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14 Apr 2014: J012417-374423 1 6288.800 6290.060 vsig=2.810. J012417-374423 1 5344.700 5346.300 vsig=2.810. J012417-374423 1 5326.200 5327.610 vsig=2.810.

10 Feb 2014: 2005). All three sources have SEDs. that peak at a wavelength of 200–300 µm, typical of high-redshift, dust-rich galaxies.

31 Jul 2014: Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 31 July 2014 (MN LATEX style file v2.2). ALMA and Herschel Observations of the Prototype Dustyand Polluted White Dwarf G29-38. J. Farihi1,2?†, M. C. Wyatt2, J. S. Greaves3, A. Bonsor4,5, B.

21 Jan 2014: 100 50 0 50 100 150X [pc]. 200. 150. 100. ... 100. 50. 0. 50Z. [p. c]. 200 150 100 50 0 50Y [pc].

22 Aug 2014: 2/2 as our like-lihood function. Chains with an ensemble of 200 “walkers” areinitialised with parameters that vary randomly1% from theχ2 fitting results, and then run for 50 steps as ... 6 shows that a typical warmcomponent would haveTwarm = 200

7 Jan 2014: Within the FEPS sample, the rate of 24 µm excessis markedly higher (15%) for stars with ages < 300 Myr,compared to 2.7% at > 200 Myr (Carpenter et al. ... Blowout limit. 10-9. 10-8. 10-7. 10-6. 10-5. 10-4. 10-3. 80 100 140 200 300.

18 Oct 2014: a) inside of the 6 mas KIN inner working angle (IWA), defined as the half transmission point at 10 µm -,. or (b) outside of its ' 200 mas outer working angle (OWA), ... zodi levels, exhibiting significantly more stars in the 200 to 400 zodi level bin

10 Dec 2014: We selected a 200-channels wide(85 km/s) spectral window around the CO line, expected at345.789 GHz (vhel=6.5 0.5 km/s, Gontcharov 2006).

2 Jul 2014: 200. 20. y (a. u). 100. 50. 0. 50. 100. ... Normalised surface density0.0 0.5 1.0. z (au. ) 200. 20. y (a.

2 Jul 2014: The decrease in C’s eccentricity between 200 and350 Myrs is not caused by Galactic tides; rather it is caused by sec-ular interactions between B and C. ... 0. 50. 100. 150. 200. 250. 300. 350. 1e06 1e05 0.0001 0.001 0.01 0.1 1.