Found 41 talks archived in The Galaxy
In this talk I present an overview of the structure, activity and goals
of the Gaia-ESO survey, a large public spectroscopic survey aimed at investigating
the origin and formation history of our Galaxy by collecting high quality spectroscopy
of representative samples (about 105 Milky Way stars) of all Galactic stellar populations,
in the field and in clusters. Briefly, I discuss the most relevant results obtained so far.
In particular, I present our study on the internal kinematics of Galactic globular clusters based on the radial estimates obtained from the survey complemented with ESO archive data.
Gaia - the ESA cornerstone astrometric mission - was launched in December 2013, with the goal of censing the Milky Way population in a 6D space (positions and velocity) of 10^9 point-like obects, with errors
100-1000 times smaller than Hipparcos, with three color magnitudes and spectra as well. The scientific impact of its data will be large in many fields of astrophysics, from Galactic science, to Solar system objects, to stellar astrophysics, to galaxies and Quasars; from the distance ladder revision to fundamental physics. I will describe the mission concept, the scientific goals, and the present status of the mission, with special attention to the flux calibration of Gaia data.
The structure, kinematics and stellar population of the Galactic bulge is very complex. Only three years ago the bulge was discovered to be X-shaped, a structure believed to originate from the dynamical instabilities of a disk, through the formation and posterior heating of a bar. The study of its kinematics reveals a cylindrical rotation, typical of a bar, suggesting the absence of a spheroidal component. Nevertheless, the bulge stellar population is old, has a radial metallicity gradient, and element ratio indicative of a short formation timescale. All these elements conflict with a simplistic view of the bulge as a heated bar, formed via "secular" evolution of a disk. I will review our knowledge of the bulge properties as traced by the 3D structure, kinematics, and chemical composition of its red clump stars.
3- Other spectroscopic surveys and analysis strategies
- eBOSS, BigBOSS, HETDEX, WEAVE, 4MOST
- data mashup: astrometry, photometry and spectroscopy together
- reconstructing the Galaxy
- 'observing' galaxy simulations
- discovery and follow-up of interesting/exotic targets: HVS, UMPS, CEMPS, RCrBs...
5- Some current problems and opportunities
- simulating kinematics
- simulating variables
- simulating non-solar scaled populations
- simulating rare and extreme populations (e.g. X-ray sources, PNe,
hot-WDs, AGB-manque', C stars, IR-emission by mass-losing stars)
- opportunities opened by asteroseismology
5- The Galactic halo
- mass, extent, shape
- substructure, inner/outer halo
5- The Galactic bulge
- observational status on bulge kinematics and chemical properties in the context of other bulges
- ideas about the formation of the bulge
5- SPH basics
- numerical viscosity
- Kelvin-Helmholtz instabilities
- other problems and their amelioration
- APOGEE, RAVE, SDSS/SEGUE/BOSS, Gaia-ESO
- Spectral classification
- radial velocities
- automated data analysis
- Transitioning from Science to Industry - Hurdles, Pros and ConsDr. Karsten BergerThursday November 2, 2017 - 10:30