The AGB population in IC 1613 using<i>JHK</i>photometry

Sibbons, L. F.; Ryan, Sean G.; Irwin, M. J.; Napiwotzki, R.

doi:10.1051/0004-6361/201423982

Cited by 19 publications

(53 citation statements)

References 73 publications

(168 reference statements)

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“…Their estimated C/M ratio was 0.53, which is higher than our C/M ratio. One of the most interesting results reported by Sibbons et al (2015) is the radial distribution of the C/M radio and the inferred metallicity with a positive radial gradient, which is in contrast to our result. The differences between our results and those of Sibbons et al (2015) seem to be due to the different methods and color limits that were used to identify of AGB stars in a galaxy.…”

Section: Importance Of the Selection Criteria For C Stars And M-giantcontrasting

confidence: 99%

“…Our C/M ratio is lower than the previous result of 0.64 (Albert et al 2000), while is consistent with 0.52 ± 0.04 (Sibbons et al 2015) when we consider the 1σ error. We attribute the difference between our results and the previous results to the method for defining the M-giant stars and C stars and the difference in the observed field of view for IC 1613.…”

Section: Spatial Distributions Of the C And M-giant Stars C/m Ratiosupporting

confidence: 90%

“…This metallicity value is not much different from the previous results for the metallicity of IC 1613 (Freedman 1988;Cole et al 1999;Zucker & Wyder 2004). More recently, Sibbons et al (2015) also derived the metallicity of [Fe/H] = −1.26±0.07 for IC 1613 from their C/M ratio. In our previous studies, the C/M ratios of three dwarf elliptical galaxies and one dwarf irregular galaxy were estimated as 0.11 ± 0.01 for NGC 185 (Kang et al 2005), 0.16 ± 0.02 for NGC 147 , 0.15 ± 0.01 for NGC 205 (Jung et al 2012), and 0.27 ± 0.03 for NGC 6822 .…”

Section: Spatial Distributions Of the C And M-giant Stars C/m Ratiomentioning

confidence: 99%

“…Recently, Sibbons et al (2015) investigated the AGB stars in IC 1613 using near-infrared imaging data obtained from UKIRT. They identified 843 AGB stars of which they classified 291 as A51, page 10 of 12 C stars and 552 as M-giant stars.…”

Section: Importance Of the Selection Criteria For C Stars And M-giantmentioning

confidence: 99%

“…On the other hand, Albert et al (2000) classified 195 C stars using narrow CN and TiO band photometry data and found that the C stars were displayed up to 15 from the center of the galaxy. Sibbons et al (2015) also investigated the distribution of the AGB stars in IC 1613, derived an average C/M ratio, and inferred a metal abundance [Fe/H] of −1.26 ± 0.07 from the C/M ratio.…”

Section: Introductionmentioning

confidence: 99%

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Near-infrared photometric properties of asymptotic giant branch stars in the dwarf irregular galaxy IC 1613

Chun

Jung

Kang

et al. 2015

A&A

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Aims. We investigated the photometric properties of asymptotic giant branch (AGB) stars of the dwarf irregular galaxy IC 1613 and its metallicity. Methods. We used near-infrared JHK s photometric data obtained with the WIRCam array on Canada-France-Hawaii Telescope (CFHT). The optical gi imaging data of a previous study were cross-matched with ours to distinguish the stellar populations in the galaxy and to select the AGB stars. We also separated the C stars from the M-giant stars in the JHK s color−color diagram. Results. We identified 140 C stars and 306 M-giant stars in IC 1613. The (J − K s ) color histogram of AGB stars shows the main peak of M-giant stars and the red tail of C stars. The broad color distribution of M-giant stars and the isochrones in the color magnitude diagram indicate that IC 1613 has a wide range of intermediate-age stars. We also know that most C stars were formed over the past 2−8 Gyr according the M bol -age relation. The C/M ratio of 0.46 ± 0.05 was estimated and [Fe/H] abundance of −1.23 ± 0.06 was derived from the C/M ratio. Radial distributions of C/M ratio and metallicity show the shallow trend of the negative metallicity gradient from the center. The local C/M ratio also indicates that the HI cavity has higher C/M values than the bright HI spot and HI gas region. However, the low [Fe/H] value near the central region of the galaxy is likely to be caused by the change in age of the dominant stellar population according to the radial distance, not the real metallicity variation. It might also be that relatively younger and metal-rich C stars are concentrated in the center of the galaxy, while the M-giant stars were homogeneously distributed from the center to the borders of the galaxy.

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Section: Importance Of the Selection Criteria For C Stars And M-giantcontrasting

confidence: 99%

Section: Spatial Distributions Of the C And M-giant Stars C/m Ratiosupporting

confidence: 90%

Section: Spatial Distributions Of the C And M-giant Stars C/m Ratiomentioning

confidence: 99%

Section: Importance Of the Selection Criteria For C Stars And M-giantmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Near-infrared photometric properties of asymptotic giant branch stars in the dwarf irregular galaxy IC 1613

Chun

Jung

Kang

et al. 2015

A&A

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The formation and cosmic evolution of dust in the early Universe: I. Dust sources

Schneider,

Maiolino

2024

Astron Astrophys Rev

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Dust-obscured star formation has dominated the cosmic history of star formation, since $$z \simeq 4$$ z ≃ 4 . However, the recent finding of significant amount of dust in galaxies out to $$z \simeq 8$$ z ≃ 8 has opened the new frontier of investigating the origin of dust also in the earliest phases of galaxy formation, within the first 1.5 billion years from the Big Bang. This is a key and rapid transition phase for the evolution of dust, as galaxy evolutionary timescales become comparable with the formation timescales of dust. It is also an area of research that is experiencing an impressive growth, especially thanks to the recent results from cutting edge observing facilities, ground-based, and in space. Our aim is to provide an overview of the several findings on dust formation and evolution at $$z > 4$$ z > 4 , and of the theoretical efforts to explain the observational results. We have organized the review in two parts. In the first part, presented here, we focus on dust sources, primarily supernovae and asymptotic giant branch stars, and the subsequent reprocessing of dust in the interstellar medium, through grain destruction and growth. We also discuss other dust production mechanisms, such as Red Super Giants, Wolf–Rayet stars, Classical Novae, Type Ia Supernovae, and dust formation in quasar winds. The focus of this first part is on theoretical models of dust production sources, although we also discuss the comparison with observations in the nearby Universe, which are key to put constraints on individual sources and processes. While the description has a general applicability at any redshift, we emphasize the relative role of different sources in the dust build-up in the early Universe. In the second part, which will be published later on, we will focus on the recent observational results at $$z > 4$$ z > 4 , discussing the theoretical models that have been proposed to interpret those results, as well as the profound implications for galaxy formation.

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Physical parameters of red supergiants in dwarf irregular galaxies in the Local Group

Britavskiy

Bonanos

Herrero

et al. 2019

A&A

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Context. Increasing the statistics of evolved massive stars in the Local Group enables investigating their evolution at different metallicities. During the late stages of stellar evolution, the physics of some phenomena, such as episodic and systematic mass loss, are not well constrained. For example, the physical properties of red supergiants (RSGs) in different metallicity regimes remain poorly understood. Thus, we initiated a systematic study of RSGs in dwarf irregular galaxies (dIrrs) in the Local Group. Aims. We aim to derive the fundamental physical parameters of RSGs and characterize the RSG population in nearby dIrrs. Methods. The target selection is based on 3.6 µm and 4.5 µm photometry from archival Spitzer Space Telescope images of nearby galaxies. We selected 46 targets in the dIrrs IC 10, IC 1613, Sextans B, and the Wolf-Lundmark-Melotte (WLM) galaxy that we observed with the GTC-OSIRIS and VLT-FORS2 instruments. We used several photometric techniques together with a spectral energy distribution analysis to derive the luminosities and effective temperatures of known and newly discovered RSGs. Results. We identified and spectroscopically confirmed 4 new RSGs, 5 previously known RSGs, and 5 massive asymptotic giant branch (AGB) stars. We added known objects from previous observations. In total, we present spectral classification and fundamental physical parameters of 25 late-type massive stars in the following dIrrs: Sextans A, Sextans B, IC 10, IC 1613, Pegasus, Phoenix, and WLM. This includes 17 RSGs and 8 AGB stars that have been identified here and previously. Conclusions. Based on our observational results and PARSEC evolutionary models, we draw the following conclusions: (i) a trend to higher minimum effective temperatures at lower metallicities and (ii) the maximum luminosity of RSGs appears to be constant at log(L/L ) ≈ 5.5, independent of the metallicity of the host environment (up to [Fe/H] ≈ −1 dex).

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The AGB population in IC 1613 usingJHKphotometry

Cited by 19 publications

References 73 publications

Near-infrared photometric properties of asymptotic giant branch stars in the dwarf irregular galaxy IC 1613

Near-infrared photometric properties of asymptotic giant branch stars in the dwarf irregular galaxy IC 1613

The formation and cosmic evolution of dust in the early Universe: I. Dust sources

Physical parameters of red supergiants in dwarf irregular galaxies in the Local Group

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