dust_mass_from_flux
Computes optically thin dust mass from measured flux using Hildebrand 1983, including redshift, CMB contrast/heating, and opacity options.
Instructions
Optically thin dust mass (Hildebrand 1983): M = S_nu D^2 / (kappa_nu B_nu(T_d)).
At redshift z (freq_ghz is the observed frequency): M = S_obs D_L^2 / ((1 + z) kappa(nu_rest) B(nu_rest, T_d)). The full Planck function is used, never the Rayleigh-Jeans 1/T form. kappa_nu = kappa0 (nu / nu0)^beta per gram of dust unless kappa_includes_gas=True (then the result is a gas+dust mass and the dust mass is that divided by gas_to_dust). cmb: 'none', 'contrast' (divide by 1 - B(T_CMB(z))/B(T_d), da Cunha 2013 eq. 18) or 'heating_and_contrast' (t_dust_k is then the z = 0 temperature and is heated by the CMB first, da Cunha 2013 eq. 12). Never apply heating twice. Limits: optically thick emission makes the mass a lower limit; kappa is uncertain by about 25% to a factor 3-5 and is NOT propagated; interferometers can resolve out extended flux.
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": {
"flux_mjy": "<flux_mjy>",
"freq_ghz": "<freq_ghz>"
},
"name": "dust_mass_from_flux"
}
}Input Schema
| Name | Required | Description | Default |
|---|---|---|---|
| cmb | No | none | |
| beta | No | ||
| nu0_ghz | No | ||
| flux_mjy | Yes | ||
| freq_ghz | Yes | ||
| redshift | No | ||
| t_dust_k | No | ||
| distance_pc | No | ||
| gas_to_dust | No | ||
| flux_err_mjy | No | ||
| kappa0_cm2_g | No | ||
| kappa_preset | No | beckwith1990 | |
| t_dust_err_k | No | ||
| flux_cal_frac | No | ||
| kappa_includes_gas | No |