dwarf galaxy catalog

2011, 2015). These galaxies are selected by visual inspection of publicly available archival imaging from two wide-field optical surveys (SDSS-III and the Legacy Survey), and they possess low-surface-brightness features that are likely the result of an interaction between dwarf galaxies. Volume 237, The stellar masses of candidate galaxies in this sample are measured from our own photometric measurements as described in Section 3. The first column is the galaxy number. It collects data on the following galaxy observables: angular diameters, apparent magnitudes in far-UV, B, and K s bands, Hα and H I fluxes, morphological types, H I-line widths, radial velocities, and distance estimates. Figure 4. To perform the photometric analysis and measure the total luminosity, we exclusively use the SDSS image data, unless explicitly mentioned otherwise. You do not need to reset your password if you login via Athens or an Institutional login. Astrophysicists announced today that the merger produced a series of telltale shell-like … Since they are mostly star-forming, almost all are detected in FUV-band and NUV-band GALEX all-sky survey images. For this work we characterize the surrounding environment by searching for neighboring giant galaxies (MK < −20 mag, corresponding to a stellar mass of >1010), within a sky-projected distance of less than 700 kpc, and a relative line-of-sight radial velocity of less than ±700 km s−1. 2016). We find that a significant fraction, 30 out 177, of merging dwarf systems have no neighbors, not even another dwarf galaxy, within our search area. This article presents a compilation and discussion of data relating to basic observational properties of all nearby (dwarf) galaxies within 3Mpc (the dwarf satellite systems of the Milky Way and M31 galaxies, the quasi-isolated dwarfs in the outer regions of the Local Group, and the isolated dwarf galaxies found in the surrounding of the Local Group out to the next nearest galaxy groups). In this work, we focus on the optical morphology of dwarf–dwarf galaxy interactions. Part of the reason for this could perhaps be that the tidal features that are produced are not as spectacular as those in merging giant galaxies, due to the relatively weak tidal forces acting upon them. First, a large aperture covering both the interacting galaxies is used to measure the total flux of the system, as done for the other classes. The Institute of Physics (IOP) is a leading scientific society promoting physics and bringing physicists together for the benefit of all. From the CHFT archive, we use the Megapipe stack7 We retrieved archival images from the SDSS-III database (Abazajian et al. Figure 11. Also, there is UM 448, a merging BCD, which possesses a pronounced tidal tail that was studied in James et al. The Astrophysical Journal Supplement Series, Computer modeling of the shells and the motion of the stars indicates that the dwarf galaxy first passed through the galactic center of the Milky Way 2.7 billion years ago. 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. , although the full catalog of 104 dwarf–dwarf pair galaxies with the names and positions of the galaxies has yet to be publicly released. Some of these resemble the dwarfs with the symmetrical-shaped shell features that were found in Paudel et al. 2017). It is located about 346 million light-years away from Earth. Wed, Nov 25, 2020. However, in Figure 6 we found no evidence for an enhanced SFR in our merging dwarf systems compared to a sample of local-volume, star-forming galaxies. The comparison data are from Leroy et al. For example, some interacting galaxies also posses multiple tidal features, like shells or stellar streams, even when the two parent dwarf galaxies are not yet fully merged. This may potentially lead to a difference in the star formation efficiency and overall evolutionary history of dwarf galaxies compared to giants. It is based on the Lyon-Meudon Extragalactic Database (LEDA), which was originally started in 1983. It is clear from this figure that our satellite merging dwarf systems are located comparatively farther than the distance of the LMC–SMC system is from the Milky Way (MW). While doing so, unrelated background and foreground objects were masked manually. As might be expected, the majority of the tidal features are created by interactions with their neighboring giant galaxies. It includes 177 nearby merging dwarf galaxies of stellar mass M 10 M $_ {\sun}$ and redshifts z 0.02. For the rest of the physical parameters that we present in this work, values are given for the total system (e.g., magnitudes, g − r colors, stellar masses, and star formation rates (SFRs)). Massachusetts Institute of Technology (MIT) astronomers have detected 18 very metal-poor stars in the Sagittarius dwarf galaxy. In the last column we provide the names of galaxies that we found in NED. It has been shown by many observational and theoretical studies that during the intermediate phases of interactions, large-scale tidal interactions trigger the formation of peculiar features like shells, streams, bridges, and tails (Toomre & Toomre 1972; Eneev et al. 1984) are mainly found in less dense environments. If this is the case, one might expect the progenitors of some dEs to exhibit characteristic features that arise during mergers, such as tidal debris. Star formation rate vs. blue-band absolute magnitude. BibTeX However, dwarf spheroidals do not possess gas in the periphery, as do bright ellipticals. springer, Dwarf galaxy research constitutes an extremely vibrant field of astrophysical research, with many long-standing questions still unsettled and new ones constantly arising. Because they are selected from visual inspection of low-surface-brightness features, this depends on the depth of the imaging survey, and on how well defined the tidal features are. 2014; Paudel et al. 2009). 2009; Duc et al. Shell Feature Early-type Dwarf Galaxies in the Virgo Cluster, UGC 4703 Interacting Pair Near the Isolated Spiral Galaxy NGC 2718: A Milky Way Magellanic Cloud Analog, TiNy Titans: The Role of Dwarf–Dwarf Interactions in Low-mass Galaxy Evolution, A Widespread, Clumpy Starburst in the Isolated Ongoing Dwarf Galaxy Merger dm1647+21, Gas, Stars, and Star Formation in ALFALFA Dwarf Galaxies. We made 2D-decompositions of the identified galaxies using GALFIT, … Id11253803 is the best example of this scenario. The complete list of images is shown in Figure 12. Thus, it is probable that many of these are not bound to their hosts, and in many cases our 700 kpc search radius and ±700 km s−1 velocity range search criteria are not robust enough to characterize whether our merging dwarfs are hosted by their nearest giant host. The Magellanic Clouds are often included but some say they are just passing by and not really in orbit. (2008). We are mostly interested in dwarf galaxies with tidal features that are likely to be produced by interacting/merging dwarf galaxies. This catalog will also be invaluable for future follow- up studies of the Fornax cluster dwarf galaxies. The black dot represents the satellite candidates and blue dots represent isolated candidates. 2008). It seems that only half of the satellite merging dwarf systems are clearly bound to their hosts, (assuming their hosts are MW-like), i.e., located below the escape velocity line. Dwarf galaxies' formation and activity are thought to be heavily influenced by interactions with … The origin of the different dwarf galaxy types and the possible evolutionary links between them are the subject of much research and debate (Lisker 2009). (2003) as appropriate to the observed g − r color. Context. In these cases, we use images from the Legacy survey. P.C.-C. was supported by CONICYT (Chile) through Programa Nacional de Becas de Doctorado 2014 folio 21140882. The total number of galaxies in this redshift range is ≈20,000. If a hint is found, we then re-examine the coadded fits file of the multiple bands available in the archive. We have collected a catalog of 177 merging dwarf systems, spanning the stellar mass range from 107 to 1010 M⊙ in a redshift range z < 0.02. The last gray bar represents the number of merging dwarf systems that have more than 10 neighbor galaxies. were very helpful for visual confirmation of the presence of low-surface-brightness features around dwarf galaxies. However, note that to derive SFR we have only used FUV flux that has been corrected for foreground Galactic extinction but not internal extinction; therefore, in many cases these values would be a lower limit. It includes 177 nearby merging dwarf galaxies of stellar mass M * < 1010 M ⊙ and redshifts z < 0.02. Also, if we see a loop of a stellar stream around the galaxies, we identify this with an "L," e.g., Id09530702. Previously in 2011, Reines and her colleagues used VLA to discover the first massive black hole in a dwarf starburst galaxy in 2011.

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