The JWST Exposure Time Calculator (ETC) offers a series of spectral energy distributions (SEDs) that may be used when building a source. Templates include many flavors of stellar and extragalactic spectra, and analytic spectral distributions. A user-supplied spectrum may also be uploaded to the ETC for use in calculations.
When creating a new source in the Exposure Time Calculator (ETC), the user may choose to apply a template spectrum for the source's continuum. Many of the commonly used stellar and extragalactic templates have been provided, which cover a wide range of observed spectral energy distributions, along with several analytic functions. The available choices for source spectral energy distributions are described below. They are accessed from the "Continuum" tab of the Source Editor pane on the Scenes and Sources page in the ETC. The "Continuum" tab is also where the redshift and extinction parameters may be entered.
Analytic spectral energy distributions include a Black Body continuum, a Power Law continuum and a Flat continuum.
The blackbody spectrum is computed at the temperature of the blackbody specified by the user.
The flux distribution is given by F(λ) = λn , where n is specified by the user. In addition to the form, flam (wavelength units) or fnu (frequency units), the user must choose an integer exponent for the power law.
A flat continuum is a special case of the power law spectrum, where n=0. This distribution is so named because the spectrum has constant (flat line) energy per unit wavelength (flam) or frequency (fnu).
Stellar template spectral energy distributions include a library of Phoenix stellar models and spectra of HST standard stars.
Phoenix stellar models
The pull-down menu of Phoenix stellar models contains synthetic spectra spanning spectral types from O3 to M5, obtained using the Star, Brown Dwarf, and Planet Simulator. They use static, spherically symmetric, 1D simulations to completely describe the atmospheric emission spectrum. The models account for the formation of molecular bands, such as those of water vapor, methane, or titanium dioxide, solving for the transfer equation over more than 20,000 wavelength points on average, producing synthetic spectra with 2 Angstrom resolution. The line selection is repeated for each iteration of the model until it has converged and the thermal structure obtained. The models here are calculated with a cloud model, valid across the entire parameter range. Each model's name contains a concatenation of the spectral type, effective temperature, and gravity (log g value).
HST stellar spectra
Several HST calibration standard spectra are available. Those provided here are the recommended spectra for the calibrator. These spectra are stored in the Calibration Database System (CDBS) and were originally chosen from the paper Spectrophotometric Standards from the Far-UV to the Near-IR on the White Dwarf Flux Scale by Bohlin (1996) and later updated as new data became available. See also Comparison of White Dwarf Models with ACS Spectrophotometry by Bohlin et al. (2001). The selection also includes a spectrum of the Sun.
More information, along with a list of the complete set of files, including older versions, can be found in the CALSPEC Calibration Database. This page provides a table with the available Flux Standards and their CDBS name. In this table the order of preference for the choice of a standard flux distribution is from left to right in the Table, i.e. from the best in column 6 to the last choice with the lowest quality in column 9. In this case, models have higher fidelity and extend to longer wavelength ranges while the more outdated are those derived applying corrections to the original IUE and optical fluxes. Note that for the cases when the CALSPEC data is updated after the ETC software is released, the ETC will not be able to access the most recent files, but only those that were available at the time of the build. If the ETC produces an error when trying to access an HST Standard Star spectrum, review the update history at the bottom of the CALSPEC page to determine when the spectrum was updated. If it was updated after the current ETC version, you may want to use the previous version of the model, or download the most recent spectrum, and apply it as a user-supplied spectrum.
Each stellar model's spectral type and related identifying information is shown in the pull-down menu listing the star by name. The related information includes the spectral type and V magnitude in parentheses, and wavelength range in Angstroms in brackets.
Extragalactic template spectral energy distributions include models from Brown et al. (2014). Wavelength coverage for these models spans UV to mid-infrared wavelengths. The atlas includes a broad range of galaxy types, including ellipticals, spirals, merging galaxies, blue compact dwarfs and luminous infrared galaxies.
JWST User Documentation Home
JWST Exposure Time Calculator (ETC)
JWST ETC Scenes and Sources Page Overview
JWST ETC Defining a New Source
JWST ETC Defining a New Scene
JWST ETC User Supplied Spectra
Star, Brown Dwarf, and Planet Simulator
Phoenix models README file
CALSPEC Calibration Database
Go to the on-line JWST Exposure Time Calculator Tool
Brown et al. 2014, ApJS, 212,18
An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-infrared
Bohlin et al. 1996, AJ, 111, 1743
Spectrophotometric Standards From the Far-UV to the Near-IR on the White Dwarf Flux Scale
Bohlin et al. 2001, AJ, 122, 2118
Spectrophotometric Standards from the Far-Ultraviolet to the Near-Infrared: STIS and NICMOS Fluxes
Pontoppidan, K. M., Pickering, T. E., Laidler, V. G. et al., 2016, Proc. SPIE 9910, Observatory Operations: Strategies, Processes, and Systems VI, 991016 ,
Pandeia: a multi-mission exposure time calculator for JWST and WFIRST
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