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Finding new interventions that slow ageing and maintain human health is a huge challenge of our time. The nematode Caenorhabditis elegansoffers a rapid in vivo method to determine whether a compound extends its 2 to 3-week lifespan. Measuring lifespan is the standard method to monitor ageing, but a compound that extends lifespan will not necessarily maintain health. Here, we describe the automated monitoring of C. elegansmovement from early to mid-adulthood as a faster healthspan-based method to measure ageing. Using the WormGazer™ technology, multiple Petri dishes each containing several C. elegansworms are imaged simultaneously and non-invasively by an array of cameras that can be scaled easily. This approach demonstrates that most functional decline in C. elegansoccurs during the first week of adulthood. We find 7 days of imaging is sufficient to measure the dose-dependent efficacy of sulfamethoxazole to slow ageing, compared to 40 days required for a parallel lifespan experiment. Understanding any negative consequences of interventions that slow ageing is important. We show that the long-lived mutant age-1(hx546)stays active for longer than the wild type but it moves slower in early adulthood. Thus, continuous analysis of movement can rapidly identify interventions that slow ageing while simultaneously revealing any negative effects on health.

Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far.

Context. We are engaged in a multi-wavelength study of several Galactic H iiregions that exhibit signposts of triggered star formation on their borders, where the collect and collapse process could be at work.

Context.To investigate the process of star formation triggered by the expansion of an H iiregion, we present a multi-wavelength analysis of the Galactic H iiregion RCW 120 and its surroundings. The collect and collapse model predicts that the layer of gas and dust accumulated between the ionization and shock fronts during the expansion of the H iiregion collapses and forms dense fragments, giving rise to potential sites of massive-star formation.

Context.Massive-star formation triggered by the expansion of H iiregions.

We present SEST-SIMBA 1.2-mm continuum maps and ESO-NTT SOFI JHKSimages of the Galactic H iiregion RCW 79. The millimetre continuum data reveal the presence of massive fragments located in a dust emission ring surrounding the ionized gas. The two most massive fragments are diametrically opposite each other in the ring. The near-IR data, centred on the compact H iiregion located at the south-eastern border of RCW 79, show the presence of an IR-bright cluster containing massive stars along with young stellar objects with near-IR excesses. A bright near- and mid-IR source is detected towards maser emissions, 1.2 pc north-east of the compact H iiregion centre. Additional information extracted from the Spitzer GLIMPSE survey is used to discuss the nature of the bright IR sources observed towards RCW 79. Twelve luminous Class I sources are identified towards the most massive millimetre fragments. All these facts strongly indicate that the massive-star formation observed at the border of the H iiregion RCW 79 has been triggered by its expansion, most probably by the collect and collapse process.

We present millimetre-line imaging of the Galactic H iiregion Sh 104. We show that it is surrounded by a ring of molecular gas and dust. Four large molecular condensations are regularly spaced around the ring. These condensations are themselves fragmented and contain several massive dense cores. A deeply embedded cluster is observed in the near IR towards the largest condensation. It contains at least one massive star ionizing an ultra-compact H iiregion. The Sh 104 region is a good illustration of the “collect and collapse” model for star formation triggered by the expansion of an H iiregion.

RAFGL7009S is a deeply embedded massive young stellar objet (YSO) showing strong ice and saturated silicate absorption features in the mid infrared. It is associated with the ultracompact H iiregion G25.65+1.05, which may be excited by a B1V star. We have obtained JHKimages of a $1\arcmin$field centred on this YSO. In Kwe detect a non-resolved object coinciding with the radio continuum emission peak. Considering the high extinction towards this source ($A_V \geq $100 mag), the observed Kemission is more than 7 mag in excess of that expected for a B1V star. We suggest that this emission is mainly due to scattering of the central zone emission, as recently found for a sample of embedded massive YSOs associated with 3.1 μm H2O ice absorption (Ishii et al. [CITE]). We estimate the YSO's age to be 2$\times$104years. The outflow, the methanol maser emission and the strong ice absorption features suggest the presence of a dense medium very close to the star, possibly a disk.

We present 3-12 μm ISOCAM observations of the five Galactic compact H iiregions Sh 61, Sh 138, Sh 152, Sh 156 and Sh 186. The unidentified infrared bands (UIBs) centred at 3.3, 6.2, 7.7, 8.6 and 11.2 μm -and underlying continuum -are imaged using the SW1, SW2, LW4, LW6 and LW8 filters. Images are also obtained at 5.985, 6.911, 8.222, 10.520 and 12.000 μm using the circular variable filter (CVF). We show that the 5.985 μm emission represents a true continuum reference for the 6.2 μm band, allowing a derivation of this band's properties. Due to uncertainties in the continuum estimates, only lower limits can be given for the 3.3, 7.7 and 11.3 μm band fluxes. These limits agree with previous results found in the literature. The distribution of the bands coincide. The 3.3 μm emission is not observed in high extinction zones, suggesting a lower temperature of the carriers and/or a higher abundance of larger molecules in those zones. The 6.2 μm band emission peaks outside the ionized zone, in the photodissociation region. The 6.2 μm band luminosity correlates with the far UV field intensity, suggesting a UV excitation. We also find a correlation between the spatial distribution of the 6.2 μm band emission and zones of strong 2.122 μm H2emission due to ultraviolet fluorescence. This suggests that both emissions are due to UV excitation. The 6.2 μm emission is slightly closer to the exciting star. This suggests that the band carriers survive in the H izone. The 12 μm emission traces the continuum emission from very small grains, when present, and follows well the distribution of UIB emission. This suggests a link between the two emission carriers. The emission peak observed on the star in Sh 61 and Sh 156 indicates that the continuum from very small grains dominates the emission in highly excited regions.

The article focuses on the history of the economy of Cyprus between 650 - 800 CE. The article covers topics including the traditional view of the Cypriot economy as impacted by Arab raids, the imperial government structure and the role of ecclesiastical power during this time. The article goes on to discuss evidence including the import of ceramics, items such as seals and coins and profiles of settlements in Cyprus.

The Far-Infrared Surveyor (FIS) onboard the AKARI satellite has a spectroscopic capability provided by a Fourier transform spectrometer (FIS–FTS). FIS–FTS is the first space-borne imaging FTS dedicated to far-infrared astronomical observations. We describe the calibration process of the FIS–FTS, and discuss its accuracy and reliability. The calibration is based on observational data of bright astronomical sources as well as two instrumental sources. We have compared the FIS–FTS spectra with the spectra obtained from the Long Wavelength Spectrometer (LWS) of the Infrared Space Observatory (ISO), having a similar spectral coverage. The present calibration method accurately reproduces the spectra of several solar system objects having a reliable spectral model. Under this condition the relative uncertainty of the calibration of the continuum is estimated to be $\pm$15% for SW, $\pm$10% for 70–85 cm$^{-1}$of LW, and $\pm$20% for 60–70 cm$^{-1}$of LW; and the absolute uncertainty is estimated to be $+$35%/$-$55% for SW, $+$35%/$-$55% for 70–85 cm$^{-1}$of LW, and $+$40%/$-$60% for 60–70 cm$^{-1}$of LW. These values have been confirmed by comparisons with theoretical models and previous observations by the ISO / LWS.

Hi-GAL, the Herschel infrared Galactic Plane Survey, is an Open Time Key Project of the Herschel Space Observatory. It will make an unbiased photometric survey of the inner Galactic plane by mapping a 2° wide strip in the longitude range ?l? < 60° in five wavebands between 70 ?m and 500 ?m. The aim of Hi-GAL is to detect the earliest phases of the formation of molecular clouds and high-mass stars and to use the optimum combination of Herschelwavelength coverage, sensitivity, mapping strategy, and speed to deliver a homogeneous census of star-forming regions and cold structures in the interstellar medium. The resulting representative samples will yield the variation of source temperature, luminosity, mass and age in a wide range of Galactic environments at all scales from massive YSOs in protoclusters to entire spiral arms, providing an evolutionary sequence for the formation of intermediate and high-mass stars. This information is essential to the formulation of a predictive global model of the role of environment and feedback in regulating the star-formation process. Such a model is vital to understanding star formation on galactic scales and in the early universe. Hi-GAL will also provide a science legacy for decades to come with incalculable potential for systematic and serendipitous science in a wide range of astronomical fields, enabling the optimum use of future major facilities such as JWSTand ALMA.

Context. Thanks to its excellent 5100?m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so?far.Aims. Our goal is to produce a large-scale, systematic database of massive pre- and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. Only a systematic survey of the Galactic Plane can provide the statistical basis for unbiased studies. A?well characterized sample of Galactic star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submillimeter wavelengths also represents a preparatory work for Herschel and ALMA.Methods. The APEX telescope is ideally located to observe the inner Milky?Way. The Large APEX Bolometer Camera (LABOCA) is a?295-element bolometer array observing at?870??m, with a beam size of?[Formula: see text]19[Formula: see text]. Taking advantage of its large field of view?(11[Formula: see text][Formula: see text]) and excellent sensitivity, we started an unbiased survey of the entire Galactic Plane accessible to APEX, with a typical noise level of 50-70?mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL).Results. As a first step, we covered ~95?deg2of the Galactic Plane. These data reveal ~6000?compact sources brighter than 0.25?Jy, or 63?sources per square degree, as well as extended structures, many of them filamentary. About two thirds of the compact sources have no bright infrared counterpart, and some of them are likely to correspond to the precursors of (high-mass) proto-stars or proto-clusters. Other compact sources harbor hot cores, compact H?ii?regions, or young embedded clusters, thus tracing more evolved stages after massive stars have formed. Assuming a typical distance of 5?kpc, most sources are clumps smaller than 1?pc with masses from a?few?10 to a?few 100?M?. In this first introductory paper, we show preliminary results from these ongoing observations, and discuss the mid- and long-term perspectives of the?survey.

Abstract: Introduction: Today breast cancer (BC) patients can expect more prolonged survival than in the past, but obesity at diagnosis and/or weight gain during adjuvant therapies increase the risk of recurrences as well as of weight-related disorders (diabetes, cardiovascular disease…). Therefore lifestyle intervention might offer a valuable approach to positively influence the prognosis of survivors. Design and objectives: The charts of 189 overweight/obese outpatients with “early-stage BC” were reviewed to evaluate the effects of nutritional intervention on weight, body mass index (BMI), waist circumference and metabolic parameters. After the first clinical evaluation, in 97 subjects (education group), dieting therapy and periodical medical examinations were connected with brief individual sessions of nutritional education. Instead, 92 patients (no-education group) were treated only with diet and routine visits. At baseline and after nearly 1 year of treatment, data (weight, waist circumference, BMI, systolic and diastolic pressure, metabolic parameters and results of a battery of self-administered questionnaires to assess Nutritional Knowledge (NK), Physical Functioning (PF) and Quality Of Life (QOL) of patients) were collected and compared. Results: Ninety-two (48.7%) patients completed a oneyear follow-up. The dropout rate was higher (73.2%) in traditionally treated women (no-education group) than in education group patients (22.8%); these data highlight that more educated patients completed the programme than non-educated patients (ODs 9.2, p < 0.000). The low follow-up rate makes any comparison between the 2 types of treatment impossible since the weight and metabolic changes of the vast majority of the non-educated subjects remain unknown. Anyway, the education group patients, in active follow-up at 1 year, showed significant weight loss (−6.6 kg, SD 3.7) and improvements of metabolic parameters and questionnaire scores. Conclusions: Data from the study show the usefulness of this simple nutritional education intervention, which appears to increase the adherence to a weight loss programme. In educated patients who completed a 1-year follow-up, the weight reduction and metabolic changes were significant, but the analysis was carried out on less than half of the subjects and this very high global dropout rate (51.3%) makes it impossible to draw generalised conclusions.

Introduction: Today breast cancer (BC) patients can expect more prolonged survival than in the past, but obesity at diagnosis and/or weight gain during adjuvant therapies increase the risk of recurrences as well as of weight-related disorders (diabetes, cardiovascular disease?…?). Therefore lifestyle intervention might offer a valuable approach to positively influence the prognosis of survivors. Design and objectives: The charts of 189 overweight/obese outpatients with “early-stage BC” were reviewed to evaluate the effects of nutritional intervention on weight, body mass index (BMI), waist circumference and metabolic parameters. After the first clinical evaluation, in 97 subjects (education group), dieting therapy and periodical medical examinations were connected with brief individual sessions of nutritional education. Instead, 92 patients (no-education group) were treated only with diet and routine visits. At baseline and after nearly 1 year of treatment, data (weight, waist circumference, BMI, systolic and diastolic pressure, metabolic parameters and results of a battery of self-administered questionnaires to assess Nutritional Knowledge (NK), Physical Functioning (PF) and Quality Of Life (QOL) of patients) were collected and compared. Results: Ninety-two (48.7%) patients completed a one-year follow-up. The dropout rate was higher (73.2%) in traditionally treated women (no-education group) than in education group patients (22.8%); these data highlight that more educated patients completed the programme than non-educated patients (ODs 9.2, p < 0.000). The low follow-up rate makes any comparison between the 2 types of treatment impossible since the weight and metabolic changes of the vast majority of the non-educated subjects remain unknown. Anyway, the education group patients, in active follow-up at 1 year, showed significant weight loss (-6.6 kg, SD 3.7) and improvements of metabolic parameters and questionnaire scores. Conclusions: Data from the study show the usefulness of this simple nutritional education intervention, which appears to increase the adherence to a weight loss programme. In educated patients who completed a 1-year follow-up, the weight reduction and metabolic changes were significant, but the analysis was carried out on less than half of the subjects and this very high global dropout rate (51.3%) makes it impossible to draw generalised conclusions.

Context. This study deals with the star formation triggered by H?ii?regions.Aims. We wish to take advantage of the very simple morphology of RCW?120?? a perfect bubble?? to understand the mechanisms triggering star formation around an H?ii?region and to establish what kind of stars are formed there.Methods. We present 870??m observations of RCW?120, obtained with the APEX-LABOCA camera. These show the distribution of cold dust, and thus of neutral material. We use Spitzer-MIPS observations at 24??m and 70??m to detect the young stellar objects present in this region and to estimate their evolutionary stages.Results. A layer of dense neutral material surrounds the entire H?ii?region, having been swept up during the region's expansion. This layer has a mass greater than 2000?M?and is fragmented, with massive fragments elongated along the ionization front?(IF). We measured the 24??m flux of 138?sources. Of these, 39 are Class?I or flat-spectrum young stellar objects (YSOs) observed in the direction of the collected layer. We show that several triggering mechanisms are acting simultaneously in the swept-up shell, where they form a second generation of stars. No massive YSOs are detected. However, a massive, compact 870??m core lies adjacent to the IF.?A 70??m source with no 24??m counterpart is detected at the same position. This source is a likely candidate for a Class?0 YSO. Also at 24??m, we detect a chain of about ten regularly spaced Class?I or flat spectrum sources, parallel to the IF, in the direction of the most massive fragment. We suggest that the formation of these YSOs is the result of Jeans gravitational instabilities in the collected layer. Finally, the 870??m emission, the 24??m emission, and the H??emission show the existence of an extended and partially ionized photodissociation region around RCW?120. This demonstrates the long-distance influence of the H?ii?region upon its surrounding medium.

Aim To evaluate the accuracy of magnetic resonance imaging in assessing tumor response following neoadjuvant chemotherapy in patients with locally advanced breast cancer.Materials and Methods Twenty-six patients entered a phase II study of neoadjuvant chemotherapy, undergoing bilateral breast magnetic resonance imaging before therapy and before surgery. Tumor response was classified using RECIST criteria, using tumor size at magnetic resonance imaging. The latter was then compared to residue found at histopathological examination.Results Magnetic resonance imaging showed 6 (23%) complete responses, 17 (65%) partial responses, 3 (11.5%) disease stabilizations and no disease progressions. Twenty-three tumors (88.5%) were considered responsive and 3 (11.5%) unresponsive. Pathological tumor response was: 6 complete responses (23%), 17 partial responses (65%), 2 stable disease (8%), 1 progression (4%). When results of the preoperative magnetic resonance imaging were compared to pathological tumor response, magnetic resonance imaging overestimated tumor size in 12 cases (46%) and underestimated it in 9 (35%). However, preoperative magnetic resonance imaging failed to detect invasive tumor in 2 false-negative cases (8%), 1 of which was multifocal. Mastectomy was performed in 12 cases: 1 case of disease progression even though the neoplasm appeared smaller at magnetic resonance imaging, 3 cases with stable disease, and 4 cases with T3 or T4 disease. The 9thpatient was T2N2 with initial retroareolar disease and negative magnetic resonance imaging after chemotherapy. The 10thpatient, affected by lobular cancer, was in partial remission but was T3N1. The 11thpatient was 57 years old but was not interested in conservative surgery. The 12thpatient requested bilateral prophylactic mastectomy due to her positive family history of breast cancer.Conclusions Magnetic resonance imaging of the breast allowed conservative surgery in 54% of the patients. This low value is primarily due to overestimation of tumor size, with a negative predictive value of 67% in our population. However, surgeons were able to choose conservative surgery with relative safety in cases of small residual disease.

Aims. We wish to establish whether sequential star formation is taking place at the periphery of the Galactic H?ii?region Sh2-212.Methods. We present CO millimetre observations of this region obtained at the IRAM 30-m telescope to investigate the distribution of associated molecular material. We also use deep JHK observations obtained at the CFHT to study the stellar content of the region, and radio observations obtained at the VLA to look for the presence of an ultra-compact (UC) H?ii?region and for maser emission.Results. In the optical, Sh2-212 is spherically symmetric around its central exciting cluster. This H?ii?region is located along a molecular filament. A thin, well-defined half ring of molecular material surrounds the brightest part of the H?ii?region at the rear and is fragmented. The most massive fragment (~200?M?) contains a massive young stellar object displaying a near-IR excess; its spectral energy distribution indicates a high-mass (~14?M?), high-temperature (~30?000?K), and high-luminosity (~17?000?L?) source. This object ionizes a UC H?ii?region.Conclusions. Sh2-212 is a good example of massive-star formation triggered via the collect and collapse process. The massive YSO observed at its periphery is a good candidate for a massive star formed in isolation.

Abstract: A novel brightness illusion in planar patterns is reported. The illusion occurs, for example, when surfaces with a luminance ramp shaded from black to white are positioned on a black homogeneous background, so that each white end of the surfaces faces a single point of the plane of the pattern. The illusion consists of the enhancement of the brightness of the background in a relatively wide area around the white ends of the surfaces. A parametric study was conducted in which participants were asked to rate the difference in brightness between the parts of the background inside and outside a virtual circle formed by disks with different luminance ramps. The results show that mean ratings of brightness depended on the luminance of the background, the luminance range of ramps, and the kind of ramp. Discussion of these results with reference to other brightness illusions (assimilation, neon color spreading, anomalous surfaces, visual phantoms, grating induction, and the glare effect) shows that the phantom illumination illusion derives from processes producing the perception of ambient illumination.

Young massive stars or clusters are often observed at the peripheries of H ii regions. What triggers star formation at such locations? Among the scenarios that have been proposed, the ”collect and collapse” process is particularly attractive because it permits the formation of massive objects via the fragmentation of the dense shocked layer of neutral gas surrounding the expanding ionized zone. However, until our recent article on Sh 104, it had not been convincingly demonstrated that this process actually takes place. In the present paper we present our selection of seventeen candidate regions for this process; all show high-luminosity near-IR clusters and/or mid-IR point sources at their peripheries. The reality of a ”collect and collapse” origin of these presumably second-generation stars and clusters will be discussed in forthcoming papers, using new near-IR and millimetre observations.

To investigate the technical, clinical and pathological findings that can, potentially, affect pre-operative lymphoscintigraphy in visualizing sentinel lymph node (SLN) and intra-operative probe detection of SLN in patients with breast cancer.

Background and objectives. More than half of patients with positive sentinel node (SN) have no metastases in non-sentinel nodes (NSNs) on axillary lymph node dissection (ALND). The aim of this study was to investigate factors predictive of NSNs involvement, in order to identify patients with metastatic disease confined to the SN which might avoid ALND. Methods. ALND was performed in 167 patients with metastatic SN. Axillary NSNs status was correlated with the size of SN metastases, the size of the primary tumor and the occurrence of lymphovascular invasion. In 72 cases, the radiotracer (Tc-99m albumin colloid) marked multiple (in most cases 2 or 3) nodes. In this group, NSNs status was correlated with the number of metastatic radioactive nodes (1 or >1), and with the above mentioned histopathologic factors. Results. NSNs metastases were found in 57/167 cases (34.1%), the rate increasing proportionate to the size of both SN metastases (p< 0.0001) and primary tumor (p= 0.0075), while no significant correlation was found for lymphovascular invasion (p= 0.1769). At univariate and multivariate analysis of findings from the 72 cases with multiple probe-detected hot nodes, positivity in more than one hot node was the strongest predictor of NSN involvement (p= 0.0019). Conclusions. The identification and excision of multiple hot nodes can be useful in the prediction of NSNs involvement in patients with metastatic SN.

Aim:Several different injection techniques are currently used for sentinel node (SN) identification in patients with breast cancer. Some studies suggest that the subareolar plexus drains lymph from the whole breast to the same axillary SN. In order to test this hypothesis, we ascertained whether subareolar blue dye injection and subdermal radioisotope injection close to the tumour identify the same axillary nodes.

One major theme for today's competition is looking at firms as learning organisations. internet-based technologies can support and revolutionise the way for learning. As a consequence e-learning assumes a strategic relevance. This paper focuses on the competitive advantages of e-learning, and presents the principal ambits of application and critical factors for implementation, such as motivation and learning-by-experience. Two successful case studies are also presented. E-learning solutions provide firms with helpful instruments for supporting an effective knowledge management, where every moment is part of a learning process.

The distribution of the main prognostic factors in different age groups was evaluated in 1226 patients operated on for primary breast cancer, in order to identify those influenced by age and/or menopausal status. Patients were divided into the following groups: 1) 40 years of age and under; 2) premenopausal over 40 years of age; 3) postmenopausal under 75 years of age and 4) 75 years of age and over. Our findings showed that the youngest patients had the worst prognostic pattern, which improves as age increases and is the best in patients over 75 years of age. Some of the parameters investigated (tumour size, histologic and nuclear grade, tumour infiltrating lymphocytes, p53 and Ki 67) were found to be influenced by age, some (necrosis and oestrogen receptors) were influenced by menopausal status and/or age, some (vascular invasion, ploidy, S-phase and progesterone receptors) showed significant differences in different age groups but there was no consistent relation with patient age or menopausal status, and others (node status, ErbB2/Neu and Cathepsin D) were not influenced by age or menopause.

Axillary lymph node dissection (ALND) is an important tool in staging patients with breast cancer. However, this procedure has several sequelae and complications and improvement in early diagnosis has led to an increasing number of cases of ALND in which axillary nodes are found to be negative. Sentinel node (SN) biopsy appears to be a less invasive alternative to ALND. The aim of the present study was to assess whether SN is a reliable indicator for axillary staging. We studied 126 consecutive patients with T1-T2 breast cancer and clinically negative axilla. In each case, 30–70 MBq of 99mTC-labelled colloidal albumin was injected subdermally close to the tumour and SN was visualised by lymphoscintigraphy. Surgery was performed 24 h after injection and the SN was removed under the guidance of a gamma ray-detecting probe. ALND was then undertaken in all cases. A histopathologic examination of the SNs was then made and the findings compared with the status of the other axillary nodes. SNs were identified and biopsied in 115/126 patients (91.3%) and correctly predicted the axillary status in 110/115 cases (95.6%). In five cases (4.4%), SNs were found to be negative, but other axillary nodes were positive. Our data confirm that SN biopsy is a good method for staging the axilla in patients with breast cancer. However, before SN biopsy can replace ALND in daily clinical practice, some technical aspects must be standardized, and clinical trials are required in order to clarify the prognostic impact of false-negative cases.

A growing body of research has suggested that different models drive the composing process of skilled and less-skilled writers. Basically, less-skilled writers extract cues from the assignment that trigger retrieval of appropriate content from memory. The composing of better writers, on the other hand, tends to begin with writers establishing goals. Those goals centering on content and genre are achieved through application of problem-solving operations. This process continues iteratively, restructuring the writer's recalled information until text is completed. Building on this theory, the authors have created an instructional design that encourages second graders to engage in advanced writing strategies generally not found until later grades.

FEEDBACK is a SOFIA (Stratospheric Observatory for Infrared Astronomy) legacy program dedicated to study the interaction of massive stars with their environment. It performs a survey of 11 galactic high mass star-forming regions in the 158 ?m (1.9 THz) line of [C ii] and the 63 ?m (4.7 THz) line of [O i]. We employ the 14 pixel Low Frequency Array and 7 pixel High Frequency Array upGREAT heterodyne instrument to spectrally resolve (0.24 MHz) these far-infrared fine structure lines. With a total observing time of 96h, we will cover ?6700 arcmin2at 14.?1) angular resolution for the [C ii] line and 6.?3 for the [O i] line. The observations started in spring 2019 (Cycle 7). Our aim is to understand the dynamics in regions dominated by different feedback processes from massive stars such as stellar winds, thermal expansion, and radiation pressure, and to quantify the mechanical energy injection and radiative heating efficiency. This is an important science topic because feedback of massive stars on their environment regulates the physical conditions and sets the emission characteristics in the interstellar medium (ISM), influences the star formation activity through molecular cloud dissolution and compression processes, and drives the evolution of the ISM in galaxies. The [C ii] line provides the kinematics of the gas and is one of the dominant cooling lines of gas for low to moderate densities and UV fields. The [O i] line traces warm and high-density gas, excited in photodissociations regions with a strong UV field or by shocks. The source sample spans a broad range in stellar characteristics from single OB stars, to small groups of O stars, to rich young stellar clusters, to ministarburst complexes. It contains well-known targets such as Aquila, the Cygnus X region, M16, M17, NGC7538, NGC6334, Vela, and W43 as well as a selection of H iiregion bubbles, namely RCW49, RCW79, and RCW120. These [C ii] maps, together with the less explored [O i] 63 ?m line, provide an outstanding database for the community. They will be made publically available and will trigger further studies and follow-up observations.

We suggest that bipolar H iiregions may be the aftermath of collisions between clouds. Such a collision will produce a shock-compressed layer, and a star cluster can then condense out of the dense gas near the center of the layer. If the clouds are sufficiently massive, the star cluster is likely to contain at least one massive star, which emits ionizing radiation, and excites an H iiregion, which then expands, sweeping up the surrounding neutral gas. Once most of the matter in the clouds has accreted onto the layer, expansion of the H iiregion meets little resistance in directions perpendicular to the midplane of the layer, and so it expands rapidly to produce two lobes of ionized gas, one on each side of the layer. Conversely, in directions parallel to the midplane of the layer, expansion of the H iiregion stalls due to the ram pressure of the gas that continues to fall towards the star cluster from the outer parts of the layer; a ring of dense neutral gas builds up around the waist of the bipolar H iiregion, and may spawn a second generation of star formation. We present a dimensionless model for the flow of ionized gas in a bipolar H iiregion created according to the above scenario, and predict the characteristics of the resulting free–free continuum and recombination-line emission. This dimensionless model can be scaled to the physical parameters of any particular system. Our intention is that these predictions will be useful in testing the scenario outlined above, and thereby providing indirect support for the role of cloud–cloud collisions in triggering star formation.