4,218 research outputs found
A kinematically decoupled component in NGC4778
We present a kinematical and photometrical study of a member, NGC4778, of the
nearest (z=0.0137) compact group: Hickson 62. Our analysis reveals that Hickson
62a, also known as NGC4778, is an S0 galaxy with kinematical and morphological
peculiarities, both in its central regions (r < 5'') and in the outer halo. In
the central regions, the rotation curve shows the existence of a kinematically
decoupled stellar component, offset with respect to the photometric center. In
the outer halo we find an asymmetric rotation curve and a velocity dispersion
profile showing a rise on the SW side, in direction of the galaxy NGC4776.Comment: Proceedings of the first workshop of astronomy and astrophysics for
student
Metallicity of the polar disk in NGC4650A: constraints for cold accretion scenario
We used high resolution spectra in the optical and near-infrared wavelength
range to study the abundance ratios and metallicities of the HII regions
associated with the polar disk in NGC4650A, in order to put constraints on the
formation of the polar disk through cold gas accretion along a filament; this
might be the most realistic way by which galaxies get their gas. We have
compared the measured metallicities for the polar structure in NGC4650A with
those of different morphological types and we have found that they are similar
to those of late-type galaxies: such results is consistent with a polar disk
formed by accretion from cosmic web filaments of external cold gas.Comment: Proceeding of the conference "Hunting for the Dark: The Hidden Side
of Galaxy Formation", Malta, 19-23 Oct. 200
Chemical abundances in the polar disk of NGC4650A: implications for cold accretion scenario
The aim of the present study is to test whether the cold accretion of gas
through a "cosmic filament" Macci\`o et al. 2006 is a possible formation
scenario for the polar disk galaxy NGC 4650A. If polar disks form from cold
accretion of gas, the abundances of the HII regions may be similar to those of
very late-type spiral galaxies, regardless of the presence of a bright central
stellar spheroid, with total luminosity of few 10^9 Lsun. We use deep long slit
spectra obtained with the FORS2 spectrograph at the VLT in the optical and
near-infrared wavelength ranges for the brightest HII regions in the disk polar
disk of NGC 4650A. The strongest emission lines ([OII] Hbeta, [OIII], Halpha)
were used to derived oxygen abundances, metallicities and the global star
formation rates for the disk. The deep spectra available allowed us to measure
the Oxygen abundances (12 + log (O/H)) using the "Empirical method" based on
intensities of the strongest emission lines, and the "Direct method", based on
the determination of the electron temperature from the detection of weak
auroral lines, as the [OIII] at 4363 Angstrom. The Oxygen abundance measured
for the polar disk is then compared with those measured for different galaxy
types of similar total luminosities, and then compared against the predictions
of different polar ring formation scenarios. The average metallicity values for
the polar disk in NGC 4650A is Z=0.2 Zsun, and it is lower that the values
measured for ordinary spirals of similar luminosity. Moreover the gradient of
the metallicity is flat along the polar disk major axis, which implies none or
negligible metal enrichment from the stars in the older central spheroid. The
low metallicity value in the polar disk NGC 4650A and the flat metallicity
gradient are both consistent with a later infall of metal-poor gas, as expected
in the cold accretion processes.Comment: 42 pages, 9 figures. Accepted for publication in Ap
Incidence of temporomandibular joint clicking in adolescents with and without unilateral posterior cross-bite: a 10-year follow-up study
Among different malocclusions, posterior cross-bite is thought to have a strong impact on the correct functioning of the masticatory system. The association between unilateral posterior cross-bite (UPCB) and temporomandibular joint (TMJ) clicking, however, remains still controversial. The aim of this study was to investigate whether the presence of UCPB during early adolescence increases the risk of reporting TMJ clicking after a long-term follow-up. A longitudinal survey design was carried out in a group of 12-year-old young adolescents, who were examined at baseline for TMJ clicking sounds and unilateral posterior cross-bite. After 10 years, 519 subjects could be reached by a telephone survey. Standardised questions were used to collect self-reported TMJ sounds and to determine whether participants had received an orthodontic treatment. Logistic regression analysis revealed a significant association between unilateral posterior cross-bite and subjectively reported TMJ clicking (odds ratio = 6·0; 95% confidence limits = 3·4-10·8; P < 0·0001). The incidence of TMJ clicking was 12%. At a ten-year follow-up, self-reports of TMJ clicking were significantly associated with the presence of UPCB at baseline, but not with the report of having received an orthodontic treatment. Within the limitation of this study, the presence of unilateral posterior cross-bite in young adolescents may increase the risk of reporting TMJ sounds at a 10-year follow-up. The provision of an orthodontic treatment, however, does not appear to reduce the risk of reporting TMJ sounds
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