Updated Nearby Galaxy Catalog

Abstract

We present an all-sky catalog of 869 nearby galaxies, having individual distance estimates within 11 Mpc or corrected radial velocities V LG < 600 km s −1 .The catalog is a renewed and expanded version of the "Catalog of Neighboring Galaxies" by Karachentsev et al. (2004). It collects data on the following observables for the galaxies: angular diameters, apparent magnitudes in F UV -, B-, and K s -bands, Hα and HI fluxes, morphological types, HI-line widths, radial velocities and distance estimates. In this Local Volume (LV) sample 108 dwarf galaxies remain to be still without measured radial velocities.The catalog yields also calculated global galaxy parameters: linear Holmberg diameter, absolute B-magnitude, surface brightness, HI-mass, stellar mass estimated via K-band luminosity, HI rotational velocity corrected for galaxy inclination, indicative mass within the Holmberg radius, and three kinds of "tidal index", which quantify the local density environment. The catalog is supplemented with the data based on the local galaxies (http://www.sao.ru/lv/lvgdb), which presents their optical and available Hα images, as well as other service.We briefly discuss the Hubble flow within the LV, and different scaling relations that characterize galaxy structure and global star formation in them. We also trace the behavior of the mean stellar mass density, HI-mass density and star formation rate density within the considered volume.

Cold H i in faint dwarf galaxies

“…9. The global Hα and FUV SFR used in the plots were taken from the Updated Nearby Galaxy Catalogue (UNGC) (Karachentsev, Makarov & Kaisina 2013). From the plots it is clear that brighter galaxies with more HI mass and higher star formation rates contain more cold HI .…”

“…1. The columns of the table are: col(1): Name of the galaxy, col(2): Other major surveys as part of which the galaxy was observed in HI , col(3): Right Ascention (J2000), col(4): Declination (J2000), col(5): the distance to the galaxy in Mpc (taken from (Karachentsev, Makarov & Kaisina 2013)) col(6): the method by which the distance is estimated, col(7): The absolute blue magnitude (MB) (again taken from (Karachentsev, Makarov & Kaisina 2013)) col(8): The log of HI mass of the galaxy, col(9): Optical inclination of the galaxy, column(10) indicates if the galaxy is included in the sample used for detecting the CNM via the Gaussian Decomposition method (see Sec.3), column(11) indicates if the galaxy is included in the sample for detecting the CNM via the Brightness Temperature (TB ) method (see Sec.4), col(12) the velocity resolution used to image the galaxy at ∼ 100 pc (as required for the TB method).…”

“…The columns are as follows: Col. (1) Galaxy name, Col. (2) and 3) the equatorial coordinates (J2000), Col. (4) and (5) log of HI mass and absolute blue magnitude, Col. (6) inclination taken from (Karachentsev, Makarov & Kaisina 2013). They have been computed from the axial ratio of the optical disc, and the typical error is ∼ 10%.…”

“…Galaxies with available Hα data are marked with superscript 3 whereas 4 represents galaxies with available FUV star formation maps. The data in table 6 were taken from (Karachentsev, Makarov & Kaisina 2013).…”

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

“…While dIs are mostly observed as more quiescent entities in isolation or loose groups including the Local Group (e.g. Mateo 1998;Karachentsev et al 2013), BCDs are encountered mostly in denser environment and galaxy clusters and harbour starburst possibly triggered by strong environmental influences (e.g. Vilchez 1995;Meyer et al 2014).…”