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Mon. Not. R. Astron. Soc. 000, 1–23 (2012) Printed ...
https://people.ast.cam.ac.uk/~wyatt/jw12.pdf19 Jun 2012: Byconsidering the luminosity of dust produced in collisions within the boulder-debris distributionwe find that the Moon-forming impact would have been readily detectable around other stars inSpitzer 24 µm surveys -
Observing Kepler stars with WISE
https://people.ast.cam.ac.uk/~wyatt/kw12.pdf7 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). -
arX iv:1 201. 1911 v1 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/kwsd12.pdf12 Jan 2012: 8 arcminaway to the SE (PA = 120) that is visible at 24, 70, and100µm. -
Searching for Saturn's Irregular Satellite Swarm with Spitzer
https://people.ast.cam.ac.uk/~wyatt/kwss11.pdf29 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 -
The Astrophysical Journal, 701:2019–2032, 2009 August 20…
https://people.ast.cam.ac.uk/~wyatt/lcwm09.pdf1 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 -
arX iv:1 211. 4898 v1 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/lmsk12.pdf24 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 -
ApJ409619o.dvi
https://people.ast.cam.ac.uk/~wyatt/lwcm11.pdf23 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. -
arX iv:1 201. 3622 v1 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/ramb12.pdf19 Jan 2012: 0 2 4 6 8 10 12 14 16 18 20 22 24 26 28 300.0. -
midi_terr_sub3_nobold.dvi
https://people.ast.cam.ac.uk/~wyatt/swh12.pdf24 Feb 2012: Mon. Not. R. Astron. Soc. 000, 1–22 (2011) Printed 24 February 2012 (MN LATEX style file v2.2). -
mnr_20522_LR
https://people.ast.cam.ac.uk/~wyatt/vw12.pdf30 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
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