Understanding the Star Formation Process in the Filamentary Dark Cloud GF 9: Near-Infrared Observations

1998 ◽  
Vol 116 (1) ◽  
pp. 349-359 ◽  
Author(s):  
David R. Ciardi ◽  
Charles E. Woodward ◽  
Dan P. Clemens ◽  
David E. Harker ◽  
Richard J. Rudy
Keyword(s):  
Star Formation ◽  
Formation Process ◽  
Near Infrared ◽  
Dark Cloud ◽  
Infrared Observations

Near-Infrared Observations of Circumnuclear Star Formation in NGC 3351, NGC 3504, and NGC 5248

1997 ◽  
Vol 114 ◽  
pp. 1850 ◽  
Author(s):  
Debra Meloy Elmegreen ◽  
Frederick R. Chromey ◽  
Michael Santos ◽  
Daniel Marshall
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Infrared Observations

scholarly journals Masers and the massive star formation process: New insights through infrared observations

2005 ◽  
Vol 1 (S227) ◽  
pp. 180-185 ◽  
Author(s):  
James M. De Buizer ◽  
James T. Radomski ◽  
Charles M. Telesco ◽  
Robert K. Piña
Keyword(s):  
Star Formation ◽  
Formation Process ◽  
Massive Star ◽  
Massive Star Formation ◽  
Infrared Observations

scholarly journals Luminosity function, star density, and star formation efficiency in regions of star formation - near infrared observations -

1991 ◽  
Vol 147 ◽  
pp. 289-292
Author(s):  
Klaus-Werner Hodapp ◽  
John Rayner ◽  
Hua Chen
Keyword(s):  
Star Formation ◽  
Luminosity Function ◽  
Near Infrared ◽  
Hii Regions ◽  
Young Stars ◽  
Young Age ◽  
Infrared Observations ◽  
Star Density ◽  
Many Sources ◽  
Formation Efficiency

Clusters of young stars have been found near a number of compact HII regions. These clusters do not show a turnover in the K-band luminosity and are probably several million years old. In L 1641 only moderate clustering tendency has been observed and many sources show signs of extremely young age.

scholarly journals Relative CNO Abundances in Upper AGB Stars of the Magellanic Clouds. A Search for Envelope Burning

1989 ◽  
Vol 106 ◽  
pp. 152-152
Author(s):  
J.M. Brett ◽  
M.S. Bessell
Keyword(s):  
Star Formation ◽  
Temperature Dependence ◽  
Near Infrared ◽  
Small Sample ◽  
Magellanic Clouds ◽  
Agb Stars ◽  
Infrared Observations ◽  
Burning Process ◽  
Synthetic Spectra ◽  
Cno Abundances

We have investigated the atmospheric abundances of upper AGB stars of the SMC, searching in particular for evidence of the hypothetical envelope burning process. To this end we have computed synthetic spectra with varying C, N, and 0 abundances selected by considering the effect of the processes of the 3rd dredge up and envelope burning of a degree sufficient to prevent C star formation. The synthetic spectra (covering 0.5 μm to 2.5 μm) were analysed for observable effects of these two atmospheric enrichment processes. By analysis of band strengths of TiO, CO and CN we have found that substantial envelope burning is detectable for stars with Teff ≥ 3000 K but not below, due to the temperature dependence of CN bands. The synthetic spectra were compared to near-infrared and infrared observations of a small sample of SMC upper AGB stars thought to be prime candidates for the occurrence of envelope burning. This comparison indicated that envelope burning, of the extent considered here, is not occurring in these stars but rather the spectra are consistent with mild C enhancements produced by the 3rd dredge up alone.

Near?Infrared Observations of N11 in the Large Magellanic Cloud: Triggered Star Formation around the Periphery of LH 9

2006 ◽  
Vol 132 (6) ◽  
pp. 2653-2664 ◽  
Author(s):  
Hirofumi Hatano ◽  
Ryota Kadowaki ◽  
Yasushi Nakajima ◽  
Motohide Tamura ◽  
Tetsuya Nagata ◽  
...  
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Infrared Observations

scholarly journals A survey of molecular cores in M 17 SWex

2019 ◽  
Author(s):  
Tomomi Shimoikura ◽  
Kazuhito Dobashi ◽  
Asha Hirose ◽  
Fumitaka Nakamura ◽  
Yoshito Shimajiri ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Star Formation ◽  
Massive Star ◽  
Near Infrared ◽  
Young Stellar Objects ◽  
High Mass ◽  
Physical Parameters ◽  
Massive Star Formation ◽  
Dark Cloud ◽  
The Magnetic Field

Abstract A survey of molecular cores covering the infrared dark cloud known as the M 17 southwest extension (M 17 SWex) has been carried out with the 45 m Nobeyama Radio Telescope. Based on the N2H+ (J = 1–0) data obtained, we have identified 46 individual cores whose masses are in the range from 43 to $3026\, {M}_{\odot }$. We examined the relationship between the physical parameters of the cores and those of young stellar objects (YSOs) associated with the cores found in the literature. The comparison of the virial mass and the core mass indicates that most of the cores can be gravitationally stable if we assume a large external pressure. Among the 46 cores, we found four massive cores with YSOs. They have large masses of $\gtrsim 1000\, M_{\odot }$ and line widths of $\gtrsim 2.5\:$km s−1 which are similar to those of clumps forming high-mass stars. However, previous studies have shown that there is no active massive star formation in this region. Recent measurements of near-infrared polarization imply that the magnetic field around M 17 SWex is likely to be strong enough to support the cores against self-gravity. We therefore suggest that the magnetic field may prevent the cores from collapsing, causing the low level of massive star formation in M 17 SWex.

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