Infrared and Laser Engineering, Volume. 53, Issue 3, 20230547(2024)
Advances in ultraviolet polarization detection for space astronomy
Figures & Tables(15)
Fig. 4. Working principle diagram of polarization system with different phase modulation methods
Fig. 9. Comparison of quantum efficiency in the UV band for different types of detectors
Table 1. Typical space astronomy UV polarization loads
View tableView in ArticleTable 1. Typical space astronomy UV polarization loads
Mission Main country Launch time Instrument Target Interkosmos 16 Sweden 1976 UVSP VUV linear polarization in Solar transition zone, etc.[ 8 ,35 ]SMM USA 1980 UVSP Solar flares, solar active regions, solar corona, etc.[ 36 –37 ]SUMI USA 2012 SUMI Chromosphere, solar transition region magnetic field, etc.[ 19 ]CLASP Japan 2015 CLASP Upper solar chromosphere, transition region, etc.[ 13 ,15 ]CLASP-2 Japan 2019 CLASP Upper solar chromosphere, transition region, etc.[ 38 ]CLASP-2.1 Japan 2021 CLASP Upper solar chromosphere, transition region, etc.[ 38 ]Pioneer Venus Orbiter USA 1978 OCPP Venus cloud layers, physical characteristics of aerosol particles in the atmosphere, and vertical distribution of aerosols, etc.[ 39 ]Hubble telescope USA 1990 FOS Active galaxies, quasars, and planetary nebulae, etc.[ 40 –43 ]ASTRO-1 USA 1990 WUPPE Interstellar dust, hot stars, material in the solar system, active galaxies, etc.[ 44 ]ASTRO-2 USA 1995 WUPPE Interstellar dust, hot stars, material in the solar system, active galaxies, etc.[ 44 ]WISP USA 1997 WISP Diffuse nebula, dust nebula, Crab Nebula , etc.[ 1 ,45 ]CUPID USA Unknown CUPID Cosmic background , etc.[ 1 ]FUSP USA Unknown FUSP Hot star systems, circumstellar disks , etc.[ 1 ]SUNRISE III Germany Pending SUSI Solar atmosphere, etc.[ 46 ]ARAGO Europe Under planning ARAGO Stellar-planetary interactions, etc.[ 47 –48 ]LUVOIR USA Under planning POLLUX Circumstellar disk, interstellar magnetic fields, etc.[ 49 –52 ]SolmeX Europe Under planning EIP; SUSP; ChroME; CUSP The structure of the solar outer atmosphere magnetic field, magnetic field variations, and magnetic field-derived effects, etc.[ 53 ]Polstar USA Under planning Polstar Circumstellar disk, interstellar magnetic fields, etc.[ 54-55 ]
Table 2. Parameters of typical space astronomy UV polarization load
View tableView in ArticleTable 2. Parameters of typical space astronomy UV polarization load
Parameter instrument Instrument type Wavelength/nm Spectral resolution/nm Stokes parameter Polarimetry precision Interkosmos 16 Spectro-polarimeter 120-150 3.9 I Q U 10−2 SMM-UVSP Spectro-polarimeter 115-360 0.002-0.004 I V 10−2 SUMI Spectro-polarimeter C IV(155) Mg II(280) 0.05@ C IV 0.08@ Mg II I Q U V 10−3 CLASP Spectro-polarimeter Ly-α(121.6) 0.01 I Q U 10−3 CLASP2/2.1 Spectro-polarimeter Mg II(280) 0.01 I Q U V 10−3 Pioneer Venus Orbiter-OCPP Photo-polarimeter 270, 365 ~18 I Q U 10−3 HST-FOS Spectro-polarimeter 115-850 ＞0.25 I Q U V 10−2 ASTRO1/2-WUPPE Spectro-polarimeter 135-330 0.6 I Q U V 10−3 WISP Photo-polarimeter 135-260 40 I Q U - CUPID Photo-polarimeter 118-161 20 I Q U 10−2 FUSP Spectro-polarimeter 105-150 0.07 I Q U 10−3 SUNRISE III-SUSI Spectro-polarimeter 300-410 0.001 I Q U V 10−3 ARAGO Spectro-polarimeter 119-888 >0.009 I Q U V - LUVOIR-POLLUX Spectro-polarimeter 90-400 0.002 I Q U V 10−4 SolmeX-CUSP Spectro-polarimeter 95-125 0.009 I Q U 10−2 SolmeX-EIP Photo-polarimeter Fe X(17.4) 0.35 I Q U 10−3 SolmeX-SUSP Spectro-polarimeter 115-155 0.0066 I Q U V 10−3 SolmeX-ChroME Spectro-polarimeter Mg II(279) 0.005 I Q U V 10−3 MIDEX-Polstar Spectro-polarimeter 122-320 ＞0.005 I Q U V 10−3
Table 3. Typical spectral range of space astrophysical UV polarization payloads and key components
View tableView in ArticleTable 3. Typical spectral range of space astrophysical UV polarization payloads and key components
Parameter instrument Wavelength/nm UV coating Detector Interkosmos 16 120-150 Al+MgF2 Au PMT SMM-UVSP 115-360 Al+MgF2 PMT SUMI C IV(155) Mg II(280) HfO2/SiO2/MgF2/LaF3 Dielectric coating BICCD CLASP Ly-α(121.6) Al+MgF2 Frame-transfer CCD CLASP2/2.1 Mg II(280) Al+MgF2 CCD Pioneer Venus Orbiter-OCPP 270, 365 SiO2/MgF2+Al UV-enhanced silicon photodiode HST-FOS 115-850 Al+Al2 O3 Digicon photon detector ASTRO1/2-WUPPE 135-330 Al+MgF2 Reticon photodiode array WISP 135-260 Al+MgF2 Thinned CCD CUPID 118-161 Al+MgF2 Thinned CCD FUSP 105-150 Al+LiF Thinned CCD SUNRISE III-SUSI 300-410 Al BICCD ARAGO 119-888 Al+MgF2 δ-CMOS LUVOIR-POLLUX 90-400 Al+MgF2+SiC δ-CCD SolmeX-CUSP 95-125 - ICCD SolmeX-EIP Fe X(17.4) Al+B4 C+Mo BTCCD SolmeX-SUSP 115-155 - ICMOS SolmeX-ChroME Mg II(279) - - MIDEX-Polstar 122-320 Al +MgF2 CCD
Table 4. Advantages and disadvantages of common polarization modulation methods
View tableView in ArticleTable 4. Advantages and disadvantages of common polarization modulation methods
Polarization modulation Modulation device Advantages Disadvantages Mechanical Modulation RWP Broader working spectral range, suitable for most UV regime; Stable in time Moving parts increase mass, power consumption and vibrations; Modulation frequency is mechanically limited by the retarder rotating speed Electro-optic modulation LCVR, FLC, DFLC High modulation frequency; Large aperture; Low power consumption Limited in-orbit application; Not suitable for most UV regime Acousto-optic modulation PEM Broader working spectral range(VUV-IR) No full-Stokes modulator has been developed; Small aperture Reflective modulation Brewster angle reflectors Suitable for FUV/EUV regime Complex structure, hard to install; large weight and volume
Table 5. Commonly used polarizing beam splitters in the UV band
View tableView in ArticleTable 5. Commonly used polarizing beam splitters in the UV band
Device Discription Working diagram Application Beam splitter cube Two beams output at a large angle and imagedin two separate detectors SUNRISE III-SUSI, SolmeX-ChroME Wollaston prism Output beams are refracted at nearly opposite angles HST-FOS, ASTRO1/2-WUPPE, ARAGO, LUVOIR-POLLUX(MUV/NUV), MIDEX-polstar Double Wollaston prism Two Wollaston prisms are combined, the first one acts as beam splitter while the second one produces two parallelbeams at the output SUMI, Pioneer venus orbiter-OCPP Brewster plane Beamsplitting is accomplished by two reflections on twoMgF2 birefringent plates placed at the Brewster angle Interkosmos 16, SMM-UVSP, SolmeX-SUSP, LUVOIR-POLLUX(FUV), CLASP Wire-grid polarizer By employing a structure with fine metal grids, selectively allow light of specific orientations to pass through CLASP2/2.1, SolmeX-EIP
Table 6. Advantages and disadvantages of different solid UV detectors
View tableView in ArticleTable 6. Advantages and disadvantages of different solid UV detectors
Device Advantages Disadvantages EMCCD High sensitivity; low noise; high frame rate; high dynamic range High cost; limited dynamic range compared to CCD and sCMOS; limited lifespan; limited resolution sCMOS High sensitivity; high frame rate; high dynamic range; large FOV High cost; limited lifespan; limited resolution; sensitivity to cosmic rays, leading to potential image artifacts or data loss CCD High sensitivity; high dynamic range; low noise Low readout speed; high power consumption; high cost; limited resolution CMOS Low power consumption; low cost; high frame rate; high resolution; large FOV Low sensitivity; low dynamic range; high noise
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Ruiyan Shan, Lianqing Dong, Kang Li, Muyao Zhang, Guoxian Zheng, Zhuo Zhang, Lixin Yang, Junjie Shao. Advances in ultraviolet polarization detection for space astronomy[J]. Infrared and Laser Engineering, 2024, 53(3): 20230547
Paper Information
Category: Space optics
Received: Sep. 22, 2023
Accepted: --
Published Online: Jun. 21, 2024
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