TemperatureResponseFundamental#

class xrtpy.response.TemperatureResponseFundamental(filter_name, observation_date, abundance_model='coronal')[source]#

Produce the temperature response for each XRT x-ray channel, assuming a spectral emission model.

Attributes Summary

`CHIANTI_temperature`	Emission model temperatures in kelvin.
`abundance_model_information`	A brief description of the abundance model used in the creation of the emission spectra.
`abundances`	Defined the name of the requested abundance model as a string.
`ccd_gain_right`	Provide the camera gain in electrons per data number.
`chianti_abundance_version`	Version of the chianti abundance model.
`density_model`	A brief description of the plasma density, emission measure, or differential emission measure used in the creation of the emission spectra.
`ev_per_electron`	Amount of energy it takes to dislodge 1 electron in the CCD.
`file_spectra`	Emission model file spectra.
`filter_name`	Name of searched filter.
`focal_len`	Focal length of the telescope in units of cm.
`ionization_model`	A brief description of the ionization equilibrium model used in the creation of the emission spectra.
`observation_date`	Date of observation.
`pixel_size`	CCD pixel size.
`solid_angle_per_pixel`	This amount represents the solid angle, which is given in units of steradians over pixel.
`wavelength`	Array of wavelengths for every X-ray channel in Å.

Methods Summary

`effective_area`()	Calculate the effective area.
`integration`()	Perform the integration of the temperature response.
`spectra`()	Interpolation between the spectra wavelength onto the channel wavelength.
`temperature_response`()	Apply gain value to the Temperature Response.

Attributes Documentation

abundance_model_information#: A brief description of the abundance model used in the creation of the emission spectra.

density_model#: A brief description of the plasma density, emission measure, or differential emission measure used in the creation of the emission spectra.

ev_per_electron#: Amount of energy it takes to dislodge 1 electron in the CCD.

ionization_model#: A brief description of the ionization equilibrium model used in the creation of the emission spectra.

solid_angle_per_pixel#: This amount represents the solid angle, which is given in units of steradians over pixel.

Methods Documentation

effective_area()[source]#

Calculate the effective area.

integration()[source]#

Perform the integration of the temperature response.

Returns:: astropy.units.Quantity – Integrated temperature response in electron cm^5 / (s pix).

Interpolation between the spectra wavelength onto the channel wavelength.

temperature_response()[source]#

Apply gain value to the Temperature Response.

Returns:: astropy.units.Quantity – Temperature response in DN cm^5 / (s pix).