Ultraviolet Imaging Telescope View of Dwarf Irregular Galaxy IC 2574: Is the Star Formation Triggered Due to Expanding H i Shells?

Mondal, Chayan; Subramaniam, Annapurni; George, Koshy

doi:10.3847/1538-3881/ab4ea1

Cited by 9 publications

(4 citation statements)

References 67 publications

(87 reference statements)

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“…The O abundance deduced from the spectra of HII regions is consistent with its M B (Miller & Hodge 1996). Mondal et al (2019) find evidence of on-going star formation throughout the galaxy. Pasquali et al (2008) examine the photometric properties of IC 2574, and find that there is a dominant 100 Myr population within the central 4 kpc, with a 10 Myr population at galactocentric radii between 4 and 8 kpc.…”

Section: Introductionsupporting

confidence: 69%

Red Variable Stars in Three M81 Group Dwarf Galaxies

Davidge

2022

Preprint

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Archival [3.6] and [4.5] images are used to identify and characterize variable stars in the Magellanic-type galaxies Holmberg II, NGC 2366, and IC 2574. Using parametric and non-parametric detection methods, 74 confirmed or suspected long period variables (LPVs) are found. The period distributions of the LPVs in NGC 2366 and IC 2574 are similar. While the period distribution of LPVs in Ho II is uncertain due to small number statistics there appears to be a deficiency of LPVs with periods between 550 and 650 days when compared with NGC 2366 and IC 2574. The LPVs are diffusely distributed on the sky, and do not follow the underlying light from unresolved stars, as expected if episodes of star formation within the past few hundred Myr have occured throughout the galaxies, including their outer regions. Distances computed for Ho II and NGC 2366 from the period-luminosity relations (PLRs) agree to within ∼ 0.1 magnitudes with those based on the tip of the red giant branch (RGB). Efforts to estimate an LPV-based distance modulus for IC 2574 are complicated by the presence of first overtone pulsators among LPVs with periods ∼ 600 days, although the PLR at the long period end is consistent with the distance estimated from the RGB-tip. In addition to the LPVs, 10 candidate sgB[e] or luminous blue variables and 2 candidate red supergiant variables are also identified. Nine candidate sgB[e] stars that do not show evidence of variability are also identified based on their locations in the color-magnitude diagram.

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Section: Introductionsupporting

confidence: 69%

Red Variable Stars in Three M81 Group Dwarf Galaxies

Davidge

2022

Preprint

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“…The characteristic size is larger than the mean and peak of our size distribution, but similar to many of those listed in Table 4. Mondal et al (2019) studied the dwarf irregular galaxy IC 2574 (3.79 Mpc) and identified 419 bright far-UV groups. With a resolution limit of 15 pc, they found that their groups have radii of 15-285 pc and they identified some of them with stellar associations.…”

Section: Comparisons With Past Work On Other Galaxiesmentioning

confidence: 99%

The VMC survey – XLVII. Turbulence-controlled hierarchical star formation in the Large Magellanic Cloud

Miller

Cioni

Grijs

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We perform a statistical clustering analysis of upper main-sequence stars in the Large Magellanic Cloud (LMC) using data from the Visible and Infrared Survey Telescope for Astronomy survey of the Magellanic Clouds. We map over 2500 young stellar structures at 15 significance levels across ∼120 square degrees centred on the LMC. The structures have sizes ranging from a few parsecs to over 1 kpc. We find that the young structures follow power-law size and mass distributions. From the perimeter–area relation, we derive a perimeter–area dimension of 1.44 ± 0.20. From the mass–size relation and the size distribution, we derive two-dimensional fractal dimensions of 1.50 ± 0.10 and 1.61 ± 0.20, respectively. We find that the surface density distribution is well-represented by a lognormal distribution. We apply the Larson relation to estimate the velocity dispersions and crossing times of these structures. Our results indicate that the fractal nature of the young stellar structures has been inherited from the gas clouds from which they form and that this architecture is generated by supersonic turbulence. Our results also suggest that star formation in the LMC is scale-free from 10 pc to 700 pc.

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“…Hi is the primary requirement for star formation as it can cool and form molecular hydrogen in dense complexes (Prochaska & Wolfe 2009;Obreschkow et al 2016). The connection between Hi and star formation has also been explored for different galactic environments, including the outer disks of galaxies (Bigiel et al 2010a,b;Mondal et al 2019). Hence, we expect to see an association of Hi with star formation for our FUV images.…”

Section: Uv Correlation With Himentioning

confidence: 72%

“…The Hi gas and star formation correlation has also been explored in different galactic environments, such as the outer parts of galaxies. It is similar in nature but has a steeper slope (Bigiel et al 2010a,b;Mondal et al 2019). The much lower star formation efficiencies (SFEs Bigiel et al 2010b) suggests that the nature of star formation in such environments may be different from the inner disks.…”

Section: Introductionmentioning

confidence: 99%

Comparing the Inner and Outer Star Forming Complexes in the Nearby Spiral Galaxies NGC 628, NGC 5457 and NGC 6946 using UVIT Observations

Yadav,

Das,

Patra

et al. 2021

Preprint

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We present a far-UV (FUV) study of the star-forming complexes (SFCs) in three nearby galaxies using the Ultraviolet Imaging Telescope (UVIT). The galaxies are close to face-on and show significant outer disk star formation. Two of them are isolated (NGC 628, NGC 6946), and one is interacting with distant companions (NGC 5457). We compared the properties of the SFCs inside and outside the optical radius (R 25 ). We estimated the sizes, star formation rates (SFRs), metallicities, and the Toomre Q parameter of the SFCs. We find that the outer disk SFCs are at least ten times smaller in area than those in the inner disk. The SFR per unit area (Σ SF R ) in both regions have similar mean values, but the outer SFCs have a much smaller range of Σ SF R . They are also metal-poor compared to the inner disk SFCs. The FUV emission is well correlated with the neutral hydrogen gas (Hi) distribution and is detected within and near several Hi holes. Our estimation of the Q parameter in the outer disks of the two isolated galaxies suggests that their outer disks are stable (Q>1). However, their FUV images indicate that there is ongoing star formation in these regions. This suggests that there may be some non-luminous mass or dark matter in their outer disks, which increases the disk surface density and supports the formation of local gravitational instabilities. In the interacting galaxy, NGC 5457, the baryonic surface density is sufficient (Q<1) to trigger local disk instabilities in the outer disk.

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Ultraviolet Imaging Telescope View of Dwarf Irregular Galaxy IC 2574: Is the Star Formation Triggered Due to Expanding H i Shells?

Cited by 9 publications

References 67 publications

Red Variable Stars in Three M81 Group Dwarf Galaxies

Red Variable Stars in Three M81 Group Dwarf Galaxies

The VMC survey – XLVII. Turbulence-controlled hierarchical star formation in the Large Magellanic Cloud

Comparing the Inner and Outer Star Forming Complexes in the Nearby Spiral Galaxies NGC 628, NGC 5457 and NGC 6946 using UVIT Observations

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