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Author

Christoffer Fremling

Other affiliations: Stockholm University
Bio: Christoffer Fremling is an academic researcher from California Institute of Technology. The author has contributed to research in topics: Supernova & Light curve. The author has an hindex of 49, co-authored 228 publications receiving 8492 citations. Previous affiliations of Christoffer Fremling include Stockholm University.
Topics: Supernova, Light curve, Physics, Galaxy, Luminosity

Papers published on a yearly basis

Papers
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Journal ArticleDOI
Eric C. Bellm1, Shrinivas R. Kulkarni2, Matthew J. Graham2, Richard Dekany2, Roger M. H. Smith2, Reed Riddle2, Frank J. Masci2, George Helou2, Thomas A. Prince2, Scott M. Adams2, Cristina Barbarino3, Tom A. Barlow2, James Bauer4, Ron Beck2, Justin Belicki2, Rahul Biswas3, Nadejda Blagorodnova2, Dennis Bodewits4, Bryce Bolin1, V. Brinnel5, Tim Brooke2, Brian D. Bue2, Mattia Bulla3, Rick Burruss2, S. Bradley Cenko6, S. Bradley Cenko4, Chan-Kao Chang7, Andrew J. Connolly1, Michael W. Coughlin2, John Cromer2, Virginia Cunningham4, Kaushik De2, Alex Delacroix2, Vandana Desai2, Dmitry A. Duev2, Gwendolyn Eadie1, Tony L. Farnham4, Michael Feeney2, Ulrich Feindt3, David Flynn2, Anna Franckowiak, Sara Frederick4, Christoffer Fremling2, Avishay Gal-Yam8, Suvi Gezari4, Matteo Giomi5, Daniel A. Goldstein2, V. Zach Golkhou1, Ariel Goobar3, Steven Groom2, Eugean Hacopians2, David Hale2, John Henning2, Anna Y. Q. Ho2, David Hover2, Justin Howell2, Tiara Hung4, Daniela Huppenkothen1, David Imel2, Wing-Huen Ip7, Wing-Huen Ip9, Željko Ivezić1, Edward Jackson2, Lynne Jones1, Mario Juric1, Mansi M. Kasliwal2, Shai Kaspi10, Stephen Kaye2, Michael S. P. Kelley4, Marek Kowalski5, Emily Kramer2, Thomas Kupfer11, Thomas Kupfer2, Walter Landry2, Russ R. Laher2, Chien De Lee7, Hsing Wen Lin7, Hsing Wen Lin12, Zhong-Yi Lin7, Ragnhild Lunnan3, Ashish Mahabal2, Peter H. Mao2, Adam A. Miller13, Adam A. Miller14, Serge Monkewitz2, Patrick J. Murphy2, Chow-Choong Ngeow7, Jakob Nordin5, Peter Nugent15, Peter Nugent16, Eran O. Ofek8, Maria T. Patterson1, Bryan E. Penprase17, Michael Porter2, L. Rauch, Umaa Rebbapragada2, Daniel J. Reiley2, Mickael Rigault18, Hector P. Rodriguez2, Jan van Roestel19, Ben Rusholme2, J. V. Santen, Steve Schulze8, David L. Shupe2, Leo Singer6, Leo Singer4, Maayane T. Soumagnac8, Robert Stein, Jason Surace2, Jesper Sollerman3, Paula Szkody1, Francesco Taddia3, Scott Terek2, Angela Van Sistine20, Sjoert van Velzen4, W. Thomas Vestrand21, Richard Walters2, Charlotte Ward4, Quanzhi Ye2, Po-Chieh Yu7, Lin Yan2, Jeffry Zolkower2 
TL;DR: The Zwicky Transient Facility (ZTF) as mentioned in this paper is a new optical time-domain survey that uses the Palomar 48 inch Schmidt telescope, which provides a 47 deg^2 field of view and 8 s readout time, yielding more than an order of magnitude improvement in survey speed relative to its predecessor survey.
Abstract: The Zwicky Transient Facility (ZTF) is a new optical time-domain survey that uses the Palomar 48 inch Schmidt telescope. A custom-built wide-field camera provides a 47 deg^2 field of view and 8 s readout time, yielding more than an order of magnitude improvement in survey speed relative to its predecessor survey, the Palomar Transient Factory. We describe the design and implementation of the camera and observing system. The ZTF data system at the Infrared Processing and Analysis Center provides near-real-time reduction to identify moving and varying objects. We outline the analysis pipelines, data products, and associated archive. Finally, we present on-sky performance analysis and first scientific results from commissioning and the early survey. ZTF's public alert stream will serve as a useful precursor for that of the Large Synoptic Survey Telescope.

1,009 citations

Journal ArticleDOI
Mansi M. Kasliwal1, Ehud Nakar2, Leo Singer3, Leo Singer4, David L. Kaplan5, David O. Cook1, A. Van Sistine5, R. M. Lau1, Christoffer Fremling1, Ore Gottlieb2, Jacob E. Jencson1, Scott M. Adams1, U. Feindt6, Kenta Hotokezaka7, Sourav Ghosh5, Daniel A. Perley8, Po-Chieh Yu9, Tsvi Piran10, James R. Allison11, James R. Allison12, G. C. Anupama13, Arvind Balasubramanian14, Keith W. Bannister15, John Bally16, Jennifer Barnes17, Sudhanshu Barway, Eric C. Bellm18, Varun Bhalerao19, Deb Sankar Bhattacharya20, Nadejda Blagorodnova1, Joshua S. Bloom21, Joshua S. Bloom22, Patrick Brady5, Chris Cannella1, Deep Chatterjee5, S. B. Cenko4, S. B. Cenko3, B. E. Cobb23, Chris M. Copperwheat8, A. Corsi24, Kaushik De1, Dougal Dobie12, Dougal Dobie11, Dougal Dobie15, S. W. K. Emery25, Phil Evans26, Ori D. Fox27, Dale A. Frail28, C. Frohmaier29, C. Frohmaier30, Ariel Goobar6, Gregg Hallinan1, Fiona A. Harrison1, George Helou1, Tanja Hinderer31, Anna Y. Q. Ho1, Assaf Horesh10, Wing-Huen Ip7, Ryosuke Itoh32, Daniel Kasen22, Hyesook Kim, N. P. M. Kuin25, Thomas Kupfer1, Christene Lynch11, Christene Lynch12, K. K. Madsen1, Paolo A. Mazzali8, Paolo A. Mazzali33, Adam A. Miller34, Adam A. Miller35, Kunal Mooley36, Tara Murphy11, Tara Murphy12, Chow-Choong Ngeow9, David A. Nichols31, Samaya Nissanke31, Peter Nugent22, Peter Nugent21, Eran O. Ofek37, H. Qi5, Robert M. Quimby38, Robert M. Quimby39, Stephan Rosswog6, Florin Rusu40, Elaine M. Sadler12, Elaine M. Sadler11, Patricia Schmidt31, Jesper Sollerman6, Iain A. Steele8, A. R. Williamson31, Y. Xu1, Lin Yan1, Yoichi Yatsu32, C. Zhang5, Weijie Zhao40 
22 Dec 2017-Science
TL;DR: It is demonstrated that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis, which is dissimilar to classical short gamma-ray bursts with ultrarelativistic jets.
Abstract: Merging neutron stars offer an excellent laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) with gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic data set, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultrarelativistic jets. Instead, we suggest that breakout of a wide-angle, mildly relativistic cocoon engulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infrared, and the delayed radio and x-ray emission. We posit that all neutron star mergers may lead to a wide-angle cocoon breakout, sometimes accompanied by a successful jet and sometimes by a choked jet.

579 citations

Journal ArticleDOI
Matthew J. Graham, Shrinivas R. Kulkarni, Eric C. Bellm, Scott M. Adams, Cristina Barbarino, Nadejda Blagorodnova, Dennis Bodewits, Bryce Bolin, Patrick Brady, S. Bradley Cenko, Chan-Kao Chang, Michael W. Coughlin, Kaushik De, Gwendolyn Eadie, Tony L. Farnham, Ulrich Feindt, Anna Franckowiak, Christoffer Fremling, Avishay Gal-Yam, Suvi Gezari, Sourav Ghosh, Daniel A. Goldstein, V. Zach Golkhou, Ariel Goobar, Anna Y. Q. Ho, Daniela Huppenkothen, Zeljko Ivezic, R. Lynne Jones, Mario Juric, David L. Kaplan, Mansi M. Kasliwal, Michael S. P. Kelley, Thomas Kupfer, Chien-De Lee, Hsing Wen Lin, Ragnhild Lunnan, Ashish Mahabal, Adam A. Miller, Chow-Choong Ngeow, Peter Nugent, Eran O. Ofek, Thomas A. Prince, L. Rauch, Jan van Roestel, Steve Schulze, Leo Singer, Jesper Sollerman, Francesco Taddia, Lin Yan, Quanzhi Ye, Po-Chieh Yu, Igor Andreoni, Tom A. Barlow, James M. Bauer, Ron Beck, Justin Belicki, Rahul Biswas, V. Brinnel, Tim Brooke, Brian D. Bue, Mattia Bulla, Kevin B. Burdge, Rick Burruss, Andrew J. Connolly, John Cromer, Virginia Cunningham, Richard Dekany, Alex Delacroix, Vandana Desai, Dmitry A. Duev, Eugean Hacopians, David Hale, George Helou, John Henning, David Hover, Lynne A. Hillenbrand, Justin Howell, Tiara Hung, David Imel, Wing-Huen Ip, Edward Jackson, Shai Kaspi, Stephen Kaye, Marek Kowalski, Emily Kramer, Michael A. Kuhn, Walter Landry, Russ R. Laher, Peter H. Mao, Frank J. Masci, Serge Monkewitz, Patrick J. Murphy, J. Nordin, Maria T. Patterson, Bryan E. Penprase, Michael Porter, Umaa Rebbapragada, Daniel J. Reiley, Reed Riddle, Mickael Rigault, Hector P. Rodriguez, Ben Rusholme, J. V. Santen, David L. Shupe, Roger M. H. Smith, Maayane T. Soumagnac, Robert Stein, Jason Surace, Paula Szkody, Scott Terek, Angela Van Sistine, Sjoert van Velzen, W. Thomas Vestrand, Richard Walters, Charlotte Ward, Chaoran Zhang, Jeffry Zolkower 
TL;DR: The Zwicky Transient Facility (ZTF) as discussed by the authors is a new time domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg$^2$ field of view and 8 second readout time.
Abstract: The Zwicky Transient Facility (ZTF), a public-private enterprise, is a new time domain survey employing a dedicated camera on the Palomar 48-inch Schmidt telescope with a 47 deg$^2$ field of view and 8 second readout time. It is well positioned in the development of time domain astronomy, offering operations at 10% of the scale and style of the Large Synoptic Survey Telescope (LSST) with a single 1-m class survey telescope. The public surveys will cover the observable northern sky every three nights in g and r filters and the visible Galactic plane every night in g and r. Alerts generated by these surveys are sent in real time to brokers. A consortium of universities which provided funding ("partnership") are undertaking several boutique surveys. The combination of these surveys producing one million alerts per night allows for exploration of transient and variable astrophysical phenomena brighter than r $\sim$ 20.5 on timescales of minutes to years. We describe the primary science objectives driving ZTF including the physics of supernovae and relativistic explosions, multi-messenger astrophysics, supernova cosmology, active galactic nuclei and tidal disruption events, stellar variability, and Solar System objects.

501 citations

Journal ArticleDOI
TL;DR: The Zwicky Transient Facility (ZTF) as mentioned in this paper is a robotic time-domain survey currently in progress using the Palomar 48-inch Schmidt Telescope, which uses a 600 megapixel camera to scan the entire northern visible sky at rates of ~3760 square degrees/hour.
Abstract: The Zwicky Transient Facility (ZTF) is a new robotic time-domain survey currently in progress using the Palomar 48-inch Schmidt Telescope. ZTF uses a 47 square degree field with a 600 megapixel camera to scan the entire northern visible sky at rates of ~3760 square degrees/hour to median depths of g ~ 20.8 and r ~ 20.6 mag (AB, 5σ in 30 sec). We describe the Science Data System that is housed at IPAC, Caltech. This comprises the data-processing pipelines, alert production system, data archive, and user interfaces for accessing and analyzing the products. The real-time pipeline employs a novel image-differencing algorithm, optimized for the detection of point-source transient events. These events are vetted for reliability using a machine-learned classifier and combined with contextual information to generate data-rich alert packets. The packets become available for distribution typically within 13 minutes (95th percentile) of observation. Detected events are also linked to generate candidate moving-object tracks using a novel algorithm. Objects that move fast enough to streak in the individual exposures are also extracted and vetted. We present some preliminary results of the calibration performance delivered by the real-time pipeline. The reconstructed astrometric accuracy per science image with respect to Gaia DR1 is typically 45 to 85 milliarcsec. This is the RMS per-axis on the sky for sources extracted with photometric S/N ≥ 10 and hence corresponds to the typical astrometric uncertainty down to this limit. The derived photometric precision (repeatability) at bright unsaturated fluxes varies between 8 and 25 millimag. The high end of these ranges corresponds to an airmass approaching ~2—the limit of the public survey. Photometric calibration accuracy with respect to Pan-STARRS1 is generally better than 2%. The products support a broad range of scientific applications: fast and young supernovae; rare flux transients; variable stars; eclipsing binaries; variability from active galactic nuclei; counterparts to gravitational wave sources; a more complete census of Type Ia supernovae; and solar-system objects.

453 citations

Journal ArticleDOI
Mansi M. Kasliwal1, Ehud Nakar2, Leo Singer3, Leo Singer4, David L. Kaplan5, David O. Cook1, A. Van Sistine5, R. M. Lau1, Christoffer Fremling1, Ore Gottlieb2, Jacob E. Jencson1, Scott M. Adams1, U. Feindt6, Kenta Hotokezaka7, Sourav Ghosh5, Daniel A. Perley8, Po-Chieh Yu9, Tsvi Piran10, James R. Allison11, James R. Allison12, G. C. Anupama13, Arvind Balasubramanian14, Keith W. Bannister15, John Bally16, Jennifer Barnes17, Sudhanshu Barway, Eric C. Bellm18, Varun Bhalerao19, Deb Sankar Bhattacharya20, Nadejda Blagorodnova1, Joshua S. Bloom21, Joshua S. Bloom22, Patrick Brady5, Chris Cannella1, Deep Chatterjee5, S. B. Cenko3, S. B. Cenko4, B. E. Cobb23, Chris M. Copperwheat8, A. Corsi24, Kaushik De1, Dougal Dobie12, Dougal Dobie15, Dougal Dobie11, S. W. K. Emery25, Phil Evans26, Ori D. Fox27, Dale A. Frail28, C. Frohmaier29, C. Frohmaier30, Ariel Goobar6, Gregg Hallinan1, Fiona A. Harrison1, George Helou1, Tanja Hinderer31, Anna Y. Q. Ho1, Assaf Horesh10, Wing-Huen Ip7, Ryosuke Itoh32, Daniel Kasen22, Hyesook Kim, N. P. M. Kuin25, Thomas Kupfer1, Christene Lynch12, Christene Lynch11, K. K. Madsen1, Paolo A. Mazzali8, Paolo A. Mazzali33, Adam A. Miller34, Adam A. Miller35, Kunal Mooley36, Tara Murphy12, Tara Murphy11, Chow-Choong Ngeow9, David A. Nichols31, Samaya Nissanke31, Peter Nugent22, Peter Nugent21, Eran O. Ofek37, H. Qi5, Robert M. Quimby38, Robert M. Quimby39, Stephan Rosswog6, Florin Rusu40, Elaine M. Sadler12, Elaine M. Sadler11, Patricia Schmidt31, Jesper Sollerman6, Iain A. Steele8, A. R. Williamson31, Y. Xu1, Lin Yan1, Yoichi Yatsu32, C. Zhang5, Weijie Zhao40 
TL;DR: In this paper, the authors established the physical association of an electromagnetic counterpart EM170817 to gravitational waves (GW 170817) detected from merging neutron stars by synthesizing a panchromatic dataset.
Abstract: Merging neutron stars offer an exquisite laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart EM170817 to gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic dataset, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma-rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultra-relativistic jets. Instead, we suggest that breakout of a wide-angle, mildly-relativistic cocoon engulfing the jet elegantly explains the low-luminosity gamma-rays, the high-luminosity ultraviolet-optical-infrared and the delayed radio/X-ray emission. We posit that all merging neutron stars may lead to a wide-angle cocoon breakout; sometimes accompanied by a successful jet and sometimes a choked jet.

403 citations


Cited by
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TL;DR: The first direct detection of gravitational waves and the first observation of a binary black hole merger were reported in this paper, with a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ.
Abstract: On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0×10(-21). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203,000 years, equivalent to a significance greater than 5.1σ. The source lies at a luminosity distance of 410(-180)(+160) Mpc corresponding to a redshift z=0.09(-0.04)(+0.03). In the source frame, the initial black hole masses are 36(-4)(+5)M⊙ and 29(-4)(+4)M⊙, and the final black hole mass is 62(-4)(+4)M⊙, with 3.0(-0.5)(+0.5)M⊙c(2) radiated in gravitational waves. All uncertainties define 90% credible intervals. These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.

4,375 citations

Journal ArticleDOI
TL;DR: A binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors.
Abstract: On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

2,746 citations

Journal ArticleDOI
TL;DR: The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the solar system, exploring the transient optical sky, and mapping the Milky Way.
Abstract: (Abridged) We describe here the most ambitious survey currently planned in the optical, the Large Synoptic Survey Telescope (LSST). A vast array of science will be enabled by a single wide-deep-fast sky survey, and LSST will have unique survey capability in the faint time domain. The LSST design is driven by four main science themes: probing dark energy and dark matter, taking an inventory of the Solar System, exploring the transient optical sky, and mapping the Milky Way. LSST will be a wide-field ground-based system sited at Cerro Pachon in northern Chile. The telescope will have an 8.4 m (6.5 m effective) primary mirror, a 9.6 deg$^2$ field of view, and a 3.2 Gigapixel camera. The standard observing sequence will consist of pairs of 15-second exposures in a given field, with two such visits in each pointing in a given night. With these repeats, the LSST system is capable of imaging about 10,000 square degrees of sky in a single filter in three nights. The typical 5$\sigma$ point-source depth in a single visit in $r$ will be $\sim 24.5$ (AB). The project is in the construction phase and will begin regular survey operations by 2022. The survey area will be contained within 30,000 deg$^2$ with $\delta<+34.5^\circ$, and will be imaged multiple times in six bands, $ugrizy$, covering the wavelength range 320--1050 nm. About 90\% of the observing time will be devoted to a deep-wide-fast survey mode which will uniformly observe a 18,000 deg$^2$ region about 800 times (summed over all six bands) during the anticipated 10 years of operations, and yield a coadded map to $r\sim27.5$. The remaining 10\% of the observing time will be allocated to projects such as a Very Deep and Fast time domain survey. The goal is to make LSST data products, including a relational database of about 32 trillion observations of 40 billion objects, available to the public and scientists around the world.

2,738 citations

Journal ArticleDOI
01 Jan 2017
TL;DR: AGILE as discussed by the authors is an ASI space mission developed with programmatic support by INAF and INFN, which includes data gathered with the 1 meter Swope and 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.
Abstract: This program was supported by the the Kavli Foundation, Danish National Research Foundation, the Niels Bohr International Academy, and the DARK Cosmology Centre. The UCSC group is supported in part by NSF grant AST-1518052, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, generous donations from many individuals through a UCSC Giving Day grant, and from fellowships from the Alfred P. Sloan Foundation (R.J.F.), the David and Lucile Packard Foundation (R.J.F. and E.R.) and the Niels Bohr Professorship from the DNRF (E.R.). AMB acknowledges support from a UCMEXUS-CONACYT Doctoral Fellowship. Support for this work was provided by NASA through Hubble Fellowship grants HST-HF-51348.001 (B.J.S.) and HST-HF-51373.001 (M.R.D.) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This paper includes data gathered with the 1 meter Swope and 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.r (AGILE) The AGILE Team thanks the ASI management, the technical staff at the ASI Malindi ground station, the technical support team at the ASI Space Science Data Center, and the Fucino AGILE Mission Operation Center. AGILE is an ASI space mission developed with programmatic support by INAF and INFN. We acknowledge partial support through the ASI grant No. I/028/12/2. We also thank INAF, Italian Institute of Astrophysics, and ASI, Italian Space Agency.r (ANTARES) The ANTARES Collaboration acknowledges the financial support of: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cite d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania;...

1,270 citations