Optical Observations of the High Mass X-ray Binary MAXI J0709$-$159/LY CMa
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2025
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| _version_ | 1866913761068056576 |
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| author | Shidatsu, Megumi Kawai, Nobuyuki Maehara, Hiroyuki Goto, Emi Urabe, Sota Iwakiri, Wataru Tsuboi, Yohko Nemoto, Noboru Nawa, Sakura Sugizaki, Mutsumi Nakajima, Motoki Niwano, Masafumi Hosokawa, Ryohei Sakamoto, Marie Matsuoka, Yoshiki |
| author_facet | Shidatsu, Megumi Kawai, Nobuyuki Maehara, Hiroyuki Goto, Emi Urabe, Sota Iwakiri, Wataru Tsuboi, Yohko Nemoto, Noboru Nawa, Sakura Sugizaki, Mutsumi Nakajima, Motoki Niwano, Masafumi Hosokawa, Ryohei Sakamoto, Marie Matsuoka, Yoshiki |
| contents | We report on the optical spectroscopic monitoring of the X-ray transient MAXI J0709$-$159 (identified as the Be star LY CMa) performed for about 1.5 months after the X-ray detection with MAXI. The observed spectrum showed a double-peaked H$α$ line with a peak-to-peak separation of $\sim 230$ km s$^{-1}$, suggestive of the Be disk origin. We also detected a broad wing of the H$α$ line with a line-of-sight velocity of $\gtrsim 900$ km s$^{-1}$, which could be explained by the accretion disk of the compact object or a stellar wind from the Be star. Initially the H$α$ line showed an asymmetric profile with an enhanced blue peak, and then the blue peak decreased in $\sim$ 3 weeks to a similar strength to the red peak. We suggest that the evolution of the blue peak is associated with the X-ray activity and generated by the turbulence of the Be disk due to the passage of the compact object. We also investigated flux variation using the archival TESS data and found quasi-periodic variations with frequencies of $\sim 1$ and $\sim 2$ day$^{-1}$, which were likely caused by the pulsation of the B star. The overall variability properties on timescales of $\sim$ day were similar to those in Be X-ray binaries, rather than supergiant X-ray binaries. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2503_21118 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Optical Observations of the High Mass X-ray Binary MAXI J0709$-$159/LY CMa Shidatsu, Megumi Kawai, Nobuyuki Maehara, Hiroyuki Goto, Emi Urabe, Sota Iwakiri, Wataru Tsuboi, Yohko Nemoto, Noboru Nawa, Sakura Sugizaki, Mutsumi Nakajima, Motoki Niwano, Masafumi Hosokawa, Ryohei Sakamoto, Marie Matsuoka, Yoshiki High Energy Astrophysical Phenomena Solar and Stellar Astrophysics We report on the optical spectroscopic monitoring of the X-ray transient MAXI J0709$-$159 (identified as the Be star LY CMa) performed for about 1.5 months after the X-ray detection with MAXI. The observed spectrum showed a double-peaked H$α$ line with a peak-to-peak separation of $\sim 230$ km s$^{-1}$, suggestive of the Be disk origin. We also detected a broad wing of the H$α$ line with a line-of-sight velocity of $\gtrsim 900$ km s$^{-1}$, which could be explained by the accretion disk of the compact object or a stellar wind from the Be star. Initially the H$α$ line showed an asymmetric profile with an enhanced blue peak, and then the blue peak decreased in $\sim$ 3 weeks to a similar strength to the red peak. We suggest that the evolution of the blue peak is associated with the X-ray activity and generated by the turbulence of the Be disk due to the passage of the compact object. We also investigated flux variation using the archival TESS data and found quasi-periodic variations with frequencies of $\sim 1$ and $\sim 2$ day$^{-1}$, which were likely caused by the pulsation of the B star. The overall variability properties on timescales of $\sim$ day were similar to those in Be X-ray binaries, rather than supergiant X-ray binaries. |
| title | Optical Observations of the High Mass X-ray Binary MAXI J0709$-$159/LY CMa |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2503.21118 |