UGC 3672: an unusual merging triplet of gas-rich galaxies in the Lynx–Cancer void

Chengalur, Jayaram N.; Pustilnik, S. A.; Egorova, E. S.

doi:10.1093/mnras/stw2841

Cited by 22 publications

(25 citation statements)

References 76 publications

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“…Hence, it can be really a very young object that formed its main stellar population not earlier than ∼1-2 Gyr ago. Several similar type very gas-rich 'unevolved' dwarfs were already found among the Lynx-Cancer void least massive galaxies Chengalur, Pustilnik 2013;Chengalur et al 2016).…”

Section: Introductionmentioning

confidence: 62%

“…One is SDSS J070623.43+302051.3 (a companion of UGC 3672) at the comparable distance of ∼17 Mpc, with the tentative record-low oxygen abundance of 12+log(O/H)=7.03 (Pustilnik, Perepelitsyna, Kniazev 2016;Chengalur et al 2016). Its star-forming region is much less prominent than those in IZw18.…”

Section: The List Of the Most Luminous Extremely Metal-poor Star In Dmentioning

confidence: 99%

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The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

Pustilnik¹,

Макарова²,

Perepelitsyna³

et al. 2016

Mon. Not. R. Astron. Soc.

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The paper presents new results of the ongoing study of the unusual Lynx-Cancer void galaxy DDO 68 with record-low-metallicity regions (12+log(O/H)∼7.14) of the current star formation (SF). They include: a) a new spectrum and photometry with the 6-m SAO RAS telescope (BTA) for the Luminous Blue Variable (LBV = DDO68-V1). Photometric data sets are complemented with those based on the Sloan Digital Sky Survey (SDSS) and the Hubble Space Telescope (HST) archive images; b) the analysis of the DDO 68 supergiant shell (SGS) and the prominent smaller Hα arcs/shells visible at the HST image coupled with kinematics maps in Hα obtained with the Fabry-Perot interferometer (FPI) at the BTA; c) the list of identified at the HST images of about 50 most luminous stars (−9.1 < M V < −6.0 mag) related to star-forming regions with the known extremely low O/H. This is intended to pave the path for the actual science with the next generation of giant telescopes. We confirm the earlier hints on significant variations of the LBV optical light deriving its amplitude of ∆V 3.7 mag for the first time. New data suggest that in 2008-2010 the LBV reached M V = -10.5 and probably underwent a giant eruption. We argue that the structure of star-forming complexes along the SGS ('Northern Ring') perimeter provides evidence for the sequential induced SF episodes caused by the shell gas instabilities and gravitational collapse. The variability of some DDO 68 luminous extremely metal-poor stars can be monitored with medium-size telescopes at sites with superb seeing.

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Section: Introductionmentioning

confidence: 62%

Section: The List Of the Most Luminous Extremely Metal-poor Star In Dmentioning

confidence: 99%

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

Pustilnik¹,

Макарова²,

Perepelitsyna³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Besides, it appeared that the substantial fraction of the faintest LSB dwarfs in the Lynx-Cancer void (mostly those with MB −13.5 mag) show the very low O/H, extremely high gas mass fraction and blue colour of stars at the galaxy periphery. These properties indicate the atypical young evolutionary status of such LSB dwarfs (Pustilnik et al 2010;Chengalur, Pustilnik 2013;Pustilnik et al 2013Chengalur, Pustilnik, Egorova 2017).…”

Section: Introductionmentioning

confidence: 99%

Void galaxies in the nearby Universe – I. Sample description

Pustilnik

Tepliakova

Макаров

2018

Monthly Notices of the Royal Astronomical Society

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The main goal of this work is to form a large, deep and representative sample of dwarf galaxies residing in voids of the nearby Universe. The formed sample is the basement for the comprehensive mass study of the galaxy content, their evolutionary status, clustering and dynamics with respect to their counterparts residing in more typical, denser regions and for study of void small-scale substructures. We present 25 voids over the entire sky within 25 Mpc from the Local Group. They are defined as groups of lumped empty spheres bounded by 'luminous' galaxies with the absolute K-band magnitudes brighter than -22.0. The identified void regions include the Local Void and other known nearby voids. The nearest nine voids occupy a substantial part of the Local Volume. Of the total number of 6792 cataloged galaxies in the considered volume, 1354 objects fall into 25 nearby voids. Of this general void galaxy sample, we separate the sub-sample of 'inner' void galaxies, residing deeper in voids, with distances to the nearest luminous galaxy D NN 2.0 Mpc. The 'inner' galaxy sample includes 1088 objects, mostly dwarfs with M B distribution peaked near -15.0 and extending down to -7.5 mag. Of them, 195 fall in the Local Volume (space within R=11 Mpc). We present the general statistical properties of this Nearby Void Galaxy sample and discuss the issues related to the sample content and the prospects of its use.

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“…The few exceptions are the following. For J0706+3620 and UGC 3672, their B magnitudes are adopted from Chengalur et al (2016). For J0736+0959, its B magnitude is adopted from the recent photometry in Haurberg et al (2015).…”

Section: Discussionmentioning

confidence: 99%

Study of galaxies in the Lynx-Cancer void

Pustilnik

Martin

2016

A&A

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Context. Void population consists mainly of late-type and low surface brightness (LSB) dwarf galaxies whose atomic hydrogen is the main component of their baryonic matter. Therefore, observations of void galaxy Hi are mandatory in order to understand their evolution and dynamics. Aims. Our aim was to obtain integrated Hi parameters for a fainter part of the nearby Lynx-Cancer void galaxy sample (total of 45 objects) with the Nançay Radio Telescope (NRT) and to conduct the comparative analysis of all the 103 void galaxies with known Hi data with a sample of similar galaxies residing in denser environments of the Local Volume. Methods. For Hi observations we used the NRT with its sensitive antenna/receiver system FORT and standard processing. The comparison of the void and control samples on the parameter M(HI)/L B is conducted with the non-parametric method , "The 2×2 Contingency Table test". Results. We obtained new Hi data for about 40 % of the Lynx-Cancer galaxy sample. Along with data from the literature, we use these new data for further analysis of 103 void objects. The proxy of the evolutional parameter M(HI)/L B of the void sample is compared with that of 82 galaxies of morphological types 8-10 residing in the Local Volume (LV) groups and aggregates. Conclusions. At the confidence level of P = 0.988, we conclude that for the same luminosity, these void galaxies are systematically gas-richer, on average by ∼39%. This result is consistent with the authors' earlier conclusion on the smaller gas metallicities and evidence for the slower low-mass galaxy evolution in voids.

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UGC 3672: an unusual merging triplet of gas-rich galaxies in the Lynx–Cancer void

Cited by 22 publications

References 76 publications

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

The extremely metal-poor galaxy DDO 68: the luminous blue variable, Hα shells and the most luminous stars

Void galaxies in the nearby Universe – I. Sample description

Study of galaxies in the Lynx-Cancer void

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