Two extremely luminous WN stars in the Galactic center with circumstellar emission from dust and gas

  title={Two extremely luminous WN stars in the Galactic center with circumstellar emission from dust and gas},
  author={Andreas Barniske and Lidia M Oskinova and W. R. Hamann},
  journal={Astronomy and Astrophysics},
Context. The central region of our Galaxy contains a large population of young massive stars. These stars are concentrated in three large star clusters, as well as being scattered in the field. Strong ionizing radiation and stellar winds of massive stars are the essential feedback agents that determine the physics of the ISM in the Galactic center. Aims. The aim is to study relatively isolated massive WN-type stars in the Galactic center in order to explore their properties and their influence… 

2MASS and WISE data analysis of Galactic Wolf-Rayet stars

We collected almost all Galactic Wolf-Rayet (hereafter WR) stars found so far from the literature. 578 WR stars are gathered in this paper. 2MASS counterparts with good quality magnitudes in all JHK

Wolf-Rayet stars in the Small Magellanic Cloud: I. Analysis of the single WN stars

Wolf-Rayet (WR) stars have a severe impact on their environments owing to their strong ionizing radiation fields and powerful stellar winds. Since these winds are considered to be driven by radiation

The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class

Context. Massive stars, although being important building blocks of galaxies, are still not fully understood. This especially holds true for Wolf-Rayet (WR) stars with their strong mass loss, whose

The Wolf-Rayet stars in M 31. I. Analysis of the late-type WN stars

Context. Comprehensive studies of Wolf-Rayet stars were performed in the past for the Galactic and the LMC population. The results revealed significant differences, but also unexpected similarities

Near- and Mid-Infrared colors of evolved stars in the Galactic plane. The Q1 and Q2 parameters.

Context. Mass-loss from evolved stars chemically enriches the interstellar medium (ISM). Stellar winds from massive stars and their explosions as supernovae shape the ISM and trigger star formation.

One of the most massive stars in the Galaxy may have formed in isolation

Very massive stars, 100 times heavier than the sun, are rare. It is not yet known whether such stars can form in isolation or only in star clusters. The answer to this question is of fundamental

On the Apparent Absence of Wolf–Rayet+Neutron Star Systems: The Curious Case of WR124

Among the different types of massive stars in advanced evolutionary stages is the enigmatic WN8h type. There are only a few Wolf–Rayet (WR) stars with this spectral type in our Galaxy. It has long

Discovery of two Galactic Wolf–Rayet stars in Circinus

I report the discovery of two new Galactic Wolf-Rayet stars in Circinus via detection of their C, N and He near-infrared emission lines, using ESO-NTT-SOFI archival data. The H- and K-band spectra of

Analysis of the WN star WR 102c, its WR nebula, and the associated cluster of massive stars in the Sickle Nebula

The massive Wolf-Rayet type star WR 102c is located near the Quintuplet Cluster - one of the three massive star clusters in the Galactic Center region. Previous studies indicated that WR 102c may

The Quintuplet cluster - II. Analysis of the WN stars

Based on K-band integral-field spectroscopy, we analyze four Wolf-Rayet stars of the nitrogen sequence (WN) found in the inner part of the Quintuplet cluster. All WN stars (WR 102d, WR 102i, WR



An extraordinary cluster of massive stars near the centre of the Milky Way

The relative numbers of newborn stars of different masses in a galaxy (the initial mass function) determines whether the galaxy's interstellar gas goes mainly into long-lived low-mass stars, as in

Searching for hidden Wolf–Rayet stars in the Galactic plane – 15 new Wolf–Rayet stars

We report the discovery of 15 previously unknown Wolf–Rayet (WR) stars found as part of an infrared (IR) broad-band study of candidate WR stars in the Galaxy. We have derived an empirically based

Massive Stars in the Quintuplet Cluster

We present near-infrared photometry and K-band spectra of newly identified massive stars in the Quintuplet cluster, one of the three massive clusters projected within 50 pc of the Galactic center. We

Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. I. The Role of ISM Pressure and the Molecular Cloud Dissipation Timescale

In this paper, we combine the stellar spectral synthesis code STARBURST99, the nebular modeling code MAPPINGS IIIq, a one-dimensional dynamical evolution model of H II regions around massive clusters

Stellar evolution with rotation X: Wolf-Rayet star populations at solar metallicity

We examine the properties of Wolf-Rayet (WR) stars predicted by models of rotating stars taking account of the new mass loss rates for O-type stars and WR stars (Vink et al. 2000. 2001; Nugis &

Detection of additional Wolf-Rayet stars in the starburst cluster Westerlund 1 with SOAR

Context. The young starburst cluster Westerlund 1 is one of the most massive clusters in the Local Group, harboring a huge population of massive stars. Aims. We searched for additional Wolf-Rayet

Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit

The mass loss from Wolf-Rayet (WR) stars is of fundamental importance for the final fate of massive stars and their chemical yields. Its Z-dependence is discussed in relation to the formation of

Hubble Space Telescope/NICMOS Observations of Massive Stellar Clusters near the Galactic Center

We report Hubble Space Telescope (HST) Near-Infrared Camera and Multiobject Spectrometer (NICMOS) observations of the Arches and Quintuplet clusters, two extraordinary young clusters near the

Massive Stars and the Energy Balance of the Interstellar Medium. I. The Impact of an Isolated 60 M☉ Star

We present results of numerical simulations carried out with a two-dimensional radiation hydrodynamics code in order to study the impact of massive stars on their surrounding interstellar medium.

Stellar Evolution with Rotation

The existing grids of star models without rotation allow us to already explain a number of properties of massive and WR stars (cf. Maeder and Conti,1994). In particular, the sequences of star