Stellar Content and Recent Star Formation History of the Local Group Dwarf Irregular Galaxy IC 1613

Bernard, Edouard J.; Aparicio, A.; Gallart, Carme; Torres, Carmen P. Padilla; Panniello, M.

doi:10.1086/520805

Cited by 39 publications

(58 citation statements)

References 38 publications

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“…A distance of 4−4.5 kpc from the galactic centre translates into an angular distance of 18−20 at a distance of 758 kpc. These measurements are consistent with previous estimates by Bernard et al (2007) who report the detection of RGB stars out to r > 16.5 and Battinelli et al (2007a) who found that the density profile of giant stars, mainly on the RGB, declined to zero at r ∼ 23 . Battinelli et al (2007a) also confirmed the findings of Tikhonov & Galazutdinova (2002) that no giants belonging to IC 1613 are seen in the HST archive images at 27 and 33 , ∼6 and ∼7 kpc respectively.…”

Section: Stellar Density Profilessupporting

confidence: 93%

The AGB population in IC 1613 usingJHKphotometry

Sibbons

Ryan

Irwin

et al. 2014

A&A

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Context. A member of the Local Group, IC 1613 is a gas rich irregular dwarf galaxy that appears to have formed stars continuously over the last 10 Gyr and is relatively independent of external influences from other galaxies. Aims. This paper aims to study the spatial distribution of the asymptotic giant branch (AGB) population in IC 1613 and its metallicity. Methods. Using WFCAM on UKIRT, high quality JHK photometry of an area of 0.8 deg 2 centered on IC 1613 was obtained. The data have been used to isolate the C-and M-type components of the AGB population and using their number ratio, C/M, a global mean metallicity has been derived. The metallicity and the tip of the red giant branch magnitude (TRGB) have been studied as a function of distance from the galactic centre and as a function of azimuthal angle. Results. The TRGB has been found to be at K 0 = 18.25 ± 0.15 mag. The colour separation between the C-and M-type components of the AGB population has been located at (J − K) 0 = 1.15 ± 0.05 mag, giving a global C/M ratio of 0.52 ± 0.04 and from this an iron abundance of [Fe/H] = −1.26 ± 0.07 dex has been calculated. Conclusions. The AGB population has been detected out to a radial distance of 4.5 kpc in the de-projected plane of the galaxy. The measured TRGB is consistent with previous measurements and no significant variation is detected in the TRGB or in metallicity either with galactocentric distance or azimuthal angle.

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Section: Stellar Density Profilessupporting

confidence: 93%

The AGB population in IC 1613 usingJHKphotometry

Sibbons

Ryan

Irwin

et al. 2014

A&A

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“…These models provide metallicity in terms of the total metallicity, Z, that when converted to iron represents an upper limit. The error in [Fe/H] given in Table B.1 coincides with the FWHM of the RGB colour from Bernard et al (2007). A similar study has been done recently in M31 resulting in [Fe/H] = −0.83 dex (Brown et al 2008).…”

Section: Appendix B: C/m Versus [Fe/h] Calibrationsupporting

confidence: 84%

The metallicity gradient as a tracer of history and structure: the Magellanic Clouds and M33 galaxies

Cioni¹

2009

A&A

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Context. The stellar metallicity and its gradient place constraints on the formation and evolution of galaxies. Aims. This is a study of the metallicity gradient of the LMC, SMC and M33 galaxies derived from their asymptotic giant branch (AGB) stars. Methods. The [Fe/H] abundance was derived from the ratio between C-and M-type AGB stars and its variation analysed as a function of galactocentric distance. Galaxy structure parameters were adopted from the literature.Results. The metallicity of the LMC decreases linearly as −0.047± 0.003 dex kpc −1 out to ∼8 kpc from the centre. In the SMC, [Fe/H] has a constant value of ∼−1.25 ± 0.01 dex up to ∼12 kpc. The gradient of the M33 disc, until ∼9 kpc, is −0.078 ± 0.003 dex kpc −1 while the outer disc/halo, out to ∼25 kpc, has [Fe/H] ∼ −1.7 dex. Conclusions. The metallicity of the LMC, as traced by different populations, bears the signature of two major star forming episodes: the first one constituting a thick disc/halo population and the second one a thin disc and bar due to a close encounter with the Milky Way and SMC. The [Fe/H] of the recent episode supports an LMC origin for the Stream. The metallicity of the SMC supports star formation, ∼3 Gyr ago, as triggered by LMC interaction and sustained by the bar in the outer region of the galaxy. The SMC [Fe/H] agrees with the present-day abundance in the Bridge and shows no significant gradient. The metallicity of M33 supports an "insideout" disc formation via accretion of metal poor gas from the interstellar medium.

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“…The stellar component of IC 1613 is known to extend little farther than 16 .5 from its centre (Bernard et al 2007). The optically brightest part is well separated into 2 regions by a central strip of H i, usually referred to as "the bar".…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

“…Sandage (1971) presented the first catalogue of targets in IC 1613, based on Baade's work on photographic plates. Subsequent photometric studies with ever improved detectors also analysed the galaxy's population from color-magnitude diagrams (Hodge 1978(Hodge , 1980Freedman 1988;Hodge et al 1991;Tikhonov & Galazutdinova 2002;Bernard et al 2007;Battinelli et al 2007, among others). The DM is well known from numerous studies of Cepheids and RR Lyrae (see for instance Udalski et al 2001).…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

The young stellar population of IC 1613

García¹,

Herrero

Vicente³

et al. 2009

A&A

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Context. Determining the parameters of massive stars is crucial to understand many processes in galaxies and the Universe, since these objects are important sources of ionization, chemical enrichment and momentum. 10m class telescopes enable us to perform detailed quantitative spectroscopic analyses of massive stars in other galaxies, sampling areas of different metallicity. Relating the stars to their environment is crucial to understand the physical processes ruling their formation and evolution. Aims. In preparation for the new instrumentation planned for the Gran Telescopio CANARIAS (GTC), our goal is to build a list of massive star candidates in the metal-poor irregular galaxy IC 1613. The catalogue must have very high astrometric accuracy, suitable for the current generation of multi-object spectrographs. A census of OB associations in this galaxy is also needed, to provide important additional information about the age and environment of the candidate OB stars. Methods. From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friendsof-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context. Results. We have produced a deep catalogue of targets in IC 1613 that covers a large field of view. To achieve high astrometric accuracy, a new astrometric procedure was developed for the INT-WFC data. We also built a catalogue of OB associations in IC 1613 and found that they concentrate in the central regions, especially in the H ii bubbles. The study of extinction confirms that it is patchy, with local values of color-excess above the foreground value.

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Stellar Content and Recent Star Formation History of the Local Group Dwarf Irregular Galaxy IC 1613

Cited by 39 publications

References 38 publications

The AGB population in IC 1613 usingJHKphotometry

The AGB population in IC 1613 usingJHKphotometry

The metallicity gradient as a tracer of history and structure: the Magellanic Clouds and M33 galaxies

The young stellar population of IC 1613

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