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J/A+A/520/A95    Abundances of red giants in M54 and Sgr dSph (Carretta+, 2010)

Detailed abundances of a large sample of giant stars in M 54 and in the Sagittarius nucleus. Carretta E. Bragaglia A., Gratton R., Lucatello S., Bellazzini M., Catanzaro G., Leone F., Momany Y., Piotto G., D'Orazi V. <Astron. Astrophys. 520, A95 (2010)> =2010A&A...520A..95C
ADC_Keywords: Stars, giant ; Stars, late-type ; Abundances, [Fe/H] Abundances, peculiar Keywords: stars: abundances - stars: atmospheres - stars: Population II - globular clusters: individual: NGC 6715 (M 54), NGC 5139 (omega Cen) - globular clusters: general Abstract: Homogeneous abundances of light elements, alpha-elements, and Fe-group elements from high-resolution FLAMES spectra are presented for 76 red giant stars in NGC 6715 (M 54), a massive globular cluster (GC) lying in the nucleus of the Sagittarius dwarf galaxy. We also derived detailed abundances for 27 red giants belonging to the Sgr nucleus. Our abundances assess the intrinsic metallicity dispersion (∼0.19dex, rms scatter) of M 54, with the bulk of stars peaking at [Fe/H]~-1.6 and a long tail extending to higher metallicities, similar to ω Cen. The spread in these probable nuclear star clusters exceeds those of most GCs: these massive clusters are located in a region intermediate between normal GCs and dwarf galaxies. M 54 shows the Na-O anticorrelation, typical signature of GCs, which is instead absent in the Sgr nucleus. The light elements (Mg, Al, Si) participating to the high temperature Mg-Al cycle show that the entire pattern of (anti)correlations produced by proton-capture reactions in H-burning is clearly different between the most metal-rich and most metal-poor components in the two most massive GCs in the Galaxy, confirming early result based on the Na-O anticorrelation. As in ω Cen, stars affected by most extreme processing, i.e. showing the signature of more massive polluters, are those of the metal-rich component. These observations can be understood if the burst of star formation giving birth to the metal-rich component was delayed by as much as 10-30Myr with respect to the metal-poor one. The evolution of these massive GCs can be easily reconciled in the general scenario for the formation of GCs recently sketched in Carretta et al.(2010a) taking into account that ω Cen could have already incorporated the surrounding nucleus of its progenitor and lost the rest of the hosting galaxy while the two are still observable as distinct components in M 54 and the surrounding field. Description: For a sample of ∼100 stars in M54 and the Sgr nucleus we give here: identifications, coordinates, BVIK magnitudes, heliocentric RV (table2); atmospheric parameters, [Fe/H] (table3); [O/Fe], [Na/Fe], [Mg/Fe], [Al/Fe] (table5); the α-elements Si, Ca, and Ti (table6); the Fe-peak elements Sc, V, Cr, Mn, Co, Ni, and Cu (table7). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 99 103 Identifications, positions, photometry and velocity table3.dat 82 103 Teff, logg, [A/H],Vt, [Fe/H]I, [Fe/H]II table5.dat 99 103 [O/Fe], [Na/Fe], [Mg/Fe], [Al/Fe] table6.dat 90 103 [Si/Fe], [Ca/Fe], [Ti/Fe] I & II table7.dat 161 103 [Sc/Fe], [V/Fe], [Cr/Fe],[Mn/Fe], [Co/Fe], [Ni/Fe], [Cu/Fe]
See also: J/AJ/118/1245 : Elemental abundances in five stars in M54 (Brown+, 1999) J/A+A/505/117 : Abundances of red giants in 15 globulars (Carretta+, 2009) J/A+A/505/139 : Abundances of red giants in 17 globulars (Carretta+, 2009) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Cl M54 or SgrN 7- 14 I8 --- ID Identification number 18- 19 I2 h RAh Right ascension (J2000.0) 21- 22 I2 min RAm Right ascension (J2000.0) 24- 28 F5.2 s RAs Right ascension (J2000.0) 31 A1 --- DE- Declination sign (J2000.0) 32- 33 I2 deg DEd Declination (J2000.0) 35- 36 I2 arcmin DEm Declination (J2000.0) 38- 42 F5.2 arcsec DEs Declination (J2000.0) 46- 51 F6.3 mag Bmag B magnitude 53- 58 F6.3 mag Vmag V magnitude 60- 65 F6.3 mag Imag I magnitude 67- 72 F6.3 mag Kmag K magnitude 75- 80 F6.2 km/s RV1 ?=0 Heliocentric radial velocity 83- 88 F6.2 km/s RV2 ?=0 Heliocentric radial velocity 91- 99 A9 --- Instr Instrument (1)
Note (1): Instruments as follows: UVES = UVES HR11 = Giraffe-HR11 HR13 = Giraffe-HR13
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Cl M54 or SgrN 7- 14 I8 --- ID Identification number 17- 20 I4 K Teff Effective temperature 23- 26 F4.2 [cm/s2] logg Gravity 29- 33 F5.2 [Sun] [A/H] Metallicity 36- 39 F4.2 km/s vt Microturbulent velocity 43- 44 I2 -- nFeI Number of FeI lines 49- 54 F6.3 [Sun] [Fe/H]1 FeI (neutral iron) abundance 57- 61 F5.3 [Sun] e_[Fe/H]1 rms on [Fe/H]1 64- 65 I2 -- nFeII ? Number of FeII lines 70- 75 F6.3 [Sun] [Fe/H]2 ? FeII (ionized iron) abundance 78- 82 F5.3 [Sun] e_[Fe/H]2 ? rms on [Fe/H]2
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Cl M54 or SgrN 7- 14 I8 --- ID Identification number 17 I1 --- nO number of O lines 22- 26 F5.2 [Sun] [O/Fe] Oxygen abundance 29- 32 F4.2 [Sun] e_[O/Fe] ? rms on [O/Fe] 37 I1 --- nNa ? Number of Na lines 42- 46 F5.2 [Sun] [Na/Fe] ? Sodium abundance 49- 52 F4.2 [Sun] e_[Na/Fe] ? rms on [Na/Fe] 57 I1 --- nMg ? Number of Mg lines 62- 66 F5.2 [Sun] [Mg/Fe] ? Magnesium abundance 69- 72 F4.2 [Sun] e_[Mg/Fe] ? rms on [Mg/Fe] 77 I1 --- nAl ? Number of Al lines 81- 85 F5.2 [Sun] [Al/Fe] ? Aluminum abundance 88- 91 F4.2 [Sun] e_[Al/Fe] ? rms on [Al/Fe] 96 I1 --- f_[O/Fe] [0,1]? 0=upper limit; 1=measure of Oxygen 99 I1 --- f_[Al/Fe] [0,1]? 0=upper limit; 1=measure of Aluminium
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Cl M54 or SgrN 6- 13 I8 --- ID Ndentification number 16- 17 I2 --- nSi Number of Si lines 21- 25 F5.2 [Sun] [Si/Fe] Silicon abundance 29- 32 F4.2 [Sun] e_[Si/Fe] ? rms on [Si/Fe] 36- 37 I2 --- nCa ? Number of Ca lines 42- 46 F5.2 [Sun] [Ca/Fe] ? Calcium abundance 50- 53 F4.2 [Sun] e_[Ca/Fe] ? rms on [Ca/Fe] 57- 58 I2 --- nTi1 ? Number of Ti I lines 64- 68 F5.2 [Sun] [Ti/Fe]1 ? Titanium (neutral) abundance 72- 75 F4.2 [Sun] e_[Ti/Fe]1 ? rms on [Ti/Fe]1 80 I1 --- nTi2 ? Number of Ti II lines 86- 90 F5.2 [Sun] [Ti/Fe]2 ? Titanium (ionized) abundance
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Cl M54 or SgrN 6- 13 I8 --- ID Identification number 16- 17 I2 --- nSc Number of Sc lines 23- 27 F5.2 [Sun] [Sc/Fe] Scandium abundance 31- 34 F4.2 [Sun] e_[Sc/Fe] ? rms on [Sc/Fe] 39- 40 I2 --- nV ? Number of V lines 46- 50 F5.2 [Sun] [V/Fe] ? Vanadium abundance 54- 57 F4.2 [Sun] e_[V/Fe] ? rms on [V/Fe] 61- 62 I2 --- nCr ? Number of Cr lines 68- 72 F5.2 [Sun] [Cr/Fe] ? Cromium abundance 76- 79 F4.2 [Sun] e_[Cr/Fe] ? rms on [Cr/Fe] 83- 84 I2 --- nMn ? Number of Mn lines 90- 94 F5.2 [Sun] [Mn/Fe] ? Manganese abundance 98-101 F4.2 [Sun] e_[Mn/Fe] ? rms on [Mn/Fe] 106-107 I2 --- nCo ? Number of Co lines 113-117 F5.2 [Sun] [Co/Fe] ? Cobalt abundance 121-124 F4.2 [Sun] e_[Co/Fe] ? rms on [Co/Fe] 129-130 I2 --- nNi ? Number of Ni lines 136-140 F5.2 [Sun] [Ni/Fe] ? Nichel abundance 144-147 F4.2 [Sun] e_[Ni/Fe] ? rms on [Ni/Fe] 152 I1 --- nCu ? Number of Cu lines 157-161 F5.2 [Sun] [Cu/Fe] ? Copper abundance
Acknowledgements: Eugenio Carretta, eugenio.carretta(at)oabo.inaf.it
(End) Eugenio Carretta [Bologna Obs.], Francois Ochsenbein [CDS] 16-Aug-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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