RAS_WEB (Page 4,690)

Electron and Proton Heating in Transrelativistic Guide Field Reconnection. (arXiv:1901.05438v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rowan_M/0/1/0/all/0/1">Michael E. Rowan</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Sironi_L/0/1/0/all/0/1">Lorenzo Sironi</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Narayan_R/0/1/0/all/0/1">Ramesh Narayan</a> (1) ((1) Harvard, (2) Columbia) The plasma in low-luminosity accretion flows, such as the one around the black hole at the center of M87 or Sgr A* at our Galactic Center, is expected to be collisioness and two-temperature, with protons hotter than electrons. Here, particle heating is expected to be controlled by magnetic reconnection in the transrelativistic regime $sigma_{w}sim 0.1$-$1$, where the magnetization $sigma_{w}$ is the ratio of magnetic energy density to plasma enthalpy density. By means of large-scale 2D particle-in-cell simulations,Read More →

Halo Concentrations and the New Baseline X-ray Luminosity-Temperature and Mass Relations of Galaxy Clusters. (arXiv:1901.05439v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fujita_Y/0/1/0/all/0/1">Yutaka Fujita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aung_H/0/1/0/all/0/1">Han Aung</a> The standard model of galaxy cluster formation predicts that the X-ray luminosity-temperature ($L_X$-$T_X$) relation of galaxy clusters should have been $L_Xpropto T_X^2$ in absence of the baryonic physics, such as radiative cooing and feedback from stars and black holes. However, this baseline relation is predicted without considering the fact that the halo concentration and the characteristic density of clusters increases as their mass decreases, which is a consequence of hierarchical structure formation of the universe. Here, we show that the actual baseline relationRead More →

Evolution of Accreting Binary Systems on the Spin-up Line. (arXiv:1401.1528v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Taani_A/0/1/0/all/0/1">Ali Taani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Al_Wardat_M/0/1/0/all/0/1">Mashhoor A. Al-Wardat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khasawneh_A/0/1/0/all/0/1">Awni Khasawneh</a> The measured characteristics of binary pulsars provide valuable insights into the evolution of these systems. We study the aspects of binary evolution particularly relevant to binary Millisecond Pulsars (MSPs), and the formation of close binaries involving degenerate stars through a spin-evolution diagram (spin-up line). For this task, we use a wide variety of binaries, including those with compact components that observed in different energy bands, which we analyze them according to the spin-up line. Their formation and evolution over timescales of binary evolutionRead More →

Detection and Implications of Laser-Induced Raman Scattering at Astronomical Observatories. (arXiv:1706.07050v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Vogt_F/0/1/0/all/0/1">F.P.A. Vogt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calia_D/0/1/0/all/0/1">D. Bonaccini Calia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hackenberg_W/0/1/0/all/0/1">W. Hackenberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Opitom_C/0/1/0/all/0/1">C. Opitom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Comin_M/0/1/0/all/0/1">M. Comin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmidtobreik_L/0/1/0/all/0/1">L. Schmidtobreik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smoker_J/0/1/0/all/0/1">J. Smoker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanchard_I/0/1/0/all/0/1">I. Blanchard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_M/0/1/0/all/0/1">M. Espinoza Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aranda_I/0/1/0/all/0/1">I. Aranda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milli_J/0/1/0/all/0/1">J. Milli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaffe_Y/0/1/0/all/0/1">Y.L. Jaffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Selman_F/0/1/0/all/0/1">F. Selman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kolb_J/0/1/0/all/0/1">J. Kolb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hibon_P/0/1/0/all/0/1">P. Hibon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuntschner_H/0/1/0/all/0/1">H. Kuntschner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madec_P/0/1/0/all/0/1">P.-Y. Madec</a> (Abr.) Laser guide stars employed at astronomical observatories provide artificial wavefront reference sources to help correct (in part) the impact of atmospheric turbulence on astrophysical observations. Following the recent commissioning of the 4 Laser Guide Star Facility (4LGSF) onRead More →

High-energy neutrino attenuation in the Earth and its associated uncertainties. (arXiv:1706.09895v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Vincent_A/0/1/0/all/0/1">Aaron C. Vincent</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Arguelles_C/0/1/0/all/0/1">Carlos A. Arg&#xfc;elles</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kheirandish_A/0/1/0/all/0/1">Ali Kheirandish</a> We describe nuFATE Neutrino Fast Attenuation Through Earth, a very rapid method of accurately computing the attenuation of high-energy neutrinos during their passage through Earth to detectors such as IceCube, ANTARES or KM3Net, including production of secondary neutrinos from $tau^pm$ lepton decay. We then use this method to quantify the error on attenuation due to uncertainties in the isotropic neutrino spectrum, the composition of the Earth, and the parton distribution functions. We show that these can be as large as 20%,Read More →

Identification of the Central Compact Object in the young supernova remnant 1E0102.2-7219. (arXiv:1803.01006v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Vogt_F/0/1/0/all/0/1">F.P.A. Vogt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartlett_E/0/1/0/all/0/1">E.S. Bartlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seitenzahl_I/0/1/0/all/0/1">I.R. Seitenzahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dopita_M/0/1/0/all/0/1">M.A. Dopita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghavamian_P/0/1/0/all/0/1">P. Ghavamian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruiter_A/0/1/0/all/0/1">A.J. Ruiter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Terry_J/0/1/0/all/0/1">J.P. Terry</a> Oxygen-rich young supernova remnants are valuable objects for probing the outcome of nucleosynthetic processes in massive stars, as well as the physics of supernova explosions. Observed within a few thousand years after the supernova explosion, these systems contain fast-moving oxygen-rich and hydrogen-poor filaments visible at optical wavelengths: fragments of the progenitor’s interior expelled at a few 1000 km/s during the supernova explosion. Here we report the first identification ofRead More →

Weak Shock Propagation with Accretion. II. Stability of Self-similar Solutions to Radial Perturbations. (arXiv:1901.04487v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_E/0/1/0/all/0/1">Eric R. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ro_S/0/1/0/all/0/1">Stephen Ro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quataert_E/0/1/0/all/0/1">Eliot Quataert</a> Coughlin et al. (2018) (Paper I) derived and analyzed a new regime of self-similarity that describes weak shocks (Mach number of order unity) in the gravitational field of a point mass. These solutions are relevant to low energy explosions, including failed supernovae. In this paper, we develop a formalism for analyzing the stability of shocks to radial perturbations, and we demonstrate that the self-similar solutions of Paper I are extremely weakly unstable to such radial perturbations. Specifically, we show thatRead More →

Characterizing circumgalactic gas around massive ellipticals at z~0.4 III. The galactic environment of a chemically-pristine Lyman limit absorber. (arXiv:1901.04488v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_H/0/1/0/all/0/1">Hsiao-Wen Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_S/0/1/0/all/0/1">Sean D. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Straka_L/0/1/0/all/0/1">Lorrie A. Straka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zahedy_F/0/1/0/all/0/1">Fakhri S. Zahedy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaye_J/0/1/0/all/0/1">Joop Schaye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Muzahid_S/0/1/0/all/0/1">Sowgat Muzahid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouche_N/0/1/0/all/0/1">Nicolas Bouche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cantalupo_S/0/1/0/all/0/1">Sebastiano Cantalupo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_R/0/1/0/all/0/1">Raffaella Anna Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wendt_M/0/1/0/all/0/1">Martin Wendt</a> This paper presents a study of the galactic environment of a chemically-pristine (Read More →

Orion Source I’s disk is salty. (arXiv:1901.04489v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ginsburg_A/0/1/0/all/0/1">Adam Ginsburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGuire_B/0/1/0/all/0/1">Brett McGuire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plambeck_R/0/1/0/all/0/1">Richard Plambeck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bally_J/0/1/0/all/0/1">John Bally</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goddi_C/0/1/0/all/0/1">Ciriaco Goddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_M/0/1/0/all/0/1">Melvyn Wright</a> We report the detection of NaCl, KCl, and their $^{37}$Cl and $^{41}$K isotopologues toward the disk around Orion SrcI. About 60 transitions of these molecules were identified. This is the first detection of these molecules in the interstellar medium not associated with the ejecta of evolved stars. It is also the first ever detection of the vibrationally excited states of these lines in the ISM above v = 1, with firm detections up to v = 6. The saltRead More →

Pulsar Timing Probes of Primordial Black Holes and Subhalos. (arXiv:1901.04490v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dror_J/0/1/0/all/0/1">Jeff A. Dror</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramani_H/0/1/0/all/0/1">Harikrishnan Ramani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trickle_T/0/1/0/all/0/1">Tanner Trickle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zurek_K/0/1/0/all/0/1">Kathryn M. Zurek</a> Pulsars act as accurate clocks, sensitive to gravitational redshift and acceleration induced by transiting clumps of matter. We study the sensitivity of pulsar timing arrays (PTAs) to single transiting compact objects, focusing on primordial black holes and compact subhalos in the mass range from $10^{-12} M _{odot}$ to well above $100~M_odot$. We find that the Square Kilometer Array can constrain such objects to be a subdominant component of the dark matter over this entire mass range, with sensitivity to aRead More →

The implications of clustered star formation for (proto)planetary systems and habitability. (arXiv:1901.04491v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kruijssen_J/0/1/0/all/0/1">J. M. Diederik Kruijssen</a> (Heidelberg), <a href="http://arxiv.org/find/astro-ph/1/au:+Longmore_S/0/1/0/all/0/1">Steven N. Longmore</a> (LJMU) Star formation is spatially clustered across a range of environments, from dense stellar clusters to unbound associations. As a result, radiative or dynamical interactions with neighbouring stars disrupt (proto)planetary systems and limit their radii, leaving a lasting impact on their potential habitability. In the solar neighbourhood, we find that the vast majority of stars form in unbound associations, such that the interaction of (proto)planetary systems with neighbouring stars is limited to the densest sub-regions. However, the fraction of star formation occurringRead More →

A Quantum Complete Prelude to Inflation. (arXiv:1901.04492v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Hofmann_S/0/1/0/all/0/1">Stefan Hofmann</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Schneider_M/0/1/0/all/0/1">Marc Schneider</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Urban_M/0/1/0/all/0/1">Maximilian Urban</a> It is shown that the inflationary paradigm admits quantum complete extensions of space-time. The extended inflationary spacetimes still have geodesic borders, but quantum fields are prohibited from migrating across these borders by their evolution semigroups. The geodesic singularities lurking across the borders lack a physical description because the evolution semigroups give vanishing probabilistic support to quantum fields for populating regions bordering on these singularities. As an example, anisotropic Bianchi type-I cosmologies are shown to be quantum complete preludes to inflation. They admit Kasner-like geometries close to their geodesicRead More →

The MUSE Atlas of Disks (MAD): Resolving Star Formation Rates and Gas Metallicities on < 100pc Scales. (arXiv:1901.04493v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Erroz_Ferrer_S/0/1/0/all/0/1">Santiago Erroz-Ferrer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carollo_C/0/1/0/all/0/1">C. Marcella Carollo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brok_M/0/1/0/all/0/1">Mark den Brok</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onodera_M/0/1/0/all/0/1">Masato Onodera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brinchmann_J/0/1/0/all/0/1">Jarle Brinchmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_R/0/1/0/all/0/1">Raffaella A. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monreal_Ibero_A/0/1/0/all/0/1">Ana Monreal-Ibero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaye_J/0/1/0/all/0/1">Joop Schaye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Woo_J/0/1/0/all/0/1">Joanna Woo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cibinel_A/0/1/0/all/0/1">Anna Cibinel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Debattista_V/0/1/0/all/0/1">Victor P. Debattista</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Inami_H/0/1/0/all/0/1">Hanae Inami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maseda_M/0/1/0/all/0/1">Michael Maseda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richard_J/0/1/0/all/0/1">Johan Richard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tacchella_S/0/1/0/all/0/1">Sandro Tacchella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wisotzki_L/0/1/0/all/0/1">Lutz Wisotzki</a> We study the physical properties of the ionized gas in local disks using the sample of 38 nearby $sim10^{8.5-11.2}$M$_odot$ Star-Forming Main Sequence (SFMS) galaxies observed so far as part of the MUSE Atlas ofRead More →

Evolution of dwarf galaxies hosting GW150914-like events. (arXiv:1901.04494v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Marassi_S/0/1/0/all/0/1">S. Marassi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graziani_L/0/1/0/all/0/1">L. Graziani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginolfi_M/0/1/0/all/0/1">M. Ginolfi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_R/0/1/0/all/0/1">R. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mapelli_M/0/1/0/all/0/1">M. Mapelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spera_M/0/1/0/all/0/1">M. Spera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alparone_M/0/1/0/all/0/1">M. Alparone</a> Here we present a detailed analysis of the properties and evolution of different dwarf galaxies, candidate to host the coalescence of black hole binary systems (BHB) generating GW150914-like events. By adopting a novel theoretical framework coupling the binary population synthesis code texttt{SeBa} with the Galaxy formation model texttt{GAMESH}, we can investigate the detailed evolution of these objects in a well resolved cosmological volume of 4~cMpc, having a Milky Way-like (MW) galaxy forming at its center.Read More →

A Pair of Planets Likely in Mean-Motion Resonance From Gravitational Microlensing. (arXiv:1901.04495v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Madsen_S/0/1/0/all/0/1">Sabrina Madsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_W/0/1/0/all/0/1">Wei Zhu</a> We combine statistical arguments and dynamical analysis to study the orbital configuration of the microlensing planetary system OGLE-2012-BLG-0026L. This system is known to host two massive planets, with both projected close to the Eintein ring at the time of the detection. Assuming an isotropic distribution for the orbital orientation, we find that the two planets should also be closely spaced in three-dimensional space and that the ratio of their orbital periods is almost certainly less than two. With N-body numerical integrations, we then identify two typesRead More →

Diffuse Radio Emission from Galaxy Clusters. (arXiv:1901.04496v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Weeren_R/0/1/0/all/0/1">R. J. van Weeren</a>, <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:+Akamatsu_H/0/1/0/all/0/1">H. Akamatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruggen_M/0/1/0/all/0/1">M. Br&#xfc;ggen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feretti_L/0/1/0/all/0/1">L. Feretti</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:+Stroe_A/0/1/0/all/0/1">A. Stroe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zandanel_F/0/1/0/all/0/1">F. Zandanel</a> In a growing number of galaxy clusters diffuse extended radio sources have been found. These sources are not directly associated with individual cluster galaxies. The radio emission reveal the presence of cosmic rays and magnetic fields in the intracluster medium (ICM). We classify diffuse cluster radio sources into radio halos, cluster radio shocks (relics), and revived AGN fossil plasma sources. Radio halo sources can be further divided into giant halos,Read More →

On the Prevalence of Super-Massive Black Holes over Cosmic Time. (arXiv:1901.04500v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Buchner_J/0/1/0/all/0/1">Johannes Buchner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Treister_E/0/1/0/all/0/1">Ezequiel Treister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bauer_F/0/1/0/all/0/1">Franz E. Bauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sartori_L/0/1/0/all/0/1">Lia F. Sartori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schawinski_K/0/1/0/all/0/1">Kevin Schawinski</a> We investigate the abundance of Super-Massive Black Hole (SMBH) seeds in primordial galaxy halos. We explore the assumption that dark matter halos outgrowing a critical halo mass M_c have some probability p of having spawned a SMBH seed. Current observations of local, intermediate-mass galaxies constrain these parameters: For $M_c=10^{11}M_odot$, all halos must be seeded, but when adopting smaller M_c masses the seeding can be much less efficient. The constraints also put lower limits on the numberRead More →

Dynamical heating across the Milky Way disc using APOGEE and $it{Gaia}$. (arXiv:1901.04502v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mackereth_J/0/1/0/all/0/1">J. Ted Mackereth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bovy_J/0/1/0/all/0/1">Jo Bovy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leung_H/0/1/0/all/0/1">Henry W. Leung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schiavon_R/0/1/0/all/0/1">Ricardo P. Schiavon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trick_W/0/1/0/all/0/1">Wilma H. Trick</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:+Cunha_K/0/1/0/all/0/1">Katia Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feuillet_D/0/1/0/all/0/1">Diane K. Feuillet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Majewski_S/0/1/0/all/0/1">Steven R. Majewski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martig_M/0/1/0/all/0/1">Marie Martig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miglio_A/0/1/0/all/0/1">Andrea Miglio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nidever_D/0/1/0/all/0/1">David Nidever</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinsonneault_M/0/1/0/all/0/1">Marc H. Pinsonneault</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguirre_V/0/1/0/all/0/1">Victor Silva Aguirre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sobeck_J/0/1/0/all/0/1">Jennifer Sobeck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tayar_J/0/1/0/all/0/1">Jamie Tayar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zasowski_G/0/1/0/all/0/1">Gail Zasowski</a> The kinematics of the Milky Way disc as a function of age are well measured at the solar radius, but have not been studied over a wider range of Galactocentric radii. Here,Read More →