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5 May 2017: Table 2. NLTE calculations of CO masses from observations (op-tically thin assumption). ... FIRS (10m) CII (158µm) 1.5 1021OI (63µm) 1.5 1021. compute the column density N of CO needed to become op-tically thick.

2 Jan 2018: Draft version January 1, 2018Typeset using LATEX twocolumn style in AASTeX61. MOLECULAR RECONNAISSANCE OF THE β PICTORIS GAS DISK WITH THE SMA:. A LOW HCN/(COCO2) OUTGASSING RATIO AND PREDICTIONS FOR FUTURE SURVEYS. L. Matrà,1, D. J. Wilner,1 K.

19 Apr 2006: 10 µm) to spiral inwards toward the star.Which of these two effects is dominant depends on the op-tical depth of the dust disk, but for all but the most

9 Oct 2012: arX. iv:1. 208. 1759. v1 [. astr. o-ph. EP. ] 8. Aug. 201. 2Mon. Not. R. Astron. Soc.000, 000–000 (0000) Printed 10 August 2012 (MN LATEX style file v2.2). Coplanar circumbinary debris disks. G. M. Kennedy1, M. C. Wyatt1, B. Sibthorpe2, N. M.

7 Jun 2016: Mon. Not. R. Astron. Soc. 000, 1–16 (2002) Printed 7 June 2016 (MN LATEX style file v2.2). A self-consistent model for the evolution of the gasproduced in the debris disc of β Pictoris. Q. Kral?, M. Wyatt, R. F. Carswell, J. E. Pringle, L. Matrà

17 Dec 2014: Thus the dividingline is usually placed at f 0.01, which is around thelevel at which the dust might be expected to become op-tically thin in the radial direction to

30 Jul 2018: MNRAS 000, 1–23 (2015) Preprint 30 July 2018 Compiled using MNRAS LATEX style file v3.0. Using warm dust to constrain unseen planets. Amy Bonsor1, Mark C. Wyatt1, Quentin Kral1, Grant Kennedy2,3, Andrew. Shannon4,5 and Steve Ertel61Institute of

8 Jul 2008: There are too many uncertaintiesregarding the expected size distribution at very small sizes (e.g., because itdepends on the size distribution created in collisions), and regarding the op-tical properties of

28 Sep 2006: arX. iv:a. stro. -ph/. 0603. 608. v2. 1 Se. p 20. 06. Mon. Not. R. Astron. Soc. 000, 1–26 (2006) Printed 4 September 2006 (MN LATEX style file v2.2). The UKIRT Infrared Deep Sky Survey Early Data Release. S. Dye1, S. J. Warren2, N. C. Hambly3, N.

23 Jul 2014: Mon. Not. R. Astron. Soc. 000, 1–26 (2006) Printed 15 May 2013 (MN LATEX style file v2.2). Pipeline processing of wide-field near-infrared data fromWFCAM (draft - not for circulation). Mike Irwin1, Jim Lewis1, Marco Riello1, Simon Hodgkin1,.