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Volume 515 (June 2010)

A&A, 515 (2010) A111

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Issue		A&A Volume515, June 2010


Article Number		A111
Number of page(s)		5
Section		Catalogs and data
DOI		https://doi.org/10.1051/0004-6361/201014247
Published online		15 June 2010

A&A 515, A111 (2010)

The PASTEL catalogue of stellar parameters

C. Soubiran¹ - J.-F. Le Campion¹ - G. Cayrel de Strobel² - A. Caillo³

1 - Laboratoire d'Astrophysique de Bordeaux (LAB-UMR 5804), CNRS, Université Bordeaux 1,2 rue de l'Observatoire, BP 89, 33271 Floirac Cedex, France
2 - GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, Place Jules Janssen, 92190 Meudon, France
3 - Observatoire Aquitain des Sciences de l'Univers (OASU-UMS 2567), CNRS, Université Bordeaux 1, 2 rue de l'Observatoire, BP 89, 33271 Floirac Cedex, France

Received 11 February 2010 / Accepted 29 March 2010

Abstract
Aims. The PASTEL catalogue is an update of the[Fe/H] catalogue, published in 1997 and 2001. It is abibliographical compilation of stellar atmospheric parameters providing( $T_{\rm eff}$ , $\log$ g , [Fe/H]) determinations obtained from the analysisof high resolution, high signal-to-noise spectra, carried out withmodel atmospheres. PASTEL also provides determinations of the oneparameter $T_{\rm eff}$ basedon various methods. It is aimed in the future to provide alsohomogenized atmospheric parameters and elemental abundances, radial androtational velocities. A web interface has been created to query thecatalogue on elaborated criteria. PASTEL is also distributed throughthe CDS database and VizieR.
Methods. To make it as complete as possible, the main journalshave been surveyed, as well as the CDS database, to find relevantpublications. The catalogue is regularly updated with newdeterminations found in the literature.
Results. As of Febuary 2010, PASTEL includes 30151 determinations of either $T_{\rm eff}$ or ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) for 16 649 different starscorresponding to 865 bibliographical references. Nearly 6000 stars havea determination of the three parameters ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) with a high quality spectroscopic metallicity.

Key words:catalogs - stars: abundances - stars: atmospheres - stars: fundamental parameters

1 Introduction

The knowledge of stellar atmospheric parameters ( $T_{\rm eff}$ , $\log g$ ,[Fe/H]) is mandatory to estimate the abundance of any chemical elementin a stellar atmosphere, which then traces either the composition ofthe interstellar medium from which the star formed or the variousphysical processes which may alter the initial composition. Atmosphericparameters are thus essential in many reasearch areas related to thephysics of stars and galaxies.

The detailed analysis of high resolution, high signal-to-noise spectrais the only primary method to estimate the chemical composition ofstellar photospheres, from which other indirect methods of metallicitydeterminations can be calibrated. The general approach of aspectroscopic detailed analysis is to derive the iron abundance bymatching equivalent widths of weak lines or spectral intervals of anobserved spectrum to those computed from a grid of model atmospheres ofvarious effective temperatures, gravities and metallicities. The higherthe resolution and signal-to-noise ratio, the better are supposedly theresults. However, each individual study has its own observationalcharacteristics, preferred stellar atmosphere models, atomic line dataand analysis methods. The consequence is a lack of homogeneity in theresults from one study to the next which makes it very cumbersome tocombine the determinations. Defining a common scale for atmosphericparameters is a mandatory but difficult task, which starts with thecompilation of the best studies available in the literature. This isthe aim of the PASTEL catalogue, which follows the previous[Fe/H] catalogue.

The publication of the [Fe/H] catalogue started with a first version in 1980 (Cayrel de Strobel et al. 1980), continued with three other versions (Cayrel de Strobel et al. 1992,1985,1981) superseded by the 1996 edition (Cayrel de Strobel et al. 1997). Then the content of the 2001 edition (Cayrel de Strobel et al. 2001)was modified by limiting the temperature range to stars cooler than7000 K and by removing references older than 1980. It was time toupdate the [Fe/H] catalogue. Since 2001, spectroscopicobservations of individual stars at high resolution and highsignal-to-noise (S/N) have been intensive. Several research topics areparticularly productive regarding the number of analysed stars. Studieson the chemical composition of stars with planets, on the metallicitydistribution and gradients in the Galaxy and on the chemicalcomposition of metal-poor stars have produced extensive lists of stars,based on high-quality data, with a good fraction of stars which havebeen observed at high spectral resolution for the first time.

The methods have evolved. Due to the growing number of spectra to beprocessed, it becomes more frequent that spectroscopic analyses areautomatised. It can be either the measurement of equivalent widths, orthe fitting of individual lines or spectral regions to computed ones.As a consequence, recent papers tend to present larger number of starsthan before. A typical example of such an extensive paper is the one by Valenti & Fischer (2005) presenting a uniform catalogue of stellar properties for 1040 nearby F, G, and K stars.

Effective temperature is a critical parameter in spectroscopic analyses, because errors in $T_{\rm eff}$ leadto significant errors in measured abundances. Several recent studieshave contributed to a significant increase of the number of stars withprecise determinations of $T_{\rm eff}$ . We have included these studies in PASTEL, even if they are not based on high-resolution spectra.

In this new catalogue we come back to the content of the 1996 editionof the [Fe/H] catalogue including hot stars, and references olderthan 1980. We complete it with the 2001 edition and with new referencesgathered from the literature. Thus, PASTEL supersedes the two previousversions of the [Fe/H] catalogue. In the two latest[Fe/H] catalogues, field and cluster stars were presented inseparate tables. Here we have them in a single catalogue.

A webserver has been created for a convenient query of the catalogue.It can be queried by a list of identifiers resolved by Simbad, or bycontraints on the atmospheric parameters, or on equatorial coordinates,B andV or 2MASSJ,H,K magnitudes, as well as by name of authors, year of publication or bibcode.

The numbers given in this paper are those corresponding to the versionof PASTEL in Febuary 2010. Because the catalogue is updated regularly,these numbers are changing accordingly.

2 Description of the catalogue

2.1 Identification and basic data

Only identifiers of stars resolved by Simbad are considered inPASTEL. As a consequence, the peculiar case of spectroscopic binariesin which the components could be resolved at high resolution andstudied separetely are not included in the catalogue. We will considerthese cases in future versions.

We have adopted a rule to identify a star with a single name in thecatalogue. We choose in priority its HD number, if that is notavailable we take by order : BD, CD, HIP, LHS, NLTT, LTT, CPD. If astar has none of these identifiers, we adopt the one given in thepublication if resolved by Simbad.

For each star entered in PASTEL, Simbad is queried to retreive its equatorial coordinates andB,V,J,H,K magnitudes. The catalogue can thus be searched either by zone in the sky or by magnitude interval.

2.2 Effective temperature

The direct approach to compute the effective temperature of a star,from its angular diameter and total flux at Earth, is only applicablefor a limited number of nearby stars. There are other indirect orsemi-empirical methods using continuum and spectral-line sensitivitiesto temperature. In practice, there are several ways to implement thesemethods, each implementation giving its own temperature scale. As aconsequence, the comparison of $T_{\rm eff}$ fromone author to another may show some systematic differences. The mostsignificant publications which have provided extensive lists of $T_{\rm eff}$ have been included in PASTEL. They are presented in Table1.

Table 1: Major publications, in terms of number of stars, providing $T_{\rm eff}$ determinations.

The histogram of all $T_{\rm eff}$ in PASTEL is shown in Fig. 1. The vast majority of $T_{\rm eff}$ determinations are in the FGK regime.

If quoted in the articles, individual errors on $T_{\rm eff}$ aregiven in PASTEL. On average these errors, which are internal, are atthe level of 1.1%. This can be compared to the dispersion around themean of $T_{\rm eff}$ determinationsfor the fraction (24%) of stars in PASTEL which have at least twoavailable values. On average this dispersion is 1.3% and reflects bothinternal and external errors, including differences in temperaturescales. We have not attempted to make a more detailed analysis of thedifferent temperature scales because the $T_{\rm eff}$ determinationsthat we compare are not independant. Most studies use common referencedata, even if the calibration methods are different.

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig1.ps}\end{figure}$	Figure 1: Histogram of all effective temperature determinations in PASTEL.
Open with DEXTER

2.3 Logarithm of surface gravity, log g

The surface gravity of a star is directly given by its mass and radius.It is a measure of the photospheric pressure of the stellar atmosphere.A direct measurement is possible from eclipsing spectroscopic binaries.Popular indirect methods use the ionization balance of iron in which $\log$ g is tuned until the metallicity obtained from the FeI andFeII lines agrees, or wings of strong lines, broadened by collisionaldamping. For nearby stars, the parallax is often used once theeffective temperature is determined. When available, errors on $\log$ g are on average around 0.10 dex.

2.4 Metallicity, [Fe/H]

As usual [Fe/H] is defined by

$\begin{displaymath}\rm\mbox{[Fe/H]~}= \log (Fe/H)_{\rm star} - \log(Fe/H)_{\rm Sun},\end{displaymath}$

where Fe/H is the ratio of the number of iron atoms to the number of hydrogen atomsin the atmosphere of either the star and the Sun.

For this bibliographical compilation, we have only gathered[Fe/H] determinations based on high resolution, highsignal-to-noise spectra. We have considered that the high spectralresolution is aboveR=30 000.In general high signal-to-noise implies a ratio higher than 100,although it is possible that some results included in PASTEL have beenobtained on slightly lower S/N.

Here again it is worthwhile comparing the typical internal errorsquoted in the publications, 0.06 dex on average, to the real dispersionof [Fe/H] determinations when several of them are available for agiven star. Among the stars which have [Fe/H] determined, 2731(44%) have at least two determinations available with a typicaldispersion of 0.08 dex. The dispersion is however related to themetallicity regime and the temperature as shown in Fig. 2.For stars more metal-rich than [Fe/H] = -1.0, the dispersion isessentially below 0.1 dex, except for stars hotter than 7000 K,which sometimes exhibit very discrepant metallicity determinations. Formetal-poor stars the dispersion is essentially below 0.2 dex. Thesituation is however slightly improved when the oldest determinationsare not considered.

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig2.ps}\end{figure}$	Figure 2: Dispersion of [Fe/H] estimations as a function of mean[Fe/H] for 2731 stars with at least two available determinations.The dashed line corresponds to the linear fit for stars hotter than7000 K, while the continuous line corresponds to FGK stars andreferences posterior to 1990.
Open with DEXTER

We have investigated the differences of metallicity scales in moredetail by comparing studies with at least 100 stars in common. Table2 gives the simple statistics, with a $3\sigma$ rejection, of two by two comparisons involving eight extensive andhomogeneous datasets. Each homogeneous set is designated by the name ofthe first author and may include several papers based on the same modelatmospheres, line data and analysis methods :

Fuhrmann =Fuhrmann et al. (1998);Fuhrmann (1998b,2004,2008,1998a), 300 stars;
Gratton =Gratton et al. (1996,2003), 398 stars;
Hekker =Hekker & Meléndez (2007), 366 stars;
Luck =Luck & Heiter (2006,2007), 222 stars;
McWilliam =McWilliam (1990), 671 stars;
Mishenina =Mishenina & Kovtyukh (2001);Mishenina et al. (2006,2004,2008), 557 stars;
Ramírez =Ramírez et al. (2007), 523 stars;
Valenti =Valenti & Fischer (2005), 1040 stars.

It is clear from these results that even though each of thesestudies can be considered of very high quality, none of them perfectlyagrees with the others. Either there is an offset between the zeropoint of the metallicities, or the dispersion is significant. The bestagreement, i.e. smallest offset and dispersion, is achieved betweenFuhrmann's datasets and the large sample ofValenti & Fischer (2005).Stars in common are however mainly G dwarfs of solar metallicity. Thelargest offset and dispersion are obtained when comparing themetallicities of giants studied byHekker & Meléndez (2007) andMcWilliam (1990).A large dispersion is also seen in the comparison of Gratton's andMishenina's datasets, which have a significant fraction of metal-poorstars in common. It is also worthwhile noting that the metallicityscales ofRamírez et al. (2007) andValenti & Fischer (2005),the two largest samples of homegeneous stellar parameters for nearbydisk stars, are shifted by 0.07 dex. This demonstrates thenon-homogeneity of spectroscopic metallicities, supposed to be of thebest quality.

Table 2: Two by two comparison of homogeneous sets of spectroscopic metallicities (see text).

2.5 Bibliographical references

The tables of content of the main astronomical journals areregularly surveyed to search for relevant publications, with dataavailable in numerical form. VizieR tables at the CDS are also checkedfor new entries, through a query by Unified Content Descriptor equal toPHYS_ABUND_FE/H and PHYS_TEMP_EFFEC. For each publication introduced inPASTEL we give the name of the first author, the year of publicationand the bibcode for an easy retrieval and citation of the correspondingarticle.

The most substantial contribution to the catalogue comes from theA&A journal with nearly 21 000 entries in PASTEL. Then ApJ andApJS are quoted $\sim$ 5000 times, followed by MNRAS with 1383 occurences.

Although PASTEL is intended to be exhaustive, the lack of manpower doesnot allow us to be complete. We recommend users of the catalogue tonotify us of missing references which should be included in thecatalogue.

3 Stellar content of the catalogue

The sample of stars in PASTEL cannot be considered as representativeof the stellar content of the solar neighbourhood. Obviously, thevarious observing programs, dealing with very different astrophysicalproblems, from which the catalogue was built, introduce some biases inthe distributions of ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) .

In Febuary 2010 PASTEL included 16649 different stars. Their histogram inV magnitude is presented in Fig. 3. Although the situation of faint stars is improving, 90% of the stars in PASTEL are still brighter thanV=9.75. There are less than 50 stars fainter thanV=15.5.

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig3.ps}\end{figure}$	Figure 3: Histogram of theV magnitude in PASTEL, available for 16 594 stars.
Open with DEXTER

There are 14817 entries in PASTEL with the full set of atmospheric parameters ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) corresponding to 5954 different stars (Figs. 4 and5).These numbers were 6000 and 3250 respectively in the 1997[Fe/H] catalogue, with similar values in the 2001 catalogue, butfor FGK stars. Despite the improvement of telescopes and spectrographs,there is still a lack of K dwarfs, which are intrinsically faint andmore difficult to observe at high resolution and high S/N than thegiants at the same $T_{\rm eff}$ $\!$ .A few M stars have been introduced in thecatalogue, but they are largely underepresented because they are difficult to analyse in detail.

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig4.ps}\end{figure}$	Figure 4: log( $T_{\rm eff}$ ) vs. $\log$ g in several regimes of metallicity for nearly 6000different stars. For stars with several entries in PASTEL the averagedparameters have been adopted.
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$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig5.ps}\end{figure}$	Figure 5: log( $T_{\rm eff}$ )vs. spectroscopic [Fe/H] for nearly 6000 different stars. Tworegimes of gravity are represented, corresponding roughly to giants(green) and dwarfs (red). For stars with several entries in PASTEL, theavaraged parameters have been adopted.
Open with DEXTER

4 Future evolutions

In general it is useful to have one single value of ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) for a given star. It is however quitedelicate to simply average determinations from different sourcesavailable in PASTEL because they are on different scales, asdemonstrated in Sect. 2. Some kind of homogenization has first tobe performed, as attempted for instance by Taylor (2005) and Twarog et al. (2007)for dwarfs and sub-giants. We are in the process of building a set ofreference stars with homogenized atmospheric parameters, selected fromthe PASTEL catalogue to cover at best the whole parameter space. Wealso plan to provide homogenized abundances in PASTEL, followingprevious work (Soubiran & Girard 2005). Radial and rotational velocities will also be included in PASTEL.

A useful functionality of the PASTEL database would be to link it witharchives of high resolution spectra through the Virtual Observatory. Weare working to have soon the PASTEL parameters available for thestellar spectra stored in the archive of the NARVAL spectropolarimeter attached to the Telescope Bernard Lyot at Pic du Midi. We are also considering such a link with the SOPHIE archive at Observatoire de Haute-Provence, as well as with the ELODIE archive (Moultaka et al. 2004).

The content of PASTEL in terms of cluster stars has not changed sincethe two previous versions of the [Fe/H] catalogue. We are now trying tomake up for filling the catalogue with recent extensive studies of openand globuler clusters which have been published since 2001. One of thedifficulties with stars in clusters is their correct identificationwith a name resolved by Simbad (sometimes only charts are available).For open clusters, we have started to work with the WEBDA team in that sense.

5 Conclusion

We have presented the PASTEL catalogue, which is to date abibliographical compilation with 30151 entries for 16649 differentstars. $T_{\rm eff}$ determinationsbased on various methods are available for all stars. Some 5954different stars have determinations of the full set of atmosphericparameters ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) with metallicity based on highresolution, high signal-to-noise spectra. The users are encouraged tocite the original analysis papers when using the determinationscompiled in PASTEL.

PASTEL offers a useful database for mining stars with known atmosphericparameters, in particular with a high-quality spectroscopicmetallicity. The users have to keep in mind that the content of thecatalogue is not homogeneous. The stellar content of catalogue, mainlybright stars, is biaised towards stars which are massively studied inpeculiar spectroscopic programmes, like solar type stars in planetsearches for instance. The ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) determinations are also not homogeneousand should not be simply averaged for most applications which look intodetailed chemical composition of stars. We have compared metallicitydeterminations available for the same stars from recent, homogeneousand high quality studies. We have found that in general these studiesdo not agree well. In some cases the offset can reach 0.07 dex and thedispersion 0.1 dex, larger than the individual errors quoted in theconsidered studies. The lack of a common ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) scaleresults from the variety ofobservational characteristics, model atmospheres, line data and methodsof analysis which are used in spectroscopy. A serious effort should beundertaken to build extensive and homogeneous catalogues of ( $T_{\rm eff}$ , $\log$ g , [Fe/H]) covering the whole HR diagram and metallicity range.

Acknowledgements

We warmly thank Ulrike Heiter,Roger Cayrel and Philippe Prugniel for their advices and help intesting the PASTEL database. We made extensive use of the CDS-SIMBADand NASA-ADS databases and VizieR Service at CDS, and we are extremelygrateful to the staff of these services for maintaining suchvaluable resources and for their assistance.

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Footnotes

... parameters: The catalogue can be queried through a dedicated web interface athttp://pastel.obs.u-bordeaux1.fr/. It is also available in electronic form at the Centre de Données Stellaires inStrasbourg (http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/pastel), at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/515/A111
... spectropolarimeter: http://tblegacy.bagn.obs-mip.fr/narval.html
... archive: http://atlas.obs-hp.fr/sophie/
... archive: http://atlas.obs-hp.fr/elodie/
... WEBDA: http://www.univie.ac.at/webda/

All Tables

Table 1: Major publications, in terms of number of stars, providing $T_{\rm eff}$ determinations.

Table 2: Two by two comparison of homogeneous sets of spectroscopic metallicities (see text).

All Figures

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig1.ps}\end{figure}$	Figure 1: Histogram of all effective temperature determinations in PASTEL.
Open with DEXTER
In the text

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig2.ps}\end{figure}$	Figure 2: Dispersion of [Fe/H] estimations as a function of mean[Fe/H] for 2731 stars with at least two available determinations.The dashed line corresponds to the linear fit for stars hotter than7000 K, while the continuous line corresponds to FGK stars andreferences posterior to 1990.
Open with DEXTER
In the text

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig3.ps}\end{figure}$	Figure 3: Histogram of theV magnitude in PASTEL, available for 16 594 stars.
Open with DEXTER
In the text

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig4.ps}\end{figure}$	Figure 4: log( $T_{\rm eff}$ ) vs. $\log$ g in several regimes of metallicity for nearly 6000different stars. For stars with several entries in PASTEL the averagedparameters have been adopted.
Open with DEXTER
In the text

$\begin{figure}\par\includegraphics[width=9cm,clip]{14247_fig5.ps}\end{figure}$	Figure 5: log( $T_{\rm eff}$ )vs. spectroscopic [Fe/H] for nearly 6000 different stars. Tworegimes of gravity are represented, corresponding roughly to giants(green) and dwarfs (red). For stars with several entries in PASTEL, theavaraged parameters have been adopted.
Open with DEXTER
In the text

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