R., Rembold, S., Falcón-Barroso, J., van de Ven, G., La Barbera, F., Vazdekis, A., Ferreras, I., Pasquali, A., Prieto, C. Allende, Martín-Navarro, I., Aguado, D. S., de Carvalho, R. R., Rembold, S., Falcón-Barroso, J., and van de Ven, G.
Abstract: Using new long-slit spectroscopy obtained with X-Shooter at ESO-VLT, we study, for the first time, radial gradients of optical and Near-Infrared IMF-sensitive features in a representative sample of galaxies at the very high-mass end of the galaxy population. The sample consists of seven early-type galaxies (ETGs) at $z\sim0.05$, with central velocity dispersion in the range $300<\sigma<350$km/s. Using state-of-art stellar population synthesis models, we fit a number of spectral indices, from different chemical species (including TiO's and Na indices), to constrain the IMF slope (i.e. the fraction of low-mass stars), as a function of galactocentric distance, over a radial range out to $\sim4$kpc. ETGs in our sample show a significant correlation of IMF slope and surface mass density. The bottom-heavy population (i.e. an excess of low-mass stars in the IMF) is confined to central galaxy regions with surface mass density above $\sim 10^{10} M_\odot kpc^{-2}$, or, alternatively, within a characteristic radius of $\sim2$~kpc. Radial distance, in physical units, and surface mass density, are the best correlators to IMF variations, with respect to other dynamical (e.g. velocity dispersion) and stellar population (e.g. metallicity) properties. Our results for the most massive galaxies suggest that there is no single parameter} that fully explains variations in the stellar IMF, but IMF radial profiles at z$\sim$0 rather result from the complex formation and mass accretion history of galaxy inner and outer regions., Comment: 23 pages, 13 figures, accepted for publication in MNRAS
Published: 2019
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35. Chronos: A NIR spectroscopic survey to target the most important phases of galaxy evolution across cosmic time

Author: Ferreras, I., Cropper, M., Sharples, R., Bland-Hawthorn, J., Bruzual, G., Charlot, S., Conselice, C. J., Driver, S., Dunlop, J., Hopkins, A. M., Kaviraj, S., Kitching, T., La Barbera, F., Lahav, O., Pasquali, A., Serjeant, S., Silk, J., Windhorst, R., Ferreras, I., Cropper, M., Sharples, R., Bland-Hawthorn, J., Bruzual, G., Charlot, S., Conselice, C. J., Driver, S., Dunlop, J., Hopkins, A. M., Kaviraj, S., Kitching, T., La Barbera, F., Lahav, O., Pasquali, A., Serjeant, S., Silk, J., and Windhorst, R.
Abstract: (Abridged summary) Responding to ESA's Voyage 2050 call to define the long-term plan for the future space missions that will address the astrophysics science questions during the 2035-2050 cycle, we propose a dedicated, ultra-deep spectroscopic survey in the near infrared (NIR), that will target a mass-limited sample of galaxies during two of the most fundamental epochs of cosmic evolution: the formation of the first galaxies (at z>6; cosmic dawn), and at the peak of galaxy formation activity (between redshift z=1 and 3; cosmic noon). By way of NIR observations, it is possible to study the Lyman-alpha region in the former, and the optical rest-frame in the latter, allowing us to extract fundamental observables such as gas and stellar kinematics, chemical abundances, and ages, providing a unique legacy database covering these two crucial stages of cosmic evolution. A dedicated, space-based facility will overcome the challenges faced by ground-based telescopes, no matter how large the aperture, or the reduced field of view and low multiplex factor of the best space-based instrument in the near future, namely NIRSpec at the JWST. Our project (codename Chronos) aims to produce about 1 million high quality spectra, with a high S/N in the continuum, where information about the underlying stellar populations is encoded., Comment: 24 pages, 14 figures. Submitted to ESA's Voyage 2050 call to shape the future space science programme. arXiv admin note: text overlap with arXiv:1306.6333
Published: 2019
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36. HAPPY - Humanity Assurance Protocol in interventional radiotheraPY (brachytherapy) - An AIRO Interventional Radiotherapy Study Group project

Author: Lancellotta, V., De Sanctis, V., Cornacchione, P., Barbera, F., Fusco, V., Vidali, C., Scalise, S., Panza, G., Tenore, A., Colloca, G. F., Corvo, R., Gambacorta, M. A., Maria Magrini, S., Tagliaferri, L., Cornacchione P., Fusco V., Panza G., Colloca G. F., Gambacorta M. A. (ORCID:0000-0001-5455-8737), Tagliaferri L. (ORCID:0000-0003-2308-0982), Lancellotta, V., De Sanctis, V., Cornacchione, P., Barbera, F., Fusco, V., Vidali, C., Scalise, S., Panza, G., Tenore, A., Colloca, G. F., Corvo, R., Gambacorta, M. A., Maria Magrini, S., Tagliaferri, L., Cornacchione P., Fusco V., Panza G., Colloca G. F., Gambacorta M. A. (ORCID:0000-0001-5455-8737), and Tagliaferri L. (ORCID:0000-0003-2308-0982)
Abstract: Purpose: Interventional procedures may produce emotional distress, particularly in interventional radiotherapy (IRT, brachytherapy - BT). This work would like to propose a series of recommendations/interventions to guarantee a human approach in order to favor the psychological well-being of the patient during interventional radiotherapy. Material and methods: Thirty patients affected by gynecological cancer and treated with endovaginal high-doserate IRT (HDR-IRT) were selected from January to March 2019. A specific Multiprofessional Task Group (MTG) was defined in order to analyze the needs of patients. Each component of the task group spoke with the patients to examine their needs and to investigate their fears and perception. The results of the MTG were subjected to evaluation by an Expert Team (ET) of 4 physicians from 4 different institutions for a final evaluation. Both teams discussed the patient's needs to generate a list of necessary interventions to fulfill every single need in order to obtain their inner well-being. Another team (Master Team - MT) performed an independent check. Results: All patients suggest that the main issue is the "lack of information and fear of the unknown". The fear of feeling pain was a significant source of concern, sadness, and vulnerability for the majority of the patients (76.6%). All patients do not appreciate the use of the word "bunker" to describe the treatment place. In 33.3% of patients the word "brachytherapy" (often unknown) determines insecurity while the term "interventional radiotherapy" reassures. Ninety percent of patients preferred to perform the external genital depilation at home and 80% of them would like the bladder catheter to be placed immediately before the procedure. MTG and ET defined nine "HAPPY recommendations". The MT approved the protocol without changes. Conclusions: The aim of the present paper was to produce a protocol consisting in intervention that could improve the internal serendipity and emoti
Published: 2019

37. The first sample of spectroscopically confirmed ultra-compact massive galaxies in the Kilo Degree Survey

Author: Tortora, C., Napolitano, N. R., Spavone, M., La Barbera, F., D'Ago, G., Spiniello, C., Kuijken, K. H., Roy, N., Raj, M. A., Cavuoti, S., Brescia, M., Longo, G., Pota, V., Petrillo, C. E., Radovich, M., Getman, F., Koopmans, L. V. E., Trujillo, I., Kleijn, G. Verdoes, Capaccioli, M., Grado, A., Covone, G., Scognamiglio, D., Blake, C., Glazebrook, K., Joudaki, S., Lidman, C., Wolf, C., Tortora, C., Napolitano, N. R., Spavone, M., La Barbera, F., D'Ago, G., Spiniello, C., Kuijken, K. H., Roy, N., Raj, M. A., Cavuoti, S., Brescia, M., Longo, G., Pota, V., Petrillo, C. E., Radovich, M., Getman, F., Koopmans, L. V. E., Trujillo, I., Kleijn, G. Verdoes, Capaccioli, M., Grado, A., Covone, G., Scognamiglio, D., Blake, C., Glazebrook, K., Joudaki, S., Lidman, C., and Wolf, C.
Abstract: We present results from an ongoing investigation using the Kilo Degree Survey (KiDS) on the VLT Survey Telescope (VST) to provide a census of ultra-compact massive galaxies (UCMGs), defined as galaxies with stellar masses $M_{\rm \star} > 8 \times 10^{10} \rm M_{\odot}$ and effective radii $R_{\rm e} < 1.5\,\rm kpc$. UCMGs, which are expected to have undergone very few merger events, provide a unique view on the accretion history of the most massive galaxies in the Universe. Over an effective sky area of nearly 330 square degrees, we select UCMG candidates from KiDS multi-colour images, which provide high quality structural parameters, photometric redshifts and stellar masses. Our sample of $\sim 1000$ photometrically selected UCMGs at $z < 0.5$ represents the largest sample of UCMG candidates assembled to date over the largest sky area. In this paper we present the first effort to obtain their redshifts using different facilities, starting with first results for 28 candidates with redshifts $z < 0.5$, obtained at NTT and TNG telescopes. We confirmed, as bona fide UCMGs, 19 out of the 28 candidates with new redshifts. A further 46 UCMG candidates are confirmed with literature spectroscopic redshifts (35 at $z < 0.5$), bringing the final cumulative sample of spectroscopically-confirmed lower-z UCMGs to 54 galaxies, which is the largest sample at redshifts below $0.5$. We use these spectroscopic redshifts to quantify systematic errors in our photometric selection, and use these to correct our UCMG number counts. We finally compare the results to independent datasets and simulations., Comment: Accepted for publication on MNRAS, 27 pages, 13 figures, 7 tables. This revised and improved version presents different updates. In particular, systematics and uncertainties in the measurement of the effective radii are now better discussed, and new plots are added
Published: 2018
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38. Evolution of galaxy size--stellar mass relation from the Kilo Degree Survey

Author: Roy, N., Napolitano, N. R., La Barbera, F., Tortora, C., Getman, F., Radovich, M., Capaccioli, M., Brescia, M., Cavuoti, S., Longo, G., Raj, M. A., Puddu, E., Covone, G., Amaro, V., Vellucci, C., Grado, A., Kuijken, K., Kleijn, G. Verdoes, Valentijn, E., Roy, N., Napolitano, N. R., La Barbera, F., Tortora, C., Getman, F., Radovich, M., Capaccioli, M., Brescia, M., Cavuoti, S., Longo, G., Raj, M. A., Puddu, E., Covone, G., Amaro, V., Vellucci, C., Grado, A., Kuijken, K., Kleijn, G. Verdoes, and Valentijn, E.
Abstract: We have obtained structural parameters of about 340,000 galaxies from the Kilo Degree Survey (KiDS) in 153 square degrees of data release 1, 2 and 3. We have performed a seeing convolved 2D single S\'ersic fit to the galaxy images in the 4 photometric bands (u, g, r, i) observed by KiDS, by selecting high signal-to-noise ratio (S/N > 50) systems in every bands. We have classified galaxies as spheroids and disc-dominated by combining their spectral energy distribution properties and their S\'ersic index. Using photometric redshifts derived from a machine learning technique, we have determined the evolution of the effective radius, \Re\ and stellar mass, \mst, versus redshift, for both mass complete samples of spheroids and disc-dominated galaxies up to z ~ 0.6. Our results show a significant evolution of the structural quantities at intermediate redshift for the massive spheroids ($\mbox{Log}\ M_*/M_\odot>11$, Chabrier IMF), while almost no evolution has found for less massive ones ($\mbox{Log}\ M_*/M_\odot < 11$). On the other hand, disc dominated systems show a milder evolution in the less massive systems ($\mbox{Log}\ M_*/M_\odot < 11$) and possibly no evolution of the more massive systems. These trends are generally consistent with predictions from hydrodynamical simulations and independent datasets out to redshift z ~ 0.6, although in some cases the scatter of the data is large to drive final conclusions. These results, based on 1/10 of the expected KiDS area, reinforce precedent finding based on smaller statistical samples and show the route toward more accurate results, expected with the the next survey releases., Comment: accepted by MNRAS
Published: 2018
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39. Evolution of galaxy size--stellar mass relation from the Kilo Degree Survey

Author: Roy, N., Napolitano, N. R., La Barbera, F., Tortora, C., Getman, F., Radovich, M., Capaccioli, M., Brescia, M., Cavuoti, S., Longo, G., Raj, M. A., Puddu, E., Covone, G., Amaro, V., Vellucci, C., Grado, A., Kuijken, K., Kleijn, G. Verdoes, Valentijn, E., Roy, N., Napolitano, N. R., La Barbera, F., Tortora, C., Getman, F., Radovich, M., Capaccioli, M., Brescia, M., Cavuoti, S., Longo, G., Raj, M. A., Puddu, E., Covone, G., Amaro, V., Vellucci, C., Grado, A., Kuijken, K., Kleijn, G. Verdoes, and Valentijn, E.
Abstract: We have obtained structural parameters of about 340,000 galaxies from the Kilo Degree Survey (KiDS) in 153 square degrees of data release 1, 2 and 3. We have performed a seeing convolved 2D single S\'ersic fit to the galaxy images in the 4 photometric bands (u, g, r, i) observed by KiDS, by selecting high signal-to-noise ratio (S/N > 50) systems in every bands. We have classified galaxies as spheroids and disc-dominated by combining their spectral energy distribution properties and their S\'ersic index. Using photometric redshifts derived from a machine learning technique, we have determined the evolution of the effective radius, \Re\ and stellar mass, \mst, versus redshift, for both mass complete samples of spheroids and disc-dominated galaxies up to z ~ 0.6. Our results show a significant evolution of the structural quantities at intermediate redshift for the massive spheroids ($\mbox{Log}\ M_*/M_\odot>11$, Chabrier IMF), while almost no evolution has found for less massive ones ($\mbox{Log}\ M_*/M_\odot < 11$). On the other hand, disc dominated systems show a milder evolution in the less massive systems ($\mbox{Log}\ M_*/M_\odot < 11$) and possibly no evolution of the more massive systems. These trends are generally consistent with predictions from hydrodynamical simulations and independent datasets out to redshift z ~ 0.6, although in some cases the scatter of the data is large to drive final conclusions. These results, based on 1/10 of the expected KiDS area, reinforce precedent finding based on smaller statistical samples and show the route toward more accurate results, expected with the the next survey releases., Comment: accepted by MNRAS
Published: 2018
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40. The first sample of spectroscopically confirmed ultra-compact massive galaxies in the Kilo Degree Survey

Author: Tortora, C., Napolitano, N. R., Spavone, M., La Barbera, F., D'Ago, G., Spiniello, C., Kuijken, K. H., Roy, N., Raj, M. A., Cavuoti, S., Brescia, M., Longo, G., Pota, V., Petrillo, C. E., Radovich, M., Getman, F., Koopmans, L. V. E., Trujillo, I., Kleijn, G. Verdoes, Capaccioli, M., Grado, A., Covone, G., Scognamiglio, D., Blake, C., Glazebrook, K., Joudaki, S., Lidman, C., Wolf, C., Tortora, C., Napolitano, N. R., Spavone, M., La Barbera, F., D'Ago, G., Spiniello, C., Kuijken, K. H., Roy, N., Raj, M. A., Cavuoti, S., Brescia, M., Longo, G., Pota, V., Petrillo, C. E., Radovich, M., Getman, F., Koopmans, L. V. E., Trujillo, I., Kleijn, G. Verdoes, Capaccioli, M., Grado, A., Covone, G., Scognamiglio, D., Blake, C., Glazebrook, K., Joudaki, S., Lidman, C., and Wolf, C.
Abstract: We present results from an ongoing investigation using the Kilo Degree Survey (KiDS) on the VLT Survey Telescope (VST) to provide a census of ultra-compact massive galaxies (UCMGs), defined as galaxies with stellar masses $M_{\rm \star} > 8 \times 10^{10} \rm M_{\odot}$ and effective radii $R_{\rm e} < 1.5\,\rm kpc$. UCMGs, which are expected to have undergone very few merger events, provide a unique view on the accretion history of the most massive galaxies in the Universe. Over an effective sky area of nearly 330 square degrees, we select UCMG candidates from KiDS multi-colour images, which provide high quality structural parameters, photometric redshifts and stellar masses. Our sample of $\sim 1000$ photometrically selected UCMGs at $z < 0.5$ represents the largest sample of UCMG candidates assembled to date over the largest sky area. In this paper we present the first effort to obtain their redshifts using different facilities, starting with first results for 28 candidates with redshifts $z < 0.5$, obtained at NTT and TNG telescopes. We confirmed, as bona fide UCMGs, 19 out of the 28 candidates with new redshifts. A further 46 UCMG candidates are confirmed with literature spectroscopic redshifts (35 at $z < 0.5$), bringing the final cumulative sample of spectroscopically-confirmed lower-z UCMGs to 54 galaxies, which is the largest sample at redshifts below $0.5$. We use these spectroscopic redshifts to quantify systematic errors in our photometric selection, and use these to correct our UCMG number counts. We finally compare the results to independent datasets and simulations., Comment: Accepted for publication on MNRAS, 27 pages, 13 figures, 7 tables. This revised and improved version presents different updates. In particular, systematics and uncertainties in the measurement of the effective radii are now better discussed, and new plots are added
Published: 2018
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41. The puzzling interpretation of NIR indices: The case of NaI2.21

Author: Röck, B., Vazdekis, A., La Barbera, F., Peletier, R. F., Knapen, J. H., Allende-Prieto, C., Aguado, D. S., Röck, B., Vazdekis, A., La Barbera, F., Peletier, R. F., Knapen, J. H., Allende-Prieto, C., and Aguado, D. S.
Abstract: We present a detailed study of the Na I line strength index centered in the $K$-band at $22100$, {\AA} (NaI2.21 hereafter) relying on different samples of early-type galaxies. Consistent with previous studies, we find that the observed line strength indices cannot be fit by state-of-art scaled-solar stellar population models, even using our newly developed models in the NIR. The models clearly underestimate the large NaI2.21 values measured for most early-type galaxies. However, we develop a Na-enhanced version of our newly developed models in the NIR, which - together with the effect of a bottom-heavy initial mass function - yield NaI2.21 indices in the range of the observations. Therefore, we suggest a scenario in which the combined effect of [Na/Fe] enhancement and a bottom-heavy initial mass function are mainly responsible for the large NaI2.21 indices observed for most early-type galaxies. To a smaller extent, also [C/Fe] enhancement might contribute to the large observed NaI2.21 values., Comment: 13 pages, 4 figures, accepted for publication in MNRAS
Published: 2017
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42. The third data release of the Kilo-Degree Survey and associated data products

Author: de Jong, J. T. A., Kleijn, G. A. Verdoes, Erben, T., Hildebrandt, H., Kuijken, K., Sikkema, G., Brescia, M., Bilicki, M., Napolitano, N. R., Amaro, V., Begeman, K. G., Boxhoorn, D. R., Buddelmeijer, H., Cavuoti, S., Getman, F., Grado, A., Helmich, E., Huang, Z., Irisarri, N., La Barbera, F., Longo, G., McFarland, J. P., Nakajima, R., Paolillo, M., Puddu, E., Radovich, M., Rifatto, A., Tortora, C., Valentijn, E. A., Vellucci, C., Vriend, W-J., Amon, A., Blake, C., Choi, A., Conti, I. Fenech, Herbonnet, R., Heymans, C., Hoekstra, H., Klaes, D., Merten, J., Miller, L., Schneider, P., Viola, M., de Jong, J. T. A., Kleijn, G. A. Verdoes, Erben, T., Hildebrandt, H., Kuijken, K., Sikkema, G., Brescia, M., Bilicki, M., Napolitano, N. R., Amaro, V., Begeman, K. G., Boxhoorn, D. R., Buddelmeijer, H., Cavuoti, S., Getman, F., Grado, A., Helmich, E., Huang, Z., Irisarri, N., La Barbera, F., Longo, G., McFarland, J. P., Nakajima, R., Paolillo, M., Puddu, E., Radovich, M., Rifatto, A., Tortora, C., Valentijn, E. A., Vellucci, C., Vriend, W-J., Amon, A., Blake, C., Choi, A., Conti, I. Fenech, Herbonnet, R., Heymans, C., Hoekstra, H., Klaes, D., Merten, J., Miller, L., Schneider, P., and Viola, M.
Abstract: The Kilo-Degree Survey (KiDS) is an ongoing optical wide-field imaging survey with the OmegaCAM camera at the VLT Survey Telescope. It aims to image 1500 square degrees in four filters (ugri). The core science driver is mapping the large-scale matter distribution in the Universe, using weak lensing shear and photometric redshift measurements. Further science cases include galaxy evolution, Milky Way structure, detection of high-redshift clusters, and finding rare sources such as strong lenses and quasars. Here we present the third public data release (DR3) and several associated data products, adding further area, homogenized photometric calibration, photometric redshifts and weak lensing shear measurements to the first two releases. A dedicated pipeline embedded in the Astro-WISE information system is used for the production of the main release. Modifications with respect to earlier releases are described in detail. Photometric redshifts have been derived using both Bayesian template fitting, and machine-learning techniques. For the weak lensing measurements, optimized procedures based on the THELI data reduction and lensfit shear measurement packages are used. In DR3 stacked ugri images, weight maps, masks, and source lists for 292 new survey tiles (~300 sq.deg) are made available. The multi-band catalogue, including homogenized photometry and photometric redshifts, covers the combined DR1, DR2 and DR3 footprint of 440 survey tiles (447 sq.deg). Limiting magnitudes are typically 24.3, 25.1, 24.9, 23.8 (5 sigma in a 2 arcsec aperture) in ugri, respectively, and the typical r-band PSF size is less than 0.7 arcsec. The photometric homogenization scheme ensures accurate colors and an absolute calibration stable to ~2% for gri and ~3% in u. Separately released are a weak lensing shear catalogue and photometric redshifts based on two different machine-learning techniques., Comment: small modifications; 27 pages, 12 figures, accepted for publication in Astronomy & Astrophysics
Published: 2017
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43. The puzzling interpretation of NIR indices: The case of NaI2.21

Author: Röck, B., Vazdekis, A., La Barbera, F., Peletier, R. F., Knapen, J. H., Allende-Prieto, C., Aguado, D. S., Röck, B., Vazdekis, A., La Barbera, F., Peletier, R. F., Knapen, J. H., Allende-Prieto, C., and Aguado, D. S.
Abstract: We present a detailed study of the Na I line strength index centered in the $K$-band at $22100$, {\AA} (NaI2.21 hereafter) relying on different samples of early-type galaxies. Consistent with previous studies, we find that the observed line strength indices cannot be fit by state-of-art scaled-solar stellar population models, even using our newly developed models in the NIR. The models clearly underestimate the large NaI2.21 values measured for most early-type galaxies. However, we develop a Na-enhanced version of our newly developed models in the NIR, which - together with the effect of a bottom-heavy initial mass function - yield NaI2.21 indices in the range of the observations. Therefore, we suggest a scenario in which the combined effect of [Na/Fe] enhancement and a bottom-heavy initial mass function are mainly responsible for the large NaI2.21 indices observed for most early-type galaxies. To a smaller extent, also [C/Fe] enhancement might contribute to the large observed NaI2.21 values., Comment: 13 pages, 4 figures, accepted for publication in MNRAS
Published: 2017
Full Text: View/download PDF

44. The third data release of the Kilo-Degree Survey and associated data products

Author: de Jong, J. T. A., Kleijn, G. A. Verdoes, Erben, T., Hildebrandt, H., Kuijken, K., Sikkema, G., Brescia, M., Bilicki, M., Napolitano, N. R., Amaro, V., Begeman, K. G., Boxhoorn, D. R., Buddelmeijer, H., Cavuoti, S., Getman, F., Grado, A., Helmich, E., Huang, Z., Irisarri, N., La Barbera, F., Longo, G., McFarland, J. P., Nakajima, R., Paolillo, M., Puddu, E., Radovich, M., Rifatto, A., Tortora, C., Valentijn, E. A., Vellucci, C., Vriend, W-J., Amon, A., Blake, C., Choi, A., Conti, I. Fenech, Herbonnet, R., Heymans, C., Hoekstra, H., Klaes, D., Merten, J., Miller, L., Schneider, P., Viola, M., de Jong, J. T. A., Kleijn, G. A. Verdoes, Erben, T., Hildebrandt, H., Kuijken, K., Sikkema, G., Brescia, M., Bilicki, M., Napolitano, N. R., Amaro, V., Begeman, K. G., Boxhoorn, D. R., Buddelmeijer, H., Cavuoti, S., Getman, F., Grado, A., Helmich, E., Huang, Z., Irisarri, N., La Barbera, F., Longo, G., McFarland, J. P., Nakajima, R., Paolillo, M., Puddu, E., Radovich, M., Rifatto, A., Tortora, C., Valentijn, E. A., Vellucci, C., Vriend, W-J., Amon, A., Blake, C., Choi, A., Conti, I. Fenech, Herbonnet, R., Heymans, C., Hoekstra, H., Klaes, D., Merten, J., Miller, L., Schneider, P., and Viola, M.
Abstract: The Kilo-Degree Survey (KiDS) is an ongoing optical wide-field imaging survey with the OmegaCAM camera at the VLT Survey Telescope. It aims to image 1500 square degrees in four filters (ugri). The core science driver is mapping the large-scale matter distribution in the Universe, using weak lensing shear and photometric redshift measurements. Further science cases include galaxy evolution, Milky Way structure, detection of high-redshift clusters, and finding rare sources such as strong lenses and quasars. Here we present the third public data release (DR3) and several associated data products, adding further area, homogenized photometric calibration, photometric redshifts and weak lensing shear measurements to the first two releases. A dedicated pipeline embedded in the Astro-WISE information system is used for the production of the main release. Modifications with respect to earlier releases are described in detail. Photometric redshifts have been derived using both Bayesian template fitting, and machine-learning techniques. For the weak lensing measurements, optimized procedures based on the THELI data reduction and lensfit shear measurement packages are used. In DR3 stacked ugri images, weight maps, masks, and source lists for 292 new survey tiles (~300 sq.deg) are made available. The multi-band catalogue, including homogenized photometry and photometric redshifts, covers the combined DR1, DR2 and DR3 footprint of 440 survey tiles (447 sq.deg). Limiting magnitudes are typically 24.3, 25.1, 24.9, 23.8 (5 sigma in a 2 arcsec aperture) in ugri, respectively, and the typical r-band PSF size is less than 0.7 arcsec. The photometric homogenization scheme ensures accurate colors and an absolute calibration stable to ~2% for gri and ~3% in u. Separately released are a weak lensing shear catalogue and photometric redshifts based on two different machine-learning techniques., Comment: small modifications; 27 pages, 12 figures, accepted for publication in Astronomy & Astrophysics
Published: 2017
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45. Inferenza causale e approccio controfattuale

Author: Pais, I, Barbera, F, Argentin, G, Pais, I, Barbera, F, and Argentin, G
Abstract: Il capitolo evidenzia la necessità per la sociologia di affrontare la difficile sfida dell'inferenza causale e illustra approcci diversi ad essa, concentrandosi su un insieme di tecniche che sono state messe a punto prevalentemente all’interno di quello che è comunemente detto “approccio "controfattuale”. Si evidenziano potenzialità e limiti di questo approccio per lo sviluppo della sociologia.
Published: 2017

46. Migrazioni e mercato del lavoro

Author: Barbera, F, Pais, I (a cura di), Fellini, I, FELLINI, IVANA, Barbera, F, Pais, I (a cura di), Fellini, I, and FELLINI, IVANA
Published: 2017

47. Mark Granovetter. radicamento dell’azione economica: le reti sociali

Author: Barbera, F, Pais, I, Andreotti, A, ANDREOTTI, ALBERTA ARGIA, Barbera, F, Pais, I, Andreotti, A, and ANDREOTTI, ALBERTA ARGIA
Abstract: Il saggio, situato all'interno di un manuale per studenti, si propone di analizzare il contributo di Mark Granovetter alla comprensione dei fenomeni economici ed economicamente rilevanti, concentrandosi in particolare sul concetto di radicamento sociale. Alla base di tale concetto vi è un modo specifico di interpretare i fenomeni economici: essi non sono mai scissi dalla struttura sociale, ed è proprio la relazione tra economia e struttura sociale, secondo questo autore, a dover essere indagata. In questa impostazione, le reti sociali sono un elemento centrale della struttura sociale e contribuiscono a spiegare il rapporto tra azione individuale e istituzioni, esse diventano uno strumento analitico di collegamento tra il livello di analisi micro e macro. Il saggio propone poi tre ricerche empiriche dell'autore che illustrano lo studio di fenomeni economici secondo questa prospettiva definita nuova sociologia economica.
Published: 2017

48. L’inclusione del consumatore nella catena del valore

Author: Barbera F., Pais I., Arcidiacono, Davide Luca, Arcidiacono D. (ORCID:0000-0003-1958-7238), Barbera F., Pais I., Arcidiacono, Davide Luca, and Arcidiacono D. (ORCID:0000-0003-1958-7238)
Abstract: Si analizza il rapporto tra trasformazione produttiva ed evoluzione dell'analisi sociologica sul consumo
Published: 2017

49. Come si fanno le domande? Intervista e Questionario

Author: Barbera F., Pais I., Arcidiacono, Davide Luca, Arcidiacono D. (ORCID:0000-0003-1958-7238), Barbera F., Pais I., Arcidiacono, Davide Luca, and Arcidiacono D. (ORCID:0000-0003-1958-7238)
Abstract: capitolo manualistico sulle diverse tecniche di rilevazione dati: questionario e intervista
Published: 2017

50. Dentro e oltre il welfare mix

Author: Barbera, F., Pais, I., Lodigiani, Rosangela, Rosangela Lodigiani (ORCID:0000-0001-9047-9761), Barbera, F., Pais, I., Lodigiani, Rosangela, and Rosangela Lodigiani (ORCID:0000-0001-9047-9761)
Abstract: Le differenze storicamente emerse tra i sistemi di welfare non riguardano solo le priorità, le forme e l’ampiezza della copertura dall’intervento pubblico, e i modi in cui tale intervento è garantito e organizzato dallo Stato attraverso forme istituzionalizzate di solidarietà collettiva, bensìanche i modi in cui nei diversi sistemi è riconosciuto e valorizzato l’apporto di altre agenzie alla produzione del benessere sociale, in particolare, mercato, famiglie e formazioni sociali intermedie. Resterebbe altrimenti in ombra un «residuo di welfare» straordinariamente ampio. Il capitolo indaga come si ridefinisce oggi il welfare mix, nella logica della pluralizzazione.
Published: 2017

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