RAS_WEB (Page 2,844)

The GALAH survey: Characterization of emission-line stars with spectral modelling using autoencoders. (arXiv:2006.03062v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cotar_K/0/1/0/all/0/1">Klemen &#x10c;otar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zwitter_T/0/1/0/all/0/1">Toma&#x17e; Zwitter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Traven_G/0/1/0/all/0/1">Gregor Traven</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bland_Hawthorn_J/0/1/0/all/0/1">Joss Bland-Hawthorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buder_S/0/1/0/all/0/1">Sven Buder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hayden_M/0/1/0/all/0/1">Michael R. Hayden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kos_J/0/1/0/all/0/1">Janez Kos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewis_G/0/1/0/all/0/1">Geraint F. Lewis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martell_S/0/1/0/all/0/1">Sarah L. Martell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nordlander_T/0/1/0/all/0/1">Thomas Nordlander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stello_D/0/1/0/all/0/1">Dennis Stello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horner_J/0/1/0/all/0/1">Jonathan Horner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ting_Y/0/1/0/all/0/1">Yuan-Sen Ting</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zerjal_M/0/1/0/all/0/1">Maru&#x161;a &#x17d;erjal</a> We present a neural network autoencoder structure that is able to extract essential latent spectral features from observed spectra and then reconstruct a spectrum from those features. Because of the training with a set of unpeculiar spectra, the network is able to reproduce a spectrum ofRead More →

Bipolar molecular outflow of the very low-mass star Par-Lup3-4. (arXiv:2006.03063v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Santamaria_Miranda_A/0/1/0/all/0/1">A. Santamar&#xed;a-Miranda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gregorio_Monsalvo_I/0/1/0/all/0/1">I. de Gregorio-Monsalvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huelamo_N/0/1/0/all/0/1">N. Hu&#xe9;lamo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plunkett_A/0/1/0/all/0/1">A. L. Plunkett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ribas_A/0/1/0/all/0/1">&#xc1;. Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Comeron_F/0/1/0/all/0/1">F. Comer&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schreiber_M/0/1/0/all/0/1">M.R. Schreiber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_C/0/1/0/all/0/1">C. L&#xf3;pez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muzic_K/0/1/0/all/0/1">K. Mu&#x17e;i&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Testi_L/0/1/0/all/0/1">L. Testi</a> Very low-mass stars are known to have jets and outflows, which is indicative of a scaled-down version of low-mass star formation. However, only very few outflows in very low-mass sources are well characterized. We characterize the bipolar molecular outflow of the very low-mass star Par-Lup3-4, a 0.12 M$_{odot}$ object known to power an optical jet. We observed Par-Lup3-4 with ALMA in BandsRead More →

Inferring the lensing rate of LIGO-Virgo sources from the stochastic gravitational wave background. (arXiv:2006.03064v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mukherjee_S/0/1/0/all/0/1">Suvodip Mukherjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Broadhurst_T/0/1/0/all/0/1">Tom Broadhurst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diego_J/0/1/0/all/0/1">Jose M. Diego</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silk_J/0/1/0/all/0/1">Joseph Silk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smoot_G/0/1/0/all/0/1">George F. Smoot</a> Strong lensing of gravitational waves is more likely for distant sources but predicted event rates are highly uncertain with many astrophysical origins proposed. Here we open a new avenue to estimate the event rate of strongly lensed systems by exploring the amplitude of the stochastic gravitational wave background (SGWB). This method can provide a direct upper bound on the high redshift binary coalescing rates, which can be translated into an upper bound onRead More →

Massive black hole merger rates: the effect of kpc separation wandering and supernova feedback. (arXiv:2006.03065v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Barausse_E/0/1/0/all/0/1">Enrico Barausse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dvorkin_I/0/1/0/all/0/1">Irina Dvorkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremmel_M/0/1/0/all/0/1">Michael Tremmel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Volonteri_M/0/1/0/all/0/1">Marta Volonteri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonetti_M/0/1/0/all/0/1">Matteo Bonetti</a> We revisit the predictions for the merger rate of massive black hole binaries detectable by the Laser Interferometer Space Antenna (LISA) and their background signal for pulsar-timing arrays. We focus on the effect of the delays between the merger of galaxies and the final coalescence of black hole binaries, and on the effect of supernova feedback on the growth of black holes. By utilizing a semi-analytic galaxy formation model, not only do we accountRead More →

Modeling Photoionized Turbulent Material in the Circumgalactic Medium II: Effect of Turbulence within a Stratified Medium. (arXiv:2006.03066v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Buie_E/0/1/0/all/0/1">Edward Buie II</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gray_W/0/1/0/all/0/1">William J. Gray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scannapieco_E/0/1/0/all/0/1">Evan Scannapieco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Safarzadeh_M/0/1/0/all/0/1">Mohammadtaher Safarzadeh</a> The circumgalactic medium (CGM) of nearby star-forming galaxies shows clear indications of OVI absorption accompanied by little to no detectable NV absorption. This unusual spectral signature, accompanied by highly non-uniform absorption from lower ionization state species, indicates that the CGM must be viewed as a dynamic, multiphase medium, such as occurs in the presence of turbulence. Motivated by previous isotropic turbulent simulations, we carry out chemodynamical simulations of stratified media in a Navarro-Frenk-WhiteRead More →

Exoplanet detection and its dependence on stochastic sampling of the stellar Initial Mass Function. (arXiv:2006.03067v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bottrill_A/0/1/0/all/0/1">Amy L. Bottrill</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Haigh_M/0/1/0/all/0/1">Molly E. Haigh</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Hole_M/0/1/0/all/0/1">Madeleine R. A. Hole</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Theakston_S/0/1/0/all/0/1">Sarah C. M. Theakston</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_R/0/1/0/all/0/1">Rosa B. Allen</a> (2,1), <a href="http://arxiv.org/find/astro-ph/1/au:+Grimmett_L/0/1/0/all/0/1">Liam P. Grimmett</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Parker_R/0/1/0/all/0/1">Richard J. Parker</a> (1) (1. University of Sheffield, UK, 2. King Edward VII High School, Sheffield, UK) Young Moving Groups (YMGs) are close (<100pc), coherent collections of young (<100Myr) stars that appear to have formed in the same star-forming molecular cloud. As such we would expect their individual initial mass functions (IMFs) to be similar toRead More →

Circumnuclear Molecular Gas in Low-redshift Quasars and Matched Star-forming Galaxies. (arXiv:2006.03072v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Izumi_T/0/1/0/all/0/1">Takuma Izumi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silverman_J/0/1/0/all/0/1">John D. Silverman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jahnke_K/0/1/0/all/0/1">Knud Jahnke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulze_A/0/1/0/all/0/1">Andreas Schulze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cen_R/0/1/0/all/0/1">Renyue Cen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schramm_M/0/1/0/all/0/1">Malte Schramm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagao_T/0/1/0/all/0/1">Tohru Nagao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wisotzki_L/0/1/0/all/0/1">Lutz Wisotzki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rujoparkan_W/0/1/0/all/0/1">Wiphu Rujoparkan</a> A series of gravitational instabilities in a circumnuclear gas disk (CND) are required to trigger gas transport to a central supermassive black hole (SMBH) and ignite Active Galactic Nuclei (AGNs). A test of this scenario is to investigate whether an enhanced molecular gas mass surface density ($Sigma_{rm mol}$) is found in the CND-scale of quasars relative to a comparison sample of inactive galaxies. Here weRead More →

The lifetimes of planetary debris discs around white dwarfs. (arXiv:2006.03073v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Veras_D/0/1/0/all/0/1">Dimitri Veras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heng_K/0/1/0/all/0/1">Kevin Heng</a> The lifetime of a planetary disc which orbits a white dwarf represents a crucial input parameter into evolutionary models of that system. Here we apply a purely analytical formalism to estimate lifetimes of the debris phase of these discs, before they are ground down into dust or are subject to sublimation from the white dwarf. We compute maximum lifetimes for three different types of white dwarf discs, formed from (i) radiative YORP breakup of exo-asteroids along the giant branch phases at 2-100 au, (ii) radiation-less spin-up disruption ofRead More →

A NICER look at the state transitions of the black hole candidate MAXI J1535-571 during its reflares. (arXiv:2006.03074v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cuneo_V/0/1/0/all/0/1">V. A. C&#xfa;neo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alabarta_K/0/1/0/all/0/1">K. Alabarta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_L/0/1/0/all/0/1">L. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altamirano_D/0/1/0/all/0/1">D. Altamirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendez_M/0/1/0/all/0/1">M. M&#xe9;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_M/0/1/0/all/0/1">M. Armas Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Remillard_R/0/1/0/all/0/1">R. Remillard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Homan_J/0/1/0/all/0/1">J. Homan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steiner_J/0/1/0/all/0/1">J. F. Steiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combi_J/0/1/0/all/0/1">J. A. Combi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munoz_Darias_T/0/1/0/all/0/1">T. Mu&#xf1;oz-Darias</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gendreau_K/0/1/0/all/0/1">K. C. Gendreau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arzoumanian_Z/0/1/0/all/0/1">Z. Arzoumanian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevens_A/0/1/0/all/0/1">A. L. Stevens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loewenstein_M/0/1/0/all/0/1">M. Loewenstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tombesi_F/0/1/0/all/0/1">F. Tombesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bult_P/0/1/0/all/0/1">P. Bult</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabian_A/0/1/0/all/0/1">A. C. Fabian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buisson_D/0/1/0/all/0/1">D. J. K. Buisson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neilsen_J/0/1/0/all/0/1">J. Neilsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basak_A/0/1/0/all/0/1">A. Basak</a> The black hole candidate and X-ray binary MAXI J1535-571 was discovered in September 2017.Read More →

Planet Migration in Self-Gravitating Discs: Survival of Planets. (arXiv:2006.03077v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rowther_S/0/1/0/all/0/1">Sahl Rowther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meru_F/0/1/0/all/0/1">Farzana Meru</a> We carry out three-dimensional SPH simulations to study whether planets can survive in self-gravitating protoplanetary discs. The discs modelled here use a cooling prescription that mimics a real disc which is only gravitationally unstable in the outer regions. We do this by modelling the cooling using a simplified method such that the cooling time in the outer parts of the disc is shorter than in the inner regions, as expected in real discs. We find that both giant (> M_Sat) and low mass (< M_Nep) planets initially migrate inwardsRead More →

A Census of Star Formation in the Outer Galaxy II: The GLIMPSE360 Field. (arXiv:2006.03080v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Winston_E/0/1/0/all/0/1">Elaine Winston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hora_J/0/1/0/all/0/1">Joseph Hora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tolls_V/0/1/0/all/0/1">Volker Tolls</a> We have conducted a study of star formation in the outer Galaxy from 65degr$< l <$265degr~in the region observed by the GLIMPSE360 program. This {it Spitzer} warm mission program mapped the plane of the outer Milky Way with IRAC at 3.6 and 4.5~$mu$m. We combine the IRAC, {it WISE}, and 2MASS catalogs and our previous results from another outer Galaxy survey and identify a total of 47,338 Young Stellar Objects (YSOs) across the field spanning $>$180degr in Galactic longitude. Using theRead More →

The synchrotron maser emission from relativistic magnetized shocks: Dependence on the pre-shock temperature. (arXiv:2006.03081v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Babul_A/0/1/0/all/0/1">Aliya-Nur Babul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sironi_L/0/1/0/all/0/1">Lorenzo Sironi</a> Electromagnetic precursor waves generated by the synchrotron maser instability at relativistic magnetized shocks have been recently invoked to explain the coherent radio emission of Fast Radio Bursts. By means of two-dimensional particle-in-cell simulations, we explore the properties of the precursor waves in relativistic electron-positron perpendicular shocks as a function of the pre-shock magnetization $sigmagtrsim 1$ (i.e., the ratio of incoming Poynting flux to particle energy flux) and thermal spread $Delta gamma equiv kT/mc^2=10^{-5}-10^{-1}$. We measure the fraction $f_xi$ of total incoming energy that isRead More →

Spin-induced black hole spontaneous scalarization. (arXiv:2006.03095v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Dima_A/0/1/0/all/0/1">Alexandru Dima</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Barausse_E/0/1/0/all/0/1">Enrico Barausse</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Franchini_N/0/1/0/all/0/1">Nicola Franchini</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Sotiriou_T/0/1/0/all/0/1">Thomas P. Sotiriou</a> We study scalar fields in a black hole background and show that, when the scalar is suitably coupled to curvature, rapid rotation can induce a tachyonic instability. This instability, which is the hallmark of spontaneous scalarization in the linearized regime, is expected to be quenched by nonlinearities and endow the black hole with scalar hair. Hence, our results demonstrate the existence of a broad class of theories that share the same stationary black hole solutions with general relativity at low spins, but which exhibit blackRead More →

The High Inclination Solar Mission. (arXiv:2006.03111v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_K/0/1/0/all/0/1">K. Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_L/0/1/0/all/0/1">L. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_H/0/1/0/all/0/1">H. Thomas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McIntosh_S/0/1/0/all/0/1">S. McIntosh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKenzie_D/0/1/0/all/0/1">D. McKenzie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Newmark_J/0/1/0/all/0/1">J. Newmark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heaton_A/0/1/0/all/0/1">A. Heaton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carr_J/0/1/0/all/0/1">J. Carr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baysinger_M/0/1/0/all/0/1">M. Baysinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_Q/0/1/0/all/0/1">Q. Bean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabisinski_L/0/1/0/all/0/1">L. Fabisinski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capizzo_P/0/1/0/all/0/1">P. Capizzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clements_K/0/1/0/all/0/1">K. Clements</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sutherlin_S/0/1/0/all/0/1">S. Sutherlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_J/0/1/0/all/0/1">J. Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Medina_K/0/1/0/all/0/1">K. Medina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Turse_D/0/1/0/all/0/1">D. Turse</a> The High Inclination Solar Mission (HISM) is a concept for an out-of-the-ecliptic mission for observing the Sun and the heliosphere. The mission profile is largely based on the Solar Polar Imager concept: initially spiraling in to a 0.48 AU ecliptic orbit, then increasing the orbital inclination atRead More →

The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation. (arXiv:2006.03113v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ortiz_J/0/1/0/all/0/1">J. L. Ortiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_Sanz_P/0/1/0/all/0/1">P. Santos-Sanz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sicardy_B/0/1/0/all/0/1">B. Sicardy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benedetti_Rossi_G/0/1/0/all/0/1">G. Benedetti-Rossi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berard_D/0/1/0/all/0/1">D. B&#xe9;rard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_N/0/1/0/all/0/1">N. Morales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duffard_R/0/1/0/all/0/1">R. Duffard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Braga_Ribas_F/0/1/0/all/0/1">F. Braga-Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hopp_U/0/1/0/all/0/1">U. Hopp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ries_C/0/1/0/all/0/1">C. Ries</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nascimbeni_V/0/1/0/all/0/1">V. Nascimbeni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marzari_F/0/1/0/all/0/1">F. Marzari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Granata_V/0/1/0/all/0/1">V. Granata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pal_A/0/1/0/all/0/1">A. P&#xe1;l</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kiss_C/0/1/0/all/0/1">C. Kiss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pribulla_T/0/1/0/all/0/1">T. Pribulla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Komzik_R/0/1/0/all/0/1">R. Kom&#x17e;&#xed;k</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hornoch_K/0/1/0/all/0/1">K. Hornoch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pravec_P/0/1/0/all/0/1">P. Pravec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacci_P/0/1/0/all/0/1">P. Bacci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maestripieri_M/0/1/0/all/0/1">M. Maestripieri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nerli_L/0/1/0/all/0/1">L. Nerli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mazzei_L/0/1/0/all/0/1">L. Mazzei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bachini_M/0/1/0/all/0/1">M. Bachini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinelli_F/0/1/0/all/0/1">F. Martinelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Succi_G/0/1/0/all/0/1">G. Succi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciabattari_F/0/1/0/all/0/1">F. Ciabattari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mikuz_H/0/1/0/all/0/1">H. Mikuz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carbognani_A/0/1/0/all/0/1">A. Carbognani</a>,Read More →