Probing the interstellar medium of NGC 1569 with Herschel★

Lianou, S.; Barmby, P.; Rémy-Ruyer, A.; Madden, S.; Galliano, F.; Lebouteiller, V.

doi:10.1093/mnras/stu1770

Cited by 7 publications

(7 citation statements)

References 120 publications

(197 reference statements)

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“…High-T w values are observed near current star-forming regions such as the SSCs, while the T c map shows a more uniform distribution than the T w map; high-T c values are found around SSCs. Those results are consistent with the spatial distribution of T c shown in Lianou et al (2014). In the IR-halo region, both T c and T w are found to Fig.…”

Section: Pixel-by-pixel Sed Fittingsupporting

confidence: 91%

“…The IRC 7 µm and 11 µm images are dominated by the PAH emission not only from the galactic disk itself but also from the halo; Onaka et al (2010) detected the PAH emission from the western arm. Overall spatial distributions in the 7 µm and 11 µm images are in good agreement with those in the 160-500 µm images which trace the spatial distribution of the cold dust component (20-30 K, Rémy-Ruyer et al 2013;Lianou et al 2014), associated mainly with the old stellar population. The fact may indicate that PAHs coexist with cold dust.…”

Section: Ir Imagessupporting

confidence: 75%

“…The fact may indicate that PAHs coexist with cold dust. The IRC 15 µm and 24 µm images trace emission from both hot (100-200 K) and warm (40-60 K) dust components (Lianou et al 2014;Galliano et al 2003), associated mainly with massive starforming regions. Therefore, the spatial distributions of cold and PAH components are more extended toward the halo region than those of hot and warm dust components.…”

Section: Ir Imagesmentioning

confidence: 99%

“…During this phase, the galaxy witnessed ∼ 10 4 supernova explosions, and the formation of star clusters including the two prominent super-star clusters (SSCs) A and B (Arp & Sandage 1985). These activities have had dramatic effects on both the ISM and the halo of NGC 1569: (i) a cavity shown in the H i, Hα and far-IR distributions centered on SSC A, most probably due to stellar winds from SSC A (Israel & van Driel 1990;Hunter et al 2000;Lianou et al 2014), (ii) chimneys in southward and northward directions from SSC A, which are considered to be major pathways to eject the ISM into the halo (Hunter et al 1993;Mühle et al 2005;Westmoquette et al 2008), (iii) a bipolar metal-enriched outflow comprising kpc-scale expanding superbubbles on the southern and northern sides of the galactic disc (Hunter et al 1993;Heckman et al 1995;Martin 1998;Martin et al 2002;Westmoquette et al 2008).…”

Section: Introductionmentioning

confidence: 99%

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Enhanced dust emissivity power-law index along the western H α filament of NGC 1569

Suzuki

Kaneda

Onaka

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We used a data set from AKARI and Herschel images at wavelengths from 7 µm to 500 µm to catch the evidence of dust processing in galactic winds in NGC 1569. Images show a diffuse infrared (IR) emission extending from the galactic disk into the halo region. The most prominent filamentary structure seen in the diffuse IR emission is spatially in good agreement with the western Hα filament (western arm). The spatial distribution of the F 350 /F 500 map shows high values in regions around the super-star clusters (SSCs) and towards the western arm, which are not found in the F 250 /F 350 map. The color-color diagram of F 250 /F 350 -F 350 /F 500 indicates high values of the emissivity power-law index (β c ) of the cold dust component in those regions. From a spectral decomposition analysis on a pixel-by-pixel basis, a β c map shows values ranging from ∼ 1 to ∼ 2 over the whole galaxy. In particular, high β c values of ∼ 2 are only observed in the regions indicated by the color-color diagram. Since the average cold dust temperature in NGC 1569 is ∼ 30 K, β c < 2.0 in the far-IR and sub-mm region theoretically suggests emission from amorphous grains, while β c = 2.0 suggests that from crystal grains. Given that the enhanced β c regions are spatially confined by the HI ridge that is considered to be a birthplace of the SSCs, the spatial coincidences may indicate that dust grains around the SSCs are grains of relatively high crystallinity injected by massive stars originating from starburst activities and that those grains are blown away along the HI ridge and thus the western arm.

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Section: Pixel-by-pixel Sed Fittingsupporting

confidence: 91%

Section: Ir Imagessupporting

confidence: 75%

Section: Ir Imagesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Enhanced dust emissivity power-law index along the western H α filament of NGC 1569

Suzuki

Kaneda

Onaka

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Perhaps the next best candidate of a proto-globular cluster after NGC 5253 is found within dwarf starburst NGC 1569, located at a distance of D = 3.4 Mpc (Grocholski et al 2012) and known for its two bright, visible SSCs, A and B (e.g., Hunter et al 2000). Currently NGC 1569's most active star formation is concentrated to an obscured region characterized by high extinction (Galliano et al 2003;Pasquali et al 2011;Lianou et al 2014;Westcott et al 2018). Intense thermal radio continuum coinciding with bright He i and Pa β emission indicates the presence of H ii regions excited by forming massive star clusters (Greve et al 2002;Clark et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Observing the influence of the youngest super star clusters in NGC 1569: Keck Brackett $α$ spectroscopy

Cohen,

Turner,

Beck

et al. 2021

Preprint

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We report Keck-NIRSPEC observations of the Brackett α 4.05 µm recombination line across the two candidate embedded super star clusters (SSCs) in NGC 1569. These SSCs power a bright H ii region and have been previously detected as radio and mid-infrared sources. Supplemented with high resolution VLA mapping of the radio continuum along with IRTF-TEXES spectroscopy of the [S iv] 10.5µm line, the Brackett α spectra data provide new insight into the dynamical state of gas ionized by these forming massive clusters. NIR sources detected in 2µm images from the Slit-viewing Camera are matched with GAIA sources to obtain accurate celestial coordinates and slit positions to within ∼ 0. 1. Br α is detected as a strong emission peak powered by the less luminous infrared source, MIR1 (L IR ∼ 2 × 10 7 L ). The second candidate SSC MIR2 is more luminous (L IR 4 × 10 8 L ) but exhibits weak radio continuum and Br α emission, suggesting the ionized gas is extremely dense (n e 10 5 cm −3 ), corresponding to hypercompact H ii regions around newborn massive stars. The Br α and [S iv] lines across the region are both remarkably symmetric and extremely narrow, with observed line widths ∆v 40 km s −1 , FWHM. This result is the first clear evidence that feedback from NGC 1569's youngest giant clusters is currently incapable of rapid gas dispersal, consistent with the emerging theoretical paradigm in the formation of giant star clusters.

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Dust properties and star formation of approximately a thousand local galaxies

Lianou

Barmby

Mosenkov

et al. 2019

A&A

Self Cite

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Aims. We derive the dust properties for 753 local galaxies and examine how these relate to some of their physical properties. We present the derived dust emission properties, including model spectral energy distribution (SEDs), star formation rates and stellar masses, as well as their relations. Methods. We model the global dust-SEDs for 753 galaxies, treated statistically as an ensemble within a hierarchical Bayesian dust-SED modeling approach, so as to derive their infrared (IR) emission properties. To create the observed dust-SEDs, we use a multiwavelength set of observations, ranging from near-IR to far-IR / submillimeter wavelengths. The model-derived properties are the dust masses (M dust ), the average interstellar radiation field intensities (U av ), the mass fraction of very small dust grains ('QPAH' fraction), as well as their standard deviations. In addition, we use mid-IR observations to derive star formation rates (SFR) and stellar masses, quantities independent of the dust-SED modeling. Results. We derive distribution functions of the properties for the galaxy ensemble and as a function of galaxy type. The mean value of M dust for the early-type galaxies (ETGs) is lower than that for the late-type and irregular galaxies (LTGs and IRs, respectively), despite ETGs and LTGs having stellar masses spanning across the whole range observed. The U av and 'QPAH' fraction show no difference among different galaxy types. When fixing U av to the Galactic value, the derived 'QPAH' fraction varies across the Galactic value (0.071). The specific SFR increases with galaxy type, while this is not the case for the dust-specific SFR (SFR/M dust ), showing an almost constant star formation efficiency per galaxy type. The galaxy sample is characterised by a tight relation between the dust mass and the stellar mass for the LTGs and Irs, while ETGs scatter around this relation and tend towards smaller dust masses. While the relation indicates that M dust may fundamentally be linked to M , metallicity and U av are the second parameter driving the scatter, which we investigate in a forthcoming work. We use the extended Kennicutt-Schmidt (KS) law to estimate the gas mass and the gas-to-dust mass ratio (GDR). The gas mass derived from the extended KS law is on average ∼20% higher than that derived from the KS law, and a large standard deviation indicates the importance of the average star formation present to regulate star formation and gas supply. The average GDR for the LTGs and Irs is 370, while including the ETGs gives an average of 550.

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Probing the interstellar medium of NGC 1569 with Herschel★

Cited by 7 publications

References 120 publications

Enhanced dust emissivity power-law index along the western H α filament of NGC 1569

Enhanced dust emissivity power-law index along the western H α filament of NGC 1569

Observing the influence of the youngest super star clusters in NGC 1569: Keck Brackett $α$ spectroscopy

Dust properties and star formation of approximately a thousand local galaxies

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