Pinpointing the location of the

Aims. The flat-spectrum radio quasar (FSRQ) 4C +01.28 is a bright and highly variable radio and γ-ray emitter. We aim to pinpoint the location of the γ-ray emitting region within its jet in order to derive strong constraints on γ-ray emission models for blazar jets. Methods. We use radio and γ-ray monitoring data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA), the Owens Valley Radio Observatory (OVRO), the Submillimeter Array (SMA), and the Large Area Telescope on board the Fermi Gamma-ray Space Telescope (Fermi/LAT) to study the cross-correlation between γ-ray and multifrequency radio light curves. Moreover, we employ Very Long Baseline Array (VLBA) observations at 43 GHz over a period of around nine years to study the parsec-scale jet kinematics of 4C +01.28. To pinpoint the location of the γ-ray emitting region, we use a model in which outbursts shown in the γ-ray and radio light curves are produced when moving jet components pass through the γ-ray emitting and the radio core regions. Results. We find two bright and compact newly ejected jet components that are likely associated with a high activity period visible in the Fermi/LAT γ-ray and different radio light curves. The kinematic analysis of the VLBA observations leads to a maximum apparent jet speed of βapp = 19 ± 10 and an upper limit on the viewing angle of ϕ ≲ 4°. Furthermore, we determine the power law indices that are characterizing the jet geometry, brightness temperature distribution, and core shift to be l = 0.974 ± 0.098, s = −3.31 ± 0.31, and kr = 1.09 ± 0.17, respectively, which are all in agreement with a conical jet in equipartition. A cross-correlation analysis shows that the radio light curves follow the γ-ray light curve. We pinpoint the location of the γ-ray emitting region with respect to the jet base to the range of 2.6 pc ≤ dγ ≤ 20 pc. Conclusions. Our observational limits places the location of γ-ray production in 4C +01.28 beyond the expected extent of the broad-line region (BLR) and therefore challenges blazar-emission models that rely on inverse Compton up-scattering of BLR seed photons.