line_luminosity
Calculate line luminosity from integrated flux and rest frequency, applying redshift, Planck18 distance, and lensing magnification corrections for local or distant sources.
Instructions
Line luminosity in the Solomon et al. (1997) / Solomon and Vanden Bout (2005) forms.
L'_line = 3.25e7 S dv nu_obs^-2 D_L^2 (1+z)^-3 [K km/s pc^2] (S dv in Jy km/s, nu_obs in GHz, D_L in Mpc) L_line = 1.04e-3 S dv nu_obs D_L^2 = 1.04e-3 S dv nu_rest (1+z)^-1 D_L^2 [Lsun] and L_line = 3.18e-11 nu_rest^3 L'. For a local source give distance_mpc (z may stay 0); for z > 0 leave distance_mpc empty and D_L comes from Planck18 (a given distance wins, with a warning if it disagrees). Lensed sources are divided by magnification. Limits: interferometric fluxes can miss extended emission.
Tool call template
Replace each placeholder with a value matching the input schema. Only required parameters are included; add optional parameters as needed.
{
"id": 1,
"jsonrpc": "2.0",
"method": "tools/call",
"params": {
"arguments": {
"integrated_flux_jy_kms": "<integrated_flux_jy_kms>",
"rest_freq_ghz": "<rest_freq_ghz>"
},
"name": "line_luminosity"
}
}Input Schema
| Name | Required | Description | Default |
|---|---|---|---|
| redshift | No | ||
| distance_mpc | No | ||
| flux_cal_frac | No | ||
| magnification | No | ||
| rest_freq_ghz | Yes | ||
| integrated_flux_jy_kms | Yes | ||
| integrated_flux_err_jy_kms | No |