deshima_sensitivity.galaxy module#

co_luminosity(z, d_l, f_obs, int)[source]#
flux_from_line_luminosity(z: ndarray | List[float] | List[int] | float | int, d_l: ndarray | List[float] | List[int] | float | int, f_obs: float, L: float) → ndarray | List[float] | List[int] | float | int[source]#

Calculate line flux from luminosity.

Parameters:

  • d_l (ndarray | List[float] | List[int] | float | int) – Luminosity distance. Units: Mpc.

  • f_obs (float) – Observing frequency. Units: GHz.

  • L (float) – Line luminosity. Units: L_Sun.

  • z (ndarray | List[float] | List[int] | float | int)

Returns:

Flux of line. Units: W m^-2.

Return type:

flux

lineflux(Lfir: float = 50000000000000.0, switch_dwarf: bool = False) → Tuple[ndarray | List[float] | List[int] | float | int, ndarray | List[float] | List[int] | float | int, ndarray | List[float] | List[int] | float | int, float, float, float, ndarray | List[float] | List[int] | float | int][source]#

Calculate astronomical line fluxes, developed by Y. Tamura.

Parameters:

  • Lfir (float) – Total infrared luminosity. Units: L_Sun.

  • switch_dwarf (bool) – Whether to use line-to-TIR ratios for dwarf galaxies (True) or not (False).

Returns:

  • Fcii_DGS – Flux(es) of [CII]. Units: W m^-2.

  • Foiii_DGS – Flux(es) of [OIII]. Units: W m^-2.

  • Foi_DGS – Flux(es) of [OI]. Units: W m^-2.

  • f_cii – Frequency of [CII]. Units: GHz.

  • f_oiii – Frequency of [OIII]. Units: GHz.

  • f_oi – Frequency of [OI]. Units: GHz.

  • z – Redshift(s) at which fluxes are calculated.

Return type:

Tuple[ndarray | List[float] | List[int] | float | int, ndarray | List[float] | List[int] | float | int, ndarray | List[float] | List[int] | float | int, float, float, float, ndarray | List[float] | List[int] | float | int]