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8 Mar 2006: 4400. 22.1. 2.6. V. 5500. 21.3. 3.5. R. 6000. 20.4. 3.9. ... 3000. 22.0. 21.2. 20.0. 19.5. 100. Galactic Plane Magellanic Clouds. 1500.

19 Apr 2006: Combining this with the beam size, the effectiveresolution is 20 arcsec or 70 au. ... Figure 1. 850-µm image of τ Ceti, smoothed to 20-arcsec resolution.

15 Apr 2006: 0.10. V. 5500. 21.3. 21.4. 9.6. 3.5. 0.15. R. 6000. 20.4. ... In some the star–formation at this level may have begun at z10-20.

17 Jan 2006: A reasonable estimate to account for this is that the 2x2 plots need to be adjusted by 20% (ie. ... However, one of the frames exhibited a large magnitude term in yamounting to 0.05 pixel (20 mas) over the observed magnitude range.

19 Apr 2006: Consideration of the collisional lifetime of different sizedbodies in the disk showed that what we are seeing is just the bottom half of the cascade(7 µ m dust to 20 ... C., and Taidakova, T. A., Astrophys. J., 537, L147–L151. (2000).20. Macintosh, B.

19 Apr 2006: 0. 20. 40. Ecl. ipti. c L. atit. ude. 70 80 90 100 110Ecliptic Longitude Relative to Sun. ... 40. -20. 0. 20. 40. 70 80 90 100 110Ecliptic Longitude Relative to Sun.

16 Nov 2006: predominantly Mg-rich olivines (80%) and crystalline pyroxenes (20%) (Figure 3). Unlike our. ... Dark blues - crystalline olivines, forsterite and fayalite, in order of 20 µm amplitude.

19 Apr 2006: areconsistent with a ring of radius 150 20 AU seen at 45 25 inclination. ... would migrate from 150to 0 AU (where it would evaporate) on timescales of 20 Myr(Burns et al.

19 Apr 2006: and Spangler et al. (2000) are also included here – ISO observed 70per cent of the single A stars but only 20 per cent of single G starswithin 25 pc. ... If the r 3 line in Fig. 2 is extrapolatedfrom 20 to 25 pc, the detections should increase to 20

14 Dec 2006: 2004).These two stars are 10–20 Myr old (see Favata et al. ... 1 AU) while (sub)mm surveys probe cold dust (20 K)distant from the star (100’s AU).