Transit timing variation analysis of the low-mass brown dwarf KELT-1 b

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BAŞTÜRK Ö., Southworth J., YALÇINKAYA S., Mancini L., ESMER E. M., Tekin M., ...Daha Fazla

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, cilt.521, sa.1, ss.1200-1209, 2023 (SCI-Expanded) identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 521 Sayı: 1
  • Basım Tarihi: 2023
  • Doi Numarası: 10.1093/mnras/stad248
  • Dergi Adı: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Applied Science & Technology Source, Communication Abstracts, Compendex, INSPEC, Metadex, zbMATH, DIALNET, Civil Engineering Abstracts
  • Sayfa Sayıları: ss.1200-1209
  • Anahtar Kelimeler: methods:data analysis, techniques:photometric, stars:fundamental parameteres, stars:individual:KELT-1-planetary systems, HIGH-PRECISION PHOTOMETRY, I., CATALOG, STARS, PLANETS, ECLIPSE, SYSTEMS, RADIUS
  • Ankara Üniversitesi Adresli: Evet

Özet

We investigate whether there is a variation in the orbital period of the short-period brown dwarf-mass KEL T-1 b, which is one of the best candidates to observe orbital decay. We obtain 19 high-precision transit light curves of the target using six different telescopes. We add all precise and complete transit light curves from open databases and the literature, as well as the available Transiting Exoplanet Survey Satellite (TESS) observations from sectors 17 and 57, to form a transit timing variation (TTV) diagram spanning more than 10 yr of observations. The analysis of the TTV diagram, however, is inconclusive in terms of a secular or periodic variation, hinting that the system might have synchronized. We update the transit ephemeris and determine an informati ve lo wer limit for the reduced tidal quality parameter of its host star of Q'(*) > (8 . 5 +/- 3 . 9) x 10 (6) assuming that the stellar rotation is not yet synchronized. Using our new photometric observations, published light curves, the TESS data, archi v al radial velocities, and broadband magnitudes, we also update the measured parameters of the system. Our results are in good agreement with those found in previous analyses.