Abundance of dwarf galaxies around low-mass spiral galaxies in the Local Volume
Oliver Müller,Helmut Jerjen +1 more
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TLDR
In this paper, the authors used the Dark Energy Camera (DEC) to survey a 72 deg2 area of the nearby Sculptor group, also encompassing the two low-mass Local Volume galaxies NGC 24 and NGC 45 residing behind the group, to search for as yet undetected dwarf galaxies.Abstract:
The abundance of satellite dwarf galaxies has long been considered a crucial test for the current model of cosmology leading to the well-known missing satellite problem. Recent advances in simulations and observations have allowed the study of dwarf galaxies around host galaxies in more detail. Using the Dark Energy Camera we surveyed a 72 deg2 area of the nearby Sculptor group, also encompassing the two low-mass Local Volume galaxies NGC 24 and NGC 45 residing behind the group, to search for as yet undetected dwarf galaxies. Apart from the previously known dwarf galaxies we found only two new candidates down to a 3σ surface brightness detection limit of 27.4 r mag arcsec−2 . Both systems are in projection close to NGC 24. However, one of these candidates could be an ultra-diffuse galaxy associated with a background galaxy. We compared the number of known dwarf galaxy candidates around NGC 24, NGC 45, and five other well-studied low-mass spiral galaxies (NGC 1156, NGC 2403, NGC 5023, M 33, and the LMC) with predictions from cosmological simulations, and found that for the stellar-to-halo mass models considered, the observed satellite numbers tend to be on the lower end of the expected range. This could mean either that there is an overprediction of luminous subhalos in ΛCDM or that we are missing some of the satellite members due to observational biases.read more
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Discovery of New Dwarf Galaxies in the M81 Group
TL;DR: The M81 group provides an almost unique opportunity for establishing membership for galaxies in a low density region complete to magnitudes as faint as M r'} = -10.06 as discussed by the authors.
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Cosmicflows-2: The Data
R. Brent Tully,Hélène M. Courtois,Hélène M. Courtois,Andrew E. Dolphin,J. Richard Fisher,Philippe Héraudeau,Bradley A. Jacobs,Igor D. Karachentsev,Dmitry Makarov,Lidia Makarova,Sofia Mitronova,Luca Rizzi,Edward J. Shaya,Jenny G. Sorce,Po-Feng Wu +14 more
TL;DR: Cosmicflows-2 as mentioned in this paper is a compilation of distances and peculiar velocities for over 8000 galaxies, with the largest contributions coming from the luminosity-linewidth correlation for spirals, the TFR, and the related Fundamental Plane relation for E/S0 systems.
Quenching and ram pressure stripping of simulated Milky Way satellite galaxies
Christine M. Simpson,Robert J. J. Grand,Robert J. J. Grand,Facundo A. Gómez,Facundo A. Gómez,Federico Marinacci,Rüdiger Pakmor,Volker Springel,Volker Springel,David J. R. Campbell,Carlos S. Frenk +10 more
TL;DR: In this paper, the authors present predictions for the quenching of star formation in satellite galaxies of the Local Group from a suite of 30 cosmological zoom simulations of Milky Way-like host galaxies and demonstrate that systems within a host galaxy's R200 radius are comprised of two populations: (i) a first infall population that has entered the host halo within the past few Gyrs and (ii) a population of returning ‘backsplash’ systems that have had a much more extended interaction with the host.
Journal ArticleDOI
Baryonic solutions and challenges for cosmological models of dwarf galaxies
TL;DR: In this article , the authors consider the most notable challenges to the dark energy plus cold dark matter (ΛCDM) cosmological model regarding dwarf galaxies and discuss how recent cosmologically numerical simulations have pinpointed baryonic solutions to these challenges.
Posted Content
The M101 Satellite Luminosity Function and the Halo to Halo Scatter Among Milky Way Analogues
P. Bennet,D. J. Sand,Denija Crnojevic,K. Spekkens,Ananthan Karunakaran,Dennis Zaritsky,Burçin Mutlu-Pakdil +6 more
TL;DR: In this paper, the satellite luminosity function of M101 was updated based on the presence of these new objects down to M_V = 8.2, which is the sparsest group probed to this depth, though M94 is even sparser to the depth it has been examined.
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