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1 - 10 of 23 search results for KaKaoTalk:PC53 24 / |u:people.ast.cam.ac.uk where 0 match all words and 23 match some words.

  1. Results that match 1 of 2 words

  2. Draft version December 10, 2012Preprint typeset using LATEX style ...

    https://people.ast.cam.ac.uk/~wyatt/bmkb12.pdf
    10 Dec 2012: There isboth cool dust (observable to Herschel) and warm dust(evident from IRS and MIPS 24 excesses). ... In the context of the wide belt imaging model, the IRSand MIPS 24 excesses are attributed to a warm innerring.

  3. https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_120926.txt

    https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_120926.txt
    5 Dec 2012: The one in question is at http://www.eso.org/sci/facilities/paranal/instruments/vircam/news.html and shows it was 2010-04-24/2010-05-06.

  4. https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_121031.txt

    https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_121031.txt
    5 Dec 2012: wrong end time and date for an OB. An example of the latter is below 2012-08-24 VIS 179.A-2010(F) 812323 0.00 A

  5. arX iv:1 211. 4898 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/lmsk12.pdf
    24 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

  6. mnr_21298_LR

    https://people.ast.cam.ac.uk/~wyatt/wksm12.pdf
    7 Nov 2012: 24.8 2,14.8 1 arcsec, 75 4.5 at 160 μm. ... Photometry on the 24 μm image was used in the spectral energydistribution (SED) modelling.

  7. mnr_20522_LR

    https://people.ast.cam.ac.uk/~wyatt/vw12.pdf
    30 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

  8. 1 A SELF-CONSISTENT MODEL OF THE CIRCUMSTELLAR DEBRIS CREATED ...

    https://people.ast.cam.ac.uk/~wyatt/jlcm12.pdf
    23 Oct 2012: which could be readily detectable around other stars by Spitzer 24 μm surveys for 25 Myr after. ... SiO h (24). which occurs with a rate coefficient m3 s-1 (Andreazza et al.

  9. Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/bksm12.pdf
    5 Oct 2012: β Uma PACS 70/160 1342220802/3 2011-04-29. PACS 100/160 1342197015/6 2010-05-24. SPIRE 1342195687 2010-04-29. ... PSF fit500 4.24.9 0.420.01 3.84.9 PSF fit.

  10. https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_120430.txt

    https://people.ast.cam.ac.uk/~wfcam/docs/minutes/minutes_120430.txt
    24 Aug 2012: transfer over the Internet some 24 hours later.

  11. The Astrophysical Journal, 701:2019–2032, 2009 August 20…

    https://people.ast.cam.ac.uk/~wyatt/lcwm09.pdf
    1 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

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