It seems that there hasn’t been any detailed specifications of the scientific instruments of the now-about-to-be-rolled-to-launch-pad of the Chinese Tianwen-1 Mars Orbiter and @PRCMarsRover missions in English from anywhere I have seen - at least till now!
Thanks to @cathirame I finally get a detailed specifications list that I have crudely translated into English! Bear in mind that my UG physics were bad and the Chinese scientific terms used are a little bit different from my familar translations so the translation is crude. 😂
Source: LI Chunlai, LIU Jianjun, GENG Yan, CAO Jinbin, ZHANG Tielong, FANG Guangyou, YANG Jianfeng, SHU Rong, ZOU Yongliao, LIN Yangting, OUYANG Ziyuan. Scientific Objectives and Payload Configuration of China's First Mars Exploration Mission[J].
Journal of Deep Space Exploration, 2018, 5(5): 406-413. doi: 10.15982/j.issn.2095-7777.2018.05.002 
Firstly, here are the specifications of the 7 instruments of the TW-1 Mars Orbiter:
1. Medium Resolution Camera
Imaging wavelength: Visible Light
Color: Standard RGB
Image Resolution: < 100 m at 400 km altitude
Image swath: >= 400 km at 400 km altitude
Pixel Resolution: >= 4096 x 3072
Imaging wavelength: Visible Light
Color: Standard RGB
Image Resolution: < 100 m at 400 km altitude
Image swath: >= 400 km at 400 km altitude
Pixel Resolution: >= 4096 x 3072
2. High Resolution Camera
Image resolution: < 2.5 m (< 0.5 m in certain regions) multi-color; < 10 m (< 2.0 m in certain regions) panchromatic
Image swath: >= 9 km at 265 km altitude
Image resolution: < 2.5 m (< 0.5 m in certain regions) multi-color; < 10 m (< 2.0 m in certain regions) panchromatic
Image swath: >= 9 km at 265 km altitude
3. Mars orbiter sub-surface radar
Radar frequency: 10-20 & 30-50 MHz
Transmitter power: >= 100 W
Receiver power: <= -87 dBm
Maximum detection depth: ~100 m for Martian sub-surface soil (εr = 3.0~4.0); ~1000 m for Martian polar ice layers (εr = 3.0)
Depth resolution: ~ 1 m
Radar frequency: 10-20 & 30-50 MHz
Transmitter power: >= 100 W
Receiver power: <= -87 dBm
Maximum detection depth: ~100 m for Martian sub-surface soil (εr = 3.0~4.0); ~1000 m for Martian polar ice layers (εr = 3.0)
Depth resolution: ~ 1 m
4. Mars mineralogy spectrometer
Wavelength bands: Visible Light - NIR band 0.45~1.05 μm; NIR-MIR band 1.00~3.40 μm
Spectral resolution: < 10 nm for Visible Light - NIR band; < 12 nm for 1.0~2.0 μm; < 25 nm for 2.0~3.4 μm
Wavelength bands: Visible Light - NIR band 0.45~1.05 μm; NIR-MIR band 1.00~3.40 μm
Spectral resolution: < 10 nm for Visible Light - NIR band; < 12 nm for 1.0~2.0 μm; < 25 nm for 2.0~3.4 μm
5. Mars magnetometer
Measurement range: +- 2000 nT
Noise level <= 0.01 nT/√Hz
Resolution: <= 0.01 nT
Precision: 0.1 nT
Measurement range: +- 2000 nT
Noise level <= 0.01 nT/√Hz
Resolution: <= 0.01 nT
Precision: 0.1 nT
6. Mars ions and neutral particles analyser
Limit of Detection of low energy ions:
Energy range: 5 eV ~ 25 keV
delta-E/E: 15%
Mass: 1~ 70 amu
delta-m/m: 25%
POV: 90° x 360°
Angular resolution: 11.2° x 22.5°
Time resolution: 8s
Limit of Detection of low energy ions:
Energy range: 5 eV ~ 25 keV
delta-E/E: 15%
Mass: 1~ 70 amu
delta-m/m: 25%
POV: 90° x 360°
Angular resolution: 11.2° x 22.5°
Time resolution: 8s
Limit of Detection of low energy neutral particles:
Energy range: 50 eV ~ 3 keV
delta-E/E: 100%
Mass: 1 ~ 32 amu
POV: 15° x 160°
Angular resolution: 10° x 25°
Time resolution: 4s
Energy range: 50 eV ~ 3 keV
delta-E/E: 100%
Mass: 1 ~ 32 amu
POV: 15° x 160°
Angular resolution: 10° x 25°
Time resolution: 4s
7. Mars energetic particles analyser
Limit of Detection:
Energy range: 0.1 ~ 12 MeV (Electrons) / 2 ~100 MeV (Protons) / 25 ~ 300 MeV (Alpha Particles/Heavy Ions)
delta-E/E: 15%
Flux: 0 ~ 10^5 cm^-2 s^-1
Atomic Number: 1 <= Z <= 26 (H - Fe)
Limit of Detection:
Energy range: 0.1 ~ 12 MeV (Electrons) / 2 ~100 MeV (Protons) / 25 ~ 300 MeV (Alpha Particles/Heavy Ions)
delta-E/E: 15%
Flux: 0 ~ 10^5 cm^-2 s^-1
Atomic Number: 1 <= Z <= 26 (H - Fe)
delta-m/m: <=25% (Z <= 9, 25 ~ 300 MeV & 10 <= Z <= 26, 100 ~ 300 MeV); <=60% (10 <= Z <= 26, 25 ~ 100 MeV)
POV: 60°
Time resolution: 4s (Electrons, Protons, Alpha Particles); 60s (Heavy Ions)
POV: 60°
Time resolution: 4s (Electrons, Protons, Alpha Particles); 60s (Heavy Ions)
And here comes the 6 instruments on the yet-to-be-named @PRCMarsRover which will get a name via a planned public naming contest:
A. Terrain Camera
Imaging wavelength: Visible Light
Color: Standard RGB
Nominal imaging distance: 0.5 m ~ ∞
Pixel Resolution: 2048 x 2048
Imaging wavelength: Visible Light
Color: Standard RGB
Nominal imaging distance: 0.5 m ~ ∞
Pixel Resolution: 2048 x 2048
B. Multi-spectral camera
Imaging bands (/nm, Full Width At Half Maximum in brackets): 480 (20), 525 (20), 650 (12), 700 (15), 800 (25), 900 (30), 950 (50), 1000 (50)
Color: Multi-spectral
Nominal imaging distance: 1.5 m ~ ∞
Pixel Resolution: 2048 x 2048
Imaging bands (/nm, Full Width At Half Maximum in brackets): 480 (20), 525 (20), 650 (12), 700 (15), 800 (25), 900 (30), 950 (50), 1000 (50)
Color: Multi-spectral
Nominal imaging distance: 1.5 m ~ ∞
Pixel Resolution: 2048 x 2048
C. Rover sub-surface radar
Channel 1:
Median frequency: 55 MHz
Working bandwidth: 40 MHz
Penetrating depth of Martian ice layers: ~1 m
Maximum detection depth: >=10 m for Martian sub-surface soil (εr = 3.0~4.0); >=100 m for Martian polar ice layers (εr = 3.0)
Channel 1:
Median frequency: 55 MHz
Working bandwidth: 40 MHz
Penetrating depth of Martian ice layers: ~1 m
Maximum detection depth: >=10 m for Martian sub-surface soil (εr = 3.0~4.0); >=100 m for Martian polar ice layers (εr = 3.0)
Channel 2:
Median frequency: 1300 MHz
Working bandwidth: 1000 MHz
Precision of layer thickness detection: ~cm
Maximum detection depth: >=3 m for Martian sub-surface soil (εr = 3.0~4.0); >=10 m for Martian polar ice layers (εr = 3.0)
Median frequency: 1300 MHz
Working bandwidth: 1000 MHz
Precision of layer thickness detection: ~cm
Maximum detection depth: >=3 m for Martian sub-surface soil (εr = 3.0~4.0); >=10 m for Martian polar ice layers (εr = 3.0)
D. Mars surface composition analyser
LIBS measurements: Detects 10+ elements; optimal working distance from sample 2~5 m (max. 10 m); imaging resolution <= 100 μrad (0.2 mm @ 2 m; 0.5 mm @ 5 m)
NIR measurments (850~2400 nm): spectral resolution <=12 nm; 130+ bands; POV >=1 mrad
LIBS measurements: Detects 10+ elements; optimal working distance from sample 2~5 m (max. 10 m); imaging resolution <= 100 μrad (0.2 mm @ 2 m; 0.5 mm @ 5 m)
NIR measurments (850~2400 nm): spectral resolution <=12 nm; 130+ bands; POV >=1 mrad
E. Mars surface magnetometer
Measurement range: +- 2000 nT
Noise level <= 0.01 nT/√Hz
Resolution: <= 0.01 nT
Stability: <= 0.01 nT/°C
Sampling rate: 1/16/32/128 Hz
Range: +- 65000 nT
Measurement range: +- 2000 nT
Noise level <= 0.01 nT/√Hz
Resolution: <= 0.01 nT
Stability: <= 0.01 nT/°C
Sampling rate: 1/16/32/128 Hz
Range: +- 65000 nT
F. Mars meteorology instrument
Temperature -120~50 °C (precision 0.1 °C); Pressure 1~1500 Pa (precision 0.1 Pa); Windspeed 0~70 m/s (precision 0.1 m/s); Wind Direction 0°~360° (precision 5°); Sound detection 20 Hz~2.5 kHz/2.5~20 kHz (Sensibility >50 mV/Pa; Dynamic Range >=90 dB)
Temperature -120~50 °C (precision 0.1 °C); Pressure 1~1500 Pa (precision 0.1 Pa); Windspeed 0~70 m/s (precision 0.1 m/s); Wind Direction 0°~360° (precision 5°); Sound detection 20 Hz~2.5 kHz/2.5~20 kHz (Sensibility >50 mV/Pa; Dynamic Range >=90 dB)
Hopefully this will be useful for interpreting what abilities the orbiter and rover will have and also assists in public data analysis when they come later. 😀 @elakdawalla @AJ_FI @doug_ellison @NASASpaceflight @plutogno @planet4589 @girlandkat
