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7 Jul 2012: Also shown is the sensitivity with MIPS at 24 and 70µm to55 Cancri, a typical nearby star at 12pc withKs 4.2 (grey lines).

12 Jan 2012: 8 arcminaway to the SE (PA = 120) that is visible at 24, 70, and100µm.

29 Jun 2012: However, progress will be difficult.Table 3 inJewitt & Haghighipour(2007) shows that the faintestknown irregulars at Saturn have R magnitudes of 24.5,3 and thedeepest survey for Uranian irregulars had ... 3 The faintest published survey hasR = 24.5

1 Aug 2012: edu. Received 2008 November 24; accepted 2009 June 16; published 2009 August 7. ... This agrees well with the200 K temperature of the large, cool grain dust grains fromthis work, and with Wyatt et al.’s (2007b) Spitzer 24/70 μmbased estimate of 4–5

24 Nov 2012: Finally, we used the SPIRE 3σ upper limits as a constraint toreject any model with a flux density of the dust emission largerthan 24 mJy at 250µm. ... The upper inset zooms on the IRS wavelengths and displays spectra asSν(λ/24)2 on a linear scale

23 Feb 2012: Gyr), and its excess emission at 24 μm lieswell outside the range defined by most stars of its age (Figure 1;Wyatt 2008). ... The median S/N of the SL data is 24 and of theSH/LH data is 37.

19 Jan 2012: 0 2 4 6 8 10 12 14 16 18 20 22 24 26 28 300.0.

24 Feb 2012: Mon. Not. R. Astron. Soc. 000, 1–22 (2011) Printed 24 February 2012 (MN LATEX style file v2.2).

30 Oct 2012: 2009), with q 24 au and a 796 au, and 2000 OO67 (Veillet, Doressoundiram &. Marsden 2001; Millis et al. 2002), with q 21 au and a 552 au.The perihelia and

7 Nov 2012: 24.8 2,14.8 1 arcsec, 75 4.5 at 160 μm. ... Photometry on the 24 μm image was used in the spectral energydistribution (SED) modelling.