2017/12/23 by Chien-Hsiu Lee, Po-Shih Chiang
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Binary number #Broadband #Exoplanet #Photometry (optics) #Planet #Star (game theory) #Stellar, planetary, and galactic studies #T Tauri star #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.3847/2041-8213/aaa40b
8 pages, 4 figures, ApJ Letter accepted
arxiv created 2017/12/23 · openalex created_date 2018/01/05 · openalex publication_date 2018/01/08 · arxiv updated 2018/01/24 · openalex updated_date 2026/08/05
Abstract We report serendipitous optical imaging of CVSO30c, an exoplanet candidate associated with the pre-main-sequence T Tauri star CVSO30 that resides in the 25 Ori stellar cluster. We perform PSF modeling on our seeing-limited optical image to remove the lights from the host star (CVSO30), allowing us to extract photometry of CVSO30c to be g = 23.2 ± 0.2 (statistic) ± 0.1 (systematic) and r = 21.5 ± 0.1 (statistic) ± 0.1 (systematic) magnitudes, respectively. This is 170 and 80 times too bright in the g and r bands, respectively, if CVSO30c were an L0 substellar object as suggested by previous studies. The optical/infrared colors of CVSO30c are indicative of a stellar, not substellar object, while the object’s color–magnitude diagram position is strikingly inconsistent with expected values for a low-mass member of 25 Ori. Broadband photometry for CVSO30c is instead better fit by contaminants such as a background K3 giant or M subdwarf. Our study demonstrates that optical seeing-limited data can help clarify the nature of candidate wide separation planet-mass companions in young star-forming regions.