PROJECT-J: the shocking H2 outflow from HH46
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arXiv
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| Main Authors: | , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866914167176298496 |
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| author | Navarro, Maria Gabriela Nisini, Brunella Giannini, Teresa Kavanagh, Patrick J. Garatti, Alessio Caratti o Antoniucci, Simone Arce, Hector G. Bacciotti, Francesca Cabrit, Sylvie Coffey, Deirdre Dougados, Catherine Eislöffel, JJochen Hartigan, Patrick Noriega-Crespo, Alberto Podio, Linda van Dishoeck, Ewine F. Whelan, Emma T. |
| author_facet | Navarro, Maria Gabriela Nisini, Brunella Giannini, Teresa Kavanagh, Patrick J. Garatti, Alessio Caratti o Antoniucci, Simone Arce, Hector G. Bacciotti, Francesca Cabrit, Sylvie Coffey, Deirdre Dougados, Catherine Eislöffel, JJochen Hartigan, Patrick Noriega-Crespo, Alberto Podio, Linda van Dishoeck, Ewine F. Whelan, Emma T. |
| contents | We analyze the H2 emission observed in the HH46 Class I system as part of PROJECT-J (Protostellar Jets Cradle Tested with JWST), to investigate the origin and excitation of the warm molecular outflow. We used NIRSpec and MIRI spectral maps (1.6-27.9 microns) to trace the structure and physical conditions of the outflow. By fitting the H2 rotational diagrams with a multi-temperature gas model, we derived key physical parameters including temperature, extinction, column densities, and the ortho-to-para ratio. This information is combined with a detailed kinematical analysis and comparison with irradiated shock models.
We find no evidence of H2 temperature or velocity stratification from the axis to the edge of the outflow, as would be expected in MHD disk-wind models and as observed in other outflows. Instead, the observations suggest that the H2 emission arises from shock interactions between jet bow shocks and/or wide-angle winds with the ambient medium and cavity walls. NIRSpec emission and velocity maps reveal expanding molecular shells, likely driven by the less luminous source in the binary system. We infer an accretion rate of less than 10^-9 solar masses per year for the secondary source, approximately one order of magnitude lower than that of the primary.
The H2 emission is consistent with excitation by low-velocity (approximately 10 km/s) J-type shocks, irradiated by an external UV field that may originate from strong dissociative shocks driven by the atomic jet. Future JWST observations will further constrain the evolution of the expanding shell and the mechanisms driving the outflow. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2511_17712 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | PROJECT-J: the shocking H2 outflow from HH46 Navarro, Maria Gabriela Nisini, Brunella Giannini, Teresa Kavanagh, Patrick J. Garatti, Alessio Caratti o Antoniucci, Simone Arce, Hector G. Bacciotti, Francesca Cabrit, Sylvie Coffey, Deirdre Dougados, Catherine Eislöffel, JJochen Hartigan, Patrick Noriega-Crespo, Alberto Podio, Linda van Dishoeck, Ewine F. Whelan, Emma T. Astrophysics of Galaxies Solar and Stellar Astrophysics We analyze the H2 emission observed in the HH46 Class I system as part of PROJECT-J (Protostellar Jets Cradle Tested with JWST), to investigate the origin and excitation of the warm molecular outflow. We used NIRSpec and MIRI spectral maps (1.6-27.9 microns) to trace the structure and physical conditions of the outflow. By fitting the H2 rotational diagrams with a multi-temperature gas model, we derived key physical parameters including temperature, extinction, column densities, and the ortho-to-para ratio. This information is combined with a detailed kinematical analysis and comparison with irradiated shock models. We find no evidence of H2 temperature or velocity stratification from the axis to the edge of the outflow, as would be expected in MHD disk-wind models and as observed in other outflows. Instead, the observations suggest that the H2 emission arises from shock interactions between jet bow shocks and/or wide-angle winds with the ambient medium and cavity walls. NIRSpec emission and velocity maps reveal expanding molecular shells, likely driven by the less luminous source in the binary system. We infer an accretion rate of less than 10^-9 solar masses per year for the secondary source, approximately one order of magnitude lower than that of the primary. The H2 emission is consistent with excitation by low-velocity (approximately 10 km/s) J-type shocks, irradiated by an external UV field that may originate from strong dissociative shocks driven by the atomic jet. Future JWST observations will further constrain the evolution of the expanding shell and the mechanisms driving the outflow. |
| title | PROJECT-J: the shocking H2 outflow from HH46 |
| topic | Astrophysics of Galaxies Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2511.17712 |