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1 - 10 of 19 search results for katalk:za33 24 |u:people.ast.cam.ac.uk where 0 match all words and 19 match some words.
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  2. https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_140122.txt

    https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_140122.txt
    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
  3. betapic-final

    https://people.ast.cam.ac.uk/~wyatt/dwra14.pdf
    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. arX iv:1 312. 5315 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kwkd13.pdf
    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
  5. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/fwgb14.pdf
    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.
  6. TLA_large

    https://people.ast.cam.ac.uk/~wyatt/tgmk14.pdf
    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.
  7. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/sjvw14.pdf
    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).
  8. arX iv:1 403. 6186 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/mmek14.pdf
    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.
  9. arX iv:1 408. 4116 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kw14.pdf
    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
  10. Constraining the Exozodiacal Luminosity Function of Main Sequence…

    https://people.ast.cam.ac.uk/~wyatt/mmsc14.pdf
    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.
  11. Observations, Modeling and Theory of Debris Disks Brenda C. ...

    https://people.ast.cam.ac.uk/~wyatt/mkwb14.pdf
    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.

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