In this work, we present scanning Fabry-Perot (FP) H{alpha} observations of the isolated interacting galaxy pair NGC 5278/79 obtained with the PUMA FP interferometer. We derived velocity fields and ...rotation curves for both galaxies. For NGC 5278 we also obtained the residual velocity map to investigate the non-circular motions, and estimated its mass by fitting the rotation curve with disk+halo components. We test three different types of halos (pseudo-isothermal, Hernquist, and Navarro-Frenk-White) and obtain satisfactory fits to the rotation curve for all profiles. The amount of dark matter required by the pseudo-isothermal profile is about 10 times smaller than that for the other two halo distributions. Finally, our kinematical results together with the analysis of dust lane distribution and of surface brightness profiles along the minor axis allowed us to determine univocally that both components of the interacting pair are trailing spirals.
In this work, we present scanning Fabry-Perot (FP) H Delta *a observations of the isolated interacting galaxy pair NGC 5278/79 obtained with the PUMA FP interferometer. We derived velocity fields and ...rotation curves for both galaxies. For NGC 5278 we also obtained the residual velocity map to investigate the non-circular motions, and estimated its mass by fitting the rotation curve with disk+halo components. We test three different types of halos (pseudo-isothermal, Hernquist, and Navarro-Frenk-White) and obtain satisfactory fits to the rotation curve for all profiles. The amount of dark matter required by the pseudo-isothermal profile is about 10 times smaller than that for the other two halo distributions. Finally, our kinematical results together with the analysis of dust lane distribution and of surface brightness profiles along the minor axis allowed us to determine univocally that both components of the interacting pair are trailing spirals.
both) to reduce the colonization of Salmonella enterica in vitro was determined. A DCA with factorial arrangement (3x3) was used, being the factors the microorganisms and diffusion methods (direct, ...filtered and diluted) in the inhibition of the confrontation of microorganisms, with the use of the Kirby-Bauer technique. Survival in bile salts performed by the CFU count, under a design that had four treatments. The microorganisms with the application of three methods against Salmonella enterica had a favorable growth at 24 hours, obtaining a greater development with Lactobacillus brevis + Bacillus subtilis by filtration method. Survival to bile salts, no variability of results was found. However, L. brevis without bile salts stood out from minute 30 to minute 120. It is concluded that both microorganisms meet physical and biological characteristics, being suitable alternatives to be used as probiotics in animal feed for animal production purposes.
We present Fabry-Perot observations in the H\(\alpha\) and S II lines to study the kinematics of the Magellanic-type dwarf irregular galaxy NGC 1569, these observations allowed us to computed the ...H\(\alpha\) velocity field of this galaxy. Doing a detailed analysis of the velocity along the line-of-sight and H\(\alpha\) velocity profiles, we identified the origin of most of the motions in the innermost parts of the galaxy and discarded the possibility of deriving a rotation curve that traces the gravitational well of the galaxy. We analysed the kinematics of the ionised gas around 31 supernova remnants previously detected in NGC 1569 by other authors, in optical and radio emission. We found that the H\(\alpha\) velocity profiles of the supernova remnants are complex indicating the presence of shocks. Fitting these profiles with several Gaussian functions, we computed their expansion velocities which rank from 87 to 188 km s\(^{-1}\) confirming they are supernova remnants. Also, we determined the physical properties such as electron density, mechanical energy, and kinematic age for 30 of the 31 supernova remnants and found they are in the radiative phase with an energy range from 1 to 39\(\times\)10\(^{50}\) erg s\(^{-1}\) and an age from 2.3 to 8.9\(\times\)10\(^4\) yr. Finally, we estimated the Surface Brightness - Diameter (\(\Sigma\)-D) Relation for NGC 1569 and obtained a slope \(\beta\) = 1.26\(\pm\)0.2, comparable with the \(\beta\) value obtained for supernova remnants in galaxies M31 and M33.
IMAGES Neichel, B.; Hammer, F.; Puech, M. ...
Astronomy and astrophysics (Berlin),
06/2008, Volume:
484, Issue:
1
Journal Article
Peer reviewed
We present a first combined analysis of the morphological and dynamical properties for the intermediate-mass Galaxy Evolution Sequence (IMAGES) sample. It is a representative sample of 52 ...$z\sim0.6$ galaxies with Mstell from 1.5 to $15 \times 10^{10}~M_{\odot}$ that possesses 3D resolved kinematics and HST deep imaging in at least two broad band filters. We aim at evaluating the evolution of rotating spirals robustly since $z\sim 0.6$, as well as at testing the different schemes for classifying galaxies morphologically. We used all the information provided by multi-band images, color maps, and 2D light fitting to assign a morphological class to each object. We divided our sample into spiral disks, peculiar objects, compact objects, and mergers. Using our morphological classification scheme, 4/5 of the identified spirals are rotating disks, and more than 4/5 of identified peculiar galaxies show complex kinematics, while automatic classification methods such as concentration-asymmetry and GINI-M20 severely overestimate the fraction of relaxed disk galaxies. Using this methodology, we find that the fraction of undisturbed rotating spirals has increased by a factor ~2 during the past 6 Gyr, a much higher fraction than was found previously based on morphologies alone. These rotating spiral disks are forming stars very rapidly, even doubling their stellar masses over the past 6 Gyr, while most of their stars were formed a few Gyr earlier, which reveals a large gas supply. Because they are the likely progenitors of local spirals, we can conjecture how their properties are evolving. Their disks show some evidence of inside-out growth, and the gas supply/accretion is not random since the disk needs to be stable in order to match the local disk properties.
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IMAGES Puech, M.; Flores, H.; Hammer, F. ...
Astronomy and astrophysics (Berlin),
06/2008, Volume:
484, Issue:
1
Journal Article
Peer reviewed
Using the multi-integral field spectrograph GIRAFFE at VLT, we have derived the K-band Tully-Fisher relation (TFR) at $z \sim 0.6$ for a representative sample of 65 galaxies with emission lines ...($W_\mathrm{0}\mathrm{(OII)}\ge15$ Å). We confirm that the scatter in the $z \sim 0.6$ TFR is caused by galaxies with anomalous kinematics, and find a positive and strong correlation between the complexity of the kinematics and the scatter that they contribute to the TFR. Considering only relaxed-rotating disks, the scatter, and possibly also the slope, of the TFR, do not appear to evolve with redshift. We detect an evolution of the K-band TFR zero point between $z \sim 0.6$ and $z=0$, which, if interpreted as an evolution of the K-band luminosity of rotating disks, would imply that a brightening of $0.66 \pm 0.14$ mag occurs between $z \sim 0.6$ and $z=0$. Any disagreement with the results of Flores et al. (2006, A&A, 455, 107) are attributed to both an improvement of the local TFR and the more detailed accurate measurement of the rotation velocities in the distant sample. Most of the uncertainty can be explained by the relatively coarse spatial-resolution of the kinematical data. Because most rotating disks at $z\sim0.6$ are unlikely to experience further merging events, one may assume that their rotational velocity, which is taken as a proxy of the total mass, does not evolve dramatically. If true, our result implies that rotating disks observed at $z\sim0.6$ are rapidly transforming their gas into stars, to be able to double their stellar masses and be observed on the TFR at $z=0$. The rotating disks observed are indeed emission-line galaxies that are either starbursts or LIRGs, which implies that they are forming stars at a high rate. Thus, a significant fraction of the rotating disks are forming the bulk of their stars within 6 to 8 Gyr, in good agreement with former studies of the evolution of the mass-metallicity relationship.
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FMFMET, NUK, UL, UM, UPUK
We aimed to compare processing speed (PS) and its subcomponents in schizophrenia (SC) and schizoaffective disorder (SA). Thirty-five patients were divided into two groups (SC=18; SA=17). PS tasks ...from the MATRICS Consensus Cognitive Battery Central/South America version were used. Additional PS subcomponents were analyzed (i.e., behavioral execution, response processing, and accuracy). SA obtained significant higher scores than SC in response processing, verbal fluency and the PS general domain. Our results indicate that PS is a potential cognitive marker to differentiate between SC and SA. Further research with larger samples must be conducted.
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