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3 Jun 2011: 200.76777495 3.7214707 25.29 24.61 23.14 23.00 19.97 4 140.21862225 30.4611002 23.07 23.08 22.58 20.84 19.00 5 ... 85138 51.536387 24.02 23.72 23.09 21.47 20.74.

23 Feb 2011: Also plotted are the detection limits at both 24 and70µm, given by Eq. ... Older disks must therefore have larger radii tobe detected at both 24 and 70µm.

5 Jul 2011: The MICHELLE fieldof view is 32”24”, but the chop throw of 15” limits the usableregion. ... The MIPS 24 µm image is shownin the first panel of Figure 3.

8 Nov 2011: arX. iv:s. ubm. it/03. 5390. 2 [. astr. o-ph. EP]. 8 N. ov 2. 011. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 8 November 2011 (MN LATEX style file v2.2). The scattering of small bodies in planetary systems:. constraints on the possible

28 Mar 2011: αa = (7 a/3)/(2 a/3), (24). in the strength regime and αb = α given by equation (14) in the gravity regime.

16 Nov 2011: 0 values of fbif if Ψbif < Ψbif,fmin (24). 1 value of fbif if Ψbif = Ψbif,fmin (25). ... fbif which satisfy Eq. (22). Figure 6 demonstrates Eqs.(24)-(26) graphically by plotting Ψbif vs.

5 Apr 2011: 2009; Carpenter et al. 2009). A stars havea significantly higher fraction of dust excesses at both 24 and70µm and the excesses themselves are brighter than for FGKstars but the dust lifetime ... These values are broadly consistentwith the fluxes