Homogeneously derived transit timings for 17 exoplanets and reassessed TTV trends for WASP-12 and WASP-4. (arXiv:1908.04505v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Baluev_R/0/1/0/all/0/1">R.V. Baluev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokov_E/0/1/0/all/0/1">E.N. Sokov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_H/0/1/0/all/0/1">H.R.A. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shaidulin_V/0/1/0/all/0/1">V.Sh. Shaidulin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sokova_I/0/1/0/all/0/1">I.A. Sokova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nielsen_L/0/1/0/all/0/1">L.D. Nielsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benni_P/0/1/0/all/0/1">P. Benni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneiter_E/0/1/0/all/0/1">E.M. Schneiter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAngelo_C/0/1/0/all/0/1">C. Villarreal D'Angelo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Lajus_E/0/1/0/all/0/1">E. Fernández-Lajús</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sisto_R/0/1/0/all/0/1">R.P. Di Sisto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basturk_O/0/1/0/all/0/1">Ö. Baştürk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bretton_M/0/1/0/all/0/1">M. Bretton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wunsche_A/0/1/0/all/0/1">A. Wunsche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hentunen_V/0/1/0/all/0/1">V.-P. Hentunen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shadick_S/0/1/0/all/0/1">S. Shadick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jongen_Y/0/1/0/all/0/1">Y. Jongen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kang_W/0/1/0/all/0/1">W. Kang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_T/0/1/0/all/0/1">T. Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pakstiene_E/0/1/0/all/0/1">E. Pakštienė</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qvam_J/0/1/0/all/0/1">J.K.T. Qvam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knight_C/0/1/0/all/0/1">C.R. Knight</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerra_P/0/1/0/all/0/1">P. Guerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchini_A/0/1/0/all/0/1">A. Marchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvaggio_F/0/1/0/all/0/1">F. Salvaggio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Papini_R/0/1/0/all/0/1">R. Papini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_P/0/1/0/all/0/1">P. Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salisbury_M/0/1/0/all/0/1">M. Salisbury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_F/0/1/0/all/0/1">F. Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molina_D/0/1/0/all/0/1">D. Molina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garlitz_J/0/1/0/all/0/1">J. Garlitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Esseiva_N/0/1/0/all/0/1">N. Esseiva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogmen_Y/0/1/0/all/0/1">Y. Ogmen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karavaev_Y/0/1/0/all/0/1">Yu. Karavaev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rusov_S/0/1/0/all/0/1">S. Rusov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ibrahimov_M/0/1/0/all/0/1">M.A. Ibrahimov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karimov_R/0/1/0/all/0/1">R.G. Karimov</a>
We homogeneously analyse $sim 3.2times 10^5$ photometric measurements for
$sim 1100$ transit lightcurves belonging to $17$ exoplanet hosts. The
photometric data cover $16$ years 2004–2019 and include amateur and
professional observations. Old archival lightcurves were reprocessed using
up-to-date exoplanetary parameters and empirically debiased limb-darkening
models. We also derive self-consistent transit and radial-velocity fits for
$13$ targets. We confirm the nonlinear TTV trend in the WASP-12 data at a high
significance, and with a consistent magnitude. However, Doppler data reveal
hints of a radial acceleration about $(-7.5pm 2.2)$~m/s/yr, indicating the
presence of unseen distant companions, and suggesting that roughly $10$ per
cent of the observed TTV was induced via the light-travel (or Roemer) effect.
For WASP-4, a similar TTV trend suspected after the recent TESS observations
appears controversial and model-dependent. It is not supported by our
homogeneus TTV sample, including $10$ ground-based EXPANSION lightcurves
obtained in 2018 simultaneously with TESS. Even if the TTV trend itself does
exist in WASP-4, its magnitude and tidal nature are uncertain. Doppler data
cannot entirely rule out the Roemer effect induced by possible distant
companions.
We homogeneously analyse $sim 3.2times 10^5$ photometric measurements for
$sim 1100$ transit lightcurves belonging to $17$ exoplanet hosts. The
photometric data cover $16$ years 2004–2019 and include amateur and
professional observations. Old archival lightcurves were reprocessed using
up-to-date exoplanetary parameters and empirically debiased limb-darkening
models. We also derive self-consistent transit and radial-velocity fits for
$13$ targets. We confirm the nonlinear TTV trend in the WASP-12 data at a high
significance, and with a consistent magnitude. However, Doppler data reveal
hints of a radial acceleration about $(-7.5pm 2.2)$~m/s/yr, indicating the
presence of unseen distant companions, and suggesting that roughly $10$ per
cent of the observed TTV was induced via the light-travel (or Roemer) effect.
For WASP-4, a similar TTV trend suspected after the recent TESS observations
appears controversial and model-dependent. It is not supported by our
homogeneus TTV sample, including $10$ ground-based EXPANSION lightcurves
obtained in 2018 simultaneously with TESS. Even if the TTV trend itself does
exist in WASP-4, its magnitude and tidal nature are uncertain. Doppler data
cannot entirely rule out the Roemer effect induced by possible distant
companions.
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