Searching for star-forming dwarf galaxies in the Antlia cluster

Văduvescu, O.; Kehrig, C.; Bassino, L. P.; Castelli, A. V. Smith; Calderón, Juan Pablo

doi:10.1051/0004-6361/201322615

Cited by 11 publications

(13 citation statements)

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“…The size of SF dwarfs from the LV and the nearby clusters has been known to scale with the absolute magnitudes (Vaduvescu et al , 2006(Vaduvescu et al , 2014. This linear trend seems to break above M SK = −19 for targets of more distant clusters, with most galaxies appearing larger at brighter luminosity end (Figs.…”

Section: Comparison and Interpretationmentioning

confidence: 88%

“…The popular large field NIR surveys 2MASS, VISTA VHS and UKIDSS LAS are pretty shallow and therefore affected by large photometric errors for dwarfs, as we pointed out in Sect. 4 and our past work (Vaduvescu et al , 2014. Deep spectroscopic surveys are even more scarce, with the SDSS remaining the main reference and being used in our paper to derive abundances of 17 galaxies in the A779, A1637, and Coma clusters.…”

Section: Sample Completenessmentioning

confidence: 98%

“…Following our past work (Vaduvescu et al 2006(Vaduvescu et al , 2011(Vaduvescu et al , 2014 one could model galaxy profiles of SF dwarfs (BCD candidates) with a sech law to account for the extended light associated with the older stellar population plus a Gaussian law to fit the inner starburst. Accordingly, the sech and Gaussian surface brightness components µ S and µ G at radius r are expressed as:…”

Section: Surface Photometrymentioning

confidence: 99%

“…Using available HI velocity line-widths which characterise the kinetic energy, another result was the apparent discovery of a "dwarf fundamental plane" (FP) which links luminosity to rotation and could be used as a distance indicator for dIs and BCDs located in the nearby universe (Vaduvescu & McCall 2008;McCall et al 2012). During the last years, we extended this study to other three nearby clusters: Fornax, Hydra (Vaduvescu et al 2011) and Antlia (Vaduvescu et al 2014). Nevertheless, the main problem remains the lack of radio detection of the very faint dIs and BCDs, especially at further distances.…”

Section: Introductionmentioning

confidence: 99%

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Studying star forming dwarf galaxies in Abell 779, Abell 1367, Coma, and Hercules clusters

Văduvescu

Petropoulou

Reverte

et al. 2018

A&A

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Context. We continue to study star formation in dwarf galaxies located in nearby clusters. Aims. Known physical and chemical relations outlining the formation and evolution of dwarfs is compared in different environments, including the Local Volume (LV) and some nearby clusters studied previously. Methods. We used the TNG telescope for four nights in 2010 to acquire deep near-infrared imaging in K of 45 star forming dwarf galaxies located in the Abell 779, Abell 1367, Abell 1656 (Coma), and Abell 2151 (Hercules) clusters. Results. Surface photometry was approached based on past experience by using the sech law to account for the outer old stellar contribution plus a Gaussian component to model the inner starburst, proving the blue compact dwarf (BCD) classification of most targets. Sech central surface brightness, semimajor axis, sech, and total apparent magnitude were measured, allowing to estimate size, absolute luminosity and mass for all targets. Conclusions. The physical correlations between size, central brightness, and NIR luminosity appear to hold, but previously known linear fits break above M SK = −19 for Abell 779, Abell 1367 and especially for Hercules, while the dwarf fundamental plane (FP) is probed by only half cluster members, suggesting harassment by the denser cluster environments. Nevertheless, the chemical relations between the oxygen abundance, luminosity, gas mass, baryonic mass, and gas fraction in a closed box model are probed by most members of the four studied clusters, and the starburst grows linearly with the K luminosity.

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Section: Comparison and Interpretationmentioning

confidence: 88%

Section: Sample Completenessmentioning

confidence: 98%

Section: Surface Photometrymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Studying star forming dwarf galaxies in Abell 779, Abell 1367, Coma, and Hercules clusters

Văduvescu

Petropoulou

Reverte

et al. 2018

A&A

Self Cite

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“…All objects with evident background morphology and/or central bars were also excluded from the present study as well as irregular or other star-forming galaxies, e.g. blue compact dwarfs (BCDs, Vaduvescu et al 2014). Fig.…”

Section: Original Samplementioning

confidence: 99%

Early-type galaxies in the Antlia Cluster: a deep look into scaling relations

Calderón

Bassino

Cellone

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present the first large-scale study of the photometric and structural relations followed by early-type galaxies (ETGs) in the Antlia cluster. Antlia is the third nearest populous galaxy cluster after Fornax and Virgo (d ∼ 35 Mpc). A photographic catalog of its galaxy content was built by Ferguson & Sandage in 1990 (FS90). Afterwards, we performed further analysis of the ETG population located at the cluster centre. Now, we extend our study covering an area four times larger, calculating new total magnitudes and colours, instead of isophotal photometry, as well as structural parameters obtained through Sérsic model fits extrapolated to infinity. Our present work involves a total of 177 ETGs, out of them 56 per cent have been cataloged by FS90 while the rest (77 galaxies) are newly discovered ones.Medium-resolution GEMINI and VLT spectra are used to confirm membership when available. Including radial velocities from the literature, 59 ETGs are confirmed as Antlia members.Antlia scaling relations mainly support the existence of unique functions (linear and curved) that join bright and dwarf ETGs, excluding compact ellipticals (cEs). Lenticular galaxies are outliers only with respect to the curved relation derived for effective surface brightness versus absolute magnitude. The small number of bright ellipticals and cEs present in Antlia, prevents us from testing if the same data can be fitted with two different linear sequences, for bright and dwarf ETGs. However, adding data from other clusters and groups, the existence of such sequences is also noticeable in the same scaling relations.

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Deep K-band surface brightness photometry of dE galaxies

Pintėr¹,

Văduvescu²

2023

A&A

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Context. Dwarf elliptical galaxies (dEs) are the most abundant in the Universe. Research into these objects in connection with late-type dwarf galaxies is important for evaluating theories of dwarf galaxy formation and evolution. Aims. Our past studies (2000-2010) suggested a possible evolutionary link between early- and late-type dwarf galaxies. These results are based on deep near-infrared (NIR) surface photometry data of dwarf irregulars (dIs), blue compact dwarfs (BCDs), and a small sample of Virgo dEs. As a continuation of those works, in 2017 we embarked on a study of dEs using the same surface photometry methods, with the aim being to compare early- and late-type dwarfs based on homogeneous datasets. Methods. We selected 74 dEs from two different environments for which we obtained deep images. Isophotal analysis was performed on the images to obtain surface brightness profiles. The two sampled environments were the Local Volume and Virgo cluster, which provide the possibility to compare isolated evolution against evolution in crowded environments. To compare dwarf datasets homogeneously, we used the NIR Ks band which is known to be a better gauge of galaxy mass, with reduced extinction compared to visible bands. Results. In this first paper, we derive apparent physical parameters for 72 dEs from deep NIR imaging and provide preliminary fitting results of their surface brightness profiles. Two targets were undetected in the Ks images, indicating possible misclassification. Physical parameters of 16 dEs are measured for the first time and the parameters of the remaining 56 dEs are compared with the literature. We obtain a mean difference between the measured physical parameters and the results from prior studies of about 0.2″ for the galaxy center coordinates, ≈20″ for the semi-major axis, ≈0.4 mag for the total apparent magnitude, ≈0.11 for the ellipticity, and ≈14° for the position angle. We find well-fitting surface brightness profiles for the dEs using the hyperbolic secant (sech) model combined with an exponential component. Alternatively, we find good agreement with observations for a sech plus a de Vaucouleurs law.

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Searching for star-forming dwarf galaxies in the Antlia cluster

Cited by 11 publications

References 50 publications

Studying star forming dwarf galaxies in Abell 779, Abell 1367, Coma, and Hercules clusters

Studying star forming dwarf galaxies in Abell 779, Abell 1367, Coma, and Hercules clusters

Early-type galaxies in the Antlia Cluster: a deep look into scaling relations

Deep K-band surface brightness photometry of dE galaxies

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