Initial conditions in the evolution of OB and Wolf-Rayet stars in N 105 of the LMC

Ambrocio-Cruz, P.; Laval, A.; Marcelin, M.; Amram, P.; Comerón, F.

doi:10.1017/s0074180900206025

Cited by 6 publications

(12 citation statements)

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“…15 (top) shows the 8 μm IRAC / Spitzer image of N 105A, dominated by hot dust and PAH emission, with the positions of N 105A IRS1 (Epchtein et al 1984; this work), water and OH maser (Brooks & Whiteoak 1997; Lazendic et al 2002) and methanol maser (Sinclair et al 1992) indicated. Although projection effects may affect our view, the morphology of N 105A shows little evidence for massive star feedback; no shell structure is seen in [O iii ] images (Ambrocio‐Cruz et al 1998), in spite of the proximity of the OB association LH 31, identified near the molecular cloud (Dopita et al 1994). Furthermore, there seems to be no link between the water and OH maser source (Brooks & Whiteoak 1997; Lazendic et al 2002) and the protostar location and any external trigger.…”

Section: Discussionmentioning

confidence: 88%

“…Several young clusters are associated with N 113 (Bica, Claria & Dottori 1992), and current star formation activity is occurring within continuum sources in the central area of the nebula (Brooks & Whiteoak 1997; Wong et al 2006). The H ii region N 105 (Henize 1956) is a complex of evacuated bubbles and dense molecular material with several young clusters associated with it (Ambrocio‐Cruz et al 1998); current star formation as indicated by maser activity seems to concentrate in the denser central part of the region, N 105A. N 160A is the brightest component in the N 160 H ii complex (Henize 1956).…”

Section: Introductionmentioning

confidence: 99%

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Massive young stellar objects in the Large Magellanic Cloud: water masers and ESO-VLT 3-4 m spectroscopy

Oliveira

Loon

Stanimirović

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We investigate the conditions of star formation in the Large Magellanic Cloud (LMC). We have conducted a survey for water maser emission arising from massive young stellar objects in the 30 Doradus region (N 157) and several other H ii regions in the LMC (N 105A, N 113 and N 160A). We have identified a new maser source in 30 Dor at the systemic velocity of the LMC. We have obtained 3–4 μm spectra, with the European Southern Observatory (ESO)‐Very Large Telescope (VLT), of two candidate young stellar objects. N 105A IRS1 shows H recombination line emission, and its Spectral Energy Distribution (SED) and mid‐infrared colours are consistent with a massive young star ionizing the molecular cloud. N 157B IRS1 is identified as an embedded young object, based on its SED and a tentative detection of water ice. The data on these four H ii regions are combined with mid‐infrared archival images from the Spitzer Space Telescope to study the location and nature of the embedded massive young stellar objects and signatures of stellar feedback. Our analysis of 30 Dor, N 113 and N 160A confirms the picture that the feedback from the massive O‐ and B‐type stars, which creates the H ii regions, also triggers further star formation on the interfaces of the ionized gas and the surrounding molecular cloud. Although in the dense cloud N 105A star formation seems to occur without evidence of massive star feedback, the general conditions in the LMC seem favourable for sequential star formation as a result of feedback. In an , we present water maser observations of the galactic red giants R Doradus and W Hydrae.

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Section: Discussionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Massive young stellar objects in the Large Magellanic Cloud: water masers and ESO-VLT 3-4 m spectroscopy

Oliveira

Loon

Stanimirović

et al. 2006

Monthly Notices of the Royal Astronomical Society

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“…They estimate the turn-off mass of these massive stars to be ∼65 M , but note that there are some evolved stars with masses ∼15−40 M , indicating either ongoing or somewhat episodic star formation. The densest central region, N105A, shows limited evidence for massive star feedback; no shell structure is seen in Oiii images (Ambrocio-Cruz et al 1998), in spite of its proximity to LH 31. Star formation is ongoing deep in its core with a massive spectroscopic YSO identified by Epchtein et al (1984) and Oliveira et al (2006) and several maser sources (water, OH, and methanol, Sinclair et al 1992;Lazendic et al 2002;Oliveira et al 2006;Green et al 2008;Ellingsen et al 2010).…”

Section: N105mentioning

confidence: 95%

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Carlson

Sewiło

Meixner

et al. 2012

A&A

110

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We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine Hii regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, AJ, 132, 2268, combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997, AJ, 114, 1002 and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, PASJ, 59, 615). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007, ApJS, 169, 328) and estimate mass functions and SFRs for each region.

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“…Henize (1956) has cataloged Hα-emitting nebulae in the Magellanic Clouds, and this region is very abundant in such nebulae, which are primarily H II regions, wind-driven shells, supernova remnants, etc., or complexes of different types (e.g. Laval et al 1992;Ambrocio-Cruz et al 1998; see also Carlson et al 2012). Some of these nebulae are associated with the abovementioned stellar groups, e.g.…”

Section: Spatial Distributionsmentioning

confidence: 99%

The VMC Survey. XXVII. Young Stellar Structures in the LMC’s Bar Star-forming Complex

Sun

Grijs

Subramanian³

et al. 2017

ApJ

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Star formation is a hierarchical process, forming young stellar structures of star clusters, associations, and complexes over a wide scale range. The star-forming complex in the bar region of the Large Magellanic Cloud is investigated with upper main-sequence stars observed by the VISTA Survey of the Magellanic Clouds. The upper main-sequence stars exhibit highly non-uniform distributions. Young stellar structures inside the complex are identified from the stellar density map as density enhancements of different significance levels. We find that these structures are hierarchically organized such that larger, lower-density structures contain one or several smaller, higher-density ones. They follow power-law size and mass distributions as well as a lognormal surface density distribution. All these results support a scenario of hierarchical star formation regulated by turbulence. The temporal evolution of young stellar structures is explored by using subsamples of upper main-sequence stars with different magnitude and age ranges. While the youngest subsample, with a median age of log(τ /yr) = 7.2, contains most substructure, progressively older ones are less and less substructured. The oldest subsample, with a median age of log(τ /yr) = 8.0, is almost indistinguishable from a uniform distribution on spatial scales of 30-300 pc, suggesting that the young stellar structures are completely dispersed on a timescale of ∼100 Myr. These results are consistent with the characteristics of the 30 Doradus complex and the entire Large Magellanic Cloud, suggesting no significant environmental effects. We further point out that the fractal dimension may be method-dependent for stellar samples with significant age spreads.

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Initial conditions in the evolution of OB and Wolf-Rayet stars in N 105 of the LMC

Cited by 6 publications

References 0 publications

Massive young stellar objects in the Large Magellanic Cloud: water masers and ESO-VLT 3-4 m spectroscopy

Massive young stellar objects in the Large Magellanic Cloud: water masers and ESO-VLT 3-4 m spectroscopy

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

The VMC Survey. XXVII. Young Stellar Structures in the LMC’s Bar Star-forming Complex

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