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5 Mar 2014: the original Vega one based on ESO std fields observed each night APASSZPT= 24.147 / APASS ZP (mags) for default extinction APASSZRR= 0.012 / APASS ZP error (mags) APASSNUM= 104 / Number ... of APASS standards used NIGHTZPT= 24.155 / Average APASS ZP

8 Apr 2014: This was interpreted as a transition from a dust-‐producing planetesimal belt to a region dominated by submicron-‐sized grains blown out by radiation pressure (9,24). ... The dashed line is an axisymmetric model for the parent body distribution

4 Dec 2014: Consequently, we find that thedisc detection rates are: 21/86 = 24 5 per cent at 100 µm and15/86 = 17 4 per cent at 160 µm. ... Mi. HD. 8769. 6A. 7V28. 24. 450. UM. a(3. ,4). 22.0.

21 Jan 2014: The expected December 2010 source position of α = 22h 48m 4.7s,δ = 24 22m 9.9s is at the centre of the images, and the PACS pointing accuracy for these ... Figure 3 shows the limits on the fractional luminosity of adisc around TW PsA given these

31 Jul 2014: 16 and MIPS 24 µm photometry (Farihi et al. 2008; Reach et al.2005). ... µMIPS 24 mµIRAC 8 m. Figure 1. Reduced infrared images of G29-38 taken with both Spitzer and Herschel.

2 Jul 2014: 24 661 5566HD 33564 100/160 219019/20 705 720HD 39091 100/160 205212/13 502 576HD 40307 70/160 203666/67 471 180. ... 2012); (22)Bonfils et al. (2005); (23) Noyes et al. (1997); (24) Butler etal.

18 Oct 2014: at wavelengths of 24 µm or shorter (Beichman et al. 2006a; Lawler et al. ... In comparison, of the. 24 stars that have no cold excess, none show a KIN excess.

22 Aug 2014: 4-35µm), three MIPS(24-160µm), and two SCUBA (450-850µm) bands. ... 2014). However, plotting their tempera-tures shows a probable correlation, with all Sun-like starshav-ing warm components<220K, but 15 out of 24 A-type starshaving warm components>220K

7 Jan 2014: 2008) and Dodson-Robinson et al. (2011)find rates of 4% at 24 µm in contrast to 16% at 70µm (Trilling et al. ... 7. 10-24. 10-22. 10-20. 10-18. 10-16. 100. 101. 102. 103. 104.

4 Dec 2014: The Large Synoptic Survey Telescope (LSST) is ex-pected to detect objects to an apparent magnitude limitof m 24.5 (Moro-Mart́ın, Turner & Loeb 2009).

10 Feb 2014: IRS pick-up camera at 16 and 22 µm and the MIPS 24 µm photometry to establish the absolute. ... and 22 µm and MIPS 24 µm broadband fluxes (listed in Table 3).

21 Jan 2014: Argon lamps were used for wave-length calibration. 24 images were taken with 1 second exposures.

11 Mar 2014: which at 50AU from the Sun corresponds to σv/vk = 0.056,0.13, 0.27, 0.55, and 1.24.

17 Dec 2014: 2007).η Tel: The debris disk of this system was resolved. in the mid-IR at a radius of 24 au, but it was shownthat there is an additional unresolved component ... limits at just one wavelength (left-pointing for upper limits at 70 µmand down-pointing

23 Jul 2014: 1 -2.4 3.8 4.84 18.4#2 3.7 4.2 4.87 20.5#3 -9.0 4.2 5.80 24.4#4 49.1

2 Jul 2014: low inclination planets. a plt (. au). 24.8. 25.0. e plt.

10 Dec 2014: 11 and 12) is solved to obtain fractional pop-ulations xj for all levels up to jmax=24.

23 Jan 2014: Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 23 January 2014 (MN LATEX style file v2.2). Stochastic accretion of planetesimals onto white dwarfs:. constraints on the mass distribution of accreted material. from atmospheric pollution. M.