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6 Jan 2006: We analyse photometry of the UKIRT faint standardsmeasured on 20 photometric nights.

19 Apr 2006: B-! &-. n u= K G %'. Í 20 10 0 -10 -20RA offset, arcsec. ... $9]! ;9:<8 - P7-& (;! (<$ra A ;{' <9];& C#20% '-&- P (--##; 0B#-3 3;,x,- )/5[?

19 Apr 2006: b) Logarithmic10.8 km levels : 1.3, 1.9, 2.8, 4.2, 6.2, 9.2, 13.7, 20.2, 29.9, 44.3, and 65.5. ... The residual emission (observed minus model ; Fig.4d) at 20 AU from the star is typically 0.2 times that of(0A.3)the lobes.

19 Apr 2006: from the disk at 160 µm (within the 1-σ contour) is 4Jy 20%. ... At 20 Å, the heating timescale has lengthenedso that larger temperature fluctuations are observed andthe temperature distribution of the grain has a significanthot tail.

19 Apr 2006: In the two older systems, BD 20 307and HD 69830, this excess is almost entirely silicate emis-sion from small grains. ... statistics suggest a cold debris disk fre-quency of 10–20 % surrounding sun–like stars with a weakdependence on stellar age (Fig.

19 Apr 2006: 103 3 20 10 6HD109573 HR4796 A0V 67 0.005 4 8 2 9. ... HD141569 0.0 10.3 2.0 55.0 2.30.5 0.0 20.1 1.9 84 40.9 0.0 99.5 2.4 114 50.5

28 Sep 2006: 1868 K 3 19.0300 H2 3. Z 1 20.4Y 1 20.3. ... centre with aFWHM of 20′′, and truncated at a maximum offset of 2′.

2 Nov 2006: expect for a belt of a given age, given its radial loca-tion (equations 15-20). ... 3 Substituting in these nominal val-ues into equation (20) and approximating M? =

19 Apr 2006: Arc. seco. nds. 20 0 -20R.A. offset, arcsec. -20. 0. 20.

28 Nov 2006: Typicaldistances range from 10 to 20 pc, closer for M and K stars andfarther for earlier spectral types. ... Stellar fluxes are measured within an aperture of 10 pixels(=1200), with a background annulus from 10 to 20 pixels.