Hwang, JihyeJihyeHwangSanhueza, PatricioPatricioSanhuezaGirart, Josep MiquelJosep MiquelGirartStephens, Ian W.Ian W.StephensBeltrán, Maria T.Maria T.BeltránLaw, Chi YanChi YanLawZhang, QizhouQizhouZhangLiu, JunhaoJunhaoLiuCortés, PauloPauloCortésOlguin, Fernando A.Fernando A.OlguinKoch, Patrick M.Patrick M.KochNakamura, FumitakaFumitakaNakamuraSaha, PiyaliPiyaliSahaWang, Jia WeiJia WeiWangXu, FengweiFengweiXuBeuther, HenrikHenrikBeutherMorii, KahoKahoMoriiFernández López, ManuelManuelFernández LópezJiao, WenyuWenyuJiaoKim, Kee TaeKee TaeKimLi, ShanghuoShanghuoLiZapata, Luis A.Luis A.ZapataKim, JongsooJongsooKimChoudhury, SpandanSpandanChoudhuryCheng, YuYuChengPattle, KateKatePattleEswaraiah, ChakaliChakaliEswaraiahSandhyarani, PanigrahyPanigrahySandhyaraniDewangan, L. K.L. K.DewanganJadhav, O. R.O. R.Jadhav2026-04-092026-04-092026-01-0210.3847/1538-3881/ae18c92-s2.0-105033946098https://repository.iitgn.ac.in/handle/IITG2025/34971We investigate the magnetic field orientation and strength in the massive star-forming region G35.20-0.74N (G35), using polarized dust emission data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) as part of the Magnetic fields in Massive star-forming Regions (MagMaR) survey. The G35 region shows a filamentary structure (a length of ∼0.1 pc) with six bright cores located along the filament’s long axis. Magnetic field strengths across the G35 region range from 0.2 to 4.4 mG with a mean value of 0.8 ± 0.4 mG. The mass-to-flux ratio (λ) varies from 0.1 to 6.0, the critical value. The highest values are found locally around cores, whereas the remains of the filament are subcritical. A H¹³CO⁺ (3-2) velocity gradient of 29 km s⁻¹ pc⁻¹ is evident along the filament’s long axis, aligned with the magnetic field direction. At larger scales (∼0.1 pc), the magnetic field lines appear roughly perpendicular to the filament’s long axis, in contrast to the smaller-scale structure (∼0.003 pc) traced by ALMA. The magnetic field lines could be dragged along the filament as a result of the gas motion induced by the gravitational potential of the filament. Six cores in the filament have similar spacings between 0.02 and 0.04 pc. The initial filament fragmentation could have produced a core spacing of 0.06 pc, following filament fragmentation theory, and the current core spacing is the result of cores comoving with the gas along the filament. This core migration could occur in a few 10⁴ yr, consistent with high-mass star formation timescales.trueArticle153838812 January 2026150arArticle