scholarly journals Observing the influence of the youngest super star clusters in NGC 1569: Keck Brackett α spectroscopy

2021 ◽  
Vol 503 (2) ◽  
pp. 2187-2194
Author(s):  
Daniel P Cohen ◽  
Jean L Turner ◽  
Sara C Beck ◽  
S Michelle Consiglio
Keyword(s):  
Near Infrared ◽  
Star Clusters ◽  
Radio Continuum ◽  
H Ii Regions ◽  
Infrared Source ◽  
H Ii Region ◽  
Super Star Clusters ◽  
Infrared Sources ◽  
Massive Clusters ◽  
Ngc 1569

ABSTRACT We report Keck–NIRSPEC observations of the Brackett α 4.05 μm recombination line across the two candidate embedded super star clusters (SSCs) in NGC 1569. These SSCs power a bright H ii region and have been previously detected as radio and mid-infrared sources. Supplemented with high-resolution VLA mapping of the radio continuum along with IRTF–TEXES spectroscopy of the [S iv] 10.5 μm line, the Brackett α data provide new insight into the dynamical state of gas ionized by these forming massive clusters. Near-infrared sources detected in 2 μm images from the slit-viewing Camera are matched with Gaia sources to obtain accurate celestial coordinates and slit positions to within ∼0${_{.}^{\prime\prime}}$1. Br α is detected as a strong emission peak powered by the less luminous infrared source, MIR1 (LIR ∼ 2 × 107 $\rm L_\odot$). The second candidate SSC MIR2 is more luminous (LIR ≳ 4 × 108 $\rm L_\odot$) but exhibits weak radio continuum and Br α emission, suggesting the ionized gas is extremely dense (ne ≳ 105 cm−3), corresponding to hypercompact H ii regions around newborn massive stars. The Br α and [S iv] lines across the region are both remarkably symmetric and extremely narrow, with observed line widths Δv ≃ 40 $\rm km\, s^{-1}$, full width at half-maximum. This result is the first clear evidence that feedback from NGC 1569’s youngest giant clusters is currently incapable of rapid gas dispersal, consistent with the emerging theoretical paradigm in the formation of giant star clusters.

scholarly journals Near-Infrared Sources in the Complex H II Region NGC 6357

1987 ◽  
Vol 115 ◽  
pp. 187-188
Author(s):  
P. Persi ◽  
M. Ferrari-Toniolo ◽  
M. Roth ◽  
M. Tapia
Keyword(s):  
Near Infrared ◽  
Baja California ◽  
Infrared Emission ◽  
Radio Continuum ◽  
Star Forming ◽  
H Ii Region ◽  
Infrared Sources ◽  
Near Infrared Emission ◽  
Water Maser

We have searched for the near-infrared emission from selected areas of the star forming region NGC 6357. Six fields of 90x90 arcsec2 centered on the far-IR peaks G353.19+0.91, G353.22+0.67, G353.13+0.64, G353.05+0.56, on the 6-cm radio continuum peak G353.035+0.78, and on the water maser source H20353.27+0.64, were scanned through the K(2.2 μm) filter at the 2.1-m telescope of the Observatorio Astronómico Nacional at S. Pedro Mártir, Baja California, México.

Hubble Space Telescope imaging of super-star clusters in NGC 1569 and NGC 1705

1994 ◽  
Vol 433 ◽  
pp. 65 ◽  
Author(s):  
Robert W. O'Connell ◽  
John S., III Gallagher ◽  
Deidre A. Hunter
Keyword(s):  
Hubble Space Telescope ◽  
Star Clusters ◽  
Space Telescope ◽  
Super Star Clusters ◽  
Ngc 1569

scholarly journals Kinematic Masses of Super Star Clusters in NGC 1569

2002 ◽  
Vol 207 ◽  
pp. 471-473
Author(s):  
Andrea M. Gilbert ◽  
James R. Graham
Keyword(s):  
High Resolution ◽  
Velocity Dispersion ◽  
Dwarf Galaxy ◽  
Star Clusters ◽  
Stellar Velocity ◽  
Super Star Clusters ◽  
Ngc 1569

We summarize recent results from our study of the massive young super star clusters (SSCs) in the dwarf galaxy NGC 1569, and present new high-resolution NIRSPEC spectra that permit the measurement of a cluster's intrinsic stellar velocity dispersion. Thus we derive kinematic masses for the two brightest SSCs: 2.3 × 105 Msun for SSC B, and 3.9 × 105 and 4.4 × 105 Msun for the two components of SSC A.

scholarly journals Radio observations of Galactic Center massive stars

2003 ◽  
Vol 212 ◽  
pp. 497-504
Author(s):  
Cornelia C. Lang
Keyword(s):  
Near Infrared ◽  
Galactic Center ◽  
Stellar Winds ◽  
Radio Sources ◽  
Stellar Clusters ◽  
X Ray ◽  
Spatial Properties ◽  
Gc Clusters ◽  
Infrared Sources ◽  
Massive Clusters

High-resolution multi-frequency observations made with the VLA have revealed the presence of stellar winds in two of the three known massive stellar clusters at the Galactic Center (GC). At a distance of only 8.0 kpc, we are able to resolve radio sources associated with individual near-infrared sources known to be losing mass at high rates. Herein, I discuss the spectral and spatial properties of the radio sources and their near-infrared counterparts, their inferred mass-loss rates, variability and the prospects for detecting stellar winds sources in the Central Cluster, near the supermassive blackhole SgrA*. Such massive clusters as these three GC clusters have a profound impact on the interstellar medium, as evidenced by radio and X-ray observations of the surrounding regions.

scholarly journals Super star clusters in the Galactic Center as revealed by HST-NICMOS

1999 ◽  
Vol 193 ◽  
pp. 459-469
Author(s):  
Donald F. Figer ◽  
Sungsoo S. Kim ◽  
Mark Morris ◽  
Eugene Serabyn
Keyword(s):  
Main Sequence ◽  
Local Group ◽  
Galactic Center ◽  
Formation Rate ◽  
Star Clusters ◽  
Initial Mass Function ◽  
Stellar Content ◽  
Multiple Star ◽  
Super Star Clusters ◽  
Massive Clusters

The three massive clusters in the Galactic Center are not only the most massive young clusters in the Galaxy, but they harbor more Wolf-Rayet stars than any other starburst region in the Local Group. An understanding of their stellar content will be valuable for extending models to starburst regions in other galaxies. We present HST-NICMOS images, luminosity functions, and color-magnitude diagrams of two of these: the Quintuplet and Arches clusters. The images allow the detection of stars over 6 magnitudes fainter than ever before and reveal previously undetected multiple star systems. For the first time, we clearly identify the main sequence in the Quintuplet cluster, and we extend earlier detections of the main sequence in the Arches cluster to Minitial < 10 M⊙. We estimate that the Arches cluster has an initial mass function slope which is greater than the Salpeter value. Given their stellar content, the Galactic Center clusters provide both the best nearby examples of super star clusters and the best nearby locale in which to investigate WR phenomena in starburst galaxies and galactic nuclei. We discuss the content of the Galactic Center clusters, with a particular emphasis on how they compare to other massive clusters of the local group. We expect that many of the massive stars in the Galactic Center will soon evolve to become WR stars, and eventually become supernovae at a rate of ∼ 1 per 20 000 years for the next several Myr. We note that our preliminary N-body simulations suggest that such dense clusters are short-lived in the strong tidal field of the Galactic Center, consistent with the fact that no older dense clusters are seen in the central 50 pc. This implies a star formation rate of 5(10−3) M⊙ yr−1 in the Galactic Center.

scholarly journals A search for radio supernovae and supernova remnants in the region of NGC 1569's super star clusters

2002 ◽  
Vol 381 (3) ◽  
pp. 825-833 ◽  
Author(s):  
A. Greve ◽  
A. Tarchi ◽  
S. Hüttemeister ◽  
R. de Grijs ◽  
J. M. van der Hulst ◽  
...  
Keyword(s):  
Supernova Remnants ◽  
Star Clusters ◽  
Supernovae And Supernova Remnants ◽  
Super Star Clusters ◽  
Ngc 1569

scholarly journals A multi-wavelength classification system for the evolution of star clusters

2015 ◽  
Vol 11 (S315) ◽  
pp. 142-145
Author(s):  
Bradley C. Whitmore ◽  
Crystal Brogan ◽  
Rupali Chandar ◽  
Aaron Evans ◽  
John Hibbard ◽  
...  
Keyword(s):  
Classification System ◽  
Near Infrared ◽  
Infrared Imaging ◽  
Cluster Formation ◽  
Star Clusters ◽  
Radio Continuum ◽  
Optical Observations ◽  
Small Scale ◽  
Molecular Gas ◽  
Multi Wavelength

AbstractThe availability of high spatial resolution molecular gas observations from ALMA, and similar resolution observations in the radio continuum using the VLA, is providing the opportunity to make comparisons with specific features seen in optical observations more directly than in the past. Using our ALMA observations of the Antennae galaxies as a springboard, we have compared the locations of small-scale CO (3−2) features with a variety of multi-wavelength observations, in particular optical and near-infrared imaging using both broad (UBVI) and narrow-band data (Hαand Paβ) taken with the HST, and radio (3.6 cm) continuum observations taken with the VLA. This comparison leads to the development of an evolutionary classification system which provides a framework for studying the sequence of star cluster formation and evolution, from diffuse Giant Molecular Clouds (GMCs), to proto, embedded, emerging, young, and intermediate/old star clusters. Using this evolutionary framework, we estimate the maximum age range of clusters formed in a single GMC is approximately 10 Myr. This suggests that the molecular gas is removed over this timescale, resulting in the cessation of star formation and the destruction of the GMC within a radius of about 200 pc.

scholarly journals Cluster formation induced by a cloud–cloud collision in [DBS2003]179

2020 ◽  
Author(s):  
Sho Kuwahara ◽  
Kazufumi Torii ◽  
Norikazu Mizuno ◽  
Shinji Fujita ◽  
Mikito Kohno ◽  
...  
Keyword(s):  
Near Infrared ◽  
Cluster Formation ◽  
Dust Emission ◽  
Star Clusters ◽  
High Ratio ◽  
Star Cluster ◽  
High Mass ◽  
Mass Star ◽  
The Galaxy ◽  
Super Star Clusters

Abstract [DBS2003]179 is a super star cluster in the Galaxy discovered in deep near-infrared observations. We carried out CO $J$ = 1–0 and $J$ = 3–2 observations of the region of [DBS2003]179 with NANTEN2, ASTE, and the Mopra 22 m telescope. We identified and mapped two molecular clouds that are likely to be associated with the cluster. This association is supported by the spatial correlation with the corresponding 8$\, \mu$m Spitzer image and by a high ratio of the two transitions of $^{12}$CO($J$ = 3–2 and $J$ = 1–0). The two clouds show complementary distributions in space, and bridging features connect them in velocity. We hypothesize that the two clouds collided with each other 1–2 Myr ago and that the collision compressed the interfacial layer, triggering the formation of the cluster. This offers an additional piece of evidence for a super star cluster formed by a cloud–cloud collision, alongside the four super star clusters Westerlund$\:2$, NGC 3603, RCW 38, and R 136. These findings indicate that the known super star clusters with closely associated dust emission were formed by cloud–cloud collisions, lending support to the important role of cloud–cloud collisions in high-mass star formation.

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