THE HERschel
                INVENTORY OF THE AGENTS OF GALAXY EVOLUTION IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM

Meixner, Margaret; Panuzzo, P.; Roman-Duval, Julia; Engelbracht, C. W.; Babler, B.; Seale, Jonathan; Hony, S.; Montiel, Edward; Sauvage, M.; Gordon, K. D.; Misselt, K. A.; Okumura, K.; Chanial, P.; Beck, Tracy; Bernard, J.-P.; Bolatto, Alberto D.; Bot, Caroline; Boyer, Martha L.; Carlson, L. R.; Clayton, Geoffrey C.; Chen, C.-H. Rosie; Cormier, D.; Fukui, Y.; Galametz, M.; Galliano, F.; Hora, J. L.; Hughes, Annie; Indebetouw, R.; Israel, F. P.; Kawamura, Akiko; Kemper, F.; Kim, S.; Kwon, E.; Lebouteiller, V.; Li, A.; Long, Knox S.; Madden, S.; Matsuura, M.; Müller, Erik; Oliveira, J. M.; Onishi, Toshikazu; Otsuka, Masaaki; Paradis, D.; Poglitsch, A.; Reach, W. T.; Robitaille, Thomas; Rubio, M.; Sargent, Benjamin; Sewiło, M.; Skibba, Ramin; Smith, L. J.; Srinivasan, S.; Tielens, A. G. G. M.; Loon, Jacco Th. van; Whitney, B. A.

doi:10.1088/0004-6256/146/3/62

Cited by 158 publications

(200 citation statements)

References 97 publications

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“…The PACS and SPIRE maps of the LMC at 100, 160 250, 350, and 500 µm were first published in Meixner et al (2013) as part of the HERITAGE project. We also use the observations of 30Dor obtained as part of the Spitzer (Werner et al 2004) Legacy program "Surveying the Agents of a Galaxy's Evolution" (SAGE; Meixner et al 2006).…”

Section: Herschel and Spitzer Photometrymentioning

confidence: 99%

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A milestone toward understanding PDR properties in the extreme environment of LMC-30 Doradus

Chevance

Madden

Lebouteiller

et al. 2016

A&A

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103

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Context. More complete knowledge of galaxy evolution requires understanding the process of star formation and the interaction between the interstellar radiation field and interstellar medium (ISM) in galactic environments traversing a wide range of physical parameter space. We focus on the impact of massive star formation on the surrounding low metallicity ISM in 30 Doradus in the Large Magellanic Cloud (LMC). A low metal abundance, which can characterizes some galaxies of the early Universe, results in less ultraviolet (UV) shielding for the formation of the molecular gas necessary for star formation to proceed. The half-solar metallicity gas in this region is strongly irradiated by the super star cluster R136, making it an ideal laboratory to study the structure of the ISM in an extreme environment. Aims. Our goal is to construct a comprehensive, self-consistent picture of the density, radiation field, and ISM structure in the most active star-forming region in the LMC, 30 Doradus. Our spatially resolved study investigates the gas heating and cooling mechanisms, particularly in the photodissociation regions (PDR) where the chemistry and thermal balance are regulated by far-UV photons (6 eV < hν < 13.6 eV). Methods. We present Herschel observations of far-infrared (FIR) fine-structure lines obtained with PACS and SPIRE/FTS. We combined atomic fine-structure lines from Herschel and Spitzer observations with ground-based CO data to provide diagnostics on the properties and structure of the gas by modeling it with the Meudon PDR code. For each tracer we estimate the possible contamination from the ionized gas to isolate the PDR component. We derive the spatial distribution of the radiation field, the pressure, the size, and the filling factor of the photodissociated gas and molecular clouds. Results. We find a range of pressure of ∼10 5 −1.7×10 6 cm −3 K and a range of incident radiation field G UV ∼ 10 2 −2.5×10 4 through PDR modeling. Assuming a plane-parallel geometry and a uniform medium, we find a total extinction A max V of 1-3 mag, which corresponds to a PDR cloud size of 0.2 to 3pc with small CO depth scale of 0.06 to 0.5 pc. At least 90% of the [C ii] originates in PDRs in this region, while a significant fraction of the L FIR (up to 70% in some places) can be associated with an ionized gas component. Theratio (2 to 60) throughout the observed map, correlated with the filling factor, reveals the porosity of the ISM in this region, which is traversed by hard UV photons surrounding small PDR clumps. We also determine the three-dimensional structure of the gas, showing that the clouds are distributed 20 to 80 pc away from the main ionizing cluster, R136.

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Section: Herschel and Spitzer Photometrymentioning

confidence: 99%

“…We use the CO J = 1-0 transition observed References. (a) SAGE (Meixner et al 2006); (b) HERITAGE (Meixner et al 2013) with Mopra (Wong et al 2011) and CO J = 3-2 observed with the Atacama Submillimeter Telescope Experiment (ASTE; Minamidani et al 2011;see Fig. 2).…”

Section: Ground-based Observationsmentioning

confidence: 99%

A milestone toward understanding PDR properties in the extreme environment of LMC-30 Doradus

Chevance

Madden

Lebouteiller

et al. 2016

A&A

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“…We use the mid-IR to submm photometric maps that have been obtained with Spitzer (SAGE-SMC: Gordon et al 2011) and Herschel (HERITAGE: Meixner et al 2013). Within these two large programs the entire SMC has been observed at IRAC (3.6, 4.5 5.8 and 8.0 µm), MIPS (24, 70, and 160 µm), PACS (100 and 160 µm) and SPIRE (250, 350 and 500 µm) wavelengths.…”

Section: Herschel and Spitzer Datamentioning

confidence: 99%

Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC★

Hony¹,

Gouliermis²,

Galliano³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The rate at which interstellar gas is converted into stars, and its dependence on environment, is one of the pillars on which our understanding of the visible Universe is build. We present a comparison of the surface density of young stars (Σ ) and dust surface density (Σ dust ) across NGC 346 (N66) in 115 independent pixels of 6×6 pc 2 . We find a correlation between Σ and Σ dust with a considerable scatter. A power law fit to the data yields a steep relation with an exponent of 2.6±0.2. We convert Σ dust to gas surface density (Σ gas ) and Σ to star formation rate (SFR) surface densities (Σ SFR ), using simple assumptions for the gas-to-dust mass ratio and the duration of star formation. The derived total SFR (4±1·10 −3 M yr −1 ) is consistent with SFR estimated from the H α emission integrated over the H α nebula. On small scales the Σ SFR derived using H α systematically underestimates the count-based Σ SFR , by up to a factor of 10. This is due to ionizing photons escaping the area, where the stars are counted. We find that individual 36 pc 2 pixels fall systematically above integrated disc-galaxies in the Schmidt-Kennicutt diagram by on average a factor of ∼7. The NGC 346 average SFR over a larger area (90 pc radius) lies closer to the relation but remains high by a factor of ∼3. The fraction of the total mass (gas plus young stars) locked in young stars is systematically high (∼10 per cent) within the central 15 pc and systematically lower outside (2 per cent), which we interpret as variations in star formation efficiency. The inner 15 pc is dominated by young stars belonging to a centrally condensed cluster, while the outer parts are dominated by a dispersed population. Therefore, the observed trend could reflect a change of star formation efficiency between clustered and non-clustered star-formation.

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“…The "host-WR" photometry almost overlaps with the total host photometry in most cases, so it is not shown. The data for the LMC are shown as black crosses (Israel et al 2010;Meixner et al 2013). Table 2.…”

Section: Basic Physical Propertiesmentioning

confidence: 99%

“…Dust masses for the KINGFISH galaxies are taken from Bianchi (2013), and stellar masses from Skibba et al (2011) are corrected to the Kennicutt et al (2011) distance scale. Finally, we mark the Large Magellanic Cloud (LMC) using the compilation in Israel et al (2010) and Meixner et al (2013).…”

Section: Flux Ratiosmentioning

confidence: 99%

Spatially-resolved dust properties of the GRB 980425 host galaxy

Michałowski

Hunt

Palazzi

et al. 2014

A&A

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Gamma-ray bursts (GRBs) have been proposed as a tool for studying star formation in the Universe, so it is crucial to investigate whether their host galaxies and immediate environments are in any way special compared with other star-forming galaxies. Here we present spatially resolved maps of dust emission of the host galaxy of the closest known GRB 980425 at z = 0.0085 using our new high-resolution observations from Herschel, Atacama Pathfinder Experiment (APEX), Atacama Large Millimeter Array (ALMA) and Australia Telescope Compact Array (ATCA). We modelled the spectral energy distributions of the host and of the star-forming region displaying the Wolf-Rayet signatures in the spectrum (WR region), located 800 pc from the GRB position. The host is characterised by low dust content and a high fraction of UV-visible star formation, similar to other dwarf galaxies. These galaxies are abundant in the local universe, so it is not surprising to find a GRB in one of them, assuming the correspondence between the GRB rate and star formation. The WR region contributes substantially to the host emission at the far-infrared, millimetre, and radio wavelengths and we propose that this is a consequence of its high gas density. If dense environments are also found close to the positions of other GRBs, then the ISM density should also be considered, along with metallicity, an important factor influencing whether a given stellar population can produce a GRB.

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THE HERschel INVENTORY OF THE AGENTS OF GALAXY EVOLUTION IN THE MAGELLANIC CLOUDS, A HERSCHEL OPEN TIME KEY PROGRAM

Cited by 158 publications

References 97 publications

A milestone toward understanding PDR properties in the extreme environment of LMC-30 Doradus

A milestone toward understanding PDR properties in the extreme environment of LMC-30 Doradus

Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC★

Spatially-resolved dust properties of the GRB 980425 host galaxy

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