RAS_WEB (Page 4,386)

The Gravitational waves merger time distribution of binary neutron star systems. (arXiv:1903.11614v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Beniamini_P/0/1/0/all/0/1">Paz Beniamini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piran_T/0/1/0/all/0/1">Tsvi Piran</a> Binary neutron stars (BNS) mergers are prime sites for r-process nucleosynthesis. As such their rate determines the chemical evolution of heavy elements in the Milky Way. The merger rate of BNS is a convolution of their birth rate and the gravitational radiation spiral-in delay time. Using the observed population of Galactic BNS we show here that at late times ($tgtrsim 1$ Gyr) the gravitational wave delay time distribution (DTD) follows the expected $ t^{-1}$. However, a significant excess of rapidly merging systems (between $40-60%$ of theRead More →

The COMBS survey I: Chemical Origins of Metal-Poor Stars in the Galactic Bulge. (arXiv:1903.11615v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lucey_M/0/1/0/all/0/1">Madeline Lucey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hawkins_K/0/1/0/all/0/1">Keith Hawkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ness_M/0/1/0/all/0/1">Melissa Ness</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asplund_M/0/1/0/all/0/1">Martin Asplund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bensby_T/0/1/0/all/0/1">Thomas Bensby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casagrande_L/0/1/0/all/0/1">Luca Casagrande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feltzing_S/0/1/0/all/0/1">Sofia Feltzing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freeman_K/0/1/0/all/0/1">Kenneth C. Freeman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_C/0/1/0/all/0/1">Chiaki Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">Anna F. Marino</a> Chemistry and kinematic studies can determine the origins of stellar population across the Milky Way. The metallicity distribution function of the bulge indicates that it comprises multiple populations, the more metal-poor end of which is particularly poorly understood. It is currently unknown if metal-poor bulge stars ([Fe/H] $Read More →

The Dynamical Roche Lobe in Hierarchical Triples. (arXiv:1903.11618v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stefano_R/0/1/0/all/0/1">Rosanne Di Stefano</a> The Roche lobe formalism describes mass transfer from one star to another. We develop an extension to hierarchical triples, considering the case in which a star donates mass to a companion which is itself a binary. The L1 point moves as the inner binary rotates, and the Roche lobe pulsates with the period of the inner binary. Signatures of mass transfer may therefore be imprinted with the orbital period of the inner binary. For some system parameters, the pulsing Roche lobe can drive mass transfer at high rates. Systems undergoing this typeRead More →

A Survey of Hot Gas in the Universe. (arXiv:1903.11630v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bregman_J/0/1/0/all/0/1">Joel N. Bregman</a> (University of Michigan), <a href="http://arxiv.org/find/astro-ph/1/au:+Hodges_Kluck_E/0/1/0/all/0/1">Edmund Hodges-Kluck</a> (University of Maryland/NASA GSFC), <a href="http://arxiv.org/find/astro-ph/1/au:+Oppenheimer_B/0/1/0/all/0/1">Benjamin D. Oppenheimer</a> (University of Colorado), <a href="http://arxiv.org/find/astro-ph/1/au:+Brenneman_L/0/1/0/all/0/1">Laura Brenneman</a> (Harvard-Smithsonian), <a href="http://arxiv.org/find/astro-ph/1/au:+Kollmeier_J/0/1/0/all/0/1">Juna Kollmeier</a> (Carnegie), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Jiangtao Li</a> (University of Michigan), <a href="http://arxiv.org/find/astro-ph/1/au:+Ptak_A/0/1/0/all/0/1">Andrew Ptak</a> (NASA GSFC), <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Randall Smith</a> (Harvard-Smithsonian), <a href="http://arxiv.org/find/astro-ph/1/au:+Temi_P/0/1/0/all/0/1">Pasquale Temi</a> (NASA Ames), <a href="http://arxiv.org/find/astro-ph/1/au:+Vikhlinin_A/0/1/0/all/0/1">Alexey Vikhlinin</a> (Harvard-Smithsonian), <a href="http://arxiv.org/find/astro-ph/1/au:+Wijers_N/0/1/0/all/0/1">Nastasha Wijers</a> (Leiden) A large fraction of the baryons and most of the metals in the Universe are unaccounted for. They likely lie in extended galaxy halos, galaxy groups, and the cosmic web, and measuring their nature is essential to understandingRead More →

GMRT Low-frequency Imaging of an Extended Sample of X-shaped Radio Galaxies. (arXiv:1903.11632v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lal_D/0/1/0/all/0/1">Dharam V. Lal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sebastian_B/0/1/0/all/0/1">Biny Sebastian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheung_C/0/1/0/all/0/1">C. C. Cheung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rao_A/0/1/0/all/0/1">A. Pramesh Rao</a> We present a low-frequency imaging study of an extended sample of X-shaped radio sources using the Giant Metrewave radio telescope (GMRT) at two frequencies (610 and 240 MHz). The sources were drawn from a Very Large Array FIRST-selected sample and extends an initial GMRT study at the same frequencies, of 12 X-shaped radio galaxies predominantly from the 3CR catalog (Lal & Rao 2007). Both the intensity maps and spectral index maps of the 16 newly observed sourcesRead More →

High-speed photometry of faint cataclysmic variables – IX. Targets from multiple transient surveys. (arXiv:1903.11643v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Paterson_K/0/1/0/all/0/1">K. Paterson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Woudt_P/0/1/0/all/0/1">P. A. Woudt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Warner_B/0/1/0/all/0/1">B. Warner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breytenbach_H/0/1/0/all/0/1">H. Breytenbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilligan_C/0/1/0/all/0/1">C. K. Gilligan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Motsoaledi_M/0/1/0/all/0/1">M. Motsoaledi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thorstensen_J/0/1/0/all/0/1">J. R. Thorstensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Worters_H/0/1/0/all/0/1">H. L. Worters</a> We present high-speed photometric observations of 25 cataclysmic variables detected by the All Sky Automated Search for Super-Novae (ASAS-SN), the Mobile Astronomical System of the TElescope-Robot (MASTER) and the Catalina Real-Time Transient Survey (CRTS). From these observations we determine 16 new orbital periods and 1 new superhump period. Two systems (ASASSN-14ik and ASASSN-14ka) have outburst periods of approximately 1 month, with aRead More →

First observations of irregular surface of interplanetary shocks at ion scales by Cluster. (arXiv:1903.11653v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+Kajdic_P/0/1/0/all/0/1">Primo&#x17e; Kajdi&#x10d;</a>, <a href="http://arxiv.org/find/physics/1/au:+Preisser_L/0/1/0/all/0/1">Luis Preisser</a>, <a href="http://arxiv.org/find/physics/1/au:+Blanco_Cano_X/0/1/0/all/0/1">X&#xf3;chitl Blanco-Cano</a>, <a href="http://arxiv.org/find/physics/1/au:+Burgess_D/0/1/0/all/0/1">David Burgess</a>, <a href="http://arxiv.org/find/physics/1/au:+Trotta_D/0/1/0/all/0/1">Domenico Trotta</a> We present the first observational evidence of the irregular surface of interplanetary (IP) shocks by using multi-spacecraft observations of the Cluster mission. In total we discuss observations of four IP shocks that exhibit moderate Alfv’enic Mach numbers (M$_Aleq$6.5). Three of them are high-$beta$ shocks with upstream $beta$ = 2.2–3.7. During the times when these shocks were observed, the Cluster spacecraft formed constellations with inter-spacecraft separations ranging from less than one upstream ion inertial length (d$_i$)Read More →

An axisymmetric limit for the width of the Hadley cell on planets with large obliquity and long seasonality. (arXiv:1903.11656v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Guendelman_I/0/1/0/all/0/1">Ilai Guendelman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaspi_Y/0/1/0/all/0/1">Yohai Kaspi</a> Hadley cells dominate the meridional circulation of terrestrial atmospheres. The Solar System terrestrial atmospheres, Venus, Earth, Mars and Titan, exhibit a large variety in the strength, width and seasonality of their Hadley circulation. Despite the Hadley cell being thermally driven, in all planets, the ascending branch does not coincide with the warmest latitude, even in cases with very long seasonality (e.g., Titan) or very small thermal inertia (e.g., Mars). In order to understand the characteristics of the Hadley circulationRead More →

A Uniform Retrieval Analysis of Ultracool Dwarfs. III. Properties of Y-Dwarfs. (arXiv:1903.11658v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zalesky_J/0/1/0/all/0/1">Joseph A. Zalesky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Line_M/0/1/0/all/0/1">Michael R. Line</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_A/0/1/0/all/0/1">Adam C. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patience_J/0/1/0/all/0/1">Jennifer Patience</a> Ultra-cool brown dwarfs offer a unique window into understanding substellar atmospheric physics and chemistry. Their strong molecular absorption bands at infrared wavelengths, Jupiter-like radii, cool temperatures, and lack of complicating stellar irradiation, make them ideal test-beds for understanding Jovian-like atmospheres. Here we report the findings of a uniform atmospheric retrieval analysis on a set of 14 Y and T-dwarfs observed with the Hubble Space Telescope Wide Field Camera 3 instrument. From our retrieval analysis, we find theRead More →

The impact of Stellar feedback from velocity-dependent ionised gas maps. — A MUSE view of Haro 11. (arXiv:1903.11662v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Menacho_V/0/1/0/all/0/1">V. Menacho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ostlin_G/0/1/0/all/0/1">G. &#xd6;stlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bik_A/0/1/0/all/0/1">A. Bik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruna_L/0/1/0/all/0/1">L. Della Bruna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melinder_J/0/1/0/all/0/1">J. Melinder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adamo_A/0/1/0/all/0/1">A. Adamo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hayes_M/0/1/0/all/0/1">M. Hayes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herenz_E/0/1/0/all/0/1">E.C. Herenz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergvall_N/0/1/0/all/0/1">N. Bergvall</a> We have used the capability of the MUSE instrument to explore the impact of stellar feedback at large scales in Haro 11, a galaxy under extreme starburst condition and one of the first galaxies where Lyman continuum (LyC) has been detected. Using Ha, [OIII] and [OI] emission lines from deep MUSE observations, we have constructed a sequence ofRead More →

Realizing the Unique Potential of ALMA to Probe the Gas Reservoir of Planet Formation. (arXiv:1903.11692v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cleeves_L/0/1/0/all/0/1">L. Ilsedore Cleeves</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loomis_R/0/1/0/all/0/1">Ryan Loomis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Teague_R/0/1/0/all/0/1">Richard Teague</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_K/0/1/0/all/0/1">Ke Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergin_E/0/1/0/all/0/1">Edwin Bergin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oberg_K/0/1/0/all/0/1">Karin Oberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brogan_C/0/1/0/all/0/1">Crystal Brogan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hunter_T/0/1/0/all/0/1">Todd Hunter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aikawa_Y/0/1/0/all/0/1">Yuri Aikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_S/0/1/0/all/0/1">Sean Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bae_J/0/1/0/all/0/1">Jaehan Bae</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergner_J/0/1/0/all/0/1">Jennifer Bergner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaherty_K/0/1/0/all/0/1">Kevin Flaherty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guzman_V/0/1/0/all/0/1">Viviana Guzman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">Jane Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hogerheijde_M/0/1/0/all/0/1">Michiel Hogerheijde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lai_S/0/1/0/all/0/1">Shih-Ping Lai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_L/0/1/0/all/0/1">Laura Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_L/0/1/0/all/0/1">Luca Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salyk_C/0/1/0/all/0/1">Colette Salyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwarz_K/0/1/0/all/0/1">Kamber Schwarz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_J/0/1/0/all/0/1">Jonathan Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">David Wilner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wootten_A/0/1/0/all/0/1">Al Wootten</a> Understanding the origin of the astonishing diversity of exoplanets is a key question for the comingRead More →

Observing Black Holes Spin. (arXiv:1903.11704v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Reynolds_C/0/1/0/all/0/1">Christopher S. Reynolds</a> The spin of a black hole retains the memory of how the black hole grew, and can be a potent source of energy for powering relativistic jets. To understand the diagnostic power and astrophysical significance of black hole spin, however, we must first devise observational methods for measuring spin. Here, I describe the current state of black hole spin measurements, highlighting the progress made by X-ray astronomers, as well as the current excitement of gravitational wave and radio astronomy based techniques. Today’s spin measurements are already constraining models for the growth of supermassive black holesRead More →

Updated extraction of the APOGEE 1.5273 {mu}m diffuse interstellar band: a Planck view on the carrier depletion in dense cores. (arXiv:1903.11707v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Elyajouri_M/0/1/0/all/0/1">Meriem Elyajouri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lallement_R/0/1/0/all/0/1">Rosine Lallement</a> The latest SDSS/APOGEE data release DR14 has provided an increased number of stellar spectra in the H band and associated stellar models using an innovative algorithm known as The Cannon. We took advantage of these novelties to extract the 15 273 {AA} near-infrared DIB and to study its link with dust extinction and emission. We modified our automated fitting methods dedicated to hot stars and used in earlier studies with some adaptations motivated by the change fromRead More →

Deriving Iodine-free spectra for high-resolution echelle spectrographs. (arXiv:1903.11718v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_M/0/1/0/all/0/1">Mat&#xed;as R. D&#xed;az</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shectman_S/0/1/0/all/0/1">Stephen A. Shectman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Butler_R/0/1/0/all/0/1">R. Paul Butler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">James S. Jenkins</a> We describe a new method to derive clean, iodine-free spectra directly from observations acquired using high-resolution echelle spectrographs equipped with iodine cells. The main motivation to obtain iodine-free spectra is to use portions of the spectrum that are superimposed with the dense forest of iodine absorption lines, in order to retrieve lines that can be used to monitor the magnetic activity of the star, helping to validate candidate planets. In short, we provide a straight-forward methodology to clean the spectraRead More →

How Martian araneiforms get their shapes: morphological analysis and diffusion-limited aggregation model for polar surface erosion. (arXiv:1903.11721v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Portyankina_G/0/1/0/all/0/1">Ganna Portyankina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hansen_C/0/1/0/all/0/1">Candice J. Hansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aye_K/0/1/0/all/0/1">Klaus-Michael Aye</a> Araneiforms are radially converging systems of branching troughs exhibiting fractal properties. They are found exclusively in the Southern polar regions of Mars and believed to be result of multiple repetitions of cold CO2 gas jets eruptions. Araneiform troughs get carved by the overpressurized gas rushing underneath a seasonal ice layer towards a newly created opening. Current work is an attempt to quantitatively analyze araneiforms patterns and model their formation mechanism. The dendritic quality of most araneiforms areRead More →

Recasting $H_0$ tension as $Omega_m$ tension at low $z$. (arXiv:1903.11743v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Colgain_E/0/1/0/all/0/1">Eoin &#xd3; Colg&#xe1;in</a> Inspired by the recent observation that local measurements of the Hubble constant $H_0$ and the Planck CMB value based on $Lambda$CDM show a discrepancy at $4.4 , sigma$ cite{Riess:2019cxk}, we study $Lambda$CDM at low redshift. Concretely, we expand $Lambda$CDM perturbatively at small $z$ and perform a two-parameter fit of the distance modulus to Pantheon data for a running cut-off $z_{textrm{max}} leq 0.3$. Moving beyond the Hubble constant $H_0$, we shift focus to matter density $Omega_m$, noting foremost that its best-fit value is sensitive to the cut-off. For $z_{textrm{max}} > 0.1$,Read More →

Tomography of the Cosmic Dawn and Reionization Eras with Multiple Tracers. (arXiv:1903.11744v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_T/0/1/0/all/0/1">Tzu-Ching Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beane_A/0/1/0/all/0/1">Angus Beane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dore_O/0/1/0/all/0/1">Olivier Dore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lidz_A/0/1/0/all/0/1">Adam Lidz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mas_Ribas_L/0/1/0/all/0/1">Lluis Mas-Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_G/0/1/0/all/0/1">Guochao Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alvarez_M/0/1/0/all/0/1">Marcelo Alvarez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thakur_R/0/1/0/all/0/1">Ritoban Basu Thakur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_P/0/1/0/all/0/1">Philippe Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bethermin_M/0/1/0/all/0/1">Matthieu Bethermin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bock_J/0/1/0/all/0/1">Jamie Bock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bradford_C/0/1/0/all/0/1">Charles M. Bradford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Breysse_P/0/1/0/all/0/1">Patrick Breysse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgarella_D/0/1/0/all/0/1">Denis Burgarella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charmandaris_V/0/1/0/all/0/1">Vassilis Charmandaris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_Y/0/1/0/all/0/1">Yun-Ting Cheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cleary_K/0/1/0/all/0/1">Kieran Cleary</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cooray_A/0/1/0/all/0/1">Asantha Cooray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">Abigail Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ewall_Wice_A/0/1/0/all/0/1">Aaron Ewall-Wice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_X/0/1/0/all/0/1">Xiaohui Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finkelstein_S/0/1/0/all/0/1">Steve Finkelstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furlanetto_S/0/1/0/all/0/1">Steve Furlanetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hewitt_J/0/1/0/all/0/1">Jacqueline Hewitt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hunacek_J/0/1/0/all/0/1">Jonathon Hunacek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korngut_P/0/1/0/all/0/1">Phil Korngut</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kovetz_E/0/1/0/all/0/1">Ely Kovetz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hallinan_G/0/1/0/all/0/1">Gregg Hallinan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heneka_C/0/1/0/all/0/1">Caroline Heneka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagache_G/0/1/0/all/0/1">Guilaine Lagache</a>,Read More →

Note on a solution to domain wall problem with the Lazarides-Shafi mechanism in axion dark matter models. (arXiv:1903.11753v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Chatterjee_C/0/1/0/all/0/1">Chandrasekhar Chatterjee</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Higaki_T/0/1/0/all/0/1">Tetsutaro Higaki</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nitta_M/0/1/0/all/0/1">Muneto Nitta</a> Axion is a promising candidate of dark matter. After the Peccei-Quinn symmetry breaking, axion strings are formed and attached by domain walls when the temperature of the universe becomes comparable to the QCD scale. Such objects can cause cosmological disasters if they are long-lived. As a solution for it, the Lazarides-Shafi mechanism is often discussed through introduction of a new non-Abelian (gauge) symmetry. We study this mechanism in detail and show configuration of strings and walls. EvenRead More →

Models and Simulations for the Photometric LSST Astronomical Time Series Classification Challenge (PLAsTiCC). (arXiv:1903.11756v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kessler_R/0/1/0/all/0/1">R. Kessler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayan_G/0/1/0/all/0/1">G. Narayan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avelino_A/0/1/0/all/0/1">A. Avelino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bachelet_E/0/1/0/all/0/1">E. Bachelet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biswas_R/0/1/0/all/0/1">R. Biswas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_P/0/1/0/all/0/1">P. J. Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chernoff_D/0/1/0/all/0/1">D. F. Chernoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connolly_A/0/1/0/all/0/1">A. J. Connolly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_M/0/1/0/all/0/1">M. Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daniel_S/0/1/0/all/0/1">S. Daniel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stefano_R/0/1/0/all/0/1">R. Di Stefano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drout_M/0/1/0/all/0/1">M. R. Drout</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galbany_L/0/1/0/all/0/1">L. Galbany</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Gaitan_S/0/1/0/all/0/1">S. Gonz&#xe1;lez-Gait&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_M/0/1/0/all/0/1">M. L. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hlozek_R/0/1/0/all/0/1">R. Hlo&#x17e;ek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishida_E/0/1/0/all/0/1">E. E. O. Ishida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guillochon_J/0/1/0/all/0/1">J. Guillochon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jha_S/0/1/0/all/0/1">S. W. Jha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_D/0/1/0/all/0/1">D. O. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mandel_K/0/1/0/all/0/1">K. S. Mandel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muthukrishna_D/0/1/0/all/0/1">D. Muthukrishna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+OGrady_A/0/1/0/all/0/1">A. O&#x27;Grady</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peters_C/0/1/0/all/0/1">C. M. Peters</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pierel_J/0/1/0/all/0/1">J. R. Pierel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ponder_K/0/1/0/all/0/1">K.Read More →

Testing the Gravitational Weak Equivalence Principle in the Standard-Model Extension with Binary Pulsars. (arXiv:1903.11760v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Shao_L/0/1/0/all/0/1">Lijing Shao</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Bailey_Q/0/1/0/all/0/1">Quentin G. Bailey</a> The Standard-Model Extension provides a framework to systematically investigate possible violation of the Lorentz symmetry. Concerning gravity, the linearized version was extensively examined. We here cast the first set of experimental bounds on the nonlinear terms in the field equation from the anisotropic cubic curvature couplings. These terms introduce body-dependent accelerations for self-gravitating objects, thus violating the gravitational weak equivalence principle (GWEP). Novel phenomena, that are absent in the linearized gravity, remain experimentally unexplored. We constrain them with precise binary-orbit measurements from pulsarRead More →