Detection-Loophole-Free Test of Quantum Nonlocality, and Applications

We present a source of entangled photons that violates a Bell inequality free of the "fair-sampling" assumption, by over 7 standard deviations. This violation is the first experiment with photons to close the detection loophole, and we demonstrate enough "efficiency" overhead to eventually perform a fully loophole-free test of local realism. The entanglement quality is verified by maximally violating additional Bell tests, testing the upper limit of quantum correlations. Finally, we use the source to generate secure private quantum random numbers at rates over 4 orders of magnitude beyond previous experiments.Comment: Main text: 5 pages, 2 figures, 1 table. Supplementary Information: 7 pages, 2 figure

Two 'b's in the Beehive: The Discovery of the First Hot Jupiters in an Open Cluster

We present the discovery of two giant planets orbiting stars in Praesepe (also known as the Beehive Cluster). These are the first known hot Jupiters in an open cluster and the only planets known to orbit Sun-like, main-sequence stars in a cluster. The planets are detected from Doppler shifted radial velocities; line bisector spans and activity indices show no correlation with orbital phase, confirming the variations are caused by planetary companions. Pr0201b orbits a V=10.52 late F dwarf with a period of 4.4264 +/- 0.0070 days and has a minimum mass of 0.540 +/- 0.039 Mjup, and Pr0211b orbits a V=12.06 late G dwarf with a period of 2.1451 +/- 0.0012 days and has a minimum mass of 1.844 +/- 0.064 Mjup. The detection of 2 planets among 53 single members surveyed establishes a lower limit on the hot Jupiter frequency of 3.8 (+5.0)(-2.4) % in this metal-rich open cluster. Given the precisely known age of the cluster, this discovery also demonstrates that, in at least 2 cases, giant planet migration occurred within 600 Myr after formation. As we endeavor to learn more about the frequency and formation history of planets, environments with well-determined properties -- such as open clusters like Praesepe -- may provide essential clues to this end.Comment: 5 pages, 3 tables, 2 figures. Published in ApJ Letter

Hat-P-28b and Hat-P-29b: Two Sub-Jupiter Mass Transiting Planets

We present the discovery of two transiting exoplanets. HAT-P-28b orbits a V = 13.03 G3 dwarf star with a period P = 3.2572 days and has a mass of 0.63 ± 0.04 M_J and a radius of 1.21^(+0.11)_(–0.08) R_J yielding a mean density of 0.44 ± 0.09 g cm^(–3). HAT-P-29b orbits a V = 11.90 F8 dwarf star with a period P = 5.7232 days and has a mass of 0.78^(+0.08)_(–0.04) M_J and a radius of 1.11^(+0.14)_(–0.08) R_J yielding a mean density of 0.71 ± 0.18 g cm^(–3). We discuss the properties of these planets in the context of other known transiting planets

Parenting and toddler self‐regulation in low‐income families: What does sleep have to do with it?

Toddlerhood is a sensitive period in the development of self‐regulation, a set of adaptive skills that are fundamental to mental health and partly shaped by parenting. Healthy sleep is known to be critical for self‐regulation; yet, the degree to which child sleep alters interactive child–parent processes remains understudied. This study examines associations between observed parenting and toddler self‐regulation, with toddler sleep as a moderator of this association. Toddlers in low‐income families (N = 171) and their mothers were videotaped during free play and a self‐regulation challenge task; videos were coded for mothers’ behavior and affect (free play) and toddlers’ self‐regulation (challenge task). Mothers reported their child’s nighttime sleep duration via questionnaire. Results revealed significant Sleep × Maternal Negative Affect and Sleep × Maternal Negative Control interactions. Children who did not experience negative parenting had good self‐regulation regardless of their nighttime sleep duration. For children who did experience negative parenting, self‐regulation was intact among those who obtained more nighttime sleep, but significantly poorer among children who were getting less nighttime sleep. Thus, among children who were reported to obtain less nighttime sleep, there were more robust associations between negative parenting and poorer self‐regulation than among toddlers who were reported to obtain more sleep.RESUMENLos primeros años de la niñez son un período sensible en el desarrollo de la auto‐regulación, un grupo de habilidades adaptables que son fundamentales para la salud mental y a las que en parte les da forma la crianza. Es sabido que el dormir bien es esencial para la auto‐regulación y, aun así, el nivel al que el sueño del niño altera los procesos interactivos entre progenitor y niño permanece poco estudiado. Este estudio examina las asociaciones entre la crianza observada y la auto‐regulación del niño pequeño, tomando como moderador de tal asociación el proceso de dormir del niño pequeño. Se grabó en video a niños pequeños de familias de bajos ingresos (N=171) y sus madres durante una sesión de juego libre y una tarea de auto‐regulación que suponía un reto; los videos fueron codificados en cuanto al comportamiento y afecto de las madres (juego libre) y la auto‐regulación de los niños pequeños (tarea que suponía reto). Las madres reportaron acerca del sueño nocturno de sus niños por medio de un cuestionario. Los resultados revelaron interacciones significativas en cuanto al dormir y el negativo afecto materno, así como el dormir y el negativo control materno. Los niños que no experimentaron una crianza negativa tenían una buena auto‐regulación independientemente de la duración de su sueño nocturno. En el caso de los niños que experimentaron una crianza negativa, la auto‐regulación quedó intacta en aquellos que lograban más tiempo nocturno de dormir, pero fue significativamente más pobre en los niños que tenían menos tiempo de sueño nocturno. Por tanto, en el caso de los niños indicados en el reporte con menos tiempo de dormir nocturno, se dieron asociaciones más robustas entre la crianza negativa y una más pobre auto‐regulación que entre los niños pequeños indicados en el reporte con más tiempo de dormir.RÉSUMÉLa petite enfance est une période sensible dans le développement de l’auto‐régulation, un ensemble de compétences qui sont fondamentales pour la santé mentale et en partie formées par le parentage. L’on sait qu’un sommeil sain est critique pour l’auto‐régulation et pourtant la mesure dans laquelle le sommeil de l’enfant altère les processus interactifs enfant‐parent demeure peu étudiée. Cette étude examine les liens entre le parentage observé et l’auto‐régulation du petit enfant, le sommeil de l’enfant ayant un effet modérateur dans ce lien. Des jeunes enfants de familles issues de milieux défavorisés (N=171) et leurs mères ont été filmés durant un jeu libre et un exercice de défi d’auto‐régulation. Les vidéos ont été codées pour le comportement des mères et l’affect (jeu libre) et l’auto‐régulation des jeunes enfants (exercice de défi). Les mères ont fait état de la durée de sommeil nocturne de leur enfant au moyen d’un questionnaire. Les résultats ont révélé que : sommeil significatif x l’affect négatif maternel et le sommeil x négatif maternel contrôle les interactions. Les enfants qui n’avaient pas fait l’expérience d’un parentage négatif avaient une bonne auto‐régulation quelle qu’ait été la durée du sommeil nocturne. Pour les enfants ayant fait l’expérience d’une parentage négatif, l’auto‐régulation était intacte chez ceux ayant plus dormi, mais bien moindre chez les enfants qui avaient moins dormi. Donc, chez les enfants ayant moins de sommeil nocturne les liens bien plus robustes ont été découverts entre le parentage négatif et une moindre auto‐régulation que chez les petits enfants dormant plus durant la nuit.ZUSAMMENFASSUNGDas Kleinkindalter ist ein sensibler Zeitraum für die Entwicklung der Selbstregulation – einer Reihe von Anpassungsfähigkeiten, die für die psychische Gesundheit grundlegend sind und teilweise durch Erziehung geprägt werden. Gesunder Schlaf ist bekanntlich entscheidend für die Selbstregulation, aber das Ausmaß, in dem der Kinderschlaf interaktive Prozesse zwischen Kind und Eltern verändert, ist bisher nur unzureichend erforscht wurden. Diese Studie untersucht Zusammenhänge zwischen beobachtetem Erziehungsverhalten und der Selbstregulation von Kleinkindern, wobei der Schlaf der Kleinkinder als Moderator dieser Assoziation fungiert. Kleinkinder aus einkommensschwachen Familien (N=171) und ihre Mütter wurden während des freien Spiels und einer herausfordernden Aufgabe zur Selbstregulation gefilmt; die Videos wurden für das Verhalten und die Affekte der Mütter (freies Spiel) und die Selbstregulation der Kleinkinder (herausfordernde Aufgabe) kodiert. Die Mütter berichteten per Fragebogen über die nächtliche Schlafdauer ihres Kindes. Die Ergebnisse zeigten signifikante Interaktionen für Schlaf und mütterlichen negativen Affekt sowie für Schlaf und mütterliche negative Kontrollinteraktionen. Kinder, die keine negative Erziehung erlebten, hatten eine gute Selbstregulation, unabhängig von ihrer nächtlichen Schlafdauer. Bei Kindern, die eine negative Erziehung erfuhren, war die Selbstregulation bei denen, die mehr Nachtschlaf erhielten, intakt und bei Kindern, die weniger Nachtschlaf erhielten, jedoch deutlich schlechter. So gab es bei Kindern, von denen berichtet wurde, dass sie weniger Nachtschlaf erhielten, robustere Assoziationen zwischen negativer Erziehung und schlechterer Selbstregulation als bei Kleinkindern, von denen berichtet wurde, dass sie mehr Schlaf erhielten.抄録低収入家庭における子育てと幼児の自己調整力:睡眠が関与するものとは何か？幼児期は、自己調整力、つまりメンタルヘルスの基礎であり、ある程度までは子育てによって形成される、一連の適応スキルの発達が影響を受けやすい時期である。健康的な睡眠は自己調整力には不可欠のものとして知られているが、子どもの睡眠が子どもと親の相互作用の過程をどの程度まで改めるかについては、いまもなお研究課題のままである。本研究は、観察によって得られた子育てと幼児の自己調整力の関連性について幼児の睡眠を仲介として検討することである。低所得家庭 (N=171) で生活している幼児と母親が自由遊びと自己調整のチャレンジタスクに取り組む間中ビデオ録画した。ビデオデータは母親の行動と感情(自由遊び)と幼児の自己調整力(チャレンジタスク)としてコード化された。子どもの夜間の睡眠時間は母親からの質問紙を通して報告された。その結果、睡眠と母親の否定的感情の間、そして睡眠と母親の否定的コントロールの間には著しい相互関連性が認められた。否定的育児を経験していない子どもは、夜間の睡眠時間に関わらず、よい自己調整力を持っていた。否定的育児を経験した子どもでは、自己調整力はより長い夜間睡眠をとっている子どもにおいては保たれていたが、より短い睡眠時間しかとっていない子どもにおいては著しく低かった。このようにより短い睡眠時間しかとっていないと報告された子どもにおいては、より長い睡眠をとっている幼児より、否定的育児とより低い自己調整力の間により確かな関連性が示された。摘要低收入家庭的育兒和幼兒自我調節:與睡眠有什麼關係？幼兒期是自我調節發展的一個敏感時期， 這是一套適應性技能， 是心理健康的基礎， 部分由養育方式塑造。眾所周知， 健康睡眠對於自我調節至關重要， 然而， 兒童睡眠如何改變兒童 ‐ 父母互動仍未得到充分研究。本研究探討觀察到的養育方式與幼兒自我調節的關聯， 及幼兒睡眠作為這種關聯的調節變數。低收入家庭的幼兒 （N = 171） 和母親在自由遊戲和自我調節挑戰任務中被錄像; 視頻被編碼為母親的行為和情感 （自由遊戲） 和幼兒的自我調節 （挑戰任務）。母親通過問卷報告孩子的夜間睡眠時間。結果顯示顯著的睡眠x母體負面情感和睡眠 x 母體負面控制相互作用。沒有經歷負面養育的孩子， 無論夜間睡眠時間長短， 都有良好的自我調節能力。對於那些經歷過負面養育的孩子， 在夜間睡眠較多的人中， 自我調節是完整的， 但在夜間睡眠較少的孩子中， 自我調節顯著較差。因此， 在夜間睡眠較少的兒童中， 負面育兒和較差的自我調節的關聯性強於較多睡眠的幼兒。ملخصالرعاية الوالدية والتنظيم الذاتي للطفل في الأسر ذات الدخل المنخفض: ما علاقة النوم بذلك ؟الطفولة هي فتره حساسة في تطوير التنظيم الذاتي ، والذي يمثل مجموعه من المهارات التكيفيه التي هي أساسيه للصحة النفسية وتتشكل جزئيا عن طريق الأبوه والأمومه. ومن المعروف ان النوم الصحي أمر بالغ الاهميه للتنظيم الذاتي ، ومع ذلك ، فان الدرجة التي يغير بها نوم الطفل في العمليات التفاعلية التي يقوم بها الطفل مع الوالدين لا تزال غير خاضعة للدراسة الكافية. تتناول هذه الدراسة العلاقات بين الرعاية الوالدية الملحوظة والتنظيم الذاتي للطفل الصغير ، حيث نوم الطفل يمثل المتغير الوسيط في هذه العلاقة. اشترك في الدراسة مجموعة من الأطفال الصغار في الأسر ذات الدخل المنخفض (العدد = 171) وأمهاتهم وتم تصويرهم بالفيديو اثناء اللعب الحر مع تكليفهم بمهمة تحدي التنظيم الذاتي ؛ تم ترميز تسجيلات الفيديو لسلوك الأمهات وعاطفتهم في (اللعب الحر) والتنظيم الذاتي للأطفال الصغار في (مهمة التحدي). وأبلغت الأمهات عن مده النوم الليلي لأطفالهن عن طريق الاستبيان. أظهرت النتائج تفاعلات ذات دلالة إحصائية بين النوم والعاطفة السلبية عند الأمهات وبين النوم والسيطرة السلبية للأمهات . الأطفال الذين لا يعانون من الابوه والامومه السلبية كان لديهم قدرات جيدة على التنظيم الذاتي بغض النظر عن مده النوم ليلا. بالنسبة للأطفال الذين يعانون من الابوه والامومه السلبية ، كان التنظيم الذاتي سليما بين أولئك الذين حصلوا علي المزيد من النوم ليلا ، ولكن أضعف بكثير بين الأطفال الذين كانوا يحصلون علي اقل النوم ليلا. وبالتالي ، فانه من بين الأطفال الذين ابلغ عن حصولهم علي قسط اقل من النوم الليلي ، كانت هناك رابطات اقوي بين الرعاية الوالدية السلبية والتنظيم الذاتي الأقل منها بين الصغار الذين أفيد بأنهم يحصلون علي المزيد من النوم.Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/150525/1/imhj21783.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/150525/2/imhj21783_am.pd

Mc Neil's Nebula in Orion: The Outburst History

We present a sequence of I-band images obtained at the Venezuela 1m Schmidt telescope during the outburst of the nebula recently discovered by J.W. McNeil in the Orion L1630 molecular cloud. We derive photometry spanning the pre-outburst state and the brightening itself, a unique record including 14 epochs and spanning a time scale of ~5 years. We constrain the beginning of the outburst at some time between Oct. 28 and Nov. 15, 2003. The light curve of the object at the vertex of the nebula, the likely exciting source of the outburst, reveals that it has brightened ~5 magnitudes in about 4 months. The time scale for the nebula to develop is consistent with the light travel time, indicating that we are observing light from the central source scattered by the ambient cloud into the line of sight. We also show recent FLWO optical spectroscopy of the exciting source and of the nearby HH 22. The spectrum of the source is highly reddened; in contrast, the spectrum of HH 22 shows a shock spectrum superimposed on a continuum, most likely due to reflected light from the exciting source reaching the HH object through a much less reddened path. The blue portion of this spectrum is consistent with an early B spectral type, similar to the early outburst spectrum of the FU Ori variable V1057 Cyg; we estimate a luminosity of L ~219 Lsun. The eruptive behavior of the McNeil nebula source, its spectroscopic characteristics and luminosity, suggest we may be witnessing an FU Ori event on its way to maximum. Further monitoring of this object will decide whether it qualifies as a member of this rare class of objects.Comment: 13 pages, 4 figures, accepted to ApJ Letter

KELT-7b: A hot Jupiter transiting a bright V=8.54 rapidly rotating F-star

We report the discovery of KELT-7b, a transiting hot Jupiter with a mass of $1.28 \pm 0.18$ MJ, radius of $1.53_{-0.047}^{+0.046}$ RJ, and an orbital period of $2.7347749 \pm 0.0000039$ days. The bright host star (HD33643; KELT-7) is an F-star with $V=8.54$, Teff $=6789_{-49}^{+50}$ K, [Fe/H] $=0.139_{-0.081}^{+0.075}$, and $\log{g}=4.149 \pm 0.019$. It has a mass of $1.535_{-0.054}^{+0.066}$ Msun, a radius of $1.732_{-0.045}^{+0.043}$ Rsun, and is the fifth most massive, fifth hottest, and the ninth brightest star known to host a transiting planet. It is also the brightest star around which KELT has discovered a transiting planet. Thus, KELT-7b is an ideal target for detailed characterization given its relatively low surface gravity, high equilibrium temperature, and bright host star. The rapid rotation of the star ($73 \pm 0.5$ km/s) results in a Rossiter-McLaughlin effect with an unusually large amplitude of several hundred m/s. We find that the orbit normal of the planet is likely to be well-aligned with the stellar spin axis, with a projected spin-orbit alignment of $\lambda=9.7 \pm 5.2$ degrees. This is currently the second most rapidly rotating star to have a reflex signal (and thus mass determination) due to a planetary companion measured.Comment: Accepted to The Astronomical Journa

Steps Toward Determination of the Size and Structure of the Broad-Line Region in Active Galactic Nuclei. XVI. A Thirteen-Year Study of Spectral Variability in NGC 5548

We present the final installment of an intensive 13-year study of variations of the optical continuum and broad H-beta emission line in the Seyfert 1 galaxy NGC 5548. The data base consists of 1530 optical continuum measurements and 1248 H-beta measurements. The H-beta variations follow the continuum variations closely, with a typical time delay of about 20 days. However, a year-by-year analysis shows that the magnitude of emission-line time delay is correlated with the mean continuum flux. We argue that the data are consistent with the simple model prediction that the size of the broad-line region is proportional to the square root of the ionizing luminosity. Moreover, the apparently linear nature of the correlation between the H-beta response time and the nonstellar optical continuum arises as a consequence of the changing shape of the continuum as it varies, specifically with the optical (5100 A) continuum luminosity proportional to the ultraviolet (1350 A) continuum luminosity to the 0.56 power.Comment: 20 pages plus 4 figures. Accepted for publication in The Astrophysical Journa

KELT-1b: A Strongly Irradiated, Highly Inflated, Short Period, 27 Jupiter-mass Companion Transiting a mid-F Star

We present the discovery of KELT-1b, the first transiting low-mass companion from the wide-field Kilodegree Extremely Little Telescope-North (KELT-North) survey. The V=10.7 primary is a mildly evolved, solar-metallicity, mid-F star. The companion is a low-mass brown dwarf or super-massive planet with mass of 27.23+/-0.50 MJ and radius of 1.110+0.037-0.024 RJ, on a very short period (P=1.21750007) circular orbit. KELT-1b receives a large amount of stellar insolation, with an equilibrium temperature assuming zero albedo and perfect redistribution of 2422 K. Upper limits on the secondary eclipse depth indicate that either the companion must have a non-zero albedo, or it must experience some energy redistribution. Comparison with standard evolutionary models for brown dwarfs suggests that the radius of KELT-1b is significantly inflated. Adaptive optics imaging reveals a candidate stellar companion to KELT-1, which is consistent with an M dwarf if bound. The projected spin-orbit alignment angle is consistent with zero stellar obliquity, and the vsini of the primary is consistent with tidal synchronization. Given the extreme parameters of the KELT-1 system, we expect it to provide an important testbed for theories of the emplacement and evolution of short-period companions, and theories of tidal dissipation and irradiated brown dwarf atmospheres.Comment: 30 pages, 19 figures. Submitted to Ap

KELT-2Ab: A Hot Jupiter Transiting the Bright (V=8.77) Primary Star of a Binary System

We report the discovery of KELT-2Ab, a hot Jupiter transiting the bright (V=8.77) primary star of the HD 42176 binary system. The host is a slightly evolved late F-star likely in the very short-lived "blue-hook" stage of evolution, with \teff=6148\pm48{\rm K}, $\log{g}=4.030_{-0.026}^{+0.015}$ and \feh=0.034\pm0.78. The inferred stellar mass is $M_*=1.314_{-0.060}^{+0.063}$\msun\ and the star has a relatively large radius of $R_*=1.836_{-0.046}^{+0.066}$\rsun. The planet is a typical hot Jupiter with period $4.11379\pm0.00001$ days and a mass of $M_P=1.524\pm0.088$\mj\ and radius of $R_P=1.290_{-0.050}^{+0.064}$\rj. This is mildly inflated as compared to models of irradiated giant planets at the $\sim$4 Gyr age of the system. KELT-2A is the third brightest star with a transiting planet identified by ground-based transit surveys, and the ninth brightest star overall with a transiting planet. KELT-2Ab's mass and radius are unique among the subset of planets with $V<9$ host stars, and therefore increases the diversity of bright benchmark systems. We also measure the relative motion of KELT-2A and -2B over a baseline of 38 years, robustly demonstrating for the first time that the stars are bound. This allows us to infer that KELT-2B is an early K-dwarf. We hypothesize that through the eccentric Kozai mechanism KELT-2B may have emplaced KELT-2Ab in its current orbit. This scenario is potentially testable with Rossiter-McLaughlin measurements, which should have an amplitude of $\sim$44 m s$^{-1}$.Comment: 9 pages, 2 tables, 4 figures. A short video describing this paper is available at http://www.youtube.com/watch?v=wVS8lnkXXlE. Revised to reflect the ApJL version. Note that figure 4 is not in the ApJL versio

KELT-3b: A Hot Jupiter Transiting a V=9.8 Late-F Star

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).Comment: 12 pages, 12 figures, accepted to Ap