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The Gaia-ESO Survey: Catalogue of Hα Emission Stars?,??

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The Gaia-ESO Survey: Catalogue of Hα Emission Stars?,?? A&A 581, A52 (2015) Astronomy DOI: 10.1051/0004-6361/201525857 & c ESO 2015 Astrophysics The Gaia-ESO Survey: Catalogue of Hα emission stars?;?? G. Traven1, T. Zwitter1, S. Van Eck2, A. Klutsch3, R. Bonito4;5, A. C. Lanzafame3;6, E. J. Alfaro7, A. Bayo8, A. Bragaglia9, M. T. Costado7, F. Damiani5, E. Flaccomio5, A. Frasca3, A. Hourihane10, F. Jimenez-Esteban11;12, C. Lardo13, L. Morbidelli14, E. Pancino9;15, L. Prisinzano5, G. G. Sacco14, and C. C. Worley10 1 Faculty of Mathematics and Physics, University of Ljubljana, Jadranska 19, 1000 Ljubljana, Slovenia e-mail: [email protected] 2 Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Boulevard du Triomphe, CP 226, 1050 Bruxelles, Belgium 3 INAF–Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy 4 Dipartimento di Fisica e Chimica Universita’ di Palermo, 90128 Palermo, Italy 5 INAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy 6 Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Universitá di Catania, via S. Sofia 78, 95123 Catania, Italy 7 Instituto de Astrofísica de Andalucía-CSIC, Apdo. 3004, 18080 Granada, Spain 8 Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, 5030 Casilla, Valparaíso, Chile 9 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 10 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 11 Centro de Astrobiología (INTA-CSIC), Departamento de Astrofísica, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 12 Suffolk University, Madrid Campus, C/ Valle de la Viña 3, 28003 Madrid, Spain 13 Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK 14 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Florence, Italy 15 ASI Science Data Center, via del Politecnico SNC, 00133 Roma, Italy Received 10 February 2015 / Accepted 29 June 2015 ABSTRACT We discuss the properties of Hα emission stars across the sample of 22035 spectra from the Gaia-ESO Survey internal data release, observed with the GIRAFFE instrument and largely belonging to stars in young open clusters. Automated fits using two independent Gaussian profiles and a third component that accounts for the nebular emission allow us to discern distinct morphological types of Hα line profiles with the introduction of a simplified classification scheme. All in all, we find 3765 stars with intrinsic emission and sort their spectra into eight distinct morphological categories: single–component emission, emission blend, sharp emission peaks, double emission, P-Cygni, inverted P-Cygni, self–absorption, and emission in absorption. We have more than one observation for 1430 stars in our sample, thus allowing a quantitative discussion of the degree of variability of Hα emission profiles, which is expected for young, active objects. We present a catalogue of stars with properties of their Hα emission line profiles, morphological classification, analysis of variability with time and the supplementary information from the SIMBAD, VizieR, and ADS databases. The records in SIMBAD indicate the presence of Hα emission for roughly 25% of all stars in our catalogue, while at least 305 of them have already been more thoroughly investigated according to the references in ADS. The most frequently identified morphological categories in our sample of spectra are emission blend (23%), emission in absorption (22%), and self–absorption (16%). Objects with repeated observations demonstrate that our classification into discrete categories is generally stable through time, but categories P-Cygni and self–absorption seem less stable, which is the consequence of discrete classification rules, as well as of the fundamental change in profile shape. Such records of emission stars can be valuable for automatic pipelines in large surveys, where it may prove very useful for pinpointing outliers when calculating general stellar properties and elemental abundances. They can be used in studies of star formation processes, interacting binaries, and other fields of stellar physics. Key words. stars: emission-line, Be – stars: peculiar – open clusters and associations: general – line: profiles – catalogs – stars: activity 1. Introduction systematically covering all major components of the Milky Way, from halo to star forming regions (Gilmore et al. 2012; Randich The Gaia-ESO Survey (GES) is a large spectroscopic survey that 5 et al. 2013). With uniform mode of observation, well-defined targets more than 10 stars in a magnitude range 8 . V < 19, samples, based primarily on ESO-VISTA photometry for the ? field stars, and by a variety of photometric surveys of open clus- Based on data products from observations made with ESO ters, GES will quantify the kinematic-multielement abundance Telescopes at the La Silla Paranal Observatory under programme distribution functions of stellar components in the bulge, the ID 188.B-3002. thick and thin discs, and the halo, as well as a significant sam- ?? Full Tables D.1–D.3 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via ple of ∼100 open clusters, covering a wide range of ages, stellar http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/581/A52 masses, metallicities, and distances from the Galactic centre. Article published by EDP Sciences A52, page 1 of 16 A&A 581, A52 (2015) Within the GES, the analysis of different types of stars is di- this would require customised treatment when identifying and vided into different working groups (WGs). WG10 is in charge analysing the very diverse physical conditions purely from ob- of the analysis of FGK-type GIRAFFE spectra (Recio-Blanco served line profiles. Instead, we try to be impartial towards dis- et al. 2014) and WG11 of FGK-type UVES spectra (Smiljanic tinct physical characteristics and treat all available spectra in a et al. 2014). WG12 focuses on sources in the field of young uniform manner. In this way, we are able to review and mor- clusters (Lanzafame et al. 2015) and WG13 on OBA-type stars phologically classify several thousand objects without particular (Blomme et al. 2015). WG14 is in charge of non-standard ob- assumptions and model dependent parameters. jects, or objects for which standard analyses produce uncertain We approach the problem first with the detection of Hα emis- or no results because of unusual spectroscopic features that are sion in spectra and secondly, we introduce a simple morpholog- not properly accounted for by automatic pipelines. ical scheme for their classification. This classification scheme, The Hα emission, indicative of accretion and outflow activ- together with supplementary information about detected objects, ity in young stars, is one of these outstanding features. Indeed, like their classification from the literature where available, might when not properly recognised, it can endanger the parameter or prove useful to those who deal with the aforementioned types of abundance determination analysis, for example because it affects active objects and could serve as a uniform and unbiased treat- the local continuum placement or the radial velocity determina- ment of largely diverse emission profiles. tion. It was therefore decided, as part of the WG14 attributions, In Sect. 2 we present the data used in this study and the to systematically detect and characterise Hα emission. methods of reduction. The results of classification and tempo- This paper presents a catalogue of 4459 Hα emission stars ral variability of objects are presented in Sect. 3. Discussion and and their 8846 spectra across the sample of 22 035 spectra of conclusions follow in Sect. 4. 12 392 stars observed with GIRAFFE instrument from the GES internal data release (first 22 months of observations). Special care is taken to distinguish intrinsic stellar emission from the 2. Data and reduction overview nebular one. Altogether, we find 7698 spectra with intrinsic emission that belong to 3765 stars. Such stars are often found in The GES employs the VLT-UT2 FLAMES high-resolution mul- stellar nurseries and nebular environments of young open clus- tiobject spectrograph (Pasquini et al. 2002). FLAMES has two ters and can therefore serve as a proxy for stellar ages. Another instruments, the higher-resolution UVES, fed by 8 fibres, and possibility is that they belong to the field and can be so far un- GIRAFFE, with about 130 fibres. In the present paper we con- recognised interacting binaries, like symbiotic stars and cata- centrate on the much more numerous GIRAFFE spectra to thor- clysmic variables. In this case GES provides a unique census oughly test our classification scheme; a similar analysis of the of interacting binaries at all Galactic latitudes, thereby helping UVES spectra will follow later. to sample the faint luminosity tail of their distribution that is We use only spectra obtained in the wavelength range with under-represented in existing catalogues. Hα line – HR15N setting (6470−6790 Å, R = 17 000), for which The Hα emission profiles display a variety of shapes de- the majority of targets selected by GES are open cluster stars. pending on the physical mechanism responsible for the emis- Along with ongoing GES observations, we also use all relevant sion and on the geometry of the source. The simplest profiles are ESO archive data, which are included to be analysed as part of symmetric with a Gaussian-like appearance and are presumably GES. Individual spectra can therefore be dated up to nine years originated in one distinct source, but other more complex line before the start of the survey. For objects with more than one profiles are frequently observed. We refer the readers to Bonito spectrum from either new or archival data, the timespan of re- et al.(2013) and Reipurth et al.(1996) for a discussion of the ex- peated observations ranges from two days up to one year, which pected Hα profile features and their physical origin.
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