Observations of H2O maser emission in the Large Magellanic Cloud

Whiteoak, J. B.; Wellington, K. J.; Jauncey, D. L.; Gardner, F. F.; Forster, J. R.; Caswell, J. L.; Batchelor, R.

doi:10.1093/mnras/205.2.275

Cited by 29 publications

(29 citation statements)

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“…Three other H ii regions in the LMC, known to show water maser emission (N 113, N 105A and N 160A; Whiteoak et al 1983; Whiteoak & Gardner 1986) are also observed at 22 GHz, as well as most of the previous non‐detections for water maser emission in the LMC and Small Magellanic Cloud (SMC; Scalise & Braz 1982; Whiteoak et al 1983). Since our observations, Lazendic et al (2002) also reported 22 GHz water maser emission towards N 159.…”

Section: Introductionsupporting

confidence: 62%

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: Introductionsupporting

confidence: 62%

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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“…At least five distinct epochs of consecutive star formation have been identified in 30 Doradus (Walborn & Blades 1997), of which the youngest is still ongoing. The detection of water maser activity near R136 betrays the presence of recently formed stars (Whiteoak et al 1983;Van Loon & Zijlstra 2001).…”

Section: Lmc: 30 Doradusmentioning

confidence: 99%

The physical structure of Magellanic Cloud HII regions

Vermeij¹,

Damour²,

Hulst³

et al. 2002

A&A

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Abstract. We present infrared and optical spectroscopic data for 11 H  regions and one Supernova Remnant in the Large and Small Magellanic Cloud. The infrared data have been obtained with the Short Wavelength Spectrometer and Long Wavelength Spectrometer on board the Infrared Space Observatory as part of a Guaranteed Time Program on H  regions in Local Group Galaxies. Aim of this project is to give a new and improved analysis of the physical structure of the sample H  regions by combining as much spectral data as possible. A detailed account is given here of the reduction process, and the quality and reliability of the presented fluxes are discussed.

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“…These usually do not unambiguously identify YSOs, but can guide other searches. The LMC surveys are somewhat inconclusive, but several agree that there is maser emission associated with N160A and the SE edge of N105 (Scalise & Braz 1982;Whiteoak et al 1983;Ellingsen et al 1994). Epchtein et al (1984) identify IR counterparts to the N105 water and OH masers and one in N160A.…”

Section: Comparison With Known Ysosmentioning

confidence: 99%

SPITZERSAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS

Whitney¹,

Sewiło²,

Indebetouw³

et al. 2008

The Astronomical Journal

190

113

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We present ∼1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations. The YSOs are biased toward intermediate-to high-mass and young evolutionary stages, because these overlap less with galaxies and evolved stars in color-magnitude space. The YSOs are highly correlated spatially with atomic and molecular gas, and are preferentially located in the shells and bubbles created by massive stars inside. They are more clustered than generic point sources, as expected if star formation occurs in filamentary clouds or shells. We applied a more stringent color-magnitude selection to produce a subset of "high-probability" YSO candidates. We fitted the spectral-energy distributions (SEDs) of this subset and derived physical properties for those that were well fitted. The total mass of these well-fitted YSOs is ∼2900 M and the total luminosity is ∼2.1 × 10 6 L . By extrapolating the mass function with a standard initial mass function and integrating, we calculate a current star-formation rate of ∼0.06 M yr −1 , which is at the low end of estimates based on total ultraviolet and IR flux from the galaxy (∼0.05 − 0.25 M yr −1 ), consistent with the expectation that our current YSO list is incomplete. Follow-up spectroscopy and further data mining will better separate the different IR-bright populations and likely increase the estimated number of YSOs. The full YSO list is available as electronic tables, and the SEDs are available as an electronic figure for further use by the scientific community.

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Observations of H2O maser emission in the Large Magellanic Cloud

Cited by 29 publications

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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

The physical structure of Magellanic Cloud HII regions

SPITZERSAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS

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