ABSORB(1)TIPSY COMMANDSABSORB(1)

absorb - calculate spectra

absorbtypespatial_bin_numbervel_minvel_maxvel_bin_numberfilenamexy

absorbcalculates absorption properties along a sight line specified byxandy.Ifxis the string "auto", then the sight line is deter- mined by a mouse click. The properties calculated depend on thetypeparameter which can be either "spectra", "column", "velocity", "dark", or "star". Iftypeis "dark" or "star" thenfilenamewill containspa-tial_bin_numberlines corresponding to spatial bins along the line of sight equally spaced across the active box. Each line contains the line of sight distance to the center of the bin, the mean mass density of "star" or "dark" (in gm/cc), the mean velocity of the material in that bin (in physical km/s, that is with Hubble flow included for cos- mological simulations), and the effective spatial resolution used in determining the density. The density is determined in the following way. For each particle, it is determined whether the line of sight intersects the smoothing kernel (as set by thesmoothcommand), and if it does the contribution of the spline kernel to the column density of each bin which overlaps the kernel is integrated along the line of sight. The mass density for each bin is then the column density divided by the bin length, the velocity is the mass weighted veloci- ties (shifted by a Hubble term for cosmological simulations) of the particles that contribute to the column density, and the resolution is the mass weighted smoothing lengths ("h" of the spline kernel). Iftypeis "column" thenfilename.colwill containspatial_bin_numberlines as above with each line containing the line of sight distance to the bin, the total gas mass density, the mass weighted velocity, the mass weighted temperature, the mass density in HI, the velocity of the HI, the temperature of the HI, the mass density, velocity and tempera- ture of the HeI, the mass density, velocity and temperature of the HeII, the effective resolution, and an estimate of the divergence of the velocity. Iftypeis "velocity" thenfilename.velwill containvel_bin_numberlines corresponding to equally spaced velocity intervals betweenvel_minandvel_max.Each line contains the central velocity of the bin, the column density per velocity interval of HI (in gm/cm2 per km/s), the total column density of gas (in atoms/cm2/(km/s)), the neu- tral fraction of the gas that contributes to the HI column den- sity(??), the mean temperature of the HI gas, the density of the HI gas (in atoms/cc), the effective resolution of the HI, the mean tem- perature of the total gas, the mean temperature squared of the gas, and the divergence of the velocity of the gas. The column densities are determined in the following way. Each spatial bin along the line of sight is divided into 10 (a compile time constant "SUBBIN") sub- bins. The velocity and temperature of these sub-bins are linearly interpolated from the adjacent bins. A velocity profile is determined for the gas in this sub-bin based on thermal broadening and damping wings. This profile is then integrated over each velocity bin to determine its contribution to the bin. Iftypeis "spectra", "column", or "velocity" thenfilenamewill con- tainvel_bin_numberlines corresponding to equally spaced velocity intervals betweenvel_minandvel_max.Each line contains the central velocity of the bin, the optical depth to HI absorption, the optical depth to HeI absorption, the optical depth to HeII absorption, the total optical depth to HI within the velocity interval (no line broad- ening), and the optical depth to deuterium absorption,

KQ Release 2.2.3a 20 JULY 2006ABSORB(1)

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