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29 Sep 2023: e) Derive an expression for the distance of the particle P from the geometric centre of the ellipse O, andhence show that to first order in eccentricity the distance OP is

16 Jun 2015: Op. tic. al. de. sig. n c. an. be. bro. ke.

13 Oct 2014: The full calculation of stellar opacities is a major endeavour. For this rea-son, the Opacity Project (op) was set-up in 1984 as an international collab-oration to calculate the ... Similar work conducted at the LawrenceLivermore National Laboratory, the

19 Apr 2006: "!# $&% ' )(# -,/.0-%12 &!$3542,67,98/:<;=?> @A>BDCFEGIHJ8K>L>MONPEQRCFSUTV8WX>YZ>L[GIEE]E[_7=?>Ya>bCFcXdGIHe_UNPEgfMhC[cA:QUeiPGkjEmlPG#QU_UmSn;opQqGI_U_#8rMhC[cX:Qq]iPG$st8vuFwPwPx>yopzV>|{-}8vuP{}Ic>yopQU]#GpPwgfT2C[Qqi:NPdEiV9bKhw{Pu&}&}P<As>.

16 Jun 2015: Look at the '.cl' files in home$wfirc/scripts for details. avgo n1 n2 chip op! ... imexam' cursor. To scale the skies to each other! use op = y dall n1 loop!

31 Jul 2018: JPL Publication. Lawson PR, Lay OP, Johnston KJ, Beichman CA (2007) Terrestrial PlanetFinder Interferometer Science Working Group Report. ... NASA STI/ReconTechnical Report N 8. Lay OP (2004) Systematic Errors in Nulling Interferometers.

10 Oct 2023: Magnitudes andluminosities are normally measured through a given filter; Figures 2.4 and2.5 show the transmission curves of some of the most commonly used op-tical and near-infrared filters.

16 Jun 2015: 2 FILTER7=Hn FILTER6=Jn FILTER5=Hl FILTER4=Hx FILTER3=Hs FILTER2=Jg FILTER1=Op FILTER0=Dk 13) Contact info, phone numbers, etc LCO during day this number is routed to

29 Apr 2008: We con-sider a detection to be whereS op > 3. 4.1.1. ... Ndθ = 0.1(dθ/θ)1010(r/θ)R0.5λ Ftot. with Nop andS op determined from equation 1.

16 Jun 2015: 2 FILTER7=Hn FILTER6=Jn FILTER5=Hl FILTER4=Hx FILTER3=Hs FILTER2=Jg FILTER1=Op FILTER0=Dk 13) Contact info, phone numbers, etc LCO during day this number is routed to

22 Mar 2024: For the clustering of data and to guide the interpretation, wealso extracted environmental data from either the adaptive op-tics telemetry3 or the Astronomical Site Monitor (ASM) of theCerro Paranal Observatory4. ... We found much lower correlation rates

26 Sep 2017: three disks. For HD 131488, even the 13CO line is op-. ... tically thick with an optical depth of 5.7, while for. HD 121191 and HD 121617 this line was found to be op-tically thin.

10 Nov 2016: With the advent of an extreme adaptive op-tics instrument like the Spectro-Polarimetric High-contrastExoplanet REsearch (SPHERE; Beuzit et al.

23 Dec 2016: It summarizes previous findings aswell as results from this work. EC acknowledges support from NASA through HubbleFellowship grant HST-HF2-51355 awarded by STScI, op-erated by AURA, Inc.

19 Apr 2006: "! $#&%(')! ,.-/%103246587797: 0<;=>&?%/3#60A@ B4%)CD0CEGFHI6KJ&0ML80ONPRQ8%S 4T0. UWVYXOZ [MV6]AXV_ba c&dfehgjiZ k.l<]m.XOV$c=nPo$Zpp.V6qUhal VC]rsZ qoftuvxw=y"z. {}|x|C) 9(A6Wf69O6AR.E&RAAA9E9 //.¡¢E£¤E(¥ª«¢¥ª<E4OP/GK=. |Y|&µEºA)»|&{f|

5 May 2017: The calculations sofar have focused on the geometrical optical depth of the op-tically thin dust, τ. ... edge. Such dust, how-ever, would produce a detectable infrared excess, as for op-tically thin discs, there is insufficient gas released for

17 Jan 2019: We can estimate a minimum CO mass by assuming that the CO emission is marginally op-.

19 Apr 2006: ApJ accepted, 7 November 2005Preprint typeset using LATEX style emulateapj v. 04/21/05. DUST IN RESONANT EXTRASOLAR KUIPER BELTS — GRAIN SIZE AND WAVELENGTH DEPENDENCEOF DISK STRUCTURE. M. C. Wyatt1. UK Astronomy Technology Centre, Royal

27 Jan 2016: 2014; Veillet et al. 2014). The LBT is locatedon Mount Graham in southeastern Arizona and is op-erated by an international collaboration among institu-tions in the United States, Italy, and ... The op-tics provide a field of view of 1010 arcsec2 with

12 Jan 2012: 2004), an adaptive op-tics image taken using the Lick Observatory Shane 3m tele-scope with the IRCAL near-IR camera as an ongoing search forfaint companions of stars in the ... To try and resolve this issue we obtained an adaptive op-tics image of 99 Her

19 Apr 2006: 4.2. Modelingg the SED. The spectral energy distribution (SED) of Corvi from op-tical to submillimeter wavelengths is plotted in Figure 4.

21 Jan 2014: However, this similarityrequires that both components are radially optically thickand op-tically thin in the viewing direction, or the opening anglesmust belarger. ... The length of this period is uncertain due to the possibilityof non-axisymmetry and an

17 Oct 2023: ARI's TAP access to the Gaia Archive. Unique source identifier (unique within a particular Data Release) Basis function coefficients for the BP spectrum representation Basis function coefficients for the RP spectrum representation

21 Feb 2019: Gas mass calculations based on opticallythick 12CO emission can lead to underestimations of as largeas two orders of magnitude in comparison to those using op-tically thin CO isotopologues (Moór et

15 Jan 2015: arX. iv:1. 412. 0675. v1 [. astr. o-ph. EP. ] 1. Dec. 201. 4DRAF T VERS IONDECEMBER 3, 2014Preprint typeset using LATEX style emulateapj v. 5/2/11. EXO-ZODI MODELLING FOR THE LARGE BINOCULAR TELESCOPE INTERFEROMETER. GRANT M. K ENNEDY1, M ARK C.

9 Feb 2015: Golimowski D. A., Burrows C. J., Kulkarni S. R., Op-penheimer B.

19 Apr 2006: " $#%&%&' ()" #$%%'-,.0/(12&34657798:";" =<>? @$$A$>;"? BC? ";D= ;" EF46 "9/ GHJI"K"KMLBNPOQ R9SOETUQ VFW"OXTMY!Z[QS W"OXW"]BV. GTMY_OXVFW"O. (a Nb?K"K&c K"K"K"KdUe(K"K"K"K"K"K"K"K"K"K"K"K"K"K"KMe. fhgji kmlon_pqnsr turwv xzy|{|}ns{|r {|wi}_. 6sJ

12 Nov 2013: The work of OP, MCW and GMK is supported by the EuropeanUnion through ERC grant number 279973.

31 Mar 2023: MNRAS 000, 1–11 (2023) Preprint 31March 2023 Compiled usingMNRASLATEXstyle file v3.0. Stirred but not shaken: a multi-wavelength view of HD 16743’s debris disc. JonathanP.Marshall,1,2 J.Milli,3 E.Choquet,4 C. delBurgo,5 G.M.Kennedy,6,7 F.Kemper,8

23 Nov 2021: The HD J = 2 1 line is stronger for low mass op-tically thin disks (1019 W m2) and fainter for opticallythick massive disks (1018 W m2).Since the line fluxes ... Due to the lower op-tical depth with respect to the main isotopologue, the13CO transitions

27 Jul 2010: The outcome is summarisedin Fig. 6. 4.4.1 Radiation pressure. Radiation pressure is a radial force which acts in the op-posite direction to the star’s gravity.

8 Jul 2020: Finally, the detection of this gas is also a new op-portunity to study mechanisms that can transport angularmomentum in discs and may be beneficial for our under-standing of the ... We also compute CN masses in non-LTE assuming op-tically thin emission

17 Jan 2020: Evidence of misaligned inner discs has also beenrecently inferred for several systems using high-contrast op-tical/infrared images, which have revealed shadows in theouter disc cast by unseen inclined inner

14 Sep 2015: map reproduces the input op-tical depths very closely.

3 Nov 2008: arX. iv:0. 810. 5087. v1 [. astr. o-ph. ] 28. Oct. 200. 8Astronomy & Astrophysicsmanuscript no. 10706 c ESO 2008October 28, 2008. Resolved debris disk emission around η Tel: a young Solar Systemor ongoing planet formation? R. Smith1, L.J. Churcher1,

23 Sep 2016: before through modelling observations of op-tical and near-IR scattered light from the dust disk (e.g.Ahmic et al.

23 Aug 2018: 2017, Fig. A1, bottom). The high op-tical depth in the mid-plane would in fact shield the smallgrains from sublimation.

8 Nov 2011: It is interesting to note that the op-timum position for the inner planet is not as close to thestar as the outer planet could possibly scatter particles

19 Apr 2006: To probe the nature of the Vega disk further, wehave fitted it with models including realistic grain op-tical properties.

2 Nov 2015: Road, Cambridge, UK9 Department of Astronomy, Yale University, New Haven, CT10 Visiting Astronomer, NASA Infrared Telescope Facility, op-.

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

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,.