However, we emphasize that we only use the aperture photometry of the individual interacting galaxies to calculate their mass ratios. Star formation rate vs. blue-band absolute magnitude. Despite their low luminosity, they may contain large amounts of dark matter, and thus contribute greatly to the mass of the Universe. For all images, the black horizontal bar represents a scale of 30''. To date, no systematic effort has been made to present a sample of interacting dwarf galaxies that is statistical enough to study the properties of interacting dwarf galaxies and their roles in the evolution of low-mass galaxies. Low-mass galaxies are also typically dominated by exponential disks. In these cases, we perform aperture photometry on the GALEX image, following the same procedure we used for the optical images. In these cases, we use images from the Legacy survey. The black dot represents the satellite candidates and blue dots represent isolated candidates. 2016). The stellar masses of candidate galaxies in this sample are measured from our own photometric measurements as described in Section 3. It is not surprising that this sample is somewhat biased toward the brighter end of our stellar mass cut. The Astrophysical Journal Supplement Series, https://www.sdss.org/collaboration/#acknowledgements, A Case Study for a Tidal Interaction between Dwarf Galaxies in UGC 6741, The Next Generation Virgo Cluster Survey. 2017). For this, we also removed those merging dwarf systems that have a line-of-sight radial velocity of less than 900 km s−1 to avoid distance uncertainties of nearby galaxies. The number of early-type galaxies is only 3 out of 177. To do this, we measure the total flux using a large aperture that covers both interacting galaxies and the stellar streams around them. We classify them, according to observed low-surface-brightness features, into various categories including shells, stellar streams, loops, antennae, or simply interacting. A dwarf galaxy indeed. However, for dwarf galaxies, a 10 km s−1 velocity dispersion can make a significant contribution to the internal dynamics. These different types of low-surface-brightness features may hint at the different stages objects undergo during their interactions. 2004; Yozin & Bekki 2012). 2013; Paudel & Ree 2014). 2018, in preparation). There are three dwarf galaxy systems (Id0202-0922, Id1448-0342, Id14503534) that can be considered dwarf analogs to the Antennae system (NGC 4038/4039). This is likely because such systems are not as easy to observe as in massive systems. In addition to this, Paudel et al. Figure 6 illustrates the relation between the B-band absolute magnitude and the SFR. A dwarf analog of the famous Antennae system (NGC 4038/NGC 4039) is represented by "A" (for Antennae e.g., Id0202-0922). A potential problem with these types of catalogs is that they are inherently inhomogeneous and incomplete. This spurred their study on, leading them to explore galaxies from the NASA-Sloan Atlas — a catalog of images and parameters of local galaxies sourced from the Sloan Digital Sky Survey and Galaxy Evolution Explorer (GALEX) data to study objects in the ultraviolet … For example, dwarf galaxies with tidal features whose origins are unclear and are located near a giant (M* > 1010) host galaxy have been selectively removed. In low-density environments, dwarfs are often much more gas-rich than giant galaxies. Number 2. We show the distribution of their mass ratios in Figure 7. A dwarf galaxy is a small galaxy composed of about 1000 up to several billion stars, as compared to the Milky Way's 200–400 billion stars. A previous study of interacting pairs of dwarf galaxies, (Stierwalt et al. Its publishing company, IOP Publishing, is a world leader in professional scientific communications. acknowledges the support by the Samsung Science & Technology Foundation under Project Number SSTF-BA1501-0. Nearly 3 billion years ago, a dwarf galaxy plunged into the center of the Milky Way and was ripped apart by the gravitational forces of the collision. DataTypeset image. We list the positions (R.A. and decl.)
Methods: As a first step we used the SExtractor fine-tuned for dwarf galaxy detection, to find galaxies from the FDS data, covering a 26 deg 2 area of the main cluster up to its virial radius, and the area around the Fornax A substructure. Streams. This may create a bias against merged dwarfs near giants; see the discussion in Section 6. We also made use of the GALEX all-sky survey imaging data. We show various examples of these classifications in Figure 2.