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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. -
Arxiv:1001.0139V1 [Astro-Ph.SR] 31 Dec 2009 Oadl Gilliland, L
Publications of the Astronomical Society of the Pacific Kepler Asteroseismology Program: Introduction and First Results Ronald L. Gilliland,1 Timothy M. Brown,2 Jørgen Christensen-Dalsgaard,3 Hans Kjeldsen,3 Conny Aerts,4 Thierry Appourchaux,5 Sarbani Basu,6 Timothy R. Bedding,7 William J. Chaplin,8 Margarida S. Cunha,9 Peter De Cat,10 Joris De Ridder,4 Joyce A. Guzik,11 Gerald Handler,12 Steven Kawaler,13 L´aszl´oKiss,7,14 Katrien Kolenberg,12 Donald W. Kurtz,15 Travis S. Metcalfe,16 Mario J.P.F.G. Monteiro,9 Robert Szab´o,14 Torben Arentoft,3 Luis Balona,17 Jonas Debosscher,4 Yvonne P. Elsworth,8 Pierre-Olivier Quirion,3,18 Dennis Stello,7 Juan Carlos Su´arez,19 William J. Borucki,20 Jon M. Jenkins,21 David Koch,20 Yoji Kondo,22 David W. Latham,23 Jason F. Rowe,20 and Jason H. Steffen24 arXiv:1001.0139v1 [astro-ph.SR] 31 Dec 2009 –2– ABSTRACT Asteroseismology involves probing the interiors of stars and quantifying their global properties, such as radius and age, through observations of normal modes of oscillation. The technical requirements for conducting asteroseismology in- clude ultra-high precision measured in photometry in parts per million, as well as nearly continuous time series over weeks to years, and cadences rapid enough 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; [email protected] 2Las Cumbres Observatory Global Telescope, Goleta, CA 93117, USA 3Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, Denmark 4Instituut voor Sterrenkunde, K.U.Leuven, Celestijnenlaan 200 D, 3001, Leuven, Belgium 5Institut d’Astrophysique Spatiale, Universit´eParis XI, Bˆatiment 121, 91405 Orsay Cedex, France 6Astronomy Department, Yale University, P.O. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Asteroseismic Inferences on Red Giants in Open Clusters NGC 6791, NGC 6819, and NGC 6811 Using Kepler
A&A 530, A100 (2011) Astronomy DOI: 10.1051/0004-6361/201016303 & c ESO 2011 Astrophysics Asteroseismic inferences on red giants in open clusters NGC 6791, NGC 6819, and NGC 6811 using Kepler S. Hekker1,2, S. Basu3, D. Stello4, T. Kallinger5, F. Grundahl6,S.Mathur7,R.A.García8, B. Mosser9,D.Huber4, T. R. Bedding4,R.Szabó10, J. De Ridder11,W.J.Chaplin2, Y. Elsworth2,S.J.Hale2, J. Christensen-Dalsgaard6 , R. L. Gilliland12, M. Still13, S. McCauliff14, and E. V. Quintana15 1 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands e-mail: [email protected] 2 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK 3 Department of Astronomy, Yale University, PO Box 208101, New Haven CT 06520-8101, USA 4 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia 5 Department of Physics and Astronomy, University of British Colombia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada 6 Department of Physics and Astronomy, Building 1520, Aarhus University, 8000 Aarhus C, Denmark 7 High Altitude Observatory, NCAR, PO Box 3000, Boulder, CO 80307, USA 8 Laboratoire AIM, CEA/DSM-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette, France 9 LESIA, UMR8109, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris, 92195 Meudon Cedex, France 10 Konkoly Observatory of the Hungarian Academy of Sciences, Konkoly Thege Miklós út 15-17, 1121 Budapest, Hungary 11 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium 12 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 13 Bay Area Environmental Research Institute/Nasa Ames Research Center, Moffett Field, CA 94035, USA 14 Orbital Sciences Corporation/Nasa Ames Research Center, Moffett Field, CA 94035, USA 15 SETI Institute/Nasa Ames Research Center, Moffett Field, CA 94035, USA Received 13 December 2010 / Accepted 19 April 2011 ABSTRACT Context. -
WIYN Open Cluster Study. XXIV. Stellar Radial-Velocity Measurements in NGC 6819
WIYN Open Cluster Study. XXIV. Stellar Radial-Velocity Measurements in NGC 6819 K. Tabetha Hole1,2 ([email protected]) Aaron M. Geller1,2 ([email protected]) Robert D. Mathieu1,2 ([email protected]) Imants Platais3 ([email protected]) Søren Meibom1,2,4 ([email protected]) and David W. Latham4 ([email protected]) ABSTRACT We present the current results from our ongoing radial-velocity survey of the intermediate-age (2.4 Gyr) open cluster NGC 6819. Using both newly observed and other available photometry and astrometry we define a primary target sample of 1454 stars that includes main-sequence, subgiant, giant, and blue straggler stars, spanning a magnitude range of 11≤V ≤16.5 and an approximate mass range of 1.1to1.6 M⊙. Our sample covers a 23 arcminute (13 pc) square field of view centered on the cluster. We have measured 6571 radial velocities for an unbiased sample of 1207 stars in the direction of the open cluster NGC 6819, with a single-measurement precision of 0.4km s−1 for most narrow-lined stars. We use our radial-velocity data to calculate membership probabilities for stars with ≥ 3 measurements, providing the first comprehensive membership study of the cluster core that includes stars from the giant branch through the upper main sequence. We identify 475 cluster members. Additionally, we identify velocity-variable systems, all of which are likely hard binaries that dynamically power the cluster. Using our single cluster members, we find a cluster radial velocity of 2.33 ± 0.05 km s−1. -
Proto-Planetary Nebula Observing Guide
Proto-Planetary Nebula Observing Guide www.reinervogel.net RA Dec CRL 618 Westbrook Nebula 04h 42m 53.6s +36° 06' 53" PK 166-6 1 HD 44179 Red Rectangle 06h 19m 58.2s -10° 38' 14" V777 Mon OH 231.8+4.2 Rotten Egg N. 07h 42m 16.8s -14° 42' 52" Calabash N. IRAS 09371+1212 Frosty Leo 09h 39m 53.6s +11° 58' 54" CW Leonis Peanut Nebula 09h 47m 57.4s +13° 16' 44" Carbon Star with dust shell M 2-9 Butterfly Nebula 17h 05m 38.1s -10° 08' 33" PK 10+18 2 IRAS 17150-3224 Cotton Candy Nebula 17h 18m 20.0s -32° 27' 20" Hen 3-1475 Garden-sprinkler Nebula 17h 45m 14. 2s -17° 56' 47" IRAS 17423-1755 IRAS 17441-2411 Silkworm Nebula 17h 47m 13.5s -24° 12' 51" IRAS 18059-3211 Gomez' Hamburger 18h 09m 13.3s -32° 10' 48" MWC 922 Red Square Nebula 18h 21m 15s -13° 01' 27" IRAS 19024+0044 19h 05m 02.1s +00° 48' 50.9" M 1-92 Footprint Nebula 19h 36m 18.9s +29° 32' 50" Minkowski's Footprint IRAS 20068+4051 20h 08m 38.5s +41° 00' 37" CRL 2688 Egg Nebula 21h 02m 18.8s +36° 41' 38" PK 80-6 1 IRAS 22036+5306 22h 05m 30.3s +53° 21' 32.8" IRAS 23166+1655 23h 19m 12.6s +17° 11' 33.1" Southern Objects ESO 172-7 Boomerang Nebula 12h 44m 45.4s -54° 31' 11" Centaurus bipolar nebula PN G340.3-03.2 Water Lily Nebula 17h 03m 10.1s -47° 00' 27" PK 340-03 1 IRAS 17163-3907 Fried Egg Nebula 17h 19m 49.3s -39° 10' 37.9" Finder charts measure 20° (with 5° circle) and 5° (with 1° circle) and were made with Cartes du Ciel by Patrick Chevalley (http://www.ap-i.net/skychart) Images are DSS Images (blue plates, POSS II or SERCJ) and measure 30’ by 30’ (http://archive.stsci.edu/cgi- bin/dss_plate_finder) and STScI Images (Hubble Space Telescope) Downloaded from www.reinervogel.net version 12/2012 DSS images copyright notice: The Digitized Sky Survey was produced at the Space Telescope Science Institute under U.S. -
Open Clusters
Open Clusters Open clusters (also known as galactic clusters) are of tremendous importance to the science of astronomy, if not to astrophysics and cosmology generally. Star clusters serve as the "laboratories" of astronomy, with stars now all at nearly the same distance and all created at essentially the same time. Each cluster thus is a running experiment, where we can observe the effects of composition, age, and environment. We are hobbled by seeing only a snapshot in time of each cluster, but taken collectively we can understand their evolution, and that of their included stars. These clusters are also important tracers of the Milky Way and other parent galaxies. They help us to understand their current structure and derive theories of the creation and evolution of galaxies. Just as importantly, starting from just the Hyades and the Pleiades, and then going to more distance clusters, open clusters serve to define the distance scale of the Milky Way, and from there all other galaxies and the entire universe. However, there is far more to the study of star clusters than that. Anyone who has looked at a cluster through a telescope or binoculars has realized that these are objects of immense beauty and symmetry. Whether a cluster like the Pleiades seen with delicate beauty with the unaided eye or in a small telescope or binoculars, or a cluster like NGC 7789 whose thousands of stars are seen with overpowering wonder in a large telescope, open clusters can only bring awe and amazement to the viewer. These sights are available to all. -
Str ¨Omgren Survey for Asteroseismology and Galactic
The Astrophysical Journal, 787:110 (25pp), 2014 June 1 doi:10.1088/0004-637X/787/2/110 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. STROMGREN¨ SURVEY FOR ASTEROSEISMOLOGY AND GALACTIC ARCHAEOLOGY: LET THE SAGA BEGIN∗ L. Casagrande1,14, V. Silva Aguirre2, D. Stello3, D. Huber4,5, A. M. Serenelli6, S. Cassisi7, A. Dotter1, A. P. Milone1, S. Hodgkin8,A.F.Marino1, M. N. Lund2, A. Pietrinferni7,M.Asplund1, S. Feltzing9, C. Flynn10, F. Grundahl2,P.E.Nissen2,R.Schonrich¨ 11,12,15, K. J. Schlesinger1, and W. Wang13 1 Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, The Australian National University, Canberra, ACT 2611, Australia; [email protected] 2 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 3 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia 4 NASA Ames Research Center, Moffett Field, CA 94035, USA 5 SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA 6 Institute of Space Sciences (IEEC-CSIC), Campus UAB, Fac. Ciencies,´ Torre C5 parell 2, E-08193 Bellaterra, Spain 7 INAF-Osservatorio Astronomico di Collurania, via Maggini, I-64100 Teramo, Italy 8 Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK 9 Lund Observatory, Department of Astronomy and Theoretical Physics, P.O. Box 43, SE-22100 Lund, Sweden 10 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia -
00E the Construction of the Universe Symphony
The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope -
FY13 High-Level Deliverables
National Optical Astronomy Observatory Fiscal Year Annual Report for FY 2013 (1 October 2012 – 30 September 2013) Submitted to the National Science Foundation Pursuant to Cooperative Support Agreement No. AST-0950945 13 December 2013 Revised 18 September 2014 Contents NOAO MISSION PROFILE .................................................................................................... 1 1 EXECUTIVE SUMMARY ................................................................................................ 2 2 NOAO ACCOMPLISHMENTS ....................................................................................... 4 2.1 Achievements ..................................................................................................... 4 2.2 Status of Vision and Goals ................................................................................. 5 2.2.1 Status of FY13 High-Level Deliverables ............................................ 5 2.2.2 FY13 Planned vs. Actual Spending and Revenues .............................. 8 2.3 Challenges and Their Impacts ............................................................................ 9 3 SCIENTIFIC ACTIVITIES AND FINDINGS .............................................................. 11 3.1 Cerro Tololo Inter-American Observatory ....................................................... 11 3.2 Kitt Peak National Observatory ....................................................................... 14 3.3 Gemini Observatory ........................................................................................ -
Angular Momentum Evolution of Young Low-Mass Stars and Brown Dwarfs: Observations and Theory
Angular momentum evolution of young low-mass stars and brown dwarfs: observations and theory Jer´ omeˆ Bouvier Observatoire de Grenoble Sean P. Matt Exeter University Subhanjoy Mohanty Imperial College London Aleks Scholz University of St Andrews Keivan G. Stassun Vanderbilt University Claudio Zanni Osservatorio Astrofisico di Torino This chapter aims at providing the most complete review of both the emerging concepts and the latest observational results regarding the angular momentum evolution of young low-mass stars and brown dwarfs. In the time since Protostars & Planets V, there have been major developments in the availability of rotation period measurements at multiple ages and in different star-forming environments that are essential for testing theory. In parallel, substantial theoretical developments have been carried out in the last few years, including the physics of the star-disk interaction, numerical simulations of stellar winds, and the investigation of angular momentum transport processes in stellar interiors. This chapter reviews both the recent observational and theoretical advances that prompted the development of renewed angular momentum evolution models for cool stars and brown dwarfs. While the main observational trends of the rotational history of low mass objects seem to be accounted for by these new models, a number of critical open issues remain that are outlined in this review. 1. INTRODUCTION vational and theoretical sides, on the issue of the angular momentum evolution of young stellar objects since Pro- The angular momentum content of a newly born star is tostars & Planets V. On the observational side, thousands one of the fundamental quantities, like mass and metallic- of new rotational periods have been derived for stars over ity, that durably impacts on the star’s properties and evolu- the entire mass range from solar-type stars down to brown tion. -
SAA 100 Club
S.A.A. 100 Observing Club Raleigh Astronomy Club Version 1.2 07-AUG-2005 Introduction Welcome to the S.A.A. 100 Observing Club! This list started on the USENET newsgroup sci.astro.amateur when someone asked about everyone’s favorite, non-Messier objects for medium sized telescopes (8-12”). The members of the group nominated objects and voted for their favorites. The top 100 objects, by number of votes, were collected and ranked into a list that was published. This list is a good next step for someone who has observed all the objects on the Messier list. Since it includes objects in both the Northern and Southern Hemispheres (DEC +72 to -72), the award has two different levels to accommodate those observers who aren't able to travel. The first level, the Silver SAA 100 award requires 88 objects (all visible from North Carolina). The Gold SAA 100 Award requires all 100 objects to be observed. One further note, many of these objects are on other observing lists, especially Patrick Moore's Caldwell list. For convenience, there is a table mapping various SAA100 objects with their Caldwell counterparts. This will facilitate observers who are working or have worked on these lists of objects. We hope you enjoy looking at all the great objects recommended by other avid astronomers! Rules In order to earn the Silver certificate for the program, the applicant must meet the following qualifications: 1. Be a member in good standing of the Raleigh Astronomy Club. 2. Observe 80 Silver observations. 3. Record the time and date of each observation.