105 research outputs found
THE IMPRINT of RADIAL MIGRATION on the VERTICAL STRUCTURE of GALAXY DISKS
We use numerical simulations to examine the effects of radial migration on the vertical structure of galaxy disks. The simulations follow three exponential disks of different mass but similar circular velocity, radial scalelength, and (constant) scale height. The disks develop different non-axisymmetric patterns, ranging from feeble, long-lived multiple arms to strong, rapidly evolving few-armed spirals. These fluctuations induce radial migration through secular changes in the angular momentum of disk particles, mixing the disk radially and blurring pre-existing gradients. Migration primarily affects stars with small vertical excursions, regardless of spiral pattern. This "provenance bias" largely determines the vertical structure of migrating stars: inward migrators thin down as they move in, whereas outward migrators do not thicken up but rather preserve the disk scale height at their destination. Migrators of equal birth radius thus develop a strong scale-height gradient, not by flaring out as commonly assumed, but by thinning down as they spread inward. Similar gradients have been observed for low-[α/Fe] mono-abundance populations (MAPs) in the Galaxy, but our results argue against interpreting them as a consequence of radial migration. This is because outward migration does not lead to thickening, implying that the maximum scale height of any population should reflect its value at birth. In contrast, Galactic MAPs have scale heights that increase monotonically outward, reaching values that greatly exceed those at their presumed birth radii. Given the strong vertical bias affecting migration, a proper assessment of the importance of radial migration in the Galaxy should take carefully into account the strong radial dependence of the scale heights of the various stellar populations. © 2016. The American Astronomical Society. All rights reserved
EXCITATION of COUPLED STELLAR MOTIONS in the GALACTIC DISK by ORBITING SATELLITES
We use a set of high-resolution N-body simulations of the Galactic disk to study its interactions with the population of cosmologically predicted satellites. One simulation illustrates that multiple passages of massive satellites with different velocities through the disk generate a wobble, which has the appearance of rings in face-on projections of the stellar disk. They also produce flares in the outer disk parts and gradually heat the disk through bending waves. A different numerical experiment shows that an individual satellite as massive as the Sagittarius dwarf galaxy passing through the disk will drive coupled horizontal and vertical oscillations of stars in underdense regions with small associated heating. This experiment shows that vertical excursions of stars in these low-density regions can exceed 1 kpc in the Solar neighborhood, resembling the recently locally detected coherent vertical oscillations. They can also induce non-zero vertical streaming motions as large as 10-20 km s-1, which is consistent with recent observations in the Galactic disk. This phenomenon appears as a local ring with modest associated disk heating. © 2016. The American Astronomical Society. All rights reserved
Stream-subhalo interactions in the Aquarius simulations
Aims. We perform the first self-consistent measurement of the rate of interactions between stellar tidal streams created by disrupting satellites and dark subhalos in a cosmological simulation of a Milky-Way-mass galaxy.
Methods. Using a retagged version of the Aquarius A dark-matter-only simulation, we selected 18 streams of tagged star particles that appear thin at the present day and followed them from the point their progenitors accrete onto the main halo, recording in each snapshot the characteristics of all dark-matter subhalos passing within several distance thresholds of any tagged star particle in each stream. We considered distance thresholds corresponding to constant impact parameters (1, 2, and 5 kpc), as well as those proportional to the region of influence of each subhalo (one and two times its half-mass radius r1=2). We then measured the age and present-day, phase-unwrapped length of each stream in order to compute the interaction rate in different mass bins and for different thresholds, and compared these to analytic predictions from the literature.
Results. We measure a median rate of 1.5^(+3.0)_(-1.1) (9.1^(+17.5)_(-7.1), 61.8^(+211)_(-40.6)) interactions within 1 (2, 5) kpc of the stream per 10 kpc of stream length per 10 Gyr. Resolution effects (both time and particle number) affect these estimated rates by lowering them
ON the CONSERVATION of the VERTICAL ACTION in GALACTIC DISKS
We employ high-resolution N-body simulations of isolated spiral galaxy models, from low-amplitude, multi-armed galaxies to Milky Way-like disks, to estimate the vertical action of ensembles of stars in an axisymmetrical potential. In the multi-armed galaxy the low-amplitude arms represent tiny perturbations of the potential, hence the vertical action for a set of stars is conserved, although after several orbital periods of revolution the conservation degrades significantly. For a Milky Way-like galaxy with vigorous spiral activity and the formation of a bar, our results show that the potential is far from steady, implying that the action is not a constant of motion. Furthermore, because of the presence of high-amplitude arms and the bar, considerable in-plane and vertical heating occurs that forces stars to deviate from near-circular orbits, reducing the degree at which the actions are conserved for individual stars, in agreement with previous results, but also for ensembles of stars. If confirmed, this result has several implications, including the assertion that the thick disk of our Galaxy forms by radial migration of stars, under the assumption of the conservation of the action describing the vertical motion of stars. © 2016. The American Astronomical Society. All rights reserved
Interacting dark matter contribution to the Galactic 511 keV gamma ray emission: constraining the morphology with INTEGRAL/SPI observations
We compare the full-sky morphology of the 511 keV gamma ray excess measured
by the INTEGRAL/SPI experiment to predictions of models based on dark matter
(DM) scatterings that produce low-energy positrons: either MeV-scale DM that
annihilates directly into e+e- pairs, or heavy DM that inelastically scatters
into an excited state (XDM) followed by decay into e+e- and the ground state.By
direct comparison to the data, we find that such explanations are consistent
with dark matter halo profiles predicted by numerical many-body simulations for
a Milky Way-like galaxy. Our results favor an Einasto profile over the cuspier
NFW distribution and exclude decaying dark matter scenarios whose predicted
spatial distribution is too broad. We obtain a good fit to the shape of the
signal using six fewer degrees of freedom than previous empirical fits to the
511 keV data. We find that the ratio of flux at Earth from the galactic bulge
to that of the disk is between 1.9 and 2.4, taking into account that 73% of the
disk contribution may be attributed to the beta decay of radioactive 26Al.Comment: 7 pages, 4 figures. Includes minor corrections, and a discussion of
threshold energies in XDM models. Published in JCA
The Impact of Stellar Migration on Disk Outskirts
Stellar migration, whether due to trapping by transient spirals (churning),
or to scattering by non-axisymmetric perturbations, has been proposed to
explain the presence of stars in outer disks. After a review of the basic
theory, we present compelling, but not yet conclusive, evidence that churning
has been important in the outer disks of galaxies with type II (down-bending)
profiles, while scattering has produced the outer disks of type III
(up-bending) galaxies. In contrast, field galaxies with type I (pure
exponential) profiles appear to not have experienced substantial migration. We
conclude by suggesting work that would improve our understanding of the origin
of outer disks.Comment: Invited review, Book chapter in "Outskirts of Galaxies", Eds. J. H.
Knapen, J. C. Lee and A. Gil de Paz, Astrophysics and Space Science Library,
Springer, in press 39 pages, 15 figure
Constraints on the shapes of galaxy dark matter haloes from weak gravitational lensing
We study the shapes of galaxy dark matter haloes by measuring the anisotropy
of the weak gravitational lensing signal around galaxies in the second
Red-sequence Cluster Survey (RCS2). We determine the average shear anisotropy
within the virial radius for three lens samples: all galaxies with
19<m_r'<21.5, and the `red' and `blue' samples, whose lensing signals are
dominated by massive low-redshift early-type and late-type galaxies,
respectively. To study the environmental dependence of the lensing signal, we
separate each lens sample into an isolated and clustered part and analyse them
separately. We also measure the azimuthal dependence of the distribution of
physically associated galaxies around the lens samples. We find that these
satellites preferentially reside near the major axis of the lenses, and
constrain the angle between the major axis of the lens and the average location
of the satellites to =43.7 deg +/- 0.3 deg for the `all' lenses,
=41.7 deg +/- 0.5 deg for the `red' lenses and =42.0 deg +/- 1.4
deg for the `blue' lenses. For the `all' sample, we find that the anisotropy of
the galaxy-mass cross-correlation function =0.23 +/- 0.12, providing
weak support for the view that the average galaxy is embedded in, and
preferentially aligned with, a triaxial dark matter halo. Assuming an
elliptical Navarro-Frenk-White (NFW) profile, we find that the ratio of the
dark matter halo ellipticity and the galaxy ellipticity
f_h=e_h/e_g=1.50+1.03-1.01, which for a mean lens ellipticity of 0.25
corresponds to a projected halo ellipticity of e_h=0.38+0.26-0.25 if the halo
and the lens are perfectly aligned. For isolated galaxies of the `all' sample,
the average shear anisotropy increases to =0.51+0.26-0.25 and
f_h=4.73+2.17-2.05, whilst for clustered galaxies the signal is consistent with
zero. (abridged)Comment: 28 pages, 23 figues, accepted for publication in A&
The Relationship Between Mono-Abundance and Mono-Age Stellar Populations in the Milky Way Disk
Studying the Milky Way disk structure using stars in narrow bins of [Fe/H] and [α/Fe] has recently been proposed as a powerful method to understand the Galactic thick and thin disk formation. It has been assumed so far that these mono-abundance populations (MAPs) are also coeval, or mono-age, populations. Here we study this relationship for a Milky Way chemodynamical model and show that equivalence between MAPs and mono-age populations exists only for the high-[α/Fe] tail, where the chemical evolution curves of different Galactic radii are far apart. At lower [α/Fe]-values an MAP is composed of stars with a range in ages, even for small observational uncertainties and a small MAP bin size. Due to the disk inside-out formation, for these MAPs younger stars are typically located at larger radii, which results in negative radial age gradients that can be as large as 2 Gyr kpcâ1. Positive radial age gradients can result for MAPs at the lowest [α/Fe] and highest [Fe/H] end. Such variations with age prevent the simple interpretation of observations for which accurate ages are not available. Studying the variation with radius of the stellar surface density and scale height in our model, we find good agreement to recent analyses of the APOGEE red-clump (RC) sample when 1â4 Gyr old stars dominate (as expected for the RC). Our results suggest that the APOGEE data are consistent with a Milky Way model for which mono-age populations flare for all ages. We propose observational tests for the validity of our predictions and argue that using accurate age measurements, such as from asteroseismology, is crucial for putting constraints on Galactic formation and evolution
The spatially-resolved star formation history of the M31 outer disc
We present deep Hubble Space Telescope Advanced Camera for Surveys
observations of the stellar populations in two fields lying at 20 and 23 kpc
from the centre of M31 along the south-west semi-major axis. These data enable
the construction of colour-magnitude diagrams reaching the oldest main-sequence
turn-offs (~13 Gyr) which, when combined with another field at 25 kpc from our
previous work, we use to derive the first precision constraints on the
spatially-resolved star formation history of the M31 disc. The star formation
rates exhibit temporal as well as field-to-field variations, but are generally
always within a factor of two of their time average. There is no evidence of
inside-out growth over the radial range probed. We find a median age of ~7.5
Gyr, indicating that roughly half of the stellar mass in the M31 outer disc was
formed before z ~ 1. We also find that the age-metallicity relations (AMRs) are
smoothly increasing from [Fe/H]~-0.4 to solar metallicity between 10 and 3 Gyr
ago, contrary to the flat AMR of the Milky Way disc at a similar number of
scale lengths. Our findings provide insight on the roles of stellar feedback
and radial migration in the formation and evolution of large disc galaxies.Comment: 5 pages, 4 figures. Re-submitted to MNRAS after addressing the
referee's comment
The Gaia-ESO Survey:New constraints on the Galactic disc velocity dispersion and its chemical dependencies
Understanding the history and the evolution of the Milky Way disc is one of
the main goals of modern astrophysics. We study the velocity dispersion
behaviour of Galactic disc stars as a function of the [Mg/Fe] ratio, which can
be used as a proxy of relative age. This key relation is essential to constrain
the formation mechanisms of the disc stellar populations as well as the cooling
processes. We used the recommended parameters and chemical abundances of 7800
FGK Milky Way field stars from the second internal data release of the Gaia-ESO
Survey. These stars were observed with the GIRAFFE spectrograph, and cover a
large spatial volume (6<R<10kpc and |Z|<2kpc). Based on the [Mg/Fe] and [Fe/H]
ratios, we separated the thin- from the thick-disc sequence. From analysing the
Galactocentric velocity of the stars for the thin disc, we find a weak positive
correlation between Vphi and [Fe/H], due to a slowly rotating Fe-poor tail. For
the thick disc, a strong correlation with [Fe/H] and [Mg/Fe] is established. We
have detected an inversion of the radial velocity dispersion with [Mg/Fe] for
thick-disc stars with [Fe/H]+0.2dex. First, the velocity
dispersion increases with [Mg/Fe] at all [Fe/H] ratios for the thin-disc stars,
and then it decreases for the thick-disc at the highest [Mg/Fe] abundances.
Similar trends are observed within the errors for the azimuthal velocity
dispersion, while a continuous increase with [Mg/Fe] is observed for the
vertical velocity dispersion. The velocity dispersion decrease agrees with
previous measurements of the RAVE survey, although it is observed here for a
greater metallicity interval and a larger spatial volume. We confirm the
existence of [Mg/Fe]-rich thick-disc stars with cool kinematics in the
generally turbulent context of the primitive Galactic disc. This is discussed
in the framework of the different disc formation scenarios.Comment: 14 pages, 13 figures, A&A accepte
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