Search

Your search keyword '"D. E. Reichart"' showing total 10 results
Start Over Author "D. E. Reichart" Topic 01 natural sciences
10 results on '"D. E. Reichart"'

1. Kojima-1Lb Is a Mildly Cold Neptune around the Brightest Microlensing Host Star

Author

A. Fukui, D. Suzuki, N. Koshimoto, E. Bachelet, T. Vanmunster, D. Storey, H. Maehara, K. Yanagisawa, T. Yamada, A. Yonehara, T. Hirano, D. P. Bennett, V. Bozza, D. Mawet, M. T. Penny, S. Awiphan, A. Oksanen, T. M. Heintz, T. E. Oberst, V. J. S. Béjar, N. Casasayas-Barris, G. Chen, N. Crouzet, D. Hidalgo, P. Klagyivik, F. Murgas, N. Narita, E. Palle, H. Parviainen, N. Watanabe, N. Kusakabe, M. Mori, Y. Terada, J. P. de Leon, A. Hernandez, R. Luque, M. Monelli, P. Montañes-Rodriguez, J. Prieto-Arranz, K. L. Murata, S. Shugarov, Y. Kubota, C. Otsuki, A. Shionoya, T. Nishiumi, A. Nishide, M. Fukagawa, K. Onodera, S. Villanueva, R. A. Street, Y. Tsapras, M. Hundertmark, M. Kuzuhara, M. Fujita, C. Beichman, J.-P. Beaulieu, R. Alonso, D. E. Reichart, N. Kawai, M. Tamura, Okayama Astrophysical Observatory, National Astronomical Observatory of Japan (NAOJ), Osaka University [Osaka], SLAC National Accelerator Laboratory (SLAC), Stanford University, Tokyo University Sci. Dept. Sci. & Technol., The University of Tokyo (UTokyo), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Neurosurgery, Tohoku University School of Medicine, Department of Physics [Notre Dame], University of Notre Dame [Indiana] (UND), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Nyrölä Observatory (NYTT), Oak Ridge National Laboratory [Oak Ridge] (ORNL), UT-Battelle, LLC, Institute of Neurosciences, University of Barcelona, Universidad de Córdoba [Cordoba], Instituto de Astrofisica de Canarias (IAC), RIKEN Nishina Center for Accelerator-Based Science [Wako] (RIKEN RNC), RIKEN - Institute of Physical and Chemical Research [Japon] (RIKEN), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Chapel Hill], University of North Carolina [Chapel Hill] (UNC), University of North Carolina System (UNC)-University of North Carolina System (UNC), Riken, Universidad de Córdoba = University of Córdoba [Córdoba], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Beaulieu, Jean-Philippe

Subjects
010504 meteorology & atmospheric sciences, Exoplanet systems (484), FOS: Physical sciences, Astrophysics, Gravitational microlensing, 01 natural sciences, Photometry (optics), Planet, Neptune, 0103 physical sciences, 010303 astronomy & astrophysics, Exoplanet systems, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Galactic anticenter, Astronomy and Astrophysics, Planetary system, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Parallax, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gravitational microlensing (672), Astrophysics - Earth and Planetary Astrophysics
Abstract

著者人数: 61名 (所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 鈴木, 大介), Number of authors: 61 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS): Suzuki, Daisuke), Accepted: 2019-09-25, 資料番号: SA1190156000

Published
2019
Full Text
View/download PDF

2. Extreme debris disk variability : exploring the diverse outcomes of large asteroid impacts during the era of terrestrial planet formation

Author

Johan Olofsson, Renu Malhotra, Keivan G. Stassun, D. E. Reichart, Kate Y. L. Su, Ruobing Dong, Wiphu Rujopakarn, Joseph E. Rodriguez, Alan Jackson, George H. Rieke, Joshua Pepper, David James, Zoë M. Leinhardt, Grant M. Kennedy, Huan Meng, Michael Hammer, and Andras Gaspar

Subjects
dynamical evolution and stability [planets and satellites], Planetesimal, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, circumstellar matter, 01 natural sciences, Astrobiology, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, planetary systems [infrared], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Cosmic dust, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, individual (2MASS J08090250-4858172, 2MASS J07354269-1450422) [stars], Debris disk, Astronomy and Astrophysics, Debris, Space and Planetary Science, Asteroid, Physics::Space Physics, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Protoplanet, Astrophysics - Earth and Planetary Astrophysics
Abstract

The most dramatic phases of terrestrial planet formation are thought to be oligarchic and chaotic growth, on timescales of up to 100-200 Myr, when violent impacts occur between large planetesimals of sizes up to proto-planets. Such events are marked by the production of large amounts of debris as has been observed in some exceptionally bright and young debris disks (termed extreme debris disks). Here we report five years of Spitzer measurements of such systems around two young solar-type stars: ID8 and P1121. The short-term (weekly to monthly) and long-term (yearly) disk variability is consistent with the aftermaths of large impacts involving large asteroid-size bodies. We demonstrate that an impact-produced clump of optically thick dust, under the influence of the dynamical and viewing geometry effects, can produce short-term modulation in the disk light curves. The long-term disk flux variation is related to the collisional evolution within the impact-produced fragments once released into a circumstellar orbit. The time-variable behavior observed in the P1121 system is consistent with a hypervelocity impact prior to 2012 that produced vapor condensates as the dominant impact product. Two distinct short-term modulations in the ID8 system argue for two violent impacts at different times and locations. Its long-term variation is consistent with the collisional evolution of two different populations of impact-produced debris dominated by either vapor condensates or escaping boulders. The bright, variable emission from the dust produced in large impacts from extreme debris disks provides a unique opportunity to study violent events during the era of terrestrial planet formation., accepted for publication in AJ. typos and latex referencing fixed

Published
2019
Full Text
View/download PDF

3. High accuracy measurement of gravitational wave back-reaction in the OJ287 black hole binary

Author

S. Haque, Kosmas Gazeas, Kozo Sadakane, D. E. Reichart, M. Kidger, René Hudec, S. Ciprini, Andrei Berdyugin, Kiran S. Baliyan, Seppo Mikkola, Mauri Valtonen, Helen Jermak, Achamveedu Gopakumar, Lankeswar Dey, Katsura Matsumoto, Daniel B. Caton, Staszek Zola, Vilppu Piirola, and K. Nilsson

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), ta115, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, BL Lacertae objects: individual (OJ287) [galaxies], Black hole, gravitational waves, Space and Planetary Science, Quantum electrodynamics, 0103 physical sciences, Back-reaction, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

Blazar OJ287 exhibits large thermal flares at least twice every 12 years. The times of these flares have been predicted successfully using the model of a quasi-Keplerian eccentric black hole binary where the secondary impacts the accretion disk of the primary, creating the thermal flares. New measurements of the historical light curve have been combined with the observations of the 2015 November/December flare to identify the impact record since year 1886, and to constrain the orbit of the binary. The orbit solution shows that the binary period, now 12.062 year, is decreasing at the rate of 36 days per century. This corresponds to an energy loss to gravitational waves that is 6.5 +- 4 % less than the rate predicted by the standard quadrupolar gravitational wave (GW) emission. We show that the difference is due to higher order gravitational radiation reaction terms that include the dominant order tail contributions., to appear in the Proceedings of Gravitational Wave Astrophysics: Early Results from Gravitational Wave Searches and Electromagnetic Counterparts. eds. Gabriela Gonzales and Robert Hynes

Published
2017

4. Follow-up of the Neutron Star Bearing Gravitational Wave Candidate Events S190425z and S190426c with MMT and SOAR

Author

L. Patton, Michael L. Calkins, João Braga, Kerry Paterson, P. K. Blanchard, Deanne L. Coppejans, V. G. Savchenko, Kate D. Alexander, Philip S. Cowperthwaite, V. A. Villar, Matt Nicholl, Peter K. G. Williams, Tarraneh Eftekhari, W. Fong, D. E. Reichart, Giacomo Terreran, Ryan Chornock, I. Pelisoli, Chun Ly, Tanmoy Laskar, Raffaella Margutti, Edo Berger, Griffin Hosseinzadeh, Régis Cartier, P. Short, and Sebastian Gomez

Subjects
close [binaries], 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, observational [methods], Binary number, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kilonova, 01 natural sciences, law.invention, Telescope, neutron [stars], law, 0103 physical sciences, black holes [stars], ddc:530, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, Institut für Physik und Astronomie, Astronomy and Astrophysics, LIGO, Neutron star, gravitational waves, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena
Abstract

On 2019 April 25.346 and 26.640 UT the LIGO and Virgo gravitational wave (GW) observatories announced the detection of the first candidate events in Observing Run 3 that contain at least one neutron star. S190425z is a likely binary neutron star (BNS) merger at $d_L = 156 \pm 41$ Mpc, while S190426c is possibly the first NS-BH merger ever detected, at $d_L = 377 \pm 100$ Mpc, although with marginal statistical significance. Here we report our optical follow-up observations for both events using the MMT 6.5-m telescope, as well as our spectroscopic follow-up of candidate counterparts (which turned out to be unrelated) with the 4.1-m SOAR telescope. We compare to publicly reported searches, explore the overall areal coverage and depth, and evaluate those in relation to the optical/NIR kilonova emission from the BNS merger GW170817, to theoretical kilonova models, and to short GRB afterglows. We find that for a GW170817-like kilonova, the partial volume covered spans up to about 40% for S190425z and 60% for S190426c. For an on-axis jet typical of short GRBs, the search effective volume is larger, but such a configuration is expected in at most a few percent of mergers. We further find that wide-field $\gamma$-ray and X-ray limits rule out luminous on-axis SGRBs, for a large fraction of the localization regions, although these searches are not sufficiently deep in the context of the $\gamma$-ray emission from GW170817 or off-axis SGRB afterglows. The results indicate that some optical follow-up searches are sufficiently deep for counterpart identification to about 300 Mpc, but that localizations better than 1000 deg$^2$ are likely essential., Comment: The first six authors contributed equally to this work

Published
2019
Full Text
View/download PDF

5. Searches After Gravitational-waves Using ARizona Observatories (SAGUARO): System Overview and First Results from Advanced LIGO/Virgo's Third Observing Run

Author

Andrea Rossi, Wen-fai Fong, Irene Shivaei, Edward W. Olszewski, Jay Strader, Armin Rest, Peter Milne, Ann I. Zabludoff, David Trilling, Kerry Paterson, Iair Arcavi, Felipe Guzman, S. Valenti, Ben Weiner, D. E. Reichart, Alessandra Corsi, Vasileios Paschalidis, Dimitrios Psaltis, Brenda Frye, E. M. Green, Daniel P. Stark, M. Lundquist, Jennifer E. Andrews, G. Schroeder, Eiichi Egami, A. E. Nugent, M. Wagner, G. Grant Williams, Laura Chomiuk, A. Gibbs, David J. Sand, Renata Cecília Amaro, F. Shelly, O. Kuhn, X. Fan, Ryan J. Foley, Nathaniel R. Butler, Christian Veillet, Catherine J. Grier, Maria R. Drout, Erika T. Hamden, P. N. Daly, S. Wyatt, D. A. Howell, E. Christensen, Maxwell Moe, Patrick L. Kelly, Peter Behroozi, John C Wheeler, Sheng Yang, Buell T. Jannuzi, Paul S. Smith, P. Gabor, Eliana Palazzi, O. Eskandari, Nathan Smith, and K. Spekkens

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Gravitational wave, Foundation (engineering), Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Gravitational-wave astronomy, LIGO, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences
Abstract

We present Searches After Gravitational-waves Using ARizona Observatories (SAGUARO), a comprehensive effort dedicated to the discovery and characterization of optical counterparts to gravitational wave (GW) events. SAGUARO utilizes ground-based facilities ranging from 1.5m to 10m in diameter, located primarily in the Northern Hemisphere. We provide an overview of SAGUARO's telescopic resources, pipeline for transient detection, and database for candidate visualization. We describe SAGUARO's discovery component, which utilizes the $5$~deg$^2$ field-of-view optical imager on the Mt. Lemmon 1.5m telescope, reaching limits of $\approx 21.3$~AB mag while rapidly tiling large areas. We also describe the follow-up component of SAGUARO, used for rapid vetting and monitoring of optical candidates. With the onset of Advanced LIGO/Virgo's third observing run, we present results from the first three SAGUARO searches following the GW events S190408an, S190425z and S190426c, which serve as a valuable proof-of-concept of SAGUARO. We triggered and searched 15, 60 and 60 deg$^{2}$ respectively, 17.6, 1.4 and 41.8 hrs after the initial GW alerts. We covered 7.8, 3.0 and 5.1\% of the total probability within the GW event localizations, reaching 3$\sigma$ limits of 19.8, 21.3 and 20.8 AB mag, respectively. Although no viable counterparts associated with these events were found, we recovered 6 known transients and ruled out 5 potential candidates. We also present Large Binocular Telescope spectroscopy of PS19eq/SN2019ebq, a promising kilonova candidate that was later determined to be a supernova. With the ability to tile large areas and conduct detailed follow-up, SAGUARO represents a significant addition to GW counterpart searches., Comment: 16 pages, 7 figures, 1 table. Accepted to ApJL

Published
2019
Full Text
View/download PDF

6. Signatures of an eruptive phase before the explosion of the peculiar core-collapse SN 2013gc

Author

Andrea Reguitti, A Pastorello, G Pignata, S Benetti, E Cappellaro, M Turatto, C Agliozzo, F Bufano, N I Morrell, F Olivares E, D E Reichart, J B Haislip, V Kouprianov, S J Smartt, and S Ciroi

Subjects
supernovae: general, supernovae: individual: SN2013gc, SN1994aj, SN1996al, SN1996L, SN2000P, Astrophysics::High Energy Astrophysical Phenomena, SN2000P, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Type (model theory), 01 natural sciences, Spectral line, Luminosity, symbols.namesake, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Absorption (logic), SN1996L, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Line (formation), SN1996al, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), SN1994aj, 010308 nuclear & particles physics, Balmer series, Astronomy and Astrophysics, supernovae: individual: SN2013gc, Light curve, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, symbols, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present photometric and spectroscopic analysis of the peculiar core-collapse SN 2013gc, spanning seven years of observations. The light curve shows an early maximum followed by a fast decline and a phase of almost constant luminosity. At +200 days from maximum, a brightening of 1 mag is observed in all bands, followed by a steep linear luminosity decline after +300 d. In archival images taken between 1.5 and 2.5 years before the explosion, a weak source is visible at the supernova location, with mag$\approx$20. The early supernova spectra show Balmer lines, with a narrow ($\sim$560 km s$^{-1}$) P-Cygni absorption superimposed on a broad ($\sim$3400 km s$^{-1}$) component, typical of type IIn events. Through a comparison of colour curves, absolute light curves and spectra of SN 2013gc with a sample of supernovae IIn, we conclude that SN 2013gc is a member of the so-called type IId subgroup. The complex profile of the H$\alpha$ line suggests a composite circumstellar medium geometry, with a combination of lower velocity, spherically symmetric gas and a more rapidly expanding bilobed feature. This circumstellar medium distribution has been likely formed through major mass-loss events, that we directly observed from 3 years before the explosion. The modest luminosity ($M_I\sim-16.5$ near maximum) of SN 2013gc at all phases, the very small amount of ejected $^{56}$Ni (of the order of $10^{-3}$ M$_\odot$), the major pre-supernova stellar activity and the lack of prominent [O I] lines in late-time spectra support a fall-back core-collapse scenario for the massive progenitor of SN~2013gc., Comment: 20 pages, 11 figures, 8 tables, accepted by MNRAS

Published
2018

7. Optical monitoring of a transitional millisecond pulsar: PSR J1023+0038

Author

J. B. Haislip, D. E. Reichart, A P Jaroenjittichai, P Jaroenjittichai, C Nilarat, and Vladimir Kouprianov

Subjects
Physics, History, 010308 nuclear & particles physics, Millisecond pulsar, 0103 physical sciences, Astronomy, 010303 astronomy & astrophysics, 01 natural sciences, Computer Science Applications, Education
Published
2018
Full Text
View/download PDF

8. Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using Its General Relativity Centenary Flare: Improved Orbital Parameters

Author

Lankeswar Dey, M. J. Valtonen, A. Gopakumar, S. Zola, R. Hudec, P. Pihajoki, S. Ciprini, K. Matsumoto, K. Sadakane, M. Kidger, K. Nilsson, S. Mikkola, A. Sillanpää, L. O. Takalo, H. J. Lehto, A. Berdyugin, V. Piirola, H. Jermak, K. S. Baliyan, T. Pursimo, D. B. Caton, F. Alicavus, A. Baransky, P. Blay, P. Boumis, D. Boyd, M. Campas Torrent, F. Campos, J. Carrillo Gómez, S. Chandra, V. Chavushyan, J. Dalessio, B. Debski, M. Drozdz, H. Er, A. Erdem, A. Escartin Pérez, V. Fallah Ramazani, A. V. Filippenko, E. Gafton, S. Ganesh, F. Garcia, K. Gazeas, V. Godunova, F. Gómez Pinilla, M. Gopinathan, J. B. Haislip, J. Harmanen, G. Hurst, J. Janík, M. Jelinek, A. Joshi, M. Kagitani, R. Karjalainen, N. Kaur, W. C. Keel, V. V. Kouprianov, T. Kundera, S. Kurowski, A. Kvammen, A. P. LaCluyze, B. C. Lee, A. Liakos, E. Lindfors, J. Lozano de Haro, M. Mugrauer, R. Naves Nogues, A. W. Neely, R. H. Nelson, W. Ogloza, S. Okano, U. Pajdosz-Śmierciak, J. C. Pandey, M. Perri, G. Poyner, J. Provencal, A. Raj, D. E. Reichart, R. Reinthal, T. Reynolds, J. Saario, S. Sadegi, T. Sakanoi, J.-L. Salto González, null Sameer, T. Schweyer, A. Simon, M. Siwak, F. C. Soldán Alfaro, E. Sonbas, I. Steele, J. T. Stocke, J. Strobl, T. Tomov, L. Tremosa Espasa, J. R. Valdes, J. Valero Pérez, F. Verrecchia, V. Vasylenko, J. R. Webb, M. Yoneda, M. Zejmo, W. Zheng, P. Zielinski, and Department of Physics

Subjects
General relativity, Astrophysics::High Energy Astrophysical Phenomena, black hole physics, OJ-287, FOS: Physical sciences, GRAVITATIONAL-RADIATION REACTION, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, individual: OJ 287 [quasars], OUTBURSTS, 01 natural sciences, General Relativity and Quantum Cosmology, law.invention, VDP::Matematikk og Naturvitenskap: 400::Fysikk: 430::Astrofysikk, astronomi: 438, Binary black hole, MOMENTS, law, quasars: general, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, QC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Orbital elements, Physics, general [quasars], COMPACT BINARIES, OJ287, 010308 nuclear & particles physics, Gravitational wave, quasars: individual (OJ 287), SYSTEMS NONSPINNING BODIES, Astronomy and Astrophysics, 115 Astronomy, Space science, Orbital period, Astrophysics - Astrophysics of Galaxies, VDP::Mathematics and natural science: 400::Physics: 430::Astrophysics, astronomy: 438, MODEL, Black hole, SPIN, gravitation, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, WAVE-FORM, Flare
Abstract

Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the binary black hole model for OJ~287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the binary black hole central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level., 24 pages, 11 figures, 3 tables, accepted for publication in ApJ

Published
2018
Full Text
View/download PDF

9. Pluto's atmosphere from stellar occultations in 2012 and 2013

Author

A. Dias-Oliveira, B. Sicardy, E. Lellouch, R. Vieira-Martins, M. Assafin, J. I. B. Camargo, F. Braga-Ribas, A. R. Gomes-Júnior, G. Benedetti-Rossi, F. Colas, A. Decock, A. Doressoundiram, C. Dumas, M. Emilio, J. Fabrega Polleri, R. Gil-Hutton, M. Gillon, J. H. Girard, G. K. T. Hau, V. D. Ivanov, E. Jehin, J. Lecacheux, R. Leiva, C. Lopez-Sisterna, L. Mancini, J. Manfroid, A. Maury, E. Meza, N. Morales, L. Nagy, C. Opitom, J. L. Ortiz, J. Pollock, F. Roques, C. Snodgrass, J. F. Soulier, A. Thirouin, L. Vanzi, T. Widemann, D. E. Reichart, A. P. LaCluyze, J. B. Haislip, K. M. Ivarsen, M. Dominik, U. Jørgensen, J. Skottfelt, Observatório Nacional/MCTI, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatório do Valongo, Universidade Federal do Rio de Janeiro, UTFPR, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Astéroïdes, comètes, météores et éphémérides (ACME), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, ESO, UEPG, Observatorio Panemno, CASLEO-CONICET, Universite de Liege, PUC, Universidade Nacional de San Juan, Max-Planck-Institut für Astronomie (MPIA), S.P.A.C.E, Instituto de Astrofisica de Andalucia, CSIC (IAA), Appalachian State University, CEPSAR, The Open University, Association T60, Observatoire Midi-Pyrénées, Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, Lowell Observatory, Flagstaff, University of North Carolina, School of Chemistry, University of St Andrews, University of Copenhagen, Observatorio Nacional [Rio de Janeiro], Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatório Nacional/MCT, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatório do Valongo/UFRJ [Rio de Janeiro], Universidade Federal do Rio de Janeiro [Rio de Janeiro] (UFRJ), Universidade Estadual de Ponta Grossa, Universidade Estadual de Ponta Grossa - State University of Ponta Grossa (UEPG), Universidad Nacional de San Juan (UNSJ), Arctic and Antarctic Research Institute (AARI), Russian Federal Service for Hydrometeorology and Environmental Monitoring (Roshydromet), European Southern Observatory (ESO), Southwest Research Institute [Boulder] (SwRI), Centre de Nanosciences et Nanotechnologies (C2N (UMR_9001)), Université Paris-Sud - Paris 11 (UP11)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Physics and Astronomy [Boone], University of North Carolina System (UNC)-University of North Carolina System (UNC), School of Physical Sciences [Milton Keynes], The Open University [Milton Keynes] (OU), Lowell Observatory [Flagstaff], Dynamiques patrimoniales et culturelles (DYPAC), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade Federal do Rio de Janeiro (UFRJ), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Universidad Nacional de San Juan [Argentine] (UNSJ), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), The Royal Society, and University of St Andrews. School of Physics and Astronomy

Subjects
010504 meteorology & atmospheric sciences, NDAS, FOS: Physical sciences, Astrophysics, 01 natural sciences, Mesosphere, Troposphere, Atmosphere, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, QB Astronomy, observational [Methods], data analysis [Methods], 010303 astronomy & astrophysics, Stratosphere, physical evolution [Planets and satellites], QC, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], photometric [Techniques], Center (category theory), Astronomy and Astrophysics, Radius, Pluto, Temperature gradient, QC Physics, 13. Climate action, Space and Planetary Science, terrestrial planets [Planets and satellites], atmospheres [Planets and satellites], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We analyze two multi-chord stellar occultations by Pluto observed on July 18th, 2012 and May 4th, 2013, and monitored respectively from five and six sites. They provide a total of fifteen light-curves, twelve of them being used for a simultaneous fit that uses a unique temperature profile, assuming a clear (no-haze) and pure N_2 atmosphere, but allowing for a possible pressure variation between the two dates. We find a solution that fits satisfactorily (i.e. within the noise level) all the twelve light-curves, providing atmospheric constraints between ~1,190 km (pressure ~ 11 \mubar) and ~ 1,450 km (pressure ~0.1 \mubar) from Pluto's center. Our main results are: (1) the best-fitting temperature profile shows a stratosphere with strong positive gradient between 1,190 km (at 36 K, 11 \mubar) and r = 1,215 km (6.0 \mubar), where a temperature maximum of 110 K is reached; above it is a mesosphere with negative thermal gradient of -0.2 K/km up to ~ 1,390 km (0.25 \mubar), where, the mesosphere connects itself to a more isothermal upper branch around 81 K; (2) the pressure shows a small (6 %) but significant increase (6-\sigma level) between the two dates; (3) without troposphere, Pluto's radius is found to be R_P = 1,190 +/- 5km. Allowing for a troposphere, R_P is constrained to lie between 1,168 and 1,195 km; (4) the currently measured CO abundance is too small to explain the mesospheric negative thermal gradient. Cooling by HCN is possible, but only if this species is largely saturated; Alternative explanations like zonal winds or vertical compositional variations of the atmosphere are unable to explain the observed mesospheric trend., Comment: 41 pages, 13 figures, 4 tables

Published
2015
Full Text
View/download PDF

10. SN 2017gmr: An Energetic Type II-P Supernova with Asymmetries

Author

Curtis McCully, Brajesh Kumar, Róbert Szakáts, Avishay Gal-Yam, Scott C. Davis, M. J. Singh, Iair Arcavi, Kuntal Misra, Nidia Morrell, Kate Maguire, Marco Berton, S. Valenti, Lluís Galbany, Peter Milne, Anjasha Gangopadhyay, S. Chen, Mattia Bulla, Paolo A. Mazzali, Ósmar Rodríguez, G. C. Anupama, Huijuan Wang, D. K. Sahu, Ferdinando Patat, G. Pignata, Jamison Burke, Mark M. Phillips, Maximilian Stritzinger, Stephen J. Smartt, Chris Ashall, Matt Nicholl, Jay Strader, Jun Mo, Nancy Elias-Rosa, Junbo Zhang, Danfeng Xiang, Christa Gall, Jennifer E. Andrews, Hanindyo Kuncarayakti, F. Olivares, J. B. Haislip, S. J. Prentice, D. E. Reichart, Griffin Hosseinzadeh, Han Lin, Morgan Fraser, Daichi Hiramatsu, John C Wheeler, S. Benetti, D. R. Young, Raya Dastidar, Peter J. Brown, P. Ochner, Melissa Shahbandeh, Enrico Congiu, Liming Rui, O. Yaron, Pankaj Sanwal, Krisztián Sárneczky, Mariusz Gromadzki, David J. Sand, Erkki Kankare, Laura Chomiuk, Aleksandar Cikota, B. Cseh, A. Pastorello, Vladimir Kouprianov, K. A. Bostroem, Tamar Faran, S. Wyatt, Leonardo Tartaglia, Eric Hsiao, D. A. Howell, Nathan Smith, Jozsef Vinko, Xiaofeng Wang, Lingzhi Wang, A. Reguitti, Cosimo Inserra, Xue Li, Avinash Singh, ITA, USA, GBR, DEU, ESP, CHL, DNK, FIN, IND, IRL, ISR, POL, CHN, RUS, SWE, HUN, University of Arizona, University of California Davis, Aryabhatta Research Institute of Observational Sciences, Indian Institute of Astrophysics, University of California Santa Barbara, Texas A&M University, Harvard University, Hungarian Academy of Sciences, Tel Aviv University, Florida State University, INAF - Osservatorio Astronomico di Padova, Metsähovi Radio Observatory, Stockholm University, Michigan State University, Lawrence Berkeley National Laboratory, Osservatorio Astronomico di Brera, CSIC, Hebrew University of Jerusalem, University College Dublin, University of Pittsburgh, Niels Bohr Institute, Weizmann Institute of Science, University of Warsaw, University of North Carolina at Chapel Hill, Cardiff University, University of Turku, Tsinghua University, Trinity College Dublin, Liverpool John Moores University, Carnegie Institution for Science, University of Edinburgh, Universidad de Atacama, European Southern Observatory, Millennium Institute of Astrophysics (MAS), Queen's University Belfast, Aarhus University, KTH Royal Institute of Technology, CAS - National Astronomical Observatories, University of Texas at Austin, Aalto-yliopisto, and Aalto University

Subjects
Type II supernovae (1731), Core-collapse supernovae (304), Massive stars (732), astro-ph.SR, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, Atomic, 01 natural sciences, 7. Clean energy, NO, Luminosity, Particle and Plasma Physics, Massive stars, 0103 physical sciences, Core-collapse supernovae, Nuclear, Red supergiant, Astronomy and Astrophysics Programme, Emission spectrum, Ejecta, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), QC, 0105 earth and related environmental sciences, QB, Type II supernovae, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Molecular, Astronomy and Astrophysics, Light curve, Supernova, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Energy source, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We present high-cadence ultraviolet (UV), optical, and near-infrared (NIR) data on the luminous Type II-P supernova SN 2017gmr from hours after discovery through the first 180 days. SN 2017gmr does not show signs of narrow, high-ionization emission lines in the early optical spectra, yet the optical lightcurve evolution suggests that an extra energy source from circumstellar medium (CSM) interaction must be present for at least 2 days after explosion. Modeling of the early lightcurve indicates a ~500R$_{\odot}$ progenitor radius, consistent with a rather compact red supergiant, and late-time luminosities indicate up to 0.130 $\pm$ 0.026 M$_{\odot}$ of $^{56}$Ni are present, if the lightcurve is solely powered by radioactive decay, although the $^{56}$Ni mass may be lower if CSM interaction contributes to the post-plateau luminosity. Prominent multi-peaked emission lines of H$\alpha$ and [O I] emerge after day 154, as a result of either an asymmetric explosion or asymmetries in the CSM. The lack of narrow lines within the first two days of explosion in the likely presence of CSM interaction may be an example of close, dense, asymmetric CSM that is quickly enveloped by the spherical supernova ejecta., Comment: Submitted to ApJ, 25 pages, plus Appendix

Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results