Author: "Malacaria, C." - Searchworks@Jio Institute Digital Library Search Results

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263 results on '"Malacaria, C."'

1. GRB 221009A: the B.O.A.T Burst that Shines in Gamma Rays

Author: Axelsson, M., Ajello, M., Arimoto, M., Baldini, L., Ballet, J., Baring, M. G., Bartolini, C., Bastieri, D., Gonzalez, J. Becerra, Bellazzini, R., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bruel, P., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Cheung, C. C., Chiaro, G., Cibrario, N., Ciprini, S., Cozzolongo, G., Orestano, P. Cristarella, Crnogorcevic, M., Cuoco, A., Cutini, S., D'Ammando, F., De Gaetano, S., Di Lalla, N., Dinesh, A., Di Tria, R., Di Venere, L., Domínguez, A., Fegan, S. J., Ferrara, E. C., Fiori, A., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Galanti, G., Gargano, F., Gasbarra, C., Germani, S., Giacchino, F., Giglietto, N., Giliberti, M., Gill, R., Giordano, F., Giroletti, M., Granot, J., Green, D., Grenier, I. A., Guiriec, S., Gustafsson, M., Hashizume, M., Hays, E., Hewitt, J. W., Horan, D., Kayanoki, T., Kuss, M., Laviron, A., Li, J., Liodakis, I., Longo, F., Loparco, F., Lorusso, L., Lott, B., Lovellette, M. N., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Martí-Devesa, G., Martinelli, R., Castellanos, I. Martinez, Mazziotta, M. N., McEnery, J. E., Mereu, I., Meyer, M., Michelson, P. F., Mirabal, N., Mitthumsiri, W., Mizuno, T., Monti-Guarnieri, P., Monzani, M. E., Morishita, T., Morselli, A., Moskalenko, I. V., Negro, M., Niwa, R., Omodei, N., Orienti, M., Orlando, E., Paneque, D., Panzarini, G., Persic, M., Pesce-Rollins, M., Petrosian, V., Pillera, R., Piron, F., Porter, T. A., Principe, G., Racusin, J. L., Rainò, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ryde, F., Sánchez-Conde, M., Parkinson, P. M. Saz, Serini, D., Sgrò, C., Sharma, V., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Tak, D., Thayer, J. B., Torres, D. F., Valverde, J., Zaharijas, G., Lesage, S., Briggs, M. S., Burns, E., Bala, S., Bhat, P. N., Cleveland, W. H., Dalessi, S., de Barra, C., Gibby, M., Giles, M. M., Hamburg, R., Hristov, B. A., Hui, C. M., Kocevski, D., Mailyan, B., Malacaria, C., McBreen, S., Poolakkil, S., Roberts, O. J., Scotton, L., Veres, P., von Kienlin, A., Wilson-Hodge, C. A., and Wood, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a complete analysis of Fermi Large Area Telescope (LAT) data of GRB 221009A, the brightest Gamma-Ray Burst (GRB) ever detected. The burst emission above 30 MeV detected by the LAT preceded by 1 s the low-energy (< 10 MeV) pulse that triggered the Fermi Gamma-Ray Burst Monitor (GBM), as has been observed in other GRBs. The prompt phase of GRB 221009A lasted a few hundred seconds. It was so bright that we identify a Bad Time Interval (BTI) of 64 seconds caused by the extremely high flux of hard X-rays and soft gamma rays, during which the event reconstruction efficiency was poor and the dead time fraction quite high. The late-time emission decayed as a power law, but the extrapolation of the late-time emission during the first 450 seconds suggests that the afterglow started during the prompt emission. We also found that high-energy events observed by the LAT are incompatible with synchrotron origin, and, during the prompt emission, are more likely related to an extra component identified as synchrotron self-Compton (SSC). A remarkable 400 GeV photon, detected by the LAT 33 ks after the GBM trigger and directionally consistent with the location of GRB 221009A, is hard to explain as a product of SSC or TeV electromagnetic cascades, and the process responsible for its origin is uncertain. Because of its proximity and energetic nature, GRB 221009A is an extremely rare event., Comment: 60 pages, 38 figures, 9 tables
Published: 2024

2. The giant outburst of EXO 2030+375 II: Broadband spectroscopy and evolution

Author: Ballhausen, R., Thalhammer, P., Pradhan, P., Sokolova-Lapa, E., Stierhof, J., Pottschmidt, K., Wilms, J., Coley, J. B., Kretschmar, P., Fuerst, F., Becker, P., West, B., Malacaria, C., Wolff, M. T., Rothschild, R., and Staubert, R.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In 2021, the high-mass X-ray binary EXO 2030+375 underwent a giant X-ray outburst, the first since 2006, that reached a peak flux of ${\sim}600\,\mathrm{mCrab}$ (3-50\,keV). The goal of this work is to study the spectral evolution over the course of the outburst, search for possible cyclotron resonance scattering features (CRSFs), and to associate spectral components with the emission pattern of the accretion column. We used broadband spectra taken with the Nuclear Spectroscopic Telescope Array (NuSTAR), the Neutron Star Interior Composition Explorer (NICER), and Chandra near the peak and during the decline phase of the outburst. We describe the data with established empirical continuum models and perform pulse-phase-resolved spectroscopy. We compare the spectral evolution with pulse phase using a proposed geometrical emission model. We find a significant spectral hardening toward lower luminosity, a behavior that is expected for super-critical sources. The continuum shape and evolution cannot be described by a simple power-law model with exponential cutoff; it requires additional absorption or emission components. We can confirm the presence of a narrow absorption feature at ${\sim}10\,\mathrm{keV}$ in both NuSTAR observations. The absence of harmonics puts into question the interpretation of this feature as a CRSF. The empirical spectral components cannot be directly associated with identified emission components from the accretion column., Comment: 12 pages, 8 figures, accepted in A&A
Published: 2024

3. Probing the emission mechanism and nature of the pulsating compact object in the X-ray binary SAX J1324.4-6200

Author: Ducci, L., Bozzo, E., Burgay, M., Malacaria, C., Ridolfi, A., Romano, P., Serim, M. M., Vercellone, S., and Santangelo, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Recently, there has been renewed interest in the Be X-ray binary (Be/XRB) SAX J1324.4-6200 because of its spatial coincidence with a gamma-ray source detected by Fermi/LAT. To explore more thoroughly its properties, new observations were carried out in 2023 by NuSTAR, XMM-Newton, and Swift, jointly covering the energy range 0.2-79 keV. The X-ray spectrum of SAX J1324.4-6200 fits well with an absorbed power law with a high energy cut-off. We measured a NuSTAR spin period of 175.8127 +/- 0.0036 s and an XMM-Newton spin period of 175.862 +/- 0.025 s. All the available spin period measurements of SAX J1324.4-6200, spanning 29 years, are correlated with time, resulting in a remarkably stable spin-down of dP/dt=(6.09 +/- 0.06)*1E-9 s/s. If SAX J1324.4-6200 hosts an accretion powered pulsar, accretion torque models indicate a surface magnetic field of ~1E12-1E13 G. The X-ray properties emerging from our analysis strenghten the hypothesis that SAX J1324.4-6200 belongs to the small group of persistent Be/XRBs. We also performed radio observations with the Parkes Murriyang telescope, to search for radio pulsations. However, no radio pulsations compatible with the rotational ephemeris of SAX J1324.4-6200 were detected. We rule out the hypothesis that SAX J1324.4-6200 is a gamma-ray binary where the emission is produced by interactions between the pulsar and the companion winds. Other models commonly used to account for the production of gamma-rays in accreting pulsars cannot reproduce the bright emission from SAX J1324.4-6200. We examined other mechanisms for the gamma-ray emission and noted that there is a ~0.5% chance probability that an unknown extragalactic AGN observed through the Galactic plane may coincidentally fall within the Fermi/LAT error circle of the source and be the responsible of the gamma-ray emission. [Abridged], Comment: Accepted for publication in Astronomy and Astrophysics
Published: 2024
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4. Unveiling the origin of the optical/UV emission from the Galactic ULX Swift J0243.6+6124 during its 2017-2018 giant outburst

Author: Alfonso-Garzón, J., Eijnden, J. van den, Kuin, N. P. M., Fürst, F., Rouco-Escorial, A., Fabregat, J., Reig, P., Mas-Hesse, J. M., Jenke, P. A., Malacaria, C., and Wilson-Hodge, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: From late September 2017 to February 2018, the Be X-ray binary (BeXB) Swift J0243.6+6124 underwent an unprecedently bright giant outburst. The reported X-ray luminosities were so high that the system was classified as an Ultraluminous X-ray source (ULX). It was also the first BeXB pulsar showing radio jet emission. The source was not only bright in X-rays and radio, but also in optical and UV wavelenghts. In this paper we aim to understand the origin of the observed optical/UV fluxes simultaneous to the X-ray emission. We studied the optical/UV light curves in comparison with the X-ray fluxes along the outburst, considering the main mechanisms that can explain the optical/UV emission in X-ray binaries. Due to the tight correlation observed between the optical/UV and X-ray light curves, reprocessing of X-rays seems to be the most plausible explanation. We calculated the timescales of the light curves decays and studied the correlation indexes between the optical and X-ray emission. Finally, we built a physical model considering X-ray heating of the surface of the donor star, irradiation of the accretion disk, and emission from a viscously heated accretion disk, in order to reproduce the observed optical/UV SEDs along the outburst. We considered in our model that the Be circumstellar disk was co-planar to the orbit, and then we neglected its irradiation in the current model. As an input of the model, we used as incident X-ray luminosities those calculated from the bolometric X-ray fluxes obtained from the spectral fit of the Swift/XRT and BAT observations. We conclude that reprocessing of X-rays as X-ray heating of the Be star surface and irradiation of the accretion disk are the two main mechanisms that can reproduce the observed optical/UV emission during the 2017-2018 giant outburst of Swift J0243.6+6124., Comment: Accepted for publication in A&A on 7 December 2023; 16 pages, 12 figures, 2 tables
Published: 2023
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5. The High Energy X-ray Probe (HEX-P): A New Window into Neutron Star Accretion

Author: Ludlam, R. M., Malacaria, C., Sokolova-Lapa, E., Fuerst, F., Pradhan, P., Shaw, A. W., Pottschmidt, K., Pike, S., Vasilopoulos, G., Wilms, J., García, J. A., Madsen, K., Stern, D., Maitra, C., Del Santo, M., Walton, D. J., Brumback, M. C., and Eijnden, J. van den
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Accreting neutron stars (NSs) represent a unique laboratory for probing the physics of accretion in the presence of strong magnetic fields ($B\gtrsim 10^8$ G). Additionally, the matter inside the NS itself exists in an ultra-dense, cold state that cannot be reproduced in Earth-based laboratories. Hence, observational studies of these objects are a way to probe the most extreme physical regimes. Here we present an overview of the field and discuss the most important outstanding problems related to NS accretion. We show how these open questions regarding accreting NSs in both low-mass and high-mass X-ray binary systems can be addressed with the High-Energy X-ray Probe (HEX-P) via simulated data. In particular, with the broad X-ray passband and improved sensitivity afforded by a low X-ray background, HEX-P will be able to 1) distinguish between competing continuum emission models; 2) provide tighter upper limits on NS radii via reflection modeling techniques that are independent and complementary to other existing methods; 3) constrain magnetic field geometry, plasma parameters, and accretion column emission patterns by characterizing fundamental and harmonic cyclotron lines and exploring their behavior with pulse phase; 4) directly measure the surface magnetic field strength of highly magnetized NSs at the lowest accretion luminosities; as well as 5) detect cyclotron line features in extragalactic sources and probe their dependence on luminosity in the super-Eddington regime in order to distinguish between geometrical evolution and accretion-induced decay of the magnetic field. In these ways HEX-P will provide an essential new tool for exploring the physics of NSs, their magnetic fields, and the physics of extreme accretion., Comment: 37 pages, 13 figures, 4 tables, To be published in a special topical issue by Frontiers in Astronomy and Space Sciences on probe-class mission concept HEX-P
Published: 2023

6. Modeling and Simulating X-ray Spectra

Author: Ducci, L. and Malacaria, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: X-ray spectroscopy is a powerful technique for the analysis of the energy distribution of X-rays from astrophysical sources. It allows for the study of the properties, composition, and physical processes taking place at the site of emission. X-ray spectral analysis methods are diverse, as they often need to be tailored to the specific type of instrument used to collect the data. In addition, these methods advance together with the improvement of the technology of the telescopes and detectors. Here, we present a compact overview of the common procedures currently employed in this field. We describe the fundamental data structure and the essential auxiliary information required for conducting spectral analysis and we explore some of the most relevant aspects related to statistical and computational challenges in X-ray spectroscopy. Furthermore, we outline some practical scenarios in the context of data reduction, modeling and fitting of spectra, and spectral simulations., Comment: Invited chapter for the "Handbook of X-ray and Gamma-ray Astrophysics" (Eds. C. Bambi and A. Santangelo, Springer); typos corrected
Published: 2023

7. A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-Wave Candidates from the Third Gravitational-wave Observing Run

Author: Fletcher, C., Wood, J., Hamburg, R., Veres, P., Hui, C. M., Bissaldi, E., Briggs, M. S., Burns, E., Cleveland, W. H., Giles, M. M., Goldstein, A., Hristov, B. A., Kocevski, D., Lesage, S., Mailyan, B., Malacaria, C., Poolakkil, S., von Kienlin, A., Wilson-Hodge, C. A., Team, The Fermi Gamma-ray Burst Monitor, Crnogorčević, M., DeLaunay, J., Tohuvavohu, A., Caputo, R., Cenko, S. B., Laha, S., Parsotan, T., Abbott, R., Abe, H., Acernese, F., Ackley, K., Adhikari, N., Adhikari, R. X., Adkins, V. K., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Albanesi, S., Alfaidi, R. A., Allocca, A., Altin, P. A., Amato, A., Anand, C., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Andrade, T., Andres, N., Andrés-Carcasona, M., Andríc, T., Angelova, S. V., Ansoldi, S., Antelis, J. M., Antier, S., Apostolatos, T., Appavuravther, E. Z., Appert, S., Apple, S. K., Arai, K., Araya, A., Araya, M. C., Areeda, J. S., Arène, M., Aritomi, N., Arnaud, N., Arogeti, M., Aronson, S. M., Arun, K. G., Asada, H., Asali, Y., Ashton, G., Aso, Y., Assiduo, M., Melo, S. Assis de Souza, Aston, S. M., Astone, P., Aubin, F., AultONeal, K., Austin, C., Babak, S., Badaracco, F., Bader, M. K. M., Badger, C., Bae, S., Bae, Y., Baer, A. M., Bagnasco, S., Bai, Y., Baird, J., Bajpai, R., Baka, T., Ball, M., Ballardin, G., Ballmer, S. W., Balsamo, A., Baltus, G., Banagiri, S., Banerjee, B., Bankar, D., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Basak, S., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becher, B. R., Becsy, B., Bedakihale, V. M., Beirnaert, F., Bejger, M., Belahcene, I., Benedetto, V., Beniwal, D., Benjamin, M. G., Bennett, T. F., Bentley, J. D., BenYaala, M., Bera, S., Berbel, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Beveridge, D., Bhandare, R., Bhandari, A. V., Bhardwaj, U., Bhatt, R., Bhattacharjee, D., Bhaumik, S., Bianchi, A., Bilenko, I. A., Billingsley, G., Bini, S., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boër, M., Bogaert, G., Boldrini, M., Bolingbroke, G. N., Bonavena, L. D., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Bucci, F., Bulik, T., Bulten, H. J., Buonanno, A., Burtnyk, K., Buscicchio, R., Buskulic, D., Buy, C., Byer, R. L., Davies, G. S. Cabourn, Cabras, G., Cabrita, R., Cadonati, L., Caesar, M., Cagnoli, G., Cahillane, C., Bustillo, J. Calderòn, Callaghan, J. D., Callister, T. A., Calloni, E., Cameron, J., Camp, J. B., Canepa, M., Canevarolo, S., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, Z., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlassara, M., Carlin, J. B., Carney, M. F., Carpinelli, M., Carrillo, G., Carullo, G., Carver, T. L., Díaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, W., Subrahmanya, S. Chalathadka, Champion, E., Chan, C. H., Chan, C., Chan, C. L., Chan, K., Chan, M., Chandra, K., Chang, I. P., Chanial, P., Chao, S., Chapman-Bird, C., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, C., Chatterjee, Debarati, Chatterjee, Deep, Chaturvedi, M., Chaty, S., Chen, C., Chen, D., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y. B., Chen, Y. R., Chen, Z., Cheng, H., Cheong, C. K., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C. Y., Chiarini, G., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, Q., Chu, Y. K., Chua, S. S. Y., Chung, K. W., Ciani, G., Ciecielag, P., Cieślar, M., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Clara, F., Clark, J. A., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Codazzo, E., Cohadon, P. F., Cohen, D. E., Colleoni, M., Collette, C. G., Colombo, A., Colpi, M., Compton, C. M., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corezzi, S., Corley, K. R., Cornish, N. J., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Cottingham, R., Coughlin, M. W., Coulon, J. P., Countryman, S. T., Cousins, B., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cunningham, L., Cuoco, E., lo, M. Cury, Dabadie, P., Canton, T. Dal, Dall'Osso, S., Dálya, G., Dana, A., D'Angelo, B., Danilishin, S., D'Antonio, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Datta, Sayak, Datta, Sayantani, Dattilo, V., Dave, I., Davier, M., Davis, D., Davis, M. C., Daw, E. J., Dean, R., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Favero, V., De Lillo, F., De Lillo, N., Dell'Aquila, D., Del Pozzo, W., DeMarchi, L. M., De Matteis, F., D'Emilio, V., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., DeSalvo, R., De Simone, R., Dhurandhar, S., D'iaz, M. C., Didio, N. A., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Michele, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Donahue, L., D'Onofrio, L., Donovan, F., Dooley, K. L., Doravari, S., Drago, M., Driggers, J. C., Drori, Y., Ducoin, J. G., Dupej, P., Dupletsa, U., Durante, O., D'Urso, D., Duverne, P. A., Dwyer, S. E., Eassa, C., Easter, P. J., Ebersold, M., Eckhardt, T., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eguchi, S., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Engelby, E., Enomoto, Y., Errico, L., Essick, R. C., Estellés, H., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Evstafyeva, T., Ewing, B. E., Fabrizi, F., Faedi, F., Fafone, V., Fair, H., Fairhurst, S., Fan, P. C., Farah, A. M., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favaro, G., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Fenyvesi, E., Ferguson, D. L., Fernandez-Galiana, A., Ferrante, I., Ferreira, T. A., Fidecaro, F., Figura, P., Fiori, A., Fiori, I., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fiumara, V., Flaminio, R., Floden, E., Fong, H. K., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Freed, J. P., Frei, Z., Freise, A., Freitas, O., Frey, R., Fritschel, P., Frolov, V. V., Fronzé, G. G., Fujii, Y., Fujikawa, Y., Fujimoto, Y., Fulda, P., Fyffe, M., Gabbard, H. A., Gabella, W. E., Gadre, B. U., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gao, D., Gaonkar, S. G., Garaventa, B., Núñez, C. García, García-Quirós, C., Garufi, F., Gateley, B., Gayathri, V., Ge, G. G., Gemme, G., Gennai, A., George, J., Gerberding, O., Gergely, L., Gewecke, P., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Ghosh, Tathagata, Giacomazzo, B., Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giesler, M., Giri, P., Gissi, F., Gkaitatzis, S., Glanzer, J., Gleckl, A. E., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Golomb, J., Goncharov, B., Gonzalez, G., Gosselin, M., Gouaty, R., Gould, D. W., Goyal, S., Grace, B., Grado, A., Graham, V., Granata, M., Granata, V., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W. L., Griggs, H. L., Grignani, G., Grimaldi, A., Grimes, E., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Gruson, A. S., Guerra, D., Guidi, G. M., Guimaraes, A. R., Guixe, G., Gulati, H. K., Gunny, A. M., Guo, H. K., Guo, Y., Gupta, Anchal, Gupta, Anuradha, Gupta, I. M., Gupta, P., Gupta, S. K., Gustafson, R., Guzman, F., Ha, S., Hadiputrawan, I. P. W., Haegel, L., Haino, S., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Han, W. B., Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O., Hansen, H., Hansen, T. J., Hanson, J., Harder, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Hasegawa, K., Haskell, B., Haster, C. J., Hathaway, J. S., Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heidt, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Hennig, M. H., Henshaw, C., Hernandez, A. G., Vivanco, F. Hernandez, Heurs, M., Hewitt, A. L., Higginbotham, S., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hirata, N., Hirose, C., Ho, T. C., Hochheim, S., Hofman, D., Hohmann, J. N., Holcomb, D. G., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma-rays from binary black hole mergers.
Published: 2023

8. Thermonuclear Type-I X-ray Bursts and Burst Oscillations from the Eclipsing AMXP Swift J1749.4-2807

Author: Albayati, A. C., Bult, P., Altamirano, D., Chenevez, J., Guillot, S., Güver, T., Jaisawal, G. K., Malacaria, C., Mancuso, G. C., Marino, A., Ng, M., Sanna, A., and Strohmayer, T. E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Swift J1749.4-2807 is the only known eclipsing accreting millisecond X-ray pulsar. In this paper, we report on 7 thermonuclear (Type-I) X-ray bursts observed by NICER during its 2021 outburst. The first 6 bursts show slow rises and long decays, indicative of mixed H/He fuel, whereas the last burst shows fast rise and decay, suggesting He-rich fuel. Time-resolved spectroscopy of the bursts revealed typical phenomenology (i.e., an increase in black body temperature during the burst rise, and steady decrease in the decay), however they required a variable $N_\mathrm{H}$. We found that the values of $N_\mathrm{H}$ during the bursts were roughly double those found in the fits of the persistent emission prior to each burst. We interpret this change in absorption as evidence of burst-disc interaction, which we observe due to the high inclination of the system. We searched for burst oscillations during each burst and detected a signal in the first burst at the known spin frequency of the neutron star (517.92 Hz). This is the first time burst oscillations have been detected from Swift J1749.4-2807. We further find that each X-ray burst occurs on top of an elevated persistent count rate. We performed time-resolved spectroscopy on the combined data of the bursts with sufficient statistics (i.e., the clearest examples of this phenomenon) and found that the black body parameters evolve to hotter temperatures closer to the onset of the bursts. We interpret this as a consequence of an unusual marginally stable burning process similar to that seen through mHz QPOs., Comment: accepted for publication in MNRAS, 12 pages, 11 figures
Published: 2023
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9. X-ray polarimetry and spectroscopy of the neutron star low-mass X-ray binary GX 9+9: an in-depth study with IXPE and NuSTAR

Author: Ursini, F., Farinelli, R., Gnarini, A., Poutanen, J., Bianchi, S., Capitanio, F., Di Marco, A., Fabiani, S., La Monaca, F., Malacaria, C., Matt, G., Mikušincová, R., Cocchi, M., Kaaret, P., Kajava, J. J. E., Pilia, M., Zhang, W., Agudo, I., Antonelli, L. A., Bachetti, M., Baldini, L., Baumgartner, W. H., Bellazzini, R., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Castellano, S., Cavazzuti, E., Chen, C. -T., Ciprini, S., Costa, E., De Rosa, A., Del Monte, E., Di Gesu, L., Di Lalla, N., Donnarumma, I., Doroshenko, V., Dovčiak, M., Ehlert, S. R., Enoto, T., Evangelista, Y., Ferrazzoli, R., Garcia, J. A., Gunji, S., Hayashida, K., Heyl, J., Iwakiri, W., Jorstad, S. G., Karas, V., Kislat, F., Kitaguchi, T., Kolodziejczak, J. J., Krawczynski, H., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marin, F., Marinucci, A., Marscher, A. P., Marshall, H. L., Massaro, F., Mitsuishi, I., Mizuno, T., Muleri, F., Negro, M., Ng, C. -Y., O'Dell, S. L., Omodei, N., Oppedisano, C., Papitto, A., Pavlov, G. G., Peirson, A. L., Perri, M., Pesce-Rollins, M., Petrucci, P. -O., Possenti, A., Puccetti, S., Ramsey, B. D., Rankin, J., Ratheesh, A., Roberts, O. J., Romani, R. W., Sgrò, C., Slane, P., Soffitta, P., Spandre, G., Swartz, D. A., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Tombesi, F., Trois, A., Tsygankov, S. S., Turolla, R., Vink, J., Weisskopf, M. C., Wu, K., Xie, F., and Zane, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report on a comprehensive analysis of simultaneous X-ray polarimetric and spectral data of the bright atoll source GX 9+9 with the Imaging X-ray Polarimetry Explorer (IXPE) and NuSTAR. The source is significantly polarized in the 4--8 keV band, with a degree of $2.2\% \pm 0.5\%$ (uncertainty at the 68% confidence level). The NuSTAR broad-band spectrum clearly shows an iron line, and is well described by a model including thermal disk emission, a Comptonized component, and reflection. From a spectro-polarimetric fit, we obtain an upper limit to the polarization degree of the disk of 4% (at 99% confidence level), while the contribution of Comptonized and reflected radiation cannot be conclusively separated. However, the polarization is consistent with resulting from a combination of Comptonization in a boundary or spreading layer, plus reflection off the disc, which gives a significant contribution in any realistic scenario., Comment: 10 pages, accepted for publication in A&A
Published: 2023
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10. Detection of millihertz quasi-periodic oscillations in the low-mass X-ray binary 4U 1730--22 with NICER

Author: Mancuso, G. C., Altamirano, D., Bult, P., Chenevez, J., Guillot, S., Guver, T., Jaisawal, G. K., Malacaria, C., Ng, M., Sanna, A., and Strohmayer, T. E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of millihertz quasi-periodic oscillations (mHz QPOs) from the neutron star (NS) low-mass X-ray binary 4U 1730--22 using the Neutron Star Interior Composition Explorer (NICER). After being inactive for almost 50 years, 4U 1730--22 went into outburst twice between June and August 2021, and between February and July 2022. We analyse all the NICER observations of this source, and detect mHz QPOs with a significance > $4\sigma$ in 35 observations. The QPO frequency of the full data set ranged between ~4.5 and ~8.1 mHz with an average fractional rms amplitude of the order of ~2%. The X-ray colour analysis strongly suggests that 4U 1730--22 was in a soft spectral state during the QPO detections. Our findings are consistent with those reported for other sources where the mHz QPOs have been interpreted as the result of a special mode of He burning on the NS surface called marginally stable nuclear burning (MSNB). We conclude that the mHz QPOs reported in this work are also associated with the MSNB, making 4U 1730--22 the eighth source that shows this phenomenology. We discuss our findings in the context of the heat flux from the NS crust., Comment: 9 pages, 6 figures. Accepted for publication in MNRAS
Published: 2023
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11. X-ray flashes from the low-mass X-ray binary IGR J17407-2808

Author: Ducci, L., Malacaria, C., Romano, P., Bozzo, E., Berton, M., Santangelo, A., and Congiu, E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: IGR J17407-2808 is an enigmatic and poorly studied X-ray binary that was recently observed quasi-simultaneously with NuSTAR and XMM-Newton. In this paper we report the results of this observational campaign. During the first 60 ks of observation, the source was caught in a relatively low emission state, characterised by a modest variability and an average flux of ~8.3E-13 erg/cm^2/s (4-60 keV). Afterwards, IGR J17407-2808 entered a significantly more active emission state that persisted for the remaining ~40 ks of the NuSTAR observation. During this state, IGR J17407-2808 displayed several fast X-ray flares, featuring durations of ~1-100 s and profiles with either single or multiple peaks. The source flux in the flaring state reached values as high as 2E-9 erg/cm^2/s (4-60 keV), leading to a measured dynamic range during the NuSTAR and XMM-Newton campaign of >~ 10^3. We also analysed available archival photometric near-infrared data of IGR J17407-2808 to improve the constraints available so far on the the nature of the donor star hosted in this system. Our analysis shows that the donor star can be either a rare K or M-type sub-subgiant or an K type main sequence star, or sub-giant star. Our findings support the classification of IGR J17407-2808 as a low-mass X-ray binary. We discuss the source X-ray behaviour as recorded by NuSTAR and XMM-Newton in view of this revised classification., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2023
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12. X-ray polarimetry of X-ray pulsar X Persei: another orthogonal rotator?

Author: Mushtukov, A. A., Tsygankov, S. S., Poutanen, J., Doroshenko, V., Salganik, A., Costa, E., Di Marco, A., Heyl, J., La Monaca, F., Lutovinov, A. A., Mereminsky, I. A., Papitto, A., Semena, A. N., Shtykovsky, A. E., Suleimanov, V. F., Forsblom, S. V., González-Caniulef, D., Malacaria, C., Sunyaev, R. A., Agudo, I., Antonelli, L. A., Bachetti, M., Baldini, L., Baumgartner, W. H., Bellazzini, R., Bianchi, S., Bongiorno, S. D., Bonino, R., Brez, A., Bucciantini, N., Capitanio, F., Castellano, S., Cavazzuti, E., Chen, C. -T., Ciprini, S., De Rosa, A., Del Monte, E., Di Gesu, L., Di Lalla, N., Donnarumma, I., Dovčiak, M., Ehlert, S. R., Enoto, T., Evangelista, Y., Fabiani, S., Ferrazzoli, R., Garcia, J. A., Gunji, S., Hayashida, K., Iwakiri, W., Jorstad, S. G., Kaaret, P., Karas, V., Kislat, F., Kitaguchi, T., Kolodziejczak, J. J., Krawczynski, H., Latronico, L., Liodakis, I., Maldera, S., Manfreda, A., Marin, F., Marscher, A. P., Marshall, H. L., Massaro, F., Matt, G., Mitsuishi, I., Mizuno, T., Muleri, F., Negro, M., Ng, C. -Y., O'Dell, S. L., Omodei, N., Oppedisano, C., Pavlov, G. G., Peirson, A. L., Perri, M., Pesce-Rollins, M., Petrucci, P. -O., Pilia, M., Possenti, A., Puccetti, S., Ramsey, B. D., Rankin, J., Ratheesh, A., Roberts, O. J., Romani, R. W., Sgrò, C., Slane, P., Soffitta, P., Spandre, G., Swartz, D. A., Tamagawa, T., Tavecchio, F., Taverna, R., Tawara, Y., Tennant, A. F., Thomas, N. E., Tombesi, F., Trois, A., Turolla, R., Vink, J., Weisskopf, M. C., Wu, K., Xie, F., and Zane, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: X Persei is a persistent low-luminosity X-ray pulsar of period of $\sim$835 s in a Be binary system. The field strength at the neutron star surface is not known precisely, but indirect signs indicate a magnetic field above $10^{13}$ G, which makes the object one of the most magnetized known X-ray pulsars. Here we present the results of observations X Persei performed with the Imaging X-ray Polarimetry Explorer (IXPE). The X-ray polarization signal was found to be strongly dependent on the spin phase of the pulsar. The energy-averaged polarization degree in 3-8 keV band varied from several to $\sim$20 per cent over the pulse with a positive correlation with the pulsed X-ray flux. The polarization angle shows significant variation and makes two complete revolutions during the pulse period resulting in nearly nil pulse-phase averaged polarization. Applying the rotating vector model to the IXPE data we obtain the estimates for the rotation axis inclination and its position angle on the sky as well as for the magnetic obliquity. The derived inclination is close to the orbital inclination reported earlier for X Persei. The polarimetric data imply a large angle between the rotation and magnetic dipole axes, which is similar to the result reported recently for the X-ray pulsar GRO J1008$-$57. After eliminating the effect of polarization angle rotation over the pulsar phase using the best-fitting rotating vector model, the strong dependence of the polarization degree with energy was discovered with its value increasing from 0% at $\sim$2 keV to 30% at 8 keV., Comment: 11 pages, 7 figures, submitted to MNRAS
Published: 2023
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13. Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow

Author: Lesage, S., Veres, P., Briggs, M. S., Goldstein, A., Kocevski, D., Burns, E., Wilson-Hodge, C. A., Bhat, P. N., Huppenkothen, D., Fryer, C. L., Hamburg, R., Racusin, J., Bissaldi, E., Cleveland, W. H., Dalessi, S., Fletcher, C., Giles, M. M., Hristov, B. A., Hui, C. M., Mailyan, B., Malacaria, C., Poolakkil, S., Roberts, O. J., von Kienlin, A., Wood, J., Ajello, M., Arimoto, M., Baldini, L., Ballet, J., Baring, M. G., Bastieri, D., Gonzalez, J. Becerra, Bellazzini, R., Blandford, R. D., Bonino, R., Bruel, P., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chiaro, G., Cibrario, N., Ciprini, S., Orestano, P. Cristarella, Crnogorcevic, M., Cuoco, A., Cutini, S., DAmmando, F., De Gaetano, S., Di Lalla, N., Di Venere, L., Dominguez, A., Fegan, S. J., Ferrara, E. C., Fleischhack, H., Fukazawa, Y., Funk, S., Fusco, P., Galanti, G., Gammaldi, V., Gargano, F., Gasbarra, C., Gasparrini, D., Germani, S., Giacchino, F., Giglietto, N., Gill, R., Giroletti, M., Granot, J., Green, D., Grenier, I. A., Guiriec, S., Gustafsson, M., Hays, E., Hewitt, J. W., Horan, D., Hou, X., Kuss, M., Latronico, L., Laviron, A., Lemoine-Goumard, M., Li, J., Liodakis, I., Longo, F., Loparco, F., Lorusso, L., Lovellette, M. N., Lubrano, P., Maldera, S., Manfreda, A., Marti-Devesa, G., Mazziotta, M. N., McEnery, J. E., Mereu, I., Meyer, M., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Panzarini, G., Persic, M., Pesce-Rollins, M., Pillera, R., Piron, F., Poon, H., Porter, T. A., Principe, G., Raino, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ryde, F., Sanchez-Conde, M., Parkinson, P. M. Saz, Scotton, L., Serini, D., Sgro, C., Sharma, V., Siskind, E. J., Spandre, G., Spinelli, P., Tajima, H., Torres, D. F., Valverde, J., Venters, T., Wadiasingh, Z., Wood, K., and Zaharijas, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of GRB 221009A, the highest flux gamma-ray burst ever observed by the Fermi Gamma-ray Burst Monitor (GBM). This GRB has continuous prompt emission lasting more than 600 seconds which smoothly transitions to afterglow visible in the GBM energy range (8 keV--40 MeV), and total energetics higher than any other burst in the GBM sample. By using a variety of new and existing analysis techniques we probe the spectral and temporal evolution of GRB 221009A. We find no emission prior to the GBM trigger time (t0; 2022 October 9 at 13:16:59.99 UTC), indicating that this is the time of prompt emission onset. The triggering pulse exhibits distinct spectral and temporal properties suggestive of the thermal, photospheric emission of shock-breakout, with significant emission up to $\sim$15 MeV. We characterize the onset of external shock at t0+600 s and find evidence of a plateau region in the early-afterglow phase which transitions to a slope consistent with Swift-XRT afterglow measurements. We place the total energetics of GRB 221009A in context with the rest of the GBM sample and find that this GRB has the highest total isotropic-equivalent energy ($\textrm{E}_{\gamma,\textrm{iso}}=1.0\times10^{55}$ erg) and second highest isotropic-equivalent luminosity ($\textrm{L}_{\gamma,\textrm{iso}}=9.9\times10^{53}$ erg/s) based on redshift of z = 0.151. These extreme energetics are what allowed us to observe the continuously emitting central engine of GBM from the beginning of the prompt emission phase through the onset of early afterglow., Comment: 26 pages 7 figures - accepted for publication in ApJL
Published: 2023
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14. On the cyclotron absorption line and evidence of the spectral transition in SMC X-2 during 2022 giant outburst

Author: Jaisawal, G. K., Vasilopoulos, G., Naik, S., Maitra, C., Malacaria, C., Chhotaray, B., Gendreau, K. C., Guillot, S., Ng, M., and Sanna, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report comprehensive spectral and temporal properties of the Be/X-ray binary pulsar SMC X-2 using X-ray observations during the 2015 and 2022 outbursts. The pulse profile of the pulsar is unique and strongly luminosity dependent. It evolves from a broad-humped into a double-peaked profile above luminosity 3$\times$10$^{38}$ ergs s$^{-1}$. The pulse fraction of the pulsar is found to be a linear function of luminosity as well as energy. We also studied the spectral evolution of the source during the latest 2022 outburst with NICER. The observed photon index shows a negative and positive correlation below and above the critical luminosity, respectively, suggesting evidence of spectral transition from the sub-critical to super-critical regime. The broadband spectroscopy of four sets of NuSTAR and XRT/NICER data from both outbursts can be described using a cutoff power-law model with a blackbody component. In addition to the 6.4 keV iron fluorescence line, an absorption-like feature is clearly detected in the spectra. The cyclotron line energy observed during the 2015 outburst is below 29.5 keV, however latest estimates in the 2022 outburst suggest a value of 31.5 keV. Moreover, an increase of 3.4 keV is detected in the cyclotron line energy at equal levels of luminosity observed in 2022 with respect to 2015. The observed cyclotron line energy variation is explored in terms of accretion induced screening mechanism or geometrical variation in line forming region., Comment: 11 Pages, 11 figures, Accepted for Publication in MNRAS
Published: 2023
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15. A Bayesian approach for torque modelling of BeXRB pulsars with application to super-Eddington accretors

Author: Karaferias, A. S., Vasilopoulos, G., Petropoulou, M., Jenke, P. A., Wilson-Hodge, C. A., and Malacaria, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In this study we present a method to estimate posterior distributions for standard accretion torque model parameters and binary orbital parameters for X-ray binaries using a nested sampling algorithm for Bayesian Parameter Estimation. We study the spin evolution of two Be X-ray binary systems in the Magellanic Clouds, RX J0520.5-6932 and RX J0209-7427, during major outbursts, in which they surpassed the Eddington-limit. Moreover, we apply our method to the recently discovered Swift J0243.6+6124; the only known Galactic pulsating ultra-luminous X-ray source. This is an excellent candidate for studying the disc evolution at super-Eddington accretion rates, for its luminosity span several orders of magnitude during its outburst, with a maximum $L_{\rm X}$ that exceeded the Eddington limit by a factor of $\sim 10$. Our method, when applied to RX J0520.5-6932 and RX J0209-7427, is able to identify the more favourable torque model for each system, while yielding meaningful ranges for the NS and orbital parameters. Our analysis for Swift J0243.6+6124 illustrates that, contrary to the standard torque model predictions, the magnetospheric radius and the Alfv\'en radius are not proportional to each other when surpassing the Eddington limit. Reported distance estimates of this source range between 5 and 7 kpc. Smaller distances require non-typical neutron star properties (i.e. mass and radius) and possibly lower radiative efficiency of the accretion column., Comment: 20 pages, 14 figures, Accepted for publication in MNRAS
Published: 2022
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16. The unaltered pulsar: GRO J1750-27, a super-critical X-ray neutron star that does not blink an eye

Author: Malacaria, C., Ducci, L., Falanga, M., Altamirano, D., Bozzo, E., Guillot, S., Jaisawal, G. K., Kretschmar, P., Ng, M., Pradhan, P., Rothschild, R., Sanna, A., Thalhammer, P., and Wilms, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: When accreting X-ray pulsars (XRPs) undergo bright X-ray outbursts, their luminosity-dependent spectral and timing features can be analysed in detail. The XRP GRO J1750-27 recently underwent one of such episodes, during which it was observed with $NuSTAR$ and monitored with $NICER$. Such a data set is rarely available, as it samples the outburst over more than a month at a luminosity that is always exceeding ${\sim}5\times10^{37}\,$erg/s. This value is larger than the typical critical luminosity value, where a radiative shock is formed above the neutron star's surface. Our data analysis of the joint spectra returns a highly ($N_H\sim(5-8)\times10^{22}\,$cm$^{-2}$) absorbed spectrum showing a K$\alpha$ iron line, a soft blackbody component likely originating from the inner edge of the accretion disk, and confirms the discovery of one of the deepest cyclotron lines, at a centroid energy of ${\sim}44\,$keV corresponding to a magnetic field strength of $4.7\times10^{12}\,$G. This value is independently supported by the best-fit physical model for spectral formation in accreting XRPs which, in agreement with recent findings, favours a distance of $14$ kpc and also reflects a bulk-Comptonization dominated accretion flow. Contrary to theoretical expectations and observational evidence from other similar sources, the pulse profiles as observed by $NICER$ through the outburst raise, peak and decay remain remarkably steady. The $NICER$ spectrum, including the iron K$\alpha$ line best-fit parameters, also remain almost unchanged at all probed outburst stages, similar to the pulsed fraction behaviour. We argue that all these phenomena are linked and interpret them as resulting from a saturation effect of the accretion column's emission, which occurs in the high-luminosity regime., Comment: Accepted on A&A -- proof version
Published: 2022
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17. Broadband study and the discovery of pulsations from the Be/X-ray binary eRASSU J052914.9-662446 in the Large Magellanic Cloud

Author: Maitra, C., Kaltenbrunner, D., Haberl, F., Buckley, D. A. H., Monageng, I. M., Udalski, A., Carpano, S., Coley, J. B., Doroshenko, V., Ducci, L., Malacaria, C., König, O., Santangelo, A., Vasilopoulos, G., and Wilms, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Context. The Magellanic Clouds are our nearest star-forming galaxies. While the population of high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) is relatively well studied, our knowledge about the Large Magellanic Cloud (LMC) is far from complete given its large angular extent and insufficient coverage with X-ray observations. Aims. We conducted a search for new HMXBs in the LMC using data from eROSITA, the soft X-ray instrument on board the Spektrum-Roentgen-Gamma (SRG) satellite. Methods. After confirming the nature of eRASSU J052914.9-662446 as a hard X-ray source positionally coincident with an early type star, we followed it up with optical spectroscopic observations from South African Large Telescope (SALT) and a dedicated NuSTAR observation. Results. We study the broadband timing and spectral behaviour of the newly discovered HMXB eRASSU J052914.9-662446 through eROSITA, Swift and NuSTAR data in X-rays and the Optical Gravitational Lensing Experiment (OGLE) and SALT RSS data at optical wavelength. We report on detection of the spin period at 1412 s and suggest an orbital period of the system of ~151 days, and thereby establish eRASSU J052914.9-662446 as an accreting pulsar. Further, through optical spectroscopic observations and the existence of H alpha emission the source is identified as a Be X-ray binary pulsar in the LMC. We also investigate the variability of the source in the optical and X-ray regime over the last decades and provide estimates on the possible magnetic field strength of the neutron star., Comment: 11 pages, 13 figures, 3 tables, accepted for publication in A&A
Published: 2022
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18. On the peculiar long-term orbital evolution of the eclipsing accreting millisecond X-ray pulsar SWIFT J1749.4-2807

Author: Sanna, A., Burderi, L., Di Salvo, T., Riggio, A., Altamirano, D., Marino, A., Bult, P., Strohmayer, T. E., Guillot, S., Malacaria, C., Ng, M., Mancuso, G., Mazzola, S. M., Albayati, A. C., Iaria, R., Manca, A., Cabras, C., and Anitra, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the pulsar timing analysis of the accreting millisecond X-ray pulsar SWIFT J1749.4-2807 monitored by NICER and XMM-Newton during its latest outburst after almost eleven years of quiescence. From the coherent timing analysis of the pulse profiles, we updated the orbital ephemerides of the system. Large phase jumps of the fundamental frequency phase of the signal are visible during the outburst, consistent with what was observed during the previous outburst. Moreover, we report on the marginally significant evidence for non-zero eccentricity ($e\simeq 4\times 10^{-5}$) obtained independently from the analysis of both the 2021 and 2010 outbursts and we discuss possible compatible scenarios. Long-term orbital evolution of SWIFT J1749.4-2807 suggests a fast expansion of both the NS projected semi-major axis $(x)$, and the orbital period $(P_{\rm orb})$, at a rate of $\dot{x}\simeq 2.6\times 10^{-13}\,\text{lt-s}\,\text{s}^{-1}$ and $\dot{P}_{\rm orb}\simeq 4 \times 10^{-10}\,\text{s}\,\text{s}^{-1}$, respectively. SWIFT J1749.4-2807 is the only accreting millisecond X-ray pulsar, so far, from which the orbital period derivative has been directly measured from appreciable changes on the observed orbital period. Finally, no significant secular deceleration of the spin frequency of the compact object is detected, which allowed us to set a constraint on the magnetic field strength at the polar caps of $B_{PC}<1.3\times 10^{8}~\text{G}$, in line with typical values reported for AMXPs., Comment: 13 pages, 3 figures, 1 table. Accepted for publication in MNRAS
Published: 2022
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19. Pulse Peak Migration during the Outburst Decay of the Magnetar SGR 1830-0645: Crustal Motion and Magnetospheric Untwisting

Author: Younes, G., Lander, S. K., Baring, M. G., Enoto, T., Kouveliotou, C., Wadiasingh, Z., Ho, W., Harding, A. K., Arzoumanian, Z., Gendreau, K. C., Guver, T., Hu, C. -P., Malacaria, C., Ray, P. S., and Strohmayer, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Magnetars, isolated neutron stars with magnetic field strengths typically $\gtrsim10^{14}$~G, exhibit distinctive months-long outburst epochs during which strong evolution of soft X-ray pulse profiles, along with nonthermal magnetospheric emission components, is often observed. Using near-daily NICER observations of the magnetar SGR 1830-0645 during the first 37 days of a recent outburst decay, a pulse peak migration in phase is clearly observed, transforming the pulse shape from an initially triple-peaked to a single-peaked profile. Such peak merging has not been seen before for a magnetar. Our high-resolution phase-resolved spectroscopic analysis reveals no significant evolution of temperature despite the complex initial pulse shape. Yet the inferred surface hot spots shrink during the peak migration and outburst decay. We suggest two possible origins for this evolution. For internal heating of the surface, tectonic motion of the crust may be its underlying cause. The inferred speed of this crustal motion is $\lesssim100$~m~day$^{-1}$, constraining the density of the driving region to $\rho\sim10^{10}$~g~cm$^{-3}$, at a depth of $\sim200$~m. Alternatively, the hot spots could be heated by particle bombardment from a twisted magnetosphere possessing flux tubes or ropes, somewhat resembling solar coronal loops, that untwist and dissipate on the 30-40~day timescale. The peak migration may then be due to a combination of field-line footpoint motion (necessarily driven by crustal motion) and evolving surface radiation beaming. These novel dataset paints a vivid picture of the dynamics associated with magnetar outbursts, yet it also highlights the need for a more generic theoretical picture where magnetosphere and crust are considered in tandem., Comment: ApJL accepted
Published: 2022
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20. Continuum, cyclotron line, and absorption variability in the high-mass X-ray binary Vela X-1

Author: Diez, C. M., Grinberg, V., Fürst, F., Sokolova-Lapa, E., Santangelo, A., Wilms, J., Pottschmidt, K., Martínez-Núñez, S., Malacaria, C., and Kretschmar, P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Because of its complex clumpy wind, prominent cyclotron resonant scattering features, intrinsic variability and convenient physical parameters (close distance, high inclination, small orbital separation) which facilitate the observation and analysis of the system, Vela X-1 is one of the key systems to understand accretion processes in high-mass X-ray binaries on all scales. We revisit Vela X-1 with two new observations taken with NuSTAR at orbital phases ~0.68-0.78 and ~0.36-0.52 which show a plethora of variability and allow us to study the accretion geometry and stellar wind properties of the system. We follow the evolution of spectral parameters down to the pulse period time-scale using a partially covered powerlaw continuum with a Fermi-Dirac cut-off to model the continuum and local absorption. We could confirm anti-correlations between the photon index and the luminosity and, for low fluxes, between the folding energy and the luminosity, implying a change of properties in the Comptonising plasma. We could not confirm a previously seen correlation between the cyclotron line energy and the luminosity of the source in the overall observation, but we observed a drop in the cyclotron line energy following a strong flare. We see strong variability in absorption between the two observations and within one observation (for the ~0.36-0.52 orbital phases) that can be explained by the presence of a large-scale structure, such as accretion- and photoionisation wakes in the system and our variable line of sight through this structure., Comment: 18 pages, 13 figures, A&A accepted
Published: 2022
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21. X-ray emission from magnetized neutron star atmospheres at low mass accretion rates. I. Phase-averaged spectrum

Author: Sokolova-Lapa, E., Gornostaev, M., Wilms, J., Ballhausen, R., Falkner, S., Postnov, K., Thalhammer, P., Fürst, F., García, J. A., Shakura, N., Becker, P. A., Wolff, M. T., Pottschmidt, K., Härer, L., and Malacaria, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Recent observations of X-ray pulsars at low luminosities allow, for the first time, to compare theoretical models for the emission from highly magnetized neutron star atmospheres at low mass accretion rates ($\dot{M} \lesssim 10^{15}$ g s$^{-1}$) with the broadband X-ray data. The purpose of this paper is to investigate the spectral formation in the neutron star atmosphere at low $\dot{M}$ and to conduct a parameter study of physical properties of the emitting region. We obtain the structure of the static atmosphere, assuming that Coulomb collisions are the dominant deceleration process. The upper part of the atmosphere is strongly heated by the braking plasma, reaching temperatures of 30-40 keV, while its denser isothermal interior is much cooler (~2 keV). We numerically solve the polarized radiative transfer in the atmosphere with magnetic Compton scattering, free-free processes, and non-thermal cyclotron emission due to possible collisional excitations of electrons. The strongly polarized emitted spectrum has a double-hump shape that is observed in low-luminosity X-ray pulsars. A low-energy "thermal" component is dominated by extraordinary photons that can leave the atmosphere from deeper layers due to their long mean free path at soft energies. We find that a high-energy component is formed due to resonant Comptonization in the heated non-isothermal part of the atmosphere even in the absence of collisional excitations. The latter, however, affect the ratio of the two components. A strong cyclotron line originates from the optically thin, uppermost zone. A fit of the model to NuSTAR and Swift/XRT observations of GX 304-1 provides an accurate description of the data with reasonable parameters. The model can thus reproduce the characteristic double-hump spectrum observed in low-luminosity X-ray pulsars and provides insights into spectral formation., Comment: 18 pages, 10 figures, A&A accepted
Published: 2021
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22. The Fermi GBM Gamma-Ray Burst Spectral Catalog: 10 Years of Data

Author: Poolakkil, S., Preece, R., Fletcher, C., Goldstein, A., Bhat, P. N., Bissaldi, E., Briggs, M. S., Burns, E., Cleveland, W. H., Giles, M. M., Hui, C. M., Kocevski, D., Lesage, S., Mailyan, B., Malacaria, C., Paciesas, W. S., Roberts, O. J., Veres, P., von Kienlin, A., and Wilson-Hodge, C. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the systematic spectral analyses of gamma-ray bursts (GRBs) detected by the Fermi Gamma-Ray Burst Monitor (GBM) during its first ten years of operation. This catalog contains two types of spectra; time-integrated spectral fits and spectral fits at the brightest time bin, from 2297 GRBs, resulting in a compendium of over 18000 spectra. The four different spectral models used for fitting the spectra were selected based on their empirical importance to the shape of many GRBs. We describe in detail our procedure and criteria for the analyses, and present the bulk results in the form of parameter distributions both in the observer frame and in the GRB rest frame. 941 GRBs from the first four years have been re-fitted using the same methodology as that of the 1356 GRBs in years five through ten. The data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center (HEASARC).
Published: 2021
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23. Dips and eclipses in the X-ray binary Swift J1858.6-0814 observed with NICER

Author: Buisson, D. J. K., Altamirano, D., Padilla, M. Armas, Arzoumanian, Z., Bult, P., Segura, N. Castro, Charles, P. A., Degenaar, N., Trigo, M. Díaz, Eijnden, J. van den, Fogantini, F., Gandhi, P., Gendreau, K., Hare, J., Homan, J., Knigge, C., Malacaria, C., Mendez, M., Darias, T. Muñoz, Ng, M., Arabacı, M. Özbey, Remillard, R., Strohmayer, T. E., Tombesi, F., Tomsick, J. A., Vincentelli, F., and Walton, D. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the discovery of eclipses in the X-ray light curves of the X-ray binary Swift J1858.6-0814. From these, we find an orbital period of $P=76841.3_{-1.4}^{+1.3}$ s ($\approx21.3$ hours) and an eclipse duration of $t_{\rm ec}=4098_{-18}^{+17}$ s ($\approx1.14$ hours). We also find several absorption dips during the pre-eclipse phase. From the eclipse duration to orbital period ratio, the inclination of the binary orbit is constrained to $i>70^\circ$. The most likely range for the companion mass suggests that the inclination is likely to be closer to this value than $90^\circ$. The eclipses are also consistent with earlier data, in which strong variability ('flares') and the long orbital period prevent clear detection of the period or eclipses. We also find that the bright flares occurred preferentially in the post-eclipse phase of the orbit, likely due to increased thickness at the disc-accretion stream interface preventing flares being visible during the pre-eclipse phase. This supports the notion that variable obscuration is responsible for the unusually strong variability in Swift J1858.6-0814., Comment: 12 pages, 11 figures, MNRAS accepted
Published: 2021
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24. The X-ray pulsar XTE J1858+034 observed with NuSTAR and Fermi/GBM: spectral and timing characterization plus a cyclotron line

Author: Malacaria, C., Kretschmar, P., Madsen, K. K., Wilson-Hodge, C. A., Coley, Joel B., Jenke, P., Lutovinov, A. A., Pottschmidt, K., Tsygankov, S. S., and Wilms, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Accreting X-ray pulsars (XRPs) undergo luminous X-ray outbursts during which the spectral and timing behavior of the neutron star can be studied in detail. We analyze a $NuSTAR$ observation of the XRP XTE J1858+034 during its outburst in 2019. The spectrum is fit with a phenomenological, a semi-empirical and a physical spectral model. A candidate cyclotron line is found at $48\,$keV, implying a magnetic field of $5.4\times10^{\rm 12}\,$G at the site of emission. This is also supported by the physical best-fit model. We propose an orbital period of about $81$ days based on the visual inspection of the X-ray outbursts recurrence time. Based on $Fermi$ Gamma-ray Burst Monitor data, the standard disk accretion-torque theory allowed us to infer a distance of $10.9\pm1.0\,$kpc. Pulse profiles are single-peaked and show a pulsed fraction that is strongly energy-dependent at least up to $40$ keV., Comment: Accepted for publication in ApJ; 9 pages, 2 tables, 7 figures
Published: 2021
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25. Discovery of Thermonuclear Type-I X-ray Bursts from the X-ray binary MAXI J1807+132

Author: Albayati, A. C., Altamirano, D., Jaisawal, G. K., Bult, P., Rapisarda, S., Mancuso, G. C., Güver, T., Arzoumanian, Z., Chakrabarty, D., Chenevez, J., Court, J. M. C., Gendreau, K. C., Guillot, S., Keek, L., Malacaria, C., and Strohmayer, T. E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: MAXI J1807+132 is a low-mass X-ray binary (LMXB) first detected in outburst in 2017. Observations during the 2017 outburst did not allow for an unambiguous identification of the nature of the compact object. MAXI J1807+132 was detected in outburst again in 2019 and was monitored regularly with NICER. In this paper we report on five days of observations during which we detected three thermonuclear (Type-I) X-ray bursts, identifying the system as a neutron star LMXB. Time-resolved spectroscopy of the three Type-I bursts revealed typical characteristics expected for these phenomena. All three Type-I bursts show slow rises and long decays, indicative of mixed H/He fuel. We find no strong evidence that any of the Type-I bursts reached the Eddington Luminosity; however, under the assumption that the brightest X-ray burst underwent photospheric radius expansion, we estimate a <12.4kpc upper limit for the distance. We searched for burst oscillations during the Type-I bursts from MAXI J1807+132 and found none (<10% amplitude upper limit at 95% confidence level). Finally, we found that the brightest Type-I burst shows a ~1.6sec pause during the rise. This pause is similar to one recently found with NICER in a bright Type-I burst from the accreting millisecond X-ray pulsar SAX J1808.4-3658. The fact that Type-I bursts from both sources can show this type of pause suggests that the origin of the pauses is independent of the composition of the burning fuel, the peak luminosity of the Type-I bursts, or whether the NS is an X-ray pulsar., Comment: 9 pages, 4 figures
Published: 2020
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26. Discovery of thermonuclear (Type I) X-ray bursts in the X-ray binary Swift J1858.6-0814 observed with NICER and NuSTAR

Author: Buisson, D. J. K., Altamirano, D., Bult, P., Mancuso, G. C., Güver, T., Jaisawal, G. K., Hare, J., Albayati, A. C., Arzoumanian, Z., Segura, N. Castro, Chakrabarty, D., Gandhi, P., Guillot, S., Homan, J., Gendreau, K. C., Jiang, J., Malacaria, C., Miller, J. M., Arabacı, M. Özbey, Remillard, R., Strohmayer, T. E., Tombesi, F., Tomsick, J. A., Vincentelli, F. M., and Walton, D. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Swift J1858.6-0814 is a recently discovered X-ray binary notable for extremely strong variability (by factors $>100$ in soft X-rays) in its discovery state. We present the detection of five thermonuclear (Type I) X-ray bursts from Swift J1858.6-0814, implying that the compact object in the system is a neutron star. Some of the bursts show photospheric radius expansion, so their peak flux can be used to estimate the distance to the system. The peak luminosity, and hence distance, can depend on several system parameters; for the most likely values, a high inclination and a helium atmosphere, $D=12.8_{-0.6}^{+0.8}$ kpc, although systematic effects allow a conservative range of $9-18$ kpc. Before one burst, we detect a QPO at $9.6\pm0.5$ mHz with a fractional rms amplitude of $2.2\pm0.2$% ($0.5-10$ keV), likely due to marginally stable burning of helium; similar oscillations may be present before the other bursts but the light curves are not long enough to allow their detection. We also search for burst oscillations but do not detect any, with an upper limit in the best case of 15% fractional amplitude (over $1-8$ keV). Finally, we discuss the implications of the neutron star accretor and this distance on other inferences which have been made about the system. In particular, we find that Swift J1858.6-0814 was observed at super-Eddington luminosities at least during bright flares during the variable stage of its outburst., Comment: 14 pages, 8 figures, 2 tables, MNRAS accepted
Published: 2020
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27. NICER Observation of the Temporal and Spectral Evolution of Swift J1818.0-1607: a Missing Link between Magnetars and Rotation Powered Pulsars

Author: Hu, Chin-Ping, Begicarslan, Beste, Guver, Tolga, Enoto, Teruaki, Younes, George, Sakamoto, Takanori, Ray, Paul S., Strohmayer, Tod E., Guillot, Sebastien, Arzoumanian, Zaven, Palmer, David M., Gendreau, Keith C., Malacaria, C., Wadiasingh, Zorawar, Jaisawal, Gaurava K., and Majid, Walid A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the hard X-ray burst and the first ~100 days NICER monitoring of the soft X-ray temporal and spectral evolution of the newly-discovered magnetar Swift J1818.0-1607. The burst properties are typical of magnetars with a duration of $T_{90}=10\pm4$ ms and a temperature of $kT=8.4\pm0.7$ keV. The 2--8 keV pulse shows a broad, single peak profile with a pulse fraction increasing with time from 30% to 43%. The NICER observations reveal strong timing noise with $\dot{\nu}$ varying erratically by a factor of 10, with an average long-term spin-down rate of $\dot{\nu}=(-2.48\pm0.03)\times10^{-11}$~s$^{-2}$, implying an equatorial surface magnetic field of $2.5\times10^{14}$ G and a young characteristic age of $\sim$470 yr. We detect a large spin-up glitch at MJD 58928.56 followed by a candidate spin-down glitch at MJD 58934.81, with no accompanying flux enhancements. The persistent soft X-ray spectrum of Swift~J1818.0-1607 can be modeled as an absorbed blackbody with a temperature of ~1 keV. Its flux decayed by ~60% while the modeled emitting area decreased by ~30% over the NICER observing campaign. This decrease, coupled with the increase in the pulse fraction points to a shrinking hot spot on the neutron star surface. Assuming a distance of 6.5 kpc, we measure a peak X-ray luminosity of $1.9\times10^{35}$ erg/s, lower than its spin-down luminosity of $7.2\times10^{35}$ erg/s. Its quiescent thermal luminosity is $\lesssim 1.7\times10^{34}$ erg/s, lower than those of canonical young magnetars. We conclude that Swift J1818.0-1607 is an important link between regular magnetars and high magnetic field rotation powered pulsars., Comment: 13 pages, 4 figures, 2tables, accepted for publication in ApJ
Published: 2020
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28. Proper motion, spectra, and timing of PSR J1813-1749 using Chandra and NICER

Author: Ho, Wynn C. G., Guillot, Sebastien, Parkinson, P. M. Saz, Limyansky, B., Ng, C. -Y., Bejger, Michal, Espinoza, Cristobal M., Haskell, B., Jaisawal, Gaurava K., and Malacaria, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: PSR J1813-1749 is one of the most energetic rotation-powered pulsars known, producing a pulsar wind nebula (PWN) and gamma-ray and TeV emission, but whose spin period is only measurable in X-ray. We present analysis of two Chandra datasets that are separated by more than ten years and recent NICER data. The long baseline of the Chandra data allows us to derive a pulsar proper motion mu_R.A.=-(0.067"+/-0.010") yr^-1 and mu_decl.=-(0.014"+/-0.007") yr^-1 and velocity v_perp~900-1600 km/s (assuming a distance d=3-5 kpc), although we cannot exclude a contribution to the change in measured pulsar position due to a change in brightness structure of the PWN very near the pulsar. We model the PWN and pulsar spectra using an absorbed power law and obtain best-fit absorption NH=(13.1+/-0.9)x10^22 cm^-2, photon index Gamma=1.5+/-0.1, and 0.3-10 keV luminosity Lx~5.4x10^34 erg/s (d/5 kpc)^2 for the PWN and Gamma=1.2+/-0.1 and Lx~9.3x10^33 erg/s (d/5 kpc)^2 for PSR J1813-1749. These values do not change between the 2006 and 2016 observations. We use NICER observations from 2019 to obtain a timing model of PSR J1813-1749, with spin frequency nu=22.35 Hz and spin frequency time derivative nudot=(-6.428+/-0.003)x10^-11 Hz/s. We also fit nu measurements from 2009-2012 and our 2019 value and find a long-term spin-down rate nudot=(-6.3445+/-0.0004)x10^-11 Hz/s. We speculate that the difference in spin-down rates is due to glitch activity or emission mode switching., Comment: 9 pages, 5 figures; accepted for publication in MNRAS
Published: 2020
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29. NICER-NuSTAR Observations of the Neutron Star Low-Mass X-ray Binary 4U 1735-44

Author: Ludlam, R. M., Cackett, E. M., García, J. A., Miller, J. M., Bult, P. M., Strohmayer, T. E., Guillot, S., Jaisawal, G. K., Malacaria, C., Fabian, A. C., and Markwardt, C. B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the first simultaneous $NICER$ and $NuSTAR$ observations of the neutron star (NS) low-mass X-ray binary 4U 1735$-$44, obtained in 2018 August. The source was at a luminosity of $\sim1.8~(D/5.6\ \mathrm{kpc})^{2}\times10^{37}$ ergs s$^{-1}$ in the $0.4-30$ keV band. We account for the continuum emission with two different continuum descriptions that have been used to model the source previously. Despite the choice in continuum model, the combined passband reveals a broad Fe K line indicative of reflection in the spectrum. In order to account for the reflection spectrum we utilize a modified version of the reflection model RELXILL that is tailored for thermal emission from accreting NSs. Alternatively, we also use the reflection convolution model of RFXCONV to model the reflected emission that would arise from a Comptonized thermal component for comparison. We determine that the innermost region of the accretion disk extends close to the innermost stable circular orbit ($R_{\mathrm{ISCO}}$) at the 90% confidence level regardless of reflection model. Moreover, the current flux calibration of $NICER$ is within 5% of the $NuSTAR$/FPMA(B)., Comment: Accepted for publication in ApJ, 8 pages, 1 table, 5 figures
Published: 2020
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30. The 2019 super-Eddington outburst of RX J0209.6-7427: Detection of pulsations and constraints on the magnetic field strength

Author: Vasilopoulos, G., Ray, P. S., Gendreau, K. C., Jenke, P. A., Jaisawal, G. K., Wilson-Hodge, C. A., Strohmayer, T. E., Altamirano, D., Iwakiri, W. B., Wolff, M. T., Guillot, S., Malacaria, C., and Stevens, A. L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In November 2019, MAXI detected an X-ray outburst from the known Be X-ray binary system RX J0209.6-7427 located in the outer wing of the Small Magellanic Cloud. We followed the outburst of the system with NICER which led to the discovery of X-ray pulsations with a period of 9.3 s. We analyzed simultaneous X-ray data obtained with NuSTAR and NICER allowing us to characterize the spectrum and provide an accurate estimate of its bolometric luminosity. During the outburst the maximum broadband X-ray luminosity of the system reached $1-2\times10^{39}$ erg/s, thus exceeding by about one order of magnitude the Eddington limit for a typical 1.4 $M_{\odot}$ mass neutron star (NS). Monitoring observations with Fermi/GBM and NICER allowed us to study the spin evolution of the NS and compare it with standard accretion torque models. We found that the NS magnetic field should be of the order of $3\times10^{12}$ G. We conclude that RX J0209.6-7427 exhibited one of the brightest outbursts observed from a Be X-ray binary pulsar in the Magellanic Clouds, reaching similar luminosity level to the 2016 outburst of SMC X-3. Despite the super-Eddington luminosity of RX J0209.6-7427, the NS appears to have only a moderate magnetic field strength., Comment: 10 pages, 8 figures, accepted for publication in MNRAS
Published: 2020
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31. The Ups & Downs of Accreting X-Ray Pulsars: Decade-long observations with the Fermi Gamma-Ray Burst Monitor

Author: Malacaria, C., Jenke, P., Roberts, O. J., Wilson-Hodge, C. A., Cleveland, W. H., and Mailyan, B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We review more than 10 years of continuous monitoring of accreting X-ray pulsars with the all-sky Gamma-ray Burst Monitor (GBM) aboard the Fermi Gamma-ray Space Telescope. Our work includes data from the start of GBM operations in August 2008, through to November 2019. Pulsations from 39 accreting pulsars are observed over an energy range of $10-50\,$keV by GBM. The GBM Accreting Pulsars Program (GAPP) performs data reduction and analysis for each accreting pulsar and makes histories of the pulse frequency and pulsed flux publicly available. We examine in detail the spin histories, outbursts and torque behaviors of the persistent and transient X-ray pulsars observed by GBM. The spin period evolution of each source is analyzed in the context of disk-accretion and quasi-spherical settling accretion driven torque models. Long-term pulse frequency histories are also analyzed over the GBM mission lifetime and compared to those available from the previous BATSE all-sky monitoring mission, revealing previously unnoticed episodes in some of the analyzed sources (such as a torque reversal in 2S 1845-024). We obtain new, or update known, orbital solutions for three sources. Our results demonstrate the capabilities of GBM as an excellent instrument for monitoring accreting X-ray pulsars and its important scientific contribution to this field., Comment: Published online by ApJ. Proofs edition + more typos fixed
Published: 2020
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32. Timing of the accreting millisecond pulsar IGR J17591-2342: evidence of spin-down during accretion

Author: Sanna, A., Burderi, L., Gendreau, K. C., Di Salvo, T., Ray, P. S., Riggio, A., Gambino, A. F., Iaria, R., Piga, L., Malacaria, C., and Jaisawal, G. K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the phase-coherent timing analysis of the accreting millisecond X-ray pulsar IGR J17591-2342, using Neutron Star Interior Composition Explorer (NICER) data taken during the outburst of the source between 2018 August 15 and 2018 October 17. We obtain an updated orbital solution of the binary system. We investigate the evolution of the neutron star spin frequency during the outburst, reporting a refined estimate of the spin frequency and the first estimate of the spin frequency derivative ($\dot{\nu} \sim -7\times 10^{-14}$ Hz s$^{-1}$), confirmed independently from the modelling of the fundamental frequency and its first harmonic. We further investigate the evolution of the X-ray pulse phases adopting a physical model that accounts for the accretion material torque as well as the magnetic threading of the accretion disc in regions where the Keplerian velocity is slower than the magnetosphere velocity. From this analysis we estimate the neutron star magnetic field $B_{eq} = 2.8(3)\times10^{8}$ G. Finally, we investigate the pulse profile dependence on energy finding that the observed behaviour of the pulse fractional amplitude and lags as a function of energy are compatible with a thermal Comptonisation of the soft photons emitted from the neutron star caps., Comment: Submitted to MNRAS. 10 pages, 6 figures, 2 tables
Published: 2020
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33. The Fourth Fermi-GBM Gamma-Ray Burst Catalog: A Decade of Data

Author: von Kienlin, A., Meegan, C. A., Paciesas, W. S., Bhat, P. N., Bissaldi, E., Briggs, M. S., Burns, E., Cleveland, W. H., Gibby, M. H., Giles, M. M., Goldstein, A., Hamburg, R., Hui, C. M., Kocevski, D., Mailyan, B., Malacaria, C., Poolakkil, S., Preece, R. D., Roberts, O. J., Veres, P., and Wilson-Hodge, C. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the fourth in a series of catalogs of gamma-ray bursts (GRBs) observed with Fermi's Gamma-Ray Burst Monitor (Fermi-GBM). It extends the six year catalog by four more years, now covering the ten year time period from trigger enabling on 2008 July 12 to 2018 July 11. During this time period GBM triggered almost twice a day on transient events of which we identifyied 2356 as cosmic GRBs. Additional trigger events were due to solar are events, magnetar burst activities, and terrestrial gamma-ray flashes. The intention of the GBM GRB catalog series is to provide updated information to the community on the most important observables of the GBM-detected GRBs. For each GRB the location and main characteristics of the prompt emission, the duration, peak flux, and fluence are derived. The latter two quantities are calculated for the 50-300 keV energy band, where the maximum energy release of GRBs in the instrument reference system is observed and also for a broader energy band from 10-1000 keV, exploiting the full energy range of GBM's low-energy detectors. Furthermore, information is given on the settings of the triggering criteria and exceptional operational conditions during years 7 to 10 in the mission. This fourth catalog is an official product of the Fermi-GBM science team, and the data files containing the complete results are available from the High-Energy Astrophysics Science Archive Research Center (HEASARC)., Comment: 273 pages, 10 figures, 8 tables. This is a 10 year catalog update of arXiv:1603.07612
Published: 2020
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34. Observations of a GX 301-2 Apastron Flare with the X-Calibur Hard X-Ray Polarimeter Supported by NICER, the Swift XRT and BAT, and Fermi GBM

Author: Abarr, Q., Baring, M., Beheshtipour, B., Beilicke, M., deGeronimo, G., Dowkontt, P., Errando, M., Guarino, V., Iyer, N., Kislat, F., Kiss, M., Kitaguchi, T., Krawczynski, H., Lanzi, J., Li, S., Lisalda, L., Okajima, T., Pearce, M., Press, L., Rauch, B., Stuchlik, D., Takahashi, H., Tang, J., Uchida, N., West, A., Jenke, P., Krimm, H., Lien, A., Malacaria, C., Miller, J. M., and Wilson-Hodge, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: The accretion-powered X-ray pulsar GX 301-2 was observed with the balloon-borne X-Calibur hard X-ray polarimeter during late December 2018, with contiguous observations by the NICER X-ray telescope, the Swift X-ray Telescope and Burst Alert Telescope, and the Fermi Gamma-ray Burst Monitor spanning several months. The observations detected the pulsar in a rare apastron flaring state coinciding with a significant spin-up of the pulsar discovered with the Fermi GBM. The X-Calibur, NICER, and Swift observations reveal a pulse profile strongly dominated by one main peak, and the NICER and Swift data show strong variation of the profile from pulse to pulse. The X-Calibur observations constrain for the first time the linear polarization of the 15-35 keV emission from a highly magnetized accreting neutron star, indicating a polarization degree of (27+38-27)% (90% confidence limit) averaged over all pulse phases. We discuss the spin-up and the X-ray spectral and polarimetric results in the context of theoretical predictions. We conclude with a discussion of the scientific potential of future observations of highly magnetized neutron stars with the more sensitive follow-up mission XL-Calibur., Comment: Accepted for publication in the Astrophysical Journal. 20 pages, 19 figures, 4 tables
Published: 2020
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35. A Joint Fermi-GBM and LIGO/Virgo Analysis of Compact Binary Mergers From the First and Second Gravitational-wave Observing Runs

Author: Team, The Fermi Gamma-ray Burst Monitor, Collaboration, the LIGO Scientific, Collaboration, the Virgo, Hamburg, R., Fletcher, C., Burns, E., Goldstein, A., Bissaldi, E., Briggs, M. S., Cleveland, W. H., Giles, M. M., Hui, C. M., Kocevski, D., Lesage, S., Mailyan, B., Malacaria, C., Poolakkil, S., Preece, R., Roberts, O. J., Veres, P., von Kienlin, A., Wilson-Hodge, C. A., Wood, J., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aich, A., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Ansoldi, S., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Arnaud, N., Aronson, S. M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baer, A. M., Baird, J., Baldaccini, F., Ballardin, G., Ballmer, S. W., Bals, A., Balsamo, A., Baltus, G., Banagiri, S., Bankar, D., Bankar, R. S., Barayoga, J. C., Barbieri, C., Barish, B. C., Barker, D., Barkett, K., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Benjamin, M. G., Bentley, J. D., Bergamin, F., Berger, B. K., Bergmann, G., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bhandari, A. V., Bidler, J., Biggs, E., Bilenko, I. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bissenbayeva, G., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderon, Callaghan, J. D., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Castaneda, J., Caudill, S., Cavaglia, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chan, C., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. P., Cheong, C. K., Chia, H. Y., Chiadini, F., Chierici, R., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciecielag, P., Cieslar, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D., Colleoni, M., Collette, C. G., Collins, C., Colpi, M., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Covas, P. B., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cunningham, L., Cuoco, E., Curylo, M., Canton, T. Dal, Dalya, G., Dana, A., Daneshgaran-Bajastani, L. M., D'Angelo, B., Danilishin, S. L., D'Antonio, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davies, G. S., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Delfavero, M., De Lillo, N., Del Pozzo, W., DeMarchi, L. M., D'Emilio, V., Demos, N., Dent, T., De Pietri, R., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Diaz, M. C., Diaz-Ortiz Jr., M., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. G., Dupej, P., Durante, O., D'Urso, D., Dwyer, S. E., Easter, P. J., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Ewing, B. E., Fafone, V., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Feng, F., Fenyvesi, E., Ferguson, D. L., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fitz-Axen, M., Fiumara, V., Flaminio, R., Floden, E., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fronze, G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Galaudage, S., Ganapathy, D., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Gill, K., Glanzer, J., Gniesmer, J., Godwin, P., Goetz, E., Goetz, R., Gohlke, N., Goncharov, B., Gonzalez, G., Gopakumar, A., Gossan, S. E., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Griggs, H. L., Grignani, G., Grimaldi, A., Grimm, S. J., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guimaraes, A. R., Guixe, G., Gulati, H. K., Guo, Y., Gupta, A., Gupta, Anchal, Gupta, P., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hasskew, R. K., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heinze, J., Heitmann, H., Hellman, F., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J., Heurs, M., Hild, S., Hinderer, T., Hoback, S. Y., Hochheim, S., Hofgard, E., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Huang, Y., Hubner, M. T., Huerta, E. A., Huet, D., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Intini, G., Isac, J. -M., Isi, M., Iyer, B. R., Jacqmin, T., Jadhav, S. J., Jadhav, S. P., James, A. L., Jani, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jaume, R., Jenkins, A. C., Jiang, J., Johns, G. R., Jones, A. W., Jones, D. I., Jones, J. D., Jones, P., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kefelian, F., Keitel, D., Keivani, A., Kennedy, R., Key, J. S., Khadka, S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z. A., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, G. J., Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kovalam, M., Kozak, D. B., Kringel, V., Krishnendu, N. V., Krolak, A., Krupinski, N., Kuehn, G., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kumar, S., Kuo, L., Kutynia, A., Lackey, B. D., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., La Rosa, I., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Leroy, N., Letendre, N., Levin, Y., Li, A. K. Y., Li, J., li, K., Li, T. G. F., Li, X., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, J., Liu, X., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Luck, H., Lumaca, D., Lundgren, A. P., Ma, Y., Macas, R., Macfoy, S., MacInnis, M., Macleod, D. M., MacMillan, I. A. O., Macquet, A., Hernandez, I. Magana, Magana-Sandoval, F., Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, V., Martynov, D. V., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Mavalvala, N., Maynard, E., McCann, J. J., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIsaac, C., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Villa, E. Mejuto, Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Middleton, H., Milano, L., Miller, A. L., Millhouse, M., Mills, J. C., Milotti, E., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. J., Moraru, D., Morawski, F., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mozzon, S., Muciaccia, F., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukherjee, Subroto, Mukund, N., Mullavey, A., Munch, J., Muniz, E. A., Murray, P. G., Nagar, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, C., Nguyen, P., Nichols, D., Nichols, S. A., Nissanke, S., Nocera, F., Noh, M., North, C., Nothard, D., Nuttall, L. K., Oberling, J., O'Brien, B. D., Oganesyan, G., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Olivetto, C., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Osthelder, C., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, H., Panda, P. K., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Payne, E., Pearlstone, B. L., Pechsiri, T. C., Pedersen, A. J., Pedraza, M., Pele, A., Penn, S., Perego, A., Perez, C. J., Perigois, C., Perreca, A., Perries, S., Petermann, J., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Piotrzkowski, K., Pirello, M., Pitkin, M., Plastino, W., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Principe, M., Prodi, G. A., Prokhorov, L., Punturo, M., Puppo, P., Purrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rafferty, H., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rettegno, P., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riemenschneider, G., Riles, K., Rizzo, M., Robertson, N. A., Robinet, F., Rocchi, A., Rodriguez-Soto, R. D., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romero-Shaw, I. M., Romie, J. H., Rose, C. A., Rose, D., Rose, K., Rosinska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, P. K., Roy, Santosh, Roy, Soumen, Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salafia, O. S., Salconi, L., Saleem, M., Samajdar, A., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Santiago, K. A., Santos, E., Sarin, N., Sassolas, B., Sathyaprakash, B. S., Sauter, O., Savage, R. L., Savant, V., Sawant, D., Sayah, S., Schaetzl, D., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schonbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwarm, O., Schwartz, E., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Sharma, A., Sharma, P., Shawhan, P., Shen, H., Shikauchi, M., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shukla, K., ShyamSundar, S., Siellez, K., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singha, A., Singhal, A., Sintes, A. M., Sipala, V., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Soni, S., Sorazu, B., Sordini, V., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Spera, M., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stocks, D., Stops, D. J., Stover, M., Strain, K. A., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudhagar, S., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepanczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Tanasijczuk, A. J., Tanner, D. 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P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhao, G., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present results from offline searches of Fermi Gamma-ray Burst Monitor (GBM) data for gamma-ray transients coincident with the compact binary coalescences observed by the gravitational-wave (GW) detectors Advanced LIGO and Advanced Virgo during their first and second observing runs. In particular, we perform follow-up for both confirmed events and low significance candidates reported in the LIGO/Virgo catalog GWTC-1. We search for temporal coincidences between these GW signals and GBM triggered gamma-ray bursts (GRBs). We also use the GBM Untargeted and Targeted subthreshold searches to find coincident gamma-rays below the on-board triggering threshold. This work implements a refined statistical approach by incorporating GW astrophysical source probabilities and GBM visibilities of LIGO/Virgo sky localizations to search for cumulative signatures of coincident subthreshold gamma-rays. All search methods recover the short gamma-ray burst GRB 170817A occurring ~1.7 s after the binary neutron star merger GW170817. We also present results from a new search seeking GBM counterparts to LIGO single-interferometer triggers. This search finds a candidate joint event, but given the nature of the GBM signal and localization, as well as the high joint false alarm rate of $1.1 \times 10^{-6}$ Hz, we do not consider it an astrophysical association. We find no additional coincidences., Comment: Accepted for publication in ApJ. 18 pages, 4 figures, 1 table
Published: 2020
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36. NICER X-ray Observations of Seven Nearby Rotation-Powered Millisecond Pulsars

Author: Guillot, S., Kerr, M., Ray, P. S., Bogdanov, S., Ransom, S., Deneva, J. S., Arzoumanian, Z., Bult, P., Chakrabarty, D., Gendreau, K. C., Ho, W. C. G., Jaisawal, G. K., Malacaria, C., Miller, M. C., Strohmayer, T. E., Wolff, M. T., Wood, K. S., Webb, N. A., Guillemot, L., Cognard, I., and Theureau, G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: NICER observed several rotation-powered millisecond pulsars to search for or confirm the presence of X-ray pulsations. When broad and sine-like, these pulsations may indicate thermal emission from hot polar caps at the magnetic poles on the neutron star surface. We report confident detections ($\ge4.7\sigma$ after background filtering) of X-ray pulsations for five of the seven pulsars in our target sample: PSR J0614-3329, PSR J0636+5129, PSR J0751+1807, PSR J1012+5307, and PSR J2241-5236, while PSR J1552+5437 and PSR J1744-1134 remain undetected. Of those, only PSR J0751+1807 and PSR J1012+5307 had pulsations previously detected at the 1.7$\sigma$ and almost 3$\sigma$ confidence levels, respectively, in XMM-Newton data. All detected sources exhibit broad sine-like pulses, which are indicative of surface thermal radiation. As such, these MSPs are promising targets for future X-ray observations aimed at constraining the neutron star mass-radius relation and the dense matter equation of state using detailed pulse profile modeling. Furthermore, we find that three of the detected millisecond pulsars exhibit a significant phase offset between their X-ray and radio pulses., Comment: 25 pages, 11 tables, 4 figures. In press in The Astrophysical Journal Letters
Published: 2019
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37. The SUrvey for Pulsars and Extragalactic Radio Bursts IV: Discovery and polarimetry of a 12.1-second radio pulsar

Author: Morello, V., Keane, E. F., Enoto, T., Guillot, S., Ho, W. C. G., Jameson, A., Kramer, M., Stappers, B. W., Bailes, M., Barr, E. D., Bhandari, S., Caleb, M., Flynn, C. M. L., Jankowski, F., Johnston, S., van Straten, W., Arzoumanian, Z., Bogdanov, S., Gendreau, K. C., Malacaria, C., Ray, P. S., and Remillard, R. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of PSR~J2251$-$3711, a radio pulsar with a spin period of 12.1 seconds, the second longest currently known. Its timing parameters imply a characteristic age of 15 Myr, a surface magnetic field of $1.3 \times 10^{13}$~G and a spin-down luminosity of $2.9 \times 10^{29}~\mathrm{erg~s}^{-1}$. Its dispersion measure of 12.12(1)~$\mathrm{pc}~\mathrm{cm}^{-3}$ leads to distance estimates of 0.5 and 1.3 kpc according to the NE2001 and YMW16 Galactic free electron density models, respectively. Some of its single pulses show an uninterrupted 180 degree sweep of the phase-resolved polarization position angle, with an S-shape reminiscent of the rotating vector model prediction. However, the fact that this sweep occurs at different phases from one pulse to another is remarkable and without straightforward explanation. Although PSR~J2251$-$3711 lies in the region of the $P-\dot{P}$ parameter space occupied by the X-ray Isolated Neutron Stars (XINS), there is no evidence for an X-ray counterpart in our Swift XRT observation; this places a 99\%-confidence upper bound on its unabsorbed bolometric thermal luminosity of $1.1 \times 10^{31}~(d / 1~\mathrm{kpc})^2~\mathrm{erg/s}$ for an assumed temperature of 85 eV, where $d$ is the distance to the pulsar. Further observations are needed to determine whether it is a rotation-powered pulsar with a true age of at least several Myr, or a much younger object such as an XINS or a recently cooled magnetar. Extreme specimens like PSR J2251$-$3711 help bridge populations in the so-called neutron star zoo in an attempt to understand their origins and evolution., Comment: Accepted for publication in MNRAS, 13 pages, 8 figures
Published: 2019
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38. Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-Energy Emission from Prompt to Afterglow

Author: Ajello, M., Arimoto, M., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Berretta, A., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costantin, D., Cutini, S., D'Ammando, F., DeKlotz, M., Luque, P. de la Torre, de Palma, F., Desai, A., Di Lalla, N., Di Venere, L., Dirirsa, F. Fana, Fegan, S. J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Gill, R., Giordano, F., Giroletti, M., Granot, J., Green, D., Grenier, I. A., Grondin, M. H., Guiriec, S., Hays, E., Horan, D., Jóhannesson, G., Kocevski, D., Kovac'evic', M., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Liodakis, I., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Martí-Devesa, G., Mazziotta, M. N., McEnery, J. E., Mereu, I., Meyer, M., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Pei, Z., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Poon, H., Porter, T. A., Principe, G., Racusin, J. L., Rainò, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ryde, F., Parkinson, P. M. Saz, Serini, D., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Tajima, H., Takagi, K., Takahashi, M. N., Tak, D., Thayer, J. B., Thompson, D. J., Torres, D. F., Troja, E., Valverde, J., Van Klaveren, B., Wood, K., Yassine, M., Zaharijas, G., Bhat, P. N., Briggs, M. S., Cleveland, W., Giles, M., Goldstein, A., Hui, M., Malacaria, C., Preece, R., Roberts, O., Veres, P., von Kienlin, A., Cenko, S. B., O'Brien, P., Beardmore, A. P., Lien, A., Osborne, J. P., Tohuvavohu, A., D'Elia, V., D'A, A., Perri, M., Gropp, J., Klingler, N., Capalbi, M., Tagliaferri, G., and Stamatikos, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report on the observations of gamma-ray burst (GRB) 190114C by the Fermi Gamma-ray Space Telescope and the Neil Gehrels Swift Observatory. The early-time observations reveal multiple emission components that evolve independently, with a delayed power-law component that exhibits significant spectral attenuation above 40 MeV in the first few seconds of the burst. This power-law component transitions to a harder spectrum that is consistent with the afterglow emission observed at later times. This afterglow component is clearly identifiable in the GBM and BAT light curves as a slowly fading emission component on which the rest of the prompt emission is superimposed. As a result, we are able to constrain the transition from internal shock to external shock dominated emission. We find that the temporal and spectral evolution of the broadband afterglow emission can be well modeled as synchrotron emission from a forward shock propagating into a wind-like circumstellar environment and find that high-energy photons observed by Fermi LAT are in tension with the theoretical maximum energy that can be achieved through synchrotron emission from a shock. These violations of the maximum synchrotron energy are further compounded by the detection of very high energy (VHE) emission above 300 GeV by MAGIC concurrent with our observations. We conclude that the observations of VHE photons from GRB 190114C necessitates either an additional emission mechanism at very high energies that is hidden in the synchrotron component in the LAT energy range, an acceleration mechanism that imparts energy to the particles at a rate that is faster than the electron synchrotron energy loss rate, or revisions of the fundamental assumptions used in estimating the maximum photon energy attainable through the synchrotron process., Comment: 24 pages, 9 figures, Accepted to ApJ
Published: 2019
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39. NICER Discovers Spectral Lines During Photospheric Radius Expansion Bursts from 4U 1820-30: Evidence for Burst-driven Winds

Author: Strohmayer, T. E., Altamirano, D., Arzoumanian, Z., Bult, P. M., Chakrabarty, D., Chenevez, J., Fabian, A. C., Gendreau, K. C., Guillot, S., Zand, J. J. M. in 't, Jaisawal, G. K., Keek, L., Kosec, P., Ludlam, R. M., Mahmoodifar, S., Malacaria, C., and Miller, J. M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery with the Neutron Star Interior Composition Explorer (NICER) of narrow emission and absorption lines during photospheric radius expansion (PRE) X-ray bursts from the ultracompact binary 4U 1820-30. NICER observed the source in 2017 August accumulating about 60 ks of exposure. Five thermonuclear X-ray bursts were detected of which four showed clear signs of PRE. We extracted spectra during the PRE phases and fit each to a model that includes a comptonized component to describe the accretion-driven emission, and a black body for the burst thermal radiation. The temperature and spherical emitting radius of the fitted black body are used to assess the strength of PRE in each burst. The two strongest PRE bursts (burst pair 1) had black body temperatures of approximately 0.6 keV and emitting radii of 100 km (at a distance of 8.4 kpc). The other two bursts (burst pair 2) had higher temperatures (~0.67 keV) and smaller radii (75 km). All of the PRE bursts show evidence of narrow line emission near 1 keV. By co-adding the PRE phase spectra of burst pairs 1 and, separately, 2 we find, in both co-added spectra, significant, narrow, spectral features near 1.0 (emission), 1.7 and 3.0 keV (both in absorption). Remarkably, all the fitted line centroids in the co-added spectrum of burst pair 1 appear systematically blue-shifted by a factor of $1.046 \pm 0.006$ compared to the centroids of pair 2, strongly indicative of a gravitational red-shift, a wind-induced blue-shift, or more likely some combination of both effects. The observed shifts are consistent with this scenario in that the stronger PRE bursts in pair 1 reach larger photospheric radii, and thus have weaker gravitational red-shifts, and they generate faster outflows, yielding higher blue-shifts. We discuss possible elemental identifications for the observed features in the context of recent burst-driven wind models., Comment: 24 pages, 9 figures, accepted for publication in The Astrophysical Journal Letters
Published: 2019
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40. High-Precision X-ray Timing of Three Millisecond Pulsars with NICER: Stability Estimates and Comparison with Radio

Author: Deneva, J. S., Ray, P. S., Lommen, A., Ransom, S. M., Bogdanov, S., Kerr, M., Wood, K. S., Arzoumanian, Z., Black, K., Doty, J., Gendreau, K. C., Guillot, S., Harding, A., Lewandowska, N., Malacaria, C., Markwardt, C. B., Price, S., Winternitz, L., Wolff, M. T., Guillemot, L., Cognard, I., Baker, P. T., Blumer, H., Brook, P. R., Cromartie, H. T., Demorest, P. B., DeCesar, M. E., Dolch, T., Ellis, J. A., Ferdman, R. D., Ferrara, E. C., Fonseca, E., Garver-Daniels, N., Gentile, P. A., Jones, M. L., Lam, M. T., Lorimer, D. R., Lynch, R. S., McLaughlin, M. A., Ng, C., Nice, D. J., Pennucci, T. T., Spiewak, R., Stairs, I. H., Stovall, K., Swiggum, J. K., Vigeland, S. J., and Zhu, W. W.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Neutron Star Interior Composition Explorer (NICER) is an X-ray astrophysics payload on the International Space Station. It enables unprecedented high-precision timing of millisecond pulsars without the pulse broadening and delays due to dispersion and scattering within the interstellar medium that plague radio timing. We present initial timing results from a year of data on the millisecond pulsars PSR B1937+21 and PSR J0218+4232, and nine months of data on PSR B1821-24. NICER time-of-arrival uncertainties for the three pulsars are consistent with theoretical lower bounds and simulations based on their pulse shape templates and average source and background photon count rates. To estimate timing stability, we use the $\sigma_z$ measure, which is based on the average of the cubic coefficients of polynomial fits to subsets of timing residuals. So far we are achieving timing stabilities $\sigma_z \approx 3 \times 10^{-14}$ for PSR B1937+21 and on the order of $10^{-12}$ for PSRs B1821$-$24 and J0218+4232. Within the span of our \textit{NICER} data we do not yet see the characteristic break point in the slope of $\sigma_z$; detection of such a break would indicate that further improvement in the cumulative root-mean-square (RMS) timing residual is limited by timing noise. We see this break point in our comparison radio data sets for PSR B1821-24 and PSR B1937+21 on time scales of $> 2$ years., Comment: 30 pages, 15 figures; accepted to ApJ
Published: 2019
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41. Fermi GBM GRBs with characteristics similar to GRB 170817A

Author: von Kienlin, A., Veres, P., Roberts, O. J., Hamburg, R., Bissaldi, E., Briggs, M. S., Burns, E., Goldstein, A., Kocevski, D., Preece, R. D., Wilson-Hodge, C. A., Hui, C. M., Mailyan, B., and Malacaria, C.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a search for gamma-ray bursts in the Fermi-GBM 10 year catalog that show similar characteristics to GRB 170817A, the first electromagnetic counterpart to a GRB identified as a binary neutron star (BNS) merger via gravitational wave observations. Our search is focused on a non-thermal pulse, followed by a thermal component, as observed for GRB 170817A. We employ search methods based on the measured catalog parameters and Bayesian Block analysis. Our multi-pronged approach, which includes examination of the localization and spectral properties of the thermal component, yields a total of 13 candidates, including GRB 170817A and the previously reported similar burst, GRB 150101B. The similarity of the candidates is likely caused by the same processes that shaped the gamma-ray signal of GRB 170817A, thus providing evidence of a nearby sample of short GRBs resulting from BNS merger events. Some of the newly identfied counterparts were observed by other space telescopes and ground observatories, but none of them have a measured redshift. We present an analysis of this sub-sample, and we discuss two models. From uncovering 13 candidates during a time period of ten years we predict that Fermi-GBM will trigger on-board on about one burst similar to GRB 170817A per year., Comment: 18 pages, 9 figures, 4 tables. Accepted for publication in ApJ
Published: 2019
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42. A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run

Author: Fletcher, C, Wood, J, Hamburg, R, Veres, P, Hui, C, Bissaldi, E, Briggs, M, Burns, E, Cleveland, W, Giles, M, Goldstein, A, Hristov, B, Kocevski, D, Lesage, S, Mailyan, B, Malacaria, C, Poolakkil, S, von Kienlin, A, Wilson-Hodge, C, Crnogorcevic, M, Delaunay, J, Tohuvavohu, A, Caputo, R, Cenko, S, Laha, S, Parsotan, T, Abbott, R, Abe, H, Acernese, F, Ackley, K, Adhikari, N, Adhikari, R, Adkins, V, Adya, V, Affeldt, C, Agarwal, D, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Albanesi, S, Alfaidi, R, Allocca, A, Altin, P, Amato, A, Anand, C, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Ando, M, Andrade, T, Andres, N, Andres-Carcasona, M, Andric, T, Angelova, S, Ansoldi, S, Antelis, J, Antier, S, Apostolatos, T, Appavuravther, E, Appert, S, Apple, S, Arai, K, Araya, A, Araya, M, Areeda, J, Arene, M, Aritomi, N, Arnaud, N, Arogeti, M, Aronson, S, Arun, K, Asada, H, Asali, Y, Ashton, G, Aso, Y, Assiduo, M, Assis de Souza Melo, S, Aston, S, Astone, P, Aubin, F, Aultoneal, K, Austin, C, Babak, S, Badaracco, F, Bader, M, Badger, C, Bae, S, Bae, Y, Baer, A, Bagnasco, S, Bai, Y, Baird, J, Bajpai, R, Baka, T, Ball, M, Ballardin, G, Ballmer, S, Balsamo, A, Baltus, G, Banagiri, S, Banerjee, B, Bankar, D, Barayoga, J, Barbieri, C, Barish, B, Barker, D, Barneo, P, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, M, Bartos, I, Basak, S, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Becher, B, Becsy, B, Bedakihale, V, Beirnaert, F, Bejger, M, Belahcene, I, Benedetto, V, Beniwal, D, Benjamin, M, Bennett, T, Bentley, J, Benyaala, M, Bera, S, Berbel, M, Bergamin, F, Berger, B, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Beveridge, D, Bhandare, R, Bhandari, A, Bhardwaj, U, Bhatt, R, Bhattacharjee, D, Bhaumik, S, Bianchi, A, Bilenko, I, Billingsley, G, Bini, S, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Biswas, B, Bitossi, M, Bizouard, M, Blackburn, J, Blair, C, Blair, D, Blair, R, Bobba, F, Bode, N, Boer, M, Bogaert, G, Boldrini, M, Bolingbroke, G, Bonavena, L, Bondu, F, Bonilla, E, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, N, Bose, S, Bossilkov, V, Boudart, V, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branch, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Bruno, G, Bruntz, R, Bryant, J, Bucci, F, Bulik, T, Bulten, H, Buonanno, A, Burtnyk, K, Buscicchio, R, Buskulic, D, Buy, C, Byer, R, Cabourn Davies, G, Cabras, G, Cabrita, R, Cadonati, L, Caesar, M, Cagnoli, G, Cahillane, C, Calderon Bustillo, J, Callaghan, J, Callister, T, Calloni, E, Cameron, J, Camp, J, Canepa, M, Canevarolo, S, Cannavacciuolo, M, Cannon, K, Cao, H, Cao, Z, Capocasa, E, Capote, E, Carapella, G, Carbognani, F, Carlassara, M, Carlin, J, Carney, M, Carpinelli, M, Carrillo, G, Carullo, G, Carver, T, Casanueva Diaz, J, Casentini, C, Castaldi, G, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, W, Chalathadka Subrahmanya, S, Champion, E, Chan, C, Chan, K, Chan, M, Chandra, K, Chang, I, Chanial, P, Chao, S, Chapman-Bird, C, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, C, Chatterjee, D, Chaturvedi, M, Chaty, S, Chen, C, Chen, D, Chen, H, Chen, J, Chen, K, Chen, X, Chen, Y, Chen, Z, Cheng, H, Cheong, C, Cheung, H, Chia, H, Chiadini, F, Chiang, C, Chiarini, G, Chierici, R, Chincarini, A, Chiofalo, M, Chiummo, A, Choudhary, R, Choudhary, S, Christensen, N, Chu, Q, Chu, Y, Chua, S, Chung, K, Ciani, G, Ciecielag, P, Cieslar, M, Cifaldi, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Clara, F, Clark, J, Clearwater, P, Clesse, S, Cleva, F, Coccia, E, Codazzo, E, Cohadon, P, Cohen, D, Colleoni, M, Collette, C, Colombo, A, Colpi, M, Compton, C, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Cottingham, R, Coughlin, M, Coulon, J, Countryman, S, Cousins, B, Couvares, P, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Criswell, A, Croquette, M, Crowder, S, Cudell, J, Cullen, T, Cumming, A, Cummings, R, Cunningham, L, Cuoco, E, Curylo, M, Dabadie, P, Dal Canton, T, Dall'Osso, S, Dalya, G, Dana, A, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Darsow-Fromm, C, Dasgupta, A, Datrier, L, Datta, S, Dattilo, V, Dave, I, Davier, M, Davis, D, Davis, M, Daw, E, Dean, R, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Del Favero, V, De Lillo, F, De Lillo, N, Dell'Aquila, D, Del Pozzo, W, Demarchi, L, De Matteis, F, D'Emilio, V, Demos, N, Dent, T, Depasse, A, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Simone, R, Dhurandhar, S, Diaz, M, Didio, N, Dietrich, T, Di Fiore, L, Di Fronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Di Michele, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, Donahue, L, D'Onofrio, L, Donovan, F, Dooley, K, Doravari, S, Drago, M, Driggers, J, Drori, Y, Ducoin, J, Dupej, P, Dupletsa, U, Durante, O, D'Urso, D, Duverne, P, Dwyer, S, Eassa, C, Easter, P, Ebersold, M, Eckhardt, T, Eddolls, G, Edelman, B, Edo, T, Edy, O, Effler, A, Eguchi, S, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Ejlli, A, Engelby, E, Enomoto, Y, Errico, L, Essick, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Evstafyeva, T, Ewing, B, Fabrizi, F, Faedi, F, Fafone, V, Fair, H, Fairhurst, S, Fan, P, Farah, A, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favaro, G, Favata, M, Fays, M, Fazio, M, Feicht, J, Fejer, M, Fenyvesi, E, Ferguson, D, Fernandez-Galiana, A, Ferrante, I, Ferreira, T, Fidecaro, F, Figura, P, Fiori, A, Fiori, I, Fishbach, M, Fisher, R, Fittipaldi, R, Fiumara, V, Flaminio, R, Floden, E, Fong, H, Font, J, Fornal, B, Forsyth, 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M., Maggiore R., Magnozzi M., Mahesh S., Majorana E., Maksimovic I., Maliakal S., Malik A., Man N., Mandic V., Mangano V., Mansell G. L., Manske M., Mantovani M., Mapelli M., Marchesoni F., Marin Pina D., Marion F., Mark Z., Marka S., Marka Z., Markakis C., Markosyan A. S., Markowitz A., Maros E., Marquina A., Marsat S., Martelli F., Martin I. W., Martin R. M., Martinez M., Martinez V. A., Martinez V., Martinovic K., Martynov D. V., Marx E. J., Masalehdan H., Mason K., Massera E., Masserot A., Masso-Reid M., Mastrogiovanni S., Matas A., Mateu-Lucena M., Matichard F., Matiushechkina M., Mavalvala N., McCann J. J., McCarthy R., McClelland D. E., McClincy P. K., McCormick S., McCuller L., McGhee G. I., McGuire S. C., McIsaac C., McIver J., McRae T., McWilliams S. T., Meacher D., Mehmet M., Mehta A. K., Meijer Q., Melatos A., Melchor D. A., Mendell G., Menendez-Vazquez A., Menoni C. S., Mercer R. A., Mereni L., Merfeld K., Merilh E. L., Merritt J. 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L., Nagano K., Nagar A., Nakamura K., Nakano H., Nakano M., Nakayama Y., Napolano V., Nardecchia I., Narola H., Naticchioni L., Nayak B., Nayak R. K., Neil B. F., Neilson J., Nelson A., Nelson T. J. N., Nery M., Neubauer P., Neunzert A., Ng K. Y., Ng S. W. S., Nguyen C., Nguyen P., Nguyen T., Nguyen Quynh L., Ni J., Ni W. -T., Nichols S. A., Nishimoto T., Nishizawa A., Nissanke S., Nitoglia E., Nocera F., Norman M., North C., Nozaki S., Nurbek G., Nuttall L. K., Obayashi Y., Oberling J., O'Brien B. D., O'Dell J., Oelker E., Ogaki W., Oganesyan G., Oh J. J., Oh K., Oh S. H., Ohashi M., Ohashi T., Ohkawa M., Ohme F., Ohta H., Okada M. A., Okutani Y., Olivetto C., Oohara K., Oram R., O'Reilly B., Ormiston R. G., Ormsby N. D., O'Shaughnessy R., O'Shea E., Oshino S., Ossokine S., Osthelder C., Otabe S., Ottaway D. J., Overmier H., Pace A. E., Pagano G., Pagano R., Page M. A., Pagliaroli G., Pai A., Pai S. A., Pal S., Palamos J. R., Palashov O., Palomba C., Pan H., Pan K. -C., Panda P. K., Pang P. T. H., Pankow C., Pannarale F., Pant B. C., Panther F. H., Paoletti F., Paoli A., Paolone A., Pappas G., Parisi A., Park H., Park J., Parker W., Pascucci D., Pasqualetti A., Passaquieti R., Passuello D., Patel M., Pathak M., Patricelli B., Patron A. S., Paul S., Payne E., Pedraza M., Pedurand R., Pegoraro M., Pele A., Pena Arellano F. E., Penano S., Penn S., Perego A., Pereira A., Pereira T., Perez C. J., Perigois C., Perkins C. C., Perreca A., Perries S., Pesios D., Petermann J., Petterson D., Pfeiffer H. P., Pham H., Pham K. A., Phukon K. S., Phurailatpam H., Piccinni O. J., Pichot M., Piendibene M., Piergiovanni F., Pierini L., Pierro V., Pillant G., Pillas M., Pilo F., Pinard L., Pineda-Bosque C., Pinto I. M., Pinto M., Piotrzkowski B. J., Piotrzkowski K., Pirello M., Pitkin M. D., Placidi A., Placidi E., Planas M. L., Plastino W., Pluchar C., Poggiani R., Polini E., Pong D. Y. T., Ponrathnam S., Porter E. K., Poulton R., Poverman A., Powell J., Pracchia M., Pradier T., Prajapati A. K., Prasai K., Prasanna R., Pratten G., Principe M., Prodi G. A., Prokhorov L., Prosposito P., Prudenzi L., Puecher A., Punturo M., Puosi F., Puppo P., Purrer M., Qi H., Quartey N., Quetschke V., Quinonez P. J., Quitzow-James R., Raab F. J., Raaijmakers G., Radkins H., Radulesco N., Raffai P., Rail S. X., Raja S., Rajan C., Ramirez K. E., Ramirez T. D., Ramos-Buades A., Rana J., Rapagnani P., Ray A., Raymond V., Raza N., Razzano M., Read J., Rees L. A., Regimbau T., Rei L., Reid S., Reid S. W., Reitze D. H., Relton P., Renzini A., Rettegno P., Revenu B., Reza A., Rezac M., Ricci F., Richards D., Richardson J. W., Richardson L., Riemenschneider G., Riles K., Rinaldi S., Rink K., Robertson N. A., Robie R., Robinet F., Rocchi A., Rodriguez S., Rolland L., Rollins J. G., Romanelli M., Romano R., Romel C. L., Romero A., Romero-Shaw I. M., Romie J. H., Ronchini S., Rosa L., Rose C. A., Rosinska D., Ross M. P., Rowan S., Rowlinson S. J., Roy S., Rozza D., Ruggi P., Ruiz-Rocha K., Ryan K., Sachdev S., Sadecki T., Sadiq J., Saha S., Saito Y., Sakai K., Sakellariadou M., Sakon S., Salafia O. S., Salces-Carcoba F., Salconi L., Saleem M., Salemi F., Samajdar A., Sanchez E. J., Sanchez J. H., Sanchez L. E., Sanchis-Gual N., Sanders J. R., Sanuy A., Saravanan T. R., Sarin N., Sassolas B., Satari H., Sauter O., Savage R. L., Savant V., Sawada T., Sawant H. L., Sayah S., Schaetzl D., Scheel M., Scheuer J., Schiworski M. G., Schmidt P., Schmidt S., Schnabel R., Schneewind M., Schofield R. M. S., Schonbeck A., Schulte B. W., Schutz B. F., Schwartz E., Scott J., Scott S. M., Seglar-Arroyo M., Sekiguchi Y., Sellers D., Sengupta A. S., Sentenac D., Seo E. G., Sequino V., Sergeev A., Setyawati Y., Shaffer T., Shahriar M. S., Shaikh M. A., Shams B., Shao L., Sharma A., Sharma P., Shawhan P., Shcheblanov N. S., Sheela A., Shikano Y., Shikauchi M., Shimizu H., Shimode K., Shinkai H., Shishido T., Shoda A., Shoemaker D. H., Shoemaker D. M., ShyamSundar S., Sieniawska M., Sigg D., Silenzi L., Singer L. P., Singh D., Singh M. K., Singh N., Singha A., Sintes A. M., Sipala V., Skliris V., Slagmolen B. J. J., Slaven-Blair T. J., Smetana J., Smith J. R., Smith L., Smith R. J. E., Soldateschi J., Somala S. N., Somiya K., Song I., Soni K., Soni S., Sordini V., Sorrentino F., Sorrentino N., Soulard R., Souradeep T., Sowell E., Spagnuolo V., Spencer A. P., Spera M., Spinicelli P., Srivastava A. K., Srivastava V., Staats K., Stachie C., Stachurski F., Steer D. A., Steinlechner J., Steinlechner S., Stergioulas N., Stops D. J., Stover M., Strain K. A., Strang L. C., Stratta G., Strong M. D., Strunk A., Sturani R., Stuver A. L., Suchenek M., Sudhagar S., Sudhir V., Sugimoto R., Suh H. G., Sullivan A. G., Summerscales T. Z., Sun L., Sunil S., Sur A., Suresh J., Sutton P. J., Suzuki T., Swinkels B. L., Szczepanczyk M. J., Szewczyk P., Tacca M., Tagoshi H., Tait S. C., Takahashi H., Takahashi R., Takano S., Takeda H., Takeda M., Talbot C. J., Talbot C., Tanaka K., Tanaka T., Tanasijczuk A. J., Tanioka S., Tanner D. B., Tao D., Tao L., Tapia R. D., Tapia San Martin E. N., Taranto C., Taruya A., Tasson J. D., Tenorio R., Terhune J. E. S., Terkowski L., Thirugnanasambandam M. P., Thomas M., Thomas P., Thompson E. E., Thompson J. E., Thondapu S. R., Thorne K. A., Thrane E., Tiwari S., Tiwari V., Toivonen A. M., Tolley A. E., Tomaru T., Tomura T., Tonelli M., Tornasi Z., Torres-Forne A., Torrie C. I., Tosta Melo I. E., Toyra D., Trapananti A., Travasso F., Traylor G., Trevor M., Tringali M. C., Tripathee A., Troiano L., Trovato A., Trozzo L., Trudeau R. J., Tsai D., Tsang K. W., Tsang T., Tsao J. -S., Tse M., Tso R., Tsuchida S., Tsukada L., Tsuna D., Tsutsui T., Turbang K., Turconi M., Tuyenbayev D., Ubhi A. S., Uchiyama T., Udall R. P., Ueda A., Uehara T., Ueno K., Ueshima G., Unnikrishnan C. S., Urban A. L., Ushiba T., Utina A., Vajente G., Vajpeyi A., Valdes G., Valentini M., Valsan V., van Bakel N., van Beuzekom M., van Dael M., van den Brand J. F. J., Van Den Broeck C., Vander-Hyde D. C., van Haevermaet H., van Heijningen J. V., van Putten M. H. P. M., van Remortel N., Vardaro M., Vargas A. F., Varma V., Vasuth M., Vecchio A., Vedovato G., Veitch J., Veitch P. J., Venneberg J., Venugopalan G., Verkindt D., Verma P., Verma Y., Vermeulen S. M., Veske D., Vetrano F., Vicere A., Vidyant S., Viets A. D., Vijaykumar A., Villa-Ortega V., Vinet J. -Y., Virtuoso A., Vitale S., Vocca H., von Reis E. R. G., von Wrangel J. S. A., Vorvick C., Vyatchanin S. P., Wade L. E., Wade M., Wagner K. J., Walet R. C., Walker M., Wallace G. S., Wallace L., Wang J., Wang J. Z., Wang W. H., Ward R. L., Warner J., Was M., Washimi T., Washington N. Y., Watchi J., Weaver B., Weaving C. R., Webster S. A., Weinert M., Weinstein A. J., Weiss R., Weller C. M., Weller R. A., Wellmann F., Wen L., Wessels P., Wette K., Whelan J. T., White D. D., Whiting B. F., Whittle C., Wilken D., Williams D., Williams M. J., Williamson A. R., Willis J. L., Willke B., Wilson D. J., Wipf C. C., Wlodarczyk T., Woan G., Woehler J., Wofford J. K., Wong D., Wong I. C. F., Wright M., Wu C., Wu D. S., Wu H., Wysocki D. M., Xiao L., Yamada T., Yamamoto H., Yamamoto K., Yamamoto T., Yamashita K., Yamazaki R., Yang F. W., Yang K. Z., Yang L., Yang Y. -C., Yang Y., Yap M. J., Yeeles D. W., Yeh S. -W., Yelikar A. B., Ying M., Yokoyama J., Yokozawa T., Yoo J., Yoshioka T., Yu H., Yuzurihara H., Zadro¿ny A., Zanolin M., Zeidler S., Zelenova T., Zendri J. -P., Zevin M., Zhan M., Zhang H., Zhang J., Zhang L., Zhang R., Zhang T., Zhang Y., Zhao C., Zhao G., Zhao Y., Zhou R., Zhou Z., Zhu X. J., Zhu Z. -H., Zimmerman A. B., Zucker M. E., and Zweizig J.
Abstract: We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift- BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers.
Published: 2024

43. X-ray and optical monitoring of the December 2017 outburst of the Be/X-ray binary AX J0049.4-7323

Author: Ducci, L., Malacaria, C., Romano, P., Ji, L., Bozzo, E., Saathoff, I., Santangelo, A., and Udalski, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: AX J0049.4-7323 is a Be/X-ray binary that shows an unusual and poorly understood optical variability that consists of periodic and bright optical outbursts, simultaneous with X-ray outbursts, characterised by a highly asymmetric profile. The periodicity of the outbursts is thought to correspond to the orbital period of the neutron star. To understand the behaviour shown by this source, we performed the first multi-wavelength monitoring campaign during the periastron passage of December 2017. The monitoring lasted for ~37 days and consisted of X-ray, near-ultraviolet, and optical data from the Neil Gehrels Swift Observatory, the optical I band from the OGLE survey, and spectroscopic observations of the H-alpha line performed with the 3.9 m Anglo-Australian Telescope. These observations revealed AX J0049.4-7323 during an anomalous outburst having remarkably different properties compared to the previous ones. In the I band, it showed a longer rise timescale (~60 days instead of 1-5 days) and a longer decay timescale. At the peak of the outburst, it showed a sudden increase in luminosity in the I band, corresponding to the onset of the X-ray outburst. The monitoring of the H-alpha emission line showed a fast and highly variable profile composed of three peaks with variable reciprocal brightness. We interpreted these results as a circumstellar disc warped by tidal interactions with the neutron star in a high eccentricity orbit during its periastron passage. The fast jump in optical luminosity at the peak of the outburst and the previous asymmetric outbursts might be caused by the reprocessing of the X-ray photons in the circumstellar disc or the tidal displacement of a large amount of material from the circumstellar disc or the outer layers of the donor star during the periastron passage of the neutron star, which led to an increase in size of the region emitting in the I band., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2018
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44. NICER and Fermi GBM Observations of the First Galactic Ultraluminous X-ray Pulsar Swift J0243.6+6124

Author: Wilson-Hodge, C. A., Malacaria, C., Jenke, P. A., Jaisawal, G. K., Kerr, M., Wolff, M. T., Arzoumanian, Z., Chakrabarty, D., Doty, J. P., Gendreau, K. C., Guillot, S., Ho, W. C. G., LaMarr, B., Markwardt, C. B., Ozel, F., Prigozhin, G. Y., Ray, P. S., Ramos-Lerate, M., Remillard, R. A., Strohmayer, T. E., Vezie, M. L., and Wood, K. S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Swift J0243.6+6124 is a newly discovered Galactic Be/X-ray binary, revealed in late September 2017 in a giant outburst with a peak luminosity of 2E+39 (d/7 kpc)^2 erg/s (0.1-10 keV), with no formerly reported activity. At this luminosity, Swift J0243.6+6124 is the first known galactic ultraluminous X-ray pulsar. We describe Neutron star Interior Composition Explorer (NICER)} and Fermi Gamma-ray Burst Monitor (GBM) timing and spectral analyses for this source. A new orbital ephemeris is obtained for the binary system using spin-frequencies measured with GBM and 15-50 keV fluxes measured with the Neil Gehrels Swift Observatory Burst Alert Telescope to model the system's intrinsic spin-up. Power spectra measured with NICER show considerable evolution with luminosity, including a quasi-periodic oscillation (QPO) near 50 mHz that is omnipresent at low luminosity and has an evolving central frequency. Pulse profiles measured over the combined 0.2-100 keV range show complex evolution that is both luminosity and energy dependent. Near the critical luminosity of L~1E+38 erg/s, the pulse profiles transition from single-peaked to double peaked, the pulsed fraction reaches a minimum in all energy bands, and the hardness ratios in both NICER and GBM show a turn-over to softening as the intensity increases. This behavior repeats as the outburst rises and fades, indicating two distinct accretion regimes. These two regimes are suggestive of the accretion structure on the neutron star surface transitioning from a Coulomb collisional stopping mechanism at lower luminosities to a radiation-dominated stopping mechanism at higher luminosities. This is the highest observed (to date) value of the critical luminosity, suggesting a magnetic field of B ~1E+13 G., Comment: 35 pages, 7 figures (main text), 5 figures (appendix); Accepted for publication in ApJ on June 19, 2018
Published: 2018
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45. Detection of Reflection Features in the Neutron Star Low-Mass X-ray Binary Serpens X-1 with NICER

Author: Ludlam, R. M., Miller, J. M., Arzoumanian, Z., Bult, P. M., Cackett, E. M., Chakrabarty, D., Dauser, T., Enoto, T., Fabian, A. C., Garcia, J. A., Gendreau, K. C., Guillot, S., Homan, J., Jaisawal, G. K., Keek, L., La Marr, B., Malacaria, C., Markwardt, C. B., Steiner, J. F., and Strohmayer, T. E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present Neutron Star Interior Composition Explorer (NICER) observations of the neutron star low-mass X-ray binary Serpens X-1 during the early mission phase in 2017. With the high spectral sensitivity and low-energy X-ray passband of NICER, we are able to detect the Fe L line complex in addition to the signature broad, asymmetric Fe K line. We confirm the presence of these lines by comparing the NICER data to archival observations with XMM-Newton/RGS and NuSTAR. Both features originate close to the innermost stable circular orbit (ISCO). When modeling the lines with the relativistic line model RELLINE, we find the Fe L blend requires an inner disk radius of $1.4_{-0.1}^{+0.2}$ $R_{\mathrm{ISCO}}$ and Fe K is at $1.03_{-0.03}^{+0.13}$ $R_{\mathrm{ISCO}}$ (errors quoted at 90%). This corresponds to a position of $17.3_{-1.2}^{+2.5}$ km and $12.7_{-0.4}^{+1.6}$ km for a canonical neutron star mass ($M_{\mathrm{NS}}=1.4\ M_{\odot}$) and dimensionless spin value of $a=0$. Additionally, we employ a new version of the RELXILL model tailored for neutron stars and determine that these features arise from a dense disk and supersolar Fe abundance., Comment: 6 pages, 4 figures, 1 table, accepted for publication in ApJL
Published: 2018
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46. In-depth study of long-term variability in the X-ray emission of the Be/X-ray binary system AX J0049.4-7323

Author: Ducci, L., Romano, P., Malacaria, C., Ji, L., Bozzo, E., and Santangelo, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: AX J0049.4-7323 is a Be/X-ray binary in the Small Magellanic Cloud hosting a ~750 s pulsar which has been observed over the last ~17 years by several X-ray telescopes. Despite numerous observations, little is known about its X-ray behaviour. Therefore, we coherently analysed archival Swift, Chandra, XMM-Newton, RXTE, and INTEGRAL data, and we compared them with already published ASCA data, to study its X-ray long-term spectral and flux variability. AX J0049.4-7323 shows a high X-ray variability, spanning more than three orders of magnitudes, from L ~ 1.6E37 erg/s (0.3-8 keV, d=62 kpc) down to L ~ 8E33 erg/s. RXTE, Chandra, Swift, and ASCA observed, in addition to the expected enhancement of X-ray luminosity at periastron, flux variations by a factor of ~ 270 with peak luminosities of ~2.1E36 erg/s far from periastron. These properties are difficult to reconcile with the typical long-term variability of Be/XRBs, traditionally interpreted in terms of type I and type II outbursts. The study of AX J0049.4-7323 is complemented with a spectral analysis of Swift, Chandra, and XMM-Newton data which showed a softening trend when the emission becomes fainter, and an analysis of optical/UV data collected by the UVOT telescope on board Swift. In addition, we measured a secular spin-up rate of $\dot{P}=(-3.00\pm0.12)\times 10^{-3}$ s day$^{-1}$, which suggests that the pulsar has not yet achieved its equilibrium period. Assuming spherical accretion, we estimated an upper limit for the magnetic field strength of the pulsar of ~3E12 G., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2018
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47. Optical spectroscopy of the Be/X-ray Binary V850 Cen/GX 304-1 during faint X-ray periodical activity

Author: Malacaria, C., Kollatschny, W., Whelan, E., Santangelo, A., Klochkov, D., McBride, V., and Ducci, L.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Be/X-ray binaries are the most populous class of High Mass X-ray Binaries. Their X-ray duty cycle is tightly related to the optical companion wind activity, which in turn can be studied through optical spectroscopical dedicated observations. We study optical spectral features of the Be circumstellar disk to test their long-term variability and their relation with the X-ray activity. Special attention has been given to the H$\alpha$ emission line, that is one of the best tracers of the disk conditions. We obtained optical broadband medium resolution spectra from a dedicated campaign with the Anglo-Australian Telescope and the Southern African Large Telescope in 2014-2015. Data span over one entire binary orbit, and cover both X-ray quiescent and moderately active periods. We used Balmer emission lines to follow the evolution of the circumstellar disk. We observe prominent spectral features, like double-peaked H$\alpha$ and H$\beta$ emission lines. The H$\alpha$ V/R ratio significantly changes over a time scale of about one year. Our observations are consistent with a system observed at a large inclination angle ($i\gtrsim60^{\circ}$). The derived circumstellar disk size shows that the disk evolves from a configuration that prevents accretion onto the neutron star, to one that allows only moderate accretion. This is in agreement with the contemporary observed X-ray activity. Our results are interpreted within the context of inefficient tidal truncation of the circumstellar disk, as expected for this source's binary configuration. We derived the H$\beta$-emitting region size, which results about half of the corresponding H$\alpha$-emitting disk, and constrain the luminosity class of V850 Cen as III-V, consistent with the previously proposed class.}, Comment: 7 pages, 5 figures, Accepted for publication on A&A
Published: 2017
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48. Probing the emission mechanism and nature of the pulsating compact object in the X-ray binary SAX J1324.4−6200

Author: Ducci, L., primary, Bozzo, E., additional, Burgay, M., additional, Malacaria, C., additional, Ridolfi, A., additional, Romano, P., additional, Serim, M. M., additional, Vercellone, S., additional, and Santangelo, A., additional
Published: 2024
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49. Unveiling the origin of the optical and UV emission during the 2017 giant outburst of the Galactic ULX pulsar Swift J0243.6+6124

Author: Alfonso-Garzón, J., primary, van den Eijnden, J., additional, Kuin, N. P. M., additional, Fürst, F., additional, Rouco Escorial, A., additional, Fabregat, J., additional, Reig, P., additional, Mas-Hesse, J. M., additional, Jenke, P. A., additional, Malacaria, C., additional, and Wilson-Hodge, C., additional
Published: 2024
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50. Two giant outbursts of V 0332+53 observed with INTEGRAL

Author: Ferrigno, C., Ducci, L., Bozzo, E., Kretschmar, P., Kühnel, M., Malacaria, C., Pottschmidt, K., Santangelo, A., Savchenko, V., and Wilms, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In July 2015, the high-mass X-ray binary V 0332+53 underwent a giant outburst, a decade after the previous one. This system hosts a strongly magnetized neutron star. During the 2004--2005 outburst, an anti-correlation between the centroid energy of its fundamental cyclotron resonance scattering features (CRSFs) and the X-ray luminosity was observed. The long ($\approx 100$ d) and bright ($L_{\rm x} \approx 10^{38}$ erg s$^{-1}$) 2015 outburst offered the opportunity to study during another outburst the unique properties of the fundamental CRSF and its dependence on the X-ray luminosity. The source was observed by the INTEGRAL satellite for $\sim 330$ ks. We exploit the spectral resolution at high energies of the SPectrometer on INTEGRAL (SPI) and the Joint European X-ray Monitors to characterize its spectral properties, focusing in particular on the CRSF-luminosity dependence. We complement the data of the 2015 outburst with those collected by SPI in 2004--2005 and left unpublished so far. We find a highly significant anti-correlation of the centroid energy of the fundamental CRSF and the $3-100$ keV luminosity of $E_1 \propto -0.095(8)L_{37}$ keV. This trend is observed for both outbursts. We confirm the correlation between the width of the fundamental CRSF and the X-ray luminosity previously found in the JEM-X and IBIS dataset of the 2004--2005 outburst. By exploiting the RXTE/ASM and Swift/BAT monitoring data we also report on the detection of a $\sim 34$ d modulation superimposed on the mean profiles and roughly consistent with the orbital period of the pulsar. We discuss possible interpretations of such variability., Comment: Accepted for publication on A&A
Published: 2016
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