The following parameters refer to the telescope design as specified in Design Cycle 7 or the 2015 WFIRST-AFTA Science Definition Team and WFIRST Study Office Report. Additional Cycle 6 and Cycle 7 reference files are also available. These include the field-of-view layout, slew times, detector properties, distortions, Zernike decompositions of the PSFs, pupil masks, transmission/effective area per filter, and more. Additional Coronagraph Instrument parameters and data are also available.
These spacecraft/instrument parameters, which are to be used in simulations and in designing science projects, are tied to a regular project design schedule. (See the pull-down menu below for the previous versions.) To ensure consistency within the community, these parameters are released here only after approval by the Roman Space Telescope Project Scientist.
| Name | Value | Unit | Description |
|---|---|---|---|
| Mission_Duration_Requirement | 5 | years | Mission duration requirement |
| Mission_Duration_Goal | 10 | years | Mission duration goal |
| Mission_Launch_Site | Cape Canaveral Air Force Station, Florida | Launch site | |
| Spacecraft_Operating_Temperature | 298 | K | Operating temperature of the spacecraft |
| Spacecraft_Orbit_Type | Sun-Earth L2 | Type of spacecraft orbit | |
| Spacecraft_Downlink_Rate | 275 | Mbps | Spacecraft downlink rate |
| Spacecraft_Downlink_Volume | 11 | Tbits/day | Spacecraft downlink volume |
| Spacecraft_Slew_Angle_Gap_Fill | 0.025 | degrees | Gap fill slew angle |
| Spacecraft_Slew_Time_Gap_Fill | 21.4 | seconds | Gap fill slew time |
| Spacecraft_Slew_Angle_Short_FoV | 0.4 | degrees | Shorter side of field-of-view slew angle (six reaction wheel operation) |
| Spacecraft_Slew_Time_Short_FoV | 49.3 | seconds | Shorter side of field-of-view slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Angle_Long_FoV | 0.8 | degrees | Long side of field-of-view slew angle (six reaction wheel operation) |
| Spacecraft_Slew_Time_Long_FoV | 67.4 | seconds | Long side of field-of-view slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Angle_Microlensing_Maximum | 2.06 | degrees | Maximum microlensing slew angle (six reaction wheel operation) |
| Spacecraft_Slew_Time_Microlensing_Maximum | 99 | seconds | Maximum microlensing slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Time_Two_Degrees | 99 | seconds | Two degree slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Time_Five_Degrees | 162 | seconds | Five degree slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Time_Ten_Degrees | 267 | seconds | Ten degree slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Time_Thirty_Degrees | 667 | seconds | Thirty degree slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Time_Ninety_Degrees | 1865 | seconds | Thirty degree slew time (including the settle time; six reaction wheel operation) |
| Spacecraft_Slew_Settling_Time_Small | 10+slew angle (degrees) | seconds | Spacecraft settling time after a slew of less than ten degrees |
| Spacecraft_Slew_Settling_Time_Large | 20 | seconds | Spacecraft settling time after a slew of more than ten degrees |
| Name | Value | Unit | Description |
|---|---|---|---|
| Telescope_Jitter | 12 | milliarcsec | Telescope jitter for high frequencies (vibration modes in the optics) per axis (rms) |
| Telescope_Primary_Diameter | 2.36 | m | Diameter of the telescope primary mirror |
| Telescope_Primary_Mirror_Temperature | 265 | K | Telescope primary mirror temperature |
| Telescope_Central_Obscuration | 30.3 | % | Linear obscuration of the telescope entrance pupil (diameter ratio) |
| Name | Value | Unit | Description |
|---|---|---|---|
| WFI_Correlated_Noise | 5 | e- | WFI detector correlated noise floor |
| WFI_Count_Rate_Zody_Minimum_F062 | 0.27 | Count rate per pixel in the F062 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F087 | 0.27 | Count rate per pixel in the F087 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F106 | 0.29 | Count rate per pixel in the F106 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F129 | 0.28 | Count rate per pixel in the F129 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F158 | 0.26 | Count rate per pixel in the F158 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F184 | 0.15 | Count rate per pixel in the F184 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F146 | 0.85 | Count rate per pixel in the F146 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_F213 | 0.13 | Count rate per pixel in the F213 filter at minimum zodiacal light | |
| WFI_Count_Rate_Zody_Minimum_Prism | 0.95 | Count rate per pixel in the Prism at minimum zodiacal light | |
| WFI_Dark_Current | < 0.1 | e-/s/pixel | WFI detector dark current per pixel (requirement) |
| WFI_Detector_Guide_Star_Update_Rate | ~5.8 | Hz | Guide star update rate |
| WFI_Detector_Type | H4RG-10 | Detector type for WFI | |
| WFI_Detector_Quantum_Efficiency_Long | >80 | % | WFI detector quantum efficiency (requirement; average over wavelengths between 0.8 and 2.1 microns |
| WFI_Detector_Quantum_Efficiency_Short | >60 | % | WFI detector quantum efficiency (requirement; average over wavelengths between 0.6 and 0.8 microns |
| WFI_Detector_Readout_Time | 3.04 | sec | Sensor Chip Assembly full frame readout time |
| WFI_Detector_Pixel_Operability | >95 | % | WFI detector pixel operability (requirement) |
| WFI_Detector_Total_Crosstalk | <12 | % | WFI detector total crosstalk (requirement) |
| WFI_Detector_Total_Noise_180s | 5-6 | electrons | WFI detector total noise (rms uncertainty in slope fit for an exposure time of 180 sec) |
| WFI_Detector_Inter_Pixel_Capacitance | 0.9119 | WFI detector inter-pixel capacitance (fraction of a pixel-centered total charge of 1 actually deposited in the central pixel) | |
| WFI_Detector_Full_Frame_Readout_Time | 2.74 | seconds | WFI detector full frame readout time |
| WFI_Field_Of_View_Effective | 0.281 | deg2 | WFI total effective field of view (ignoring gaps between detectors) |
| WFI_Field_Of_View_Total | 0.32 | deg2 | WFI total field of view (including gaps between detectors) |
| WFI_Focal_Ratio | 7.9 | WFI instrument and telescope's combined focal ratio | |
| WFI_Number_Of_Active_Columns | 4088 | pixel | Number of active detector columns (also known as the number of pixels in the x-direction) in (the image section of) a detector |
| WFI_Number_Of_Active_Rows | 4088 | pixel | Number of active detector rows (also known as the number of pixels in the y-direction) in (the image section of) a detector |
| WFI_Jitter_Wavefront_Error | < 0.707 | nm | Telescope intermediate focus wavefront error jitter (requirement) |
| WFI_Image_Stability | 1.0 | nm | RMS wave front error (WFE) variation in 180 sec |
| WFI_Pixel_Scale | 0.11 | arcsec | WFI detector pixel scale in arcseconds/pixel |
| WFI_Pixel_Size | 10 | 10-6 m | WFI wide-field channel pixel size in each dimension |
| WFI_PSF_Ellipticity | < 0.00047 | WFI point spread function ellipticity per 184 seconds at WFI focus | |
| WFI_Readout_Noise | < 20 | e- | WFI detector pixel readout noise rms for correlated double sampling (two successive detector readouts) |
| WFI_Temperature | < 100 | K | WFI detector operating temperature |
| WFI_Number | 18 | Total number of scientific detectors in WFI | |
| WFI_Prism_Spectral_Resolving_Power_P127 | 80-180 | WFI Prism resolving power (delta lambda = two pixels) |
| Name | Value | Unit | Description |
|---|---|---|---|
| WFI_Filter_F062_Center | 0.620 | 10-6 m | WFI filter F062 central wavelength |
| WFI_Filter_F087_Center | 0.869 | 10-6 m | WFI filter F087 central wavelength |
| WFI_Filter_F106_Center | 1.060 | 10-6 m | WFI filter F106 central wavelength |
| WFI_Filter_F129_Center | 1.293 | 10-6 m | WFI filter F129 central wavelength |
| WFI_Filter_F158_Center | 1.577 | 10-6 m | WFI filter F158 central wavelength |
| WFI_Filter_F184_Center | 1.842 | 10-6 m | WFI filter F184 central wavelength |
| WFI_Filter_F213_Center | 2.125 | 10-6 m | WFI filter F213 central wavelength |
| WFI_Filter_F146_Center | 1.464 | 10-6 m | WFI filter F146 central wavelength |
| WFI_Filter_F062_Resolving_Power | 2.2 | WFI filter F062 resolving power | |
| WFI_Filter_F087_Resolving_Power | 4 | WFI filter F087 resolving power | |
| WFI_Filter_F106_Resolving_Power | 4 | WFI filter F106 resolving power | |
| WFI_Filter_F129_Resolving_Power | 4 | WFI filter F129 resolving power | |
| WFI_Filter_F158_Resolving_Power | 4 | WFI filter F158 resolving power | |
| WFI_Filter_F184_Resolving_Power | 5.81 | WFI filter F184 resolving power | |
| WFI_Filter_F213_Resolving_Power | 6.07 | WFI filter F213 resolving power | |
| WFI_Filter_F146_Resolving_Power | 1.42 | WFI filter F146 resolving power | |
| WFI_Filter_F062_Wavelength_Range | 0.480-0.760 | 10-6 m | WFI filter F062 wavelength range |
| WFI_Filter_F087_Wavelength_Range | 0.760-0.977 | 10-6 m | WFI filter F087 wavelength range |
| WFI_Filter_F106_Wavelength_Range | 0.927-1.192 | 10-6 m | WFI filter F106 wavelength range |
| WFI_Filter_F129_Wavelength_Range | 1.131-1.454 | 10-6 m | WFI filter F129 wavelength range |
| WFI_Filter_F158_Wavelength_Range | 1.380-1.774 | 10-6 m | WFI filter F158 wavelength range |
| WFI_Filter_F184_Wavelength_Range | 1.683-2.000 | 10-6 m | WFI filter F184 wavelength range |
| WFI_Filter_F213_Wavelength_Range | 1.950-2.300 | 10-6 m | WFI filter F213 wavelength range |
| WFI_Filter_F146_Wavelength_Range | 0.927-2.000 | 10-6 m | WFI filter F146 wavelength range |
| WFI_Filter_Wavelength_Blank | WFI blank for dark current, flat field and other calibrations with internal light source |
| Name | Value | Unit | Description |
|---|---|---|---|
| WFI_Count_Rate_Zody_Minimum_Grism | 0.65 | Count rate per pixel in the Grism at minimum zodiacal light | |
| WFI_Grism_Dispersion | 1.04-1.14 | nm/pixel | WFI Grism dispersion, dependent mostly on the FPA Y value in degrees (Y axis is positive towards payload origin and FPA Y axis origin is between detectors 1 and 10) as -0.1945Y + 1.0764. |
| WFI_Grism_Wavelength_Range_G150 | 1.00-1.93 | 10-6 m | WFI Grism wavelength range |
| WFI_Grism_Spectral_Resolving_Power_G150 | 461lambda | WFI Grism resolving power (lambda in microns; two pixels) | |
| WFI_Sensitivity_Grism_Point_Source_Short | 21.0 | AB mag | WFI Grism limiting point source sensitivity (10-sigma per pixel in continuum) at 1.2 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_Grism_Point_Source_Long | 20.7 | AB mag | WFI Grism limiting point source sensitivity (10-sigma per pixel in continuum) at 1.5 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| Name | Value | Unit | Description |
|---|---|---|---|
| WFI_Prism_Wavelength_Range_P127 | 0.75-1.80 | 10-6 m | WFI prism wavelength range |
| WFI_Prism_Spectral_Resolving_Power_P127 | 80-180 | WFI Prism resolving power (delta lambda = two pixels) |
| Name | Value | Unit | Description |
|---|---|---|---|
| WFI_Sensitivity_Grism_Point_Source_Short | 21.0 | AB mag | WFI Grism limiting point source sensitivity (10-sigma per pixel in continuum) at 1.2 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_Grism_Point_Source_Long | 20.7 | AB mag | WFI Grism limiting point source sensitivity (10-sigma per pixel in continuum) at 1.5 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_Prism_Point_Source_Short | 22.2 | AB mag | WFI prism limiting point source sensitivity (10-sigma per pixel in continuum) at 0.8 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_Prism_Point_Source_Medium | 23.0 | AB mag | WFI prism limiting point source sensitivity (10-sigma per pixel in continuum) at 1.2 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_Prism_Point_Source_Long | 23.0 | AB mag | WFI prism limiting point source sensitivity (10-sigma per pixel in continuum) at 1.5 microns in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F062_Point_Source | 28.6 | AB mag | WFI filter F062 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F087_Point_Source | 28.2 | AB mag | WFI filter F087 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F106_Point_Source | 28.1 | AB mag | WFI filter F106 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F129_Point_Source | 28.0 | AB mag | WFI filter F129 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F158_Point_Source | 28.0 | AB mag | WFI filter F158 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F184_Point_Source | 27.5 | AB mag | WFI filter F184 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F213_Point_Source | 26.2 | AB mag | WFI filter F213 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_F146_Point_Source | 28.3 | AB mag | WFI filter F146 limiting point source sensitivity (5-sigma) in 1 hour of exposure time, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_110_Point_Source_Emission_Line | 5.7 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.1 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_110_Extended_Source_Emission_Line | 11.0 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.1 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_120_Point_Source_Emission_Line | 4.3 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.2 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_120_Extended_Source_Emission_Line | 8.2 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.2 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_130_Point_Source_Emission_Line | 3.8 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.3 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_130_Extended_Source_Emission_Line | 7.1 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.3 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_140_Point_Source_Emission_Line | 3.6 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.4 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_140_Extended_Source_Emission_Line | 6.7 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.4 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_150_Point_Source_Emission_Line | 3.6 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.5 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_150_Extended_Source_Emission_Line | 7.0 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.5 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_160_Point_Source_Emission_Line | 3.9 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.6 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_160_Extended_Source_Emission_Line | 7.2 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.6 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_170_Point_Source_Emission_Line | 4.2 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.7 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_170_Extended_Source_Emission_Line | 7.2 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.7 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_180_Point_Source_Emission_Line | 5.0 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a point source at 1.8 microns, zodiacal light set at twice the minimum value |
| WFI_Sensitivity_180_Extended_Source_Emission_Line | 8.4 | 10-17 ergs cm-2sec-1 | WFI emission line detected at 6.5-sigma in one hour for a source with half light radius = 0.2 arcsec at 1.8 microns, zodiacal light set at twice the minimum value |
| Name | Value | Unit | Description |
|---|
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Mode_Imaging_N | Narrow FoV imaging. Currently implemented as HLC coronagraph + Band 1 filter + imaging camera | ||
| CGI_Mode_Imaging_W | Wide FoV imaging. Currently implemented as SPC_A coronagraph + Band 4 filter + imaging camera | ||
| CGI_Mode_Spectroscopy | Single Slit, Prism-based Spectroscopy. Currently implemented as SPC_B coronagraph + Band 3 filter + Spectroscopy |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Coronagraph_HLC | HLC = Hybrid Lyot Coronagraph | ||
| CGI_Coronagraph_SPC_A | SPC_A = Shaped Pupil Coronagraph for large outer working angle in an annular field of view | ||
| CGI_Coronagraph_SPC_B | SPC_B = Shaped Pupil Coronagraph for small inner working angle in a `bowtie' shaped field of view | ||
| CGI_Coronagraph_Inner_Working_Angle_HLC | 3 | lambda/D | Inner radius of region of highest contrast |
| CGI_Coronagraph_Inner_Working_Angle_SPC_A | 5.9 | lambda/D | Inner radius of region of highest contrast |
| CGI_Coronagraph_Inner_Working_Angle_SPC_B | 3 | lambda/D | Inner radius of region of highest contrast |
| CGI_Coronagraph_Outer_Working_Angle_HLC | 9.7 | lambda/D | Outer radius of region of highest contrast |
| CGI_Coronagraph_Outer_Working_Angle_SPC_A | 20.1 | lambda/D | Outer radius of region of highest contrast |
| CGI_Coronagraph_Outer_Working_Angle_SPC_B | 9.1 | lambda/D | Outer radius of region of highest contrast |
| CGI_Coronagraph_Annular_Size_HLC | 360 | degrees | Suppression region annular extent |
| CGI_Coronagraph_Annular_Size_SPC_A | 360 | degrees | Suppression region annular extent |
| CGI_Coronagraph_Annular_Size_SPC_B | 130 | degrees | Suppression region annular extent |
| CGI_Predicted_Performance_45offaxis_scattered_light | 3.4x10-9 | Scattered light flux ratio per resolution element from a source 45 arcsec off axis. Applicable to all coronagraph modes | |
| CGI_Predicted_Performance_100offaxis_scattered_light | 3.5x10-10 | Scattered light flux ratio per resolution element from a source 100 arcsec off axis. Applicable to all coronagraph modes | |
| CGI_Host_Star_Vmag_Requirement | =< 5 | AB mag | CGI host star requirement is V_AB mag<=5; CGI could potentially observe dimmer targets (V = 6-7 AB mag), but this is TBD |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Bandpass_Center1 | 573.8 | nm | Central wavelength for bandpass 1 |
| CGI_Bandpass_FWHM1 | 56.5 | nm | Nominal FWHM (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 1 |
| CGI_Bandpass_Center2 | 659.4 | nm | Central wavelength for bandpass 2 |
| CGI_Bandpass_FWHM2 | 110.9 | nm | Nominal FWHM (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 2 |
| CGI_Bandpass_Center3 | 729.3 | nm | Central wavelength for bandpass 3 |
| CGI_Bandpass_FWHM3 | 122.3 | nm | Nominal FWHM (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3 |
| CGI_Bandpass_Center4 | 825.5 | nm | Central wavelength for bandpass 4 |
| CGI_Bandpass_FWHM4 | 96.8 | nm | Nominal FWHM (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 4 |
| CGI_Bandpass_ND_2pt25_FPAM | 102.25 | Attenuation factor of Neutral Density filter used for target acquisition (ND 2.25) mounted in FPAM | |
| CGI_Bandpass_ND_4pt75_FPAM | 104.75 | Attenuation factor of Neutral Density filter used for target acquisition (ND 4.75) mounted in FPAM | |
| CGI_Bandpass_ND_4pt75_FSAM | 104.75 | Attenuation factor of Neutral Density filter used for target acquisition (ND 4.75) mounted in FSAM |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Bandpass_Engineering_Center1a | 554.8 | nm | Central wavelength for engineering filter 1a (WFSC), Wavefront Sensing and Control (WFSC) |
| CGI_Bandpass_Engineering_FWHM1a | 18 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 1a |
| CGI_Bandpass_Engineering_Center1b | 574.5 | nm | Central wavelength for engineering filter 1b (WFSC) |
| CGI_Bandpass_Engineering_FWHM1b | 18 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 1b |
| CGI_Bandpass_Engineering_Center1c | 594.7 | nm | Central wavelength for engineering filter 1c (WFSC) |
| CGI_Bandpass_Engineering_FWHM1c | 19 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 1c |
| CGI_Bandpass_Engineering_Center2a | 614.2 | nm | Central wavelength for engineering filter 2a |
| CGI_Bandpass_Engineering_FWHM2a | 21.6 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 2a |
| CGI_Bandpass_Engineering_Center2b | 639.4 | nm | Central wavelength for engineering filter 2b |
| CGI_Bandpass_Engineering_FWHM2b | 15.1 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 2b |
| CGI_Bandpass_Engineering_Center2c | 656 | nm | Central wavelength for engineering filter 2c |
| CGI_Bandpass_Engineering_FWHM2c | 6.2 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 2c |
| CGI_Bandpass_Engineering_Center3a | 680.6 | nm | Central wavelength engineering filter 3a (Spectroscopy calibration) |
| CGI_Bandpass_Engineering_FWHM3a | 24.9 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3a |
| CGI_Bandpass_Engineering_Center3b | 702.3 | nm | Central wavelength engineering filter 3b (Spectroscopy calibration) |
| CGI_Bandpass_Engineering_FWHM3b | 23 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3b |
| CGI_Bandpass_Engineering_Center3c | 725.9 | nm | Central wavelength engineering filter 3c (Spectroscopy calibration) |
| CGI_Bandpass_Engineering_FWHM3c | 20 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3c |
| CGI_Bandpass_Engineering_Center3g | 752.5 | nm | Central wavelength engineering filter 3g (Spectroscopy calibration) |
| CGI_Bandpass_Engineering_FWHM3g | 24.1 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3g |
| CGI_Bandpass_Engineering_Center3d | 753.3 | nm | Central wavelength engineering filter 3d (Spectroscopy calibration) |
| CGI_Bandpass_Engineering_FWHM3d | 7.2 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3d |
| CGI_Bandpass_Engineering_Center3e | 777.1 | nm | Central wavelength engineering filter 3e (Spectroscopy calibration) |
| CGI_Bandpass_Engineering_FWHM3e | 27.1 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 3e |
| CGI_Bandpass_Engineering_Center4a | 791.7 | nm | Central wavelength for engineering filter 4a (WFSC) |
| CGI_Bandpass_Engineering_FWHM4a | 29.8 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 4a |
| CGI_Bandpass_Engineering_Center4b | 823.9 | nm | Central wavelength for engineering filter 4b (WFSC) |
| CGI_Bandpass_Engineering_FWHM4b | 28 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 4b |
| CGI_Bandpass_Engineering_Center4c | 856.5 | nm | Central wavelength for engineering filter 4c (WFSC) |
| CGI_Bandpass_Engineering_FWHM4c | 30.2 | nm | Nominal FWHM [nm] (from 50% peak transmission cut-on to 50% peak transmission cut-off wavelength) for bandpass 4c |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Detector_Model | T-e2v CCD 311 | Detector make and model | |
| CGI_Detector_Pixel_Number_X | 1056 | The EXCAM image array size in detector pixels in x-dimension for imaging and spectroscopy | |
| CGI_Detector_Pixel_Number_Y | 1037 | The EXCAM image array size in detector pixels in y-dimension for imaging and spectroscopy | |
| CGI_Detector_Pixel_Size | 13 | 10-6 m | Pixel size of CGI detector pixels in each dimension, both imaging and spectroscopy |
| CGI_Detector_Pixel_Scale | 0.0218 | arcsec/pixel | Coronagraph imaging pixel scale, Nyquist sampled (lambda/2D) at 500 nm |
| CGI_Detector_Readnoise | 120 | e- | Current best estimate read noise when using the electron multiplying (EM) gain in photon counting mode |
| CGI_Detector_Saturation | 50000 | e- | CGI detector full well requirement (EM gain dependent), assuming no EM gain applied |
| CGI_Detector_Dark_Current_BOL_CBE | 0.76 | e-/pixel/hr | CGI dark current for T = 168 K (beginning of life current best estimate) |
| CGI_Detector_Dark_Current_EOL_CBE | 0.77 | e-/pixel/hr | CGI dark current for T = 168 K (end of life current best estimate) |
| CGI_Detector_Dark_Current_BOL_REQ | 1.65 | e-/pixel/hr | CGI dark current for T = 168 K for 95% of all pixels (beginning of life requirement) |
| CGI_Detector_Dark_Current_EOL_REQ | 3.00 | e-/pixel/hr | CGI dark current for T = 168 K for 95% of all pixels (end of life requirement) |
| CGI_Detector_Clock_Induced_Charge_BOL | 0.01 | e-/pixel/frame | CGI clock-induced charge (beginning of life), 10 MHz horizontal frequency; 1 MHz vertical frequency; serial clock swing < 10 V |
| CGI_Detector_Clock_Induced_Charge_EOL | 0.02 | e-/pixel/frame | CGI clock-induced charge (end of life), 10 MHz horizontal frequency; 1 MHz vertical frequency; serial clock swing < 10 V |
| CGI_Detector_Quantum_Efficiency_Band1_REQ | 85 | % | The unity gain, imaging mode quantum efficiency at 580 nm shall be greater than 85% |
| CGI_Detector_Quantum_Efficiency_Band2_REQ | 75 | % | The unity gain, imaging mode quantum efficiency at 685 nm shall be greater than 75% |
| CGI_Detector_Quantum_Efficiency_Band3_REQ | 65 | % | The unity gain, imaging mode quantum efficiency at 730 nm shall be greater than 65% |
| CGI_Detector_Quantum_Efficiency_Band4_REQ | 35 | % | The unity gain, imaging mode quantum efficiency at 830 nm shall be greater than 35% |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Mode_Imaging_N | Narrow FoV imaging. Currently implemented as HLC coronagraph + Band 1 filter + imaging camera | ||
| CGI_Mode_Imaging_W | Wide FoV imaging. Currently implemented as SPC_A coronagraph + Band 4 filter + imaging camera | ||
| CGI_Imaging_FoV | 7.2 | arcsec | Unvignetted coronagraph imaging field-of-view diameter without coronagraph masks |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Spectroscopy_FoV | 4 | arcsec | Unvignetted FoV diameter without masks in each spectral channel |
| CGI_Spectroscopy_Footprint_Of_Dispersed_Point_Source_Band2 | 42x4 | pixels | Spectroscopic footprint of dispersed point source in pixels; the smaller axis (cross-dispersion) includes only the main lobe of the PSF |
| CGI_Spectroscopy_Footprint_Of_Dispersed_Point_Source_Band3 | 47x4 | pixels | Spectroscopic footprint of dispersed point source in pixels; the smaller axis (cross-dispersion) includes only the main lobe of the PSF |
| CGI_Spectroscopy_Band2_Short_Slit_Width | 0.115 | arcsec | Band 2 spectroscopy slit width for 2lambda/D wide, 6lambda/D long "short" slit |
| CGI_Spectroscopy_Band2_Short_Slit_Height | 0.345 | arcsec | Band 2 spectroscopy slit height for 2lambda/D wide, 6lambda/D long "short" slit |
| CGI_Spectroscopy_Band2_Tall_Slit_Width | 0.115 | arcsec | Band 2 spectroscopy slit width for 2lambda/D wide, 10lambda/D long "tall" slit |
| CGI_Spectroscopy_Band2_Tall_Slit_Height | 0.575 | arcsec | Band 2 spectroscopy slit height for 2lambda/D wide, 10lambda/D long "tall" slit |
| CGI_Spectroscopy_Band3_Short_Slit_Width | 0.127 | arcsec | Band 3 spectroscopy slit width for 2lambda/D wide, 6lambda/D long "short" slit |
| CGI_Spectroscopy_Band3_Short_Slit_Height | 0.381 | arcsec | Band 3 spectroscopy slit height for 2lambda/D wide, 6lambda/D long "short" slit |
| CGI_Spectroscopy_Band3_Tall_Slit_Width | 0.127 | arcsec | Band 3 spectroscopy slit width for 2lambda/D wide, 10lambda/D long "tall" slit |
| CGI_Spectroscopy_Band3_Tall_Slit_Height | 0.635 | arcsec | Band 3 spectroscopy slit height for 2lambda/D wide, 10lambda/D long "tall" slit |
| CGI_Spectroscopy_Bands23_Mean_Short_Slit_Width | 0.243 | arcsec | Bands 2-3 mean (695 nm) spectroscopy slit width for 4lambda/D wide, 6lambda/D long "short" slit |
| CGI_Spectroscopy_Bands23_Mean_Short_Slit_Height | 0.3645 | arcsec | Bands 2-3 mean (695 nm) spectroscopy slit height for 4lambda/D wide, 6lambda/D long "short" slit |
| CGI_Spectroscopy_Bands23_Mean_Tall_Slit_Width | 0.243 | arcsec | Bands 2-3 mean (695 nm) spectroscopy slit width for 4lambda/D wide, 10lambda/D long "tall" slit |
| CGI_Spectroscopy_Bands23_Mean_Tall_Slit_Height | 0.6075 | arcsec | Bands 2-3 mean (695 nm) spectroscopy slit height for 4lambda/D wide, 10lambda/D long "tall" slit |
| CGI_Spectroscopy_Spectral_Resolution | 50 | lambda/(delta lambda) | Spectral resolution at the centers of Band 2 (660 nm) and Band 3 (730 nm) |
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Polarimetry_FoV | 3.8 | arcsec | Unvignetted FoV diameter without masks in each polarization angle |
| CGI_Polarimetry_Wollaston_Prism1 | 0 and 90 | degrees | Polarization angles for the first Wollaston prism |
| CGI_Polarimetry_Wollaston_Prism2 | 45 and 135 | degrees | Polarization angles for the second Wollaston prism |
| Name | Value | Unit | Description |
|---|
| Name | Value | Unit | Description |
|---|---|---|---|
| CGI_Predicted_Performance_Imaging_N_Contrast_Pred | 2.94x10-9 | Predicted planet-to-star flux ratio for an SNR=5 imaging detection in band 1 with HLC, 100hr integration, after post-processing at a separation of 4.34lambda/D (=218.11 mas). This prediction is based on modeling and error budgeting of Nancy Grace Roman Space Telescope observatory and CGI, including: observatory and instrument stability during CGI con-ops, coronagraph starlight suppression performance, detector properties, and post-processing gains. Coronagraph and detector models have been validated against experimental results. Does not include model uncertainty factors on observatory or coronagraph performance (i.e., MUF=1) | |
| CGI_Predicted_Performance_Imaging_W_Contrast_Pred | 1.95x10-9 | Predicted planet-to-star flux ratio for an SNR=5 imaging detection in band 4 with SPC with FOV coronagraph based on OS6, 100hr integration, after post-processing at a separation of 6lambda/D (=432.63 mas). This prediction is based on modeling and error budgeting of Nancy Grace Roman Space Telescope observatory and CGI, including: observatory and instrument stability during CGI con-ops, coronagraph starlight suppression performance, detector properties, and post-processing gains. Coronagraph and detector models have been validated against experimental results. Does not include model uncertainty factors on observatory or coronagraph performance (i.e., MUF=1) | |
| CGI_Predicted_Performance_Spectroscopy_Contrast_Pred | 2.2x10-9 | Predicted planet-to-star flux ratio for an SNR=5 spectrum in band 3 with SPC_B (bowtie), 100hr integration, after post-processing at a separation of 4.39lambda/D (=280.09 mas). This prediction is based on modeling and error budgeting of Nancy Grace Roman Space Telescope observatory and CGI, including: observatory and instrument stability during CGI con-ops, coronagraph starlight suppression performance, detector properties, and post-processing gains. Coronagraph and detector models have been validated against experimental results. Does not include model uncertainty factors on observatory or coronagraph performance (i.e., MUF=1) | |
| CGI_Predicted_Performance_45offaxis_scattered_light | 3.4x10-9 | Scattered light flux ratio per resolution element from a source 45 arcsec off axis. Applicable to all coronagraph modes | |
| CGI_Predicted_Performance_100offaxis_scattered_light | 3.5x10-10 | Scattered light flux ratio per resolution element from a source 100 arcsec off axis. Applicable to all coronagraph modes |
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