Infrared Narrowband Tomography of the Local Starburst NGC 1569 With the Large Binocular Telescope/Lucifer

Pasquali, A.; Bik, Arjan; Zibetti, S.; Ageorges, N.; Seifert, W.; Brandner, W.; Rix, H. W.; Jütte, M.; Knierim, Volker; Buschkamp, P.; Feiz, C.; Gemperlein, Hans; Germeroth, A.; Hofmann, R.; Laun, W.; Lederer, R.; Lehmitz, Michael; Lenzen, R.; Mall, U.; Mandel, H.; Müller, P.; Naranjo, V.; Polsterer, Kai Lars; Quirrenbach, A.; Schäffner, L.; Storz, Clemens; Weiser, P.

doi:10.1088/0004-6256/141/4/132

Cited by 20 publications

(21 citation statements)

References 64 publications

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“…This picture is also observed in NGC 1569 (Pasquali et al 2011). In SBS 0335-052 the [FeII] is presumably shocked and at the same location of the HII regions, however our spatial resolution is significantly lower for this galaxy.…”

Section: Discussionsupporting

confidence: 68%

Integral field spectroscopy in the near infrared of NGC 3125-A and SBS 0335-052

Vanzi

Cresci

Sauvage

et al. 2011

A&A

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We present integral field spectroscopy in the near infrared of the nearby dwarf starburst galaxy NGC 3125-A and of the low metallicity dwarf galaxy SBS 0335-052. The use of adaptive optics in the observations produces sub-arcsecond angular resolution. We pinpoint the star forming cores of both galaxies, identify relevant ISM components such as dust, photo ionized gas, shock excited gas and molecular gas. We relate these components to the large scale star formation process of the galaxies. In particular we find the emission of the near infrared lines of H 2 and especially [FeII] does not coincide with the HII region in NGC 3125. We have the first clear detection of [FeII] in SBS 0335-052.

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Section: Discussionsupporting

confidence: 68%

Integral field spectroscopy in the near infrared of NGC 3125-A and SBS 0335-052

Vanzi

Cresci

Sauvage

et al. 2011

A&A

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“…3. This pixel probes the part of the cavity seen in both warm ionised and atomic hydrogen observations, but several other cavities in the ISM of smaller scale have been uncovered in the central part of the galaxy (e.g., Pasquali et al 2011). These smaller scale cavities are smoothed out due to the relatively large angular resolution.…”

Section: Ism Cmentioning

confidence: 88%

“…1 2000; Pasquali et al 2011) that has been initially observed in H i (Israel & van Driel 1990 (Tokura et al 2006;Taylor et al 1999;Waller 1991). SC 10, which is not considered an SSC, has a stellar mass of ∼10 3 M⊙ and consists of two components, both with young ages: one of 5-7 Myr, and another with less than 5 Myr (Westmoquette & et al 2007a).…”

Section: Multiwavelength Emission Morphologymentioning

confidence: 98%

“…There are several dust knots revealed at 100 µm, which are located outside the very central starbursting region and mark the periphery of the cavity. At the location of these knots, several H ii regions and giant molecular clouds are found (Waller 1991;Taylor et al 1999;Pasquali et al 2011;Johnson et al 2012). These molecular clouds host embedded star formation (Tokura et al 2006;Westmoquette & et al 2007a;Clark et al 2013).…”

Section: Multiwavelength Emission Morphologymentioning

confidence: 99%

“…The motivation for this choice of reddening is from past studies on the internal extinction across the galaxy, which found the total reddening, i.e. Galactic foreground plus internal, to vary between 0.56 to 0.80 mag (Pasquali et al 2011;Relaño et al 2006;Devost et al 1997;Kobulnicky & Skillman 1997;Calzetti et al 1996). We do not perform internal extinction corrections to the data set for the SED modelling procedure, 1 http://galex.stsci.edu/GR6/ 2 http://www2.lowell.edu/users/dah/littlethings/n1569.html 3 As the MIPS 70 µm and MIPS 160 µm images cover only a small part of the galaxy, we make use of only the MIPS 24 µm image.…”

Section: Introductionmentioning

confidence: 99%

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Probing the interstellar medium of NGC 1569 with Herschel★

Lianou

Barmby

Rémy-Ruyer

et al. 2014

Monthly Notices of the Royal Astronomical Society

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NGC 1569 has some of the most vigorous star formation among nearby galaxies. It hosts two super star clusters (SSCs) and has a higher star formation rate (SFR) per unit area than other starburst dwarf galaxies. Extended emission beyond the galaxy's optical body is observed in warm and hot ionised and atomic hydrogen gas; a cavity surrounds the SSCs. We aim to understand the impact of the massive star formation on the surrounding interstellar medium in NGC 1569 through a study of its stellar and dust properties. We use Herschel and ancillary multiwavelength observations, from the ultraviolet to the submillimeter regime, to construct its spectral energy distribution, which we model with magphys on ∼300 pc scales at the SPIRE 250 µm resolution. The multiwavelength morphology shows low levels of dust emission in the cavity, and a concentration of several dust knots in its periphery. The extended emission seen in the ionised and neutral hydrogen observations is also present in the far-infrared emission. The dust mass is higher in the periphery of the cavity, driven by ongoing star formation and dust emission knots. The SFR is highest in the central region, while the specific SFR is more sensitive to the ongoing star formation. The region encompassing the cavity and SSCs contains only 12 per cent of the dust mass of the central starburst, in accord with other tracers of the interstellar medium. The gas-to-dust mass ratio is lower in the cavity and fluctuates to higher values in its periphery.

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The Lifecycle of Clusters in Galaxies

Adamo

Bastian

2017

The Birth of Star Clusters

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We review many of the basic properties of star cluster systems, and focus in particular on how they relate to their host galaxy properties and ambient environment. The cluster mass and luminosity functions are well approximated by power-laws of the form Ndm ∝ M α dm, with α ∼ −2 over most of the observable range. However, there is now clear evidence that both become steeper at high masses/luminosities, with the value of the downward turn dependent on environment. The host galaxy properties also appear to affect the cluster formation efficiency (Γ -i.e., the fraction of stars that form in bound clusters), with higher starformation rate density galaxies having higher Γ values. Within individual galaxies, there is evidence for Γ to vary by a factor of 3 − 4, likely following the molecular gas surface density, in agreement with recent predictions. Finally, we discuss cluster disruption and its effect on the observed properties of a population, focussing on the age distribution of clusters. We briefly discuss the expectations of theoretical and numerical studies, and also the observed distributions in a number of galaxies. Most observational studies now find agreement with theoretical expectations, namely nearly a constant cluster age distribution for ages up to ∼ 100 Myr (i.e. little disruption), and a drastic steepening above this value caused by a combination of cluster disruption and incompleteness. Rapid cluster disruption for clusters with ages < 100 Myr is ruled out for most galaxies.

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Infrared Narrowband Tomography of the Local Starburst NGC 1569 With the Large Binocular Telescope/Lucifer

Cited by 20 publications

References 64 publications

Integral field spectroscopy in the near infrared of NGC 3125-A and SBS 0335-052

Integral field spectroscopy in the near infrared of NGC 3125-A and SBS 0335-052

Probing the interstellar medium of NGC 1569 with Herschel★

The Lifecycle of Clusters in Galaxies

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