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https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_140122.txt
https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_140122.txt5 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 -
betapic-final
https://people.ast.cam.ac.uk/~wyatt/dwra14.pdf8 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 -
arX iv:1 312. 5315 v1 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/kwkd13.pdf21 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 -
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...
https://people.ast.cam.ac.uk/~wyatt/fwgb14.pdf31 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. -
TLA_large
https://people.ast.cam.ac.uk/~wyatt/tgmk14.pdf4 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. -
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...
https://people.ast.cam.ac.uk/~wyatt/sjvw14.pdf4 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). -
arX iv:1 403. 6186 v1 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/mmek14.pdf2 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. -
Constraining the Exozodiacal Luminosity Function of Main Sequence…
https://people.ast.cam.ac.uk/~wyatt/mmsc14.pdf18 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. -
arX iv:1 408. 4116 v1 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/kw14.pdf22 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 -
Observations, Modeling and Theory of Debris Disks Brenda C. ...
https://people.ast.cam.ac.uk/~wyatt/mkwb14.pdf7 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. -
arX iv:1 402. 1184 v1 [ astr o-ph .SR ...
https://people.ast.cam.ac.uk/~wyatt/dawk14.pdf10 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). -
arX iv:1 312. 4531 v2 [ astr o-ph .EP ...
https://people.ast.cam.ac.uk/~wyatt/kmlm13.pdf21 Jan 2014: Argon lamps were used for wave-length calibration. 24 images were taken with 1 second exposures. -
Mon. Not. R. Astron. Soc. 000, 1–22 (2013) Printed ...
https://people.ast.cam.ac.uk/~wyatt/jwbv14.pdf11 Mar 2014: which at 50AU from the Sun corresponds to σv/vk = 0.056,0.13, 0.27, 0.55, and 1.24. -
Five steps in the evolution from protoplanetary to debrisdisk ...
https://people.ast.cam.ac.uk/~wyatt/wpkm15.pdf17 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 -
Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed ...
https://people.ast.cam.ac.uk/~wyatt/mpwd15.pdf10 Dec 2014: 11 and 12) is solved to obtain fractional pop-ulations xj for all levels up to jmax=24. -
Mon. Not. R. Astron. Soc. 000, 1–22 (2002) Printed ...
https://people.ast.cam.ac.uk/~wyatt/pw14.pdf2 Jul 2014: low inclination planets. a plt (. au). 24.8. 25.0. e plt. -
Irwin06draft.dvi
https://people.ast.cam.ac.uk/~wfcam/ukreview/Irwin06draft.pdf23 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 -
mn.dvi
https://people.ast.cam.ac.uk/~wyatt/wfpb14.pdf23 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.
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