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Register a new userKELT-14b and KELT-15b: An Independent Discovery of WASP-122b and a New Hot Jupiter
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Joseph Rodriguez Jr.
Publication date
2015
fields
Physics
and research's language is
English
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We report the discovery of KELT-14b and KELT-15b, two hot Jupiters from the KELT-South survey. KELT-14b, an independent discovery of the recently announced WASP-122b, is an inflated Jupiter mass planet that orbits a $sim5.0^{+0.3}_{-0.7}$ Gyr, $V$ = 11.0, G2 star that is near the main sequence turnoff. The host star, KELT-14 (TYC 7638-981-1), has an inferred mass $M_{*}$=$1.18_{-0.07}^{+0.05}$$M_{odot}$ and radius $R_{*}$=$1.37pm{-0.08}$$R_{odot}$, and has $T_{eff}$=$5802_{-92}^{+95}$K, $log{g_*}$=$4.23_{-0.04}^{+0.05}$ and =$0.33pm{0.09}$. The planet orbits with a period of $1.7100588 pm 0.0000025$ days ($T_{0}$=2457091.02863$pm$0.00047) and has a radius R$_{p}$=$1.52_{-0.11}^{+0.12}$$R_{J}$ and mass M$_{p}$=$1.196pm0.072$$M_{J}$, and the eccentricity is consistent with zero. KELT-15b is another inflated Jupiter mass planet that orbits a $sim$ $4.6^{+0.5}_{-0.4}$ Gyr, $V$ = 11.2, G0 star (TYC 8146-86-1) that is near the blue hook stage of evolution prior to the Hertzsprung gap, and has an inferred mass $M_{*}$=$1.181_{-0.050}^{+0.051}$$M_{odot}$ and radius $R_{*}$=$1.48_{-0.04}^{+0.09}$$R_{odot}$, and $T_{eff}$=$6003_{-52}^{+56}$K, $log{g_*}$=$4.17_{-0.04}^{+0.02}$ and [Fe/H]=$0.05pm0.03$. The planet orbits on a period of $3.329441 pm 0.000016$ days ($T_{0}$ = 2457029.1663$pm$0.0073) and has a radius R$_{p}$=$1.443_{-0.057}^{+0.11}$$R_{J}$ and mass M$_{p}$=$0.91_{-0.22}^{+0.21}$$M_{J}$ and an eccentricity consistent with zero. KELT-14b has the second largest expected emission signal in the K-band for known transiting planets brighter than $K<10.5$. Both KELT-14b and KELT-15b are predicted to have large enough emission signals that their secondary eclipses should be detectable using ground-based observatories.
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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 companions 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 discovery of KELT-22Ab, a hot Jupiter from the KELT-South survey. KELT-22Ab transits the moderately bright ($Vsim 11.1$) Sun-like G2V star TYC 7518-468-1. The planet has an orbital period of $P = 1.3866529 pm 0.0000027 $ days, a radius of $R_{P} = 1.285_{-0.071}^{+0.12}~R_{J}$, and a relatively large mass of $M_{P} = 3.47_{-0.14}^{+0.15}~ M_{J}$. The star has $R_{star} = 1.099_{-0.046}^{+0.079}~ R_{odot}$, $M_{star} = 1.092_{-0.041}^{+0.045}~ M_{odot}$, ${T_{rm eff},} = 5767_{-49}^{+50}~$ K, ${log{g_star}} = 4.393_{-0.060}^{+0.039}~$ (cgs), and [m/H] = $+0.259_{-0.083}^{+0.085}~$, and thus, other than its slightly super-solar metallicity, appears to be a near solar twin. Surprisingly, KELT-22A exhibits kinematics and a Galactic orbit that are somewhat atypical for thin disk stars. Nevertheless, the star is rotating quite rapidly for its estimated age, shows evidence of chromospheric activity, and is somewhat metal rich. Imaging reveals a slightly fainter companion to KELT-22A that is likely bound, with a projected separation of 6arcsec ($sim$1400 AU). In addition to the orbital motion caused by the transiting planet, we detect a possible linear trend in the radial velocity of KELT-22A suggesting the presence of another relatively nearby body that is perhaps non-stellar. KELT-22Ab is highly irradiated (as a consequence of the small semi-major axis of $a/R_{star} = 4.97$), and is mildly inflated. At such small separations, tidal forces become significant. The configuration of this system is optimal for measuring the rate of tidal dissipation within the host star. Our models predict that, due to tidal forces, the semi-major axis of KELT-22Ab is decreasing rapidly, and is thus predicted to spiral into the star within the next Gyr.
We present broad-band photometry of 30 planetary transits of the ultra-hot Jupiter KELT-16b, using five medium-class telescopes. The transits were monitored through standard B, V, R, I filters and four were simultaneously observed from different places, for a total of 36 new light curves. We used these new photometric data and those from the TESS space telescope to review the main physical properties of the KELT-16 planetary system. Our results agree with previous measurements but are more precise. We estimated the mid-transit times for each of these transits and combined them with others from the literature to obtain 69 epochs, with a time baseline extending over more than four years, and searched for transit time variations. We found no evidence for a period change, suggesting a lower limit for orbital decay at 8 Myr, with a lower limit on the reduced tidal quality factor of $Q^{prime}_{star}>(1.9 pm 0.8) times 10^5$ with $95%$ confidence. We built up an observational, low-resolution transmission spectrum of the planet, finding evidence of the presence of optical absorbers, although with a low significance. Using TESS data, we reconstructed the phase curve finding that KELT-16b has a phase offset of $25.25 pm 14.03$ $^{circ}$E, a day- and night-side brightness temperature of $3190 pm 61$ K and $2668 pm 56$ K, respectively. Finally, we compared the flux ratio of the planet over its star at the TESS and Spitzer wavelengths with theoretical emission spectra, finding evidence of a temperature inversion in the planets atmosphere, the chemical composition of which is preferably oxygen-rich rather than carbon-rich.
We report the discovery of KELT-3b, a moderately inflated transiting hot Jupiter with a mass of 1.477 (-0.067, +0.066) M_J, and radius of 1.345 +/- 0.072 R_J, with an orbital period of 2.7033904 +/- 0.000010 days. The host star, KELT-3, is a V=9.8 late F star with M_* = 1.278 (-0.061, +0.063) M_sun, R_* = 1.472 (-0.067, +0.065) R_sun, T_eff = 6306 (-49, +50) K, log(g) = 4.209 (-0.031, +0.033), and [Fe/H] = 0.044 (-0.082, +0.080), and has a likely proper motion companion. KELT-3b is the third transiting exoplanet discovered by the KELT survey, and is orbiting one of the 20 brightest known transiting planet host stars, making it a promising candidate for detailed characterization studies. Although we infer that KELT-3 is significantly evolved, a preliminary analysis of the stellar and orbital evolution of the system suggests that the planet has likely always received a level of incident flux above the empirically-identified threshold for radius inflation suggested by Demory & Seager (2011).
We report the discovery of KELT-4Ab, an inflated, transiting Hot Jupiter orbiting the brightest component of a hierarchical triple stellar system. The host star is an F star with $T_{rm eff}=6206pm75$ K, $log g=4.108pm0.014$, $left[{rm Fe}/{rm H}right]=-0.116_{-0.069}^{+0.065}$, ${rm M_*}=1.201_{-0.061}^{+0.067} {rm M}_{odot}$, and ${rm R_*}=1.610_{-0.068}^{+0.078} {rm R}_{odot}$. The best-fit linear ephemeris is $rm {BJD_{TDB}} = 2456193.29157 pm 0.00021 + Eleft(2.9895936 pm 0.0000048right)$. With a magnitude of $Vsim10$, a planetary radius of $1.699_{-0.045}^{+0.046} {rm R_J}$, and a mass of $0.902_{-0.059}^{+0.060} {rm M_J}$, it is the brightest host among the population of inflated Hot Jupiters ($R_P > 1.5R_J$), making it a valuable discovery for probing the nature of inflated planets. In addition, its existence within a hierarchical triple and its proximity to Earth ($210$ pc) provides a unique opportunity for dynamical studies with continued monitoring with high resolution imaging and precision radial velocities. In particular, the motion of the binary stars around each other and of both stars around the primary star relative to the measured epoch in this work should be detectable when it rises in October 2015.
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