18 research outputs found
The globular cluster NGC 2419: a crucible for theories of gravity
We present the analysis of a kinematic data set of stars in the globular
cluster NGC 2419, taken with Keck/DEIMOS. Combined with a reanalysis of deep
HST and Subaru imaging data, which provide an accurate luminosity profile of
the cluster, we investigate the validity of a large set of dynamical models of
the system, which are checked for stability via N-body simulations. We find
that isotropic models in either Newtonian or Modified Newtonian Dynamics (MOND)
are ruled out with extremely high confidence. However, a simple Michie model in
Newtonian gravity with anisotropic velocity dispersion provides an excellent
representation of the luminosity profile and kinematics. In contrast, with MOND
we find that Michie models that reproduce the luminosity profile either
over-predict the velocity dispersion on the outskirts of the cluster if the
mass to light ratio is kept at astrophysically-motivated values, or else they
under-predict the central velocity dispersion if the mass to light ratio is
taken to be very small. We find that the best Michie model in MOND is a factor
of 10000 less likely than the Newtonian model that best fits the system. A
likelihood ratio of 350 is found when we investigate more general models by
solving the Jeans equation with a Markov-Chain Monte Carlo scheme. We verified
with N-body simulations that these results are not significantly different when
the MOND external field effect is accounted for. If the assumptions that the
cluster is in dynamical equilibrium, spherical, not on a peculiar orbit, and
possesses a single dynamical tracer population of constant M/L are correct, we
conclude that the present observations provide a very severe challenge for
MOND. [abridged]Comment: 25 pages, 19 figures, accepted for publication in Ap
NGC 2419: a large and extreme second generation in a currently undisturbed cluster
We analyse complementary HST and SUBARU data for the globular cluster NGC
2419. We make a detailed analysis of the horizontal branch (HB), that appears
composed by two main groups of stars: the luminous blue HB stars ---that extend
by evolution into the RR Lyrae and red HB region--- and a fainter, extremely
blue population. We examine the possible models for this latter group and
conclude that a plausible explanation is that they correspond to a significant
(~30 %) extreme second generation with a strong helium enhancement (Y~0.4). We
also show that the color dispersion of the red giant branch is consistent with
this hypothesis, while the main sequence data are compatible with it, although
the large observational error blurs the possible underlying splitting. While it
is common to find an even larger (50 -- 80) percentage of second generation in
a globular cluster, the presence of a substantial and extreme fraction of these
stars in NGC 2419 might be surprising, as the cluster is at present well inside
the radius beyond which the galactic tidal field would be dominant. If a
similar situation had been present in the first stages of the cluster life, the
cluster would have retained its initial mass, and the percentage of second
generation stars should have been quite small (up to ~10 %). Such a large
fraction of extreme second generation stars implies that the system must have
been initially much more massive and in different dynamical conditions than
today. We discuss this issue in the light of existing models of the formation
of multiple populations in globular clusters.Comment: 14 pages, 14 figures (5 in low resolution format), 3 tables, accepted
for publication in MNRA
A spectroscopic survey of thick disc stars outside the solar neighbourhood
We performed a spectroscopic survey of nearly 700 stars probing the galactic
thick disc far from the solar neighbourhood towards the galactic coordinates
(l~277, b~47). The derived effective temperatures, surface gravities and
overall metallicities were then combined with stellar evolution isochrones,
radial velocities and proper motions to derive the distances, kinematics and
orbital parameters of the sample stars. The targets belonging to each galactic
component (thin disc, thick disc, halo) were selected either on their
kinematics or according to their position above the galactic plane, and the
vertical gradients were also estimated. We present here atmospheric parameters,
distances and kinematics for this sample, and a comparison of our kinematic and
metallicity distributions with the Besancon model of the Milky Way. The thick
disc far from the solar neighbourhood is found to differ only slightly from the
thick disc properties as derived in the solar vicinity. For regions where the
thick disc dominates, we measured vertical velocity and metallicity trends of
d(V_phi)/dZ = 19 +/- 8 km/s/kpc and d[M/H]/dZ = -0.14 +/- 0.05 dex/kpc,
respectively. These trends can be explained as a smooth transition between the
different galactic components, although intrinsic gradients could not be
excluded. In addition, a correlation d(V_phi)/d[M/H] = -45 +/- 12 km/s/dex
between the orbital velocity and the metallicity of the thick disc is detected.
This gradient is inconsistent with the SDSS photometric survey analysis, which
did not detect any such trend, and challenges radial migration models of thick
disc formation. Estimations of the scale heights and scale lengths for
different metallicity bins of the thick disc result in consistent values, with
hR~3.4 \pm 0.7 kpc, and hZ~694 \pm 45 pc, showing no evidence of relics of
destroyed massive satellites.Comment: 19 pages, 15 figures, accepted for publication in A&
Formation of Multiple Populations in Globular Clusters: Another Possible Scenario
While chemical composition spreads are now believed to be a universal
characteristic of globular clusters (GCs), not all of them present multiple
populations in their color-magnitude diagrams (CMDs). Here we present a new
scenario for the formation of GCs, in an attempt to qualitatively explain this
otherwise intriguing observational framework. Our scenario divides GCs into
three groups, depending on the initial mass (M_I) of the progenitor structure
(PS), as follows. i) Massive PSs can retain the gas ejected by massive stars,
including the ejecta of core-collapse SNe. ii) Intermediate-mass PSs can retain
at least a fraction of the fast winds of massive stars, but none of the
core-collapse SNe ejecta. iii) Low-mass PSs can only retain the slow winds of
intermediate-mass stars. Members of the first group would include omega
Centauri (NGC 5139), M54 (NGC 6715), M22 (NGC 6656), and Terzan 5, whereas NGC
2808 (and possibly NGC 2419) would be members of the second group. The
remaining GCs which only present a spread in light elements, such as O and Na,
would be members of the third group. According to our scenario, the different
components in omega Cen should not display a sizeable spread in age. We argue
that this is consistent with the available observations. We give other simple
arguments in favor of our scenario, which can be described in terms of two main
analytical relations: i) Between the actual observed ratio between first and
second generation stars (R_SG^FG) and the fraction of first generation stars
that have been lost by the GC (S_L); and ii) Between S_L and M_I. We also
suggest a series of future improvements and empirical tests that may help
decide whether the proposed scenario properly describes the chemical evolution
of GCs.Comment: Accepted for publication in Astronomy and Astrophysic
Evidence for multiple populations in the massive globular cluster NGC 2419 from deep uVI LBT photometry
We present accurate wide-field uVI photometry of the remote and massive Galactic globular cluster NGC 2419, aimed at searching for the u-V color spread along the Red Giant Branch (RGB) that is generally interpreted as the photometric signature of the presence of multiple populations in globular clusters. Focusing on the RGB stars in the magnitude range 19.80.0 lie preferentially on the blue side
Thick disk kinematics from RAVE and the solar motion
Radial velocity surveys such as the Radial Velocity Experiment (RAVE) provide
us with measurements of hundreds of thousands of nearby stars most of which
belong to the Galactic thin, thick disk or halo. Ideally, to study the Galactic
disks (both thin and thick) one should make use of the multi-dimensional
phase-space and the whole pattern of chemical abundances of their stellar
populations. In this paper, with the aid of the RAVE Survey, we study the thin
and thick disks of the Milky Way, focusing on the latter. We present a
technique to disentangle the stellar content of the two disks based on the
kinematics and other stellar parameters such as the surface gravity of the
stars. Using the Padova Galaxy Model, we checked the ability of our method to
correctly isolate the thick disk component from the Galaxy mixture of stellar
populations. We introduce selection criteria in order to clean the observed
radial velocities from the Galactic differential rotation and to take into
account the partial sky coverage of RAVE. We developed a numerical technique to
statistically disentangle thin and thick disks from their mixture. We deduce
the components of the solar motion relative to the Local Standard of Rest (LSR)
in the radial and vertical direction, the rotational lag of the thick disk
component relative to the LSR, and the square root of the absolute value of the
velocity dispersion tensor for the thick disk alone. The analysis of the thin
disk is presented in another paper. We find good agreement with previous
independent parameter determinations. In our analysis we used photometrically
determined distances. In the Appendix we show that similar values can be found
for the thick disk alone as derived in the main sections of our paper even
without the knowledge of photometric distances.Comment: accepted on A&A, please see companion paper "THIN disk kinem...
The stellar halo of the Galaxy
Stellar halos may hold some of the best preserved fossils of the formation
history of galaxies. They are a natural product of the merging processes that
probably take place during the assembly of a galaxy, and hence may well be the
most ubiquitous component of galaxies, independently of their Hubble type. This
review focuses on our current understanding of the spatial structure, the
kinematics and chemistry of halo stars in the Milky Way. In recent years, we
have experienced a change in paradigm thanks to the discovery of large amounts
of substructure, especially in the outer halo. I discuss the implications of
the currently available observational constraints and fold them into several
possible formation scenarios. Unraveling the formation of the Galactic halo
will be possible in the near future through a combination of large wide field
photometric and spectroscopic surveys, and especially in the era of Gaia.Comment: 46 pages, 16 figures. References updated and some minor changes.
Full-resolution version available at
http://www.astro.rug.nl/~ahelmi/stellar-halo-review.pd
Science-Driven Optimization of the LSST Observing Strategy
The Large Synoptic Survey Telescope is designed to provide an unprecedented optical imaging dataset that will support investigations of our Solar System, Galaxy and Universe, across half the sky and over ten years of repeated observation. However, exactly how the LSST observations will be taken (the observing strategy or "cadence") is not yet finalized. In this dynamically-evolving community white paper, we explore how the detailed performance of the anticipated science investigations is expected to depend on small changes to the LSST observing strategy. Using realistic simulations of the LSST schedule and observation properties, we design and compute diagnostic metrics and Figures of Merit that provide quantitative evaluations of different observing strategies, analyzing their impact on a wide range of proposed science projects. This is work in progress: we are using this white paper to communicate to each other the relative merits of the observing strategy choices that could be made, in an effort to maximize the scientific value of the survey. The investigation of some science cases leads to suggestions for new strategies that could be simulated and potentially adopted. Notably, we find motivation for exploring departures from a spatially uniform annual tiling of the sky: focusing instead on different parts of the survey area in different years in a "rolling cadence" is likely to have significant benefits for a number of time domain and moving object astronomy projects. The communal assembly of a suite of quantified and homogeneously coded metrics is the vital first step towards an automated, systematic, science-based assessment of any given cadence simulation, that will enable the scheduling of the LSST to be as well-informed as possible