RAS_WEB (Page 4,561)

Nitrogen-containing Anions and Tholin Growth in Titan’s Ionosphere: Implications for Cassini CAPS-ELS Observations. (arXiv:1902.05585v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dubois_D/0/1/0/all/0/1">David Dubois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carrasco_N/0/1/0/all/0/1">Nathalie Carrasco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourgalais_J/0/1/0/all/0/1">J&#xe9;r&#xe9;my Bourgalais</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vettier_L/0/1/0/all/0/1">Ludovic Vettier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_R/0/1/0/all/0/1">Ravindra T. Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wellbrock_A/0/1/0/all/0/1">Anne Wellbrock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coates_A/0/1/0/all/0/1">Andrew J. Coates</a> The Cassini Plasma Spectrometer (CAPS) Electron Spectrometer (ELS) instrument onboard Cassini revealed an unexpected abundance of negative ions above 950 km in Titan’s ionosphere. textit{In situ} measurements indicated the presence of negatively charged particles with mass-over-charge ratios up to 13,800 textit{u/q}. At present, only a handful of anions have been characterized by photochemical models, consisting mainly of C$_n$H$^-$ carbon chain and C$_{n-1}$N$^-$ cyano compounds ($n=2-6$); their formationRead More →

Photoionization Emission Models for the Cyg X-3 X-ray Spectrum. (arXiv:1902.05589v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kallman_T/0/1/0/all/0/1">T. Kallman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCollough_M/0/1/0/all/0/1">M. McCollough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koljonen_K/0/1/0/all/0/1">K. Koljonen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liedahl_D/0/1/0/all/0/1">D. Liedahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_J/0/1/0/all/0/1">J. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paerels_F/0/1/0/all/0/1">F. Paerels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pooley_G/0/1/0/all/0/1">G. Pooley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sako_M/0/1/0/all/0/1">M. Sako</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulz_N/0/1/0/all/0/1">N. Schulz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trushkin_S/0/1/0/all/0/1">S. Trushkin</a> We present model fits to the X-ray line spectrum of the well known High Mass X-ray binary Cyg X-3. The primary observational dataset is a spectrum taken with the $Chandra$ X-ray Observatory High Energy Transmission Grating (HETG) in 2006, though we compare it to all the other observations of this source taken so far by this instrument. We show that the density must beRead More →

A theoretical model for realistic local climates. (arXiv:1902.05598v1 [physics.ao-ph]) <a href="http://arxiv.org/find/physics/1/au:+Bona_G/0/1/0/all/0/1">Gabriele Di Bona</a>, <a href="http://arxiv.org/find/physics/1/au:+Giacobbe_A/0/1/0/all/0/1">Andrea Giacobbe</a> We address the question of writing a model that —considering the doubly-periodic forcing induced by solar radiation and the laws of irradiance and conduction— reproduces realistic annual and daily modulations of temperatures on the surface of a small region on Earth. The interest in such exercise on theoretical and numeric integration is twofold: the application of this model can give realistic projections of local climate evolution on Earth or on a chosen exoplanet; the creation of such model can shed some light on the effective exchanges of energy amongRead More →

Limits on Mode Coherence Due to a Non-static Convection Zone. (arXiv:1902.05615v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Montgomery_M/0/1/0/all/0/1">M. H. Montgomery</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hermes_J/0/1/0/all/0/1">J. J. Hermes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winget_D/0/1/0/all/0/1">D. E. Winget</a> The standard theory of pulsations deals with the frequencies and growth rates of infinitesimal perturbations in a stellar model. Modes which are calculated to be linearly driven should increase their amplitudes exponentially with time; the fact that nearly constant amplitudes are usually observed is evidence that nonlinear mechanisms inhibit the growth of finite amplitude pulsations. Models predict that the mass of DAV convection zones is very sensitive to temperature (i.e., $M_{text{CZ}} propto T_{text{eff}}^{-90}$) leading to the possibility that even “small amplitude”Read More →

Mapping the Interstellar Reddening and Extinction towards Baade’s Window Using Minimum Light Colors of ab-type RR Lyrae Stars. Revelations from the De-reddened Color-Magnitude Diagrams. (arXiv:1902.05637v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Saha_A/0/1/0/all/0/1">Abhijit Saha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vivas_A/0/1/0/all/0/1">A. Katherina Vivas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olszewski_E/0/1/0/all/0/1">Edward W. Olszewski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_V/0/1/0/all/0/1">Verne Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olsen_K/0/1/0/all/0/1">Knut Olsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blum_R/0/1/0/all/0/1">Robert Blum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valdes_F/0/1/0/all/0/1">Francisco Valdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Claver_J/0/1/0/all/0/1">Jenna Claver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calamida_A/0/1/0/all/0/1">Annalisa Calamida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walker_A/0/1/0/all/0/1">Alistair R. Walker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matheson_T/0/1/0/all/0/1">Thomas Matheson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayan_G/0/1/0/all/0/1">Gautham Narayan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soraisam_M/0/1/0/all/0/1">Monika Soraisam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_K/0/1/0/all/0/1">Katia Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Axelrod_T/0/1/0/all/0/1">T. Axelrod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bloom_J/0/1/0/all/0/1">Joshua S. Bloom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cenko_S/0/1/0/all/0/1">S. Bradley Cenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frye_B/0/1/0/all/0/1">Brenda Frye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juric_M/0/1/0/all/0/1">Mario Juric</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaleida_C/0/1/0/all/0/1">Catherine Kaleida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kunder_A/0/1/0/all/0/1">Andrea Kunder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_A/0/1/0/all/0/1">Adam Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nidever_D/0/1/0/all/0/1">David Nidever</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ridgway_S/0/1/0/all/0/1">Stephen Ridgway</a> We haveRead More →

The SAMI Galaxy Survey: Satellite galaxies undergo little structural change during their quenching phase. (arXiv:1902.05652v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cortese_L/0/1/0/all/0/1">L. Cortese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sande_J/0/1/0/all/0/1">J. van de Sande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagos_C/0/1/0/all/0/1">C. P. Lagos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catinella_B/0/1/0/all/0/1">B. Catinella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_L/0/1/0/all/0/1">L. J. M. Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Croom_S/0/1/0/all/0/1">S. .M. Croom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brough_S/0/1/0/all/0/1">S. Brough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bryant_J/0/1/0/all/0/1">J. J. Bryant</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lawrence_J/0/1/0/all/0/1">J. S. Lawrence</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Owers_M/0/1/0/all/0/1">M. S. Owers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richards_S/0/1/0/all/0/1">S. N. Richards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sweet_S/0/1/0/all/0/1">S. M. Sweet</a> At fixed stellar mass, satellite galaxies show higher passive fractions than centrals, suggesting that environment is directly quenching their star formation. Here, we investigate whether satellite quenching is accompanied by changes in stellar spin (quantified by the ratio of the rotational toRead More →

Magnetic field vector maps of nearby spiral galaxies. (arXiv:1902.05728v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nakanishi_H/0/1/0/all/0/1">Hiroyuki Nakanishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurahara_K/0/1/0/all/0/1">Kohei Kurahara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anraku_K/0/1/0/all/0/1">Kenta Anraku</a> We present a method for determining directions of magnetic field vectors in a spiral galaxy using two synchrotron polarization maps, an optical image, and a velocity field. The orientation of the transverse magnetic field is determined with a synchrotron polarization map of higher frequency band and the $180^circ$-ambiguity is solved by using sign of the Rotation Measure (RM) after determining geometrical orientation of a disk based on a assumption of trailing spiral arms. The advantage of this method is that direction of magnetic vector for eachRead More →

Constraining Single Dark Matter Particle Mass by Primordial Gravitational Wave. (arXiv:1902.05738v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">Changhong Li</a> We report on a new relation between dark matter (DM) particle mass, $m_chi$, and the tensor-to-scalar ratio of cosmic microwave background (CMB) anisotropies, $r$. Once $r$ is determined in a future search of primordial gravitational wave (PGW), $m_chi$ can be constrained by using this relation. Due to the resonance interplay between metric and DM density perturbations, a small local fluctuation of spacetime can be generated in a pair production of DM particles. Such fluctuations, arising from the DM pair productions, encode information of DM mass and slightly change the amplitudeRead More →

Wormhole as a possible accelerator of high-energy cosmic-ray particles. (arXiv:1902.05742v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Savelova_A/0/1/0/all/0/1">A.A. Kirillov E.P. Savelova</a> We present the simplest topological classification of wormholes and demonstrate that in open Friedmann models the genus $ngeq 1$ wormholes are stable and do not require the presence of exotic forms of matter, or any modification of general relativity. We show that such wormholes may also possess magnetic fields. It is found that when the wormhole gets into a galaxy or a surrounding region, it works as an accelerator of charged particles, or as a generator of synchrotron radiation. Estimates show that the threshold energy of such an acceleratorRead More →

The core and stellar mass functions in massive collapsing filaments. (arXiv:1902.05744v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ntormousi_E/0/1/0/all/0/1">Evangelia Ntormousi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hennebelle_P/0/1/0/all/0/1">Patrick Hennebelle</a> The connection between the pre-stellar core mass function (CMF) and the stellar initial mass function (IMF) lies at the heart of all star formation theories. In this paper, we study the earliest phases of star formation with a series of high-resolution numerical simulations that include the formation of sinks. In particular, we focus on the transition from cores to sinks within a massive molecular filament. We compare the CMF and IMF between magnetized and unmagnetized simulations, and between different resolutions. We find that selecting cores based onRead More →

Ruprecht 147 DANCe I. Members, empirical isochrone, luminosity and mass distributions. (arXiv:1902.05753v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Olivares_J/0/1/0/all/0/1">J. Olivares</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouy_H/0/1/0/all/0/1">H. Bouy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarro_L/0/1/0/all/0/1">L. M. Sarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miret_Roig_N/0/1/0/all/0/1">N. Miret-Roig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berihuete_A/0/1/0/all/0/1">A. Berihuete</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">E. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barrado_D/0/1/0/all/0/1">D. Barrado</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:+Tamura_M/0/1/0/all/0/1">M. Tamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_L/0/1/0/all/0/1">L. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beletsky_Y/0/1/0/all/0/1">Y. Beletsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serre_S/0/1/0/all/0/1">S. Serre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuillandre_J/0/1/0/all/0/1">J.C. Cuillandre</a> Context. Ruprecht 147 is the oldest (2.5 Gyr) open cluster in the solar vicinity (< 300 pc), making it an important target for stellar evolution studies and exoplanet searches. Aims. Derive a census of members and the luminosity, mass, and spatial distributions of the cluster. Methods. We use an astro-photometric data setRead More →

Evidence for Electron Landau Damping in Space Plasma Turbulence. (arXiv:1902.05785v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+Chen_C/0/1/0/all/0/1">C. H. K. Chen</a>, <a href="http://arxiv.org/find/physics/1/au:+Klein_K/0/1/0/all/0/1">K. G. Klein</a>, <a href="http://arxiv.org/find/physics/1/au:+Howes_G/0/1/0/all/0/1">G. G. Howes</a> How turbulent energy is dissipated in weakly collisional space and astrophysical plasmas is a major open question. Here, we present the application of a field-particle correlation technique to directly measure the transfer of energy between the turbulent electromagnetic field and electrons in the Earth’s magnetosheath, the region of solar wind downstream of the Earth’s bow shock. The measurement of the secular energy transfer from the parallel electric field as a function of electron velocity shows a signature consistent with Landau damping.Read More →

Neutrinos below 100 TeV from the southern sky employing refined veto techniques to IceCube data. (arXiv:1902.05792v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_IceCube/0/1/0/all/0/1">IceCube Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Aartsen_M/0/1/0/all/0/1">M. G. Aartsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ackermann_M/0/1/0/all/0/1">M. Ackermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_J/0/1/0/all/0/1">J. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguilar_J/0/1/0/all/0/1">J. A. Aguilar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahlers_M/0/1/0/all/0/1">M. Ahlers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahrens_M/0/1/0/all/0/1">M. Ahrens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alispach_C/0/1/0/all/0/1">C. Alispach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altmann_D/0/1/0/all/0/1">D. Altmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andeen_K/0/1/0/all/0/1">K. Andeen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_T/0/1/0/all/0/1">T. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansseau_I/0/1/0/all/0/1">I. Ansseau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anton_G/0/1/0/all/0/1">G. Anton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arguelles_C/0/1/0/all/0/1">C. Arg&#xfc;elles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auffenberg_J/0/1/0/all/0/1">J. Auffenberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Axani_S/0/1/0/all/0/1">S. Axani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Backes_P/0/1/0/all/0/1">P. Backes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bagherpour_H/0/1/0/all/0/1">H. Bagherpour</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">X. Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbano_A/0/1/0/all/0/1">A. Barbano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barwick_S/0/1/0/all/0/1">S. W. Barwick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baum_V/0/1/0/all/0/1">V. Baum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bay_R/0/1/0/all/0/1">R. Bay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beatty_J/0/1/0/all/0/1">J. J. Beatty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_K/0/1/0/all/0/1">K.-H. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tjus_J/0/1/0/all/0/1">J. Becker Tjus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+BenZvi_S/0/1/0/all/0/1">S. BenZvi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berley_D/0/1/0/all/0/1">D.Read More →

Nonthermal emission in the lobes of Fornax A. (arXiv:1902.05797v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Persic_M/0/1/0/all/0/1">Massimo Persic</a> (INAF Trieste, Italy, Physics &amp; Astronomy Dept., Bologna U., Italy), <a href="http://arxiv.org/find/astro-ph/1/au:+Rephaeli_Y/0/1/0/all/0/1">Yoel Rephaeli</a> (School of Physics &amp; Astronomy, Tel Aviv U., Israel, Center for Astrophysics &amp; Space Sciences, UC San Diego, USA) Current measurements of the spectral energy distribution in radio, X-and-gamma-ray provide a sufficiently wide basis for determining basic properties of energetic electrons and protons in the extended lobes of the radio galaxy Fornax A. Of particular interest is establishing observationally, for the first time, the level of contribution of energetic protons to the extended emission observed by the Fermi satellite.Read More →

M31 circum-nuclear region: a molecular survey with the IRAM-interferometer. (arXiv:1902.05822v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dassa_Terrier_J/0/1/0/all/0/1">Julien Dassa-Terrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melchior_A/0/1/0/all/0/1">Anne-Laure Melchior</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combes_F/0/1/0/all/0/1">Francoise Combes</a> We analyse molecular observations performed at IRAM interferometer in CO(1-0) of the circum-nuclear region (within 250 pc) of Andromeda, with 2.9 arcsec = 11 pc resolution. We detect 12 molecular clumps in this region, corresponding to a total molecular mass of (8.4 +- 0.4) x 10**4 Msol. They follow the Larson’s mass-size relation, but lie well above the velocity-size relation. We discuss that these clumps are probably not virialised, but transient agglomerations of smaller entities that might be virialised. Three of these clumps have beenRead More →

Extra-tidal structures around the Gaia Sausage candidate globular cluster NGC6779 (M56). (arXiv:1902.05824v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Piatti_A/0/1/0/all/0/1">Andr&#xe9;s E. Piatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carballo_Bello_J/0/1/0/all/0/1">Julio A. Carballo-Bello</a> We present results on the stellar density radial profile of the outer regions of NGC6779, a Milky Way globular cluster recently proposed as a candidate member of the Gaia Sausage structure, a merger remnant of a massive dwarf galaxy with the Milky Way. Taking advantage of the Pan-STARRS PS1 public astrometric and photometric catalogue, we built the radial profile for the outermost cluster regions using horizontal branch and main sequence stars, separately, in order to probe for different profile trends because of difference stellarRead More →

Submillimeter spectroscopy and astronomical searches of vinyl mercaptan, C$_2$H$_3$SH. (arXiv:1902.05833v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_Drumel_M/0/1/0/all/0/1">Marie-Aline Martin-Drumel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_K/0/1/0/all/0/1">Kin Long Kelvin Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belloche_A/0/1/0/all/0/1">Arnaud Belloche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zingsheim_O/0/1/0/all/0/1">Oliver Zingsheim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thorwirth_S/0/1/0/all/0/1">Sven Thorwirth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mueller_H/0/1/0/all/0/1">Holger S.P. Mueller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewen_F/0/1/0/all/0/1">Frank Lewen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garrod_R/0/1/0/all/0/1">Robin T. Garrod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">Karl M. Menten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCarthy_M/0/1/0/all/0/1">Michael C. McCarthy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlemmer_S/0/1/0/all/0/1">Stephan Schlemmer</a> We have extended the pure rotational investigation of the two isomers syn and anti vinyl mercaptan to the millimeter domain using a frequency-multiplication spectrometer. The species were produced by a radiofrequency discharge in 1,2-ethanedithiol. Additional transitions have been re-measured in the centimeter band using Fourier-transform microwave spectroscopy to better determine rest frequencies of transitions withRead More →

Anisotropic $2$-form dark energy. (arXiv:1902.05846v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Almeida_J/0/1/0/all/0/1">Juan P. Beltr&#xe1;n Almeida</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Guarnizo_A/0/1/0/all/0/1">Alejandro Guarnizo</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Kase_R/0/1/0/all/0/1">Ryotaro Kase</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Tsujikawa_S/0/1/0/all/0/1">Shinji Tsujikawa</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Valenzuela_Toledo_C/0/1/0/all/0/1">C&#xe9;sar A. Valenzuela-Toledo</a> We study the dynamics of dark energy in the presence of a 2-form field coupled to a canonical scalar field $phi$. We consider the coupling proportional to $e^{-mu phi/M_{rm pl}} H_{alpha beta gamma}H^{alpha beta gamma}$ and the scalar potential $V(phi) propto e^{-lambda phi/M_{rm pl}}$, where $H_{alpha beta gamma}$ is the 2-form field strength, $mu, lambda$ are constants, and $M_{rm pl}$ is the reduced Planck mass. We show the existence of an anisotropic matter-dominated scaling solution followed by a stable accelerated fixedRead More →

Optical detection of a GMRT-detected candidate high-redshift radio galaxy with 3.6-m Devasthal optical telescope. (arXiv:1902.05856v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Omar_A/0/1/0/all/0/1">A. Omar</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Saxena_A/0/1/0/all/0/1">A. Saxena</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Chand_K/0/1/0/all/0/1">K. Chand</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Paswan_A/0/1/0/all/0/1">A. Paswan</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Rottgering_H/0/1/0/all/0/1">H. J. A. Rottgering</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Duncan_K/0/1/0/all/0/1">K. J. Duncan</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_T/0/1/0/all/0/1">T. S. Kumar</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Krishnareddy_B/0/1/0/all/0/1">B. Krishnareddy</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Pant_J/0/1/0/all/0/1">J. Pant</a> (1) ((1) ARIES, Nainital (2) Leiden University, Leiden (3) IUCAA, Pune) We report optical observations of TGSS J1054+5832, a candidate high-redshift ($z=4.8pm2$) steep-spectrum radio galaxy, in $r$ and $i$ bands using the faint object spectrograph and camera mounted on 3.6-m Devasthal Optical Telescope (DOT). The source previously detected at 150Read More →