The OB associations LH 101 and LH 104 
 in the HII region N158 of the LMC

Testor, G.; Niemelä, Virpi Sinikka

doi:10.1051/aas:1998241

Cited by 34 publications

(59 citation statements)

References 22 publications

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“…Notes. Sources of classifications: SOI (Stock et al 1976); M85 (Melnick 1985); C86 (Conti et al 1986); F88 (Fitzpatrick 1988); F91 (Fitzpatrick 1991); M95 (Massey et al 1995); O96b (Oey 1996b); WB97 (Walborn & Blades 1997); TN98 (Testor & Niemela 1998); M00 (Massey et al 2000); J01 (Jaxon et al 2001); W02 (Walborn et al 2002a); W02b (Walborn et al 2002b); W04 (Walborn et al 2004); M05 (Massey et al 2005); F09 (Fariña et al 2009); E10 ); W10 ); M12 ); M14 (Muraveva et al 2014, which were earlier classifications of the AAOmega spectra by CJE); W14 (Walborn et al 2014). …”

Section: Discussionmentioning

confidence: 99%

2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds

Evans

Loon

Hainich

et al. 2015

A&A

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We present spectral classifications from optical spectroscopy of 263 massive stars in the north-eastern region of the Large Magellanic Cloud. The observed two-degree field includes the massive 30 Doradus star-forming region, the environs of SN1987A, and a number of star-forming complexes to the south of 30 Dor. These are the first classifications for the majority (203) of the stars and include eleven double-lined spectroscopic binaries. The sample also includes the first examples of early OC-type spectra (AAΩ 30 Dor 248 and 280), distinguished by the weakness of their nitrogen spectra and by C IV λ4658 emission. We propose that these stars have relatively unprocessed CNO abundances compared to morphologically normal O-type stars, indicative of an earlier evolutionary phase. From analysis of observations obtained on two consecutive nights, we present radial-velocity estimates for 233 stars, finding one apparent single-lined binary and nine (>3σ) outliers compared to the systemic velocity; the latter objects could be runaway stars or large-amplitude binary systems and further spectroscopy is required to investigate their nature.

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Section: Discussionmentioning

confidence: 99%

2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds

Evans

Loon

Hainich

et al. 2015

A&A

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“…The northern part of N 158 comprises a superbubble around the OB association LH 104. Testor & Niemela (1998) have constructed H-R diagrams for the upper main-sequence of the two associations LH 101 and LH 104. These observations are consistent with the 2 objects having stellar populations of 2-6 Myr and ≤2 Myr respectively.…”

Section: General Metallicitymentioning

confidence: 99%

The present-day chemical composition of the LMC

Rolleston

Trundle

Dufton

2002

A&A

121

113

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Abstract. High-resolution observations of five OB-type main-sequence stars in the Large Magellanic Cloud (LMC) have been obtained with the UCLéchelle spectrograph on the 3.9-m Anglo-Australian Telescope. These spectra have been analysed using LTE model-atmosphere techniques, to derive stellar atmospheric parameters and chemical compositions. As these stars are located within the hydrogen burning main-sequence band, their surface abundances should reflect those of the present-day interstellar medium. Detailed line-by-line differential analyses have been undertaken relative to Galactic comparison stars. We conclude that there exists a general metal deficiency of −0.31 ± 0.04 dex within the LMC, and find no significant abundance variations between cluster and field stars. There is also tentative evidence to suggest a lower oxygen to iron abundance ratio, and an over-deficiency of magnesium relative to the other α-elements. These are discussed in terms of previous abundance analyses and models of discontinuous (or bursting) star formation within the LMC. Finally, there is some evidence to suggest a greater chemical enrichment of material within the H  region LH 104.

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“…For example, the two top mass bins, absent in Testor & Niemela (1998), contain a single star each (a Wolf-Rayet star and an O8 I((f)) star to which these authors assign 40 M , while we assign 66 M ). For lower masses our counts reveal a steeper PDMF, probably an effect of our better observational material (0.…”

Section: Gauging the Methods With Previous Workmentioning

confidence: 99%

“…Testor & Niemela (1998) report the PDMF as the IMF despite the fact that they find a complex star-formation history: "LH 104 consists mainly of a young population spreading out between 2 and 6 Myr ( Table 4). The HR diagrams also show ... a group of older and less massive stars."…”

Section: Gauging the Methods With Previous Workmentioning

confidence: 99%

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The IMF of the field population of 30 Doradus

Selman¹,

Melnick²

2005

A&A

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The star-formation history and IMF of the field population of the 30 Doradus super-association is determined using Wide Field Imager photometry. The cluster NGC 2070 and the OB association LH104 are also studied and used for comparison. The star-formation history of the 30 Doradus super-association appears to be characterized by a large increase in star-formation activity 10 Myr to 20 Myr ago. This seems to be the case across the whole eastern half of the LMC as demonstrated by the ages of stellar populations as far away as 30 Doradus and Shapley's Constellation III. Star-formation appears to be occurring at a constant rate in the field and in loose associations, and in bursts in the clusters. The field IMF is found to have almost the exact Salpeter slope in the range 7 M ≤ M ≤ 40 M , at odds with previous claims. We find that, for objects with more complex star-formation histories, Be stars and selective incompleteness strongly affect the determination of the IMF for M > 40 M , naturally explaining the observed deviation of the high mass IMF slope from the Salpeter value. The present work supports the idea of a universal IMF.

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The OB associations LH 101 and LH 104 in the HII region N158 of the LMC

Cited by 34 publications

References 22 publications

2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds

2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds

The present-day chemical composition of the LMC

The IMF of the field population of 30 Doradus

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