Search

Your search keyword '"Domínguez Palmero, L."' showing total 20 results
Start Over Author "Domínguez Palmero, L."
20 results on '"Domínguez Palmero, L."'

1. WEAVE First Light Observations: Origin and Dynamics of the Shock Front in Stephan's Quintet

Author

Arnaudova, M. I., Das, S., Smith, D. J. B., Hardcastle, M. J., Hatch, N., Trager, S. C., Smith, R. J., Drake, A. B., McGarry, J. C., Shenoy, S., Stott, J. P., Knapen, J. H., Hess, K. M., Duncan, K. J., Gloudemans, A., Best, P. N., García-Benito, R., Kondapally, R., Balcells, M., Couto, G. S., Abrams, D. C., Aguado, D., Aguerri, J. A. L., Barrena, R., Benn, C. R., Bensby, T., Berlanas, S. R., Bettoni, D., Cano-Infantes, D., Carrera, R., Concepción, P. J., Dalton, G. B., D'Ago, G., Dee, K., Domínguez-Palmero, L., Drew, J. E., Escott, E. L., Fariña, C., Fossati, M., Fumagalli, M., Gafton, E., Gribbin, F. J., Hughes, S., Iovino, A., Jin, S., Lewis, I. J., Longhetti, M., Méndez-Abreu, J., Mercurio, A., Molaeinezhad, A., Molinari, E., Monguió, M., Murphy, D. N. A., Picó, S., Pieri, M. M., Ridings, A. W., Romero-Gómez, M., Schallig, E., Shimwell, T. W., Skvarĉ, R., Stuik, R., Vallenari, A., van der Hulst, J. M., Walton, N. A., and Worley, C. C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a detailed study of the large-scale shock front in Stephan's Quintet, a byproduct of past and ongoing interactions. Using integral-field spectroscopy from the new William Herschel Telescope Enhanced Area Velocity Explorer (WEAVE), recent 144 MHz observations from the LOFAR Two-metre Sky Survey (LoTSS), and archival data from the Very Large Array and James Webb Space Telescope (JWST), we obtain new measurements of key shock properties and determine its impact on the system. Harnessing the WEAVE large integral field unit's (LIFU) field of view (90 $\times$ 78 arcsec$^{2}$), spectral resolution ($R\sim2500$) and continuous wavelength coverage across the optical band, we perform robust emission line modeling and dynamically locate the shock within the multi-phase intergalactic medium (IGM) with higher precision than previously possible. The shocking of the cold gas phase is hypersonic, and comparisons with shock models show that it can readily account for the observed emission line ratios. In contrast, we demonstrate that the shock is relatively weak in the hot plasma visible in X-rays (with Mach number of $\mathcal{M} \sim 2 - 4$), making it inefficient at producing the relativistic particles needed to explain the observed synchrotron emission. Instead, we propose that it has led to an adiabatic compression of the medium, which has increased the radio luminosity ten-fold. Comparison of the Balmer line-derived extinction map with the molecular gas and hot dust observed with JWST suggests that pre-existing dust may have survived the collision, allowing the condensation of H$_{2}$ - a key channel for dissipating the shock energy., Comment: 23 pages, 15 figures, accepted for publication in MNRAS

Published
2024
Full Text
View/download PDF

2. Optical spectral characterization of the gamma-ray blazars S4 0954+65, TXS 1515-273 and RX J0812.0+0237

Author

González, J. Becerra, Acosta-Pulido, J. A., Boschin, W., Clavero, R., Otero-Santos, J., Carballo-Bello, J. A., and Domínguez-Palmero, L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

The study of gamma-ray blazars is usually hindered due to the lack of information on their redshifts and on their low energy photon fields. This information is key to understand the effect on the gamma-ray absorption due to either extragalactic background light and/or intrinsic absorption and emission processes. All this information has also an impact on the determination of the location of the emitting region within the relativistic jets. In this work a new optical spectroscopic characterization is presented for three gamma-ray blazars: S4 0954+65, TXS 1515-273 and RX J0812.0+0237. For all the three targets the redshift determination is successful, and for the first time in the case of TXS 1515-273 and RX J0812.0+0237. Their classification as BL~Lac type is confirmed based on these new optical spectra. For S4 0954+65 (z=$0.3694\pm0.0011$) an estimation on the disk, broad line region and torus luminosities is performed based on the observed optical emission lines. The results from this study are compatible with the nature of S4 0954+65 as a transitional blazar. In the case of TXS 1515-273 ($z=0.1281\pm 0.0004$), although its optical spectrum is dominated by the continuum emission from the jet, applying the pPXF technique, the stellar population can be unveiled and is compatible with an old and metallic population. It is also the case of RX J0812.0+0237 ($z=0.1721\pm 0.0002$). Moreover, this work confirms that the optical spectrum from RX J0812.0+0237 is compatible with an extreme blazar classification., Comment: Submitted to MNRAS

Published
2020
Full Text
View/download PDF

3. Fossil group origins: VIII RXJ075243.6+455653 a transitionary fossil group

Author

Aguerri, J. A. L., Longobardi, A., Zarattini, S., Kundert, A., D'Onghia, E., and Dominguez-Palmero, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

It is thought that fossil systems are relics of structure formation in the primitive Universe. They are galaxy aggregations that have assembled their mass at high redshift with few or no subsequent accretion. Observationally these systems are selected by large magnitude gaps between their 1st and 2nd ranked galaxies. Nevertheless, there is still debate over whether or not this observational criterium selects dynamically evolved ancient systems. We have studied the properties of the nearby fossil group RXJ075243.6+455653 in order to understand the mass assembly of this system. Deep spectroscopic observations allow us to construct the galaxy luminosity function (LF) of RXJ075243.6+455653 down to M*+ 6. The analysis of the faint-end of the LF in groups and clusters provides valuable information about the mass assembly of the system. In addition, we have analyzed the nearby large-scale structure around this group. We identified 26 group members within r200=0.9 Mpc. The LF of the group shows a flat faint-end slope ( -1.08 +/- 0.33). This low density of dwarf galaxies is confirmed by the low value of the dwarf-to-giant ratio (DGR = 0.99 +/- 0.49) for this system. Both the lack of dwarf galaxies and the low luminosity of the BGG suggests that RXJ075243.6+455653 still has to accrete mass from its nearby environment. This mass accretion will be achieved because it is the dominant structure of a rich environment formed by several groups of galaxies (15) within 7 Mpc from the group center and with +/- 1000$ km/s. RXJ075243.6+455653 is a group of galaxies that has not yet completed the process of its mass assembly. This new mass accretion will change the fossil state of the group. This group is an example of a galaxy aggregation selected by a large magnitude gap but still in the process of the accretion of its mass (Abridged)., Comment: 9 pages, 9 figures, accepted in A&A

Published
2017
Full Text
View/download PDF

4. 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

5. Bulges of disk galaxies at intermediate redshifts. I. Samples with and without bulges in the Groth Strip Survey

Author

Dominguez-Palmero, L., Balcells, M., Erwin, P., Prieto, M., Cristobal-Hornillos, D., Eliche-Moral, M. C., and Guzman, R.

Subjects
Astrophysics
Abstract

We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measures quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85 kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6"-diameter apertures. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1 < z < 1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and restframe) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples., Comment: 38 pages, 10 figures, appendix A (6 tables), appendix B (54 pstamps), appendix C (7 figures). Accepted for publication in A&A

Published
2008
Full Text
View/download PDF

6. Galactic bulges from Hubble Space Telescope NICMOS observations: the lack of r^{1/4} bulges

Author

Balcells, M., Graham, A. W., Dominguez-Palmero, L., and Peletier, R. F.

Subjects
Astrophysics
Abstract

We use HST near-infrared imaging to explore the shapes of the surface brightness profiles of bulges of S0-Sbc galaxies at high resolution. Modeling extends to the outer bulge via bulge-disk decompositions of combined HST - ground based profiles. Compact, central unresolved components similar to those reported by others are found in ~84% of the sample. We also detect a moderate frequency (~34%) of nuclear components with exponential profiles which may be disks or bars. Adopting the S\'ersic r^{1/n} functional form for the bulge, none of the bulges have an r^{1/4} behaviour; derived S\'ersic shape-indices are = 1.7 \pm 0.7. For the same sample, fits to NIR ground-based profiles yield S\'ersic indices up to n = 4-6. The high-$n$ of ground-based profiles are a result of nuclear point sources blending with the bulge extended light due to seeing. The low S\'ersic indices are not expected from merger violent relaxation, and argue against significant merger growth for most bulges., Comment: 4 pages, 3 figures, accepted for the Astrophysical Journal Letters

Published
2002
Full Text
View/download PDF

7. Nuclear Components in the Bulges of Disk Galaxies

Author

Balcells, M., Dominguez-Palmero, L., Graham, A., and Peletier, R. F.

Subjects
Astrophysics
Abstract

By combining surface brightness profiles from images taken in the HST/NICMOS F160W and ground-based (GB) $K$ bands, we have obtained NIR profiles for a well studied sample of inclined disk galaxies, spanning radial ranges from 20 pc to a few kpc. We fit PSF-convolved Sersic-plus-exponential laws to the profiles, and compare the results with the fits to the ground-based data alone. HST profiles show light excesses over the best-fit Sersic law in the inner ~1 arcsec. This is often as a result of inner power-law cusps similar to the inner profiles of intermediate-luminosity elliptical galaxies., Comment: 4 pages, 5 figures. Poster paper to "The Central kpc of Starbursts and AGN: the La Palma connection'', Eds. J.H. Knapen, J.E. Beckman, I. Shlosman and T.J. Mahoney, ASP conf. series, in press (2001)

Published
2001

8. Bulges of disk galaxies at intermediate redshifts I. Samples with and without bulges in the Groth Strip survey

Author

Domínguez Palmero., L., Balcells, M., Erwin, P., Prieto, M., Cristóbal Hornillos, D., Eliche Moral, María del Carmen, Guzmán, R., Domínguez Palmero., L., Balcells, M., Erwin, P., Prieto, M., Cristóbal Hornillos, D., Eliche Moral, María del Carmen, and Guzmán, R.

Abstract

© ESO 2008. We thank the anonymous referee for suggestions that improved the paper and Ignacio Trujillo, Carlos López, David Abreu, Marc Vallbe, Enrique García Dabo, Alfonso Aragón Salamanca, David Koo, and Reynier Peletier, for useful discussions. This work was supported by the Spanish Programa Nacional de Astronomía y Astrofísica through project number AYA2006-12955. Some/all of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. This work uses data obtained with support of the National Science Foundation grants AST 95-29028 and AST 00-71198., Context. Analysis of bulges to redshifts of up to z∽1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. Aims. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. Methods. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measures quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85 kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6 '' diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. Results. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1 < z < 1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well a, Programa Nacional de Astronomia y Astrofisica (PNAYA), España, NASA, Ministerio de Economía y Competitividad (MINECO), España, National Science Foundation (NFS), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

10. First results of the GOYA survey: low-mass star-forming galaxies at different redshifts with the MOS mode of EMIR

Author

Cabello, C., Gallego, J., Cardiel, N., Pascual, S., Garzón, F., Balcells, M., Castro-Rodríguez, N., Domínguez-Palmero, L., Hammersley, P., Laporte, N., Patrick, L. R., Pello, R., Prieto, M., Streblyanska, A., Arnouts, S., Chanchaiworawit, S., Guzmán, R., Team, Emir-Goya, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), European Commission [Brussels], Departamento de Astrofisica, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), INSTITUTO DE INVESTIGACIONES MARINAS ECOBIOMAR VIGO ESP, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Instituto de Astrofisica de Canarias (IAC), Department of Chemistry, RIDER UNIVERSITY, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Cognition, Langues, Langage, Ergonomie (CLLE-ERSS), École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Bordeaux Montaigne (UBM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de Tarapaca, Universidad de La Laguna [Tenerife - SP] (ULL), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2020

14. Reducing EMIR spectroscopic data with Python

Author

Cardiel, N., Pascual, S., Gallego, J., Cabello, C., Garzón, F., Balcells, M., Castro-Rodríguez, N., Domínguez-Palmero, L., Hammersley, P., Laporte, N., Patrick, L. R., Pelló, R., Prieto, M., Streblyanska, A., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Montesinos, B. and Asensio Ramos, A. and Buitrago, F. and Schödel, R. and Villaver, E. and Pérez-Hoyos, S. and Ordó nez-Etxeberria, and I.

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2019

15. Fossil group origins

Author

Aguerri, J. A. L., primary, Longobardi, A., additional, Zarattini, S., additional, Kundert, A., additional, D’Onghia, E., additional, and Domínguez-Palmero, L., additional

Published
2018
Full Text
View/download PDF

16. The evolutionary paths among galaxy types on the red sequence at 0.3 < Z < 1.5

Author

Eliche Moral, María del Carmen, Prieto, M., Balcells, M., Abreu, D., Barro, Guillermo, Cristobal Hornillos, D., Domínguez Palmero, L., Erwin, P., Gallego Maestro, Jesús, Guzmán, R., Hempel, A., López Sanjuan, C., Pérez González, Pablo Guillermo, and Zamorano Calvo, Jaime

Subjects
Astrofísica, Astronomía
Abstract

We have studied the main evolutionary paths among the galaxy types residing on the massive end of the Red Sequence and nearby locations on the Green Valley during the last ∼9 Gyr. The morphological and star formation properties of a sample of these galaxies at 0 . 3 < z < 1 .5 with stellar masses M_∗ > 5 × 10^10 M_⊙ have been analysed. We present direct observational evidence for the first time of the existence of two main evolutionary paths among the different red galaxy types since z ∼ 1 .5, which provide some clues on the nature of the processes that have governed the assembly of present-day massive quiescent galaxies. The results are in excellent agreement with the hierarchical evolutionary framework proposed in the Eliche-Moral et al. (2010) model. Data from SHARDS (one of the ESO/GTC Large Programmes approved in 2009A) will complement and improve the present findings, shedding some light into many of the still unsettled questions concerning the migration of galaxies from the Blue Cloud to the Red Sequence at z < 1 .5.

Published
2013

17. Fossil group origins VIII. RX J075243.6+455653 a transitionary fossil group.

Author

Aguerri, J. A. L., Longobardi, A., Zarattini, S., Kundert, A., D'Onghia, E., and Domínguez-Palmero, L.

Subjects
GALACTIC redshift, ASTRONOMICAL observations, STELLAR mass, STELLAR structure, SPECTRUM analysis
Abstract

Context. It is thought that fossil systems are relics of structure formation in the primitive Universe. They are galaxy aggregations that have assembled their mass at high redshift with few or no subsequent accretion. Observationally these systems are selected by large magnitude gaps between their 1st and 2nd ranked galaxies (Δm12). Nevertheless, there is still debate over whether or not this observational criterium selects dynamically evolved ancient systems. Aims. We have studied the properties of the nearby fossil group RX J075243.6+455653 in order to understand the mass assembly of this system. Methods. Deep spectroscopic observations allow us to construct the galaxy luminosity function (LF) of RX J075243.6+455653 down to Mr*+6. The analysis of the faint-end of the LF in groups and clusters provides valuable information about the mass assembly of the system. In addition, we have analyzed the nearby large-scale structure around this group. Results. We identified 26 group members within r200 ~ 0.96 Mpc. These galaxies are located at Vc = 15551 ± 65 km s-1 and have a velocity dispersion of σc = 333 ± 46 km s-1. The X-ray luminosity of the group is LX = 2.2 × 1043 h70-2 erg s-1, resulting in a mass of M = 4.2 × 1013 h70-1 within 0.5r200. The group has Δm12 = 2.1 within 0.5r200, confirming the fossil nature of this system. RX J075243.6+455653 has a central brightest group galaxy (BGG) with Mr = -22.67, one of the faintest BGGs observed in fossil systems. The LF of the group shows a flat faint-end slope (α = -1.08 ± 0.33). This low density of dwarf galaxies is confirmed by the low value of the dwarf-to-giant ratio (DGR = 0.99 ± 0.49) for this system. Both the lack of dwarf galaxies and the low luminosity of the BGG suggests that RX J075243.6+455653 still has to accrete mass from its nearby environment. This mass accretion will be achieved because it is the dominant structure of a rich environment formed by several groups of galaxies (15) within ~ 7 Mpc from the group center and with ± 1000 km s-1. Conclusions. RX J075243.6+455653 is a group of galaxies that has not yet completed the process of its mass assembly. This new mass accretion will change the fossil state of the group. This group is an example of a galaxy aggregation selected by a large magnitude gap but still in the process of the accretion of its mass. [ABSTRACT FROM AUTHOR]

Published
2018
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results