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1. The ASAS-SN bright supernova catalogue – IV. 2017

Author

T W-S Holoien, J S Brown, P J Vallely, K Z Stanek, C S Kochanek, B J Shappee, J L Prieto, Subo Dong, J Brimacombe, D W Bishop, S Bose, J F Beacom, D Bersier, Ping Chen, L Chomiuk, E Falco, S Holmbo, T Jayasinghe, N Morrell, G Pojmanski, J V Shields, J Strader, M D Stritzinger, Todd A Thompson, P R Woźniak, G Bock, P Cacella, J G Carballo, I Cruz, E Conseil, R G Farfan, J M Fernandez, S Kiyota, R A Koff, G Krannich, P Marples, G Masi, L A G Monard, J A Muñoz, B Nicholls, R S Post, G Stone, D L Trappett, and W S Wiethoff

Published
2019
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2. The ASAS-SN Bright Supernova Catalog -- V. 2018-2020

Author

K D Neumann, T W-S Holoien, C S Kochanek, K Z Stanek, P J Vallely, B J Shappee, J L Prieto, T Pessi, T Jayasinghe, J Brimacombe, D Bersier, E Aydi, C Basinger, J F Beacom, S Bose, J S Brown, P Chen, A Clocchiatti, D D Desai, Subo Dong, E Falco, S Holmbo, N Morrell, J V Shields, K V Sokolovsky, J Strader, M D Stritzinger, S Swihart, T A Thompson, Z Way, L Aslan, D W Bishop, G Bock, J Bradshaw, P Cacella, N Castro-Morales, E Conseil, R Cornect, I Cruz, R G Farfan, J M Fernandez, A Gabuya, J-L Gonzalez-Carballo, M R Kendurkar, S Kiyota, R A Koff, G Krannich, P Marples, G Masi, L A G Monard, J A Muñoz, B Nicholls, R S Post, Z Pujic, G Stone, L Tomasella, D L Trappett, and W S Wiethoff

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We catalog the 443 bright supernovae discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN) in $2018-2020$ along with the 519 supernovae recovered by ASAS-SN and 516 additional $m_{peak}\leq18$ mag supernovae missed by ASAS-SN. Our statistical analysis focuses primarily on the 984 supernovae discovered or recovered in ASAS-SN $g$-band observations. The complete sample of 2427 ASAS-SN supernovae includes earlier $V$-band samples and unrecovered supernovae. For each supernova, we identify the host galaxy, its UV to mid-IR photometry, and the offset of the supernova from the center of the host. Updated light curves, redshifts, classifications, and host galaxy identifications supersede earlier results. With the increase of the limiting magnitude to $g\leq18$ mag, the ASAS-SN sample is roughly complete up to $m_{peak}=16.7$ mag and is $90\%$ complete for $m_{peak}\leq17.0$ mag. This is an increase from the $V$-band sample where it was roughly complete up to $m_{peak}=16.2$ mag and $70\%$ complete for $m_{peak}\leq17.0$ mag., Comment: 14 pages, 7 figures, 4 tables. Updated to reflect changes made in the published version. Tables containing the catalog data presented in this submission are included in machine-readable format as ancillary files

Published
2022
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3. International observational campaign of the 2014 eclipse of EE Cephei

Author

Ian Miller, Diana P. Kjurkchieva, D. Pieńkowski, Andrzej S. Baran, Sunay Ibryamov, G. Apostolovska, K. Wiersema, P. Bruś, Marek Drozdz, Michal Siwak, L. Corp, Z. Garai, J. Menke, P. Wychudzki, A. Capetillo Blanco, Staszek Zola, J. Ribeiro, Waldemar Ogloza, D. Rodriguez, L. Logie, Bart Staels, Maciej Mikolajewski, E. Kardasis, D. Moździerski, J. Kare Trandem Qvam, M. Rodriguez, Noel D. Richardson, Cezary Galan, M. Biskupski, T. Kamiński, T. Kundera, Z. Donchev, M. Winiarski, M. Martignoni, Z. Kołaczkowski, L. Hambálek, I. Plauchu-Frayn, Toma Tomov, P. McDonald, I. Sergey, G. J. Conidis, E. Zahajkiewicz, Dinko Dimitrov, A. Armiński, T. Pribulla, Dragomir Marchev, E. Conseil, E. Świerczyński, Kosmas Gazeas, B. Dȩbski, Emil Kundra, Stoyanka Peneva, Andrzej Pigulski, F. Dubois, R. Kneip, A. Sanchez, David Boyd, J. L. Gonzalez Carballo, Evgeni Semkov, T. Smela, Paweł Kankiewicz, D. Kubicki, T. A. Heras, P. Pakońska, and S. Dean

Subjects
Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Ephemeris, 01 natural sciences, Spectral line, Photometry (optics), Amplitude, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Primary (astronomy), 0103 physical sciences, Precession, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Eclipse
Abstract

Context. EE Cep is one of few eclipsing binary systems with a dark, dusty disk around an invisible object similar to {\epsilon} Aur. The system is characterized by grey and asymmetric eclipses every 5.6 yr, with a significant variation in their photometric depth, ranging from ~ 0 m .5 to ~ 2 m .0. Aims. The main aim of the observational campaign of the EE Cep eclipse in 2014 was to test the model of disk precession (Galan et al. 2012). We expected that this eclipse would be one of the deepest with a depth of ~ 2 m .0. Methods. We collected multicolor observations from almost 30 instruments located in Europe and North America. This photometric data covers 243 nights during and around the eclipse. We also analyse the low- and high-resolution spectra from several instruments. Results. The eclipse was shallow with a depth of 0 m .71 in V-band. The multicolor photometry illustrates small color changes during the eclipse with a total amplitude of order ~ +0 m . 15 in B-I color index. The linear ephemeris for this system is updated by including new times of minima, measured from the three most recent eclipses at epochs E = 9, 10 and 11. New spectroscopic observations were acquired, covering orbital phases around the eclipse, which were not observed in the past and increased the data sample, filling some gaps and giving a better insight into the evolution of the H {\alpha} and NaI spectral line profiles during the primary eclipse. Conclusions. The eclipse of EE Cep in 2014 was shallower than expected 0 m .71 instead of ~ 2 m . 0. This means that our model of disk precession needs revision., Comment: 10 pages, 13 figures, 29 tables in appendix, submited to Astronomy & Astrophysics

Published
2020

4. SN 2012fr: Ultraviolet, Optical, and Near-Infrared Light Curves of a Type Ia Supernova Observed Within a Day of Explosion

Author

David Rabinowitz, C. Baltay, Wendy L. Freedman, Peter Nugent, Richard Scalzo, M. Childress, Damien Turpin, Peter Hoeflich, Christopher Cain, Nicholas B. Suntzeff, Nidia Morrell, Emma S. Walker, S. Castellon, Brian P. Schmidt, E. Conseil, Carlos Contreras, Alain Klotz, Maximilian Stritzinger, Gastón Folatelli, Brad E. Tucker, Christopher R. Burns, Eric Hsiao, Peter J. Brown, Kevin Krisciunas, C. Corco, Benjamin J. Shappee, S. Parker, Anthony L. Piro, J. Serón, S. E. Persson, Mario Hamuy, Mark M. Phillips, C. Gonzalez, Abdo Campillay, E. Baron, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Infrared, DELAY-TIME DISTRIBUTION, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Ciencias Físicas, CHEMICAL EVOLUTION, Astrophysics, medicine.disease_cause, 01 natural sciences, Atomic, Physical Chemistry, purl.org/becyt/ford/1 [https], Particle and Plasma Physics, 010303 astronomy & astrophysics, Ultraviolet radiation, Physics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), supernovae: individual (SN 2012fr), Visible radiation, Supernova, IMPROVED DISTANCES, Astrophysics - High Energy Astrophysical Phenomena, Astronomical and Space Sciences, CIENCIAS NATURALES Y EXACTAS, Physical Chemistry (incl. Structural), INDIVIDUAL (SN 2012FR) [SUPERNOVAE], MAXIMUM BRIGHTNESS, FOS: Physical sciences, Astronomy & Astrophysics, NEBULAR-PHASE SPECTRA, GENERAL [SUPERNOVAE], supernovae: general, ABUNDANCE RATIOS, individual [supernovae], 0103 physical sciences, medicine, Nuclear, WHITE-DWARFS, supernovae: individual, Near infrared light, 010308 nuclear & particles physics, STANDARD STARS, Molecular, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Astronomía, Space and Planetary Science, DIGITAL SKY SURVEY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Near infrared radiation, Ultraviolet, HUBBLE CONSTANT
Abstract

We present detailed ultraviolet, optical, and near-infrared light curves of the Type Ia supernova (SN) 2012fr, which exploded in the Fornax cluster member NGC 1365. These precise high-cadence light curves provide a dense coverage of the flux evolution from −12 to +140 days with respect to the epoch of B-band maximum (tBmax). Supplementary imaging at the earliest epochs reveals an initial slow and nearly linear rise in luminosity with a duration of ∼2.5 days, followed by a faster rising phase that is well reproduced by an explosion model with a moderate amount of 56Ni mixing in the ejecta. From our analysis of the light curves, we conclude that: (i) the explosion occurred 1800 Å) luminosity was 16.5 ± 0.6 days, (iii) the supernova suffered little or no host-galaxy dust reddening, (iv) the peak luminosity in both the optical and near-infrared was consistent with the bright end of normal Type Ia diversity, and (v) 0.60 ± 0.15 M⊙ of 56Ni was synthesized in the explosion. Despite its normal luminosity, SN 2012fr displayed unusually prevalent high-velocity Ca II and Si II absorption features, and a nearly constant photospheric velocity of the Si II λ6355 line at ∼12,000 km s-1 that began ∼5 days before tBmax. We also highlight some of the other peculiarities in the early phase photometry and the spectral evolution. SN 2012fr also adds to a growing number of Type Ia supernovae that are hosted by galaxies with direct Cepheid distance measurements., Facultad de Ciencias Astronómicas y Geofísicas, Instituto de Astrofísica de La Plata

Published
2018
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5. The ASAS-SN Bright Supernova Catalog $-$ II. 2015

Author

J. M. F. Andújar, U. Basu, Przemysław Woźniak, Subo Dong, Krzysztof Z. Stanek, Zhen Guo, G. Krannich, D. Godoy-Rivera, D. M. Skowron, G. Pojmanski, C. G. Ávila, Peter Marples, J. Nicolas, G. Bock, Nidia Morrell, Christopher S. Kochanek, E. Conseil, Thomas W.-S. Holoien, Eric Hsiao, S. Kiyota, R. M. Wagner, J. S. Brown, B. Nicholls, G. V. Simonian, D. Bersier, Todd A. Thompson, Carlos Contreras, Robert Koff, Ping Chen, Juan-Carlos Muñoz-Mateos, Joseph Brimacombe, J. L. Prieto, I. Cruz, John F. Beacom, Benjamin J. Shappee, E. E. Falco, J. G. Carballo, W. Wiethoff, Barry F. Madore, L. A. G. Monard, N. Goss, G. Masi, D. W. Bishop, and A. B. Danilet

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Supernova, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB
Abstract

This manuscript presents information for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during 2015, its second full year of operations. The same information is presented for bright ($m_V\leq17$), spectroscopically confirmed supernovae discovered by other sources in 2015. As with the first ASAS-SN bright supernova catalog, we also present redshifts and near-UV through IR magnitudes for all supernova host galaxies in both samples. Combined with our previous catalog, this work comprises a complete catalog of 455 supernovae from multiple professional and amateur sources, allowing for population studies that were previously impossible. This is the second of a series of yearly papers on bright supernovae and their hosts from the ASAS-SN team., 16 pages, 6 figures, 4 tables. Submitted to MNRAS. Tables containing the catalog data presented in this submission are included in machine-readable format as ancillary files. Manuscript updated to reflect changes made in the published version and to correct an error in the host galaxy magnitudes presented in Tables 3 and 4. For a brief video explaining this paper, see https://youtu.be/iqYJp1AmyMw

Published
2016

6. Astronomy. ASASSN-15lh: A highly super-luminous supernova

Author

Subo, Dong, B J, Shappee, J L, Prieto, S W, Jha, K Z, Stanek, T W-S, Holoien, C S, Kochanek, T A, Thompson, N, Morrell, I B, Thompson, U, Basu, J F, Beacom, D, Bersier, J, Brimacombe, J S, Brown, F, Bufano, Ping, Chen, E, Conseil, A B, Danilet, E, Falco, D, Grupe, S, Kiyota, G, Masi, B, Nicholls, F, Olivares E, G, Pignata, G, Pojmanski, G V, Simonian, D M, Szczygiel, and P R, Woźniak

Abstract

We report the discovery of ASASSN-15lh (SN 2015L), which we interpret as the most luminous supernova yet found. At redshift z = 0.2326, ASASSN-15lh reached an absolute magnitude of Mu ,AB = -23.5 ± 0.1 and bolometric luminosity Lbol = (2.2 ± 0.2) × 10(45) ergs s(-1), which is more than twice as luminous as any previously known supernova. It has several major features characteristic of the hydrogen-poor super-luminous supernovae (SLSNe-I), whose energy sources and progenitors are currently poorly understood. In contrast to most previously known SLSNe-I that reside in star-forming dwarf galaxies, ASASSN-15lh appears to be hosted by a luminous galaxy (MK ≈ -25.5) with little star formation. In the 4 months since first detection, ASASSN-15lh radiated (1.1 ± 0.2) × 10(52) ergs, challenging the magnetar model for its engine.

Published
2016

7. Asassn-15lh: a highly super-luminous supernova

Author

G. Masi, F. Bufano, J. Brimacombe, D. Bersier, E. Conseil, Thomas W.-S. Holoien, Dirk Grupe, John F. Beacom, Krzysztof Z. Stanek, Christopher S. Kochanek, G. Pignata, U. Basu, P. R. Wozniak, Subo Dong, A. B. Danilet, G. Pojmanski, D. M. Szczygiel, J. L. Prieto, E. E. Falco, Benjamin J. Shappee, F. Olivares, B. Nicholls, G. V. Simonian, J. S. Brown, Saurabh Jha, Nidia Morrell, S. Kiyota, Todd A. Thompson, Ping Chen, and Ian B. Thompson

Subjects
Absolute magnitude, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, 010308 nuclear & particles physics, Star formation, FOS: Physical sciences, Astrophysics, Magnetar, 01 natural sciences, Galaxy, Luminosity, Supernova, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Energy source, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Dwarf galaxy
Abstract

We report the discovery of ASASSN-15lh (SN 2015L), which we interpret as the most luminous supernova yet found. At redshift z = 0.2326, ASASSN-15lh reached an absolute magnitude of M_{u,AB} = -23.5+/-0.1 and bolometric luminosity L_bol = (2.2+/-0.2)x 10^45 ergs s^-1, which is more than twice as luminous as any previously known supernova. It has several major features characteristic of the hydrogen-poor super-luminous supernovae (SLSNe-I), whose energy sources and progenitors are currently poorly understood. In contrast to most previously known SLSNe-I that reside in star-forming dwarf galaxies, ASASSN-15lh appears to be hosted by a luminous galaxy (M_K ~ -25.5) with little star formation. In the 4 months since first detection, ASASSN-15lh radiated (1.1+/- 0.2)x10^52 ergs, challenging the magnetar model for its engine., Comment: Published in the January 15, 2016 Issue of Science Magazine

Published
2016

8. Historical vanishing of the Blazhko effect of RR Lyr from the GEOS and Kepler surveys

Author

F. Kugel, C Drillaud, E. Conseil, J. F. Le Borgne, Alain Klotz, E. Poretti, D Loughney, Kenji Hirosawa, S. T. Bryson, E. Denoux, Katrien Kolenberg, Róbert Szabó, K. Graham, P. M Ruscitti, J Caron, Mónica Rodríguez, C. Buil, A. Klotz, Horace A. Smith, Kenneth Menzies, L Corp, and M. Audejean

Subjects
oscillations [stars], Physics, Brightness, 010308 nuclear & particles physics, Blazhko effect, Astronomy, Astronomy and Astrophysics, Astrophysics, RR Lyrae variable, Light curve, 01 natural sciences, variables: RR Lyrae [stars], photometric [techniques], Stars, Amplitude, Space and Planetary Science, 0103 physical sciences, individual: RR Lyrae [stars], Variable star, Maxima, 010303 astronomy & astrophysics
Abstract

RR Lyr is one of the most studied variable stars. Its light curve has been regularly monitored since the discovery of its periodic variability in 1899. The analysis of all observed maxima allows us to identify two primary pulsation states, defined as pulsation over a long (P0 longer than 0.56684 d) and a short (P0 shorter than 0.56682 d) primary pulsation period. These states alternate with intervals of 13-16 yr, and are well defined after 1943. The 40.8-d periodical modulations of the amplitude and the period (i.e. the Blazhko effect) were noticed in 1916. We provide homogeneous determinations of the Blazhko period in the different primary pulsation states. The Blazhko period does not follow the variations of P0 and suddenly diminished from 40.8 d to around 39.0 d in 1975. The monitoring of these periodicities deserved, and still deserves, a continuous and intensive observational effort. For this purpose, we have built dedicated, transportable and autonomous small instruments, Very Tiny Telescopes (VTTs), to observe the times of maximum brightness of RR Lyr. As immediate results, the VTTs recorded the last change of the P0 state in mid-2009 and extended the time coverage of the Kepler observations, thus recording a maximum O - C amplitude of the Blazhko effect at the end of 2008, followed by the historically smallest O - C amplitude in late 2013. This decrease is still ongoing and the VTTs are ready to monitor the expected increase in the next few years. 10 pages, 6 figures. Accepted for publication in MNRAS. Contents of appendix B may be requested to first author ispartof: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY vol:441 issue:2 pages:1435-1443 status: published

Published
2014

9. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

Author

A. Santerne, G. Hébrard, J. Lillo-Box, D. J. Armstrong, S. C. C. Barros, O. Demangeon, D. Barrado, A. Debackere, M. Deleuil, E. Delgado Mena, M. Montalto, D. Pollacco, H. P. Osborn, S. G. Sousa, L. Abe, V. Adibekyan, J.-M. Almenara, P. André, G. Arlic, G. Barthe, P. Bendjoya, R. Behrend, I. Boisse, F. Bouchy, H. Boussier, M. Bretton, D. J. A. Brown, B. Carry, A. Cailleau, E. Conseil, G. Coulon, B. Courcol, B. Dauchet, J.-C. Dalouzy, M. Deldem, O. Desormières, P. Dubreuil, J.-M. Fehrenbach, S. Ferratfiat, R. Girelli, J. Gregorio, S. Jaecques, F. Kugel, J. Kirk, O. Labrevoir, J.-C. Lachurié, K. W. F. Lam, P. Le Guen, P. Martinez, L. P. A. Maurin, J. McCormac, J-B. Pioppa, U. Quadri, A. Rajpurohit, J. Rey, J.-P. Rivet, R. Roy, N. C. Santos, F. Signoret, L. Strabla, O. Suarez, D. Toublanc, M. Tsantaki, J.-M. Vienney, P. A. Wilson, M. Bachschmidt, F. Colas, O. Gerteis, P. Louis, J.-C. Mario, C. Marlot, J. Montier, V. Perroud, V. Pic, D. Romeuf, S. Ubaud, D. Verilhac, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Virologia, Laboratorio Nacional de Investigacao Veterinaria (LNIV), Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, 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), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Geneva Observatory, University of Geneva [Switzerland], CdR & CdL group, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire Chante-Perdrix, School of Physics and Astronomy [Cardiff], Cardiff University, Hôpital Européen Georges Pompidou [APHP] (HEGP), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département RadioChimie et Procédés (DRCP), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval [Québec] (ULaval), Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), Universidade do Porto [Porto], Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - 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Paris 6 (UPMC), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Paris-Sud - Paris 11 ( UP11 ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), LAEX, Depto. 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Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), School of Physis & Astronomy, Hôpital Européen Georges Pompidou [APHP] ( HEGP ), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux ( EPOC ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -École pratique des hautes études ( EPHE ) -Centre National de la Recherche Scientifique ( CNRS ), Département RadioChimie et Procédés ( DRCP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), 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 Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables ( CdR & CdL group ), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Genève = University of Geneva (UNIGE), Environnements et Paléoenvironnements OCéaniques (EPOC), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École Pratique des Hautes Études (EPHE), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-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)-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 -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), 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 do Porto-Universidade do Porto, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
Physics, 010308 nuclear & particles physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Stellar rotation, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, 01 natural sciences, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Magnitude (astronomy), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Visual binary
Abstract

International audience; In the present paper we report the discovery of a new hot Jupiter, K2-29 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25 days, a mass of 0.73 +/- 0.04M(sic), and a radius of 1.19 +/- 0.02 R(sic). The host star is a relatively bright (V = 12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of lithium, we find that the system might be as young as similar to 450 Myr. The observation of the Rossiter-McLaughlin effect shows that the planet is aligned with respect to the stellar spin. Given the deep transit (20 mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where both stars are relatively bright.

Published
2016
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10. New and updated convex shape models of asteroids based on optical data from a large collaboration network

Author

J. Hanuš, J. Ďurech, D. A. Oszkiewicz, R. Behrend, B. Carry, M. Delbo, O. Adam, V. Afonina, R. Anquetin, P. Antonini, L. Arnold, M. Audejean, P. Aurard, M. Bachschmidt, B. Baduel, E. Barbotin, P. Barroy, P. Baudouin, L. Berard, N. Berger, L. Bernasconi, J-G. Bosch, S. Bouley, I. Bozhinova, J. Brinsfield, L. Brunetto, G. Canaud, J. Caron, F. Carrier, G. Casalnuovo, S. Casulli, M. Cerda, L. Chalamet, S. Charbonnel, B. Chinaglia, A. Cikota, F. Colas, J.-F. Coliac, A. Collet, J. Coloma, M. Conjat, E. Conseil, R. Costa, R. Crippa, M. Cristofanelli, Y. Damerdji, A. Debackère, A. Decock, Q. Déhais, T. Déléage, S. Delmelle, C. Demeautis, M. Dróżdż, G. Dubos, T. Dulcamara, M. Dumont, R. Durkee, R. Dymock, A. Escalante del Valle, N. Esseiva, R. Esseiva, M. Esteban, T. Fauchez, M. Fauerbach, M. Fauvaud, S. Fauvaud, E. Forné, C. Fournel, D. Fradet, J. Garlitz, O. Gerteis, C. Gillier, M. Gillon, R. Giraud, J.-P. Godard, R. Goncalves, Hiroko Hamanowa, Hiromi Hamanowa, K. Hay, S. Hellmich, S. Heterier, D. Higgins, R. Hirsch, G. Hodosan, M. Hren, A. Hygate, N. Innocent, H. Jacquinot, S. Jawahar, E. Jehin, L. Jerosimic, A. Klotz, W. Koff, P. Korlevic, E. Kosturkiewicz, P. Krafft, Y. Krugly, F. Kugel, O. Labrevoir, J. Lecacheux, M. Lehký, A. Leroy, B. Lesquerbault, M. J. Lopez-Gonzales, M. Lutz, B. Mallecot, J. Manfroid, F. Manzini, A. Marciniak, A. Martin, B. Modave, R. Montaigut, J. Montier, E. Morelle, B. Morton, S. Mottola, R. Naves, J. Nomen, J. Oey, W. Ogłoza, M. Paiella, H. Pallares, A. Peyrot, F. Pilcher, J.-F. Pirenne, P. Piron, M. Polińska, M. Polotto, R. Poncy, J. P. Previt, F. Reignier, D. Renauld, D. Ricci, F. Richard, C. Rinner, V. Risoldi, D. Robilliard, D. Romeuf, G. Rousseau, R. Roy, J. Ruthroff, P. A. Salom, L. Salvador, S. Sanchez, T. Santana-Ros, A. Scholz, G. Séné, B. Skiff, K. Sobkowiak, P. Sogorb, F. Soldán, A. Spiridakis, E. Splanska, S. Sposetti, D. Starkey, R. Stephens, A. Stiepen, R. Stoss, J. Strajnic, J.-P. Teng, G. Tumolo, A. Vagnozzi, B. Vanoutryve, J. M. Vugnon, B. D. Warner, M. Waucomont, O. Wertz, M. Winiarski, M. Wolf, Charles University [Prague] (CU), Astronomical Institute of Charles University, Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Geneva Observatory, Université de Genève = University of Geneva (UNIGE), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Bédoin, Observatoire de Chinon, Association des Utilisateurs de Détecteurs Electroniques, Laboratoire de Physique de la Matière Condensée - UR UPJV 2081 (LPMC), Université de Picardie Jules Verne (UPJV), Harfleur Observatory, Ressources des terroirs - UMR 8575, Centre National de la Recherche Scientifique (CNRS), Les Engarouines Observatory, Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Chercheur indépendant, Laboratoire d'optique des solides (LOS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de l'Université de Genève (ObsGE), Centre de Recherche Saint-Antoine (UMRS893), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de la Santé et de la Recherche Médicale (INSERM), 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, Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), CdR & CdL group, Physik-Institut, Universität Zürich [Zürich] = University of Zurich (UZH), Gestion environnementale et traitement biologique des déchets (UR GERE), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Observatorio de San Gervasi, Observatoire de Cabris, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronómico de Tradate, Observatoire N°139 d'Antibes, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 138 Village-Neuf, Science et Ingénierie des Matériaux et Procédés (SIMaP ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Shed of Science Observatory, Association AstroQueyras, Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire du Bois de Bardon, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Ciências Exatas e Tecnológicas [Viçosa], Universidade Federal de Viçosa = Federal University of Viçosa (UFV), Hamanowa Astronomical Observatory, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), European Southern Observatory (ESO), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-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 -Centre National de la Recherche Scientifique (CNRS), Observatoire Chante-Perdrix, 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), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Stazione Astronomica di Sozzago, Milieux aquatiques, écologie et pollutions (UR MALY), German Aerospace Center (DLR), Observatorio Montcabre, Observatorio Astronómico de Mallorca (OAM), Observatorio Astronómico de Mallorca, Kingsgrove Observatory, Gestion Territoriale de l'Eau et de l'environnement (UMR GESTE), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Organ Mesa Observatory, Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Association des Utilisateurs de Détecteurs Electroniques (AUDE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon, Laboratoire de Recherche sur la Réactivité des Solides (LRRS), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'intégration, du matériau au système (IMS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), Gnosca Observatory, DeKalb Observatory, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Observatoire astronomique des Makes, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Argelander Institute for Astronomy (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Institute of Neuropathology, University hospital of Zurich [Zurich], Charles University [Prague], University of Helsinki-University of Helsinki, University of Geneva [Switzerland], European Space Agency (ESA), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de la Matière Condensée (EA 2081), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Université de Genève (UNIGE), Centre de Recherche Saint-Antoine (CR Saint-Antoine), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées, Universität Zürich [Zürich] (UZH), L2EP - Équipe Réseaux, Laboratoire d’Électrotechnique et d’Électronique de Puissance - EA 2697 (L2EP), Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille-Ecole Centrale de Lille-École Nationale Supérieure d'Arts et Métiers (ENSAM), HESAM Université (HESAM)-HESAM Université (HESAM)-Haute Etude d'Ingénieurs-Université de Lille, Science et Ingénierie des Matériaux et Procédés (SIMaP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Observatoire Midi-Pyrénées and Association T60, Laboratoire de photonique et de nanostructures (LPN), Universidade Federal de Vicosa (UFV), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Centre d'études de chimie métallurgique (CECM), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut Polytechnique de Bordeaux-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Laboratoire d’Électrotechnique et d’Électronique de Puissance - ULR 2697 (L2EP), Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM)-Centrale Lille-Haute Etude d'Ingénieurs-Université de Lille-Arts et Métiers Sciences et Technologies, HESAM Université (HESAM)-HESAM Université (HESAM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), National Science Centre (Poland), Czech Science Foundation, Centre National D'Etudes Spatiales (France), Charles University [Prague] [CU], European Space Astronomy Centre [ESAC], Joseph Louis LAGRANGE [LAGRANGE], Institut de Recherches Subatomiques [IReS], Laboratoire d'Annecy de Physique des Particules [LAPP], Géosciences Paris Sud [GEOPS], Laboratoire d'optique des solides [LOS], Observatoire Astronomique de l'Université de Genève [ObsGE], Gestion environnementale et traitement biologique des déchets [UR GERE], Observatoire astronomique de Strasbourg [ObAS], Science et Ingénierie des Matériaux et Procédés [SIMaP], Laboratoire d’Optique Atmosphérique - UMR 8518 [LOA], Interactions et dynamique des environnements de surface [IDES], Laboratoire de photonique et de nanostructures [LPN], European Southern Observatory [ESO], Institut de recherche en astrophysique et planétologie [IRAP], Laboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA], Milieux aquatiques, écologie et pollutions [UR MALY], German Aerospace Center [DLR], Laboratoire de l'Accélérateur Linéaire [LAL], Université Claude Bernard Lyon 1 [UCBL], Laboratoire de Recherche sur la Réactivité des Solides [LRRS], Laboratoire de l'intégration, du matériau au système [IMS], Laboratoire de Physique Atmosphérique et Planétaire [LPAP], INAF - Osservatorio Astronomico di Padova [OAPD], Argelander Institute for Astronomy [AlfA], ITA, USA, GBR, FRA, DEU, and ESP

Subjects
Solar System, 010504 meteorology & atmospheric sciences, Computer science, media_common.quotation_subject, FOS: Physical sciences, Inverse transform sampling, 01 natural sciences, Gravitation, Photometry (optics), Methods: observational, 0103 physical sciences, QB Astronomy, observational [Methods], Shape optimization, asteroids: general / techniques: photometric / methods: observational / methods: numerical, 010303 astronomy & astrophysics, Scaling, QC, ComputingMilieux_MISCELLANEOUS, QB, 0105 earth and related environmental sciences, media_common, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], numerical [Methods], Methods: numerical, photometric [Techniques], Minor planets, Astronomy, Astronomy and Astrophysics, 3rd-DAS, QC Physics, Minor planets, asteroids: general, Space and Planetary Science, Sky, Asteroid, Physics::Space Physics, minor planets, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [Asteroids], Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics, general [minor planets, asteroids]
Abstract

Context. Asteroid modeling efforts in the last decade resulted in a comprehensive dataset of almost 400 convex shape models and their rotation states. These efforts already provided deep insight into physical properties of main-belt asteroids or large collisional families. Going into finer detail (e.g., smaller collisional families, asteroids with sizes 20 km) requires knowledge of physical parameters of more objects. Aims. We aim to increase the number of asteroid shape models and rotation states. Such results provide important input for further studies, such as analysis of asteroid physical properties in different populations, including smaller collisional families, thermophysical modeling, and scaling shape models by disk-resolved images, or stellar occultation data. This provides bulk density estimates in combination with known masses, but also constrains theoretical collisional and evolutional models of the solar system. Methods. We use all available disk-integrated optical data (i.e., classical dense-in-time photometry obtained from public databases and through a large collaboration network as well as sparse-in-time individual measurements from a few sky surveys) as input for the convex inversion method, and derive 3D shape models of asteroids together with their rotation periods and orientations of rotation axes. The key ingredient is the support of more that 100 observers who submit their optical data to publicly available databases. Results. We present updated shape models for 36 asteroids, for which mass estimates are currently available in the literature, or for which masses will most likely be determined from their gravitational influence on smaller bodies whose orbital deflections will be observed by the ESA Gaia astrometric mission. Moreover, we also present new shape model determinations for 250 asteroids, including 13 Hungarias and three near-Earth asteroids. The shape model revisions and determinations were enabled by using additional optical data from recent apparitions for shape optimization. © 2016 ESO., J.H. greatly appreciates the CNES post-doctoral fellowship program. J.H. and M.D. were supported by the project under the contract 11-BS56-008 (SHOCKS) of the French Agence National de la Recherche (ANR), JD by grant GACR 15-04816S of the Czech Science Foundation, DO by the grant NCN 2012/S/ST9/00022 of Polish National Science Center, and A. Marciniak by grant 2014/13/D/ST9/01818 of Polish National Science Center.

Published
2016
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13. The Young and Bright Type Ia Supernova ASASSN-14lp: Discovery, Early-Time Observations, First-Light Time, Distance to NGC 4666, and Progenitor Constraints

Author

A. B. Danilet, Przemysław Woźniak, Subo Dong, J. Nicolas, E. Conseil, John F. Beacom, Krzysztof Z. Stanek, U. Basu, D. M. Szczygiel, D. Bersier, Christopher S. Kochanek, Eric Hsiao, John R. Thorstensen, Christopher R. Burns, Thomas W.-S. Holoien, K. Itagaki, Dirk Grupe, Francesco Taddia, S. Kiyota, Mark M. Phillips, Todd A. Thompson, E. E. Falco, M. Wagner, G. Pojmanski, Nidia Morrell, J. Brimacombe, Carlos Contreras, Benjamin J. Shappee, E. Alper, Maximilian Stritzinger, Anthony L. Piro, G. V. Simonian, and J. L. Prieto

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Higher education, 010308 nuclear & particles physics, business.industry, Library science, FOS: Physical sciences, Astronomy and Astrophysics, First light, 01 natural sciences, Chinese academy of sciences, Spitzer Space Telescope, Space and Planetary Science, Observatory, 0103 physical sciences, Christian ministry, Time distance, business, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Administration (government), Astrophysics - Cosmology and Nongalactic Astrophysics, QB
Abstract

On 2014 Dec. 9.61, the All-Sky Automated Survey for SuperNovae (ASAS-SN or "Assassin") discovered ASASSN-14lp just $\sim2$ days after first light using a global array of 14-cm diameter telescopes. ASASSN-14lp went on to become a bright supernova ($V = 11.94$ mag), second only to SN 2014J for the year. We present prediscovery photometry (with a detection less than a day after first light) and ultraviolet through near-infrared photometric and spectroscopic data covering the rise and fall of ASASSN-14lp for more than 100 days. We find that ASASSN-14lp had a broad light curve ($\Delta m_{15}(B) = 0.80 \pm 0.05$), a $B$-band maximum at $2457015.82 \pm 0.03$, a rise time of $16.94^{+ 0.11 }_{- 0.10 }$ days, and moderate host--galaxy extinction ($E(B-V)_{\textrm{host}} = 0.33 \pm 0.06$). Using ASASSN-14lp we derive a distance modulus for NGC 4666 of $\mu = 30.8 \pm 0.2$ corresponding to a distance of $14.7 \pm 1.5$ Mpc. However, adding ASASSN-14lp to the calibrating sample of Type Ia supernovae still requires an independent distance to the host galaxy. Finally, using our early-time photometric and spectroscopic observations, we rule out red giant secondaries and, assuming a favorable viewing angle and explosion time, any non-degenerate companion larger than $0.34 R_{\textrm{sun}}$., Comment: 12 pages, 9 figures, 4 tables. Accepted to ApJ. Photometric data presented in this submission are included as an ancillary file. For a brief video explaining this paper, see https://www.youtube.com/watch?v=1bOV-Cqs-ag

14. The ASAS-SN Bright Supernova Catalog I: 2013-2014

Author

Przemysław Woźniak, S. Kiyota, J. Hissong, Subo Dong, J. Brimacombe, E. E. Falco, Thomas W.-S. Holoien, Carlos Contreras, J. Nicolas, J. L. Prieto, Jessy Jose, A. B. Danilet, J. M. Fernandez, Krzysztof Z. Stanek, Robert Koff, D. W. Bishop, Gregory J. Herczeg, G. Pojmanski, Feng Long, E. Conseil, W. Wiethoff, Christopher S. Kochanek, Eric Hsiao, B. Nicholls, G. V. Simonian, Zhen Guo, U. Basu, D. Bersier, Benjamin J. Shappee, D. M. Skowron, C. G. Ávila, L. A. G. Monard, I. Cruz, John F. Beacom, and J. S. Brown

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Supernova, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, QB
Abstract

We present basic statistics for all supernovae discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN) during its first year-and-a-half of operations, spanning 2013 and 2014. We also present the same information for all other bright ($m_V\leq17$), spectroscopically confirmed supernovae discovered from 2014 May 1 through the end of 2014, providing a comparison to the ASAS-SN sample starting from the point where ASAS-SN became operational in both hemispheres. In addition, we present collected redshifts and near-UV through IR magnitudes, where available, for all host galaxies of the bright supernovae in both samples. This work represents a comprehensive catalog of bright supernovae and their hosts from multiple professional and amateur sources, allowing for population studies that were not previously possible because the all-sky emphasis of ASAS-SN redresses many previously existing biases. In particular, ASAS-SN systematically finds bright supernovae closer to the centers of host galaxies than either other professional surveys or amateurs, a remarkable result given ASAS-SN's poorer angular resolution. This is the first of a series of yearly papers on bright supernovae and their hosts that will be released by the ASAS-SN team., 14 pages, 6 figures, 4 tables. Tables containing the catalog data presented in this submission are included in machine-readable format as ancillary files. Manuscript updated to reflect changes made in the published version. For a brief video explaining this paper, see https://youtu.be/jmlDUcpI_-s

15. THE YOUNG AND BRIGHT TYPE IA SUPERNOVA ASASSN-14lp: DISCOVERY, EARLY-TIME OBSERVATIONS, FIRST-LIGHT TIME, DISTANCE TO NGC 4666, AND PROGENITOR CONSTRAINTS.

Author

B. J. Shappee, A. L. Piro, T. W.-S. Holoien, J. L. Prieto, C. Contreras, K. Itagaki, C. R. Burns, C. S. Kochanek, K. Z. Stanek, E. Alper, U. Basu, J. F. Beacom, D. Bersier, J. Brimacombe, E. Conseil, A. B. Danilet, Subo Dong, E. Falco, D. Grupe, and E. Y. Hsiao

Subjects
SUPERNOVAE, SPECTRUM analysis, PHOTOMETRY, ULTRAVIOLET astronomy, INTRINSIC optical imaging, BAYESIAN analysis, INTERPLANETARY dust
Abstract

On 2014 December 9.61, the All-sky Automated Survey for SuperNovae (ASAS-SN or “Assassin”) discovered ASASSN-14lp just ∼2 days after first light using a global array of 14 cm diameter telescopes. ASASSN-14lp went on to become a bright supernova (V = 11.94 mag), second only to SN 2014J for the year. We present prediscovery photometry (with a detection less than a day after first light) and ultraviolet through near-infrared photometric and spectroscopic data covering the rise and fall of ASASSN-14lp for more than 100 days. We find that ASASSN-14lp had a broad light curve (), a B-band maximum at 2457015.82 ± 0.03, a rise time of days, and moderate host-galaxy extinction (). Using ASASSN-14lp, we derive a distance modulus for NGC 4666 of , corresponding to a distance of 14.7 ± 1.5 Mpc. However, adding ASASSN-14lp to the calibrating sample of Type Ia supernovae still requires an independent distance to the host galaxy. Finally, using our early-time photometric and spectroscopic observations, we rule out red giant secondaries and, assuming a favorable viewing angle and explosion time, any nondegenerate companion larger than 0.34 . [ABSTRACT FROM AUTHOR]

Published
2016
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16. Astronomy. ASASSN-15lh: A highly super-luminous supernova.

Author

Dong S, Shappee BJ, Prieto JL, Jha SW, Stanek KZ, Holoien TW, Kochanek CS, Thompson TA, Morrell N, Thompson IB, Basu U, Beacom JF, Bersier D, Brimacombe J, Brown JS, Bufano F, Chen P, Conseil E, Danilet AB, Falco E, Grupe D, Kiyota S, Masi G, Nicholls B, Olivares E F, Pignata G, Pojmanski G, Simonian GV, Szczygiel DM, and Woźniak PR

Abstract

We report the discovery of ASASSN-15lh (SN 2015L), which we interpret as the most luminous supernova yet found. At redshift z = 0.2326, ASASSN-15lh reached an absolute magnitude of Mu ,AB = -23.5 ± 0.1 and bolometric luminosity Lbol = (2.2 ± 0.2) × 10(45) ergs s(-1), which is more than twice as luminous as any previously known supernova. It has several major features characteristic of the hydrogen-poor super-luminous supernovae (SLSNe-I), whose energy sources and progenitors are currently poorly understood. In contrast to most previously known SLSNe-I that reside in star-forming dwarf galaxies, ASASSN-15lh appears to be hosted by a luminous galaxy (MK ≈ -25.5) with little star formation. In the 4 months since first detection, ASASSN-15lh radiated (1.1 ± 0.2) × 10(52) ergs, challenging the magnetar model for its engine., (Copyright © 2016, American Association for the Advancement of Science.)

Published
2016
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