Adaptive optics $\vec{L}$-band observations   of the Galactic Center region

Clénet, Y.; Rouan, D.; Gendron, É.; Montri, J.; Rigaut, François; Léna, Pierre; Lacombe, F.

doi:10.1051/0004-6361:20010931

Cited by 39 publications

(63 citation statements)

References 43 publications

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“…Infrared Spectra of the IRS 13 and IRS 13N complexes.-The flux density originating in the IRS 13N region is dominated by the cluster of newly found compact sources. In previously published images of this region (e.g., Eckart et al 1995;Stolovy et al 1999;Paumard et al 2001;Clénet et al 2001;Maillard et al 2003), these were either not detected or not spatially resolved. From the NAOS/CONICA L-band images we estimate that only a maximum amount of 1 4 of the emission may be attributed to a more extended interstellar component.…”

Section: A Cluster Of Young Starsmentioning

confidence: 80%

“…The detailed comparison of the images shows that with the exception of the sources and , the IRS 13N objects are very red (Fig. 3) compared to other sources in the field (see KÀL colors given by Clénet et al 2001). The objects and could not be identified in the H-band image, resulting in lower limits for their HÀK colors.…”

Section: The New Ir-excess Sourcesmentioning

confidence: 94%

“…are listed in Table 2. For the flux calibration we used several reference sources taken from the lists of Blum, Sellgren, & Depoy (1996), Ott et al (1999), and Clénet et al (2001). Since in H-and K s bands several of the bright reference sources were saturated in the AO exposures, we used several weaker secondary reference stars identified in high-resolution SHARP H-and K-band images (Eckart et al 1995;Ott et al 1999).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Initially, Gezari et al (1985) suggested that IRS 21 is an externally heated, high-density dust clump. Given the mid-infrared (MIR) excess and the featureless near-infrared (NIR) spectra, several other classifications have been proposed, including an embedded early-type star and a protostar (Krabbe et al 1995;Genzel et al 1996;Clénet et al 2001). Tanner et al (2002) suggest that IRS 21 is an optically thick dust shell surrounding a mass-losing source, such as a dusty WC9 Wolf-Rayet star.…”

Section: Introductionmentioning

confidence: 99%

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Young Stars at the Center of the Milky Way?

Eckart

Moultaka

Viehmann

et al. 2004

ApJ

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We present results from the first diffraction-limited images of the Galactic center (GC) at 1.6, 2.1, and 3.8 m with the new adaptive optics (AO) camera NAOS/CONICA at the ESO Very Large Telescope, as well as 3-4 m low-resolution spectroscopy. We have discovered a small (0.13 lt-yr diameter) cluster of compact sources about 0B5 north of IRS 13 with strong IR excesses due to T > 500 K dust. The nature of the sources is unclear. They may be a cluster of highly extincted stars that heat the local environment of the minispiral. We also consider an explanation that involves the presence of young stars at evolutionary stages between young stellar objects and Herbig Ae/Be objects with ages of about 0.1 to 1 million yr. This scenario would imply more recent star formation in the GC than previously suspected. The AO observations also resolve the central IRS 13 complex. In addition to the previously known bright stars E1 and E2, the K-and L 0 -band images for the first time resolve object E3 into two components, E3N and E3c. The latter one is closest to the 7 mm Very Large Array radio continuum source found at the location of the IRS 13 complex. E3c may be associated with a strong stellar wind or a dusty Wolf-Rayet-like star at that location.

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Section: A Cluster Of Young Starsmentioning

confidence: 80%

Section: The New Ir-excess Sourcesmentioning

confidence: 94%

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Young Stars at the Center of the Milky Way?

Eckart

Moultaka

Viehmann

et al. 2004

ApJ

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“…Recently, it has been shown that the center of the Milky Way is inhabited by a SMBH of ∼ 3.6 × 10 6 M (Schödel et al 2002;Ghez et al 2003). The entire central parsec is powered by a cluster of young and massive stars as the IRS 16 complex (Blum et al 1988, Krabbe et al 1995, Genzel et al 1996, Eckart et al 1999, Clénet et al 2001. In addition to the massive supergiants, a population of dust embedded objects associated with dust emission are also found in the Galactic Center stellar cluster as IRS 1, IRS 3 and also the IRS 21 and IRS 8 sources that have been identified as bowshock sources (Tanner et al 2002, Rigaut et al 2003.…”

Section: Introductionmentioning

confidence: 99%

IR excess stars and shock filaments at the Galactic center

Moultaka¹,

Eckart²,

Viehmann³

et al. 2004

Proc. IAU

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Abstract. In this paper we report on our recent results connected with the direct environment of the super massive black hole of the Milky Way. The data are obtained using the VLT facilities (ISAAC and NAOS/CONICA instruments) in the near-and mid-infrared wavelength ranges. We provide a calibration of the foreground and local differential (in wavelength and spatially) extinction of the Galactic Center and report on the discovery of a new complex of infrared excess sources (possibly young stars) located at the northern part of the IRS 13 cluster. Finally, we discuss the origin of filamentary structures observed in the L-band images.

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The Galactic Center Source IRS 13E: a Star Cluster

Maillard

Paumard

Stolovy

et al. 2003

Proceedings of the Galactic Center Workshop 2002

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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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Adaptive optics $\vec{L}$-band observations of the Galactic Center region

Cited by 39 publications

References 43 publications

Young Stars at the Center of the Milky Way?

Young Stars at the Center of the Milky Way?

IR excess stars and shock filaments at the Galactic center

The Galactic Center Source IRS 13E: a Star Cluster

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