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1,193 results on '"Di Mauro, M"'

1. Constraining Dark Matter Annihilation with Fermi-LAT Observations of Ultra-Faint Compact Stellar Systems

Author: Circiello, A., McDaniel, A., Drlica-Wagner, A., Karwin, C., Ajello, M., Di Mauro, M., and Sánchez-Conde, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Recent results from numerical simulations and models of galaxy formation suggest that recently discovered ultra-faint compact stellar systems (UFCSs) in the halo of the Milky Way (MW) may be some of the smallest and faintest galaxies. If this is the case, these systems would be attractive targets for indirect searches of weakly interacting massive particle (WIMP) dark matter (DM) annihilation due to their relative proximity and high expected DM content. In this study, we analyze 14.3 years of gamma-ray data collected by the Fermi-LAT coincident with 26 UFCSs. No significant excess gamma-ray emission is detected, and we present gamma-ray flux upper limits for these systems. Assuming that the UFCSs are dark-matter-dominated galaxies consistent with being among the faintest and least massive MW dwarf spheroidal (dSphs) satellite galaxies, we derive the projected sensitivity for a dark matter annihilation signal. We find that observations of UFCSs have the potential to yield some of the most powerful constraints on DM annihilation, with sensitivity comparable to observations of known dSphs and the Galactic center. This result emphasizes the importance of precise kinematic studies of UFCSs to empirically determine their DM content., Comment: 11 pages, 4 figures, 1 table, submitted to ApJL
Published: 2024

2. A new catalog of magnetically active solar-like oscillators

Author: Corsaro, E., Bonanno, A., Kayhan, C., Di Mauro, M. P., Reda, R., and Giovannelli, L.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present a new catalog of stars for which detected solar-like oscillations and magnetic activity measurements are both available from chromospheric spectroscopic observations. Our results were obtained by exploiting NASA TESS mission light curves for active stars observed within the Mount Wilson Observatory HK project and the HK survey of the Hamburg Robotic Telescope TIGRE. We analyzed the light curves for a total of 191 stars by adopting recent techniques based on Bayesian analysis and model comparison to assess the detection of a power excess originating from solar-like oscillations. We characterized the oscillations in a total of 34 targets, for which we provide estimates for the global asteroseismic parameters of $\nu_\mathrm{max}$ (the frequency of maximum oscillation power), $\Delta\nu$ (the large frequency separation), and for the amplitude of the solar-like oscillation envelope $A_\mathrm{max}$. We provide strong statistical evidence for the detection of solar-like oscillations in 15 stars of our sample, identify six further stars where a detection is likely, and 13 stars for which oscillations cannot be ruled out. The key parameters extracted in this work will be exploited for a detailed stellar modeling of the targets and to calibrate relations that connect the level of the measured magnetic activity to the suppression induced on the global oscillation amplitudes. This opens the possibility of shedding light on the interplay between magnetic fields and oscillations. Because of their relatively high brightness, the targets may also be of interest for future dedicated follow-up observations using both photometry and spectropolarimetry., Comment: 9 pages, 3 figures, 2 tables. Accepted for publication in A&A
Published: 2024

3. The GAPS Programme at TNG. XLI. The climate of KELT-9b revealed with a new approach to high spectral resolution phase curves

Author: Pino, L., Brogi, M., Désert, J. M., Nascimbeni, V., Bonomo, A. S., Rauscher, E., Basilicata, M., Biazzo, K., Bignamini, A., Borsa, F., Claudi, R., Covino, E., Di Mauro, M. P., Guilluy, G., Maggio, A., Malavolta, L., Micela, G., Molinari, E., Molinaro, M., Montalto, M., Nardiello, D., Pedani, M., Piotto, G., Poretti, E., Rainer, M., Scandariato, G., Sicilia, D., and Sozzetti, A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: [Abridged] We present a novel method to study the thermal emission of exoplanets as a function of orbital phase at very high spectral resolution, and apply it to investigate the climate of the ultra-hot Jupiter KELT-9b. We combine 3 nights of HARPS-N and 2 nights of CARMENES optical spectra, covering orbital phases between quadratures (0.25 < phi < 0.75), when the planet shows its day-side hemisphere with different geometries. We co-add the signal of thousands of FeI lines through cross-correlation, which we map to a likelihood function. We investigate the phase-dependence of: (i) the line depths of FeI, and (ii) their Doppler shifts, by introducing a new method that exploits the very high spectral resolution of our observations. We confirm a previous detection of FeI emission and demonstrate a combined precision of 0.5 km s-1 on the orbital properties of KELT-9b. By studying the phase-resolved Doppler shift of FeI lines, we detect an anomaly in the planet's orbital radial velocity well-fitted with a slightly eccentric orbit (e = 0.016$\pm$0.003, w = 150$^{+13\circ}_{-11},~5\sigma$ preference). However, we argue that such anomaly can be explained by a day-night wind of a few km s-1 blowing neutral iron gas. Additionally, we find that the FeI emission line depths are symmetric around the substellar point within 10 deg ($2\sigma$). We show that these results are qualitatively compatible with predictions from general circulation models for ultra-hot Jupiter planets. Very high-resolution spectroscopy phase curves have the sensitivity to reveal a phase dependence in both the line depths and their Doppler shifts throughout the orbit. They are highly complementary to space-based phase curves obtained with HST and JWST, and open a new window into the still poorly understood climate and atmospheric structure of the hottest planets known., Comment: Recommended for publication on A&A after referee report, awaiting acceptance. 25 pages, 19 figures, 3 tables
Published: 2022
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4. The GAPS Programme with HARPS-N at TNG. XXXV. Fundamental properties of transiting exoplanet host stars

Author: Biazzo, K., D'Orazi, V., Desidera, S., Turrini, D., Benatti, S., Gratton, R., Magrini, L., Sozzetti, A., Baratella, M., Bonomo, A. S., Borsa, F., Claudi, R., Covino, E., Damasso, M., Di Mauro, M. P., Lanza, A. F., Maggio, A., Malavolta, L., Maldonado, J., Marzari, F., Micela, G., Poretti, E., Vitello, F., Affer, L., Bignamini, A., Carleo, I., Cosentino, R., Fiorenzano, A. F. M., Giacobbe, P., Harutyunyan, A., Leto, G., Mancini, L., Molinari, E., Molinaro, M., Nardiello, D., Nascimbeni, V., Pagano, I., Pedani, M., Piotto, G., Rainer, M., and Scandariato, G.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Exoplanetary properties depend on stellar properties: to know the planet with accuracy and precision it is necessary to know the star as accurately and precisely as possible. Our immediate aim is to characterize in a homogeneous and accurate way a sample of 27 transiting planet-hosting stars observed within the GAPS program. We determined stellar parameters (effective temperature, surface gravity, rotational velocity) and abundances of 26 elements (Li,C,N,O,Na,Mg,Al,Si,S,Ca,Sc,Ti,V,Cr,Fe,Mn,Co,Ni,Cu,Zn,Y,Zr,Ba,La,Nd,Eu). Our study is based on high-resolution HARPS-N@TNG and FEROS@ESO spectra and uniform techniques. We derived kinematic properties from Gaia data and estimated for the first time in exoplanet host stars ages using elemental ratios as chemical clocks. Teff of our stars is of 4400-6700 K, while [Fe/H] is within -0.3 and 0.4 dex. Lithium is present in 7 stars. [X/H] and [X/Fe] abundances vs [Fe/H] are consistent with the Galactic Chemical Evolution. The dependence of [X/Fe] with the condensation temperature is critically analyzed with respect to stellar and kinematic properties. All targets with measured C and O abundances show C/O<0.8, compatible with Si present in rock-forming minerals. Most of targets show 1.0
Published: 2022
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5. Dark Matter search in dwarf irregular galaxies with the Fermi Large Area Telescope

Author: Gammaldi, V., Pérez-Romero, J., Coronado-Blázquez, J., Di Mauro, M., Karukes, E. V., Sánchez-Conde, M. A., and Salucci, P.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We analyze 11 years of Fermi-LAT data corresponding to the sky regions of 7 dwarf irregular (dIrr) galaxies. DIrrs are dark matter (DM) dominated systems, proposed as interesting targets for the indirect search of DM with gamma rays. The galaxies represent interesting cases with a strong disagreement between the density profiles (core vs. cusp) inferred from observations and numerical simulations. In this work, we addressed the problem by considering two different DM profiles, based on both the fit to the rotation curve (in this case a Burkert cored profile) and results from N-body cosmological simulations (i.e., NFW cuspy profile). We also include halo substructures in our analysis, which is expected to boost the DM signal a factor of ten in halos such as those of dIrrs. For each DM model and dIrr, we create a spatial template of the expected DM-induced gamma-ray signal to be used in the analysis of Fermi-LAT data. No significant emission is detected from any of the targets in our sample. Thus, we compute upper limits on the DM annihilation cross-section versus mass parameter space. Among the 7 dIrrs, we find IC10 and NGC6822 to yield the most stringent individual constraints, independently of the adopted DM profile. We also produce combined DM limits for all objects in the sample, which turn out to be dominated by IC10 for all DM models and annihilation channels, i.e. $b\bar{b}$, $\tau^+\tau^-$ and $W^+W^-$. The strongest constraints are obtained for $b\bar{b}$ and are at the level of $\langle\sigma v \rangle \sim 7 \times 10^{-26}\text{cm}^{3}\text{s}^{-1}$ at $m_\chi\sim 6$ GeV. Though these limits are a factor of 3 higher than the thermal relic cross section at low WIMP masses, they are independent from and complementary to those obtained by means of other targets., Comment: 19 pages, 9 figures, Accepted for Publication in PRD
Published: 2021
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6. Asteroseismogyrometry of low-mass red giants I. The SOLA inversion method

Author: Pijpers, F. P., Di Mauro, M. P., and Ventura, R.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: During the past 10 years the unprecedented quality and frequency resolution of asteroseismic data provided by space photometry has revolutionized the study of red-giant stars providing us with the possibility to probe the interior of thousands of these targets. Our aim is to present an asteroseismic tool which allows to determine the total angular momentum of stars, without a priori inference of their internal rotational profile. We adopt and adapt to red giants the asteroseismic inversion technique developed for the case of the Sun. The method has been tested assuming different artificial sets of data, including also modes with harmonic degree l> 1. We estimate with an accuracy of 14.5% the total angular momentum of the red-giant star KIC 4448777 observed by Kepler during the first four consecutive years of operation.} Our results indicate that the measurement of the total angular momentum of red-giant stars can be determined with a fairly high precision by means of asteroseismology by using a small set of rotational splittings of only dipolar modes and that our method, based on observations of stellar pulsations, provides a powerful mean for testing and modeling transport of angular momentum in stars., Comment: 11 pages, 8 figures
Published: 2021
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7. The GAPS Programme with HARPS-N at TNG. XXXI. The WASP-33 system revisited with HARPS-N

Author: Borsa, F., Lanza, A. F., Raspantini, I., Rainer, M., Fossati, L., Brogi, M., Di Mauro, M. P., Gratton, R., Pino, L., Benatti, S., Bignamini, A., Bonomo, A. S., Claudi, R., Esposito, M., Frustagli, G., Maggio, A., Maldonado, J., Mancini, L., Micela, G., Nascimbeni, V., Poretti, E., Scandariato, G., Sicilia, D., Sozzetti, A., Boschin, W., Cosentino, R., Covino, E., Desidera, S., Di Fabrizio, L., Fiorenzano, A. F. M., Harutyunyan, A., Knapic, C., Molinari, E., Pagano, I., Pedani, M., and Piotto, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: [abridged] We analyse four transits of WASP-33b observed with the optical high-resolution HARPS-N spectrograph to confirm its nodal precession, study its atmosphere and investigate the presence of star-planet interactions.We extract the mean line profiles of the spectra by using the LSD method, and analyse the Doppler shadow and the RVs. We also derive the transmission spectrum of the planet, correcting it for the stellar contamination due to rotation, CLV and pulsations. We confirm the previously discovered nodal precession of WASP-33b, almost doubling the time coverage of the inclination and projected spin-orbit angle variation. We find that the projected obliquity reached a minimum in 2011 and use this constraint to derive the geometry of the system, in particular its obliquity at that epoch ($\epsilon=113.99^{\circ}\pm 0.22^{\circ}$) and the inclination of the stellar spin axis ($i_{\rm s}=90.11^{\circ}\pm 0.12^{\circ}$), as well as the gravitational quadrupole moment of the star $J_2=(6.73\pm 0.22)\times 10^{-5}$. We present detections of H$\alpha$ and H$\beta$ absorption in the atmosphere of the planet with a contrast almost twice smaller than previously detected in the literature. We also find evidence for the presence of a pre-transit signal, which repeats in all four analysed transits. The most likely explanation lies in a possible excitation of a stellar pulsation mode by the presence of the planetary companion. Future common analysis of all available datasets in the literature will help shedding light on the possibility that the observed Balmer lines transit depth variations are related to stellar activity and/or pulsation, and to set constraints on the energetics possibly driving atmospheric escape. A complete orbital phase coverage of WASP-33b with high-resolution spectroscopic (spectro-polarimetric) observations could help understanding the nature of the pre-transit signal., Comment: Accepted for publication in A&A
Published: 2021
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8. Smart Anomaly Detection in Sensor Systems: A Multi-Perspective Review

Author: Erhan, L., Ndubuaku, M., Di Mauro, M., Song, W., Chen, M., Fortino, G., Bagdasar, O., and Liotta, A.
Subjects: Computer Science - Machine Learning
Abstract: Anomaly detection is concerned with identifying data patterns that deviate remarkably from the expected behaviour. This is an important research problem, due to its broad set of application domains, from data analysis to e-health, cybersecurity, predictive maintenance, fault prevention, and industrial automation. Herein, we review state-of-the-art methods that may be employed to detect anomalies in the specific area of sensor systems, which poses hard challenges in terms of information fusion, data volumes, data speed, and network/energy efficiency, to mention but the most pressing ones. In this context, anomaly detection is a particularly hard problem, given the need to find computing-energy accuracy trade-offs in a constrained environment. We taxonomize methods ranging from conventional techniques (statistical methods, time-series analysis, signal processing, etc.) to data-driven techniques (supervised learning, reinforcement learning, deep learning, etc.). We also look at the impact that different architectural environments (Cloud, Fog, Edge) can have on the sensors ecosystem. The review points to the most promising intelligent-sensing methods, and pinpoints a set of interesting open issues and challenges.
Published: 2020
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9. The GAPS Programme at TNG XXVII. Reassessment of a young planetary system with HARPS-N: is the hot Jupiter V830 Tau b really there?

Author: Damasso, M., Lanza, A. F., Benatti, S., Rajpaul, V. M., Mallonn, M., Desidera, S., Biazzo, K., D'Orazi, V., Malavolta, L., Nardiello, D., Rainer, M., Borsa, F., Affer, L., Bignamini, A., Bonomo, A. S., Carleo, I., Claudi, R., Cosentino, R., Covino, E., Giacobbe, P., Gratton, R., Harutyunyan, A., Knapic, C., Leto, G., Maggio, A., Maldonado, J., Mancini, L., Micela, G., Molinari, E., Nascimbeni, V., Pagano, I., Piotto, G., Poretti, E., Scandariato, G., Sozzetti, A., Dolcetta, R. Capuzzo, Di Mauro, M. P., Carosati, D., Fiorenzano, A., Frustagli, G., Pedani, M., Pinamonti, M., Stoev, H., and Turrini, D.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Detecting and characterising exoworlds around very young stars (age$<$10 Myr) are key aspects of exoplanet demographic studies, especially for understanding the mechanisms and timescales of planet formation and migration. However, detection using the radial velocity method alone can be very challenging, since the amplitude of the signals due to magnetic activity of such stars can be orders of magnitude larger than those induced even by massive planets. We observed the very young ($\sim$2 Myr) and very active star V830 Tau with the HARPS-N spectrograph to independently confirm and characterise the previously reported hot Jupiter V830 Tau b ($K_{\rm b}=68\pm11$ m/s; $m_{\rm b}sini_{\rm b}=0.57\pm0.10$ $M_{jup}$; $P_{\rm b}=4.927\pm0.008$ d). Due to the observed $\sim$1 km/s radial velocity scatter clearly attributable to V830 Tau's magnetic activity, we analysed radial velocities extracted with different pipelines and modelled them using several state-of-the-art tools. We devised injection-recovery simulations to support our results and characterise our detection limits. The analysis of the radial velocities was aided by using simultaneous photometric and spectroscopic diagnostics. Despite the high quality of our HARPS-N data and the diversity of tests we performed, we could not detect the planet V830 Tau b in our data and confirm its existence. Our simulations show that a statistically-significant detection of the claimed planetary Doppler signal is very challenging. Much as it is important to continue Doppler searches for planets around young stars, utmost care must be taken in the attempt to overcome the technical difficulties to be faced in order to achieve their detection and characterisation. This point must be kept in mind when assessing their occurrence rate, formation mechanisms and migration pathways, especially without evidence of their existence from photometric transits., Comment: Accepted for publication on Astronomy and Astrophysics. Abstract slightly modified to fulfill arxiv requirements
Published: 2020
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10. The GAPS Programme at TNG -- XXIII. HD 164922 d: a close-in super-Earth discovered with HARPS-N in a system with a long-period Saturn mass companion

Author: Benatti, S., Damasso, M., Desidera, S., Marzari, F., Biazzo, K., Claudi, R., Di Mauro, M. P., Lanza, A. F., Pinamonti, M., Barbato, D., Malavolta, L., Poretti, E., Sozzetti, A., Affer, L., Bignamini, A., Bonomo, A. S., Borsa, F., Brogi, M., Bruno, G., Carleo, I., Cosentino, R., Covino, E., Frustagli, G., Giacobbe, P., Gonzalez, M., Gratton, R., Harutyunyan, A., Knapic, C., Leto, G., Lodi, M., Maggio, A., Maldonado, J., Mancini, L., Fiorenzano, A. Martinez, Micela, G., Molinari, E., Molinaro, M., Nardiello, D., Nascimbeni, V., Pagano, I., Pedani, M., Piotto, G., Rainer, M., and Scandariato, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: In the framework of the Global Architecture of Planetary Systems (GAPS) project we collected more than 300 spectra with HARPS-N at the TNG for the bright G9V star HD164922. This target is known to host one gas giant planet in a wide orbit (Pb~1200 days, semi-major axis ~2 au) and a Neptune-mass planet with a period Pc ~76 days. We searched for additional low-mass companions in the inner region of the system. We compared the radial velocities (RV) and the activity indices derived from the HARPS-N time series to measure the rotation period of the star and used a Gaussian process regression to describe the behaviour of the stellar activity. We exploited this information in a combined model of planetary and stellar activity signals in an RV time-series composed of almost 700 high-precision RVs, both from HARPS-N and literature data. We performed a dynamical analysis to evaluate the stability of the system and the allowed regions for additional potential companions. Thanks to the high sensitivity of the HARPS-N dataset, we detect an additional inner super-Earth with an RV semi-amplitude of 1.3+/-0.2 m/s, a minimum mass of ~4+/-1 M_E and a period of 12.458+/-0.003 days. We disentangle the planetary signal from activity and measure a stellar rotation period of ~42 days. The dynamical analysis shows the long term stability of the orbits of the three-planet system and allows us to identify the permitted regions for additional planets in the semi-major axis ranges 0.18-0.21 au and 0.6-1.4 au. The latter partially includes the habitable zone of the system. We did not detect any planet in these regions, down to minimum detectable masses of 5 and 18 M_E, respectively. A larger region of allowed planets is expected beyond the orbit of planet b, where our sampling rules-out bodies with minimum mass > 50 M_E., Comment: 23 pages, 16 Figures. Accepted for publication on A&A
Published: 2020
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11. The $\gamma$-ray Emission of Star-Forming Galaxies

Author: Ajello, M., Di Mauro, M., Paliya, V. S., and Garrappa, S.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: A majority of the $\gamma$-ray emission from star-forming galaxies is generated by the interaction of high-energy cosmic rays with the interstellar gas and radiation fields. Star-forming galaxies are expected to contribute to both the extragalactic $\gamma$-ray background and the IceCube astrophysical neutrino flux. Using roughly 10\,years of $\gamma$-ray data taken by the {\it Fermi} Large Area Telescope, in this study we constrain the $\gamma$-ray properties of star-forming galaxies. We report the detection of 11 bona-fide $\gamma$-ray emitting galaxies and 2 candidates. Moreover, we show that the cumulative $\gamma$-ray emission of below-threshold galaxies is also significantly detected at $\sim$5\,$\sigma$ confidence. The $\gamma$-ray luminosity of resolved and unresolved galaxies is found to correlate with the total (8-1000\,$\mu$m) infrared luminosity as previously determined. Above 1\,GeV, the spectral energy distribution of resolved and unresolved galaxies is found to be compatible with a power law with a photon index of $\approx2.2-2.3$. Finally, we find that star-forming galaxies account for roughly 5\,\% and 3\,\% of the extragalactic $\gamma$-ray background and the IceCube neutrino flux, respectively., Comment: Accepted for publication in The Astrophysical Journal
Published: 2020
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12. Identifying TeV Source Candidates among Fermi-LAT Unclassified Blazars

Author: Chiaro, G., Meyer, M., Di Mauro, M., Salvetti, D., La Mura, G., and Thompson, D. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Blazars and in particular the subclass of high synchrotron peaked Active Galactic Nuclei are among the main targets for the present generation of Imaging Atmospheric Cherenkov Telescopes (IACTs) and will remain of great importance for very high-energy $\gamma$-ray science in the era of the Cherenkov Telescope Array (CTA). Observations by IACTs, which have relatively small fields of view ($\sim$ few degrees), are limited by viewing conditions; therefore, it is important to select the most promising targets in order to increase the number of detections. The aim of this paper is to search for unclassified blazars among known $\gamma$-ray sources from the Fermi Large Area Telescope (LAT) third source catalog that are likely detectable with IACTs or CTA. We use an artificial neural network algorithm and updated analysis of Fermi-LAT data. We found 80 $\gamma$-ray source candidates, and for the highest-confidence candidates, we calculate their potential detectability with IACTs and CTA based on an extrapolation of their energy spectra. Follow-up observations of our source candidates could significantly increase the current TeV source population sample and could ultimately confirm the efficiency of our algorithm to select TeV sources., Comment: 11 pages, 3 figures, accepted for publication in ApJ
Published: 2019
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13. MAGIC and Fermi-LAT gamma-ray results on unassociated HAWC sources

Author: Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babić, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J. A., González, J. Becerra, Bednarek, W., Bernardini, E., Berse, R. Ch., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Domínguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fernández-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., López, R. J. García, Garczarczyk, M., Gaug, M., Giammaria, P., Godinović, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuveždić, D., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., López, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Masuda, S., Mazin, D., Mielke, K., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Stamerra, A., Strzys, M., Surić, T., Takahashi, M., Takalo, L., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Treves, A., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zarić, D., Albert, A., Alfaro, R., Alvarez, C., Arceo, R., Arteaga-Velázquez, J. C., Rojas, D. Avila, Solares, H. A. Ayala, Becerril, A., Belmont-Moreno, E., BenZvi, S. Y., Bernal, A., Braun, J., Caballero-Mora, K. S., Capistrán, T., Carramiñana, A., Casanova, S., Castillo, M., Cotti, U., Cotzomi, J., de León, S. Coutiño, De León, C., De la Fuente, E., Hernandez, R. Diaz, Dichiara, S., Dingus, B. L., DuVernois, M. A., Díaz-Vélez, J. C., Ellsworth, R. W., Engel, K., Enriquez-Rivera, O., Fiorino, D. W., Fleischhack, H., Fraija, N., García-González, J. A., Garfias, F., González-Muñoz, A., González, M. M., Goodman, J. A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hueyotl-Zahuantitla, F., Hui, C. M., Hüntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Lara, A., Lauer, R. J., Lee, W. H., Lennarz, D., Vargas, H. León, Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Luna-García, R., López-Coto, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martínez-Castro, J., Martínez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafá, M., Nayerhoda, A., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Pérez-Pérez, E. G., Ren, Z., Rho, C. D., Rivière, C., Rosa-González, D., Rosenberg, M., Ruiz-Velasco, E., Greus, F. Salesa, Sandoval, A., Schneider, M., Arroyo, M. Seglar, Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Taboada, I., Tibolla, O., Tollefson, K., Torres, I., Ukwatta, T. N., Vianello, G., Villaseñor, L., Werner, F., Westerhoff, S., Wood, J., Yapici, T., Yodh, G., Zepeda, A., Zhou, H., Álvarez, J. D., Ajello, M., Baldini, L., Barbiellini, G., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Brandt, T. J., Bregeon, J., Bruel, P., Cameron, R. A., Caputo, R., Caraveo, P. A., Castro, D., Cavazzuti, E., Chiaro, G., Ciprini, S., Costantin, D., D'Ammando, F., de Palma, F., Desai, A., Di Lalla, N., Di Mauro, M., Di Venere, L., Favuzzi, C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Green, D., Grenier, I. A., Guiriec, S., Harding, A. K., Hays, E., Hewitt, J. W., Horan, D., Jóhannesson, G., Kuss, M., Larsson, S., Liodakis, I., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Manfreda, A., Mazziotta, M. N., Mereu, I., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Palatiello, M., Paliya, V. S., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Tajima, H., Thayer, J. B., Thompson, D. J., Torres, D. F., Torresi, E., Troja, E., Valverde, J., Wood, K., and Yassine, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The HAWC Collaboration released the 2HWC catalog of TeV sources, in which 19 show no association with any known high-energy (HE; E > 10 GeV) or very-high-energy (VHE; E > 300 GeV) sources. This catalog motivated follow-up studies by both the MAGIC and Fermi-LAT observatories with the aim of investigating gamma-ray emission over a broad energy band. In this paper, we report the results from the first joint work between HAWC, MAGIC and Fermi-LAT on three unassociated HAWC sources: 2HWC J2006+341, 2HWC J1907+084* and 2HWC J1852+013*. Although no significant detection was found in the HE and VHE regimes, this investigation shows that a minimum 1 degree extension (at 95% confidence level) and harder spectrum in the GeV than the one extrapolated from HAWC results are required in the case of 2HWC J1852+013*, while a simply minimum extension of 0.16 degrees (at 95% confidence level) can already explain the scenario proposed by HAWC for the remaining sources. Moreover, the hypothesis that these sources are pulsar wind nebulae is also investigated in detail., Comment: 12 pages, 3 figures. Accepted for publication in MNRAS
Published: 2019
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14. Unresolved Gamma-Ray Sky through its Angular Power Spectrum

Author: Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Costantin, D., Cuoco, A., Cutini, S., D'Ammando, F., Luque, P. de la Torre, de Palma, F., Desai, A., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Dirirsa, F. Fana, Favuzzi, C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Guillemot, L., Guiriec, S., Horan, D., Johannesson, G., Kuss, M., Larsson, S., Latronico, L., Li, J., Liodakis, I., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Mereu, I., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Raino, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Serini, D., Sgro, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, M., Thayer, J. B., Tibaldo, L., Torres, D. F., Troja, E., Venters, T. M., Vianello, G., Wood, K., Yassine, M., Zaharijas, G., Ammazzalorso, S., Fornengo, N., and Regis, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology
Abstract: The gamma-ray sky has been observed with unprecedented accuracy in the last decade by the Fermi large area telescope (LAT), allowing us to resolve and understand the high-energy Universe. The nature of the remaining unresolved emission (unresolved gamma-ray background, UGRB) below the LAT source detection threshold can be uncovered by characterizing the amplitude and angular scale of the UGRB fluctuation field. This work presents a measurement of the UGRB autocorrelation angular power spectrum based on eight years of Fermi LAT Pass 8 data products. The analysis is designed to be robust against contamination from resolved sources and noise systematics. The sensitivity to subthreshold sources is greatly enhanced with respect to previous measurements. We find evidence (with $\sim$3.7$\sigma$ significance) that the scenario in which two classes of sources contribute to the UGRB signal is favored over a single class. A double power law with exponential cutoff can explain the anisotropy energy spectrum well, with photon indices of the two populations being 2.55 $\pm$ 0.23 and 1.86 $\pm$ 0.15., Comment: 8 + 12 (SOM) pages, Contact author: Michela Negro (michela.negro@to.infn.it). (Typos in Tab. VII in previous versions)
Published: 2018
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15. VERITAS and Fermi-LAT observations of new HAWC sources

Author: VERITAS Collaboration, Abeysekara, A. U., Archer, A., Benbow, W., Bird, R., Brose, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Chromey, A. J., Connolly, M. P., Cui, W., Daniel, M. K., Falcone, A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Hutten, M., Hanna, D., Hervet, O., Holder, J., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., McArthur, S., Moriarty, P., Mukherjee, R., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rulten, C., Sadeh, I., Santander, M., Sembroski, G. H., Shahinyan, K., Sushch, I., Tyler, J., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Williamson, T. J., Zitzer, B., Collaboration, Fermi-LAT, Abdollahi, S., Ajello, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buehler, R., Cameron, R. A., Caputo, R., Caraveo, P. A., Castro, D., Cavazzuti, E., Charles, E., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costantin, D., Cutini, S., D'Ammando, F., de Palma, F., Di Lalla, N., Di Mauro, M., Di Venere, L., Dominguez, A., Favuzzi, C., Fegan, S. J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Guillemot, L., Guiriec, S., Hays, E., Hewitt, J. W., Horan, D., Johannesson, G., Kensei, S., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J. D., Maldera, S., Mazziotta, M. N., McEnery, J. E., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ojha, R., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Perkins, J. S., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Raino, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Sgro, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Torres, D. F., Tosti, G., Troja, E., Valverde, J., Vianello, G., Vogel, M., Wood, K., Yassine, M., Collaboration, HAWC, Alfaro, R., Alvarez, C., Alvarez, J. D., Arceo, R., Arteaga-Velazquez, J. C., Rojas, D. Avila, Solares, H. A. Ayala, Becerril, A., Belmont-Moreno, E., BenZvi, S. Y., Bernal, A., Braun, J., Brisbois, C., Caballero-Mora, K. S., Capistran, T., Carraminana, A., Casanova, S., Castillo, M., Cotti, U., Cotzomi, J., de Leon, S. Coutino, De Leon, C., De la Fuente, E., Dichiara, S., Dingus, B. L., DuVernois, M. A., Diaz-Velez, J. C., Engel, K., Enriquez-Rivera, O., Fiorino, D. W., Fleischhack, H., Fraija, N., Garcia-Gonzalez, J. A., Garfias, F., Munoz, A. Gonzalez, Gonzalez, M. M., Goodman, J. A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hernandez-Almada, A., Hona, B., Hueyotl-Zahuantitla, F., Hui, C. M., Huntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Lara, A., Lauer, R. J., Lee, W. H., Lennarz, D., Vargas, H. Leon, Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Luna-Garcia, R., Lopez-Coto, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martinez-Castro, J., Martinez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafa, M., Nayerhoda, A., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Perez-Perez, E. G., Ren, Z., Rho, C. D., Riviere, C., Rosa-Gonzalez, D., Rosenberg, M., Ruiz-Velasco, E., Salazar, H., Greus, F. Salesa, Sandoval, A., Schneider, M., Arroyo, M. Seglar, Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Taboada, I., Tibolla, O., Tollefson, K., Torres, I., Ukwatta, T. N., Villasenor, L., Weisgarber, T., Westerhoff, S., Wisher, I. G., Wood, J., Yapici, T., Yodh, G., Zepeda, A., and Zhou, H.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The HAWC (High Altitude Water Cherenkov) collaboration recently published their 2HWC catalog, listing 39 very high energy (VHE; >100~GeV) gamma-ray sources based on 507 days of observation. Among these, there are nineteen sources that are not associated with previously known TeV sources. We have studied fourteen of these sources without known counterparts with VERITAS and Fermi-LAT. VERITAS detected weak gamma-ray emission in the 1~TeV-30~TeV band in the region of DA 495, a pulsar wind nebula coinciding with 2HWC J1953+294, confirming the discovery of the source by HAWC. We did not find any counterpart for the selected fourteen new HAWC sources from our analysis of Fermi-LAT data for energies higher than 10 GeV. During the search, we detected GeV gamma-ray emission coincident with a known TeV pulsar wind nebula, SNR G54.1+0.3 (VER J1930+188), and a 2HWC source, 2HWC J1930+188. The fluxes for isolated, steady sources in the 2HWC catalog are generally in good agreement with those measured by imaging atmospheric Cherenkov telescopes. However, the VERITAS fluxes for SNR G54.1+0.3, DA 495, and TeV J2032+4130 are lower than those measured by HAWC and several new HAWC sources are not detected by VERITAS. This is likely due to a change in spectral shape, source extension, or the influence of diffuse emission in the source region., Comment: Accepted for publication in the ApJ, Corresponding author: Nahee Park (VERITAS Collaboration), John W. Hewitt (Fermi-LAT Collaboration), Ignacio Taboada (HAWC Collaboration), 30 pages, 12 figures
Published: 2018
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16. The rotational shear layer inside the early red-giant star KIC 4448777

Author: Di Mauro, M. P., Ventura, R., Corsaro, E., and De Moura, B. Lustosa
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the asteroseismic study of the early red-giant star KIC 4448777, complementing and integrating a previous work (Di Mauro et al. 2016), aimed at characterizing the dynamics of its interior by analyzing the overall set of data collected by the {\it Kepler} satellite during the four years of its first nominal mission. We adopted the Bayesian inference code DIAMOND (Corsaro \& De Ridder 2014) for the peak bagging analysis and asteroseismic splitting inversion methods to derive the internal rotational profile of the star. The detection of new splittings of mixed modes, more concentrated in the very inner part of the helium core, allowed us to reconstruct the angular velocity profile deeper into the interior of the star and to disentangle the details better than in Paper I: the helium core rotates almost rigidly about 6 times faster than the convective envelope, while part of the hydrogen shell seems to rotate at a constant velocity about 1.15 times lower than the He core. In particular, we studied the internal shear layer between the fast-rotating radiative interior and the slow convective zone and we found that it lies partially inside the hydrogen shell above $r \simeq 0.05R$ and extends across the core-envelope boundary. Finally, we theoretically explored the possibility for the future to sound the convective envelope in the red-giant stars and we concluded that the inversion of a set of splittings with only low-harmonic degree $l\leq 3$, even supposing a very large number of modes, will not allow to resolve the rotational profile of this region in detail., Comment: accepted for publication on ApJ
Published: 2018
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17. Phase time and transmission probability in the traversal of a PT-symmetric potential: the case of an electromagnetic waveguide

Author: Di Mauro, M., Esposito, S., and Naddeo, A.
Subjects: Quantum Physics, Condensed Matter - Materials Science, Physics - Optics
Abstract: We study the unconventional transmission properties of a wave-packet through a PT-symmetric potential region, as describing actual electromagnetic wave propagation along a waveguide filled with gain and loss media. The non-trivial behavior of the transmission probability manifests in the giant amplification of the incident electromagnetic signal of given wavelengths for well-defined configurations, depending on the gain/loss contrast. Maximum transmission peaks are related to spectral singularities and a strict correlation exists between the "resonant" wavelengths and the gain/loss contrast. The transit times are as well calculated, showing their surprising vanishing in the opaque barrier limit, independently of the gain/loss contrast, which is reminiscent of some sort of Hartman effect. Also, non-local effects manifest in the presence of negative delay times for given configurations, while a correlation is apparent between maximum delay times and transmission probability peaks, though appreciably depending on the gain/loss contrast., Comment: Latex, 8 pages, 5 figures
Published: 2017

18. PLATO as it is: a legacy mission for Galactic archaeology

Author: Miglio, A., Chiappini, C., Mosser, B., Davies, G. R., Freeman, K., Girardi, L., Jofre, P., Kawata, D., Rendle, B. M., Valentini, M., Casagrande, L., Chaplin, W. J., Gilmore, G., Hawkins, K., Holl, B., Appourchaux, T., Belkacem, K., Bossini, D., Brogaard, K., Goupil, M. -J., Montalban, J., Noels, A., Anders, F., Rodrigues, T., Piotto, G., Pollacco, D., Rauer, H., Prieto, C. Allende, Avelino, P. P., Babusiaux, C., Barban, C., Barbuy, B., Basu, S., Baudin, F., Benomar, O., Bienayme, O., Binney, J., Bland-Hawthorn, J., Bressan, A., Cacciari, C., Campante, T. L., Cassisi, S., Christensen-Dalsgaard, J., Combes, F., Creevey, O., Cunha, M. S., de Jong, R. S., de Laverny, P., Degl'Innocenti, S., Deheuvels, S., Depagne, E., DeRidder, J., DiMatteo, P., Di Mauro, M. P., Dupret, M. -A., Eggenberger, P., Elsworth, Y., Famaey, B., Feltzing, S., Garcia, R. A., Gerhard, O., Gibson, B. K., Gizon, L., Haywood, M., Handberg, R., Heiter, U., Hekker, S., Huber, D., Ibata, R., Katz, D., Kawaler, S. D., Kjeldsen, H., Kurtz, D. W., Lagarde, N., Lebreton, Y., Lund, M. N., Majewski, S. R., Marigo, P., Martig, M., Mathur, S., Minchev, I., Morel, T., Ortolani, S., Pinsonneault, M. H., Plez, B., Moroni, P. G. Prada, Pricopi, D., Recio-Blanco, A., Reyle, C., Robin, A., Roxburgh, I. W., Salaris, M., Santiago, B. X., Schiavon, R., Serenelli, A., Sharma, S., Aguirre, V. Silva, Soubiran, C., Steinmetz, M., Stello, D., Strassmeier, K. G., Ventura, P., Ventura, R., Walton, N. A., and Worley, C. C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Deciphering the assembly history of the Milky Way is a formidable task, which becomes possible only if one can produce high-resolution chrono-chemo-kinematical maps of the Galaxy. Data from large-scale astrometric and spectroscopic surveys will soon provide us with a well-defined view of the current chemo-kinematical structure of the Milky Way, but will only enable a blurred view on the temporal sequence that led to the present-day Galaxy. As demonstrated by the (ongoing) exploitation of data from the pioneering photometric missions CoRoT, Kepler, and K2, asteroseismology provides the way forward: solar-like oscillating giants are excellent evolutionary clocks thanks to the availability of seismic constraints on their mass and to the tight age-initial-mass relation they adhere to. In this paper we identify five key outstanding questions relating to the formation and evolution of the Milky Way that will need precise and accurate ages for large samples of stars to be addressed, and we identify the requirements in terms of number of targets and the precision on the stellar properties that are needed to tackle such questions. By quantifying the asteroseismic yields expected from PLATO for red-giant stars, we demonstrate that these requirements are within the capabilities of the current instrument design, provided that observations are sufficiently long to identify the evolutionary state and allow robust and precise determination of acoustic-mode frequencies. This will allow us to harvest data of sufficient quality to reach a 10% precision in age. This is a fundamental pre-requisite to then reach the more ambitious goal of a similar level of accuracy, which will only be possible if we have to hand a careful appraisal of systematic uncertainties on age deriving from our limited understanding of stellar physics, a goal which conveniently falls within the main aims of PLATO's core science., Comment: 17 pages, 9 figures, accepted for publication in Astronomical Notes
Published: 2017
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19. L'eliosismologia: onde sismiche per studiare l'interno del Sole

Author: Di Mauro, M. P.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: During the last 50 years we have been witness of an extraordinary revolution in the knowledge and understanding of our star thanks to the development of Helioseismology, the study of solar oscillations. Similar to what happens on the Earth during earthquakes, the interior of the Sun is continuously pervaded by seismic waves which produce small oscillations on the photosphere. These oscillations bring the signature of several processes which happen in the interior of the solar structure and the seismic frequencies of the oscillation modes detected on the solar surface are directly related to physical parameters of the internal layers crossed by the seismic waves. The study of oscillations represents, then, the only method to infer directly the internal structure and dynamics of the Sun. This article will present the general characteristics of solar oscillations, the main important results and the advances obtained in stellar physics thanks to the methods of Helioseismology., Comment: in Italian
Published: 2017

20. Cosmic-ray electron+positron spectrum from 7 GeV to 2 TeV with the Fermi Large Area Telescope

Author: Collaboration, Fermi-LAT, Abdollahi, S., Ackermann, M., Ajello, M., Atwood, W. B., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Bloom, E. D., Bonino, R., Brandt, T. J., Bregeon, J., Bruel, P., Buehler, R., Cameron, R. A., Caputo, R., Caragiulo, M., Castro, D., Cavazzuti, E., Cecchi, C., Chekhtman, A., Ciprini, S., Cohen-Tanugi, J., Costanza, F., Cuoco, A., Cutini, S., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Focke, W. B., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Guillemot, L., Guiriec, S., Harding, A. K., Jogler, T., Jóhannesson, G., Kamae, T., Kuss, M., La Mura, G., Latronico, L., Longo, F., Loparco, F., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Michelson, P. F., Mirabal, N., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Orlando, E., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Principe, G., Rainò, S., Rando, R., Razzano, M., Reimer, A., Reimer, O., Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Tajima, H., Thayer, J. B., Tibaldo, L., Torres, D. F., Troja, E., Wood, M., Worley, A., Zaharijas, G., and Zimmer, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a measurement of the cosmic-ray electron+positron spectrum between 7 GeV and 2 TeV performed with almost seven years of data collected with the Fermi Large Area Telescope. We find that the spectrum is well fit by a broken power law with a break energy at about 50 GeV. Above 50 GeV, the spectrum is well described by a single power law with a spectral index of $3.07 \pm 0.02 \; (\text{stat+syst}) \pm 0.04 \; (\text{energy measurement})$. An exponential cutoff lower than 1.8 TeV is excluded at 95\% CL.
Published: 2017
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21. Fermi-LAT Observations of High-energy Behind-the-limb Solar Flares

Author: Ackermann, M., Allafort, A., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Cecchi, C., Charles, E., Ciprini, S., Costanza, F., Cutini, S., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Drell, P. S., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Giglietto, N., Giordano, F., Giroletti, M., Grenier, I. A., Guillemot, L., Guiriec, S., Jogler, T., Jóhannesson, G., Kashapova, L., Krucker, S., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Liu, W., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Manfreda, A., Mazziotta, M. N., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orlando, E., Pal'shin, V., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Petrosian, V., Piron, F., Principe, G., Rainò, S., Rando, R., Razzano, M., Reimer, O., da Costa, F. Rubio, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Tajima, H., Thayer, J. B., Torres, D. F., Troja, E., and Vianello, G.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the Fermi-LAT detection of high-energy emission from the behind-the-limb (BTL) solar flares that occurred on 2013 October 11, and 2014 January 6 and September 1. The Fermi-LAT observations are associated with flares from active regions originating behind both the eastern and western limbs, as determined by STEREO. All three flares are associated with very fast coronal mass ejections (CMEs) and strong solar energetic particle events. We present updated localizations of the >100 MeV photon emission, hard X-ray (HXR)and EUV images, and broadband spectra from 10 keV to 10 GeV, as well as microwave spectra. We also provide a comparison of the BTL flares detected by Fermi-LAT with three on-disk flares and present a study of some of the significant quantities of these flares as an attempt to better understand the acceleration mechanisms at work during these occulted flares. We interpret the HXR emission to be due to electron bremsstrahlung from a coronal thin-target loop top with the accelerated electron spectra steepening at semirelativistic energies. The >100 MeV gamma-rays are best described by a pion-decay model resulting from the interaction of protons (and other ions) in a thick-target photospheric source. The protons are believed to have been accelerated (to energies >10 GeV) in the CME environment and precipitate down to the photosphere from the downstream side of the CME shock and landed on the front side of the Sun, away from the original flare site and the HXR emission., Comment: 13 pages, 14 figures published on ApJ
Published: 2017
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22. Search for extended sources in the Galactic Plane using 6 years of Fermi-Large Area Telescope Pass 8 data above 10 GeV

Author: The Fermi LAT Collaboration, Ackermann, M., Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Bissaldi, E., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bregeon, J., Bruel, P., Buehler, R., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Castro, D., Cavazzuti, E., Cecchi, C., Charles, E., Chekhtman, A., Cheung, C. C., Chiaro, G., Ciprini, S., Cohen, J. M., Costantin, D., Costanza, F., Cutini, S., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Grondin, M. -H., Guillemot, L., Guiriec, S., Harding, A. K., Hays, E., Hewitt, J. W., Horan, D., Hou, X., Jóhannesson, G., Kamae, T., Kuss, M., La Mura, G., Larsson, S., Lemoine-Goumard, M., Li, J., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paliya, V. S., Paneque, D., Perkins, J. S., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Raino, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Sgro, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tak, D., Thayer, J. B., Thompson, D. J., Torres, D. F., Tosti, G., Troja, E., Vianello, G., Wood, K. S., and Wood, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The spatial extension of a gamma-ray source is an essential ingredient to determine its spectral properties as well as its potential multi-wavelength counterpart. The capability to spatially resolve gamma-ray sources is greatly improved by the newly delivered Fermi-Large Area Telescope (LAT) Pass 8 event-level analysis which provides a greater acceptance and an improved point spread function, two crucial factors for the detection of extended sources. Here, we present a complete search for extended sources located within 7 degrees from the Galactic plane, using 6 years of LAT data above 10 GeV. We find 46 extended sources and provide their morphological and spectral characteristics. This constitutes the first catalog of hard LAT extended sources, named the Fermi Galactic Extended Source Catalog, which allows a thorough study of the properties of the Galactic plane in the sub-TeV domain., Comment: 33 pages, 22 figures & 3 tables. Published by The Astrophysical Journal. Available on the Fermi Science Support Center (FSSC) together with the 3FHL catalog
Published: 2017
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23. The second catalog of flaring gamma-ray sources from the Fermi All-sky Variability Analysis

Author: Abdollahi, S., Ackermann, M., Ajello, M., Albert, A., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Gonzalez, J. Becerra, Bellazzini, R., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Buson, S., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Cecchi, C., Chekhtman, A., Cheung, C. C., Chiaro, G., Ciprini, S., Conrad, J., Costantin, D., Costanza, F., Cutini, S., D'Ammando, F., de Palma, F., Desai, A., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Donaggio, B., Drell, P. S., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giomi, M., Giordano, F., Giroletti, M., Glanzman, T., Green, D., Grenier, I. A., Grove, J. E., Guillemot, L., Guiriec, S., Hays, E., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J. D., Maldera, S., Manfreda, A., Mayer, M., Mazziotta, M. N., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Paliya, V. S., Paneque, D., Perkins, J. S., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Stawarz, L., Suson, D. J., Takahashi, M., Tanaka, K., Thayer, J. B., Thompson, D. J., Torres, D. F., Torresi, E., Tosti, G., Troja, E., Vianello, G., and Wood, K. S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the second catalog of flaring gamma-ray sources (2FAV) detected with the Fermi All-sky Variability Analysis (FAVA), a tool that blindly searches for transients over the entire sky observed by the Large Area Telescope (LAT) on board the \textit{Fermi} Gamma-ray Space Telescope. With respect to the first FAVA catalog, this catalog benefits from a larger data set, the latest LAT data release (Pass 8), as well as from an improved analysis that includes likelihood techniques for a more precise localization of the transients. Applying this analysis on the first 7.4 years of \textit{Fermi} observations, and in two separate energy bands 0.1$-$0.8 GeV and 0.8$-$300 GeV, a total of 4547 flares has been detected with a significance greater than $6\sigma$ (before trials), on the time scale of one week. Through spatial clustering of these flares, 518 variable gamma-ray sources are identified. Likely counterparts, based on positional coincidence, have been found for 441 sources, mostly among the blazar class of active galactic nuclei. For 77 2FAV sources, no likely gamma-ray counterpart has been found. For each source in the catalog, we provide the time, location, and spectrum of each flaring episode. Studying the spectra of the flares, we observe a harder-when-brighter behavior for flares associated with blazars, with the exception of BL Lac flares detected in the low-energy band. The photon indexes of the flares are never significantly smaller than 1.5. For a leptonic model, and under the assumption of isotropy, this limit suggests that the spectrum of the freshly accelerated electrons is never harder than $p\sim$2., Comment: Accepted for publication by The Astrophysical Journal Supplement. Online analysis results available at http://fermi.gsfc.nasa.gov/ssc/data/access/lat/FAVA/index.php . Corresponding authors: M. Giomi, R. Buehler, D. Kocevski, and M. Ajello
Published: 2016
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24. Gamma-ray blazar spectra with H.E.S.S. II mono analysis: the case of PKS 2155-304 and PG 1553+113

Author: Collaboration, H. E. S. S., Abdalla, H., Abramowski, A., Aharonian, F., Benkhali, F. Ait, Akhperjanian, A. G., Andersson, T., Angüner, E. O., Arrieta, M., Aubert, P., Backes, M., Balzer, A., Barnard, M., Becherini, Y., Tjus, J. Becker, Berge, D., Bernhard, S., Bernlöhr, K., Blackwell, R., Böttcher, M., Boisson, C., Bolmont, J., Bordas, P., Brun, F., Brun, P., Bryan, M., Bulik, T., Capasso, M., Carr, J., Casanova, S., Cerruti, M., Chakraborty, N., Chalme-Calvet, R., Chaves, R. C. G., Chen, A., Chevalier, J., Chrétien, M., Colafrancesco, S., Cologna, G., Condon, B., Conrad, J., Couturier, C., Cui, Y., Davids, I. D., Degrange, B., Deil, C., Devin, J., deWilt, P., Dirson, L., Djannati-Ataï, A., Domainko, W., Donath, A., Drury, L. O'C., Dubus, G., Dutson, K., Dyks, J., Edwards, T., Egberts, K., Eger, P., Ernenwein, J. -P., Eschbach, S., Farnier, C., Fegan, S., Fern, M. V., Fiasson, A., Fontaine, G., Förster, A., Funk, S., Füßling, M., Gabici, S., Gajdus, M., Gallant, Y. A., Garrigoux, T., Giavitto, G., Giebels, B., Glicenstein, J. F., Gottschall, D., Goyal, A., Grondin, M. -H., Hadasch, D., Hahn, J., Haupt, M., Hawkes, J., Heinzelmann, G., Henri, G., Hermann, G., Hervet, O., Hillert, A., Hinton, J. A., Hofmann, W., Hoischen, C., Holler, M., Horns, D., Ivascenko, A., Jacholkowska, A., Jamrozy, M., Janiak, M., Jankowsky, D., Jankowsky, F., Jingo, M., Jogler, T., Jouvin, L., Jung-Richardt, I., Kastendieck, M. A., Katarzyński, K., Katz, U., Kerszberg, D., Khélifi, B., Kieffer, M., King, J., Klepser, S., Klochkov, D., Kluźniak, W., Kolitzus, D., Komin, Nu., Kosack, K., Krakau, S., Kraus, M., Krayzel, F., Krüger, P. P., Laffon, H., Lamanna, G., Lau, J., Lees, J. -P., Lefaucheur, J., Lefranc, V., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Leser, E., Lohse, T., Lorentz, M., Liu, R., López-Coto, R., Lypova, I., Mar, V., Marcowith, A., Mariaud, C., Marx, R., Maurin, G., Maxted, N., Mayer, M., Meintjes, P. J., Meyer, M., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mohrmann, L., Morå, K., Moulin, E., Murach, T., de Naurois, M., Niederwanger, F., Niemiec, J., Oakes, L., O'Brien, P., Odaka, H., Öttl, S., Ohm, S., Ostrowski, M., Oya, I., Padovani, M., Panter, M., Parsons, R. D., Arribas, M. Paz, Pekeur, N. W., Pelletier, G., Perennes, C., Petrucci, P. -O., Peyaud, B., Pita, S., Poon, H., Prokhorov, D., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Reimer, A., Reimer, O., Renaud, M., Reyes, R. de los, Rieger, F., Romoli, C., Rosier-Lees, S., Rowell, G., Rudak, B., Rulten, C. B., Sahakian, V., Salek, D., Sanchez, D. A., Santangelo, A., Sasaki, M., Schlickeiser, R., Schüssler, F., Schulz, A., Schwanke, U., Schwemmer, S., Settimo, M., Seyffert, A. S., Shafi, N., Shilon, I., Simoni, R., Sol, H., Spanier, F., Spengler, G., Spies, F., Stawarz, Ł., Steenkamp, R., Stegmann, C., Stinzing, F., Stycz, K., Sushch, I., Tavernet, J. -P., Tavernier, T., Taylor, A. M., Terrier, R., Tibaldo, L., Tiziani, D., Tluczykont, M., Trichard, C., Tuffs, R., Uchiyama, Y., van der Walt, D. J., van Eldik, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Voisin, F., Völk, H. J., Vuillaume, T., Wadiasingh, Z., Wagner, S. J., Wagner, P., Wagner, R. M., White, R., Wierzcholska, A., Willmann, P., Wörnlein, A., Wouters, D., Yang, R., Zabalza, V., Zaborov, D., Zacharias, M., Zdziarski, A. A., Zech, A., Zefi, F., Ziegler, A., Żywucka, N., Collaboration, LAT, Ackermann, M., Ajello, M., Baldini, L., Barbiellini, G., Bellazzini, R., Bl, R. D., Bonino, R., Bregeon, J., Bruel, P., Buehler, R., Cali, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Cecchi, C., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costanza, F., Cutini, S., D'Amm, F., de Palma, F., Desiante, R., Di Lalla, N., Di Mauro, M., Di Venere, L., Donaggio, B., Favuzzi, C., Focke, W. B., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Guillemot, L., Guiriec, S., Horan, D., Jóhannesson, G., Kamae, T., Kensei, S., Kocevski, D., Larsson, S., Li, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Manfreda, A., Mazziotta, M. N., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Negro, M., Nuss, E., Orienti, M., Orl, E., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Principe, G., Rainò, S., Razzano, M., Simone, D., Siskind, E. J., Spada, F., Spinelli, P., Thayer, J. B., Torres, D. F., Torresi, E., Troja, E., Vianello, G., and Wood, K. S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The addition of a 28 m Cherenkov telescope (CT5) to the H.E.S.S. array extended the experiment's sensitivity to lower energies. The lowest energy threshold is obtained using monoscopic analysis of data taken with CT5, providing access to gamma-ray energies below 100 GeV. Such an extension of the instrument's energy range is particularly beneficial for studies of Active Galactic Nuclei with soft spectra, as expected for those at a redshift > 0.5. The high-frequency peaked BL Lac objects PKS 2155-304 (z = 0.116) and PG 1553+113 (0.43 < z < 0.58) are among the brightest objects in the gamma-ray sky, both showing clear signatures of gamma-ray absorption at E > 100 GeV interpreted as being due to interactions with the extragalactic background light (EBL). Multiple observational campaigns of PKS 2155-304 and PG 1553+113 were conducted during 2013 and 2014 using the full H.E.S.S. II instrument. A monoscopic analysis of the data taken with the new CT5 telescope was developed along with an investigation into the systematic uncertainties on the spectral parameters. The energy spectra of PKS 2155-304 and PG 1553+113 were reconstructed down to energies of 80 GeV for PKS 2155-304, which transits near zenith, and 110 GeV for the more northern PG 1553+113. The measured spectra, well fitted in both cases by a log-parabola spectral model (with a 5.0 sigma statistical preference for non-zero curvature for PKS 2155-304 and 4.5 sigma for PG 1553+113), were found consistent with spectra derived from contemporaneous Fermi-LAT data, indicating a sharp break in the observed spectra of both sources at E ~ 100 GeV. When corrected for EBL absorption, the intrinsic H.E.S.S. II mono and Fermi-LAT spectrum of PKS 2155-304 was found to show significant curvature. For PG 1553+113, however, no significant detection of curvature in the intrinsic spectrum could be found within statistical and systematic uncertainties., Comment: 13 pages, 9 figures, accepted for publication in A&A
Published: 2016
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25. A double blind randomized controlled trial investigating efficacy and safety of varenicline for smoking cessation in patients with type 2 diabetes: study protocol

Author: Russo, C., Caponnetto, P., Cibella, F., Maglia, M., Alamo, A., Campagna, D., Frittitta, L., Di Mauro, M., Leotta, C., Mondati, E., Krysiński, A., Franek, E., and Polosa, R.
Published: 2021
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26. Searching the Gamma-ray Sky for Counterparts to Gravitational Wave Sources: Fermi GBM and LAT Observations of LVT151012 and GW151226

Author: Racusin, J. L., Burns, E., Goldstein, A., Connaughton, V., Wilson-Hodge, C. A., Jenke, P., Blackburn, L., Briggs, M. S., Broida, J., Camp, J., Christensen, N., Hui, C. M., Littenberg, T., Shawhan, P., Singer, L., Veitch, J., Bhat, P. N., Cleveland, W., Fitzpatrick, G., Gibby, M. H., von Kienlin, A., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O. J., Stanbro, M., Veres, P., Zhang, B. -B., Ackermann, M., Albert, A., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Baring, M. G., Bastieri, D., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bonino, R., Bregeon, J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caputo, R., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chiang, J., Ciprini, S., Costanza, F., Cuoco, A., Cutini, S., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Drell, P. S., Favuzzi, C., Ferrara, E. C., Focke, W. B., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Gill, R., Giroletti, M., Glanzman, T., Granot, J., Green, D., Grove, J. E., Guillemot, L., Guiriec, S., Harding, A. K., Jogler, T., Johannesson, G., Kamae, T., Kensei, S., Kocevski, D., Kuss, M., Larsson, S., Latronico, L., Li, J., Longo, F., Loparco, F., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., McEnery, J. E., Michelson, P. F., Mizuno, T., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Principe, G., Raino, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Parkinson, P. M. Saz, Scargle, J. D., Sgro, C., Simone, D., Siskind, E. J., Smith, D. A., Spada, F., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Torres, D. F., Troja, E., Uchiyama, Y., Vianello, G., Wood, K. S., and Wood, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the Fermi Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) observations of the LIGO binary black hole merger event GW151226 and candi- date LVT151012. No candidate electromagnetic counterparts were detected by either the GBM or LAT. We present a detailed analysis of the GBM and LAT data over a range of timescales from seconds to years, using automated pipelines and new techniques for char- acterizing the upper limits across a large area of the sky. Due to the partial GBM and LAT coverage of the large LIGO localization regions at the trigger times for both events, dif- ferences in source distances and masses, as well as the uncertain degree to which emission from these sources could be beamed, these non-detections cannot be used to constrain the variety of theoretical models recently applied to explain the candidate GBM counterpart to GW150914., Comment: 27 pages, 1 table, 11 figures, Submitted to ApJ
Published: 2016
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27. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McCormick, S., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal-Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. -P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey-Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., McConnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro-Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. -D., Kubánek, P., Guziy, S., Castellón, A., García-Cerezo, A., Muñoz, V. F., del Pulgar, C. Pérez, Castillo-Carrión, S., Cerón, J. M. Castro, Hudec, R., Caballero-García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Sanguino, T. de J. Mateo, Fernández-Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, Ch., Fan, Y., Wang, Ch., Hiriart, D., Lee, W. H., Claret, A., Sánchez-Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau-Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. -B., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., von Kienlin, A., Kippen, R. M., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. 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L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492
Published: 2016
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28. Localization and broadband follow-up of the gravitational-wave transient GW150914

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. 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S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Weßels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. -P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey-Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., McConnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro-Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. -D., Kubánek, P., Guziy, S., Castellón, A., García-Cerezo, A., Muñoz, V. F., del Pulgar, C. Pérez, Castillo-Carrión, S., Cerón, J. M. Castro, Hudec, R., Caballero-García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Sanguino, T. de J. Mateo, Fernández-Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, Ch., Fan, Y., Wang, Ch., Hiriart, D., Lee, W. H., Claret, A., Sánchez-Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau-Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit-Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. -F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares-Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. -B., Hui, C. M., Jenke, P., Wilson-Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., von Kienlin, A., Kippen, R. M., McBreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. -F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., de Palma, F., Desiante, R., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., McEnery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., E., F. Olivares, Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W., Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., DePoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. de U., Thoene, C. C., Cano, Z., and Rosswog, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864
Published: 2016
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29. Supervised feature selection techniques in network intrusion detection: A critical review

Author: Di Mauro, M., Galatro, G., Fortino, G., and Liotta, A.
Published: 2021
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30. Smart anomaly detection in sensor systems: A multi-perspective review

Author: Erhan, L., Ndubuaku, M., Di Mauro, M., Song, W., Chen, M., Fortino, G., Bagdasar, O., and Liotta, A.
Published: 2021
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31. Internal rotation of the red-giant star KIC 4448777 by means of asteroseismic inversion

Author: Di Mauro, M . P., Ventura, R., Cardini, D., Stello, D., Christensen-Dalsgaard, J., Dziembowski, W. A., Paterno', L., Beck, P. G., Bloemen, S., Davies, G. R., De Smedt, K., Elsworth, Y., Garcia, R. A., Hekker, S., Mosser, B., and Tkachenko, A.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: In this paper we study the dynamics of the stellar interior of the early red-giant star KIC 4448777 by asteroseismic inversion of 14 splittings of the dipole mixed modes obtained from {\it Kepler} observations. In order to overcome the complexity of the oscillation pattern typical of red-giant stars, we present a procedure which involves a combination of different methods to extract the rotational splittings from the power spectrum. We find not only that the core rotates faster than the surface, confirming previous inversion results generated for other red giants (Deheuvels et al. 2012,2014), but we also estimate the variation of the angular velocity within the helium core with a spatial resolution of $\Delta r=0.001R$ and verify the hypothesis of a sharp discontinuity in the inner stellar rotation (Deheuvels et al. 2014). The results show that the entire core rotates rigidly with an angular velocity of about $\langle\Omega_c/2\pi\rangle=748\pm18$~nHz and provide evidence for an angular velocity decrease through a region between the helium core and part of the hydrogen burning shell; however we do not succeed to characterize the rotational slope, due to the intrinsic limits of the applied techniques. The angular velocity, from the edge of the core and through the hydrogen burning shell, appears to decrease with increasing distance from the center, reaching an average value in the convective envelope of $\langle\Omega_s/2\pi\rangle=68\pm22$~nHz. Hence, the core in KIC~4448777 is rotating from a minimum of 8 to a maximum of 17 times faster than the envelope. We conclude that a set of data which includes only dipolar modes is sufficient to infer quite accurately the rotation of a red giant not only in the dense core but also, with a lower level of confidence, in part of the radiative region and in the convective envelope., Comment: accepted for publication on ApJ
Published: 2015
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32. Oscillating red giants observed during Campaign 1 of the Kepler K2 mission: New prospects for galactic archaeology

Author: Stello, D., Huber, D., Sharma, S., Johnson, J., Lund, M. N., Handberg, R., Buzasi, D. L., Aguirre, V. Silva, Chaplin, W. J., Miglio, A., Pinsonneault, M., Basu, S., Bedding, T. R., Bland-Hawthorn, J., Casagrande, L., Davies, G., Elsworth, Y., Garcia, R. A., Mathur, S., Di Mauro, M. Pia, Mosser, B., Schneider, D. P., Serenelli, A., and Valentini, M.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: NASA's re-purposed Kepler mission -- dubbed K2 -- has brought new scientific opportunities that were not anticipated for the original Kepler mission. One science goal that makes optimal use of K2's capabilities, in particular its 360-degree ecliptic field of view, is galactic archaeology -- the study of the evolution of the Galaxy from the fossil stellar record. The thrust of this research is to exploit high-precision, time-resolved photometry from K2 in order to detect oscillations in red giant stars. This asteroseismic information can provide estimates of stellar radius (hence distance), mass and age of vast numbers of stars across the Galaxy. Here we present the initial analysis of a subset of red giants, observed towards the North Galactic Gap, during the mission's first full science campaign. We investigate the feasibility of using K2 data for detecting oscillations in red giants that span a range in apparent magnitude and evolutionary state (hence intrinsic luminosity). We demonstrate that oscillations are detectable for essentially all cool giants within the $\log g$ range $\sim 1.9-3.2$. Our detection is complete down to $\mathit{Kp}\sim 14.5$, which results in a seismic sample with little or no detection bias. This sample is ideally suited to stellar population studies that seek to investigate potential shortcomings of contemporary Galaxy models., Comment: 6 pages, 4 figures, submitted to ApJL
Published: 2015
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33. The GAPS Programme with HARPS-N at TNG. VII. Putting exoplanets in the stellar context: magnetic activity and asteroseismology of $\tau$ Bootis A

Author: Borsa, F., Scandariato, G., Rainer, M., Bignamini, A., Maggio, A., Poretti, E., Lanza, A. F., Di Mauro, M. P., Benatti, S., Biazzo, K., Bonomo, A. S., Damasso, M., Esposito, M., Gratton, R., Affer, L., Barbieri, M., Boccato, C., Claudi, R. U., Cosentino, R., Covino, E., Desidera, S., Fiorenzano, A. F. M., Gandolfi, D., Harutyunyan, A., Maldonado, J., Micela, G., Molaro, P., Molinari, E., Pagano, I., Pillitteri, I., Piotto, G., Shkolnik, E., Silvotti, R., Smareglia, R., Southworth, J., Sozzetti, A., and Stelzer, B.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Aims. We observed the $\tau$ Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the CaII H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of $0.9\pm0.5$ Gyr for $\tau$ Boo and further constrains the value of the stellar mass to $1.38\pm0.05$ M$_\odot$., Comment: 14 pages, accepted for publication in Astronomy and Astrophysics
Published: 2015
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34. Majorana and the theoretical problem of photon-electron scattering

Author: Di Mauro, M., Esposito, S., and Naddeo, A.
Subjects: Physics - History and Philosophy of Physics, Astrophysics - High Energy Astrophysical Phenomena, Condensed Matter - Strongly Correlated Electrons, High Energy Physics - Phenomenology, Quantum Physics
Abstract: Relevant contributions by Majorana regarding Compton scattering off free or bound electrons are considered in detail, where a (full quantum) generalization of the Kramers-Heisenberg dispersion formula is derived. The role of intermediate electronic states is appropriately pointed out in recovering the standard Klein-Nishina formula (for free electron scattering) by making recourse to a limpid physical scheme alternative to the (then unknown) Feynman diagram approach. For bound electron scattering, a quantitative description of the broadening of the Compton line was obtained for the first time by introducing a finite mean life for the excited state of the electron system. Finally, a generalization aimed to describe Compton scattering assisted by a non-vanishing applied magnetic field is as well considered, revealing its relevance for present day research., Comment: latex, amsart, 10 pages, 1 figure
Published: 2015

35. Renal Involvement in COVID-19: A Review of the Literature

Author: Migliaccio MG, Di Mauro M, Ricciolino R, Spiniello G, Carfora V, Verde N, Mottola FF, and Coppola N
Subjects: kidney injury, acute kidney injury, covid-19, sars-cov-2, Infectious and parasitic diseases, RC109-216
Abstract: Marco Giuseppe Migliaccio,1,* Marco Di Mauro,1,* Riccardo Ricciolino,1 Giorgio Spiniello,1 Vincenzo Carfora,1 Nicoletta Verde,1 Filiberto Fausto Mottola,1 Nicola Coppola2 On behalf of the Vanvitelli COVID-19 Group1Department of Translational Medical Sciences, University of Campania “Luigi Vanvitelli”, Naples, Italy; 2Department of Mental Health and Public Medicine, Infectious Diseases Unit, University of Campania “Luigi Vanvitelli”, Naples, Italy*These authors contributed equally to this workCorrespondence: Nicola CoppolaDepartment of Mental Health and Public Medicine, Infectious Diseases Unit, University of Campania “Luigi Vanvitelli”, Via: L. Armanni 5, Naples, 80131, ItalyTel +39 081 5666719Fax +39 081 5666013Email nicola.coppola@unicampania.itAbstract: Kidney injury may be a severe complication of acute respiratory syndrome coronavirus 2 (SARS-CoV-2) and contributes to worsen the prognosis. Various pathophysiological mechanisms can contribute to organ damage and impair renal function, proving the complexity of the virus activity and the resulting immunity response. We summarized the evidence of the literature on the prevalence of kidney involvement, on the pathogenic pathways and on its management.Keywords: kidney injury, acute kidney injury, COVID-19, SARS-CoV-2
Published: 2021

36. Diffuse gamma-ray emission from galactic pulsars

Author: Calore, F., Di Mauro, M., and Donato, F.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Millisecond Pulsars are second most abundant source population discovered by the Fermi-LAT. They might contribute non-negligibly to the diffuse emission measured at high latitudes by Fermi-LAT, the IDGRB. Gamma-ray sources also contribute to the anisotropy of the IDGRB measured on small scales by Fermi-LAT. We aim to assess the contribution of the unresolved counterpart of the detected MSPs population to the IDGRB and the maximal fraction of the measured anisotropy produced by this source class. We model the MSPs spatial distribution in the Galaxy and the gamma-ray emission parameters by considering radio and gamma-ray observational constraints. By simulating a large number of MSPs populations, we compute the average diffuse emission and the anisotropy 1-sigma upper limit. The emission from unresolved MSPs at 2 GeV, where the peak of the spectrum is located, is at most 0.9% of the measured IDGRB above 10 degrees in latitude. The 1-sigma upper limit on the angular power for unresolved MSP sources turns out to be about a factor of 60 smaller than Fermi-LAT measurements above 30 degrees. Our results indicate that this galactic source class represents a negligible contributor to the high-latitude gamma-ray sky and confirm that most of the intensity and geometrical properties of the measured diffuse emission are imputable to other extragalactic source classes. Nevertheless, given the MSP distribution, we expect them to contribute significantly to the gamma-ray diffuse emission at low latitudes. Since, along the galactic disk, the population of young Pulsars overcomes in number the one of MSPs, we compute the gamma-ray emission from the whole population of unresolved Pulsars in two low-latitude regions: the inner Galaxy and the galactic center., Comment: 19 pages, 26 figures. It matches the published version, minor changes only
Published: 2014
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37. Properties of 42 Solar-type Kepler Targets from the Asteroseismic Modeling Portal

Author: Metcalfe, T. S., Creevey, O. L., Dogan, G., Mathur, S., Xu, H., Bedding, T. R., Chaplin, W. J., Christensen-Dalsgaard, J., Karoff, C., Trampedach, R., Benomar, O., Brown, B. P., Buzasi, D. L., Campante, T. L., Celik, Z., Cunha, M. S., Davies, G. R., Deheuvels, S., Derekas, A., Di Mauro, M. P., Garcia, R. A., Guzik, J. A., Howe, R., MacGregor, K. B., Mazumdar, A., Montalban, J., Monteiro, M. J. P. F. G., Salabert, D., Serenelli, A., Stello, D., Steslicki, M., Suran, M. D., Yildiz, M., Aksoy, C., Elsworth, Y., Gruberbauer, M., Guenther, D. B., Lebreton, Y., Molaverdikhani, K., Pricopi, D., Simoniello, R., and White, T. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a decade ago, the Kepler mission has produced suitable observations for hundreds of new targets. This rapid expansion in observational capacity has been accompanied by a shift in analysis and modeling strategies to yield uniform sets of derived stellar properties more quickly and easily. We use previously published asteroseismic and spectroscopic data sets to provide a uniform analysis of 42 solar-type Kepler targets from the Asteroseismic Modeling Portal (AMP). We find that fitting the individual frequencies typically doubles the precision of the asteroseismic radius, mass and age compared to grid-based modeling of the global oscillation properties, and improves the precision of the radius and mass by about a factor of three over empirical scaling relations. We demonstrate the utility of the derived properties with several applications., Comment: 12 emulateapj pages, 9 figures, 1 online-only extended figure, 1 table, ApJS accepted (typo corrected in Eq.8)
Published: 2014
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38. Gamma-ray anisotropies from dark matter in the Milky Way: the role of the radial distribution

Author: Calore, F., De Romeri, V., Di Mauro, M., Donato, F., Herpich, J., Maccio', A. V., and Maccione, L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology
Abstract: The annihilation of dark matter particles in the halo of galaxies may end up into gamma rays, which travel almost unperturbed till to their detection at Earth. This annihilation signal can exhibit an anisotropic behavior quantified by the angular power spectrum, whose properties strongly depend on the dark matter distribution and its clumpiness. We use high resolution pure dark matter N-body simulations to quantify the contribution of different components (main halo and satellites) to the global signal as a function of the analytical profile adopted to describe the numerical results. We find that the smooth main halo dominates the angular power spectrum of the gamma-ray signal up to quite large multipoles, where the sub-haloes anisotropy signal starts to emerge, but the transition multipole strongly depends on the assumed radial profile. The extrapolation down to radii not resolved by current numerical simulations can affect both the normalization and the shape of the gamma-ray angular power spectrum. For the sub-haloes described by an asymptotically cored dark matter distribution, the angular power spectrum shows an overall smaller normalization and a flattening at high multipoles. Our results show the criticality of the dark matter density profile shape in gamma-ray anisotropy searches, and evaluate quantitatively the intrinsic errors occurring when extrapolating the dark matter radial profiles down to spatial scales not yet explored by numerical simulations., Comment: 7 pages, 8 figures. It matches the version published in MNRAS
Published: 2014
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39. Interpretation of AMS-02 electrons and positrons data

Author: Di Mauro, M., Donato, F., Fornengo, N., Lineros, R., and Vittino, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology
Abstract: We perform a combined analysis of the recent AMS-02 data on electrons, positrons, electrons plus positrons and positron fraction, in a self-consistent framework where we realize a theoretical modeling of all the astrophysical components that can contribute to the observed fluxes in the whole energy range. The primary electron contribution is modeled through the sum of an average flux from distant sources and the fluxes from the local supernova remnants in the Green catalog. The secondary electron and positron fluxes originate from interactions on the interstellar medium of primary cosmic rays, for which we derive a novel determination by using AMS-02 proton and helium data. Primary positrons and electrons from pulsar wind nebulae in the ATNF catalog are included and studied in terms of their most significant (while loosely known) properties and under different assumptions (average contribution from the whole catalog, single dominant pulsar, a few dominant pulsars). We obtain a remarkable agreement between our various modeling and the AMS-02 data for all types of analysis, demonstrating that the whole AMS-02 leptonic data admit a self-consistent interpretation in terms of astrophysical contributions., Comment: 33 pages, 26 figures and 4 tables, v2: accepted for publication in JCAP, minor changes relative to v1
Published: 2014
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40. Inferring mode inertias in evolved solar-like stars

Author: Benomar, O., Belkacem, K., Bedding, T. R., Stello, D., Di Mauro, M. P., Ventura, R., Mosser, B., Goupil, M. J., Samadi, R., and Garcia, R. A.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Asteroseismology of evolved solar-like stars is experiencing a growing interest due to the wealth of observational data from space-borne instruments such as the \emph{CoRoT} and \emph{Kepler} spacecraft. In particular, the recent detection of mixed modes, which probe both the innermost and uppermost layers of stars, paves the way for inferring the internal structure of stars along their evolution through the subgiant and red giant phases. Mixed modes can also place stringent constraints on the physics of such stars and on their global properties (mass, age, etc...). Here, using two \emph{Kepler} stars (KIC 4351319 and KIC 6442183), we demonstrate that measurements of mixed mode characteristics allow us to estimate the mode inertias, providing a new and additional diagnostics on the mode trapping and subsequently on the internal structure of evolved stars. We however stress that the accuracy may be sensitive to non-adiabatic effects., Comment: ApJ Letter
Published: 2014
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41. Bouncing Balls and Geometric Progressions

Author: De Luca, R., Di Mauro, M., and Naddeo, A.
Abstract: Observing the bouncing of a marble on a table is a rather common experience. The tic-tac sound of the rigid ball, nevertheless, carries quite a pleasant surprise. In fact, by measuring the total time of bouncing [delta]t, the coefficient of restitution can be estimated. As is well known, in an inelastic collision the kinetic energy is not conserved, and therefore the speed decreases. The speeds v[subscript i] and v[subscript f], before and after the collision occurs, respectively, are related as follows:[nu][subscript f]=[epsilon][nu][subscript i], (1) where [epsilon] < 1. By measuring the initial height h[subscript 0] from which the marble is released, we find that [equation omitted], (2) where g is the acceleration due to gravity and T is the total time from initial release until the ball stops bouncing.
Published: 2020
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42. In-hospital and 6-month outcomes in patients with COVID-19 supported with extracorporeal membrane oxygenation (EuroECMO-COVID): a multicentre, prospective observational study

Author: Lorusso, R, De Piero, M, Mariani, S, Di Mauro, M, Folliguet, T, Taccone, F, Camporota, L, Swol, J, Wiedemann, D, Belliato, M, Broman, L, Vuylsteke, A, Kassif, Y, Scandroglio, A, Fanelli, V, Gaudard, P, Ledot, S, Barker, J, Boeken, U, Maier, S, Kersten, A, Meyns, B, Pozzi, M, Pedersen, F, Schellongowski, P, Kirali, K, Barrett, N, Riera, J, Mueller, T, Belohlavek, J, Lo Coco, V, Van der Horst, I, Van Bussel, B, Schnabel, R, Delnoij, T, Bolotin, G, Lorini, L, Schmiady, M, Schibilsky, D, Kowalewski, M, Pinto, L, Silva, P, Kornilov, I, Blandino Ortiz, A, Vercaemst, L, Finney, S, Roeleveld, P, Di Nardo, M, Hennig, F, Antonini, M, Davidson, M, Jones, T, Staudinger, T, Mair, P, Kilo, J, Krapf, C, Erbert, K, Peer, A, Bonaros, N, Kotheletner, F, Krenner Mag, N, Shestakova, L, Hermans, G, Dauwe, D, Meersseman, P, Stockman, B, Nobile, L, Lhereux, O, Nrasseurs, A, Creuter, J, De Backer, D, Giglioli, S, Michiels, G, Foulon, P, Raes, M, Rodrigus, I, Allegaert, M, Jorens, P, Debeucklare, G, Piagnerelli, M, Biston, P, Peperstraete, H, Vandewiele, K, Germay, O, Vandeweghe, D, Havrin, S, Bourgeois, M, Lagny, M, Alois, G, Lavios, N, Misset, B, Courcelle, R, Timmermans, P, Yilmaz, A, Vantomout, M, Lehaen, J, Jassen, A, Guterman, H, Strauven, M, Lormans, P, Verhamme, B, Vandewaeter, C, Bonte, F, Vionne, D, Balik, M, Blaha, J, Lips, M, Othal, M, Bursa, F, Spacek, R, Christensen, S, Jorgensen, V, Sorensen, M, Madsen, S, Puss, S, Beljantsev, A, Saiydoun, G, Fiore, A, Colson, P, Bazalgette, F, Capdevila, X, Kollen, S, Muller, L, Obadia, J, Dubien, P, Ajrhourh, L, Guinot, P, Zarka, J, Besserve, P, Malfertheiner, M, Dreier, E, Heinze, B, Akhyari, P, Lichtenberg, A, Aubin, H, Assman, A, Saeed, D, Thiele, H, Baumgaertel, M, Schmitto, J, Ruslan, N, Haverich, A, Thielmann, M, Brenner, T, Ruhpawar, A, Benk, C, Czerny, M, Staudacher, D, Beyersdorf, F, Kalbhenn, J, Henn, P, Popov, A, Iuliu, T, Muellenbach, R, Reyher, C, Rolfes, C, Lotz, G, Sonntagbauer, M, Winkels, H, Fichte, J, Stohr, R, Kalverkamp, S, Karagiannidis, C, Schafer, S, Svetlitchny, A, Hopf, H, Jarczak, D, Groesdonk, H, Rommer, M, Hirsch, J, Kaehny, C, Soufleris, D, Gavriilidis, G, Pontikis, K, Kyriakopoulou, M, Kyriakoudi, A, O'Brien, S, Conrick-Martin, I, Carton, E, Makhoul, M, Ben-Ari, J, Hadash, A, Kogan, A, Kassif Lerner, R, Abu-Shakra, A, Matan, M, Balawona, A, Kachel, E, Altshuler, R, Galante, O, Fuchs, L, Almog, Y, Ishay, Y, Lichter, Y, Gal-oz, A, Carmi, U, Nini, A, Soroksky, A, Dekel, H, Rozman, Z, Tayem, E, Ilgiyaev, E, Hochman, Y, Miltau, D, Rapoport, A, Eden, A, Kompanietz, D, Yousif, M, Golos, M, Grazioli, L, Ghitti, D, Loforte, A, Di Luca, D, Baiocchi, M, Pacini, D, Cappai, A, Meani, P, Mondino, M, Russo, C, Ranucci, M, Fina, D, Cotza, M, Ballotta, A, Landoni, G, Nardelli, P, Fominski, E, Brazzi, L, Montrucchio, G, Sales, G, Simonetti, U, Livigni, S, Silengo, D, Arena, G, Sovatzis, S, Degani, A, Riccardi, M, Milanesi, E, Raffa, G, Martucci, G, Arcadipane, A, Panarello, G, Chiarini, G, Cattaneo, S, Puglia, C, Benussi, S, Foti, G, Giani, M, Bombino, M, Costa, M, Rona, R, Avalli, L, Donati, A, Carozza, R, Gasparri, F, Carsetti, A, Piciche, M, Marinello, A, Danzi, V, Zanin, A, Condello, I, Fiore, F, Moscarelli, M, Nasso, G, Speziale, G, Sandrelli, L, Montalto, A, Musumeci, F, Circelli, A, Russo, E, Agnoletti, V, Rociola, R, Milano, A, Pilato, E, Comentale, G, Montisci, A, Alessandri, F, Tosi, A, Pugliese, F, Giordano, G, Carelli, S, Grieco, D, Dell'Anna, A, Antonelli, M, Ramoni, E, Zulueta, J, Del Giglio, M, Petracca, S, Bertini, P, Guarracino, F, De Simone, L, Angeletti, P, Forfori, F, Taraschi, F, Quintiliani, V, Samalavicius, R, Jankuviene, A, Scupakova, N, Urbonas, K, Kapturauskas, J, Soerensen, G, Suwalski, P, Linhares Santos, L, Marques, A, Miranda, M, Teixeira, S, Salgueiro, A, Pereira, F, Ketskalo, M, Tsarenko, S, Shilova, A, Afukov, I, Popugaev, K, Minin, S, Shelukhin, D, Malceva, O, Gleb, M, Skopets, A, Kornelyuk, R, Kulikov, A, Okhrimchuk, V, Turchaninov, A, Petrushin, M, Sheck, A, Mekulov, A, Ciryateva, S, Urusov, D, Gorjup, V, Golicnik, A, Goslar, T, Ferrer, R, Martinez-Martinez, M, Argudo, E, Palmer, N, De Pablo Sanchez, R, Juan Higuera, L, Arnau Blasco, L, Marquez, J, Sbraga, F, Fuset, M, De Gopegui, P, Claraco, L, De Ayala, J, Peiro, M, Ricart, P, Martinez, S, Chavez, F, Fabra, M, Sandoval, E, Toapanta, D, Carraminana, A, Tellez, A, Ososio, J, Milan, P, Rodriguez, J, Andoni, G, Gutierrez, C, Perez de la Sota, E, Eixeres-Esteve, A, Garcia-Maellas, M, Gutierrez-Gutierrez, J, Arboleda-Salazar, R, Santa Teresa, P, Jaspe, A, Garrido, A, Castaneda, G, Alcantara, S, Martinez, N, Perez, M, Villanueva, H, Vidal Gonzalez, A, Paez, J, Santon, A, Perez, C, Lopez, M, Rubio Lopez, M, Gordillo, A, Naranjo-Izurieta, J, Munoz, J, Alcalde, I, Onieva, F, Gimeno Costa, R, Perez, F, Madrid, I, Gordon, M, Albacete Moreno, C, Perez, D, Lopez, N, Martinenz, D, Blanco-Schweizer, P, Diez, C, Prieto, A, Renedo, G, Bustamante, E, Cicuendez, R, Citores, R, Boado, V, Garcia, K, Voces, R, Domezain, M, Nunez Martinez, J, Vicente, R, Martin, D, Andreu, A, Gomez Casal, V, Chico, I, Menor, E, Vara, S, Gamacho, J, Perez-Chomon, H, Javier Gonzales, F, Barrero, I, Martin-Villen, L, Fernandez, E, Mendoza, M, Navarro, J, Colomina Climent, J, Gonzales-Perez, A, Muniz-Albaceita, G, Amado, L, Rodriguez, R, Ruiz, E, Eiras, M, Grins, E, Magnus, R, Kanetoft, M, Eidevald, M, Watson, P, Vogt, P, Steiger, P, Aigner, T, Weber, A, Grunefelder, J, Kunz, M, Grapow, M, Aymard, T, Reser, D, Agus, G, Consiglio, J, Haenggi, M, Hansjoerg, J, Iten, M, Doeble, T, Zenklusen, U, Bechtold, X, Faedda, G, Iafrate, M, Rohjer, A, Bergamaschi, L, Maessen, J, Reis Miranda, D, Endeman, H, Gommers, D, Meuwese, C, Maas, J, Van Gijlswijk, M, Van Berg, R, Candura, D, Van der Linden, M, Kant, M, Van der Heijden, J, Scholten, E, Van Belle-van Haren, N, Lagrand, W, Vlaar, A, De Jong, S, Cander, B, Sargin, M, Ugur, M, Kaygin, M, Daly, K, Agnew, N, Head, L, Kelly, L, Anoma, G, Russell, C, Aquino, V, Scott, I, Flemming, L, Gillon, S, Moore, O, Gelandt, E, Auzinger, G, Patel, S, Loveridge, R, Lorusso R., De Piero M. E., Mariani S., Di Mauro M., Folliguet T., Taccone F. S., Camporota L., Swol J., Wiedemann D., Belliato M., Broman L. M., Vuylsteke A., Kassif Y., Scandroglio A. M., Fanelli V., Gaudard P., Ledot S., Barker J., Boeken U., Maier S., Kersten A., Meyns B., Pozzi M., Pedersen F. M., Schellongowski P., Kirali K., Barrett N., Riera J., Mueller T., Belohlavek J., Lo Coco V., Van der Horst I. C. C., Van Bussel B. C. T., Schnabel R. M., Delnoij T., Bolotin G., Lorini L., Schmiady M. O., Schibilsky D., Kowalewski M., Pinto L. F., Silva P. E., Kornilov I., Blandino Ortiz A., Vercaemst L., Finney S., Roeleveld P. P., Di Nardo M., Hennig F., Antonini M. V., Davidson M., Jones T. J., Staudinger T., Mair P., Kilo J., Krapf C., Erbert K., Peer A., Bonaros N., Kotheletner F., Krenner Mag N., Shestakova L., Hermans G., Dauwe D., Meersseman P., Stockman B., Nobile L., Lhereux O., Nrasseurs A., Creuter J., De Backer D., Giglioli S., Michiels G., Foulon P., Raes M., Rodrigus I., Allegaert M., Jorens P., Debeucklare G., Piagnerelli M., Biston P., Peperstraete H., Vandewiele K., Germay O., Vandeweghe D., Havrin S., Bourgeois M., Lagny M. -G., Alois G., Lavios N., Misset B., Courcelle R., Timmermans P. J., Yilmaz A., Vantomout M., Lehaen J., Jassen A., Guterman H., Strauven M., Lormans P., Verhamme B., Vandewaeter C., Bonte F., Vionne D., Balik M., Blaha J., Lips M., Othal M., Bursa F., Spacek R., Christensen S., Jorgensen V., Sorensen M., Madsen S. A., Puss S., Beljantsev A., Saiydoun G., Fiore A., Colson P., Bazalgette F., Capdevila X., Kollen S., Muller L., Obadia J. -F., Dubien P. -Y., Ajrhourh L., Guinot P. G., Zarka J., Besserve P., Malfertheiner M. V., Dreier E., Heinze B., Akhyari P., Lichtenberg A., Aubin H., Assman A., Saeed D., Thiele H., Baumgaertel M., Schmitto J. D., Ruslan N., Haverich A., Thielmann M., Brenner T., Ruhpawar A., Benk C., Czerny M., Staudacher D. L., Beyersdorf F., Kalbhenn J., Henn P., Popov A. -F., Iuliu T., Muellenbach R., Reyher C., Rolfes C., Lotz G., Sonntagbauer M., Winkels H., Fichte J., Stohr R., Kalverkamp S., Karagiannidis C., Schafer S., Svetlitchny A., Hopf H. -B., Jarczak D., Groesdonk H., Rommer M., Hirsch J., Kaehny C., Soufleris D., Gavriilidis G., Pontikis K., Kyriakopoulou M., Kyriakoudi A., O'Brien S., Conrick-Martin I., Carton E., Makhoul M., Ben-Ari J., Hadash A., Kogan A., Kassif Lerner R., Abu-Shakra A., Matan M., Balawona A., Kachel E., Altshuler R., Galante O., Fuchs L., Almog Y., Ishay Y. S., Lichter Y., Gal-oz A., Carmi U., Nini A., Soroksky A., Dekel H., Rozman Z., Tayem E., Ilgiyaev E., Hochman Y., Miltau D., Rapoport A., Eden A., Kompanietz D., Yousif M., Golos M., Grazioli L., Ghitti D., Loforte A., Di Luca D., Baiocchi M., Pacini D., Cappai A., Meani P., Mondino M., Russo C. F., Ranucci M., Fina D., Cotza M., Ballotta A., Landoni G., Nardelli P., Fominski E. V., Brazzi L., Montrucchio G., Sales G., Simonetti U., Livigni S., Silengo D., Arena G., Sovatzis S. S., Degani A., Riccardi M., Milanesi E., Raffa G., Martucci G., Arcadipane A., Panarello G., Chiarini G., Cattaneo S., Puglia C., Benussi S., Foti G., Giani M., Bombino M., Costa M. C., Rona R., Avalli L., Donati A., Carozza R., Gasparri F., Carsetti A., Piciche M., Marinello A., Danzi V., Zanin A., Condello I., Fiore F., Moscarelli M., Nasso G., Speziale G., Sandrelli L., Montalto A., Musumeci F., Circelli A., Russo E., Agnoletti V., Rociola R., Milano A. D., Pilato E., Comentale G., Montisci A., Alessandri F., Tosi A., Pugliese F., Giordano G., Carelli S., Grieco D. L., Dell'Anna A. M., Antonelli M., Ramoni E., Zulueta J., Del Giglio M., Petracca S., Bertini P., Guarracino F., De Simone L., Angeletti P. M., Forfori F., Taraschi F., Quintiliani V. N., Samalavicius R., Jankuviene A., Scupakova N., Urbonas K., Kapturauskas J., Soerensen G., Suwalski P., Linhares Santos L., Marques A., Miranda M., Teixeira S., Salgueiro A., Pereira F., Ketskalo M., Tsarenko S., Shilova A., Afukov I., Popugaev K., Minin S., Shelukhin D., Malceva O., Gleb M., Skopets A., Kornelyuk R., Kulikov A., Okhrimchuk V., Turchaninov A., Petrushin M., Sheck A., Mekulov A., Ciryateva S., Urusov D., Gorjup V., Golicnik A., Goslar T., Ferrer R., Martinez-Martinez M., Argudo E., Palmer N., De Pablo Sanchez R., Juan Higuera L., Arnau Blasco L., Marquez J. A., Sbraga F., Fuset M. P., De Gopegui P. R., Claraco L. M., De Ayala J. A., Peiro M., Ricart P., Martinez S., Chavez F., Fabra M., Sandoval E., Toapanta D., Carraminana A., Tellez A., Ososio J., Milan P., Rodriguez J., Andoni G., Gutierrez C., Perez de la Sota E., Eixeres-Esteve A., Garcia-Maellas M. T., Gutierrez-Gutierrez J., Arboleda-Salazar R., Santa Teresa P., Jaspe A., Garrido A., Castaneda G., Alcantara S., Martinez N., Perez M., Villanueva H., Vidal Gonzalez A., Paez J., Santon A., Perez C., Lopez M., Rubio Lopez M. I., Gordillo A., Naranjo-Izurieta J., Munoz J., Alcalde I., Onieva F., Gimeno Costa R., Perez F., Madrid I., Gordon M., Albacete Moreno C. L., Perez D., Lopez N., Martinenz D., Blanco-Schweizer P., Diez C., Prieto A., Renedo G., Bustamante E., Cicuendez R., Citores R., Boado V., Garcia K., Voces R., Domezain M., Nunez Martinez J. M., Vicente R., Martin D., Andreu A., Gomez Casal V., Chico I., Menor E. M., Vara S., Gamacho J., Perez-Chomon H., Javier Gonzales F., Barrero I., Martin-Villen L., Fernandez E., Mendoza M., Navarro J., Colomina Climent J., Gonzales-Perez A., Muniz-Albaceita G., Amado L., Rodriguez R., Ruiz E., Eiras M., Grins E., Magnus R., Kanetoft M., Eidevald M., Watson P., Vogt P. R., Steiger P., Aigner T., Weber A., Grunefelder J., Kunz M., Grapow M., Aymard T., Reser D., Agus G., Consiglio J., Haenggi M., Hansjoerg J., Iten M., Doeble T., Zenklusen U., Bechtold X., Faedda G., Iafrate M., Rohjer A., Bergamaschi L., Maessen J., Reis Miranda D., Endeman H., Gommers D., Meuwese C., Maas J., Van Gijlswijk M. J., Van Berg R. N., Candura D., Van der Linden M., Kant M., Van der Heijden J. J., Scholten E., Van Belle-van Haren N., Lagrand W. K., Vlaar A. P., De Jong S., Cander B., Sargin M., Ugur M., Kaygin M. A., Daly K., Agnew N., Head L., Kelly L., Anoma G., Russell C., Aquino V., Scott I., Flemming L., Gillon S., Moore O., Gelandt E., Auzinger G., Patel S., Loveridge R., Lorusso, R, De Piero, M, Mariani, S, Di Mauro, M, Folliguet, T, Taccone, F, Camporota, L, Swol, J, Wiedemann, D, Belliato, M, Broman, L, Vuylsteke, A, Kassif, Y, Scandroglio, A, Fanelli, V, Gaudard, P, Ledot, S, Barker, J, Boeken, U, Maier, S, Kersten, A, Meyns, B, Pozzi, M, Pedersen, F, Schellongowski, P, Kirali, K, Barrett, N, Riera, J, Mueller, T, Belohlavek, J, Lo Coco, V, Van der Horst, I, Van Bussel, B, Schnabel, R, Delnoij, T, Bolotin, G, Lorini, L, Schmiady, M, Schibilsky, D, Kowalewski, M, Pinto, L, Silva, P, Kornilov, I, Blandino Ortiz, A, Vercaemst, L, Finney, S, Roeleveld, P, Di Nardo, M, Hennig, F, Antonini, M, Davidson, M, Jones, T, Staudinger, T, Mair, P, Kilo, J, Krapf, C, Erbert, K, Peer, A, Bonaros, N, Kotheletner, F, Krenner Mag, N, Shestakova, L, Hermans, G, Dauwe, D, Meersseman, P, Stockman, B, Nobile, L, Lhereux, O, Nrasseurs, A, Creuter, J, De Backer, D, Giglioli, S, Michiels, G, Foulon, P, Raes, M, Rodrigus, I, Allegaert, M, Jorens, P, Debeucklare, G, Piagnerelli, M, Biston, P, Peperstraete, H, Vandewiele, K, Germay, O, Vandeweghe, D, Havrin, S, Bourgeois, M, Lagny, M, Alois, G, Lavios, N, Misset, B, Courcelle, R, Timmermans, P, Yilmaz, A, Vantomout, M, Lehaen, J, Jassen, A, Guterman, H, Strauven, M, Lormans, P, Verhamme, B, Vandewaeter, C, Bonte, F, Vionne, D, Balik, M, Blaha, J, Lips, M, Othal, M, Bursa, F, Spacek, R, Christensen, S, Jorgensen, V, Sorensen, M, Madsen, S, Puss, S, Beljantsev, A, Saiydoun, G, Fiore, A, Colson, P, Bazalgette, F, Capdevila, X, Kollen, S, Muller, L, Obadia, J, Dubien, P, Ajrhourh, L, Guinot, P, Zarka, J, Besserve, P, Malfertheiner, M, Dreier, E, Heinze, B, Akhyari, P, Lichtenberg, A, Aubin, H, Assman, A, Saeed, D, Thiele, H, Baumgaertel, M, Schmitto, J, Ruslan, N, Haverich, A, Thielmann, M, Brenner, T, Ruhpawar, A, Benk, C, Czerny, M, Staudacher, D, Beyersdorf, F, Kalbhenn, J, Henn, P, Popov, A, Iuliu, T, Muellenbach, R, Reyher, C, Rolfes, C, Lotz, G, Sonntagbauer, M, Winkels, H, Fichte, J, Stohr, R, Kalverkamp, S, Karagiannidis, C, Schafer, S, Svetlitchny, A, Hopf, H, Jarczak, D, Groesdonk, H, Rommer, M, Hirsch, J, Kaehny, C, Soufleris, D, Gavriilidis, G, Pontikis, K, Kyriakopoulou, M, Kyriakoudi, A, O'Brien, S, Conrick-Martin, I, Carton, E, Makhoul, M, Ben-Ari, J, Hadash, A, Kogan, A, Kassif Lerner, R, Abu-Shakra, A, Matan, M, Balawona, A, Kachel, E, Altshuler, R, Galante, O, Fuchs, L, Almog, Y, Ishay, Y, Lichter, Y, Gal-oz, A, Carmi, U, Nini, A, Soroksky, A, Dekel, H, Rozman, Z, Tayem, E, Ilgiyaev, E, Hochman, Y, Miltau, D, Rapoport, A, Eden, A, Kompanietz, D, Yousif, M, Golos, M, Grazioli, L, Ghitti, D, Loforte, A, Di Luca, D, Baiocchi, M, Pacini, D, Cappai, A, Meani, P, Mondino, M, Russo, C, Ranucci, M, Fina, D, Cotza, M, Ballotta, A, Landoni, G, Nardelli, P, Fominski, E, Brazzi, L, Montrucchio, G, Sales, G, Simonetti, U, Livigni, S, Silengo, D, Arena, G, Sovatzis, S, Degani, A, Riccardi, M, Milanesi, E, Raffa, G, Martucci, G, Arcadipane, A, Panarello, G, Chiarini, G, Cattaneo, S, Puglia, C, Benussi, S, Foti, G, Giani, M, Bombino, M, Costa, M, Rona, R, Avalli, L, Donati, A, Carozza, R, Gasparri, F, Carsetti, A, Piciche, M, Marinello, A, Danzi, V, Zanin, A, Condello, I, Fiore, F, Moscarelli, M, Nasso, G, Speziale, G, Sandrelli, L, Montalto, A, Musumeci, F, Circelli, A, Russo, E, Agnoletti, V, Rociola, R, Milano, A, Pilato, E, Comentale, G, Montisci, A, Alessandri, F, Tosi, A, Pugliese, F, Giordano, G, Carelli, S, Grieco, D, Dell'Anna, A, Antonelli, M, Ramoni, E, Zulueta, J, Del Giglio, M, Petracca, S, Bertini, P, Guarracino, F, De Simone, L, Angeletti, P, Forfori, F, Taraschi, F, Quintiliani, V, Samalavicius, R, Jankuviene, A, Scupakova, N, Urbonas, K, Kapturauskas, J, Soerensen, G, Suwalski, P, Linhares Santos, L, Marques, A, Miranda, M, Teixeira, S, Salgueiro, A, Pereira, F, Ketskalo, M, Tsarenko, S, Shilova, A, Afukov, I, Popugaev, K, Minin, S, Shelukhin, D, Malceva, O, Gleb, M, Skopets, A, Kornelyuk, R, Kulikov, A, Okhrimchuk, V, Turchaninov, A, Petrushin, M, Sheck, A, Mekulov, A, Ciryateva, S, Urusov, D, Gorjup, V, Golicnik, A, Goslar, T, Ferrer, R, Martinez-Martinez, M, Argudo, E, Palmer, N, De Pablo Sanchez, R, Juan Higuera, L, Arnau Blasco, L, Marquez, J, Sbraga, F, Fuset, M, De Gopegui, P, Claraco, L, De Ayala, J, Peiro, M, Ricart, P, Martinez, S, Chavez, F, Fabra, M, Sandoval, E, Toapanta, D, Carraminana, A, Tellez, A, Ososio, J, Milan, P, Rodriguez, J, Andoni, G, Gutierrez, C, Perez de la Sota, E, Eixeres-Esteve, A, Garcia-Maellas, M, Gutierrez-Gutierrez, J, Arboleda-Salazar, R, Santa Teresa, P, Jaspe, A, Garrido, A, Castaneda, G, Alcantara, S, Martinez, N, Perez, M, Villanueva, H, Vidal Gonzalez, A, Paez, J, Santon, A, Perez, C, Lopez, M, Rubio Lopez, M, Gordillo, A, Naranjo-Izurieta, J, Munoz, J, Alcalde, I, Onieva, F, Gimeno Costa, R, Perez, F, Madrid, I, Gordon, M, Albacete Moreno, C, Perez, D, Lopez, N, Martinenz, D, Blanco-Schweizer, P, Diez, C, Prieto, A, Renedo, G, Bustamante, E, Cicuendez, R, Citores, R, Boado, V, Garcia, K, Voces, R, Domezain, M, Nunez Martinez, J, Vicente, R, Martin, D, Andreu, A, Gomez Casal, V, Chico, I, Menor, E, Vara, S, Gamacho, J, Perez-Chomon, H, Javier Gonzales, F, Barrero, I, Martin-Villen, L, Fernandez, E, Mendoza, M, Navarro, J, Colomina Climent, J, Gonzales-Perez, A, Muniz-Albaceita, G, Amado, L, Rodriguez, R, Ruiz, E, Eiras, M, Grins, E, Magnus, R, Kanetoft, M, Eidevald, M, Watson, P, Vogt, P, Steiger, P, Aigner, T, Weber, A, Grunefelder, J, Kunz, M, Grapow, M, Aymard, T, Reser, D, Agus, G, Consiglio, J, Haenggi, M, Hansjoerg, J, Iten, M, Doeble, T, Zenklusen, U, Bechtold, X, Faedda, G, Iafrate, M, Rohjer, A, Bergamaschi, L, Maessen, J, Reis Miranda, D, Endeman, H, Gommers, D, Meuwese, C, Maas, J, Van Gijlswijk, M, Van Berg, R, Candura, D, Van der Linden, M, Kant, M, Van der Heijden, J, Scholten, E, Van Belle-van Haren, N, Lagrand, W, Vlaar, A, De Jong, S, Cander, B, Sargin, M, Ugur, M, Kaygin, M, Daly, K, Agnew, N, Head, L, Kelly, L, Anoma, G, Russell, C, Aquino, V, Scott, I, Flemming, L, Gillon, S, Moore, O, Gelandt, E, Auzinger, G, Patel, S, Loveridge, R, Lorusso R., De Piero M. E., Mariani S., Di Mauro M., Folliguet T., Taccone F. S., Camporota L., Swol J., Wiedemann D., Belliato M., Broman L. M., Vuylsteke A., Kassif Y., Scandroglio A. M., Fanelli V., Gaudard P., Ledot S., Barker J., Boeken U., Maier S., Kersten A., Meyns B., Pozzi M., Pedersen F. M., Schellongowski P., Kirali K., Barrett N., Riera J., Mueller T., Belohlavek J., Lo Coco V., Van der Horst I. C. C., Van Bussel B. C. T., Schnabel R. M., Delnoij T., Bolotin G., Lorini L., Schmiady M. O., Schibilsky D., Kowalewski M., Pinto L. F., Silva P. E., Kornilov I., Blandino Ortiz A., Vercaemst L., Finney S., Roeleveld P. P., Di Nardo M., Hennig F., Antonini M. V., Davidson M., Jones T. J., Staudinger T., Mair P., Kilo J., Krapf C., Erbert K., Peer A., Bonaros N., Kotheletner F., Krenner Mag N., Shestakova L., Hermans G., Dauwe D., Meersseman P., Stockman B., Nobile L., Lhereux O., Nrasseurs A., Creuter J., De Backer D., Giglioli S., Michiels G., Foulon P., Raes M., Rodrigus I., Allegaert M., Jorens P., Debeucklare G., Piagnerelli M., Biston P., Peperstraete H., Vandewiele K., Germay O., Vandeweghe D., Havrin S., Bourgeois M., Lagny M. -G., Alois G., Lavios N., Misset B., Courcelle R., Timmermans P. J., Yilmaz A., Vantomout M., Lehaen J., Jassen A., Guterman H., Strauven M., Lormans P., Verhamme B., Vandewaeter C., Bonte F., Vionne D., Balik M., Blaha J., Lips M., Othal M., Bursa F., Spacek R., Christensen S., Jorgensen V., Sorensen M., Madsen S. A., Puss S., Beljantsev A., Saiydoun G., Fiore A., Colson P., Bazalgette F., Capdevila X., Kollen S., Muller L., Obadia J. -F., Dubien P. -Y., Ajrhourh L., Guinot P. G., Zarka J., Besserve P., Malfertheiner M. V., Dreier E., Heinze B., Akhyari P., Lichtenberg A., Aubin H., Assman A., Saeed D., Thiele H., Baumgaertel M., Schmitto J. D., Ruslan N., Haverich A., Thielmann M., Brenner T., Ruhpawar A., Benk C., Czerny M., Staudacher D. L., Beyersdorf F., Kalbhenn J., Henn P., Popov A. -F., Iuliu T., Muellenbach R., Reyher C., Rolfes C., Lotz G., Sonntagbauer M., Winkels H., Fichte J., Stohr R., Kalverkamp S., Karagiannidis C., Schafer S., Svetlitchny A., Hopf H. -B., Jarczak D., Groesdonk H., Rommer M., Hirsch J., Kaehny C., Soufleris D., Gavriilidis G., Pontikis K., Kyriakopoulou M., Kyriakoudi A., O'Brien S., Conrick-Martin I., Carton E., Makhoul M., Ben-Ari J., Hadash A., Kogan A., Kassif Lerner R., Abu-Shakra A., Matan M., Balawona A., Kachel E., Altshuler R., Galante O., Fuchs L., Almog Y., Ishay Y. S., Lichter Y., Gal-oz A., Carmi U., Nini A., Soroksky A., Dekel H., Rozman Z., Tayem E., Ilgiyaev E., Hochman Y., Miltau D., Rapoport A., Eden A., Kompanietz D., Yousif M., Golos M., Grazioli L., Ghitti D., Loforte A., Di Luca D., Baiocchi M., Pacini D., Cappai A., Meani P., Mondino M., Russo C. F., Ranucci M., Fina D., Cotza M., Ballotta A., Landoni G., Nardelli P., Fominski E. V., Brazzi L., Montrucchio G., Sales G., Simonetti U., Livigni S., Silengo D., Arena G., Sovatzis S. S., Degani A., Riccardi M., Milanesi E., Raffa G., Martucci G., Arcadipane A., Panarello G., Chiarini G., Cattaneo S., Puglia C., Benussi S., Foti G., Giani M., Bombino M., Costa M. C., Rona R., Avalli L., Donati A., Carozza R., Gasparri F., Carsetti A., Piciche M., Marinello A., Danzi V., Zanin A., Condello I., Fiore F., Moscarelli M., Nasso G., Speziale G., Sandrelli L., Montalto A., Musumeci F., Circelli A., Russo E., Agnoletti V., Rociola R., Milano A. D., Pilato E., Comentale G., Montisci A., Alessandri F., Tosi A., Pugliese F., Giordano G., Carelli S., Grieco D. L., Dell'Anna A. M., Antonelli M., Ramoni E., Zulueta J., Del Giglio M., Petracca S., Bertini P., Guarracino F., De Simone L., Angeletti P. M., Forfori F., Taraschi F., Quintiliani V. N., Samalavicius R., Jankuviene A., Scupakova N., Urbonas K., Kapturauskas J., Soerensen G., Suwalski P., Linhares Santos L., Marques A., Miranda M., Teixeira S., Salgueiro A., Pereira F., Ketskalo M., Tsarenko S., Shilova A., Afukov I., Popugaev K., Minin S., Shelukhin D., Malceva O., Gleb M., Skopets A., Kornelyuk R., Kulikov A., Okhrimchuk V., Turchaninov A., Petrushin M., Sheck A., Mekulov A., Ciryateva S., Urusov D., Gorjup V., Golicnik A., Goslar T., Ferrer R., Martinez-Martinez M., Argudo E., Palmer N., De Pablo Sanchez R., Juan Higuera L., Arnau Blasco L., Marquez J. A., Sbraga F., Fuset M. P., De Gopegui P. R., Claraco L. M., De Ayala J. A., Peiro M., Ricart P., Martinez S., Chavez F., Fabra M., Sandoval E., Toapanta D., Carraminana A., Tellez A., Ososio J., Milan P., Rodriguez J., Andoni G., Gutierrez C., Perez de la Sota E., Eixeres-Esteve A., Garcia-Maellas M. T., Gutierrez-Gutierrez J., Arboleda-Salazar R., Santa Teresa P., Jaspe A., Garrido A., Castaneda G., Alcantara S., Martinez N., Perez M., Villanueva H., Vidal Gonzalez A., Paez J., Santon A., Perez C., Lopez M., Rubio Lopez M. I., Gordillo A., Naranjo-Izurieta J., Munoz J., Alcalde I., Onieva F., Gimeno Costa R., Perez F., Madrid I., Gordon M., Albacete Moreno C. L., Perez D., Lopez N., Martinenz D., Blanco-Schweizer P., Diez C., Prieto A., Renedo G., Bustamante E., Cicuendez R., Citores R., Boado V., Garcia K., Voces R., Domezain M., Nunez Martinez J. M., Vicente R., Martin D., Andreu A., Gomez Casal V., Chico I., Menor E. M., Vara S., Gamacho J., Perez-Chomon H., Javier Gonzales F., Barrero I., Martin-Villen L., Fernandez E., Mendoza M., Navarro J., Colomina Climent J., Gonzales-Perez A., Muniz-Albaceita G., Amado L., Rodriguez R., Ruiz E., Eiras M., Grins E., Magnus R., Kanetoft M., Eidevald M., Watson P., Vogt P. R., Steiger P., Aigner T., Weber A., Grunefelder J., Kunz M., Grapow M., Aymard T., Reser D., Agus G., Consiglio J., Haenggi M., Hansjoerg J., Iten M., Doeble T., Zenklusen U., Bechtold X., Faedda G., Iafrate M., Rohjer A., Bergamaschi L., Maessen J., Reis Miranda D., Endeman H., Gommers D., Meuwese C., Maas J., Van Gijlswijk M. J., Van Berg R. N., Candura D., Van der Linden M., Kant M., Van der Heijden J. J., Scholten E., Van Belle-van Haren N., Lagrand W. K., Vlaar A. P., De Jong S., Cander B., Sargin M., Ugur M., Kaygin M. A., Daly K., Agnew N., Head L., Kelly L., Anoma G., Russell C., Aquino V., Scott I., Flemming L., Gillon S., Moore O., Gelandt E., Auzinger G., Patel S., and Loveridge R.
Abstract: Background: Extracorporeal membrane oxygenation (ECMO) has been widely used in patients with COVID-19, but uncertainty remains about the determinants of in-hospital mortality and data on post-discharge outcomes are scarce. The aims of this study were to investigate the variables associated with in-hospital outcomes in patients who received ECMO during the first wave of COVID-19 and to describe the status of patients 6 months after ECMO initiation. Methods: EuroECMO-COVID is a prospective, multicentre, observational study developed by the European Extracorporeal Life Support Organization. This study was based on data from patients aged 16 years or older who received ECMO support for refractory COVID-19 during the first wave of the pandemic—from March 1 to Sept 13, 2020—at 133 centres in 21 countries. In-hospital mortality and mortality 6 months after ECMO initiation were the primary outcomes. Mixed-Cox proportional hazards models were used to investigate associations between patient and management-related variables (eg, patient demographics, comorbidities, pre-ECMO status, and ECMO characteristics and complications) and in-hospital deaths. Survival status at 6 months was established through patient contact or institutional charts review. This study is registered with ClinicalTrials.gov, NCT04366921, and is ongoing. Findings: Between March 1 and Sept 13, 2020, 1215 patients (942 [78%] men and 267 [22%] women; median age 53 years [IQR 46–60]) were included in the study. Median ECMO duration was 15 days (IQR 8–27). 602 (50%) of 1215 patients died in hospital, and 852 (74%) patients had at least one complication. Multiorgan failure was the leading cause of death (192 [36%] of 528 patients who died with available data). In mixed-Cox analyses, age of 60 years or older, use of inotropes and vasopressors before ECMO initiation, chronic renal failure, and time from intubation to ECMO initiation of 4 days or more were associated with higher in-hospital mortality. 613 patients
Published: 2023

43. Diffuse $\gamma$-ray emission from unresolved BL Lac objects

Author: Di Mauro, M., Donato, F., Lamanna, G., Sanchez, D. A., and Serpico, P. D.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Blazars represent the most abundant class of high-energy extragalactic $\gamma$-ray sources. The subset of blazars known as BL Lac objects is on average closer to Earth and characterized by harder spectra at high energy than the whole sample. The fraction of BL Lacs that is too dim to be detected and resolved by current $\gamma$-ray telescopes is therefore expected to contribute to the high-energy isotropic diffuse $\gamma$-ray background (IGRB). The IGRB has been recently measured over a wide energy range by the Large Area Telescope (LAT) on board the Gamma-ray Space Telescope ({\it Fermi}). We present a new prediction of the diffuse $\gamma$-ray flux due to the unresolved BL Lac blazar population. The model is built upon the spectral energy distribution and the luminosity function derived from the fraction of BL Lacs detected (and spectrally characterized) in the $\gamma$-ray energy range. We focus our attention on the ${\cal O}(100)$ GeV energy range, predicting the emission up to the TeV scale and taking into account the absorption on the extragalactic background light. In order to better shape the BL Lac spectral energy distribution, we combine the {\it Fermi}-LAT data with Imaging Atmospheric Cerenkov Telescopes measurements of the most energetic sources. Our analysis is carried on separately for low- and intermediate-synchrotron-peaked BL Lacs on one hand, and high-synchrotron-peaked BL Lacs on the other one: we find in fact statistically different features for the two. The diffuse emission from the sum of both BL Lac classes increases from about 10$\%$ of the measured IGRB at 100 MeV to $\sim$100$\%$ of the data level at 100 GeV. At energies greater than 100 GeV, our predictions naturally explain the IGRB data, accommodating their softening with increasing energy. Uncertainties are estimated to be within of a factor of two of the best-fit flux up to 500 GeV., Comment: 14 pages, 6 figures. Version 4: Minor typos corrections, notably minus sign in the exponent of the square brackets of Eq.s A2, A6 and luminosity units in Table 2
Published: 2013
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44. Diffuse $\gamma$-ray emission from misaligned active galactic nuclei

Author: Di Mauro, M., Donato, F., and Calore, F.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics, High Energy Physics - Phenomenology, High Energy Physics - Theory
Abstract: We calculate the diffuse $\gamma$-ray emission due to the population of misaligned AGN (MAGN) unresolved by the Large Area Telescope (LAT) on the {\it Fermi} Gamma-ray Space Telescope ({\it Fermi}). A correlation between the $\gamma$-ray luminosity and the radio-core luminosity is established and demonstrated to be physical by statistical tests, as well as compatible with upper limits based on {\it Fermi}-LAT data for a large sample of radio-loud MAGN. We constrain the derived $\gamma$-ray luminosity function by means of the source count distribution of the MAGN detected by the {\it Fermi}-LAT. We finally estimate the diffuse $\gamma$-ray flux due to the whole MAGN population which ranges from 10% up to nearly the entire measured Isotropic Gamma-Ray Background (IGRB). We evaluate also the room left to galactic DM at high latitudes ($>10^\circ$), by taking into account the results on the MAGN together with the other significant galactic and extragalactic $\gamma$-rays emitting sources., Comment: Proceedings of Rencontres de Moriond, La Thuile, March 9th - 16th, 2013
Published: 2013

45. The GAPS programme with HARPS-N at TNG. I: Observations of the Rossiter-McLaughlin effect and characterisation of the transiting system Qatar-1

Author: Covino, E., Esposito, M., Barbieri, M., Mancini, L., Nascimbeni, V., Claudi, R., Desidera, S., Gratton, R., Lanza, A. F., Sozzetti, A., Biazzo, K., Affer, L., Gandolfi, D., Munari, U., Pagano, I., Bonomo, A. S., Cameron, A. Collier, Hébrard, G., Maggio, A., Messina, S., Micela, G., Molinari, E., Pepe, F., Piotto, G., Ribas, I., Santos, N. C., Southworth, J., Shkolnik, E., Triaud, A. H. M. J., Bedin, L., Benatti, S., Boccato, C., Bonavita, M., Borsa, F., Borsato, L., Brown, D., Carolo, E., Ciceri, S., Cosentino, R., Damasso, M., Faedi, F., Fiorenzano, A. F. Martínez, Latham, D. W., Lovis, C., Mordasini, C., Nikolov, N., Poretti, E., Rainer, M., López, R. Rebolo, Scandariato, G., Silvotti, R., Smareglia, R., Alcala, J. M., Cunial, A., Di Fabrizio, L., Di Mauro, M. P., Giacobbe, P., Granata, V., Harutyunyan, A., Knapic, C., Lattanzi, M., Leto, G., Lodato, G., Malavolta, L., Marzari, F., Molinaro, M., Nardiello, D., Pedani, M., Prisinzano, L., and Turrini, D.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: A long-term multi-purpose observational programme has started with HARPS-N@TNG aimed to characterise the global architectural properties of exoplanetary systems. In this first paper we fully characterise the transiting system Qatar-1. We exploit HARPS-N high-precision radial velocity measurements obtained during a transit to measure the Rossiter-McLaughlin effect in the Qatar-1 system, and out-of-transit measurements to redetermine the spectroscopic orbit. New photometric transit light-curves are analysed and a spectroscopic characterisation of the host star atmospheric parameters is performed based on various methods (line equivalent width ratios, spectral synthesis, spectral energy distribution). We achieved a significant improvement in the accuracy of the orbital parameters and derived the spin-orbit alignment of the system; this information, combined with the spectroscopic determination of the host star properties, allows us to derive the fundamental physical parameters for star and planet (masses and radii). The orbital solution for the Qatar-1 system is consistent with a circular orbit and the system presents a sky-projected obliquity of lambda = -8.4+-7.1 deg. The planet, with a mass of 1.33+-0.05 M_J, is found to be significantly more massive than previously reported. The host star is confirmed to be metal-rich ([Fe/H]= 0.20+-0.10) and slowly rotating (vsinI = 1.7+-0.3 km/s), though moderately active, as indicated by strong chromospheric emission in the Ca II H&K line cores (logR'_HK about -4.60). The system is well aligned and fits well within the general lambda vs Teff trend. We definitely rule out any significant orbital eccentricity. The evolutionary status of the system is inferred based on gyrochronology, and the present orbital configuration and timescale for orbital decay are discussed in terms of star-planet tidal interactions., Comment: 12 pages, 8 figures
Published: 2013
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46. Theoretical aspects of asteroseismology: small steps towards a golden future

Author: Di Mauro, M. P.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The current status of asteroseismic studies is here reviewed and the adequate techniques of analysis available today for the study of the oscillation frequencies are presented. Comments on prospects for future investigations through the possibility of getting ever more precise asteroseismic observations from ground and space are given., Comment: 15 pages, SOHO 14/GONG 2004 Workshop - Helio- and Asteroseismology: Towards a Golden Future
Published: 2012

47. Helioseismology: a fantastic tool to probe the interior of the Sun

Author: Di Mauro, M. P.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Helioseismology, the study of global solar oscillations, has proved to be an extremely powerful tool for the investigation of the internal structure and dynamics of the Sun. Studies of time changes in frequency observations of solar oscillations from helioseismology experiments on Earth and in space have shown, for example, that the Sun's shape varies over solar cycle timescales. In particular, far-reaching inferences about the Sun have been obtained by applying inversion techniques to observations of frequencies of oscillations. The results, so far, have shown that the solar structure is remarkably close to the predictions of the standard solar model and, recently, that the near-surface region can be probed with sufficiently high spatial resolution as to allow investigations of the equation of state and of the solar envelope helium abundance. The same helioseismic inversion methods can be applied to the rotational frequency splittings to deduce with high accuracy the internal rotation velocity of the Sun, as function of radius and latitude. This also allows us to study some global astrophysical properties of the Sun, such as the angular momentum, the grativational quadrupole moment and the effect of distortion induced on the surface (oblateness). The helioseismic approach and what we have learnt from it during the last decades about the interior of the Sun are reviewed here., Comment: 36 pages
Published: 2012
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48. Internal rotation of red giants by asteroseismology

Author: Di Mauro, M. P., Cardini, D., Ventura, R., Stello, D., Beck, P. G., Davies, G., Elsworth, Y., Garcıa, R. A., Hekker, S., Mosser, B., Christensen-Dalsgaard, J., Bloemen, S., Catanzaro, G., De Smedt, K., and Tkachenko, A.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present an asteroseismic approach to study the dynamics of the stellar interior in red-giant stars by asteroseismic inversion of the splittings induced by the stellar rotation on the oscillation frequencies. We show preliminary results obtained for the red giant KIC4448777 observed by the space mission Kepler., Comment: 3 pages, 4 figures, the 40th Liege International Astrophysical Colloquium Liac40, 'Ageing low mass stars: from red giants to white dwarfs', to be published on EPJ Web of Conferences
Published: 2012
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49. From Helio- to Asteroseismology and the progress in stellar physics

Author: Di Mauro, M. P.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: During the last decades, numerous observational and theoretical efforts in the study of solar oscillations, have brought to a detailed knowledge of the interior of the Sun. While this discipline has not yet exhausted its resources and scientists are still working on further refinements of the solar models and to solve the numerous still open questions, Asteroseismology, which aims to infer the structural properties of stars which display multi-mode pulsations, has just entered in its golden age. In fact, the space missions CoRoT and Kepler dedicated to the observation of stellar oscillations, have already unveiled primary results on the structural properties of the stars producing a revolution in the way we study the stellar interiors. Here, the modern era of Helio- and Asteroseismology is reviewed with emphasis on results obtained for the Sun and its solar-like counterparts., Comment: 10 pages, EWASS 2012 Conference, Special Session 11 "From solar physics to astrophysics: the Sun as Rosetta stone for understanding astrophysical processes', to be published on Mem. SaIt
Published: 2012

50. Characterizing two solar-type Kepler subgiants with asteroseismology: KIC10920273 and KIC11395018

Author: Dogan, G., Metcalfe, T. S., Deheuvels, S., Di Mauro, M. P., Eggenberger, P., Creevey, O. L., Monteiro, M. J. P. F. G., Pinsonneault, M., Frasca, A., Karoff, C., Mathur, S., Sousa, S. G., Brandao, I. M., Campante, T. L., Handberg, R., Thygesen, A. O., Biazzo, K., Bruntt, H., Niemczura, E., Bedding, T. R., Chaplin, W. J., Christensen-Dalsgaard, J., Garcia, R. A., Molenda-Zakowicz, J., Stello, D., Van Saders, J. L., Kjeldsen, H., Still, M., Thompson, S. E., and Van Cleve, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Determining fundamental properties of stars through stellar modeling has improved substantially due to recent advances in asteroseismology. Thanks to the unprecedented data quality obtained by space missions, particularly CoRoT and Kepler, invaluable information is extracted from the high-precision stellar oscillation frequencies, which provide very strong constraints on possible stellar models for a given set of classical observations. In this work, we have characterized two relatively faint stars, KIC10920273 and KIC11395018, using oscillation data from Kepler photometry and atmospheric constraints from ground-based spectroscopy. Both stars have very similar atmospheric properties; however, using the individual frequencies extracted from the Kepler data, we have determined quite distinct global properties, with increased precision compared to that of earlier results. We found that both stars have left the main sequence and characterized them as follows: KIC10920273 is a one-solar-mass star (M=1.00 +/- 0.04 M_sun), but much older than our Sun (t=7.12 +/- 0.47 Gyr), while KIC11395018 is significantly more massive than the Sun (M=1.27 +/- 0.04 M_sun) with an age close to that of the Sun (t=4.57 +/- 0.23 Gyr). We confirm that the high lithium abundance reported for these stars should not be considered to represent young ages, as we precisely determined them to be evolved subgiants. We discuss the use of surface lithium abundance, rotation and activity relations as potential age diagnostics., Comment: 12 pages, 3 figures, 5 tables. Accepted by ApJ
Published: 2012
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