RAS_WEB (Page 4,570)

A Curved 150 Parsec Long Jet in the Double-Peaked Emission-Line AGN KISSR 434. (arXiv:1812.11074v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kharb_P/0/1/0/all/0/1">Preeti Kharb</a> (NCRA-TIFR), <a href="http://arxiv.org/find/astro-ph/1/au:+Vaddi_S/0/1/0/all/0/1">Sravani Vaddi</a> (NCRA-TIFR), <a href="http://arxiv.org/find/astro-ph/1/au:+Sebastian_B/0/1/0/all/0/1">Biny Sebastian</a> (NCRA-TIFR), <a href="http://arxiv.org/find/astro-ph/1/au:+Subramanian_S/0/1/0/all/0/1">Smitha Subramanian</a> (IIA), <a href="http://arxiv.org/find/astro-ph/1/au:+Das_M/0/1/0/all/0/1">Mousumi Das</a> (IIA), <a href="http://arxiv.org/find/astro-ph/1/au:+Paragi_Z/0/1/0/all/0/1">Zsolt Paragi</a> (JIVE) Double-peaked emission lines in the narrow- and/or broad-line spectra of AGN have been suggested to arise due to disky broad/narrow line regions, jet-medium interaction, or the presence of binary supermassive black holes. We present the results from 1.5 and 4.9 GHz phase-referenced Very Long Baseline Interferometry (VLBI) observations of the Seyfert type 2 galaxy KISSR 434, which exhibits double-peaked emission lines in its optical spectrum. WeRead More →

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A. (arXiv:1812.11083v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Utrobin_V/0/1/0/all/0/1">Victor Utrobin</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Wongwathanarat_A/0/1/0/all/0/1">Annop Wongwathanarat</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Janka_H/0/1/0/all/0/1">H.-Thomas Janka</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Mueller_E/0/1/0/all/0/1">Ewald Mueller</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ertl_T/0/1/0/all/0/1">T. Ertl</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Woosley_S/0/1/0/all/0/1">Stan Woosley</a> (3) ((1) MPI Astrophysics, Garching, (2) ITEP, Moscow, (3) University of California, Santa Cruz) In the framework of the neutrino-driven explosion mechanism, we study the dependence of macroscopic mixing on the structure of different blue supergiant progenitors and compare the results with observations of SN 1987A. All of our seven 3D neutrino-driven explosion models, with SN 1987A-like explosion energies, produce Ni-56 in rough agreement with the amount deducedRead More →

M subdwarf research. I. Identification, modified classification system, and sample construction. (arXiv:1812.11088v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">Shuo Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_A/0/1/0/all/0/1">A-Li Luo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Comte_G/0/1/0/all/0/1">Georges Comte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gizis_J/0/1/0/all/0/1">John E. Gizis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_R/0/1/0/all/0/1">Rui Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Y/0/1/0/all/0/1">Yinbi Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qin_L/0/1/0/all/0/1">Li Qin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kong_X/0/1/0/all/0/1">Xiao Kong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_Y/0/1/0/all/0/1">Yu Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yi_Z/0/1/0/all/0/1">Zhenping Yi</a> We propose a revision of the system developed by L’epine et al. (2007) for spectroscopic M subdwarf classification. Based on an analysis of subdwarf spectra and templates from Savcheva et al. (2014), we show thatthe CaH1 feature originally proposed by Gizis (1997) is important in selecting reliable cool subdwarf spectra. This index should be used in combination with the [TiO5, CaH2+CaH3]Read More →

Chiral effects in magnetized quantum spinor matter in particle and astroparticle physics. (arXiv:1812.11099v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Sitenko_Y/0/1/0/all/0/1">Yu. A. Sitenko</a> Quantum spinor matter in extremal conditions (high densities and temperatures, presence of strong magnetic fields) have drawn the attention of researchers in diverse areas of contemporary physics, ranging from cosmology, high-energy and astroparticle physics to condensed matter physics. We study an impact of the confining boundary conditions on the properties of physical systems with hot dense magnetized ultrarelativistic spinor matter and elucidate a significant role of boundaries for such systems. Quantum spinor matter in extremal conditions (high densities and temperatures, presence of strong magnetic fields) have drawnRead More →

Evidence of Hubble flow-like motion of young stellar populations away from the Perseus arm. (arXiv:1812.11102v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Roman_Zuniga_C/0/1/0/all/0/1">Carlos Rom&#xe1;n-Z&#xfa;&#xf1;iga</a> (1,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Roman_Lopes_A/0/1/0/all/0/1">Alexandre Roman-Lopes</a> (2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Tapia_M/0/1/0/all/0/1">Mauricio Tapia</a> (1,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_J/0/1/0/all/0/1">Jes&#xfa;s Hern&#xe1;ndez</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_Preciado_V/0/1/0/all/0/1">Valeria Ram&#xed;rez-Preciado</a> ((1) Instituto de Astronom&#xed;a UNAM, Unidad Acad&#xe9;mica en Ensenada BC, Mexico, (2) Departamento de F&#xed;sica y Astronom&#xed;a, Universidad La Serena Chile, (3) Programa de Estancias de Investigaci&#xf3;n (PREI), DGAPA-UNAM, Mexico) In this letter we present evidence of coherent outward motion of a sample of young stars ($tRead More →

Foraging for dark matter in large volume liquid scintillator neutrino detectors with multiscatter events. (arXiv:1812.09325v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Bramante_J/0/1/0/all/0/1">Joseph Bramante</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Broerman_B/0/1/0/all/0/1">Benjamin Broerman</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kumar_J/0/1/0/all/0/1">Jason Kumar</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Lang_R/0/1/0/all/0/1">Rafael F. Lang</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Pospelov_M/0/1/0/all/0/1">Maxim Pospelov</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Raj_N/0/1/0/all/0/1">Nirmal Raj</a> We show that dark matter with a per-nucleon scattering cross section $gtrsim 10^{-28}~{rm cm^2}$ could be discovered by liquid scintillator neutrino detectors like BOREXINO, SNO+, and JUNO. Due to the large dark matter fluxes admitted, these detectors could find dark matter with masses up to $10^{21}$ GeV, surpassing the mass sensitivity of current direct detection experiments (such as XENON1T and PICO) by over two orders of magnitude. We derive theRead More →

Emergent long-range interactions in Bose-Einstein Condensates. (arXiv:1812.09332v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Berezhiani_L/0/1/0/all/0/1">Lasha Berezhiani</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Khoury_J/0/1/0/all/0/1">Justin Khoury</a> We consider a massive complex scalar field with contact interactions with a source and show that, upon Bose-Einstein condensation, there is an emergent long-range interaction between sources. This interaction becomes long-range in the limit of vanishing self-interaction between Bose-Einstein constituents. More generally, the range is given by $ell^{-1}propto sqrt{lambda n/m}$, with $lambda$ being the 2-body self-interaction coupling constant, $n$ the particle number density in the condensate, and $m$ the mass of the condensed particles. Naively this may sound surprising since in $lambdarightarrow 0$ limit gapless excitations of the condensate have dispersionRead More →

Collider and Gravitational Wave Complementarity in Exploring the Singlet Extension of the Standard Model. (arXiv:1812.09333v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Alves_A/0/1/0/all/0/1">Alexandre Alves</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ghosh_T/0/1/0/all/0/1">Tathagata Ghosh</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Guo_H/0/1/0/all/0/1">Huai-Ke Guo</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Sinha_K/0/1/0/all/0/1">Kuver Sinha</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Vagie_D/0/1/0/all/0/1">Daniel Vagie</a> We present a dedicated complementarity study of gravitational wave and collider measurements of the simplest extension of the Higgs sector: the singlet scalar augmented Standard Model. We study the following issues: (i) the electroweak phase transition patterns admitted by the model, and the proportion of parameter space for each pattern; (ii) the regions of parameter space that give detectable gravitational waves at future space-based detectors; and (iii) the current and future collider measurements ofRead More →

Baryogenesis, Dark Matter, and Flavor Structure in Non-thermal Moduli Cosmology. (arXiv:1812.09341v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Chen_M/0/1/0/all/0/1">Mu-Chun Chen</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Takhistov_V/0/1/0/all/0/1">Volodymyr Takhistov</a> The appearance of scalar/moduli fields in the early universe, as motivated by string theory, naturally leads to non-thermal “moduli cosmology”. Such cosmology provides a consistent framework where the generation of radiation, baryons, and dark matter can occur while maintaining successful Big Bang Nucleosynthesis and avoiding the cosmological moduli problem. We present a relatively economical construction with moduli cosmology, building on a variety of string-inspired components (e.g. supersymmetry, discrete symmetries, Green-Schwarz anomaly cancellation). We address a range of outstanding problems of particle physics and cosmology simultaneously, including theRead More →

ISW in $Lambda$CDM or something else?. (arXiv:1812.09348v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Soltan_A/0/1/0/all/0/1">Andrzej M. So&#x142;tan</a> We investigate a correlation between the Planck’s CMB temperature map and statistics based on the space density of quasars in the SDSS catalogue. A positive signal at $3,sigma$ is found. Amplitude of the correlation indicates that the rms of temperature fluctuations associated with the quasars distributed between $1500$ and $3000$ Mpc likely exceed $11-12,mu$K. The calculations are not related with any particular structures like supervoids in the quasars distribution. Although, the estimates are subject to sizable uncertainties, the signal seems to exceed the predictions of the Integrated Sachs-Wolfe effect for the standard $Lambda$CMBRead More →

Globular cluster systems as tracers of the evolutionary history in NGC 3258 and NGC 3268. (arXiv:1812.09364v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Caso_J/0/1/0/all/0/1">Juan Pablo Caso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bassino_L/0/1/0/all/0/1">Lilia P. Bassino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_M/0/1/0/all/0/1">Mat&#xed;as G&#xf3;mez</a> We present a new photometric study of NGC 3258 and NGC 3268 globular cluster systems (GCSs), using images in filters $B,C,V,R,I$ and $z’$, obtained from four different telescopes. The wide spatial coverage allow us to estimate the whole extension of both GCSs more precisely than in previous works, and new values for the richness of GCs subpopulations. We find differences in the azimuthal distribution between blue (metal-poor) and red (metal-rich) globular clusters (GCs), and confirm that radialRead More →

He white dwarfs with large H contamination: Convective mixing or accretion?. (arXiv:1812.09405v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wachlin_F/0/1/0/all/0/1">F. C. Wachlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vauclair_G/0/1/0/all/0/1">G. Vauclair</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vauclair_S/0/1/0/all/0/1">S. Vauclair</a> White dwarfs are compact objects with atmospheres containing mainly light elements, hydrogen or helium. Because of their surface high gravitational field, heavy elements diffuse downwards in a very short timescale compared to the evolutionary timescale, leaving the lightest ones on the top of the envelope. This results in the main classification of white dwarfs as hydrogen rich or helium rich. But many helium rich white dwarfs show also the presence of hydrogen traces in their atmosphere, whose origin is still unsettled. HereRead More →

HATS-71b: A giant planet transiting an M3 dwarf star in TESS Sector 1. (arXiv:1812.09406v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bakos_G/0/1/0/all/0/1">G. &#xc1;. Bakos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayliss_D/0/1/0/all/0/1">D. Bayliss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bento_J/0/1/0/all/0/1">J. Bento</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhatti_W/0/1/0/all/0/1">W. Bhatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brahm_R/0/1/0/all/0/1">R. Brahm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Csubry_Z/0/1/0/all/0/1">Z. Csubry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espinoza_N/0/1/0/all/0/1">N. Espinoza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartman_J/0/1/0/all/0/1">J. D. Hartman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Th. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jordan_A/0/1/0/all/0/1">A. Jord&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mancini_L/0/1/0/all/0/1">L. Mancini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penev_K/0/1/0/all/0/1">K. Penev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rabus_M/0/1/0/all/0/1">M. Rabus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkis_P/0/1/0/all/0/1">P. Sarkis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suc_V/0/1/0/all/0/1">V. Suc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Val_Borro_M/0/1/0/all/0/1">M. de Val-Borro</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:+Butler_R/0/1/0/all/0/1">R. P. Butler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crane_J/0/1/0/all/0/1">J. Crane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Durkan_S/0/1/0/all/0/1">S. Durkan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shectman_S/0/1/0/all/0/1">S. Shectman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">J. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lazar_J/0/1/0/all/0/1">J. L&#xe1;z&#xe1;r</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Papp_I/0/1/0/all/0/1">I. Papp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sari_P/0/1/0/all/0/1">P. S&#xe1;ri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">G. Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderspek_R/0/1/0/all/0/1">R. Vanderspek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">D. W. Latham</a>, <aRead More →

ROSETTA/OSIRIS observations of the 67P nucleus during the April 2016 flyby: high-resolution spectrophotometry. (arXiv:1812.09415v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Feller_C/0/1/0/all/0/1">C. Feller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fornasier_S/0/1/0/all/0/1">S. Fornasier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrari_S/0/1/0/all/0/1">S. Ferrari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasselmann_P/0/1/0/all/0/1">P.H. Hasselmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barucci_A/0/1/0/all/0/1">A. Barucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massironi_M/0/1/0/all/0/1">M. Massironi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deshapriya_J/0/1/0/all/0/1">J.D.P Deshapriya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sierks_H/0/1/0/all/0/1">H. Sierks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naletto_G/0/1/0/all/0/1">G. Naletto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lamy_P/0/1/0/all/0/1">P. L. Lamy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodrigo_R/0/1/0/all/0/1">R. Rodrigo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koschny_D/0/1/0/all/0/1">D. Koschny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davidsson_B/0/1/0/all/0/1">B.J.R. Davidsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertaux_J/0/1/0/all/0/1">J.-L. Bertaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertini_I/0/1/0/all/0/1">I. Bertini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodewits_D/0/1/0/all/0/1">D. Bodewits</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cremonese_G/0/1/0/all/0/1">G. Cremonese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deppo_V/0/1/0/all/0/1">V. Da Deppo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Debei_S/0/1/0/all/0/1">S. Debei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cecco_M/0/1/0/all/0/1">M. De Cecco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fulle_M/0/1/0/all/0/1">M. Fulle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_P/0/1/0/all/0/1">P. J. Guti&#xe9;rrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guttler_C/0/1/0/all/0/1">C. G&#xfc;ttler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ip_W/0/1/0/all/0/1">W.-H. Ip</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keller_H/0/1/0/all/0/1">H. U. Keller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lara_L/0/1/0/all/0/1">L. M. Lara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lazzarin_M/0/1/0/all/0/1">M. Lazzarin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Moreno_J/0/1/0/all/0/1">J. J.Read More →

Multi-epoch VLBI of a double maser super burst. (arXiv:1812.09454v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Burns_R/0/1/0/all/0/1">Ross A. Burns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayandina_O/0/1/0/all/0/1">Olga Bayandina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orosz_G/0/1/0/all/0/1">Gabor Orosz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olech_M/0/1/0/all/0/1">Mateusz Olech</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Immer_K/0/1/0/all/0/1">Katharina Immer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanchard_J/0/1/0/all/0/1">Jay Blanchard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marcote_B/0/1/0/all/0/1">Benito Marcote</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Langevelde_H/0/1/0/all/0/1">Huib van Langevelde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirota_T/0/1/0/all/0/1">Tomoya Hirota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_K/0/1/0/all/0/1">Kee-Tae Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valtts_I/0/1/0/all/0/1">Irina Valtts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shakhvorostova_N/0/1/0/all/0/1">Nadya Shakhvorostova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rudnitskii_G/0/1/0/all/0/1">Georgij Rudnitskii</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Volvach_A/0/1/0/all/0/1">Alexandr Volvach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Volvach_L/0/1/0/all/0/1">Larisa Volvach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacLeod_G/0/1/0/all/0/1">Gordon MacLeod</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chibueze_J/0/1/0/all/0/1">James O. Chibueze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Surcis_G/0/1/0/all/0/1">Gabriele Surcis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kramer_B/0/1/0/all/0/1">Busaba Kramer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baan_W/0/1/0/all/0/1">Willem Baan</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:+Kurtz_S/0/1/0/all/0/1">Stan Kurtz</a> In a rare and spectacular display, two well-known massive star forming regions, W49N and G25.65+1.05, recently underwent maser ‘super burst’ – their fluxesRead More →