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21 - 30 of 65 search results for KaKaoTalk:po03 op |u:people.ast.cam.ac.uk where 0 match all words and 65 match some words.

  1. Results that match 1 of 2 words

  2. https://people.ast.cam.ac.uk/~vasily/data/TAP_1697550531535.vot

    https://people.ast.cam.ac.uk/~vasily/data/TAP_1697550531535.vot
    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

  3. SUBMILLIMETER IMAGES OF A DUSTY KUIPER BELT AROUND � ...

    https://people.ast.cam.ac.uk/~wyatt/wgdc05.pdf
    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.

  4. arX iv:1 312. 4531 v2 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kmlm13.pdf
    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

  5. MNRAS 000, 000–000 (2018) Preprint 21 February 2019 Compiled ...

    https://people.ast.cam.ac.uk/~wyatt/mphp19.pdf
    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

  6. Mon. Not. R. Astron. Soc. 000, 1–11 (2002) Printed ...

    https://people.ast.cam.ac.uk/~wyatt/pwk15.pdf
    9 Feb 2015: Golimowski D. A., Burrows C. J., Kulkarni S. R., Op-penheimer B.

  7. arX iv:1 412. 0675 v1 [ astr o-ph .EP ...

    https://people.ast.cam.ac.uk/~wyatt/kwbb14.pdf
    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.

  8. ����������� ��� ������������ ������� �!�"���…

    https://people.ast.cam.ac.uk/~wyatt/wyat05a.pdf
    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

  9. MNRAS 435, 1037–1046 (2013) doi:10.1093/mnras/stt1293Advance Access…

    https://people.ast.cam.ac.uk/~wyatt/phwk13.pdf
    12 Nov 2013: The work of OP, MCW and GMK is supported by the EuropeanUnion through ERC grant number 279973.

  10. MNRAS 000, 1–11 (2023) Preprint 31March 2023 Compiled…

    https://people.ast.cam.ac.uk/~wyatt/mmcb23.pdf
    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

  11. Publications of the Astronomical Society of Australia (PASA)doi:…

    https://people.ast.cam.ac.uk/~wyatt/khna21.pdf
    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

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