The Splash Survey: Spectroscopy of 15 M31 Dwarf Spheroidal Satellite Galaxies

Tollerud, Erik; Beaton, Rachael L.; Geha, Marla; Bullock, James S.; Guhathakurta, Puragra; Kalirai, Jason; Majewski, Steven R.; Kirby, Evan N.; Gilbert, Karoline M.; Yniguez, B.; Patterson, Richard J.; Ostheimer, J. C.; Cooke, Jeff; Dorman, Claire E.; Choudhury, A.; Cooper, Michael C.

doi:10.1088/0004-637x/752/1/45

Cited by 186 publications

(310 citation statements)

References 101 publications

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“…They are interpreted as non-equilibrium dynamics due to harassment through tidal fields (e.g. Kroupa 1997), the presence of a large amount of non-baryonic dark matter (e.g Wolf et al 2010;Tollerud et al 2012), or as a modification of the Newtonian law of gravity at very low accelerations (e.g. Angus 2008;McGaugh & Milgrom 2013).…”

Section: Detailed Description Of the Datamentioning

confidence: 99%

An extensive catalogue of early-type galaxies in the nearby Universe

Dabringhausen

Fellhauer

2016

Mon. Not. R. Astron. Soc.

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We present a catalogue of 1715 early-type galaxies from the literature, spanning the luminosity range from faint dwarf spheroidal galaxies to giant elliptical galaxies. The aim of this catalogue is to be one of the most comprehensive and publicly available collections of data on early-type galaxies. The emphasis in this catalogue lies on dwarf elliptical galaxies, for which some samples with detailed data have been published recently. For almost all of the early-type galaxies included in it, this catalogue contains data on their locations, distances, redshifts, half-light radii, the masses of their stellar populations and apparent magnitudes in various passbands. Data on metallicity and various colours are available for a majority of the galaxies presented here. The data on magnitudes, colours, metallicities and masses of the stellar populations is supplemented with entries that are based on fits to data from simple stellar population models and existing data from observations. Also, some simple transformations have been applied to the data on magnitudes, colours and metallicities in this catalog, in order to increase the homogeneity of this data. Estimates on the Sérsic profiles, internal velocity dispersions, maximum rotational velocities, dynamical masses and ages are listed for several hundreds of the galaxies in this catalogue. Finally, each quantity listed in this catalogue is accompanied with information on its source, so that users of this catalogue can easily exclude data that they do not consider as reliable enough for their purposes.

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Section: Detailed Description Of the Datamentioning

confidence: 99%

An extensive catalogue of early-type galaxies in the nearby Universe

Dabringhausen

Fellhauer

2016

Mon. Not. R. Astron. Soc.

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“…In general, young dEs (asterisks) are rotationally supported (blue) while the old ones (circles) are pressure supported (red). Grey open triangles and squares are Milky Way and M31 dwarf spheroidal galaxies (Wolf et al 2010;Brasseur et al 2011;Tollerud et al 2012). Figure 2 shows the (V − K) e colour versus σ e -both measured within the R e -of the SAURON galaxies and T11 Virgo dEs.…”

Section: Scaling Relationsmentioning

confidence: 99%

“…In the V band we have added dSph galaxies from the Milky Way and Andromeda (Wolf et al 2010;Brasseur et al 2011;Tollerud et al 2012). …”

Section: Fundamental Plane In the κ-Spacementioning

confidence: 99%

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

Toloba

Boselli

Peletier³

et al. 2012

A&A

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We place our sample of 18 Virgo dwarf early-type galaxies (dEs) on the (V − K) e -velocity dispersion, Faber-Jackson, and fundamental plane (FP) scaling relations for massive early-type galaxies (Es). We use a generalized velocity dispersion, which includes rotation, to be able to compare the location of both rotationally and pressure supported dEs with those of early and late-type galaxies. We find that dEs seem to bend the Faber-Jackson relation of Es to lower velocity dispersions, being the link between Es and dwarf spheroidal galaxies (dSphs). Regarding the FP relation, we find that dEs are significantly offset with respect to massive hot stellar systems, and re-casting the FP into the so-called κ-space suggests that this offset is related to dEs having a total mass-to-light ratio higher than Es but still significantly lower than dSph galaxies. Given a stellar mass-to-light ratio based on the measured line indices of dEs, the FP offset allows us to infer that the dark matter fraction within the half light radii of dEs is on average 42% (uncertainties of 17% in the K band and 20% in the V band), fully consistent with an independent estimate in an earlier paper in this series. We also find that dEs in the size-luminosity relation in the near-infrared, like in the optical, are offset from early-type galaxies, but seem to be consistent with late-type galaxies. We thus conclude that the scaling relations show that dEs are different from Es, and that they further strengthen our previous findings that dEs are closer to and likely formed from late-type galaxies.

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“…Chemin et al (2011) removed the baryon contribution and found that the dark matter distribution in the central regions of a large array of galaxies may well be fitted by the Einasto profile with a low index (n 0.5) that corresponds to a cored profile. The central densities of the dwarf spheroidal satellites of the Andromeda galaxy are also low and favor the cored profiles (Tollerud et al 2012), although the profiles in this case can be modified by the dynamical friction and tidal effects, since the satellites are situated inside the virial radius of the host galaxy. However, recent observations of dwarf spheroidal galaxies also indicate no cusps in their centers (Oh et al 2011;Governato et al 2012).…”

Section: )) τ R = N(r)mentioning

confidence: 94%

Relaxation of dark matter halos: how to match observational data?

Baushev

2014

A&A

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We show that moderate energy relaxation in the formation of dark matter halos invariably leads to profiles that match those observed in the central regions of galaxies. The density profile of the central region is universal and insensitive to either the seed perturbation shape or the details of the relaxation process. The profile has a central core; the multiplication of the central density by the core radius is almost independent of the halo mass, in accordance with observations. In the core area the density distribution behaves as an Einasto profile with low index (n ∼ 0.5); it has an extensive region with ρ ∝ r −2 at larger distances. This is exactly the shape that observations suggest for the central region of galaxies. On the other hand, this shape does not fit the galaxy cluster profiles. A possible explanation of this fact is that the relaxation is violent in the case of galaxy clusters; however, it is not violent enough when galaxies or smaller dark matter structures are considered. We discuss the reasons for this.

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The Splash Survey: Spectroscopy of 15 M31 Dwarf Spheroidal Satellite Galaxies

Cited by 186 publications

References 101 publications

An extensive catalogue of early-type galaxies in the nearby Universe

An extensive catalogue of early-type galaxies in the nearby Universe

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

Relaxation of dark matter halos: how to match observational data?

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