TARDIS Paper II: Synergistic Density Reconstruction from Lyman-alpha Forest and Spectroscopic Galaxy Surveys with Applications to Protoclusters and the Cosmic Web. (arXiv:2007.15994v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Horowitz_B/0/1/0/all/0/1">Benjamin Horowitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">Benjamin Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_K/0/1/0/all/0/1">Khee-Gan Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kooistra_R/0/1/0/all/0/1">Robin Kooistra</a> In this work we expand upon the Tomographic Absorption Reconstruction and Density Inference Scheme (TARDIS) in order to include multiple tracers while reconstructing matter density fields at Cosmic Noon (z ~ 2-3). In particular, we jointly reconstruct the underlying density field from simulated Lyman-Alpha forest observations at $zsim 2.5$ and an overlapping galaxy survey. We find that these data are synergistic, with the Lyman Alpha forest providing reconstruction of lowRead More →

Theoretical Study of Extensive Air Shower Effects in Atmosphere by Simulating the Lateral structure of Several Cosmic Radiations. (arXiv:2007.16004v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jassim_H/0/1/0/all/0/1">Hassanen Abdulhussaen Jassim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Al_Rubaiee_A/0/1/0/all/0/1">A. A. Al-Rubaiee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Al_Alawy_I/0/1/0/all/0/1">Iman Tarik Al-Alawy</a> Extensive air showers (EAS) are a cascade of electromagnetic radiation and ionized particles that produced in the atmosphere through the interaction of a primary cosmic ray with the atom of nucleus in the air producing a huge amount of secondary particles such as X-ray, electrons, neutrons, muons, alpha particles, etc. In this work, EAS effects were demonstrated by estimating the lateral distribution function (LDF) at ultrahigh energies of the various cosmic ray particles.Read More →

Low mass strange stars and the compact star 1E1207.4-5209. (arXiv:2007.16022v1 [nucl-th]) <a href="http://arxiv.org/find/nucl-th/1/au:+Pereira_F/0/1/0/all/0/1">F. I. M Pereira</a> We study the anomalous mass defects in the first (ascendant) branch of stellar sequences of static strange stars. We employ the nonperturbative equation of state derived in the framework of the Field Correlator Method to describe the hydrostatic equilibrium of the strange matter. The large distance static $q{bar q}$ potential $V_1$ and the gluon condensate $G_2$ are the model parameters that characterize the equation of state. An attempt is made to determine, from the surface gravitational redshift measurements, the ratio $({cal P}/{cal E})_C$ at the center of strange stars.Read More →

SpaceX Just Completed a Static Fire of Starship Prototype SN5. Next Comes the Hop SpaceX successfully completed a static fire test with its SN5, which will be followed shortly by a hop test! The post SpaceX Just Completed a Static Fire of Starship Prototype SN5. Next Comes the Hop appeared first on Universe Today. Universe Today Go to SourceRead More →

Black hole fails to do its job Astronomers have discovered what can happen when a giant black hole does not intervene in the life of a galaxy cluster. Using NASA’s Chandra X-ray Observatory and other telescopes they have shown that passive black hole behavior may explain a remarkable torrent of star formation occurring in a distant cluster of galaxies. phys.org Go to SourceRead More →

ALMA captures stirred-up planet factory Planet-forming environments can be much more complex and chaotic than previously expected. This is evidenced by a new image of the star RU Lup, made with the Atacama Large Millimeter/submillimeter Array (ALMA). phys.org Go to SourceRead More →

Unequal neutron-star mergers create unique ‘bang’ in simulations When two neutron stars slam together, the result is sometimes a black hole that swallows all but the gravitational evidence of the collision. However, in a series of simulations, an international team of researchers including a Penn State scientist determined that these typically quiet—at least in terms of radiation we can detect on Earth—collisions can sometimes be far noisier. phys.org Go to SourceRead More →

How Loop Quantum Gravity Could Match Anomalies in the CMB with Large Structures in the Modern Universe A strange celestial tension could be caused by a cosmic tango between events at very small and very large scales. The post How Loop Quantum Gravity Could Match Anomalies in the CMB with Large Structures in the Modern Universe appeared first on Universe Today. Universe Today Go to SourceRead More →

Searching for where very unequal mass black hole binaries come from The direct detection of gravitational waves from at least eleven sources during the past five years has offered spectacular confirmation of Einstein’s model of gravity and space-time, while the modeling of these events has provided information on star formation, gamma-ray bursts,neutron stars, the age of the universe, and even verification of ideas about how very heavy elements are produced. The majority of these gravitational wave events arose from the merger of two black holes of comparable masses in an orbiting pair. Near-equal mass pairs are strongly preferred in models of binary black hole formation,Read More →

Interstellar medium of SDSS J2310+1855 explored with ALMA Using the ALMA Observatory, an international team of astronomers has conducted an observational campaign of interstellar medium (ISM) in a host galaxy of a high-redshift quasar known as SDSS J231038.88+185519.7 (SDSS J2310+1855 for short). Results of the observations, published July 24 on arXiv.org, could improve the knowledge of the properties and nature of this quasar. phys.org Go to SourceRead More →

Reaching thermal noise at ultra-low radio frequencies: the Toothbrush radio relic downstream of the shock front. (arXiv:2007.16043v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gasperin_F/0/1/0/all/0/1">F. de Gasperin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brunetti_G/0/1/0/all/0/1">G. Brunetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruggen_M/0/1/0/all/0/1">M. Bruggen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weeren_R/0/1/0/all/0/1">R. van Weeren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williams_W/0/1/0/all/0/1">W. L. Williams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botteon_A/0/1/0/all/0/1">A. Botteon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuciti_V/0/1/0/all/0/1">V. Cuciti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dijkema_T/0/1/0/all/0/1">T. J. Dijkema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edler_H/0/1/0/all/0/1">H. Edler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iacobelli_M/0/1/0/all/0/1">M. Iacobelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kang_H/0/1/0/all/0/1">H. Kang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Offringa_A/0/1/0/all/0/1">A. Offringa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orru_E/0/1/0/all/0/1">E. Orru</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pizzo_R/0/1/0/all/0/1">R. Pizzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rafferty_D/0/1/0/all/0/1">D. Rafferty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rottgering_H/0/1/0/all/0/1">H. Rottgering</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shimwell_T/0/1/0/all/0/1">T. Shimwell</a> Ultra-low frequency observations (<100 MHz) are particularly challenging because they are usually performed in a low signal-to-noise ratio regime due to the high sky temperature and because of ionospheric disturbances whose effectsRead More →

Search for event bursts in XMASS-I associated with gravitational-wave events. (arXiv:2007.16046v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_XMASS/0/1/0/all/0/1">XMASS Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abe_K/0/1/0/all/0/1">K. Abe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hiraide_K/0/1/0/all/0/1">K. Hiraide</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ichimura_K/0/1/0/all/0/1">K. Ichimura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kishimoto_Y/0/1/0/all/0/1">Y. Kishimoto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_K/0/1/0/all/0/1">K. Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_M/0/1/0/all/0/1">M. Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moriyama_S/0/1/0/all/0/1">S. Moriyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakahata_M/0/1/0/all/0/1">M. Nakahata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogawa_H/0/1/0/all/0/1">H. Ogawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sato_K/0/1/0/all/0/1">K. Sato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sekiya_H/0/1/0/all/0/1">H. Sekiya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_T/0/1/0/all/0/1">T. Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takeda_A/0/1/0/all/0/1">A. Takeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tasaka_S/0/1/0/all/0/1">S. Tasaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamashita_M/0/1/0/all/0/1">M. Yamashita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_B/0/1/0/all/0/1">B. S. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_N/0/1/0/all/0/1">N. Y. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_Y/0/1/0/all/0/1">Y. D. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Itow_Y/0/1/0/all/0/1">Y. Itow</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kanzawa_K/0/1/0/all/0/1">K. Kanzawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Masuda_K/0/1/0/all/0/1">K. Masuda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martens_K/0/1/0/all/0/1">K. Martens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_Y/0/1/0/all/0/1">Y. Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_B/0/1/0/all/0/1">B. D. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miuchi_K/0/1/0/all/0/1">K. Miuchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oka_N/0/1/0/all/0/1">N. Oka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takeuchi_Y/0/1/0/all/0/1">Y. Takeuchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_Y/0/1/0/all/0/1">Y. H. Kim</a>, <aRead More →

Constraints on a cubic Galileon disformally coupled to Standard Model matter. (arXiv:2007.16052v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Lawrence_M/0/1/0/all/0/1">Michaela G. Lawrence</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Seery_D/0/1/0/all/0/1">David Seery</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Byrnes_C/0/1/0/all/0/1">Christian T. Byrnes</a> We consider a disformal coupling between Standard Model matter and a cubic Galileon scalar sector, assumed to be a relict of some other physics that solves the cosmological constant problem rather than a solution in its own right. This allows the energy density carried by the Galileon scalar to be sufficiently small that it evades stringent constraints from the integrated Sachs-Wolfe effect, which otherwise rules out the cubic Galileon theory. Although the model with disformal coupling does not exhibit screening, weRead More →

LOUPE: Observing Earth from the Moon to prepare for detecting life on Earth-like exoplanets. (arXiv:2007.16078v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Klindzic_D/0/1/0/all/0/1">Dora Klind&#x17e;i&#x107;</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Stam_D/0/1/0/all/0/1">Daphne M. Stam</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Snik_F/0/1/0/all/0/1">Frans Snik</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Hoeijmakers_H/0/1/0/all/0/1">H. Jens Hoeijmakers</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Willebrands_M/0/1/0/all/0/1">Michelle Willebrands</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Karalidi_T/0/1/0/all/0/1">Teodora Karalidi</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Pallichadath_V/0/1/0/all/0/1">Vidhya Pallichadath</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dijk_C/0/1/0/all/0/1">Chris N. van Dijk</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Esposito_M/0/1/0/all/0/1">Marco Esposito</a> (5) ((1) Delft University of Technology, Faculty of Aerospace Engineering, (2) Leiden University, Leiden Observatory, (3) University of Bern, Center for Space and Habitability (CSH), (4) UCF Department of Physics, (5) cosine Remote Sensing) LOUPE, the Lunar Observatory for Unresolved Polarimetry of the Earth, is a small, robustRead More →

Deep-sea deployment of the KM3NeT neutrino telescope detection units by self-unrolling. (arXiv:2007.16090v1 [astro-ph.IM]) The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_KM3NeT/0/1/0/all/0/1">KM3NeT Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Aiello_S/0/1/0/all/0/1">S. Aiello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albert_A/0/1/0/all/0/1">A. Albert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garre_S/0/1/0/all/0/1">S. Alves Garre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aly_Z/0/1/0/all/0/1">Z. Aly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ameli_F/0/1/0/all/0/1">F. Ameli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anassontzis_E/0/1/0/all/0/1">E.G. Anassontzis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andre_M/0/1/0/all/0/1">M. Andre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Androulakis_G/0/1/0/all/0/1">G. Androulakis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anghinolfi_M/0/1/0/all/0/1">M. Anghinolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anguita_M/0/1/0/all/0/1">M. Anguita</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:+Ardid_M/0/1/0/all/0/1">M. Ardid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aublin_J/0/1/0/all/0/1">J. Aublin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bagatelas_C/0/1/0/all/0/1">C. Bagatelas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakker_R/0/1/0/all/0/1">R. Bakker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbarino_G/0/1/0/all/0/1">G. Barbarino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baret_B/0/1/0/all/0/1">B. Baret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pree_S/0/1/0/all/0/1">S. Basegmez du Pree</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bendahman_M/0/1/0/all/0/1">M. Bendahman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berbeen_E/0/1/0/all/0/1">E. Berbeen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berg_A/0/1/0/all/0/1">A.M. van den Berg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_V/0/1/0/all/0/1">V. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biagi_S/0/1/0/all/0/1">S. Biagi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Billault_M/0/1/0/all/0/1">M. Billault</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bissinger_M/0/1/0/all/0/1">M. Bissinger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boettcher_M/0/1/0/all/0/1">M. Boettcher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boumaaza_J/0/1/0/all/0/1">J. Boumaaza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouta_M/0/1/0/all/0/1">M.Read More →

Cosmological Constraint on Vector Mediator of Neutrino-Electron Interaction in light of XENON1T Excess. (arXiv:2007.16105v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Ibe_M/0/1/0/all/0/1">Masahiro Ibe</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kobayashi_S/0/1/0/all/0/1">Shin Kobayashi</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Nakayama_Y/0/1/0/all/0/1">Yuhei Nakayama</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Shirai_S/0/1/0/all/0/1">Satoshi Shirai</a> Recently, the XENON1T collaboration reported an excess in the electron recoil energy spectrum. One of the simplest new physics interpretation is a new neutrino-electron interaction mediated by a light vector particle. However, for the parameter region favored by this excess, the constraints from the stellar cooling are severe. Still, there are astrophysical uncertainties on those constraints. In this paper, we discuss the constraint on the light mediator from the effective number of neutrino Neff in the CMB era,Read More →

X-ray spectroscopy in the microcalorimeter era II: A new Diagnostic on Column Density from the Case A to B Transition in H- and He-like Iron. (arXiv:2007.16106v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chakraborty_P/0/1/0/all/0/1">P. Chakraborty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatzikos_M/0/1/0/all/0/1">M. Chatzikos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guzman_F/0/1/0/all/0/1">F. Guzm&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Su_Y/0/1/0/all/0/1">Y. Su</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferland_G/0/1/0/all/0/1">G. J. Ferland</a> The Soft X-ray Spectrometer (SXS) on board textit{Hitomi}, with the unprecedented resolving power of R$sim$1250, allowed the detection of members of the Fe XXV ka complex emission spectra from the center of the Perseus Cluster. In this paper, we introduce a novel method of measuring the column density using the optically thin (Case A) to optically thick (Case B) transition for one-Read More →

Patterns of galaxy spin directions in SDSS and Pan-STARRS show parity violation and multipoles. (arXiv:2007.16116v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Shamir_L/0/1/0/all/0/1">Lior Shamir</a> The distribution of spin directions of $sim6.4cdot10^4$ SDSS spiral galaxies with spectra was examined, and compared to the distribution of $sim3.3cdot10^4$ Pan-STARRS galaxies. The analysis shows a statistically significant asymmetry between the number of SDSS galaxies with opposite spin directions, and the magnitude and direction of the asymmetry changes with the direction of observation and with the redshift. The redshift dependence shows that the distribution of the spin direction of SDSS galaxies becomes more asymmetric as the redshift gets higher. Fitting the distribution of the galaxyRead More →

Pre-construction estimates of the Cherenkov Telescope Array sensitivity to a dark matter signal from the Galactic centre. (arXiv:2007.16129v1 [astro-ph.HE]) The <a href="http://arxiv.org/find/astro-ph/1/au:+Consortium_C/0/1/0/all/0/1">Cherenkov Telescope Array Consortium</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Acharyya_A/0/1/0/all/0/1">A. Acharyya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adam_R/0/1/0/all/0/1">R. Adam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_C/0/1/0/all/0/1">C. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agudo_I/0/1/0/all/0/1">I. Agudo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguirre_Santaella_A/0/1/0/all/0/1">A. Aguirre-Santaella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alfaro_R/0/1/0/all/0/1">R. Alfaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alfaro_J/0/1/0/all/0/1">J. Alfaro</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:+Aloisio_R/0/1/0/all/0/1">R. Aloisio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batista_R/0/1/0/all/0/1">R. Alves Batista</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amati_L/0/1/0/all/0/1">L. Amati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ambrosi_G/0/1/0/all/0/1">G. Ambrosi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anguner_E/0/1/0/all/0/1">E.O. Ang&#xfc;ner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antonelli_L/0/1/0/all/0/1">L.A. Antonelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aramo_C/0/1/0/all/0/1">C. Aramo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araudo_A/0/1/0/all/0/1">A. Araudo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Armstrong_T/0/1/0/all/0/1">T. Armstrong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arqueros_F/0/1/0/all/0/1">F. Arqueros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asano_K/0/1/0/all/0/1">K. Asano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ascasibar_Y/0/1/0/all/0/1">Y. Ascas&#xed;bar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashley_M/0/1/0/all/0/1">M. Ashley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balazs_C/0/1/0/all/0/1">C. Balazs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballester_O/0/1/0/all/0/1">O. Ballester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larriva_A/0/1/0/all/0/1">A. Baquero Larriva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martins_V/0/1/0/all/0/1">V. Barbosa Martins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barkov_M/0/1/0/all/0/1">M.Read More →

Natural starshades would help astronomers image exoplanets In the past few decades, the study of extrasolar planets has grown by leaps and bounds, with the confirmation of over 4000 exoplanets. With so many planets available for study, the focus of exoplanet researchers is shifting from discovery to characterization. In the coming years, new technologies and next-generation telescopes will also enable direct imaging studies, which will vastly improve our understanding of exoplanet atmospheres. phys.org Go to SourceRead More →