Multiple Star Systems Observed with Corot and Kepler
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BRAS Newsletter August 2013
www.brastro.org August 2013 Next meeting Aug 12th 7:00PM at the HRPO Dark Site Observing Dates: Primary on Aug. 3rd, Secondary on Aug. 10th Photo credit: Saturn taken on 20” OGS + Orion Starshoot - Ben Toman 1 What's in this issue: PRESIDENT'S MESSAGE....................................................................................................................3 NOTES FROM THE VICE PRESIDENT ............................................................................................4 MESSAGE FROM THE HRPO …....................................................................................................5 MONTHLY OBSERVING NOTES ....................................................................................................6 OUTREACH CHAIRPERSON’S NOTES .........................................................................................13 MEMBERSHIP APPLICATION .......................................................................................................14 2 PRESIDENT'S MESSAGE Hi Everyone, I hope you’ve been having a great Summer so far and had luck beating the heat as much as possible. The weather sure hasn’t been cooperative for observing, though! First I have a pretty cool announcement. Thanks to the efforts of club member Walt Cooney, there are 5 newly named asteroids in the sky. (53256) Sinitiere - Named for former BRAS Treasurer Bob Sinitiere (74439) Brenden - Named for founding member Craig Brenden (85878) Guzik - Named for LSU professor T. Greg Guzik (101722) Pursell - Named for founding member Wally Pursell -
Asteroseismology with Corot, Kepler, K2 and TESS: Impact on Galactic Archaeology Talk Miglio’S
Asteroseismology with CoRoT, Kepler, K2 and TESS: impact on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 AsteroseismologyPlato as it is : a Legacy with CoRoT Mission, Kepler for Galactic, K2 and TESS: impactArchaeology on Galactic Archaeology talk Miglio’s CRISTINA CHIAPPINI Leibniz-Institut fuer Astrophysik Potsdam PLATO PIC, Padova 09/2019 Galactic Archaeology strives to reconstruct the past history of the Milky Way from the present day kinematical and chemical information. Why is it Challenging ? • Complex mix of populations with large overlaps in parameter space (such as Velocities, Metallicities, and Ages) & small volume sampled by current data • Stars move away from their birth places (migrate radially, or even vertically via mergers/interactions of the MW with other Galaxies). • Many are the sources of migration! • Most of information was confined to a small volume Miglio, Chiappini et al. 2017 Key: VOLUME COVERAGE & AGES Chiappini et al. 2018 IAU 334 Quantifying the impact of radial migration The Rbirth mix ! Stars that today (R_now) are in the green bins, came from different R0=birth Radial Migration Sources = bar/spirals + mergers + Inside-out formation (gas accretion) GalacJc Center Z Sun R Outer Disk R = distance from GC Minchev, Chiappini, MarJg 2013, 2014 - MCM I + II A&A A&A 558 id A09, A&A 572, id A92 Two ways to expand volume for GA • Gaia + complementary photometric information (but no ages for far away stars) – also useful for PIC! • Asteroseismology of RGs (with ages!) - also useful for core science PLATO (miglio’s talk) The properties at different places in the disk: AMR CoRoT, Gaia+, K2 + APOGEE Kepler, TESS, K2, Gaia CoRoT, Gaia+, K2 + APOGEE PLATO + 4MOST? Predicon: AMR Scatter increases towards outer regions Age scatter increasestowars outer regions ExtracGng the best froM GaiaDR2 - Anders et al. -
Data Mining in the Spanish Virtual Observatory. Applications to Corot and Gaia
Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society held on September 13 - 17, 2010, in Madrid, Spain. M. R. Zapatero Osorio et al. (eds.) Data mining in the Spanish Virtual Observatory. Applications to Corot and Gaia. Mauro L´opez del Fresno1, Enrique Solano M´arquez1, and Luis Manuel Sarro Baro2 1 Spanish VO. Dep. Astrof´ısica. CAB (INTA-CSIC). P.O. Box 78, 28691 Villanueva de la Ca´nada, Madrid (Spain) 2 Departamento de Inteligencia Artificial. ETSI Inform´atica.UNED. Spain Abstract Manual methods for handling data are impractical for modern space missions due to the huge amount of data they provide to the scientific community. Data mining, understood as a set of methods and algorithms that allows us to recover automatically non trivial knowledge from datasets, are required. Gaia and Corot are just a two examples of actual missions that benefits the use of data mining. In this article we present a brief summary of some data mining methods and the main results obtained for Corot, as well as a description of the future variable star classification system that it is being developed for the Gaia mission. 1 Introduction Data in Astronomy is growing almost exponentially. Whereas projects like VISTA are pro- viding more than 100 terabytes of data per year, future initiatives like LSST (to be operative in 2014) and SKY (foreseen for 2024) will reach the petabyte level. It is, thus, impossible a manual approach to process the data returned by these surveys. It is impossible a manual approach to process the data returned by these surveys. -
Photometry of Be Stars in the Vicinity of COROT Primary Targets for Asteroseismology
Comm. in Asteroseismology Vol. 143, 2003 Photometry of Be stars in the vicinity of COROT primary targets for asteroseismology J. Guti´errez-Soto1, J. Fabregat1, J. Suso2, A.M. Hubert3, M. Floquet3 and R. Garrido4 1 Observatori Astron`omic, Universitat de Val`encia 2 Instituto Ciencia de los Materiales, Universitat de Val`encia 3GEPI, Observatoire de Paris-Meudon 4Instituto de Astrof´ısica de Andaluc´ıa Abstract We present differential photometry of Be stars close to potential COROT pri- mary targets for asteroseismology. Several stars are found to be short pe- riod variables. We propose them to be considered as secondary targets in the COROT asteroseismology fields. Introduction The observation of classical Be stars by COROT will provide important keys to understand the physics of these objects and the nature of the Be phenomenon. In particular, the detection of photospheric multiperiodicity will confirm the presence of non radial pulsations (nrp) as the origin of the short term variability. COROT observations will allow the study of the beat phenomenon of nrp modes and its relation with recurrent outbursts and the building of the circumstellar disc. Our group is proposing the observation of Be stars as secondary targets for the asteroseismology fields. A sample of stars in the vicinity of the main target candidates is under study for this purpose. Hubert et al. (2001, 2003) presented the selected objects and performed a study of their short term variability using Hipparcos photometric data. We have obtained new ground based photometry with a more suitable time sampling to further characterize their variability. 2 Photometry of Be stars in the vicinity of COROT primary targets for asteroseismology Observations and data analysis Observations were done at the 0.9 m telescope of the Observatorio de Sierra Nevada (Granada, Spain). -
2014 Observers Challenge List
2014 TMSP Observer's Challenge Atlas page #s # Object Object Type Common Name RA, DEC Const Mag Mag.2 Size Sep. U2000 PSA 18h31m25s 1 IC 1287 Bright Nebula Scutum 20'.0 295 67 -10°47'45" 18h31m25s SAO 161569 Double Star 5.77 9.31 12.3” -10°47'45" Near center of IC 1287 18h33m28s NGC 6649 Open Cluster 8.9m Integrated 5' -10°24'10" Can be seen in 3/4d FOV with above. Brightest star is 13.2m. Approx 50 stars visible in Binos 18h28m 2 NGC 6633 Open Cluster Ophiuchus 4.6m integrated 27' 205 65 Visible in Binos and is about the size of a full Moon, brightest star is 7.6m +06°34' 17h46m18s 2x diameter of a full Moon. Try to view this cluster with your naked eye, binos, and a small scope. 3 IC 4665 Open Cluster Ophiuchus 4.2m Integrated 60' 203 65 +05º 43' Also check out “Tweedle-dee and Tweedle-dum to the east (IC 4756 and NGC 6633) A loose open cluster with a faint concentration of stars in a rich field, contains about 15-20 stars. 19h53m27s Brightest star is 9.8m, 5 stars 9-11m, remainder about 12-13m. This is a challenge obJect to 4 Harvard 20 Open Cluster Sagitta 7.7m integrated 6' 162 64 +18°19'12" improve your observation skills. Can you locate the miniature coathanger close by at 19h 37m 27s +19d? Constellation star Corona 5 Corona Borealis 55 Trace the 7 stars making up this constellation, observe and list the colors of each star asterism Borealis 15H 32' 55” Theta Corona Borealis Double Star 4.2m 6.6m .97” 55 Theta requires about 200x +31° 21' 32” The direction our Sun travels in our galaxy. -
A Triply Eclipsing System with Intrinsically Variable Red Giant Component A
Title : will be set by the publisher Editors : will be set by the publisher EAS Publications Series, Vol. ?, 2013 HD181068: A TRIPLY ECLIPSING SYSTEM WITH INTRINSICALLY VARIABLE RED GIANT COMPONENT A. Derekas1, T. Borkovits21, 3, J. Fuller4, D. Huber5 and H. Lehmann6 Abstract. We present the analysis of HD 181068 which is one of the first triply eclipsing triple system discovered. Using Kepler photome- try, ground based spectroscopic and interferometric measurements, we determined the stellar and orbital parameters of the system. We show that the oscillations observed in the red giant component of the system are tidally forced oscillations, while one of the most surprising results is that it does not show solar-like oscillations. 1 Introduction The ultraprecise and continous photometry of Kepler space telescope led to great discoveries not just in the field of exoplanets but in stellar astrophysics too. Among others, it opened a new era in the investigation of multiple star systems, such as dis- coveries of the first triply eclipsing triple systems, KOI-126 (Carter et al. (2011)) and HD 181068 (Derekas et al. (2011)). The special geometry of these triply (or mutually) eclipsing triple systems, enables us fast and easy determination of fur- ther characteristics that otherwise could only be studied with great effort on a long time-scale. Here we present the analysis of the triply eclipsing hierarchical triple sys- tem HD 181068 based on Kepler photometry, ground based high-resolution spec- troscopy and interferometry. HD 181068 has a magnitude of V = 7.1 and a dis- tance of about 250 pc (van Leeuwen (2007)). -
Binocular Double Star Logbook
Astronomical League Binocular Double Star Club Logbook 1 Table of Contents Alpha Cassiopeiae 3 14 Canis Minoris Sh 251 (Oph) Psi 1 Piscium* F Hydrae Psi 1 & 2 Draconis* 37 Ceti Iota Cancri* 10 Σ2273 (Dra) Phi Cassiopeiae 27 Hydrae 40 & 41 Draconis* 93 (Rho) & 94 Piscium Tau 1 Hydrae 67 Ophiuchi 17 Chi Ceti 35 & 36 (Zeta) Leonis 39 Draconis 56 Andromedae 4 42 Leonis Minoris Epsilon 1 & 2 Lyrae* (U) 14 Arietis Σ1474 (Hya) Zeta 1 & 2 Lyrae* 59 Andromedae Alpha Ursae Majoris 11 Beta Lyrae* 15 Trianguli Delta Leonis Delta 1 & 2 Lyrae 33 Arietis 83 Leonis Theta Serpentis* 18 19 Tauri Tau Leonis 15 Aquilae 21 & 22 Tauri 5 93 Leonis OΣΣ178 (Aql) Eta Tauri 65 Ursae Majoris 28 Aquilae Phi Tauri 67 Ursae Majoris 12 6 (Alpha) & 8 Vul 62 Tauri 12 Comae Berenices Beta Cygni* Kappa 1 & 2 Tauri 17 Comae Berenices Epsilon Sagittae 19 Theta 1 & 2 Tauri 5 (Kappa) & 6 Draconis 54 Sagittarii 57 Persei 6 32 Camelopardalis* 16 Cygni 88 Tauri Σ1740 (Vir) 57 Aquilae Sigma 1 & 2 Tauri 79 (Zeta) & 80 Ursae Maj* 13 15 Sagittae Tau Tauri 70 Virginis Theta Sagittae 62 Eridani Iota Bootis* O1 (30 & 31) Cyg* 20 Beta Camelopardalis Σ1850 (Boo) 29 Cygni 11 & 12 Camelopardalis 7 Alpha Librae* Alpha 1 & 2 Capricorni* Delta Orionis* Delta Bootis* Beta 1 & 2 Capricorni* 42 & 45 Orionis Mu 1 & 2 Bootis* 14 75 Draconis Theta 2 Orionis* Omega 1 & 2 Scorpii Rho Capricorni Gamma Leporis* Kappa Herculis Omicron Capricorni 21 35 Camelopardalis ?? Nu Scorpii S 752 (Delphinus) 5 Lyncis 8 Nu 1 & 2 Coronae Borealis 48 Cygni Nu Geminorum Rho Ophiuchi 61 Cygni* 20 Geminorum 16 & 17 Draconis* 15 5 (Gamma) & 6 Equulei Zeta Geminorum 36 & 37 Herculis 79 Cygni h 3945 (CMa) Mu 1 & 2 Scorpii Mu Cygni 22 19 Lyncis* Zeta 1 & 2 Scorpii Epsilon Pegasi* Eta Canis Majoris 9 Σ133 (Her) Pi 1 & 2 Pegasi Δ 47 (CMa) 36 Ophiuchi* 33 Pegasi 64 & 65 Geminorum Nu 1 & 2 Draconis* 16 35 Pegasi Knt 4 (Pup) 53 Ophiuchi Delta Cephei* (U) The 28 stars with asterisks are also required for the regular AL Double Star Club. -
Lick Observatory Records: Photographs UA.036.Ser.07
http://oac.cdlib.org/findaid/ark:/13030/c81z4932 Online items available Lick Observatory Records: Photographs UA.036.Ser.07 Kate Dundon, Alix Norton, Maureen Carey, Christine Turk, Alex Moore University of California, Santa Cruz 2016 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Lick Observatory Records: UA.036.Ser.07 1 Photographs UA.036.Ser.07 Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Photographs Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.07 Physical Description: 101.62 Linear Feet127 boxes Date (inclusive): circa 1870-2002 Language of Material: English . https://n2t.net/ark:/38305/f19c6wg4 Conditions Governing Access Collection is open for research. Conditions Governing Use Property rights for this collection reside with the University of California. Literary rights, including copyright, are retained by the creators and their heirs. The publication or use of any work protected by copyright beyond that allowed by fair use for research or educational purposes requires written permission from the copyright owner. Responsibility for obtaining permissions, and for any use rests exclusively with the user. Preferred Citation Lick Observatory Records: Photographs. UA36 Ser.7. Special Collections and Archives, University Library, University of California, Santa Cruz. Alternative Format Available Images from this collection are available through UCSC Library Digital Collections. Historical note These photographs were produced or collected by Lick observatory staff and faculty, as well as UCSC Library personnel. Many of the early photographs of the major instruments and Observatory buildings were taken by Henry E. Matthews, who served as secretary to the Lick Trust during the planning and construction of the Observatory. -
Onze Melkweg , Door Willy Acke ON4AW
Sterrenkunde 1 door Willy Acke, ON4AW We bekijken nu gedetailleerder enkele sterren en sterrenbeelden, waarnaar in de reeks weerstanden een inleidende beschrijving te lezen was. 1) Het Sterrenstelsel Perseus Hierboven werd reeds vermeld dat de Zon in de Orionarm of in een vertakking van de Perseusarm ligt. De plaats waar de vertakking zich afsplitst, ligt in het sterrenbeeld Cygnus. De Perseusarm zelf loopt door aan de buitenkant van de vertakking, op ongeveer 2600 lichtjaren van de Zon (de Zon ligt op 22000 tot 30000 lichtjaren van het centrum van de Melkweg). In dit sterrenbeeld ligt de dubbele open sterrenhoop h + χ Persei (NGC 869 en 884), met het blote oog vanop de Aarde zichtbaar. Persei is de tweede helderste ster in het sterrenbeeld Perseus en is een variabele ster. De open sterrenhoop h + χ Perseus bestaat uit een zeer jonge populatie sterren (106 tot 107 jaren), terwijl NGC 188 in het kader van de sterrenevolutie ongeveer tot de oudste sterren (=1010 jaren) van ons melkwegstelsel behoort. De dubbele cluster van Perseus is zichtbaar met het blote oog als een sterke concentratie in de Melkweg. Gevestigd in de noordelijke sterrenhemelhemisfeer ligt ze dichtbij verscheidene andere constellaties of aangrenzende sterrenbeelden uit de legende van Perseus, met inbegrip van Andromeda (het meisje dat hij heeft gered), Cetus (het zeemonster dat hij overwonnen heeft), Cepheus en Cassiopeia (de koninklijke ouders van Andromeda), Driehoek (Triangulum), Ram (Aries), Stier (Taurus), Voerman (Auriga), Giraffe (Camelopardalis). 1 - - In het wintersterrenbeeld Perseus is er een ster die knipoogt. Gedurende 2 dagen aan een stuk blijft ze op een bijna constante helderheid, maar de daaropvolgende 5 uren dempt deze met meer dan 1 magnitude. -
Using Asteroseismology to Characterise Exoplanet Host Stars
Using asteroseismology to characterise exoplanet host stars Mia S. Lundkvist, Daniel Huber, Victor Silva Aguirre, and William J. Chaplin Abstract The last decade has seen a revolution in the field of asteroseismology – the study of stellar pulsations. It has become a powerful method to precisely characterise exoplanet host stars, and as a consequence also the exoplanets themselves. This syn- ergy between asteroseismology and exoplanet science has flourished in large part due to space missions such as Kepler, which have provided high-quality data that can be used for both types of studies. Perhaps the primary contribution from aster- oseismology to the research on transiting exoplanets is the determination of very precise stellar radii that translate into precise planetary radii, but asteroseismology has also proven useful in constraining eccentricities of exoplanets as well as the dy- namical architecture of planetary systems. In this chapter, we introduce some basic principles of asteroseismology and review current synergies between the two fields. Mia S. Lundkvist Zentrum fur¨ Astronomie der Universitat¨ Heidelberg, Landessternwarte, Konigstuhl¨ 12, 69117 Hei- delberg, DE, and Stellar Astrophysics Centre, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, DK, e-mail: [email protected] Daniel Huber Institute for Astronomy, University of Hawai‘i, 2680 Woodlawn Drive, Honolulu, HI 96822, US and Sydney Institute for Astronomy, School of Physics, University of Sydney, NSW 2006, Aus- tralia, e-mail: [email protected] Victor Silva Aguirre arXiv:1804.02214v2 [astro-ph.SR] 9 Apr 2018 Stellar Astrophysics Centre, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, DK, e-mail: [email protected] William J. -
Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al. -
2014 Science with the Hubble Space
Beyond HST: The Universe in High-Definition – UVOIR Space Astronomy in 2030 Julianne Dalcanton & Marc Postman Science with HST IV Meeting Rome, Italy March 18, 2014 Long History of Large Space UVOIR Telescope Concepts • VLST – 10m-16m concept (ca. 1989) • SUVO – 4m concept (ca. 1998-1999) • Workshop on 10m - 30m VLST (2003) • MUST – 10m concept (ca. 2004-2005) • ATLAST – 8m-16m concepts (ca. 2008-2010) • EUVO – European 8m concept (ca. 2013) • Modular Assembled 20m concept (ca. 2013) Scientifically compelling for over 2 decades! (Average Aperture Diameter – 13.5 meters) “Can we find another planet like Earth orbiting a nearby star? To find such a planet would complete the revolution, started by Copernicus nearly 500 years ago, that displaced the Earth as the center of the universe… The observational challenge is great but armed with new technologies… astronomers are poised to rise to it.” - U.S. 2010 Astronomy Decadal Review This is a question whose answer is sought by all of humanity and the search will demand international cooperation. The path has been laid ! for characterizing Earth 2.0 Kepler Hubble Spitzer CoRoT Ground-based Coronagraphs Gaia WFIRST 30-m class telescopes TESS JWST PLATO !"#$%&'('$)*+%&'($,)(%&$+-%$%&'('./$ Thick Atmosphere Methane Oxygen Fraction with terrestrial planets = !Earth FractionWater with detectable biosignature = fBio OpticalIf : ! Near-Infrared $ f ~ 1 then D ~ 4m Earth Bio0'12'($('#-2%#$ 8-meterTel 16-meter The signature of life is encoded inf the < 1 then D 8m spectrum! Earthof the Earth$ Bio $ tel ~ 70 !Earth $ fBio << 1 then DTel ~ 16m a > 12 Earths $ 60 50 40 30 # 4 Earths 20 4-meter 10 of total integration time of total integration time 0 Above: Distribution of all FGK stars within 45 pc of the Sun Number of Exo-Earths in 1 year 2-m 4-m 8-m 16-m where a R=70 spectrum of an Earth-twin could be acquired Telescope Size in <500 ksec shown as a function of telescope aperture.