The Mid-Infrared Imager Spectrometer Coronagraph (MISC)
for Origins Space Telescope (OST)
"Origins Space Telescope (OST) MISC Instrument Presentation" at Instrument Interface Meeting on June 13, 2017 (pdf)
"Origins Space Telescope (OST) MISC Instrument Summary" (pdf)
"Origins Space Telescope (OST) MISC Instrument Presentation" at Instrument Interface Meeting on September 14, 2017 (pdf)
"Origins Space Telescope (OST) Mid-Infrared Imager, Spectrometer, Coronagraph (MISC)" at AKARI 4th International Conference on October 18, 2017 (pdf)
OSTwithFIPprelimupdate_misc-all_170823_64.exe (3D data; MISC-Imager and Spectrometer, MISC-Coronagraph and MISC-Transit Spectrometer)
OSTwithFIPprelimupdate_misc-all_170823_64.exe.gz (3D data; MISC-Imager and Spectrometer, MISC-Coronagraph and MISC-Transit Spectrometer)
OSTwithFIPprelimupdate_misc-all_170823.STEP (3D data; MISC-Imager and Spectrometer, MISC-Coronagraph and MISC-Transit Spectrometer)
Optical Design of MISC MIR Imager and Spectrometer Module, MISC Coronagraph Module and MISC Transit Spectrometer Module;
Deformable Mirror (DM) + Tip-Tilt Mirror (TTM)
- Type of Coronagraph; PIAACMC
[A-2] Normal Imaging and Spectroscopy Channel (WFI, MRS, HRS)
[A-3] Transit Channel (TRA)
- 2 x "1kx1k Si:Sb Detector Array"
- 1 x "2kx2k Si:Sb Detector Array"
【Block Diagram】
【Optical Design (ver. 2017/06/12)】(prepared by Dr. Naofumi Fujishiro)
Optical Design of MISC Coronagraph channel ;
OST_MISC_COR_20170612.pdf
Download CAD Data (COR-S)
Download ZEMAX Data (COR-S)
Download ZDA Data (COR-S)
Download CAD Data (COR-L)
Download ZEMAX Data (COR-L)
Download ZDA Data (COR-L)
【design concept】
- Wavelength Coverage; 6-16um for COR-S, 15-38um for COR-L
- Detector 2k x 2k Si:As for COR-S, 1k x 1k Si:Sb for COR-L
- Plate scale;
0”.05 for COR-S (Airy FWHM at 7um (0”.2) spans 4 pixels)
0”.1 for COR-L (Airy FWHM at 14um (0”.4) spans 4 pixels)
- FOV;
5.5 arcsec x 5.5 arcsec for COR-S
5.5 arcsec x 5.5 arcsec for COR-L
(corrsponding to 16λ/D x 16λ/D at 15µm)
- Length of the slit; 5.5” for COR-S, 5.5” for COR-L
- Width of the slit;
0”.26 for WFC-SG1 (PSF FWHM at 10um, R=300)
0”.40 for WFC-SG2 (PSF FWHM at 15um, R=300)
0”.65 for WFC-LG1 (PSF FWHM at 25um, R=300)
1”.00 for WFC-LG2 (PSF FWHM at 38um, R=300)
- 0.75-0.95λ/D for the IWA of OST/MISC
(for D=9m, λ=9µm, IWA is 0.15-0.20 arcsec)
- Contrast at the IWA (based on Guyon et al. 2014)
average contrast in 0.88-3.6λ/D --> 7.07E-6 for 10% band, 1.16E-6 for 4% band (@1.65um)
to the Mid-Infrared Camera and Spectrometers (MCS; Kataza, H., et al. 2012)
studied for old SPICA mission.
【Block Diagram】
【Conceptual Design (Schematics)】
【Optical Design (ver. 2017/06/08)】(prepared by Dr. Yuji Ikeda)
Optical Desgn of MISC Normal Imager and Spectrometer channel (WFI, MRS, HRS)
updated taking account of the allocated volume for MISC.
misc_opt_170608_64.exe (3D data; WFI-S, WFI-L, HRS-S, HRS-L, MRS-S, MRS-M, MRS-L)
misc_opt_170608_64.exe.gz (3D data; WFI-S, WFI-L, HRS-S, HRS-L, MRS-S, MRS-M, MRS-L)
OSTwithFIPprelimupdate_misc-im_170608.STEP (3D data; WFI-S, WFI-L, HRS-S, HRS-L, MRS-S, MRS-M, MRS-L)
Camera without lens (MIRACLE; Wada, T., et al. 2010) studied for old SPICA mission,
except for the WFC system in the foreoptics.
【Design Concept】
- Wavelength coverage; 6-16um for WFI-S, 15-38um for WFI-L
- Detector; 2k x 2k Si:As for WFI-S, 2k x 2k Si:Sb for WFI-L
- Plate scale;
0”.088 for WFI-S (Airy FWHM at 7um (0”.2) spans 2.27 pixels)
0”.088 for WFI-L (Airy FWHM at 14um (0”.4) spans 4.54 pixels)
- FOV; 3 arcmin x 3 arcmin for WFI-S, 3 arcmin x 3 arcmin for WFI-L
- Low-resolution long-slit spectroscopy (R~150-300) is possible by using grisms
- Slit length; 180” for WFI-S, 180” for WFI-L
- Width of the slit;
0”.26 for WFI-SG1 (PSF FWHM at 10um, R=300)
0”.40 for WFI-SG2 (PSF FWHM at 15um, R=300)
0”.65 for WFI-LG1 (PSF FWHM at 25um, R=300)
1”.00 for WFI-LG2 (PSF FWHM at 38um, R=300)
to Medium Reolution Spectrometer (MRS; Sakon, I., et al. 2010; 2012)
studied for old SPICA mission.
【Design Concept】
- No moving parts
- the same FOV is shared between MRS-S, MRS-M and MRS-L via beamsplitter
BS#1; reflection <18.5um [MRS-S & MRS-M] / transmission 18.5-37um [MRS-L]
BS#2; reflection <9.7um [MRS-S] / transmission 9.7-19µm - Spectral resolving power; R=1000-3000 for MRS-S, R=1000-3000 for MRS-L
- Plate scale; 0.0615 arcsec/pix for MRS-S, 0.10 arcsec/pix for MRS-M, and 0.15 arcsec/pix for MRS-L
- Spectral resolving power; R~1000 for MRS-S, R~1000 for MRS-L
- IFU format and FOV;
3 arcsec (length) x 0.33 arcsec (width) x 11 (# of slices) [IFU FOV; 3 arcsec x 3.6 arcsec (MRS-S)]
3 arcsec (length) x 0.55 arcsec (width) x 9 (# of slices) [IFU FOV; 3 arcsec x 5 arcsec (MRS-M)]
3 arcsec (length) x 1.00 arcsec (width) x 5 (# of slices) [IFU FOV; 3 arcsec x 5 arcsec (MRS-M)]
- Detector; 2k x 2k Si:As for MRS-S and MRS-M, 1k x 1k Si:Sb for MRS-L
Note: The present design covers 10-37um with MRS-M and MRS-L (baseline) and 5-37 with MRS-S, MRS-M and MRS-L (goal). This helps meet the science case #18, Galaxy Feedback from SNe and AGN to z~3 which needs this spectral coverage for 20-350 um.
the similar design to the High Reolution Spectrometer (HRS; Kobayashi, N., et al. 2008;
Sarugaku, Y., et al. 2012) studied for old SPICA mission.
【Design Conept】
- Wavelength coverage; 12-18um for HRS-S, 25-35um for HRS-L
- Detector; 2k x 2k Si:As for HRS-S, 1k x 1k Si:Sb for HRS-L
- Spectral Resolving Power; R=20,000-30,000
- Plate scale; 0”.17 for HRS-S, 0”.34 for HRS-L
- Slit width; 0”.5 for HRS-S, 0”.94 for HRS-L
Note: Science case #9 (Water content of planet-forming disks) and #15 ( Direct detection of protoplanetary disk mass) requested R>25,000 for 25-200um. Development of immersion grating for 25-38um is needed to achieve HRS-L capability. Science case #5 (Galaxy feedback mechanisms at z<1) requested R=10,000 for 10-500um. This design provides part of that wavelength coverage. Science gap assessment needed.
as a transit spectroscopic function for MISC is shown below.
【Feasibility Study Report (ver. 2017/08/30)】(prepared by Dr. Taro Matsuo)
OST/MISC Transit Spectrometer Module (OST_MISC_TRANSIT_Feasibility_Study_v1_20170830.pdf)
【Sensitivity Analysis (ver. 2017/10/04)】(prepared by Dr. Taro Matsuo)
The Sensitivity for the OST/MISC Transit Spectrometer Module with a calibration technique of the gain fluctuation (sensitivity_for_OST_transit_spectrograph_calibration.pdf)
【Block Diagram】
【Optical Design (ver. 2017/06/12)】(prepared by Dr. Taro Matsuo)
OST/MISC Transit Spectrometer channel ;
Download CAD Data (TRA-S)
Download ZEMAX Data (TRA-S)
Download CAD Data (TRA-M)
Download ZEMAX Data (TRA-M)
Download CAD Data (TRA-L)
Download ZEMAX Data (TRA-L)
【Design Concept】
- Wavelength coverage; 6-10.5µm for TRA-S, 10-18µm for TRA-M, 17.5-25µm for TSC-L
- Detector; 2k x 2k Si:As for TRA-S, 2k x 2k Si:As for TRA-M, 2k x 2k Si:As for TRA-L
- Spectral resolution; R~100 for TRA-S and TRA-M, R~300 for TRA-L
- Photometric precision; 3--5 ppm (a few x 10^-6)
- Full Field of View; 3 arcsec x 3 arcsec
for Origins Space Telescope (OST)
version 2017.10.16 (Itsuki Sakon)
Presentation Material on OST/MISC
"Origins Space Telescope (OST) MISC Instrument Presentation" at STDT F2F Meeting on March 21-22, 2017 (pdf)"Origins Space Telescope (OST) MISC Instrument Presentation" at Instrument Interface Meeting on June 13, 2017 (pdf)
"Origins Space Telescope (OST) MISC Instrument Summary" (pdf)
"Origins Space Telescope (OST) MISC Instrument Presentation" at Instrument Interface Meeting on September 14, 2017 (pdf)
"Origins Space Telescope (OST) Mid-Infrared Imager, Spectrometer, Coronagraph (MISC)" at AKARI 4th International Conference on October 18, 2017 (pdf)
Fact Sheet of OST/MISC
Black Box Input
Black_Box_Input_MISC_20170901.xlsxMaster Equipment List (OST/MISC)
OST_MEL_MISC_V10.xlsxThe Latest Result of Optical and Structural Design of OST/MISC (ver. 2017/08/24)
Optical Desgn of MISC; MISC Imager and Spectrometer Module + MISC Coronagraph Module + MISC Transit Spectrometer ModuleOSTwithFIPprelimupdate_misc-all_170823_64.exe (3D data; MISC-Imager and Spectrometer, MISC-Coronagraph and MISC-Transit Spectrometer)
OSTwithFIPprelimupdate_misc-all_170823_64.exe.gz (3D data; MISC-Imager and Spectrometer, MISC-Coronagraph and MISC-Transit Spectrometer)
OSTwithFIPprelimupdate_misc-all_170823.STEP (3D data; MISC-Imager and Spectrometer, MISC-Coronagraph and MISC-Transit Spectrometer)
Optical Design of MISC MIR Imager and Spectrometer Module, MISC Coronagraph Module and MISC Transit Spectrometer Module;
The Structural Design and Mass Estimates of OST/MISC (ver. 2017/07/24)
1. MISC Imager and Spectrometer Module
2. MISC Transit Spectrometer Module
3. MISC Coronagraph Module
Optical Design Forms of Case A (full capability)
1. Basic Concept
- Wave Front Control (WFC) System in the fore-optics;Deformable Mirror (DM) + Tip-Tilt Mirror (TTM)
- Type of Coronagraph; PIAACMC
2. Configuration
[A-1] Coronagraph Channel (COR)[A-2] Normal Imaging and Spectroscopy Channel (WFI, MRS, HRS)
[A-3] Transit Channel (TRA)
3. Resources
Detectors
- 8 x "2kx2k Si:As Detector Array"- 2 x "1kx1k Si:Sb Detector Array"
- 1 x "2kx2k Si:Sb Detector Array"
4. Design Ideas
4.1 [A-1] Coronagraph Channel (COR-S, COR-L)
PIAA Complex Mask Lyot Coronagraph (PIAACMC; Guyon, O., et al. 2010; 2014 )【Block Diagram】
【Optical Design (ver. 2017/06/12)】(prepared by Dr. Naofumi Fujishiro)
Optical Design of MISC Coronagraph channel ;
OST_MISC_COR_20170612.pdf
Download CAD Data (COR-S)
Download ZEMAX Data (COR-S)
Download ZDA Data (COR-S)
Download CAD Data (COR-L)
Download ZEMAX Data (COR-L)
Download ZDA Data (COR-L)
【design concept】
- Wavelength Coverage; 6-16um for COR-S, 15-38um for COR-L
- Detector 2k x 2k Si:As for COR-S, 1k x 1k Si:Sb for COR-L
- Plate scale;
0”.05 for COR-S (Airy FWHM at 7um (0”.2) spans 4 pixels)
0”.1 for COR-L (Airy FWHM at 14um (0”.4) spans 4 pixels)
- FOV;
5.5 arcsec x 5.5 arcsec for COR-S
5.5 arcsec x 5.5 arcsec for COR-L
(corrsponding to 16λ/D x 16λ/D at 15µm)
- Length of the slit; 5.5” for COR-S, 5.5” for COR-L
- Width of the slit;
0”.26 for WFC-SG1 (PSF FWHM at 10um, R=300)
0”.40 for WFC-SG2 (PSF FWHM at 15um, R=300)
0”.65 for WFC-LG1 (PSF FWHM at 25um, R=300)
1”.00 for WFC-LG2 (PSF FWHM at 38um, R=300)
- 0.75-0.95λ/D for the IWA of OST/MISC
(for D=9m, λ=9µm, IWA is 0.15-0.20 arcsec)
- Contrast at the IWA (based on Guyon et al. 2014)
average contrast in 0.88-3.6λ/D --> 7.07E-6 for 10% band, 1.16E-6 for 4% band (@1.65um)
4.2 [A-2] Normal Imager and Spectrometers Channel
A part of normal imager and spectrometer modules for MISC has the similar designto the Mid-Infrared Camera and Spectrometers (MCS; Kataza, H., et al. 2012)
studied for old SPICA mission.
【Block Diagram】
【Conceptual Design (Schematics)】
【Optical Design (ver. 2017/06/08)】(prepared by Dr. Yuji Ikeda)
Optical Desgn of MISC Normal Imager and Spectrometer channel (WFI, MRS, HRS)
updated taking account of the allocated volume for MISC.
misc_opt_170608_64.exe (3D data; WFI-S, WFI-L, HRS-S, HRS-L, MRS-S, MRS-M, MRS-L)
misc_opt_170608_64.exe.gz (3D data; WFI-S, WFI-L, HRS-S, HRS-L, MRS-S, MRS-M, MRS-L)
OSTwithFIPprelimupdate_misc-im_170608.STEP (3D data; WFI-S, WFI-L, HRS-S, HRS-L, MRS-S, MRS-M, MRS-L)
4.2.1 [A-2.a] Wide Field Imager Channel (WFI-S, WFI-L)
Wide Field Imager (WFI-S, WFI-L) for MISC has the similar design to Mid-InfraredCamera without lens (MIRACLE; Wada, T., et al. 2010) studied for old SPICA mission,
except for the WFC system in the foreoptics.
【Design Concept】
- Wavelength coverage; 6-16um for WFI-S, 15-38um for WFI-L
- Detector; 2k x 2k Si:As for WFI-S, 2k x 2k Si:Sb for WFI-L
- Plate scale;
0”.088 for WFI-S (Airy FWHM at 7um (0”.2) spans 2.27 pixels)
0”.088 for WFI-L (Airy FWHM at 14um (0”.4) spans 4.54 pixels)
- FOV; 3 arcmin x 3 arcmin for WFI-S, 3 arcmin x 3 arcmin for WFI-L
- Low-resolution long-slit spectroscopy (R~150-300) is possible by using grisms
- Slit length; 180” for WFI-S, 180” for WFI-L
- Width of the slit;
0”.26 for WFI-SG1 (PSF FWHM at 10um, R=300)
0”.40 for WFI-SG2 (PSF FWHM at 15um, R=300)
0”.65 for WFI-LG1 (PSF FWHM at 25um, R=300)
1”.00 for WFI-LG2 (PSF FWHM at 38um, R=300)
4.2.2 [A-2.b] Medium Resolution Spectrometer Channel (MRS-S, MRS-L)
Medium Resolution Spectrometer (MRS-S, MRS-L) for MISC has the similar designto Medium Reolution Spectrometer (MRS; Sakon, I., et al. 2010; 2012)
studied for old SPICA mission.
【Design Concept】
- No moving parts
- the same FOV is shared between MRS-S, MRS-M and MRS-L via beamsplitter
BS#1; reflection <18.5um [MRS-S & MRS-M] / transmission 18.5-37um [MRS-L]
BS#2; reflection <9.7um [MRS-S] / transmission 9.7-19µm - Spectral resolving power; R=1000-3000 for MRS-S, R=1000-3000 for MRS-L
- Plate scale; 0.0615 arcsec/pix for MRS-S, 0.10 arcsec/pix for MRS-M, and 0.15 arcsec/pix for MRS-L
- Spectral resolving power; R~1000 for MRS-S, R~1000 for MRS-L
- IFU format and FOV;
3 arcsec (length) x 0.33 arcsec (width) x 11 (# of slices) [IFU FOV; 3 arcsec x 3.6 arcsec (MRS-S)]
3 arcsec (length) x 0.55 arcsec (width) x 9 (# of slices) [IFU FOV; 3 arcsec x 5 arcsec (MRS-M)]
3 arcsec (length) x 1.00 arcsec (width) x 5 (# of slices) [IFU FOV; 3 arcsec x 5 arcsec (MRS-M)]
- Detector; 2k x 2k Si:As for MRS-S and MRS-M, 1k x 1k Si:Sb for MRS-L
Note: The present design covers 10-37um with MRS-M and MRS-L (baseline) and 5-37 with MRS-S, MRS-M and MRS-L (goal). This helps meet the science case #18, Galaxy Feedback from SNe and AGN to z~3 which needs this spectral coverage for 20-350 um.
4.2.3 [A-2.c] High Resolution Spectrometer Channel (HRS-S, HRS-L)
The short-wave module of High Resolution Spectrometer (HRS-S) for MISC hasthe similar design to the High Reolution Spectrometer (HRS; Kobayashi, N., et al. 2008;
Sarugaku, Y., et al. 2012) studied for old SPICA mission.
【Design Conept】
- Wavelength coverage; 12-18um for HRS-S, 25-35um for HRS-L
- Detector; 2k x 2k Si:As for HRS-S, 1k x 1k Si:Sb for HRS-L
- Spectral Resolving Power; R=20,000-30,000
- Plate scale; 0”.17 for HRS-S, 0”.34 for HRS-L
- Slit width; 0”.5 for HRS-S, 0”.94 for HRS-L
Note: Science case #9 (Water content of planet-forming disks) and #15 ( Direct detection of protoplanetary disk mass) requested R>25,000 for 25-200um. Development of immersion grating for 25-38um is needed to achieve HRS-L capability. Science case #5 (Galaxy feedback mechanisms at z<1) requested R=10,000 for 10-500um. This design provides part of that wavelength coverage. Science gap assessment needed.
4.3 [A-3] Transit Spectroscopic Channel
An idea to employ the densified pupil spectrometer (Matsuo, T., et al. 2016)as a transit spectroscopic function for MISC is shown below.
【Feasibility Study Report (ver. 2017/08/30)】(prepared by Dr. Taro Matsuo)
OST/MISC Transit Spectrometer Module (OST_MISC_TRANSIT_Feasibility_Study_v1_20170830.pdf)
【Sensitivity Analysis (ver. 2017/10/04)】(prepared by Dr. Taro Matsuo)
The Sensitivity for the OST/MISC Transit Spectrometer Module with a calibration technique of the gain fluctuation (sensitivity_for_OST_transit_spectrograph_calibration.pdf)
【Block Diagram】
【Optical Design (ver. 2017/06/12)】(prepared by Dr. Taro Matsuo)
OST/MISC Transit Spectrometer channel ;
Download CAD Data (TRA-S)
Download ZEMAX Data (TRA-S)
Download CAD Data (TRA-M)
Download ZEMAX Data (TRA-M)
Download CAD Data (TRA-L)
Download ZEMAX Data (TRA-L)
【Design Concept】
- Wavelength coverage; 6-10.5µm for TRA-S, 10-18µm for TRA-M, 17.5-25µm for TSC-L
- Detector; 2k x 2k Si:As for TRA-S, 2k x 2k Si:As for TRA-M, 2k x 2k Si:As for TRA-L
- Spectral resolution; R~100 for TRA-S and TRA-M, R~300 for TRA-L
- Photometric precision; 3--5 ppm (a few x 10^-6)
- Full Field of View; 3 arcsec x 3 arcsec