The transverse velocity of the Andromeda system, derived from the M31 satellite population

Salomon, J.-B.; Ibata, Rodrigo; Famaey, Benoît; Martín, Nicolás F.; Lewis, Geraint F.

doi:10.1093/mnras/stv2865

Cited by 40 publications

(58 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The choice of the LG model and the CF2 constraint allows us to study the way the structure of the LG and the nearby universe affects our knowledge of masses of the MW and M31. A particular emphasis has been placed also on the effects of using a low-vtan estimate (the value found by Sohn et al (2012), referred to as v (I) tan ) and a high one (v (II) tan , derived by Salomon et al (2016)). We applied these models to objects drawn from two different types of simulations: a series of constrained simulations (CS), from which it was possible to gather halo pairs living in a large scale environment akin to the observational one, and a standard, random ΛCDM (Rand).…”

Section: Discussionmentioning

confidence: 99%

“…In the case of the latter, in fact, there is yet no clear consensus on its real value, for which currently two incompatible estimates exist. These were obtained using different techniques: the one of Sohn et al (2012), who found vtan= 17 ± 17 (referred to as v (I) tan ) directly measuring the motion stellar population within M31 against background galaxies; and the one of Salomon et al (2016), who inferred vtan=164 ± 62 (referred to as v (II) tan ) using precise satellite galaxies data of the PAndAS survey (McConnachie et al 2009;Martin et al 2013a,b).…”

Section: The Local Group Modelmentioning

confidence: 99%

“…This kind of Bayesian approach is in turn simi-lar to the what Busha et al (2011) used to constrain MMW and to that of González et al (2014) for the MLG. In the present work, most of the emphasis is put on the consequences that the different vtan estimates of Sohn et al (2012) and Salomon et al (2016) (referred to as v (I) tan and v (II) tan hereafter) have on the mass of the Local Group of galaxies, and on the masses of the two largest DM haloes, M31 and MW. In fact, whereas the first authors directly measured an extremely small value of vtan, compatible with zero at the 1σ level, the latter found that new satellite data favour a much higher vtan≈ 160 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Constraining the mass of the Local Group

Carlesi¹,

Hoffman²,

Sorce

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The mass of the Local Group (LG) is a crucial parameter for galaxy formation theories. However, its observational determination is challenging -its mass budget is dominated by dark matter which cannot be directly observed. To meet this end the posterior distributions of the LG and its massive constituents have been constructed by means of constrained and random cosmological simulations. Two priors are assumed -the ΛCDM model that is used to set up the simulations and a LG model, which encodes the observational knowledge of the LG and is used to select LG-like objects from the simulations. The constrained simulations are designed to reproduce the local cosmography as it is imprinted onto the Cosmicflows-2 database of velocities. Several prescriptions are used to define the LG model, focusing in particular on different recent estimates of the tangential velocity of M31. It is found that (a) different v tan choices affect the peak mass values up to a factor of 2, and change mass ratios of M M31 to M MW by up to 20%; (b) constrained simulations yield more sharply peaked posterior distributions compared with the random ones; (c) LG mass estimates are found to be smaller than those found using the timing argument; (d) preferred MW masses lie in the range of (0.6 − 0.8) × 10 12 M whereas (e) M M31 is found to vary between (1.0 − 2.0) × 10 12 M , with a strong dependence on the v tan values used.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: The Local Group Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Constraining the mass of the Local Group

Carlesi¹,

Hoffman²,

Sorce

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…Nowadays, even the tangential velocity of M31 is very uncertain. Two recent measurements give very different, inconsistent results: a value of 17 km s −1 from Sohn et al (2012) and 164 km s −1 by Salomon et al (2016). For And II the tangential velocity is completely unknown.…”

Section: Observational Test Of the Modelmentioning

confidence: 95%

Formation of Andromeda II via a gas-rich major merger and an interaction with M31

Fouquet

Łokas

Pino

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Andromeda II (And II) has been known for a few decades but only recently observations have unveiled new properties of this dwarf spheroidal galaxy. The presence of two stellar populations, the bimodal star formation history (SFH) and an unusual rotation velocity of And II put strong constrains on its formation and evolution. Following Lokas et al. (2014), we propose a detailed model to explain the main properties of And II involving (1) a gas-rich major merger between two dwarf galaxies at high redshift in the field and (2) a close interaction with M31 about 5 Gyr ago. The model is based on N -body/hydrodynamical simulations including gas dynamics, star formation and feedback. One simulation is designed to reproduce the gas-rich major merger explaining the origin of stellar populations and the SFH. Other simulations are used to study the effects of tidal forces and the ram pressure stripping during the interaction between And II and M31. The model successfully reproduces the SFH of And II including the properties of stellar populations, its morphology, kinematics and the lack of gas. Further improvements to the model are possible via joint modelling of all processes and better treatment of baryonic physics.

show abstract

“…The common orbital history of these galaxies has been repeatedly studied in the past in response to improvements in the measurement of their PM (e.g. van der Marel et al 2012b;Salomon et al 2016;Patel et al 2017;Semczuk et al 2018). Most recently, van der Marel et al (2019) have explored the implications of the new Gaia DR2 PM for these galaxies.…”

Section: Preliminariesmentioning

confidence: 99%

The M31/M33 tidal interaction: a hydrodynamic simulation of the extended gas distribution

Tepper-García

Bland-Hawthorn

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We revisit the orbital history of the Triangulum galaxy (M33) around the Andromeda galaxy (M31) in view of the recent Gaia Data Release 2 proper motion measurements for both Local Group galaxies. Earlier studies consider highly idealised dynamical friction, but neglect the effects of dynamical mass loss. We show the latter process to be important using mutually consistent orbit integration and N-body simulations. Following this approach we find an orbital solution that brings these galaxies to within ∼ 50 kpc of each other in the past, ∼ 6.5 Gyr ago. We explore the implications of their interaction using an N-body/hydrodynamical simulation with a focus on the origin of two prominent features: 1) M31's Giant Stellar Stream; and 2) the M31-M33 H i filament. We find that the tidal interaction does not produce a structure reminiscent of the stellar stream that survives up to the present day. In contrast, the M31-M33 H i filament is likely a fossil structure dating back to the time of the ancient encounter between these galaxies. Similarly, the observed outer disc warp in M33 may well be a relic of this past event. Our model suggests the presence of a tidally induced gas envelope around these galaxies, and the existence of a diffuse gas stream, the 'Triangulum stream', stretching for tens of kpc from M33 away from M31. We anticipate upcoming observations with the recently commissioned, Five-hundred-meter Aperture Spherical radio Telescope (FAST) that will target the putative stream in its first years of operation.

show abstract

The transverse velocity of the Andromeda system, derived from the M31 satellite population

Cited by 40 publications

References 40 publications

Constraining the mass of the Local Group

Constraining the mass of the Local Group

Formation of Andromeda II via a gas-rich major merger and an interaction with M31

The M31/M33 tidal interaction: a hydrodynamic simulation of the extended gas distribution

Contact Info

Product

Resources

About