Miracle-dz/UniFAR-FTUs huggingface dataset:
A perspective of teachers’ appropriation of educational innovations

Purpose This paper proposes a framework describing teachers’ affective and cognitive thought processes, as well as the sensemaking and decision-making ongoing within them, during the various stages of the appropriation of an educational innovation. Design/methodology/approach The Rubicon model of action phases, borrowed from psychology, is first used as a lens to understand teacher will. The model is subsequently adapted to reconcile it with existing literature on teacher beliefs, teacher sensemaking, and teacher resistance. Findings The proposed framework shows that teachers’ appropriation of an educational innovation is multi-layered and multi-dimensional. This contradicts appropriation as simply a procedural implementation of research recommendations, culminating in only success or failure. Originality/value The paper sensitises policy makers, school leaders, and teacher educators to the complexity of the appropriation process. The proposed framework serves as a starting point for school and reform lea.
The ambitions and challenges of SROI

With the growing interest in measuring the social impact of third sector activities, there have been a range of approaches developed. One of these, social return on investment (SROI) has received particular attention and is being promoted by third sector organisations, as well as public and private bodies. This paper examines this approach in detail and identifies a series of issues that require further investigation. These include technical and methodological issues related to this adjusted cost-benefit analysis such as quantifying the value of social benefits, and attribution; the judgement involved in setting indicators; whether projects deemed successful based on an SROI analysis can provide the basis for replicability and scaling up; and the ways in which SROI is being used by stakeholders. Through examining these challenges in detail, the approaches to measuring social impact can be strengthened, standardised and made more rigorous. While the issues raised here are essential to developing SROI further, they are also valid for more general discussions regarding the proving and improving of the value added by the UK third sector.
1 Introduction to Fragment-based Drug Discovery

Fragment screening is the process of identifying relatively simple, often weakly potent, bioactive molecules. It is gaining wide acceptance as a successful hit-finding technique both in its own right and as a method of finding hit molecules when traditional high-throughput screening (HTS) methods fail. Fragment hits are typically highly ‘ligand efficient’, i.e. possess a high binding affinity per heavy atom, and thus are ideal for optimisation into clinical candidates with good drug-like properties. Fragment screening is being increasingly proven as a successful means of generating novel chemical starting material for drug discovery programmes. It has been the subject of numerous publications and reviews in the last few years. [1 5] Fragment screening was initially developed to generate hit compounds against targets for which other methods, such as HTS, had been unsuccessful. [6] At the same time, many shortcomings of HTS were becoming increasingly apparent:
Evaluating cooperative ITS

Cooperative Intelligent Transport Systems (C-ITS) is a subset of ITS which involves communicating and sharing information between ITS-stations. These ITS-stations comprise personal devices, vehicles, the roadside infrastructure and the back-office. The objective of C-ITS is `. to give advice or facilitate actions to improving safety, sustainability, efficiency and comfort beyond the scope of stand-alone systems'. C-ITS is also known as `connected vehicles' and require a substantial value chain to deliver the services and include vehicle manufacturers, in-vehicle product developers, electronics companies, app developers and mobile network operators.
Covariate Assisted Variable Ranking

Consider a linear model $y = X \beta + z$, $z \sim N(0, \sigma^2 I_n)$. The Gram matrix $\Theta = \frac{1}{n} X'X$ is non-sparse, but it is approximately the sum of two components, a low-rank matrix and a sparse matrix, where neither component is known to us. We are interested in the Rare/Weak signal setting where all but a small fraction of the entries of $\beta$ are nonzero, and the nonzero entries are relatively small individually. The goal is to rank the variables in a way so as to maximize the area under the ROC curve. We propose Factor-adjusted Covariate Assisted Ranking (FA-CAR) as a two-step approach to variable ranking. In the FA-step, we use PCA to reduce the linear model to a new one where the Gram matrix is approximately sparse. In the CAR-step, we rank variables by exploiting the local covariate structures. FA-CAR is easy to use and computationally fast, and it is effective in resolving signal cancellation, a challenge we face in regression models. FA-CAR is related to the recent idea of Covariate Assisted Screening and Estimation (CASE), but two methods are for different goals and are thus very different. We compare the ROC curve of FA-CAR with some other ranking ideas on numerical experiments, and show that FA-CAR has several advantages. Using a Rare/Weak signal model, we derive the convergence rate of the minimum sure-screening model size of FA-CAR. Our theoretical analysis contains several new ingredients, especially a new perturbation bound for PCA.
An Intermediate-Mass Black Hole Candidate in M51?

We present the current results of an investigation into M51 ULX-7, using archival data from XMM-Newton, Chandra and NuSTAR, and optical and radio data from HST and VLA. The source has a consistently hard power-law X-ray spectrum and high short-term variability. This is unusual variability behaviour for a ULX, as we would expect highly variable ULXs to have soft energy spectra. The power spectrum features a break at ~1e-3 Hz, from low frequency spectral index alpha=0.1 to high frequency spectral index alpha=0.8, analogous to the low frequency break found in power spectra of black holes accreting in the low/hard state. We do not observe a corresponding high frequency break, however taking the white noise level as a frequency lower limit of the break, we can calculate a black hole mass upper limit of 9.12e4 solar masses, assuming that the ULX is in the low/hard state. While there is no radio detection, we find a flux density upper limit of 87 micro-Jy/beam. Using the X-ray/radio fundamental plane, we calculate a black hole mass upper limit of 1.95e5 solar masses. Therefore, this ULX is consistent with being an IMBH accreting in the low/hard state.
News Shocks, Productivity and the U.S. Investment Boom-Bust Cycle

Overly optimistic expectations concerning productivity and consequent downward revisions are commonly viewed as a key determinant of U.S. investment during the boom-bust cycle of 1995--2003. This view is formalized and evaluated in a general equilibrium model with news shocks about future productivity and preferences for financial wealth. The model generates a boom-bust cycle in response to good news that is not realized. A method is devised to estimate "the productivity prospects": a series that captures the effects of news shocks on economic decisions. The estimated series rises during the boom, falls during the recession and helps forecast future productivity shocks at several horizons. The model's predictions for sample paths of hours worked, output, investment, consumption, wages and stock prices are largely in conformity with U.S. data. The model therefore offers a possible solution to several puzzles identified in the literature regarding the 1990's boom and the 2001 recession.
DEMOGRAPHICS OF THE GALAXIES HOSTING SHORT-DURATION GAMMA-RAY BURSTS

We present observations of the afterglows and host galaxies of three short-duration gamma-ray bursts (GRBs): 100625A, 101219A, and 110112A. We find that GRB 100625A occurred in a z = 0.452 early-type galaxy with a stellar mass of ≈4.6 × 109 M☉ and a stellar population age of ≈0.7 Gyr, and GRB 101219A originated in a star-forming galaxy at z = 0.718 with a stellar mass of ≈1.4 × 109 M☉, a star formation rate of ≈16 M☉ yr−1, and a stellar population age of ≈50 Myr. We also report the discovery of the optical afterglow of GRB 110112A, which lacks a coincident host galaxy to i ≳ 26 mag, and we cannot conclusively identify any field galaxy as a possible host. From afterglow modeling, the bursts have inferred circumburst densities of ≈10−4–1 cm−3 and isotropic-equivalent gamma-ray and kinetic energies of ≈1050–1051 erg. These three events highlight the diversity of galactic environments that host short GRBs. To quantify this diversity, we use the sample of 36 Swift short GRBs with robust associations to an environment (∼1/2 of 68 short bursts detected by Swift to 2012 May) and classify bursts originating from four types of environments: late-type (≈50%), early-type (≈15%), inconclusive (≈20%), and “host-less” (lacking a coincident host galaxy to limits of ≳ 26 mag; ≈15%). To find likely ranges for the true late- and early-type fractions, we assign each of the host-less bursts to either the late- or early-type category using probabilistic arguments and consider the scenario that all hosts in the inconclusive category are early-type galaxies to set an upper bound on the early-type fraction. We calculate most likely ranges for the late- and early-type fractions of ≈60%–80% and ≈20%–40%, respectively. We find no clear trend between gamma-ray duration and host type. We also find no change to the fractions when excluding events recently claimed as possible contaminants from the long GRB/collapsar population. Our reported demographics are consistent with a short GRB rate driven by both stellar mass and star formation.
Frivillighed blandt ældre: Aktiv aldring i civilsamfundet

This is a pre-copyedited, author-produced version of a book-chapter accepted for publication in “Det aldrende samfund: Udfordringer og nye muligheder” following peer review. The version of record is: Frederiksen, M. & Qvist, H-P: 2015: ”Frivillighed blandt ældre: Aktiv aldring i civilsamfundet”. In Jensen, P & Rostgaard, T (eds.): (pp. 113-133). Frydenlund Academic.
Unpacking Subjective Creativity Ratings: Using Embeddings to Explain and Measure Idea Novelty

Assessing similarity between design ideas is an inherent part of many design evaluations to measure novelty. In such evaluation tasks, humans excel at making mental connections among diverse knowledge sets and scoring ideas on their uniqueness. However, their decisions on novelty are often subjective and difficult to explain. In this paper, we demonstrate a way to uncover human judgment of design idea similarity using two dimensional idea maps. We derive these maps by asking humans for simple similarity comparisons of the form “Is idea A more similar to idea B or to idea C? ” We show that these maps give insight into the relationships between ideas and help understand the domain. We also propose that the novelty of ideas can be estimated by measuring how far items are on these maps. We demonstrate our methodology through the experimental evaluations on two datasets of colored polygons (known answer) and milk frothers (unknown answer) sketches. We show that these maps shed light on factors considered by raters in judging idea similarity. We also show how maps change when less data is ∗Address all correspondence to this author. available or false/noisy ratings are provided. This method provides a new direction of research into deriving ground truth novelty metrics by combining human judgments and computational
An Improved Cortical Surface Identification Method

Skull stripping head magnetic resonance (MR) images is a classification problem. Accurate segmentation is a difficult task due to the convoluted brain surface and the inapparent brain/non-brain boundaries in images.This paper presents an automated, robust, and accurate brain volume extraction method. The results show that our method can obtain more accurate results.
Patient safety: a core value of nursing - so why is achieving it so difficult?

Patient safety in the perioperative setting is determined by many interdependent factors including reliable systems, good teamwork, psychological safety, optimal communications and most crucially shared vision and goals. The necessary organizational, environmental and behavioural conditions for quality care are not new and were in fact known to Florence Nightingale as much as 150 years ago. As noted by Nightingale, and something that remains unchanged today, the greatest threat to patient safety are the frailties of the human condition, complacent attitudes and unconscious behaviours. Recognizing that error is normal and somewhat inevitable, given the complexity of modern surgery, is undoubtedly the first step to mitigating error and harm, and the basis from which to tackle variability and sub-optimal conditions to deliver quality improvement.
Influence of time and temperature of frozen storage and packaging method on functional properties and quality characteristics of beef and pork livers

2. When an image on the film is obliterated with a round black mark, it is an indication o f either blurred copy because o f movement during exposure, duplicate copy, or copyrighted materials that should not have been filmed. For blurred pages, a good image o f the page can be found in the adjacent frame. I f copyrighted materials were deleted, a target note will appear listing the pages in the adjacent frame.
THE OLD, SUPER-METAL-RICH OPEN CLUSTER, NGC 6791—ELEMENTAL ABUNDANCES IN TURN-OFF STARS FROM KECK/HIRES SPECTRA

The study of star clusters has advanced our understanding of stellar evolution, Galactic chemical evolution, and nucleosynthesis. Here we investigate the composition of turn-off stars in the intriguing open cluster, NGC 6791, which is old, but super-metal-rich with high-resolution (R = 46,000) Keck/HIRES spectra. We find [Fe/H] = +0.30 ± 0.02 from measurements of some 40 unblended, unsaturated lines of both Fe i and Fe ii in eight turn-off stars. Our O abundances come from the O i triplet near 7774 Å and we perform a differential analysis relative to the Sun from our Lunar spectrum also obtained with Keck/HIRES. The O results are corrected for small nLTE effects. We find consistent ratios of [O/Fe]n with a mean of −0.06 ± 0.02. This is low with respect to field stars that are also both old and metal-rich and continue the trend of decreasing [O/Fe] with increasing [Fe/H]. The small range in our oxygen abundances is consistent with a single population of stars. Our results for the alpha elements [Mg/Fe], [Si/Fe], [Ca/Fe], and [Ti/Fe] are near solar and compare well with those of the old, metal-rich field stars. The two Fe-peak elements, Cr and Ni, are consistent with Fe. These turn-off-star abundances provide benchmark abundances to investigate whether there are any observable abundance differences with the giants that might arise from nuclear-burning and dredge-up processes. Determinations of upper limits were found for Li by spectrum synthesis and are consistent with the upper limits in similar stars in the relatively old, super-metal-rich cluster NGC 6253. Our results support the prediction from standard theory that higher-metallicity stars deplete more Li. Probably no stars in NGC 6791 have retained their initial Li.
PARTICLE ACCELERATION IN SHOCK–SHOCK INTERACTION: MODEL TO DATA COMPARISON

Shock–shock interaction is a well-established particle acceleration mechanism in astrophysical and space plasmas, but difficult to study observationally. Recently, the interplanetary shock collision with the bow shock of the Earth on 1998 August 10 was identified as one of the rare events where detailed in situ observations of the different acceleration phases can be made. Due to the advantageous spacecraft and magnetic field configurations, in 2011, Hietala et al. were able to distinguish the seed population and its reacceleration at the bow shock, as well as the Fermi acceleration of particles trapped between the shocks. They also interpreted their results as being the first in situ evidence of the release of particles from the trap as the two shocks collided. In the present study we use a global 2.5D test-particle simulation to further study particle acceleration in this event. We concentrate on the last phases of the shock–shock interaction, when the shocks approach and pass through each other. The simulation results verify that the main features of the measurements can be explained by shock–shock interaction in this magnetic geometry, and are in agreement with the previous interpretation of particle release. Shock–shock collisions of this type occur commonly in many astrophysical locations such as stellar coronae, planetary and cometary bow shocks, and the distant heliosphere.
Nurmikasvuston puna-apilapitoisuuden voi ennustaa kalsiumpitoisuudesta

Tiivistelmä Puna-apilan lisäämisellä rehunurmiseoksiin on monia hyviä puolia. Apilapitoisuuden vaihtelu nurmissa on kuitenkin suurta. Biologisen typensidonnan arvioimiseen, sadonkorjuun ajoittamiseen ja rehun syöntipotentiaalin ennustamiseen tarvitaan tietoa apilan osuudesta nurmikasvustossa. Apilapitoisuuden määrittäminen botaanisella analyysillä on työlästä ja muilla menetelmillä kuten silmämääräisesti arvioiden varsin epätarkkaa. Puna-apilan kalsiumin (Ca) pitoisuus on huomattavasti korkeampi kuin nurmiheinien. Tämän tutkimuksen tarkoituksena oli selvittää, pystytäänkö nurmikasvuston puna-apilapitoisuus arvioimaan nurminäytteen Ca-pitoisuuden perusteella. Puna-apilan ja nurmiheinien seoskasvustoja seurattiin MTT:n tutkimuspaikoilla Juvalla ja Sotkamossa vuosina 2004-2006. Lohkot olivat luomuviljelyssä. Näytteiden Ca-pitoisuus määritettiin Valio Oy:n laboratoriossa XRF-menetelmällä (X-ray fluorescence). Näytteiden kalsiumpitoisuuden ja puna-apilan osuuden yhteyttä tarkasteltiin regressioanalyysillä. Yksinkertaisin yhtälö, jossa on mukana vain Ca-pitoisuus, toimi varsin hyvin. Selitysaste oli 0.800 ja mallin jäännösvaihtelu 10.7 %. Sen mukaan apilapitoisuus voitiin ennustaa yhtälöllä: Apilan osuus nurmikasvuston kuiva-aineessa (%) = -3.1 + 4.22 × Ca-pitoisuus (g(kg KA) Sadon (1 vs. 2. sato) huomioiminen paransi ennustetarkkuutta. Myös maan Ca-pitoisuudella oli merkitsevä vaikutus. Jos nämä lähtötiedot ovat käytettävissä, niiden hyödyntäminen on suositeltavaa. Artturi-verkkopalvelun (www.mtt.fi/artturi) Laskurit-sivulla on käytettävissä laskuri, johon voi tallentaa näytteen lähtötiedot ja saada tulokseksi nurmikasvuston apilapitoisuuden. Nurminäytteen Ca-pitoisuus määritetään Artturi-rehuanalyysin suppeassa kivennäisanalyysissä ja rehujen kivennäispitoisuudet ovat hyödyllisiä tietoja myös eläinten ruokinnan suunnittelussa, mikä puoltaa Ca-pitoisuuden käyttöä myös apilapitoisuuden arviointiin. Tämän tarkastelun perusteella yhteys vaikuttaa niin selvältä, että lähestymistapa on toimiva. Aineisto on kuitenkin pieni ja sisältää vain luomunurmista kerättyjä näytteitä. Muut tiedot mm. kasvuston kehitysvaiheesta (D-arvo) ja kemiallisesta koostumuksesta saattaisivat parantaa ennustetarkkuutta. Ca:n ja puna-apilan pitoisuuksien yhteys määritettiin tässä nurmikasvustosta kerätyistä ja kuivatuista näytteistä. Menetelmää voi käyttää myös säilörehunäytteiden apilapitoisuuden arvioimiseen, koska Ca-pitoisuudessa ei ole odotettavissa muutoksia säilönnän aikana.
SUPERNOVA PTF 09UJ: A POSSIBLE SHOCK BREAKOUT FROM A DENSE CIRCUMSTELLAR WIND

Type-IIn supernovae (SNe IIn), which are characterized by strong interaction of their ejecta with the surrounding circumstellar matter (CSM), provide a unique opportunity to study the mass-loss history of massive stars shortly before their explosive death. We present the discovery and follow-up observations of an SN IIn, PTF 09uj, detected by the Palomar Transient Factory (PTF). Serendipitous observations by Galaxy Evolution Explorer (GALEX) at ultraviolet (UV) wavelengths detected the rise of the SN light curve prior to the PTF discovery. The UV light curve of the SN rose fast, with a timescale of a few days, to a UV absolute AB magnitude of about −19.5. Modeling our observations, we suggest that the fast rise of the UV light curve is due to the breakout of the SN shock through the dense CSM (n ≈ 1010 cm−3). Furthermore, we find that prior to the explosion the progenitor went through a phase of high mass-loss rate (∼0.1 M☉ yr−1) that lasted for a few years. The decay rate of this SN was fast relative to that of other SNe IIn.
THE DENSE MOLECULAR GAS IN THE CIRCUMNUCLEAR DISK OF NGC 1068

We present a 190–307 GHz broadband spectrum obtained with Z-Spec of NGC 1068 with new measurements of molecular rotational transitions. After combining our measurements with those previously published and considering the specific geometry of this Seyfert 2 galaxy, we conduct a multi-species Bayesian likelihood analysis of the density, temperature, and relative molecular abundances of HCN, HNC, CS, and HCO+. We find that these molecules trace warm (T>100 K) gas of H2 number densities 104.2–104.9 cm−3. Our models also place strong constraints on the column densities and relative abundances of these molecules, as well as on the total mass in the circumnuclear disk. Using the uniform calibration afforded by the broad Z-Spec bandpass, we compare our line ratios to X-ray-dominated region (XDR) and photon-dominated region models. The majority of our line ratios are consistent with the XDR models at the densities indicated by the likelihood analysis, lending substantial support to the emerging interpretation that the energetics in the circumnuclear disk of NGC 1068 are dominated by accretion onto an active galactic nucleus.
Spitzer IRS data on λ Boötis stars : debris disks or di ff use ISM dust ?

λ Boötis stars are late-B to early-F type stars that are known to have a peculiar chemical abundance pattern. While they have roughly solar abundances of light elements (C, N, O, and S), the Fe-peak elements are significantly depleted. The abundance pattern of λ Boötis stars may be physically connected to their infrared (IR) excess. We investigate the circumstellar environment of a sample of λ Boötis stars in an effort to distinguish between different scenarios. If a debris disk gives rise to the infrared excess, the λ Boötis phenomenon may be related to the properties and evolution of the disk and be circumstellar in origin. On the other hand, if the anomalous abundance pattern is a result of selective accretion of interstellar gas, the infrared excess may be caused by an interstellar reflection nebula. SED modeling alone is not sufficient to constrain the properties of the stellar environment. Therefore we have performed a spectroscopic study with Spitzer IRS data to analyze the composition of the surrounding material of λ Boötis stars. This analysis also included a search for PAH features, since they would be a clear indication of the presence of interstellar matter. One of the conclusions of our project is that no signatures of PAHs could be detected in the IRS spectra. On the other hand, we have found that the onset of the infrared excess seems to indicate the presence of small sized grains. This implicates an interstellar origin of these grains, which may be an indication for the accretion of interstellar matter onto the stars. However, conclusive evidence has not been found.