A 1.48-2.48 $\mathrmμ$m R=28000 spectroscopic atlas of the L7.5 and T0.5 components of the nearest pair of brown dwarfs: Luhman 16AB
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866910979422420992 |
|---|---|
| author | Ishikawa, Hiroyuki Tako Metchev, Stanimir Tannock, Megan E. Mace, Gregory N. Hood, Callie E. Fortney, Jonathan J. Mukherjee, Sagnick Miles-Páez, Paulo Kurtev, Radostin |
| author_facet | Ishikawa, Hiroyuki Tako Metchev, Stanimir Tannock, Megan E. Mace, Gregory N. Hood, Callie E. Fortney, Jonathan J. Mukherjee, Sagnick Miles-Páez, Paulo Kurtev, Radostin |
| contents | We present a high signal-to-noise (SNR $\sim$ 450), high-dispersion ($R \equiv λ/ Δλ\sim 28\,000$) H- and K-band spectroscopic atlas of the L7.5 and T0.5 components of the Luhman 16AB binary (WISE J104915.57$-$531906.1AB): the closest pair of brown dwarfs, and one of the best substellar benchmarks. The spectra were combined from a 70-day spectroscopic monitoring campaign of the binary with IGRINS on Gemini South. We fit model photospheres to the combined high-quality spectra to estimate atmospheric parameters. The model is based on the Sonora model atmosphere further incorporating the effects of clouds and disequilibrium. We detect ammonia (NH3) lines in both binary components, making Luhman 16A the warmest object where individual NH3 lines were identified. We discover hydrogen (H2), hydrogen sulfide (H2S), and hydrogen fluoride (HF) lines in both components, following recent reports of these species in either cooler (H2, H2S in a T6 dwarf) or warmer (HF in young late-M or mid-L dwarfs) objects. Methane (CH4) shows a small contribution, with lines sensitive to the slight temperature difference spanning the L/T transition. Against model expectations, we do not detect FeH lines, implying more efficient iron rainout than incorporated in the models. We find various unidentified features in water-dominated regions, likely the result of residual inaccuracies in the water line lists. We searched for planetary-mass companions by periodogram analysis of radial velocities over 70 days but detected no significant signal. The upper limits of projected planetary mass are $M\sin{i}=$ 0.2 $M_{\mathrm{J}}$ and 0.3 $M_{\mathrm{J}}$ at P $\sim$ 1 day, and 0.4 $M_{\mathrm{J}}$ and 0.7 $M_{\mathrm{J}}$ at P $\sim$ 10 days for Luhman 16A and B, respectively. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_19322 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A 1.48-2.48 $\mathrmμ$m R=28000 spectroscopic atlas of the L7.5 and T0.5 components of the nearest pair of brown dwarfs: Luhman 16AB Ishikawa, Hiroyuki Tako Metchev, Stanimir Tannock, Megan E. Mace, Gregory N. Hood, Callie E. Fortney, Jonathan J. Mukherjee, Sagnick Miles-Páez, Paulo Kurtev, Radostin Solar and Stellar Astrophysics Earth and Planetary Astrophysics We present a high signal-to-noise (SNR $\sim$ 450), high-dispersion ($R \equiv λ/ Δλ\sim 28\,000$) H- and K-band spectroscopic atlas of the L7.5 and T0.5 components of the Luhman 16AB binary (WISE J104915.57$-$531906.1AB): the closest pair of brown dwarfs, and one of the best substellar benchmarks. The spectra were combined from a 70-day spectroscopic monitoring campaign of the binary with IGRINS on Gemini South. We fit model photospheres to the combined high-quality spectra to estimate atmospheric parameters. The model is based on the Sonora model atmosphere further incorporating the effects of clouds and disequilibrium. We detect ammonia (NH3) lines in both binary components, making Luhman 16A the warmest object where individual NH3 lines were identified. We discover hydrogen (H2), hydrogen sulfide (H2S), and hydrogen fluoride (HF) lines in both components, following recent reports of these species in either cooler (H2, H2S in a T6 dwarf) or warmer (HF in young late-M or mid-L dwarfs) objects. Methane (CH4) shows a small contribution, with lines sensitive to the slight temperature difference spanning the L/T transition. Against model expectations, we do not detect FeH lines, implying more efficient iron rainout than incorporated in the models. We find various unidentified features in water-dominated regions, likely the result of residual inaccuracies in the water line lists. We searched for planetary-mass companions by periodogram analysis of radial velocities over 70 days but detected no significant signal. The upper limits of projected planetary mass are $M\sin{i}=$ 0.2 $M_{\mathrm{J}}$ and 0.3 $M_{\mathrm{J}}$ at P $\sim$ 1 day, and 0.4 $M_{\mathrm{J}}$ and 0.7 $M_{\mathrm{J}}$ at P $\sim$ 10 days for Luhman 16A and B, respectively. |
| title | A 1.48-2.48 $\mathrmμ$m R=28000 spectroscopic atlas of the L7.5 and T0.5 components of the nearest pair of brown dwarfs: Luhman 16AB |
| topic | Solar and Stellar Astrophysics Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2503.19322 |