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Your search keyword '"Schultz, A. S. B."' showing total 5 results
Start Over Author "Schultz, A. S. B." Topic astrophysics - astrophysics of galaxies
5 results on '"Schultz, A. S. B."'

1. The Foundation Supernova Survey: Photospheric Velocity Correlations in Type Ia Supernovae

Author

Dettman, Kyle G., Jha, Saurabh W., Dai, Mi, Foley, Ryan J., Rest, Armin, Scolnic, Daniel M., Siebert, Matthew R., Chambers, K. C., Coulter, D. A., Huber, M. E., Johnson, E., Jones, D. O., Kilpatrick, C. D., Kirshner, R. P., Pan, Y. -C., Riess, A. G., and Schultz, A. S. B.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

The ejecta velocities of type-Ia supernovae (SNe Ia), as measured by the Si II $\lambda 6355$ line, have been shown to correlate with other supernova properties, including color and standardized luminosity. We investigate these results using the Foundation Supernova Survey, with a spectroscopic data release presented here, and photometry analyzed with the SALT2 light-curve fitter. We find that the Foundation data do not show significant evidence for an offset in color between SNe Ia with high and normal photospheric velocities, with $\Delta c = 0.005 \pm 0.014$. Our SALT2 analysis does show evidence for redder high-velocity SN Ia in other samples, including objects from the Carnegie Supernova Project, with a combined sample yielding $\Delta c = 0.017 \pm 0.007$. When split on velocity, the Foundation SN Ia also do not show a significant difference in Hubble diagram residual, $\Delta HR = 0.015 \pm 0.049$ mag. Intriguingly, we find that SN Ia ejecta velocity information may be gleaned from photometry, particularly in redder optical bands. For high-redshift SN Ia, these rest-frame red wavelengths will be observed by the Nancy Grace Roman Space Telescope. Our results also confirm previous work that SN Ia host-galaxy stellar mass is strongly correlated with ejecta velocity: high-velocity SN Ia are found nearly exclusively in high-stellar-mass hosts. However, host-galaxy properties alone do not explain velocity-dependent differences in supernova colors and luminosities across samples. Measuring and understanding the connection between intrinsic explosion properties and supernova environments, across cosmic time, will be important for precision cosmology with SNe Ia., Comment: Submitted to AAS Journals

Published
2021
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2. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv

Author

Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, M., Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, T. -W., Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F. I., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., González-Fernández, C., González-Gaitán, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutiérrez, C. P., Heikkilä, T., Heintz, K. E., Hjorth, J., Hu, Y. -D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, A., Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, E. C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michałowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Guelbenzu, A. Nicuesa, Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vásquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, S., Sabha, N. B., Carracedo, A. Sagués, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, T., Smartt, S. J., Smith, K. W., Smith, M., Sollerman, J., Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, S., Yi, S. -X., and Young, D. R.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. Preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope (ENGRAVE) collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical/near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS and VINROUGE projects also carried out a search on this event. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN) possibly generated by this NS-BH merger, and for the strategy of future searches. Altogether, our observations allow us to exclude a KN with large ejecta mass $M\gtrsim 0.1\,\mathrm{M_\odot}$ to a high ($>90\%$) confidence, and we can exclude much smaller masses in a subsample of our observations. This disfavours the tidal disruption of the neutron star during the merger. Despite the sensitive instruments involved in the campaign, given the distance of S190814bv we could not reach sufficiently deep limits to constrain a KN comparable in luminosity to AT 2017gfo on a large fraction of the localisation probability. This suggests that future (likely common) events at a few hundreds Mpc will be detected only by large facilities with both high sensitivity and large field of view. Galaxy-targeted observations can reach the needed depth over a relevant portion of the localisation probability with a smaller investment of resources, but the number of galaxies to be targeted in order to get a fairly complete coverage is large, even in the case of a localisation as good as that of this event., Comment: 52 pages, revised version now accepted for publication in A&A. Abstract abridged to meet arXiv requirements

Published
2020
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3. Should Type Ia Supernova Distances be Corrected for their Local Environments?

Author

Jones, D. O., Riess, A. G., Scolnic, D. M., Pan, Y. -C., Johnson, E., Coulter, D. A., Dettman, K. G., Foley, M. M., Foley, R. J., Huber, M. E., Jha, S. W., Kilpatrick, C. D., Kirshner, R. P., Rest, A., Schultz, A. S. B., and Siebert, M. R.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Recent analyses suggest that distance residuals measured from Type Ia supernovae (SNe Ia) are correlated with local host galaxy properties within a few kpc of the SN explosion. However, the well-established correlation with global host galaxy properties is nearly as significant, with a shift of 0.06 mag across a low to high mass boundary (the mass step). Here, with 273 SNe Ia at $z<0.1$, we investigate whether stellar masses and rest-frame $u-g$ colors of regions within 1.5 kpc of the SN Ia explosion site are significantly better correlated with SN distance measurements than global properties or properties measured at random locations in SN hosts. At $\lesssim2\sigma$ significance, local properties tend to correlate with distance residuals better than properties at random locations, though despite using the largest low-$z$ sample to date we cannot definitively prove that a local correlation is more significant than a random correlation. Our data hint that SNe observed by surveys that do not target a pre-selected set of galaxies may have a larger local mass step than SNe from surveys that do, an increase of $0.071\pm0.036$ mag (2.0$\sigma$). We find a $3\sigma$ local mass step after global mass correction, evidence that SNe Ia should be corrected for their local mass, but we note that this effect is insignificant in the targeted low-$z$ sample. Only the local mass step remains significant at $>2\sigma$ after global mass correction, and we conservatively estimate a systematic shift in H$_0$ measurements of -0.14 $\textrm{km}\,\textrm{s}^{-1}\textrm{Mpc}^{-1}$ with an additional uncertainty of 0.14 $\textrm{km}\,\textrm{s}^{-1}\textrm{Mpc}^{-1}$, $\sim$10\% of the present uncertainty., Comment: Accepted for publication in ApJ

Published
2018
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4. The Pan-STARRS1 Surveys

Author

Chambers, K. C., Magnier, E. A., Metcalfe, N., Flewelling, H. A., Huber, M. E., Waters, C. Z., Denneau, L., Draper, P. W., Farrow, D., Finkbeiner, D. P., Holmberg, C., Koppenhoefer, J., Price, P. A., Rest, A., Saglia, R. P., Schlafly, E. F., Smartt, S. J., Sweeney, W., Wainscoat, R. J., Burgett, W. S., Chastel, S., Grav, T., Heasley, J. N., Hodapp, K. W., Jedicke, R., Kaiser, N., Kudritzki, R. -P., Luppino, G. A., Lupton, R. H., Monet, D. G., Morgan, J. S., Onaka, P. M., Shiao, B., Stubbs, C. W., Tonry, J. L., White, R., Bañados, E., Bell, E. F., Bender, R., Bernard, E. J., Boegner, M., Boffi, F., Botticella, M. T., Calamida, A., Casertano, S., Chen, W. -P., Chen, X., Cole, S., Deacon, N., Frenk, C., Fitzsimmons, A., Gezari, S., Gibbs, V., Goessl, C., Goggia, T., Gourgue, R., Goldman, B., Grant, P., Grebel, E. K., Hambly, N. C., Hasinger, G., Heavens, A. F., Heckman, T. M., Henderson, R., Henning, T., Holman, M., Hopp, U., Ip, W. -H., Isani, S., Jackson, M., Keyes, C. D., Koekemoer, A. M., Kotak, R., Le, D., Liska, D., Long, K. S., Lucey, J. R., Liu, M., Martin, N. F., Masci, G., McLean, B., Mindel, E., Misra, P., Morganson, E., Murphy, D. N. A., Obaika, A., Narayan, G., Nieto-Santisteban, M. A., Norberg, P., Peacock, J. A., Pier, E. A., Postman, M., Primak, N., Rae, C., Rai, A., Riess, A., Riffeser, A., Rix, H. W., Röser, S., Russel, R., Rutz, L., Schilbach, E., Schultz, A. S. B., Scolnic, D., Strolger, L., Szalay, A., Seitz, S., Small, E., Smith, K. W., Soderblom, D. R., Taylor, P., Thomson, R., Taylor, A. N., Thakar, A. R., Thiel, J., Thilker, D., Unger, D., Urata, Y., Valenti, J., Wagner, J., Walder, T., Walter, F., Watters, S. P., Werner, S., Wood-Vasey, W. M., and Wyse, R.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Pan-STARRS1 has carried out a set of distinct synoptic imaging sky surveys including the $3\pi$ Steradian Survey and the Medium Deep Survey in 5 bands ($grizy_{P1}$). The mean 5$\sigma$ point source limiting sensitivities in the stacked 3$\pi$ Steradian Survey in $grizy_{P1}$ are (23.3, 23.2, 23.1, 22.3, 21.4) respectively. The upper bound on the systematic uncertainty in the photometric calibration across the sky is 7-12 millimag depending on the bandpass. The systematic uncertainty of the astrometric calibration using the Gaia frame comes from a comparison of the results with Gaia: the standard deviation of the mean and median residuals ($ \Delta ra, \Delta dec $) are (2.3, 1.7) milliarcsec, and (3.1, 4.8) milliarcsec respectively. The Pan-STARRS system and the design of the PS1 surveys are described and an overview of the resulting image and catalog data products and their basic characteristics are described together with a summary of important results. The images, reduced data products, and derived data products from the Pan-STARRS1 surveys are available to the community from the Mikulski Archive for Space Telescopes (MAST) at STScI., Comment: 38 pages, 29 figures, 12 tables

Published
2016

5. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv

Author

F. D'Ammando, Mattia Bulla, A. Fiore, P. T. O'Brien, Patricia Schady, T. Heikkilä, Matt Nicholl, Giorgos Leloudas, K. C. Chambers, Luciano Nicastro, Riccardo Ciolfi, Michela Mapelli, Armin Rest, R. Cutter, Tassilo Schweyer, J. Gillanders, G. De Cesare, Lorenzo Amati, L. Nuttal, Lána Salmon, Nancy Elias-Rosa, O. McBrien, A. Grado, David Alexander Kann, Ruben Salvaterra, P. D'Avanzo, M. T. Botticella, Johan P. U. Fynbo, M. G. Bernardini, Francesco Longo, Danny Steeghs, S. X. Yi, Peter G. Jonker, Eliana Palazzi, Y. D. Hu, Zhi-Ping Jin, Seppo Mattila, A. Gomboc, G. Ghirlanda, Alexis Coleiro, Sylvain Chaty, S. Yang, Elizabeth R. Stanway, D. R. Young, Rubina Kotak, Luca Izzo, Franz E. Bauer, Massimo Turatto, Christa Gall, A. Melandri, Eric Thrane, S. R. Oates, Francesca Onori, S. Srivastav, M. Branchesi, Michael S. Smith, Christopher W. Stubbs, Vincenzo Testa, Anders Jerkstrand, J. Japelj, Carlos González-Fernández, Elena Pian, Lluís Galbany, Luca Sbordone, Enrico Cappellaro, A. Possenti, Paul J. Groot, S. Rosetti, L. Denneau, Mark Kennedy, Jesper Sollerman, Klaas Wiersema, Chris M. Copperwheat, Cosimo Inserra, Kasper E. Heintz, E. C. Kool, M. de Pasquale, G. Greco, Krzysztof Ulaczyk, Daniel A. Perley, Om Sharan Salafia, Eugene A. Magnier, T. M. Reynolds, Andrew J. Levan, A. J. van der Horst, G. Stratta, B. Milvang-Jensen, Erkki Kankare, Darach Watson, B. Patricelli, N. B. Sabha, T. W. Chen, Kendall Ackley, Maria Letizia Pumo, Nial R. Tanvir, P. A. Evans, Michał J. Michałowski, S. Klose, R. L. C. Starling, A. J. Castro-Tirado, Sandra Savaglio, J. Quirola-Vásquez, Martin J. Dyer, Pietro Schipani, K. W. Smith, Lukasz Wyrzykowski, M. Della Valle, G. Pignata, S. D. Vergani, Jens Hjorth, A. S. B. Schultz, Mariusz Gromadzki, Saran Poshyachinda, Santiago González-Gaitán, Eugenio Maiorano, D. K. Galloway, Cesare Barbieri, V. D'Elia, Andrea Rossi, G. Ramsay, Seung-Lee Kim, Kornpob Bhirombhakdi, V. S. Dhillon, Enzo Brocato, Ilya Mandel, S. Benetti, J. D. Lyman, Sergio Campana, Fedor Getman, A. Sagués Carracedo, Kate Maguire, Arne Rau, A. S. Fruchter, John L. Tonry, B. P. Gompertz, Hanindyo Kuncarayakti, Kaj Wiik, Morgan Fraser, N. A. Walton, Stephan Rosswog, M. A.P. Torres, Claudia P. Gutiérrez, F. Ragosta, S. Piranomonte, A. Nicuesa Guelbenzu, S. H. Bruun, T. B. Lowe, M. E. Huber, S. J. Smartt, Gavin P. Lamb, S. Moran, Albino Perego, R. Eyles-Ferris, Stefano Covino, Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), Istituto Nazionale di Fisica Nucleare (INFN), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), 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), Departamento de Astronomía y Astrofísica [Santiago], Pontificia Universidad Católica de Chile (UC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universitá degli Studi dell’Insubria = University of Insubria [Varese] (Uninsubria), Ecole Polytechnique Fédérale de Lausanne (EPFL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, University of Sheffield [Sheffield], COBRA Research Institute, Eindhoven University of Technology, Aberystwyth University, AUTRES, Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Department of Physics [Pittsburgh], Carnegie Mellon University [Pittsburgh] (CMU), United States Geological Survey [Reston] (USGS), Faculty of Mathematics and Physics [Ljubljana] (FMF), University of Ljubljana, Department of Physics [Denver], University of Colorado [Denver], Laboratoire d'Acoustique de l'Université du Mans (LAUM), Le Mans Université (UM)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Oskar Klein Centre [Stockholm], Stockholm University, SRON Netherlands Institute for Space Research (SRON), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Institut Lavoisier de Versailles (ILV), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Scottish Universities Physics Alliance, Institute for Astronomy (SUPA), University of Edinburgh, Department of Agricultural and Environmental Sciences – Production, Landscape, Agroenergy, Università degli Studi di Milano = University of Milan (UNIMI), Universidad Nacional de Entre Ríos [Argentine] (UNER), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Roma (OAR), INAF - Osservatorio Astronomico di Cagliari (OAC), Max-Planck-Institut für Extraterrestrische Physik (MPE), Bioénergétique fondamentale et appliquée, Université Joseph Fourier - Grenoble 1 (UJF)-Institut National de la Santé et de la Recherche Médicale (INSERM), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), University College Dublin [Dublin] (UCD), INAF-IASF Milano, Università della Calabria [Arcavacata di Rende] (Unical), INAF - Osservatorio Astronomico di Capodimonte (OAC), Woods Hole Oceanographic Institution (WHOI), National Institute of Water and Atmospheric Research [Wellington] (NIWA), Centre d'étude spatiale des rayonnements (CESR), 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), University of Minnesota System, INAF - Osservatorio Astronomico di Padova (OAPD), Astronomical Observatory [Warsaw], Faculty of Physics [Warsaw] (FUW), University of Warsaw (UW)-University of Warsaw (UW), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Department of Physics and Astronomy [Leicester], University of Leicester, UniVersity, Nano Science and Technology Program, Department of Chemistry, The Hong Kong UniVersity of Science and Technology, Clear Water Bay, Kowloon, Hong Kong, Hong Kong University of Science and Technology (HKUST), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universitá degli Studi dell’Insubria, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], University of Milan, Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, M., Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, T. -W., Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F. I., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., Gonzalez-Fernandez, C., Gonzalez-Gaitan, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutierrez, C. P., Heikkila, T., Heintz, K. E., Hjorth, J., Hu, Y. -D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, A., Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, E. C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., Mcbrien, O. R., Melandri, A., Michalowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Nicuesa Guelbenzu, A., Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vasquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, S., Sabha, N. B., Sagues Carracedo, A., Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, T., Smartt, S. J., Smith, K. W., Smith, M., Sollerman, J., Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., Van Der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, S., Yi, S. -X., Young, D. R., National Aeronautics and Space Administration (US), University of Hawaii, Queen's University Belfast, Space Telescope Science Institute (US), National Research Foundation (South Africa), National Astronomical Research Institute of Thailand, University of Portsmouth, Instituto de Astrofísica de Canarias, Science and Technology Facilities Council (UK), Ministerio de Economía, Fomento y Turismo (Chile), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Danish National Research Foundation, Alexander von Humboldt Foundation, Villum Fonden, Fundação para a Ciência e a Tecnologia (Portugal), Polish National Agency for Academic Exchange, Centre National de la Recherche Scientifique (CNRS)-Le Mans Université (UM), 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)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Low Energy Astrophysics (API, FNWI), and API Other Research (FNWI)

Subjects
Astronomy, ELECTROMAGNETIC COUNTERPARTS, Supernovae: general, general [Supernovae], Binary number, Astrophysics, 7. Clean energy, 01 natural sciences, GW170817, neutron, Supernovae: general [Gravitational waves, Stars], 010303 astronomy & astrophysics, QC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, [PHYS]Physics [physics], HAWK-I, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], EJECTA, Astrophysics - Solar and Stellar Astrophysics, GRAVITATIONAL-WAVE SOURCE, ST/P000495/1, Space Science, Astrophysics - High Energy Astrophysical Phenomena, Gravitational wave, astro-ph.SR, astro-ph.GA, FOS: Physical sciences, Context (language use), MASS, NO, GAMMA-RAY BURST, Gravitational waves, 0103 physical sciences, ST/T007184/1, Solar and Stellar Astrophysics (astro-ph.SR), STFC, 010308 nuclear & particles physics, Near-infrared spectroscopy, KILONOVA, RCUK, Stars: neutron, Astronomy and Astrophysics, neutron [Stars], R-PROCESS NUCLEOSYNTHESIS, Astrophysics - Astrophysics of Galaxies, EVOLUTION, Black hole, Neutron star, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), ST/P000312/1, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gravitational waves, Stars: neutron, Supernovae: general
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.--Full list of authors: Ackley, K.; Amati, L.; Barbieri, C.; Bauer, F. E.; Benetti, S.; Bernardini, M. G.; Bhirombhakdi, K.; Botticella, M. T.; Branchesi, M.; Brocato, E.; Bruun, S. H.; Bulla, M.; Campana, S.; Cappellaro, E.; Castro-Tirado, A. J.; Chambers, K. C.; Chaty, S.; Chen, T. -W.; Ciolfi, R.; Coleiro, A.; Copperwheat, C. M.; Covino, S.; Cutter, R.; D'Ammando, F.; D'Avanzo, P.; De Cesare, G.; D'Elia, V.; Della Valle, M.; Denneau, L.; De Pasquale, M.; Dhillon, V. S.; Dyer, M. J.; Elias-Rosa, N.; Evans, P. A.; Eyles-Ferris, R. A. J.; Fiore, A.; Fraser, M.; Fruchter, A. S.; Fynbo, J. P. U.; Galbany, L.; Gall, C.; Galloway, D. K.; Getman, F. I.; Ghirlanda, G.; Gillanders, J. H.; Gomboc, A.; Gompertz, B. P.; González-Fernández, C.; González-Gaitán, S.; Grado, A.; Greco, G.; Gromadzki, M.; Groot, P. J.; Gutiérrez, C. P.; Heikkilä, T.; Heintz, K. E.; Hjorth, J.; Hu, Y. -D.; Huber, M. E.; Inserra, C.; Izzo, L.; Japelj, J.; Jerkstrand, A.; Jin, Z. P.; Jonker, P. G.; Kankare, E.; Kann, D. A.; Kennedy, M.; Kim, S.; Klose, S.; Kool, E. C.; Kotak, R.; Kuncarayakti, H.; Lamb, G. P.; Leloudas, G.; Levan, A. J.; Longo, F.; Lowe, T. B.; Lyman, J. D.; Magnier, E.; Maguire, K.; Maiorano, E.; Mandel, I.; Mapelli, M.; Mattila, S.; McBrien, O. R.; Melandri, A.; Michałowski, M. J.; Milvang-Jensen, B.; Moran, S.; Nicastro, L.; Nicholl, M.; Nicuesa Guelbenzu, A.; Nuttal, L.; Oates, S. R.; O'Brien, P. T.; Onori, F.; Palazzi, E.; Patricelli, B.; Perego, A.; Torres, M. A. P.; Perley, D. A.; Pian, E.; Pignata, G.; Piranomonte, S.; Poshyachinda, S.; Possenti, A.; Pumo, M. L.; Quirola-Vásquez, J.; Ragosta, F.; Ramsay, G.; Rau, A.; Rest, A.; Reynolds, T. M.; Rosetti, S. S.; Rossi, A.; Rosswog, S.; Sabha, N. B.; Sagués Carracedo, A.; Salafia, O. S.; Salmon, L.; Salvaterra, R.; Savaglio, S.; Sbordone, L.; Schady, P.; Schipani, P.; Schultz, A. S. B.; Schweyer, T.; Smartt, S. J.; Smith, K. W.; Smith, M.; Sollerman, J.; Srivastav, S.; Stanway, E. R.; Starling, R. L. C.; Steeghs, D.; Stratta, G.; Stubbs, C. W.; Tanvir, N. R.; Testa, V.; Thrane, E.; Tonry, J. L.; Turatto, M.; Ulaczyk, K.; van der Horst, A. J.; Vergani, S. D.; Walton, N. A.; Watson, D.; Wiersema, K.; Wiik, K.; Wyrzykowski, Ł.; Yang, S.; Yi, S. -X.; Young, D. R., Context. Gravitational wave (GW) astronomy has rapidly reached maturity, becoming a fundamental observing window for modern astrophysics. The coalescences of a few tens of black hole (BH) binaries have been detected, while the number of events possibly including a neutron star (NS) is still limited to a few. On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. A preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. Aims. In this paper, we present our extensive search campaign aimed at uncovering the potential optical and near infrared electromagnetic counterpart of S190814bv. We found no convincing electromagnetic counterpart in our data. We therefore use our non-detection to place limits on the properties of the putative outflows that could have been produced by the binary during and after the merger. Methods. Thanks to the three-detector observation of S190814bv, and given the characteristics of the signal, the LIGO and Virgo Collaborations delivered a relatively narrow localisation in low latency - a 50% (90%) credible area of 5 deg2 (23 deg2) - despite the relatively large distance of 267 ± 52 Mpc. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical and near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS, and VINROUGE projects also carried out a search on this event. In this paper, we describe the combined observational campaign of these groups. Results. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN), which was possibly generated by this NS-BH merger, and for the strategy of future searches. The typical depth of our wide-field observations, which cover most of the projected sky localisation probability (up to 99.8%, depending on the night and filter considered), is r ∼ 22 (resp. K ∼ 21) in the optical (resp. near infrared). We reach deeper limits in a subset of our galaxy-targeted observations, which cover a total ∼50% of the galaxy-mass-weighted localisation probability. Altogether, our observations allow us to exclude a KN with large ejecta mass M 0.1 M- to a high (> 90%) confidence, and we can exclude much smaller masses in a sub-sample of our observations. This disfavours the tidal disruption of the neutron star during the merger. Conclusions. Despite the sensitive instruments involved in the campaign, given the distance of S190814bv, we could not reach sufficiently deep limits to constrain a KN comparable in luminosity to AT 2017gfo on a large fraction of the localisation probability. This suggests that future (likely common) events at a few hundred megaparsecs will be detected only by large facilities with both a high sensitivity and large field of view. Galaxy-targeted observations can reach the needed depth over a relevant portion of the localisation probability with a smaller investment of resources, but the number of galaxies to be targeted in order to get a fairly complete coverage is large, even in the case of a localisation as good as that of this event. © K. Ackley et al. 2020., Based on observations collected at the European Southern Observatory under ESO programmes 1102.D-0353(E), 1102.D0353(F), 1102.D-0353(Q), 1102.D-0353(G), 0103.D-0070(A), 0103.D-0070(B), 0103.D-0703(A), 0103.D-0722(A), 0103.A-9099(A), 198.D-2010(D) and 60.A9285(A). ATLAS is primarily funded through NEO NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575. The ATLAS science products have been made possible through the contributions of the University of Hawaii IfA, the Queen's University Belfast, the Space Telescope Science Institute, and the South African Astronomical Observatory. PanSTARRS is primarily funded through NEO NASA grants NASA Grants NNX08AR22G, NNX14AM74G. The PanSTARRS science products for LIGO-Virgo follow-up are made possible through the contributions of the University of Hawaii IfA and the Queen's University Belfast. The Gravitational-wave Optical Transient Observer (GOTO) project acknowledges the support of the Monash-Warwick Alliance; Warwick University; Monash University; She ffield University; Leicester University; Armagh Observatory & Planetarium; the National Astronomical Research Institute of Thailand (NARIT); University of Portsmouth; Turku University and the Instituto de Astrofisica de Canarias (IAC). Part of the funding for GROND was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The WHT and its override programme are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; part of these data were taken under program (19A)N3. FEB thanks CONICYT Basal AFB-170002 and Chile's Ministry of Economy fund IC120009. MGB, PDA and AM acknowledge support from ASI grant I/004/11/3. MBr, EC, AP and SPi acknowledge support from MIUR (PRIN 2017 grant 20179ZF5KS). EB, EM and MT acknowledge funding from GRAWITA. SHB is indebted to the Danish National Research Foundation (DNRF132) for support. SCa acknowledges support from grant MAE0065741. EC acknowledges the support of the H2020 OPTICON programme 730890. TWC acknowledges the Humboldt Foundation and Marie Sklodowska-Curie grant 842471. MDP thanks Istanbul University for support. PAE acknowledges UKSA support. RAJEF is supported by an STFC studentship. MF is supported by a Royal Society -SFI University Research Fellowship. LG was funded by the EU H2020 programme under MSCA grant no. 839090. CG, JH and LI were supported by a research grant from VILLUM FONDEN (project 16599). CG and LI were supported by a research grant from VILLUM FONDEN (25501). GGh acknowledges the PRIN MIUR "Figaro" for financial support. AGo acknowledges financial support from the Slovenian Research Agency (grants P1-0031, I0-0033, and J1-8136). BPG, AJL and JDL acknowledge support from ERC grant 725246 (TEDE, PI Levan). SGG acknowledges support by FCT Fundacao para a Ciencia e Tecnologia and by Project PTDC/FIS-AST-31546. GGr acknowledges the ESCAPE H2020 project no. 824064. MG is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. PJG acknowledges support from NOVA and from the South African NRF SARChI grant 111692. CPG and MS acknowledge support from EU/FP7-ERC grant no. 615929. KEH acknowledges support by a Project Grant from The Icelandic Research Fund. YDH acknowledges support from the China Scholarships Council. JJ acknowledges support from NOVA and NWO-FAPESP grant for instrumentation. AJ acknowledges funding from the European Research Council (ERC). ZPJ was supported by the Foundation for Distinguished Young Scholars of Jiangsu Province (no. BK20180050). PGJ acknowledges funding from the ERC under Consolidator Grant agreement no. 647208. DAK acknowledges Spanish research project RTI2018-098104-J-I00 (GRBPhot). SKl acknowledges support by DFG grant Kl 766/16-3. ECK acknowledges support from the GREAT research environment. GPL acknowledges support from STFC via grant ST/N000757/1. GL was supported by a research grant (19054) from VILLUM FONDEN. KM acknowledges support from the ERC (grant no. 758638). IM is partially supported by OzGrav (ARC project CE17010000). MMacknowledges support from ERC through ERC-2017-CoG no. 770017. MJM acknowledges the National Science Centre, Poland, grant 2018/30/E/ST9/00208. BMJ and DW are supported by Independent Research Fund Denmark grant DFF-7014-00017. MN is supported by a Royal Astronomical Society Research Fellowship. ANG acknowledges support by grant DFG Kl 766/16-3. PTOB acknowledges funding from STFC. SRO gratefully acknowledges the support of the Leverhulme Trust. FO acknowledges the support of the H2020 Hemera program, grant no. 730970. MAPT was supported by grants RYC-2015-17854 and AYA201783216-P. EP aknowledges financial support from INAF. GP is supported by the Millennium Science Initiative through grant IC120009. MLP is partially supported by a "Linea 2" project of the Catania University. JQV acknowledges support from CONICYT folio 21180886. TMR acknowledges the support of the Vilho, Yrjo and Kalle Vaisala Foundation. ARo acknowledges support from Premiale LBT 2013. SR is supported by VR grants 2016-03657_3 and the research environment grant GREAT, Dnr. 2016-06012, and the Swedish National Space board, Dnr. 107/16. OSS acknowledges the Italian Ministry of Research (MIUR) grant 1.05.06.13. LSa acknowledges the Irish Research Council Scholarship no. GOIPG/2017/1525. SJS acknowledges support from STFC Grant ST/P000312/1. ERS and DS acknowledge funding from UK STFC CG ST/P000495/1. RLCS acknowledges funding from STFC. DS acknowledges support from STFC via grant ST/T007184/1. SDV acknowledges the support of the CNES. LWsupported by Polish NCN DAINA 2017/27/L/ST9/03221. The Cosmic DAWN center is funded by the Danish National Research Foundation.

Published
2020
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