170 research outputs found
Kepler eclipsing binary stars. VII. the catalogue of eclipsing binaries found in the entire Kepler data set
The primary Kepler Mission provided nearly continuous monitoring of ~200,000 objects with unprecedented photometric precision. We present the final catalog of eclipsing binary systems within the 105 deg2 Kepler field of view. This release incorporates the full extent of the data from the primary mission (Q0-Q17 Data Release). As a result, new systems have been added, additional false positives have been removed, ephemerides and principal parameters have been recomputed, classifications have been revised to rely on analytical models, and eclipse timing variations have been computed for each system. We identify several classes of systems including those that exhibit tertiary eclipse events, systems that show clear evidence of additional bodies, heartbeat systems, systems with changing eclipse depths, and systems exhibiting only one eclipse event over the duration of the mission. We have updated the period and galactic latitude distribution diagrams and included a catalog completeness evaluation. The total number of identified eclipsing and ellipsoidal binary systems in the Kepler field of view has increased to 2878, 1.3% of all observed Kepler targets
A rocky composition for an Earth-sized exoplanet
Planets with sizes between that of Earth (with radius R[subscript circle in cross]) and Neptune (about 4 R[subscript circle in cross]) are now known to be common around Sun-like stars. Most such planets have been discovered through the transit technique, by which the planet’s size can be determined from the fraction of starlight blocked by the planet as it passes in front of its star. Measuring the planet’s mass—and hence its density, which is a clue to its composition—is more difficult. Planets of size 2–4 R[subscript circle in cross] have proved to have a wide range of densities, implying a diversity of compositions, but these measurements did not extend to planets as small as Earth. Here we report Doppler spectroscopic measurements of the mass of the Earth-sized planet Kepler-78b, which orbits its host star every 8.5 hours (ref. 6). Given a radius of 1.20 ± 0.09 R[subscript circle in cross] and a mass of 1.69 ± 0.41 M[subscript circle in cross], the planet’s mean density of 5.3 ± 1.8 g cm[superscript −3] is similar to Earth’s, suggesting a composition of rock and iron.Kepler Participating Scientist Progra
Liveable Open Public Space - From Flaneur to Cyborg
Open public spaces have always been key elements of the city. Now they are also crucial for mixed reality. It is the main carrier of urban life, place for socialization, where users rest, have fun and talk. Moreover, “Seeing others and being seen” is a condition of socialization. Intensity of life in public spaces provides qualities like safety, comfort and attractiveness. Furthermore, open public spaces represent a spatial framework for meetings and multileveled interactions, and should include virtual flows, stimulating merging of physical and digital reality. Aim of the chapter is to present a critical analysis of public open spaces, aspects of their social role and liveability. It will also suggest how new technologies, in a mixed reality world, may enhance design approaches and upgrade the relationship between a user and his surroundings. New technologies are necessary for obtaining physical/digital spaces, becoming playable and liveable which will encourage walking, cycling, standing and interacting. Hence, they will attract more citizens and visitors, assure a healthy environment, quality of life and sociability. Public space, acting as an open book of the history of the city and of its future, should play a new role, being a place of reference for the flaneur/cyborg citizen personal and social life. The key result is a framework for understanding the particular importance of cyberparks in contemporary urban life in order to better adapt technologies in the modern urban life needs
Disintegrating Rocky Exoplanets
We discuss a new class of exoplanets that appear to be emitting a tail of
dusty effluents. These disintegrating planets are found close to their host
stars and have very hot, and likely molten, surfaces. The properties of the
dust should provide a direct probe of the constituent material of these rocky
bodies
The Orbit and Mass of the Third Planet in the Kepler-56 System
While the vast majority of multiple-planet systems have their orbital angular
momentum axes aligned with the spin axis of their host star, Kepler-56 is an
exception: its two transiting planets are coplanar yet misaligned by at least
40 degrees with respect to their host star. Additional follow-up observations
of Kepler-56 suggest the presence of a massive, non-transiting companion that
may help explain this misalignment. We model the transit data along with
Keck/HIRES and HARPS-N radial velocity data to update the masses of the two
transiting planets and infer the physical properties of the third,
non-transiting planet. We employ a Markov Chain Monte Carlo sampler to
calculate the best-fitting orbital parameters and their uncertainties for each
planet. We find the outer planet has a period of 1002 5 days and minimum
mass of 5.61 0.38 Jupiter masses. We also place a 95% upper limit of 0.80
m/s/yr on long-term trends caused by additional, more distant companions.Comment: 7 pages, 1 figure, 2 tables; accepted for publication in AJ. Minor
edits made after referee repor
Solitary median maxillary central incisor (SMMCI) syndrome
Solitary median maxillary central incisor syndrome (SMMCI) is a complex disorder consisting of multiple, mainly midline defects of development resulting from unknown factor(s) operating in utero about the 35th–38th day(s) from conception. It is estimated to occur in 1:50,000 live births. Aetiology is uncertain. Missense mutation in the SHH gene (I111F) at 7q36 may be associated with SMMCI. The SMMCI tooth differs from the normal central incisor, in that the crown form is symmetric; it develops and erupts precisely in the midline of the maxillary dental arch in both primary and permanent dentitions. Congenital nasal malformation (choanal atresia, midnasal stenosis or congenital pyriform aperture stenosis) is positively associated with SMMCI. The presence of an SMMCI tooth can predict associated anomalies and in particular the serious anomaly holoprosencephaly. Common congenital anomalies associated with SMMCI are: severe to mild intellectual disability, congenital heart disease, cleft lip and/or palate and less frequently, microcephaly, hypopituitarism, hypotelorism, convergent strabismus, oesophageal and duodenal atresia, cervical hemivertebrae, cervical dermoid, hypothyroidism, scoliosis, absent kidney, micropenis and ambiguous genitalia. Short stature is present in half the children. Diagnosis should be made by eight months of age, but can be made at birth and even prenatally at 18–22 weeks from the routine mid-trimester ultrasound scan. Management depends upon the individual anomalies present. Choanal stenosis requires emergency surgical treatment. Short stature may require growth hormone therapy. SMMCI tooth itself is mainly an aesthetic problem, which is ideally managed by combined orthodontic, prosthodontic and oral surgical treatment; alternatively, it can be left untreated
Precise Masses in the WASP-47 System
We present precise radial velocity observations of WASP-47, a star known to
host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional
transiting planets in short-period orbits: a super-Earth in a ~19 hour orbit,
and a Neptune in a ~9 day orbit. We analyze our observations from the HARPS-N
spectrograph along with previously published data to measure the most precise
planet masses yet for this system. When combined with new stellar parameters
and reanalyzed transit photometry, our mass measurements place strong
constraints on the compositions of the two small planets. We find unlike most
other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83
+/- 0.66 Me) and radius (1.810 +/- 0.027 Re) inconsistent with an Earth-like
composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding
an Earth-like core and mantle. We also perform a dynamical analysis to
constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This
planet likely orbits close to the plane of the inner three planets, suggesting
a quiet dynamical history for the system. Our dynamical constraints also imply
that WASP-47 c is much more likely to transit than a geometric calculation
would suggest. We calculate a transit probability for WASP-47 c of about 10%,
more than an order of magnitude larger than the geometric transit probability
of 0.6%.Comment: 15 pages, 3 figures, 3 tables. Accepted in A
Planetary Rings
Planetary rings are the only nearby astrophysical disks, and the only disks
that have been investigated by spacecraft. Although there are significant
differences between rings and other disks, chiefly the large planet/ring mass
ratio that greatly enhances the flatness of rings (aspect ratios as small as
1e-7), understanding of disks in general can be enhanced by understanding the
dynamical processes observed at close-range and in real-time in planetary
rings. We review the known ring systems of the four giant planets, as well as
the prospects for ring systems yet to be discovered. We then review planetary
rings by type. The main rings of Saturn comprise our system's only dense broad
disk and host many phenomena of general application to disks including spiral
waves, gap formation, self-gravity wakes, viscous overstability and normal
modes, impact clouds, and orbital evolution of embedded moons. Dense narrow
rings are the primary natural laboratory for understanding shepherding and
self-stability. Narrow dusty rings, likely generated by embedded source bodies,
are surprisingly found to sport azimuthally-confined arcs. Finally, every known
ring system includes a substantial component of diffuse dusty rings. Planetary
rings have shown themselves to be useful as detectors of planetary processes
around them, including the planetary magnetic field and interplanetary
impactors as well as the gravity of nearby perturbing moons. Experimental rings
science has made great progress in recent decades, especially numerical
simulations of self-gravity wakes and other processes but also laboratory
investigations of coefficient of restitution and spectroscopic ground truth.
The age of self-sustained ring systems is a matter of debate; formation
scenarios are most plausible in the context of the early solar system, while
signs of youthfulness indicate at least that rings have never been static
phenomena.Comment: 82 pages, 34 figures. Final revision of general review to be
published in "Planets, Stars and Stellar Systems", P. Kalas and L. French
(eds.), Springer (http://refworks.springer.com/sss
A large ground-based observing campaign of the disintegrating planet K2-22b
We present 45 ground-based photometric observations of the K2-22 system collected between 2016 December and 2017 May, which we use to investigate the evolution of the transit of the disintegrating planet K2-22b. Last observed in early 2015, in these new observations we recover the transit at multiple epochs and measure a typical depth of <1.5%. We find that the distribution of our measured transit depths is comparable to the range of depths measured in observations from 2014 and 2015. These new observations also support ongoing variability in the K2-22b transit shape and time, although the overall shallowness of the transit makes a detailed analysis of these transit parameters difficult. We find no strong evidence of wavelength-dependent transit depths for epochs where we have simultaneous coverage at multiple wavelengths, although our stacked Las Cumbres Observatory data collected over days-to-months timescales are suggestive of a deeper transit at blue wavelengths. We encourage continued high-precision photometric and spectroscopic monitoring of this system in order to further constrain the evolution timescale and to aid comparative studies with the other few known disintegrating planets
Breast cancer risk variants at 6q25 display different phenotype associations and regulate ESR1, RMND1 and CCDC170.
We analyzed 3,872 common genetic variants across the ESR1 locus (encoding estrogen receptor α) in 118,816 subjects from three international consortia. We found evidence for at least five independent causal variants, each associated with different phenotype sets, including estrogen receptor (ER(+) or ER(-)) and human ERBB2 (HER2(+) or HER2(-)) tumor subtypes, mammographic density and tumor grade. The best candidate causal variants for ER(-) tumors lie in four separate enhancer elements, and their risk alleles reduce expression of ESR1, RMND1 and CCDC170, whereas the risk alleles of the strongest candidates for the remaining independent causal variant disrupt a silencer element and putatively increase ESR1 and RMND1 expression.This is the author accepted manuscript. The final version is available from Nature Publishing Group via http://dx.doi.org/10.1038/ng.352
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