English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present a detailed study of the dwarf galaxy VV124, recently recognized asa isolated member of the Local Group. We have obtained deep (r=26.5) wide-fieldg,r photometry of individual stars with the LBT under sub-arcsec seeingconditions. The Color-Magnitude Diagram suggests that the stellar content ofthe galaxy is dominated by an old, metal-poor population, with a significantmetallicity spread. A very clean detection of the RGB tip allows us to derivean accurate distance of D=1.3 +/- 0.1 Mpc. Combining surface photometry withstar counts, we are able to trace the surface brightness profile of VV124 outto ~ 5' = 1.9 kpc radius (where mu_r=30 mag/arcsec^2), showing that it is muchmore extended than previously believed. Moreover, the surface density mapreveals the presence of two symmetric flattened wings emanating from thecentral elongated spheroid and aligned with its major axis, resembling astellar disk seen nearly edge-on. We also present HI observations obtained withthe WSRT, the first ever of this object. A total amount of 10^6 M_sun of HI gasis detected in VV124. Compared to the total luminosity, this gives a value ofM_HI/L_V=0.11, which is particularly low for isolated Local Group dwarfs. Thespatial distribution of the gas does not correlate with the observed stellarwings. The systemic velocity of the HI in the region superposed to the stellarmain body of the galaxy is V_h=-25 km/s. The velocity field shows substructurestypical of galaxies of this size but no sign of rotation. The HI spectraindicates the presence of a two-phase interstellar medium, again typical ofmany dwarf galaxies.

An optical and HI study of the dwarf Local Group galaxy VV124=UGC4879. A gas-poor dwarf with a stellar disk?