Dust and Recent Star Formation in the Core of NGC 5253

Calzetti, D.; Meurer, G. R.; Bohlin, R. C.; Garnett, D. R.; Kinney, A. L.; Leitherer, Claus; Storchi‐Bergmann, Thaisa

doi:10.1086/118609

Cited by 141 publications

(320 citation statements)

References 55 publications

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“…Calzetti et al (1997) found that they span a range of masses and ages, and identified six main clusters, one of which powers a giant HII region that is the most prominent object in the galaxy (Vanzi & Sauvage 2004). Cresci et al (2005) detected more than 300 clusters combining high-resolution NIR and optical imaging, with derived ages spanning a range between 2 and 50 Myr and masses of up to 10 6 M .…”

Section: Ngc 5253mentioning

confidence: 99%

“…Moreover, star-forming regions with properties consistent with the more massive HII regions detected locally are observed up to z ∼ 5 (Swinbank et al 2009), and local dwarf galaxies have been identified as scaled down analogs of clumpy starforming galaxies at high redshift (Elmegreen et al 2009). Dwarf for He 2-10, the clusters (L1-6) from Cabanac et al (2005) and the radio knots (knot 1-5) from Kobulnicky & Johnson (1999) are marked, while for NGC 5253 the clusters from Calzetti et al (1997) and Vanzi & Sauvage (2004).…”

Section: Introductionmentioning

confidence: 99%

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Integral-field near-infrared spectroscopy of two blue dwarf galaxies: NGC 5253 and He 2-10

Cresci

Vanzi

Sauvage

et al. 2010

A&A

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We present integral field spectroscopy in the near infrared (NIR) of He 2-10 and NGC 5253, two well known nearby dwarf irregular galaxies showing high star-formation rates. Our data provide an unprecedented detailed view of the interstellar medium and star formation in these galaxies, allowing us to obtain spatially resolved information from the NIR emission and absorption line tracers. We study the spatial distribution and kinematics of different components of the interstellar medium (ISM) mostly through the Bracket series lines, the molecular hydrogen spectrum, [FeII] emission, and CO absorptions. Although the ISM is mostly photo-excited, as derived by the [FeII]/Brγ and H 2 line ratios, some regions corresponding to non-thermal radio sources show a [FeII]/Brγ excess due to a significant contribution of SN driven shocks. In He 2-10 we find that the molecular gas clouds, as traced by CO(2−1) and H 2 infrared line, show consistent morphologies and velocities when studied with the two different tracers. Moreover, there is a clear association with the youngest super star clusters as traced by the ionized gas. In the same galaxy we observe a cavity depleted of gas, which is surrounded by some of the most active regions of star formation, that we interpret as a signature of feedback-induced star formation from older episodes of star formation. Finally, we measured high turbulence in the ISM of both galaxies, σ ∼ 30−80 km s −1 , driven by the high star-formation activity.

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Section: Ngc 5253mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Integral-field near-infrared spectroscopy of two blue dwarf galaxies: NGC 5253 and He 2-10

Cresci

Vanzi

Sauvage

et al. 2010

A&A

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“…Caldwell & Phillips 1989;Martin & Kennicutt 1995;Calzetti et al 1997Calzetti et al , 1999). We will highlight here only those observations that are relevant to our present work.…”

Section: Introductionmentioning

confidence: 99%

Dust and super star clusters in NGC 5253

Vanzi

Sauvage²

2004

A&A

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Abstract. We present new observations of the famous starburst galaxy NGC 5253 which owes its celebrity to possibly being the youngest and closest starburst galaxy known. Our observations in the infrared and millimeter contribute to shed light on the properties of this interesting object. We have used our new data along with data from the literature to study the properties of the young stellar clusters present in NGC 5253. We find that the brightest optical clusters are all characterized by a near-infrared excess that is explained by the combined effect of extinction and emission by dust. For the brightest infrared cluster we model the spectral energy distribution from the optical to the radio. We find that this cluster dominates the galaxy emission longward of 3 µm, that it has a bolometric luminosity of 1.2 × 10 9 L and a mass of 1.2 × 10 6 M , giving L/M ≈ 10 3 . The cluster is obscured by 7 mag of optical extinction produced by about 1.5 × 10 5 M of dust. The dust properties are peculiar with respect to the dust properties in the solar neighbourhood with a composition characterized by a lack of silicates and a flatter size distribution than the standard one, i.e. a bias toward larger grains. We find that NGC 5253 is a striking example of a galaxy where the infrared-submillimeter and ultraviolet-optical emissions originate in totally decoupled regions of vastly different physical sizes.

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“…4 (≈ 5 pc). The eastern cluster coincides with the peak of the Hα emission in NGC 5253 and is the youngest optical star cluster identified by Calzetti et al (1997). The western cluster is very reddened and is coincident with the supernebula of Turner et al (2000).…”

Section: Introductionmentioning

confidence: 63%

The very massive star content of the nuclear star clusters in NGC 5253

2016

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The blue compact dwarf galaxy NGC 5253 hosts a very young starburst containing twin nuclear star clusters, separated by a projected distance of 5 pc. One cluster (#5) coincides with the peak of the Hα emission and the other (#11) with a massive ultracompact H ii region. A recent analysis of these clusters shows that they have a photometric age of 1 ± 1 Myr, in apparent contradiction with the age of 3-5 Myr inferred from the presence of Wolf-Rayet features in the cluster #5 spectrum. We examine Hubble Space Telescope ultraviolet and Very Large Telescope optical spectroscopy of #5 and show that the stellar features arise from very massive stars (VMS), with masses greater than 100 M , at an age of 1-2 Myr. We further show that the very high ionizing flux from the nuclear clusters can only be explained if VMS are present. We investigate the origin of the observed nitrogen enrichment in the circum-cluster ionized gas and find that the excess N can be produced by massive rotating stars within the first 1 Myr. We find similarities between the NGC 5253 cluster spectrum and those of metal poor, high redshift galaxies. We discuss the presence of VMS in young, star-forming galaxies at high redshift; these should be detected in rest frame UV spectra to be obtained with the James Webb Space Telescope. We emphasize that population synthesis models with upper mass cut-offs greater than 100 M are crucial for future studies of young massive star clusters at all redshifts.

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Dust and Recent Star Formation in the Core of NGC 5253

Cited by 141 publications

References 55 publications

Integral-field near-infrared spectroscopy of two blue dwarf galaxies: NGC 5253 and He 2-10

Integral-field near-infrared spectroscopy of two blue dwarf galaxies: NGC 5253 and He 2-10

Dust and super star clusters in NGC 5253

The very massive star content of the nuclear star clusters in NGC 5253

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