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351. Effect of packed cell volume on blood glucose estimations

Author

D J Goldie, R G Dalton, J P Osborne, and C M Dacombe

Subjects
Blood Glucose, medicine.medical_specialty, Reagent strip, Filter paper, medicine.diagnostic_test, business.industry, Spot method, Cell volume, Hematocrit, Surgery, Pediatrics, Perinatology and Child Health, Methods, Medicine, Humans, Diagnostic Errors, business, Biomedical engineering, Reagent Strips, Research Article
Abstract

The effect of changes in packed cell volume was studied in two commonly used reagent strip methods (Dextrostix and Reflotest) of measuring blood glucose and in a filter paper blood spot method. It was found that the results with both the reagent strip methods were greatly haematocrit-dependent. Attention is drawn to the possibility of false diagnoses of hypoglycaemia in haemoconcentrated patients and of normoglycaemia in anaemic patients.

Published
1981

353. Time-Resolved Optical Spectroscopy of AM Her X-Ray Sources

Author

Jean-Marc Bonnet-Bidaud, S. van Amerongen, J. P. Osborne, and M. Mouchet

Subjects
Physics, business.industry, Resolution (electron density), Polarimetry, Balmer series, Astrophysics, Light curve, Radial velocity, symbols.namesake, Optics, Temporal resolution, symbols, Emission spectrum, Spectroscopy, business
Abstract

We present high-time resolution spectroscopy of two AM Her sources E1405-451 and E1013–477. For E1405–451, the Balmer emission lines profiles can be divided into a narrow component and a broad one. The amplitudes of the radial velocity curves of these components are respectively 265±30 km/s and 390±50 km/s. The orientation of the column determined from polarimetry is not compatible with the broad component being formed in the lowest parts of the column. Photometric and spectroscopic results on E1013-477 do not confirm the previous reported 103 min. period. Rapid variability ( 3.3h) is present in these data.

Published
1987

354. Ariel 6 Observations of the Hot White Dwarf HZ43

Author

C. V. Goodall, A. M. Cruise, R. Cole, A. M. T. Pollock, D. K. Bedford, J. P. Osborne, and E. Carpenter

Subjects
Physics, Black body, White dwarf, Astronomy, Black-body radiation, Photon density, Satellite, Astrophysics, Pulse height, Astronomical spectroscopy
Abstract

The hot white dwarf HZ43 was observed by the soft X-ray experiment on the Ariel 6 satellite from 1980 March 1.8 to March 8.7. The pulse height spectrum has been fit to an input black body spectrum of temperature 140 000 K. An upper limit of 10% has been placed on the source variability on time scales of minutes.

Published
1981

355. Ariel VI Observations of Sco X-1

Author

C. V. Goodall, A. M. Cruise, J. L. Culhane, J. P. Osborne, G. F. Carpenter, A. M. T. Pollock, D. K. Bedford, and R. Cole

Subjects
Physics, Wavelength, Spectral shape analysis, Spectral flux, Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), medicine, Plasma, Astrophysics, medicine.disease_cause, Isothermal process, Ultraviolet
Abstract

It has been popular and empirically quite successful to describe the entire continuum electromagnetic spectrum of Sco X-1 in terms of emission from an isothermal plasma at a temperature of about 50 million degrees K. Many workers have emphasised the need to consider multiple Compton scatterings in the calculation of the emergent spectrum and have pointed out that this process produces important modifications to the spectral shape at X-ray and ultraviolet wavelengths.

Published
1981

356. Diver Performance—Nitrogen Narcosis and Anxiety

Author

F. M. Davis, J. P. Osborne, A. D. Baddeley, and I. M. Graham

Subjects
medicine.medical_specialty, Injury control, business.industry, Human factors and ergonomics, Poison control, medicine.disease, Suicide prevention, Occupational safety and health, Emergency medicine, Injury prevention, medicine, Anxiety, medicine.symptom, Nitrogen narcosis, business
Published
1976

357. Huntington's chorea. Report of 3 cases and review of the literature

Author

J P Osborne, D Burman, and P Munson

Subjects
Adult, Male, Pediatrics, medicine.medical_specialty, Time Factors, Adolescent, business.industry, Progressive mental deterioration, Chorea, Disease, Dysarthria, Huntington Disease, Child, Preschool, Pediatrics, Perinatology and Child Health, medicine, Disease early, Humans, Female, medicine.symptom, business, Child, Research Article
Abstract

Three cases of Huntington's chorea with onset before age 10 years are reported. Each child presented with rigidity and indistinct speech, and there was progressive deterioration. Necropsy examination confirmed the diagnosis in 2 of them. A review of reports showed a further 43 cases with onset before 10 years. The rigid variety of disease was seen most often, but isolated chorea and isolated progressive mental deterioration occurred. Fits were common but occurred late and were often difficult to control. Dysarthria was common and occurred early. The duration of illness was very variable and ranged from 2 to 38 years. Symptoms can occur in a child before appearing in the affected parent who is most likely to be the father. Affected siblings develop the disease early, often in the first decade. Siblings of patients with onset before age 10 years who are unaffected by age 25 years had only an 8% chance of developing the disease, compared with a 50% chance in unselected at risk individuals of the same age.

Published
1982

358. Ariel VI Soft X-Ray Observations of Cygnus X-1

Author

C. V. Goodall, D. K. Bedford, R. Cole, J. P. Osborne, A. M. Cruise, A. M. T. Pollock, and G. F. Carpenter

Subjects
Physics, X-ray astronomy, Soft x ray, Soft photon, Accretion disc, Astrophysics::High Energy Astrophysical Phenomena, Energy spectrum, Flux, Astronomy, Astrophysics, Astronomical spectroscopy
Abstract

Observations of Cygnus X-1 during the high-low transition of June-July 1980 reveal an intense flux between 0.5 and 1.5 keV. Although the intensity broadly follows the 1–12 keV flux through the transition, there is no evidence of variations in the shape of the energy spectrum. The implications of these results and derived limits on the minute-to-minute variability are discussed.

Published
1981

359. Diver performance: nitrogen narcosis and anxiety

Author

F M, Davis, J P, Osborne, A D, Baddeley, and I M, Graham

Subjects
Adult, Male, Psychological Tests, Mental Processes, Memory, Motor Skills, Nitrogen, Diving, Immersion, Humans, Anxiety
Published
1972

360. GRB 070724B: the first Gamma Ray Burst localized by SuperAGILE

Author

E. Del Monte, E. Costa, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov, F. Lazzarotto, M. Rapisarda, P. Soffitta, A. Argan, G. Barbiellini, M. Basset, A. Bulgarelli, P. Caraveo, A. Chen, G. Di Cocco, L. Foggetta, F. Fuschino, M. Galli, F. Gianotti, A. Giuliani, C. Labanti, P. Lipari, F. Longo, M. Marisaldi, F. Mauri, S. Mereghetti, A. Morselli, A. Pellizzoni, F. Perotti, P. Picozza, M. Prest, G. Pucella, M. Tavani, M. Trifoglio, A. Trois, E. Vallazza, S. Vercellone, V. Vittorini, A. Zambra, P. Romano, D. N. Burrows, G. Chincarini, N. Gehrels, V. La Parola, P. T. O'Brien, J. P. Osborne, B. Preger, C. Pittori, L. A. Antonelli, F. Verrecchia, P. Giommi, L. Salotti, M. Galassi, David Palmer, and Ed Fenimore

Subjects
Physics, Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Gamma ray spectra, Astrophysics, Gamma-ray burst, Gamma detection
Abstract

GRB070724B is the first Gamma Ray Burst localized by the SuperAGILE instrument aboard the AGILE space mission. The SuperAGILE localization has been confirmed after the after‐glow observation by the XRT aboard the Swift satellite. No significant gamma ray emission above 50 MeV has been detected for this GRB. In this paper we describe the SuperAGILE capabilities in detecting Gamma Ray Burst and the AGILE observation of GRB 070724B.

361. Ginga and ROSAT observations of AO Psc and V1223 Sgr

Author

J. P. Osborne, Philip Taylor, M. G. Watson, A. P. Beardmore, and Andrew Norton

Subjects
Physics, Line-of-sight, Pulsar, Space and Planetary Science, Inclination angle, ROSAT, Modulation (music), Astronomy, White dwarf, Astronomy and Astrophysics, Astrophysics, Orbital period, Lower energy
Abstract

We present results from X-ray observations of the intermediate polars AD Psc and V1223 Sgr, taken with the ROSAT HRI and the Ginga LAC. Both sources show sinusoidal modulation at the white dwarf spin period in all energy bands, possibly with the exception of the highest. The depths of these modulations increase at lower energy, but the rates at which they do so are not consistent with single column densities of absorbing material. Neither source shows any significant pulse at the beat period, which argues for a predominantly disc-fed accretion model in each case. The AD Psc observations show a modulation at the orbital period, which in the ROSAT data may indicate an extended absorbing structure, with a dip at orbital phase ~0.50.8 superimposed. The V1223 Sgr ROSAT data show short dips which occur intermittently at around orbital phase 0.8. These dips vary in duration and phase of commencement and suggest that the system inclination angle is just sufficient for our line of sight to graze the upper extent of the material thrown out of the disc plane.

362. X-Ray Flashes in Recurrent Novae: M31N 2008-12a and the Implications of the Swift Non-detection

Author

Allen W. Shafter, Michael F. Bode, Jan-Uwe Ness, J. A. Kennea, Mariko Kato, Izumi Hachisu, M. J. Darnley, K. L. Page, Martin Henze, J. P. Osborne, Hideyuki Saio, Neil Gehrels, and Margarita Hernanz

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Context (language use), Astrophysics, Nova (laser), Light curve, 01 natural sciences, Stars, Flash (photography), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Binary star, Variable star, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB
Abstract

Models of nova outbursts suggest that an X-ray flash should occur just after hydrogen ignition. However, this X-ray flash has never been observationally confirmed. We present four theoretical light curves of the X-ray flash for two very massive white dwarfs (WDs) of 1.380 and 1.385 M_sun and for two recurrence periods of 0.5 and 1 years. The duration of the X-ray flash is shorter for a more massive WD and for a longer recurrence period. The shortest duration of 14 hours (0.6 days) among the four cases is obtained for the 1.385 M_sun WD with one year recurrence period. In general, a nova explosion is relatively weak for a very short recurrence period, which results in a rather slow evolution toward the optical peak. This slow timescale and the predictability of very short recurrence period novae give us a chance to observe X-ray flashes of recurrent novae. In this context, we report the first attempt, using the Swift observatory, to detect an X-ray flash of the recurrent nova M31N 2008-12a (0.5 or 1 year recurrence period), which resulted in the non-detection of X-ray emission during the period of 8 days before the optical detection. We discuss the impact of these observations on nova outburst theory. The X-ray flash is one of the last frontiers of nova studies and its detection is essentially important to understand the pre-optical-maximum phase. We encourage further observations., Comment: 12 pages, including 9 figures and 3 tables. To appear in the Astrophysical Journal

363. The optical afterglow of the short gamma-ray burst associated with GW170817

Author

Phil Evans, Iain A. Steele, Patrick J. Sutton, Ilya Mandel, Benjamin P. Gompertz, Elizabeth R. Stanway, Andrew J. Levan, Bo Milvang-Jensen, Daniel A. Perley, Gavin P. Lamb, Antonia Rowlinson, Darach Watson, Chris M. Copperwheat, Shiho Kobayashi, Tuomas Kangas, Danny Steeghs, Elena Pian, Eliana Palazzi, Zach Cano, J. P. Osborne, J. D. Lyman, A. de Ugarte Postigo, Ralph A. M. J. Wijers, Pall Jakobsson, Steve Schulze, Christa Gall, Johan P. U. Fynbo, Luca Izzo, A. S. Fruchter, Klaas Wiersema, Christina C. Thöne, Nial R. Tanvir, Myungshin Im, Jens Hjorth, P. T. O'Brien, Stephan Rosswog, High Energy Astrophys. & Astropart. Phys (API, FNWI), National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), European Commission, European Research Council, Science and Technology Facilities Council (UK), Villum Fonden, National Research Foundation of Korea, Danish National Research Foundation, Swedish National Space Board, and Swedish Research Council

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kilonova, 01 natural sciences, Luminosity, Afterglow, Interstellar medium, Neutron star, 13. Climate action, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

The binary neutron star merger GW170817 was the first multi-messenger event observed in both gravitational and electromagnetic waves. The electromagnetic signal began approximately two seconds post-merger with a weak, short burst of gamma rays, which was followed over the next hours and days by the ultraviolet, optical and near-infrared emission from a radioactively powered kilonova. Later, non-thermal rising X-ray and radio emission was observed. The low luminosity of the gamma rays and the rising non-thermal flux from the source at late times could indicate that we are outside the opening angle of the beamed relativistic jet. Alternatively, the emission could be arising from a cocoon of material formed from the interaction between a jet and the merger ejecta. Here we present late-time optical detections and deep near-infrared limits on the emission from GW170817 at 110 days post-merger. Our new observations are at odds with expectations of late-time emission from kilonova models, being too bright and blue. Instead, the emission arises from the interaction between the relativistic ejecta of GW170817 and the interstellar medium. We show that this emission matches the expectations of a Gaussian-structured relativistic jet, which would have launched a high-luminosity, short gamma-ray burst to an aligned observer. However, other jet structure or cocoon models can also match current data—the future evolution of the afterglow will directly distinguish the origin of the emission., Based on observations made with the NASA/European Space Agency Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. These observations are associated with programmes GO 14771 (N.R.T.) and GO 14270 (A.J.L.). We thank the staff at STScI for their excellent support of these observations. A.J.L. acknowledges that this project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement no 725246). J.D.L., A.J.L., D.S. and K.W. acknowledge support from the Science and Technology Facilities Council (STFC) via grant ST/P000495/1. N.R.T., P.O., J.P.O., G.P.L., I.M. and S.K. acknowledge support from STFC. G.P.L. acknowledges partial support from the Royal Astronomical Society and International Astronomical Union grants. J.H. was supported by a VILLUM FONDEN Investigator grant (project number 16599). The Cosmic Dawn Center is funded by the Danish National Research Foundation. A.d.U.P., C.C.T. and Z.C. acknowledge support from the Spanish project AYA 2014-58381-P. Z.C. also acknowledges support from the Juan de la Cierva Incorporation fellowship IJCI-2014-21669. M.I. acknowledges the support from the National Research Foundation of Korea grant, No. 2017R1A3A3001362. S.R. has been supported by the Swedish Research Council (VR) under grant number 2016-03657_3, by the Swedish National Space Board under grant number Dnr. 107/16 and by the research environment grant 'Gravitational Radiation and Electromagnetic Astrophysical Transients (GREAT)' funded by the Swedish Research council (VR) under Dnr 2016-06012. P.A.E. acknowledges United Kingdom Space Agency support. D.J.W. is supported by the the Danish Agency for Science, Technology and Innovation under grant number DFF - 7014-00017. G.P.L. thanks A. Higgins and L. Raynard for useful conversations regarding Markov chain Monte Carlo, and G.P.L. and S.K. thank E. Nakar for helpful comments. I.M. thanks J. Granot for useful discussions.

364. Stream-fed and disc-fed accretion in TX Columbae

Author

Coel Hellier, A. P. Beardmore, Philip Taylor, Andrew Norton, J. P. Osborne, and Peter J. Wheatley

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Attenuation, White dwarf, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Accretion (astrophysics), Spectral line, Intermediate polar, Space and Planetary Science, ROSAT, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report on two recent X-ray observations of the intermediate polar TX Col made with ASCA and ROSAT. From a consideration of the power spectra of their light curves, we show that the system was accreting predominantly via a disc in 1994 October, but had reverted to a disc­ overflow mode of accretion by 1995 October, at which time a substantial amount of the accretion was directly via a stream. We discuss possible reasons for this change. By considering the relative phases of the spin and beat pulsations seen in the ROSAT data, as well as their orbital harmonics, we demonstrate that the stream-fed accretion regions on the white dwarf surface remain fixed at about orbital phase 0.7, and thus migrate around the white dwarf. We suggest that the observed orbital modulation results from a combination of two effects: first, attenuation of emission sites by material located at the stream-disc boundary at orbital phase 0.8, and, secondly, the changing visibility of the stream-fed accretion sites which are always on the side of the white dwarf facing the stream.

365. Multiwavelength observations of V407 Lupi (ASASSN-16kt) --- a very fast nova erupting in an intermediate polar

Author

A. Y. Kniazev, A. P. Beardmore, A. Dobrotka, N. P. M. Kuin, G. Myers, Laura Chomiuk, Martin Henze, Jay Strader, M. J. Darnley, Charles E. Woodward, N. Ospina, Marina Orio, Brent Miszalski, K. L. Page, Sumner Starrfield, F. M. Walter, J. P. Osborne, Patricia A. Whitelock, D. A. H. Buckley, Shazrene Mohamed, E. Aydi, and Jan-Uwe Ness

Subjects
Physics, Rotation period, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, Light curve, 01 natural sciences, Accretion (astrophysics), Optical spectra, Intermediate polar, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QC, 0105 earth and related environmental sciences, QB
Abstract

We present a detailed study of the 2016 eruption of nova V407 Lupi (ASASSN-16kt), including optical, near-infrared, X-ray, and ultraviolet data from SALT, SMARTS, SOAR, Chandra, Swift, and XMM-Newton. Timing analysis of the multiwavelength light-curves shows that, from 168 days post-eruption and for the duration of the X-ray supersoft source phase, two periods at 565 s and 3.57 h are detected. We suggest that these are the rotational period of the white dwarf and the orbital period of the binary, respectively, and that the system is likely to be an intermediate polar. The optical light-curve decline was very fast ($t_2 \leq$ 2.9 d), suggesting that the white dwarf is likely massive ($\gtrsim 1.25$ M$_{\odot}$). The optical spectra obtained during the X-ray supersoft source phase exhibit narrow, complex, and moving emission lines of He II, also characteristics of magnetic cataclysmic variables. The optical and X-ray data show evidence for accretion resumption while the X-ray supersoft source is still on, possibly extending its duration., Comment: 39 pages, 32 figures, 23 tables, accepted for publication in MNRAS

366. The changing X-ray light curves of the intermediate polar FO Aquarii

Author

Coel Hellier, Koji Mukai, Andrew Norton, A. P. Beardmore, and J. P. Osborne

Subjects
Physics, Field line, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, White dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, Accretion (astrophysics), Spectral line, Magnetic field, Intermediate polar, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Polar, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Comparison of five X-ray observations of the intermediate polar FO Aqr reveals that the morphology of the X-ray light curve changes considerably with time. In particular, power spectra of the 1988 Ginga and 1993 ASCA data reveal strong sideband and orbital variations, whereas the 1990 Ginga observation does not. This suggests that the amount of stream-fed accretion varies with epoch, and the system was accreting predominantly from a disc in 1990. In contrast to other intermediate polars, the X-ray spin-pulse profiles show significant variations between observations, ranging from relatively sinusoidal to sawtooth-shaped at medium energies. During the 1988 and 1990 observations a notch is visible at spin phase zero, due to the presence of an interpulse at phase 0.85, which is absent during the other observations. At lower energies a narrow pulse of emission is seen at spin phase 0.2. We interpret the pulse profile from the 1990 Ginga observation using a model for accretion from a disc on to a dipolar magnetic field, the axis of which is offset from the white dwarf centre by ~ 0.15 white dwarf radii. In order to account for the later occurrence of the hardness-ratio maximum in 1988 and 1993, we suggest that the accretion-rate profile changes so that accretion is favoured along the field lines which trail the magnetic pole. This also accounts for the disappearance of the interpulse and notch in 1993.

367. Investigation of jet break features in Swift gamma-ray bursts

Author

A. M. Parsons, Kunihito Ioka, J. P. Osborne, Makoto Tashiro, Ryo Yamazaki, Kenji Toma, Scott Barthelmy, David N. Burrows, Kazuhiro Nakazawa, G. Chincarini, H. A. Krimm, G. Sato, D. Hullinger, P. T. O'Brien, T. Takahashi, D. Q. Lamb, N. Gehrels, T. Sakamoto, and Nakamura Tetsuhisa

Subjects
Swift, Physics, Jet (fluid), Astronomy, Astrophysics, Gamma-ray burst, computer, computer.programming_language

368. Pan-Chromatic observations of the Recurrent Nova LMC 2009a (LMC 1971b)

Author

K. L. Page, Joachim Krautter, M. F. Bode, Greg J. Schwarz, Jan-Uwe Ness, Andrew P. Beardmore, Sumner Starrfield, Michael M. Shara, J. P. Osborne, M. J. Darnley, A. Melandri, Marina Orio, F. M. Walter, and Tim O'Brien

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, Binary star, novae, cataclysmic variables, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, white dwarfs, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), White dwarf, Astronomy and Astrophysics, individual (LMC) [galaxies], Accretion (astrophysics), Galaxy, Stars, Astrophysics - Solar and Stellar Astrophysics, individual (Nova LMC 2009a, Nova LMC 1971b) [stars], Space and Planetary Science, Spectral energy distribution, Variable star, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Nova LMC 2009a is confirmed as a Recurrent Nova (RN) from positional coincidence with nova LMC 1971b. The observational data set is one of the most comprehensive for any Galactic or extragalactic RN: optical and near-IR photometry from outburst until over 6 years later; optical spectra for the first 6 months, and Swift satellite Ultraviolet and X-ray observations from 9 days to almost 1 year post-outburst. We find $M_V = -8.4\pm0.8_{\mathrm{r}}\pm0.7_{\mathrm{s}}$ and expansion velocities between 1000 and 4000 km s$^{-1}$. Coronal line emission before day 9 indicates shocks in the ejecta. Strengthening of He II $\lambda$4686 preceded the emergence of the Super-Soft Source (SSS) in X-rays at $\sim63-70$ days, which was initially very variable. Periodic modulations, $P=1.2$ days, most probably orbital in nature, were evident in the UV and optical from day 43. Subsequently, the SSS shows an oscillation with the same period but with a delay of 0.28P. The progenitor system has been identified; the secondary is most likely a sub-giant feeding a luminous accretion disk. Properties of the SSS infer a white dwarf (WD) mass $1.1 \mathrm{M}_\odot \lesssim M_{\rm WD} \lesssim 1.3 \mathrm{M}_\odot$. If the accretion occurs at constant rate, $\dot{\it{M}}_{\rm acc} \simeq 3.6^{+4.7}_{-2.5} \times 10^{-7} \mathrm{M}_\odot$ yr$^{-1}$ is needed, consistent with nova models for an inter-eruption interval of 38 years, low outburst amplitude, progenitor position in the color-magnitude diagram, and spectral energy distribution at quiescence. We note striking similarities between LMC 2009a and the Galactic nova KT Eri, suggesting that KT Eri is a candidate RN., Comment: 20 pages, 23 figures, accepted for publication in the Astrophysical Journal

369. XMM-Newton slew survey discovery of the nova XMMSL1 J070542.7-381442 (V598 Pup)

Author

P.G. Jonker, E. Kuulkers, Michael Freyberg, P. Esquej, Manuel A. P. Torres, A. M. Read, P. Challis, J. P. Osborne, and Richard Saxton

Subjects
Physics, Brightness, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Nova (laser), Light curve, law.invention, Telescope, Space and Planetary Science, law, ROSAT, Emission spectrum
Abstract

In an attempt to catch new X-ray transients while they are still bright, the data taken by XMM-Newton as it slews between targets is being processed and cross-correlated with other X-ray observations as soon as the slew data appears in the XMM-Newton archive. A bright source, XMMSL1 J070542.7-381442, was detected on 9 Oct 2007 at a position where no previous X-ray source had been seen. The XMM slew data and optical data acquired with the Magellan Clay 6.5m telescope were used to classify the new object. No XMM slew X-ray counts are detected above 1keV and the source is seen to be ~750 times brighter than the ROSAT All-Sky Survey upper limit at that position. The normally m(V)~16 star, USNO-A2.0 0450-03360039, which lies 3.5" from the X-ray position, was seen in our Magellan data to be very much enhanced in brightness. Our optical spectrum showed emission lines which identified the source as a nova in the auroral phase. Hence this optical source is undoubtedly the progenitor of the X-ray source - a new nova (now also known as V598 Pup). The X-ray spectrum indicates that the nova was in a super-soft state (with kT(eff)~35eV). We estimate the distance to the nova to be ~3kpc. Analysis of archival robotic optical survey data shows a rapid decline light curve consistent with that expected for a very fast nova. The XMM-Newton slew data present a powerful opportunity to find new X-ray transient objects while they are still bright. Here we present the first such source discovered by the analysis of near real-time slew data., 4 pages, 4 figures, accepted for publication in A&A Letters

370. Optical and X-ray early follow-up of ANTARES neutrino alerts

Author

A. Gleixner, Jörn Wilms, Th. Stolarczyk, C. Distefano, D. F. E. Samtleben, P. Migliozzi, S. Mangano, Guillaume Lambard, J.A. Martínez-Mora, H. van Haren, I. Al Samarai, A. Enzenhöfer, S. Loucatos, Christian Tamburini, A. Heijboer, C. Mueller, C. W. James, Thomas Eberl, Jürgen Brunner, C. Donzaud, S. Adrián-Martínez, D. Dornic, Stéphane Basa, Stefan Wagner, B. Vallage, Uli Katz, Jos Steijger, Maurizio Spurio, Ingo Kreykenbohm, Neil Gehrels, D. Drouhin, Gisela Anton, Ivan Dekeyser, R. Lahmann, A. Herrero, R. Bruijn, Annarita Margiotta, Tommaso Chiarusi, L. Caramete, A. Trovato, Daniele Vivolo, C. Vallée, M. de Jong, Michel André, D. Turpin, J. Schmid, S. Biagi, J. Hößl, L.A. Fusco, A. Moussa, G. De Bonis, A. Le Van Suu, M. Taiuti, C. Perrina, J. A. Kennea, V. Giordano, M. Neff, C. Hugon, M.C. Bouwhuis, Alain Klotz, F. Schüssler, S. Galatà, Dominique Lefèvre, M. Bou-Cabo, K. Roensch, J. Zúñiga, J. Carr, Oleg Kalekin, C. Pellegrino, J. Hofestädt, R. Bormuth, K. Fehn, C. Sieger, D. Kießling, R. Gracia-Ruiz, V. Bertin, K. Geyer, E. Leonora, Dominik Elsässer, P. Coyle, Juan José Hernández-Rey, F. Folger, C. Bogazzi, Séverine Martini, S. Schulte, T. Seitz, Jutta Schnabel, C. Tönnis, B. Baret, P.M. Kooijman, R. Coniglione, G.E. Păvălaş, E. Nezri, H. Costantini, A. Creusot, Yann Hello, C. Racca, M. Tselengidou, M. Ageron, A. Rostovtsev, Arnauld Albert, K. Graf, A. Dumas, S. Geißelsöder, V. Van Elewyck, Paolo Piattelli, A. Kouchner, M. Boer, Rainer Richter, A. Sánchez-Losa, J. Busto, Phil Evans, V. Kulikovskiy, Piera Sapienza, P. Fermani, M. Marcelin, Miguel Ardid, A. Capone, David Coward, D. Lattuada, M. Saldaña, A. Mathieu, V. Popa, Marco Circella, Anne Deschamps, Matteo Sanguineti, Carl W. Akerlof, Ivan Felis, E. Visser, J. P. Osborne, J-J. Aubert, WeiKang Zheng, Giorgio Riccobene, J.D. Zornoza, T. Pradier, M. Vecchi, Matthias Kadler, T. Michael, J. Barrios-Martí, Adrián Martínez, S., Ageron, M., Albert, A., Al Samarai, I., André, M., Anton, G., Ardid, M., Aubert, J. J., Baret, B., Barrios Martí, J., Basa, S., Bertin, V., Biagi, S., Bogazzi, C., Bormuth, R., Bou Cabo, M., Bouwhuis, M. C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Chiarusi, T., Circella, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Dekeyser, I., Deschamps, A., De Bonis, G., Distefano, C., Donzaud, C., Dornic, D., Drouhin, D., Dumas, A., Eberl, T., Elsässer, D., Enzenhöfer, A., Fehn, K., Felis, I., Fermani, P., Folger, F., Fusco, LUIGI ANTONIO, Galatà, S., Gay, P., Geißelsöder, S., Geyer, K., Giordano, V., Gleixner, A., Gracia Ruiz, R., Graf, K., Van Haren, H., Heijboer, A. J., Hello, Y., Hernández Rey, J. J., Herrero, A., Hößl, J., Hofestädt, J., Hugon, C., James, C. W., De Jong, M., Kadler, M., Kalekin, O., Katz, U., Kießling, D., Kooijman, P., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lambard, G., Lattuada, D., Lefèvre, D., Leonora, E., Loucatos, S., Mangano, S., Marcelin, M., Margiotta, Annarita, Martínez Mora, J. A., Martini, S., Mathieu, A., Michael, T., Migliozzi, P., Moussa, A., Mueller, C., Neff, M., Nezri, E., Pǎvǎlaş, G. E., Pellegrino, Carmelo, Perrina, C., Piattelli, P., Popa, V., Pradier, T., Racca, C., Riccobene, G., Richter, R., Roensch, K., Rostovtsev, A., Saldaña, M., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schmid, J., Schnabel, J., Schulte, S., Schüssler, F., Seitz, T., Sieger, C., Spurio, Maurizio, Steijger, J. J. M., Stolarczyk, T. h., Sánchez Losa, A., Taiuti, M., Tamburini, C., Trovato, A., Tselengidou, M., Tönnis, C., Turpin, D., Vallage, B., Vallée, C., Van Elewyck, V., Vecchi, M., Visser, E., Vivolo, D., Wagner, S., Wilms, J., Zornoza, J. D., Zúñiga, J., Klotz, A., Boer, M., Le Van Suu, A., Akerlof, C., Zheng, W., Evans, P., Gehrels, N., Kennea, J., Osborne, J. P., Coward, D. M., Institut d’Investigació per a la Gestió Integrada de Zones Costaneres (IGIC), Universitat Politècnica de València (UPV), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Groupe de Recherche en Physique des Hautes Energies (GRPHE), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, Laboratory of Applied Bioacoustics (LAB-UPC), Universidad Polytecnica de Cataluña (UPC), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Enrico Fermi - Dipartimento di Fisica, University of Pisa - Università di Pisa, Department of Physics [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Corpusculaire - Clermont-Ferrand (LPC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), National Institute for Subatomic Physics [Amsterdam] (NIKHEF), Faculteit Betawetenschappen, Universiteit Utrecht, Universiteit van Amsterdam (UvA), LTI, ENSA de Tanger, Département Recherches Subatomiques (DRS-IPHC), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Elettra Light source (ELETTRA), Sincrotrone Trieste S.C.p.A., Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), School of Physics, University of Western Australia, The University of Western Australia (UWA), Institut d'Investigació per a la Gestió Integrada de Zones Costaneres (IGIC), Laboratory of Applied Bioacoustics, Technical University of Catalonia, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Instituto de Física Corpuscular, Edificios Investigación de Paterna, CSIC - Universitat de València (IFIC), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INFN---Laboratori Nazionali del Sud (LNS), Via S. Sofia 62, 95123 Catania, Italy, National Institute for Subatomic Physics (NIKHEF), Istituto Nazionale di Fisica Nucleare, Sezione di Roma La Sapienza (INFN), Institute for Space Sciences, INFN---Sezione di Bologna, Viale Berti-Pichat 6/2, 40127 Bologna, Italy, INFN---Sezione di Bari, Via E. Orabona 4, 70126 Bari, Italy, Université du Sud Toulon-Var (USTV), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut fur Theoretische Physik und Astrophysik, Universitat Wurzburg, Emil-Fischer Str. 31, 97074 Wurzburg, Germany, INFN---Sezione di Catania, Via S. Sofia, 64, 95123, Catania, Italy, Royal Netherlands Institute for Sea Research (NIOZ), Istituto Nazionale di Fisica Nucleare, Sezione di Genova (INFN), Dr. Karl Remeis-Sternwarte, Astronomisches Institut, Universität Erlangen-Nuremberg, INFN -Sezione di Napoli, Via Cintia 80126 Napoli, Italy, Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institute for Theoretical and Experimental Physics (ITEP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), University of Michigan, Department of Astronomy, University of California, Department of Physics and Astronomy, NASA/Goddard Space Flight Center (NASA/GSFC), Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, U.S.A., University of Western Australia, Adrian-Martinez, S., Andre, M., Aubert, J. -J., Barrios-Marti, J., Bou-Cabo, M., Elsasser, D., Enzenhofer, A., Fusco, L. A., Galata, S., Geisselsoder, S., Gracia-Ruiz, R., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., Kiessling, D., Lefevre, D., Margiotta, A., Martinez-Mora, J. A., Pavalas, G. E., Pellegrino, C., Saldana, M., Schussler, F., Spurio, M., Stolarczyk, T., Sanchez-Losa, A., Tonnis, C., Vallee, C., Zuniga, J., Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire des technologies Innovantes [Tanger] (LTI), Ecole Nationale des Sciences Appliquées [Tanger] (ENSAT), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de Technologie de Colmar-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), Adrian-Martinez, S, Ageron, M, Albert, A, Al Samarai, I, Andre, M, Anton, G, Ardid, M, Aubert, Jj, Baret, B, Barrios-Marti, J, Basa, S, Bertin, V, Biagi, S, Bogazzi, C, Bormuth, R, Bou-Cabo, M, Bouwhuis, Mc, Bruijnk, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Chiarusi, T, Circella, M, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Dekeyser, I, Deschamps, A, Bonis, G, Distefano, C, Donzaud, C, Dornic, D, Drouhin, D, Dumas, A, Eberl, T, Elsasser, D, Enzenhofer, A, Fehn, K, Feis, I, Fermani, P, Folger, F, Fusco, La, Galata, S, Gay, P, Geisselsoder, S, Geyer, K, Giordano, V, Gleixner, A, Gracia-Ruiz, R, Graf, K, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Herrero, A, Hossl, J, Hofestadt, J, Hugon, C, James, Cw, De Jong, M, Kadler, M, Kalekin, O, Katz, U, Kiessling, D, Kooijman, P, Kouchner, A, Kreykenbohm, I, Kulikovskiy, V, Lahmann, R, Lambard, G, Lattuada, D, Lefevre, D, Leonora, E, Loucatos, S, Mangano, S, Marcelin, M, Margiotta, A, Martinez-Mora, Ja, Martini, S, Mathieu, A, Michael, T, Migliozzi, P, Moussa, A, Mueller, C, Neff, M, Nezri, E, Pavalas, Ge, Pellegrino, C, Perrina, C, Piattelli, P, Popa, V, Pradier, T, Racca, C, Riccobene, G, Richter, R, Roensch, K, Rostovtsev, A, Saldana, M, Samtleben, Dfe, Sanguinetiz, M, Sapienza, P, Schmid, J, Schnabel, J, Schulte, S, Schussler, F, Seitz, T, Sieger, C, Spurio, M, Steijger, Jjm, Stolarczyk, T, Sanchez-Losa, A, Taiuti, M, Tamburini, C, Trovato, A, Tselengidou, M, Tonnis, C, Turpin, D, Vallage, B, Vallee, C, Van Elewyck, V, Vecchi, M, Visser, E, Vivolo, D, Wagner, S, Wilms, J, Zornoza, Jd, Zuniga, J, Klotz, A, Boer, M, Le Van Suu, A, Akerlof, C, Zheng, W, Evans, P, Gehrels, N, Kennea, J, Osborne, Jp, and Coward, Dm

Subjects
HIGH-ENERGY NEUTRINOS, Active galactic nucleus, TELESCOPE, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Gamma ray burst experiments, 01 natural sciences, ICECUBE, Optical telescope, SEARCH, 0103 physical sciences, ROTSE-III, BURSTS, 010306 general physics, 010303 astronomy & astrophysics, FERMI-DETECTED BLAZARS, X-ray telescopes, High Energy Astrophysical Phenomena (astro-ph.HE), LIGHT CURVES, astro-ph.HE, Physics, Astronomy, Astronomy and Astrophysics, ASTROFÍSICA, Supernova, Neutrino detector, Neutrino astronomy, gamma ray burst experiment, FISICA APLICADA, gamma ray burst experiments, neutrino astronomy, EMISSION, SYSTEM, Transient (oscillation), Neutrino, Astrophysics - High Energy Astrophysical Phenomena, MATEMATICA APLICADA, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Event (particle physics)
Abstract

High-energy neutrinos could be produced in the interaction of charged cosmic rays with matter or radiation surrounding astrophysical sources. Even with the recent detection of extraterrestrial high-energy neutrinos by the IceCube experiment, no astrophysical neutrino source has yet been discovered. Transient sources, such as gamma-ray bursts, core-collapse supernovae, or active galactic nuclei are promising candidates. Multi-messenger programs offer a unique opportunity to detect these transient sources. By combining the information provided by the ANTARES neutrino telescope with information coming from other observa-tories, the probability of detecting a source is enhanced, allowing the possibility of identifying a neutrino progenitor from a single detected event. A method based on optical and X-ray follow-ups of high-energy neutrino alerts has been developed within the ANTARES collaboration. This method does not require any assumptions on the relation between neutrino and photon spectra other than time-correlation. This program, denoted as TAToO, triggers a network of robotic optical telescopes (TAROT and ROTSE) and the Swift-XRT with a delay of only a few seconds after a neutrino detection, and is therefore well-suited to search for fast transient sources. To identify an optical or X-ray counterpart to a neutrino signal, the images provided by the follow-up observations are analysed with dedicated pipelines. A total of 42 alerts with optical and 7 alerts with X-ray images taken with a maximum delay of 24 hours after the neutrino trigger have been analysed. No optical or X-ray counterparts associated to the neutrino triggers have been found, and upper limits on transient source magnitudes have been derived. The probability to reject the gamma-ray burst origin hypothesis has been computed for each alert., The authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung and Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Ciencia e Innovacion (MICINN), Prometeo of Generalitat Valenciana and MultiDark, Spain; Agence de l'Oriental and CNRST, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities. We gratefully acknowledge financial support from the OCEVU LabEx, France. PAE andJPO acknowledge support from the U.K. Space Agency.

371. The WASP Project and the SuperWASP Cameras

Author

Stephen R. Kane, Will Clarkson, B. Enoch, Coel Hellier, Ian Skillen, N. R. Parley, Carole A. Haswell, Alan Fitzsimmons, Robert Ryans, Barry Smalley, A. Evans, Keith Horne, Richard G. West, J. P. Osborne, Andrew Norton, Jonathan Irwin, T. A. Lister, Simon Hodgkin, Damian J. Christian, Francis P. Keenan, Rachel Street, Hans J. Deeg, David R. Anderson, Peter J. Wheatley, Don Pollacco, A. Collier Cameron, Pierre F. L. Maxted, D. M. Wilson, PPARC - Now STFC, and University of St Andrews. School of Physics and Astronomy

Subjects
Star, Data products, media_common.quotation_subject, Gravitational lensing experiment, FOS: Physical sciences, Field of view, Astrophysics, Data rate, Luminosity object transits, Wide-angle search, Observatory, Photmetry, Prospects, QB Astronomy, Galactic disk, Remote sensing, media_common, QB, Physics, Pixel, 2001 campaign, Astrophysics (astro-ph), Planets prototype wasp0, Astronomy and Astrophysics, Pegasus field, Photometry (astronomy), Space and Planetary Science, Sky, Data quality
Abstract

The SuperWASP Cameras are wide-field imaging systems sited at the Observatorio del Roque de los Muchachos on the island of La Palma in the Canary Islands, and the Sutherland Station of the South African Astronomical Observatory. Each instrument has a field of view of some ~482 square degrees with an angular scale of 13.7 arcsec per pixel, and is capable of delivering photometry with accuracy better than 1% for objects having V ~ 7.0 - 11.5. Lower quality data for objects brighter than V ~15.0 are stored in the project archive. The systems, while designed to monitor fields with high cadence, are capable of surveying the entire visible sky every 40 minutes. Depending on the observational strategy, the data rate can be up to 100GB per night. We have produced a robust, largely automatic reduction pipeline and advanced archive which are used to serve the data products to the consortium members. The main science aim of these systems is to search for bright transiting exo-planets systems suitable for spectroscopic followup observations. The first 6 month season of SuperWASP-North observations produced lightcurves of ~6.7 million objects with 12.9 billion data points., Comment: 42 pages, 2 plates, 5 figures PASP in press

372. Effect on the white cell count of contaminating cerebrospinal fluid with blood

Author

J P Osborne and B Pizer

Subjects
Pathology, medicine.medical_specialty, business.industry, Infant, Newborn, Infant, Spinal Puncture, Infant newborn, humanities, Peripheral blood, Specimen Handling, Leukocyte Count, Blood, White Cell, Cerebrospinal fluid, Child, Preschool, Pediatrics, Perinatology and Child Health, Retrospective analysis, Humans, Medicine, Child, business, Research Article, Cerebrospinal Fluid, Retrospective Studies
Abstract

Retrospective analysis of heavily blood-stained cerebrospinal fluid shows that there are fewer white cells found in this fluid than would be expected by calculations using the peripheral blood red to white cell ratio. This phenomenon may disguise a true leucocytosis.

Published
1981

373. Forehead plaque: a presenting skin sign in tuberous sclerosis

Author

W Schutt, A E Fryer, and J P Osborne

Subjects
Male, Pathology, medicine.medical_specialty, integumentary system, business.industry, Genetic counseling, fungi, Infant, food and beverages, Angiofibroma, medicine.disease, Tuberous sclerosis, medicine.anatomical_structure, Tuberous Sclerosis, Pediatrics, Perinatology and Child Health, Forehead, Humans, Medicine, Female, business, Skin, Research Article
Abstract

The forehead plaque can be the earliest skin manifestation of tuberous sclerosis and its presence may lead to early diagnosis and appropriate genetic counselling.

Published
1987

374. Variable stars and galaxies

Author

R. Cole and J. P. Osborne

Subjects
Physics, Luminous infrared galaxy, Multidisciplinary, Spiral galaxy, Bulge, Surface brightness fluctuation, Elliptical galaxy, Astrophysics, Disc, Dwarf galaxy, Luminosity function (astronomy)
Published
1980

375. Terbutaline and Ketotifen in Cold Urticaria in a Child

Author

J P Osborne and J A Edge

Subjects
Ketotifen, Urticaria, business.industry, Terbutaline, General Medicine, Cold urticaria, medicine.disease, Histamine Release, 030227 psychiatry, Cold Temperature, 03 medical and health sciences, 0302 clinical medicine, Immunology, medicine, Humans, Female, 030212 general & internal medicine, Child, business, Research Article, medicine.drug
Published
1989

376. Tuberous sclerosis: a large family with no history of seizures or mental retardation

Author

J P Osborne, R Tan, D C Siggers, and A E Fryer

Subjects
Adult, Male, Pediatrics, medicine.medical_specialty, business.industry, fungi, food and beverages, Mentally retarded, medicine.disease, Pedigree, Tuberous sclerosis, Seizures, Tuberous Sclerosis, Intellectual Disability, Genetics, medicine, Humans, Female, business, Genetics (clinical), Research Article
Abstract

A family is reported where tuberous sclerosis has probably affected five generations, but where none of the members has been mentally retarded and there is no history of seizures.

Published
1987

377. A Multimessenger Picture of the Flaring Blazar TXS 0506+056: Implications for High-energy Neutrino Emission and Cosmic-Ray Acceleration.

Author

A. Keivani, K. Murase, M. Petropoulou, D. B. Fox, S. B. Cenko, S. Chaty, A. Coleiro, J. J. DeLaunay, S. Dimitrakoudis, P. A. Evans, J. A. Kennea, F. E. Marshall, A. Mastichiadis, J. P. Osborne, M. Santander, A. Tohuvavohu, and C. F. Turley

Subjects
SOLAR neutrinos, SOLAR flares, BL Lacertae objects, COSMIC rays, PARTICLE acceleration
Abstract

Detection of the IceCube-170922A neutrino coincident with the flaring blazar TXS 0506+056, the first and only ∼3σ high-energy neutrino source association to date, offers a potential breakthrough in our understanding of high-energy cosmic particles and blazar physics. We present a comprehensive analysis of TXS 0506+056 during its flaring state, using newly collected Swift, NuSTAR, and X-shooter data with Fermi observations and numerical models to constrain the blazar’s particle acceleration processes and multimessenger (electromagnetic (EM) and high-energy neutrino) emissions. Accounting properly for EM cascades in the emission region, we find a physically consistent picture only within a hybrid leptonic scenario, with γ-rays produced by external inverse-Compton processes and high-energy neutrinos via a radiatively subdominant hadronic component. We derive robust constraints on the blazar’s neutrino and cosmic-ray emissions and demonstrate that, because of cascade effects, the 0.1–100 keV emissions of TXS 0506+056 serve as a better probe of its hadronic acceleration and high-energy neutrino production processes than its GeV–TeV emissions. If the IceCube neutrino association holds, physical conditions in the TXS 0506+056 jet must be close to optimal for high-energy neutrino production, and are not favorable for ultrahigh-energy cosmic-ray acceleration. Alternatively, the challenges we identify in generating a significant rate of IceCube neutrino detections from TXS 0506+056 may disfavor single-zone models, in which γ-rays and high-energy neutrinos are produced in a single emission region. In concert with continued operations of the high-energy neutrino observatories, we advocate regular X-ray monitoring of TXS 0506+056 and other blazars in order to test single-zone blazar emission models, clarify the nature and extent of their hadronic acceleration processes, and carry out the most sensitive possible search for additional multimessenger sources. [ABSTRACT FROM AUTHOR]

Published
2018
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378. What We Learn from the X-Ray Grating Spectra of Nova SMC 2016.

Author

M. Orio, J.-U. Ness, A. Dobrotka, E. Gatuzz, N. Ospina, E. Aydi, E. Behar, D. A. H. Buckley, S. Ciroi, M. Della Valle, M. Hernanz, M. Henze, J. P. Osborne, K. L. Page, T. Rauch, G. Sala, S. Starrfield, R. E. Williams, C. E. Woodward, and P. Zemko

Subjects
MAGELLANIC clouds, DWARF galaxies, GALAXIES, WHITE dwarf stars, DWARF stars
Abstract

Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between days 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera, and the Low Energy Transmission Grating on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon, and sulfur on day 39, and oxygen, nitrogen, and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blueshifted, by about 1800 km s−1 on day 39 and up to 2100 km s−1 in the following observations. Spectral lines attributed to low-ionization potential transitions in the interstellar medium are also observed. Assuming the distance to the Small Magellanic Cloud, the bolometric luminosity exceeded the Eddington level for at least three months. A preliminary analysis with atmospheric models indicates an effective temperature of around 700,000 K on day 39, peaking at the later dates in the 850,000–900,000 K range, as expected for a ≃1.25 M⊙ WD. We suggest a possible classification as an oxygen–neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show a large, aperiodic flux variability, which is not associated with spectral variability. We detected red noise, but did not find periodic or quasiperiodic modulations. [ABSTRACT FROM AUTHOR]

Published
2018
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379. The Temporal Development of Dust Formation and Destruction in Nova Sagittarii 2015#2 (V5668 SGR): A Panchromatic Study.

Author

R. D. Gehrz, A. Evans, C. E. Woodward, L. A. Helton, D. P. K. Banerjee, M. K. Srivastava, N. M. Ashok, V. Joshi, S. P. S. Eyres, Joachim Krautter, N. P. M. Kuin, K. L. Page, J. P. Osborne, G. J. Schwarz, D. P. Shenoy, S. N. Shore, S. G. Starrfield, and R. M. Wagner

Subjects
AMORPHOUS carbon, AMORPHOUS substances, X-ray diffraction, ASTROPHYSICS, DWARF galaxies
Abstract

We present 5–28 μm SOFIA FORECAST spectroscopy complemented by panchromatic X-ray through infrared observations of the CO nova V5668 Sgr documenting the formation and destruction of dust during ∼500 days following outburst. Dust condensation commenced by 82 days after outburst at a temperature of ∼1090 K. The condensation temperature indicates that the condensate was amorphous carbon. There was a gradual decrease of the grain size and dust mass during the recovery phase. Absolute parameter values given here are for an assumed distance of 1.2 kpc. We conclude that the maximum mass of dust produced was 1.2 × 10−7M⊙ if the dust was amorphous carbon. The average grain radius grew to a maximum of ∼2.9 μm at a temperature of ∼720 K around day 113 when the shell visual optical depth was τv ∼ 5.4. Maximum grain growth was followed by a period of grain destruction. X-rays were detected with Swift from day 95 to beyond day 500. The Swift X-ray count rate due to the hot white dwarf peaked around day 220, when its spectrum was that of a kT = 35 eV blackbody. The temperature, together with the supersoft X-ray turn-on and turn-off times, suggests a white dwarf mass of ∼1.1 M⊙. We show that the X-ray fluence was sufficient to destroy the dust. Our data show that the post-dust event X-ray brightening is not due to dust destruction, which certainly occurred, as the dust is optically thin to X-rays. [ABSTRACT FROM AUTHOR]

Published
2018
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380. POSTOPERATIVE HYPOGLYCAEMIA IN SMALL CHILDREN

Author

J. P. Osborne and S. Ware

Subjects
Blood Glucose, medicine.medical_specialty, Time Factors, Postoperative recovery, Hypoglycemia, Anesthesia, General, Growth hormone, Postoperative Complications, medicine, Humans, General Environmental Science, Postoperative Care, business.industry, General Engineering, Infant, Newborn, Small children, Infant, General Medicine, Fasting, Surgical procedures, medicine.disease, Infant newborn, Surgery, Food, Child, Preschool, Growth Hormone, General Earth and Planetary Sciences, business, Research Article
Abstract

Six of 57 children under 4 years old became hypoglycaemic during postoperative recovery from various surgical procedures. Fluids either by mouth or intravenously did not always prevent this. Children at risk could not be predicted on the basis of age or weight-for-age. Small children should be fed as soon as practicable after operations, preferably with milk.

Published
1977

381. 178: 'Urinary Enzymes in Neonates after Asphyxia and during Gentamycin therapy'

Author

J P Osborne, S M Tucker, and J W Scopes

Subjects
Asphyxia, medicine.medical_specialty, Creatinine, biology, business.industry, Urinary system, Acid phosphatase, Physiology, Urine, medicine.disease, Surgery, Perinatal asphyxia, Excretion, chemistry.chemical_compound, chemistry, Pediatrics, Perinatology and Child Health, biology.protein, medicine, medicine.symptom, business, Feces
Abstract

Two β-Glycosidases, N-Acetyl-β-Glucosaminidase (N.A.G.), and β-Galactosidase (G.A.L.), and Acid Phosphatase (A.P.) have been estimated fluorimetrically in the urine of neonates to detect renal damage and the results expressed per m.mole urinary creatinine. Bag urines were collected, but to minimise contamination were discarded if faeces were passed simultaneously. A.P. is less affected by contamination than are G.A.L. or N.A.G.. There is no sex difference in the excretion of A.P. N.A.G. and G.A.L. can be stored ae 4°C before estimation for more than one month;A.P. should be estimated within four days. N.A.G. levels were raised in three cases of perinatal asphyxia and normal in one. Acute asphyxia in two cases did not cause any elevated enzyme levels. G.A.L. was raised in only one of the three cases while A.P. was raised once only in the same case. These results support the theory that acute asphyxia does not damage the renal tubules, while more prolonged asphyxia may. Two neonates have been studied during treatment with Gentamycin. N.A.G. levels are markedly raised during treatment - in one case eight times higher than pre-treatment levels within 24 hours. G.A.L. was intermittently raised and A.P. was not raised during treatment. The consistently raised levels of N.A.G. during Gentamycin therapy in neonates is suggestive of renal tubular cell dysfunction. We gratefully acknowledge the financial assistance of the Research Endowments Fund of St.Thomas' Hospital.

Published
1976

382. The discovery of the 2 hour modulated X-ray source EXO 033319-2554.2, an AM Herculis system

Author

G. Tagliaferri, Paolo Giommi, J. P. Osborne, Lorella Angelini, and Luigi Stella

Subjects
Physics, AM Herculis, Stars, Space and Planetary Science, Binary star, Magnitude (astronomy), Phase (waves), X-ray binary, White dwarf, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve
Abstract

The discovery of EXO 033319-2554.2, a soft X-ray source modulated at a period of about 128 minutes, is reported. The bright part of the cycle lasts 0.55 in phase and is cut by an eclipse-like feature lasting eight minutes, with unresolved ingress and egress 0.13 after maximum intensity. The soft X-ray color requires blackbody temperatures less than 25 eV. The optical counterpart has a magnitude m(v) of roughly 18.5. These data imply that the object is an AM Her system. 31 references.

Published
1988

383. A new soft X-ray mode in the AM Herculis object E2003 + 225

Author

Philip D. Charles, Klaus Beuermann, Aldo Treves, Laura Maraschi, J. P. Osborne, and Koji Mukai

Subjects
Physics, Radiation flux, AM Herculis, Space and Planetary Science, Binary star, Flux, Astronomy, Astronomy and Astrophysics, Astrophysics, Luminous intensity, Light curve, Electromagnetic radiation, Intensity (physics)
Abstract

Exosat observations of the AM Her object E2003 + 225 made in June and September 1985, are presented together with optical and ultraviolet observations. The averages of soft X-ray count rate doubled between October 1983 and June 1985; the simultaneously measured V band intensity fell by a factor of 3 and the UV flux by 20 percent. The medium-energy X-ray flux did not increase significantly. In September 1985, E2003 + 225 was observed to have a radically different soft X-ray light curve from that seen previously, but an average intensity similar to that of June 1985. The new soft X-ray light curve showed two similar peaks and two unequal minima separated by half a period. The optical light curve observed 2 days earlier showed no major change in shape. These observations provide a serious challenge to the standard model of AM Her objects. 18 references.

Published
1987

384. An X-ray flare from a B9 + post-T Tauri star system in the field of the Seyfert Galaxy III ZW 2

Author

Roberto Pallavicini, P. Giommi, G. Tagliaferri, Lorella Angelini, and J. P. Osborne

Subjects
Physics, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve, Galaxy, Astronomical spectroscopy, law.invention, T Tauri star, Space and Planetary Science, law, Binary star, Late-type star, Visual binary, Flare
Abstract

The serendipitous detection of X-ray emission from the visual binary HD 560, consisting of a B-type primary and a later-type secondary, is reported. This system was seen in the field of the Seyfert type I galaxy III Zw 2, which was observed four times by Exosat. During one of these observations, the serendipitous source was observed to flare in both low-energy and medium-energy experiments. It is shown here that the observed variability was entirely due to the serendipitous source. It is argued that virtually all of the X-ray flux from the binary came from this late-type component, and that this component is probably a post-T Tauri star. 33 references.

Published
1988

385. X-ray, ultraviolet, and optical observations of the intermediate polar FO Aquarii (H2215-086)

Author

D. de Martino, E. G. Tanzi, L. Maraschi, Tomaso Belloni, C. del Gratta, Jean-Marc Bonnet-Bidaud, M. Mouchet, Koji Mukai, J. P. Osborne, Aldo Treves, Robin H. D. Corbet, and L. Chiappetti

Subjects
Physics, Rotation period, Sideband, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, Astronomy, Astronomy and Astrophysics, Astrophysics, Ephemeris, Light curve, Intermediate polar, Space and Planetary Science, Binary star, Astrophysics::Solar and Stellar Astrophysics, Dwarf nova
Abstract

An extensive set of quasi-simultaneous, multiwavelength observations of the intermediate polar FO Aqr (H2215-086) obtained in 1983-1985 with the Exosat and IUE satellites and from La Palma Observatory are presented. The rotational 21 minute period and sideband periods due to beating with the orbital modulation are observed in the optical band and in X-rays. In particular, it is noticeable that an unusual sideband frequency at Omega(rot) + 2 Omega(orb) is present in X-rays. Variability of the spectrum with the rotation period is detected, which can be interpreted as modulation by an absorbing envelope. A possible improvement to the current orbital ephemeris, based on photometric data, is also presented. 42 refs.

Published
1989

386. EXOSAT and IUE observations of SW UMa during superoutburst

Author

Paula Szkody, J. P. Osborne, and B. J. M. Hassall

Subjects
Physics, Accretion rate, Stars, Space and Planetary Science, Thick disk, White dwarf, Astronomy, Astronomy and Astrophysics, Astrophysics, Variable star, Light curve, Stellar evolution, Dwarf nova
Abstract

IUE and Exosat observations obtained during the March 1986 superoutburst of the SU UMa type dwarf nova SW UMa are presented. The observations show the presence of a hot, extensive, optically thick disk. The UV fluxes show an increase of 1000 over the quiescent values, implying a large increase in mass accretion rate. The Exosat obserations show an increase in the soft X-ray count rate by a factor of 44 over quiescence, while the medium-energy flux remains undetected. The most surprising result is that the softness ratio in superoutburst is similar to the quiescent value of 0.3. No variation at the orbital or spin periods or at the superhump period are evident in the superoutburst X-ray data. A transient variation is observed at 5.1 minutes similar to that observed in the optical a few days after the X-ray observations.

Published
1988

387. Points: Cold comfort for hot children

Author

J P Osborne

Subjects
World Wide Web, Computer science, Correspondence, General Engineering, General Earth and Planetary Sciences, General Medicine, Data science, General Environmental Science
Published
1983

388. M31N 2008-12a—THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION.

Author

M. J. Darnley, M. Henze, M. F. Bode, I. Hachisu, M. Hernanz, K. Hornoch, R. Hounsell, M. Kato, J.-U. Ness, J. P. Osborne, K. L. Page, V. A. R. M. Ribeiro, P. Rodríguez-Gil, A. W. Shafter, M. M. Shara, I. A. Steele, S. C. Williams, A. Arai, I. Arcavi, and E. A. Barsukova

Subjects
NOVAE (Astronomy), WHITE dwarf stars, ANDROMEDA Galaxy, OPTICAL spectroscopy, BINARY stars, CATACLYSMIC variable stars, M stars
Abstract

The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground- and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swift observatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28 ± 0.12 UT. The 2013–2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s−1, possibly collimated outflows. Photometric and spectroscopic observations of the eruption provide strong evidence supporting a red giant donor. An apparently stochastic variability during the early supersoft X-ray phase was comparable in amplitude and duration to past eruptions, but the 2013 and 2015 eruptions show evidence of a brief flux dip during this phase. The multi-eruption Swift/XRT spectra show tentative evidence of high-ionization emission lines above a high-temperature continuum. Following Henze et al. (2015a), the updated recurrence period based on all known eruptions is days, and we expect the next eruption of M31N 2008-12a to occur around 2016 mid-September. [ABSTRACT FROM AUTHOR]

Published
2016
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389. PAN-CHROMATIC OBSERVATIONS OF THE RECURRENT NOVA LMC 2009a (LMC 1971b).

Author

M. F. Bode, M. J. Darnley, A. P. Beardmore, J. P. Osborne, K. L. Page, F. M. Walter, J. Krautter, A. Melandri, J.-U. Ness, T. J. O’Brien, M. Orio, G. J. Schwarz, M. M. Shara, and S. Starrfield

Subjects
SIMULTANEITY (Physics), ELECTROMAGNETIC waves, VACUUM tubes, IONIZING radiation, FLUOROSCOPY
Abstract

Nova LMC 2009a is confirmed as a recurrent nova (RN) from positional coincidence with nova LMC 1971b. The observational data set is one of the most comprehensive for any Galactic or extragalactic RN: optical and near-IR photometry from outburst until over 6 years later; optical spectra for the first 6 months, and Swift satellite ultraviolet (UV) and X-ray observations from 9 days to almost 1 year post-outburst. We find MV = −8.4 ± 0.8r ± 0.7s and expansion velocities between 1000 and 4000 km s−1. Coronal line emission before day 9 indicates shocks in the ejecta. Strengthening of He iiλ4686 preceded the emergence of the super-soft source (SSS) in X-rays at ∼63–70 days, which was initially very variable. Periodic modulations, P = 1.2 days, most probably orbital in nature, were evident in the UV and optical from day 43. Subsequently, the SSS shows an oscillation with the same period but with a delay of 0.28P. The progenitor system has been identified; the secondary is most likely a sub-giant feeding a luminous accretion disk. Properties of the SSS infer a white dwarf (WD) mass 1.1 M⊙ ≲ MWD ≲ 1.3 M⊙. If the accretion occurs at a constant rate, yr−1 is needed, consistent with nova models for an inter-eruption interval of 38 years, low outburst amplitude, progenitor position in the color–magnitude diagram, and spectral energy distribution at quiescence. We note striking similarities between LMC 2009a and the Galactic nova KT Eri, suggesting that KT Eri is a candidate RN. [ABSTRACT FROM AUTHOR]

Published
2016
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390. The LOFT mission concept: a status update

Author

Feroci, M, Bozzo, E, Brandt, S, Hernanz, M, Van Der Klis, M, Liu, L, Orleanski, P, Pohl, M, Santangelo, A, Schanne, S, Stella, L, Takahashi, T, Tamura, H, Watts, A, Wilms, J, Zane, S, Zhang, S, Bhattacharyya, S, Agudo, I, Ahangarianabhari, M, Albertus, C, Alford, M, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Artigues, B, Atteia, J, Azzarello, P, Bakala, P, Ballantyne, Dr, Baldazzi, G, Baldo, M, Balman, S, Barbera, M, Van Baren, C, Barret, D, Baykal, A, Begelman, M, Behar, E, Behar, O, Belloni, T, Bellutti, P, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bode, M, Bodin, P, Bombaci, I, Bonnet Bidaud, J, Borghi, G, Boutloukos, S, Bouyjou, F, Bradley, L, Braga, J, Briggs, Ms, Brown, E, Buballa, M, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jorgensen, C, Cackett, E, Cadoux, Fr, Cais, P, Caliandro, Ga, Campana, R, Campana, S, Cao, X, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, Aj, Cavazzuti, E, Cavechi, Y, Celestin, S, Cerda-Duran, P, Chakrabarty, D, Chamel, N, Chateau, F, Chen, C, Chen, Y, Chenevez, J, Chernyakova, M, Coker, J, Cole, R, Collura, A, Coriat, M, Cornelisse, R, Costamante, L, Cros, A, Cui, W, Cumming, A, Cusumano, G, Czerny, B, D'Ai, A, D'Ammando, F, D'Elia, V, Dai, Z, Del Monte, E, De Luca, A, De Martino, D, Dercksen, Jpc, De Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Degenaar, N, Den Herder, Jw, Diebold, S, Di Salvo, T, Dong, Y, Donnarumma, I, Doroshenko, V, Doyle, G, Drake, Sa, Durant, M, Emmanoulopoulos, D, Enoto, T, Erkut, Mh, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, Favre, Y, Feldman, C, Fender, R, Feng, H, Ferrari, V, Ferrigno, C, Ficorella, F, Finger, M, Finger, Mh, Fraser, Gw, Frericks, M, Fullekrug, M, Fuschino, F, Gabler, M, Galloway, Dk, Galvez Sanchez, Jl, Gandhi, P, Gao, Z, Garcia-Berro, E, Gendre, B, Gevin, O, Gezari, S, Giles, Ab, Gilfanov, M, Giommi, P, Giovannini, G, Giroletti, M, Gogus, E, Goldwurm, A, Goluchova, K, Gotz, D, Gou, L, Gouiffes, C, Grandi, P, Grassi, M, Greiner, J, Grinberg, V, Groot, P, Gschwender, M, Gualtieri, L, Guedel, M, Guidorzi, C, Guy, L, Haas, D, Haensel, P, Hailey, M, Hamuguchi, K, Hansen, F, Hartmann, Dh, Haswell, Ca, Hebeler, K, Heger, A, Hempel, M, Hermsen, W, Homan, J, Hornstrup, A, Hudec, R, Huovelin, J, Huppenkothen, D, Inam, Sc, Ingram, A, In'Tzand, Jjm, Israel, G, Iwasawa, K, Izzo, L, Jacobs, Hm, Jetter, F, Johannsen, T, Jenke, Pa, Jonker, P, Jose, J, Kaaret, P, Kalamkar, M, Kalemci, E, Kanbach, G, Karas, V, Karelin, D, Kataria, D, Keek, L, Kennedy, T, Klochkov, D, Kluzniak, W, Koerding, E, Kokkotas, K, Komossa, S, Korpela, S, Kouveliotou, C, Kowalski, Af, Kreykenbohm, I, Kuiper, Lm, Kunneriath, D, Kurkela, A, Kuvvetli, I, La Franca, F, Labanti, C, Lai, D, Lamb, Fk, Lachaud, C, Laubert, Pp, Lebrun, F, Li, X, Liang, E, Limousin, O, Lin, D, Linares, M, Linder, D, Lodato, G, Longo, F, Lu, F, Lund, N, Maccarone, Tj, Macera, D, Maestre, S, Mahmoodifar, S, Maier, D, Malcovati, P, Malzac, J, Malone, C, Mandel, I, Mangano, V, Manousakis, A, Marelli, M, Margueron, J, Marisaldi, M, Markoff, Sb, Markowitz, A, Marinucci, A, Martindale, A, Martinez, G, Mchardy, Im, Medina-Tanco, G, Mehdipour, M, Melatos, A, Mendez, M, Mereghetti, S, Migliari, S, Mignani, R, Michalska, M, Mihara, T, Miller, Mc, Miller, Jm, Mineo, T, Miniutti, G, Morsink, S, Motch, C, Motta, S, Mouchet, M, Mouret, G, Mulacova, J, Muleri, F, Munoz-Darias, T, Negueruela, I, Neilsen, J, Neubert, T, Norton, Aj, Nowak, M, Nucita, A, O'Brien, P, Oertel, M, Olsen, Peh, Orienti, M, Orio, M, Orlandini, M, Osborne, Jp, Osten, R, Ozel, F, Pacciani, L, Paerels, F, Paltani, S, Paolillo, M, Papadakis, I, Papitto, A, Paragi, Z, Paredes, Jm, Patruno, A, Paul, B, Pederiva, F, Perinati, E, Pellizzoni, A, Penacchioni, Av, Peretz, U, Perez, Ma, Perez-Torres, M, Peterson, Bm, Petracek, V, Picciotto, A, Piemonte, C, Pittori, C, Pons, J, Portell, J, Possenti, A, Postnov, K, Poutanen, J, Prakash, M, Prandoni, I, Le Provost, H, Psaltis, D, Pye, J, Qu, J, Rambaud, D, Ramon, P, Ramsay, G, Rapisarda, M, Rachevski, A, Rashevskaya, I, Ray, Ps, Rea, N, Reddy, S, Reig, P, Reina Aranda, M, Remillard, R, Reynolds, C, Rezzolla, L, Ribo, M, De La Rie, R, Riggio, A, Rios, A, Rischke, Dh, Rodriguez-Gil, P, Rodriguez, J, Rohlfs, R, Romano, P, Rossi, Emr, Rozanska, A, Rousseau, A, Rudak, B, Russell, Dm, Ryde, F, Sabau-Graziati, L, Sakamoto, T, Sala, G, Salvaterra, R, Salvetti, D, Sanna, A, Sandberg, J, Savolainen, T, Scaringi, S, Schaffner-Bielich, J, Schatz, H, Schee, J, Schmid, C, Serino, M, Shakura, N, Shore, S, Schnittman, Jd, Schneider, R, Schwenk, A, Schwope, Ad, Sedrakian, A, Seyler, J, Shearer, A, Slowikowska, A, Sims, M, Smith, A, Smith, Dm, Smith, Pj, Sobolewska, M, Sochora, V, Soffitta, P, Soleri, P, Song, L, Spencer, A, Stamerra, A, Stappers, B, Staubert, R, Steiner, Aw, Stergioulas, N, Stevens, Al, Stratta, G, Strohmayer, Te, Stuchlik, Z, Suchy, S, Suleimanov, V, Tamburini, F, Tauris, T, Tavecchio, F, Tenzer, C, Thielemann, Fk, Tiengo, A, Tolos, L, Tombesi, F, Tomsick, J, Torok, G, Torrejon, Jm, Torres, Df, Torresi, E, Tramacere, A, Traulsen, I, Trois, A, Turolla, R, Turriziani, S, Typel, S, Uter, P, Uttley, P, Vacchi, A, Varniere, P, Vaughan, S, Vercellone, S, Vietri, M, Vincent, Fh, Vrba, V, Walton, D, Wang, J, Wang, Z, Watanabe, S, Wawrzaszek, R, Webb, N, Weinberg, N, Wende, H, Wheatley, P, Wijers, R, Wijnands, R, Wille, M, Wilson-Hodge, Ca, Winter, B, Walk, Sj, Wood, K, Woosley, Se, Wu, X, Xiao, L, Xu, R, Yu, W, Yuan, F, Yuan, W, Yuan, Y, Zampa, G, Zampa, N, Zampieri, L, Zdunik, L, Zdziarski, A, Zech, A, Zhang, B, Zhang, C, Zingale, M, Zorzi, N, Zwart, F, High Energy Astrophys. & Astropart. Phys (API, FNWI), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Icahn School of Medicine at Mount Sinai [New York] (MSSM), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Scienze e Tecnologie Chimiche, Università degli Studi di Roma Tor Vergata [Roma], Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Centre Interdisciplinaire de Nanoscience de Marseille (CINaM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Tampere University of Technology [Tampere] (TUT), University of Maryland [College Park], University of Maryland System, Department of Biological Sciences [Mississippi], University of Southern Mississippi (USM), School of Physics and Astronomy [Southampton], University of Southampton, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Università di Roma La Sapienza, Università di Roma Tor Vergata, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Swedish Institute of Space Physics [Uppsala] (IRF), INAF - Osservatorio Astronomico di Brera (OAB), Department of Computer Sciences [Scheffield], University of Sheffield [Sheffield], Colgate University, Bibliothèque nationale de France (BnF), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), ARC Centre of Excellence for Environmental Decisions (ARC CEED), The University of Western Australia (UWA)-Australian National University (ANU)-University of Queensland [Brisbane]-Royal Melbourne Institute of Technology University (RMIT University)-School of BioSciences [Melbourne], Faculty of Science [Melbourne], University of Melbourne-University of Melbourne-Faculty of Science [Melbourne], University of Melbourne-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), Lund University [Lund], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse (AMIS), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), INAF - Osservatorio Astronomico di Cagliari (OAC), ELECTRONIQUE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), School of Geosciences, Monash University [Clayton], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université libre de Bruxelles (ULB), National Oceanography Centre [Southampton] (NOC), Dublin Institute for Advanced Studies (DIAS), Dublin City University [Dublin] (DCU), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Institut Parisien de Chimie Moléculaire (IPCM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center (CNITSEC), Department of Applied Mathematics and Computer Science [Lyngby] (DTU Compute), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), PCAS, Anton Pannekoek Institute for Astronomy, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), International Space Science Institute [Bern] (ISSI), Université Grenoble Alpes - UFR Médecine (UGA UFRM), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), CALVIN research group [Edinburgh], Institute of Perception, Action and Behaviour (IPAB), University of Edinburgh-University of Edinburgh, Department of Electronics and Electrical Engineering [Bath], University of Bath [Bath], United States Geological Survey [Reston] (USGS), Sr. PLM Consultant, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Dept Ind Engn & Informat Techonolgy, Università degli studi di Trieste = University of Trieste, Max-Planck-Institut für Extraterrestrische Physik (MPE), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Wisconsin Regional Primate Research Center, University of Wisconsin-Madison, SRON Netherlands Institute for Space Research (SRON), Opole University of Technology, University of Technology (Opole), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Radboud University [Nijmegen], NASA Goddard Space Flight Center (GSFC), Dept Fis Aplicada, Universidad de Granada = University of Granada (UGR), Victoria University [Melbourne], The Hong Kong Polytechnic University [Hong Kong] (POLYU), Chinese Academy of Sciences [Changchun Branch] (CAS), Department of Physics, Chemistry and Biology [Linköping] (IFM), Linköping University (LIU), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Centre de recherche en Biologie cellulaire de Montpellier (CRBM), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Zielona Góra, Department of Electronics and Computer Systems, Takushoku University, Instituto Nacional de Pesquisas da Amazônia (INPA), Università degli studi di Catania = University of Catania (Unict), Centre d'Ecologie et des Sciences de la COnservation (CESCO), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ecologie Alpine (LECA ), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS), HEPL, Solar Physics, Stanford University, Institut des Sciences Moléculaires de Marseille (ISM2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Columbia University [New York], Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Department of Anthropology [University of Arkansas], University of Arkansas [Fayetteville], Hu county ventre for disease control and prevention of Shaanxi province, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Istituto Nazionale di Fisica Nucleare (INFN), Institut Jean le Rond d'Alembert (DALEMBERT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Reading (UOR), Departamento de Matemática Aplicada, Universidade de Santiago de Compostela [Spain] (USC ), Osservatorio Astrofisico di Catania, Équipe Robotique et InteractionS (LAAS-RIS), Laboratoire d'analyse et d'architecture des systèmes (LAAS), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Centro Euro-Mediterraneo per i Cambiamenti Climatici [Bologna] (CMCC), Institut für Theoretische Physik, Universität Heidelberg [Heidelberg] = Heidelberg University, Augsburg Hospital, Leibniz-Institut für Astrophysik Potsdam (AIP), Daimler Chrysler AG (Daimler), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Montserrat Volcano Observatory (MVO), Institut Armand Frappier (INRS-IAF), Institut National de la Recherche Scientifique [Québec] (INRS)-Réseau International des Instituts Pasteur (RIIP), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], FICLIT, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Radioastronomie (MPIFR), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Christian-Albrechts-Universität zu Kiel (CAU), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Xinjiang Astronomical Observatory, Mitsubishi Electric Research Laboratories (MERL), Mitsubishi Research Institute, Inc., School of Urban and Regional Planning, University of Southern California (USC), National University of Defense Technology [China], Princeton University, Department of Microtechnology and Nanoscience (MC2), Chalmers University of Technology [Gothenburg, Sweden], Feroci, M., Bozzo, E., Brandt, S., Hernanz, M., van der Klis, M., Liu, L., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Zhang, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, E., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M., Brown, E., Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Cais, P., Caliandro, G., Campana, R., Campana, S., Cao, X., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, C., Chen, Y., Chenevez, J., Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Z., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J., Diebold, S., DI SALVO, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, H., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D., Gálvez Sanchez, J., Gandhi, P., Gao, Z., Garcia Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jenke, P., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A., Kreykenbohm, I., Kuiper, L., Kunneriath, D., Kurkela, A., Kuvvetli, I., La Franca, F., Labanti, C., Lai, D., Lamb, F., Lachaud, C., Laubert, P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., Mchardy, I., Medina Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Neubert, T., Norton, A., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A., Peretz, U., Perez, M., Perez Torres, M., Peterson, B., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, J., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Rudak, B., Russell, D., Ryde, F., Sabau Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J., Schneider, R., Schwenk, A., Schwope, A., Sedrakian, A., Seyler, J., Shearer, A., Slowikowska, A., Sims, M., Smith, A., Smith, D., Smith, P., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A., Stergioulas, N., Stevens, A., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Torresi, E., Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F., Vrba, V., Walton, D., Wang, J., Wang, Z., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Walk, S., Wood, K., Woosley, S., Wu, X., Xu, R., Yu, W., Yuan, F., Yuan, W., Yuan, Y., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, B., Zhang, C., Zingale, M., Zwart, F., University of Geneva [Switzerland], Eberhard Karls Universität Tübingen, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Graduate School of the Natural Science and Technology, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), School of BioSciences [Melbourne], University of Melbourne-University of Melbourne-Royal Melbourne Institute of Technology University (RMIT University)-University of Queensland [Brisbane]-Australian National University (ANU)-The University of Western Australia (UWA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Libre de Bruxelles [Bruxelles] (ULB), Dublin City University, Dublin 9, Ireland, Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center, Technical University of Denmark [Lyngby] (DTU), Université Grenoble Alpes (UGA), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Trieste, Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie Intégrative de la Cellule (I2BC), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Università degli Studi di Roma 'La Sapienza' [Rome], Radboud university [Nijmegen]-Radboud university [Nijmegen], Radboud university [Nijmegen], Universidad de Granada (UGR), Centre National de la Recherche Scientifique (CNRS), Centre de recherche en Biologie Cellulaire (CRBM), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Catania [Catania], Laboratoire d'Ecologie Alpine (LECA), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université du Littoral Côte d'Opale, Stanford University [Stanford], Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Università degli studi di Napoli Federico II, IFP Energies nouvelles (IFPEN), National Institute for Nuclear Physics (INFN), Institut Jean Le Rond d'Alembert (DALEMBERT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J), Ingénierie des Matériaux Polymères (IMP), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Centro Euro-Mediterraneo per i Cambiamenti Climatici (CMCC), Universität Heidelberg [Heidelberg], Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP)-Institut National de la Recherche Scientifique [Québec] (INRS), Università di Bologna [Bologna] (UNIBO), University of California [Berkeley], University of California-University of California, Universita degli Studi di Padova, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Chalmers University of Technology [Göteborg], Astronomy, Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa, Van Der Klis, M., Liu, L. -P., Zhang, S. -N., Atteia, J. -L., Ballantyne, D. R., Van Baren, C., Bellutti, P., Bonnet Bidaud, J. -M., Borghi, G., Briggs, M. S., Budtz-Jorgensen, C., Cadoux, F. R., Caliandro, G. A., Castro-Tirado, A. J., Cerda-Duran, P., Chateau, F., D'Ai, A., Dercksen, J. P. C., Den Herder, J. W., Di Salvo, T., Drake, S. A., Erkut, M. H., Ficorella, F., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Garcia-Berro, E., Giles, A. B., Goluchova, K., Gotz, D., Hartmann, D. H., Haswell, C. A., Inam, S. C., In'Tzand, J. J. M., Jacobs, H. M., Jenke, P. A., Jose, J., Kalamkar, M., Kowalski, A. F., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Markoff, S. B., Martinez, G., Mchardy, I. M., Medina-Tanco, G., Miller, M. C., Miller, J. M., Mulacova, J., Munoz-Darias, T., Norton, A. J., Olsen, P. E. H., Osborne, J. P., Paredes, J. M., Penacchioni, A. V., Perez, M. A., Perez-Torres, M., Peterson, B. M., Picciotto, A., Piemonte, C., Rachevski, A., Ray, P. S., De La Rie, R., Rischke, D. H., Rodriguez-Gil, P., Rossi, E. M. R., Russell, D. M., Sabau-Graziati, L., Schaffner-Bielich, J., Schnittman, J. D., Schwope, A. D., Seyler, J. -Y., Smith, D. M., Smith, P. J., Steiner, A. W., Stevens, A. L., Strohmayer, T. E., Thielemann, F. K., Torrejon, J. M., Torres, D. F., Vincent, F. H., Wilson-Hodge, C. A., Walk, S. J., Woosley, S. E., Xiao, L., Zorzi, N., Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université Montpellier 1 (UM1), Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Department of Psychiatry (Icahn School of Medicine at Mount Sinai) ( ISMMS ), Rutgers, The State University of New Jersey [New Brunswick] ( RUTGERS ), Institut fur Astronomie und Astrophysik, Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Kanazawa University ( KU ), Department of Earth Sciences, University of Oxford [Oxford], Centre Interdisciplinaire de Nanoscience de Marseille ( CINaM ), Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Tampere University of Technology [Tampere] ( TUT ), University of Southern Mississippi ( USM ), University of Southampton [Southampton], Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), Istituto Nazionale di Astrofisica ( INAF ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Osservatorio Astronomico di Brera ( INAF ), Bibliothèque nationale de France ( BnF ), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo ( IASF-Pa ), ARC Centre of Excellence for Environmental Decisions ( ARC CEED ), The University of Western Australia ( UWA ) -Australian National University ( ANU ) -University of Queensland [Brisbane]-RMIT University [Melbourne]-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies ( CoralCoE ), James Cook University ( JCU ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse ( AMIS ), PRES Université de Toulouse-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de synthèse organique ( DCSO ), École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Pathology, University of Alabama at Birmingham, University of Alabama at Birmingham Comprehensive Cancer Center, Birmingham, Alabama, INAF-Osservatorio di Cagliari, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique et Modèles Statistiques ( LPTMS ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Université Libre de Bruxelles [Bruxelles] ( ULB ), Ocean and Earth Sciences, National Oceanography Centre Southampton, Dublin Institute for advanced studies, 31 Fitzwilliam Place, Dublin 2, Ireland, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Institut Parisien de Chimie Moléculaire ( IPCM ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Chinese Academy of Sciences [Beijing] ( CAS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Applied Mathematics and Computer Science [Lyngby] ( DTU Compute ), Technical University of Denmark [Lyngby] ( DTU ), Institut für Astronomie und Astrophysik ( IAAT ), Anton Pannekoek Institute for Astronomy, University of Amsterdam, University of Cambridge [UK] ( CAM ), International Space Science Institute ( ISSI ), Université Grenoble Alpes - UFR Médecine ( UGA UFRM ), Université Grenoble Alpes ( UGA ), Institute of Perception, Action and Behaviour ( IPAB ), United States Geological Survey [Reston] ( USGS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Max-Planck-Institut für Extraterrestrische Physik ( MPE ), Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology ( MIT ), Institut de Physique du Globe de Paris ( IPGP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie Intégrative de la Cellule ( I2BC ), Université Paris-Sud - Paris 11 ( UP11 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Matériaux, ingénierie et science [Villeurbanne] ( MATEIS ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ) -Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ), University of Wisconsin-Madison [Madison], SRON Netherlands Institute for Space Research ( SRON ), University of Technology ( Opole ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Grp Fis Atmosfera, Ctr Andaluz Medio Ambiente CEAMA, Universidad de Granada ( UGR ), The Hong Kong Polytechnic University [Hong Kong] ( POLYU ), Chinese Academy of Sciences [Changchun Branch] ( CAS ), Department of Physics, Chemistry and Biology, Linköping University ( LIU ), Institut de Chimie des Substances Naturelles ( ICSN ), Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Nucléaire de Lyon ( IPNL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Erlangen Centre for Astroparticle Physics ( ECAP ), Friedrich-Alexander Universität Erlangen-Nürnberg ( FAU ), Centre de recherches de biochimie macromoléculaire ( CRBM ), Université Montpellier 1 ( UM1 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto Nacional de Pesquisas da Amazônia ( INPA ), Instituto Nacional de Pesquisas da Amazônia, Centre d'Ecologie et des Sciences de la COnservation ( CESCO ), Muséum National d'Histoire Naturelle ( MNHN ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Ecologie Alpine ( LECA ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physico-Chimie de l'Atmosphère ( LPCA ), Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique ( CNRS ), Institut des Sciences Moléculaires de Marseille ( ISM2 ), Aix Marseille Université ( AMU ) -Ecole Centrale de Marseille ( ECM ) -Centre National de la Recherche Scientifique ( CNRS ), Space Telescope Science Institute ( STSci ), IFP Energies nouvelles ( IFPEN ), Laboratoire de Biométrie et Biologie Evolutive ( LBBE ), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique ( Inria ) -Centre National de la Recherche Scientifique ( CNRS ), University of Arkansas, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste ( INFN, Sezione di Trieste ), National Institute for Nuclear Physics ( INFN ), Institut Jean Le Rond d'Alembert ( DALEMBERT ), Institut de Ciencies de l'Espai [Barcelona] ( ICE-CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), University of Reading ( UOR ), Universidade de Santiago de Compostela, Équipe Robotique et InteractionS ( LAAS-RIS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ), Ingénierie des Matériaux Polymères - Site INSA Lyon ( IMP ), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Jean Monnet [Saint-Étienne] ( UJM ) -Centre National de la Recherche Scientifique ( CNRS ), Leibniz-Institut für Astrophysik Potsdam ( AIP ), Daimler Chrysler AG ( Daimler ), Centre d'Etudes Nucléaires de Bordeaux Gradignan ( CENBG ), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Montserrat Volcano Observatory ( MVO ), Institut Armand Frappier ( INRS-IAF ), Institut National de la Recherche Scientifique [Québec] ( INRS ) -Réseau International des Instituts Pasteur ( RIIP ) -Institut Armand Frappier, Università di Bologna [Bologna] ( UNIBO ), Max-Planck-Institut für Radioastronomie, Argelander Institut für Astronomie, Bonn Universität [Bonn], Space Sciences Laboratory [Berkeley] ( SSL ), Christian-Albrechts-Universität zu Kiel ( CAU ), Universita degli Studi di Padova = University of Padua = Université de Padoue, APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, California Institute of Technology ( CALTECH ), Mitsubishi Electric Research Laboratories ( MERL ), Mitsubishi Electric Research Laboratories, Institute for Astronomy, University of Amsterdam, The Netherland, University of Southern California ( USC ), National University of Defense Technology [Changsha], Department of Microtechnology and Nanoscience ( MC2 ), Université Chalmers, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Nice Sophia Antipolis (UNS), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Den Herder, Jan-Willem A., Bautz, M., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Liu, L. P., Zhang, S. N., Atteia, J. L., Bonnet Bidaud, J. M., Castro Tirado, A. J., D'Aı, A., den Herder, J. W., Gálvez Sanchez, J. L., In't Zand, J. J. M., Nucita, Achille, Seyler, J. Y., Wilson Hodge, C. A., Baldazzi, Giuseppe, Fuschino, Fabio, Bianchi, Stefano, Casella, Piergiorgio, DE ROSA, Alessandra, Giovannini, Gabriele, LA FRANCA, Fabio, Marinucci, Andrea, Paredes, M. J., Schneider, Raffaella, Vietri, Mario, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), M., Feroci, E., Bozzo, S., Brandt, M., Hernanz, M., van der Kli, L. P., Liu, P., Orleanski, M., Pohl, A., Santangelo, S., Schanne, L., Stella, T., Takahashi, H., Tamura, A., Watt, J., Wilm, S., Zane, S. N., Zhang, S., Bhattacharyya, I., Agudo, M., Ahangarianabhari, C., Albertu, M., Alford, A., Alpar, D., Altamirano, L., Alvarez, L., Amati, C., Amoro, N., Andersson, A., Antonelli, A., Argan, R., Artigue, B., Artigue, J. L., Atteia, P., Azzarello, P., Bakala, D., Ballantyne, G., Baldazzi, M., Baldo, S., Balman, M., Barbera, C., van Baren, D., Barret, A., Baykal, M., Begelman, E., Behar, O., Behar, T., Belloni, F., Bernardini, G., Bertuccio, S., Bianchi, A., Bianchini, P., Binko, P., Blay, F., Bocchino, M., Bode, P., Bodin, I., Bombaci, J. M., Bonnet Bidaud, S., Boutlouko, F., Bouyjou, L., Bradley, J., Braga, M. S., Brigg, E., Brown, M., Buballa, N., Bucciantini, L., Burderi, M., Burgay, M., Bursa, C., Budtz Jørgensen, E., Cackett, F., Cadoux, P., Cai, G. A., Caliandro, R., Campana, S., Campana, X., Cao, F., Capitanio, J., Casare, P., Casella, A. J., Castro Tirado, E., Cavazzuti, Y., Cavechi, S., Celestin, P., Cerda Duran, D., Chakrabarty, N., Chamel, F., Château, C., Chen, Y., Chen, J., Chenevez, M., Chernyakova, J., Coker, R., Cole, A., Collura, M., Coriat, R., Cornelisse, L., Costamante, A., Cro, W., Cui, A., Cumming, G., Cusumano, B., Czerny, A., D'Aì, F., D'Ammando, V., D'Elia, Z., Dai, E., Del Monte, A., De Luca, D., De Martino, J. P. C., Dercksen, M., De Pasquale, A., De Rosa, M., Del Santo, S., Di Cosimo, N., Degenaar, J. W., den Herder, S., Diebold, T., Di Salvo, Y., Dong, I., Donnarumma, V., Doroshenko, G., Doyle, S. A., Drake, M., Durant, D., Emmanoulopoulo, T., Enoto, M. H., Erkut, P., Esposito, Y., Evangelista, A., Fabian, M., Falanga, Y., Favre, C., Feldman, R., Fender, H., Feng, V., Ferrari, C., Ferrigno, M., Finger, M. H., Finger, G. W., Fraser, M., Frerick, M., Fullekrug, F., Fuschino, M., Gabler, D. K., Galloway, J. L., Gálvez Sanchez, P., Gandhi, Z., Gao, E., Garcia Berro, B., Gendre, O., Gevin, S., Gezari, A. B., Gile, M., Gilfanov, P., Giommi, G., Giovannini, M., Giroletti, E., Gogu, A., Goldwurm, K., Goluchová, D., Götz, L., Gou, C., Gouiffe, P., Grandi, M., Grassi, J., Greiner, V., Grinberg, P., Groot, M., Gschwender, L., Gualtieri, M., Guedel, C., Guidorzi, L., Guy, D., Haa, P., Haensel, M., Hailey, K., Hamuguchi, F., Hansen, D. H., Hartmann, C. A., Haswell, K., Hebeler, A., Heger, M., Hempel, W., Hermsen, J., Homan, A., Hornstrup, R., Hudec, J., Huovelin, D., Huppenkothen, S. C., Inam, A., Ingram, J. J. M., In't Zand, G., Israel, K., Iwasawa, L., Izzo, H. M., Jacob, F., Jetter, T., Johannsen, P. A., Jenke, P., Jonker, J., Josè, P., Kaaret, K., Kalamkar, E., Kalemci, G., Kanbach, V., Kara, D., Karelin, D., Kataria, L., Keek, T., Kennedy, D., Klochkov, W., Kluzniak, E., Koerding, K., Kokkota, S., Komossa, S., Korpela, C., Kouveliotou, A. F., Kowalski, I., Kreykenbohm, L. M., Kuiper, D., Kunneriath, A., Kurkela, I., Kuvvetli, F., La Franca, C., Labanti, D., Lai, F. K., Lamb, C., Lachaud, P. P., Laubert, F., Lebrun, X., Li, E., Liang, O., Limousin, D., Lin, M., Linare, D., Linder, G., Lodato, F., Longo, F., Lu, N., Lund, T. J., Maccarone, D., Macera, S., Maestre, S., Mahmoodifar, D., Maier, P., Malcovati, J., Malzac, C., Malone, I., Mandel, V., Mangano, A., Manousaki, M., Marelli, J., Margueron, M., Marisaldi, S. B., Markoff, A., Markowitz, A., Marinucci, A., Martindale, G., Martínez, I. M., Mchardy, G., Medina Tanco, M., Mehdipour, A., Melato, M., Mendez, S., Mereghetti, S., Migliari, R., Mignani, M., Michalska, T., Mihara, M. C., Miller, J. M., Miller, T., Mineo, G., Miniutti, S., Morsink, C., Motch, S., Motta, M., Mouchet, G., Mouret, J., Mulačová, F., Muleri, T., Muñoz Daria, I., Negueruela, J., Neilsen, T., Neubert, A. J., Norton, M., Nowak, A., Nucita, P., O'Brien, M., Oertel, P. E. H., Olsen, M., Orienti, M., Orio, M., Orlandini, J. P., Osborne, R., Osten, F., Ozel, L., Pacciani, F., Paerel, S., Paltani, Paolillo, Maurizio, I., Papadaki, A., Papitto, Z., Paragi, J. M., Parede, A., Patruno, B., Paul, F., Pederiva, E., Perinati, A., Pellizzoni, A. V., Penacchioni, U., Peretz, M. A., Perez, M., Perez Torre, B. M., Peterson, V., Petracek, C., Pittori, J., Pon, J., Portell, A., Possenti, K., Postnov, J., Poutanen, M., Prakash, I., Prandoni, H., Le Provost, D., Psalti, J., Pye, J., Qu, D., Rambaud, P., Ramon, G., Ramsay, M., Rapisarda, A., Rashevski, I., Rashevskaya, P. S., Ray, N., Rea, S., Reddy, P., Reig, M., Reina Aranda, R., Remillard, C., Reynold, L., Rezzolla, M., Ribo, R., de la Rie, A., Riggio, A., Rio, D. H., Rischke, P., Rodríguez Gil, J., Rodriguez, R., Rohlf, P., Romano, E. M. R., Rossi, A., Rozanska, A., Rousseau, B., Rudak, D. M., Russell, F., Ryde, L., Sabau Graziati, T., Sakamoto, G., Sala, R., Salvaterra, D., Salvetti, A., Sanna, J., Sandberg, T., Savolainen, S., Scaringi, J., Schaffner Bielich, H., Schatz, J., Schee, C., Schmid, M., Serino, N., Shakura, S., Shore, J. D., Schnittman, R., Schneider, A., Schwenk, A. D., Schwope, A., Sedrakian, J. Y., Seyler, A., Shearer, A., Slowikowska, M., Sim, A., Smith, D. M., Smith, P. J., Smith, M., Sobolewska, V., Sochora, P., Soffitta, P., Soleri, L., Song, A., Spencer, A., Stamerra, B., Stapper, R., Staubert, A. W., Steiner, N., Stergioula, A. L., Steven, G., Stratta, T. E., Strohmayer, Z., Stuchlik, S., Suchy, V., Suleimanov, F., Tamburini, T., Tauri, F., Tavecchio, C., Tenzer, F. K., Thielemann, A., Tiengo, L., Tolo, F., Tombesi, J., Tomsick, G., Torok, J. M., Torrejon, D. F., Torre, E., Torresi, A., Tramacere, I., Traulsen, A., Troi, R., Turolla, S., Turriziani, S., Typel, P., Uter, P., Uttley, A., Vacchi, P., Varniere, S., Vaughan, S., Vercellone, M., Vietri, F. H., Vincent, V., Vrba, D., Walton, J., Wang, Z., Wang, S., Watanabe, R., Wawrzaszek, N., Webb, N., Weinberg, H., Wende, P., Wheatley, R., Wijer, R., Wijnand, M., Wille, C. A., Wilson Hodge, B., Winter, S. J., Walk, K., Wood, S. E., Woosley, X., Wu, R., Xu, W., Yu, F., Yuan, W., Yuan, Y., Yuan, G., Zampa, N., Zampa, L., Zampieri, L., Zdunik, A., Zdziarski, A., Zech, B., Zhang, C., Zhang, S., Zhang, M., Zingale, and F., Zwart

Subjects
X-ray timing, [ SDU.ASTR.GA ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Field of view, Astrophysics, 01 natural sciences, law.invention, law, Observatory, timing, 010303 astronomy & astrophysics, QB, Physics, microchannel plates. PROPORTIONAL COUNTER ARRAY, CALIBRATION, X-ray astronomy, Electronic, Optical and Magnetic Material, Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, X-ray detectors, Condensed Matter Physics, compact objects, X-ray spectroscopy, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], spectroscopy, Cosmic Vision, [ INFO ] Computer Science [cs], Silicon detector, Astrophysics::High Energy Astrophysical Phenomena, Condensed Matter Physic, Telescope, X-ray, Silicon detectors, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Electronic, [INFO]Computer Science [cs], Optical and Magnetic Materials, Spectral resolution, DETECTOR, ta115, X-ray astronomy, Silicon detectors, timing, spectroscopy, 010308 nuclear & particles physics, X-ray imaging, Applied Mathematic, Neutron star, QB460-466 Astrophysics, Large Observatory For x-ray Timing (LOFT), Large Area Detector (LAD), Wide Field Monitor (WFM), Large Area Silicon Drift Detectors (SDD), Gamma-ray burst
Abstract

The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, >8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission. © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

Published
2016

391. Gamma-ray burst science in the era of the Cherenkov Telescope Array

Author

Inoue, S., Granot, J., O'Brien, P. T., Asano, K., Bouvier, A., Carosi, A., Connaughton, V., Garczarczyk, M., Gilmore, R., Hinton, J., Inoue, Y., Ioka, K., Kakuwa, J., Markoff, S., Murase, K., Osborne, J. P., Otte, A. N., Starling, R., Tajima, H., Teshima, M., Toma, K., Wagner, S., R. A. M., Williams, D. A., Yamamoto, T., Yamazaki, R., Cta, Consortium, Acharya, B. S., Actis, M., Aghajani, T., Bissaldi, Elisabetta, High Energy Astrophys. & Astropart. Phys (API, FNWI), S., Inoue, J., Granot, P. T., O'Brien, K., Asano, A., Bouvier, A., Carosi, V., Connaughton, M., Garczarczyk, R., Gilmore, J., Hinton, Y., Inoue, K., Ioka, J., Kakuwa, S., Markoff, K., Murase, J. P., Osborne, A. N., Otte, R., Starling, H., Tajima, M., Teshima, K., Toma, S., Wagner, R. A., M., D. A., William, T., Yamamoto, R., Yamazaki, Cta, Consortium, Acharya, B. S., Actis, M., Aghajani, T., and Bissaldi, Elisabetta

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Cherenkov telescopes, Astrophysics, Gamma-ray bursts, High-energy gamma rays, Cosmic Rays, cosmology: observations, Cosmic Ray, 01 natural sciences, Observatory, Observational cosmology, 0103 physical sciences, Gamma-ray burst, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, High-energy gamma ray, Cherenkov Telescope Array, observations [cosmology], Cherenkov telescope, Extragalactic background light, Intergalactic travel, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We outline the science prospects for gamma-ray bursts (GRBs) with the Cherenkov Telescope Array (CTA), the next-generation ground-based gamma-ray observatory operating at energies above few tens of GeV. With its low energy threshold, large effective area and rapid slewing capabilities, CTA will be able to measure the spectra and variability of GRBs at multi-GeV energies with unprecedented photon statistics, and thereby break new ground in elucidating the physics of GRBs, which is still poorly understood. Such measurements will also provide crucial diagnostics of ultra-high-energy cosmic ray and neutrino production in GRBs, advance observational cosmology by probing the high-redshift extragalactic background light and intergalactic magnetic fields, and contribute to fundamental physics by testing Lorentz invariance violation with high precision. Aiming to quantify these goals, we present some simulated observations of GRB spectra and light curves, together with estimates of their detection rates with CTA. Although the expected detection rate is modest, of order a few GRBs per year, hundreds or more high-energy photons per burst may be attainable once they are detected. We also address various issues related to following up alerts from satellites and other facilities with CTA, as well as follow-up observations at other wavelengths. The possibility of discovering and observing GRBs from their onset including short GRBs during a wide-field survey mode is also briefly discussed., Astroparticle Physics, in press, for the special issue on "Physics with the Cherenkov Telescope Array"; 28 pages, 19 figures; replaced with cosmetically revised version

Published
2013

392. The Transient High Energy Sky and Early Universe Surveyor (THESEUS)

Author

Amati, L., O Brien, P., Goetz, D., Bozzo, E., Tenzer, C., Frontera, F., Ghirlanda, G., Labanti, C., Osborne, J. P., Stratta, G., Tanvir, N., Willingale, R., Attina, P., Campana, R., Castro-Tirado, A. J., Contini, C., Fuschino, F., Gomboc, A., Hudec, R., Orleanski, P., Renotte, E., Rodic, T., Bagoly, Z., Blain, A., Callanan, P., Covino, S., Ferrara, A., Le Floch, E., Marisaldi, M., Mereghetti, S., Rosati, P., Vacchi, A., D Avanzo, P., Giommi, P., Piranomonte, S., Piro, L., Reglero, V., Rossi, A., Santangelo, A., Salvaterra, R., Tagliaferri, G., Vergani, S., Vinciguerra, S., Briggs, M., Campolongo, E., Ciolfi, R., Connaughton, V., Cordier, B., Morelli, B., Orlandini, M., Adami, C., Argan, A., Atteia, J. -L, Auricchio, N., Balazs, L., Baldazzi, G., Basa, S., Basak, R., Bellutti, P., Bernardini, M. G., Bertuccio, G., Braga, J., Branchesi, M., Brandt, S., Brocato, E., Budtz-Jorgensen, C., Bulgarelli, A., Burderi, L., Camp, J., Capozziello, S., Caruana, J., Casella, P., Cenko, B., Chardonnet, P., Ciardi, B., Colafrancesco, S., Dainotti, M. G., D Elia, V., Martino, D., Pasquale, M., Del Monte, E., Della Valle, M., Drago, A., Evangelista, Y., Feroci, M., Finelli, F., Fiorini, M., Fynbo, J., Gal-Yam, A., Gendre, B., Ghisellini, G., Grado, A., Guidorzi, C., Hafizi, M., Hanlon, L., Hjorth, J., Izzo, L., Kiss, L., Kumar, P., Kuvvetli, I., Lavagna, M., Li, T., Longo, F., Lyutikov, M., Maio, U., Maiorano, E., Malcovati, P., Malesani, D., Margutti, R., Martin-Carrillo, A., Masetti, N., Mcbreen, S., Mignani, R., Morgante, G., Mundell, C., Nargaard-Nielsen, H. U., Nicastro, L., Palazzi, E., Paltani, S., Panessa, F., Pareschi, G., Pe Er, A., Penacchioni, A. V., Pian, E., Piedipalumbo, E., Piran, T., Rauw, G., Razzano, M., Read, A., Rezzolla, L., Romano, P., Ruffini, R., Savaglio, S., Sguera, V., Schady, P., Skidmore, W., Song, L., Stanway, E., Starling, R., Topinka, M., Troja, E., Putten, M., Vanzella, E., Vercellone, S., Wilson-Hodge, C., Yonetoku, D., Zampa, G., Zampa, N., Zhang, B., Zhang, B. B., Zhang, S., Zhang, S. -N, Antonelli, A., Bianco, F., Boci, S., Boer, M., Botticella, M. T., Boulade, O., Butler, C., Campana, S., Capitanio, F., Celotti, A., Chen, Y., Colpi, M., Comastri, A., Cuby, J. -G, Dadina, M., Andrea De Luca, Dong, Y. -W, Ettori, S., Gandhi, P., Geza, E., Greiner, J., Guiriec, S., Harms, J., Hernanz, M., Hornstrup, A., Hutchinson, I., Israel, G., Jonker, P., Kaneko, Y., Kawai, N., Wiersema, K., Korpela, S., Lebrun, V., Lu, F., Macfadyen, A., Malaguti, G., Maraschi, L., Melandri, A., Modjaz, M., Morris, D., Omodei, N., Paizis, A., Pata, P., Petrosian, V., Rachevski, A., Rhoads, J., Ryde, F., Sabau-Graziati, L., Shigehiro, N., Sims, M., Soomin, J., Szecsi, D., Urata, Y., Uslenghi, M., Valenziano, L., Vianello, G., Vojtech, S., Watson, D., Zicha, J., and L. Amati, P. O’Brien, D. Goetz, E. Bozzo, C. Tenzer, F. Frontera, G. Ghirlanda, C. Labanti, J. P. Osborne, G. Stratta, N. Tanvir, R. Willingale , P. Attina, R. Campana, A.J. Castro-Tirado, C. Contini, F. Fuschino, A. Gomboc, R. Hudec, P. Orleanski, E. Renotte, T. Rodic, Z. Bagoly, A. Blain, P. Callanan, S. Covino, A. Ferrara, E. Le Floch, M. Marisaldi, S. Mereghetti, P. Rosati, A. Vacchi, P. D’Avanzo, P. Giommi, A. Gomboc, S. Piranomonte, L. Piro, V. Reglero, A. Rossi, A. Santangelo, R. Salvaterra, G. Tagliaferri, S. Vergani, S. Vinciguerra, M. Briggs, E. Campolongo, R. Ciolfi, V. Connaughton, B. Cordier, B. Morelli, M. Orlandini, C. Adami, A. Argan, J.-L. Atteia, N. Auricchio, L. Balazs, G. Baldazzi, S. Basa, R. Basak, P. Bellutti, M. G. Bernardini, G. Bertuccio, J. Braga, M. Branchesi, S. Brandt, E. Brocato, C. Budtz-Jorgensen, A. Bulgarelli, L. Burderi, J. Camp, S. Capozziello, J. Caruana, P. Casella, B. Cenko, P. Chardonnet, B. Ciardi, S. Colafrancesco, M. G. Dainotti, V. D’Elia, D. De Martino, M. De Pasquale, E. Del Monte, M. Della Valle, A. Drago, Y. Evangelista, M. Feroci, F. Finelli, M. Fiorini, J. Fynbo, A. Gal-Yam, B. Gendre, G. Ghisellini, A. Grado, C. Guidorzi, M. Hafizi, L. Hanlon, J. Hjorth, L. Izzo, L. Kiss, P. Kumar, I. Kuvvetli, M. Lavagna, T. Li, F. Longo, M. Lyutikov, U. Maio, E. Maiorano, P. Malcovati, D. Malesani, R. Margutti, A. Martin-Carrillo, N. Masetti, S. McBreen, R. Mignani, G. Morgante, C. Mundell, H. U. Nargaard-Nielsen, L. Nicastro, E. Palazzi, S. Paltani, F. Panessa, G. Pareschi, A. Pe’er, A. V. Penacchioni, E. Pian, E. Piedipalumbo, T. Piran, G. Rauw, M. Razzano, A. Read, L. Rezzolla, P. Romano, R. Ruffini, S. Savaglio, V. Sguera, P. Schady, W. Skidmore, L. Song, E. Stanway, R. Starling, M. Topinka, E. Troja, M. van Putten, E. Vanzella, S. Vercellone, C. Wilson-Hodge, D. Yonetoku, G. Zampa, N. Zampa, B. Zhang, B. B. Zhang, S. Zhang, S.-N. Zhang, A. Antonelli, F. Bianco, S. Boci, M. Boer, M. T. Botticella, O. Boulade, C. Butler, S. Campana, F. Capitanio, A. Celotti, Y. Chen, M. Colpi, A. Comastri, J.-G. Cuby, M. Dadina, A. De Luca, Y.-W. Dong, S. Ettori, P. Gandhi, E. Geza, J. Greiner, S. Guiriec, J. Harms, M. Hernanz, A. Hornstrup, I. Hutchinson, G. Israel, P. Jonker, Y. Kaneko, N. Kawai, K. Wiersema, S. Korpela, V. Lebrun, F. Lu, A. MacFadyen, G. Malaguti, L. Maraschi, A. Melandri, M. Modjaz, D. Morris, N. Omodei, A. Paizis, P. P´ata, V. Petrosian, A. Rachevski, J. Rhoads, F. Ryde, L. Sabau-Graziati, N. Shigehiro, M. Sims, J. Soomin, D. Szecsi, Y. Urata, M. Uslenghi, L. Valenziano, G. Vianello, S. Vojtech, D. Watson, J. Zicha

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gamma-ray bursts, Cosmology: observations, dark ages, re-ionization, first stars, Astrophysics::Galaxy Astrophysics
Abstract

THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRBs and X-ray transients detection over a broad FOV (more than 1sr) with 0.5-1 arcmin localization, an energy band extending from several MeVs down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift ∼10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late '20s / early '30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).

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