SGR 1806-20 Is a Set of Independent Relaxation Systems

The Soft Gamma Repeater 1806-20 produced patterns of bursts during its 1983 outburst that indicate multiple independent energy accumulation sites, each driven by a continuous power source, with sudden, incomplete releases of the accumulated energy. The strengths of the power sources and their durations of activity vary over several orders of magnitude.Comment: Accepted ApJLett, 15 pages, 3 figure

Keck Deep Fields. III. Luminosity-dependent Evolution of the Ultraviolet Luminosity and Star Formation Rate Densities at z~4, 3, and 2

We use the Keck Deep Fields UGRI catalog of z~4, 3, and 2 UV-selected galaxies to study the evolution of the rest-frame 1700A luminosity density at high redshift. The ability to reliably constrain the contribution of faint galaxies is critical and our data do so as they reach to M*+2 even at z~4 and deeper still at lower redshifts. We find that the luminosity density at high redshift is dominated by the hitherto poorly studied galaxies fainter than L*, and, indeed, the the bulk of the UV light in the high-z Universe comes from galaxies in the luminosity range L=0.1-1L*. It is these faint galaxies that govern the behavior of the total UV luminosity density. Overall, there is a gradual rise in luminosity density starting at z~4 or earlier, followed by a shallow peak or a plateau within z~3--1, and then followed by the well-know plunge at lower redshifts. Within this total picture, luminosity density in sub-L* galaxies evolves more rapidly at high redshift, z>~2, than that in more luminous objects. However, this is reversed at lower redshifts, z<~1, a reversal that is reminiscent of galaxy downsizing. Within the context of the models commonly used in the observational literature, there seemingly aren't enough faint or bright LBGs to maintain ionization of intergalactic gas even as late as z~4. This is particularly true at earlier epochs and even more so if the faint-end evolutionary trends we observe at z~3 and 4 continue to higher redshifts. Apparently the Universe must be easier to reionize than some recent studies have assumed. Nevertheless, sub-L* galaxies do dominate the total UV luminosity density at z>~2 and this dominance further highlights the need for follow-up studies that will teach us more about these very numerous but thus far largely unexplored systems.Comment: Accepted for publication in the Astrophysical Journal. Abstract abridge

Trigonometric Parallaxes for 1,507 Nearby Mid-to-Late M-dwarfs

The MEarth survey is a search for small rocky planets around the smallest, nearest stars to the Sun as identified by high proper motion with red colors. We augmented our planetary search time series with lower cadence astrometric imaging and obtained two million images of approximately 1800 stars suspected to be mid-to-late M dwarfs. We fit an astrometric model to MEarth's images for 1507 stars and obtained trigonometric distance measurements to each star with an average precision of 5 milliarcseconds. Our measurements, combined with the 2MASS photometry, allowed us to obtain an absolute K_s magnitude for each star. In turn, this allows us to better estimate the stellar parameters than those obtained with photometric estimates alone and to better prioritize the targets chosen to monitor at high cadence for planetary transits. The MEarth sample is mostly complete out to a distance of 25 parsecs for stars of type M5.5V and earlier, and mostly complete for later type stars out to 20 parsecs. We find eight stars that are within ten parsecs of the Sun for which there did not exist a published trigonometric parallax distance estimate. We release with this work a catalog of the trigonometric parallax measurements for 1,507 mid-to-late M-dwarfs, as well as new estimates of their masses and radii.Comment: ApJ, accepted. 36 pages, 8 figures, 2 tables. Please find our data table here: http://www.cfa.harvard.edu/MEarth/DataDR2.htm

Ultrasonic NDE of Tubing Pinch Welds

Resistance tube closure welds, referred to as pinch welds, are used to reliably seal small stainless steel tubing. The pinch welding process, discussed in detail by Thomas et al [1], involves applying a load to force electrodes together to collapse the tube, sometimes in the presence of confining dies which prevent lateral expansion. Electric current is injected through the electrodes to soften the tube through Joule heating. The resulting hot plastic deformation causes contact and welding of the inner surfaces of the tube

Variation in Piglet Weights: Relationship to Suckling Behavior, Parity Number and Farrowing Crate Design

Suckling behavior and weight change of piglets were studied during the first 2 wk after birth. Thirty-six litters comprised a balanced comparison of parity number (first or second), litter size (8, 10 or 12), and two farrowing crate designs, one of which had a low horizontal bar that tended to impede the piglets\u27 access to the udder. Piglets showed the expected preference for the anterior teats although the preference was more apparent in the second parity than in the first. Teat fidelity was most pronounced at the two ends of the udder; piglets occupying the middle positions did more fighting during suckling and missed the milk ejection more often. Within litter variation in 14-day weight increased with increasing parity number of the dam. Initial weight explained 30-40% of within-litter variation in 14-day weight. Behavioral variables explained 2.6% of additional variation in first-parity litters, 18.1% in second-parity litters, and 22.9% in litters of older sows. Suckling position (anterior to posterior) and teat fidelity (consistency of suckling position) were the two behavioral factors most closely associated with 14-day weight. Mean litter 14-day weight showed the expected effect of litter size, but showed no differences attributable to parity number or farrowing crate design. However, within-litter variation in 14-day weight was greater (P \u3c 0.025) in the type of crate that impeded access to the udder. This may have been due to the somewhat higher levels of fighting, and to higher within-litter variance in fighting scores, seen in these crates

A Search for Additional Bodies in the GJ 1132 Planetary System from 21 Ground-based Transits and a 100 Hour Spitzer Campaign

We present the results of a search for additional bodies in the GJ 1132 system through two methods: photometric transits and transit timing variations of the known planet. We collected 21 transit observations of GJ 1132b with the MEarth-South array since 2015. We obtained 100 near-continuous hours of observations with the $Spitzer$ Space Telescope, including two transits of GJ 1132b and spanning 60\% of the orbital phase of the maximum period at which bodies coplanar with GJ 1132b would pass in front of the star. We exclude transits of additional Mars-sized bodies, such as a second planet or a moon, with a confidence of 99.7\%. When we combine the mass estimate of the star (obtained from its parallax and apparent $K_s$ band magnitude) with the stellar density inferred from our high-cadence $Spitzer$ light curve (assuming zero eccentricity), we measure the stellar radius of GJ 1132 to be $0.2105^{+0.0102}_{-0.0085} R_\odot$, and we refine the radius measurement of GJ 1132b to $1.130 \pm 0.056 R_\oplus$. Combined with HARPS RV measurements, we determine the density of GJ 1132b to be $6.2 \pm 2.0$\ g cm$^{-3}$, with the mass determination dominating this uncertainty. We refine the ephemeris of the system and find no evidence for transit timing variations, which would be expected if there was a second planet near an orbital resonance with GJ 1132b.Comment: 29 pages, 4 Tables, 8 Figures, Submitted to ApJ. Comments welcom

A Novel Fabrication Technique for Prescribed Interior Cracks in a Metal

One of the major concerns in nondestructive evaluation (NDE) is the detection and characterization of cracks in structural materials. In the development of NDE methodologies, laboratory samples containing known flaws are very useful for the experimental verification of models and algorithms. Simulated flaws made to specific design serve to check the correctness of various aspects of an NDE technique under development. In addition, model flaws are also used in the calibration of nondestructive testing equipments. A familiar example is the ubiquitous flat bottom hole test blocks

Selective Tooth Clipping in the Management of Low-Birth-Weight Piglets

A study was designed to test the potential benefits of selective tooth clipping (the practice of leaving the eye teeth intact in the smallest piglets of a litter to make them more competitive) under commercial conditions. A total of 346 litters were assigned to either the control treatment where all piglets had their teeth clipped, or the experimental treatment where one or more piglets of low birth weight had their teeth left intact. Piglets were weighed within 24 h of birth and at 7, 21 and 56 d. In litters of 12-14 animals, but not in smaller litters, the lower-birth-weight piglets had lower mortality in experimental than in control litters (32.0 vs. 39.8%), whereas higher-birth-weight piglets showed a trend in the opposite direction, with 14.4% mortality in experimental vs. 13.2% in control litters (P = 0.05. The weight gain of lower-birth-weight piglets was greater (166 vs. 143 g d‒1) in experimental than in control litters of 9-11 piglets, but the heavier piglets competing against the small litter-mates with intact teeth had lower weight gains than the controls (177 vs. 187 g d‒1) (P \u3c 0.02). Within-litter variance of 21-d weights was about 15% smaller (P \u3c 0.005) in experimental than in control litters. Thus, selective tooth-clipping does not improve overall growth and survival, but it contributes to more uniform weaning weights and may help the most vulnerable piglets to remain alive until fostering or other intervention can be accomplished

Hypermedia by coincidence

We introduce an approach to linking hypermedia documents dynamically in a decentralised, peer-to-peer manner using resources that are available by coincidence, without explicit configuration. The particular approach presented utilises an open platform in combination with Distributed Link Service technology enabling dynamic hypertext generation

The rotation and Galactic kinematics of mid M dwarfs in the Solar Neighborhood

Rotation is a directly-observable stellar property, and drives magnetic field generation and activity through a magnetic dynamo. Main sequence stars with masses below approximately 0.35Msun (mid-to-late M dwarfs) are fully-convective, and are expected to have a different type of dynamo mechanism than solar-type stars. Measurements of their rotation rates provide insights into these mechanisms, but few rotation periods are available for these stars at field ages. Using photometry from the MEarth transit survey, we measure rotation periods for 387 nearby, mid-to-late M dwarfs in the Northern hemisphere, finding periods from 0.1 to 140 days. The typical detected rotator has stable, sinusoidal photometric modulations at a semi-amplitude of 0.5 to 1%. We find no period-amplitude relation for stars below 0.25Msun and an anti-correlation between period and amplitude for higher-mass M dwarfs. We highlight the existence of older, slowly-rotating stars without H{\alpha} emission that nevertheless have strong photometric variability. The Galactic kinematics of our sample is consistent with the local population of G and K dwarfs, and rotators have metallicities characteristic of the Solar Neighborhood. We use the W space velocities and established age-velocity relations to estimate that stars with P<10 days are on average <2 Gyrs, and that those with P>70 days are about 5 Gyrs. The period distribution is mass dependent: as the mass decreases, the slowest rotators at a given mass have longer periods, and the fastest rotators have shorter periods. We find a lack of stars with intermediate rotation periods. [Abridged]Comment: Accepted to ApJ. Machine readable tables and additional figures are available in the published article or on reques