Two compact H ii regions at the remote outskirts of the Magellanic Clouds

Selier, R.; Heydari-Malayeri, M.

doi:10.1051/0004-6361/201219706

Cited by 7 publications

(9 citation statements)

References 36 publications

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“…belongs to a small class of compact, HEBs in the MCs of which only five other examples are presently known in the SMC: N88A (Testor et al 2010), N81 (Heydari-Malayeri et al 1999), N66A (Heydari-Malayeri & Selier 2010, N33 (Selier et al 2011), and N77A (Selier & Heydari-Malayeri 2012). This region has the particularity of being one of the most compact members of this class.…”

Section: Discussionmentioning

confidence: 99%

Optical and infrared observations of the young SMC blob N26 and its environment

Testor¹,

Heydari-Malayeri²,

Chen³

et al. 2014

A&A

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Context. High-excitation compact H  regions of the Magellanic Clouds are sites of recent massive star formation in low metallicity environments. Aims. Detailed study of these regions and their environments using high-spatial resolution observations is necessary to better understand massive star formation, which is still an unsolved problem. We aim at a detailed study of the Small Magellanic Cloud compact H  region N26, which is only ∼4 in diameter.Methods. This study is based on high spatial resolution imaging (∼0. 1-0. 3) in JHKs and L bands, using the VLT equipped with the NAOS adaptive optics system. A larger region (∼50 pc × 76 pc) was also imaged at medium spatial resolution, using the ESO 2.2 m telescope in optical wavelengths. We also used the JHKs archival data from the IRSF survey and the Spitzer Space Telescope SAGE-SMC survey. Results. Our high-resolution JHKs data of the compact high-excitation H  region N26 reveal a new, bright component (C) between the two already known optical components A and B. Components A and C are resolved into several stars. Component A is the main ionization source of N26 and coincides with the radio continuum source B0046-7333. A new compact H  region with very faint [O ] λ5007 emission has been discovered. In the mid-infrared, our field resembles a shell formed by filaments and dust clumps, coinciding with the molecular cloud SMCB2. Region N22, located in the center of the shell, is the most excited H  region of the complex and seems to have created a cavity in SMCB2. We derive nebular parameters from spectra, and using color-magnitude and color-color diagrams, we identify stellar sources that show significant near-infrared excess emission in order to identify the best YSO candidates.

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Section: Discussionmentioning

confidence: 99%

Optical and infrared observations of the young SMC blob N26 and its environment

Testor¹,

Heydari-Malayeri²,

Chen³

et al. 2014

A&A

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“…N191A is more compact and brighter between the two components, which has a diameter of 5 2 (1.2 pc at LMC distance; Selier & Heydari-Malayeri 2012). The broad V-band image reveals that the ionized gas in N191A is excited by an O-star located at the center of the nebula (Selier & Heydari-Malayeri 2012). SMC N77A is a spherical H II region having a radius of 10″ (Selier & Heydari-Malayeri 2012).…”

Section: The Samplementioning

confidence: 95%

“…LMC N191 is a complex H II region that presents two components in Hα, [O III], and Hβ narrow band images (Henize 1956). N191A is more compact and brighter between the two components, which has a diameter of 5 2 (1.2 pc at LMC distance; Selier & Heydari-Malayeri 2012). The broad V-band image reveals that the ionized gas in N191A is excited by an O-star located at the center of the nebula (Selier & Heydari-Malayeri 2012).…”

Section: The Samplementioning

confidence: 99%

“…The broad V-band image reveals that the ionized gas in N191A is excited by an O-star located at the center of the nebula (Selier & Heydari-Malayeri 2012). SMC N77A is a spherical H II region having a radius of 10″ (Selier & Heydari-Malayeri 2012). A dust lane crosses SMC N77A along the east-west direction (Selier & Heydari-Malayeri 2012;Toribio San Cipriano et al 2017).…”

Section: The Samplementioning

confidence: 99%

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Spatially Resolved Temperature and Density Structures of Nearby H ii Regions

Jin 金,

Sutherland,

Kewley

et al. 2023

ApJ

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Photoionization models frequently assume constant temperature or density within H ii regions. We investigate this assumption by measuring the detailed temperature and density structures of four H ii regions in the Large Magellanic Cloud and the Small Magellanic Cloud, using integral-field spectroscopic data from the Wide-Field Spectrograph on the ANU 2.3 m telescope. We analyze the distribution of emission lines of low-ionization, intermediate-ionization, and high-ionization species. We present the complex electron temperature and density structures within H ii regions. All four nebulae present a negative gradient in the electron density profile. Both positive and negative temperature gradients are observed in the nebulae. We create a series of nebula models with constant interstellar medium (ISM) pressure and varying temperature and density distributions. A comparison of the line ratios between our H ii regions and models suggests that none of the simple nebula models can reproduce the observed temperature and density structures. Comparison between the models and the data suggests that the ISM pressure of nebulae in the LMC and SMC is between log(P/k) = 6 and 7.5. Complex internal structures of the nebulae highlight the importance of future Monte Carlo photoionization codes for accurate nebula modeling, which include a comprehensive consideration of arbitrary geometries of H ii regions.

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“…We have adopted here the average of the positions reported in the paper. Selier & Heydari-Malayeri (2012) presented chemical abundances of He, O, N, and Ne for two outer HII regions in the Magellanic Clouds, LMC N191 and SMC N77. The data come from optical imaging and spectroscopic ESO NTT observations along with archive data.…”

Section: The Datamentioning

confidence: 99%

Abundances in photoionized nebulae of the Local Group and nucleosynthesis of intermediate mass stars

Maciel,

Costa,

Cavichia

2017

Preprint

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Photoionized nebulae, comprising HII regions and planetary nebulae, are excellent laboratories to investigate the nucleosynthesis and chemical evolution of several elements in the Galaxy and other galaxies of the Local Group. Our purpose in this investigation is threefold: (i) compare the abundances of HII regions and planetary nebulae in each system in order to investigate the differences derived from the age and origin of these objects, (ii) compare the chemical evolution in different systems, such as the Milky Way, the Magellanic Clouds, and other galaxies of the Local Group, and (iii) investigate to what extent the nucleosynthesis contributions from the progenitor stars affect the observed abundances in planetary nebulae, which constrains the nucleosynthesis of intermediate mass stars. We show that all objects in the samples present similar trends concerning distance-independent correlations, and some constraints can be defined on the production of He and N by the PN progenitor stars.

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Two compact H ii regions at the remote outskirts of the Magellanic Clouds

Cited by 7 publications

References 36 publications

Optical and infrared observations of the young SMC blob N26 and its environment

Optical and infrared observations of the young SMC blob N26 and its environment

Spatially Resolved Temperature and Density Structures of Nearby H ii Regions

Abundances in photoionized nebulae of the Local Group and nucleosynthesis of intermediate mass stars

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