Hα Emission from the Magellanic Bridge

Müller, Erik; Parker, Quentin A.

doi:10.1071/as07010

Cited by 12 publications

(20 citation statements)

References 31 publications

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“…The simultaneous presence of far-UV and far-IR emission indicates young, embedded star forming regions. These cluster regions also have strong Hα emission (Muller & Parker 2007) providing the indication that they harbor massive star formation. The IR stellar properties of these clusters will be investigated in more detail in Chen et al (in prep.…”

Section: Embedded Clustersmentioning

confidence: 98%

The Dust-to-Gas Ratio in the Small Magellanic Cloud Tail

Gordon¹,

Bot

Müller

et al. 2008

ApJ

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The Tail region of the Small Magellanic Cloud (SMC) was imaged using the MIPS instrument on the Spitzer Space Telescope as part of the SAGE-SMC Spitzer Legacy. Diffuse infrared emission from dust was detected in all the MIPS bands. The Tail gas-to-dust ratio was measured to be 1200 ± 350 using the MIPS observations combined with existing IRAS and H i observations. This gas-to-dust ratio is higher than the expected 500-800 from the known Tail metallicity indicating possible destruction of dust grains. Two cluster regions in the Tail were resolved into multiple sources in the MIPS observations and local gas-to-dust ratios were measured to be ∼ 440 and ∼ 250 suggest dust formation and/or significant amounts of ionized gas in these regions. These results support the interpretation that the SMC Tail is a tidal Tail recently stripped from the SMC that includes gas, dust, and young stars.

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Section: Embedded Clustersmentioning

confidence: 98%

The Dust-to-Gas Ratio in the Small Magellanic Cloud Tail

Gordon¹,

Bot

Müller

et al. 2008

ApJ

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“…Also included are H ii regions in the Bridge that Muller & Parker (2007) cross‐identified with associations from Bica & Schmitt (1995), Bica & Dutra (2000) and probable UV ionising stellar sources (FAUST –Bowyer et al 1995).…”

Section: The Updated Cataloguementioning

confidence: 99%

A general catalogue of extended objects in the Magellanic System

Bica

Bonatto

Dutra

et al. 2008

Monthly Notices of the Royal Astronomical Society

185

276

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We update the SMC, Bridge, and LMC catalogues of extended objects that were constructed by members of our group from 1995 to 2000. In addition to the rich subsequent literature for the previous classes, we now also include HI shells and supershells. A total of 9305 objects were cross-identified, while our previous catalogues amounted to 7900 entries, an increase of $\approx12%$. We present the results in subcatalogues containing 1445 emission nebulae, 3740 star clusters, 3326 associations, and 794 HI shells and supershells. Angular and apparent size distributions of the extended objects are analysed. We conclude that the objects, in general, appear to respond to tidal effects arising from the LMC, SMC, and Bridge. Number-density profiles extracted along directions parallel and perpendicular to the LMC bar, can be described by two exponential-disks. A single exponential-disk fits the equivalent SMC profiles. Interestingly, when angular-averaged number-densities of most of the extended objects are considered, the profiles of both Clouds do not follow an exponential-disk. Rather, they are best described by a tidally-truncated, core/halo profile, despite the fact that the Clouds are clearly disturbed disks. On the other hand, the older star clusters taken isolately, distribute as an exponential disk. The present catalogue is an important tool for the unambiguous identification of previous objects in current CCD surveys and to establish new findings.Comment: 15 pages, 10 figures, MNRAS, accepte

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“…Simulations suggest that the Magellanic Bridge is the result of a close gravitational interaction between the LMC and SMC that happened around 200-300 Myrs ago (Murai & Fujimoto 1980;Gardiner et al 1994;Besla et al 2012). Star formation has and is taking place in the Magellanic Bridge: there are young stars and clusters of less than 100 Myr in age (Bica & Schmitt 1995;Harris 2007;Bica et al 2015;Kalari et al 2018) and evidence of current star formation in the form of Hα filamentary shells Reduced maps and images are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http: //cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/641/A97 (Muller & Parker 2007) and young stellar objects (YSOs; Chen et al 2014). Its metallicity is low and seems to present a gradient, from values similar to the SMC main body (Z ∼ 1/5 Z , Lee et al 2005) to about half (or even less) of the SMC metallicity (Z ∼ 1/10 Z , Rolleston et al 2003;Lehner et al 2008).…”

Section: Introductionmentioning

confidence: 99%

“…Magellanic Bridge A is one of the faintest of the eight molecular clouds detected by Mizuno et al (2006), with a 12 CO(1−0) intensity of 30 mK km s −1 and a molecular mass of 10 3 M , estimated from its 12 CO(1−0) emission. Magellanic Bridge A is located between two faint compact H II regions (Muller & Parker 2007) and is within a stellar association (Bica & Schmitt 1995). There is recent star formation in this region, revealed by two YSO candidates within the molecular cloud (Chen et al 2014) and its proximity to H II regions and 24 µm bright sources (Muller et al 2014).…”

Section: Introductionmentioning

confidence: 99%

ALMA resolves molecular clouds in metal-poor Magellanic Bridge A

Valdivia-Mena

Rubio

Bolatto

et al. 2020

A&A

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Context. The Magellanic Bridge is a tidal feature located between the Magellanic Clouds, containing young stars formed in situ. Its proximity allows high-resolution studies of molecular gas, dust, and star formation in a tidal low-metallicity environment. Aims. Our goal is to characterize gas and dust emission in Magellanic Bridge A, the source with the highest 870 μm excess of emission found in single-dish surveys. Methods. Using the ALMA telescope including the Morita Array, we mapped a 3′ field of view centered on the Magellanic Bridge A molecular cloud, in 1.3 mm continuum emission and 12CO(2−1) line emission at subparsec resolution. This region was also mapped in continuum at 870 μm and in 12CO(2−1) line emission at ~6 pc resolution with the APEX telescope. To study its dust properties, we also use archival Herschel and Spitzer data. We combine the ALMA and APEX 12CO(2−1) line cubes to study the molecular gas emission. Results. Magellanic Bridge A breaks up into two distinct molecular clouds in dust and 12CO(2−1) emission, which we call North and South. Dust emission in the North source, according to our best parameters from fitting the far-infrared fluxes, is ≈3 K colder than in the South source in correspondence to its less developed star formation. Both dust sources present large submillimeter excesses in LABOCA data: according to our best fits the excess over the modified blackbody (MBB) fit to the Spitzer/Herschel continuum is E(870 μm) ~ 7 and E(870 μm) ~ 3 for the North and South sources, respectively. Nonetheless, we do not detect the corresponding 1.3 mm continuum with ALMA. Our limits are compatible with the extrapolation of the MBB fits, and therefore we cannot independently confirm the excess at this longer wavelength. The 12CO(2−1) emission is concentrated in two parsec-sized clouds with virial masses of around 400 and 700 M⊙. Their bulk volume densities are n(H2) ~ 0.7−2.6 × 103 cm−3, higher than typical bulk densities of Galactic molecular clouds. The 12CO luminosity to H2 mass conversion factor αCO is 6.5 and 15.3 M⊙ (K km s−1 pc2)−1 for the North and South clouds, calculated using their respective virial masses and 12CO(2−1) luminosities. Gas mass estimates from our MBB fits to dust emission yields masses M ~ 1.3 × 103 M⊙ and 2.9 × 103 M⊙ for North and South, respectively, a factor of ~4 higher than the virial masses we infer from 12CO.

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Hα Emission from the Magellanic Bridge

Cited by 12 publications

References 31 publications

The Dust-to-Gas Ratio in the Small Magellanic Cloud Tail

The Dust-to-Gas Ratio in the Small Magellanic Cloud Tail

A general catalogue of extended objects in the Magellanic System

ALMA resolves molecular clouds in metal-poor Magellanic Bridge A

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