dwarf galaxy catalog
We expect that this public catalog can be used as a reference sample to investigate the effects of the tidal interaction on the evolution of star formation, and the morphology/structure of dwarf galaxies. All rights reserved. It is based on the Lyon-Meudon Extragalactic Database (LEDA), which was originally started in 1983. We find that only 41 dwarf galaxy merging systems have giant neighbors. So far, the study of interacting dwarf galaxies has largely been done on an individual basis, and lacks a sufficiently large catalog to give statistics on the properties of interacting dwarf galaxies, and their role in the evolution of low-mass galaxies. We also show the local-volume (<11 Mpc), star-forming galaxy sample of Lee et al. The wide range of dwarf galaxy luminosity reveals the dependence of dwarf galaxy chemical evolution on galaxy stellar … In S15's sample, the pair galaxies needed to have a separation velocity of less than 300 km s−1, which means they required that there be a measured radial velocity for both galaxies. It has a worldwide membership of around 50 000 comprising physicists from all sectors, as well as those with an interest in physics. We are mostly interested in dwarf galaxies with tidal features that are likely to be produced by interacting/merging dwarf galaxies. Astrophysicists announced today that the merger produced a series of telltale shell-like … Top: examples where we conclude a dwarf galaxy is interacting with and being deformed by the tidal field of a nearby giant galaxy and they have been excluded from the catalog. For comparison, we also show a sample of early-type galaxies from Janz & Lisker (2009), which clearly offsets from our sample galaxies, creating a red sequence above the star-forming galaxies in the color–magnitude relation. Additionally, we also search for the availability of deeper images in various publicly available archives. We classify them, according to observed low-surface-brightness features, into various categories including shells, stellar streams, loops, antennae, or simply interacting. This procedure is quite straightforward if the interacting galaxies are not well separated or already merged. For example, we have shown that shell features about dwarf galaxies are reliably produced by mergers (Paudel et al. In addition, while comparing radial velocity separation between interacting pairs, although we find a relatively low number of systems that have radial velocity measurements for both the interacting member dwarf galaxies of our sample, we find a clear difference from S15—only 2 out of 36 (5%) have a relative line-of-sight velocity larger than 100 km s−1 and 15 out of 60 (25%) interacting dwarf pairs in the S15 sample have relative line-of-sight velocities larger than 100 km s−1. 2016; Pearson et al. The field of view and color stretching are arbitrarily chosen to yield the best view of both interacting galaxies and low-surface-brightness features. Published 2018 August 22, galaxies: dwarf; galaxies: evolution; galaxies: interactions; galaxies: star formation. The comparison samples are early-type galaxies (gray square) and BCDs (green dots) taken from Janz & Lisker (2009) and Meyer et al. As the right panel of Figure 7 indicates, the relative line-of-sight velocity between the interacting dwarf pairs is relatively low, and only in two cases is it higher than 100 km s−1. From this figure, it is clear that these interacting dwarfs galaxies do not differ from the trend established by local-volume, star-forming galaxies. If the two interacting dwarf galaxies are visibly distinct, we simply designate them with an "I" (e.g., Id0217-0742), and if they are overlapping, or the progenitor galaxies are not distinct, we also give them an "M" (Merged, e.g., Id01250759). Context. For the aperture photometry, procedures similar to those applied for the SDSS images are used. A subset of this sample was studied in Pearson et al. Thus, we suspect that our selection criteria may be simply enhancing a real dependency on distance to the nearest giant galaxy. Some of these resemble the dwarfs with the symmetrical-shaped shell features that were found in Paudel et al. Like in this study, S15 also uses SDSS imaging to select their sample galaxies, therefore we expect both samples to cover the same areas of sky. 2005; Naab et al. Our visual inspection process involves multiple steps. Low-mass galaxies are also typically dominated by exponential disks. Despite the very similar visual morphology of the UGC 6741 system to Arp 104, Paudel et al. It is worth noting that the above classification scheme is not mutually exclusive, and in a number of cases there are overlaps. Another interesting difference is that S15 found there is an enhanced SFR between dwarf galaxies at small separations from their partner, compared to a control sample of isolated dwarf galaxies. Our main aim is to create a large catalog of merging dwarf galaxies. DataTypeset images: 1 2 3. We encourage the completeness of the catalog to be viewed cautiously, as there may be many possible biases in our selection procedure. The black dot represents the satellite candidates and blue dots represent isolated candidates. From this figure, it is clear that the probability of finding a merging dwarf system increases in low-density environments. 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. Wed, Nov 25, 2020. DE-AC02-05CH1123, by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract; and by the U.S. National Science Foundation, Division of Astronomical Sciences under Contract No. 2012; Johnson 2013; Nidever et al. (2002). Next we list FUV-band and NUV-band magnitudes in columns 7 and 8, respectively. (2009; see the gray plots), who studied the FUV-derived SFRs of local-volume (<11 Mpc), star-forming galaxies. Note that this is actually the flux ratio (larger flux/smaller flux), but under the assumption of similar stellar populations in both galaxies, we simply use the the term mass ratio. Galaxies in the original PGC catalogue are numbered with their original PGC number in HyperLEDA. The Virgo Stellar Stream is a stream of stars that is believed to have once been an orbiting dwarf galaxy that has been … 2012). On the other hand, it is a common belief that the shallow potential well of low-mass galaxies causes them to be more sensitive to their surrounding environments than massive galaxies. The Catalogue of Principal Galaxies (PGC) is an astronomical catalog published in 1989 that lists B1950 and J2000 equatorial coordinates and cross-identifications for 73,197 galaxies. 2013; Paudel & Ree 2014). 2012; Toloba et al. Meanwhile dwarfs with ongoing star formation activity (such as blue compact dwarf galaxies (BCDs, Papaderos et al. This large sample of disrupted galaxies or galaxies that exhibit tidal debris contains more than 700 candidates. In the case of interacting systems, when the galaxies involved are well separated (class I), the apertures are chosen in two different ways. In addition to this, Paudel et al. This may create a bias against merged dwarfs near giants; see the discussion in Section 6. Using an Hα equivalent width threshold of 2.8 Å, the final sample of AGN dwarf galaxies is reduced to 37. The American Astronomical Society. (A A S ) journals as soon as they are published. In this regard, the archival images of the CHFT6 DataTypeset image. 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. For example, the neutral hydrogen in galaxies has a typical velocity dispersion of ~10 km s−1. We classify the morphologies of the low-surface-brightness features into various categories: shells, stellar streams, loops, Antennae-like systems, or interacting. An image scale of 30'' is shown by the black horizontal bar. They are mostly gas-rich and star-forming systems, located in low-density environments. The g − r color distribution shown in the right panel of Figure 5 reveals that this sample is overwhelmingly dominated by star-forming galaxies with similar colors to BCDs (Meyer et al. 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 … Arp realized that the reason why galaxies formed into spiral or elliptical ... is a blue compact dwarf galaxy with extremely strong star formation activity; it is clearly too small to be the merger remnant of two spiral galaxies like the other merger remnants in this … More than 80% of the LV galaxies are dwarfs and nearly all of the undetected galaxies must be dwarf irregular (dIrr) galaxies and dwarf spheroidal (dSph) galaxies which are the most challenging to detect. UGC 7639 is an example of blue dwarf galaxy whose global properties are well matched by our multiwavelength approach, that is, a suitable approach to highlight the evolution also of these galaxies as a class. Dwarf galaxies' formation and activity are thought to be heavily influenced by interactions with … 2014; Mihos et al. (2015) reported interactions between dwarf galaxies where the overall morphological appearance is similar to that of the well known giant system Arp 104. Figure 12. Column (6): mass ratio of interacting galaxies. This table contains an all-sky catalog of 869 nearby galaxies having individual distance estimates within 11 Mpc or corrected radial velocities relative to the Local Group centroid V LG < 600 km s -1. acknowledges support from the Center for Galaxy Evolution Research (No. Whitmore6, A. Mok5, J.E. We list the Interacting dwarf (Id), coordinates (R.A. and decl.) The catalog contains SDSS photometry for 5634 individual objects, and also the photometry from matches to any of the … Figure 2. The last bin (the gray histogram) represents the number of merging dwarf systems that have more than 10 neighbors within our search area. In any case, we find that there is no significant difference in the phase-space diagram of dwarf interacting pairs (I class) and the rest of the sample.
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