A very young component in the pre-eminent starburst region of the Small Magellanic Cloud

Heydari-Malayeri, M.; Selier, R.

doi:10.1051/0004-6361/201014230

Cited by 15 publications

(5 citation statements)

References 50 publications

(81 reference statements)

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“…Alternately, this star could be the first to emerge from an embedded cluster (cf. Walborn et al 1999Walborn et al , 2002Heyderi-Malayeri & Selier 2010, for similar examples in 30 Doradus and N 66) the O star may exhibit a mid-IR excess due to free-free emission in the stellar wind (as described in Bonanos et al 2009), or it could be a chance superposition.…”

Section: Stellar Fitsmentioning

confidence: 98%

A PANCHROMATIC VIEW OF NGC 602: TIME-RESOLVED STAR FORMATION WITH THEHUBBLEANDSPITZERSPACE TELESCOPES

Carlson

Sewiło

Meixner

et al. 2011

ApJ

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We present the photometric catalogs for the star-forming cluster NGC 602 in the wing of the Small Magellanic Cloud covering a range of wavelengths from optical (HST/ACS F555W, F814W and SMARTS/ANDICAM V, I) to infrared (Spitzer /IRAC 3.6, 4.5, 5.8, and 8 µm and MIPS 24 µm). Combining this with IRSF (InfraRed Survey Facility) near-infrared photometry (J, H, K s ), we compare the young main sequence (MS) and pre-main sequence (PMS) populations prominent in the optical with the current young stellar object (YSO) populations revealed by the infrared (IR). We analyze the MS and PMS population with isochrones in color-magnitude diagrams to derive ages and masses.

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Section: Stellar Fitsmentioning

confidence: 98%

A PANCHROMATIC VIEW OF NGC 602: TIME-RESOLVED STAR FORMATION WITH THEHUBBLEANDSPITZERSPACE TELESCOPES

Carlson

Sewiło

Meixner

et al. 2011

ApJ

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“…The core consists of a long ionization front in the form of a curved ridge with various bright patches of ionized gas scattered about, centered on the prominent star cluster NGC 346, which is the main source of ionization. At the southeastern edge of the ridge is a bright patch known as N66 A by Heydari-Malayeri & Selier (2010); the bright area at the opposite, northwestern edge of the ridge is called N66 B, and there is another, slightly detached patch to the northeast of the ridge, which is referred to as N66 C, a nomenclature we follow here (see Fig. 2 in Reid & Wilson 2006).…”

Section: Introductionmentioning

confidence: 99%

Carbon gas in SMC low-metallicity star-forming regions

Requeña-Torres

Israel

Okada

et al. 2016

A&A

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This paper presents [C II], [C I] and CO emission line maps of the star-forming regions N 66, N 25+N 26, and N 88 in the metalpoor Local Group dwarf galaxy SMC. The spatial and velocity structure of the large H II region N 66 reveals an expanding ring of shocked molecular gas centered on the exciting star cluster NGC 346, whereas a more distant dense molecular cloud is being eroded by UV radiation from the same cluster. In the N 25+N 26 and N 88 maps, diffuse [C II] emission at a relatively low surface brightness extends well beyond the compact boundaries of the bright emission associated with the H II regions. In all regions, the distribution of this bright [C II] emission and the less prominent [C I] emission closely follows the outline of the CO complexes, but the intensity of the [C II] and [C I] emission is generally anticorrelated, which can be understood by the action of photodissociation and photoionization processes. Notwithstanding the overall similarity of CO and [C II] maps, the intensity ratio of these lines varies significantly, mostly due to changes in CO brightness. [C II] emission line profiles are up to 50% wider in velocity than corresponding CO profiles. A radiative transfer analysis shows that the [C II] line is the dominant tracer of (CO-dark) molecular hydrogen in the SMC. CO emission traces only a minor fraction of the total amount of gas. The similarity of the spatial distribution and line profile shape, and the dominance of molecular gas associated with [C II] rather than CO emission imply that in the low-metallicity environment of the SMC the small amount of dense molecular gas traced by CO is embedded in the much more extended molecular gas traced only by [C II] emission. The contribution from neutral atomic and ionized hydrogen zones is negligible in the star-forming regions observed.

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“…The abundance of small-scale features in the Bar of the SMC, extending from the north to the south-west and outlined by the white rectangle, trace the stellar feedback effects from the strong ongoing star formation in this region as seen in (Winkler et al 2015) and other star burst regions such as the N66/NGC 346 complex (Heydari-Malayeri & Selier 2010). The detail in small-scale features in a single spectral channel from our new GASKAP-HI data approaches those traced by the far-infrared dust image produced as part of the HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) project (Meixner et al 2013).…”

Section: Gas Morphologymentioning

confidence: 86%

GASKAP-HI pilot survey science I: ASKAP zoom observations of Hi emission in the Small Magellanic Cloud

Pingel

Dempsey

McClure‐Griffiths

et al. 2022

Publ. Astron. Soc. Aust.

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We present the most sensitive and detailed view of the neutral hydrogen ( ${\rm H\small I}$ ) emission associated with the Small Magellanic Cloud (SMC), through the combination of data from the Australian Square Kilometre Array Pathfinder (ASKAP) and Parkes (Murriyang), as part of the Galactic Australian Square Kilometre Array Pathfinder (GASKAP) pilot survey. These GASKAP-HI pilot observations, for the first time, reveal ${\rm H\small I}$ in the SMC on similar physical scales as other important tracers of the interstellar medium, such as molecular gas and dust. The resultant image cube possesses an rms noise level of 1.1 K ( $1.6\,\mathrm{mJy\ beam}^{-1}$ ) $\mathrm{per}\ 0.98\,\mathrm{km\ s}^{-1}$ spectral channel with an angular resolution of $30^{\prime\prime}$ ( ${\sim}10\,\mathrm{pc}$ ). We discuss the calibration scheme and the custom imaging pipeline that utilises a joint deconvolution approach, efficiently distributed across a computing cluster, to accurately recover the emission extending across the entire ${\sim}25\,\mathrm{deg}^2$ field-of-view. We provide an overview of the data products and characterise several aspects including the noise properties as a function of angular resolution and the represented spatial scales by deriving the global transfer function over the full spectral range. A preliminary spatial power spectrum analysis on individual spectral channels reveals that the power law nature of the density distribution extends down to scales of 10 pc. We highlight the scientific potential of these data by comparing the properties of an outflowing high-velocity cloud with previous ASKAP+Parkes ${\rm H\small I}$ test observations.

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A very young component in the pre-eminent starburst region of the Small Magellanic Cloud

Cited by 15 publications

References 50 publications

A PANCHROMATIC VIEW OF NGC 602: TIME-RESOLVED STAR FORMATION WITH THEHUBBLEANDSPITZERSPACE TELESCOPES

A PANCHROMATIC VIEW OF NGC 602: TIME-RESOLVED STAR FORMATION WITH THEHUBBLEANDSPITZERSPACE TELESCOPES

Carbon gas in SMC low-metallicity star-forming regions

GASKAP-HI pilot survey science I: ASKAP zoom observations of Hi emission in the Small Magellanic Cloud

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