KELT-25b and KELT-26b: A Hot Jupiter and a Substellar Companion Transiting Young A-stars Observed by TESS. (arXiv:1912.01017v1 [astro-ph.EP])

KELT-25b and KELT-26b: A Hot Jupiter and a Substellar Companion Transiting Young A-stars Observed by TESS. (arXiv:1912.01017v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_R/0/1/0/all/0/1">Romy Rodr&#xed;guez Mart&#xed;nez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaudi_B/0/1/0/all/0/1">B. Scott Gaudi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_J/0/1/0/all/0/1">Joseph E. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_G/0/1/0/all/0/1">George Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Labadie_Bartz_J/0/1/0/all/0/1">Jonathan Labadie-Bartz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quinn_S/0/1/0/all/0/1">Samuel N. Quinn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penev_K/0/1/0/all/0/1">Kaloyan Minev Penev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tan_T/0/1/0/all/0/1">Thiam-Guan Tan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">David W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paredes_L/0/1/0/all/0/1">Leonardo A. Paredes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kielkopf_J/0/1/0/all/0/1">John Kielkopf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Addison_B/0/1/0/all/0/1">Brett C. Addison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_D/0/1/0/all/0/1">Duncan J. Wright</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Teske_J/0/1/0/all/0/1">Johanna K. Teske</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Howell_S/0/1/0/all/0/1">Steve B. Howell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciardi_D/0/1/0/all/0/1">David R. Ciardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ziegler_C/0/1/0/all/0/1">Carl Ziegler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stassun_K/0/1/0/all/0/1">Keivan G. Stassun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_M/0/1/0/all/0/1">Marshall C. Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eastman_J/0/1/0/all/0/1">Jason D. Eastman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siverd_R/0/1/0/all/0/1">Robert J. Siverd</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beatty_T/0/1/0/all/0/1">Thomas G. Beatty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouma_L/0/1/0/all/0/1">Luke G. Bouma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pepper_J/0/1/0/all/0/1">Joshua Pepper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lund_M/0/1/0/all/0/1">Michael B. Lund</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villanueva_S/0/1/0/all/0/1">Steven Villanueva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevens_D/0/1/0/all/0/1">Daniel J. Stevens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jensen_E/0/1/0/all/0/1">Eric L. N. Jensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kilby_C/0/1/0/all/0/1">Coleman Kilby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cohen_D/0/1/0/all/0/1">David H. Cohen</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:+Bieryla_A/0/1/0/all/0/1">Allyson Bieryla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cargile_P/0/1/0/all/0/1">Phillip A. Cargile</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_K/0/1/0/all/0/1">Karen A. Collins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conti_D/0/1/0/all/0/1">Dennis M. Conti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colon_K/0/1/0/all/0/1">Knicole D. Colon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Curtis_I/0/1/0/all/0/1">Ivan A. Curtis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DePoy_D/0/1/0/all/0/1">Darren L. DePoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_P/0/1/0/all/0/1">Phil A. Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feliz_D/0/1/0/all/0/1">Dax Feliz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gregorio_J/0/1/0/all/0/1">Joao Gregorio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rothenberg_J/0/1/0/all/0/1">Jason Rothenberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+James_D/0/1/0/all/0/1">David J. James</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Penny_M/0/1/0/all/0/1">Matthew T. Penny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reed_P/0/1/0/all/0/1">Phillip A. Reed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Relles_H/0/1/0/all/0/1">Howard M. Relles</a>, et al. (46 additional authors not shown)

We present the discoveries of KELT-25b (TIC 65412605, TOI-626.01) and
KELT-26b (TIC 160708862, TOI-1337.01), two transiting companions orbiting
relatively bright, early A-stars. The transit signals were initially detected
by the KELT survey, and subsequently confirmed by textit{TESS} photometry.
KELT-25b is on a 4.40-day orbit around the V = 9.66 star CD-24 5016 ($T_{rm
eff} = 8280^{+440}_{-180}$ K, $M_{star}$ = $2.18^{+0.12}_{-0.11}$
$M_{odot}$), while KELT-26b is on a 3.34-day orbit around the V = 9.95 star HD
134004 ($T_{rm eff}$ =$8640^{+500}_{-240}$ K, $M_{star}$ =
$1.93^{+0.14}_{-0.16}$ $M_{odot}$), which is likely an Am star. We have
confirmed the sub-stellar nature of both companions through detailed
characterization of each system using ground-based and textit{TESS}
photometry, radial velocity measurements, Doppler Tomography, and
high-resolution imaging. For KELT-25, we determine a companion radius of
$R_{rm P}$ = $1.64^{+0.039}_{-0.043}$ $R_{rm J}$, and a 3-sigma upper limit
on the companion’s mass of $sim64~M_{rm J}$. For KELT-26b, we infer a
planetary mass and radius of $M_{rm P}$ = $1.41^{+0.43}_{-0.51}$ $M_{rm J}$
and $R_{rm P}$ = $1.940^{+0.060}_{-0.058}$ $R_{rm J}$. From Doppler
Tomographic observations, we find KELT-26b to reside in a highly misaligned
orbit. This conclusion is weakly corroborated by a subtle asymmetry in the
transit light curve from the textit{TESS} data. KELT-25b appears to be in a
well-aligned, prograde orbit, and the system is likely a member of a cluster or
moving group.

We present the discoveries of KELT-25b (TIC 65412605, TOI-626.01) and
KELT-26b (TIC 160708862, TOI-1337.01), two transiting companions orbiting
relatively bright, early A-stars. The transit signals were initially detected
by the KELT survey, and subsequently confirmed by textit{TESS} photometry.
KELT-25b is on a 4.40-day orbit around the V = 9.66 star CD-24 5016 ($T_{rm
eff} = 8280^{+440}_{-180}$ K, $M_{star}$ = $2.18^{+0.12}_{-0.11}$
$M_{odot}$), while KELT-26b is on a 3.34-day orbit around the V = 9.95 star HD
134004 ($T_{rm eff}$ =$8640^{+500}_{-240}$ K, $M_{star}$ =
$1.93^{+0.14}_{-0.16}$ $M_{odot}$), which is likely an Am star. We have
confirmed the sub-stellar nature of both companions through detailed
characterization of each system using ground-based and textit{TESS}
photometry, radial velocity measurements, Doppler Tomography, and
high-resolution imaging. For KELT-25, we determine a companion radius of
$R_{rm P}$ = $1.64^{+0.039}_{-0.043}$ $R_{rm J}$, and a 3-sigma upper limit
on the companion’s mass of $sim64~M_{rm J}$. For KELT-26b, we infer a
planetary mass and radius of $M_{rm P}$ = $1.41^{+0.43}_{-0.51}$ $M_{rm J}$
and $R_{rm P}$ = $1.940^{+0.060}_{-0.058}$ $R_{rm J}$. From Doppler
Tomographic observations, we find KELT-26b to reside in a highly misaligned
orbit. This conclusion is weakly corroborated by a subtle asymmetry in the
transit light curve from the textit{TESS} data. KELT-25b appears to be in a
well-aligned, prograde orbit, and the system is likely a member of a cluster or
moving group.

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