The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902
A transiting planet was recently discovered around a star in the Taurus star-forming region, IRAS 04125+2902, making it one of the youngest known planets. The discovery paper cited two age estimates for IRAS 04125+2902, one based on a comparison to two sets of model isochrones in the Hertzsprung–Rus...
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IOP Publishing
2025-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/adb0cd |
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| author | K. L. Luhman |
| author_facet | K. L. Luhman |
| author_sort | K. L. Luhman |
| collection | DOAJ |
| description | A transiting planet was recently discovered around a star in the Taurus star-forming region, IRAS 04125+2902, making it one of the youngest known planets. The discovery paper cited two age estimates for IRAS 04125+2902, one based on a comparison to two sets of model isochrones in the Hertzsprung–Russell diagram and a second age reported by an earlier study for a putative population in Taurus that includes IRAS 04125+2902 (D4-North). However, the model isochrones in question differ significantly for most temperatures and luminosities of young low-mass stars, and do not reproduce the observed sequences for the TW Hya and 32 Ori associations (10 and 21 Myr). Meanwhile, as found in my previous work, D4-North is a collection of field stars and fragments of several distinct Taurus groups and older associations, so its quoted age is not meaningful. The true parent population for IRAS 04125+2902 is a small group that is ∼35 pc behind the L1495 and B209 clouds (B209N). I have analyzed the age of B209N through a comparison to TW Hya and 32 Ori. The M-star sequences in the latter two associations have the same shapes, but the sequence for B209N is flatter, indicating that >M4 stars at ages of <10 Myr fade more quickly than stars at earlier types and older ages. For the one member of B209N that is earlier than M4 (IRAS 04125+2902), I estimate an age of 3.0 ± 0.4 Myr based on its offsets from TW Hya and 32 Ori, which by happenstance is similar to the value derived through the comparison to model isochrones. |
| format | Article |
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| institution | DOAJ |
| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-61c0348c3bc24edcb52acaa6f86a56312025-08-20T03:12:48ZengIOP PublishingThe Astronomical Journal1538-38812025-01-01169317910.3847/1538-3881/adb0cdThe Membership and Age of the Planet-hosting Young Star IRAS 04125+2902K. L. Luhman0https://orcid.org/0000-0003-2822-2951Department of Astronomy and Astrophysics, The Pennsylvania State University , University Park, PA 16802, USA ; kll207@psu.edu; Center for Exoplanets and Habitable Worlds, The Pennsylvania State University , University Park, PA 16802, USAA transiting planet was recently discovered around a star in the Taurus star-forming region, IRAS 04125+2902, making it one of the youngest known planets. The discovery paper cited two age estimates for IRAS 04125+2902, one based on a comparison to two sets of model isochrones in the Hertzsprung–Russell diagram and a second age reported by an earlier study for a putative population in Taurus that includes IRAS 04125+2902 (D4-North). However, the model isochrones in question differ significantly for most temperatures and luminosities of young low-mass stars, and do not reproduce the observed sequences for the TW Hya and 32 Ori associations (10 and 21 Myr). Meanwhile, as found in my previous work, D4-North is a collection of field stars and fragments of several distinct Taurus groups and older associations, so its quoted age is not meaningful. The true parent population for IRAS 04125+2902 is a small group that is ∼35 pc behind the L1495 and B209 clouds (B209N). I have analyzed the age of B209N through a comparison to TW Hya and 32 Ori. The M-star sequences in the latter two associations have the same shapes, but the sequence for B209N is flatter, indicating that >M4 stars at ages of <10 Myr fade more quickly than stars at earlier types and older ages. For the one member of B209N that is earlier than M4 (IRAS 04125+2902), I estimate an age of 3.0 ± 0.4 Myr based on its offsets from TW Hya and 32 Ori, which by happenstance is similar to the value derived through the comparison to model isochrones.https://doi.org/10.3847/1538-3881/adb0cdStar forming regionsPlanet hosting starsStellar ages |
| spellingShingle | K. L. Luhman The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 The Astronomical Journal Star forming regions Planet hosting stars Stellar ages |
| title | The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 |
| title_full | The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 |
| title_fullStr | The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 |
| title_full_unstemmed | The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 |
| title_short | The Membership and Age of the Planet-hosting Young Star IRAS 04125+2902 |
| title_sort | membership and age of the planet hosting young star iras 04125 2902 |
| topic | Star forming regions Planet hosting stars Stellar ages |
| url | https://doi.org/10.3847/1538-3881/adb0cd |
| work_keys_str_mv | AT klluhman themembershipandageoftheplanethostingyoungstariras041252902 AT klluhman membershipandageoftheplanethostingyoungstariras041252902 |