"Sitte se menee koulus" : Eri kieli- ja kulttuuritaustaisen lapsen suomen kielen taito esiopetuksen päättövaiheessa

A child learns new things, creates social relationships and participates in play with the help of language. How can a child overcome these challenges if the surrounding language is not his mother tongue? The objective of learning a new language in the Pre-school education is an active bilingualism in all fields of the language. Theoretical context of the research rises from bilingualism, learning a language, language skills and evaluating them. Object of the research was to understand language skills of a child from a different linguistic and cultural background in the final stage of Pre-school education and to clarify how learning Finnish was supported during the Pre-school year. Answers to the research issues will be searched with the following questions: 1) What kind of language skills does a child from a different linguistic and cultural backgrounds have at the final stage of Pre-school education?, 1.1) What kind of listening comprehension skills?, 1.2) What kind of speech and vocabulary skills?, 1.3) What kind of structural skills?, 2) What kind of individual differences are there in language skills of children from different linguistic and cultural backgrounds?, and 3) How has a child from a different linguistic and cultural background been supported in learning Finnish during the Pre-school education? The view of language skills in this research is holistic even though it will be analysed in separate fields. The aim of this research is to form an overall impression of Finnish skills of the children participating in the research. Eight Pre-school-aged children with different linguistic and cultural backgrounds and their kindergarten teachers participated in this research. The children had taken part in Finnish activities for about three years. The research material consists of the test series (KITA), which evaluate children’s language skills – and of the questionnaire to the kindergarten teachers. The purpose of the questionnaire was to provide additional information on children’s language skills in Pre-school teaching situations and on supporting Finnish in Pre-school education. This research is qualitative and processing of the material is based on content analysis. According to the kindergarten teachers, the children’s social language skills were sufficient to cope in everyday life but children needed assistance with longer instructions. The same phenomenon could also be seen with the KITA tests – in which long and abstract instructions turned out to be difficult. Individual differences of the children were perceived in productivity skills, which were realised in fluent or influent speech. The children were supported in learning Finnish individually, in small-groups and in the activities of a whole group. ‘Finnish as the second language’ small-groups were the most common form of support in learning the language. The support at understanding activities was emphasized in whole group situations as well as in individual situations while assisting the child’s language skills. Generally, the children’s language skills were in the same level with developing basic language skills. The data of this research help to understand children’s language skills after three years of adopting Finnish. The results can be utilised in planning and evaluation of teaching another language.

Immunomodulatory effects of probiotic bacteria in healthy adults

Probiooteilla kantakohtaisia vaikutuksia ihmisen immuunijärjestelmään terveillä aikuisilla Probiooteilla on kantakohtaisia tulehduksen välittäjäaineita vähentäviä vaikutuksia ja probioottien yhdistelmien vaikutukset eroavat yksittäisten kantojen vaikutuksista selviää TtM Riina Kekkosen tuoreesta väitöstutkimuksesta. TtM Riina Kekkonen on selvittänyt väitöskirjassaan eri probioottikantojen vaikutuksia immuunivasteeseen valkosolumallissa sekä terveillä aikuisilla lumekontrolloiduissa kliinisissä tutkimuksissa. Aikaisemmin probioottien vaikutuksia on tutkittu lähinnä allergian ja erilaisten vatsavaivojen ehkäisyssä ja hoidossa. Probiootteja sisältäviä tuotteita käyttävät kuluttajat ovat kuitenkin useimmiten terveitä aikuisia, ja probioottien vaikutus terveiden aikuisten immuunijärjestelmään on ollut puutteellisesti selvitettyä. Valkosolumallissa probioottikantojen havaittiin poikkeavan toisistaan niiden kyvyssä aktivoida immuunivasteen välittäjäaineiden, sytokiinien, tuotantoa. Anti-inflammatorisia, eli tulehdusta lievittäviä vaikutuksia nähtiin lähinnä Bifidobacterium ja Propionibacterium sukuihin kuuluvilla kannoilla. Streptococcus ja Leuconostoc sukuihin kuuluvat kannat puolestaan aktivoivat Th1 tyyppistä, soluvälitteistä immuunivastetta. Eri probioottien kombinaatiot eivät saaneet aikaan voimakkaampaa aktivaatiota yksittäisiin kantoihin verrattuna, joka viittaa probioottien keskinäiseen kilpailuun niiden ollessa kontaktissa ihmisen solujen kanssa. Probioottikantojen valinta kliinisiin tutkimuksiin tehtiin niiden anti-inflammatoristen ominaisuuksien perusteella. Parhaita anti-inflammatorisia kantoja olivat B. lactis ssp. animalis Bb12 ja P. freudenreichii ssp. shermanii JS, joiden lisäksi tutkimuksiin valittiin myös L. rhamnosus GG (LGG) hyvin tutkittuna referenssikantana. Solutöiden tulokset eivät olleet täysin verrannollisia kliinisen työn tuloksiin, koska LGG näytti omaavan parhaat anti-inflammatoriset ominaisuudet kliinisissä tutkimuksissa vaikka solutyössä sen aikaansaamat vasteet olivat melko vaimeita. Kolmen viikon kliinisessä tutkimuksessa terveillä aikuisilla LGG alensi mm. tulehdusta kuvaavan C-reaktiivisen proteiinin ja inflammatoristen sytokiinien määrää. Pidemmässä kolmen kuukauden pituisessa kliinisessä tutkimuksessa LGG:llä ei ollut vaikutusta terveiden aikuisten infektiosairastavuuteen, mutta LGG lyhensi vatsavaivojen kestoa. Probioottien vaikutukset immuunijärjestelmään näyttävät olevan kantakohtaisia ja erityisesti Lactobacillus rhamnosus GG:llä havaittiin anti-inflammatorisia vaikutuksia. Valkosolumallia ei tulisi käyttää ainoana probioottikantojen skriinausmenetelmänä niiden immunologisia vaikutuksia selvitettäessä, koska solutöiden tulokset eivät olleet täysin verrannollisia kliinisten tutkimusten tuloksiin. Sen sijaan veren perifeeristen lymfosyyttien eristäminen ja niiden aktivoitumisen selvittäminen lyhytaikaisessa kliinisessä tutkimuksessa voisi toimia suhteellisen helppona skiinausmenetelmänä.

Individual variation in in vitro efficacy of antiplatelet medication - aspirin and clopidogrel

Antiplatelet medication is known to decrease adverse effects in patients with atherothrombotic disease. However, despite ongoing antiplatelet medication considerable number of patients suffer from atherothrombotic events. The aims of the study were 1) to evaluate the individual variability in platelet functions and compare the usability of different methods in detecting it, 2) to assess variability in efficacy of antiplatelet medication with aspirin (acetylsalicylic acid) or the combination of aspirin and clopidogrel and 3) to investigate the main genetic and clinical variables as well as potential underlying mechanisms of variability in efficacy of antiplatelet medication. In comparisons of different platelet function tests in 19 healthy individuals PFA-100® correlated with traditional methods of measuring platelet function and was thus considered appropriate for testing individual variability in platelet activity. Efficacy of ongoing 100mg aspirin daily was studied in 101 patients with coronary artery disease (CAD). Aspirin response was measured with arachidonic acid (AA)-induced platelet aggregation, which reflects cyclo-oxygenase (COX)-1 dependent thromboxane (Tx) A2 formation, and PFA-100®, which evaluates platelet activation under high shear stress in the presence of collagen and epinephrine. Five percent of patients failed to show inhibition of AA-aggregation and 21% of patients had normal PFA-100® results despite aspirin and were thus considered non-responders to aspirin. Interestingly, the two methods of assessing aspirin efficacy, platelet aggregation and PFA-100®, detected different populations as being aspirin non-responders. It could be postulated that PFA-100® actually measures enhanced platelet function, which is not directly associated with TxA2 inhibition exerted by aspirin. Clopidogrel efficacy was assessed in 50 patients who received a 300mg loading dose of clopidogrel 2.5 h prior to percutaneous coronary intervention (PCI) and in 51 patients who were given a loading dose of 300mg combined with a five day treatment of 75mg clopidogrel daily mimicking ongoing treatment. Clopidogrel response was assessed with ADP-induced aggregations, due to its mechanism of action as an inhibitor of ADP-induced activation. When patients received only a loading dose of clopidogrel prior to PCI, 40% did not gain measurable inhibition of their ADP-induced platelet activity (inhibition of 10% or less). Prolongation of treatment so that all patients had reached a plateau of inhibition exerted by clopidogrel, decreased the incidence of non-responders to 20%. Polymorphisms of COX-1 and GP VI, as well as diabetes and female gender, were associated with decreased in vitro aspirin efficacy. Diabetes also impaired the in vitro efficacy of short-term clopidogrel. Decreased response to clopidogrel was associated with limited inhibition by ARMX, an antagonist of P2Y12-receptor, suggesting the reason for clopidogrel resistance to be receptor-dependent. Conclusions: Considerable numbers of CAD patients were non-responders either to aspirin, clopidogrel or both. In the future, platelet function tests may be helpful to individually select effective and safe antiplatelet medication for these patients.

Genetic polymorphisms and laboratory variables as predictors of blood pressure response to antihypertensive drugs

Hypertension is one of the major risk factors for cardiovascular morbidity. The advantages of antihypertensive therapy have been clearly demonstrated, but only about 30% of hypertensive patients have their blood pressure (BP) controlled by such treatment. One of the reasons for this poor BP control may lie in the difficulty in predicting BP response to antihypertensive treatment. The average BP reduction achieved is similar for each drug in the main classes of antihypertensive agents, but there is a marked individual variation in BP responses to any given drug. The purpose of the present study was to examine BP response to four different antihypertensive monotherapies with regard to demographic characteristics, laboratory test results and common genetic polymorphisms. The subjects of the present study are participants in the pharmacogenetic GENRES Study. A total of 208 subjects completed the whole study protocol including four drug treatment periods of four weeks, separated by four-week placebo periods. The study drugs were amlodipine, bisoprolol, hydrochlorothiazide and losartan. Both office (OBP) and 24-hour ambulatory blood pressure (ABP) measurements were carried out. BP response to study drugs were related to basic clinical characteristics, pretreatment laboratory test results and common polymorphisms in genes coding for components of the renin-angiotensin system, alpha-adducin (ADD1), beta1-adrenergic receptor (ADRB1) and beta2-adrenergic receptor (ADRB2). Age was positively correlated with BP responses to amlodipine and with OBP and systolic ABP responses to hydrochlorothiazide, while body mass index was negatively correlated with ABP responses to amlodipine. Of the laboratory test results, plasma renin activity (PRA) correlated positively with BP responses to losartan, with ABP responses to bisoprolol, and negatively with ABP responses to hydrochlorothiazide. Uniquely to this study, it was found that serum total calcium level was negatively correlated with BP responses to amlodipine, whilst serum total cholesterol level was negatively correlated with ABP responses to amlodipine. There were no significant associations of angiotensin II type I receptor 1166A/C, angiotensin converting enzyme I/D, angiotensinogen Met235Thr, ADD1 Gly460Trp, ADRB1 Ser49Gly and Gly389Arg and ADRB2 Arg16Gly and Gln27Glu polymorphisms with BP responses to the study drugs. In conclusion, this study confirmed the relationship between pretreatment PRA levels and response to three classes of antihypertensive drugs. This study is the first to note a significant inverse relation between serum calcium level and responsiveness to a calcium channel blocker. However, this study could not replicate the observations that common polymorphisms in angiotensin II type I receptor, angiotensin converting enzyme, angiotensinogen, ADD1, ADRB1, or ADRB2 genes can predict BP response to antihypertensive drugs.

A search for line intensity enhancements in the far-UV spectra of active late-type stars arising from opacity

Context. Radiative transfer calculations have predicted intensity enhancements for optically thick emission lines, as opposed to the normal intensity reductions, for astrophysical plasmas under certain conditions. In particular, the results are predicted to be dependent both on the geometry of the emitting plasma and the orientation of the observer. Hence in principle the detection of intensity enhancement may provide a way of determining the geometry of an unresolved astronomical source.
Aims. To investigate such enhancements we have analysed a sample of active late-type stars observed in the far ultraviolet spectral region.
Methods. Emission lines of O vi in the FUSE satellite spectra of ϵ Eri, II Peg and Prox Cen were searched for intensity enhancements due to opacity.
Results. We have found strong evidence for line intensity enhancements due to opacity during active or flare-like activity for all three stars. The O vi 1032/1038 line intensity ratios, predicted to have a value of 2.0 in the optically thin case, are found to be up to ~30% larger during several orbital phases.
Conclusions. Our measurements, combined with radiative transfer models, allow us to constrain both the geometry of the O vi emitting regions in our stellar sources and the orientation of the observer. A spherical emitting plasma can be ruled out, as this would lead to no intensity enhancement. In addition, the theory tells us that the line-of-sight to the plasma must be close to perpendicular to its surface, as observations at small angles to the surface lead to either no intensity enhancement or the usual line intensity decrease over the optically thin value. For the future, we outline a laboratory experiment, that could be undertaken with current facilities, which would provide an unequivocal test of predictions of line intensity enhancement due to opacity, in particular the dependence on plasma geometry.

Blue luminous stars in nearby galaxies: Quantitative spectral analysis of M33 B-type supergiant stars

We present the detailed spectral analysis of a sample of M33 B-type supergiant stars, aimed at the determination of their fundamental parameters and chemical composition. The analysis is based on a grid of non-LTE metal line-blanketed model atmospheres including the effects of stellar winds and spherical extension computed with the code FASTWIND. Surface abundance ratios of C, N, and O are used to discuss the chemical evolutionary status of each individual star. The comparison of observed stellar properties with theoretical predictions of massive star evolutionary models shows good agreement within the uncertainties of the analysis. The spatial distribution of the sample allows us to investigate the existence of radial abundance gradients in the disk of M33. The comparison of stellar and H II region O abundances ( based on direct determinations of the electron temperature of the nebulae) shows good agreement. Using a simple linear radial representation, the stellar oxygen abundances result in a gradient of -0.0145 +/- 0.005 dex arcmin(-1) (or -0.06 +/- 0.02 dex kpc(-1)) up to a distance equal to similar to 1.1 times the isophotal radius of the galaxy. A more complex representation cannot be completely discarded by our stellar sample. The stellar Mg and Si abundances follow the trend displayed by O abundances, although with shallower gradients. These differences in gradient slope cannot be explained at this point. The derived abundances of the three alpha-elements yield solar metallicity in the central regions of the disk of M33. A comparison with recent planetary nebula data from Magrini and coworkers indicates that the disk of M33 has not suffered from a significant O enrichment in the last 3 Gyr.

Spitzer Space Telescope spectra of post-AGB stars in the large magellanic Cloud-polycyclic aromatic hydrocarbons at low metallicities

This paper reports variations of polycyclic aromatic hydrocarbons (PAHs) features that were found in Spitzer Space Telescope spectra of carbon-rich post-asymptotic giant branch (post-AGB) stars in the Large Magellanic Cloud (LMC). The paper consists of two parts. The first part describes our Spitzer spectral observing programme of 24 stars including post-AGB candidates. The latter half of this paper presents the analysis of PAH features in 20 carbon-rich post-AGB stars in the LMC, assembled from the Spitzer archive as well as from our own programme.We found that five post-AGB stars showed a broad feature with a peak at 7.7 μm, that had not been classified before. Further, the 10-13 μm PAH spectra were classified into four classes, one of which has three broad peaks at 11.3, 12.3 and 13.3 μm rather than two distinct sharp peaks at 11.3 and 12.7 μm, as commonly found in HII regions. Our studies suggest that PAHs are gradually processed while the central stars evolve from post-AGB phase to planetary nebulae, changing their composition before PAHs are incorporated into the interstellar medium. Although some metallicity dependence of PAH spectra exists, the evolutionary state of an object is more significant than its metallicity in determining the spectral characteristics of PAHs for LMC and Galactic post-AGB stars. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Massive stars exploding in a He-rich circumstellar medium - VI. Observations of two distant Type Ibn supernova candidates discovered by La Silla-QUEST

We present optical observations of the peculiar stripped-envelope supernovae (SNe) LSQ12btw and LSQ13ccw discovered by the La Silla-QUEST survey. LSQ12btw reaches an absolute peak magnitude of M-g = -19.3 +/- 0.2, and shows an asymmetric light curve. Stringent pre-discovery limits constrain its rise time to maximum light to less than 4 d, with a slower post-peak luminosity decline, similar to that experienced by the prototypical SN Ibn 2006jc. LSQ13ccw is somewhat different: while it also exhibits a very fast rise to maximum, it reaches a fainter absolute peak magnitude (M-g =-18.4 +/- 0.2), and experiences an extremely rapid post-peak decline similar to that observed in the peculiar SN Ib 2002bj. A stringent pre-discovery limit and an early marginal detection of LSQ13ccw allow us to determine the explosion time with an uncertainty of +/- 1 d. The spectra of LSQ12btw show the typical narrow He I emission lines characterizing Type Ibn SNe, suggesting that the SN ejecta are interacting with He-rich circumstellar material. The He I lines in the spectra of LSQ13ccw exhibit weak narrow emissions superposed on broad components. An unresolved H alpha line is also detected, suggesting a tentative Type Ibn/IIn classification. As for other SNe Ibn, we argue that LSQ12btw and LSQ13ccw likely result from the explosions of Wolf-Rayet stars that experienced instability phases prior to core collapse. We inspect the host galaxies of SNe Ibn, and we show that all of them but one are hosted in spiral galaxies, likely in environments spanning a wide metallicity range.

Massive stars exploding in a He-rich circumstellar medium - V. Observations of the slow-evolving SN Ibn OGLE-2012-SN-006

We present optical observations of the peculiar Type Ibn supernova (SN Ibn) OGLE-2012-SN-006, discovered and monitored by the Optical Gravitational Lensing Experiment-IV survey, and spectroscopically followed by Public ESO Spectroscopic Survey of Transient Objects (PESSTO) at late phases. Stringent pre-discovery limits constrain the explosion epoch with fair precision to JD = 245 6203.8 +/- 4.0. The rise time to the I-band light-curve maximum is about two weeks. The object reaches the peak absolute magnitude M-I = -19.65 +/- 0.19 on JD = 245 6218.1 +/- 1.8. After maximum, the light curve declines for about 25 d with a rate of 4 mag (100 d)(-1). The symmetric I-band peak resembles that of canonical Type Ib/c supernovae (SNe), whereas SNe Ibn usually exhibit asymmetric and narrower early-time light curves. Since 25 d past maximum, the light curve flattens with a decline rate slower than that of the Co-56-Fe-56 decay, although at very late phases it steepens to approach that rate. However, other observables suggest that the match with the Co-56 decay rate is a mere coincidence, and the radioactive decay is not the main mechanism powering the light curve of OGLE-2012-SN-006. An early-time spectrum is dominated by a blue continuum, with only a marginal evidence for the presence of He I lines marking this SN type. This spectrum shows broad absorptions bluewards than 5000 angstrom, likely O II lines, which are similar to spectral features observed in superluminous SNe at early epochs. The object has been spectroscopically monitored by PESSTO from 90 to 180 d after peak, and these spectra show the typical features observed in a number of SN 2006jc-like events, including a blue spectral energy distribution and prominent and narrow (v(FWHM) approximate to 1900 km s(-1)) He I emission lines. This suggests that the ejecta are interacting with He-rich circumstellar material. The detection of broad (10(4) km s(-1)) O I and Ca II features likely produced in the SN ejecta (including the [OI] lambda lambda 6300,6364 doublet in the latest spectra) lends support to the interpretation of OGLE-2012-SN-006 as a core-collapse event.

Massive stars exploding in a He-rich circumstellar medium - IV. Transitional Type Ibn supernovae

We present ultraviolet, optical and near-infrared data of the Type Ibn supernovae (SNe) 2010al and 2011hw. SN 2010al reaches an absolute magnitude at peak of M-R = -18.86 +/- 0.21. Its early light curve shows similarities with normal SNe Ib, with a rise to maximum slower than most SNe Ibn. The spectra are dominated by a blue continuum at early stages, with narrow P-Cygni He I lines indicating the presence of a slow-moving, He-rich circumstellar medium. At later epochs, the spectra well match those of the prototypical SN Ibn 2006jc, although the broader lines suggest that a significant amount of He was still present in the stellar envelope at the time of the explosion. SN 2011hw is somewhat different. It was discovered after the first maximum, but the light curve shows a double peak. The absolute magnitude at discovery is similar to that of the second peak (M-R = -18.59 +/- 0.25), and slightly fainter than the average of SNe Ibn. Though the spectra of SN 2011hw are similar to those of SN 2006jc, coronal lines and narrow Balmer lines are clearly detected. This indicates substantial interaction of the SN ejecta with He-rich, but not H-free, circumstellar material. The spectra of SN 2011hw suggest that it is a transitional SN Ibn/IIn event similar to SN 2005la. While for SN 2010al the spectrophotometric evolution favours a H-deprived Wolf-Rayet progenitor (of WN-type), we agree with the conclusion of Smith et al. that the precursor of SN 2011hw was likely in transition from a luminous blue variable to an early Wolf-Rayet (Ofpe/WN9) stage.

The VLT-FLAMES Tarantula Survey XXII. Multiplicity properties of the B-type stars

We investigate the multiplicity properties of 408 B-type stars observed in the 30 Doradus region of the Large Magellanic Cloud with multi-epoch spectroscopy from the VLT-FLAMES Tarantula Survey (VFTS). We use a cross-correlation method to estimate relative radial velocities from the helium and metal absorption lines for each of our targets. Objects with significant radial-velocity variations (and with an amplitude larger than 16 km s^-1) are classified as spectroscopic binaries. We find an observed spectroscopic binary fraction (defined by periods of <10^3.5 d and mass ratios >0.1) for the B-type stars, f<inf>B</inf>(obs) = 0.25 ± 0.02, which appears constant across the field of view, except for the two older clusters (Hodge 301 and SL 639). These two clusters have significantly lower binary fractions of 0.08 ± 0.08 and 0.10 ± 0.09, respectively. Using synthetic populations and a model of our observed epochs and their potential biases, we constrain the intrinsic multiplicity properties of the dwarf and giant (i.e. relatively unevolved) B-type stars in 30 Dor. We obtain a present-day binary fraction f<inf>B</inf>(true) = 0.58 ± 0.11, with a flat period distribution. Within the uncertainties, the multiplicity properties of the B-type stars agree with those for the O stars in 30 Dor from the VFTS.

Coronal properties of planet-bearing stars

Context. Do extrasolar planets affect the activity of their host stars? Indications for chromospheric activity enhancement have been found for a handful of targets, but in the X-ray regime, conclusive observational evidence is still missing. Aims: We want to establish a sound observational basis to confirm or reject major effects of Star-Planet Interactions (SPI) in stellar X-ray emissions. Methods: We therefore conduct a statistical analysis of stellar X-ray activity of all known planet-bearing stars within 30 pc distance for dependencies on planetary parameters such as mass and semimajor axis. Results: In our sample, there are no significant correlations of X-ray luminosity or the activity indicator L_X/L_bol with planetary parameters which cannot be explained by selection effects. Conclusions: Coronal SPI seems to be a phenomenon which might only manifest itself as a strong effect for a few individual targets, but not to have a major effect on planet-bearing stars in general.

Alfa : mètode d'autocorrecció gramatical assistida. 'Alfa : método de autocorrección gramatical asistida'.

Alfa es un manual pensado para los alumnos de educación secundaria y cursos de adultos, para los que realizan reciclaje e incluso para aquellos de los primeros cursos universitarios. Quiere ser una herramienta de apoyo en la tarea de corregir de manera eficaz sus escritos y conseguir motivarlos en esta tarea tan ardua como inaludible de su formación en el uso de la lengua. Alfa propone un método de autocorrección gramatical basado en la guía individual sobre aquellos aspectos concretos y adecuados que permiten a cada cual corregir sus textos. El contenido se distribuye en dos partes de diez capítulos repartidos en unidades codificadas. En la primera parte, los códigos son todos de tres cifras: la primera hace referencia al capítulo, la segunda puede hacer referencia a un subcapítulo o, como siempre pasa con la tercera, al número de orden de la serie. En la segunda parte, los párrafos con códigos de cuatro cifras incorporan las explicaciones teóricas a las que remiten los correspondientes de la primera parte. Esta codificación tiene un doble objetivo: facilitar al profesor la identificación del error y posibilitar el tratamiento informático.

Tratamiento de Artritis reumatoide con antagonistas del factor de necrosis tumoral alfa y su asociación con el desarrollo de melanoma cutáneo: revisión sistemática de la literatura y meta-análisis.

Introducción: El tratamiento con antagonistas del factor de necrosis tumoral alfa (anti TNF) ha impactado el pronóstico y la calidad de vida de los pacientes con artritis reumatoide (AR) positivamente, sin embargo, se interroga un incremento en el riesgo de desarrollar melanoma. Objetivo: Conocer la asociación entre el uso de anti TNF y el desarrollo de melanoma maligno en pacientes con AR. Metodología: Se realizó una búsqueda sistemática en MEDLINE, EMBASE, COCHRANE LIBRARY y LILACS para ensayos clínicos, estudios observacionales, revisiones y meta-análisis en pacientes adultos con diagnóstico de AR y manejo con anti TNF (Certolizumab pegol, Adalimumab, Etanercept, Infliximab y Golimumab). Resultados: 37 estudios clínicos cumplieron los criterios de inclusión para el meta-análisis, con una población de 16567 pacientes. El análisis de heterogeneidad no fue significativo (p=1), no se encontró diferencia en el riesgo entre los grupos comparados DR -0.00 (IC 95% -0.001; -0.001). Un análisis adicional de los estudios en los que se reportó al menos 1 caso de melanoma (4222 pacientes) tampoco mostró diferencia en el riesgo DR -0.00 (IC 95% -0.004 ; -0.003). Conclusión: En la evidencia disponible a la fecha no encontramos asociación significativa entre el tratamiento con anti TNF en pacientes con diagnóstico de AR y el desarrollo de melanoma cutáneo.

Global properties of `ordinary` early-type galaxies: photometry and spectroscopy of stars and globular clusters in NGC 4494

We present a comprehensive analysis of the spatial, kinematic and chemical properties of stars and globular clusters (GCs) in the `ordinary` elliptical galaxy NGC 4494 using data from the Keck and Subaru telescopes. We derive galaxy surface brightness and colour profiles out to large galactocentric radii. We compare the latter to metallicities derived using the near-infrared Calcium Triplet. We obtain stellar kinematics out to similar to 3.5 effective radii. The latter appear flattened or elongated beyond similar to 1.8 effective radii in contrast to the relatively round photometric isophotes. In fact, NGC 4494 may be a flattened galaxy, possibly even an S0, seen at an inclination of similar to 45 degrees. We publish a catalogue of 431 GC candidates brighter than i(0) = 24 based on the photometry, of which 109 are confirmed spectroscopically and 54 have measured spectroscopic metallicities. We also report the discovery of three spectroscopically confirmed ultra-compact dwarfs around NGC 4494 with measured metallicities of -0.4 less than or similar to [Fe/H] less than or similar to -0.3. Based on their properties, we conclude that they are simply bright GCs. The metal-poor GCs are found to be rotating with similar amplitude as the galaxy stars, while the metal-rich GCs show marginal rotation. We supplement our analysis with available literature data and results. Using model predictions of galaxy formation, and a suite of merger simulations, we find that many of the observational properties of NGC 4494 may be explained by formation in a relatively recent gas-rich major merger. Complete studies of individual galaxies incorporating a range of observational avenues and methods such as the one presented here will be an invaluable tool for constraining the fine details of galaxy formation models, especially at large galactocentric radii.