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Dust-seeding Molecules in a Massive Protostar—Detection of TiO in Orion Source I

  • Authors: Ziwei E. Zhang, Nami Sakai, Marcelino Agúndez, Linda Podio, Claudio Codella, Tomoya Hirota, Adam Ginsburg, Brett McGuire, Nadia M. Murillo, Yuki Okoda, Yoko Oya, Giovanni Sabatini, Aki Takigawa, Kei E. I. Tanaka, Yichen Zhang, Qiuyi Luo, Yu Cheng, Izaskun Jiménez-Serra, Shogo Tachibana

Ziwei E. Zhang et al 2026 The Astrophysical Journal Letters 1011 .

  • Provider: AAS Journals

Caption: Figure B1.

PV diagrams and spectra for the three blended TiO transitions. The red contours are plotted at intervals of 4σ, starting from 4σ. The mean spectra are extracted from a circular area within 100 au from the continuum center. At 415 pc, 100 au = 0﹩\mathop{.}\limits^{{\unicode{x02033}}}﹩24. The effective emission range (Vpeak = 8.0 km s−1 and ΔVFWHM = 13 km s−1, Table 1) of TiO is shaded with light green. Noise levels at 1σ are marked with orange dashed lines. The spectrum at 646 GHz is truncated at the edge of the spectral window. The 484 GHz transition is blended with extended emission, characterized by low-velocity-gradient features at offsets of ≳±100 au. The 646 GHz transition is blended with compact emission from SiS and SO2, while the 355 GHz transition is contaminated by both extended and compact emission, including KCl. From left to right, the rms of the molecular emission are 5.5 × 10−5, 4.0 × 10−2, and 4.0 × 10−2 Jy beam −1.

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