Deep Ccd Surface Photometry of Galaxy Clusters
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Better Tapit
Barn 3 Hip No. Consigned by Claiborne Farm, Agent 1 Abrupt First Samurai . Giant’s Causeway Lea . {Freddie Frisson {Greenery . Galileo Abrupt . {High Savannah (GB) Bay colt; Political Force . Unbridled’s Song foaled 2017 {Ire . {Glitter Woman (2009) {Clash . Arch {Hit By LEA (2009), $2,362,398, Donn H. [G1]-ntr, Hal’s Hope S. [G3] twice, Com- monwealth Turf S. [G3], 2nd Woodbine Mile S. [G1], Breeders’ Cup Dirt Mile [G1], etc. His first foals are 3-year-olds of 2020. Sire of 16 wnrs, $932,816, including Muskoka Gold ($155,587, Cup and Saucer S., 2nd Grey S. [G3], etc.), Vast (to 3, 2020, $120,150, Hollywood Wildcat S.). 1st dam Ire, by Political Force. 4 wins at 3 and 4, $202,639, 2nd Mariah’s Storm S. (AP, $13,186), Meafara S. (AP, $13,014), 3rd Arlington Oaks [G3] (AP, $16,170), Mardi Gras H. (FG, $7,500), Happy Ticket S. (FG, $6,000). Sister to Flashy Campaign. Dam of 2 other foals of racing age-- Enrage (f. by Algorithms). Winner at 2, $64,086, 2nd Gin Talking S. (LRL, $20,000). Wrath (c. by Flatter). Winner at 3 and 4, 2020, $50,812. 2nd dam CLASH, by Arch. 2 wins, $86,771. Dam of 6 foals to race, 5 winners, incl.-- FASHION FAUX PAS (f. by Flatter). 3 wins at 2 and 3, 2019, $177,817, Sandpiper S. (TAM, $30,000), Light Hearted S. (DEL, $30,000), 2nd Delaware Oaks [G3] (DEL, $55,000), Mizdirection S. (AQU, $20,000), 3rd Hilltop S. (PIM, $10,000). Ire (f. -
Interferometric Observations of Rapidly Rotating Stars
Astron Astrophys Rev (2012) 20:51 DOI 10.1007/s00159-012-0051-2 REVIEW ARTICLE Interferometric observations of rapidly rotating stars Gerard T. van Belle Received: 10 October 2011 © The Author(s) 2012. This article is published with open access at Springerlink.com Abstract Optical interferometry provides us with a unique opportunity to improve our understanding of stellar structure and evolution. Through direct observation of rotationally distorted photospheres at sub-milliarcsecond scales, we are now able to characterize latitude dependencies of stellar radius, temperature structure, and even energy transport. These detailed new views of stars are leading to revised thinking in a broad array of associated topics, such as spectroscopy, stellar evolution, and exoplanet detection. As newly advanced techniques and instrumentation mature, this topic in astronomy is poised to greatly expand in depth and influence. Keywords Stars: rotation · Stars: imaging · Stars: fundamental parameters · Techniques: interferometric · Techniques: high angular resolution · Stars: individual: Altair, Alderamin, Achernar, Regulus, Vega, Rasalhague, Caph 1 Introduction One of the most fundamental stellar characteristics that is most frequently taken for granted is the shape of a star. This is perhaps somewhat unsurprising—in our direct experience of seeing stellar disks, there is only the sun, which is very nearly a perfect sphere: on an average radius of 959.28 ± 0.15 (Kuhn et al. 2004) there is only a variation of only 9.0 ± 1.8 mas (Rozelot et al. 2003) from equator to pole, indicating an oblateness (b/a − 1) of less than 10−5. However, for a surprisingly non-trivial number of stars, this degree of oblateness is in excess of 20% and, in certain cases, Portions of this manuscript were prepared while in residence at European Southern Observatory Karl-Schwarzschild-Str. -
Smartstar Cubepro Telescope Mount Instruction Manual
® SmartStar® CubeProTM Telescope Mount Instruction Manual Table of Content Table of Content ................................................................................................................................... 2 1. SmarStar® CubeProTM Mount Overview ............................................................................................ 4 1.1. SmartStar® CubeProTM Mount .................................................................................................... 4 1.2. Assembly Terms ......................................................................................................................... 5 1.3. Go2Nova® 8408 Hand Controller ............................................................................................... 5 1.3.1. Key Description .................................................................................................................... 6 1.3.2. The LCD Screen .................................................................................................................. 6 1.4. Check the Battery ....................................................................................................................... 7 2. CubeProTM Mount Assembly ............................................................................................................. 8 2.1. Setup a Mount in AA Mode ......................................................................................................... 8 2.2. Install Counterweight ............................................................................................................... -
Instruction Manual
iOptron® GEM28 German Equatorial Mount Instruction Manual Product GEM28 and GEM28EC Read the included Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument and uses a magnetic gear meshing mechanism. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging or adjusting the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper gear meshing/slippage will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ................................................................................................................................................. 3 1. GEM28 Overview .......................................................................................................................................... 5 2. GEM28 Terms ................................................................................................................................................ 6 2.1. Parts List ................................................................................................................................................. -
A Near-Infrared Interferometric Survey of Debris-Disk Stars VII
Astronomy & Astrophysics manuscript no. PIONIER_exozodi20_final ©ESO 2021 April 30, 2021 A near-infrared interferometric survey of debris-disk stars VII. The hot/warm dust connection? O. Absil1,??, L. Marion1, S. Ertel2; 3, D. Defrère4, G. M. Kennedy5, A. Romagnolo6, J.-B. Le Bouquin7, V. Christiaens8, J. Milli7, A. Bonsor9, J. Olofsson10; 11, K. Y. L. Su3, and J.-C. Augereau7 1 STAR Institute, Université de Liège, 19c Allée du Six Août, 4000 Liège, Belgium 2 Large Binocular Telescope Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA 3 Steward Observatory, Department of Astronomy, University of Arizona, 993 N. Cherry Ave, Tucson, AZ, 85721, USA 4 Institute of Astronomy, KU Leuven, Celestijnlaan 200D, 3001 Leuven, Belgium 5 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK 6 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716, Warsaw, Poland 7 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France 8 School of Physics and Astronomy, Monash University, Clayton, Vic 3800, Australia 9 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 10 Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Playa Ancha, Val- paraíso, Chile 11 Núcleo Milenio Formación Planetaria - NPF, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile Received 6 June 2017; accepted 21 April 2021 ABSTRACT Context. Hot exozodiacal dust has been shown to be present in the innermost regions of an increasing number of main sequence stars over the past fifteen years. The origin of hot exozodiacal dust and its connection with outer dust reservoirs remains however unclear. -
Interferometric Observations of Rapidly Rotating Stars
Accepted for publication in A&ARv Interferometric Observations of Rapidly Rotating Stars Gerard T. van Belle1 ABSTRACT Optical interferometry provides us with a unique opportunity to improve our under- standing of stellar structure and evolution. Through direct observation of rotationally distorted photospheres at sub-milliarcsecond scales, we are now able to characterize latitude dependencies of stellar radius, temperature structure, and even energy trans- port. These detailed new views of stars are leading to revised thinking in a broad array of associated topics, such as spectroscopy, stellar evolution, and exoplanet detection. As newly advanced techniques and instrumentation mature, this topic in astronomy is poised to greatly expand in depth and influence. Subject headings: stars: rotation; stars: imaging; stars: fundamental parameters; tech- niques: interferometric; techniques: high angular resolution; stars: individual: Altair, Alderamin, Achernar, Regulus, Vega, Rasalhague, Caph 1. Introduction One of the most fundamental stellar characteristics that is most frequently taken for granted is the shape of a star. This is perhaps somewhat unsurprising — in our direct experience of seeing stellar disks, there is only the sun, which is very nearly a perfect sphere: on an average radius of 959′′.28 0′′.15 (Kuhn et al. 2004) there is only a variation of only 9.0 1.8mas (Rozelot et al. ± ± 2003) from equator to pole, indicating an oblateness (b/a 1) of less than 10−5. However, for − a surprisingly non-trivial number of stars, this degree of oblateness is in excess of 20% and, in arXiv:1204.2572v1 [astro-ph.SR] 11 Apr 2012 certain cases, even 30%. Hints of this have been seen for decades in stellar spectroscopy, but this phenomenon has eluded direct observation until only recently. -
Instruction Manual
iOptron® GEM45 German Equatorial Mount Instruction Manual Product GEM45 (#7600A series) and GEM45EC (#7600ECA series, as shown) Please read the included GEM45 Quick Setup Guide (QSG) BEFORE taking the mount out of the case! This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. You must hold the mount firmly when disengaging the gear switches. Otherwise personal injury and/or equipment damage may occur. Any worm system damage due to improper operation will not be covered by iOptron’s limited warranty. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while using a telescope. 2 Table of Contents Table of Contents ........................................................................................................................................ 3 1. GEM45 Introduction ............................................................................................................................... 5 2. GEM45 Overview ................................................................................................................................... 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification -
Ioptron Ieq30 Pro Equatorial Mount Instruction Manual
® iOptron® iEQ30 ProTM Equatorial Mount Instruction Manual Product #3000E This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ......................................................................................................................................... 3 1. iEQ30 ProTM German Equatorial Mount Overview ................................................................................ 5 2. iEQ30 ProTM Mount Assembly ............................................................................................................... 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification of Parts ....................................................................................................................... 7 2.3. iEQ30 Pro Mount Ports .................................................................................................................... 8 2.4. Go2Nova® 8407+ Hand Controller ................................................................................................. -
Chromospheric and Coronal Activity in Solar-Like Stars
Chromospheric and coronal activity in solar-like stars Dissertation zur Erlangung des Doktorgrades des Departments Physik der Universitat¨ Hamburg vorgelegt von Christian Schroder¨ geboren in Hamburg Hamburg 2008 ii Gutachter der Dissertation: Prof. J.H.M.M. Schmitt Dr. Ansgar Reiners Gutachter der Disputation: Prof. J.H.M.M. Schmitt Prof. P.H. Hauschildt Datum der Disputation: 18.07.2008 Vorsitzender des Pr¨ufungsausschusses: Prof. G. Wiedemann Vorsitzender des Promotionsausschusses: Prof. J. Bartels Dekan der Fakult¨at f¨ur Mathematik, Informatik und Naturwissenschaften: Prof. Dr. Arno Fr¨uhwald iv Zusammenfassung Der Begriff ”stellare Aktivit¨at” fasst diverse Ph¨anomene auf der Sternenoberfl¨ache und in der Stern- atmosph¨are zusammen. Die Ursache f¨ur diese Ph¨anomene sind Ver¨anderungen in den Magnetfeldern der Sterne. W¨ahrend es bei der Sonne m¨oglich ist, die verschiedenen Formen der Aktivit¨at direkt und detailliert zu beobachten, ist dies bei anderen Sternen nicht m¨oglich. Durch eine genaue Analyse der Spektren von Sternen lassen sich dennoch Informationen ¨uber deren Aktivit¨at gewinnen. Die folgende Arbeit befasst sich mit zwei Arten der stellaren Aktivit¨at: zum einen mit der R¨ontgenaktivit¨at von Sternen des Spektraltyps A und ihrer potentiellen Ursache, zum zweiten mit der chromosph¨arischen Aktivit¨at von Sternen im Bereich der sp¨aten A- bis sp¨aten K-Sterne. Da im Bereich der sp¨aten A- bis fr¨uhen F-Sterne der Dynamo, der f¨ur die Aktivit¨at in sonnen¨ahnlichen Sternen verant- wortlich ist, entsteht, ist dieser Spektralbereich f¨ur das Verst¨andnis der stellaren Aktivit¨at von besonderer Bedeutung. -
Rotation-And Temperature-Dependence of Stellar
Astronomy & Astrophysics manuscript no. 3911 August 11, 2018 (DOI: will be inserted by hand later) Rotation- and temperature-dependence of stellar latitudinal differential rotation⋆ A. Reiners1,2⋆⋆ 1 Astronomy Department, 521 Campbell Hall, University of California, Berkeley, CA 94720 e-mail: [email protected] 2 Hamburger Sternwarte, Universit¨at Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany August 11, 2018 Abstract. More than 600 high resolution spectra of stars with spectral type F and later were obtained in order to search for signatures of differential rotation in line profiles. In 147 stars the rotation law could be measured, with 28 of them found to be differentially rotating. Comparison to rotation laws in stars of spectral type A reveals that differential rotation sets in at the convection boundary in the HR-diagram; no star that is significantly hotter than the convection boundary exhibits the 1 signatures of differential rotation. Four late A-/early F-type stars close to the convection boundary and at v sin i 100 km s− ≈ show extraordinarily strong absolute shear at short rotation periods around one day. It is suggested that this is due to their small convection zone depth and that it is connected to a narrow range in surface velocity; the four stars are very similar in Teff and v sin i. Detection frequencies of differential rotation α = ∆Ω/Ω > 0 were analyzed in stars with varying temperature and rotation velocity. Measurable differential rotation is more frequent in late-type stars and slow rotators. The strength of absolute shear, ∆Ω, and differential rotation α are examined as functions of the stellar effective temperature and rotation period. -
New Measurements of Rotation and Differential Rotation in AF Stars: Are There Two Populations of Differentially Rotating Stars?
Astronomy & Astrophysics manuscript no. diffrot c ESO 2018 November 1, 2018 New measurements of rotation and differential rotation in A-F stars: Are there two populations of differentially rotating stars? ⋆⋆⋆ Ammler-von Eiff, M.1,2,3 and Reiners, A.2 1 Th¨uringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany e-mail: [email protected] 2 Institut f¨ur Astrophysik, Georg-August-Universit¨at G¨ottingen, Friedrich-Hund-Platz 1, 37077 G¨ottingen, Germany e-mail: [email protected] 3 Max Planck Institute for Solar System Research, Max-Planck-Straße 2, 37191 Katlenburg-Lindau, Germany Received September 15, 1996; accepted March 16, 1997 ABSTRACT Context. The Sun displays differential rotation that is intimately connected to the solar dynamo and hence related to solar activity, the solar cycle, and the solar wind. Considering the detectability and habitability of planets around other stars it is important to understand the role of differential rotation in other stars. Aims. We present projected rotational velocities and new measurements of the rotational profile of some 180 nearby stars with spectral types A-F. The results are consolidated by a homogeneous compilation of basic stellar data from photometry and the identification of multiple stellar systems. New and previous measurements of rotation by line profile analysis are compiled and made available. Methods. The overall broadening profile is derived analysing spectral line shape from hundreds of spectral lines by the method of least-squares deconvolution, reducing spectral noise to a minimum. The effect of differential rotation on the broadening profile is best measured in inverse wavelength space by the first two zeros of its Fourier transform. -
Characterising the Young Sco-Cen Association
Characterising the Young Sco-Cen Association By Aaron Rizzuto A thesis submitted to Macquarie University for the degree of Doctor of Philosophy Department of Physics and Astronomy March 2015 ii c Aaron Rizzuto, 2015. Typeset in LATEX 2". iii Except where acknowledged in the customary manner, the material presented in this thesis is, to the best of my knowledge, original and has not been submitted in whole or part for a degree in any university. Aaron Rizzuto iv Acknowledgements Firstly, I would like to express enormous gratitude to my PhD supervisor Mike Ireland, for providing just the right balance of direction and freedom to allow me to develop my own ideas while not losing track of the goals we had planned, for providing me with the opportunity to be involved in international collaborations, and for always treating me like a friend and colleague rather than a student. I would also like to thank Gordon Robertson, for providing carefully thought-out comments to reports and papers I had written and for his encouraging words, and Dan Zucker, for lots of proof reading. Thanks to the SUSI group members for assistance in observing and engineering for SUSI. A particular mention to Yitping Kok, for our interesting nights tandem observing. I also thank our Adam Kraus for our various discussions which helped improve this thesis. Thanks to fellow PhD students and postdocs, including Niyas Alikutty, Dimitri Douchin, Izabella Spelaniak, Joao Bento, and Carlos Bacigalupo for providing good conversation and company, and thanks to Bjorn Sturmberg for the climbing excursions. Thank you to my family, including my mother who set me on this path that I have taken and supported me along the way, and to my brothers David and Michael who always provided encouragement and showed pride in what I was doing.