Galaxy And Mass Assembly (GAMA): the Stellar Mass Budget by Galaxy Type

We report an expanded sample of visual morphological classifications from the Galaxy and Mass Assembly (GAMA) survey phase two, which now includes 7,556 objects (previously 3,727 in phase one). We define a local (z <0.06) sample and classify galaxies into E, S0-Sa, SB0-SBa, Sab-Scd, SBab-SBcd, Sd-Irr, and "little blue spheroid" types. Using these updated classifications, we derive stellar mass function fits to individual galaxy populations divided both by morphological class and more general spheroid- or disk-dominated categories with a lower mass limit of log(Mstar/Msun) = 8 (one dex below earlier morphological mass function determinations). We find that all individual morphological classes and the combined spheroid-/bulge-dominated classes are well described by single Schechter stellar mass function forms. We find that the total stellar mass densities for individual galaxy populations and for the entire galaxy population are bounded within our stellar mass limits and derive an estimated total stellar mass density of rho_star = 2.5 x 10^8 Msun Mpc^-3 h_0.7, which corresponds to an approximately 4% fraction of baryons found in stars. The mass contributions to this total stellar mass density by galaxies that are dominated by spheroidal components (E and S0-Sa classes) and by disk components (Sab-Scd and Sd-Irr classes) are approximately 70% and 30%, respectively

Antidoping: From health tests to the athlete biological passport.

The athlete biological passport (ABP) was implemented by the International Cycling Union (UCI) in 2008. However, this improvement in the fight against doping was preceded with different milestones since 1996. In this paper, a detailed evolution of the ABP from traditional direct (urine) testing for antidoping purposes is presented. A chronological overview of the ABP including earlier non-disclosed information and contemporary documentation are shown and documented. The strategic development from on-site competition blood testing, called "health tests", to the structure of the ABP is explained in this historical overview which provides information to the antidoping community and general public regarding the beginning of blood doping tests

On the lack of correlation between [O III ]/[O II ] and Lyman continuum escape fraction

We present the first results of our pilot study of eight photometrically selected Lyman-continuum (LyC) emitting galaxy candidates from the COSMOS field and focus on their optical emission line ratios. Observations were performed in the H and K bands using the Multi-Object Spectrometer for Infra-Red Exploration (MOSFIRE) instrument at the Keck Observatory, targeting the [O ii], H β, and [Oiii] emission lines. We find that photometrically selected LyC emitting galaxy candidates have high ionization parameters, based on their high [O iii]/[O ii] ratios (O32), with an average ratio for our sample of 2.5 ± 0.2. Preliminary results of our companion Low-Resolution Imaging Spectrometer (LRIS) observations, targeting LyC and Ly α, show that those galaxies with the largest O32 are typically found to also be Ly α emitters. High O32 galaxies are also found to have tentative non-zero LyC escape fractions (f esc (LyC)) based on u band photometric detections. These results are consistent with samples of highly ionized galaxies, including confirmed LyC emitting galaxies from the literature. We also perform a detailed comparison between the observed emission line ratios and simulated line ratios from density bounded H ii regions modelled using the photoionization code MAPPINGS V. Estimates of f esc (LyC) for our sample fall in the range from 0.0 to 0.23 and suggest possible tension with published correlations between O32 and f esc (LyC), adding weight to dichotomy of arguments in the literature. We highlight the possible effects of clumpy geometry and mergers that may account for such tension.Fil: Bassett, R.. Swinburne University of Technology; Australia. Australian Research Council. Centre of Excellence for All Sky Astrophysics in 3 Dimensions; AustraliaFil: Ryan-Weber, E.V.. Swinburne University of Technology; Australia. Australian Research Council. Centre of Excellence for All Sky Astrophysics in 3 Dimensions; AustraliaFil: Cooke, J.. Swinburne University of Technology; AustraliaFil: Diaz, Carlos Gonzalo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; Argentina. Gemini Observatory; ChileFil: Nanayakkara, T.. Leiden University; Países BajosFil: Yuan, T. T.. Swinburne University of Technology; Australia. Australian Research Council. Centre of Excellence for All Sky Astrophysics in 3 Dimensions; AustraliaFil: Spitler, L.R.. Australian Astronomical Observatories; Australia. Macquarie University; Australia. Macquarie University; AustraliaFil: Mestric, U.. Swinburne University of Technology; Australia. Australian Research Council. Centre of Excellence for All Sky Astrophysics in 3 Dimensions; AustraliaFil: Garel, T.. Centre de Recherche Astrophysique de Lyon; FranciaFil: Sawicki, Silvana Mabel. Saint Mary's University; CanadáFil: Gwyn, S.. National Research Council Canada; CanadáFil: Golob, A.. Saint Mary's University; Canad

Clues on the presence and segregation of very massive stars in the Sunburst Lyman-continuum cluster at z = 2.37

We report the identification of very massive stars (VMS; mass &gt; 100 Mθ) that may be segregated in the center of the young massive star cluster at z = 2:37 hosted in the lensed galaxy called Sunburst galaxy. This result is based on two pieces of evidence: (1) VLT/MUSE spectra of several multiple images of the same star cluster show key spectral signatures of VMS, such as the Heiiλ1640 broad emission, Nivλ1486 emission, and an Nivλ1720 P Cygni profile. In particular, Heiiλ1640 is broad (~1610 ± 300 km s-1), with an equivalent width of 3 Å, and asymmetric profile. These features require an extremely young (~2:5 Myr) stellar population component in which the masses of the stars exceed 100 Mθ. When a Salpeter initial mass function and BPASS models for normal massive stars are assumed, the observed spectral features require ~400 VMS. (2) The same star cluster is detected at a signal-to-noise ratio of ~100 in the Lyman continuum domain (λ &lt; 900 Å). The Lyman continuum emission emerges from a region with a radius that is at least twice smaller than what is observed at 1700Å (independently of magnification) and is located in the center of the cluster. After delensing, the effective radii in absolute scales are Reff[LyC] ~ 4:7 ± 1.5 pc and Reff[1700] = 7.8 ± 1.4 pc. The Lyman continuum radiation is mainly produced by hot and massive stars, which implies that their spatial distribution (including that of VMS) is preferentially more confined in the central parts of the cluster. Approximately 400 VMS hosted by a cluster of ~107Mθproduce ~15% of the escaping Lyman continuum photons, and the remaining photons are produced by other massive early-type stars

Differences in routine laboratory parameters related to cachexia between patients with hematological diseases and patients with solid tumors or heart failure – is there only one cachexia?

<p>Abstract</p> <p>Background</p> <p>Cachexia is a state of involuntary weight loss common to many chronic diseases. Experimental data, showing that cachexia is related to the enhancement of acute phase response reaction, led to the new definition of cachexia that included, aside from the principal criterion of weight loss, other “minor criteria”, Amongst them are levels of C-reactive protein (CRP), albumin and hemoglobin. However, there is paucity of data regarding possible differences of these laboratory parameters in patients with various diseases known to be related to cachexia.</p> <p>Methods</p> <p>CRP, albumin and hemoglobin were evaluated in 119 patients, divided into two disease groups, hematological (ones with diagnosis of non-Hodgkin lymphoma or Hodgkin disease) and non-hematological (solid tumor patients and patients with chronic heart failure). Patients were further subdivided into two nutritional groups, cachectic and non-cachectic ones according to the principal criterion for cacxehia i.e. loss of body weight.</p> <p>Results</p> <p>We found that cachectic patients had higher levels of CRP, and lower levels of both hemoglobin and albumin compared to non-cachectic patients, regardless of the disease group they fitted. On the other hand, the group of hematological patients had lower levels of CRP primarily due to the differences found in the non-cachectic group. Higher levels of albumin were also found in the hematological group regardless of the nutritional group they fitted. Limitations of cut-off values, proposed by definition, were found, mostly regarding their relatively low sensitivity and low negative predictive value.</p> <p>Conclusions</p> <p>As expected, differences in values of routine laboratory parameters used in definition of cachexia were found between cachectic and non-cachectic patients. Their values differed between hematological and non-hematological patients both in cachectic and non-cachectic group. Cut-off levels currently used in definition of cachexia have limitations and should be further evaluated.</p