DAOSPEC: An Automatic Code for Measuring Equivalent Widths in High-Resolution Stellar Spectra

Stetson, P. B.; Pancino, E.

doi:10.1086/596126

Cited by 248 publications

(276 citation statements)

References 35 publications

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“…EWs and RVs have been measured with the code DAOSPEC (Stetson & Pancino 2008), automatically launched by using the package 4DAO (Mucciarelli 2013), which allows a visual inspection of all the performed Gaussian fits. We started by adopting as input value the nominal full width at half-maximum (FWHM) of the gratings, leaving DAOSPEC free to re-adjust the FWHM in order to minimize the median value of the distribution of residuals (see Stetson & Pancino 2008). For some RHB stars the final FWHM is larger than those found for the RGB stars, indicating the presence of a (Gratton et al 2011(Gratton et al , 2013.…”

Section: Discussionmentioning

confidence: 99%

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

Mucciarelli

Dalessandro

Massari

et al. 2016

ApJ

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We present the first measure of Fe and Na abundances in NGC 6362, a low-mass globular cluster (GC) where firstand second-generation stars are fully spatially mixed. A total of 160 member stars (along the red giant branch (RGB) and the red horizontal branch (RHB)) were observed with the multi-object spectrograph FLAMES at the Very Large Telescope. We find that the cluster has an iron abundance of [Fe/H] = −1.09 ± 0.01 dex, without evidence of intrinsic dispersion. On the other hand, the [Na/Fe] distribution turns out to be intrinsically broad and bimodal. The Na-poor and Na-rich stars populate, respectively, the bluest and the reddest RGBs detected in the color-magnitude diagrams including the U filter. The RGB is composed of a mixture of first-and secondgeneration stars in a similar proportion, while almost all the RHB stars belong to the first cluster generation. To date, NGC 6362 is the least massive GC where both the photometric and spectroscopic signatures of multiple populations have been detected.

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Section: Discussionmentioning

confidence: 99%

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

Mucciarelli

Dalessandro

Massari

et al. 2016

ApJ

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“…We then measured equivalent widths (EWs) for a set of lines using iraf 5 and daospec (Stetson & Pancino 2008). The line list is presented in Table 4.…”

Section: Discussionmentioning

confidence: 99%

CNO abundances in the globular clusters NGC 1851 and NGC 6752★

Yong¹,

Grundahl²,

Norris³

2014

Monthly Notices of the Royal Astronomical Society

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We measure the C+N+O abundance sum in red giant stars in two Galactic globular clusters, NGC 1851 and NGC 6752. NGC 1851 has a split subgiant branch which could be due to different ages or C+N+O content while NGC 6752 is representative of the least complex globular clusters. For NGC 1851 and NGC 6752, we obtain average values of A(C+N+O) = 8.16 ± 0.10 (σ = 0.34) and 7.62 ± 0.02 (σ = 0.06), respectively. When taking into account the measurement errors, we find a constant C+N+O abundance sum in NGC 6752. The C+N+O abundance dispersion is only 0.06 dex, and such a result requires that the source of the light element abundance variations does not increase the C+N+O sum in this cluster. For NGC 1851, we confirm a large spread in C+N+O. In this cluster, the anomalous RGB has a higher C+N+O content than the canonical RGB by a factor of four (∼0.6 dex). This result lends further support to the idea that the two subgiant branches in NGC 1851 are roughly coeval, but with different CNO abundances.

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“…We measured the equivalent widths (EWs) of the absorption lines with DAOSPEC (Stetson & Pancino, 2008), which is an automatic tool optimised for the characteristics of GIRAFFE HR spectra. Lines are fitted by saturated gaussians because at the resolution of our data, the line profile is dominated by the instrumental effects and not astrophysical processes.…”

Section: Determination Of Stellar Parameters and Abundancesmentioning

confidence: 99%

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

Lemasle

Hill

Tolstoy

et al. 2012

A&A

191

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Context. The ages of individual Red Giant Branch stars can range from 1 Gyr old to the age of the Universe, and it is believed that the abundances of most chemical elements in their photospheres remain unchanged with time (those that are not affected by the first dredge-up). This means that they trace the interstellar medium in the galaxy at the time the star formed, and hence the chemical enrichment history of the galaxy. Aims. Colour-Magnitude Diagram analysis has shown the Carina dwarf spheroidal to have had an unusually episodic star formation history and this is expected to be reflected in the abundances of different chemical elements. Methods. We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R≈20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.

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DAOSPEC: An Automatic Code for Measuring Equivalent Widths in High-Resolution Stellar Spectra

Cited by 248 publications

References 35 publications

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

NGC 6362: The Least Massive Globular Cluster With Chemically Distinct Multiple Populations*

CNO abundances in the globular clusters NGC 1851 and NGC 6752★

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy

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