اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدChemical abundances in Terzan 7 from UVES spectra
55
0
0.0
(
0
)
تأليف
L. Sbordone
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
We present chemical abundances for Mg, Si, Ca and Fe for three red giants in the sparse globular cluster Terzan 7, physically associated to the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph), which is presently being tidally disrupted by the Milky Way. The data has been obtained with VLT-UVES and show a mean [Fe/H]=-0.57, with solar alpha content, mean [alpha/Fe]=-0.03. This enforces Ter 7s membership to the Sgr dSph system, which shows a similar pattern of abundance.
قيم البحث
اقرأ أيضاً
We present here the first measurements of sulphur abundances in extragalactic stars. We make use of high resolution spectra, obtained with UVES at the ESO 8.2 m Kueyen telescope, of three giants of the Globular Cluster Terzan 7, which belongs to the
Sagittarius dwarf galaxy. We measure the sulphur abundances using the lines of S I multiplet 1. The S/Fe ratios for all three stars are nearly solar, thus considerably lower than what is found in Galactic stars of comparable iron content ([Fe/H] ~ -0.50). This finding is in keeping with the abundances of other alpha-chain elements in this cluster and in Sagittarius and other dSphs in general. These low alpha-chain elements to iron ratios suggest that Sagittarius and its Globular Clusters have experienced a low or bursting star-formation rate. Our sulphur abundances imply <log (S/O)> = -1.61 which is comparable to what is found in many H II regions of similar oxygen content, and is slightly lower than the solar value (log (S/O)sun = -1.51). These are also the first measurements of sulphur abundances in a Globular Cluster, thus a direct comparison of Terzan 7 and Galactic Globular Clusters is not possible yet. However our analysis suggests that the lines of S I multiplet 1 should be measurable for other Globular Clusters at least down to a metallicity ~ -1.5.
This chapter presents a review on the latest advances in the computation of physical conditions and chemical abundances of elements present in photoionized gas H II regions and planetary nebulae). The arrival of highly sensitive spectrographs attache
d to large telescopes and the development of more sophisticated and detailed atomic data calculations and ionization correction factors have helped to raise the number of ionic species studied in photoionized nebulae in the last years, as well as to reduce the uncertainties in the computed abundances. Special attention will be given to the detection of very faint lines such as heavy-element recombination lines of C, N and O in H II regions and planetary nebulae, and collisionally excited lines of neutron-capture elements (Z >30) in planetary nebulae.
The aim of the present work is to determine accurate metallicities for a group of red giant branch stars in the field of the bulge Globular Cluster NGC 6441. This is the third paper of a series resulting from a large project aimed at determining the
extent of the Na-O anticorrelation among Globular Cluster stars and exploring its relationship with HB morphology. We present an LTE abundance analysis of these objects, based on data gathered with the FLAMES fiber facility and the UVES spectrograph at VLT2. Five of the thirteen stars observed are members of the cluster. The average Fe abundance for these five stars is [Fe/H]=$-0.39pm 0.04pm 0.05$~dex, where the first error bar includes the uncertainties related to star-to-star random errors, and the second one the systematic effects related to the various assumptions made in the analysis.The overall abundance pattern is quite typical of Globular Clusters, with an excess of the $alpha-$elements and of Eu. There is evidence that the stars of NGC 6441 are enriched in Na and Al, while they have been depleted of O and Mg, due to H-burning at high temperatures, in analogy with extensive observations for other Globular Clusters: in particular, one star is clearly Na and Al-rich and O and Mg-poor. We obtained also quite high V abundances, but it is possible that this is an artifact of the analysis, since similar large V abundances are derived also for the field stars. These last are all more metal-rich than NGC 6441 and probably belong to the bulge population.
The validity of oxygen and nitrogen abundances derived from the global emission-line spectra of galaxies via the P-method has been investigated using a collection of published spectra of individual HII regions in irregular and spiral galaxies. The co
nclusions of Kobulnicky, Kennicutt & Pizagno (1999) that global emission-line spectra can reliably indicate the chemical properties of galaxies has been confirmed. It has been shown that the comparison of the global spectrum of a galaxy with a collection of spectra of individual HII regions can be used to distinguish high and low metallicity objects and to estimate accurate chemical abundances in a galaxy. The oxygen and nitrogen abundances in samples of UV-selected and normal nearby galaxies have been determined. It has been found that the UV-selected galaxies occupy the same area in the N/O -- O/H diagram as individual HII regions in nearby galaxies. Finally, we show that intermediate-redshift galaxies systematically deviate from the metallicity -- luminosity trend of local galaxies.
Based on high resolution, high signal-to-noise (S/N) ratio spectra from Keck/HIRES, we have determined abundances of 20 elements for 18 Ba candidates. The parameter space of these stars are in the range of 4880 $leq$ $rm{T_{eff}}$ $leq$ 6050 K, 2.56
$leq$ log $g$ $leq$ 4.53 dex and -0.27 $leq$ [Fe/H] $leq$ 0.09 dex. It is found that four of them can be identified as Ba stars with [s/Fe] $>$ 0.25 dex (s: Sr, Y, Zr, Ba, La, Ce and Nd), and three of them are newly discovered, which includes two Ba giants (HD 16178 and HD 22233) and one Ba subgiant (HD 2946). Our results show that the abundances of $alpha$, odd and iron-peak elements (O, Na, Mg, Al, Si, Ca, Sc, Ti, Mn, Ni and Cu) for our program stars are similar to those of the thin disk, while the distribution of [hs/ls] (hs: Ba, La, Ce and Nd, ls: Sr, Y and Zr) ratios of our Ba stars is similar to those of the known Ba objects. None of the four Ba stars show clear enhancement in carbon including the known CH subgiant HD 4395. It is found that three of the Ba stars present clear evidences of hosting stellar or sub-stellar companions from the radial velocity data.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
