Object 17: Another cluster of emission-line stars near the galactic center

Abstract.We use the data published in Paper I and Curran et al. (2000) to determine the global molecular gas luminosities and distributions in a sample of 22 Seyfert galaxies. From this we find definite differences in the CO to HCN luminosity ratios between the near-by and distant galaxies of the sample. This is perhaps due to a selection effect where we only observe the brightest of the distant sources. With regard to distributions, we find in the near-by (mapped) sample that the CO is usually much wider distributed than the central telescope beam and that the HCN is considerably more extended beyond the ∼1 kpc often cited in the literature. In fact this molecule has been detected as far as ≈5 kpc from the centre of NGC 1365. We may also have detected a bar in HCN in NGC 5033. Also, using the data to complement the results of.e. no difference in the molecular gas luminosities between the two main Seyfert classes. In fact we consider it more meaningful to discuss the differences between the near-by and distant sample (irrespective of Seyfert type), although both of these samples may show evidence that much of the far infrared luminosity could arise from an active galactic nucleus as opposed to being predominantly due to vigorous star formation. We do believe, however, that improved statistics would be of little value in distinguishing between these two scenarios and that future high resolution observations are the key to resolving this issue.

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“…Kormendy & Richstone 1995), young stars are observed very close to this (e.g. Okuda et al 1990;Nagata et al 1990Nagata et al , 1995.…”

Section: Fig 22 Detail Ofmentioning

confidence: 79%

Global molecular gas properties of Seyfert galaxies

Curran

Polatidis

Aalto

et al. 2001

A&A

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“…A census of WR stars in the region covered by our images (but outside the Galactic center) shows that there are ∼35 known WRs in the Arches cluster (Nagata et al 1995;Cotera et al 1996;Blum et al 2001;Figer et al 2002), 10 in the Quintuplet cluster (Figer et al 1999), and at least 2 apparently isolated WR stars near Sgr A (Cotera et al 1999), for a total of 47. Most of these are brighter than K = 12, which was the limit considered in the estimate.…”

Section: Wrs In the Inner Galaxymentioning

confidence: 90%

Results from a near infrared search for emission-line stars in the Inner Galaxy: Spectra of new Wolf-Rayet stars

Homeier

Blum

Pasquali

et al. 2003

A&A

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Abstract. We present follow-up spectroscopy of emission line candidates detected on near-infrared narrow band images in the inner Galaxy (Homeier et al. 2003). The filters are optimized for the detection of Wolf-Rayet stars and other objects which exhibit emission-lines in the 2 µm region. Approximately three square degrees along the Galactic plane have been analyzed in seven narrow-filters (four emission-lines and three continuum). We have discovered 4 new Wolf-Rayet stars and present coordinates, finding charts, and K-band spectra.

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“…Both clusters have been studied extensively with near-infrared imaging and spectroscopy (e.g. Nagata et al 1995;Cotera et al 1996;Figer et al 1999;Stolte et al 2005;Espinoza et al 2009). However, many of the cluster properties derived from these works have been limited by lack of membership information.…”

Section: The Arches and Quintuplet Clustersmentioning

confidence: 99%

Young stars in the Galactic center

Lu¹,

Ghez

Morris

et al. 2013

Proc. IAU

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Abstract. The central parsec of our Galaxy hosts not only a supermassive black hole, but also a large population of young stars (age <6 Myr) whose presence is puzzling given how inhospitable the region is for star formation. The strong tidal forces require gas densities many orders of magnitude higher than is found in typical molecular clouds. Kinematic observations of this young nuclear cluster show complex structures, including a well-defined inner disk, but also a substantial off-disk population. Spectroscopic and photometric measurements indicate the initial mass function (IMF) differs significantly from the canonical IMF found in the solar neighborhood. These observations have led to a number of proposed star formation scenarios, such as an infalling massive star cluster, a single infalling molecular cloud, or cloud-cloud collisions. I will review recent works on the young stars in the central parsec and discuss connections with young nuclear star clusters in other galaxies, such as M31, and with star formation in the larger central molecular zone.

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Object 17: Another cluster of emission-line stars near the galactic center

Cited by 138 publications

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Global molecular gas properties of Seyfert galaxies

Global molecular gas properties of Seyfert galaxies

Results from a near infrared search for emission-line stars in the Inner Galaxy: Spectra of new Wolf-Rayet stars

Young stars in the Galactic center

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