The Galactic Center Source IRS 13E: a Star Cluster
Identifieur interne : 000371 ( Main/Exploration ); précédent : 000370; suivant : 000372The Galactic Center Source IRS 13E: a Star Cluster
Auteurs : Jean-Pierre Maillard [France] ; Thibaut Paumard [France] ; Susan Stolovy [États-Unis] ; François Rigaut [États-Unis]Source :
- Astronomische Nachrichten [ 0004-6337 ] ; 2003-09.
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Abstract
High spatial resolution, near‐infrared observations of the Galactic Center source, close to Sgr A*, known historically as IRS13, are presented. These observations include ground‐based adaptive optics images in the H, K' and L bands, HST‐NICMOS observations in filters between 1.1 and 2.2 μm, and spectroimaging data in the He I 2.06 μm line and the Brγ line. Analysis of all these data has made possible the resolution of the main component, IRS 13E, into a cluster of seven individual stars within a projected diameter of ∼0.5″ (0.02 pc), and to build their SED. The main sources, 13E1, 13E2, 13E3 (a binary), and 13E4, are hot stars of different nature. 13E2 and 13E4 are emission line stars. The spectral type of the various members goes from O5I to WR, including dusty WRs like IRS 21 (Tanner et al. 2002). All these sources have a common westward proper motion. Two weaker sources, 13E5 and 13E6, are also detected within the compact cluster, with 13E5 proposed as another dusty WR and 13E6 as a O5V star. An extended halo seen around the cluster, part of the mini‐spiral of dust is particularly enhanced in the L band. It is interpreted as a contribution of the scattered light from the inner cluster and the thermal emission from the dust. IRS 13E is proposed to be the remaining core of a massive, young star cluster which was disrupted in the vicinity of Sgr A*, and hence, the possible source of the young stars in the central parsec, from the helium stars to the S stars.
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DOI: 10.1002/asna.200385108
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These observations include ground‐based adaptive optics images in the H, K' and L bands, HST‐NICMOS observations in filters between 1.1 and 2.2 μm, and spectroimaging data in the He I 2.06 μm line and the Brγ line. Analysis of all these data has made possible the resolution of the main component, IRS 13E, into a cluster of seven individual stars within a projected diameter of ∼0.5″ (0.02 pc), and to build their SED. The main sources, 13E1, 13E2, 13E3 (a binary), and 13E4, are hot stars of different nature. 13E2 and 13E4 are emission line stars. The spectral type of the various members goes from O5I to WR, including dusty WRs like IRS 21 (Tanner et al. 2002). All these sources have a common westward proper motion. Two weaker sources, 13E5 and 13E6, are also detected within the compact cluster, with 13E5 proposed as another dusty WR and 13E6 as a O5V star. An extended halo seen around the cluster, part of the mini‐spiral of dust is particularly enhanced in the L band. It is interpreted as a contribution of the scattered light from the inner cluster and the thermal emission from the dust. IRS 13E is proposed to be the remaining core of a massive, young star cluster which was disrupted in the vicinity of Sgr A*, and hence, the possible source of the young stars in the central parsec, from the helium stars to the S stars.</div></front></TEI><affiliations><list><country><li>France</li><li>États-Unis</li></country><region><li>Île-de-France</li></region><settlement><li>Paris</li></settlement></list><tree><country name="France"><region name="Île-de-France"><name sortKey="Maillard, Jean Ierre" sort="Maillard, Jean Ierre" uniqKey="Maillard J" first="Jean-Pierre" last="Maillard">Jean-Pierre Maillard</name></region><name sortKey="Paumard, Thibaut" sort="Paumard, Thibaut" uniqKey="Paumard T" first="Thibaut" last="Paumard">Thibaut Paumard</name></country><country name="États-Unis"><noRegion><name sortKey="Stolovy, Susan" sort="Stolovy, Susan" uniqKey="Stolovy S" first="Susan" last="Stolovy">Susan Stolovy</name></noRegion><name sortKey="Rigaut, Francois" sort="Rigaut, Francois" uniqKey="Rigaut F" first="François" last="Rigaut">François Rigaut</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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