Search

3 Dec 2010: The faulty CCD has been replaced and the whole array is co-planar to /- 20 microns. ... Approximately 20% of the band-merged VHS tile products investigated had a serious problem with the photometry due to this effect (though it is a moot point if most of

1 Mar 2010: Consider the process. ˜ χ 20 ˜   ˜ χ 1.

24 Mar 2010: 4. Data archives update AAT, ING, WFCAM, VISTA: all going smoothly UKIRT: JRL reported that he was still awaiting the last 20 or so nights of missing data.

5 Oct 2010: start of cupconf.sty %%%%%%%%%%%%%%%%%%%%%% % CUPconf.sty -- CUP conference proceedings style file % V0.1 released 20 September 1993, by Alison Woollatt % Copyright (1993) Cambridge University Press % This software may only be used ... 2,space}}% %

30 Aug 2010: Although only a few % in the Ks band the effect is approaching 15-20% in the Y and Z-bands.

5 May 2010: 5 new BLADES (20 cores) have been acquired and added to the VISTA processing kit and SC is in the process of connecting them up and installing an operating system on

27 May 2010: For point-source mode ob-servations, seven contiguous repeat chop/nod observations wereperformed. Scan map observations had eight repeats in a singlescan direction at a rate of 20′′/s. ... 20 Dept. of Physics & Astronomy, University of California,

24 Mar 2010: March 2008. 18-20 March - UltraVista meeting in Leiden, MJI and JRL part attended and gave talks.

2 Sep 2010: In the general stellar population, theextrapolated planet total is 17-20 % (Cumming et al. ... 2008; Greaves & Wyatt 2010), which agreewell with the predictions of 21 and 20 % respectively.

29 Jan 2010: The high-est mass appears realistic, for example it is comparable tothe 20-30 M of colliders inferred around the A-star Fomal-haut (Wyatt & Dent 2002), which hosts a bright ... 2008) estimate that 18 % of Sun-likestars host giant planets, of above about

10 Nov 2010: 0 20 40 60 80 10090. 95. 100. 105. 110. Radius! ... The expected flux density calculated withthis relation agrees with the flux density values both from ob-servations and from our model to within 20% at 0.57, 1.1, and1.6µm.

15 Dec 2010: 127271 39.081915 1734.49 69459.2 20.3629 1798.92 127704 24.029317 2272.84 68903.7 13.6835 2346.56 128024 15.814919 2883.61 68472.8 9.63420

6 Apr 2010: SiC 11.85 1800 VISIR 124 120 23 3 7Q2 18.72 3760 VISIR 50 119 11 9 20. ... The recent 24µm and 18µmdetections presented here suggest a lower excess than that sug-gested by IRAS photometry (275 20 mJy at 25µm).

27 Jul 2010: larly at 70µmFdiscF. = 1-5 (diamond:small excess), 5-20 (square:. medium excess), >20 (triangle: large excess). ... that extends down to 1010m,the contribution of particles less than 108m in size to the24µm disc flux is only 20%.

22 Aug 2010: 1.32 46.8 2.64 5.9 104 20 1 6HD 181327 F5/6V 1.3 51 3.1 3103 20 [86] 7,1,6,12,13 7 (Resolved

19 Feb 2010: This differentemphasis changes the values obtained in the formal fit at24 µm by 10–20%.3. ... For belts rmid = 20, 30, 40,50, 60, and 70 AU, dr = rmid/2, and η = 1.

25 Nov 2010: Integrating equation (19) yields. Dc =Dmax. (1 0.4(t tnleft)/tnleft)α. (20). where α = 1/1.2. ... When there are only Nstr largest objects left, Dcbegins to decay as dictated by Equation (20).