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coron_readme.txt
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The LUVOIR coronagraph simulator tool is based off Tyler Robinson's coronagraph noise model (Robinson et al. 2016). The python version of this tool was produced by Jacob Lustig-Yaeger (available at https://github.com/jlustigy/coronagraph). The Bokeh rendering was produced by Jason Tumlinson and Giada Arney from the python version.
The coronagraph noise model used here assumes most of the same nominal parameters as those used in Robinson et al. (2016). The values of internal (i.e. non-slider) input parameters used here are:
Dark current = 1e-4 counts/s
Read noise = 0.1 counts per pixel
Contrast ratio = 1e-10
Detector temperature = 50 K
Emissivity = 0.9
DNHpix = 3.0 (= number of horizontal/spatial pixels in dispersed spectrum)
width of photometric aperture = 1.5 (times lambda/D)
quantum efficiency factor = 0.9
MzV = 23.0 ( = V-band zodiacal light surface brightness)
MezV = 22.0 ( = V-band exozodiacal light surface brightness)
Note that this simulator differs from the simulator described in Robinson et al. (2016) because here we assume a constant quantum efficiency as a function of wavelength ( = 0.9), whereas Robinson et al. (2016) assumes wavelength dependence.
All planets are assumed to be orbiting the sun except as noted (the O2 False Positive planet orbits an F2V star).
When the ground based option is selected from the Observation menu, the simulator accounts for Earth’s atmospheric transmittance and downwelling thermal radiation from the atmosphere. Atmospheric airglow is not yet included.
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Details on input spectra are:
Earth:
Type: Synthetic spectrum
Generated by: Tyler Robinson
Citaiton:
Robinson, T. D., Meadows, V. S., Crisp, D., Deming, D., A'Hearn, M. F., Charbonneau, D., & Hewagama, T. (2011). Earth as an extrasolar planet: Earth model validation using EPOXI Earth observations. Astrobiology, 11(5), 393-408.
Archean Earth:
Type: Synthetic spectrum
Generated by: Giada Arney
Citation:
Arney, G. N., Domagal-Goldman, S. D., Meadows, V. S., Wolf, E. T., Schwieterman, E., Charnay, B., Claire, M., Hebrard, E., Trainer, M. (2016) The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth. Astrobiology 16(11)
Hazy Archean Earth:
Type: Synthetic spectrum
Generated by: Giada Arney
Citation:
Arney, G. N., Domagal-Goldman, S. D., Meadows, V. S., Wolf, E. T., Schwieterman, E., Charnay, B., Claire, M., Hebrard, E., Trainer, M. (2016) The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth. Astrobiology 16(11)
1% PAL O2 Proterozoic Earth:
Type: Synthetic spectrum
Generated by: Giada Arney
Citation:
Arney, G. N., Domagal-Goldman, S. D., Meadows, V. S., Wolf, E. T., Schwieterman, E., Charnay, B., Claire, M., Hebrard, E., Trainer, M. (2016) The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth. Astrobiology 16(11)
0.1% PAL O2 Proterozoic Earth:
Type: Synthetic spectrum
Generated by: Giada Arney
Citation:
Arney, G. N., Domagal-Goldman, S. D., Meadows, V. S., Wolf, E. T., Schwieterman, E., Charnay, B., Claire, M., Hebrard, E., Trainer, M. (2016) The Pale Orange Dot: The Spectrum and Habitability of Hazy Archean Earth. Astrobiology 16(11)
Venus:
Type: Synthetic spectrum
Generated by: Giada Arney
Citation: n/a
Early Mars
Type: Synthetic spectrum
Generated by: Giada Arney
Citation:
Smith, M. L., Claire, M. W., Catling, D. C., & Zahnle, K. J. (2014). The formation of sulfate, nitrate and perchlorate salts in the martian atmosphere. Icarus, 231, 51-64.
Mars:
Type: Synthetic spectrum
Generated by: Tyler Robinson
Citation: n/a
Jupiter:
Type: Observed spectrum
Observatory for 0.3-0.9 microns: 1.52-meter European Southern Observatory
Citation for 0.3-0.9 microns:
Karkoschka, E. (1998). Methane, Ammonia, and Temperature Measurements of the Jovian Planets and Titan from CCD-Spectrophotometry. Icarus, 133(1), 134-146.
Observatory for 0.9-2.5 microns: SPEX instrument on the NASA Infrared Telescope Facility (IRTF)
Citation for 0.9-2.5 microns:
Rayner, J. T., Cushing, M. C., Vacca, W. D. (2009) The Infared Telescope Facility (IRTF) Spectral Library: Cool Stars. The Astrophysical Journal Supplement Series, 185(2)
Saturn:
Type: Observed spectrum
Observatory for 0.3-0.9 microns: 1.52-meter European Southern Observatory
Citation for 0.3-0.9 microns:
Karkoschka, E. (1998). Methane, Ammonia, and Temperature Measurements of the Jovian Planets and Titan from CCD-Spectrophotometry. Icarus, 133(1), 134-146.
Observatory for 0.9-2.5 microns: SPEX instrument on the NASA Infrared Telescope Facility (IRTF)
Citation for 0.9-2.5 microns:
Rayner, J. T., Cushing, M. C., Vacca, W. D. (2009) The Infared Telescope Facility (IRTF) Spectral Library: Cool Stars. The Astrophysical Journal Supplement Series, 185(2)
Uranus:
Type: Observed spectrum
Observatory for 0.3-0.9 microns: 1.52-meter European Southern Observatory
Citation for 0.3-0.9 microns:
Karkoschka, E. (1998). Methane, Ammonia, and Temperature Measurements of the Jovian Planets and Titan from CCD-Spectrophotometry. Icarus, 133(1), 134-146.
Observatory for 0.9-2.5 microns: SPEX instrument on the NASA Infrared Telescope Facility (IRTF)
Citation for 0.9-2.5 microns:
Rayner, J. T., Cushing, M. C., Vacca, W. D. (2009) The Infared Telescope Facility (IRTF) Spectral Library: Cool Stars. The Astrophysical Journal Supplement Series, 185(2)
Neptune:
Type: Observed spectrum
Observatory for 0.3-0.9 microns: 1.52-meter European Southern Observatory
Citation for 0.3-0.9 microns:
Karkoschka, E. (1998). Methane, Ammonia, and Temperature Measurements of the Jovian Planets and Titan from CCD-Spectrophotometry. Icarus, 133(1), 134-146.
Observatory for 0.9-2.5 microns: SPEX instrument on the NASA Infrared Telescope Facility (IRTF)
Citation for 0.9-2.5 microns:
Rayner, J. T., Cushing, M. C., Vacca, W. D. (2009) The Infared Telescope Facility (IRTF) Spectral Library: Cool Stars. The Astrophysical Journal Supplement Series, 185(2)
Warm Neptune planets:
Type: Synthetic spectra
Generated by: Renyu Hu
Citation:
Hu, R., & Seager, S. (2014). Photochemistry in terrestrial exoplanet atmospheres. III. Photochemistry and thermochemistry in thick atmospheres on super Earths and mini Neptunes. The Astrophysical Journal, 784(1), 63.
Warm Jupiter planets:
Type: Synthetic spectra
Generated by: Kerri Cahoy
Citation:
Cahoy, K. L., Marley, M. S., & Fortney, J. J. (2010). Exoplanet albedo spectra and colors as a function of planet phase, separation, and metallicity. The Astrophysical Journal, 724(1), 189.
False O2 Planet (F2V star):
Type: Synthetic spectrum
Generated by: Shawn Domagal-Goldman
Citaiton:
Domagal-Goldman, S. D., Segura, A., Claire, M. W., Robinson, T. D., & Meadows, V. S. (2014). Abiotic ozone and oxygen in atmospheres similar to prebiotic Earth. The Astrophysical Journal, 792(2), 90.