December 2018

Characterisation of dust events on Earth and Mars: the ExoMars/DREAMS experiment and the field campaigns in the Sahara desert. (arXiv:1812.10480v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Franzese_G/0/1/0/all/0/1">Gabriele Franzese</a> Atmospheric dust plays an important role on the terrestrial climate, regulating the amount of solar radiation coming to the surface, affecting the development and the life time of the clouds and providing fundamental nutrients to the growth of the terrestrial and oceanic biomes. On Mars, the global effect of dust is even stronger due to the widespread presence of sources and the lack of vegetation and oceans able to mitigate its contribution. The DREAMS station and the Dust Complex, on boardRead More →

Design and modelling of spectrographs with holographic gratings on freeform surfaces. (arXiv:1812.10484v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Muslimov_E/0/1/0/all/0/1">Eduard R. Muslimov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrari_M/0/1/0/all/0/1">Marc Ferrari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hugot_E/0/1/0/all/0/1">Emmanuel Hugot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouret_J/0/1/0/all/0/1">Jean-Claude Bouret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neiner_C/0/1/0/all/0/1">Coralie Neiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lombardo_S/0/1/0/all/0/1">Simona Lombardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lemaitre_G/0/1/0/all/0/1">Gerard Lemaitre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grange_R/0/1/0/all/0/1">Robert Grange</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guskov_I/0/1/0/all/0/1">Ilya A. Guskov</a> In the present paper we demonstrate the approach of using a holographic grating on a freeform surface for advanced spectrographs design. We discuss the surface and groove pattern description used for ray-tracing. Moreover, we present a general procedure of diffraction efficiency calculation, which accounts for the change of hologram recording and operation conditions across the surface. The primary application of this approach isRead More →

Surface brightness profile of the 3.5 keV line in the Milky Way halo. (arXiv:1812.10488v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Boyarsky_A/0/1/0/all/0/1">A. Boyarsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iakubovskyi_D/0/1/0/all/0/1">D. Iakubovskyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruchayskiy_O/0/1/0/all/0/1">O. Ruchayskiy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Savchenko_D/0/1/0/all/0/1">D. Savchenko</a> We report a detection of 3.5 keV line in the Milky Way in 5 regions offset from the Galactic Center by distances from 10′ to 35 degrees. We build an angular profile of this line and compare it with profiles of several astrophysical lines detected in the same observations. We compare our results with other detections and bounds previously obtained using observations of the Milky Way. We report a detection of 3.5 keV line in the Milky WayRead More →

Serendipitous Discoveries of Kilonovae in the LSST Main Survey: Maximising Detections of Sub-Threshold Gravitational Wave Events. (arXiv:1812.10492v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Setzer_C/0/1/0/all/0/1">Christian N. Setzer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biswas_R/0/1/0/all/0/1">Rahul Biswas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peiris_H/0/1/0/all/0/1">Hiranya V. Peiris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosswog_S/0/1/0/all/0/1">Stephan Rosswog</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korobkin_O/0/1/0/all/0/1">Oleg Korobkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wollaeger_R/0/1/0/all/0/1">Ryan T. Wollaeger</a> (The LSST Dark Energy Science Collaboration) We investigate the ability of the Large Synoptic Survey Telescope (LSST) to discover kilonovae (kNe) from binary neutron star (BNS) and neutron star-black hole (NSBH) mergers, focusing on serendipitous detections in the Wide-Fast-Deep (WFD) survey. We simulate observations of kNe with proposed LSST survey strategies, paying particular attention to cadence choices that are compatible with the broader LSST cosmology programme.Read More →

Cosmic ray feedback in the FIRE simulations: constraining cosmic ray propagation with GeV gamma ray emission. (arXiv:1812.10496v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chan_T/0/1/0/all/0/1">T.K. Chan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keres_D/0/1/0/all/0/1">D. Keres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hopkins_P/0/1/0/all/0/1">P.F. Hopkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quataert_E/0/1/0/all/0/1">E. Quataert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Su_K/0/1/0/all/0/1">K.-Y. Su</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hayward_C/0/1/0/all/0/1">C.C. Hayward</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Faucher_Giguere_C/0/1/0/all/0/1">C.-A. Faucher-Giguere</a> We present the first results of cosmic ray (CR) feedback implemented in the Feedback In Realistic Environments (FIRE) simulations. We investigate CR feedback in non-cosmological simulations of dwarf, sub-$Lstar$ starburst, and $Lstar$ galaxies with different propagation models, including advection, isotropic and anisotropic diffusion, and streaming along field lines with different transport coefficients. We simulate CR diffusion and streaming simultaneously in galaxies with high resolution, using aRead More →

Inefficient volatile loss from the Moon-forming disk: reconciling the giant impact hypothesis and a wet Moon. (arXiv:1812.10502v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nakajima_M/0/1/0/all/0/1">Miki Nakajima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevenson_D/0/1/0/all/0/1">David J. Stevenson</a> The Earth’s Moon is thought to have formed from a circumterrestrial disk generated by a giant impact between the proto-Earth and an impactor approximately 4.5 billion years ago. Since the impact was energetic, the disk would have been hot and partially vaporized. This formation process is thought to be responsible for the geochemical observation that the Moon is depleted in volatiles. This model predicts that the Moon should be significantly depleted in water as well, but this appears to contradictRead More →

Marvel analysis of the measured high-resolution rovibrational spectra of H2S. (arXiv:1812.10503v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chubb_K/0/1/0/all/0/1">Katy L. Chubb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naumenko_O/0/1/0/all/0/1">Olga Naumenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keely_S/0/1/0/all/0/1">Stefan Keely</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartolotto_S/0/1/0/all/0/1">Sebestiano Bartolotto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macdonald_S/0/1/0/all/0/1">Skye Macdonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mukhtar_M/0/1/0/all/0/1">Mahmoud Mukhtar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grachov_A/0/1/0/all/0/1">Andrey Grachov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+White_J/0/1/0/all/0/1">Joe White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coleman_E/0/1/0/all/0/1">Eden Coleman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_A/0/1/0/all/0/1">Anwen Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fazliev_A/0/1/0/all/0/1">Alexander Z. Fazliev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Polovtseva_E/0/1/0/all/0/1">Elena R. Polovtseva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Horneman_V/0/1/0/all/0/1">Veli-Matti Horneman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campargue_A/0/1/0/all/0/1">Alain Campargue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furtenbacher_T/0/1/0/all/0/1">Tibor Furtenbacher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Csaszar_A/0/1/0/all/0/1">Attila G. Cs&#xe1;sz&#xe1;r</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yurchenko_S/0/1/0/all/0/1">Sergei N. Yurchenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tennyson_J/0/1/0/all/0/1">Jonathan Tennyson</a> 44325 measured and assigned transitions of H$_2^{32}$S, the parent isotopologue of the hydrogen sulfide molecule, are collated from 33 publications into a single database and reviewed critically. Based on this information, rotation-vibration energy levelsRead More →

Machine Learning on Difference Image Analysis: A comparison of methods for transient detection. (arXiv:1812.10518v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_B/0/1/0/all/0/1">B. S&#xe1;nchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+R%2E_M/0/1/0/all/0/1">M. J. Dom&#xed;nguez R.</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lares_M/0/1/0/all/0/1">M. Lares</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beroiz_M/0/1/0/all/0/1">M. Beroiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabral_J/0/1/0/all/0/1">J. B. Cabral</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gurovich_S/0/1/0/all/0/1">S. Gurovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quinones_C/0/1/0/all/0/1">C. Qui&#xf1;ones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Artola_R/0/1/0/all/0/1">R. Artola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colazo_C/0/1/0/all/0/1">C. Colazo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneiter_M/0/1/0/all/0/1">M. Schneiter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girardini_C/0/1/0/all/0/1">C. Girardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tornatore_M/0/1/0/all/0/1">M. Tornatore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castellon_J/0/1/0/all/0/1">J. L. Nilo Castell&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lambas_D/0/1/0/all/0/1">D. Garc&#xed;a Lambas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_M/0/1/0/all/0/1">M. C. D&#xed;az</a> We present a comparison of several Difference Image Analysis (DIA) techniques, in combination with Machine Learning (ML) algorithms, applied to the identification of optical transients associated with gravitational wave events. Each technique is assessed based on the scoringRead More →

Non-thermal Dark Matter from Modified Early Matter Domination. (arXiv:1812.10522v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Allahverdi_R/0/1/0/all/0/1">Rouzbeh Allahverdi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Osinski_J/0/1/0/all/0/1">Jacek K. Osi&#x144;ski</a> Thermal freeze-out or freeze-in during a period of early matter domination can give rise to the correct dark matter abundance for $langle sigma_{rm ann} v rangle_{rm f} < 3 times 10^{-26}$ cm$^3$ s$^{-1}$. In the standard scenario, a single field that behaves like matter drives the early matter dominated era. However, in realistic models, this epoch may involve more than one field. In this paper, we study the effect of such a modification on the production of dark matter during early matter domination. We show that even aRead More →

Probing Cosmic Acceleration by Using Model-Independent Parametrizations and Three Kinds of Supernova Statistics Techniques. (arXiv:1812.10542v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_X/0/1/0/all/0/1">Xiaolin Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_S/0/1/0/all/0/1">Shuang Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wen_S/0/1/0/all/0/1">Sixiang Wen</a> In this work, we explore the evolution of the dark energy equation of state {omega} by using Chevalliear-PolarskiLinder (CPL) parametrization and the binned parametrizations. For binned parametrizations, we adopt three methods to choose the redshift interval: I. Ensure that “{Delta}z = const”, where {Delta}z is the width of each bin; II.Ensure that “n{Delta}z = const”, where n is the number of SNIa in each bin; III. Treat redshift discontinuity points as models parameters, i.e. “free {Delta}z”. For observational data, weRead More →

Time evolution of rotating and magnetized white dwarf stars. (arXiv:1812.10543v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Becerra_L/0/1/0/all/0/1">Laura Becerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boshkayev_K/0/1/0/all/0/1">Kuantay Boshkayev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rueda_J/0/1/0/all/0/1">Jorge. A. Rueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruffini_R/0/1/0/all/0/1">Remo Ruffini</a> We investigate the evolution of isolated, zero and finite temperature, massive, uniformly rotating and highly magnetized white dwarf stars under angular momentum loss driven by magnetic dipole braking. We consider the structure and thermal evolution of the white dwarf isothermal core taking also into account the nuclear burning and neutrino emission processes. We estimate the white dwarf lifetime before it reaches the condition either for a type Ia supernova explosion or for the gravitational collapse to a neutron star. We analyzeRead More →

Overstable Convective Modes of Rotating Hot Jupiters. (arXiv:1812.10598v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_U/0/1/0/all/0/1">Umin Lee</a> We calculate overstable convective modes of uniformly rotating hot Jupiters, which have a convective core and a thin radiative envelope. Convective modes in rotating planets have complex frequency $omega$ and are stabilized by rapid rotation so that their growth rates $proptoomega_{rm I}={rm Im}(omega)$ are much smaller than those for the non-rotating planets. The stabilized convective modes excite low frequency gravity waves in the radiative envelope by frequency resonance between them. We find that the convective modes that excite envelope gravity waves remain unstable even in the presence of non-adiabatic dissipations in the envelope.Read More →

Melanopogenesis: Dark Matter of (almost) any Mass and Baryonic Matter from the Evaporation of Primordial Black Holes weighing a Ton (or less). (arXiv:1812.10606v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Morrison_L/0/1/0/all/0/1">Logan Morrison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Profumo_S/0/1/0/all/0/1">Stefano Profumo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_Y/0/1/0/all/0/1">Yan Yu</a> The evaporation of primordial black holes with a mass in the $1 {rm gram}lesssim M_{rm PBH}lesssim$1000 kg range can lead to the production of dark matter particles of almost any mass in the range $0.1 {rm MeV}lesssim m_{rm DM}lesssim 10^{18}$ GeV with the right relic density at very early times, $taulesssim 10^{-10}$ s. We calculate, as a function of the primordial black holes mass and initial abundance, the combination of dark matterRead More →

Intra-Night Optical Variability Monitoring of Fermi Blazars: First Results from 1.3 m J C Bhattacharya Telescope. (arXiv:1812.10614v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Paliya_V/0/1/0/all/0/1">Vaidehi S. Paliya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stalin_C/0/1/0/all/0/1">C. S. Stalin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ajello_M/0/1/0/all/0/1">M. Ajello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaur_A/0/1/0/all/0/1">A. Kaur</a> We report the first results obtained from our campaign to characterize the intranight-optical variability (INOV) properties of {it Fermi}~detected blazars, using the observations from the recently commissioned 1.3 m J C Bhattacharya telescope (JCBT). During the first run, we were able to observe 17 blazars in the Bessel $R$ filter for $sim$137 hrs. Using $C$ and scaled $F$-statistics, we quantify the extent of INOV and derive the duty cycle (DC) which is theRead More →

Secondary eclipses of WASP-18b — Near Infrared observations with the Anglo Australian Telescope, the Magellan Clay Telescope and the LCOGT network. (arXiv:1812.10623v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kedziora_Chudczer_L/0/1/0/all/0/1">L. Kedziora-Chudczer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_G/0/1/0/all/0/1">G. Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailey_J/0/1/0/all/0/1">J. Bailey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayliss_D/0/1/0/all/0/1">D.D.R. Bayliss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tinney_C/0/1/0/all/0/1">C.G. Tinney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osip_D/0/1/0/all/0/1">D. Osip</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colon_K/0/1/0/all/0/1">K.D. Colon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shporer_A/0/1/0/all/0/1">A. Shporer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dragomir_D/0/1/0/all/0/1">D. Dragomir</a> We present new eclipse observations for one of the hottest “hot Jupiters” WASP-18b, for which previously published data from HST WFC3 and Spitzer have led to radically conflicting conclusions about the composition of this planet’s atmosphere. We measure eclipse depths of $0.15pm0.02%$ at $Ks$ and $0.07pm0.01%$ at $z’$ bands. Using the VSTAR line-by-line radiative transferRead More →

Influence of Ohmic and ambipolar heating on thermal structure of accretion discs. (arXiv:1812.10634v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Khaibrakhmanov_S/0/1/0/all/0/1">Sergey A. Khaibrakhmanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dudorov_A/0/1/0/all/0/1">Alexander E. Dudorov</a> We investigate dynamics of accretion discs of young stars with fossil large-scale magnetic field. Our magneto-gas-dynamic (MHD) model of the accretion discs includes equations of Shakura and Sunyaev, induction equation, equations of thermal and collisional ionization. Induction equation takes into account Ohmic and magnetic ambipolar diffusion, magnetic buoyancy. We also consider the influence of Ohmic and ambipolar heating on thermal structure of the accretion discs. We analyse the influence of considered dissipative MHD effects on the temperature of the accretion discs around classicalRead More →

CMB lensing bi-spectrum: assessing analytical predictions against full-sky lensing simulations. (arXiv:1812.10635v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Namikawa_T/0/1/0/all/0/1">Toshiya Namikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bose_B/0/1/0/all/0/1">Benjamin Bose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouchet_F/0/1/0/all/0/1">Fran&#xe7;ois R. Bouchet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takahashi_R/0/1/0/all/0/1">Ryuichi Takahashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taruya_A/0/1/0/all/0/1">Atsushi Taruya</a> Cosmic microwave background (CMB) lensing is an integrated effect whose kernel is greater than half the peak value in the range $1Read More →