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1. Two Classes of Gamma-ray Bursts Distinguished within the First Second of Their Prompt Emission

Author: Lána Salmon, Lorraine Hanlon, and Antonio Martin-Carrillo
Subjects: gamma-ray burst, feature extraction, machine learning, Astronomy, QB1-991
Abstract: Studies of Gamma-Ray Burst (GRB) properties, such as duration and spectral hardness, have found evidence for additional classes, beyond the short/hard and long/soft prototypes, using model-dependent methods. In this paper, a model-independent approach was used to analyse the gamma-ray light curves of large samples of GRBs detected by BATSE, Swift/BAT and Fermi/GBM. All the features were extracted from the GRB time profiles in four energy bands using the Stationary Wavelet Transform and Principal Component Analysis. t-distributed Stochastic Neighbourhood Embedding (t-SNE) visualisation of the features revealed two distinct groups of Swift/BAT bursts using the T100 interval with 64 ms resolution data. When the same analysis was applied to 4 ms resolution data, two groups were seen to emerge within the first second (T1) post-trigger. These two groups primarily consisted of short/hard (Group 1) and long/soft (Group 2) bursts, and were 95% consistent with the groups identified using the T100 64 ms resolution data. Kilonova candidates, arising from compact object mergers, were found to belong to Group 1, while those events with associated supernovae fell into Group 2. Differences in cumulative counts between the two groups in the first second, and in the minimum variability timescale, identifiable only with the 4 ms resolution data, may account for this result. Short GRBs have particular significance for multi-messenger science as a distinctive EM signature of a binary merger, which may be discovered by its gravitational wave emissions. Incorporating the T1 interval into classification algorithms may support the rapid classification of GRBs, allowing for an improved prioritisation of targets for follow-up observations.
Published: 2022
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2. Two Dimensional Clustering of Swift/BAT and Fermi/GBM Gamma-ray Bursts

Author: Lána Salmon, Lorraine Hanlon, and Antonio Martin-Carrillo
Subjects: gamma-ray burst, clustering, statistical analysis, Astronomy, QB1-991
Abstract: Studies of Gamma-ray Burst (GRB) properties, such as duration and spectral hardness, have found evidence for additional classes beyond the short-hard (merger) and long-soft (collapsar) prototypes. Several clustering analyses of the duration-hardness plane identified a third, intermediate duration, class. In this work, Gaussian Mixture Model-based (GMM) clustering is applied to the Swift/BAT and Fermi/GBM samples of GRBs. The results obtained by the hierarchical combination of Gaussian components (or clusters) based on an entropy criterion are presented. This method counteracts possible overfitting arising from the application of Gaussian models to non-Gaussian underlying data. While the initial GMM clustering of the hardness-duration plane identifies three components (short/intermediate/long) for the Swift/BAT and Fermi/GBM samples, only two components (short/long) remain once the entropy criterion is applied. The analysis presented here suggests that the intermediate duration class may be the result of overfitting, rather than evidence of a distinct underlying population.
Published: 2022
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3. Mission Test Campaign for the EIRSAT-1 Engineering Qualification Model

Author: Maeve Doyle, Rachel Dunwoody, Gabriel Finneran, David Murphy, Jack Reilly, Joseph Thompson, Sai Krishna Reddy Akarapu, Joseph Mangan, Sarah Walsh, Jessica Erkal, Fergal Marshall, Lána Salmon, Eoghan Somers, Lily Ha, David Palma, Antonio Martin-Carrillo, Sheila McBreen, David McKeown, William O’Connor, Brian Shortt, Alexey Uliyanov, Ronan Wall, and Lorraine Hanlon
Subjects: CubeSat, EIRSAT-1, Fly Your Satellite!, testing, reliability, operations, Motor vehicles. Aeronautics. Astronautics, TL1-4050
Abstract: The compact, standardised form factor of CubeSats allows for the use of commercial off-the-shelf components, reducing traditional barriers to entry, such as cost and development time. More than 1500 of these small spacecraft have been launched in the past 20 years, with improving capabilities that enable a wide range of mission profiles. The Educational Irish Research Satellite, EIRSAT-1, is a CubeSat being developed by a student-led team with goals that span education, technology demonstration and science. A comprehensive mission test plan, in which in-flight conditions are simulated, has been developed for EIRSAT-1 and implemented using an engineering qualification model of the spacecraft. In addition to verifying 41 mission requirements, the successful execution of the mission test plan established that the full satellite system can perform the intended mission. Mission testing also proved to be an invaluable tool to prepare for launch and operations, providing the team with a more complete understanding of the satellite’s expected on-orbit behaviour. This work presents a detailed description of the mission test planning process and implementation, as well as key results and lessons learned. In doing so, this work aims to improve the on-orbit reliability of CubeSats by disseminating resources and good practice around mission testing.
Published: 2022
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4. Development of the EIRSAT-1 CubeSat through Functional Verification of the Engineering Qualification Model

Author: Sarah Walsh, David Murphy, Maeve Doyle, Jack Reilly, Joseph Thompson, Rachel Dunwoody, Jessica Erkal, Gabriel Finneran, Gianluca Fontanesi, Joseph Mangan, Fergal Marshall, Lána Salmon, Daithí de Faoite, Lorraine Hanlon, Antonio Martin-Carrillo, David McKeown, William O’Connor, Alexey Uliyanov, Ronan Wall, and Sheila McBreen
Subjects: CubeSat, spacecraft verification, testing, Fly Your Satellite, EIRSAT-1, Motor vehicles. Aeronautics. Astronautics, TL1-4050
Abstract: The Educational Irish Research Satellite (EIRSAT-1) is a 2U CubeSat developed at University College Dublin. The project aims to build, test, launch, and operate Ireland’s first satellite and to perform in-orbit demonstrations of three novel payloads developed in-house. To reduce risk within the mission, the project employs a prototype model philosophy in which two models of the spacecraft exist: an engineering qualification model (EQM) and a flight model (FM). This paper presents the verification approach of the functional tests implemented for the EIRSAT-1 project. The activities of the FlatSat and system level full functional tests of the EQM are presented and the results obtained during the test campaigns are discussed. Four test anomalies were encountered during the full functional test campaign resulting in two minor redesigns, and subsequent reassembly, of the CubeSat. The functional test campaigns highlighted the importance of FlatSat level testing of CubeSats to ensure compatibility of all subsystems prior to assembly and of thorough documentation to diagnose any unexpected behaviour of the hardware efficiently. The functional verification of the EQM proved that the system conformed to its design, verifying 57 mission requirements, and is a crucial step towards the development of the EIRSAT-1 FM.
Published: 2021
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5. A magnetar giant flare in the nearby starburst galaxy M82

Author: Mereghetti, S, Rigoselli, M, Salvaterra, R, Pacholski, D, Craig Rodi, J, Gotz, D, Arrigoni, E, D’Avanzo, P, Adami, C, Bazzano, A, Bozzo, E, Brivio, R, Campana, S, Cappellaro, E, Chenevez, J, De Luise, F, Ducci, L, Esposito, P, Ferrigno, C, Ferro, M, Luca Israel, G, Le Floc’h, E, Martin-Carrillo, A, Onori, F, Rea, N, Reguitti, A, Savchenko, V, Souami, D, Tartaglia, L, Thuillot, W, Tiengo, A, Tomasella, L, Topinka, M, Turpin, D, Ubertini, P, Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Dominik Patryk Pacholski, James Craig Rodi, Diego Gotz, Edoardo Arrigoni, Paolo D’Avanzo, Christophe Adami, Angela Bazzano, Enrico Bozzo, Riccardo Brivio, Sergio Campana, Enrico Cappellaro, Jerome Chenevez, Fiore De Luise, Lorenzo Ducci, Paolo Esposito, Carlo Ferrigno, Matteo Ferro, Gian Luca Israel, Emeric Le Floc’h, Antonio Martin-Carrillo, Francesca Onori, Nanda Rea, Andrea Reguitti, Volodymyr Savchenko, Damya Souami, Leonardo Tartaglia, William Thuillot, Andrea Tiengo, Lina Tomasella, Martin Topinka, Damien Turpin, Pietro Ubertini, Mereghetti, S, Rigoselli, M, Salvaterra, R, Pacholski, D, Craig Rodi, J, Gotz, D, Arrigoni, E, D’Avanzo, P, Adami, C, Bazzano, A, Bozzo, E, Brivio, R, Campana, S, Cappellaro, E, Chenevez, J, De Luise, F, Ducci, L, Esposito, P, Ferrigno, C, Ferro, M, Luca Israel, G, Le Floc’h, E, Martin-Carrillo, A, Onori, F, Rea, N, Reguitti, A, Savchenko, V, Souami, D, Tartaglia, L, Thuillot, W, Tiengo, A, Tomasella, L, Topinka, M, Turpin, D, Ubertini, P, Sandro Mereghetti, Michela Rigoselli, Ruben Salvaterra, Dominik Patryk Pacholski, James Craig Rodi, Diego Gotz, Edoardo Arrigoni, Paolo D’Avanzo, Christophe Adami, Angela Bazzano, Enrico Bozzo, Riccardo Brivio, Sergio Campana, Enrico Cappellaro, Jerome Chenevez, Fiore De Luise, Lorenzo Ducci, Paolo Esposito, Carlo Ferrigno, Matteo Ferro, Gian Luca Israel, Emeric Le Floc’h, Antonio Martin-Carrillo, Francesca Onori, Nanda Rea, Andrea Reguitti, Volodymyr Savchenko, Damya Souami, Leonardo Tartaglia, William Thuillot, Andrea Tiengo, Lina Tomasella, Martin Topinka, Damien Turpin, and Pietro Ubertini
Abstract: Magnetar giant flares are rare explosive events releasing up to 1047 erg in gamma rays in less than 1 second from young neutron stars with magnetic fields up to 1015−16 G (refs. 1,2). Only three such flares have been seen from magnetars in our Galaxy3,4 and in the Large Magellanic Cloud5 in roughly 50 years. This small sample can be enlarged by the discovery of extragalactic events, as for a fraction of a second giant flares reach luminosities above 1046 erg s−1, which makes them visible up to a few tens of megaparsecs. However, at these distances they are difficult to distinguish from short gamma-ray bursts (GRBs); much more distant and energetic (1050−53 erg) events, originating in compact binary mergers6. A few short GRBs have been proposed7–11, with different amounts of confidence, as candidate giant magnetar flares in nearby galaxies. Here we report observations of GRB 231115A, positionally coincident with the starburst galaxy M82 (ref. 12). Its spectral properties, along with the length of the burst, the limits on its X-ray and optical counterparts obtained within a few hours, and the lack of a gravitational wave signal, unambiguously qualify this burst as a giant flare from a magnetar in M82.
Published: 2024

6. GALAXY-TARGETED ROBOTIC TELESCOPE FOLLOW-UP OF GRAVITATIONAL WAVE EVENTS

Author: Lána Salmon, Lorraine Hanlon, Antonio Martin-Carrillo, and R. M. Jeffrey
Subjects: Physics, Robotic telescope, Gravitational wave, Astronomy, General Medicine, Galaxy
Abstract: Robotic telescopes and networks are well equipped to respond rapidly to transient events. However, the era of multi-messenger astronomy presents new challenges in the search for electromagnetic counterparts to gravitational wave events. Specifically, these sources can be distant, faint, poorly localised, and quickly decaying. Effciently searching for counterparts requires coverage of large localisation regions and/or targeted observations. This paper presents a galaxy retrieval and ranking algorithm for targeted observations, and a public web interface to retrieve ranked galaxy lists following a gravitational wave event. The website is publicly available at https://gwtool.watchertelescope.ie/.
Published: 2021
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7. OPTICAL SPECTROSCOPY OF CANDIDATES IN THE LIGO/VIRGO BINARY MERGER ERROR BOXES

Author: Elena Pian, J. Cepa, Y. D. Hu, E. Fernandez-Garcia, Bin-Bin Zhang, S. R. Oates, Seok Ho Jeong, A. M. Sintes, Shashi B. Pandey, I. Agudo, J. A. Font, A. J. Castro-Tirado, A. F. Valeev, V. V. Sokolov, R. Sanchez-Ramirez, M. D. Caballero-Garcia, and Antonio Martin-Carrillo
Subjects: Physics, Binary number, General Medicine, Astrophysics, Spectroscopy, LIGO
Abstract: We performed optical spectroscopy of the candidates inside the gravitational wave errorboxes (S190408an, S190425z, S190426c, S190510g, S190728q, S190814bv). The spectral classification of 34 transients observed with the 10.4m Gran Telescopio de Canarias prior to 1 Sep 2019 is presented. We ruled out the association of these candidates with gravitational wave events.
Published: 2021
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8. Design, development, and testing of flight software for EIRSAT-1: a university-class CubeSat enabling astronomical research

Author: Maeve Doyle, Andrew Gloster, Meadhbh Griffin, Mike Hibbett, Jack Kyle, Conor O'Toole, Joseph Mangan, David Murphy, Nicholas L. Wong, Sai Krishna Reddy Akarapu, Rachel Dunwoody, Jessica Erkal, Gabriel Finneran, Jack Reilly, Lána Salmon, Joseph Thompson, Sarah Walsh, Brian Shortt, Antonio Martin-Carrillo, Sheila McBreen, David McKeown, William O'Connor, Alexei Ulyanov, Ronan Wall, and Lorraine Hanlon
Subjects: Space and Planetary Science, Control and Systems Engineering, Mechanical Engineering, Astronomy and Astrophysics, Instrumentation, Electronic, Optical and Magnetic Materials
Published: 2022
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9. Two Classes of Gamma-ray Bursts Distinguished within the First Second of Their Prompt Emission

Author: Lorraine Hanlon, Lána Salmon, and Antonio Martin Carrillo
Subjects: gamma-ray burst, feature extraction, machine learning, Astrophysics::High Energy Astrophysical Phenomena, Machine learning, Feature extraction, Astronomy and Astrophysics, Gamma-ray burst
Abstract: Studies of Gamma-Ray Burst (GRB) properties, such as duration and spectral hardness, have found evidence for additional classes, beyond the short/hard and long/soft prototypes, using model-dependent methods. In this paper, a model-independent approach was used to analyse the gamma-ray light curves of large samples of GRBs detected by BATSE, Swift/BAT and Fermi/GBM. All the features were extracted from the GRB time profiles in four energy bands using the Stationary Wavelet Transform and Principal Component Analysis. t-distributed Stochastic Neighbourhood Embedding (t-SNE) visualisation of the features revealed two distinct groups of Swift/BAT bursts using the T100 interval with 64 ms resolution data. When the same analysis was applied to 4 ms resolution data, two groups were seen to emerge within the first second (T1) post-trigger. These two groups primarily consisted of short/hard (Group 1) and long/soft (Group 2) bursts, and were 95% consistent with the groups identified using the T100 64 ms resolution data. Kilonova candidates, arising from compact object mergers, were found to belong to Group 1, while those events with associated supernovae fell into Group 2. Differences in cumulative counts between the two groups in the first second, and in the minimum variability timescale, identifiable only with the 4 ms resolution data, may account for this result. Short GRBs have particular significance for multi-messenger science as a distinctive EM signature of a binary merger, which may be discovered by its gravitational wave emissions. Incorporating the T1 interval into classification algorithms may support the rapid classification of GRBs, allowing for an improved prioritisation of targets for follow-up observations. European Commission Horizon 2020 Science Foundation Ireland Irish Research Council Postgraduate Scholarship
Published: 2022

10. Two Dimensional Clustering of Swift/BAT and Fermi/GBM Gamma-ray Bursts

Author: Lorraine Hanlon, Lána Salmon, and Antonio Martin Carrillo
Subjects: gamma-ray burst, clustering, statistical analysis, Statistical analysis, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Gamma-ray burst, Clustering
Abstract: Studies of Gamma-ray Burst (GRB) properties, such as duration and spectral hardness, have found evidence for additional classes beyond the short-hard (merger) and long-soft (collapsar) prototypes. Several clustering analyses of the duration-hardness plane identified a third, intermediate duration, class. In this work, Gaussian Mixture Model-based (GMM) clustering is applied to the Swift/BAT and Fermi/GBM samples of GRBs. The results obtained by the hierarchical combination of Gaussian components (or clusters) based on an entropy criterion are presented. This method counteracts possible overfitting arising from the application of Gaussian models to non-Gaussian underlying data. While the initial GMM clustering of the hardness-duration plane identifies three components (short/intermediate/long) for the Swift/BAT and Fermi/GBM samples, only two components (short/long) remain once the entropy criterion is applied. The analysis presented here suggests that the intermediate duration class may be the result of overfitting, rather than evidence of a distinct underlying population. European Commission Horizon 2020 Science Foundation Ireland Irish Research Council Postgraduate Scholarship
Published: 2022
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11. New insight into the origin of the GeV flare in the binary system PSR B1259-63/LS 2883 from the 2017 periastron passage

Author: Johannes Petrus Marais, B. van Soelen, Antonio Martin-Carrillo, Masha Chernyakova, S. Mc Keague, David Murphy, and D. Malyshev
Subjects: Physics, Brightness, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Bremsstrahlung, Astronomy and Astrophysics, Astrophysics, Electron, Light curve, 01 natural sciences, Synchrotron, law.invention, Luminosity, Pulsar, Space and Planetary Science, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Flare
Abstract: PSR B1259-63 is a gamma-ray binary system hosting a radio pulsar orbiting around an O9.5Ve star, LS 2883, with a period of ∼3.4 yr. The interaction of the pulsar wind with the LS 2883 outflow leads to unpulsed broad-band emission in the radio, X-rays, GeV, and TeV domains. While the radio, X-ray, and TeV light curves show rather similar behaviour, the GeV light curve appears very different with a huge outburst about a month after a periastron. The energy release during this outburst seems to significantly exceed the spin-down luminosity of the pulsar and both the GeV light curve and the energy release vary from one orbit to the next. In this paper, we present for the first time the results of optical observations of the system in 2017, and also reanalyse the available X-ray and GeV data. We present a new model in which the GeV data are explained as a combination of the bremsstrahlung and inverse Compton emission from the unshocked and weakly shocked electrons of the pulsar wind. The X-ray and TeV emission is produced by synchrotron and inverse Compton emission of energetic electrons accelerated on a strong shock arising due to stellar/pulsar winds collision. The brightness of the GeV flare is explained in our model as a beaming effect of the energy released in a cone oriented, during the time of the flare, in the direction of the observer.
Published: 2020
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12. Update on the status of the Educational Irish Research Satellite (EIRSAT-1)

Author: Maeve Doyle, David Murphy, Jack Reilly, Joseph Thompson, Sarah Walsh, Sai Krishna Reddy Akarapu, Rachel Dunwoody, Jessica Erkal, Gabriel Finneran, Joseph Mangan, Fergal Marshall, Lána Salmon, Eoghan Somers, Loris Franchi, Lily Ha, David Palma, Alexey Ulyanov, Antonio Martin Carrillo, Sheila McBreen, David McKeown, William O'Connor, Ronan Wall, and Lorraine Hanlon
Subjects: Satèl·lits artificials, Aerospace engineering, Education, Higher, EIRSAT-1, Artificial satellites, Fly Your Satellite!, CubeSat, Ensenyament i aprenentatge::Ensenyament universitari [Àrees temàtiques de la UPC], Ensenyament universitari, Aeronàutica i espai::Astronàutica::Enginyeria aeroespacial [Àrees temàtiques de la UPC], Enginyeria aeroespacial
Abstract: The Educational Irish Research Satellite, EIRSAT-1, is a 2U CubeSat being implemented by a student-led team at University College Dublin, as part of the 2nd round of the European Space Agency’s Fly Your Satellite! programme. In development since 2017, the mission has several scientific, technological and outreach goals. It will fly an in-house developed antenna deployment module, along with three custom payloads, which are integrated with commercial off-the-shelf subsystems. In preparation for the flight model, a full-system engineering qualification model of the spacecraft has undergone an extensive period of test campaigns, including full functional tests, a mission test, and environmental testing at the European Space Agency’s CubeSat Support Facility in Redu, Belgium. Beyond the technical, educational, and capacity-building goals of the mission, EIRSAT-1 aims to inspire wider study of STEM subjects, while highlighting the importance of multidisciplinary teams and creating greater awareness of space in everyday life. A wide range of outreach activities are being undertaken to realise these aims. This paper provides a status update on key aspects of the EIRSAT-1 project and the next steps towards launch
Published: 2022

13. Thermal characterization testing of a robust and reliable thermal knife HDRM (Hold Down and Release Mechanism) for CubeSat deployables

Author: Joseph Thompson, David Murphy, Jack Reilly, Lána Salmon, Rachel Dunwoody, Maeve Doyle, Sarah Walsh, Sai Krishna Reddy Akarapu, Jessica Erkal, Gabriel Finneran, Joseph Mangan, Fergal Marshall, Loris Franchi, Lily Ha, David Palma, Alexey Ulyanov, Antonio Martin-Carrillo, Sheila McBreen, William O'Connor, Ronan Wall, Lorraine Hanlon, and David McKeown
Subjects: Satèl·lits artificials, CubeSat deployable, EIRSAT-1, Artificial satellites, Polyethylene, Antennas (Electronics), Hold down and release mechanism, Antenes (Electrònica), Enginyeria de la telecomunicació::Radiocomunicació i exploració electromagnètica::Satèl·lits i ràdioenllaços [Àrees temàtiques de la UPC], Aeronàutica i espai [Àrees temàtiques de la UPC], Thermal knife, Polietilè
Abstract: Thermal knife HDRMs (Hold Down and Release Mechanisms) are commonly used in CubeSats and other small satellites. However, detailed information on proven designs is difficult to find. Design of a robust and reliable mechanism can present technical challenges which may only become apparent during testing, and often only when tested in a space representative environment. A custom thermal knife HDRM was designed and built for the antenna deployment module of EIRSAT-1 to deploy four coil spring antenna elements, but the same or a similar design could be repurposed quite easily to release a wide range of CubeSat deployables. In this design resistors are used to cut dyneema lines. For robustness and reliability, the thermal response of the mechanism must be well understood. To reach the melting point of the dyneema (150C) the power dissipated in the resistors must often exceed the maximum rated value. Therefore, choosing the operating current and the burn time is a careful trade-off between ensuring that the resistor reliably cuts the dyneema line and ensuring that the resistor, solder joints, PCB and nearby components are not damaged by the high temperatures. These choices are further complicated by the requirement that the mechanism operates over a range of temperatures. A thermal vacuum test campaign was carried out to better understand and characterise the thermal behaviour of the EIRSAT-1 mechanism. For the test a model of the mechanism was built with several temperature sensors installed. Two of these sensors were installed directly on the body of the resistors using a thermally conductive epoxy. Burn tests were performed in vacuum at temperatures between -37C and +56C. The test shows many interesting results including the effect of the dyneema lines on the thermal response, the possibility of desoldering the burn resistors and a comparison between the performance at ambient and vacuum conditions. Finally, a summary is given of the key technical challenges associated with this type of mechanism along with some recommendations to help make future designs more robust and reliable.
Published: 2022
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14. Teaching computational thinking to space science students

Author: Robert Jeffrey, Megan Lundy, Deirdre Coffey, Sheila McBreen, Antonio Martin-Carrillo, and Lorraine Hanlon
Subjects: Problem solving, Physics - Physics Education, FOS: Physical sciences, Space -- Study and teaching, Solució de problemes, Aeronàutica i espai::Astronàutica::Enginyeria aeroespacial [Àrees temàtiques de la UPC], Space education, Postgraduate Education, Espai -- Ensenyament, Vocational education, Physics Education (physics.ed-ph), ComputingMilieux_COMPUTERSANDEDUCATION, Formació professional, Computational thinking
Abstract: Computational thinking is a key skill for space science graduates, who must apply advanced problem-solving skills to model complex systems, analyse big data sets, and develop control software for mission-critical space systems. We describe our work using Design Thinking to understand the challenges that students face in learning these skills. In the MSc Space Science & Technology at University College Dublin, we have used insights from this process to develop new teaching strategies, including improved assessment rubrics, supported by workshops promoting collaborative programming techniques. We argue that postgraduate level space science courses play a valuable role in developing more advanced computational skills in early-career space scientists., 6 pages, 3 figures, presented at 4th Symposium on Space Educational Activities, Barcelona, 27-29 April 2022
Published: 2022
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15. Optical Spectropolarimetry Observations of the BL Lac-type object PKS 0537-441 after a period of quiescence

Author: Joleen Barnard, Brian van Soelen, Justin Cooper, Richard Britto, Johannes Petrus Marais, Izak van der Westhuizen, David Buckley, Hester Schutte, Markus Böttcher, Bhargav Vaidya, Sriyasriti Achariya, and Antonio Martin-Carrillo
Published: 2021
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16. Mission testing for improved reliability of CubeSats

Author: Sarah Walsh, Joseph Mangan, Ronan Wall, Derek Greene, Maeve Doyle, Alexei Uliyanov, Daithí de Faoite, Gabriel Finneran, Jessica Erkal, Gianluca Fontanesi, Lily Ha, David McKeown, Sheila McBreen, David Palma, Jack Reilly, Fergal Marshall, Aldous Mills, David Murphy, Joseph Thompson, Kenneth T. Stanton, Antonio Martin-Carrillo, Rachel Dunwoody, Lorraine Hanlon, William J. O'Connor, and Lána Salmon
Subjects: Computer science, Reliability (statistics), Reliability engineering
Published: 2021
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17. A compact instrument for gamma-ray burst detection on a CubeSat platform I: Design drivers and expected performance

Author: Maeve Doyle, David Murphy, Joseph Mangan, Brian Shortt, Sheila McBreen, Joseph Thompson, Antonio Martin-Carrillo, Rachel Dunwoody, A. Ulyanov, and Lorraine Hanlon
Subjects: Simulations, CubeSats, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Field of view, Scintillator, 01 natural sciences, 7. Clean energy, 010309 optics, Silicon photomultiplier, Optics, 0103 physical sciences, CubeSat, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Spectrometer, Spacecraft, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Detectors, Space and Planetary Science, Satellite, Original Article, Cerium bromide, Gamma-ray bursts, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Educational Irish Research Satellite 1 (EIRSAT-1) is a 2U CubeSat being developed under ESA's Fly Your Satellite! programme. The project has many aspects, which are primarily educational, but also include space qualification of new detector technologies for gamma-ray astronomy and the detection of gamma-ray bursts (GRBs). The Gamma-ray Module (GMOD), the main mission payload, is a small gamma-ray spectrometer comprising a 25 mm $\times$ 25 mm $\times$ 40 mm cerium bromide scintillator coupled to an array of 16 silicon photomultipliers. The readout is provided by IDE3380 (SIPHRA), a low-power and radiation tolerant readout ASIC. GMOD will detect gamma-rays and measure their energies in a range from tens of keV to a few MeV. Monte Carlo simulations were performed using the Medium Energy Gamma-ray Astronomy Library to evaluate GMOD's capability for the detection of GRBs in low Earth orbit. The simulations used a detailed mass model of the full spacecraft derived from a very high-fidelity 3D CAD model. The sky-average effective area of GMOD on board EIRSAT-1 was found to be 10 cm$^2$ at 120 keV. The instrument is expected to detect between 11 and 14 GRBs, at a significance greater than 10$\sigma$ (and up to 32 at 5$\sigma$), during a nominal one-year mission. The shape of the scintillator in GMOD results in omni-directional sensitivity which allows for a nearly all-sky field of view., Comment: 27 pages, 13 figures. This is an author accepted manuscript of an article published in Experimental Astronomy. The final open-access version is available at: https://doi.org/10.1007/s10686-021-09779-9
Published: 2021

18. A compact instrument for gamma-ray burst detection on a CubeSat platform II: Detailed design, assembly and validation

Author: David Murphy, Alexey Ulyanov, Sheila McBreen, Joseph Mangan, Rachel Dunwoody, Maeve Doyle, Conor O’Toole, Joseph Thompson, Jack Reilly, Sarah Walsh, Brian Shortt, Antonio Martin-Carrillo, and Lorraine Hanlon
Subjects: Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The Gamma-ray Module, GMOD, is a miniaturised novel gamma-ray detector which will be the primary scientific payload on the Educational Irish Research Satellite (EIRSAT-1) 2U CubeSat mission. GMOD comprises a compact (25mm $\times$ 25mm $\times$ 40mm) cerium bromide scintillator coupled to a tiled array of 4$\times$4 silicon photomultipliers, with front-end readout provided by the IDE3380 SIPHRA. This paper presents the detailed GMOD design and the accommodation of the instrument within the restrictive CubeSat form factor. The electronic and mechanical interfaces are compatible with many off-the-shelf CubeSat systems and structures. The energy response of the GMOD engineering qualification model has been determined using radioactive sources, and an energy resolution of 5.4% at 662keV has been measured. EIRSAT-1 will perform on-board processing of GMOD data. Trigger results, including light-curves and spectra, will be incorporated into the spacecraft beacon and transmitted continuously. Inexpensive hardware can be used to decode the beacon signal, making the data accessible to a wide community. GMOD will have scientific capability for the detection of gamma-ray bursts, in addition to the educational and technology demonstration goals of the EIRSAT-1 mission. The detailed design and measurements to date demonstrate the capability of GMOD in low Earth orbit, the scalability of the design for larger CubeSats and as an element of future large gamma-ray missions., Comment: 31 pages, 16 figures. This is an author accepted manuscript of an article accepted for publication in Experimental Astronomy. The final open-access version will be available at: https://doi.org/10.1007/s10686-022-09842-z
Published: 2021

19. Multi-messenger astronomy with INTEGRAL

Author: E. Kuulkers, Maeve Doyle, Andrea Goldwurm, Elisabeth Jourdain, Alexis Coleiro, A. Domingo, Diego Götz, Jean-Pierre Roques, Pietro Ubertini, V. G. Savchenko, Carlo Ferrigno, J. Rodi, Enrico Bozzo, Angela Bazzano, Celia Sanchez-Fernandez, Francesca Onori, Lorenzo Natalucci, Sandro Mereghetti, Jérôme Chenevez, Francesca Panessa, Antonio Martin-Carrillo, Andreas von Kienlin, 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), and 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)
Subjects: neutron star: binary, exceptional, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Neutron, gamma ray: burst, Magnetar, 01 natural sciences, blazar, Gravitational waves, Radio telescope, 0103 physical sciences, Neutrinos, Blazar, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), radio wave: burst, 010308 nuclear & particles physics, Gravitational wave, background, Astronomy, Astronomy and Astrophysics, magnetar, stability, Stars, gravitational radiation detector, messenger, electromagnetic, neutrino: detector, gamma ray: emission, Neutrino detector, black hole: binary, Space and Planetary Science, cosmic radiation, Spectral energy distribution, spectral, Fast radio bursts, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Radio wave
Abstract: At the time of defining the science objectives of the INTernational Gamma-Ray Astrophysics Laboratory (INTEGRAL), such a rapid and spectacular development of multi-messenger astronomy could not have been predicted, with new impulsive phenomena becoming accessible through different channels. Neutrino telescopes have routinely detected energetic neutrino events coming from unknown cosmic sources since 2013. Gravitational wave detectors opened a novel window on the sky in 2015 with the detection of the merging of two black holes and in 2017 with the merging of two neutron stars, followed by signals in the full electromagnetic range. Finally, since 2007, radio telescopes detected extremely intense and short burst of radio waves, known as Fast Radio Bursts (FRBs) whose origin is for most cases extragalactic, but enigmatic. The exceptionally robust and versatile design of the INTEGRAL mission has allowed researchers to exploit data collected not only with the pointed instruments, but also with the active cosmic-ray shields of the main instruments to detect impulses of gamma-rays in coincidence with unpredictable phenomena. The full-sky coverage, mostly unocculted by the Earth, the large effective area, the stable background, and the high duty cycle (85%) put INTEGRAL in a privileged position to give a major contribution to multi-messenger astronomy. In this review, we describe how INTEGRAL has provided upper limits on the gamma-ray emission from black-hole binary mergers, detected a short gamma-ray burst in coincidence with a binary neutron star merger, contributed to define the spectral energy distribution of a blazar associated with a neutrino event, set upper limits on impulsive and steady gamma-ray emission from cosmological FRBs, and detected a magnetar flare associated with fast radio bursting emission., Comment: Accepted for publication on New Astronomy Reviews as invited contribution
Published: 2021
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20. INTEGRAL Results on Gamma-Ray Bursts and Polarization of Hard X-ray Sources

Author: Diego Götz, Philippe Laurent, J. Rodriguez, Lorraine Hanlon, E. Jourdain, V. G. Savchenko, Sandro Mereghetti, P. Moran, Antonio Martin-Carrillo, J. P. Roques, Alexander A. Lutovinov, Christian Gouiffes, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), 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), 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), and 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)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Field of view, Gamma-Ray Burts, 01 natural sciences, Polarization, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Compact objects, 010303 astronomy & astrophysics, Alert system, Ibis, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Black hole binaries, biology, 010308 nuclear & particles physics, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Polarization (waves), biology.organism_classification, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Gamma-rays, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In this paper we first review the results obtained by the INTEGRAL mission in the domain of Gamma-Ray Bursts (GRBs), thanks to the INTEGRAL Burst Alert System, which is able to deliver near real-time alerts for GRBs detected within the IBIS field of view. More than 120 GRBs have been detected to date and we summarize their properties here. In the second part of this review we focus on the polarimetric results obtained by IBIS and SPI on GRBs and Galactic compact objects., Comment: 24 pages, 8 figures, accepted for publication in New Astronomy Reviews volume "Fifteen-plus years of INTEGRAL Science"
Published: 2021
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21. 10.4 m GTC observations of the nearby VHE-detected GRB 190829A/SN 2019oyw

Author: Rahul Gupta, Amit Kumar, A. J. Castro-Tirado, Elena Pian, A. Castellon, A. Aryan, Bin-Bin Zhang, I. Agudo, Y. D. Hu, R. Sanchez-Ramirez, V. V. Sokolov, S. R. Oates, Antonio Martin-Carrillo, M. D. Caballero-Garcia, David Alexander Kann, A. F. Valeev, Shashi B. Pandey, S. Guziy, Russian Foundation for Basic Research, Fundamental Research Funds for the Central Universities (China), National Key Research and Development Program (China), National Natural Science Foundation of China, Ministerio de Ciencia, Innovación y Universidades (España), and European Commission
Subjects: Gran Telescopio Canarias, individual: SN 2019oyw [Supernovae], High energy, FOS: Physical sciences, Spectral domain, Astrophysics, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, Supernovae: individual: SN 2019oyw, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), individual: GRB 190829A [Gamma-ray burst], 010308 nuclear & particles physics, Gamma-ray burst: general, Astronomy and Astrophysics, Afterglow, general [Gamma-ray burst], Supernova, Space and Planetary Science, Gamma-ray burst: individual: GRB 190829A, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: Aims. Gamma-ray burst (GRB) 190829A (z=0.0785) was detected by Fermi and Swift and also at very high energy (VHE) by the High-Energy Stereoscopic System (H.E.S.S.) telescopes. The prompt emission displayed two emission episodes separated by a quiescent gap of similar to 40 s. We present the 10.4 m Gran Telescopio Canarias (GTC) observations of the afterglow of GRB 190829A and its underlying supernova. We also compare GRB 190829A to GRB 180728A, a GRB with similar behaviour, and discuss the implications on underlying physical mechanisms producing these two GRBs.Methods. We present multi-band photometric data along with spectroscopic follow-up observations taken with the 10.4 m GTC telescope. Together with the data from the prompt emission, the 10.4 m GTC data are used to understand the emission mechanisms and possible progenitor.Results. A detailed analysis of the multi-band observations of the afterglow requires the cooling frequency to pass between the optical and X-ray bands at early epochs. The afterglow then transitions to the underlying supernova (SN) 2019oyw, which dominates later on.Conclusions. Although the prompt emission temporal properties of GRB 190829A and GRB 180728A are similar, the two pulses are different in the spectral domain. We find that SN 2019oyw associated with GRB 190829A is powered by Ni decay and is a Type Ic-BL SN. The spectroscopic and photometric properties of this SN are consistent with those observed for SN 1998bw, but evolved earlier. © ESO 2021., Based on observations made with the GTC telescope, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, part of them under Director's Discretionary Time. This work has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) and the Leicester Database and Archive Service (LEDAS), provided by NASA's Goddard Space Flight Center and the Department of Physics and Astronomy, Leicester University, UK, respectively. Y.-D.H., A.J.C.-T., I.A. and D.A.K. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the `Center of Excellence Severo Ochoa' award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). R.G, S.B.P., and A.A. acknowledge BRICS grant DST/IMRCD/BRICS/PilotCall1/ProFCheap/2017(G) for part of the work. V.A.F. was supported by RFBR 18-29-21030 grant. S.B.P. also acknowledges DST/INT/JSPS/P/281/2018 for the present work. B.-B.Z. acknowledges the supported by the Fundamental Research Funds for the Central Universities (14380035). This work is supported by National Key Research and Development Programs of China (2018YFA0404204), the National Natural Science Foundation of China (Grant Nos. 11833003) and the Program for Innovative Talents, Entrepreneur in Jiangsu. D.A.K. acknowledges support from Spanish research project RTI2018-098104-J-I00 (GRBPhot). Finally, the authors extend their thanks to the anonymous referee for their valuable comments that helped to improve the manuscript substantially.
Published: 2021

22. Synergies of THESEUS with the large facilities of the 2030s and guest observer opportunities

Author: Stefan Grimm, Enrico Bozzo, P. T. O'Brien, Antonio Martin-Carrillo, Andrea Ferrara, Sandro Mereghetti, Piero Rosati, G. Oganesyan, G. Guidorzi, Nikolaos Stergioulas, S. Turriziani, Francesco Longo, Marica Branchesi, J. P. Osborne, D. Porquet, Lorenzo Amati, S. Basa, Stéphane Paltani, Giancarlo Ghirlanda, Dafne Guetta, Solen Balman, M. H. Erkut, Sarah L. Casewell, Olga Sergijenko, Ruben Salvaterra, Joseph Caruana, Andrew Blain, S. D. Vergani, Giulia Stratta, Michele Maggiore, R. Ciolfi, Maurizio Spurio, E. Le Floc'h, Andreja Gomboc, Andrea Rossi, Lise Christensen, Nial R. Tanvir, Filippo Frontera, F. Schüssler, Jan Harms, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Rosati, P, Basa, S, Blain, A W, Bozzo, E, Branchesi, M, Christensen, L, Ferrara, A, Gomboc, A, O'Brien, P T, Osborne, J P, Rossi, A, Schüssler, F, Spurio, M, Stergioulas, N, Stratta, G, Amati, L, Casewell, S, Ciolfi, R, Ghirlanda, G, Grimm, S, Guetta, D, Harms, J, Le Floc'h, E, Longo, F, Maggiore, M, Mereghetti, S, Oganesyan, G, Salvaterra, R, Tanvir, N R, Turriziani, S, Vergani, S D, Balman, S, Caruana, J, Erkut, M H, Guidorzi, G, Frontera, F, Martin-Carrillo, A, Paltani, S, Porquet, D, Sergijenko, O, Rosati P., Basa S., Blain A.W., Bozzo E., Branchesi M., Christensen L., Ferrara A., Gomboc A., O'Brien P.T., Osborne J.P., Rossi A., Schussler F., Spurio M., Stergioulas N., Stratta G., Amati L., Casewell S., Ciolfi R., Ghirlanda G., Grimm S., Guetta D., Harms J., Le Floc'h E., Longo F., Maggiore M., Mereghetti S., Oganesyan G., Salvaterra R., Tanvir N.R., Turriziani S., Vergani S.D., Balman S., Caruana J., Erkut M.H., Guidorzi G., Frontera F., Martin-Carrillo A., Paltani S., Porquet D., and Sergijenko O.
Subjects: cosmological model, neutron star: binary, Cherenkov Telescope Array, Computer science, 01 natural sciences, 7. Clean energy, Cosmology, GW170817, multi-messenger astrophysics, 010303 astronomy & astrophysics, media_common, COSMIC cancer database, gamma-ray bursts, REIONIZATION, gravitation wave sources, star: formation, AFTERGLOWS, neutrino: detector, Neutrino detector, Gravitation wave sources, Gamma-ray bursts, Astrophysics - Instrumentation and Methods for Astrophysics, Exploit, media_common.quotation_subject, FOS: Physical sciences, gamma ray: burst, Observer (physics), X-ray sources, NO, electromagnetic field: production, neutrino: production, binary: coalescence, Neutrino sources, 0103 physical sciences, gamma ray: detector, X-ray: emission, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Gamma-ray burst, Neutrino source, Multi-messenger astrophysics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Multi-messenger astrophysic, neutrino: particle source, binary: compact, Data science, Universe, gravitational radiation detector, detector: sensitivity, black hole: binary, Space and Planetary Science, gravitational radiation: emission, Gravitation wave source, gravitational radiation: localization, X-ray: detector
Abstract: The proposed THESEUS mission will vastly expand the capabilities to monitor the high-energy sky, and will exploit large samples of gamma-ray bursts to probe the early Universe back to the first generation of stars, and to advance multi-messenger astrophysics by detecting and localizing the counterparts of gravitational waves and cosmic neutrino sources. The combination and coordination of these activities with multi-wavelength, multi-messenger facilities expected to be operating in the thirties will open new avenues of exploration in many areas of astrophysics, cosmology and fundamental physics, thus adding considerable strength to the overall scientific impact of THESEUS and these facilities. We discuss here a number of these powerful synergies., Revised version after submission to Experimental Astronomy
Published: 2021
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23. Multi-messenger astrophysics with THESEUS in the 2030s

Author: Marica Branchesi, Lijing Shao, A. Gomboc, Stefanie Komossa, Luca Izzo, Gor Oganesyan, Bruce Gendre, Antonio Martin-Carrillo, Silvia Celli, Lorenzo Amati, Diego Götz, Nial R. Tanvir, S. Vinciguerra, J. P. Osborne, Antonio Capone, Irene Di Palma, Giancarlo Ghirlanda, S. Ronchini, Gavin P. Lamb, Roberto Mignani, Bing Zhang, René Hudec, Francesco Longo, Albert K. H. Kong, Michela Fasano, Dafne Guetta, Lorraine Hanlon, Antonios Nathanail, Andrea Rossi, Simone Dall'Osso, Emeric Le Floc'h, Riccardo Ciolfi, Enrico Bozzo, G. Stratta, Piero Rosati, S. Ascenzi, Luciano Rezzolla, Silvia Piranomonte, S. Turriziani, F. Schüssler, P. D'Avanzo, Eric Howell, Silvia Zane, Paolo Fermani, Ayden McCann, Sandro Mereghetti, Sylvain Chaty, Hüsne Dereli-Bégué, Eliana Palazzi, István T. Horváth, Jan Harms, Om Sharan Salafia, Sandra Savaglio, Stéphane Paltani, Lána Salmon, Asaf Pe'er, A. Zegarelli, Andrew Blain, S. D. Vergani, Liang Li, Stefan Grimm, Olga Sergijenko, fnmMassimiliano De Pasquale, Maurice H. P. M. van Putten, Yuji Urata, P. T. O'Brien, 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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Ciolfi, Riccardo, Stratta, Giulia, Branchesi, Marica, Gendre, Bruce, Grimm, Stefan, Harms, Jan, Paul Lamb, Gavin, Martin-Carrillo, Antonio, Mccann, Ayden, Oganesyan, Gor, Palazzi, Eliana, Ronchini, Samuele, Rossi, Andrea, Sharan Salafia, Om, Salmon, Lana, Ascenzi, Stefano, Capone, Antonio, Celli, Silvia, Dall???osso, Simone, Di Palma, Irene, Fasano, Michela, Fermani, Paolo, Guetta, Dafne, Hanlon, Lorraine, Howell, Eric, Paltani, Stephane, Rezzolla, Luciano, Vinciguerra, Serena, Zegarelli, Angela, Amati, Lorenzo, Blain, Andrew, Bozzo, Enrico, Chaty, Sylvain, D???avanzo, Paolo, De Pasquale, Fnmmassimiliano, Dereli-B??gu??, H??sne, Ghirlanda, Giancarlo, Gomboc, Andreja, G??tz, Diego, Horvath, Istvan, Hudec, Rene, Izzo, Luca, Le Floch, Emeric, Li, Liang, Longo, Francesco, Komossa, S., Kong, Albert K. H., Mereghetti, Sandro, Mignani, Roberto, Nathanail, Antonio, O???brien, Paul T., Osborne, Julian P., Pe???er, Asaf, Piranomonte, Silvia, Rosati, Piero, Savaglio, Sandra, Sch??ssler, Fabian, Sergijenko, Olga, Shao, Lijing, Tanvir, Nial, Turriziani, Sara, Urata, Yuji, van Putten, Maurice, Vergani, Susanna, Zane, Silvia, and Zhang, Bing
Subjects: HIGH-ENERGY NEUTRINOS, cosmological model, neutron star: binary, ELECTROMAGNETIC COUNTERPARTS, Compact binary merger, EXTENDED EMISSION, Astrophysics, 01 natural sciences, GRAVITATIONAL-WAVES, Cosmology, MAGNETAR, NEUTRON-STAR, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), GAMMA-RAY BURSTS, Physics, Hubble constant, Multi-messenger astrophysics, Gamma-ray burst, Kilonova, X-ray sources, Neutrino sources, Detection rate, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Multi-messenger astrophysics, Gamma-ray burst, Compact binary merger, Kilonova, X-ray sources, Neutrino source, FOS: Physical sciences, Context (language use), gamma ray: burst, NO, electromagnetic field: production, X-ray source, neutrino: production, binary: coalescence, 0103 physical sciences, gamma ray: detector, X-ray: emission, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Neutrino source, LIGHT CURVES, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Multi-messenger astrophysic, neutrino: particle source, magnetar, redshift, binary: compact, gravitational radiation detector, detector: sensitivity, black hole: binary, Space and Planetary Science, gravitational radiation: emission, BLACK-HOLE, Fundamental physics, gravitational radiation: localization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM, astro-ph.HE, X-ray: detector
Abstract: Multi-messenger astrophysics is becoming a major avenue to explore the Universe, with the potential to span a vast range of redshifts. The growing synergies between different probes is opening new frontiers, which promise profound insights into several aspects of fundamental physics and cosmology. In this context, THESEUS will play a central role during the 2030s in detecting and localizing the electromagnetic counterparts of gravitational wave and neutrino sources that the unprecedented sensitivity of next generation detectors will discover at much higher rates than the present. Here, we review the most important target signals from multi-messenger sources that THESEUS will be able to detect and characterize, discussing detection rate expectations and scientific impact., Submitted to Experimental Astronomy
Published: 2021
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24. Detection capabilities of the Athena X-IFU for the warm-hot intergalactic medium using gamma-ray burst X-ray afterglows

Author: Sarah Walsh, Joop Schaye, Thomas Dauser, Didier Barret, Jörn Wilms, Nastasha Wijers, Antonio Martin-Carrillo, Sheila McBreen, 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), and 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)
Subjects: Active galactic nucleus, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Warm–hot intergalactic medium, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, 7. Clean energy, Spectral line, 0103 physical sciences, Absorption (logic), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Line search, instrumentation: detectors, Astronomy and Astrophysics, Redshift, Afterglow, Space and Planetary Science, large-scale structure of Universe, intergalactic medium, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: At low redshifts, the observed baryonic density falls far short of the total number of baryons predicted. Cosmological simulations suggest that these baryons reside in filamentary gas structures, known as the warm-hot intergalactic medium (WHIM). As a result of the high temperatures of these filaments, the matter is highly ionised such that it absorbs and emits far-UV and soft X-ray photons. Athena, the proposed European Space Agency X-ray observatory, aims to detect the `missing' baryons in the WHIM up to redshifts of $z=1$ through absorption in active galactic nuclei and gamma-ray burst afterglow spectra, allowing for the study of the evolution of these large-scale structures of the Universe. This work simulates WHIM filaments in the spectra of GRB X-ray afterglows with Athena using the SImulation of X-ray TElescopes (SIXTE) framework. We investigate the feasibility of their detection with the X-IFU instrument, through O VII ($E=573$ eV) and O VIII ($E=674$ eV) absorption features, for a range of equivalent widths imprinted onto GRB afterglow spectra of observed starting fluxes ranging between $10^{-12}$ and $10^{-10}$ erg cm$^{-2}$ s$^{-1}$, in the 0.3-10 keV energy band. The analyses of X-IFU spectra by blind line search show that Athena will be able to detect O VII-O VIII absorption pairs with EW$_\mathrm{O VII} > 0.13$ eV and EW$_\mathrm{O VIII} > 0.09$ eV for afterglows with $F>2 \times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$. This allows for the detection of $\approx$ 45-137 O VII-O VIII absorbers during the four-year mission lifetime. The work shows that to obtain an O VII-O VIII detection of high statistical significance, the local hydrogen column density should be limited at $N_\mathrm{H}, Accepted for publication in Astronomy & Astrophysics
Published: 2020
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25. Development of the EIRSAT-1 CubeSat through Functional Verification of the Engineering Qualification Model

Author: Lorraine Hanlon, William J. O'Connor, Antonio Martin-Carrillo, David Murphy, Ronan Wall, Jessica Erkal, Gianluca Fontanesi, David McKeown, Joseph Thompson, Alexey Uliyanov, Joseph Mangan, Lána Salmon, Sarah Walsh, Jack Reilly, Gabriel Finneran, Sheila McBreen, Fergal Marshall, Rachel Dunwoody, Daithí de Faoite, and Maeve Doyle
Subjects: spacecraft verification, Functional verification, EIRSAT-1, Spacecraft, business.industry, Computer science, CubeSat, Aerospace Engineering, TL1-4050, testing, Test (assessment), Documentation, Flight model, Systems engineering, System level, business, Fly Your Satellite, Motor vehicles. Aeronautics. Astronautics
Abstract: The Educational Irish Research Satellite (EIRSAT-1) is a 2U CubeSat developed at University College Dublin. The project aims to build, test, launch, and operate Ireland’s first satellite and to perform in-orbit demonstrations of three novel payloads developed in-house. To reduce risk within the mission, the project employs a prototype model philosophy in which two models of the spacecraft exist: an engineering qualification model (EQM) and a flight model (FM). This paper presents the verification approach of the functional tests implemented for the EIRSAT-1 project. The activities of the FlatSat and system level full functional tests of the EQM are presented and the results obtained during the test campaigns are discussed. Four test anomalies were encountered during the full functional test campaign resulting in two minor redesigns, and subsequent reassembly, of the CubeSat. The functional test campaigns highlighted the importance of FlatSat level testing of CubeSats to ensure compatibility of all subsystems prior to assembly and of thorough documentation to diagnose any unexpected behaviour of the hardware efficiently. The functional verification of the EQM proved that the system conformed to its design, verifying 57 mission requirements, and is a crucial step towards the development of the EIRSAT-1 FM.
Published: 2021
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26. Web application for galaxy-targeted follow-up of electromagnetic counterparts to gravitational wave sources

Author: Antonio Martin-Carrillo, Lána Salmon, Lorraine Hanlon, and R. M. Jeffrey
Subjects: Gravitational-wave observatory, ComputerSystemsOrganization_COMPUTERSYSTEMIMPLEMENTATION, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, Web application, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, business.industry, Detector, Astronomy, Astronomy and Astrophysics, Python (programming language), Galaxy, LIGO, Space and Planetary Science, User interface, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, computer
Abstract: The Laser Interferometer Gravitational Wave Observatory (LIGO) and Virgo Collaboration's Observing Run 3 has demanded the development of widely-applicable tools for gravitational wave follow-up. These tools must address the main challenges of the multi-messenger era, namely covering large localisation regions and quickly identifying decaying transients. To address these challenges, we present a public web interface to assist astronomers in conducting galaxy-targeted follow-up of gravitational wave events by offering a fast and public list of targets post-gravitational wave trigger. After a gravitational wave trigger, the back-end galaxy retrieval algorithm identifies and scores galaxies based on the LIGO and Virgo computed probabilities and properties of the galaxies taken from the Galaxy List for the Advanced Detector Era (GLADE) V2 galaxy catalogue. Within minutes, the user can retrieve, download, and limit ranked galaxy lists from the web application. The algorithm and website have been tested on past gravitational wave events, and execution times have been analysed. The algorithm is being triggered automatically during Observing Run 3 and its features will be extended if needed. The web application was developed using the Python based Flask web framework. The web application is freely available and publicly accessible at gwtool.watchertelescope.ie., Accepted for publication in Astronomy & Astrophysics
Published: 2019

27. INTEGRAL search for GW counterparts and the GRB170817A/GW170817 detection

Author: Angela Bazzano, Roland Diehl, Sl Brandt, Lorenzo Natalucci, T. J. L. Courvoisier, P. Laurent, Jean-Pierre Roques, R. A. Sunyaev, Francois Lebrun, J. Rodi, Jérôme Chenevez, Elisabeth Jourdain, Lorraine Hanlon, Pietro Ubertini, E. Kuulkers, A. von Kienlin, Antonio Martin-Carrillo, Carlo Ferrigno, V. G. Savchenko, Sandro Mereghetti, Enrico Bozzo, A. A. Lutovinov, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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, and 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)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Gamma ray counterpart, Astrophysics, Kilonova, Magnetar, 01 natural sciences, Gravitational waves, GW170817, 03 medical and health sciences, 0103 physical sciences, 010303 astronomy & astrophysics, General Environmental Science, Physics, 0303 health sciences, GRB170817A, Gravitational wave, Neutron star inspiral, LIGO, Afterglow, Neutron star, 030301 anatomy & morphology, [SDU]Sciences of the Universe [physics], General Earth and Planetary Sciences, General Agricultural and Biological Sciences, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: International audience; The INTernational Gamma-ray Astrophysics Laboratory (INTEGRAL) has detected the Short Gamma-Ray Burst (SGRB), GRB170817A with a signal-to-noise ratio of 4.6 and demonstrated its association with the binary neutron star merging event GW170817 detected by the LIGO and Virgo gravitational wave observatories. The association was immediately evident due to the timing and positional coincidence of this event with the initial error box, derived from gravitational wave (GW) measurements and the contemporaneous detection of a similar gamma-ray signal by Fermi/GBM. This SGRB was detected by the INTEGRAL SPI ACS about 1.7 s after the end of the GW emission, with a fluence of (1.4 ±0.4 ) ×10-7ergcm-2 in the 75-2000 keV energy range. After the serendipitous detection of the short prompt GRB, INTEGRAL continued the planned observation for about 20 h, and then performed a targeted follow-up ToO observation lasting several days. This ToO observation provided a stringent upper limit on any electromagnetic signal in a very broad energy range, from 3 keV to 8 MeV, in particular constraining the soft gamma-ray afterglow flux to 1ergcm-2s-1 in the range 80-300 keV. Exploiting the unique capabilities of INTEGRAL, we constrained the gamma-ray line emission intensity from radioactive decays expected to be the principal source of the energy behind a kilonova event following a NS-NS coalescence. Finally, we put a stringent upper limit on any delayed bursting activity, for example, from a newly formed magnetar. The INTEGRAL prompt detection and the subsequent continuous observations at all wavelengths have provided important constraints on the high energy emission of the resulting kilonova and the post inspiral object: NS, BH, or a new exotic object.
Published: 2019
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28. Transient emission of selected CRTS Cataclysmic Variables

Author: Pieter Meintjes, Johannes Petrus Marais, A. Odendaal, R. J. Britto, Brian van Soelen, David Murphy, Miriam M Nyamai, Mokhine Motsoaledi, Helene Szegedi, Andry Rajoelimanana, Antonio Martin-Carrillo, John R. Thorstensen, and Lorraine Hanlon
Subjects: Physics, Absorption spectroscopy, Accretion disc, Magnitude (astronomy), Emission spectrum, Astrophysics, Mass ratio, Light curve, Spectral line, Optical spectra
Abstract: We present optical photometric and spectroscopic observations of three SU UMa-type dwarf novae, i.e. AR Pic, QW Ser and V521 Peg, conducted in 2016 and 2017. These sources were selected from the Catalina Real-Time Transient Survey and observed during quiescence, outburst (AR Pic and QW Ser) and superoutburst (V521 Peg). For AR Pic, strong flickering in the light curves and an asymmetric double-peaked H$\beta$ emission line in the spectra, confirmed the presence of a very active hot spot. During outburst, detected on 18 February 2017, it exhibited a $\sim 3.3$ magnitude brightening. The projected velocity of the inner edge of the accretion disc is $\sim 2000 \rm~km~s^{-1}$. An outburst of QW Ser was detected on 8 August 2016. Absorption lines, characteristic of an optically thick disc during outburst, were detected and an outflow velocity of $\sim 1000 \rm ~km~s^{-1}$ was determined. Optical spectra during the superoutburst of V521 Peg were obtained for the first time, confirming the superoutburst nature of the outburst, as also observed in other SU UMa-type dwarf novae. The superoutburst was detected on 1 September 2017. Well-defined superhumps were observed, with an average superhump period of $P_{\rm sh} \sim 1.48$ hr. A mass ratio of $q \sim 0.14$ was determined from the period excess of $\varepsilon \sim 3 \%$.
Published: 2018
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29. $INTEGRAL$ Observations of Gravitational-Wave Counterparts & Future Perspectives: Searching for GBM Un-Triggered SGRB with PICsIT

Author: A. A. Lutovinov, Thierry J.-L. Courvoisier, Lorraine Hanlon, R. A. Sunyaev, Flebrun Lebrun, A. von Kienlin, Pietro Ubertini, Søren Brandt, Jérôme Chenevez, E. Jourdain, Erik Kuulkers, J. P. Roques, Sadro Mereghetti, Antonio Martin-Carrillo, V. G. Savchenko, Carlo Ferrigno, Rod Diehl, Philippe Laurent, Enrico Bozzo, Angela Bazzano, Lorenzo Natalucci, James Rodi, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Département d'Astrophysique (ex SAP) (DAP), 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 national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Physics, neutron star: binary, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, gravitational radiation, Binary number, Electromagnetic signal, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, trigger, gamma ray: burst, 01 natural sciences, gravitational radiation detector, electromagnetic field: production, Neutron star, gravitational radiation: emission, 0103 physical sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Gamma-ray burst, 010303 astronomy & astrophysics, Event (particle physics), X-ray: detector, Fermi Gamma-ray Space Telescope
Abstract: International audience; The X-ray/gamma-ray mission \emph{INTEGRAL} detected the short GRB170817A and demonstrated its association to a gravitational wave trigger, GW170817. This marks the first time a binary neutron star merger was detected by the LIGO-Virgo collaboration and that an electromagnetic counterpart to a gravitational wave event has been observed. GRB170817A was detected by the SPI-ACS on-board \emph{INTEGRAL} and the \emph{Fermi}/GBM instruments $ \sim 1.7$ s after the GW event. Following the prompt emission, \emph{INTEGRAL} performed pointed observations for 5.4 days. During this time the instruments provided stringent upper limits on any electromagnetic signal in the 3 keV to 8 MeV range. Interestingly, the GRB was found to be extremely subluminous.In light of these results from GRB170817A, we have begun analysis of soft gamma-ray data ($200 \textrm{ keV } - 2.6 \textrm{ MeV }$) from \emph{INTEGRAL}/PICsIT. With this wide field-of-view instrument, we have begun searching for untriggered SGRBs reported by \emph{Fermi}/GBM as well as preparing for real-time analysis during future LIGO-Virgo observing runs.
Published: 2018
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30. GRB 240529A: A Tale of Two Shocks

Author: Tian-Rui Sun, Jin-Jun Geng, Jing-Zhi Yan, You-Dong Hu, Xue-Feng Wu, Alberto J. Castro-Tirado, Chao Yang, Yi-Ding Ping, Chen-Ran Hu, Fan Xu, Hao-Xuan Gao, Ji-An Jiang, Yan-Tian Zhu, Yongquan Xue, Ignacio Pérez-García, Si-Yu Wu, Emilio Fernández-García, María D. Caballero-García, Rubén Sánchez-Ramírez, Sergiy Guziy, I. Olivares, Carlos Jesus Pérez del Pulgar, A. Castellón, S. Castillo, Ding-Rong Xiong, Shashi B. Pandey, David Hiriart, Guillermo García-Segura, William H. Lee, I. M. Carrasco-García, Il H. Park, S. Jeong, Petrus J. Meintjes, Hendrik J. van Heerden, Antonio Martín-Carrillo, Lorraine Hanlon, Bin-Bin Zhang, L. Hernández-García, Maria Gritsevich, Andrea Rossi, Elisabetta Maiorano, Felice Cusano, Paolo D’Avanzo, Matteo Ferro, Andrea Melandri, Massimiliano De Pasquale, Riccardo Brivio, Min Fang, Lu-Lu Fan, Wei-Da Hu, Zhen Wan, Lei Hu, Ying-Xi Zuo, Jin-Long Tang, Xiao-Ling Zhang, Xian-Zhong Zheng, Bin Li, Wen-Tao Luo, Wei Liu, Jian Wang, Hong-Fei Zhang, Hao Liu, Jie Gao, Ming Liang, Hai-Ren Wang, Da-Zhi Yao, Jing-Quan Cheng, Wen Zhao, and Zi-Gao Dai
Subjects: Gamma-ray bursts, High energy astrophysics, Non-thermal radiation sources, Optical observation, Relativistic jets, Astrophysics, QB460-466
Abstract: Thanks to the rapidly increasing time-domain facilities, we are entering a golden era of research on gamma-ray bursts (GRBs). In this Letter, we report our observations of GRB 240529A with the Burst Optical Observer and Transient Exploring System, the 1.5 m telescope at Observatorio de Sierra Nevada, the 2.5 m Wide Field Survey Telescope of China, the Large Binocular Telescope, and the Telescopio Nazionale Galileo. The prompt emission of GRB 240529A shows two comparable energetic episodes separated by a quiescence time of roughly 400 s. Combining all available data on the GRB Coordinates Network, we reveal the simultaneous apparent X-ray plateau and optical rebrightening around 10 ^3 –10 ^4 s after the burst. Rather than the energy injection from the magnetar as widely invoked for similar GRBs, the multiwavelength emissions could be better explained as two shocks launched from the central engine separately. The optical peak time and our numerical modeling suggest that the initial bulk Lorentz factor of the later shock is roughly 50, which indicates that the later jet should be accretion driven and have a higher mass loading than a typical one. The quiescence time between the two prompt emission episodes may be caused by the transition between different accretion states of a central magnetar or black hole, or the fallback accretion process. A sample of similar bursts with multiple emission episodes in the prompt phase and sufficient follow-up could help to probe the underlying physics of GRB central engines.
Published: 2024
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31. X-shooter and ALMA spectroscopy of GRB 161023A - A study of metals and molecules in the line of sight towards a luminous GRB

Author: Da Xu, A. Gomboc, Steve Schulze, Lekshmi Resmi, Morten W. Hansen, C. Guidorzi, I. de Gregorio-Monsalvo, Shiho Kobayashi, J. Bolmer, Jochen Greiner, Lorraine Hanlon, Stefano Covino, S. R. Oates, David Coward, M. de Pasquale, D. A. Kann, P. J. Meintjes, Alain Klotz, R. Sanchez-Ramirez, Franz E. Bauer, Michał J. Michałowski, Christina C. Thöne, A. de Ugarte Postigo, Antonio Martin-Carrillo, R. Martone, Zach Cano, Johan P. U. Fynbo, Sergio Martín, Sergio Campana, Valerio D'Elia, Luca Izzo, Nial R. Tanvir, David Murphy, Lána Salmon, K. Bensch, Tayyaba Zafar, Klaas Wiersema, S. Kim, A. De Cia, Daniel A. Perley, Carole Mundell, D. H. Hartmann, Jonatan Selsing, B. van Soelen, D. Malesani, D. Turpin, Kasper E. Heintz, Pall Jakobsson, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Ministerio de Economía y Competitividad (España), European Commission, Fundación BBVA, Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Economía, Fomento y Turismo (Chile), German Research Foundation, Alexander von Humboldt Foundation, National Science Centre (Poland), Slovak Research and Development Agency, European Cooperation in Science and Technology, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and 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)
Subjects: Metallicity, Socio-culturale, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, ISM: abundances, spectroscopic [Techniques], 0103 physical sciences, Spectroscopy, ISM [submillimeter], 010303 astronomy & astrophysics, individual: GRB 161023A [Gamma-ray burst], molecules [ISM], QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), abundances [ISM], ISM [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxy, Redshift, ISM: molecules, Afterglow, Stars, gamma-ray burst: individual: GRB 161023A, 13. Climate action, Space and Planetary Science, Content (measure theory), submillimeter: ISM, gamma-ray burst: individual: GRB 161023A / techniques: spectroscopic / ISM: abundances / ISM: molecules / galaxies: ISM / submillimeter: ISM, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, galaxies: ISM
Abstract: Context. Long gamma-ray bursts (GRBs) are produced during the dramatic deaths of massive stars with very short lifetimes, meaning that they explode close to the birth place of their progenitors. Over a short period they become the most luminous objects observable in the Universe, being perfect beacons to study high-redshift star-forming regions. Aims. We aim to use the afterglow of GRB 161023A at a redshift z = 2.710 as a background source to study the environment of the explosion and the intervening systems along its line of sight. Methods. For the first time, we complement ultraviolet (UV), optical and near-infrared (NIR) spectroscopy with millimetre spectroscopy using the Atacama Large Millimeter Array (ALMA), which allows us to probe the molecular content of the host galaxy. The X-shooter spectrum shows a plethora of absorption features including fine-structure and metastable transitions of Fe, Ni, Si, C, and O. We present photometry ranging from 43 s to over 500 days after the burst. Results. We infer a host-galaxy metallicity of [Zn/H] = -1.11 ± 0.07, which, corrected for dust depletion, results in [X/H] = -0.94 ± 0.08. We do not detect molecular features in the ALMA data, but we derive limits on the molecular content of log(N/cm) < 15.7 and log(N/cm, which are consistent with those that we obtain from the optical spectra, log(N/cm)< 15.2 and log(N/cm) < 14.5. Within the host galaxy, we detect three velocity systems through UV, optical and NIR absorption spectroscopy, all with levels that were excited by the GRB afterglow. We determine the distance from these systems to the GRB to be in the range between 0.7 and 1.0 kpc. The sight line to GRB 161023A shows nine independent intervening systems, most of them with multiple components. Conclusions. Although no molecular absorption was detected for GRB 161023A, we show that GRB millimetre spectroscopy is now feasible and is opening a new window on the study of molecular gas within star-forming galaxies at all redshifts. The most favoured lines of sight for this purpose will be those with high metallicity and dust.© ESO 2018., AdUP and CT acknowledge support from Ramon y Cajal fellowships RyC-2012-09975 and RyC-2012-09984 and the Spanish Ministry of Economy and Competitiveness through projects AYA2014-58381-P and AYA2017-89384-P, AdUP furthermore from the BBVA foundation. DAK acknowledges support from the Spanish research project AYA 2014-58381-P, and from Juan de la Cierva Incorporacion fellowship IJCI-2015-26153. FEB acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007) and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). JB acknowledges support through the Sofja Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation of Germany. MJM acknowledges the support of the National Science Centre, Poland through the POLONEZ grant 2015/19/P/ST9/04010; this project has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 665778. AG acknowledges the financial support from the Slovenian Research Agency (research core funding No. P1-0031 and project grant No. J1-8136) and networking support by the COST Action GWverse CA16104. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes 098.A-0055, 098.D-0710 and 0100.D-0649. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00862. T. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.
Published: 2018
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32. The THESEUS space mission concept: science case, design and expected performances

Author: Martino Marisaldi, Enrico Bozzo, Valerie Connaughton, Dorottya Szécsi, D. Malesani, L. Maraschi, B. Cordier, P. D'Avanzo, Salvatore Capozziello, Darach Watson, C. Contini, Maryam Modjaz, Pierluigi Bellutti, M. de Pasquale, C. Guidorzi, Colleen A. Wilson-Hodge, O. Boulade, C. Adami, Y. Evangelista, A. Argan, Johan P. U. Fynbo, Y.-W. Dong, Poshak Gandhi, Allan Hornstrup, Eliana Palazzi, Andrea Bulgarelli, Andrea Comastri, E. Geza, Luciano Burderi, Giuseppe Malaguti, D. de Martino, Irfan Kuvvetli, S.-N. Zhang, Claudio Labanti, Fiamma Capitanio, Luca Izzo, Bradley Cenko, A. Melandri, Umberto Maio, Nicola Omodei, Stefano Ettori, C. Butler, S. D. Vergani, S. Zhang, Lajos G. Balázs, Patricia Schady, Federica B. Bianco, M. Branchesi, Jens Hjorth, Jochen Greiner, Felix Ryde, Jean-Gabriel Cuby, Piero Malcovati, Lorraine Hanlon, Peter G. Jonker, M. Della Valle, Elena Pian, Piotr Orleanski, Etienne Renotte, W. Skidmore, L. Sabau-Graziati, Mauro Dadina, Carl Budtz-Jørgensen, Tomaz Rodic, Giancarlo Ghirlanda, Luigi Piro, Sheila McBreen, M. Fiorini, M. Topinka, Jan Harms, Riccardo Ciolfi, Yi Chen, Giacomo Vianello, Ester Piedipalumbo, Zsolt Bagoly, Aniello Grado, Yuki Kaneko, Vito Sguera, B. Morelli, E. Le Floc'h, Luciano Rezzolla, K. Wiersema, Remo Ruffini, E. Del Monte, J. P. Osborne, M. G. Bernardini, A. Gomboc, A. De Luca, Stefano Covino, Ian Hutchinson, A. Antonelli, Enzo Brocato, Mark R. Sims, M. Razzano, Elisabetta Maiorano, Jean-Luc Atteia, J. Zicha, S. Korpela, Eros Vanzella, V. D'Elia, M. H. P. M. van Putten, Marco Feroci, Carole Mundell, A. V. Penacchioni, J. Soomin, Gabriele Ghisellini, Sandra Savaglio, N. Shigehiro, Andrea Santangelo, Antonio Martin-Carrillo, Avishay Gal-Yam, A. M. Read, Piergiorgio Casella, Giuseppe Baldazzi, B. Ciardi, Pawan Kumar, Li Song, V. Lebrun, G. Zampa, Daisuke Yonetoku, S. Vojtech, Gregor Rauw, Piero Rosati, A. J. Castro-Tirado, Bruce Gendre, Tsvi Piran, A. Rachevski, S. Basa, T. Li, Michela Uslenghi, Gianluca Morgante, Michèle Lavagna, Pascal Chardonnet, Andrew MacFadyen, Asaf Pe'er, Sandro Mereghetti, Alessandro Drago, M. Hafizi, Richard Willingale, D. Morris, Bing Zhang, Paolo Giommi, Andrea Ferrara, Mauro Orlandini, Maria Giovanna Dainotti, N. Masetti, Yuji Urata, Maxim Lyutikov, A. Vacchi, László L. Kiss, E. Campolongo, M. Boer, Lorenzo Amati, Diego Götz, Andrew Blain, M. T. Botticella, C. Tenzer, Monica Colpi, Victor Reglero, Roberto Mignani, Michael S. Briggs, Joseph Caruana, Elizabeth R. Stanway, S. Colafrancesco, Francesca Panessa, H. U. Nargaard-Nielsen, F. Lu, Giuseppe Bertuccio, A. Paizis, P. Romano, S. Vercellone, Luciano Nicastro, S. Paltani, G. Pareschi, G. Stratta, V. Petrosian, João Braga, N. Zampa, Nial Tanvir, James E. Rhoads, Raffaella Margutti, Luca Valenziano, Søren Brandt, S. Boci, Andrea Rossi, Paul J. Callanan, Annalisa Celotti, N. Kawai, René Hudec, Francesco Longo, Primo Attina, G. L. Israel, F. Fuschino, Fabio Finelli, M. Hernanz, Ruben Salvaterra, F. Frontera, P. T. O'Brien, Sergio Campana, Rupal Basak, Riccardo Campana, Eleonora Troja, Jordan Camp, Petr Páta, S. Piranomonte, G. Tagliaferri, Sylvain Guiriec, R. L. C. Starling, B. B. Zhang, Natalia Auricchio, Serena Vinciguerra, Département d'Astrophysique (ex SAP) (DAP), 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, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), 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), Agenzia Spaziale Italiana, European Commission, Czech Grant Agency, ITA, 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), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), 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), THESEUS, Amati, L, O'Brien, P, Götz, D, Bozzo, E, Tenzer, C, Frontera, F, Ghirlanda, G, Labanti, C, Osborne, J, Stratta, G, Tanvir, N, Willingale, R, Attina, P, Campana, R, Castro-Tirado, A, 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, Auricchio, N, Balazs, L, Baldazzi, G, Basa, S, Basak, R, Bellutti, P, Bernardini, M, 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, D'Elia, V, De Martino, D, De 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, Nicastro, L, Palazzi, E, Paltani, S, Panessa, F, Pareschi, G, Pe'Er, A, Penacchioni, A, 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, van Putten, M, Vanzella, E, Vercellone, S, Wilson-Hodge, C, Yonetoku, D, Zampa, G, Zampa, N, Zhang, B, Zhang, S, Antonelli, A, Bianco, F, Boci, S, Boer, M, Botticella, M, Boulade, O, Butler, C, Campana, S, Capitanio, F, Celotti, A, Chen, Y, Colpi, M, Comastri, A, Cuby, J, Dadina, M, De Luca, A, Dong, Y, 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, Páta, P, Petrosian, V, Rachevski, A, Rhoads, J, Ryde, F, Sabau-Graziati, L, Shigehiro, N, Sims, M, Soomin, J, Szécsi, D, Urata, Y, Uslenghi, M, Valenziano, L, Vianello, G, Vojtech, S, Watson, D, Zicha, J, Amati, L., O'Brien, P., Götz, 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., Gian Luca, Israel, 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., De Martino, D., De 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., van 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., De Luca, A., 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., Páta, P., Petrosian, V., Rachevski, A., Rhoads, J., Ryde, F., Sabau-Graziati, L., Shigehiro, N., Sims, M., Soomin, J., Szécsi, D., Urata, Y., Uslenghi, M., Valenziano, L., Vianello, G., Vojtech, S., Watson, D., Zicha, J., 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), 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), ANR-16-CE31-0003,BEaPro,Using the most powerful explosion as probes of the high-redshift Universe(2016), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), 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 ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -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 ), Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Gotz, D., Pata, P., Szecsi, D., Department of Physics, and Amati, L. and O'Brien, P. and Götz, D. and Bozzo, E. and Tenzer, C. and Frontera, F. and Ghirlanda, G. and Labanti, C. and Osborne, J.P. and Stratta, G. and Tanvir, N. and Willingale, R. and Attina, P. and Campana, R. and Castro-Tirado, A.J. and Contini, C. and Fuschino, F. and Gomboc, A. and Hudec, R. and Orleanski, P. and Renotte, E. and Rodic, T. and Bagoly, Z. and Blain, A. and Callanan, P. and Covino, S. and Ferrara, A. and Le Floch, E. and Marisaldi, M. and Mereghetti, S. and Rosati, P. and Vacchi, A. and D'Avanzo, P. and Giommi, P. and Piranomonte, S. and Piro, L. and Reglero, V. and Rossi, A. and Santangelo, A. and Salvaterra, R. and Tagliaferri, G. and Vergani, S. and Vinciguerra, S. and Briggs, M. and Campolongo, E. and Ciolfi, R. and Connaughton, V. and Cordier, B. and Morelli, B. and Orlandini, M. and Adami, C. and Argan, A. and Atteia, J.-L. and Auricchio, N. and Balazs, L. and Baldazzi, G. and Basa, S. and Basak, R. and Bellutti, P. and Bernardini, M.G. and Bertuccio, G. and Braga, J. and Branchesi, M. and Brandt, S. and Brocato, E. and Budtz-Jorgensen, C. and Bulgarelli, A. and Burderi, L. and Camp, J. and Capozziello, S. and Caruana, J. and Casella, P. and Cenko, B. and Chardonnet, P. and Ciardi, B. and Colafrancesco, S. and Dainotti, M.G. and D'Elia, V. and De Martino, D. and De Pasquale, M. and Del Monte, E. and Della Valle, M. and Drago, A. and Evangelista, Y. and Feroci, M. and Finelli, F. and Fiorini, M. and Fynbo, J. and Gal-Yam, A. and Gendre, B. and Ghisellini, G. and Grado, A. and Guidorzi, C. and Hafizi, M. and Hanlon, L. and Hjorth, J. and Izzo, L. and Kiss, L. and Kumar, P. and Kuvvetli, I. and Lavagna, M. and Li, T. and Longo, F. and Lyutikov, M. and Maio, U. and Maiorano, E. and Malcovati, P. and Malesani, D. and Margutti, R. and Martin-Carrillo, A. and Masetti, N. and McBreen, S. and Mignani, R. and Morgante, G. and Mundell, C. and Nargaard-Nielsen, H.U. and Nicastro, L. and Palazzi, E. and Paltani, S. and Panessa, F. and Pareschi, G. and Pe'er, A. and Penacchioni, A.V. and Pian, E. and Piedipalumbo, E. and Piran, T. and Rauw, G. and Razzano, M. and Read, A. and Rezzolla, L. and Romano, P. and Ruffini, R. and Savaglio, S. and Sguera, V. and Schady, P. and Skidmore, W. and Song, L. and Stanway, E. and Starling, R. and Topinka, M. and Troja, E. and van Putten, M. and Vanzella, E. and Vercellone, S. and Wilson-Hodge, C. and Yonetoku, D. and Zampa, G. and Zampa, N. and Zhang, B. and Zhang, B.B. and Zhang, S. and Zhang, S.-N. and Antonelli, A. and Bianco, F. and Boci, S. and Boer, M. and Botticella, M.T. and Boulade, O. and Butler, C. and Campana, S. and Capitanio, F. and Celotti, A. and Chen, Y. and Colpi, M. and Comastri, A. and Cuby, J.-G. and Dadina, M. and De Luca, A. and Dong, Y.-W. and Ettori, S. and Gandhi, P. and Geza, E. and Greiner, J. and Guiriec, S. and Harms, J. and Hernanz, M. and Hornstrup, A. and Hutchinson, I. and Israel, G. and Jonker, P. and Kaneko, Y. and Kawai, N. and Wiersema, K. and Korpela, S. and Lebrun, V. and Lu, F. and MacFadyen, A. and Malaguti, G. and Maraschi, L. and Melandri, A. and Modjaz, M. and Morris, D. and Omodei, N. and Paizis, A. and Páta, P. and Petrosian, V. and Rachevski, A. and Rhoads, J. and Ryde, F. and Sabau-Graziati, L. and Shigehiro, N. and Sims, M. and Soomin, J. and Szécsi, D. and Urata, Y. and Uslenghi, M. and Valenziano, L. and Vianello, G. and Vojtech, S. and Watson, D. and Zicha, J.
Subjects: Ionization, Atmospheric Science, cosmological model, Cherenkov Telescope Array, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, Dark age, MASSIVE SINGLE STARS, Star formation rates, Gamma ray, 01 natural sciences, Cosmology: observation, localization, law.invention, Astrophysic, Einstein Telescope, observational cosmology, law, Observational cosmology, Re-ionization, Cosmology: observations, Dark ages, First stars, Gamma-ray: bursts, LIGO, observations [Cosmology], Telescope, 010303 astronomy & astrophysics, High sensitivity, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Multi-wavelength, energy: high, sezele, gamma-ray bursts, Aerospace Engineering, Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, star: formation, burst [Gamma-ray], observatory, Geophysics, X rays, Cosmology: observation, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, signature, Star, TIDAL DISRUPTION, Gamma-ray: burst, Astrophysics::High Energy Astrophysical Phenomena, SIMILAR-TO 6, Socio-culturale, FOS: Physical sciences, observation [Cosmology], galaxy: luminosity, X-ray astronomy: instrumentation, 7 CANDIDATE GALAXIES, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, 114 Physical sciences, Settore FIS/03 - Fisica della Materia, X-ray, bursts [Gamma-ray], FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, First star, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], KAGRA, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, LIGHT CURVES, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, Astronomy and Astrophysics, 115 Astronomy, Space science, redshift, sensitivity, Redshift, NEUTRON-STAR MERGER, messenger, VIRGO, electromagnetic, LUMINOSITY FUNCTION, BLACK-HOLE, General Earth and Planetary Sciences, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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 GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5¿1 arcmin localization, an energy band extending from several MeV 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).© 2018 COSPAR, S.E. acknowledges the financial support from contracts ASI-INAF 1/009/10/0, NARO15 ASI-INAF 1/037/12/0 and ASI 2015-046-R.0. R.H. acknowledges GACR grant 13-33324S. S.V. research leading to these results has received funding from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement no 606176. D.S. was supported by the Czech grant 1601116S GA CR. Maria Giovanna Dainotti acknowledges funding from the European Union through the Marie Curie Action FP7-PEOPLE-2013-IOF, under grant agreement No. 626267 (>Cosmological Candles>).
Published: 2018
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33. A kilonova as the electromagnetic counterpart to a gravitational-wave source

Author: Markus Kromer, Łukasz Wyrzykowski, M. Smith, A. Franckowiak, John L. Tonry, Phil A. James, H. Flewelling, O. McBrien, Thomas Krühler, Andy Lawrence, Christopher W. Stubbs, Ilan Manulis, R. E. Firth, Franz E. Bauer, Giorgos Leloudas, Jesper Sollerman, B. Stalder, T. Schweyer, Nicholas A. Walton, Christopher Waters, Lluís Galbany, Zach Cano, André Müller, S. J. Prentice, Joseph P. Anderson, Ashley J. Ruiter, Nancy Elias-Rosa, Peter G. Jonker, M. E. Huber, Wolfgang Kerzendorf, Helene Szegedi, Eugene A. Magnier, T. M. Reynolds, P. Clark, A. Razza, J. Palmerio, A. S. B. Schultz, Mariusz Gromadzki, C. Frohmaier, Giacomo Terreran, Jochen Greiner, Lorraine Hanlon, Luc Dessart, Stephen J. Smartt, A. Rest, Antonio Martin-Carrillo, Maria Letizia Pumo, Stefan Taubenberger, Arne Rau, Richard J. Wainscoat, Régis Cartier, J. Bulger, Rupak Roy, Ferdinando Patat, Larry Denneau, Giacomo Cannizzaro, Francesco Taddia, D. Homan, Isobel Hook, Darryl Wright, Claudia P. Gutiérrez, A. Nicuesa Guelbenzu, P. Wiseman, Hanindyo Kuncarayakti, J. Vos, K. C. Chambers, Seppo Mattila, Cristina Barbarino, Mark Sullivan, G. Pignata, Luke J. Shingles, Morgan Fraser, Kate Maguire, A. Hamanowicz, F. Onori, M.-S. Hernandez, Marco Berton, Mark Willman, Ting-Wan Chen, A. Heinze, Jussi Harmanen, A. De Cia, Mattia Bulla, Luca Izzo, David Young, M. Della Valle, Aleksandar Cikota, Michael W. Coughlin, K. W. Smith, Marek Kowalski, T. Lowe, C. Agliozzo, Patricia Schady, Anders Jerkstrand, Georgios Dimitriadis, Lána Salmon, M. R. Magee, Erkki Kankare, A. Flörs, C. Angus, O. Yaron, H. Weiland, Avishay Gal-Yam, M. T. Botticella, Ph. Podsiadlowski, Simon Hodgkin, Cosimo Inserra, Santiago González-Gaitán, S. Klose, Krzysztof A. Rybicki, Chris Ashall, Ivo R. Seitenzahl, Andrea Pastorello, Z. Kostrzewa-Rutkowska, Stuart A. Sim, Rubina Kotak, M. Dennefeld, Kasper E. Heintz, Jakob Nordin, J. D. Lyman, B. van Soelen, D. O'Neill, Oskar Klein Centre [Stockholm], Stockholm University, Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Aberystwyth University, Federal Institute for Geosciences and Natural Resources (BGR), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Department of Particle Physics and Astrophysics, Weizmann Institute of Science [Rehovot, Israël], Laboratoire de recherche en Hydrodynamique, Énergétique et Environnement Atmosphérique (LHEEA), École Centrale de Nantes (ECN)-Centre National de la Recherche Scientifique (CNRS), Physik-Institut, Universität Zürich [Zürich] (UZH), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), SLAC National Accelerator Laboratory (SLAC), Stanford University, Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), Max-Planck-Institut für Extraterrestrische Physik (MPE), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), University of Oxford Astrophysics, Università degli Studi di Roma 'La Sapienza' [Rome], Institut de biologie et chimie des protéines [Lyon] (IBCP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Laboratoire des signaux et systèmes (L2S), Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), The Oskar Klein Centre for Cosmoparticle Physics and Department of Physics, Stockholm University, Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Institut Lavoisier de Versailles (ILV), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), AUTRES, CIC Tours, Centre Hospitalier Régional Universitaire de Tours (CHRU Tours)-Hôpital Bretonneau-Université de Tours-Institut National de la Santé et de la Recherche Médicale (INSERM), Simulation et Traitement de l'information pour l'Exploitation des systèmes de Production (EDF R&D STEP), EDF R&D (EDF R&D), EDF (EDF)-EDF (EDF), Commissariat à l'Energie Atomique, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut de Recherche Contre les Cancers de l'Appareil Digestif-European Institute of Telesurgery (IRCAD/EITS), Université Louis Pasteur - Strasbourg I, Crop and Weed Ecology, Plant Sciences Group, Wageningen University and Research [Wageningen] (WUR), Astronomical Observatory [Warsaw], Faculty of Physics [Warsaw] (FUW), University of Warsaw (UW)-University of Warsaw (UW), Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )
Subjects: neutron star: binary, Astronomy, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics, Kilonova, 01 natural sciences, ddc:070, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, nuclide, QC, ComputingMilieux_MISCELLANEOUS, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], Solar mass, Multidisciplinary, neutron star: mass, radioactivity, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, r-process, Astrophysics::Earth and Planetary Astrophysics, ST/P000495/1, Astrophysics - High Energy Astrophysical Phenomena, velocity, radiation: electromagnetic, Opacity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, gravitational radiation: direct detection, Electromagnetic radiation, 0103 physical sciences, General, STFC, Astrophysics::Galaxy Astrophysics, ta115, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, RCUK, opacity, ST/M005348/1, Galaxy, black hole: binary, 13. Climate action, gravitational radiation: emission, ST/P000312/1, galaxy, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Gravitational waves were discovered with the detection of binary black hole mergers and they should also be detectable from lower mass neutron star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal called a kilonova. The gravitational wave source GW170817 arose from a binary neutron star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC4993, which is spatially coincident with GW170817 and a weak short gamma-ray burst. The transient has physical parameters broadly matching the theoretical predictions of blue kilonovae from neutron star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 +/- 0.01 Msol, with an opacity of kappa, Nature, in press, DOI 10.1038/nature24303. Data files will be made available at http://www.pessto.org
Published: 2017
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34. Colour variations in the GRB 120327A afterglow

Author: Nobuyuki Kawai, Stefano Covino, A. S. Trotter, Om Sharan Salafia, Jochen Greiner, Lorraine Hanlon, D. B. Malesani, F. Nappo, J. Japelj, Aaron P. LaCluyze, M. G. Bernardini, Robert J. Smith, Paul Kuin, Sergio Campana, K. M. Ivarsen, Giancarlo Ghirlanda, Daisuke Kuroda, Gianpiero Tagliaferri, P. D'Avanzo, Ruben Salvaterra, B. E. Cobb, Javier Gorosabel, F. J. Virgili, Valerio D'Elia, Dino Fugazza, H. Hanayama, J. Bolmer, C. Guidorzi, Shiho Kobayashi, Josh Haislip, M. Topinka, A. Gomboc, Martin Jelínek, Iain A. Steele, Antonio Martin-Carrillo, Carole Mundell, Jae Woo Kim, B. Sbarufatti, Drejc Kopač, Daniel E. Reichart, A. Melandri, E. Zaninoni, S. D. Vergani, Myungshin Im, David Murphy, European Commission, Slovenian Research Agency, National Research Foundation of Korea, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), 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), Laboratoire Univers et Particules de Montpellier ( LUPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ), Galaxies, Etoiles, Physique, Instrumentation ( GEPI ), and 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 )
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: individual: GRB 120327A, dust, extinction, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, NO, 0103 physical sciences, Spectral analysis, individual: GRB 120327A [Gamma-ray burst], 010303 astronomy & astrophysics, QC, Dust, extinction, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, 010308 nuclear & particles physics, extinction, Spectral density, Astronomy and Astrophysics, Light curve, gamma-ray burst: individual: GRB 120327A, Afterglow, Space and Planetary Science, dust, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Event (particle physics), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Aims. We present a comprehensive temporal and spectral analysis of the long Swift GRB 120327A afterglow data to investigate possible causes of the observed early-time colour variations. Methods. We collected data from various instruments and telescopes in X-ray, ultraviolet, optical, and near-infrared bands, and determined the shapes of the afterglow early-time light curves. We studied the overall temporal behaviour and the spectral energy distributions from early to late times. Results. The ultraviolet, optical, and near-infrared light curves can be modelled with a single power-law component between 200 and 2 × 10 s after the burst event. The X-ray light curve shows a canonical steep-shallow-steep behaviour that is typical of long gamma-ray bursts. At early times a colour variation is observed in the ultraviolet/optical bands, while at very late times a hint of a re-brightening is visible. The observed early-time colour change can be explained as a variation in the intrinsic optical spectral index, rather than an evolution of the optical extinction.© 2017 ESO., A.M., S.Co., S.Ca., B.S., P.D.A., and G.T. acknowledge support from the ASI grant I/004/11/3. E.Z. acknowledges the support by the International Cooperation Program CAPES-ICRANet financed by CAPES Brazilian Federal Agency for Support and Evaluation of Graduate Education within the Ministry of Education of Brazil. D.M. acknowledges support from the Instrument center for Danish Astrophysics (IDA). C.G.M. acknowledges support from the Royal Society, the Wolfson Foundation, and the Science and Technology Facilities Council. L.H. acknowledges support from SFI (07-RFP-PHYF295, 11/RFP.1/AST/3188) and the EU-FP7/GLORIA (grant No. 283783). M.I. and J.W.K. acknowledge the support from the National Research Foundation of Korea grant Nos. 2017R1A3A3001362 and 2016R1D1A1B03934815. D.K. acknowledges the financial support from the Slovenian Research Agency (P1-0188). This work has been supported by ASI grant I/004/11/0 and by PRIN-MIUR 2009 grants.
Published: 2017
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35. INTEGRAL IBIS, SPI, and JEM-X observations of LVT151012

Author: Lorraine Hanlon, V. G. Savchenko, Thomas Siegert, J. P. Roques, Carlo Ferrigno, Søren Brandt, Lorenzo Natalucci, Ph. Laurent, Erik Kuulkers, Alexander A. Lutovinov, Rashid Sunyaev, A. von Kienlin, Angela Bazzano, Roland Diehl, Jérôme Chenevez, Pietro Ubertini, Sandro Mereghetti, Antonio Martin-Carrillo, Enrico Bozzo, F. Lebrun, Thierry J.-L. Courvoisier, 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 ), CEA/DSM, Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, 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 ), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-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 de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), bursts [X-rays], media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, black hole physics, satellite, FOS: Physical sciences, Astrophysics, Radiation, 01 natural sciences, localization, Gravitational waves, X-ray, Coincident, 0103 physical sciences, gravitational radiation: energy, LIGO, 010306 general physics, X-rays: bursts, 010303 astronomy & astrophysics, detectors [Instrumentation], media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, instrumentation: detectors, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, Astronomy and Astrophysics, trigger, Black hole physics, Afterglow, VIRGO, electromagnetic, gravitational waves, Space and Planetary Science, Sky, gamma ray, spectral, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Event (particle physics), Energy (signal processing), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: During the first observing run of LIGO, two gravitational wave events and one lower-significance trigger (LVT151012) were reported by the LIGO/Virgo collaboration. At the time of LVT151012, the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) was pointing at a region of the sky coincident with the high localization probability area of the event and thus permitted us to search for its electromagnetic counterpart (both prompt and afterglow emission). The imaging instruments on-board INTEGRAL (IBIS/ISGRI, IBIS/PICsIT, SPI, and the two JEM-X modules) have been exploited to attempt the detection of any electromagnetic emission associated with LVT151012 over 3 decades in energy (from 3 keV to 8 MeV). The omni-directional instruments on-board the satellite, i.e. the SPI-ACS and IBIS monitored the entire LVT151012 localization region at energies above 75 keV. We did not find any significant transient source that was spatially and/or temporally coincident with LVT151012, obtaining tight upper limits on the associated hard X-ray and $\gamma$-ray radiation. For typical spectral models, the upper limits on the fluence of the emission from any 1 s long-lasting counterpart of LVT151012 ranges from $F_{\gamma}=$3.5$\times$10$^{-8}$ erg cm$^{-2}$ (20 - 200 keV) to $F_{\gamma}$=7.1$\times$10$^{-7}$ erg cm$^{-2}$ (75 - 2000 keV), constraining the ratio of the isotropic equivalent energy released in the electromagnetic emission to the total energy of the gravitational waves: $E_{75-2000~keV}/E_{GW}, Comment: accepted for publication in A&A
Published: 2017
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36. INTEGRAL Detection of the First Prompt Gamma-Ray Signal Coincident with the Gravitational-wave Event GW170817

Author: Lorraine Hanlon, Pietro Ubertini, Antonio Martin-Carrillo, James Rodi, Thierry J.-L. Courvoisier, Roland Diehl, R. A. Sunyaev, Sandro Mereghetti, Søren Brandt, A. Domingo, J. P. Roques, V. G. Savchenko, Carlo Ferrigno, Elisabeth Jourdain, Enrico Bozzo, Erik Kuulkers, F. Lebrun, Alexander A. Lutovinov, Jérôme Chenevez, A. von Kienlin, Ph. Laurent, Angela Bazzano, Lorenzo Natalucci, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), 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), Département d'Astrophysique (ex SAP) (DAP), 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, 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), 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 ), 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 ), Département d'Astrophysique (ex SAP) ( DAP ), 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 national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: noise, coalescence, neutron star: binary, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, general [Gamma rays], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Kilonova, gamma ray: burst, Magnetar, 01 natural sciences, GLAST, decay, Gravitational waves, 0103 physical sciences, gamma ray: flux, LIGO, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Gravitational wave, Gamma ray, gravitational radiation, Astronomy and Astrophysics, magnetar, gamma rays: general, Afterglow, general [Gamma-ray burst], observatory, Neutron star, error: statistical, VIRGO, electromagnetic, gravitational waves, Space and Planetary Science, radioactivity, spectral, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We report the e INTernational Gamma-ray Astrophysics Laboratory (INTEGRAL) detection of the short gamma-ray burst GRB 170817A (discovered by Fermi-GBM) with a signal-to-noise ratio of 4.6, and, for the first time, its association with the gravitational waves (GWs) from binary neutron star (BNS) merging event GW170817 detected by the LIGO and Virgo observatories. The significance of association between the gamma-ray burst observed by INTEGRAL and GW170817 is 3.2 $\sigma$, while the association between the Fermi-GBM and INTEGRAL detections is 4.2 $\sigma$. GRB 170817A was detected by the SPI-ACS instrument about 2 s after the end of the gravitational wave event. We measure a fluence of $(1.4 \pm 0.4 \pm 0.6) \times$10$^{-7}$ erg cm$^{-2})$ (75--2000 keV), where, respectively, the statistical error is given at the 1 $\sigma$ confidence level, and the systematic error corresponds to the uncertainty in the spectral model and instrument response. We also report on the pointed follow-up observations carried out by INTEGRAL, starting 19.5 h after the event, and lasting for 5.4 days. We provide a stringent upper limit on any electromagnetic signal in a very broad energy range, from 3 keV to 8 MeV, constraining the soft gamma-ray afterglow flux to $, Comment: ApJ Letters published
Published: 2017
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37. High energy emission and polarisation limits for the INTEGRAL burst GRB 061122

Author: Sinéad McGlynn, R. O'Connor, Suzanne Foley, Sheila McBreen, A. J. Dean, Lorraine Hanlon, Antonio Martin-Carrillo, B. McBreen, and D. J. Clark
Subjects: Physics, Jet (fluid), Range (particle radiation), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Field of view, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spitzer Space Telescope, Space and Planetary Science, Black-body radiation, Gamma-ray burst, Ejecta, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: (Abridged) GRB 061122 is one of the brightest GRBs detected within INTEGRAL's field of view to date. The two gamma-ray detectors on INTEGRAL were used to investigate the spectral characteristics of GRB 061122. A search for linear polarisation in the prompt emission was carried out using the SPI multiple event data in the energy range 100 keV-1 MeV. The prompt spectrum was best fit by a combination of a blackbody and a power--law model (the quasithermal model), with evidence for high energy emission continuing above 8 MeV. A pseudo-redshift value of pz = 0.95 +/- 0.18 was determined using the spectral fit parameters. The isotropic energy at this pseudo-redshift is 8.5 x 10^{52} erg. The jet opening angle was estimated to be smaller than 2.8 deg or larger than 11.9 deg from the X-ray lightcurve. An upper limit of 60% polarisation was determined for the prompt emission of GRB 061122, using the multiple event data. The high energy emission observed in the spectrum may be due to the reverse shock interacting with the GRB ejecta when it is decelerated by the circumburst medium. This behaviour has been observed in a small fraction of GRBs to date, but is expected to be more commonly observed by the Fermi Gamma-ray Space Telescope. The conditions for polarisation are met if the jet opening angle is less than 2.8 deg, but further constraints on the level of polarisation are not possible., Comment: 9 pages, 6 figures, accepted for publication in Astronomy & Astrophysics
Published: 2009
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38. Python in Astronomy 2015 links: initial release

Author: Pauline Barmby and Antonio Martin-Carrillo
Subjects: GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries)
Abstract: List of links to packages discussed by workshop participants
Published: 2015
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39. talk_slides: Talk slides from Python in Astronomy 2015, v1.0

Author: Pauline Barmby, Vanessa Moss, Nadia Dencheva, Steve Crawford, Becky Smethurst, Perry Greenfield, Emillie Ishida, Wolfgang Kerzendorf, Víctor Terrón, Matt Craig, Mathieu Servillat, Kyle Barbary, Antonio Martin-Carrillo, Erik Tollerud, Britton Smith, and Joe Zuntz
Abstract: Initial release.
Published: 2015
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40. The accretion environment in Vela X-1 during a flaring period using XMM-Newton

Author: Felix Fürst, Peter Kretschmar, S. Martínez-Núñez, Joern Wilms, A. M. T. Pollock, J. J. Rodes-Roca, Jose M. Torrejon, Antonio Martin-Carrillo, Matthias Kühnel, M. Stuhlinger, Ingo Kreykenbohm, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, and Astronomía y Astrofísica
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Vela, Luminosity, law.invention, individual: Vela X-1 [Pulsars], Neutron star, Space and Planetary Science, law, Light echo, Física Aplicada, Astrophysics::Solar and Stellar Astrophysics, binaries [X-rays], Emission spectrum, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Flare, Eclipse
Abstract: We present analysis of 100 ks contiguous XMM-Newton data of the prototypical wind accretor Vela X-1. The observation covered eclipse egress between orbital phases 0.134 and 0.265, during which a giant flare took place, enabling us to study the spectral properties both outside and during the flare. This giant flare with a peak luminosity of $3.92^{+0.42}_{-0.09} \times 10^{37}$ erg s$^{-1}$ allows estimates of the physical parameters of the accreted structure with a mass of $\sim$ $10^{21}$ g. We have been able to model several contributions to the observed spectrum with a phenomenological model formed by three absorbed power laws plus three emission lines. After analysing the variations with orbital phase of the column density of each component, as well as those in the Fe and Ni fluorescence lines, we provide a physical interpretation for each spectral component. Meanwhile, the first two components are two aspects of the principal accretion component from the surface of the neutron star, and the third component seems to be the \textit{X-ray light echo} formed in the stellar wind of the companion., Accepted. Astronomy and Astrophysics, 2013
Published: 2014

41. GRB 120711A: an intense INTEGRAL burst with long-lasting soft γ-ray emission and a powerful optical flash

Author: A. S. Trotter, Stefano Covino, Sinéad McGlynn, M. Topinka, D. A. Kann, S. Meehan, Patricia Schady, V. Savchenko, D. Fugazza, A. P. LaCluyze, D. Reichart, Colin Wade, Jochen Greiner, David Murphy, P. Tisdall, Lorraine Hanlon, A. M. Rossi, B. McBreen, Antonio Martin-Carrillo, Thomas Krühler, J. B. Haislip, S. Klose, J. Elliott, 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), European Project: 283783,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2011-2,GLORIA(2011), 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), Observatoire de Paris, and 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)
Subjects: Brightness, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Synchrotron radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, 0103 physical sciences, gamma-ray burst: individual: GRB 041219A, gamma-ray burst: individual: GRB 130427A, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma ray, GRB 130427A, Astronomy and Astrophysics, Afterglow, Lorentz factor, 13. Climate action, Space and Planetary Science, gamma-ray burst: individual: GRB 120711A, symbols, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract: A long and intense gamma-ray burst (GRB) was detected by INTEGRAL on July 11 2012 with a duration of ~115s and fluence of 2.8x10^-4 erg cm^-2 in the 20 keV-8 MeV energy range. GRB 120711A was at z~1.405 and produced soft gamma-ray emission (>20 keV) for at least ~10 ks after the trigger. The GRB was observed by several ground-based telescopes that detected a powerful optical flash peaking at an R-band brightness of ~11.5 mag at ~126 s after the trigger. We present a comprehensive temporal and spectral analysis of the long-lasting soft gamma-ray emission detected in the 20-200 keV band with INTEGRAL, the Fermi/LAT post-GRB detection above 100 MeV, the soft X-ray afterglow from XMM-Newton, Chandra, and Swift and the optical/NIR detections from Watcher, Skynet, GROND, and REM. We modelled the long-lasting soft gamma-ray emission using the standard afterglow scenario, which indicates a forward shock origin. The combination of data extending from the NIR to GeV energies suggest that the emission is produced by a broken power-law spectrum consistent with synchrotron radiation. The afterglow is well modelled using a stratified wind-like environment with a density profile k~1.2, suggesting a massive star progenitor (i.e. Wolf-Rayet). The analysis of the reverse and forward shock emission reveals an initial Lorentz factor of ~120-340, a jet half-opening angle of ~2deg-5deg, and a baryon load of ~10^-5-10^-6 Msun consistent with the expectations of the fireball model when the emission is highly relativistic. Long-lasting soft gamma-ray emission from other INTEGRAL GRBs with high peak fluxes, such as GRB 041219A, was not detected, suggesting that a combination of high Lorentz factor, emission above 100 MeV, and possibly a powerful reverse shock are required. Similar long-lasting soft gamma-ray emission has recently been observed from the nearby and extremely bright Fermi/LAT burst GRB 130427A., 21 pages, 10 figures. Accepted for publication in Astronomy and Astrophysics
Published: 2014
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42. X-ray behaviour of GRBs detected by INTEGRAL/JEM-X

Author: Lorraine Hanlon and Antonio Martin-Carrillo
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), X-ray, Phase (waves), FOS: Physical sciences, Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Astrophysics - Cosmology and Nongalactic Astrophysics, Afterglow
Abstract: INTEGRAL's JEM-X instrument offers a very rare opportunity to observe the full prompt X-ray emission from GRBs and the transition to the afterglow phase. A study of prompt X-ray flares in some bursts from the INTEGRAL GRB sample and the early X-ray post-GRB emission from 3-35 keV is presented here. Significant post-GRB emission above 10 keV is observed for GRB 041219A and GRB 081003A., Comment: Proceedings of the 9th INTEGRAL Workshop "An INTEGRAL view of the high-energy sky (the first 10 years)", Paris, 15-19 October 2012
Published: 2013
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43. Temporal properties of Swift GRBs with known redshifts

Author: Lorraine Hanlon, B. McBreen, Roger Edwin O'Connor, Antonio Martin-Carrillo, Sheila McBreen, and Suzanne Foley
Subjects: Physics, Swift, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Pulse (physics), Wavelet, Amplitude, Log-normal distribution, Frequency distribution, Gamma-ray burst, computer, computer.programming_language
Abstract: The Swift Gamma Ray Burst (GRB) mission has enabled the rapid detection of GRBs and the determination of the redshift of a greater proportion of source counterparts than previous missions. The mean redshift of the Swift GRBs is significantly higher than that of earlier missions. We present the results of a temporal analysis performed on 134 Swift long GRBs with known redshift. ‡ The GRBs were denoised using wavelets and subjected to an automatic pulse selection algorithm with the objective of identifying pulses. The rise times, fall times, full-width at half-maxima (FWHM), pulse amplitudes and pulse areas were measured and the frequency distributions of some of them are presented here. The results provide a comprehensive description of the pulse profiles in Swift GRBs with known redshift, determining that the temporal properties are consistent with lognormal distributions and that correcting for the known redshift of the source does not have a significant impact on the distributions. Lognormal distributions arise from random multiplicative processes and abound in a variety of natural phenomena.
Published: 2011
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44. Classiﬁcation of gamma-ray bursts observed by INTEGRAL

Author: Antonio Martin-Carrillo
Subjects: Physics, Astrophysics, Gamma-ray burst
Published: 2011
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45. Spectral Cross-Calibration of Fermi-GBM and INTEGRAL-ISGRI using Gamma-Ray Bursts

Author: Lorraine Hanlon, S. Meehan, Antonio Martin-Carrillo, Sheila McBreen, M. Topinka, Dave Tierney, and Suzanne Foley
Subjects: Physics, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Measure (physics), Flux, Astrophysics, Power law, law.invention, Data set, Optics, Data acquisition, law, Radar, business, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: We present an extended cross‐calibration study between the Fermi Gamma‐Ray Burst Monitor (GBM) and the INTEGRAL Soft Gamma‐Ray Imager ISGRI. A previous sample contained 4 GRBs; GRB081226B; GRB090107B; GRB090625B and GRB090704. A long burst detected by both instruments, GRB090817, provides us with the opportunity to further test the agreement between the previous sample and the new data. GRB090817 contains significant telemetry gaps in the ISGRI data set and methods were devised to account for these gaps. The combined datasets from both instruments for GRB090817 were fit with 3 separate spectral models—a Power Law (PL), Cut‐Off Power Law (COPL) and a Band model. The best fit joint spectral model is shown for the time averaged and time resolved joint spectral fits. As a measure of relative flux between the two instruments, a normalisation constant was calculated from the joint spectral fitting.
Published: 2011
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46. Search for late post-GRB emission with IBIS

Author: S. Meehan, M. Topinka, Antonio Martin-Carrillo, B. McBreen, Lorraine Hanlon, and Suzanne Foley
Subjects: Ibis, Physics, biology, Astronomy, Gamma-ray burst, biology.organism_classification
Published: 2010
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47. Short Gamma Ray Bursts Detected by INTEGRAL

Author: B. McBreen, Suzanne Foley, Lorraine Hanlon, M. Topinka, R. O'Connor, S. Meehan, and Antonio Martin-Carrillo
Subjects: Physics, Astrophysics, Gamma-ray burst
Published: 2010
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48. Observations of GRB 080723B with INTEGRAL

Author: Martin Topinka, Antonio Martin-Carrillo, Seamus Meehan, Lorraine Hanlon, Brian McBreen, Nobuyuki Kawai, and Shigehiro Nagataki
Subjects: Ibis, Physics, Photon, biology, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Cosmic ray, Astrophysics, Light curve, biology.organism_classification, Spectral line, Particle detector, Spectral evolution, Astrophysics::Solar and Stellar Astrophysics, Gamma-ray burst
Abstract: GRB 080723B was a long and intense gamma‐ray burst detected and localized by the INTEGRAL satellite featuring combined observations from both main instruments on‐board, IBIS and SPI. The burst was composed of several well separated peaks, allowing the time‐resolved spectral evolution to be studied. IBIS and SPI spectra and light curves for the prompt emission are presented.
Published: 2010
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49. Spectral and temporal properties of long GRBs detected by INTEGRAL from 3 keV to 8 MeV

Author: Lorraine Hanlon, M. Topinka, B. McBreen, Antonio Martin-Carrillo, Dave Tierney, S. Meehan, Søren Brandt, and Suzanne Foley
Subjects: Physics, Range (particle radiation), Astrophysics::High Energy Astrophysical Phenomena, Detector, Field of view, Astrophysics, Gamma-ray burst, Light curve, Afterglow
Abstract: Since its launch in 2002, INTEGRAL has triggered onmore than 78 g –ray bursts in the 20-200 keV energy range with the IBIS/ISGRI instrument. Almost 30% of these bursts occurred within the fully coded field of view of the JEM-X detector (5) which operates in the 3-35 keV energy range. A detailed study of the spectral and temporal evolution of a subset of 7 INTEGRAL g – ray bursts across a wide energy range from 3 keV to 8MeV has been carried out. This GRBsample is characterised by long multi-peaked bursts that are bright in the JEM-X energy range and encompass X-ray rich bursts, X-ray flashes and classical GRBs. We report the detection of X-ray prompt and afterglow emission from GRB 041219A and GRB081003A with JEM-X for the first time. At least two temporal breaks have been identified in the X-ray afterglow light curve of GRB 081003A. These results demonstrate INTEGRAL’s broadband capabilities for the studyof the transition from X-ray prompt to afterglow emission in g –ray bursts.
Published: 2010

50. The relative and absolute timing accuracy of the EPIC-pn camera onXMM-Newton, from X-ray pulsations of the Crab and other pulsars

Author: Uwe Lammers, M. Stuhlinger, Eckhard Kendziorra, Isabel Caballero, Natalie A. Webb, Michael Freyberg, R. D. Saxton, Matteo Guainazzi, K. Mukerjee, Antonio Martin-Carrillo, A. Ibarra, Slawomir Suchy, Marcus Kirsch, G. Schönherr, A. Wellbrock, and Ruediger Staubert
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Crab Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Ranging, Time shifting, Astrophysics, Light curve, Pulsar, Space and Planetary Science, Observatory, Calibration, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM), Noise (radio)
Abstract: Reliable timing calibration is essential for the accurate comparison of XMM-Newton light curves with those from other observatories, to ultimately use them to derive precise physical quantities. The XMM-Newton timing calibration is based on pulsar analysis. However, as pulsars show both timing noise and glitches, it is essential to monitor these calibration sources regularly. To this end, the XMM-Newton observatory performs observations twice a year of the Crab pulsar to monitor the absolute timing accuracy of the EPIC-pn camera in the fast Timing and Burst modes. We present the results of this monitoring campaign, comparing XMM-Newton data from the Crab pulsar (PSR B0531+21) with radio measurements. In addition, we use five pulsars (PSR J0537-69, PSR B0540-69, PSR B0833-45, PSR B1509-58 and PSR B1055-52) with periods ranging from 16 ms to 197 ms to verify the relative timing accuracy. We analysed 38 XMM-Newton observations (0.2-12.0 keV) of the Crab taken over the first ten years of the mission and 13 observations from the five complementary pulsars. All the data were processed with the SAS, the XMM-Newton Scientific Analysis Software, version 9.0. Epoch folding techniques coupled with \chi^{2} tests were used to derive relative timing accuracies. The absolute timing accuracy was determined using the Crab data and comparing the time shift between the main X-ray and radio peaks in the phase folded light curves. The relative timing accuracy of XMM-Newton is found to be better than 10^{-8}. The strongest X-ray pulse peak precedes the corresponding radio peak by 306\pm9 \mus, which is in agreement with other high energy observatories such as Chandra, INTEGRAL and RXTE. The derived absolute timing accuracy from our analysis is \pm48 \mus., Comment: 16 pages, 9 figures. Accepted for publication on A&A
Published: 2012
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