@article{YangZhuWolfetal.2018, author = {Yang, Jie and Zhu, Xiaolei and Wolf, Thomas J. A. and Li, Zheng and Nunes, Jo{\~a}o Pedro Figueira and Coffee, Ryan and Cryan, James P. and G{\"u}hr, Markus and Hegazy, Kareem and Heinz, Tony F. and Jobe, Keith and Li, Renkai and Shen, Xiaozhe and Veccione, Theodore and Weathersby, Stephen and Wilkin, Kyle J. and Yoneda, Charles and Zheng, Qiang and Martinez, Todd J. and Centurion, Martin and Wang, Xijie}, title = {Imaging CF3I conical intersection and photodissociation dynamics with ultrafast electron diffraction}, series = {Science}, volume = {361}, journal = {Science}, number = {6397}, publisher = {American Assoc. for the Advancement of Science}, address = {Washington}, issn = {0036-8075}, doi = {10.1126/science.aat0049}, pages = {64 -- 67}, year = {2018}, abstract = {Conical intersections play a critical role in excited-state dynamics of polyatomic molecules because they govern the reaction pathways of many nonadiabatic processes. However, ultrafast probes have lacked sufficient spatial resolution to image wave-packet trajectories through these intersections directly. Here, we present the simultaneous experimental characterization of one-photon and two-photon excitation channels in isolated CF3I molecules using ultrafast gas-phase electron diffraction. In the two-photon channel, we have mapped out the real-space trajectories of a coherent nuclear wave packet, which bifurcates onto two potential energy surfaces when passing through a conical intersection. In the one-photon channel, we have resolved excitation of both the umbrella and the breathing vibrational modes in the CF3 fragment in multiple nuclear dimensions. These findings benchmark and validate ab initio nonadiabatic dynamics calculations.}, language = {en} } @article{WilkinParrishYangetal.2019, author = {Wilkin, Kyle J. and Parrish, Robert M. and Yang, Jie and Wolf, Thomas J. A. and Nunes, J. Pedro F. and G{\"u}hr, Markus and Li, Renkai and Shen, Xiaozhe and Zheng, Qiang and Wang, Xijie and Martinez, Todd J. and Centurion, Martin}, title = {Diffractive imaging of dissociation and ground-state dynamics in a complex molecule}, series = {Physical review : A, Atomic, molecular, and optical physics}, volume = {100}, journal = {Physical review : A, Atomic, molecular, and optical physics}, number = {2}, publisher = {American Physical Society}, address = {College Park}, issn = {2469-9926}, doi = {10.1103/PhysRevA.100.023402}, pages = {10}, year = {2019}, abstract = {We have investigated the structural dynamics in photoexcited 1,2-diiodotetrafluoroethane molecules (C2F4I2) in the gas phase experimentally using ultrafast electron diffraction and theoretically using FOMO-CASCI excited-state dynamics simulations. The molecules are excited by an ultraviolet femtosecond laser pulse to a state characterized by a transition from the iodine 5p perpendicular to orbital to a mixed 5p parallel to sigma hole and CF2 center dot antibonding orbital, which results in the cleavage of one of the carbon-iodine bonds. We have observed, with sub-Angstrom resolution, the motion of the nuclear wave packet of the dissociating iodine atom followed by coherent vibrations in the electronic ground state of the C2F4I radical. The radical reaches a stable classical (nonbridged) structure in less than 200 fs.}, language = {en} } @article{TorrejonReigFuerstetal.2018, author = {Torrejon, J. M. and Reig, Pablo and F{\"u}rst, F. and Martinez-Chicharro, M. and Postnov, K. and Oskinova, Lida}, title = {NuSTAR rules out a cyclotron line in the accreting magnetar candidate 4U2206+54}, series = {Monthly notices of the Royal Astronomical Society}, volume = {479}, journal = {Monthly notices of the Royal Astronomical Society}, number = {3}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnras/sty1628}, pages = {3366 -- 3372}, year = {2018}, abstract = {Based on our new NuSTAR X-ray telescope data, we rule out any cyclotron line up to 60 keV in the spectra of the high-mass X-ray binary 4U2206+54. In particular, we do not find any evidence of the previously claimed line around 30 keV, independently of the source flux, along the spin pulse. The spin period has increased significantly, since the last observation, up to 5750 +/- 10 s, confirming the rapid spin-down rate (nu)over dot = -1.8 x 10(-14) Hz s(-1). This behaviour might be explained by the presence of a strongly magnetized neutron star (B-s > several times 10(13) G) accreting from the slow wind of its main-sequence O9.5 companion.}, language = {en} } @inproceedings{TatischeffDeAngelisTavanietal.2018, author = {Tatischeff, V. and De Angelis, A. and Tavani, M. and Grenier, I. and Oberlack, U. and Hanlon, L. and Walter, R. and Argan, A. and von Ballmoos, P. and Bulgarelli, A. and Donnarumma, I. and Hernanz, Margarita and Kuvvetli, I. and Mallamaci, M. and Pearce, M. and Zdziarski, A. and Aboudan, A. and Ajello, M. and Ambrosi, G. and Bernard, D. and Bernardini, E. and Bonvicini, V. and Brogna, A. and Branchesi, M. and Budtz-Jorgensen, C. and Bykov, A. and Campana, R. and Cardillo, M. and Ciprini, S. and Coppi, P. and Cumani, P. and da Silva, R. M. Curado and De Martino, D. and Diehl, R. and Doro, M. and Fioretti, V. and Funk, S. and Ghisellini, G. and Giordano, F. and Grove, J. E. and Hamadache, C. and Hartmann, D. H. and Hayashida, M. and Isern, J. and Kanbach, G. and Kiener, J. and Knodlseder, J. and Labanti, C. and Laurent, P. and Leising, M. and Limousin, O. and Longo, F. and Mannheim, K. and Marisaldi, M. and Martinez, M. and Mazziotta, M. N. and McEnery, J. E. and Mereghetti, S. and Minervini, G. and Moiseev, A. and Morselli, A. and Nakazawa, K. and Orleanski, P. and Paredes, J. M. and Patricelli, B. and Peyre, J. and Piano, G. and Pohl, Martin and Rando, R. and Roncadelli, M. and Tavecchio, F. and Thompson, D. J. and Turolla, R. and Ulyanov, A. and Vacchi, A. and Wu, X. and Zoglauer, A.}, title = {The e-ASTROGAM gamma-ray space observatory for the multimessenger astronomy of the 2030s}, series = {Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray}, volume = {10699}, booktitle = {Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray}, editor = {DenHerder, JWA Nikzad}, publisher = {SPIE - The International Society for Optical Engineering}, address = {Bellingham}, isbn = {978-1-5106-1952-4}, issn = {0277-786X}, doi = {10.1117/12.2315151}, pages = {15}, year = {2018}, abstract = {e-ASTROGAM is a concept for a breakthrough observatory space mission carrying a gamma-ray telescope dedicated to the study of the non-thermal Universe in the photon energy range from 0.15 MeV to 3 GeV. The lower energy limit can be pushed down to energies as low as 30 keV for gamma-ray burst detection with the calorimeter. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with remarkable polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous and current generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will be a major player of the multiwavelength, multimessenger time-domain astronomy of the 2030s, and provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LISA, LIGO, Virgo, KAGRA, the Einstein Telescope and the Cosmic Explorer, IceCube-Gen2 and KM3NeT, SKA, ALMA, JWST, E-ELT, LSST, Athena, and the Cherenkov Telescope Array.}, language = {en} } @article{NideverOlsenWalkeretal.2017, author = {Nidever, David L. and Olsen, Knut and Walker, Alistair R. and Katherina Vivas, A. and Blum, Robert D. and Kaleida, Catherine and Choi, Yumi and Conn, Blair C. and Gruendl, Robert A. and Bell, Eric F. and Besla, Gurtina and Munoz, Ricardo R. and Gallart, Carme and Martin, Nicolas F. and Olszewski, Edward W. and Saha, Abhijit and Monachesi, Antonela and Monelli, Matteo and de Boer, Thomas J. L. and Johnson, L. Clifton and Zaritsky, Dennis and Stringfellow, Guy S. and van der Marel, Roeland P. and Cioni, Maria-Rosa L. and Jin, Shoko and Majewski, Steven R. and Martinez-Delgado, David and Monteagudo, Lara and Noel, Noelia E. D. and Bernard, Edouard J. and Kunder, Andrea and Chu, You-Hua and Bell, Cameron P. M. and Santana, Felipe and Frechem, Joshua and Medina, Gustavo E. and Parkash, Vaishali and Seron Navarrete, J. C. and Hayes, Christian}, title = {SMASH: Survey of the MAgellanic Stellar History}, series = {The astronomical journal}, volume = {154}, journal = {The astronomical journal}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {0004-6256}, doi = {10.3847/1538-3881/aa8d1c}, pages = {310 -- 326}, year = {2017}, abstract = {The Large and Small Magellanic Clouds are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community Dark Energy Camera (DECam) survey of the Clouds mapping 480 deg2 (distributed over similar to 2400 square degrees at similar to 20\% filling factor) to similar to 24th. mag in ugriz. The primary goals of SMASH are to identify low surface brightness stellar populations associated with the stellar halos and tidal debris of the Clouds, and to derive spatially resolved star formation histories. Here, we present a summary of the survey, its data reduction, and a description of the first public Data Release (DR1). The SMASH DECam data have been reduced with a combination of the NOAO Community Pipeline, the PHOTRED automated point-spread-function photometry pipeline, and custom calibration software. The astrometric precision is similar to 15 mas and the accuracy is similar to 2 mas with respect to the Gaia reference frame. The photometric precision is similar to 0.5\%-0.7\% in griz and similar to 1\% in u with a calibration accuracy of similar to 1.3\% in all bands. The median 5s point source depths in ugriz are 23.9, 24.8, 24.5, 24.2, and 23.5 mag. The SMASH data have already been used to discover the Hydra II Milky Way satellite, the SMASH 1 old globular cluster likely associated with the LMC, and extended stellar populations around the LMC out to R. similar to. 18.4 kpc. SMASH DR1 contains measurements of similar to 100 million objects distributed in 61 fields. A prototype version of the NOAO Data Lab provides data access and exploration tools.}, language = {en} } @article{MartinezChicharroTorrejonOskinovaetal.2018, author = {Martinez-Chicharro, M. and Torrejon, J. M. and Oskinova, Lida and Furst, F. and Postnov, K. and Rodes-Roca, J. J. and Hainich, Rainer and Bodaghee, A.}, title = {Evidence of Compton cooling during an X-ray flare supports a neutron star nature of the compact object in 4U1700-37}, series = {Monthly notices of the Royal Astronomical Society}, volume = {473}, journal = {Monthly notices of the Royal Astronomical Society}, number = {1}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnrasl/slx165}, pages = {L74 -- L78}, year = {2018}, abstract = {Based on new Chandra X-ray telescope data, we present empirical evidence of plasma Compton cooling during a flare in the non-pulsating massive X-ray binary 4U1700-37. This behaviour might be explained by quasi-spherical accretion on to a slowly rotating magnetized neutron star (NS). In quiescence, the NS in 4U1700-37 is surrounded by a hot radiatively cooling shell. Its presence is supported by the detection of mHz quasi-periodic oscillations likely produced by its convection cells. The high plasma temperature and the relatively low X-ray luminosity observed during the quiescence, point to a small emitting area similar to 1 km, compatible with a hotspot on an NS surface. The sudden transition from a radiative to a significantly more efficient Compton cooling regime triggers an episode of enhanced accretion resulting in a flare. During the flare, the plasma temperature drops quickly. The predicted luminosity for such transitions, similar to 3 x 10(35) erg s(-1), is very close to the luminosity of 4U1700-37 during quiescence. The transition may be caused by the accretion of a clump in the stellar wind of the donor star. Thus, a magnetized NS nature of the compact object is strongly favoured.}, language = {en} } @article{MartinezGonzalezPastorYabarLaggetal.2016, author = {Martinez Gonzalez, M. J. and Pastor Yabar, A. and Lagg, A. and Asensio Ramos, A. and Collados Vera, M. and Solanki, S. K. and Balthasar, H. and Berkefeld, T. and Denker, Carsten and Doerr, H. P. and Feller, A. and Franz, M. and Gonz{\´a}lez Manrique, Sergio Javier and Hofmann, A. and Kneer, F. and Kuckein, Christoph and Louis, R. and von der L{\"u}he, O. and Nicklas, H. and Orozco, D. and Rezaei, R. and Schlichenmaier, R. and Schmidt, D. and Schmidt, W. and Sigwarth, M. and Sobotka, M. and Soltau, D. and Staude, J. and Strassmeier, Klaus G. and Verma, Meetu and Waldman, T. and Volkmer, R.}, title = {Inference of magnetic fields in the very quiet Sun}, series = {Journal of geophysical research : Earth surface}, volume = {596}, journal = {Journal of geophysical research : Earth surface}, publisher = {EDP Sciences}, address = {Les Ulis}, issn = {1432-0746}, doi = {10.1051/0004-6361/201628449}, pages = {11}, year = {2016}, abstract = {Context. Over the past 20 yr, the quietest areas of the solar surface have revealed a weak but extremely dynamic magnetism occurring at small scales (<500 km), which may provide an important contribution to the dynamics and energetics of the outer layers of the atmosphere. Understanding this magnetism requires the inference of physical quantities from high-sensitivity spectro-polarimetric data with high spatio-temporal resolution. Aims. We present high-precision spectro-polarimetric data with high spatial resolution (0.4") of the very quiet Sun at 1.56 mu m obtained with the GREGOR telescope to shed some light on this complex magnetism. Methods. We used inversion techniques in two main approaches. First, we assumed that the observed profiles can be reproduced with a constant magnetic field atmosphere embedded in a field-free medium. Second, we assumed that the resolution element has a substructure with either two constant magnetic atmospheres or a single magnetic atmosphere with gradients of the physical quantities along the optical depth, both coexisting with a global stray-light component. Results. Half of our observed quiet-Sun region is better explained by magnetic substructure within the resolution element. However, we cannot distinguish whether this substructure comes from gradients of the physical parameters along the line of sight or from horizontal gradients (across the surface). In these pixels, a model with two magnetic components is preferred, and we find two distinct magnetic field populations. The population with the larger filling factor has very weak (similar to 150 G) horizontal fields similar to those obtained in previous works. We demonstrate that the field vector of this population is not constrained by the observations, given the spatial resolution and polarimetric accuracy of our data. The topology of the other component with the smaller filling factor is constrained by the observations for field strengths above 250 G: we infer hG fields with inclinations and azimuth values compatible with an isotropic distribution. The filling factors are typically below 30\%. We also find that the flux of the two polarities is not balanced. From the other half of the observed quiet-Sun area similar to 50\% are two-lobed Stokes V profiles, meaning that 23\% of the field of view can be adequately explained with a single constant magnetic field embedded in a non-magnetic atmosphere. The magnetic field vector and filling factor are reliable inferred in only 50\% based on the regular profiles. Therefore, 12\% of the field of view harbour hG fields with filling factors typically below 30\%. At our present spatial resolution, 70\% of the pixels apparently are non-magnetised.}, language = {en} } @article{MartinNideverBeslaetal.2015, author = {Martin, Nicolas F. and Nidever, David L. and Besla, Gurtina and Olsen, Knut and Walker, Alistair R. and Vivas, A. Katherina and Gruendl, Robert A. and Kaleida, Catherine C. and Munoz, Ricardo R. and Blum, Robert D. and Saha, Abhijit and Conn, Blair C. and Bell, Eric F. and Chu, You-Hua and Cioni, Maria-Rosa L. and de Boer, Thomas J. L. and Gallart, Carme and Jin, Shoko and Kunder, Andrea and Majewski, Steven R. and Martinez-Delgado, David and Monachesi, Antonela and Monelli, Matteo and Monteagudo, Lara and Noel, Noelia E. D. and Olszewski, Edward W. and Stringfellow, Guy S. and van der Marel, Roeland P. and Zaritsky, Dennis}, title = {Hydra II: A faint and compact milky way dwarf galaxy found in the survey of the magellanic stellar history}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, volume = {804}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, number = {1}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {2041-8205}, doi = {10.1088/2041-8205/804/1/L5}, pages = {6}, year = {2015}, abstract = {We present the discovery of a new dwarf galaxy, Hydra II, found serendipitously within the data from the ongoing Survey of the Magellanic Stellar History conducted with the Dark Energy Camera on the Blanco 4 m Telescope. The new satellite is compact (r(h) = 68 +/- 11 pc) and faint (MV = -4.8 +/- 0.3), but well within the realm of dwarf galaxies. The stellar distribution of Hydra II in the color-magnitude diagram is well-described by a metal-poor ([Fe/H] = -2.2) and old (13 Gyr) isochrone and shows a distinct blue horizontal branch, some possible red clump stars, and faint stars that are suggestive of blue stragglers. At a heliocentric distance of 134 +/- 10 kpc, Hydra II is located in a region of the Galactic halo that models have suggested may host material from the leading arm of the Magellanic Stream. A comparison with N-body simulations hints that the new dwarf galaxy could be or could have been a satellite of the Magellanic Clouds.}, language = {en} } @article{MartinJungbluthNideveretal.2016, author = {Martin, Nicolas F. and Jungbluth, Valentin and Nidever, David L. and Bell, Eric F. and Besla, Gurtina and Blum, Robert D. and Cioni, Maria-Rosa L. and Conn, Blair C. and Kaleida, Catherine C. and Gallart, Carme and Jin, Shoko and Majewski, Steven R. and Martinez-Delgado, David and Monachesi, Antonela and Munoz, Ricardo R. and Noel, Noelia E. D. and Olsen, Knut and Stringfellow, Guy S. and van der Marel, Roeland P. and Vivas, A. Katherina and Walker, Alistair R. and Zaritsky, Dennis}, title = {SMASH 1: A VERY FAINT GLOBULAR CLUSTER DISRUPTING IN THE OUTER REACHES OF THE LMC?}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, volume = {830}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {2041-8205}, doi = {10.3847/2041-8205/830/1/L10}, pages = {92 -- 98}, year = {2016}, language = {en} } @article{FurnissNodaBoggsetal.2015, author = {Furniss, A. and Noda, K. and Boggs, S. and Chiang, J. and Christensen, F. and Craig, W. and Giommi, P. and Hailey, C. and Harisson, F. and Madejski, G. and Nalewajko, K. and Perri, M. and Stern, D. and Urry, M. and Verrecchia, F. and Zhang, W. and Ahnen, M. L. and Ansoldi, S. and Antonelli, L. A. and Antoranz, P. and Babic, A. and Banerjee, B. and Bangale, P. and de Almeida, U. Barres and Barrio, J. A. and Becerra Gonzalez, J. and Bednarek, W. and Bernardini, E. and Biasuzzi, B. and Biland, A. and Blanch Bigas, O. and Bonnefoy, S. and Bonnoli, G. and Borracci, F. and Bretz, T. and Carmona, E. and Carosi, A. and Chatterjee, A. and Clavero, R. and Colin, P. and Colombo, E. and Contreras, J. L. and Cortina, J. and Covino, S. and Da Vela, P. and Dazzi, F. and De Angelis, A. and De Caneva, G. and De Lotto, B. and de Ona Wilhelmi, E. and Delgado Mendez, C. and Di Pierro, F. and Prester, Dijana Dominis and Dorner, D. and Doro, M. and Einecke, S. and Eisenacher Glawion, D. and Elsaesser, D. and Fernandez-Barral, A. and Fidalgo, D. and Fonseca, M. V. and Font, L. and Frantzen, K. and Fruck, C. and Galindo, D. and Garcia Lopez, R. J. and Garczarczyk, M. and Garrido Terrats, D. and Gaug, M. and Giammaria, P. and Godinovic, N. and Gonzalez Munoz, A. and Guberman, D. and Hanabata, Y. and Hayashida, M. and Herrera, J. and Hose, J. and Hrupec, D. and Hughes, G. and Idec, W. and Kellermann, H. and Kodani, K. and Konno, Y. and Kubo, H. and Kushida, J. and La Barbera, A. and Lelas, D. and Lewandowska, N. and Lindfors, E. and Lombardi, S. and Longo, F. and Lopez, M. and Lopez-Coto, R. and Lopez-Oramas, A. and Lorenz, E. and Majumdar, P. and Makariev, M. and Mallot, K. and Maneva, G. and Manganaro, M. and Mannheim, K. and Maraschi, L. and Marcote, B. and Mariotti, M. and Martinez, M. and Mazin, D. and Menzel, U. and Miranda, J. M. and Mirzoyan, R. and Moralejo, A. and Nakajima, D. and Neustroev, V. and Niedzwiecki, A. and Nievas Rosillo, M. and Nilsson, K. and Nishijima, K. and Orito, R. and Overkemping, A. and Paiano, S. and Palacio, J. and Palatiello, M. and Paneque, D. and Paoletti, R. and Paredes, J. M. and Paredes-Fortuny, X. and Persic, M. and Poutanen, J. and Moroni, P. G. Prada and Prandini, E. and Puljak, I. and Reinthal, R. and Rhode, W. and Ribo, M. and Rico, J. and Garcia, J. Rodriguez and Saito, T. and Saito, K. and Satalecka, K. and Scapin, V. and Schultz, C. and Schweizer, T. and Shore, S. N. and Sillanpaa, A. and Sitarek, J. and Snidaric, I. and Sobczynska, D. and Stamerra, A. and Steinbring, T. and Strzys, M. and Takalo, L. and Takami, H. and Tavecchio, F. and Temnikov, P. and Terzic, T. and Tescaro, D. and Teshima, M. and Thaele, J. and Torres, D. F. and Toyama, T. and Treves, A. and Verguilov, V. and Vovk, I. and Will, M. and Zanin, R. and Archer, A. and Benbow, W. and Bird, R. and Biteau, Jonathan and Bugaev, V. and Cardenzana, J. V. and Cerruti, M. and Chen, Xuhui and Ciupik, L. and Connolly, M. P. and Cui, W. and Dickinson, H. J. and Dumm, J. and Eisch, J. D. and Falcone, A. and Feng, Q. and Finley, J. P. and Fleischhack, H. and Fortin, P. and Fortson, L. and Gerard, L. and Gillanders, G. H. and Griffin, S. and Griffiths, S. T. and Grube, J. and Gyuk, G. and Hakansson, Nils and Holder, J. and Humensky, T. B. and Johnson, C. A. and Kaaret, P. and Kertzman, M. and Kieda, D. and Krause, M. and Krennrich, F. and Lang, M. J. and Lin, T. T. Y. and Maier, G. and McArthur, S. and McCann, A. and Meagher, K. and Moriarty, P. and Mukherjee, R. and Nieto, D. and Ong, R. A. and Park, N. and Petry, D. and Pohl, Martin and Popkow, A. and Ragan, K. and Ratliff, G. and Reyes, L. C. and Reynolds, P. T. and Richards, G. T. and Roache, E. and Santander, M. and Sembroski, G. H. and Shahinyan, K. and Staszak, D. and Telezhinsky, Igor O. and Tucci, J. V. and Tyler, J. and Vassiliev, V. V. and Wakely, S. P. and Weiner, O. M. and Weinstein, A. and Wilhelm, Alina and Williams, D. A. and Zitzer, B. and Vince, O. and Fuhrmann, L. and Angelakis, E. and Karamanavis, V. and Myserlis, I. and Krichbaum, T. P. and Zensus, J. A. and Ungerechts, H. and Sievers, A. and Bachev, R. and Boettcher, Markus and Chen, W. P. and Damljanovic, G. and Eswaraiah, C. and Guver, T. and Hovatta, T. and Hughes, Z. and Ibryamov, S. I. and Joner, M. D. and Jordan, B. and Jorstad, S. G. and Joshi, M. and Kataoka, J. and Kurtanidze, O. M. and Kurtanidze, S. O. and Lahteenmaki, A. and Latev, G. and Lin, H. C. and Larionov, V. M. and Mokrushina, A. A. and Morozova, D. A. and Nikolashvili, M. G. and Raiteri, C. M. and Ramakrishnan, V. and Readhead, A. C. R. and Sadun, A. C. and Sigua, L. A. and Semkov, E. H. and Strigachev, A. and Tammi, J. and Tornikoski, M. and Troitskaya, Y. V. and Troitsky, I. S. and Villata, M.}, title = {First NuSTAR observations of MRK 501 within a radio to TeV multi-instrument campaign}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, volume = {812}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, number = {1}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, organization = {NuSTAR Team, MAGIC Collaboration, VERITAS Collaboration, F-Gamma Consortium}, issn = {0004-637X}, doi = {10.1088/0004-637X/812/1/65}, pages = {22}, year = {2015}, abstract = {We report on simultaneous broadband observations of the TeV-emitting blazar Markarian 501 between 2013 April 1 and August 10, including the first detailed characterization of the synchrotron peak with Swift and NuSTAR. During the campaign, the nearby BL Lac object was observed in both a quiescent and an elevated state. The broadband campaign includes observations with NuSTAR, MAGIC, VERITAS, the Fermi Large Area Telescope, Swift X-ray Telescope and UV Optical Telescope, various ground-based optical instruments, including the GASP-WEBT program, as well as radio observations by OVRO, Metsahovi, and the F-Gamma consortium. Some of the MAGIC observations were affected by a sand layer from the Saharan desert, and had to be corrected using event-by-event corrections derived with a Light Detection and Ranging (LIDAR) facility. This is the first time that LIDAR information is used to produce a physics result with Cherenkov Telescope data taken during adverse atmospheric conditions, and hence sets a precedent for the current and future ground-based gamma-ray instruments. The NuSTAR instrument provides unprecedented sensitivity in hard X-rays, showing the source to display a spectral energy distribution (SED) between 3 and 79 keV consistent with a log-parabolic spectrum and hard X-ray variability on hour timescales. None (of the four extended NuSTAR observations) show evidence of the onset of inverse-Compton emission at hard X-ray energies. We apply a single-zone equilibrium synchrotron self-Compton (SSC) model to five simultaneous broadband SEDs. We find that the SSC model can reproduce the observed broadband states through a decrease in the magnetic field strength coinciding with an increase in the luminosity and hardness of the relativistic leptons responsible for the high-energy emission.}, language = {en} }