Radio Channel Model Tuning

Radio propagation channel Model tuning overview Peter Cheung Mentum (HK) 29 Sep 2009

Overview of propagation model used in planet

• Input – Scanner or CW drive test – Map, projection – Site configurations used (e.g, link budget, GPS)

• Planet general model (PGM) – Slope based Okumura-Hata type model

• CRC- predict4 model – Deterministic (i.e., map dependent, instead of survey), physical-optics based model

• Universal model (UM) – Additional license required – Unmasked and masked version – Unmasked means that antenna correction is done by planet prediction engine, instead of UM calculation 2

PGM overview – (1)

PGM overview – (2)

This is why only CW should be used for PGM tuning, since only CW can estimate K2 slope accurately

• Account for FSL – K1 (freq-dependent intercept), – K2 (slope) – K5 (multiplier for effective antenna height)

• Effective antenna height gain – BTS ht gain side as K3 – MS ht gain as K6 – Use absolute spot height as effective base station height

• Clutter effect – Weight factor K in last 1km to rx

• Diffraction – multiply by K4 for non-LOS – Calculation based on Epstein-Peterson method for 3 diffracting edge – Use clutter height evaluate diffraction for non-LOS – Use Clutter separation as distance between last effective diffracting clutter obstruction to rx antenna

PGM tuning • PGM only compute vertical diffraction – In DU/U environment where horizontal diffraction can be significant, PGM often over-estimate vertical diffraction loss – Compensate with clutter gain – PGM effective where BTS ht >= surrounding clutter • Using AMT – manual • Use Hata for K3 and K5, clutter offset = optimize • Optimize K1, K2 and K4 – smart • Optimize K1 to K5 and CAL in one pass – Optional 2nd step • Fix tuned K and using clutter tuner to re-tune CAL or do manual change

CRC--predict4 CRC

Clutter effect specified as clear distance and obstacle height to receiver Map pixel

Huygen principle (vector summation of secondary radiation sources)

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Comparison of PGM and CRC predict4 PGM

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CRC predict

Application

Urban to suburban

Accurate clutter/terrain maps, secondary radiation sources

Advantage

Fast, good for long distance propagation

Detailed prediction along many radials

Typical prediction resolution (No of radial)

720

360

Weakness

Needs more CW data to estimate slope

Easy to tune, since accuracy dependent on clutter/terrain, NOT DT data

Model

Similar to COST231/HataOkumura, slope-based model with various K parameters

Deterministic model based on Physical optics to calculate diffraction over terrain/clutter

Receiver height

Different value assigned to each clutter

All mobile have same height for all clutter class

Auto tune tool

Optimize K, clutter absorption/ separation

Optimize clutter absorption property

Before model tuning • Add new sites – Setup link budget to get correct EIRP (e..g., PA power, pilot %, cable loss, rx antenna gain) – Add combined gain/loss = receiver antenna gain – receiver cable loss, • to DL link budget for all sectors • Similar to manually adjust K1 in PGM

• If scanner DT is used – Planet uses RSSI as CPICH RSCP/pilot power for CDMA based network – Allocate scanner record to sector and export as survey

• If needed, combine multiple scanner log from same sector to 1 log • Create header for each survey data per sector • Filter survey data • Average survey data • Assign filtered/averaged survey data to associated sector

Model tuning work flow – (1) import survey

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Model tuning work flow – (2) create header Site configuration is assigned to that survey

Select sector which survey belongs to

Survey changes color after header is generated 10

Model tuning work flow – (3) filter survey

Extract valid survey data for model tuning

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Model tuning work flow – (4) average survey

• Remove fast Rayleigh fading (e.g., Lee criterion is 40 λ) à 10~20 λ or about 2m for 2.5GHz • Average by distance to avoid bias effect à ½ or 1/3 of map pixel or 5m (use 2m since it is smaller) 12

Model tuning work flow – (5) assign to sector

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Used to compare prediction coverage with survey data by calculating mean/std/RMS error

Survey histogram (after filter and averaging) Dense urban sites

Smooth monotonically rolloff on both ends of dBm

urban sites

suburban sites

Clutter distribution (after filter and averaging) Dense urban sites

urban sites (recommend 2000~3000 sample per clutter class for good model tuning, absolute minimum is 200~300 sample per clutter class)

suburban sites

Distance regression (after filter and averaging) Dense urban sites DU model should has steepest slope (i.e., larger K2 magnitude) compared to U and SU model

urban sites

suburban sites

Model tuning (1) – create untuned version

•Clutter separation ~ 1 or 2 pixel distance, depending on environment •Most clutter have some diffraction loss (except water) •For PGM à Diffraction loss is pre-calculated based on clutter separation/height, only clutter absorption loss is tuned 17

Model tuning (2) – automatic model tuner (PGM)

•Use smart to tune all K values and CAL in one pass •Optional 2nd step à after running AMT, run CAL tuner to tune CAL only with fixed K values obtained from AMT 18

Model tuning (3) – verify tuned model (PGM) Check model tuning report K and CAL comparison BEFORE and AFTER running AMT (automatic model tuner)

Check error •If negative model error à model is over-predicting (i.e., predicted dBm is higher than survey) •CAL is only calculated if survey available in that clutter class (if no survey, set to 0 by default) •If clutter separation is too short, diffraction loss calculated will be too high. •If clutter has gain, it basically means clutter separation is too low or clutter height too high • uses clutter class with most sample as a reference to compute K1 and compare with other clutter type à give -/+ clutter absorption loss

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Model tuning (4) – check error between survey vs prediction based on tuned model Rerun prediction using tuned model, and check error for each sector (if scanner DT is used, mean and std will be expected to be larger than CW survey) Rule of thumb à