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| <div id="title"> | ||
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| # Demographics of M Dwarf Binary Exoplanet Hosts Discovered by TESS | ||
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| <div id="comments"> | ||
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| [](https://arxiv.org/abs/2412.08465)<mark>Appeared on: 2024-12-12</mark> - _28 pages, 13 figures, 5 tables, accepted for publication in The Astronomical Journal_ | ||
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| <div id="authors"> | ||
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| R. A. Matson, et al. -- incl., <mark>I. J. M. Crossfield</mark> | ||
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| <div id="abstract"> | ||
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| **Abstract:** M dwarfs have become increasingly important in the detection of exoplanets and the study of Earth-sized planets and their habitability. However, 20 $-$ 30 \% of M dwarfs have companions that can impact the formation and evolution of planetary systems. We use high-resolution imaging and Gaia astrometry to detect stellar companions around M dwarf exoplanet hosts discovered by TESS and determine the projected separation and estimated stellar masses for each system. We find 47 companions around 216 M dwarfs and a multiplicity rate of $19.4\pm2.7$ \% that is consistent with field M dwarfs. The binary projected separation distribution is shifted to larger separations, confirming the lack of close binaries hosting transiting exoplanets seen in previous studies.We correct the radii of planets with nearby companions and examine the properties of planets in M dwarf multi-star systems. We also note three multi-planet systems that occur in close binaries ( $\lesssim 50$ au) where planet formation is expected to be suppressed. | ||
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| <div id="div_fig1"> | ||
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| <img src="tmp_2412.08465/./Final_Separation_and_Delta_Mag_of_Gaia_Companions.png" alt="Fig5" width="100%"/> | ||
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| **Figure 5. -** _Left_: Magnitude difference as a function of angular separation for companions detected via common proper motion and parallax using Gaia DR3. Companions also detected with high-resolution imaging are shown in light blue. _Right_: Companions detected via Gaia DR3 and the CPM companions of TOI-2221 are plotted in blue, with companions detected using high-resolution imaging and not also detected using Gaia shown in orange. Open circles are companions unresolved by Gaia, or with no proper motion and/or parallax data, which are assumed to be bound (see text for details). Blue $\times$'s show companions present in Gaia with parallax and proper motion data indicating they are not physically bound. Each companion is only plotted once, with overlapping companions a result of the magnitude differences measured in different filters. Comparing the separation ranges of the high resolution and CPM detections demonstrates that while there is overlap, they provide complementary samples. (*fig:Gaiacomps*) | ||
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| <div id="div_fig2"> | ||
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| <img src="tmp_2412.08465/./Final_Sep_and_Per_Histograms.png" alt="Fig10" width="100%"/> | ||
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| **Figure 10. -** _Left:_ The projected separation distribution in au for M dwarf TOI's with companions. The subset of companions detected with high-resolution (HR) is highlighted in light blue. We converted the observed separations of each system from arcseconds to au using parallaxes from Gaia, then fit both the total sample (dot dash black line) and the high-resolution subset with Gaussian curves with $\sigma =$ 1.06 and $\sigma =$ 0.65 $\log$(AU), respectively. For the high-resolution sample, the peak is $\mu =$ 66 au, whereas for the total sample, the peak is $\mu =$ 596 au. The separation distributions of non-planet hosting, planet hosting, and TOI M stars from 2024AJ....167..174C are shown for comparison. The region shaded in gray highlights the inner angular resolution limits of the various high-resolution imaging techniques at 75pc, the mean distance for M dwarfs in our sample. These limits demonstrate that we are sensitive to stellar companions with separations of a few au where the M-dwarf distribution of 2024AJ....167..174C peaks. | ||
| _Right:_ A normalized cumulative distribution function for the projected companion separation in au. The function highlights the deficit of companions within 45 au (indicated by the vertical dashed line). Half of the M dwarf TOI companions are within 500 au (denoted by the vertical dotted line), reflecting the high concentration of companions between $45-500$ au as seen in the histogram on the left. The change in slope at $\sim50$ au is consistent with the semi-major axis cutoffs for close binaries with exoplanets determined by [Kraus, et. al (2016)]() and [Ziegler, Tokovinin and Latiolais (2021)](). | ||
| (*fig:logsep*) | ||
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| </div> | ||
| <div id="div_fig3"> | ||
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| <img src="tmp_2412.08465/./Final_HR_Diagram.png" alt="Fig1" width="100%"/> | ||
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| **Figure 1. -** H-R Diagram of TESS TOI candidates. Grey symbols are randomly chosen F, G, K stars taken from the TOI list and plotted here to give a perspective for their locations in an H-R Diagram. Red dots are M star TOIs which have already been deemed to be false positives, while blue dots show the location of the remaining M star TOI candidates. The blue dots above the main sequence are deemed to be giants and are removed from any subsequent analysis. (*fig:hrdiagram*) | ||
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| </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.08465"></div> |
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| <div class="macros" style="visibility:hidden;"> | ||
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| <div id="title"> | ||
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| # Characterization of seven transiting systems including four warm Jupiters from SOPHIE and TESS | ||
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| <div id="comments"> | ||
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| [](https://arxiv.org/abs/2412.08527)<mark>Appeared on: 2024-12-12</mark> - _46 pages, 21 figures, accepted for publication in A&A_ | ||
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| </div> | ||
| <div id="authors"> | ||
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| N. Heidari, et al. -- incl., <mark>J. Eberhardt</mark>, <mark>T. Henning</mark> | ||
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| <div id="abstract"> | ||
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| **Abstract:** While several thousand exoplanets are now confirmed, the number of known transiting warm Jupiters ( $10 \text{d} < \text{period} < 200 \text{d}$ ) remains relatively small. These planets are generally believed to have formed outside the snowline and migrated to their current orbits. Because they are sufficiently distant from their host stars, they mitigate proximity effects and so offer valuable insights into planet formation and evolution. Here, we present the study of seven systems, three of which—TOI-2295, TOI-2537, and TOI-5110—are newly discovered planetary systems. Through the analysis of TESS photometry, SOPHIE radial velocities, and high-spatial resolution imaging, we found that TOI-2295b, TOI-2537b, and TOI-5110b are transiting warm Jupiters with orbital periods ranging from 30 to 94 d, masses between 0.9 and 2.9 $M_{\rm{J}}$ , and radii ranging from 1.0 to 1.5 $R_{\rm{J}}$ . Both TOI-2295 and TOI-2537 each harbor at least one additional, outer planet. Their outer planets —TOI-2295c and TOI-2537c— are characterized by orbital periods of 966.5 $^{+4.3}_{-4.2}$ and 1920 $^{+230}_{-140}$ d, respectively, and minimum masses of 5.61 $^{+0.23}_{-0.24}$ and 7.23 $^{+0.52}_{-0.45}$ $M_{\rm{J}}$ , respectively. We also investigated and characterized the two recently reported warm Jupiters TOI-1836b and TOI-5076b, which we independently detected in SOPHIE RVs. Our new data allow for further discussion of their nature and refinement of their parameters. Additionally, we study the planetary candidates TOI-4081.01 and TOI-4168.01. For TOI-4081.01, despite our detection in radial velocities, we cannot rule out perturbation by a blended eclipsing binary and thus exercise caution regarding its planetary nature. On the other hand, we identify TOI-4168.01 as a firm false positive; its radial velocity curve exhibits a large amplitude in an anti-phase relation with the transit ephemeris observed by TESS, indicating that the detected event is the eclipse of a secondary star rather than a planetary transit. Finally, we highlight interesting characteristics of these new planetary systems. The transits of TOI-2295b are highly grazing, with an impact parameter of 1.056 $^{+0.063}_{-0.043}$ . This leaves its radius uncertain but potentially makes it an interesting probe of gravitational dynamics in its two-planet system, as transit shapes for grazing planets are highly sensitive to even small variations in inclination. TOI-2537b, in turn, is a temperate Jupiter with an effective temperature of 307 $\pm$ 15 K and can serve as a valuable low-irradiation control for models of hot Jupiter inflation anomalies. We also detected significant transit timing variations (TTVs) for TOI-2537b, which are likely caused by gravitational interactions with the outer planet TOI-2537c. Further transit observations are needed to refine the analysis of these TTVs and enhance our understanding of the system’s dynamics. Finally, TOI-5110b stands out due to its orbital eccentricity of 0.745 $^{+0.030}_{-0.027}$ , one of the highest planetary eccentricities discovered thus far. We find no conclusive evidence for an external companion, but an unseen planet with a semi-amplitude smaller than 10 m/s could nonetheless still be exciting its eccentricity. | ||
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| <img src="tmp_2412.08527/./tpf_toi1836.png" alt="Fig19.1" width="14%"/><img src="tmp_2412.08527/./tpf_toi2295.png" alt="Fig19.2" width="14%"/><img src="tmp_2412.08527/./tpf_toi2537.png" alt="Fig19.3" width="14%"/><img src="tmp_2412.08527/./tpf_toi4081.png" alt="Fig19.4" width="14%"/><img src="tmp_2412.08527/./4168/tpf_toi4168.png" alt="Fig19.5" width="14%"/><img src="tmp_2412.08527/./tpf_toi5076.png" alt="Fig19.6" width="14%"/><img src="tmp_2412.08527/./tpf_toi5110.png" alt="Fig19.7" width="14%"/> | ||
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| **Figure 19. -** Target Pixel Files (TPFs) images from the first observed TESS sector for the seven targets in our analysis, created by \texttt{tpfplotter} ([Aller, et. al 2020]()) . The images depict electron counts, with red-contoured pixels marking the SPOC aperture mask. Additionally, red circles highlight the primary target (numbered as 1) and nearby sources (rest of the numbers) at their Gaia DR3 positions. The area of these circles reflects the relative magnitudes of the sources in comparison to the target star. Arrows represent the proper motion of each star. (*tpfplotter*) | ||
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| <img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S23.png" alt="Fig23.1" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S24.png" alt="Fig23.2" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S25.png" alt="Fig23.3" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S49.png" alt="Fig23.4" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S50.png" alt="Fig23.5" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S51.png" alt="Fig23.6" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S52.png" alt="Fig23.7" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S56.png" alt="Fig23.8" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S76.png" alt="Fig23.9" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S77.png" alt="Fig23.10" width="9%"/><img src="tmp_2412.08527/./TPF_Gaia_TIC207468071_S78.png" alt="Fig23.11" width="9%"/> | ||
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| **Figure 23. -** The TPFs for TOI-1836, created by \texttt{tpfplotter} ([Aller, et. al 2020]()) . The images display electron counts, with the SPOC aperture mask outlined in red. Red circles are used to indicate the primary target (marked as 1) and nearby sources (rest of the numbers) based on their positions in Gaia DR3. The size of these circles corresponds to the relative magnitudes of the sources compared to the target star. Additionally, arrows illustrate the proper motion of each star. (*tpfplotter_1836*) | ||
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| <img src="tmp_2412.08527/./high_image_all.png" alt="Fig20" width="100%"/> | ||
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| **Figure 20. -** Contrast curves for the speckle interferometry observations of TOI-1836, TOI-2295, TOI-2537, TOI-4081, TOI-4168, TOI-5076, and TOI-5110 are shown with black, blue, and red solid lines. The name of each star is indicated on the corresponding plot. TOI-1836, TOI-4081, TOI-4168, TOI-5076, and TOI-5110 were observed by SPP in 625 or 880 nm band. Meanwhile, TOI-2295 was observed using Gemini 'Alopeke, which provides simultaneous speckle imaging in two bands: 562 nm (blue line) and 832 nm (red line). Additionally, TOI-2537 was observed by SOAR in 880 nm band. Each plot includes the final reconstructed image inset in the upper right corner. (*spp*) | ||
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| </div><div id="qrcode"><img src=https://api.qrserver.com/v1/create-qr-code/?size=100x100&data="https://arxiv.org/abs/2412.08527"></div> |
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