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11 results on '"K. Noysena"'

1. Self-Supervised Clustering on Image-Subtracted Data with Deep-Embedded Self-Organizing Map

Author

Y-L Mong, K Ackley, T L Killestein, D K Galloway, C Vassallo, M Dyer, R Cutter, M J I Brown, J Lyman, K Ulaczyk, D Steeghs, V Dhillon, P O’Brien, G Ramsay, K Noysena, R Kotak, R Breton, L Nuttall, E Pallé, D Pollacco, E Thrane, S Awiphan, U Burhanudin, P Chote, A Chrimes, E Daw, C Duffy, R Eyles-Ferris, B P Gompertz, T Heikkilä, P Irawati, M Kennedy, A Levan, S Littlefair, L Makrygianni, T Marsh, D Mata Sánchez, S Mattila, J R Maund, J McCormac, D Mkrtichian, J Mullaney, E Rol, U Sawangwit, E Stanway, R Starling, P Strøm, S Tooke, and K Wiersema

Subjects
FOS: Computer and information sciences, Space and Planetary Science, Computer Vision and Pattern Recognition (cs.CV), Computer Science - Computer Vision and Pattern Recognition, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Developing an effective automatic classifier to separate genuine sources from artifacts is essential for transient follow-ups in wide-field optical surveys. The identification of transient detections from the subtraction artifacts after the image differencing process is a key step in such classifiers, known as real-bogus classification problem. We apply a self-supervised machine learning model, the deep-embedded self-organizing map (DESOM) to this ‘real-bogus’ classification problem. DESOM combines an autoencoder and a self-organizing map to perform clustering in order to distinguish between real and bogus detections, based on their dimensionality-reduced representations. We use 32 × 32 normalized detection thumbnails as the input of DESOM. We demonstrate different model training approaches, and find that our best DESOM classifier shows a missed detection rate of $6.6{{\ \rm per\,cent}}$ with a false-positive rate of $1.5{{\ \rm per\,cent}}$. DESOM offers a more nuanced way to fine-tune the decision boundary identifying likely real detections when used in combination with other types of classifiers, e.g. built on neural networks or decision trees. We also discuss other potential usages of DESOM and its limitations.

Published
2022

2. GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Author

D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, X. F. Zhao, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Polytechnique des Sciences Avancées (IPSA), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), and Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Space and Planetary Science, Astronomy and Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

GRB 221009A is the brightest Gamma-Ray Burst detected in more than 50 yearsof study. Here, we present observations in the X-ray and optical domainsranging from the prompt emission (optical coverage by all-sky cameras) up to 20days after the GRB obtained by the GRANDMA Collaboration (which includesobservations from more than 30 professional and amateur telescopes) and the\textit{Insight}-HXMT Collaboration operating the X-ray telescope HXMT-LE. Westudy the optical afterglow both with empirical fitting procedures andnumerical modeling. We find that the GRB afterglow, extinguished by a largedust column, is most likely behind a combination of a large Milky-Way dustcolumn combined with moderate low-metallicity dust in the host galaxy. We findthat numerical models describing the synchrotron radiation at the forward shockof a relativistic top-hat jet propagating through a constant density mediumrequire extreme parameters to fit the observational data. Based on theseobservations, we constrain the isotropic afterglow energy $E_{0} \sim 3.7\times 10^{54}$ erg, the density of the ambient medium $n_{\mathrm{ism}}\gtrsim 1~\mathrm{cm}^{-3}$ and the opening angle of the jet core to be$\gtrsim10.7^\circ$. We do not find evidence (for or against) of jet structure,a potential jet break and the presence or absence of a SN. Placed in the globalcontext of GRB optical afterglows, we find the afterglow of GRB 221009A isluminous but not extraordinarily so, highlighting that some aspects of this GRBdo not deviate from the known sample despite its extreme energetics and thepeculiar afterglow evolution.

Published
2023

3. GRANDMA Observations of ZTF/Fink Transients during Summer 2021

Author

V Aivazyan, M Almualla, S Antier, A Baransky, K Barynova, S Basa, F Bayard, S Beradze, D Berezin, M Blazek, D Boutigny, D Boust, E Broens, O Burkhonov, A Cailleau, N Christensen, D Cejudo, A Coleiro, M W Coughlin, D Datashvili, T Dietrich, F Dolon, J-G Ducoin, P-A Duverne, G Marchal-Duval, C Galdies, L Granier, V Godunova, P Gokuldass, H B Eggenstein, M Freeberg, P Hello, R Inasaridze, E E O Ishida, P Jaquiery, D A Kann, G Kapanadze, S Karpov, R W Kiendrebeogo, A Klotz, R Kneip, N Kochiashvili, W Kou, F Kugel, C Lachaud, S Leonini, A Leroy, N Leroy, A Le Van Su, D Marchais, M Mašek, T Midavaine, A Möller, D Morris, R Natsvlishvili, F Navarete, K Noysena, S Nissanke, K Noonan, N B Orange, J Peloton, A Popowicz, T Pradier, M Prouza, G Raaijmakers, Y Rajabov, M Richmond, Ya Romanyuk, L Rousselot, T Sadibekova, M Serrau, O Sokoliuk, X Song, A Simon, C Stachie, A Taylor, Y Tillayev, D Turpin, M Vardosanidze, J Vlieghe, I Tosta e Melo, X F Wang, J Zhu, Ministerio de Ciencia e Innovación (España), European Commission, Centre National D'Etudes Spatiales (France), Netherlands Organization for Scientific Research, Dutch Research Council, National Natural Science Foundation of China, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and GRANDMA

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Neutron stars -- Mathematical models, FOS: Physical sciences, Astronomy and Astrophysics, Space telescopes, Neutron stars, Gravitational waves, Space and Planetary Science, Methods: data analysis, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Neutron star mergers
Abstract

Full list of authors: Aivazyan, V; Almualla, M.; Antier, S.; Baransky, A.; Barynova, K.; Basa, S.; Bayard, F.; Beradze, S.; Berezin, D.; Blazek, M.; Boutigny, D.; Boust, D.; Broens, E.; Burkhonov, O.; Cailleau, A.; Christensen, N.; Cejudo, D.; Coleiro, A.; Coughlin, M. W.; Datashvili, D.; Dietrich, T.; Dolon, F.; Ducoin, J-G; Duverne, P-A; Marchal-Duval, G.; Galdies, C.; Granier, L.; Godunova, V; Gokuldass, P.; Eggenstein, H. B.; Freeberg, M.; Hello, P.; Inasaridze, R.; Ishida, E. E. O.; Jaquiery, P.; Kann, D. A.; Kapanadze, G.; Karpov, S.; Kiendrebeogo, R. W.; Klotz, A.; Kneip, R.; Kochiashvili, N.; Kou, W.; Kugel, F.; Lachaud, C.; Leonini, S.; Leroy, A.; Leroy, N.; Su, A. Le Van; Marchais, D.; Midavaine, T.; Moeller, A.; Morris, D.; Natsvlishvili, R.; Navarete, F.; Noysena, K.; Nissanke, S.; Noonan, K.; Orange, N. B.; Peloton, J.; Popowicz, A.; Pradier, T.; Prouza, M.; Raaijmakers, G.; Rajabov, Y.; Richmond, M.; Romanyuk, Ya; Rousselot, L.; Sadibekova, T.; Serrau, M.; Sokoliuk, O.; Song, X.; Simon, A.; Stachie, C.; Taylor, A.; Tillayev, Y.; Turpin, D.; Vardosanidze, M.; Vlieghe, J.; Tosta e Melo, I; Wang, X. F.; Zhu, J., We present our follow-up observations with GRANDMA of transient sources revealed by the Zwicky Transient Facility (ZTF). Over a period of six months, all ZTF alerts were examined in real time by a dedicated science module implemented in the Fink broker, which will be used in filtering of transients discovered by the Vera C. Rubin Observatory. In this article, we present three selection methods to identify kilonova candidates. Out of more than 35 million alerts, a hundred sources have passed our selection criteria. Six were then followed-up by GRANDMA (by both professional and amateur astronomers). The majority were finally classified either as asteroids or as supernovae events. We mobilized 37 telescopes, bringing together a large sample of images, taken under various conditions and quality. To complement the orphan kilonova candidates, we included three additional supernovae alerts to conduct further observations during summer 2021. We demonstrate the importance of the amateur astronomer community that contributed images for scientific analyses of new sources discovered in a magnitude range r′ = 17 − 19 mag. We based our rapid kilonova classification on the decay rate of the optical source that should exceed 0.3 mag d−1. GRANDMA’s follow-up determined the fading rate within 1.5 ± 1.2 d post-discovery, without waiting for further observations from ZTF. No confirmed kilonovae were discovered during our observing campaign. This work will be continued in the coming months in the view of preparing for kilonova searches in the next gravitational-wave observing run O4. © 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society., SA and CL acknowledge the financial support of the Programme National Hautes Energies (PNHE). SA acknowledges the financial support of CNES. SA is grateful for financial support from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) through the VIDI (PI: Nissanke). SA dedicates her contribution to Rayan Ouram, who is a source of inspiration for bravity and humanity for GRANDMA. DT acknowledges the financial support of CNES post-doctoral program. UBAI acknowledges support from the Ministry of Innovative Development through projects FA-Atech-2018-392 and VA-FA-F-2-010. RI acknowledges Shota Rustaveli National Science Foundation (SRNSF) grant No - RF/18-1193. TAROT. has been built with the support of the Institut National des Sciences de l’Univers, CNRS, France. MP, SK, and MM are supported by European Structural and Investment Fund and the Czech Ministry of Education, Youth and Sports (Projects CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/15_003/0000437). The FRAM telescope is also supported by the Czech Ministry of Education, Youth and Sports (projects LM2015046, LM2018105, LTT17006). NBO and DM acknowledge financial support from NASA MUREP MIRO award 80NSSC21M0001, NASA EPSCoR award 80NSSC19M0060, and NSF EiR award 1901296. PG acknowledges financial support from NSF EiR award 1901296. DAK acknowledges support from Spanish National Research Project RTI2018-098104-J-I00 (GRBPhot) XW is supported by the National Science Foundation of China (NSFC grants 12033003 and 11633002), the Scholar Program of Beijing Academy of Science and Technology (DZ:BS202002), and the Tencent Xplorer Prize. The work of FN is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The GRANDMA consortium thank the amateur participants to the kilonova-catcher program. The kilonova-catcher program is supported by the IdEx Université de Paris, ANR-18-IDEX-0001. This research made use of the cross-match service provided by CDS, Strasbourg. MC acknowledges support from the National Science Foundation with grant numbers PHY-2010970 and OAC-2117997. GR acknowledges financial support from the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) through the Projectruimte and VIDI grants (PI: Nissanke). Thanks to the National Astronomical Research Institute of Thailand (Public Organization), based on observations made with the Thai Robotic Telescope under program ID TRTC08D_005 and TRTC09A_002. S., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Published
2022

4. Searching for Fermi GRB optical counterparts with the prototype Gravitational-wave Optical Transient Observer (GOTO)

Author

Rene P. Breton, B. P. Gompertz, Seppo Mattila, S. P. Littlefair, James Mullaney, J. D. Lyman, K. Noysena, Y. L. Mong, Eric Thrane, Danny Steeghs, Justyn R. Maund, T. R. Marsh, Klaas Wiersema, Michael J. I. Brown, E. Rol, Christopher J. Duffy, G. Ramsay, David Mkrtichian, Duncan K. Galloway, L. K. Nuttall, Martin J. Dyer, Puji Irawati, P. A. Strøm, P. T. O'Brien, T. Heikkilä, K. Ackley, Mark Kennedy, D. Mata-Sanchez, A. Chrimes, Utane Sawangwit, Don Pollacco, Elizabeth R. Stanway, V. S. Dhillon, R. L. C. Starling, E. J. Daw, Supachai Awiphan, Krzysztof Ulaczyk, S. Tooke, T. Killestein, Rubina Kotak, R. Cutter, Paul Chote, R. Eyles-Ferris, James McCormac, Andrew J. Levan, L. Makrygianni, U. Burhanudin, and Enric Palle

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Large field of view, Goto, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Observer (physics), 01 natural sciences, Square (algebra), Space and Planetary Science, 0103 physical sciences, Transient (oscillation), Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, QC, Fermi Gamma-ray Space Telescope, QB
Abstract

The typical detection rate of $\sim1$ gamma-ray burst (GRB) per day by the \emph{Fermi} Gamma-ray Burst Monitor (GBM) provides a valuable opportunity to further our understanding of GRB physics. However, the large uncertainty of the \emph{Fermi} localization typically prevents rapid identification of multi-wavelength counterparts. We report the follow-up of 93 \emph{Fermi} GRBs with the Gravitational-wave Optical Transient Observer (GOTO) prototype on La Palma. We selected 53 events (based on favourable observing conditions) for detailed analysis, and to demonstrate our strategy of searching for optical counterparts. We apply a filtering process consisting of both automated and manual steps to 60\,085 candidates initially, rejecting all but 29, arising from 15 events. With $\approx3$ GRB afterglows expected to be detectable with GOTO from our sample, most of the candidates are unlikely to be related to the GRBs. Since we did not have multiple observations for those candidates, we cannot confidently confirm the association between the transients and the GRBs. Our results show that GOTO can effectively search for GRB optical counterparts thanks to its large field of view of $\approx40$ square degrees and its depth of $\approx20$ mag. We also detail several methods to improve our overall performance for future follow-up programs of \emph{Fermi} GRBs.

Published
2021

5. The Gravitational-wave Optical Transient Observer (GOTO): prototype performance and prospects for transient science

Author

D Steeghs, D K Galloway, K Ackley, M J Dyer, J Lyman, K Ulaczyk, R Cutter, Y-L Mong, V Dhillon, P O’Brien, G Ramsay, S Poshyachinda, R Kotak, L K Nuttall, E Pallé, R P Breton, D Pollacco, E Thrane, S Aukkaravittayapun, S Awiphan, U Burhanudin, P Chote, A Chrimes, E Daw, C Duffy, R Eyles-Ferris, B Gompertz, T Heikkilä, P Irawati, M R Kennedy, T Killestein, H Kuncarayakti, A J Levan, S Littlefair, L Makrygianni, T Marsh, D Mata-Sanchez, S Mattila, J Maund, J McCormac, D Mkrtichian, J Mullaney, K Noysena, M Patel, E Rol, U Sawangwit, E R Stanway, R Starling, P Strøm, S Tooke, R West, D J White, and K Wiersema

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB
Abstract

The Gravitational-wave Optical Transient Observer (GOTO) is an array of wide-field optical telescopes, designed to exploit new discoveries from the next generation of gravitational wave detectors (LIGO, Virgo, KAGRA), study rapidly evolving transients, and exploit multi-messenger opportunities arising from neutrino and very high energy gamma-ray triggers. In addition to a rapid response mode, the array will also perform a sensitive, all-sky transient survey with few day cadence. The facility features a novel, modular design with multiple 40-cm wide-field reflectors on a single mount. In June 2017 the GOTO collaboration deployed the initial project prototype, with 4 telescope units, at the Roque de los Muchachos Observatory (ORM), La Palma, Canary Islands. Here we describe the deployment, commissioning, and performance of the prototype hardware, and discuss the impact of these findings on the final GOTO design. We also offer an initial assessment of the science prospects for the full GOTO facility that employs 32 telescope units across two sites., 19 pages, 16 Figures, accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2021

6. Light curve classification with recurrent neural networks for GOTO:dealing with imbalanced data

Author

Y. L. Mong, Duncan K. Galloway, V. S. Dhillon, James McCormac, U. Burhanudin, R. Eyles-Ferris, P. T. O'Brien, Danny Steeghs, Martin J. Dyer, S. P. Littlefair, Kendall Ackley, K. Noysena, Utane Sawangwit, L. K. Nuttall, Don Pollacco, R. L. C. Starling, T. Heikkilä, Mark Kennedy, Andrew J. Levan, J. D. Lyman, David Mkrtichian, Enric Palle, P. A. Strøm, Seppo Mattila, A. Chrimes, Klaas Wiersema, Elizabeth R. Stanway, James Mullaney, D. Mata-Sanchez, Puji Irawati, B. P. Gompertz, Christopher J. Duffy, Eric Thrane, Supachai Awiphan, Rene P. Breton, Krzysztof Ulaczyk, S. Tooke, T. Killestein, E. J. Daw, Rubina Kotak, Justyn R. Maund, G. Ramsay, Paul Chote, R. Cutter, and L. Makrygianni

Subjects
Data stream, Goto, FOS: Physical sciences, Scale-invariant feature transform, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, photometric [techniques], 0103 physical sciences, Classifier (linguistics), data analysis [methods], survey, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, STFC, Physics, 010308 nuclear & particles physics, business.industry, Deep learning, RCUK, Astronomy and Astrophysics, Pattern recognition, Object (computer science), Class (biology), Recurrent neural network, ST/R000964/1, Space and Planetary Science, Artificial intelligence, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

The advent of wide-field sky surveys has led to the growth of transient and variable source discoveries. The data deluge produced by these surveys has necessitated the use of machine learning (ML) and deep learning (DL) algorithms to sift through the vast incoming data stream. A problem that arises in real-world applications of learning algorithms for classification is imbalanced data, where a class of objects within the data is underrepresented, leading to a bias for over-represented classes in the ML and DL classifiers. We present a recurrent neural network (RNN) classifier that takes in photometric time-series data and additional contextual information (such as distance to nearby galaxies and on-sky position) to produce real-time classification of objects observed by the Gravitational-wave Optical Transient Observer (GOTO), and use an algorithm-level approach for handling imbalance with a focal loss function. The classifier is able to achieve an Area Under the Curve (AUC) score of 0.972 when using all available photometric observations to classify variable stars, supernovae, and active galactic nuclei. The RNN architecture allows us to classify incomplete light curves, and measure how performance improves as more observations are included. We also investigate the role that contextual information plays in producing reliable object classification., Comment: 16 pages, 12 figures, to be published in Monthly Notices of the Royal Astronomical Society

Published
2021

7. The first six months of the Advanced LIGO’s and Advanced Virgo’s third observing run with GRANDMA

Author

Jicheng Zhang, M. Boer, C. Delattre, Wenxiong Li, V. Aivazyan, Jérôme Berthier, N. Ismailov, Stéphane Basa, A. de Ugarte Postigo, N. Kochiashvili, M. Blažek, J. C. Chen, A. Cailleau, A. Simon, E. Arbouch, A. Baransky, Christina C. Thöne, Michael W. Coughlin, Bruce Gendre, Frédéric Vachier, Alain Klotz, O. A. Burkhonov, P. Thierry, Jun Mo, Xuhui Han, S. Perrigault, A. Burrell, S. Beradze, S. Antier, P. Fock-Hang, J. Moore, Jun-Jie Wei, Eric Howell, G. Marchal-Duval, D. Corre, Jie Zhang, K. Noysena, M. Vardosanidze, Shengyu Yan, D. Turpin, J. G. Ducoin, R. Inasaridze, J. P. Teng, T. Sadibekova, Patrice Hello, C. Wang, C. Lachaud, R. Marron, Z. Vidadi, S. Alishov, A. Le Van Su, G. Kapanadze, P.-A. Duverne, Xinghan Zhang, H. Crisp, V. Vasylenko, J. M. Bai, B. Chabert, A. Peyrot, R. Natsvlishvili, S. Agayeva, David Coward, P. Lognone, X. F. Wang, N. Leroy, David Alexander Kann, Tim Dietrich, K. Barynova, Alexis Coleiro, L. Eymar, Weili Lin, E. Bertin, B. Cordier, D. Samadov, Yusufjon Tillayev, Nelson Christensen, C. Stachie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), GRANDMA, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Australian Research Council, Ministerio de Economía y Competitividad (España), European Commission, California Institute of Technology, Centre National D'Etudes Spatiales (France), Sorbonne Université, Chinese Academy of Sciences, Agence Nationale de la Recherche (France), and Shota Rustaveli National Science Foundation

Subjects
neutron star: binary, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, Kilonova, 01 natural sciences, localization, Gravitational waves, stars: neutron, 0103 physical sciences, optical, observational [Methods], Spatial localization, structure, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], LIGO, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, gravitational radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, neutron [Stars], Astronomy and Astrophysics, Methods observational, messenger, Neutron star, electromagnetic, VIRGO, gravitational waves, efficiency, Space and Planetary Science, Sky, network, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-ray burst
Abstract

We present the Global Rapid Advanced Network Devoted to the Multi-messenger Addicts (GRANDMA). The network consists of 21 telescopes with both photometric and spectroscopic facilities. They are connected together thanks to a dedicated infrastructure. The network aims at coordinating the observations of large sky position estimates of transient events to enhance their follow-up and reduce the delay between the initial detection and optical confirmation. The GRANDMA programme mainly focuses on follow-up of gravitational-wave alerts to find and characterize the electromagnetic counterpart during the third observational campaign of the Advanced LIGO and Advanced Virgo detectors. But it allows for follow-up of any transient alerts involving neutrinos or gamma-ray bursts, even those with poor spatial localization. We present the different facilities, tools, and methods we developed for this network and show its efficiency using observations of LIGO/Virgo S190425z, a binary neutron star merger candidate.We furthermore report on allGRANDMAfollow-up observations performed during the first six months of the LIGO-Virgo observational campaign, and we derive constraints on the kilonova properties assuming that the events' locations were imaged by our telescopes. © 2019 The Author(s)., Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE170100004. EJH acknowledges support from a Australian Research Council DECRA Fellowship (DE170100891). AdUP and CCT acknowledge support from Ramon y Cajal fellowships RyC-2012-09975 and RyC-201209984 and the Spanish Ministry of Economy and Competitiveness through project AYA2017-89384-P. DAK acknowledges support from the Spanish research projectAYA2017-89384-P. MBacknowledges funding as `personal tecnico de apoyo' under fellowship number PTA2016-13192-I. MC is supported by the David and Ellen Lee Postdoctoral Fellowship at the California Institute of Technology. SA is supported by the CNES Postdoctoral Fellowship at Laboratoire AstroParticule et Cosmologie. SA, AC, CL, and RM acknowledge the financial support of the UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). SA and NL acknowledge the financial support of the Programme National Hautes Energies (PNHE). DT acknowledges the financial support of the Chinese Academy of Sciences (CAS) PIFI post-doctoral fellowship program (program C). UBAI acknowledges support from the Ministry of Innovative Development through projects FA-Atech-2018-392 and VA-FAF-2-010. IRiS has been carried out thanks to the support of the OCEVU Labex (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02) funded by the 'Investissements d'Avenir' French government program. IRiS and T120 thank all the Observatoire de Haute-Provence staff for the permanent support. SB, NK, RN, and MV acknowledge the Shota Rustaveli National Science Foundation (SRNSF grant No 218070). TAROT has been built with the support of the Institut National des Sciences de l'Univers, CNRS,France. TAROT is funded by theCNESand thanks the help of the technical staff of the Observatoire de Haute Provence, OSU-Pytheas.

Published
2019

8. Evidence that short period AM CVn systems are diverse in outburst behaviour

Author

Kendall Ackley, G. Ramsay, D. Mata Sánchez, P. T. O'Brien, L. K. Nuttall, Don Pollacco, V. S. Dhillon, Duncan K. Galloway, K. Noysena, Martin J. Dyer, Krzysztof Ulaczyk, C. Duffy, Danny Steeghs, and J. D. Lyman

Subjects
astro-ph.SR, close [binaries], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, Instability, accretion, surveys, Accretion disc, 0103 physical sciences, ST/T007184/1, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Accretion (meteorology), 010308 nuclear & particles physics, RCUK, Astronomy and Astrophysics, ST/T003103/1, accretion discs, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, dwarf novae [stars]
Abstract

We present results of our analysis of up to 15 years of photometric data from eight AM CVn systems with orbital periods between 22.5 and 26.8 min. Our data has been collected from the GOTO, ZTF, Pan-STARRS, ASAS-SN and Catalina all-sky surveys and amateur observations collated by the AAVSO. We find evidence that these interacting ultra-compact binaries show a similar diversity of long term optical properties as the hydrogen accreting dwarf novae. We found that AM CVn systems in the previously identified accretion disc instability region are not a homogenous group. Various members of the analysed sample exhibit behaviour reminiscent of Z Cam systems with long super outbursts and standstills, SU UMa systems with regular, shorter super outbursts, and nova-like systems which appear only in a high state. The addition of TESS full frame images of one of these systems, KL Dra, reveals the first evidence for normal outbursts appearing as a precursor to super outbursts in an AM CVn system. Our results will inform theoretical modelling of the outbursts of hydrogen deficient systems., Comment: 11 Pages, 7 Figures, 2 Tables. Accepted for publication in MNRAS. Author's final submitted version

Published
2021
Full Text
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9. GRANDMA observations of advanced LIGO's and advanced Virgo's third observational campaign

Author

David Alexander Kann, Bruce Gendre, Tim Dietrich, A. Baransky, N. Ismailov, Christina C. Thöne, Z. Vidadi, Yusufjon Tillayev, Nelson Christensen, V. Vasylenko, P. Gokuldass, Weili Lin, C. Stachie, R. Menard, D. Turpin, Jun Mo, D. Corre, D. Morris, J.-G. Ducoin, A. de Ugarte Postigo, C. Lachaud, H. Crisp, Supachai Awiphan, M. Was, K. Barynova, S. Antier, L. Eymar, G. Marchal-Duval, N. Leroy, N. B. Orange, O. A. Burkhonov, Jie Zhang, R. Rattanamala, M. Serrau, Wenxiong Li, S. Beradze, Sergey Karpov, K. Noysena, M. Boer, X. F. Wang, T. Zhang, Patrice Hello, Mouza Almualla, D. Saint-Gelais, Xinghan Zhang, Heinz-Bernd Eggenstein, Alain Klotz, S. Agayeva, M. Prouza, T. Sadibekova, N. Kochiashvili, Eric Howell, M. Blažek, Martin Mašek, P. A. Duverne, A. Simon, Michael W. Coughlin, Alexis Coleiro, Australian Research Council, Ministerio de Economía y Competitividad (España), European Commission, Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Ministry of Education, Youth and Sports (Czech Republic), Shota Rustaveli National Science Foundation, National Aeronautics and Space Administration (US), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), ANR-18-IDEX-0001,Université de Paris,Université de Paris(2018), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Nice Sophia Antipolis (... - 2019) (UNS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
observational [methods], Binary number, FOS: Physical sciences, Kilonova, 01 natural sciences, Gravitational waves, stars: neutron, neutron [stars], 0103 physical sciences, 010306 general physics, Large distance, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, Astronomy, Astronomy and Astrophysics, Methods observational, LIGO, Neutron star, gravitational waves, Space and Planetary Science, Observational study, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Full list of authors: Antier, S.; Agayeva, S.; Almualla, M.; Awiphan, S.; Baransky, A.; Barynova, K.; Beradze, S.; Blažek, M.; Boër, M.; Burkhonov, O.; Christensen, N.; Coleiro, A.; Corre, D.; Coughlin, M. W.; Crisp, H.; Dietrich, T.; Ducoin, J. -G.; Duverne, P. -A.; Marchal-Duval, G.; Gendre, B.; Gokuldass, P.; Eggenstein, H. B.; Eymar, L.; Hello, P.; Howell, E. J.; Ismailov, N.; Kann, D. A.; Karpov, S.; Klotz, A.; Kochiashvili, N.; Lachaud, C.; Leroy, N.; Lin, W. L.; Li, W. X.; Mašek, M.; Mo, J.; Menard, R.; Morris, D.; Noysena, K.; Orange, N. B.; Prouza, M.; Rattanamala, R.; Sadibekova, T.; Saint-Gelais, D.; Serrau, M.; Simon, A.; Stachie, C.; Thöne, C. C.; Tillayev, Y.; Turpin, D.; de Ugarte Postigo, A.; Vasylenko, V.; Vidadi, Z.; Was, M.; Wang, X. F.; Zhang, J. J.; Zhang, T. M.; Zhang, X. H., GRANDMA (Global Rapid Advanced Network Devoted to the Multi-messenger Addicts) is a network of 25 telescopes of different sizes, including both photometric and spectroscopic facilities. The network aims to coordinate follow-up observations of gravitational-wave (GW) candidate alerts, especially those with large localization uncertainties, to reduce the delay between the initial detection and the optical confirmation. In this paper, we detail GRANDMA's observational performance during Advanced LIGO/Advanced Virgo Observing Run 3 (O3), focusing on the second part of O3; this includes summary statistics pertaining to coverage and possible astrophysical origin of the candidates. To do so, we quantify our observation efficiency in terms of delay between GW candidate trigger time, observations, and the total coverage. Using an optimized and robust coordination system, GRANDMA followed-up about 90 per cent of the GW candidate alerts, that is 49 out of 56 candidates. This led to coverage of over 9000 deg2 during O3. The delay between the GW candidate trigger and the first observation was below 1.5 h for 50 per cent of the alerts. We did not detect any electromagnetic counterparts to the GW candidates during O3, likely due to the very large localization areas (on average thousands of degrees squares) and relatively large distance of the candidates (above 200 Mpc for 60 per cent of binary neutron star, BNS candidates). We derive constraints on potential kilonova properties for two potential BNS coalescences (GW190425 and S200213t), assuming that the events' locations were imaged. © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society., Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through project number CE170100004. EJH acknowledges support from an Australian Research Council DECRA Fellowship (DE170100891). AdUP and CCT acknowledge support from Ramon y Cajal fellowships RyC-2012-09975 and RyC-2012-09984 and the Spanish Ministry of Economy and Competitiveness through project AYA2017-89384-P. DAK acknowledges Spanish research project RTI2018-098104-J-I00 (GRBPhot). MB acknowledges funding as 'personal tecnico de apoyo' under fellowship number PTA2016-13192-I. SA is supported by the CNES Postdoctoral Fellowship at Laboratoire AstroParticule et Cosmologie. SA and CL acknowledge the financial support of the Programme National Hautes Energies (PNHE). DT acknowledges the financial support of CNES postdoctoral program. UBAI acknowledges support from the Ministry of Innovative Development through projects FA-Atech-2018-392 and VA-FA-F-2-010. SB acknowledges Shota Rustaveli National Science Foundation (SRNSF) grant no. -PHDF/18-1327. TAROT has been built with the support of the Institut National des Sciences de l'Univers, CNRS, France. TAROT is funded by the CNES and thanks the help of the technical staff of the Observatoire de Haute Provence, OSUPytheas. MP, SK, and MM are supported by European Structural and Investment Fund and the Czech Ministry of Education, Youth and Sports (Projects CZ.02.1.01/0.0/0.0/16 013/0001402, CZ.02.1.01/0.0/0.0/16 013/0001403, and CZ.02.1.01/0.0/0.0/15 003/0000437). NBO, DM, and PG acknowledge financial support from NASA-MUREP-MIRO grant NNX15AP95A, NASA-EPSCoR grant NNX13AD28A, and NSF EiR AST Award 1901296. The GRANDMA collaboration thank the amateur participants to the kilonova-catcher program. The kilonova-catcher program is supported by the IdEx Universite de Paris, ANR-18-IDEX-0001. This research made use of the crossmatch service provided by CDS, Strasbourg. We thank Ulrich Hopp to provide the precise date of observations for AT2019wxt Wendelstein optical observations.

Published
2020

10. Limits on the Electro-Magnetic Counterpart of Binary Black Hole Coalescence at Visible Wavelengths

Author

R. Laugier, M. Boer, K. Noysena, Alain Klotz, D. Turpin, Siramas Komonjinda, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Chiang Mai University (CMU), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, FOS: Physical sciences, Astrophysics, 01 natural sciences, Binary black hole, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Coalescence (physics), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Large field of view, Gravitational wave, Angular distance, Astronomy and Astrophysics, LIGO, gravitational waves, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data release, stars: black holes, Visible spectrum
Abstract

We used the TAROT network of telescopes to search for the electromagnetic counterparts of GW150914, GW170104 and GW170814, which were reported to originate from binary black hole merger events by the LIGO and Virgo collaborations. Our goal is to constrain the emission from a binary black hole coalescence at visible wavelengths. We developed a simple and effective algorithm to detect new sources by matching the image data with the Gaia catalog data release 1. Machine learning was used and an algorithm was designed to locate unknown sources in a large field of view image. The angular distance between objects in the image and in the catalog was used to find new sources; we then process the candidates to validate them as possible new unknown celestial objects. Though several possible candidates were detected in the three gravitational wave source error boxes studied, none of them were confirmed as a viable counterpart. The algorithm was effective for the identification of unknown candidates in a very large field and provided candidates for GW150914, GW170104 and GW170814. The entire 90\% GW170814 error box was surveyed extensively within 0.6 days after the GW emission resulting in an absolute limiting R magnitude of -23.8. This strong limit excludes to a great extent a possible emission of a gamma-ray burst with an optical counterpart associated with GW170814., Submitted to ApJ, 14 pages, 6 figures

Published
2019

11. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programs

Author

I. Andreoni, K. Ackley, J. Cooke, A. Acharyya, J. R. Allison, G. E. Anderson, M. C. B. Ashley, D. Baade, M. Bailes, K. Bannister, A. Beardsley, M. S. Bessell, F. Bian, P. A. Bland, M. Boer, T. Booler, A. Brandeker, I. S. Brown, D. A. H. Buckley, S.-W. Chang, D. M. Coward, S. Crawford, H. Crisp, B. Crosse, A. Cucchiara, M. Cupák, J. S. de Gois, A. Deller, H. A. R. Devillepoix, D. Dobie, E. Elmer, D. Emrich, W. Farah, T. J. Farrell, T. Franzen, B. M. Gaensler, D. K. Galloway, B. Gendre, T. Giblin, A. Goobar, J. Green, P. J. Hancock, B. A. D. Hartig, E. J. Howell, L. Horsley, A. Hotan, R. M. Howie, L. Hu, Y. Hu, C. W. James, S. Johnston, M. Johnston-Hollitt, D. L. Kaplan, M. Kasliwal, E. F. Keane, D. Kenney, A. Klotz, R. Lau, R. Laugier, E. Lenc, X. Li, E. Liang, C. Lidman, L. C. Luvaul, C. Lynch, B. Ma, D. Macpherson, J. Mao, D. E. McClelland, C. McCully, A. Möller, M. F. Morales, D. Morris, T. Murphy, K. Noysena, C. A. Onken, N. B. Orange, S. Osłowski, D. Pallot, J. Paxman, S. B. Potter, T. Pritchard, W. Raja, R. Ridden-Harper, E. Romero-Colmenero, E. M. Sadler, E. K. Sansom, R. A. Scalzo, B. P. Schmidt, S. M. Scott, N. Seghouani, Z. Shang, R. M. Shannon, L. Shao, M. M. Shara, R. Sharp, M. Sokolowski, J. Sollerman, J. Staff, K. Steele, T. Sun, N. B. Suntzeff, C. Tao, S. Tingay, M. C. Towner, P. Thierry, C. Trott, B. E. Tucker, P. Väisänen, V. Venkatraman Krishnan, M. Walker, L. Wang, X. Wang, R. Wayth, M. Whiting, A. Williams, T. Williams, C. Wolf, C. Wu, X. Wu, J. Yang, X. Yuan, H. Zhang, J. Zhou, H. Zovaro, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Observatoire Midi-Pyrénées ( OMP ), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université Fédérale Toulouse Midi-Pyrénées, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)

Subjects
neutron star: binary, coalescence, velocity, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, gamma-ray burst: individual: GRB170817A, 01 natural sciences, star: binary, stars: neutron, Pulsar, supernovae: general, pulsar: binary, 0103 physical sciences, Binary star, optical, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), radio wave: burst, 010308 nuclear & particles physics, Gravitational wave, Star formation, gravitational radiation, Astronomy, imaging, Astronomy and Astrophysics, star: formation, Light curve, Galaxy, observatory, messenger, Neutron star, electromagnetic, Astrophysics - Solar and Stellar Astrophysics, gravitational waves, Space and Planetary Science, infrared, spectral, Astrophysics::Earth and Planetary Astrophysics, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], supernovae: individual: AT2017gfo
Abstract

The discovery of the first electromagnetic counterpart to a gravitational wave signal has generated follow-up observations by over 50 facilities world-wide, ushering in the new era of multi-messenger astronomy. In this paper, we present follow-up observations of the gravitational wave event GW170817 and its electromagnetic counterpart SSS17a/DLT17ck (IAU label AT2017gfo) by 14 Australian telescopes and partner observatories as part of Australian-based and Australian-led research programs. We report early- to late-time multi-wavelength observations, including optical imaging and spectroscopy, mid-infrared imaging, radio imaging, and searches for fast radio bursts. Our optical spectra reveal that the transient source afterglow cooled from approximately 6400K to 2100K over a 7-day period and produced no significant optical emission lines. The spectral profiles, cooling rate, and photometric light curves are consistent with the expected outburst and subsequent processes of a binary neutron star merger. Star formation in the host galaxy probably ceased at least a Gyr ago, although there is evidence for a galaxy merger. Binary pulsars with short (100 Myr) decay times are therefore unlikely progenitors, but pulsars like PSR B1534+12 with its 2.7 Gyr coalescence time could produce such a merger. The displacement (about 2.2 kpc) of the binary star system from the centre of the main galaxy is not unusual for stars in the host galaxy or stars originating in the merging galaxy, and therefore any constraints on the kick velocity imparted to the progenitor are poor., 26 pages, 9 figures, 15 tables

Published
2017

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