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122 results on '"Blay, Pere"'

1. Photometric classification of QSOs from ALHAMBRA survey using random forest

Author: Arroquia-Cuadros, Benjamin, Sanchez, Nestor, Gomez, Vicent, Blay, Pere, Martinez-Badenes, Vicent, and Nieves-Seoane, Lorena
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Context: Given the current big data era in Astronomy, machine learning based methods have being applied over the last years to identify or classify objects like quasars, galaxies and stars from full sky photometric surveys. Aims: Here we systematically evaluate the performance of Random Forests (RF) in classifying quasars using either magnitudes or colours, both from broad and narrow-band filters, as features. Methods: The working data consists of photometry from the ALHAMBRA Gold Catalogue that we cross-matched with the Sloan Digital Sky Survey (SDSS) and with the Million Quasars Catalogue (Milliquas) for objects labelled as quasars, galaxies or stars. A RF classifier is trained and tested to evaluate the effect on final accuracy and precision of varying the free parameters and the effect of using narrow or broad-band magnitudes or colours. Results: Best performances of the classifier yielded global accuracy and quasar precision around 0.9. Varying model free parameters (within reasonable ranges of values) has no significant effects on the final classification. Using colours instead of magnitudes as features results in better performances of the classifier, especially using colours from the ALHAMBRA Survey. Colours that contribute the most to the classification are those containing the near-infrared $JHK$ bands., Comment: 7 pages including 6 figures and 3 tables. Accepted for publication in Astronomy and Astrophysics
Published: 2023
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2. Study of the open cluster Alessi-Teutsch 9 (ASCC 10) using multiband photometry and Gaia EDR3

Author: Sanchez, Nestor, Lopez-Martinez, Fatima, Ocando, Sandra, and Blay, Pere
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: There is a growing interest in the automated characterization of open clusters using data from the Gaia mission. This work evidences the importance of choosing an appropriate sampling radius (the radius of the circular region around the cluster used to extract the data) and the usefulness of additional multiband photometry in order to achieve accurate results. We address this issue using as a case study the cluster Alessi-Teutsch 9. The optimal sampling is determined by counting the number of assigned members at different sampling radii. By using this strategy with data from Gaia EDR3 and with observed photometry in 12 bands spanning the optical range from 3000 to 10000 \AA, approximately, we are able to obtain reliable members and to determine the properties of the cluster. The spatial distribution of stars show a two-component structure with a central core of radius ~12-13 arcmin and an outer halo extending out to 35 arcmin. With the derived cluster distance (654 pc) we obtain that the number density of stars is ~0.06 star/pc^3, making Alessi-Teutsch 9 one of the less dense known open clusters. The short relaxation time reveals that it is a dynamically relaxed and gravitationally bound system., Comment: 16 pages including 9 figures and 3 tables (Table 2 will be available online). Accepted for publication in Astrophysics and Space Science
Published: 2021
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3. Advances in Understanding High-Mass X-ray Binaries with INTEGRAL and Future Directions

Author: Kretschmar, Peter, Fürst, Felix, Sidoli, Lara, Bozzo, Enrico, Alfonso-Garzón, Julia, Bodaghee, Arash, Chaty, Sylvain, Chernyakova, Masha, Ferrigno, Carlo, Manousakis, Antonios, Negueruela, Ignacio, Postnov, Konstantin, Paizis, Adamantia, Reig, Pablo, Rodes-Roca, José Joaquín, Tsygankov, Sergey, Bird, Antony J., Kühnel, Matthias Bissinger né, Blay, Pere, Caballero, Isabel, Coe, Malcolm J., Domingo, Albert, Doroshenko, Victor, Ducci, Lorenzo, Falanga, Maurizio, Grebenev, Sergei A., Grinberg, Victoria, Hemphill, Paul, Kreykenbohm, Ingo, Fritz, Sonja Kreykenbohm né, Li, Jian, Lutovinov, Alexander A., Martínez-Núñez, Silvia, Mas-Hesse, J. Miguel, Masetti, Nicola, McBride, Vanessa A., Neronov, Andrii, Pottschmidt, Katja, Rodriguez, Jérôme, Romano, Patrizia, Rothschild, Richard E., Santangelo, Andrea, Sguera, Vito, Staubert, Rüdiger, Tomsick, John A., Torrejón, José Miguel, Torres, Diego F., Walter, Roland, Wilms, Jörn, Wilson-Hodge, Colleen A., and Zhang, Shu
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: High mass X-ray binaries are among the brightest X-ray sources in the Milky Way, as well as in nearby Galaxies. Thanks to their highly variable emissions and complex phenomenology, they have attracted the interest of the high energy astrophysical community since the dawn of X-ray Astronomy. In more recent years, they have challenged our comprehension of physical processes in many more energy bands, ranging from the infrared to very high energies. In this review, we provide a broad but concise summary of the physical processes dominating the emission from high mass X-ray binaries across virtually the whole electromagnetic spectrum. These comprise the interaction of stellar winds with the high gravitational and magnetic fields of compact objects, the behaviour of matter under extreme magnetic and gravity conditions, and the perturbation of the massive star evolutionary processes by presence in a binary system. We highlight the role of the INTEGRAL mission in the discovery of many of the most interesting objects in the high mass X-ray binary class and its contribution in reviving the interest for these sources over the past two decades. We show how the INTEGRAL discoveries have not only contributed to significantly increase the number of high mass X-ray binaries known, thus advancing our understanding of the population as a whole, but also have opened new windows of investigation that stimulated the multi-wavelength approach nowadays common in most astrophysical research fields. We conclude the review by providing an overview of future facilities being planned from the X-ray to the very high energy domain that will hopefully help us in finding an answer to the many questions left open after more than 18 years of INTEGRAL scientific observations., Comment: 61 pages, 22 figures, 1 table, will be published in New Astronomy Reviews
Published: 2020
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4. K2-280b -- a low density warm sub-Saturn around a mildly evolved star

Author: Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Deeg, Hans J., Hirano, Teruyuki, Barragán, Oscar, Kuzuhara, Masayuki, Dai, Fei, Luque, Rafael, Persson, Carina M., Fridlund, Malcolm, Johnson, Marshall C., Korth, Judith, Livingston, John H., Grziwa, Sascha, Mathur, Savita, Hatzes, Artie P., Prieto-Arranz, Jorge, Nespral, David, Hidalgo, Diego, Hjorth, Maria, Albrecht, Simon, Van Eylen, Vincent, Lam, Kristine W. F., Cochran, William D., Esposito, Massimiliano, Csizmadia, Szilárd, Guenther, Eike W., Kabath, Petr, Blay, Pere, Brahm, Rafael, Jordán, Andrés, Espinoza, Néstor, Rojas, Felipe, Barris, Núria Casasayas, Rodler, Florian, Sobrino, Roi Alonso, Cabrera, Juan, Carleo, Ilaria, Chaushev, Alexander, de Leon, Jerome, Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Fukui, Akihiko, Georgieva, Iskra, González-Cuesta, Lucía, Knudstrup, Emil, Lund, Mikkel N., Rodríguez, Pilar Montañes, Murgas, Felipe, Narita, Norio, Niraula, Prajwal, Pätzold, Martin, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M. S., and Subjak, Jano
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present an independent discovery and detailed characterisation of K2-280b, a transiting low density warm sub-Saturn in a 19.9-day moderately eccentric orbit (e = 0.35_{-0.04}^{+0.05}) from K2 campaign 7. A joint analysis of high precision HARPS, HARPS-N, and FIES radial velocity measurements and K2 photometric data indicates that K2-280b has a radius of R_b = 7.50 +/- 0.44 R_Earth and a mass of M_b = 37.1 +/- 5.6 M_Earth, yielding a mean density of 0.48_{-0.10}^{+0.13} g/cm^3. The host star is a mildly evolved G7 star with an effective temperature of T_{eff} = 5500 +/- 100 K, a surface gravity of log(g) = 4.21 +/- 0.05 (cgs), and an iron abundance of [Fe/H] = 0.33 +/- 0.08 dex, and with an inferred mass of M_star = 1.03 +/- 0.03 M_sun and a radius of R_star = 1.28 +/- 0.07 R_sun. We discuss the importance of K2-280b for testing formation scenarios of sub-Saturn planets and the current sample of this intriguing group of planets that are absent in the Solar System., Comment: 14 pages, 9 figures, 5 tables, accepted for publication in MNRAS
Published: 2020
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5. Multi-wavelength observations of PSRJ 2032+4127 during the 2017 periastron passage

Author: Chernyakova, Maria, Malyshev, Denys, Blay, Pere, van Soelen, Brian, and Tsygankov, Sergey
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: PSRJ 2032+4127 is only the second known gamma-ray binary where it is confirmed that a young radio pulsar is in orbit around a Be-star. The interaction of the pulsar wind with the mass outflow from the companion leads to broad band emission from radio up to TeV energies. In the current paper we present results of optical monitoring of the 2017 periastron passage with the Nordic Optical Telescope. These observations are complemented by X-ray (Swift/XRT, NuSTAR) and GeV (Fermi/LAT) monitoring. Joint analysis of the evolution of the parameters of the Halpha line and the broadband (X-ray to TeV) spectral shape allows us to propose a model linking the observed emission to the interaction of the pulsar and Be-star winds under the assumption of the inclined disc geometry. Our model allows the observed flux and spectral evolution of the system to be explained in a self-consistent way., Comment: accepted to MNRAS
Published: 2020
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6. Observatory science with eXTP

Author: Zand, Jean J. M. in 't, Bozzo, Enrico, Qu, Jinlu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, Xuefeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Chichuan, Jin, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aı, Antonino, Dai, Zi-Gao, D'Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D'Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, Xilong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, Mingyu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, Fangjun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, Yunpeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O'Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Torres, Miguel A. Pérez, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodrıguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, Lijing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jirı, Thielemann, F. -K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, Junfeng, Watts, Anna L., Weng, Shanshan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, Shaolin, Xu, Yupeng, Yan, Zhen, Younes, George, Yu, Wenfei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2018
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7. EXO 2030+375 Restarts in Reverse

Author: Kretschmar, Peter, Fuerst, Felix, Wilson-Hodge, Colleen A., Blay, Pere, Kajava, Jari, Alfonso-Garzón, Julia, Kühnel, Matthias, Kreykenbohm, Ingo, Wilms, Jörn, Jenke, Peter A., and Pottschmidt, Katja
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Be X-ray binary pulsar EXO 2030+375, first detected in 1985, has shown a significant detected X-ray outburst at nearly every periastron passage of its 46-day orbit for the past ~25 years, with one low state accompanied by a torque reversal in the 1990s. In early 2015 the outbursts progressively became fainter and less regular while the monotonic spin-up flattened. At the same time a decrease in the H$\alpha$ line equivalent width was reported, indicating a change in the disk surrounding the mass donor. In order to explore the source behaviour in the poorly explored low-flux state with a possible transition to a state of centrifugal inhibition of accretion we have undertaken an observing campaign with Swift/XRT, NuSTAR and the Nordic Optical Telescope (NOT). This conference contribution reports the preliminary results obtained from our campaign., Comment: 11th INTEGRAL Conference Gamma-Ray Astrophysics in Multi-Wavelength Perspective, 10-14 October 2016, Amsterdam, The Netherlands. 7 pages
Published: 2017

8. The transiting multi-planet system HD3167: a 5.7 MEarth Super-Earth and a 8.3 MEarth mini-Neptune

Author: Gandolfi, Davide, Barragán, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Dai, Fei, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmüller, Philipp, Erikson, Anders, Hernández, Jonay I. González, Guenther, Eike W., Hirano, Teruyuki, Mascareño, Alejandro S., Narita, Norio, Palle, Enric, Parviainen, Hannu, Pätzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., and Zakhozhay, Olga V.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: HD3167 is a bright (V=8.9 mag) K0V star observed by the NASA's K2 space mission during its Campaign 8. It has been recently found to host two small transiting planets, namely, HD3167b, an ultra short period (0.96 d) super-Earth, and HD3167c, a mini-Neptune on a relatively long-period orbit (29.85 d). Here we present an intensive radial velocity follow-up of HD3167 performed with the FIES@NOT, HARPS@ESO-3.6m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69+/-0.44 MEarth, radius of 1.574+/-0.054 REarth, and mean density of 8.00(+1.0)(-0.98) g/cm^3, HD3167b joins the small group of ultra-short period planets known to have a rocky terrestrial composition. HD3167c has a mass of 8.33 (+1.79)(-1.85) MEarth and a radius of 2.740(+0.106)(-0.100) REarth, yielding a mean density of 2.21(+0.56)(-0.53) g/cm^3, indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (about 350 km) and the brightness of the host star make HD3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the radial velocity measurements but the currently available data set does not allow us to draw any firm conclusion on the origin of the observed variation., Comment: 18 pages, 11 figures, 5 tables
Published: 2017
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9. Stellar Winds in Massive X-ray Binaries

Author: Kretschmar, Peter, Martínez-Núñez, Silvia, Bozzo, Enrico, Oskinova, Lidia M., Puls, Joachim, Sidoli, Lara, Sundqvist, Jon Olof, Blay, Pere, Falanga, Maurizio, Fürst, Felix, Gímenez-García, Angel, Kreykenbohm, Ingo, Kühnel, Matthias, Sander, Andreas, Torrejón, José Miguel, Wilms, Jörn, Podsiadlowski, Philipp, and Manousakis, Antonios
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Strong winds from massive stars are a topic of interest to a wide range of astrophysical fields. In High-Mass X-ray Binaries the presence of an accreting compact object on the one side allows to infer wind parameters from studies of the varying properties of the emitted X-rays; but on the other side the accretor's gravity and ionizing radiation can strongly influence the wind flow. Based on a collaborative effort of astronomers both from the stellar wind and the X-ray community, this presentation attempts to review our current state of knowledge and indicate avenues for future progress., Comment: 4 pages, 1 figure, to be published in the Proceedings of the IAU Symposium No. 329 "The lives and death-throes of massive stars"
Published: 2017
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10. Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries

Author: Martínez-Núñez, Silvia, Kretschmar, Peter, Bozzo, Enrico, Oskinova, Lidia M., Puls, Joachim, Sidoli, Lara, Sundqvist, Jon Olof, Blay, Pere, Falanga, Maurizio, Fürst, Felix, Gímenez-García, Ángel, Kreykenbohm, Ingo, Kühnel, Matthias, Sander, Andreas, Torrejón, José Miguel, and Wilms, Jörn
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Massive stars, at least $\sim$ 10 times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy. [...] This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems., Comment: Published at Journal of Space Science Reviews, Springer
Published: 2017
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11. Advances in Understanding High-Mass X-ray Binaries with INTEGRALand Future Directions

Author: Kretschmar, Peter, Fürst, Felix, Sidoli, Lara, Bozzo, Enrico, Alfonso-Garzón, Julia, Bodaghee, Arash, Chaty, Sylvain, Chernyakova, Masha, Ferrigno, Carlo, Manousakis, Antonios, Negueruela, Ignacio, Postnov, Konstantin, Paizis, Adamantia, Reig, Pablo, Rodes-Roca, José Joaquín, Tsygankov, Sergey, Bird, Antony J., Bissinger né Kühnel, Matthias, Blay, Pere, Caballero, Isabel, Coe, Malcolm J., Domingo, Albert, Doroshenko, Victor, Ducci, Lorenzo, Falanga, Maurizio, Grebenev, Sergei A., Grinberg, Victoria, Hemphill, Paul, Kreykenbohm, Ingo, Kreykenbohm né Fritz, Sonja, Li, Jian, Lutovinov, Alexander A., Martínez-Núñez, Silvia, Mas-Hesse, J. Miguel, Masetti, Nicola, McBride, Vanessa A., Neronov, Andrii, Pottschmidt, Katja, Rodriguez, Jérôme, Romano, Patrizia, Rothschild, Richard E., Santangelo, Andrea, Sguera, Vito, Staubert, Rüdiger, Tomsick, John A., Torrejón, José Miguel, Torres, Diego F., Walter, Roland, Wilms, Jörn, Wilson-Hodge, Colleen A., and Zhang, Shu
Published: 2019
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12. Building galaxies, stars, planets and the ingredients for life between the stars. A scientific proposal for a European Ultraviolet-Visible Observatory (EUVO)

Author: de Castro, Ana I. Gómez, Appourchaux, Thierry, Barstow, Martin, Barthelemy, Mathieu, Baudin, Fréderic, Benetti, France Stefano, Blay, Pere, Brosch, Noah, Bunce, Enma, de Martino, Domitilla, Deharveng, Jean-Michel, France, Kevin, Ferlet, Roger, García, Miriam, Gaensicke, Boris, Gry, Cecile, Hillenbrand, Lynne, Josselin, Eric, Kehrig, Carolina, Lamy, Laurent, Lapington, Jon, Etangs, Alain Lecavelier des, LePetit, Frank, Santiago, Javier Lopez, Milliard, Bruno, Monier, Richard, Naletto, Giampiero, Nazé, Yael, Neiner, Coralie, Nichols, Jonathan, Orio, Marina, Pagano, Isabella, Peroux, Céline, Rauw, Gregor, Shore, Steven, Spaans, Marco, Tovmassian, Gagik, ud-Doula, Asif, and Vilchez, Jose
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: The growth of luminous structures and the building blocks of life in the Universe began as primordial gas was processed in stars and mixed at galactic scales. The mechanisms responsible for this development are not well understood and have changed over the intervening 13 billion years. To follow the evolution of matter over cosmic time, it is necessary to study the strongest (resonance) transitions of the most abundant species in the Universe. Most of them are in the ultraviolet (UV; 950A-3000A) spectral range that is unobservable from the ground. A versatile space observatory with UV sensitivity a factor of 50-100 greater than existing facilities will revolutionize our understanding of the Universe. Habitable planets grow in protostellar discs under ultraviolet irradiation, a by-product of the star-disk interaction that drives the physical and chemical evolution of discs and young planetary systems. The electronic transitions of the most abundant molecules are pumped by the UV field, providing unique diagnostics of the planet-forming environment that cannot be accessed from the ground. Earth's atmosphere is in constant interaction with the interplanetary medium and the solar UV radiation field. A 50-100 times improvement in sensitivity would enable the observation of the key atmospheric ingredients of Earth-like exoplanets (carbon, oxygen, ozone), provide crucial input for models of biologically active worlds outside the solar system, and provide the phenomenological baseline to understand the Earth atmosphere in context. In this white paper, we outline the key science that such a facility would make possible and outline the instrumentation to be implemented., Comment: White paper submitted to the European Space Agency Call for definition of the L2 and L3 missions in the ESA science (http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=51454)
Published: 2013
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13. A multiwavelength approach to BD+53$^\circ$2790: the O9.5V counterpart to the X-ray binary system 4U~2206+54

Author: Blay, Pere and Reglero, Víctor
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The X-ray binary system 4U 2206+54 hides many mysteries. Among them, the surprising behavior of both of its components: the O9.5 dwarf star BD+53$^\circ$2790 and a slowly rotating neutron star. BD+53$^\circ$2790 misled the astronomers showing itself very likely as a Be star. However, a deeper spectral analysis and more intense monitoring, revealed that the real picture was a bit more complicated: a) Although it shows evidence of a circumstellar envelope, its observable properties differ from those typical envelopes in Be stars. b) Comparison with spectral standards and models indicates a possible over-abundance in He. This would open the possibility to link the behavior of BD+53$^\circ$2790 to the He-rich class of stars. c) UV spectra shows an abnormally slow and dense wind for an O9.5V star. d) Spectral classification in the IR wavelength region suggest a more likely supergiant nature of the source, in contradiction with the optical classification. e) The presence of an intense magnetic field is under investigation. BD+53$^\circ$2790 stands as a perfect laboratory for testing stellar structure, as well as wind and evolutionary theories. The observable properties of this source in a wide range of spectral bands are discussed, and some interpretations outlined., Comment: Accepted for publication in the proceedings of the 39th Liege International Astroph. Colloquium, 12-16 July 2010, The multi-wavelength view of hot, massive stars, 8 pages, 6 figures
Published: 2011

14. First observations of the X-ray transient EXO 2030+375 with IBIS/ISGRI

Author: Kuznetsov, Sergey, Falanga, Maurizio, Blay, Pere, Goldwurm, Andrea, Goldoni, Paolo, and Reglero, Victor
Subjects: Astrophysics
Abstract: We present a first INTEGRAL observation of the 42s transient X-ray pulsar EXO 2030+375 with IBIS/ISGRI. The source was detected during Cyg X-1 observations in December 2002. We analyzed observations during the outburst period from 9 to 21 December 2002 with a total exposure time of ~770 kiloseconds. EXO 2030+375 was almost always detected during single ~30 minute exposures in the 18-45 energy bands. The source light curve shows the characteristic outburst shape observed in this source., Comment: 4 pages, 3 figures (1 in CMYK color), accepted by Astronomy and Astrophysics, INTEGRAL special issue, 2003
Published: 2003
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15. A polarimetric census of Be X-Ray Binaries with FAPOL@NOT

Author: Blay, Pere and Reig, Pablo
Subjects: x-ray binaries, polarization, stars:emission line, stars:Be
Abstract: Late O or early B stars showing Balmer lines in emission and infrared excess are classified as Be stars. Both, the emission in Balmer lines and the infrared excess, have their origin in a circumstelar disk-alike decretion structure. Rapid rotation and pulsations are known to be part of the mechanism of formation of such a structure but the process is still unknown. Be stars are also known to show a characteristic polarization due mainly to electron scattering of photons in the disk. Size of the disk, density and orientation with respect to the observer are factors that influence the total degree of polarization observed. They also present a characteristic variation of polarization with wavelength. Be stars accompanied by a compact object (neutron star or black hole) are the most common type of x-ray binary systems with massive optical companion. In these systems, known as Be X-Ray Binary systems (BeXRBs), the disk-alike structure is more compact and dense than that in isolated Be stars. We have started the very first polarization census of BeXRBs, with the goal to identify peculiar objects and compare the polarimetric porperties of Be stars in binary systems with the isolated ones. We present here the very first results of the survey, showing that Be stars in BeXRBs tend to show higher degrees of polarization than those of isolated Be stars and helping to identify and study some peculiar targets.
Published: 2022
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16. Photometric Classification of QSOs with Machine Learning Techniques

Author: Sánchez, Néstor, Arroquia-Cuadros, Benjamín, Gómez, Vicent, Blay, Pere, and Martínez-Badénez, Vicent
Subjects: methods: statistical, surveys, quasars: general, galaxies: general, catalogs
Abstract: With the advent of wide-area photometric surveys and the large amount of available data, the use of machine learning techniques is becoming more and more frequent to classify stars, galaxies and QSOs. In this work we investigate the performance of random forest in classifying QSOs using photometry of the 20 contiguous, equal-width, -nonoverlapping, medium-bands filters of the ALHAMBRA Survey. We systematically analyse the effects of the main free parameters on the final classification results and the advantages and limitations of using ALHAMBRA photometry in comparison to other surveys like Sloan (SDSS). The best performance is obtained when using colours from the ALHAMBRA survey.
Published: 2022
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17. Observatory science with eXTP

Author: in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael
Published: 2018
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18. Legri Instrument Health. A Historical Review

Author: Suso, Julia, Blay, Pere, Robert, Almudena, Reglero, Victor, Eyles, Chris J., and Gimenez, Alvaro, editor
Published: 2001
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19. Legri Science Operation Center. Architecture and Operations

Author: Blay, Pere, Suso, Julia, Robert, Almudena, Requena, Jose Luis, Alamo, Jorge, Reglero, Victor, Eyles, Chris J., and Gimenez, Alvaro, editor
Published: 2001
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20. Building galaxies, stars, planets and the ingredients for life between the stars. The science behind the European Ultraviolet-Visible Observatory

Author: Gómez de Castro, Ana I., Appourchaux, Thierry, Barstow, Martin A., Barthelemy, Mathieu, Baudin, Frederic, Benetti, Stefano, Blay, Pere, Brosch, Noah, Bunce, Emma, de Martino, Domitilla, Deharveng, Jean-Michel, Ferlet, Roger, France, Kevin, García, Miriam, Gänsicke, Boris, Gry, Cecile, Hillenbrand, Lynne, Josselin, Eric, Kehrig, Carolina, Lamy, Laurent, Lapington, Jon, Lecavelier des Etangs, Alain, LePetit, Frank, López-Santiago, Javier, Milliard, Bruno, Monier, Richard, Naletto, Giampiero, Nazé, Yael, Neiner, Coralie, Nichols, Jonathan, Orio, Marina, Pagano, Isabella, Peroux, Céline, Rauw, Gregor, Shore, Steven, Spaans, Marco, Tovmassian, Gagik, ud-Doula, Asif, and Vilchez, José
Published: 2014
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21. Study of the open cluster Alessi-Teutsch 9 (ASCC 10) using multiband photometry and Gaia EDR3

Author: Sánchez, Néstor, primary, López-Martínez, Fátima, additional, Ocando, Sandra, additional, and Blay, Pere, additional
Published: 2021
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22. Changes in Alcohol Consumption Pattern Based on Gender during COVID-19 Confinement in Spain

Author: Villanueva-Blasco, Víctor J., primary, Villanueva Silvestre, Verónica, additional, Isorna, Manuel, additional, Motos, Patricia, additional, Blay, Pere, additional, and Vázquez-Martínez, Andrea, additional
Published: 2021
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23. Impacto de las medidas de confinamiento durante la pandemia de COVID-19 en el consumo de riesgo de alcohol

Author: Villanueva Blasco, Víctor J., Motos Sellés, Patricia, Isorna Folgar, Manuel, Blay, Pere, Vázquez Martínez, Andrea, Villanueva Silvestre, Verónica, Villanueva Blasco, Víctor J., Motos Sellés, Patricia, Isorna Folgar, Manuel, Blay, Pere, Vázquez Martínez, Andrea, and Villanueva Silvestre, Verónica
Abstract: Fundamentos: Las estrategias de salud pública adoptadas para la contención del COVID-19 han generado estresores psicosociales que actúan como factores de riesgo del consumo de alcohol. Los objetivos del estudio fueron establecer si el consumo de riesgo de alcohol varió durante el confinamiento por COVID-19 durante los meses de abril y mayo de 2020, y cómo estas variaciones se manifestaban en función de distintas variables sociodemográficas. Métodos: El estudio se desarrolló durante el confinamiento con 3.779 participantes en España. Se utilizó una encuesta online con variables sociodemográficas (sexo, edad y situación laboral) y el AUDIT-C. Se realizó análisis de frecuencias y diferencia de medias (t de Student, ANOVA y Kruskal- Wallis) para establecer las variaciones a nivel intragrupo entre antes de la pandemia y durante el confinamiento, e intergrupo para cada periodo temporal, reportando tamaño del efecto. Resultados: El consumo de riesgo de alcohol presentó una prevalencia elevada antes del confinamiento (25,9% de los consumidores de alcohol), mostrando un descenso durante el confinamiento (15,1%), tanto en hombres (X2=224,829; p<0,001) como en mujeres (X2=214,324; p<0,001). Las mujeres presentaron una mayor prevalencia de consumo de riesgo antes de la pandemia (X2=13,124; p<0,001; d=1,067) como durante el confinamiento (X2=26,316; p<0,001; d=2,85); sin embargo, los hombres reportaron mayores puntuaciones que las mujeres en el AUDIT-C antes de la pandemia (t(2343)=-7,887; p<0,001; d=0,322) y durante el confinamiento (t(2343)=-5,664; p<0,001; d=0,231). A nivel de edad, se encontraron diferencias significativas de prevalencia entre los distintos grupos antes de la pandemia (X2=22,889; p<0,001) y durante el confinamiento (X2=38,302; p<0,001), siendo el rango de 18-24 años el de menor prevalencia. También se observaron diferencias entre los grupos de edad en las puntuaciones de consumo de riesgo durante el confinamiento (F(5,2338)=43,849; p=0,001), aumentando confo, Background: The public health strategies adopted for the containment of COVID-19 have generated psychosocial stressors that act as risk factors for alcohol consumption. The objectives of this study were to establish whether alcohol risk consumption varied during COVID-19 confinement, and how these variations manifested as a function of different sociodemographic variables. Methods: The study was conducted during confinement with 3,779 participants in Spain. We used an online survey with sociodemographic variables (sex, age and employment situation) and AUDIT-C. Frequency and mean difference analysis were performed (Student t, ANOVA and Kruskal-Wallis) to establish intra-group variations before the pandemic compared to during confinement, and intergroup for each time period, reporting effect size. Results: Alcohol risky consumption presented high prevalence rates before confinement (25,9% of alcohol consumers), showing a general decrease during confinement (15,1%), both in men (X2=224,829; p<0,001) and women (X2=214,324; p<0,001). Women had higher risk consumption rates both before the pandemic (X2=13,124; p<0,001; d=1,067) and during confinement (X2=26,316; p<0,001; d=2,85); however, men reported higher score in AUDIT-C before the pandemic (t(2343)=-7,887; p<0,001; d=0,322) and during confinement (t(2343)=-5,664; p<0,001; d=0,231). Considering age, significant differences in prevalence among groups were found before the pandemic (X2=22,889; p<0,001) and during confinement (X2=38,302; p<0,001), with the age range 18-24 showing less prevalence. Differences among age groups were also found in the risky consumption scores during confinement (F(5,2338)=43,849; p=0,001), increasing with age. With regards to the employment situation, differences before the pandemic (KW(5,2933)=13,467; p=0,019; E2 R=0,44), and during confinement (KW(5,2933)=149,818; p<0,001; E2 R=0,51) were also found. Self-employed workers showed a higher score in alcohol risky consumption with respect to
Published: 2021

24. Study of the open cluster Alessi-Teutsch 9 (ASCC 10) using multiband photometry and Gaia EDR3

Author: European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Sánchez, Néstor, López-Martínez, Fátima, Ocando, Sandra, Blay, Pere, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Sánchez, Néstor, López-Martínez, Fátima, Ocando, Sandra, and Blay, Pere
Abstract: There is a growing interest in the automated characterization of open clusters using data from the Gaia mission. This work evidences the importance of choosing an appropriate sampling radius (the radius of the circular region around the cluster used to extract the data) and the usefulness of additional multiband photometry in order to achieve accurate results. We address this issue using as a case study the cluster Alessi-Teutsch 9. The optimal sampling is determined by counting the number of assigned members at different sampling radii. By using this strategy with data from Gaia EDR3 and with observed photometry in 12 bands spanning the optical range from 3000 to 10000 Å, approximately, we are able to obtain reliable members and to determine the properties of the cluster. The spatial distribution of stars show a two-component structure with a central core of radius ∼ 12 − 13 arcmin and an outer halo extending out to 35 arcmin. With the derived cluster distance (654 pc) we obtain that the number density of stars is ≃ 0.06 star/pc3, making Alessi-Teutsch 9 one of the less dense known open clusters. The short relaxation time reveals that it is a dynamically relaxed and gravitationally bound system. © 2021, The Author(s), under exclusive licence to Springer Nature B.V.
Published: 2021

25. UV view of High Mass X-Ray Binary systems (what we know and perspectives for WSO-UV)

Author: Blay, Pere
Published: 2011
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26. Observatory science with eXTP

Author: in't Zand, Jean J. M., Bozzo, Enrico, Qu, Jinlu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, De Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, Xuefeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, Joao, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, Chichuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aì, Antonino, Dai, Zi-Gao, D'Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D'Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, Xilong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, Mingyu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, Fangjun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, Yunpeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O'Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, Lijing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, Junfeng, Watts, Anna L., Weng, Shanshan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, Shaolin, Xu, Yupeng, Yan, Zhen, Younes, George, Yu, Wenfei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean, Drake, Stephen, Jenke, Peter, Maccarone, Thomas, Rossi, Elena, Tauris, Thomas, Andersson, Nils, Ballantyne, David, Brown, Edward, Cackett, Edward, D’Aì, Antonino, D’Ammando, Filippo, D’Elia, Valerio, Ferdman, Robert, Galloway, Duncan, Gambino, Angelo, Heinke, Craig, Jonker, Peter, Kaastra, Jelle, Lutovinov, Alexander, Mignani, Roberto, O’Brien, Paul, Osborne, Julian, Papadakis, Iossif, Pérez Torres, Miguel, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Torres, Diego, Watts, Anna, Weinberg, Nevin, Wheatley, Peter, Woods, Tyrone, Woosley, Stan, Zdziarski, Andrzej, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Lauren, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Deny, Malzac, Julien, Manousakis, Antonio, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joona, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuoma, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jirí, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), eXTP, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherche en Information Biomédicale sino-français (CRIBS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Southeast University [Jiangsu]-Institut National de la Santé et de la Recherche Médicale (INSERM), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), ASI Science Data Center (ASDC), Italian Space Agency, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Anthropobiologie (LA), École des hautes études en sciences sociales (EHESS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), SRON Netherlands Institute for Space Research (SRON), Istituto di Radioastronomia [Bologna] (IRA), KAUST Catalysis Center (KCC), King Abdullah University of Sciences & Technologie, IASF, Area di Ricerca di Tor Vergata, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Southampton], University of Southampton, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut für Astrophysik [Wien], Universität Wien, Sabanci University [Istanbul], The George Washington University (GW), Department of Physics, Tokyo Institute of Technology [Tokyo] (TITECH), Deakin University [Burwood], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), University of New Hampshire (UNH), Department of Mechanical and Industrial Engineering [Trondheim] (MTP NTNU), Norwegian University of Science and Technology [Trondheim] (NTNU), Norwegian University of Science and Technology (NTNU)-Norwegian University of Science and Technology (NTNU), Ethoikos, Radicondoli, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Sichuan University [Chengdu] (SCU), University of Warwick [Coventry], U.S. Department of Energy [Washington] (DOE), University College of London [London] (UCL), Medical School (University of Nanjing), Nanjing University (NJU), Beijing Municipal Climate Center, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Informática [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), NLD, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, National Natural Science Foundation of China (NSFC), European Research Council (ERC), National Aeronautics and Space Administration (NASA), Agencia Estatal de Investigación (AEI), Royal Society, Strategic Priority Research Program of the Chinese Academy of Sciences, National Science Centre, Poland (NCN), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, Astronomy, Discrete Technology and Production Automation, in't Zand, Jean J. M., Qu, Jinlu, Tauris, Thomas M., Wilm, Joern, Wu, Xuefeng, Jin, Chichuan, D'Aì, Antonino, D'Ammando, Filippo, D'Elia, Valerio, Fan, Xilong, Ge, Mingyu, Lu, Fangjun, Mchardy, Ian, Men, Yunpeng, O'Brien, Paul T., Shao, Lijing, Svoboda, Jir̆í, Thielemann, F. -K., Wang, Junfeng, Weng, Shanshan, Xiong, Shaolin, Xu, Yupeng, Yu, Wenfei, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Osservatorio Astronomico di Brera, Istituto di Radioastronomia (IRA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), George Washington University (GW), Department of Mechanical and Industrial Engineering [Trondheim], Sichuan University, U.S. Department of Energy (DOE), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), SRON Netherlands Institute for Space Research, University of Geneva, CAS - Institute of High Energy Physics, Nanjing University, INAF/IASF Bologna, National Institute for Astrophysics, University of Tübingen, NASA Goddard Space Flight Center, ICREA, University of Alabama in Huntsville, Texas Tech University, Osservatorio Astronomico di Capodimonte, Leiden University, University of Amsterdam, Polytechnic University of Catalonia, University of Urbino, Max Planck Institute for Radio Astronomy, Friedrich-Alexander University Erlangen-Nürnberg, CAS - Purple Mountain Observatory, CSIC, IRAP, New York University Abu Dhabi, Georgia Institute of Technology, Middle East Technical University, Technion-Israel Institute of Technology, Tata Institute of Fundamental Research, Roma Tre University, Instituto de Astrofísica de Canarias, Instituto Nacional de Pesquisas Espaciais, Danmarks Tekniske Universitet, Michigan State University, Osservatorio Astrofisico Di Arcetri, Florence, University of Cagliari, Wayne State University, Osservatorio Astronomico Roma, CAS - Shanghai Astronomical Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: cataclysmic binaries, Astronomy, FIELD CAMERAS OBSERVATIONS, space research instruments nuclear astrophysics flare stars accretion and accretion disks mass loss and stellar winds cataclysmic binaries X-ray binaries supernova remnants active galactic nuclei X-ray bursts gamma-ray bursts gravitational waves, General Physics and Astronomy, gamma-ray burst, space research instrument, 01 natural sciences, Gamma ray bursts, Observatory, Accretion and accretion disks, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, gravitational wave, accretion and accretion disk, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], flare stars, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, accretion and accretion disks, active galactic nuclei, gravitational waves, mass loss and stellar winds, nuclear astrophysics, space research instruments, X-ray binaries, X-ray bursts, Physics and Astronomy (all), Space research instruments, X ray burst, Supernova, QUIET, High mass, X-ray binarie, Mass loss and stellar winds, Nuclear astrophysics, Gamma-ray bursts, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, FAST RADIO-BURSTS, Astrofísica nuclear, Active galactic nucleus, TIDAL DISRUPTION, Supernova remnants, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, ACCRETING NEUTRON-STARS, Gravitational waves, cataclysmic binarie, Settore FIS/05 - Astronomia e Astrofisica, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, 010306 general physics, X-ray burst, Astrophysics::Galaxy Astrophysics, Cataclysmic binaries, Active galactic nuclei, flare star, White dwarf, Flare stars, Stars, supernova remnant, QB460-466 Astrophysics, [SDU]Sciences of the Universe [physics], mass loss and stellar wind, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], X-RAY, Supernova remmants, X ray binaries, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SEYFERT 1 GALAXY, nuclear astrophysic
Abstract: Disponible preprint en: arXiv:1812.04023v1 [astro-ph.HE] [v1] Mon, 10 Dec 2018 19:00:52 UTC (4,376 KB), In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.© 2018, Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature., This work was supported by the Royal Society, ERC Starting (Grant No. 639217), the European Union Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Global Fellowship (Grant No. 703916), the National Natural Science Foundation of China (Grant Nos. 11233001, 11773014, 11633007, 11403074, 11333005, 11503008, and 11590781), the National Basic Research Program of China (Grant No. 2015CB857100), NASA (Grant No. NNX13AD28A), an ARC Future Fellowship (Grant No. FT120100363), the National Science Foundation (Grant No. PHY-1430152), the Spanish MINECO (Grant No. AYA2016-76012-C3-1-P), the ICCUB (Unidad de Excelencia 'Maria de Maeztu') (Grant No. MDM-2014-0369), EU's Horizon Programme through a Marie Sklodowska-Curie Fellowship (Grant No. 702638), the Polish National Science Center (Grant Nos. 2015/17/B/ST9/03422, 2015/18/M/ST9/00541, 2013/10/M/ST9/00729, and 2015/18/A/ST9/00746), the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA15020100), and the NWO Veni Fellowship (Grant No. 639.041.647).
Published: 2019

27. K2-280 b - a low density warm sub-Saturn around a mildly evolved star

Author: Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Deeg, Hans J., Hirano, Teruyuki, Barragan, Oscar, Kuzuhara, Masayuki, Dai, Fei, Luque, Rafael, Persson, Carina M., Fridlund, Malcolm, Johnson, Marshall C., Korth, Judith, Livingston, John H., Grziwa, Sascha, Mathur, Savita, Hatzes, Artie P., Prieto-Arranz, Jorge, Nespral, David, Hidalgo, Diego, Hjorth, Maria, Albrecht, Simon, Van Eylen, Vincent, Lam, Kristine W. F., Cochran, William D., Esposito, Massimiliano, Csizmadia, Szilard, Guenther, Eike W., Kabath, Petr, Blay, Pere, Brahm, Rafael, Jordan, Andres, Espinoza, Nestor, Rojas, Felipe, Casasayas Barris, Nuria, Rodler, Florian, Alonso Sobrino, Roi, Cabrera, Juan, Carleo, Ilaria, Chaushev, Alexander, de Leon, Jerome, Eigmueller, Philipp, Endl, Michael, Erikson, Anders, Fukui, Akihiko, Georgieva, Iskra, Gonzalez-Cuesta, Lucia, Knudstrup, Emil, Lund, Mikkel N., Montanes Rodriguez, Pilar, Murgas, Felipe, Narita, Norio, Niraula, Prajwal, Paetzold, Martin, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M. S., Subjak, Jano, Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Deeg, Hans J., Hirano, Teruyuki, Barragan, Oscar, Kuzuhara, Masayuki, Dai, Fei, Luque, Rafael, Persson, Carina M., Fridlund, Malcolm, Johnson, Marshall C., Korth, Judith, Livingston, John H., Grziwa, Sascha, Mathur, Savita, Hatzes, Artie P., Prieto-Arranz, Jorge, Nespral, David, Hidalgo, Diego, Hjorth, Maria, Albrecht, Simon, Van Eylen, Vincent, Lam, Kristine W. F., Cochran, William D., Esposito, Massimiliano, Csizmadia, Szilard, Guenther, Eike W., Kabath, Petr, Blay, Pere, Brahm, Rafael, Jordan, Andres, Espinoza, Nestor, Rojas, Felipe, Casasayas Barris, Nuria, Rodler, Florian, Alonso Sobrino, Roi, Cabrera, Juan, Carleo, Ilaria, Chaushev, Alexander, de Leon, Jerome, Eigmueller, Philipp, Endl, Michael, Erikson, Anders, Fukui, Akihiko, Georgieva, Iskra, Gonzalez-Cuesta, Lucia, Knudstrup, Emil, Lund, Mikkel N., Montanes Rodriguez, Pilar, Murgas, Felipe, Narita, Norio, Niraula, Prajwal, Paetzold, Martin, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M. S., and Subjak, Jano
Abstract: We present an independent discovery and detailed characterization of K2-280 b, a transiting low density warm sub-Saturn in a 19.9-d moderately eccentric orbit (e = 0.35(-0.04)(+0.05)) from K2 campaign 7. A joint analysis of high precision HARPS, HARPS-N, and FIES radial velocity measurements and K2 photometric data indicates that K2-280 b has a radius of R-b = 7.50 +/- 0.44 R-circle plus and a mass of M-b = 37.1 +/- 5.6 M-circle plus, yielding a mean density of rho(b) = 0.48(-0.10)(+0.13) g cm(-3). The host star is a mildly evolved G7 star with an effective temperature of T-eff = 5500 +/- 100 K, a surface gravity of log g(star) = 4.21 +/- 0.05 (cgs), and an iron abundance of [Fe/H] = 0.33 +/- 0.08 dex, and with an inferred mass of M-star = 1.03 +/- 0.03 M-circle dot and a radius of R-star = 1.28 +/- 0.07 R-circle dot. We discuss the importance of K2-280 b for testing formation scenarios of sub-Saturn planets and the current sample of this intriguing group of planets that are absent in the Solar system.
Published: 2020

28. Advances in Understanding High-Mass X-ray Binaries with INTEGRAL and Future Directions

Author: Universidad de Alicante. Departamento de Física Aplicada, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Kretschmar, Peter, Fürst, Felix, Sidoli, Lara, Bozzo, Enrico, Alfonso-Garzón, Julia, Bodaghee, Arash, Chaty, Sylvain, Chernyakova, Masha, Ferrigno, Carlo, Manousakis, Antonios, Negueruela, Ignacio, Postnov, Konstantin, Paizis, Adamantia, Reig, Pablo, Rodes Roca, José Joaquín, Tsygankov, Sergey, Bird, Antony J., Bissinger né Kühnel, Matthias, Blay, Pere, Caballero, Isabel, Coe, Malcolm J., Domingo, Albert, Doroshenko, Victor, Ducci, Lorenzo, Falanga, Maurizio, Grebenev, Sergei A., Grinberg, Victoria, Hemphill, Paul, Kreykenbohm, Ingo, Kreykenbohm né Fritz, Sonja, Li, Jian, Lutovinov, Alexander A., Martínez Núñez, Silvia, Mas-Hesse, J. Miguel, Masetti, Nicola, McBride, Vanessa A., Neronov, Andrii, Pottschmidt, Katja, Rodriguez, Jérôme, Romano, Patrizia, Rothschild, Richard E., Santangelo, Andrea, Sguera, Vito, Staubert, Rüdiger, Tomsick, John A., Torrejon, Jose M., Torres, Diego F., Walter, Roland, Wilms, Jörn, Wilson-Hodge, Colleen A., Zhang, Shu, Universidad de Alicante. Departamento de Física Aplicada, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Kretschmar, Peter, Fürst, Felix, Sidoli, Lara, Bozzo, Enrico, Alfonso-Garzón, Julia, Bodaghee, Arash, Chaty, Sylvain, Chernyakova, Masha, Ferrigno, Carlo, Manousakis, Antonios, Negueruela, Ignacio, Postnov, Konstantin, Paizis, Adamantia, Reig, Pablo, Rodes Roca, José Joaquín, Tsygankov, Sergey, Bird, Antony J., Bissinger né Kühnel, Matthias, Blay, Pere, Caballero, Isabel, Coe, Malcolm J., Domingo, Albert, Doroshenko, Victor, Ducci, Lorenzo, Falanga, Maurizio, Grebenev, Sergei A., Grinberg, Victoria, Hemphill, Paul, Kreykenbohm, Ingo, Kreykenbohm né Fritz, Sonja, Li, Jian, Lutovinov, Alexander A., Martínez Núñez, Silvia, Mas-Hesse, J. Miguel, Masetti, Nicola, McBride, Vanessa A., Neronov, Andrii, Pottschmidt, Katja, Rodriguez, Jérôme, Romano, Patrizia, Rothschild, Richard E., Santangelo, Andrea, Sguera, Vito, Staubert, Rüdiger, Tomsick, John A., Torrejon, Jose M., Torres, Diego F., Walter, Roland, Wilms, Jörn, Wilson-Hodge, Colleen A., and Zhang, Shu
Abstract: High mass X-ray binaries are among the brightest X-ray sources in the Milky Way, as well as in nearby Galaxies. Thanks to their highly variable emissions and complex phenomenology, they have attracted the interest of the high energy astrophysical community since the dawn of X-ray Astronomy. In more recent years, they have challenged our comprehension of physical processes in many more energy bands, ranging from the infrared to very high energies. In this review, we provide a broad but concise summary of the physical processes dominating the emission from high mass X-ray binaries across virtually the whole electromagnetic spectrum. These comprise the interaction of stellar winds with the high gravitational and magnetic fields of compact objects, the behaviour of matter under extreme magnetic and gravity conditions, and the perturbation of the massive star evolutionary processes by presence in a binary system. We highlight the role of the INTEGRAL mission in the discovery of many of the most interesting objects in the high mass X-ray binary class and its contribution in reviving the interest for these sources over the past two decades. We show how the INTEGRAL discoveries have not only contributed to significantly increase the number of high mass X-ray binaries known, thus advancing our understanding of the population as a whole, but also have opened new windows of investigation that stimulated the multi-wavelength approach nowadays common in most astrophysical research fields. We conclude the review by providing an overview of future facilities being planned from the X-ray to the very high energy domain that will hopefully help us in finding an answer to the many questions left open after more than 18 years of INTEGRAL scientific observations.
Published: 2020

29. UV view of High Mass X-Ray Binary systems (what we know and perspectives for WSO-UV)

Author: Blay, Pere, primary
Published: 2011
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30. K2-280 b – a low density warm sub-Saturn around a mildly evolved star

Author: Nowak, Grzegorz, primary, Palle, Enric, additional, Gandolfi, Davide, additional, Deeg, Hans J, additional, Hirano, Teruyuki, additional, Barragán, Oscar, additional, Kuzuhara, Masayuki, additional, Dai, Fei, additional, Luque, Rafael, additional, Persson, Carina M, additional, Fridlund, Malcolm, additional, Johnson, Marshall C, additional, Korth, Judith, additional, Livingston, John H, additional, Grziwa, Sascha, additional, Mathur, Savita, additional, Hatzes, Artie P, additional, Prieto-Arranz, Jorge, additional, Nespral, David, additional, Hidalgo, Diego, additional, Hjorth, Maria, additional, Albrecht, Simon, additional, Van Eylen, Vincent, additional, Lam, Kristine W F, additional, Cochran, William D, additional, Esposito, Massimiliano, additional, Csizmadia, Szilárd, additional, Guenther, Eike W, additional, Kabath, Petr, additional, Blay, Pere, additional, Brahm, Rafael, additional, Jordán, Andrés, additional, Espinoza, Néstor, additional, Rojas, Felipe, additional, Casasayas Barris, Núria, additional, Rodler, Florian, additional, Alonso Sobrino, Roi, additional, Cabrera, Juan, additional, Carleo, Ilaria, additional, Chaushev, Alexander, additional, de Leon, Jerome, additional, Eigmüller, Philipp, additional, Endl, Michael, additional, Erikson, Anders, additional, Fukui, Akihiko, additional, Georgieva, Iskra, additional, González-Cuesta, Lucía, additional, Knudstrup, Emil, additional, Lund, Mikkel N, additional, Montañes Rodríguez, Pilar, additional, Murgas, Felipe, additional, Narita, Norio, additional, Niraula, Prajwal, additional, Pätzold, Martin, additional, Rauer, Heike, additional, Redfield, Seth, additional, Ribas, Ignasi, additional, Skarka, Marek, additional, Smith, Alexis M S, additional, and Subjak, Jano, additional
Published: 2020
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31. Observatory science with eXTP

Author: in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael
Abstract: In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.
Published: 2019

32. Observatory science with eXTP

Author: Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, in´t Zand, J. J. M., Bozz, Enrico, Qu, J. L., Li, X. D., Amati, L., Chen, Yang, Donnarumma, I., Doroshenko, V., Drake, S. A., Hernanz, Margarita, Jenke, P. A., Maccarone, T. J., Mahmoodifar, S., De Martino, D., De Rosa, Alessandra, Rossi, E. M., Rowlinson, A., Sala, Gloria, Stratta, G., Tauris, T. M., Wilms, Jörn, Wu, X. F., Zhou, P., Agudo, Iván, Atteia, J. L., Andersson, N., Baglio, Maria Cristina, Ballantyne, D. R., Baykal, A., Behar, E., Belloni, T., Bhattacharyya, S., Bianchi, Stefano, Bilous, A., Blay, Pere, Braga, J., Brandt, S., Brown, E. F., Bucciantini, N., Burderi, L., Cackett, E.M., Campana, R., Campana, Sergio, Casella, P., Cavecchi, Y., Chambers, F., Chen, L., Chen, Y. P., Iwasawa, Kazushi, Izzo, L., José, Jordi, Linares, Manuel, Miniutti, Giovanni, Pérez-Torres, Miguel A., Rodríguez-Gil, Pablo, Torres, Diego F., Altamirano, Diego, Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, in´t Zand, J. J. M., Bozz, Enrico, Qu, J. L., Li, X. D., Amati, L., Chen, Yang, Donnarumma, I., Doroshenko, V., Drake, S. A., Hernanz, Margarita, Jenke, P. A., Maccarone, T. J., Mahmoodifar, S., De Martino, D., De Rosa, Alessandra, Rossi, E. M., Rowlinson, A., Sala, Gloria, Stratta, G., Tauris, T. M., Wilms, Jörn, Wu, X. F., Zhou, P., Agudo, Iván, Atteia, J. L., Andersson, N., Baglio, Maria Cristina, Ballantyne, D. R., Baykal, A., Behar, E., Belloni, T., Bhattacharyya, S., Bianchi, Stefano, Bilous, A., Blay, Pere, Braga, J., Brandt, S., Brown, E. F., Bucciantini, N., Burderi, L., Cackett, E.M., Campana, R., Campana, Sergio, Casella, P., Cavecchi, Y., Chambers, F., Chen, L., Chen, Y. P., Iwasawa, Kazushi, Izzo, L., José, Jordi, Linares, Manuel, Miniutti, Giovanni, Pérez-Torres, Miguel A., Rodríguez-Gil, Pablo, Torres, Diego F., and Altamirano, Diego
Abstract: In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.© 2018, Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature.
Published: 2019

33. The Transiting Multi-planet System HD3167:A 5.7M(circle plus) Super-Earth and an 8.3M(circle plus) Mini-Neptune

Author: Gandolfi, Davide, Barragan, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Dai, Fei, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmller, Philipp, Erikson, Anders, Gonzalez Hernandez, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suarez Mascareno, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Paetzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., and Zakhozhay, Olga V.
Subjects: LIGHT CURVES, ARCHITECTURE, SPECTROSCOPY, detection [planets and satellites], fundamental parameters [stars], KEPLER, DWARF STARS, HABITABLE-ZONE, individual (HD 3167) [stars], individual (HD 3167b, HD 3167c) [planets and satellites], STELLAR, DENSITY, SPACED DATA, MISSION
Abstract: HD3167 is a bright (V = 8.9 mag) K0V star observed by the NASA's K2 space mission during its Campaign 8. It has been recently found to host two small transiting planets, namely, HD 3167b, an ultra short period (0.96 days) super-Earth, and HD 3167c, a mini-Neptune on a relatively long-period orbit (29.85 d). Here we present an intensive radial velocity follow-up of HD 3167 performed with the FIES@NOT, HARPS@ESO-3.6m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69 +/- -0.44 M-circle plus, radius of 1.574 +/- -0.054 R-circle plus, and mean density of 8.00(-0.98)(+1.0) g/cm(-3), HD 3167b joins the small group of ultra-short period planets known to have a rocky terrestrial composition. HD 3167c has a mass of 8.33(-1.85)(+1.79) M-circle plus and a radius of 2.740(-0.100)(+0.106) R-circle plus, yielding a mean density of 2.21(-0.53)(+0.56) g/cm(-3), indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (similar to 350 km) and the brightness of the host star make HD 3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the radial velocity measurements but the currently available data set does not allow us to draw any firm conclusion on the origin of the observed variation.
Published: 2017

34. K2 Campaign 5 observations of pulsating subdwarf B stars: binaries and super-Nyquist frequencies

Author: Reed, M D, primary, Armbrecht, E L, additional, Telting, J H, additional, Baran, A S, additional, Østensen, R H, additional, Blay, Pere, additional, Kvammen, A, additional, Kuutma, Teet, additional, Pursimo, T, additional, Ketzer, L, additional, and Jeffery, C S, additional
Published: 2017
Full Text: View/download PDF

35. The Transiting Multi-planet System HD3167: A 5.7M(circle plus) Super-Earth and an 8.3M(circle plus) Mini-Neptune

Author: Gandolfi, Davide, Barragan, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Dai, Fei, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmller, Philipp, Erikson, Anders, Gonzalez Hernandez, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suarez Mascareno, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Paetzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., Zakhozhay, Olga V., Gandolfi, Davide, Barragan, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Dai, Fei, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmller, Philipp, Erikson, Anders, Gonzalez Hernandez, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suarez Mascareno, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Paetzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., and Zakhozhay, Olga V.
Abstract: HD3167 is a bright (V = 8.9 mag) K0V star observed by the NASA's K2 space mission during its Campaign 8. It has been recently found to host two small transiting planets, namely, HD 3167b, an ultra short period (0.96 days) super-Earth, and HD 3167c, a mini-Neptune on a relatively long-period orbit (29.85 d). Here we present an intensive radial velocity follow-up of HD 3167 performed with the FIES@NOT, HARPS@ESO-3.6m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69 +/- -0.44 M-circle plus, radius of 1.574 +/- -0.054 R-circle plus, and mean density of 8.00(-0.98)(+1.0) g/cm(-3), HD 3167b joins the small group of ultra-short period planets known to have a rocky terrestrial composition. HD 3167c has a mass of 8.33(-1.85)(+1.79) M-circle plus and a radius of 2.740(-0.100)(+0.106) R-circle plus, yielding a mean density of 2.21(-0.53)(+0.56) g/cm(-3), indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (similar to 350 km) and the brightness of the host star make HD 3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the radial velocity measurements but the currently available data set does not allow us to draw any firm conclusion on the origin of the observed variation.
Published: 2017

36. Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Martínez Núñez, Silvia, Kretschmar, Peter, Bozzo, Enrico, Oskinova, Lidia M., Puls, Joachim, Sidoli, Lara, Sundqvist, Jon Olof, Blay, Pere, Falanga, Maurizio, Fürst, Felix, Giménez García, Ángel, Kreykenbohm, Ingo, Kühnel, Matthias, Sander, Andreas, Torrejon, Jose M., Wilms, Jörn, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Martínez Núñez, Silvia, Kretschmar, Peter, Bozzo, Enrico, Oskinova, Lidia M., Puls, Joachim, Sidoli, Lara, Sundqvist, Jon Olof, Blay, Pere, Falanga, Maurizio, Fürst, Felix, Giménez García, Ángel, Kreykenbohm, Ingo, Kühnel, Matthias, Sander, Andreas, Torrejon, Jose M., and Wilms, Jörn
Abstract: Massive stars, at least ∼10 times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy. In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense “clumps”. The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution. Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources
Published: 2017

37. Towards a unified view of inhomogeneous stellar winds in isolated supergiant stars and supergiant high mass X-ray binaries

Author: Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), German Research Foundation, German Centre for Air and Space Travel, Ministerio de Ciencia e Innovación (España), Universidad de Alicante, Federal Ministry of Economics and Technology (Germany), Martínez-Núñez, Silvia, Kretschmar, Peter, Bozz, Enrico, Oskinova, Lidia M., Puls, Joachim, Sidoli, Lara, Sundqvist, Jon Olof, Blay, Pere, Falanga, Maurizio, Fürst, Felix, Giménez-García, Angel, Kreykenbohm, Ingo, Kühnel, Matthias, Sander, Andreas, Torrejón, José Miguel, Wilms, Jörn, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), German Research Foundation, German Centre for Air and Space Travel, Ministerio de Ciencia e Innovación (España), Universidad de Alicante, Federal Ministry of Economics and Technology (Germany), Martínez-Núñez, Silvia, Kretschmar, Peter, Bozz, Enrico, Oskinova, Lidia M., Puls, Joachim, Sidoli, Lara, Sundqvist, Jon Olof, Blay, Pere, Falanga, Maurizio, Fürst, Felix, Giménez-García, Angel, Kreykenbohm, Ingo, Kühnel, Matthias, Sander, Andreas, Torrejón, José Miguel, and Wilms, Jörn
Abstract: Massive stars, at least ∼ 10 times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy. In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense “clumps”. The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution. Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray source
Published: 2017

38. The Transiting Multi-Planet System HD 3167: A 5.7 M ⊕ Super-Earth and an 8.3 M ⊕ Mini-Neptune

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Dai, Fei, Gandolfi, Davide, Barragán, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmüller, Philipp, Erikson, Anders, González Hernández, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suárez Mascareño, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Pätzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., Zakhozhay, Olga V., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Dai, Fei, Gandolfi, Davide, Barragán, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmüller, Philipp, Erikson, Anders, González Hernández, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suárez Mascareño, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Pätzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., and Zakhozhay, Olga V.
Published: 2017

39. The Transiting Multi-planet System HD 3167: A 5.7M⊕Super-Earth and an 8.3M⊕Mini-Neptune

Author: Gandolfi, Davide, primary, Barragán, Oscar, additional, Hatzes, Artie P., additional, Fridlund, Malcolm, additional, Fossati, Luca, additional, Donati, Paolo, additional, Johnson, Marshall C., additional, Nowak, Grzegorz, additional, Prieto-Arranz, Jorge, additional, Albrecht, Simon, additional, Dai, Fei, additional, Deeg, Hans, additional, Endl, Michael, additional, Grziwa, Sascha, additional, Hjorth, Maria, additional, Korth, Judith, additional, Nespral, David, additional, Saario, Joonas, additional, Smith, Alexis M. S., additional, Antoniciello, Giuliano, additional, Alarcon, Javier, additional, Bedell, Megan, additional, Blay, Pere, additional, Brems, Stefan S., additional, Cabrera, Juan, additional, Csizmadia, Szilard, additional, Cusano, Felice, additional, Cochran, William D., additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, González Hernández, Jonay I., additional, Guenther, Eike W., additional, Hirano, Teruyuki, additional, Suárez Mascareño, Alejandro, additional, Narita, Norio, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Pätzold, Martin, additional, Persson, Carina M., additional, Rauer, Heike, additional, Saviane, Ivo, additional, Schmidtobreick, Linda, additional, Van Eylen, Vincent, additional, Winn, Joshua N., additional, and Zakhozhay, Olga V., additional
Published: 2017
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40. EXO 2030+375 Restarts in Reverse

Author: Kretschmar, Peter, primary, Fuerst, Felix, additional, Wilson-Hodge, Colleen A., additional, Blay, Pere, additional, Kajava, Jari, additional, Alfonso-Garzón, Julia, additional, Kühnel, Matthias, additional, Kreykenbohm, Ingo, additional, Wilms, Jörn, additional, Jenke, Peter A., additional, and POTTSCHMIDT, Katja, additional
Published: 2017
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41. Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

Author: Martínez-Núñez, Silvia, primary, Kretschmar, Peter, additional, Bozzo, Enrico, additional, Oskinova, Lidia M., additional, Puls, Joachim, additional, Sidoli, Lara, additional, Sundqvist, Jon Olof, additional, Blay, Pere, additional, Falanga, Maurizio, additional, Fürst, Felix, additional, Gímenez-García, Angel, additional, Kreykenbohm, Ingo, additional, Kühnel, Matthias, additional, Sander, Andreas, additional, Torrejón, José Miguel, additional, and Wilms, Jörn, additional
Published: 2017
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42. Stellar Winds in Massive X-ray Binaries

Author: Kretschmar, Peter, primary, Martínez-Núñez, Silvia, additional, Bozzo, Enrico, additional, Oskinova, Lidia M., additional, Puls, Joachim, additional, Sidoli, Lara, additional, Sundqvist, Jon Olof, additional, Blay, Pere, additional, Falanga, Maurizio, additional, Fürst, Felix, additional, Gímenez-García, Angel, additional, Kreykenbohm, Ingo, additional, Kühnel, Matthias, additional, Sander, Andreas, additional, Torrejón, José Miguel, additional, Wilms, Jörn, additional, Podsiadlowski, Philipp, additional, and Manousakis, Antonios, additional
Published: 2016
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43. K2 Campaign 5 observations of pulsating subdwarf B stars: binaries and super-Nyquist frequencies.

Author: Reed, M. D., Armbrecht, E. L., Telting, J. H., Baran, A. S., Østensen, R. H., Blay, Pere, Kvammen, A., Kuutma, Teet, Pursimo, T., Ketzer, L., and Jeffery, C. S.
Subjects: B stars, ASTRONOMICAL observations, NYQUIST frequency, STELLAR oscillations
Abstract: We report the discovery of three pulsating subdwarf B stars in binary systems observed with the Kepler space telescope during Campaign 5 of K2. EPIC 211696659 (SDSS J083603.98+155216.4) is a g-mode pulsator with a white dwarf companion and a binary period of 3.16 d. EPICs 211823779 (SDSS J082003.35+173914.2) and 211938328 (LB 378) are both p-mode pulsators with main-sequence F companions. The orbit of EPIC 211938328 is long (635 ± 146 d) while we cannot constrain that of EPIC 211823779. The p modes are near the Nyquist frequency and so we investigate ways to discriminate super- from sub-Nyquist frequencies. We search for rotationally induced frequency multiplets and all three stars appear to be slow rotators with EPIC 211696659 subsynchronous to its orbit. [ABSTRACT FROM AUTHOR]
Published: 2018
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44. Observatory science with eXTP

Author: in ’t Zand, Jean, Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen, Hernanz, Margarita, Jenke, Peter, Maccarone, Thomas, Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena, Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas, Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils, Baglio, M., Ballantyne, David, Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward, Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward, Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert, Feroci, Marco, Fraschetti, Federico, Galloway, Duncan, Gambino, Angelo, Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig, Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter, José, Jordi, Kaastra, Jelle, Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander, Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto, Mikusincova, Romana, Miller, M., Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul, Orlandini, Mauro, Osborne, Julian, Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif, Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel, Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego, Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna, Weng, ShanShan, Weinberg, Nevin, Wheatley, Peter, Wijnands, Rudy, Woods, Tyrone, Woosley, Stan, Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej, Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, and Zingale, Michael
Abstract: In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.
Published: 2019
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45. Atmosphere-Space Interactions Monitor (ASIM): State of the Art

Author: Blay, Pere, primary, Sabau-Graziati, Lola, additional, Reglero, Víctor, additional, Connell, Paul H., additional, Rodrigo, Juana M., additional, Macián, Juan M. Macian, additional, Biosca, José T., additional, and Eyles, Chris, additional
Published: 2014
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46. Highly Magnetized Accreting Pulsars: Are There Accreting Magnetars?

Author: Blay, Pere, primary, Reig, Pablo, additional, and Reglero, Víctor, additional
Published: 2014
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47. Accreting magnetars: a new type of high-mass X-ray binaries?

Author: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reig, Pablo, Torrejon, Jose M., Blay, Pere, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Reig, Pablo, Torrejon, Jose M., and Blay, Pere
Abstract: The discovery of very slow pulsations (Pspin =5560 s) has solved the long-standing question of the nature of the compact object in the high-mass X-ray binary 4U 2206+54 but has posed new ones. According to spin evolutionary models in close binary systems, such slow pulsations require a neutron star magnetic field strength larger than the quantum critical value of 4.4 × 1013 G, suggesting the presence of a magnetar. We present the first XMM–Newton observations of 4U 2206+54 and investigate its spin evolution. We find that the observed spin-down rate agrees with the magnetar scenario. We analyse Integral Spacecraft Gamma-Ray Imager (ISGRI)/INTErnational Gamma-RAy Laboratory (INTEGRAL) observations of 4U 2206+54 to search for the previously suggested cyclotron resonance scattering feature at ∼30 keV. We do not find a clear indication of the presence of the line, although certain spectra display shallow dips, not always at 30 keV. The association of these dips with a cyclotron line is very dubious because of its apparent transient nature. We also investigate the energy spectrum of 4U 2206+54 in the energy range 0.3–10 keV with unprecedented detail and report for the first time the detection of very weak 6.5 keV fluorescence iron lines. The photoelectric absorption is consistent with the interstellar value, indicating very small amount of local matter, which would explain the weakness of the florescence lines. The lack of matter locally to the source may be the consequence of the relatively large orbital separation of the two components of the binary. The wind would be too tenuous in the vicinity of the neutron star.
Published: 2012

48. An INTEGRAL spectral and timing history of 1A 1118-615

Author: Blay, Pere, primary
Published: 2013
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49. X Per pulse period evolution

Author: Blay, Pere, primary and Reglero, Victor, additional
Published: 2013
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50. The paradigm of atypical HMXRBs: 4U 2206+54

Author: Blay, Pere, primary
Published: 2013
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