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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.

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

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

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

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

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,.

18 Jan 2018: arX. iv:1. 801. 0542. 9v1. [as. tro-. ph.E. P] 1. 6 Ja. n 20. 18Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 18 January 2018 (MN LATEX style file v2.2). ALMA observations of the narrow HR 4796A debris ring. Grant M. Kennedy1, Sebastian

2 Dec 2021: MNRAS 000, 1–23 (2021) Preprint 1December 2021 Compiled usingMNRASLATEXstyle file v3.0. Comet fragmentation as a source of the zodiacal cloud. JessicaK.Rigley,1 MarkC.Wyatt,11Institute of Astronomy, University of Cambridge, Madingley Road,

28 Sep 2006: The low sensitivityof most optical CCD detectors at 1 µm, coupled with therelatively bright sky-background curtailed interest from op-tical astronomers.

24 May 2022: DRAFT VERSION MAY 24, 2022Typeset using LATEX twocolumn style in AASTeX62. The JWST Early Release Science Program for the Direct Imaging & Spectroscopyof Exoplanetary Systems. Sasha Hinkley ,1 Aarynn L. Carter ,2 Shrishmoy Ray ,1 Andrew Skemer,2

16 Jul 2021: MNRAS 000, 1–23 (2020) Preprint 14 June 2021 Compiled usingMNRASLATEXstyle file v3.0. High resolution ALMA and HST images of q1 Eri: an asymmetricdebris disc with an eccentric Jupiter. J. B. Lovell1, S.Marino1,2,M.C.Wyatt1,

22 Nov 2018: Mon. Not. R. Astron. Soc. 000, 1–23 (2002) Printed 22 November 2018 (MN LATEX style file v2.2). Imaging [CI] around HD 131835: reinterpreting youngdebris discs with protoplanetary disc levels of CO gas asshielded secondary discs. Quentin Kral,1,2?

2 Apr 2018: arX. iv:1. 803. 1126. 5v1. [as. tro-. ph.S. R]. 29. Mar. 201. 8Draft version April 2, 2018. Typeset using LATEX twocolumn style in AASTeX61. THE HOSTS SURVEY – EXOZODIACAL DUST MEASUREMENTS FOR 30 STARS. Ertel, S.,1 Defrère, D.,2 Hinz, P.,1

26 Sep 2005: The low sensitivityof most optical CCD detectors at 1 µm, coupled with therelatively bright sky-background curtailed interest from op-tical astronomers.

2 Jul 2014: yielding the ratio of the total cross-sectional area on op-posing sides of the disc.

30 Jan 2020: MNRAS 000, 1–22 (2019) Preprint 30 January 2020 Compiled using MNRAS LATEX style file v3.0. Population synthesis of exocometary gas around A stars. S. Marino1?, M. Flock1, Th. Henning1, Q. Kral2, L. Matrà3 and M. C. Wyatt41Max Planck Institute

14 Jun 2018: Note that the derivation above has only accounted for the op-tical depth along the line of sight from the star to the dust.