Directory 'deirm' contains the tables of dust phase functions, opacities, temperatures, and radiative accelerations of dust grains. They are described in more detail in Budaj, J., Kocifaj, M., Salmeron, R., \& Hubeny I. 2015, MNRAS, 454, 2-27 Basic assumptions are homogeneous spherical particles and Deirmendjian (1964) particle size distribution. An output is in the form of four separate files for each dust species. For example: iron_opac_all, iron_phase_all, iron_temp, iron_radacc Results are calculated for a grid of: different species, 21 modal particle radii (0.01-100 mic), 400 wavelengths (0.2-500 mic), apart from that phase functions are for 65-angles (0-180 deg), and grain equlibrium temperatures for 13 effective temperatures of the irradiating object (700-7000K) and 15 solid angles <2pi,1e-6> subtended by the star / brown dwarf. iron_opac_all contains several blocks. Each block referes to a particulal modal particle radius $r_{c}$. It has five columns: $\log(r_{c})$ in micron (logarithm with the base 10) , wavelength in micron, scattering opacity and absorption opacity in $cm^2/g$ where per gram means per gram of iron dust, and the mean cosine of the phase function. iron_phase_all contains several blocks. Each block starts with $\log(r_{c})$ in micron and refers to a particular modal radius. Each block has several sub-blocks, which apply to a certain frequency and are preceded with its value in Hz, the mean cosine value, scattering and absorption opacities in $cm^2/g$ where per gram means per gram of iron condesates. Each sub-block has two columns: phase angle in degrees and phase function normalized to $4 \pi$. iron_temp contains several blocks. Each block is for a particular temperature of the star and modal particle radius. There are four columns: stellar effective temperature [K], base 10 logarithm of mode particle radius [micron], solid angle subtended by the star [sr], and grain equilibrium temperature [K]. Note that, because of the long wavelength opacity cut-off, dust temperatures which are less than about 30K are not reliable (for ammonia less than about 60K). iron_radacc contains radiative to gravity acceleration ration, $\beta$, (3-rd column, dimensionles) as a fuction of the particle size ($\log(r_{c})$ in micron, 2-nd column) and the stellar effective temperature (in Kelvin, 1-st column). It assumes that mass and radius of the irradiating object are M_sol, R_sol, respectively. User has to adjust it accordingly: beta_user= beta*(R^2/R_sol^2)*(M_sol/M) Opacities were set to zero and the phase functions to one in the wavelength regions where the refraction index measurements were not available. Equilibrium grain temperatures which are below about 30-60 K are not reliable (see the manuscript for detailes). Apart from that there is a directory 'diskaver' which contains a code DISKAVER.F90 in Fortran90 which reads the phase function tables and calculates the disk-averaged phase functions to take into account a finite dimension of the source of light. Jan Budaj Dec. 9, 2013, Mt. Stromlo budaj@ta3.sk References to n,k measurements: species lambda[mic] ref.code ----------------------------------- alumina 0.2-400 K corundum 6.7-1e4 Z perovskite 2.0-5843 P iron 0.19-1.9 J\&C iron 0.62-286 O forsterite 0.20-949 J03 olivine50 0.20-500 D enstatite 0.20-500 D pyroxene20 0.20-500 D pyroxene60 0.20-500 D carbon1000C 0.20-794 J98 carbon0400C 0.20-518 J98 water ice 0.04-2e6 W\&B water liq 0.01-1e7 S ammonia 0.14-200 M K - \cite{koike95}, Z - \cite{zeidler13}, P - \cite{posch03}, J\&C - \cite{johnson74}, O - \cite{ordal88}, J03 - \cite{jager03}, D - \cite{dorschner95}, J98 - \cite{jager98}, W\&B - \cite{warren08}, S - \cite{segelstein81}, M - \cite{martonchik84}. Dorschner, J., Begemann, B., Henning, T., Jaeger, C., \& Mutschke, H. 1995, A\&A, 300, 503 J\"ager, C., Dorschner, J., Mutschke, H., Posch, T., \& Henning,T. 2003, A\&A, 408, 193 Jager, C., Mutschke, H., \& Henning, Th. 1998, A\&A, 332, 291 Johnson, P. B., \& Christy, R. W. 1974, Physical Review B, 9, 5056 Koike, C., Kaito, C., Yamamoto, T., Shibai, H., Kimura} S., \& Suto, H. 1995, Icarus, 114, 203 Martonchik, J.V., Orton, G.S., \& Appleby, J.F. 1984, Appl.Opt. 23, 541 Ordal, M.A., Bell, R.J., Alexander, R.W.Jr., Newquist, L.A., \& Querry, M.R. 1988, Applied Optics, 27, 1203 Posch, Th., Kerschbaum, F., Fabian, D., Mutschke, H., Dorschner, J., Tamanai, A., \& Henning, Th. 2003, ApJS, 149, 437 Segelstein, D. 1981, M.S.Thesis, University of Missouri--Kansas City Warren, S.G., \& Brandt R.E. 2008, J. Geophys. Res., 113, D14220 Zeidler, S., Posch, T. \& Mutschke, H. 2013, A\&A, 553, A81