A RAVE Investigation on Galactic Open Clusters II
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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:0804.4630V1 [Astro-Ph] 29 Apr 2008 I Ehnv20;Ficao 06) Ti Nti Oeas Role This in Is It 2006A)
DRAFT VERSION NOVEMBER 9, 2018 Preprint typeset using LATEX style emulateapj v. 05/04/06 OPEN CLUSTERS AS GALACTIC DISK TRACERS: I. PROJECT MOTIVATION, CLUSTER MEMBERSHIP AND BULK THREE-DIMENSIONAL KINEMATICS PETER M. FRINCHABOY1,2,3 AND STEVEN R. MAJEWSKI2 Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA Draft version November 9, 2018 ABSTRACT We have begun a survey of the chemical and dynamical properties of the Milky Way disk as traced by open star clusters. In this first contribution, the general goals of our survey are outlined and the strengths and limita- tions of using star clusters as a Galactic disk tracer sample are discussed. We also present medium resolution (R 15,0000) spectroscopy of open cluster stars obtained with the Hydra multi-object spectrographs on the Cerro∼ Tololo Inter-American Observatory 4-m and WIYN 3.5-m telescopes. Here we use these data to deter- mine the radial velocities of 3436 stars in the fields of open clusters within about 3 kpc, with specific attention to stars having proper motions in the Tycho-2 catalog. Additional radial velocity members (without Tycho-2 proper motions) that can be used for future studies of these clusters were also identified. The radial velocities, proper motions, and the angular distance of the stars from cluster center are used to derive cluster member- ship probabilities for stars in each cluster field using a non-parametric approach, and the cluster members so-identified are used, in turn, to derive the reliable bulk three-dimensional motion for 66 of 71 targeted open clusters. -
Astronomy Astrophysics
A&A 468, 151–161 (2007) Astronomy DOI: 10.1051/0004-6361:20077073 & c ESO 2007 Astrophysics Towards absolute scales for the radii and masses of open clusters A. E. Piskunov1,2,3, E. Schilbach1, N. V. Kharchenko1,3,4, S. Röser1, and R.-D. Scholz3 1 Astronomisches Rechen-Institut, Mönchhofstraße 12-14, 69120 Heidelberg, Germany e-mail: [apiskunov;elena;nkhar;roeser]@ari.uni-heidelberg.de 2 Institute of Astronomy of the Russian Acad. Sci., 48 Pyatnitskaya Str., 109017 Moscow, Russia e-mail: [email protected] 3 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany e-mail: [apiskunov;nkharchenko;rdscholz]@aip.de 4 Main Astronomical Observatory, 27 Academica Zabolotnogo Str., 03680 Kiev, Ukraine e-mail: [email protected] Received 10 January 2007 / Accepted 19 February 2007 ABSTRACT Aims. In this paper we derive tidal radii and masses of open clusters in the nearest kiloparsecs around the Sun. Methods. For each cluster, the mass is estimated from tidal radii determined from a fitting of three-parameter King profiles to the observed integrated density distribution. Different samples of members are investigated. Results. For 236 open clusters, all contained in the catalogue ASCC-2.5, we obtain core and tidal radii, as well as tidal masses. The distributions of the core and tidal radii peak at about 1.5 pc and 7–10 pc, respectively. A typical relative error of the core radius lies between 15% and 50%, whereas, for the majority of clusters, the tidal radius was determined with a relative accuracy better than 20%. Most of the clusters have tidal masses between 50 and 1000 m, and for about half of the clusters, the masses were obtained with a relative error better than 50%. -
Open Clusters in Gaia
Sede Amministrativa: Università degli Studi di Padova Dipartimento di Fisica e Astronomia “G. Galilei” Corso di Dottorato di Ricerca in Astronomia Ciclo XXX OPEN CLUSTERS IN GAIA ERA Coordinatore: Ch.mo Prof. Giampaolo Piotto Supervisore: Dr.ssa Antonella Vallenari Dottorando: Francesco Pensabene i Abstract Context. Open clusters (OCs) are optimal tracers of the Milky Way disc. They are observed at every distance from the Galactic center and their ages cover the entire lifespan of the disc. The actual OC census contain more than 3000 objects, but suffers of incom- pleteness out of the solar neighborhood and of large inhomogeneity in the parameter deter- minations present in literature. Both these aspects will be improved by the on-going space mission Gaia . In the next years Gaia will produce the most precise three-dimensional map of the Milky Way by surveying other than 1 billion of stars. For those stars Gaia will provide extremely precise measure- ment of proper motions, parallaxes and brightness. Aims. In this framework we plan to take advantage of the first Gaia data release, while preparing for the coming ones, to: i) move the first steps towards building a homogeneous data base of OCs with the high quality Gaia astrometry and photometry; ii) build, improve and test tools for the analysis of large sample of OCs; iii) use the OCs to explore the prop- erties of the disc in the solar neighborhood. Methods and Data. Using ESO archive data, we analyze the photometry and derive physical parameters, comparing data with synthetic populations and luminosity functions, of three clusters namely NGC 2225, NGC 6134 and NGC 2243. -
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). -
LIST of PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute
LIST OF PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute of Department of Science and Technology, Govt. of India) Manora Peak, Naini Tal - 263 129, India (1955−2020) ABBREVIATIONS AA: Astronomy and Astrophysics AASS: Astronomy and Astrophysics Supplement Series ACTA: Acta Astronomica AJ: Astronomical Journal ANG: Annals de Geophysique Ap. J.: Astrophysical Journal ASP: Astronomical Society of Pacific ASR: Advances in Space Research ASS: Astrophysics and Space Science AE: Atmospheric Environment ASL: Atmospheric Science Letters BA: Baltic Astronomy BAC: Bulletin Astronomical Institute of Czechoslovakia BASI: Bulletin of the Astronomical Society of India BIVS: Bulletin of the Indian Vacuum Society BNIS: Bulletin of National Institute of Sciences CJAA: Chinese Journal of Astronomy and Astrophysics CS: Current Science EPS: Earth Planets Space GRL : Geophysical Research Letters IAU: International Astronomical Union IBVS: Information Bulletin on Variable Stars IJHS: Indian Journal of History of Science IJPAP: Indian Journal of Pure and Applied Physics IJRSP: Indian Journal of Radio and Space Physics INSA: Indian National Science Academy JAA: Journal of Astrophysics and Astronomy JAMC: Journal of Applied Meterology and Climatology JATP: Journal of Atmospheric and Terrestrial Physics JBAA: Journal of British Astronomical Association JCAP: Journal of Cosmology and Astroparticle Physics JESS : Jr. of Earth System Science JGR : Journal of Geophysical Research JIGR: Journal of Indian -
Gaia Data Release 2 Special Issue
Observational Hertzsprung-Russell diagrams Babusiaux, C.; van Leeuwen, F.; Barstow, M. A.; Cayuso, Jordi; Vallenari, A.; Lindstrøm, Hans Erik Peter; Bossini, D.; Bressan, Rodrigo A; Prusti, T.; de Bruijne, JHJ; Ulla, Anna; Taylor, MB; Vogt, S.; Essen, C. von; Yoldas, A.; Zerjal, M.; Zwitter, Tomaz Published in: Astronomy & Astrophysics DOI: 10.1051/0004-6361/201832843 Publication date: 2018 Document version Publisher's PDF, also known as Version of record Citation for published version (APA): Babusiaux, C., van Leeuwen, F., Barstow, M. A., Cayuso, J., Vallenari, A., Lindstrøm, H. E. P., Bossini, D., Bressan, R. A., Prusti, T., de Bruijne, JHJ., Ulla, A., Taylor, MB., Vogt, S., Essen, C. V., Yoldas, A., Zerjal, M., & Zwitter, T. (2018). Observational Hertzsprung-Russell diagrams. Astronomy & Astrophysics, 616, [A10]. https://doi.org/10.1051/0004-6361/201832843 Download date: 08. Oct. 2021 A&A 616, A10 (2018) Astronomy https://doi.org/10.1051/0004-6361/201832843 & © ESO 2018 Astrophysics Gaia Data Release 2 Special issue Gaia Data Release 2 Observational Hertzsprung-Russell diagrams? ?? Gaia Collaboration, C. Babusiaux1; 2; , F. van Leeuwen3, M. A. Barstow4, C. Jordi5, A. Vallenari6, D. Bossini6, A. Bressan7, T. Cantat-Gaudin6; 5, M. van Leeuwen3, A. G. A. Brown8, T. Prusti9, J. H. J. de Bruijne9, C. A. L. Bailer-Jones10, M. Biermann11, D. W. Evans3, L. Eyer12, F. Jansen13, S. A. Klioner14, U. Lammers15, L. Lindegren16, X. Luri5, F. Mignard17, C. Panem18, D. Pourbaix19; 20, S. Randich21, P. Sartoretti2, H. I. Siddiqui22, C. Soubiran23, N. A. Walton3, F. Arenou2, U. Bastian11, M. Cropper24, R. Drimmel25, D. Katz2, M. G. Lattanzi25, J. -
Characterising Open Clusters in the Solar Neighbourhood with the Tycho-Gaia Astrometric Solution? T
A&A 615, A49 (2018) Astronomy https://doi.org/10.1051/0004-6361/201731251 & © ESO 2018 Astrophysics Characterising open clusters in the solar neighbourhood with the Tycho-Gaia Astrometric Solution? T. Cantat-Gaudin1, A. Vallenari1, R. Sordo1, F. Pensabene1,2, A. Krone-Martins3, A. Moitinho3, C. Jordi4, L. Casamiquela4, L. Balaguer-Núnez4, C. Soubiran5, and N. Brouillet5 1 INAF-Osservatorio Astronomico di Padova, vicolo Osservatorio 5, 35122 Padova, Italy e-mail: [email protected] 2 Dipartimento di Fisica e Astronomia, Università di Padova, vicolo Osservatorio 3, 35122 Padova, Italy 3 SIM, Faculdade de Ciências, Universidade de Lisboa, Ed. C8, Campo Grande, 1749-016 Lisboa, Portugal 4 Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain 5 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, UMR 5804, 33615 Pessac, France Received 26 May 2017 / Accepted 29 January 2018 ABSTRACT Context. The Tycho-Gaia Astrometric Solution (TGAS) subset of the first Gaia catalogue contains an unprecedented sample of proper motions and parallaxes for two million stars brighter than G 12 mag. Aims. We take advantage of the full astrometric solution available∼ for those stars to identify the members of known open clusters and compute mean cluster parameters using either TGAS or the fourth U.S. Naval Observatory CCD Astrograph Catalog (UCAC4) proper motions, and TGAS parallaxes. Methods. We apply an unsupervised membership assignment procedure to select high probability cluster members, we use a Bayesian/Markov Chain Monte Carlo technique to fit stellar isochrones to the observed 2MASS JHKS magnitudes of the member stars and derive cluster parameters (age, metallicity, extinction, distance modulus), and we combine TGAS data with spectroscopic radial velocities to compute full Galactic orbits. -
108 Afocal Procedure, 105 Age of Globular Clusters, 25, 28–29 O
Index Index Achromats, 70, 73, 79 Apochromats (APO), 70, Averted vision Adhafera, 44 73, 79 technique, 96, 98, Adobe Photoshop Aquarius, 43, 99 112 (software), 108 Aquila, 10, 36, 45, 65 Afocal procedure, 105 Arches cluster, 23 B1620-26, 37 Age Archinal, Brent, 63, 64, Barkhatova (Bar) of globular clusters, 89, 195 catalogue, 196 25, 28–29 Arcturus, 43 Barlow lens, 78–79, 110 of open clusters, Aricebo radio telescope, Barnard’s Galaxy, 49 15–16 33 Basel (Bas) catalogue, 196 of star complexes, 41 Aries, 45 Bayer classification of stellar associations, Arp 2, 51 system, 93 39, 41–42 Arp catalogue, 197 Be16, 63 of the universe, 28 Arp-Madore (AM)-1, 33 Beehive Cluster, 13, 60, Aldebaran, 43 Arp-Madore (AM)-2, 148 Alessi, 22, 61 48, 65 Bergeron 1, 22 Alessi catalogue, 196 Arp-Madore (AM) Bergeron, J., 22 Algenubi, 44 catalogue, 197 Berkeley 11, 124f, 125 Algieba, 44 Asterisms, 43–45, Berkeley 17, 15 Algol (Demon Star), 65, 94 Berkeley 19, 130 21 Astronomy (magazine), Berkeley 29, 18 Alnilam, 5–6 89 Berkeley 42, 171–173 Alnitak, 5–6 Astronomy Now Berkeley (Be) catalogue, Alpha Centauri, 25 (magazine), 89 196 Alpha Orionis, 93 Astrophotography, 94, Beta Pictoris, 42 Alpha Persei, 40 101, 102–103 Beta Piscium, 44 Altair, 44 Astroplanner (software), Betelgeuse, 93 Alterf, 44 90 Big Bang, 5, 29 Altitude-Azimuth Astro-Snap (software), Big Dipper, 19, 43 (Alt-Az) mount, 107 Binary millisecond 75–76 AstroStack (software), pulsars, 30 Andromeda Galaxy, 36, 108 Binary stars, 8, 52 39, 41, 48, 52, 61 AstroVideo (software), in globular clusters, ANR 1947 -
Open Clusters in APOGEE and GALAH Combining Gaia and Ground-Based Spectroscopic Surveys?
A&A 623, A80 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834546 & c ESO 2019 Astrophysics Open clusters in APOGEE and GALAH Combining Gaia and ground-based spectroscopic surveys? R. Carrera1, A. Bragaglia2, T. Cantat-Gaudin3, A. Vallenari1, L. Balaguer-Núñez3, D. Bossini1, L. Casamiquela4, C. Jordi3, R. Sordo1, and C. Soubiran4 1 INAF-Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy e-mail: [email protected] 2 INAF-Osservatorio di Astrofisica e Scienza dello Spazio, via P. Gobetti 93/3, 40129 Bologna, Italy 3 Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain 4 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France Received 31 October 2018 / Accepted 26 January 2019 ABSTRACT Context. Open clusters are ideal laboratories to investigate a variety of astrophysical topics, from the properties of the Galactic disc to stellar-evolution models. Knowing their metallicity and possibly detailed chemical abundances is therefore important. However, the number of systems with chemical abundances determined from high-resolution spectroscopy remains small. Aims. Our aim is to increase the number of open clusters with radial velocities and chemical abundances determined from high- resolution spectroscopy using publicly available catalogues of surveys in combination with Gaia data. Methods. Open cluster stars have been identified in the APOGEE and GALAH spectroscopic surveys by cross-matching their latest data releases with stars for which high-probability astrometric membership has been derived in many clusters on the basis of the Gaia second data release. -
An Analysis of the First Three Catalogues of Southern Star Clusters and Nebulae
ResearchOnline@JCU This file is part of the following reference: Cozens, Glendyn John (2008) An analysis of the first three catalogues of southern star clusters and nebulae. PhD thesis, James Cook University. Access to this file is available from: http://eprints.jcu.edu.au/24051/ The author has certified to JCU that they have made a reasonable effort to gain permission and acknowledge the owner of any third party copyright material included in this document. If you believe that this is not the case, please contact [email protected] and quote http://eprints.jcu.edu.au/24051/ APPENDIX A – THE ORIGINAL LACAILLE CATALOGUE This is a copy of the original Lacaille catalogue, as it was published in French, in Mémoires de l'Académie de la même année, 1755, page 194. 194 MtMOIRES DE L'AcADEMIE ROYALE SUR LES ETOILES NEBULEUSES DU CIEL AUSTRAL. Par lIl. 1' ..\1,0<' DE LA CAILLE. E s ftoiles qt,'on :lppelle nebuleufes olIent ~'l.'\ yeux L des Obfer\"Jtt:urs m fl ~e c1;lcle Ii nrie. {ille lem def criplion exaCle & J et:lilll-e pourroit occuper long·temps un Aflronoille. & donn er lit'LI :lUX Philo(ophes de [aire lIll grand nomhre de rt:flexions cllrieufes. Quelque fingulieres que foient les Il t:buleufes qlle nOLls POUVOIlS voir ell Europe. celles qtli font dans le voifin<lge du Pole aunral ne leur cedent en rien. lli pou r Ie 110mbre, oi pou r IJ figure. Je VJi5 en c:ballcher ici l" hilloire & b line: cel eff.d pOllrra guider ceux qui aucont la commodilc & Ie loiiir de It's cOllfiJcrer ::wec de longs 1t le[copes. -
Lacaille’S Catalogue of Southern Deep-Sky Objects
Lacaille’s Catalogue of Southern Deep-sky Objects Deep-sky Observing Challenge ASSA Deep-Sky Observing Section. Version 5, 2015 March 12 Lac number Other catalogue designations / Lacaille’s description Object type RA (J2000.0) Dec Con Lac number Other catalogue designations / Lacaille’s description Object type RA (J2000.0) Dec Con Lacaille I.1 NGC 104, 47 Tuc, Dunlop 18, Ben 2, C 106 globular cluster 00 24 06 –72° 04’ 53’’ Tuc Lacaille II.9 IC 2602, Southern Pleiades, C 102 open cluster 10 43 12 –64° 24’ 00’’ Car It resembles the nucleus of a fairly bright small comet. The star Theta Navis, of the third magnitude or less, surrounded by a large number of stars of sixth, seventh and eighth magnitude, which make it resemble the Pleiades. Lacaille I.2 NGC 2070, Tarantula Nebula, Dunlop 142, Ben 35, C 103 bright nebula 05 38 42 –69° 06’ 00’’ Dor It resembles the preceding, but it is fainter. Lacaille II.10 NGC 3532, Pincushion Cluster, Dunlop 323, C 91 open cluster 11 05 33 –58° 43’ 48’’ Car Prodigious cluster of faint stars, very compressed, filling up in the shape of semi-circle of 20’ to 25’ in diameter. Lacaille I.3 NGC 2477, Dunlop 535, C 71 open cluster 07 52 06 –38° 32’ 00’’ Pup Large nebulosity of 15’ to 20’ in diameter. Lacaille II.11 Dunlop 324 asterism 11 22 55 –58° 19’ 36’’ Cen Seven or eight faint stars compressed in a straight line. Lacaille I.4 NGC 4833, Dunlop 164, Ben 56, C 105 globular cluster 12 59 35 –70° 52’ 29’’ Mus It resembles a small comet, faint.