J/A+A/713/A310 Kinematic properties of Perseus YSOs (Gu+, 2026) ================================================================================ Tracing expansion-driven star formation in the Perseus molecular cloud using young young stellar objects. Gu C.-R., Zhu Z.-K., Lu Z.-J., Fang M., Yang L., He C.-Y. =2026A&A...713A.310G (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Molecular clouds ; YSOs ; Stars, distances ; Space velocities ; Optical Keywords: star formation - stars: kinematics and dynamics - ISM: molecules Abstract: Recent studies have increasingly linked star formation in the solar neighbourhood to the expansion of the Local Bubble. The Per-Tau Shell (PTS), a vast 3D dust structure hosting the Perseus and Taurus clouds on its surface, is a candidate for such triggered formation. While the Local Bubble primarily drives star formation in Taurus, Perseus is kinematically distinct from this flow. Consequently, the dynamical influence of the PTS on the Perseus cloud remains an open question. We aim to reconstruct the star formation history of the Perseus molecular cloud and investigate its potential link to the historical expansion of the Per-Tau Shell (PTS). We aim to reconstruct the star formation history of the Perseus molecular cloud and investigate its potential link to the historical expansion of the PTS. We performed a 6D phase-space analysis of 406 young stellar objects (YSOs) of Perseus. Our approach integrates Gaia DR3 kinematics with Bayesian age inference and a heteroscedastic likelihood framework to resolve radial gradients in YSO ages and intrinsic tangential velocity dispersions relative to the PTS centre. Additionally, we constructed a unified catalogue by integrating existing infrared-based classifications from the literature to examine the projected spatial segregation of different evolutionary stages and compared stellar 3D kinematics with molecular gas velocity fields to assess kinematic coherence. The YSOs exhibit coherent outward motions relative to the centre of the PTS, a negative age-distance gradient with younger populations at larger radii, and a radial decline in tangential velocity dispersions. Younger YSO classes also show a stronger directional concentration towards the PTS centre. Furthermore, both the coherent proper motions and the line-of-sight velocity gradients of these YSOs align with the gas velocity field, indicating large-scale kinematic coherence. The Perseus YSOs exhibit concordant kinematic and temporal signatures consistent with an expansion-driven origin. These results provide robust evidence for a layered, inside-out pattern of star formation, suggesting that the historical expansion of the PTS triggered a sequential progression of star birth and effectively shaped the star formation history of the Perseus complex. Description: This catalogue provides the 6D phase-space data (positions and velocities) for 406 Young Stellar Objects (YSOs) in the Perseus molecular cloud, along with infrared-based YSO classifications compiled from the literature. The data were used to study the expansion-driven star formation triggered by the Per-Tau Shell (PTS). Table1 contains the kinematic sample with Gaia DR3 astrometry, radial velocities, extinctions, and derived distances. Table2 contains the unified infrared classifications of YSOs from various surveys. Objects: ---------------------------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------------------------- 03 34 59.99 +31 12 59.9 Perseus molecular cloud = NAME Per Molecular Cloud ---------------------------------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tablec1.dat 247 406 Kinematic properties of 406 Perseus YSOs tablec2.dat 69 610 Infrared YSO classifications -------------------------------------------------------------------------------- See also: J/A+A/671/A1 : Cosmic DANCe of Perseus (Olivares+, 2023) Byte-by-byte Description of file: tablec1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 --- Group Kinematic group designation (1) 12- 29 I18 --- GaiaDR3 Gaia DR3 source identifier 31- 48 F18.15 deg RAdeg Right Ascension (ICRS) at Ep=2016.0 50- 67 F18.15 deg DEdeg Declination (ICRS) at Ep=2016.0 69- 87 F19.15 pc dPTS 3D distance from the PTS centre 89-106 F18.14 pc dplx Heliocentric distance from parallax 108-125 F18.16 mag AV Line-of-sight visual extinction 127-136 F10.7 mag Gmag Gaia G-band magnitude 138-143 F6.3 km/s meanU ICRS Cartesian velocity U 145-150 F6.3 km/s meanV ICRS Cartesian velocity V 152-157 F6.3 km/s meanW ICRS Cartesian velocity W 159-176 F18.16 mag bmapAv Extinction from map 178-195 F18.16 mag bmapaVlc Extinction from map (low-column) 197-215 F19.16 pc e_dplx Uncertainty in dplx 217-229 F13.11 mag e_Gmag Uncertainty in Gmag 231-235 F5.3 km/s e_meanU Uncertainty in meanU 237-241 F5.3 km/s e_meanV Uncertainty in meanV 243-247 F5.3 km/s e_meanW Uncertainty in meanW -------------------------------------------------------------------------------- Note (1): kinematic groups defined in Olivares et al. (2023A&A...671A...1O, Cat. J/A+A/671/A1). -------------------------------------------------------------------------------- Byte-by-byte Description of file: tablec2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 26 A26 --- Name Source designation 28- 31 A4 --- YSOType YSO evolutionary class (Flat, 0+I, II, III) 33- 50 F18.15 deg RAdeg Right Ascension (J2000) 52- 69 F18.15 deg DEdeg Declination (J2000) -------------------------------------------------------------------------------- Acknowledgements: From Chen-Rui Gu, richardcherryguchenrui(at)gmail.com The authors would like to thank the anonymous referee for comments that improved the content and presentation of this paper. This research is supported by Guangxi Natural Science Foundation under Grant No.2024GXNSFBA010436 and Guangxi Key Research and Development Program (Guike FN2504240040). ZJL acknowledges support by NSFC grant No.12563005, 12494571 and the National Key R&D Program of China (Grant Nos. 2024YFA1611704, 2024YFA1611700). This research is also supported by Guangxi Qingmiao Talent Support Program, Bagui Scholars Programme (W.X.-G., GXR-6BG2424001), Guangxi Talent Program ("Highland of Innovation Talents"). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. License: CC-BY-4.0 ================================================================================ (End) Patricia Vannier [CDS] 07-Aug-2026