Physical conditions in the dwarf local irregular galaxy IC 10

Hidalgo-Gámez, A. M.

doi:10.1051/0004-6361:20041663

Cited by 14 publications

(20 citation statements)

References 36 publications

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“…Still, our results for the clump depth, between 0.75 to 0.90, imply that a significant fraction of ionizing photons is able to escape the clumps. Such results are compatible with the investigation performed by Hidalgo-Gámez (2005), that shows that the photons leaking from H ii regions, in addition to the ionisation provided by the WR stars, are responsable for the extended diffuse ionised gas in IC 10. This has implication for the PDRs, which are the neutral zones bordering only the radiationbounded clouds.…”

Section: Porosity Of the Ismsupporting

confidence: 92%

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Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC 10

Polles

Madden

Lebouteiller

et al. 2019

A&A

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Context. Star formation activity is an important driver of galaxy evolution and is influenced by the physical properties of the interstellar medium. Dwarf galaxies allow us to understand how the propagation of radiation and the physical conditions of the different ISM phases are affected by the low-metallicity environment. Aims. Our objective is to investigate the physical properties of the ionised gas of the low-metallicity dwarf galaxy, IC 10, at various spatial scales: from individual H ii regions to the entire galaxy scale and examine whether diagnostics for integrated measurements introduce bias in the results. Methods. We modeled the ionised gas combining the mid-and far-infrared fine-structure cooling lines observed with Spitzer/IRS and Herschel/PACS, with the photoionisation code Cloudy. The free parameters of the models are the age of the stellar cluster, the density and the ionisation parameter of the ionised gas as well as the depth of the cloud. The latter is used to investigate the leakage of the ionising photons from the analysed regions of IC 10. We investigate H ii regions in the main star-forming body, on scales of ∼25 pc, three in the main star-forming region in the center of the galaxy and two on the first arc. We then consider larger sizes on the scale of ∼200 pc. Results. Most clumps have nearly identical properties, density ∼10 2. -10 2.6 cm −3 , ionisation parameter between 10 −2.2 and 10 −1.6 and age of the stellar cluster ∼5.5 Myr. All of them are matter-bounded regions, allowing ionising photons to leak. The relatively uniform physical properties of the clumps suggest a common origin for their star formation activity, which could be related to the feedback from stellar winds or supernovae of a previous generation of stars. The properties derived for ∼200 pc size "zones" have similar properties as the H ii regions they encompass, but with the larger regions tending to be more radiation-bounded. Finally, we investigate the fraction of [CII] 157.7 µm , [SiII] 34.8 µm and [FeII] 25.9 µm emission arising from the ionised gas phase and we find that most of the emission originates from the neutral gas, not from the ionised gas.

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Section: Porosity Of the Ismsupporting

confidence: 92%

“…Supernova remnants and winds from WR stars have been identified as the main driver of the gas kinematics (Thurow & Wilcots 2005). The hard radiation from the WR stars, together with photons leaking from the H ii regions, are the sources of such extended ionised gas emission (Hidalgo-Gámez 2005).…”

Section: Overview Of Ic10mentioning

confidence: 99%

Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC 10

Polles

Madden

Lebouteiller

et al. 2019

A&A

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“…On the other hand, the DIG properties of irregular galaxies are not known very well, as very few galaxies have been studied so far. This small amount of data has prevented us from making any conclusions about their spectral characteristics (Martin 1997;Hidalgo-Gámez 2005;Hidalgo-Gámez & Peimbert 2006). However, these data show that the line ratios differ from those in spiral galaxies.…”

Section: Introductionmentioning

confidence: 95%

Diffuse Ionized Gas in Irregular Galaxies. I. GR 8 and ESO 245-G05

Hidalgo-Gámez¹

2006

Astron J

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We have studied the spectral characteristics of the diffuse ionized gas (DIG) in two irregular galaxies with low metallicities and intermediate star formation rates: ESO 245-G05 and GR 8. The [O iii]/H ratio in these galaxies is higher than in the DIG of spiral galaxies but not as high as in other irregular galaxies previously studied, such as IC 10 and NGC 6822. The [N ii]/H and [S ii]/ H ratios have very small values, indicating the absence of shocks as the ionization source for this gas. This ionization can be explained in both galaxies with photon leakage from the H ii regions as the only source. The percentage of photons that have escaped from the H ii regions is small in ESO 245-G05, only 35%, but varies from 35% up to 60% in GR 8. We also investigated whether the differences found between spiral and irregular galaxies in the [O iii]/H and the [N ii]/H ratios are due to differences in the metal content between these types of galaxies. Although the number of galaxies studied is not very large, it can be concluded that the [O iii]/ H ratio is not related to the oxygen content, while the situation is more ambiguous for the [N ii]/ H ratio.

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“…1 in Rosado et al (1999) and fig. 4 in Hidalgo-Gamez (2005) also point to the bright [S II] emission in the region.…”

Section: R E S U Lt S O F O B S E Rvat I O N Smentioning

confidence: 76%

A synchrotron superbubble in the IC 10 galaxy: a hypernova remnant?

Lozinskaya¹,

Моисеев

2007

Monthly Notices of the Royal Astronomical Society: Letters

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The nature of the synchrotron superbubble in the IC 10 galaxy is discussed using the results of our investigation of its ionized gas structure, kinematics and emission spectrum from observations made with the 6‐m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences, and based on our analysis of the radio emission of the region. The hypernova explosion is shown to be a more plausible mechanism of formation of the synchrotron superbubble compared with the earlier proposed model of multiple supernova explosions. A compact remnant of this hypernova may be identified with the well‐known X‐ray binary X‐1 – an accreting black hole.

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Physical conditions in the dwarf local irregular galaxy IC 10

Cited by 14 publications

References 36 publications

Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC 10

Modeling ionized gas in low-metallicity environments: the Local Group dwarf galaxy IC 10

Diffuse Ionized Gas in Irregular Galaxies. I. GR 8 and ESO 245-G05

A synchrotron superbubble in the IC 10 galaxy: a hypernova remnant?

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