1. Introduction
2. Submillimeter and infrared data
2.1. The CAFFEINE imaging survey with ArTéMiS
2.2. Herschel imaging data
3. Constructing column density maps
3.1. Combining ArTéMiS and Herschel data
3.2. Constructing high-resolution column density maps
4. Methods and analysis
4.1. Evaluating and subtracting the line-of-sight contamination
4.2. Star formation rates
5. Results
5.1. Star formation efficiencies in CAFFEINE clouds
5.2. Comparing the two types of SFE estimates for the CAFFEINE sample
5.3. Star formation rates and efficiencies in nearby clouds
6. Discussion
6.1. Simple models for the star formation efficiency
6.2. Global picture of the star formation efficiency
6.3. Caveat: Difference between Class I and Class II YSO SFE estimates in nearby clouds
6.4. Role of stellar feedback
7. Summary and conclusions