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19 Feb 2003: data/cass36h/wfc_nonsurvey/watson_jul2000_reduced/:Y:Y:Y:S:S:S:S:0.080/0.004/0.016/17:a href=./lplogs/20000725.int:: ... Y:Y /data/cass36h/wfc_nonsurvey/watson_jul2000_reduced/:Y:Y:Y:S:S:S:S:0.095/0.005/0.022/18:a href=./lplogs/20000726.int::

10 Jul 2024: Sefilian A. A., Rafikov R., Wyatt M. C. 2023, ApJ, 954, 100. ... Sefilian A. A., Rafikov R., Wyatt M. C. 2021, ApJ, 910, 13.

12 Oct 2021: The survey observational results. A&A, 555:A11, 2013. [24] S. Ertel, O. ... H. Chen, A. Morlok, D. M. Watson, P. Manoj, P. Sheehan, T.

2 Jul 2010: Since, as noted before, a sensible observing sequence precludes it being a problem. ... There has been a further shrinkage of staff at UKIRT. Tom Kerr is now our main contact with Watson the other UKIRT contact.

28 Sep 2009: MJI is in communication with Watson Varricatt regarding the low light level non-linearity tests and also a revisit of the normal non-linearity tests. ... Watson and MJI will also be comparing dome flats with twilight sky flats.

22 May 2012: REFERENCES. Absil, O., di Folco, E., Mérand, A., et al. 2006, A&A, 452, 237. ... H., Sheehan, P., Watson, D. M., Manoj, P., & Najita, J.

22 Feb 2011: odd spatial effects they were finding in a few tiles (saved us looking). ... Finally we note that Watson Varricatt took over from Chris Davis a few months ago as the official contact person for all matters relating to WFCAM data processing.

4 Sep 2012: The extra history records and the "CU8" were a bit of a giveaway. ... Watson Varricat came up with an interesting problem relating to WFCAM and crowded field photometry, e.g.

22 Aug 2010: This was then subtracted from the final. image to ensure a flat background. ... 2006), compared to a belt at 55AU with a width of50AU for HD191089.

24 Nov 2023: Top pair: SN2008bkin the Scd spiral NGC7793 at a distance of 4 Mpc. ... Watson, E. Westra, T. Wold & C. WolfNature 461, 1254-1257(29 October 2009)doi:10.1038/nature08459.

18 Sep 2007: assumingF /F p 0.1disk a limit of , based on Su et al. ... 3. Stellar multiplicity.—With 50% of target stars havinganother star as a companion.

8 Jan 2019: a sharp outer edge, similar to the morphology seen byHST (Golimowski et al. ... 2. One way of describingthis is to define Σr(a) = n(a)/(2πa), where a = a(r, φ) andΣr(a) is the surface density that would have resulted fromthe given

7 Jul 2012: Previous effortsfor theHerschel (Pilbratt et al. 2010) Disc Emission via a Bias-free. ... A total of 144655sources have a WISE detection in at least one band.

6 Apr 2010: possibilitiesinclude dynamical scattering by a migrating planet, see e.g.Gomes et al. ... This source together with HD 31295 andHD 38206 are described in Appendix A.

19 Feb 2010: Weshow that there is no significant statistical difference between fractional excessesof A-stars. ... 5). We also assume that the central star acts like a black-body.

21 Jan 2014: a useful evolutionary sequence it is important to interpret in-dividual objects carefully. ... 4.8. Schneider et al. (2013)report a detection in the XMM-Newton Serendipitous Source Cat-alog (Watson et al.

25 Oct 2009: by postulating a populationof parent planetesimals on highly eccentric orbits (e 0.3). ... Rcc(Dmax) = KMtotv8/3k (a)a. 3(4πImax)1S(e), (16). S2d(e) =X. r̄. r̄2dr̄1σ̄(r̄)2〈[vrel/vk(a)]8/3〉(r̄), (17).

5 Jul 2011: Four 3’ scan legs wereperformed per map with a 2” separation between legs. ... 2008) and to a theoretical PSF (gen-. 2010 RAS, MNRAS 000, 1–20.

5 Oct 2007: within a massive comet or asteroid (processed, differentiated planetesimals) belt, (iv) recent col-. ... performed (Watson et al. 2004). The reduction and analysis of the spectra was conducted with.

23 Nov 2021: These instru-ments reveal a wealth of substructures within disks, forboth targeted (e.g. ... We assumehere a gas-to-dust mass ratio of 100 and indicate the.