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Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born. -
Arxiv:2012.09981V1 [Astro-Ph.SR] 17 Dec 2020 2 O
Contrib. Astron. Obs. Skalnat´ePleso XX, 1 { 20, (2020) DOI: to be assigned later Flare stars in nearby Galactic open clusters based on TESS data Olga Maryeva1;2, Kamil Bicz3, Caiyun Xia4, Martina Baratella5, Patrik Cechvalaˇ 6 and Krisztian Vida7 1 Astronomical Institute of the Czech Academy of Sciences 251 65 Ondˇrejov,The Czech Republic(E-mail: [email protected]) 2 Lomonosov Moscow State University, Sternberg Astronomical Institute, Universitetsky pr. 13, 119234, Moscow, Russia 3 Astronomical Institute, University of Wroc law, Kopernika 11, 51-622 Wroc law, Poland 4 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotl´aˇrsk´a2, 611 37 Brno, Czech Republic 5 Dipartimento di Fisica e Astronomia Galileo Galilei, Vicolo Osservatorio 3, 35122, Padova, Italy, (E-mail: [email protected]) 6 Department of Astronomy, Physics of the Earth and Meteorology, Faculty of Mathematics, Physics and Informatics, Comenius University in Bratislava, Mlynsk´adolina F-2, 842 48 Bratislava, Slovakia 7 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, H-1121 Budapest, Konkoly Thege Mikl´os´ut15-17, Hungary Received: September ??, 2020; Accepted: ????????? ??, 2020 Abstract. The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from TESS mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type ob- jects. Of all flares, 63 % were detected in sample of cool stars (Teff < 5000 K), and 29 % { in stars of spectral type G, while 23 % in K-type stars and ap- proximately 34% of all detected flares are in M-type stars. -
The HARPS Search for Southern Extra-Solar Planets XXXV. The
Astronomy & Astrophysics manuscript no. santos_print c ESO 2021 July 9, 2021 The HARPS search for southern extra-solar planets.? XXXV. The interesting case of HD41248: stellar activity, no planets? N.C. Santos1; 2, A. Mortier1, J. P. Faria1; 2, X. Dumusque3; 4, V. Zh. Adibekyan1, E. Delgado-Mena1, P. Figueira1, L. Benamati1; 2, I. Boisse8, D. Cunha1; 2, J. Gomes da Silva1; 2, G. Lo Curto5, C. Lovis3, J. H. C. Martins1; 2, M. Mayor3, C. Melo5, M. Oshagh1; 2, F. Pepe3, D. Queloz3; 9, A. Santerne1, D. Ségransan3, A. Sozzetti7, S. G. Sousa1; 2; 6, and S. Udry3 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 3 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland 4 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA 5 European Southern Observatory, Casilla 19001, Santiago, Chile 6 Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain 7 INAF - Osservatorio Astrofisico di Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy 8 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France 9 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK Received XXX; accepted XXX ABSTRACT Context. The search for planets orbiting metal-poor stars is of uttermost importance for our understanding of the planet formation models. However, no dedicated searches have been conducted so far for very low mass planets orbiting such objects. -
Durham E-Theses
Durham E-Theses First visibility of the lunar crescent and other problems in historical astronomy. Fatoohi, Louay J. How to cite: Fatoohi, Louay J. (1998) First visibility of the lunar crescent and other problems in historical astronomy., Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/996/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk me91 In the name of Allah, the Gracious, the Merciful >° 9 43'' 0' eji e' e e> igo4 U61 J CO J: lic 6..ý v Lo ý , ý.,, "ý J ýs ýºý. ur ý,r11 Lýi is' ý9r ZU LZJE rju No disaster can befall on the earth or in your souls but it is in a book before We bring it into being; that is easy for Allah. In order that you may not grieve for what has escaped you, nor be exultant at what He has given you; and Allah does not love any prideful boaster. -
Arxiv:2006.14546V1 [Astro-Ph.EP] 25 Jun 2020
Draft version June 26, 2020 Typeset using LATEX twocolumn style in AASTeX62 TOI-1728b: The Habitable-zone Planet Finder confirms a warm super Neptune orbiting an M dwarf host Shubham Kanodia,1, 2 Caleb I. Canas~ ,1, 2, 3 Gudmundur Stefansson,4, 5 Joe P. Ninan,1, 2 Leslie Hebb,6 Andrea S.J. Lin,1, 2 Helen Baran,1, 2 Marissa Maney,1, 2 Ryan C. Terrien,7 Suvrath Mahadevan,1, 2 William D. Cochran,8, 9 Michael Endl,8, 9 Jiayin Dong,1, 2 Chad F. Bender,10 Scott A. Diddams,11, 12 Eric B. Ford,1, 2, 13 Connor Fredrick,11, 12 Samuel Halverson,14 Fred Hearty,1, 2 Andrew J. Metcalf,15, 16, 17 Andrew Monson,1, 2 Lawrence W. Ramsey,1, 2 Paul Robertson,18 Arpita Roy,19, 20 Christian Schwab,21 and Jason T. Wright1, 2 1Department of Astronomy & Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA, 16802, USA 2Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA, 16802, USA 3NASA Earth and Space Science Fellow 4Henry Norris Russell Fellow 5Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08540, USA 6Department of Physics, Hobart and William Smith Colleges, 300 Pulteney Street, Geneva, NY, 14456, USA 7Department of Physics and Astronomy, Carleton College, One North College Street, Northfield, MN 55057, USA 8McDonald Observatory and Department of Astronomy, The University of Texas at Austin 9Center for Planetary Systems Habitability, The University of Texas at Austin 10Steward Observatory, The University of Arizona, 933 N. -
Observing List
day month year Epoch 2000 local clock time: 23.98 Observing List for 23 7 2019 RA DEC alt az Constellation object mag A mag B Separation description hr min deg min 20 50 Andromeda Gamma Andromedae (*266) 2.3 5.5 9.8 yellow & blue green double star 2 3.9 42 19 28 69 Andromeda Pi Andromedae 4.4 8.6 35.9 bright white & faint blue 0 36.9 33 43 30 55 Andromeda STF 79 (Struve) 6 7 7.8 bluish pair 1 0.1 44 42 16 52 Andromeda 59 Andromedae 6.5 7 16.6 neat pair, both greenish blue 2 10.9 39 2 45 67 Andromeda NGC 7662 (The Blue Snowball) planetary nebula, fairly bright & slightly elongated 23 25.9 42 32.1 31 60 Andromeda M31 (Andromeda Galaxy) large sprial arm galaxy like the Milky Way 0 42.7 41 16 31 61 Andromeda M32 satellite galaxy of Andromeda Galaxy 0 42.7 40 52 32 60 Andromeda M110 (NGC205) satellite galaxy of Andromeda Galaxy 0 40.4 41 41 17 55 Andromeda NGC752 large open cluster of 60 stars 1 57.8 37 41 17 48 Andromeda NGC891 edge on galaxy, needle-like in appearance 2 22.6 42 21 45 69 Andromeda NGC7640 elongated galaxy with mottled halo 23 22.1 40 51 46 57 Andromeda NGC7686 open cluster of 20 stars 23 30.2 49 8 30 121 Aquarius 55 Aquarii, Zeta 4.3 4.5 2.1 close, elegant pair of yellow stars 22 28.8 0 -1 12 120 Aquarius 94 Aquarii 5.3 7.3 12.7 pale rose & emerald 23 19.1 -13 28 32 152 Aquarius M72 globular cluster 20 53.5 -12 32 31 151 Aquarius M73 Y-shaped asterism of 4 stars 20 59 -12 38 16 117 Aquarius NGC7606 Galaxy 23 19.1 -8 29 32 149 Aquarius NGC7009 Saturn Neb planetary nebula, large & bright pale green oval 21 4.2 -11 21.8 38 135 -
An Extreme Planetary System Around HD 219828 One Long-Period Super Jupiter to a Hot-Neptune Host Star?,??
A&A 592, A13 (2016) Astronomy DOI: 10.1051/0004-6361/201628374 & c ESO 2016 Astrophysics An extreme planetary system around HD 219828 One long-period super Jupiter to a hot-Neptune host star?,?? N. C. Santos1; 2, A. Santerne1, J. P. Faria1; 2, J. Rey3, A. C. M. Correia4; 5, J. Laskar5, S. Udry3, V. Adibekyan1, F. Bouchy3; 6, E. Delgado-Mena1, C. Melo7, X. Dumusque3, G. Hébrard8; 9, C. Lovis3, M. Mayor3, M. Montalto1, A. Mortier10, F. Pepe3, P. Figueira1, J. Sahlmann11, D. Ségransan3, and S. G. Sousa1 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 3 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 4 CIDMA, Departamento de Física, Universidade de Aveiro, Campus de Santiago, 3810-193 Aveiro, Portugal 5 ASD, IMCCE-CNRS UMR 8028, Observatoire de Paris, PSL Research University, 77 Av. Denfert-Rochereau, 75014 Paris, France 6 Aix-Marseille Université, CNRS, Laboratoire d’Astrophysique de Marseille UMR 7326, 13388 Marseille Cedex 13, France 7 European Southern Observatory (ESO), 19001 Casilla, Santiago, Chile 8 Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l’Observatoire, France 9 Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France 10 SUPA, School of Physics and Astronomy, University of St. Andrews, St. Andrews, KY16 9SS, UK 11 European Space Agency (ESA), Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Received 24 February 2016 / Accepted 10 May 2016 ABSTRACT Context. -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Double Star Measurements at the Southern Sky with a 50 Cm Reflector in 2016
Vol. 13 No. 4 October 1, 2017 Journal of Double Star Observations Page 495 Double Star Measurements at the Southern Sky with a 50 cm Reflector in 2016 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: A 50 cm Ritchey-Chrétien reflector was used for recordings of double stars with a CCD webcam, and measurements of 95 pairs were mostly obtained from “lucky images”, and in some cases by speckle interferometry. The image scale was calibrated with reference systems from the recently published Gaia catalogue of precise position data. For several pairs, deviations from currently assumed orbits were found. Some images of noteworthy systems are also pre- sented. “Chameleon” (PointGrey) with exposure times ranging Introduction from less than a millisecond to several tens of msec, Recordings of double star images were mostly eval- depending on the star brightness, on the filter being uated with “lucky imaging”: Seeing effects are effec- used, and on the seeing. Recordings were usually made tively reduced by using short exposure times, and selec- with a red or near infrared filter, in order to reduce ef- tion of only the best images for stacking, which results fects from chromatic aberrations of the Barlow lens, as in virtually diffraction limited images. In addition, well as from the seeing. Only the best frames, typically speckle interferometry was applied in some cases, as several tens and up to more than 100, were selected, large numbers of speckle images were found in several registered, and stacked. The pixel size of 3.75 µm recordings, caused by rather variable seeing conditions square results in a nominal resolution of 0.096 arcsec/ during this observing campaign. -
Fy10 Budget by Program
AURA/NOAO FISCAL YEAR ANNUAL REPORT FY 2010 Revised Submitted to the National Science Foundation March 16, 2011 This image, aimed toward the southern celestial pole atop the CTIO Blanco 4-m telescope, shows the Large and Small Magellanic Clouds, the Milky Way (Carinae Region) and the Coal Sack (dark area, close to the Southern Crux). The 33 “written” on the Schmidt Telescope dome using a green laser pointer during the two-minute exposure commemorates the rescue effort of 33 miners trapped for 69 days almost 700 m underground in the San Jose mine in northern Chile. The image was taken while the rescue was in progress on 13 October 2010, at 3:30 am Chilean Daylight Saving time. Image Credit: Arturo Gomez/CTIO/NOAO/AURA/NSF National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2010 Revised (October 1, 2009 – September 30, 2010) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 March 16, 2011 Table of Contents MISSION SYNOPSIS ............................................................................................................ IV 1 EXECUTIVE SUMMARY ................................................................................................ 1 2 NOAO ACCOMPLISHMENTS ....................................................................................... 2 2.1 Achievements ..................................................................................................... 2 2.2 Status of Vision and Goals ................................................................................ -
Arxiv:2009.08338V2 [Astro-Ph.EP] 30 Nov 2020 Loses It Over Time
Astronomy & Astrophysics manuscript no. main ©ESO 2020 December 1, 2020 A planetary system with two transiting mini-Neptunes near the radius valley transition around the bright M dwarf TOI-776? R. Luque1;2, L. M. Serrano3, K. Molaverdikhani4;5, M. C. Nixon6, J. H. Livingston7, E. W. Guenther8, E. Pallé1;2, N. Madhusudhan6, G. Nowak1;2, J. Korth9, W. D. Cochran10, T. Hirano11, P. Chaturvedi8, E. Goffo3, S. Albrecht12, O. Barragán13, C Briceño14, J. Cabrera15, D. Charbonneau16, R. Cloutier16, K. A. Collins16, K. I. Collins17, K. D. Colón18, I. J. M. Crossfield19, Sz. Csizmadia15, F. Dai20, H. J. Deeg1;2, M. Esposito8, M. Fridlund21;22, D. Gandolfi3, I. Georgieva22, A. Glidden23;24, R. F. Goeke23, S. Grziwa9, A. P. Hatzes8, C. E. Henze25, S. B. Howell25, J. Irwin16, J. M. Jenkins25, E. L. N. Jensen26, P. Kábath27, R. C. Kidwell Jr.28, J. F. Kielkopf29, E. Knudstrup12, K. W. F. Lam30, D. W. Latham16, J. J. Lissauer25, A. W. Mann31, E. C. Matthews24, I. Mireles24, N. Narita32;33;34;1, M. Paegert16, C. M. Persson22, S. Redfield35, G. R. Ricker24, F. Rodler36, J. E. Schlieder18, N. J. Scott25, S. Seager24;23;37, J. Šubjak27, T. G. Tan38, E. B. Ting25, R. Vanderspek24, V. Van Eylen39, J. N. Winn40, and C. Ziegler41 (Affiliations can be found after the references) Received 17.09.2020 / Accepted 30.11.2020 ABSTRACT We report the discovery and characterization of two transiting planets around the bright M1 V star LP 961-53 (TOI-776, J = 8:5 mag,M = 0:54±0:03 M ) detected during Sector 10 observations of the Transiting Exoplanet Survey Satellite (TESS). -
Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55