petitRADTRANS.nat_cst

Module Contents

Functions

b(T, nu)	Returns the Planck function \(B_{\nu}(T)\) in units of
get_PHOENIX_spec(temperature)	Returns a matrix where the first column is the wavelength in cm
get_PHOENIX_spec_rad(temperature)	Returns a matrix where the first column is the wavelength in cm
convolve_rebin(input_wavelengths, input_flux, ...)
radiosity_erg_hz2radiosity_erg_cm(radiosity_erg_hz, ...)	Convert a radiosity from erg.s-1.cm-2.sr-1/Hz to erg.s-1.cm-2.sr-1/cm at a given frequency. # TODO move to physics

Attributes

c
h
kB
nA
e
G
m_elec
sigma
L0
R
bar
atm
AU
pc
light_year
amu
r_sun
r_jup
r_earth
m_sun
m_jup
m_earth
l_sun
r_jup_mean
s_earth
molecular_weight
pathinp
spec_path
description
logTempGrid
StarRadGrid
specDats

petitRADTRANS.nat_cst.c

petitRADTRANS.nat_cst.h

petitRADTRANS.nat_cst.kB

petitRADTRANS.nat_cst.nA

petitRADTRANS.nat_cst.e

petitRADTRANS.nat_cst.G

petitRADTRANS.nat_cst.m_elec

petitRADTRANS.nat_cst.sigma

petitRADTRANS.nat_cst.L0

petitRADTRANS.nat_cst.R

petitRADTRANS.nat_cst.bar = 1000000.0

petitRADTRANS.nat_cst.atm

petitRADTRANS.nat_cst.AU

petitRADTRANS.nat_cst.pc

petitRADTRANS.nat_cst.light_year

petitRADTRANS.nat_cst.amu

petitRADTRANS.nat_cst.r_sun

petitRADTRANS.nat_cst.r_jup

petitRADTRANS.nat_cst.r_earth

petitRADTRANS.nat_cst.m_sun

petitRADTRANS.nat_cst.m_jup

petitRADTRANS.nat_cst.m_earth

petitRADTRANS.nat_cst.l_sun

petitRADTRANS.nat_cst.r_jup_mean = 6991100000.0

petitRADTRANS.nat_cst.s_earth = 1365400.0

petitRADTRANS.nat_cst.molecular_weight

petitRADTRANS.nat_cst.b(T, nu)

Returns the Planck function \(B_{\nu}(T)\) in units of \(\rm erg/s/cm^2/Hz/steradian\).

Args:

T (float):

Temperature in K.

nu:

numpy array containing the frequency in Hz.

petitRADTRANS.nat_cst.pathinp

petitRADTRANS.nat_cst.spec_path

petitRADTRANS.nat_cst.description

petitRADTRANS.nat_cst.logTempGrid

petitRADTRANS.nat_cst.StarRadGrid

petitRADTRANS.nat_cst.specDats = []

petitRADTRANS.nat_cst.get_PHOENIX_spec(temperature)

Returns a matrix where the first column is the wavelength in cm and the second is the stellar flux \(F_\nu\) in units of \(\rm erg/cm^2/s/Hz\), at the surface of the star. The spectra are PHOENIX models from (Husser et al. 2013), the spectral grid used here was described in van Boekel et al. (2012).

Args:

temperature (float):

stellar effective temperature in K.

petitRADTRANS.nat_cst.get_PHOENIX_spec_rad(temperature)

Returns a matrix where the first column is the wavelength in cm and the second is the stellar flux \(F_\nu\) in units of \(\rm erg/cm^2/s/Hz\), at the surface of the star. The spectra are PHOENIX models from (Husser et al. 2013), the spectral grid used here was described in van Boekel et al. (2012).

UPDATE: It also returns a float that is the corresponding estimate of the stellar radius.

Args:

temperature (float):

stellar effective temperature in K.

petitRADTRANS.nat_cst.convolve_rebin(input_wavelengths, input_flux, instrument_resolving_power, pixel_sampling, instrument_wavelength_range)

petitRADTRANS.nat_cst.radiosity_erg_hz2radiosity_erg_cm(radiosity_erg_hz, frequency)

Convert a radiosity from erg.s-1.cm-2.sr-1/Hz to erg.s-1.cm-2.sr-1/cm at a given frequency. # TODO move to physics

Steps:

[cm] = c[cm.s-1] / [Hz] => d[cm]/d[Hz] = d(c / [Hz])/d[Hz] => d[cm]/d[Hz] = c / [Hz]**2 => d[Hz]/d[cm] = [Hz]**2 / c integral of flux must be conserved: radiosity_erg_cm * d[cm] = radiosity_erg_hz * d[Hz] radiosity_erg_cm = radiosity_erg_hz * d[Hz]/d[cm] => radiosity_erg_cm = radiosity_erg_hz * frequency**2 / c

Args:

radiosity_erg_hz: (erg.s-1.cm-2.sr-1/Hz) frequency: (Hz)

Returns:

(erg.s-1.cm-2.sr-1/cm) the radiosity in converted units