A synthetic view on structure and evolution of the Milky Way

By Annie Robin, Céline Reylé, S. Derriere, S. Picaud. 2003

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Since the Hipparcos mission and recent large scale surveys in the optical and the near-infrared, new constraints have been obtained on the structure and evolution history of the Milky Way. The population synthesis approach is a useful tool to interpret such data sets and to test scenarios of evolution of the Galaxy. We present here new constraints on evolution parameters obtained from the Besancon model of population synthesis and analysis of optical and near-infrared star counts. The Galactic potential is computed self-consistently, in agreement with Hipparcos results and the observed rotation curve. Constraints are posed on the outer bulge structure, the warped and flared disc, the thick disc and the spheroid populations. The model is tuned to produce reliable predictions in the visible and the near-infrared in wide photometric bands from U to K. Finally, we describe applications such as photometric and astrometric simulations and a new classification tool based on a Bayesian probability estimator, which could be used in the framework of Virtual Observatories. As examples, samples of simulated star counts at different wavelengths and directions are also given.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/76364f4fe41008afe0f61d7c1f739bd7158a343b

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Citations in the corpus

MODELING KEPLER TRANSIT LIGHT CURVES AS FALSE POSITIVES: REJECTION OF BLEND SCENARIOS FOR KEPLER-9, AND VALIDATION OF KEPLER-9 d, A SUPER-EARTH-SIZE PLANET IN A MULTIPLE SYSTEM (2010, methodology): “The frequency of stars in the mass range permitted by BLENDER was estimated using the Besançon Galactic structure models of Robin et al. (2003), specifically for the R band, which is the closest available to the Kepler passband.”
DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R⨁ SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR (2015, methodology): “…for the blend frequency calculation included the number density of stars in the vicinity of the target from the Besançon Galactic structure model (Robin et al. 2003, 2012),12 and the rates of occurrence of eclipsing bina- 12http://model.obs-besancon.fr . ries (Slawson et al. 2011) and of…”
A STELLAR-MASS-DEPENDENT DROP IN PLANET OCCURRENCE RATES (2014, methodology): “Howard et al. (2012) explored the metallicity gradient as a function of spectral type in the Kepler sample using the Besancon galactic model (Robin et al. 2003).”
TRANSIT TIMING OBSERVATIONS FROM KEPLER. IV. CONFIRMATION OF FOUR MULTIPLE-PLANET SYSTEMS BY SIMPLE PHYSICAL MODELS (2012, methodology): “For the former, we used the Besancon model of the galaxy (Robin et al. 2003) to estimate the number of background stars within the region allowed by the centroid shift result and the region in the allowed magnitude difference (or stellar mass).”
The DART Imaging And CaT Survey of the Fornax Dwarf Spheroidal Galaxy (2006, methodology): “A similar result is obtained by adding a Galactic component to the simulated velocities of Fornax, as a Gaussian with parameters determined from the Besançon model (Robin et al. 2003).”
KiDS+VIKING-450: Cosmic shear tomography with optical and infrared data (2018, methodology): “Stars are injected as PSF images at random positions, with their magnitude distribution derived from the Besançon model (Robin et al. 2003).”
Predictions of the WFIRST Microlensing Survey. I. Bound Planet Detection Rates (2018, methodology): “It is intermediate to the original, publicly available version (Robin et al. 2003), and a more recent version (Robin et al. 2012).”
On the Accretion Origin of a Vast Extended Stellar Disk around the Andromeda Galaxy (2005, methodology): “We have superimposed the expected Galactic contribution over a 0.25◦ area in the direction of M31 according to the Besançon Galactic starcounts model (Robin et al. 2004), onto which we have applied the color-magnitude selection window used for spectroscopic target selection.”
THE LARGE-SCALE STRUCTURE OF THE HALO OF THE ANDROMEDA GALAXY. I. GLOBAL STELLAR DENSITY, MORPHOLOGY AND METALLICITY PROPERTIES (2013, methodology): “However, since not every candidate star in their colormagnitude selection box within the DEIMOS fields could be observed, they further used the Besançon Galactic model (Robin et al. 2003) to weight the relative number of M31 RGB stars in each field.”
The GALAH survey: observational overview and Gaia DR1 companion (2016, methodology): “Using the Galaxia software (Sharma et al. 2011), which simulates synthetic observation of the Milky Way using a Besançon model (Robin et al. 2003) and Padova isochrones (Bertelli et al. 1994; Marigo et al. 2008), we predict that 75% of these stars belong to the thin disk, 24% to the thick disk,…”
Limits on the Macho Content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds (2006, background): “(3) Much excitement was generated by the MACHO collaboration’s measurement of the LMC microlensing rate which suggested that a significant amount of the Milky Way’s Halo is comprised of machos.”
The UKIDSS galactic plane survey (2007, methodology): “The Besançon Galactic stellar population model2 (Robin et al.2003) is used to help interpret the diagrams and we then compare some diagrams for the synthetic population with the real data.”
Gaia Universe model snapshot - A statistical analysis of the expected contents of the Gaia catalogue (2012, methodology): “Contrarily to Robin et al. (2003) metallicities [Fe/H] are computed through an empirical age-metallicity relation ψ (Z,Age) from Haywood (2008).”
THE EXTREMELY RED, YOUNG L DWARF PSO J318.5338−22.8603: A FREE-FLOATING PLANETARY-MASS ANALOG TO DIRECTLY IMAGED YOUNG GAS-GIANT PLANETS (2013, methodology): “We applied a relative-to-absolute parallax correction of 0.74± 0.13mas derived from the Besançon model of the Galaxy (Robin et al. 2003).”
Star formation rates and efficiencies in the Galactic Centre (2017, methodology): “The Robin et al. (2003) and Launhardt et al. (2002) estimate are around half of the total measured luminosity we find within |l| < 1◦ and |b| < 0.5◦ (5.7 ± 1.7 × 108 L ).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, background): “…local stellar surface density of 38 M / pc2 (Bovy & Rix 2013) and scale lengths Rd = 2.15 kpc (Bissantz & Gerhard 2002, Bovy & Rix 2013), 2.6 kpc (Robin et al. 2003, Jurić et al. 2008), and 3.0 kpc (Kent et al. 1991, Gould et al. 1996) and includes a gas disk with surface density of 13 M / pc2…”
CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD (2013, methodology): “We use the model of stellar population synthesis of our Milky Way of Robin et al. (2003)1 to estimate the metallicity distribution of stars in GOODS-S and find a median value of [Fe/H]∼-0.5.”
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) (2007, neutral): “In initial planning all “visits” would be kept to less than 60 minutes to limit the amount of MARVELS fringe broadening from geocentric velocity changes over the exposure. in expected distributions were seen when comparing the results of the TRILEGAL and Besançon models.”