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tokens: 6′′ of the central source detected by M98 and compare it with the current number (including objects from the WDS catalog, Gaia DR2, and companions detected in this paper, see below) the number has grown from 12 to 28, an equally impressive advancement. As we will show in future papers, there is still room for significant improvements in the case of new spectroscopic orbits. The same should be true for the discovery of new astrometric companions, not only using lucky imaging but also more sophisticated techniques such as the ones used in the southern hemisphere by the SMaSH+ survey ( Sana et al. 2014 ). The value of our results lies mostly in the updated detailed information, such as the homogeneous revision of the spectral classification of the sample applying the criteria we have developed for GOSSS, that can be used for future global analyses of the multiplicity in O stars. We indeed plan to do such analyses in future papers ourselves but it is also worthy to point out some results for individual systems in this work. We present first-time O-type GOSSS spectral classifications for 17 objects: HD 170 097 A, QR Ser, BD − 13 4923, HD 190 967, HD 193 611, HDE 228 989, HDE 229 234, Cyg OB2-3 A, ALS 15 133, ALS 15 148, Cyg OB2-1, ALS 15 131, Cyg OB2-20, Cyg OB2-15, ALS 12 502, DN Cas, and IU Aur AB. For another six objects we present their first-time B-type GOSSS spectral classifications: HD 193 322 B, Cyg OB2-3 B, HD 15 558 B, HD 16 429 C, MY Cam B, and LY Aur B. We have identified one eclipsing system as SB2 for the first time, HD 170 097 A, and derived its separate spectral classifications. To that one we can add a second eclipsing system in the sample, ALS 12 688, that was identified as having double absorption lines for the first time in GOSSS III. For another eclipsing binary, V747 Cep, we detect moving lines (SB1) for the first time using our LiLiMaRlin spectra. For two systems that have published SB1 orbits, BD − 16 4826 and θ 2 Ori A, we publish the first spectrograms with double lines (SB2) and derive their first true separate spectral classifications. For HD 168 112 AB we also publish the first SB2 spectrograms and separate spectral classification. We have also detected nine new astrometric components, one each around HD 190 967, ALS 15 133, Cyg OB2-A11, Cyg OB2-1, ALS 12 502, DN Cas, and MY Cam A and two around IU Aur AB. The results of this paper will be added to GOSC at the time of publication, which will reach version 4.2. With them, GOSC will contain a total of 655 objects: 611 in the main catalog (Galactic O stars), 32 in supplement 2 (Galactic early-type stars), and 12 in supplement 3 (Galactic late-type stars). It is not possible to do a full multiplicity analysis based on our 92 stars for two reasons: the sample is too small and is biased. The most obvious bias is that we selected our stars from systems that had spectroscopic orbits previously published, so no single targets are included. Note, however, that several SB1?