Galaxy and Mass Assembly (GAMA): Mid-infrared properties as tracers of galaxy environment

We investigate how different mid-infrared (mid-IR) properties of galaxies are correlated with the environment in which the galaxies are located. For this purpose, we first study the dependence of galaxy clustering on the absolute magnitude at 3.4 µm and redshift. Then, we look into the environmental dependence of mid-IR luminosities and the galaxy properties derived from these luminosities. We also explore how various IR galaxy luminosity selections influence the galaxy clustering measurements. We used a set of W1 (3.4 µm) absolute magnitude (MW1) selected samples from the Galaxy and Mass Assembly (GAMA) survey matched with mid-IR properties from the Wide-field Infrared Survey Explorer (WISE) in the redshift range 0.07 ≤ z < 0.43. We computed the galaxy two-point correlation function (2pCF) and compared the clustering lengths between subsamples binned in MW1 and in redshift. We also measured the marked correlation function (MCF), in which the galaxies are weighted by marks when measuring clustering statistics, using the luminosities in the WISE W1 to W4 (3.4 to 22 µm) bands as marks. Additionally, we compared the measurements of MCFs with different estimates of stellar mass and star formation rate (SFR) used as marks. Finally, we checked how different selections applied to the sample affect the clustering measurements

Evidence of Mycoplasma spp. Transmission by Migratory Wild Geese

Mycoplasma infections have been found in different species of waterfowl worldwide. However, the question of how the pathogens have been transmitted and dispersed is still poorly understood. Samples collected from clinically healthy greater white-fronted geese (Anser albifrons) (N = 12), graylag geese (Anser anser) (N = 6), taiga bean geese (Anser fabalis) (N = 10), and barnacle geese (Branta leucopsis) (N = 1) were tested for Mycoplasma spp. All Mycoplasma-positive samples were specified by species-specific PCR for Mycoplasma anserisalpingitidis (formerly known as Mycoplasma sp. 1220), M. anseris, M. anatis, and M. cloacale. The presence of Mycoplasma spp. was confirmed in 22 of 29 sampled birds (75.9%). Mycoplasma anserisalpingitidis was the most frequently detected species (15 of 22, 68.2%). However, we did not detect any of the other Mycoplasma spp. typical for geese, among which are M. anatis, M. anseris, and M. cloacale. Phylogenetic analysis revealed that Polish sequences of M. anserisalpingitidis formed a distinct branch, along with 2 Hungarian isolates obtained from domestic geese. Eight of the samples identified as Mycoplasma spp.-positive were negative for the aforementioned Mycoplasma species. A phylogenetic tree constructed based on partial 16S rRNA gene analysis showed that Mycoplasma spp. sequences collected from Polish wild geese represent a distinct phylogenetic group with Mycoplasma sp. strain 2445 isolated from a domestic goose from Austria. The results of our study showed that wild geese could be a reservoir and vector of different species of the Mycoplasma genus that can cause significant economic losses in the domestic goose industry

Optically detected galaxy cluster candidates in the <i>AKARI</i> North Ecliptic Pole field based on photometric redshift from the Subaru Hyper Suprime-Cam

Galaxy clusters provide an excellent probe in various research fields in astrophysics and cosmology. However, the number of galaxy clusters detected so far in the AKARI North Ecliptic Pole (NEP) field is limited. In this work, we provide galaxy cluster candidates in the AKARI NEP field with the minimum requisites based only on the coordinates and photometric redshift (photo-z) of galaxies. We used galaxies detected in five optical bands (g, r, i, z, and Y) by the Subaru Hyper Suprime-Cam (HSC), with additional data from the u band obtained from the Canada-France-Hawaii Telescope (CFHT) MegaPrime/MegaCam, and from the IRAC1 and IRAC2 bands from the Spitzer space telescope for photo-z estimation. We calculated the local density around every galaxy using the 10th-nearest neighbourhood. Cluster candidates were determined by applying the friends-of-friends algorithm to over-densities. A total of 88 cluster candidates containing 4390 member galaxies below redshift 1.1 in 5.4 deg2 were identified. The reliability of our method was examined through false-detection tests, redshift-uncertainty tests, and applications on the Cosmic Evolution Survey (COSMOS) data, giving false-detection rates of 0.01 to 0.05 and a recovery rate of 0.9 at high richness. Three X-ray clusters previously observed by ROSAT and Chandra were recovered. The cluster galaxies show a higher stellar mass and lower star formation rate compared with the field galaxies in two-sample Z-tests. These cluster candidates are useful for environmental studies of galaxy evolution and future astronomical surveys in the NEP, where AKARI has performed unique nine-band mid-infrared photometry for tens of thousands of galaxies

Properties and evolution of galaxy clustering at 2<z<5 based on the VIMOS Ultra Deep Survey

Cette thèse porte sur l'étude des propriétés et l'évolution de regroupement de galaxies pour les galaxies de la gamme de 22. Je ai pu mesurer la distribution spatiale d'une population générale de galaxie à redshift z~3 pour la première fois avec une grande précision. Je ai quantifié le regroupement de galaxie en estimation et la modélisation de la fonction de corrélation projetée (espace réel) à deux points, pour une population générale de 3022 galaxies. Je ai prolongé les mesures de regroupement à la luminosité et des sous-échantillons de masse sélectionné stellaires. Mes résultats montrent que la force de regroupement de la population générale de la galaxie ne change pas de redshift z~3,5 à z~2,5, mais dans les deux redshift va plus lumineux et des galaxies plus massives sont plus regroupées que les moins lumineux (massives). En utilisant la distribution d'occupation de halo (HOD) formalisme je mesuré une masse moyenne de halo hôte au redshift z~3 significativement plus faible que les masses halo moyens observés à faible redshift. Je ai conclu que la population de formation d'étoiles observé des galaxies à z~3 aurait évolué dans le massif et lumineux la population de galaxies au z=0. Aussi, je interpréter les mesures de regroupement en termes de biais de galaxies à grande échelle linéaire. Je trouve que ce est nettement plus élevé que le biais des galaxies redshift intermédiaire et faible. Enfin, je ai calculé le ratio-stellaire Halo masse (SHMR) et l'efficacité intégrée de formation d'étoiles (ISFE) pour étudier l'efficacité de la formation des étoiles et l'assemblage masse stellaire.This thesis focuses on the study of the properties and evolution of galaxy clustering for galaxies in the redshift range 22. I was able to measure the spatial distribution of a general galaxy population at redshift z~3 for the first time with a high accuracy. I quantified the galaxy clustering by estimating and modelling the projected (real-space) two-point correlation function, for a general population of 3022 galaxies. I extended the clustering measurements to the luminosity and stellar mass-selected sub-samples. My results show that the clustering strength of the general galaxy population does not change significantly from redshift z~3.5 to z~2.5, but in both redshift ranges more luminous and more massive galaxies are more clustered than less luminous (massive) ones. Using the halo occupation distribution (HOD) formalism I measured an average host halo mass at redshift z~3 significantly lower than the observed average halo masses at low redshift. I concluded that the observed star-forming population of galaxies at z~3 might have evolved into the massive and bright (Mr<-21.5) galaxy population at redshift z=0. Also, I interpret clustering measurements in terms of a linear large-scale galaxy bias. I find it to be significantly higher than the bias of intermediate and low redshift galaxies. Finally, I computed the stellar-to-halo mass ratio (SHMR) and the integrated star formation efficiency (ISFE) to study the efficiency of star formation and stellar mass assembly. I find that the integrated star formation efficiency is quite high at ~16% for the average galaxies at z~3

The VVDS-WIDE survey. Clustering of galaxies as a function of absolute luminosities from z = 1.2 to z = 0.

We investigate the dependence of galaxy clustering on the galaxy absolute luminosities, using 7975 galaxies, with the apparentmagnitude range 17.5<I_{AB}<22.5, from the wide part of VIMOS VLT Deep Survey (VVDS-Wide). This large number of galaxies allows usto measure the projected two-point correlation function of galaxies, w_p(r_p), for a set of volume-limited and luminosity-limitedsubsemples of galaxies at different redshifts (wide and narrow redshift samples).Fitting w_p(r_p) with a single power-law model for the real-space correlation function \\xi(r)=(r/r_0)^{-\\gamma}, we measurethe relationship between the correlation length r_0 and slope \\gamma and the sample median luminosity.For all redshift samples we observed strong luminosity dependence of galaxy clustering. Correlation length rises with luminosity, which means that brighter galaxies are more strongly clustered than fainter ones. On the other hand, correlation function slope \\gamma remains constant regardless of luminosity and redshift, and in our redshift range varies around \\gamma=1.60, in contrast to other similar surveys at z\\sim1, where correlation slope steepens for the brightes galaxies (one halo term).This can be both an observational effect (associated with VVDS-Wide properties) and/or simply absence of this phenomen.Comparision of our results with those for large local surveys (as 2dFGRS) shows us that nowadays (z\\sim0.1) galaxies of allluminosities are more clustered than their counterparts in previous epochs (z~0.9).For a concordance cosmology we compute the galaxy bias in linear approximation. We observe that the galaxybias rises with redshift, between z=0.1 and z=1.2 its value changes by b = 0.68 - 1.48. These results are ingood agreement with the hierarchical model of galaxy formation. Also in the framework of this model we can explain the luminosity dependence of the relative bias which we found. Our results suggest that the brightest (most massive) galaxies correspond to the highest fluctuations of the total mass density field and they are highly biased. The galaxy bias decreases with time, whichcan be explained by the relocation of the star formation to the less dense regions of the Universe between z=1.2 and current epoch.Wykorzystując 7975 galaktyk o jasnościach 17.5<I_{AB}<22.5 obserwowanych w polu F22 przeglądu VVDS-Wide, zbadano zależność grupowania galaktyk od ich jasności abosultnej pomiędzy epokami odpowiadającymi przesunięciom ku czerwieni z=1.2, a z=0. Tak duża próbka galaktyk pozwoliła na oszacowanie 2-punktowej funkcji korelacyjnej, zrzutowanej na płaszczyznę prostopadłą do linii widzenia w_p(r_p) dla galaktyk jednostronnie (volume linited) oraz dwustronnie (luminosity limited) ograniczonych jasnościowo wróżnych przedziałach przesunięć ku czerwieni z.Dopasowując do w_p(r_p) funkcję potęgową \xi(r)=(r/r_0)^{-\gamma}, zmierzono związek pomiędzy długością korelacji r_0 i nachyleniem \gamma a medianą jasności absolutnych galaktyk. Dla wszystkich przesunięć ku czerwieni zaobserwowano zdecydowany wzrost wartości r_0 wraz z jasnością, co oznacza silniejsze grupowanie najjaśniejszych galaktyk, w porównaniu do grupowania tych słabszych. W przeciwieństwie do niektórych innych przeglądów dla z~1, w większościprzypadków nie zaobserwowano zwiększonego nachylenia funkcji korelacji jasnych galaktyk w małych skalach (tzw. onehalo term) co można tłumaczyć zarówno brakiem tego zjawiska, ale także specyficznymi obciążeniami obserwacyjnymiprzeglądu VVDS-Wide. Porównując otrzymane wyniki z innymi wynikami uzyskanymi dla dużych przeglądów lokalnych, zauważono, że we wszystkich jasnościach galaktykisą bardziej pogrupowane obecnie (z~0.2), niż ich odpowiedniki we wcześniejszych epokach (z~0.9).Przyjmując Standardowy Model Kosmologiczny oszacowano dla całej próbki galaktyk tzw. bias galaktyczny (obciążenie) uzyskując jego zależność od przesunięcia ku czerwieni. Pomiędzy z=0.1 a z=1.2 jego wartość wzrasta o b =0.68-1.48.Uzyskane wyniki dobrze wpisują się w hierarchiczny model formowania struktur. Również w ramach tego modelu dobrze tłumaczy się uzyskana zależność biasu względnego (obciążenia) od jasności absolutnej. Nasze wyniki wskazują, że zgodnie zhierarchicznym modelem wzrostu struktury, jasne (masywniejsze) galaktyki są związanez najsilniejszymi fluktuacjami gęstości i są najbardziej obciążone w stosunkudo pola gęstości ciemnej materii. Obciążenie to maleje z czasem, co można wytłumaczyć przenoszeniemsię procesów gwiazdotwórczych w mniej gęste obszary Wszechświata w okresie od z=1.2 doepoki obecnej

In Search of the Specificity of Scientific Originality in the Discipline of Management Science

Celem artykułu jest analiza znaczenia specyfiki dyscypliny nauki o zarządzaniu i jakości (NZJ) dla rozumienia oryginalności naukowej w dyscyplinie. W części pierwszej opracowania omówiono wyzwania związane z niejednoznacznością pojęcia oryginalności naukowej oraz przytoczono wyniki badań dotyczące różnic w konceptualizacji oryginalności naukowej między dziedzinami i dyscyplinami. Następnie dokonano analizy znaczenia specyficznych cech dyscypliny NZJ dla rozumienia oryginalności i preferowanych rodzajów oryginalności w dyscyplinie. Przeprowadzona analiza pozwala stwierdzić, że można mówić o szczególnym rozumieniu oryginalności właściwemu NZJ, co stanowi przyczynek teoretyczny do konceptualizacji pojęcia oryginalności naukowej w dyscyplinie oraz wyznaczenia kierunków dalszych badań w tym obszarze. Zastosowano narracyjny, krytyczny przegląd literatury przedmiotu.The aim of the paper was to explore the relevance of the specificity of the management science discipline to the understanding of scientific originality in the discipline. The ambiguity of the concept of scientific originality is discussed and the differences in the conceptualisation of scientific originality between scientific fields and disciplines are presented. This is followed by an analysis of the relevance of discipline-specific characteristics of management science to the understanding of originality. The study supports the view that there is a particular understanding of originality inherent in a management science. It provides a theoretical contribution to the conceptualisation of scientific originality in the discipline and outlines directions for further research. A narrative critical literature review was conducted

Assessment of Dietary Intake and Nutritional Status in CrossFit-Trained Individuals: A Descriptive Study

CrossFit is a discipline with high training and nutritional requirements. To date, there is only scarce data evaluating nutrition among CrossFit training and they mostly focus on selected nutritional interventions. Therefore, the purpose of this descriptive study was the assessment of dietary intake and nutritional status in a selected group of CrossFit-trained participants. The study consisted of 62 CrossFit athletes (31 men and 31 women, aged 31.0 &plusmn; 5.2 and 30.0 &plusmn; 4.3 years, respectively). Body composition was analyzed by electrical bioimpedance. Dietary intake was assessed using a standardized 3-day food record. Body fat percentage for females and males was 20.3 &plusmn; 4.3% and 13.7 &plusmn; 3.3% respectively. The energy intake in the diet was lower (~1700 kcal in women and ~2300 kcal in men) than the recommended demand. Moreover, low consumption of carbohydrates was stated, as well as an inadequate intake of folate, vitamin E (in women), and minerals, such as Fe and Ca (in women). The energy, carbohydrate, iron, and calcium intake in the CrossFit participants&rsquo; diet was too low in comparison to recommendations. It seems justified to educate athletes and coaches about nutritional habits, and individual energy and nutrients requirements

Occurrence of Mycoplasma gallisepticum in wild birds: A systematic review and meta-analysis.

Mycoplasma gallisepticum is one of the most important poultry pathogens that can also infect wild birds, but knowledge of potential non-poultry hosts that could be reservoirs of M. gallisepticum is limited. For the paper presented here, we screened three databases (PubMed, Scopus, and the Web of Knowledge) to find articles on the occurrence of M. gallisepticum in different wild bird species that were published between 1951 and 2018. Among 314 studies found, we selected and included 50 original articles that met the pre-established criteria. From those publications we extracted the following information: name of the first author, year of publication, year of sample isolation, country, region, number of birds sampled, number of birds tested by each method, number of positive samples, diagnostic criteria, and if birds were wild or captive. Because different detection techniques were used to confirm the presence of M. gallisepticum in one animal, we decided to perform the meta analyses separately for each method. The estimated prevalence of M. gallisepticum in wild birds was different by each method of detection. Our summary revealed that M. gallisepticum was present in 56 species of bird belonging to 11 different orders, of which 21 species were reported suffering both past and current infection. Our work provides information on wild bird species that could be considered potential reservoirs or carriers of M. gallisepticum and could be helpful to set the direction for future research on the spread and phylogeny of M. gallisepticum in different hosts