Unified Cloudy Models of M, L, and T Dwarfs ver.2 23 July 2014 T. Tsuji 1. Revisions in ver.2 vs. ver.1: 1) The grid is extended to the two chemical compositions, one is based on the classical solar C & O abundances (Ref.1), and the other based on the downward revised solar C & O abundances (Ref.2) as in ver.1. 2) We assume an average collision half-width of gamma0 = 0.08 cm-1/atm at T = 296 K for all the transitions of all the molecules. Although this value is by no means well established for the collision-partners (e.g, H2, He, H) at elevaled temperatures of stellar photospheres (Ref.3), this value was assumed to be too large (gamma0 = 0.32 cm-1/atm) in ver.1. 3) We replaced the H2O line-list based on Ref.4 in ver.1 by the new one based on BT2 (Ref.5) - HITEMP2010 (Ref.6). 4) We use the line list of CH4 kindly made available by Richard Freedman (2005 version) for lambda > 1.9 micron and the band model opacity for lambda < 1.9 micron for the reason noted in the "Note added in proofs" of Ref.7. 2. This directory "ucm2" consists of the following sub-directories: The sub-directory "tables" includes: case_a.dat: chemical composition based on the classical solar C & O abundances (Ref.1) case_c.dat: chemical composition based on the downward revised solar C & O abundances (Ref.2) The following sub-directories are based on the classical solar C & O abundances (case_a.dat) Ca45 : Tcr = Tcond (case C), log g = 4.5, Teff = 800 - 4000K 475 : 4.75, Teff = 2600 - 4000K 50 : 5.0, Teff = 800 - 4000K 525 : 5.25, Teff = 2600 - 4000K 55 : 5.5, Teff = 800 - 4000K T17a45 : Tcr = 1700K, log g = 4.5, Teff = 800 - 2600K 50 : 5.0, Teff = 800 - 2600K 55 : 5.5, Teff = 800 - 2600K T18a45 : Tcr = 1800K, log g = 4.5, Teff = 800 - 2600K 50 : 5.0, Teff = 800 - 2600K 55 : 5.5, Teff = 800 - 2600K T19a45 : Tcr = 1900K, log g = 4.5, Teff = 800 - 2600K 50 : 5.0, Teff = 800 - 2600K 55 : 5.5, Teff = 800 - 2600K The following sub-directories are based on the downward revised solar C & O abundances (case_c.dat) Bc50 : Tcr = T0 (case B), log g = 5.0, Teff = 1000 - 2600K Cc45 : Tcr = Tcond (case C), log g = 4.5, Teff = 700 - 4000K 475 : 4.75, Teff = 2600 - 4000K 50 : 5.0, Teff = 700 - 4000K 525 : 5.25, Teff = 2600 - 4000K 55 : 5.5, Teff = 700 - 4000K T17c45 : Tcr = 1700K, log g = 4.5, Teff = 700 - 2600K 50 : 5.0, Teff = 700 - 2600K 55 : 5.5, Teff = 700 - 2600K T18c45 : Tcr = 1800K, log g = 4.5, Teff = 700 - 2600K 50 : 5.0, Teff = 700 - 2600K 55 : 5.5, Teff = 700 - 2600K T19c45 : Tcr = 1900K, log g = 4.5, Teff = 700 - 2600K 50 : 5.0, Teff = 700 - 2600K 55 : 5.5, Teff = 700 - 2600K where "a" and "c" (e.g. Ca45, T19c55 etc.) indicate that the chemical composition assumed are as in case_a.dat (Ref.1) and case_c.dat (Ref.2), respectively. (Vmicro = 1 km/s throughout and not explicitly shown). Tcr and Tcond are the critical temperature where dust clouds disappear and the condensation temperature where dust forms (as for detail, see Refs.7 & 8), respectively. T0 is the surface temperature. 3. Each sub-directory consists of sub-subdirectories: str: model photospheres in radiative-convective equilibrium. We hoped that the flux constancy can be attained within 1 % error, but this constraint was not necessarily met especilally at the layers where dust clouds appear or convection sets in as can be checked by the plots of total fluxes (see the "plt" below). ceq: abundances of the molecules (log P_mol) and dust species (log P_dust as defined in ref.2), to be used for the evaluation of opacities. The values given are for the strict thermal equilibrium; i.e. dust abundances are given for all the layers in which T < Tcond (and hence in which T < Tcr), while dust should be considered as sources of opacity only in the layers Tcr < T < Tcond in the UCMs. For example, dust abundances are given even for case C, in which these dust species were not considered as sources of opacity at all. For any application (e.g. to evaluate synthetic spectra), dust abundances should be reduced to null in all the layers with T < Tcr (e.g., this is to be done by considering dust opacities only in the layers with Tcr < T < Tcond, in a subroutine to compute opacities). bmf: emergent fluxes (SED; 0.2 - 46 micron) based on the band model opacities (Ref.8). These are the direct result of the iterative model constructions and not for detailed comparison with observed data (for an assessment of bmf, compare it with sed based on the detailed high resolution spectra - lrs). Ff(C) and Fwl(C) are the continuum fluxes including the effect of dust and quasi- continuous opacity sources due to H2 CIA & KI, NaI lines. lrs: low resolution spectra (FWHM = 500km/s, 0.8 - 2.6 micron) & based on the high resolution spectra (with a resolution of 0.1cm-1) computed with the line lists except for CH4 in lambda < 1.9 micron. sed: spectral energy distributions (SED; 0.8 - 2.6 micron) based on the high resolution spectra computed with the opacities as for lrs. Ff(C) & Fwl(C) are the continuum fluxes including the effect of dust and quasi-continuous opacity sources due to H2 CIA (but KI and NaI lines are not included). plt: plots of some results for verification and quick look. For case C, early (Teff = 2700 - 4000 K) and late (Teff = 700/800 - 2600 K) types are in separate files, e.g., Ca50E,pdf and Ca50L.pdf. In each plot: upper left.....blue : total flux red : radiative flux green : convective flux lower left.....blue : Tem - logTAU0 of the final model sky : condensation temperature of corundum red : condensation temperature of iron green : condensation temperature of enstatite upper right....blue : low resolution spectra (lrs) based on line-list red : black-body for T = Teff lower right....green : SED by the band model opacities (bmf) yellow : line-free continuum flux red : black-body for T = Teff 4. Each data file in the sub-subdirectory is identified by Tcr, chemical composition, Teff and log g; e.g., T18c1800c50, where T18, c, 1800, and 50 imply Tcr = 1800K, chemical composition of case c, Teff = 1800K, and log g=5.0. The "c" between 1800 and 50 distinguishes convective from radiative model. The value of V_micro (assumed to be 1.0 km/sec throughout) is not explicitly shown on each file name. For models for which fine integration step of 0.05 is used instead of 0.1 in logTAU0 (see Refs.7-8), "f" is attached to the fine name; e.g., T18c1000fc50. 5. References: 1) Anders, E., & Grevesse, N. 1989, Geochim. Cosmochem. Acta, 53, 197 Grevesse, N. et al. 1991, A&A, 242, 488 2) Allende Prieto, C., Lambert, D. L., & Asplund, M. 2002, ApJ, 573, L137 3) Tsuji, T., & Nakajima, T. 2014, PASJ in press (ArXiv.1407.5829 in astro-ph.SR) 4) Partidge, H., & Schwenke, D. W. 1997, J. Chem. Phys., 106, 4618 5) Barber, R. J., Tennyson, J., Harris, G. J., & Tolchenov, R. N. 2006, MNRAS, 368, 1087 6) Rothman, L. S., et al. 2010, JQSRT, 111, 2139 7) Tsuji, T. 2005, ApJ, 621, 1033 8) Tsuji, T. 2002, ApJ, 575, 264 6. Contact address: Takashi Tsuji Institute of Astronomy The University of Tokyo 2-21-1 Osawa, Mitaka, Tokyo 181-0015 Japan e-mail: ttsuji@ioa.s.u-tokyo.ac.jp -----------------------------------