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29 Sep 2006: Data:. • Average of 200 Gb of science data per night (about 14 hours long). • ... Average night: 200 Gb/0.27 Gb = 740 images per night.

19 Apr 2006: This 200-AU-sized regioncoincides with the slightly tilted inner disk identified optically withthe Hubble Space Telescope5. ... The possible relationship of these components has yetto be explored, but the lower inferred temperatures of the clumpparticles

6 Jun 2006: Execute tiles that overlap with 200 deepest XMM pointings. • Fornax galaxy cluster(50deg2). ... The black filled circles are 200 deep public XMM pointings from the 2XMMcatalogue.

21 Sep 2006: Dense rings at 200 and 325 AU with tightly wound spiral structure (Clampin et al.

19 Apr 2006: the range 110–200 AU with low eccentricitiesand inclinations (e < 0.01, I < 0.573). ... One problem is thatboth the 200 and 325 AU spirals have large azimuthal densityvariations which make them appear clumpy.

19 Apr 2006: Accurate telescope pointing wascrucial to these observations and was checked before andafter each map using the nearby blazar 2255282 with rmserror of less than 200. ... Very littleinformation can be deduced about sizes or positions differ-ing by 200,

28 Sep 2006: Data Flow System. Document Title: UK VISTA User Requirements Document Number: VDF-SPE-IOA-00009-0001 Issue: 3.0 Date: 2005-07-05 Document Prepared by:. Will Sutherland (VISTA Project Scientist). Signature And date:. Document Approved by:. Jim

19 Apr 2006: 200 100 0 -100 -200RA offset, AU. -200. -100. 0. 100. ... 200. Dec. off. set,. AU. FIGURE 5. Impact of the outward migration of a Neptune mass planet on a planetesimal disk aroundVega [27]: orbital distribution of planetesimals at the beginning (top

19 Apr 2006: Dust emissionpeaks are resolved with source sizes of 200 to 500 (1.7 104 to4.3 104 AU).

29 Sep 2006: VISTA DATA FLOW SYSTEM(VDFS). —————————–. for VISTA & WFCAM data. Pipeline / Science Archive Interface Control Document. authorN.C.Hambly (WFAU Edinburgh)Science Archive Project Scientist. numberVDF-WFA-VSA-004. issueDraft 1.0.

19 Apr 2006: Compared to the fullextent of the mid-IR–emitting size of the disk (200 AU), therelatively small values of the dust FWHM sizes suggest thatthe mid-IR emission is sharply peaked ... extends out to at least a radius of 100 (200 AU) fromthe star in the

14 Dec 2006: 2004), we estimate for the firsttime the detection rate of cold debris disks around field M-dwarfs with ages between 20 and 200 Myr. ... al. 2005), the Castor moving group(200 Myr), the Ursa Maj moving group (500 100 Myr asrevised by King et al.

19 Apr 2006: higher surface brightness at r >200 AU compared to the r4 power law. ... but has slightlyhigher surface brightness at r > 200 AU compared to ther4 power law.

28 Sep 2006: event that observations of a secondary photometric standard field with a density of 100-200 objects per detector are available, then the illumination correction can be measured by looking at the

19 Apr 2006: 1984). This excess emission comes from dust in orbitaround the stars and its relatively cold temperature implies thatit resides at large distances from the stars, 30–200 AU, some-thing which ... 2003a) and IRAS observations at 60 and 100 µmhad 3σ

2 Nov 2006: belt width isdr = 0.5r; planetesimal strength is Q?D = 200 J kg. ... kg m3, e = 0.05, e/I = 1,Q?D = 200 J kg.

19 Apr 2006: ac-count and 200 dust particles were produced with exactlythe same positions and velocities as the parent popula-tion. ... for the librationparameters to be fitted for each particle, and the meanparameters for each population of 200 dust grains to

28 Sep 2006: Data Flow System Document Title: VISTA Data Reduction Library Design Document Number: VIS-SPE-IOA-20000-0010 Issue: 1.5 Date: 2006-09-28 Document Prepared by:. Jim Lewis Peter Bunclark Simon Hodgkin (CASU). Signature and Date:. Document Approved by:.

19 Apr 2006: Fitting a Gaussian to therebinned 850 m data indicates that the 850 m emission has aFWHM of 19B4 0B2 and is centered on the star to within 200. ... the disk around star Fomalhaut, which has anage of 200 Myr (Wyatt & Dent 2002).

19 Apr 2006: 20. -10. 0. 10. 20. Dec. off. set,. arcs. ec. É6 200 100 0 -100 -200RA offset, AU. ... 200. -100. 0. 100. 200. Dec. off. set,. AU. Î: Ì î Ï?Ð «0£sU6¤0 09¢&£¤¢?_M«XÓ¢ 9ªsM«ºs¤Ò_Ü£MX?ß 6_ºs_ºs_¡Çà Í

19 Apr 2006: HD207129 G0V 15.6 1.0 104 Spline 603022901660 8. HD22049 ǫ Eri K2V 3.22 1.1 104 Best fit model 730 200 10HD39060 β Pic A5V 19.3 3 ... HD109085 0.0 4.2 4.0 180 40HD38393 0.0 2.7 0.4 200 50HD48682 0.0 2.3 7.0 71 15a.

19 Apr 2006: Not Avail. no 16HD 107146 G2 30-250 130 red (V-I) 0.3 0.1 yes 17,18Fomalhaut A3 200 140 Not Avail. ... Emission (Additional)Vega A0 200 >90 23,24,25 Eridani K2 <1000 60 26,27η Corvi F2 1000 100 28τ Ceti G8 5000 55 29.

19 Apr 2006: up to 200 km in diameter) for impacts with a range ofimpact parameters and with relative velocities comparable to thoseexpected in extrasolar planetesimal discs. ... 6b), all models predict a lifetimethat is shorter than the age of the system (200 Myr)

19 Apr 2006: 1995, 1998). J98 andK98 determined that the diskÏs diameter is D3@@, which cor-responds to 200 AU at the starÏs distance of 67 pc, and theyconÐrmed directly the existence of the

19 Apr 2006: Including only dwarf stars, about 200 disccandidates remain. However, some of these are very young starsstill in the pre-main-sequence phase, which still possess primordialdiscs.

19 Apr 2006: RESONANT TRAPPING OF PLANETESIMALS BY PLANET MIGRATION: DEBRIS DISK CLUMPSAND VEGA’S SIMILARITY TO THE SOLAR SYSTEM. M. C. WyattUK Astronomy Technology Centre, Royal Observatory, Edinburgh EH9 3HJ, UK; wyatt@roe.ac.uk. Received 2003 June 11;

28 Nov 2006: 2004; Kim et al.2005), have conducted photometric surveys of about 200 nearbystars at 24 and 70m.

19 Apr 2006: "$# %&('). ,.-0/21436587$9;:<3=?>A@0B+CDFE!3GH+?I JK=?@ML,-N/FONDF:!-0/2GH31P:Q9;:!RS=?TU-MV0DWXRU>AGH+.-ZY,-5X-N=.-N>"-0/2[,D I2@M>"-0]Y29;Y29;E!3IU@X3MCD_X+?36UI23/8Y29UEa@N=B+?3/Sb0-0>AFc6d e0DUfg-N=BbihK92jk5X-NBml. Cno/2GHp,36=?]BGHq5@Mrs7)1H@0=

19 Apr 2006: THE ASTROPHYSICAL JOURNAL, 527 : 918È944, 1999 December 20The American Astronomical Society. All rights reserved. Printed in U.S.A.(1999. HOW OBSERVATIONS OF CIRCUMSTELLAR DISK ASYMMETRIES CAN REVEAL HIDDEN PLANETS :. PERICENTER GLOW AND ITS