Excitation of Planetary Obliquities Through Planet-Disk Interactions. (arXiv:1904.07338v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Millholland_S/0/1/0/all/0/1">Sarah Millholland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batygin_K/0/1/0/all/0/1">Konstantin Batygin</a> The tilt of a planet’s spin axis off its orbital axis (“obliquity”) is a basic physical characteristic that plays a central role in determining the planet’s global circulation and energy redistribution. Moreover, recent studies have also highlighted the importance of obliquities in sculpting not only the physical features of exoplanets but also their orbital architectures. It is therefore of key importance to identify and characterize the dominant processes of excitation of non-zero axial tilts. Here we highlight a simple mechanism that operates early on and is likely fundamental for manyRead More →

Investigating the Stellar Mass Growth Histories of Satellite Galaxies as a Function of Infall Time using Phase-Space. (arXiv:1904.07340v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Rory Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pacifici_C/0/1/0/all/0/1">Camilla Pacifici</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pasquali_A/0/1/0/all/0/1">Anna Pasquali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calderon_Castillo_P/0/1/0/all/0/1">Paula Calderon-Castillo</a> We compile a large sample of nearby galaxies that are satellites of hosts using a well known SDSS group catalogue. From this sample, we create an `ancient infallers’ and `recent infallers’ subsample, based on the mean infall time predicted from cosmological simulations for galaxies with their location in phase-space. We compare the stellar mass growth histories of the galaxies in these two subsamples, as determined from multi-wavelength SED fitting that uses a comprehensive libraryRead More →

A global view of the inner accretion/ejection flow around super massive black holes: radiation driven accretion disk winds in a physical context. (arXiv:1904.07341v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Giustini_M/0/1/0/all/0/1">Margherita Giustini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Proga_D/0/1/0/all/0/1">Daniel Proga</a> Understanding the physics and geometry of accretion and ejection around super massive black holes (SMBHs) is important to understand the evolution of active galactic nuclei (AGN) and therefore of the large scale structures of the Universe. We aim at providing a simple, coherent, and global view of the sub-parsec accretion/ejection flow in AGN with varying Eddington ratio, $dot{m}$ and black hole mass, $M_{BH}$. We make use of theoretical insights, results of numerical simulations, as wellRead More →

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) VIII. A less biased view of the early co-evolution of black holes and host galaxies. (arXiv:1904.07345v1 [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:+Onoue_M/0/1/0/all/0/1">Masafusa Onoue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matsuoka_Y/0/1/0/all/0/1">Yoshiki Matsuoka</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:+Strauss_M/0/1/0/all/0/1">Michael A. Strauss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imanishi_M/0/1/0/all/0/1">Masatoshi Imanishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kashikawa_N/0/1/0/all/0/1">Nobunari Kashikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fujimoto_S/0/1/0/all/0/1">Seiji Fujimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">Kotaro Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toba_Y/0/1/0/all/0/1">Yoshiki Toba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Umehata_H/0/1/0/all/0/1">Hideki Umehata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goto_T/0/1/0/all/0/1">Tomotsugu Goto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ueda_Y/0/1/0/all/0/1">Yoshihiro Ueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shirakata_H/0/1/0/all/0/1">Hikari Shirakata</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:+Greene_J/0/1/0/all/0/1">Jenny E. Greene</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harikane_Y/0/1/0/all/0/1">Yuichi Harikane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hashimoto_Y/0/1/0/all/0/1">Yasuhiro Hashimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ikarashi_S/0/1/0/all/0/1">Soh Ikarashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iono_D/0/1/0/all/0/1">Daisuke Iono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iwasawa_K/0/1/0/all/0/1">Kazushi Iwasawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_C/0/1/0/all/0/1">Chien-Hsiu Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minezaki_T/0/1/0/all/0/1">Takeo Minezaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakanishi_K/0/1/0/all/0/1">Kouichiro Nakanishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tamura_Y/0/1/0/all/0/1">Yoichi Tamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tang_J/0/1/0/all/0/1">Ji-Jia Tang</a>,Read More →

The Pulsating Eclipsing Binary TIC 309658221 in a 7.59 Day Orbit. (arXiv:1904.07362v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_J/0/1/0/all/0/1">Jae Woo Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kristiansen_M/0/1/0/all/0/1">Martti H. Kristiansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_K/0/1/0/all/0/1">Kyeongsoo Hong</a> We present a new eclipsing binary (EB) showing multiperiodic oscillations using the first three sectors of {it TESS} photometry. The eclipse and pulsation light curves of TIC 309658221 were modeled using an iterative method to obtain a consistent photometric solution. The {it TESS} target is a circular-orbit, detached binary system with a mass ratio of 0.349, an inclination angle of 80.42 deg, and a temperature difference of 847 K between the components. The primary component of the system lies near theRead More →

Effects of dynamical breaking in SUSY SU(5) to two standard models. (arXiv:1904.07371v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Kim_J/0/1/0/all/0/1">Jihn E. Kim</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Kyae_B/0/1/0/all/0/1">Bumseok Kyae</a> Supersymmetric (SUSY) models and dynamical breaking of symmetries have been used to explain hierarchies of mass scales. We find that a chiral representation, $bar{bf 10}, oplus, bar{bf 5}, oplus, 2cdot {bf 5}$ in SUSY SU(5) in the hidden sector, breaks global SUSY dynamically, by producing a composite field $phi$ below the SU(5) confinement scale. Starting with this dynamincally generated scale, we attempt to explain two vastly different mass scales in two standard models of physics, one in particle physics and the other in cosmology. GavitationalRead More →

A strange phenomenon of XZ Andromedae: two Keplerian periods with a 1:3 ratio. (arXiv:1904.07373v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_J/0/1/0/all/0/1">Jin-Zhao Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qian_S/0/1/0/all/0/1">Sheng-Bang Qian</a> Six mid-eclipse times of the eclipsing binary XZ And are obtained, which are analysed together with others collected from the literature. Two sets of cyclic variations with periods of 33.43 and 100.4 yr are found if a double-Keplerian model is used to fit the data. The 1:3 ratio of the periods suggests that both cyclic variations arise from dynamic motions of two companions rather than magnetic activity of the eclipsing pair. According to the double-Keplerian model, the companions have the masses of about 1.32Read More →

Modelling DESTINY+ interplanetary and interstellar dust measurements en route to the active asteroid (3200) Phaethon. (arXiv:1904.07384v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kruger_H/0/1/0/all/0/1">Harald Kr&#xfc;ger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Strub_P/0/1/0/all/0/1">Peter Strub</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Srama_R/0/1/0/all/0/1">Ralf Srama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_M/0/1/0/all/0/1">Masanori Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arai_T/0/1/0/all/0/1">Tomoko Arai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kimura_H/0/1/0/all/0/1">Hiroshi Kimura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirai_T/0/1/0/all/0/1">Takayuki Hirai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moragas_Klostermeyer_G/0/1/0/all/0/1">Georg Moragas-Klostermeyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altobelli_N/0/1/0/all/0/1">Nicolas Altobelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sterken_V/0/1/0/all/0/1">Veerle J. Sterken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agarwal_J/0/1/0/all/0/1">Jessica Agarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sommer_M/0/1/0/all/0/1">Maximilian Sommer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grun_E/0/1/0/all/0/1">Eberhard Gr&#xfc;n</a> The JAXA/ISAS spacecraft DESTINY$^+$ will be launched to the active asteroid (3200) Phaethon in 2022. Among the proposed core payload is the DESTINY+ Dust Analyzer (DDA) which is an upgrade of the Cosmic Dust Analyzer flown on the Cassini spacecraft to Saturn (Srama et al. 2011). We useRead More →

Self-gravitational Force Calculation of High-Order Accuracy for Infinitesimally Thin Gaseous Disks. (arXiv:1904.07400v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_H/0/1/0/all/0/1">Hsiang-Hsu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shiue_M/0/1/0/all/0/1">Ming-Cheng Shiue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_R/0/1/0/all/0/1">Rui-Zhu Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yen_C/0/1/0/all/0/1">Chien-Chang Yen</a> Self-gravitational force calculation for infinitesimally thin disks is important for studies on the evolution of galactic and protoplanetary disks. Although high-order methods have been developed for hydrodynamic and magneto-hydrodynamic equations, high-order improvement is desirable for solving self-gravitational forces for thin disks. In this work, we present a new numerical algorithm that is of linear complexity and of high-order accuracy. This approach is fast since the force calculation is associated with a convolution form, and the fast calculation can be achievedRead More →

Principal Components of Short-term Variability in Venus’ UV Albedo. (arXiv:1904.07413v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kopparla_P/0/1/0/all/0/1">Pushkar Kopparla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Y/0/1/0/all/0/1">Yeon Joo Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imamura_T/0/1/0/all/0/1">Takeshi Imamura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamazaki_A/0/1/0/all/0/1">Atsushi Yamazaki</a> We explore the dominant modes of variability in the observed albedo at the cloud tops of Venus using the Akatsuki UVI 283-nm and 365-nm observations, which are sensitive to SO2 and unknown UV absorber distributions respectively, over the period Dec 2016 to May 2018. The observations consist of images of the dayside of Venus, most often observed at intervals of 2 hours, but interspersed with longer gaps. The orbit of the spacecraft does not allow for continuous observation of the fullRead More →

Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?. (arXiv:1904.07465v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_K/0/1/0/all/0/1">KJ Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_J/0/1/0/all/0/1">JC Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yin_Z/0/1/0/all/0/1">ZQ Yin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feng_W/0/1/0/all/0/1">W Feng</a> Coronal heating is a big question for modern astronomy. Daily measurement of 985 solar spectral irradiances (SSIs) at the spectral intervals 1-39 nm and 116-2416 nm during March 1 2003 to October 28 2017 is utilized to investigate characteristics of solar rotation in the solar atmosphere by means of the Lomb ,-, Scargle periodogram method to calculate their power spectra. The rotation period of coronal plasma is obtained to be 26.3 days, and that of the solar atmosphere at theRead More →

The lowest detected stellar Fe abundance: The halo star SMSS J160540.18-144323.1. (arXiv:1904.07471v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nordlander_T/0/1/0/all/0/1">T. Nordlander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bessell_M/0/1/0/all/0/1">M.S. Bessell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_G/0/1/0/all/0/1">G.S. Da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mackey_A/0/1/0/all/0/1">A.D. Mackey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asplund_M/0/1/0/all/0/1">M. Asplund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casey_A/0/1/0/all/0/1">A.R. Casey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiti_A/0/1/0/all/0/1">A. Chiti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ezzeddine_R/0/1/0/all/0/1">R. Ezzeddine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frebel_A/0/1/0/all/0/1">A. Frebel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lind_K/0/1/0/all/0/1">K. Lind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">A.F. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murphy_S/0/1/0/all/0/1">S.J. Murphy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Norris_J/0/1/0/all/0/1">J.E. Norris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmidt_B/0/1/0/all/0/1">B.P. Schmidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yong_D/0/1/0/all/0/1">D. Yong</a> We report the discovery of SMSS J160540.18-144323.1, a new ultra-metal poor halo star discovered with the SkyMapper telescope. We measure [Fe/H] = -6.2 +- 0.2 (1D LTE), the lowest ever detected abundance of iron in a star. The star is strongly carbon-enhanced, [C/Fe] = 3.9 +-Read More →

Are primordial black holes produced by entropy perturbations in single field inflationary models?. (arXiv:1904.07503v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vallejo_Pena_S/0/1/0/all/0/1">Sergio Andr&#xe9;s Vallejo-Pe&#xf1;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romano_A/0/1/0/all/0/1">Antonio Enea Romano</a> We show that in single field inflationary models the super-horizon evolution of curvature perturbations on comoving slices $mathcal{R}$, which can cause the production of primordial black holes (PBH), is not due to entropy perturbations but to a fast variation of the equation of state $w$. As an example we analyze curvature and entropy perturbations in quasi-inflection inflation, showing that while entropy perturbations are decreasing, $mathcal{R}$ can grow on super-horizon scales. This happens in the time interval during which a sufficiently fast decreaseRead More →

Nebular Line Emission During the Epoch of Reionization. (arXiv:1904.07504v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wilkins_S/0/1/0/all/0/1">Stephen M. Wilkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lovell_C/0/1/0/all/0/1">Christopher C. Lovell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fairhurst_C/0/1/0/all/0/1">Ciaran Fairhurst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feng_Y/0/1/0/all/0/1">Yu Feng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matteo_T/0/1/0/all/0/1">Tiziana Di Matteo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Croft_R/0/1/0/all/0/1">Rupert Croft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuusisto_J/0/1/0/all/0/1">Jussi Kuusisto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vijayan_A/0/1/0/all/0/1">Aswin P. Vijayan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thomas_P/0/1/0/all/0/1">Peter Thomas</a> Nebular emission lines associated with galactic HII regions carry information about both physical properties of the ionised gas and the source of ionising photons as well as providing the opportunity of measuring accurate redshifts and thus distances once a cosmological model is assumed. While nebular line emission has been extensively studied at lower redshift there are currently only few constraints within the epoch ofRead More →

Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning. (arXiv:1904.07505v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ho_W/0/1/0/all/0/1">Wynn C.G. Ho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wijngaarden_M/0/1/0/all/0/1">M.J.P. Wijngaarden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_P/0/1/0/all/0/1">Philip Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heinke_C/0/1/0/all/0/1">Craig O. Heinke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Page_D/0/1/0/all/0/1">Dany Page</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beznogov_M/0/1/0/all/0/1">Mikhail Beznogov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patnaude_D/0/1/0/all/0/1">Daniel J. Patnaude</a> The study of how neutron stars cool over time can provide invaluable insights into fundamental physics such as the nuclear equation of state and superconductivity and superfluidity. A critical relation in neutron star cooling is the one between observed surface temperature and interior temperature. This relation is determined by the composition of the neutron star envelope and can be influenced by the process of diffusiveRead More →

Constraining Chaplygin models using diffuse supernova neutrino background. (arXiv:1904.07510v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Yang_N/0/1/0/all/0/1">Nan Yang</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Jia_J/0/1/0/all/0/1">Junji Jia</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Liu_X/0/1/0/all/0/1">Xionghui Liu</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Zhang_H/0/1/0/all/0/1">Hongbao Zhang</a> In this work, we examine the possibility of using the diffuse supernova neutrino background (DSNB) to test the Chaplygin gas (CG) models of the Universe. With a typical star formation rate $psi(z)$, supernova rate $R_{mathrm{SN}}(z)$ and single supernova neutrino spectrum $mathrm{d} N(E_nu)/mathrm{d} E_nu$, the DSNB flux spectrum $n(E_nu)$ in three categories of CG models, the generalized CG (GCG), modified CG (MCG) and extended CG (ECG) models, are studied. It is found that generally the flux spectra take a form similar to a Fermi-DiracRead More →

The mass-richness relation of optically-selected clusters from weak gravitational lensing and abundance with Subaru HSC first-year data. (arXiv:1904.07524v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Murata_R/0/1/0/all/0/1">Ryoma Murata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oguri_M/0/1/0/all/0/1">Masamune Oguri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishimichi_T/0/1/0/all/0/1">Takahiro Nishimichi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takada_M/0/1/0/all/0/1">Masahiro Takada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandelbaum_R/0/1/0/all/0/1">Rachel Mandelbaum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+More_S/0/1/0/all/0/1">Surhud More</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shirasaki_M/0/1/0/all/0/1">Masato Shirasaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishizawa_A/0/1/0/all/0/1">Atsushi J. Nishizawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osato_K/0/1/0/all/0/1">Ken Osato</a> Constraining the relation between the richness $N$ and the halo mass $M$ over a wide redshift range for optically-selected clusters is a key ingredient for cluster-related science in optical surveys, including the Subaru Hyper Suprime-Cam (HSC) survey. We measure stacked weak lensing profiles around 1747 HSC CAMIRA clusters over a redshift range of $0.1leq z_{rm cl}leq 1.0$ withRead More →

Modelling the multi-wavelength emissions from PSR B1259-63/LS 2883: the effects of the stellar disc on shock radiations. (arXiv:1904.07527v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_A/0/1/0/all/0/1">A. M. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takata_J/0/1/0/all/0/1">J. Takata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yi_S/0/1/0/all/0/1">S. X. Yi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_Y/0/1/0/all/0/1">Y. W. Yu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_K/0/1/0/all/0/1">K. S. Cheng</a> PSR B1259-63/LS 2883 is an elliptical pulsar/Be star binary and emits broadband emissions from radio to TeV $gamma$-rays. The massive star possesses an equatorial disc, which is inclined with the orbital plane of the pulsar. The non-thermal emission from the system is believed to be produced by the pulsar wind shock and the double-peak profiles in the X-ray and TeV $gamma$-ray light curves are related to theRead More →

The rare extended radio-loud narrow-line Seyfert 1 galaxy SDSS J1030+5516 at high resolution. (arXiv:1904.07540v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gabanyi_K/0/1/0/all/0/1">Krisztina &#xc9;va Gab&#xe1;nyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frey_S/0/1/0/all/0/1">S&#xe1;ndor Frey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veres_P/0/1/0/all/0/1">P&#xe9;ter Veres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moor_A/0/1/0/all/0/1">Attila Mo&#xf3;r</a> Recently, Rakshit et al. (2018) reported the discovery of SDSS J103024.95$+$551622.7, a radio-loud narrow-line Seyfert 1 galaxy having a $sim 100$ kpc scale double-lobed radio structure. Here we analyse archival radio interferometric imaging data taken with the Very Large Array (VLA) at 5 GHz, and with the Very Long Baseline Array (VLBA) at 4.3 and 7.6 GHz. Two hotspots and a compact core are detected with the VLA at arcsec scale, while a single milliarcsec-scale compact radioRead More →

The footprint of cometary dust analogues: II. Morphology as a tracer of tensile strength and application to dust collection by the Rosetta spacecraft. (arXiv:1904.07543v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ellerbroek_L/0/1/0/all/0/1">L.E. Ellerbroek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gundlach_B/0/1/0/all/0/1">B. Gundlach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Landeck_A/0/1/0/all/0/1">A. Landeck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dominik_C/0/1/0/all/0/1">C. Dominik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blum_J/0/1/0/all/0/1">J. Blum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Merouane_S/0/1/0/all/0/1">S. Merouane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilchenbach_M/0/1/0/all/0/1">M. Hilchenbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+John_H/0/1/0/all/0/1">H. John</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veen_H/0/1/0/all/0/1">H. A. van Veen</a> The structure of cometary dust is a tracer of growth processes in the formation of planetesimals. Instrumentation on board the Rosetta mission to comet 67P/Churyumov- Gerasimenko captured dust particles and analysed them in situ. However, these deposits are a product of a collision within the instrument. We conducted laboratory experiments withRead More →