Relation between the parameters of dust and of molecular and atomic gas in extragalactic star-forming regions

Смирнова, К. И.; Murga, M. S.; Wiebe, D. S.; Sobolev, A. M.

doi:10.1134/s1063772917070083

Cited by 9 publications

(29 citation statements)

References 42 publications

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“…Blue diamonds show SFRs in galaxies of low metallicity. As noted in Smirnova et al (2017), data points for low metallicity SFRs in this diagram are located slightly above the points for SFRs of high metallicity. This indicates a known dependence of flux ratio at 8 µm to 24 µm (or 22 µm) on metallicity (Engelbracht et al 2005).…”

Section: Resultsmentioning

confidence: 51%

“…This indicates a known dependence of flux ratio at 8 µm to 24 µm (or 22 µm) on metallicity (Engelbracht et al 2005). Clearly, the SFRs from the NGC660 disk (green circles) are located in the same region of the diagram as the high-metallicity SFRs from the other star-forming galaxies (the sample from Smirnova et al (2017) includes both spirals and irregulars). The SFRs from the NGC660 ring (red circles) occupy a different position in the diagram.…”

Section: Resultsmentioning

confidence: 84%

“…The general relation of fluxes at 8 and 22 µm is shown in Figure 2. Also in this graph we show fluxes at 8 and 24 µm from SFRs studied in Smirnova et al (2017). Orange circles correspond to SFRs in galaxies of high metallicity.…”

Section: Resultsmentioning

confidence: 99%

“…In Smirnova et al (2017), we investigated relations between various components of the ISM in 11 galaxies included in a number of observational surveys, including THINGS (H I line observations at 21 cm using the Karl G. Jansky Very Large Array), KINGFISH (observations in the far infrared region at 70, 100, and 160 µm using the Herschel Space Observatory), SINGS (observations in the near-infrared and mid-infrared bands at 3.6, 4.5, 5.8, 8.0 and 24 µm using the Spitzer Space Telescope), and HERA-CLES (CO 2-1 line observations using the IRAM 30 m telescope). Infrared (IR) data were also used in Smirnova et al (2017) to estimate the total dust mass (M), the fractional mass of polycyclic aromatic hydrocarbons (q PAH ), and the radiation field strength (U) using the model by Draine and Li (2007).…”

Section: Introductionmentioning

confidence: 99%

“…Infrared (IR) data were also used in Smirnova et al (2017) to estimate the total dust mass (M), the fractional mass of polycyclic aromatic hydrocarbons (q PAH ), and the radiation field strength (U) using the model by Draine and Li (2007). In this study, we want to take advantage of the obtained patterns for these 'normal' galaxies and to compare them with the similar results for the galaxy NGC660.…”

Section: Introductionmentioning

confidence: 99%

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Star-forming complexes in the polar ring galaxy NGC660

2017

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Galaxies with polar rings consist of two subsystems, a disk and a ring, which rotate almost in orthogonal planes. In this paper, we analyze the parameters characterizing the composition of the interstellar medium and star formation in star-forming complexes belonging to polar ring galaxy NGC660. We show that star-forming regions in the ring of the galaxy are distinctly different from those in the galaxy disk. They possess substantially lower infrared luminosities, which is indicative of less dust mass in these regions than in a typical disk star-forming region. UV and Hα luminosities also appear to be lower in the ring, which is likely a consequence of its relatively recent formation.

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Section: Resultsmentioning

confidence: 51%

Section: Resultsmentioning

confidence: 84%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Star-forming complexes in the polar ring galaxy NGC660

2017

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Stellar feedback in a clumpy galaxy at z ∼ 3.4

Iani

Zanella

Vernet

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Giant star-forming regions (clumps) are widespread features of galaxies at z ≈ 1 − 4. Theory predicts that they can play a crucial role in galaxy evolution if they survive to stellar feedback for >50 Myr. Numerical simulations show that clumps’ survival depends on the stellar feedback recipes that are adopted. Up to date, observational constraints on both clumps’ outflows strength and gas removal timescale are still uncertain. In this context, we study a line-emitting galaxy at redshift z ≃ 3.4 lensed by the foreground galaxy cluster Abell 2895. Four compact clumps with sizes ≲ 280 pc and representative of the low-mass end of clumps’ mass distribution (stellar masses ≲ 2 × 108 M⊙) dominate the galaxy morphology. The clumps are likely forming stars in a starbursting mode and have a young stellar population (∼10 Myr). The properties of the Lyman-α (Lyα) emission and nebular far-ultraviolet absorption lines indicate the presence of ejected material with global outflowing velocities of ∼200–300 km s−1. Assuming that the detected outflows are the consequence of star formation feedback, we infer an average mass loading factor (η) for the clumps of ∼1.8 − 2.4 consistent with results obtained from hydro-dynamical simulations of clumpy galaxies that assume relatively strong stellar feedback. Assuming no gas inflows (semi-closed box model), the estimates of η suggest that the timescale over which the outflows expel the molecular gas reservoir (≃ 7 × 108 M⊙) of the four detected low-mass clumps is ≲ 50 Myr.

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shiva: a dust destruction model

Murga

Wiebe

Sivkova

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a numerical tool Shiva designed to simulate the dust destruction in warm neutral, warm ionized, and hot ionized media under the influence of photo-processing, sputtering, and shattering. The tool is designed primarily to study the evolution of hydrogenated amorphous carbons (HACs), but options to simulate polycyclic aromatic hydrocarbons (PAHs), silicate and graphite grains are also implemented. HAC grain photo-processing includes both dehydrogenation and carbon atom loss. Dehydrogenation leads to material transformation from aliphatic to aromatic structure. Simultaneously, some other physical properties (band gap energy, optical properties, etc.) of the material change as well. The Shiva tool allows calculating the time-dependent evolution of the dust size distribution depending on hydrogen, helium, and carbon number densities and ionization state, gas temperature, radiation flux, relative gasdust and grain-grain velocities. For HAC grains the evolution of band gap energy distribution is also computed. We describe a dust evolution model, on which the tool relies, and present evolutionary time-scales for dust grains of different sizes depending on external conditions. This allows a user to estimate quickly a lifetime of a specific dust grain under relevant conditions. As an example of the tool usage, we demonstrate how grain properties and corresponding infrared spectra evolve in photo-dissociation regions, HII regions, and supernova remnant shocks.

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Relation between the parameters of dust and of molecular and atomic gas in extragalactic star-forming regions

Cited by 9 publications

References 42 publications

Star-forming complexes in the polar ring galaxy NGC660

Star-forming complexes in the polar ring galaxy NGC660

Stellar feedback in a clumpy galaxy at z ∼ 3.4

shiva: a dust destruction model

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