RAS_WEB (Page 2,757)

Subaru through a different lens: microlensing by extended dark matter structures. (arXiv:2007.12697v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Croon_D/0/1/0/all/0/1">Djuna Croon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKeen_D/0/1/0/all/0/1">David McKeen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raj_N/0/1/0/all/0/1">Nirmal Raj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Z/0/1/0/all/0/1">Zihui Wang</a> We investigate gravitational microlensing signals produced by a spatially extended object transiting in front of a finite-sized source star. The most interesting features arise for lens and source sizes comparable to the Einstein radius of the setup. Using this information, we obtain constraints from the Subaru-HSC survey of M31 on the dark matter populations of NFW subhalos and boson stars of asteroid to Earth masses. These lens profiles capture the qualitative behavior of a wide range of dark matter substructures.Read More →

Axial Asymmetry Studies in Gaia Data Release 2 Yield the Pattern Speed of the Galactic Bar. (arXiv:2007.12699v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hinkel_A/0/1/0/all/0/1">Austin Hinkel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gardner_S/0/1/0/all/0/1">Susan Gardner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yanny_B/0/1/0/all/0/1">Brian Yanny</a> Our recent studies of axial-symmetry breaking in the nearby ($d <3 ,{rm kpc}$) star counts are sensitive to the distortions of stellar orbits perpendicular and parallel to the orientation of the bar just within and beyond the outer Lindblad resonance (OLR) radius. Using the location of the sign flip in the left-right asymmetry in stars counts about the anticenter line to determine the OLR radius $R_{rm OLR}$, and treating the bar as if it were a weakly non-axisymmetricRead More →

Zodiacal Exoplanets in Time. XI. The Orbit and Radiation Environment of the Young M Dwarf-Hosted Planet K2-25b. (arXiv:2007.12701v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gaidos_E/0/1/0/all/0/1">E. Gaidos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirano_T/0/1/0/all/0/1">T. Hirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_D/0/1/0/all/0/1">D. J. Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+France_K/0/1/0/all/0/1">K. France</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rockcliffe_K/0/1/0/all/0/1">K. Rockcliffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Newton_E/0/1/0/all/0/1">E. Newton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feiden_G/0/1/0/all/0/1">G. Feiden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krishnamurthy_V/0/1/0/all/0/1">V. Krishnamurthy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harakawa_H/0/1/0/all/0/1">H. Harakawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hodapp_K/0/1/0/all/0/1">K. W. Hodapp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishizuka_M/0/1/0/all/0/1">M. Ishizuka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jacobson_S/0/1/0/all/0/1">S. Jacobson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Konishi_M/0/1/0/all/0/1">M. Konishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kotani_T/0/1/0/all/0/1">T. Kotani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kudo_T/0/1/0/all/0/1">T. Kudo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurokawa_T/0/1/0/all/0/1">T. Kurokawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuzuhara_M/0/1/0/all/0/1">M. Kuzuhara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishikawa_J/0/1/0/all/0/1">J. Nishikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omiya_M/0/1/0/all/0/1">M. Omiya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serizawa_T/0/1/0/all/0/1">T. Serizawa</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:+Ueda_A/0/1/0/all/0/1">A. Ueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vievard_S/0/1/0/all/0/1">S. Vievard</a> M dwarf stars are high-priority targets for searches for Earth-size and potentially Earth-like planets, butRead More →

Saturn’s rings as a seismograph to probe Saturn’s internal structure. (arXiv:2007.12703v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mankovich_C/0/1/0/all/0/1">Christopher R. Mankovich</a> As it has already done for Earth, the sun, and the stars, seismology has the potential to radically change the way the interiors of giant planets are studied. In a sequence of events foreseen by only a few, observations of Saturn’s rings by the Cassini spacecraft have rapidly broken ground on giant planet seismology. Gravity directly couples the planet’s normal mode oscillations to the orbits of ring particles, generating spiral waves whose frequencies encode Saturn’s internal structure and rotation. These modes have revealed a stably stratified region near Saturn’sRead More →

Strong bound on canonical ultra-light axion dark matter from the Lyman-alpha forest. (arXiv:2007.12705v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rogers_K/0/1/0/all/0/1">Keir K. Rogers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peiris_H/0/1/0/all/0/1">Hiranya V. Peiris</a> We present a new bound on the ultra-light axion (ULA) dark matter mass $m_text{a}$, using the Lyman-alpha forest to look for suppressed cosmic structure growth: a 95% lower limit $m_text{a} > 2 times 10^{-20},text{eV}$. This strongly disfavors ($> 99.7%$ credibility) the canonical ULA with $10^{-22},text{eV} < m_text{a} < 10^{-21},text{eV}$, motivated by the string axiverse and solutions to possible tensions in the cold dark matter model. We strengthen previous equivalent bounds by about an order of magnitude. We demonstrate the robustness of our resultsRead More →

Revisiting AGN as the Source of IceCube’s Diffuse Neutrino Flux. (arXiv:2007.12706v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_D/0/1/0/all/0/1">Daniel Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hooper_D/0/1/0/all/0/1">Dan Hooper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vieregg_A/0/1/0/all/0/1">Abby Vieregg</a> The origin of the astrophysical neutrino flux reported by the IceCube Collaboration remains an open question. In this study, we use three years of publicly available IceCube data to search for evidence of neutrino emission from the blazars and non-blazar Active Galactic Nuclei (AGN) contained the Fermi 4LAC catalog. We find no evidence that these sources produce high-energy neutrinos, and conclude that blazars can produce no more than 15% of IceCube’s observed flux. The constraint we derive on the contribution from non-blazar AGN, whichRead More →

Aluminum-26 Enrichment in the Surface of Protostellar Disks Due to Protostellar Cosmic Rays. (arXiv:2007.12707v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gaches_B/0/1/0/all/0/1">Brandt A. L. Gaches</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walch_S/0/1/0/all/0/1">Stefanie Walch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walch_S/0/1/0/all/0/1">Stella S. R. Walch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munker_C/0/1/0/all/0/1">Carsten M&#xfc;nker</a> The radioactive decay of aluminum-26 ($^{26}$Al) is an important heating source in early planet formation. Since its discovery, there have been several mechanisms proposed to introduce $^{26}$Al into protoplanetary disks, primarily through contamination by external sources. We propose a local mechanism to enrich protostellar disks with $^{26}$Al through irradiation of the protostellar disk surface by cosmic rays accelerated in the protostellar accretion shock. We calculate the $^{26}$Al enrichment, [$^{26}$Al/$^{27}$Al], at the surface of theRead More →

Search for Lensed Gravitational Waves Including Morse Phase Information: An Intriguing Candidate in O2. (arXiv:2007.12709v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_L/0/1/0/all/0/1">Liang Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zackay_B/0/1/0/all/0/1">Barak Zackay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venumadhav_T/0/1/0/all/0/1">Tejaswi Venumadhav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roulet_J/0/1/0/all/0/1">Javier Roulet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zaldarriaga_M/0/1/0/all/0/1">Matias Zaldarriaga</a> We search for strongly lensed and multiply imaged gravitational wave signals in the second observing run of Advanced LIGO and Advanced Virgo (O2). We exploit a new source of information, the so-called Morse phase, which further mitigates the search background and constrains viable lenses. The best candidate we find is consistent with a strongly lensed signal from a massive binary black hole (BBH) merger, with three detected images consisting of the previously catalogued eventsRead More →

Constraining the host galaxy halos of massive black holes from LISA event rates. (arXiv:2007.12710v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Padmanabhan_H/0/1/0/all/0/1">Hamsa Padmanabhan</a> (CITA), <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard) The coalescence of massive black hole binaries (with masses $10^4 – 10^7 M_{odot}$) leads to gravitational wave emission that is detectable out to high redshifts ($z sim 20$) with the forthcoming LISA observatory. We combine the theoretically derived merger rates for dark matter haloes at various redshifts, with an empirically motivated prescription that connects the mass of a dark matter halo and that of its central black hole. Using the expected constraints on the (chirp or reduced) masses of binary black holes,Read More →

Sterile Neutrino Dark Matter and Leptogenesis in Left-Right Higgs Parity. (arXiv:2007.12711v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Dunsky_D/0/1/0/all/0/1">David Dunsky</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Hall_L/0/1/0/all/0/1">Lawrence J. Hall</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Harigaya_K/0/1/0/all/0/1">Keisuke Harigaya</a> The standard model Higgs quartic coupling vanishes at $(10^{9}-10^{13})$ GeV. We study $SU(2)_L times SU(2)_R times U(1)_{B-L}$ theories that incorporate the Higgs Parity mechanism, where this becomes the scale of Left-Right symmetry breaking, $v_R$. Furthermore, these theories solve the strong CP problem and predict three right-handed neutrinos. We introduce cosmologies where $SU(2)_R times U(1)_{B-L}$ gauge interactions produce right-handed neutrinos via the freeze-out or freeze-in mechanisms. In both cases, we find the parameter space where the lightest right-handed neutrino is dark matter and theRead More →

Lessons on Star-forming Ultra-diffuse Galaxies from The Stacked Spectra of Sloan Digital Sky Survey. (arXiv:2007.12712v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rong_Y/0/1/0/all/0/1">Yu Rong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_K/0/1/0/all/0/1">Kai Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnston_E/0/1/0/all/0/1">Evelyn J. Johnston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_H/0/1/0/all/0/1">Hong-Xin Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cao_T/0/1/0/all/0/1">Tianwen Cao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puzia_T/0/1/0/all/0/1">Thomas H. Puzia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galaz_G/0/1/0/all/0/1">Gaspar Galaz</a> We investigate the on-average properties for 28 star-forming ultra-diffuse galaxies (UDGs) located in low-density environments, by stacking their spectra from the Sloan Digital Sky Survey. These relatively-isolated UDGs, with stellar masses of $log_{10}(M_*/M_{odot})sim 8.57pm0.29$, have the on-average total-stellar-metallicity [M/H]$sim -0.82pm0.14$, iron-metallicity [Fe/H]$sim -1.00pm0.16$, stellar age $t_*sim5.2pm0.5$ Gyr, $alpha$-enhancement [$alpha$/Fe]$sim 0.24pm0.10$, and oxygen abundance 12+log(O/H)$sim 8.16pm0.06$, as well as central stellar velocity dispersion $54pm12$ km/s. On theRead More →

The Most Metal-poor Stars in the Inner Bulge. (arXiv:2007.12728v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Reggiani_H/0/1/0/all/0/1">Henrique Reggiani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlaufman_K/0/1/0/all/0/1">Kevin C. Schlaufman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casey_A/0/1/0/all/0/1">Andrew R. Casey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ji_A/0/1/0/all/0/1">Alexander P. Ji</a> The bulge is the oldest component of the Milky Way. Since numerous simulations of Milky Way formation have predicted that the oldest stars at a given metallicity are found on tightly bound orbits, the Galaxy’s oldest stars are likely metal-poor stars in the inner bulge with small apocenters (i.e., $R_{mathrm{apo}}lesssim4$ kpc). In the past, stars with these properties have been impossible to find due to extreme reddening and extinction along the line of sight to the inner bulge. We haveRead More →

Planetary candidates transiting cool dwarf stars from Campaigns 12 to 15 of K2. (arXiv:2007.12744v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_A/0/1/0/all/0/1">A. Castro Gonz&#xe1;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_E/0/1/0/all/0/1">E. D&#xed;ez Alonso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanco_J/0/1/0/all/0/1">J. Men&#xe9;ndez Blanco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Livingston_J/0/1/0/all/0/1">John H. Livingston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leon_J/0/1/0/all/0/1">Jerome P. de Leon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_S/0/1/0/all/0/1">S. L. Su&#xe1;rez G&#xf3;mez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_C/0/1/0/all/0/1">C. Gonz&#xe1;lez Guti&#xe9;rrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riesgo_F/0/1/0/all/0/1">F. Garc&#xed;a Riesgo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonavera_L/0/1/0/all/0/1">L. Bonavera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_F/0/1/0/all/0/1">F.J. Iglesias Rodr&#xed;guez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muniz_R/0/1/0/all/0/1">R. Mu&#xf1;iz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Everett_M/0/1/0/all/0/1">Mark E. Everett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scott_N/0/1/0/all/0/1">N. J. Scott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howell_S/0/1/0/all/0/1">Steve B. Howell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciardi_D/0/1/0/all/0/1">David R. Ciardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzales_E/0/1/0/all/0/1">Erica J. Gonzales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schlieder_J/0/1/0/all/0/1">Joshua E. Schlieder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Juez_F/0/1/0/all/0/1">F. J. de Cos Juez</a> We analyzed the photometry of 20038 cool stars from campaigns 12, 13, 14 and 15 ofRead More →

The Evolution of Rotation and Magnetic Activity in 94 Aqr Aa from Asteroseismology with TESS. (arXiv:2007.12755v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Metcalfe_T/0/1/0/all/0/1">Travis S. Metcalfe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saders_J/0/1/0/all/0/1">Jennifer L. van Saders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_S/0/1/0/all/0/1">Sarbani Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buzasi_D/0/1/0/all/0/1">Derek Buzasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chaplin_W/0/1/0/all/0/1">William J. Chaplin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egeland_R/0/1/0/all/0/1">Ricky Egeland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_R/0/1/0/all/0/1">Rafael A. Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaulme_P/0/1/0/all/0/1">Patrick Gaulme</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huber_D/0/1/0/all/0/1">Daniel Huber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reinhold_T/0/1/0/all/0/1">Timo Reinhold</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schunker_H/0/1/0/all/0/1">Hannah Schunker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stassun_K/0/1/0/all/0/1">Keivan G. Stassun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Appourchaux_T/0/1/0/all/0/1">Thierry Appourchaux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ball_W/0/1/0/all/0/1">Warrick H. Ball</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bedding_T/0/1/0/all/0/1">Timothy R. Bedding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deheuvels_S/0/1/0/all/0/1">Sebastien Deheuvels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_Cuesta_L/0/1/0/all/0/1">Lucia Gonzalez-Cuesta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Handberg_R/0/1/0/all/0/1">Rasmus Handberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_A/0/1/0/all/0/1">Antonio Jimenez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kjeldsen_H/0/1/0/all/0/1">Hans Kjeldsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_T/0/1/0/all/0/1">Tanda Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lund_M/0/1/0/all/0/1">Mikkel N. Lund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mathur_S/0/1/0/all/0/1">Savita Mathur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mosser_B/0/1/0/all/0/1">Benoit Mosser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_M/0/1/0/all/0/1">Martin B. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Noll_A/0/1/0/all/0/1">Anthony Noll</a>,Read More →

The Habitable-zone Planet Finder Reveals A High Mass and a Low Obliquity for the Young Neptune K2-25b. (arXiv:2007.12766v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stefansson_G/0/1/0/all/0/1">Gudmundur Stefansson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mahadevan_S/0/1/0/all/0/1">Suvrath Mahadevan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maney_M/0/1/0/all/0/1">Marissa Maney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ninan_J/0/1/0/all/0/1">Joe P. Ninan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robertson_P/0/1/0/all/0/1">Paul Robertson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rajagopal_J/0/1/0/all/0/1">Jayadev Rajagopal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haase_F/0/1/0/all/0/1">Flynn Haase</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_L/0/1/0/all/0/1">Lori Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ford_E/0/1/0/all/0/1">Eric B. Ford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">Joshua Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolfgang_A/0/1/0/all/0/1">Angie Wolfgang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_R/0/1/0/all/0/1">Rebekah I. Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wisniewski_J/0/1/0/all/0/1">John Wisniewski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_C/0/1/0/all/0/1">Chad F. Bender</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canas_C/0/1/0/all/0/1">Caleb Ca&#xf1;as</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cochran_W/0/1/0/all/0/1">William Cochran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diddams_S/0/1/0/all/0/1">Scott A. Diddams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fredrick_C/0/1/0/all/0/1">Connor Fredrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halverson_S/0/1/0/all/0/1">Samuel Halverson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hearty_F/0/1/0/all/0/1">Fred Hearty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hebb_L/0/1/0/all/0/1">Leslie Hebb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kanodia_S/0/1/0/all/0/1">Shubham Kanodia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levi_E/0/1/0/all/0/1">Eric Levi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Metcalf_A/0/1/0/all/0/1">Andrew J. Metcalf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monson_A/0/1/0/all/0/1">Andrew Monson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramsey_L/0/1/0/all/0/1">Lawrence Ramsey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_A/0/1/0/all/0/1">ArpitaRead More →

Transformable Reflective Telescope for optical testing and education. (arXiv:2007.12771v1 [physics.ed-ph]) <a href="http://arxiv.org/find/physics/1/au:+Park_W/0/1/0/all/0/1">Woojin Park</a>, <a href="http://arxiv.org/find/physics/1/au:+Pak_S/0/1/0/all/0/1">Soojong Pak</a>, <a href="http://arxiv.org/find/physics/1/au:+Kim_G/0/1/0/all/0/1">Geon Hee Kim</a>, <a href="http://arxiv.org/find/physics/1/au:+Lee_S/0/1/0/all/0/1">Sunwoo Lee</a>, <a href="http://arxiv.org/find/physics/1/au:+Chang_S/0/1/0/all/0/1">Seunghyuk Chang</a>, <a href="http://arxiv.org/find/physics/1/au:+Kim_S/0/1/0/all/0/1">Sanghyuk Kim</a>, <a href="http://arxiv.org/find/physics/1/au:+Jeong_B/0/1/0/all/0/1">Byeongjoon Jeong</a>, <a href="http://arxiv.org/find/physics/1/au:+Brendel_T/0/1/0/all/0/1">Trenton James Brendel</a>, <a href="http://arxiv.org/find/physics/1/au:+Kim_D/0/1/0/all/0/1">Dae Wook Kim</a> We propose and experimentally demonstrate the Transformable Reflective Telescope (TRT) Kit for educational purposes and for performing various optical tests with a single kit. The TRT Kit is a portable optical bench setup suitable for interferometry, spectroscopy, measuring stray light, and developing adaptive optics, among other uses. Supplementary modules may be integrated easily thanks to the modular design of the TRT Kit. The Kit consistsRead More →

Synthetic Spectra of Rotating Stars. (arXiv:2007.12779v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lipatov_M/0/1/0/all/0/1">Mikhail Lipatov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandt_T/0/1/0/all/0/1">Timothy D. Brandt</a> Many early-type stars have oblate surfaces, spatial temperature variations, and spectral line broadening that indicate large rotational velocities. Rotation ought to have a significant effect on the full spectra of such stars. To infer structural and life history parameters from their spectra, one must integrate specific intensity over the two-dimensional surfaces of corresponding stellar models. Toward this end, we offer PARS (Paint the Atmospheres of Rotating Stars) — an integration scheme based on models that incorporate solid body rotation, Roche mass distribution, and collinearity of gravity and energy flux (https://github.com/mlipatov/paint_atmospheres). TheRead More →

Multiband gravitational-wave searches for ultralight bosons. (arXiv:2007.12793v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Ng_K/0/1/0/all/0/1">Ken K. Y. Ng</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Isi_M/0/1/0/all/0/1">Maximiliano Isi</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Haster_C/0/1/0/all/0/1">Carl-Johan Haster</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Vitale_S/0/1/0/all/0/1">Salvatore Vitale</a> Gravitational waves may be one of the few direct observables produced by ultralight bosons, conjectured dark matter candidates that could be the key to several problems in particle theory, high-energy physics and cosmology. These axion-like particles could spontaneously form “clouds” around astrophysical black holes, leading to potent emission of continuous gravitational waves that could be detected by instruments on the ground and in space. Although this scenario has been thoroughly studied, it has not been yet appreciated that both types of detector mayRead More →

Domain walls and other defects in Eddington-inspired Born-Infeld gravity. (arXiv:2007.12794v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Avelino_P/0/1/0/all/0/1">P. P. Avelino</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Sousa_L/0/1/0/all/0/1">L. Sousa</a> We investigate domain wall and other defect solutions in the weak-field limit of Eddington-inspired Born-Infeld gravity as a function of $kappa$, the only additional parameter of the theory with respect to General Relativity. We determine, both analytically and numerically, the internal structure of domain walls, quantifying its dependency on $kappa$ as well as the impact of such dependency on the value of the tension measured by an outside observer. We find that the pressure in the direction perpendicular to the domain wall can be, in contrast toRead More →

Photo-z outlier self-calibration in weak lensing surveys. (arXiv:2007.12795v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Schaan_E/0/1/0/all/0/1">Emmanuel Schaan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seljak_U/0/1/0/all/0/1">Uro&#x161; Seljak</a> Calibrating photometric redshift errors in weak lensing surveys with external data is extremely challenging. We show that both Gaussian and outlier photo-z parameters can be self-calibrated from the data alone. This comes at no cost for the neutrino masses, curvature and dark energy equation of state $w_0$, but with a 65% degradation when both $w_0$ and $w_a$ are varied. We perform a realistic forecast for the Vera Rubin Observatory (VRO) Legacy Survey of Space and Time (LSST) 3×2 analysis, combining cosmic shear, projected galaxy clustering and galaxyRead More →