HATS-54b-HATS-58Ab: five new transiting hot Jupiters including one with a possible temperate companion. (arXiv:1812.07668v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Espinoza_N/0/1/0/all/0/1">Néstor Espinoza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartman_J/0/1/0/all/0/1">Joel D. Hartman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakos_G/0/1/0/all/0/1">Gaspar Á. Bakos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">Thomas Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayliss_D/0/1/0/all/0/1">Daniel Bayliss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bento_J/0/1/0/all/0/1">Joao Bento</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhatti_W/0/1/0/all/0/1">Waqas Bhatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brahm_R/0/1/0/all/0/1">Rafael Brahm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Csubry_Z/0/1/0/all/0/1">Zoltan Csubry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suc_V/0/1/0/all/0/1">Vincent Suc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jordan_A/0/1/0/all/0/1">Andrés Jordán</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mancini_L/0/1/0/all/0/1">Luigi Mancini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tan_T/0/1/0/all/0/1">T. G. Tan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penev_K/0/1/0/all/0/1">Kaloyan Penev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rabus_M/0/1/0/all/0/1">Markus Rabus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkis_P/0/1/0/all/0/1">Paula Sarkis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Val_Borro_M/0/1/0/all/0/1">Miguel de Val-Borro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Durkan_S/0/1/0/all/0/1">Stephen Durkan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lazar_J/0/1/0/all/0/1">Josef Lazar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Papp_I/0/1/0/all/0/1">Istvan Papp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sari_P/0/1/0/all/0/1">Pal Sari</a>
We report the discovery by the HATSouth project of 5 new transiting hot
Jupiters (HATS-54b through HATS-58Ab). HATS-54b, HATS-55b and HATS-58Ab are
prototypical short period ($P = 2.5-4.2$ days, $R_psim1.1-1.2$ $R_J$)
hot-Jupiters that span effective temperatures from 1350 K to 1750 K, putting
them in the proposed region of maximum radius inflation efficiency. The HATS-58
system is composed of two stars, HATS-58A and HATS-58B, which are detected
thanks to Gaia DR2 data and which we account for in the joint modelling of the
available data — with this, we are led to conclude that the hot jupiter
orbits the brighter HATS-58A star. HATS-57b is a short-period (2.35-day)
massive (3.15 $M_J$) 1.14 $R_J$, dense ($2.65pm0.21$ g cm$^{-3}$) hot-Jupiter,
orbiting a very active star ($2%$ peak-to-peak flux variability). Finally,
HATS-56b is a short period (4.32-day) highly inflated hot-Jupiter (1.7 $R_J$,
0.6 $M_J$), which is an excellent target for future atmospheric follow-up,
especially considering the relatively bright nature ($V=11.6$) of its F dwarf
host star. This latter exoplanet has another very interesting feature: the
radial velocities show a significant quadratic trend. If we interpret this
quadratic trend as arising from the pull of an additional planet in the system,
we obtain a period of $P_c = 815^{+253}_{-143}$ days for the possible planet
HATS-56c, and a minimum mass of $M_csin i_c = 5.11 pm 0.94$ $M_J$. The
candidate planet HATS-56c would have a zero-albedo equilibrium temperature of
$T_textrm{eq}=332pm 50$ K, and thus would be orbiting close to the habitable
zone of HATS-56. Further radial-velocity follow-up, especially over the next
two years, is needed to confirm the nature of HATS-56c.
We report the discovery by the HATSouth project of 5 new transiting hot
Jupiters (HATS-54b through HATS-58Ab). HATS-54b, HATS-55b and HATS-58Ab are
prototypical short period ($P = 2.5-4.2$ days, $R_psim1.1-1.2$ $R_J$)
hot-Jupiters that span effective temperatures from 1350 K to 1750 K, putting
them in the proposed region of maximum radius inflation efficiency. The HATS-58
system is composed of two stars, HATS-58A and HATS-58B, which are detected
thanks to Gaia DR2 data and which we account for in the joint modelling of the
available data — with this, we are led to conclude that the hot jupiter
orbits the brighter HATS-58A star. HATS-57b is a short-period (2.35-day)
massive (3.15 $M_J$) 1.14 $R_J$, dense ($2.65pm0.21$ g cm$^{-3}$) hot-Jupiter,
orbiting a very active star ($2%$ peak-to-peak flux variability). Finally,
HATS-56b is a short period (4.32-day) highly inflated hot-Jupiter (1.7 $R_J$,
0.6 $M_J$), which is an excellent target for future atmospheric follow-up,
especially considering the relatively bright nature ($V=11.6$) of its F dwarf
host star. This latter exoplanet has another very interesting feature: the
radial velocities show a significant quadratic trend. If we interpret this
quadratic trend as arising from the pull of an additional planet in the system,
we obtain a period of $P_c = 815^{+253}_{-143}$ days for the possible planet
HATS-56c, and a minimum mass of $M_csin i_c = 5.11 pm 0.94$ $M_J$. The
candidate planet HATS-56c would have a zero-albedo equilibrium temperature of
$T_textrm{eq}=332pm 50$ K, and thus would be orbiting close to the habitable
zone of HATS-56. Further radial-velocity follow-up, especially over the next
two years, is needed to confirm the nature of HATS-56c.
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