Galaxy Evolution at High Resolution: The New View of the Milky Way's Disc. Jo Bovy (University of Toronto; Canada Research Chair)
|
|
|
- Francine Jennings
- 5 years ago
- Views:
Transcription
1 Galaxy Evolution at High Resolution: The New View of the Milky Way's Disc Jo Bovy (University of Toronto; Canada Research Chair)
2
3 WHY THE MILKY WAY?
4 WHY THE MILKY WAY? Detailed measurements of position, velocity, age, abundances [X/ H] of individual stars
5 WHY THE MILKY WAY? Detailed measurements of position, velocity, age, abundances [X/ H] of individual stars Detailed chemical evolution and star-formation history: gas inflows/outflows, SNe yields, IMF,
6 WHY THE MILKY WAY? Detailed measurements of position, velocity, age, abundances [X/ H] of individual stars Detailed chemical evolution and star-formation history: gas inflows/outflows, SNe yields, IMF, Detailed measurements of spatial and kinematical distributions of stellar populations of different abundances, ages
7 WHY THE MILKY WAY? Detailed measurements of position, velocity, age, abundances [X/ H] of individual stars Detailed chemical evolution and star-formation history: gas inflows/outflows, SNe yields, IMF, Detailed measurements of spatial and kinematical distributions of stellar populations of different abundances, ages Archaeological record: metal-poor stars & early galaxy formation, chemical tagging
8 WHY THE MILKY WAY? Detailed measurements of position, velocity, age, abundances [X/ H] of individual stars Detailed chemical evolution and star-formation history: gas inflows/outflows, SNe yields, IMF, Detailed measurements of spatial and kinematical distributions of stellar populations of different abundances, ages Archaeological record: metal-poor stars & early galaxy formation, chemical tagging Detailed dynamical modeling: 3D distribution of mass (stars, dark matter), importance of non-axisymmetric flows, resonances,
9 MILKY WAY DISK MASS BUDGET Double-exponential-ish with h Z ~ 350 pc, h R ~ 2-3 kpc (e.g., Juric et al. 2008, Bovy & Rix 2013)
10 MILKY WAY DISK MASS BUDGET Double-exponential-ish with h Z ~ 350 pc, h R ~ 2-3 kpc (e.g., Juric et al. 2008, Bovy & Rix 2013) Mass ~ 5.5 x M sun, maximal or close to it (Bovy & Rix 2013)
11 MILKY WAY DISK MASS BUDGET Double-exponential-ish with h Z ~ 350 pc, h R ~ 2-3 kpc (e.g., Juric et al. 2008, Bovy & Rix 2013) Mass ~ 5.5 x M sun, maximal or close to it (Bovy & Rix 2013) See Bland-Hawthorn & Gerhard (2016, ARAA) for most up-todate Galactic parameters
12 Bland-Hawthorn & Gerhard (2016)
13 MILKY WAY DISK MASS BUDGET: SOLAR NEIGHBORHOOD Solar neighborhood inventories from counting (McKee et al. 2015, Flynn et al. 2006) and dynamics (e.g., Kuijken & Gilmore 1989, Zhang et al. 2013) McKee et al. (2015)
14 MILKY WAY DISK MASS BUDGET: SOLAR NEIGHBORHOOD McKee et al. (2015)
15 MILKY WAY DISK MASS BUDGET: SOLAR NEIGHBORHOOD McKee et al. (2015) > Mass dominated by massive stellar disk
16 OBSERVABLES AND SURVEYS
17 OBSERVABLES AND SURVEYS Individual-star measurements > trace populations
18 OBSERVABLES AND SURVEYS Individual-star measurements > trace populations (x,v) > combination of astrometry (celestial positions, parallaxes, proper motions), photometric distances, spectroscopic line-of-sight velocities > Gaia
19 OBSERVABLES AND SURVEYS Individual-star measurements > trace populations (x,v) > combination of astrometry (celestial positions, parallaxes, proper motions), photometric distances, spectroscopic line-of-sight velocities > Gaia [Fe/H], [a/fe], [C/Fe], : medium-to-high resolution surveys: SEGUE, RAVE now, DESI, PFS future
20 OBSERVABLES AND SURVEYS Individual-star measurements > trace populations (x,v) > combination of astrometry (celestial positions, parallaxes, proper motions), photometric distances, spectroscopic line-of-sight velocities > Gaia [Fe/H], [a/fe], [C/Fe], : medium-to-high resolution surveys: SEGUE, RAVE now, DESI, PFS future Individual abundances for many elements [X/Fe]: high-resolution spec. surveys: APOGEE, GALAH, Gaia-ESO now, 4MOST, WEAVE, MOONS, MSE, future
21 OBSERVABLES AND SURVEYS Individual-star measurements > trace populations (x,v) > combination of astrometry (celestial positions, parallaxes, proper motions), photometric distances, spectroscopic line-of-sight velocities > Gaia [Fe/H], [a/fe], [C/Fe], : medium-to-high resolution surveys: SEGUE, RAVE now, DESI, PFS future Individual abundances for many elements [X/Fe]: high-resolution spec. surveys: APOGEE, GALAH, Gaia-ESO now, 4MOST, WEAVE, MOONS, MSE, future Ages: difficult, but possible for large samples now and in near future
22 CHEMICAL EVOLUTION IN THE MILKY WAY
23 THE ABUNDANCE PLANE IN THE SOLAR NEIGHBORHOOD Kinematically- and (~)metallicity unbiased sample of ~1,000 stars within ~50 pc from the Sun Improves on abundant earlier work by Fuhrmann, Prochaska, Reddy, Bensby, et al. Adibeykan et al. (2012) Blue: high-velocity stars Red: low-velocity stars
24 METALLICITY DISTRIBUTION IN THE SOLAR NEIGHBORHOOD Peaked at solar, but broad and largely symmetric Casagrande et al. (2011) High-[Fe/H] tail hard to explain with a one-zone model Vertical gradient about -0.3 dex/kpc, radial gradient about -0.1 dex/kpc Largely flat behavior w/ Z when split by [α/fe] Calculated from Bovy et al. (2012); see also Schlesinger et al. (2014)
25
26 APOGEE HI-RES BEYOND THE Infrared H-band spectrograph SOLAR NEIGHBORHOOD high resolution (R ~ 22,500) S/N > 100 / pixel (J-Ks)0 > 0.5, H <~ 13.8 vlos, logg, Teff, + 15 abundances (C,N,O,Na,Mg,Al,Si,S,K,Ca,Ti,V,Mn,Fe,Ni) APOGEE-1survey complete: 500k high-res spectra for ~150,000 stars PI: Steve Majewski, + many people
27 Majewski et al. (2016) Credit: Michael Hayden, Background: R. Hurt, JPL-Caltech, NASA
![ABUNDANCE DISTRIBUTION Nidever, Bovy et al. (2014) Solar neighborhood [α/fe] vs.](/docs-images/90/102866869/images/28-6.jpg "[Fe/H] similar to previous high-resolution studies, e.g., HARPS sample (Adibekyan et al.")
28 ABUNDANCE DISTRIBUTION Nidever, Bovy et al. (2014) Solar neighborhood [α/fe] vs. [Fe/H] similar to previous high-resolution studies, e.g., HARPS sample (Adibekyan et al. 2012) <~ 50 pc Data from Adibekyan et al. (2012) Haywood et al. (2013)
29 ABUNDANCE DISTRIBUTION Nidever, Bovy et al. (2014) Solar neighborhood [α/fe] vs. [Fe/H] similar to previous high-resolution studies, e.g., HARPS sample (Adibekyan et al. 2012)
30 ABUNDANCE DISTRIBUTION Nidever, Bovy et al. (2014) 6 kpc 8 kpc 10 kpc
31 ABUNDANCE DISTRIBUTION Nidever, Bovy et al. (2014) 6 kpc 8 kpc 10 kpc High-[α/Fe] sequence remarkably uniform throughout the Galaxy
32 ABUNDANCE DISTRIBUTION Nidever, Bovy et al. (2014) 6 kpc 8 kpc 10 kpc High-[α/Fe] sequence remarkably uniform throughout the Galaxy Increasing radii = high-[α/ Fe] sequence disappears
33 LARGER-SCALE ABUNDANCE DISTRIBUTION Hayden, Bovy, et al. (2015) ~whole disk!
34 CHEMICAL EVOLUTION [α/fe] (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
35 CHEMICAL EVOLUTION Early: SNe II: rich in α elements and ironpeak [α/fe] (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
36 CHEMICAL EVOLUTION Early: SNe II: rich in α elements and ironpeak [α/fe] (O,Mg,Si,S, Ca,Ti) SNe Ia only produce iron-peak elements and drive down the relative abundance of α to Fe [Fe/H] (Fe,Ni)
37 CHEMICAL EVOLUTION [α/fe] (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
38 CHEMICAL EVOLUTION [α/fe] Efficiency of star formation (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
39 CHEMICAL EVOLUTION [α/fe] (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
40 CHEMICAL EVOLUTION [α/fe] Efficiency of outflows (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
41 CHEMICAL EVOLUTION [α/fe] (O,Mg,Si,S, Ca,Ti) [Fe/H] (Fe,Ni)
42 HIGH-ALPHA SEQUENCE Nidever, Bovy et al. (2014) Star formation Early evolution of the Disk Gas outflows
43 HIGH-ALPHA SEQUENCE Nidever, Bovy et al. (2014) Star formation Early evolution of the Disk Star formation and gas in/outflow must have been very similar everywhere at R < 10 kpc within the first ~4 Gyr of the Disk s existence Gas outflows
44 HIGH-ALPHA SEQUENCE Nidever, Bovy et al. (2014) Star formation Early evolution of the Disk Star formation and gas in/outflow must have been very similar everywhere at R < 10 kpc within the first ~4 Gyr of the Disk s existence Gas outflows SFR constant to within ~15%
45 METALLICITY DISTRIBUTION Hayden, Bovy, et al. (2015) Beyond the [α/fe] vs. [Fe/H] track, APOGEE can measure the MDF = p([fe/h]) over the entire radial range of the disk
46 METALLICITY DISTRIBUTION Hayden, Bovy, et al. (2015) Beyond the [α/fe] vs. [Fe/H] track, APOGEE can measure the MDF = p([fe/h]) over the entire radial range of the disk Inner disk MDF (R 7 kpc) is negatively skewed in the way a one-zone model would be skewed
47 METALLICITY DISTRIBUTION Hayden, Bovy, et al. (2015) Beyond the [α/fe] vs. [Fe/H] track, APOGEE can measure the MDF = p([fe/h]) over the entire radial range of the disk Inner disk MDF (R 7 kpc) is negatively skewed in the way a one-zone model would be skewed Center disk MDF (7 kpc R 11 kpc) broad and symmetric
48 METALLICITY DISTRIBUTION Hayden, Bovy, et al. (2015) Beyond the [α/fe] vs. [Fe/H] track, APOGEE can measure the MDF = p([fe/h]) over the entire radial range of the disk Inner disk MDF (R 7 kpc) is negatively skewed in the way a one-zone model would be skewed Center disk MDF (7 kpc R 11 kpc) broad and symmetric Outer disk MDF (R 11 kpc) is strongly positively skewed
49 CHEMICAL EVOLUTION ~constant SFH N [Fe/H] (Fe,Ni)
50 CHEMICAL EVOLUTION ~constant SFH ~declining SFH (gas starved) N [Fe/H] (Fe,Ni)
51 CHEMICAL EVOLUTION Metallicity gradient N [Fe/H] (Fe,Ni) Hayden, Bovy, et al. (2015)
52 CHEMICAL EVOLUTION Metallicity gradient N [Fe/H] (Fe,Ni) Hayden, Bovy, et al. (2015)
53 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS N [Fe/H] (Fe,Ni)
54 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS N [Fe/H] (Fe,Ni)
55 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS N [Fe/H] (Fe,Ni)
56 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS N [Fe/H] (Fe,Ni)
57 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS+MIGRATION N [Fe/H] (Fe,Ni)
58 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS+MIGRATION N [Fe/H] (Fe,Ni)
59 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS+MIGRATION N [Fe/H] (Fe,Ni)
60 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS+MIGRATION N [Fe/H] (Fe,Ni)
61 CHEMICAL EVOLUTION: NON-CIRCULAR ORBITS+MIGRATION N [Fe/H] (Fe,Ni)
62 METALLICITY DISTRIBUTION Hayden, Bovy, et al. (2015) Same Rg, w/ velocity dispersion Rg diffusion, w/ velocity dispersion Radial trend of skewness is difficult to explain with simple chemical evolution and epicyclic blurring Migration of stars (or gas) over ~5 kpc is required to supply the metal-rich tail of the middle and outer disk MDFs (see Loebman et al for a simulation)
63 < At formation Stars Today > Gas Loebman et al. (2016)
64 DISSECTING THE MILKY WAY S STELLAR POPULATIONS
65 IDENTIFYING DISK POPULATIONS (currently) impossible to identify single-stellar populations, but would like to get as close to that as possible Previously, populations were typically defined based on position or velocity (bad!) Even integrals of the motion likely change significantly over the lifetime of a star Surface abundance of stars don t change * over the stellar lifetime and uniform for SSPs Natural to define populations based on abundances (~chemical tagging)
66 IDENTIFYING DISK POPULATIONS (currently) impossible to identify single-stellar populations, but would like to get as close to that as possible Previously, populations were typically defined based on position or velocity (bad!) Even integrals of the motion likely change significantly over the lifetime of a star Surface abundance of stars don t change * over the stellar lifetime and uniform for SSPs Natural to define populations based on abundances (~chemical tagging) SDSS/SEGUE
67 IDENTIFYING DISK POPULATIONS (currently) impossible to identify single-stellar populations, but would like to get as close to that as possible Previously, populations were typically defined based on position or velocity (bad!) Even integrals of the motion likely change significantly over the lifetime of a star Surface abundance of stars don t change * over the stellar lifetime and uniform for SSPs Natural to define populations based on abundances (~chemical tagging) SDSS/SEGUE
68 MONO-ABUNDANCE POPULATIONS vertical profile: scale height radial profile: scale length thick short thin long Bovy et al. (2012abc) using SDSS/SEGUE data
69 MONO-ABUNDANCE POPULATIONS velocity dispersion: vertical vertical profile: detailed distribution of mass warm cool Bovy et al. (2012abc) using SDSS/SEGUE data
70 APOGEE MAPS Bovy et al. (2016a)
71 APOGEE MAPS Bovy et al. (2016a)
72 Combination of Green et al. (2015), Marshall et al. (2006), Drimmel et al. (2003) see Bovy et al. (2016b)
73 APOGEE MAPS: RADIAL PROFILE Bovy et al. (2016a) old younger
74 APOGEE MAPS: RADIAL PROFILE Bovy et al. (2016a) old younger
75 APOGEE MAPS: RADIAL PROFILE Bovy et al. (2016a) old younger
76 APOGEE MAPS: RADIAL PROFILE Bovy et al. (2016a)? old younger
77 APOGEE MAPS: VERTICAL PROFILE Bovy et al. (2016a) old younger
78 MAPS AND THE OVERALL DISK Bovy & Rix (2013) Rd ~ 2.15 kpc
79 MAPS AND THE OVERALL DISK
80 MAPS AND THE OVERALL DISK Bird et al. (2013)
81 MAPS AND THE OVERALL DISK Bird et al. (2013)
82 MAPS AND THE OVERALL DISK Bird et al. (2013) Minchev et al. (2015) Martig et al. (2014)
83 SEGUE/APOGEE MAPS: IMPLICATIONS
84 SEGUE/APOGEE MAPS: IMPLICATIONS High-alpha / old disk: centrally-concentrated, pure exponential > MW formed inside-out
85 SEGUE/APOGEE MAPS: IMPLICATIONS High-alpha / old disk: centrally-concentrated, pure exponential > MW formed inside-out Low-alpha donuts: strong correspondence between [Fe/ H] and (birth) radius > equilibrium chemical evolution over last ~6-8 Gyr
86 SEGUE/APOGEE MAPS: IMPLICATIONS High-alpha / old disk: centrally-concentrated, pure exponential > MW formed inside-out Low-alpha donuts: strong correspondence between [Fe/ H] and (birth) radius > equilibrium chemical evolution over last ~6-8 Gyr Flaring of low-alpha, cool populations > consistent with radial migration
87 SEGUE/APOGEE MAPS: IMPLICATIONS High-alpha / old disk: centrally-concentrated, pure exponential > MW formed inside-out Low-alpha donuts: strong correspondence between [Fe/ H] and (birth) radius > equilibrium chemical evolution over last ~6-8 Gyr Flaring of low-alpha, cool populations > consistent with radial migration No flaring of high-alpha populations > likely formed thick in turbulent ISM (cf. high-z studies)
88 MILKY WAY EVOLUTION
89 MILKY WAY EVOLUTION Great progress in the last few years
90 MILKY WAY EVOLUTION Great progress in the last few years Radial migration: good theoretical underpinnings, shown to be important in various ways
91 MILKY WAY EVOLUTION Great progress in the last few years Radial migration: good theoretical underpinnings, shown to be important in various ways Disk evolution appears to have been very quiescent over the last ~10 Gyr, with no large fraction of stars accreted by mergers
92 MILKY WAY EVOLUTION Great progress in the last few years Radial migration: good theoretical underpinnings, shown to be important in various ways Disk evolution appears to have been very quiescent over the last ~10 Gyr, with no large fraction of stars accreted by mergers Disk formed inside-out, and was likely turbulent at redshift ~ 2
93 MILKY WAY EVOLUTION Great progress in the last few years Radial migration: good theoretical underpinnings, shown to be important in various ways Disk evolution appears to have been very quiescent over the last ~10 Gyr, with no large fraction of stars accreted by mergers Disk formed inside-out, and was likely turbulent at redshift ~ 2 But no coherent picture has yet emerged that ties everything together
94 AGES
95 AGES FROM PARALLAXES AND ISOCHRONES Many methods, but difficult to measure Traditional method: turn-off stars have widely different magnitudes at different ages > abs. mag. from parallaxes give tance uncertainties 1. ages Uncertainties ~ 1 Gyr Figure 3: Overview of Gaia data: shown are isochrones of solar metallicity in absolute magnitude in the Gaia G bandpass and effective temperature. The isochrones are colorcoded by the maximum distance for which Gaia will deliver 10% dis- In the context of this proposal their most important characteristics are: Turnoff/subgiant stars: Isochrones of different ages for these stars separate widely (shown are isochrones of 1, 2, 3, 5, 7, 10, and 12.6Gyr), allowing ages to be estimated up to 3kpc without age bias. Redclump and giant stars: The intrinsic brightness of these stars means that they can be traced throughout the whole extent of the disk in regions of low extinction and Gaia can measure their proper mo- Possible with Gaia over ~3-4 kpc in the disk > limited tions everywhere. Similar method for giants + surface gravity > APOGEE+Gaia tal abundances. (Feuillet, Bovy et al. 2016) MG Red clump stars 10% distance uncertainty log T eff Turn off/ subgiant stars 3.6 Giants Main sequence APOGEE can additionally measure their line-ofsight velocities and detailed elemen- Maximum distance for 10% distance uncertainty (kpc) Main-sequence stars: Millions of main-sequence stars will have accurate positions and velocities from Gaia out to 2kpc and many millions more beyond can be studied using photometric distances. 3.2 The Gaia revolution: ages and precise phase-space coordinates for millions of stars /63 10/25 4/10 2/4 1/2 0/1 3.4 distance for G = 15/17 (kpc)
96 AGES IN THE ABUNDANCE PLANE IN THE SOLAR NEIGHBORHOOD Haywood et al. (2013) Data from Adibekyan et al. (2012) Haywood et al. (2013) measured ages for ~400 turnoff/sub-giant stars in the Adibekyan sample See also earlier work by Edvardsson et al. (1993) and Nordstrom et al. (2004)
![AGES IN THE ABUNDANCE PLANE IN THE SOLAR NEIGHBORHOOD [α/fe] vs.](/docs-images/90/102866869/images/97-2.jpg "age (mostly) confirms to expectations Large [Fe/H] scatter at a given age for stars younger than ~8 Gyr Haywood et al.")
97 AGES IN THE ABUNDANCE PLANE IN THE SOLAR NEIGHBORHOOD [α/fe] vs. age (mostly) confirms to expectations Large [Fe/H] scatter at a given age for stars younger than ~8 Gyr Haywood et al. (2013) Well-defined age-[fe/h] relation for high-alpha stars (filled blue dots)
98 NEW METHODS: AGES FOR GIANTS
99 NEW METHODS: AGES FOR GIANTS Giants: mass+z > main-sequence lifetime > age
100 NEW METHODS: AGES FOR GIANTS Giants: mass+z > main-sequence lifetime > age Asteroseismology: oscillations in the convective surface layer related to density and surface-gravity > mass and radius
101 NEW METHODS: AGES FOR GIANTS Giants: mass+z > main-sequence lifetime > age Asteroseismology: oscillations in the convective surface layer related to density and surface-gravity > mass and radius Sub-giants/giants: deepening of convective layer leads to C & N mixing and partial C burning > C/N decreases Martig et al. (2015)
102 NEW METHODS: AGES FOR GIANTS Giants: mass+z > main-sequence lifetime > age Asteroseismology: oscillations in the convective surface layer related to density and surface-gravity > mass and radius Sub-giants/giants: deepening of convective layer leads to C & N mixing and partial C burning > C/N decreases Mass-dependence of this effect: C/N > mass > age (Masseron & Gilmore 2015, Martig et al. 2016) Martig et al. (2015)
103 NEW METHODS: AGES FOR GIANTS Giants: mass+z > main-sequence lifetime > age Asteroseismology: oscillations in the convective surface layer related to density and surface-gravity > mass and radius Sub-giants/giants: deepening of convective layer leads to C & N mixing and partial C burning > C/N decreases Mass-dependence of this effect: C/N > mass > age (Masseron & Gilmore 2015, Martig et al. 2016) Bright giants in APOGEE: potential to get ages out to ~10 kpc and beyond Martig et al. (2015)
104 Can start to look at age distributions of large samples: RC in APOGEE (Martig et al. 2016): High-[a/Fe] sequence is > 8 Gyr Low-[a/Fe] sequence younger than 8 Gyr; no metallicity trend
105 AGE ISSUES All methods have large, non-symmetric uncertainties on the ages: sub-giants ~1 Gyr, giants ~3 Gyr > Need to deal with this: Hierarchical modeling (Feuillet et al. 2016) < Feuillet et al. (2016) > Systematics not well-understood, esp. in newer C/N methods, need more empirical and theoretical work to understand these Giants are age-biased, so recovering underlying age distribution requires stellar models, IMF
106 CONCLUSIONS Exciting time for Milky Way studies with much new data on the way
107 CONCLUSIONS Exciting time for Milky Way studies with much new data on the way Now have abundance patterns over the entire radial range of the disk
108 CONCLUSIONS Exciting time for Milky Way studies with much new data on the way Now have abundance patterns over the entire radial range of the disk Chemical tracks (Nidever et al. 2014, Hayden et al. 2015): Early evolution of the Milky Way disk uniform
109 CONCLUSIONS Exciting time for Milky Way studies with much new data on the way Now have abundance patterns over the entire radial range of the disk Chemical tracks (Nidever et al. 2014, Hayden et al. 2015): Early evolution of the Milky Way disk uniform Metallicity distribution functions (Hayden et al. 2015): Change in skew from negative (inner) to positive (outer) > radial migration
110 CONCLUSIONS Exciting time for Milky Way studies with much new data on the way Now have abundance patterns over the entire radial range of the disk Chemical tracks (Nidever et al. 2014, Hayden et al. 2015): Early evolution of the Milky Way disk uniform Metallicity distribution functions (Hayden et al. 2015): Change in skew from negative (inner) to positive (outer) > radial migration Spatial decomposition in metallicity/age reveals stellar donuts: [Fe/H] > birth radius
111 CONCLUSIONS Exciting time for Milky Way studies with much new data on the way Now have abundance patterns over the entire radial range of the disk Chemical tracks (Nidever et al. 2014, Hayden et al. 2015): Early evolution of the Milky Way disk uniform Metallicity distribution functions (Hayden et al. 2015): Change in skew from negative (inner) to positive (outer) > radial migration Spatial decomposition in metallicity/age reveals stellar donuts: [Fe/H] > birth radius Starting to obtain large samples of ages > mono-age studies and comparison with simulations
112 MILKY WAY EVOLUTION
113 REPORT CARD: MW DISK EVOLUTION Satellite interaction (Quinn et al. 1993, Abadi et al. 2003, ) Radial migration (Sellwood & Binney 2002, Schoenrich & Binney 2009, ) State of SF gas (Bournaud et al. 2009, Stinson et al., Bird et al. 2013, ) Gas outflows low [α/fe] high [α/fe]
114 REPORT CARD: MW DISK EVOLUTION Satellite interaction Radial migration State of SF gas Gas outflows low [α/fe] No high [α/fe] > few
115 REPORT CARD: MW DISK EVOLUTION Satellite interaction Radial migration State of SF gas Gas outflows low [α/fe] No Yes high [α/fe] > few
116 REPORT CARD: MW DISK EVOLUTION Satellite interaction Radial migration State of SF gas Gas outflows low [α/fe] No Yes high [α/fe] > few No*
117 REPORT CARD: MW DISK EVOLUTION Satellite interaction Radial migration State of SF gas Gas outflows low [α/fe] No Yes high [α/fe] No No*
118 REPORT CARD: MW DISK EVOLUTION Satellite interaction Radial migration State of SF gas Gas outflows low [α/fe] No Yes cold high [α/fe] No No* warm
119 REPORT CARD: MW DISK EVOLUTION Satellite interaction Radial migration State of SF gas Gas outflows low [α/fe] No Yes cold High high [α/fe] No No* warm Low
Chemo-dynamical disk modeling. Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP)
Chemo-dynamical disk modeling Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP) Talk outline Effect of disk asymmetries on disk dynamics. Radial migration in galactic disks. Chemo-dynamical disk
Galaxy simulations in the Gaia era. Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP)
Galaxy simulations in the Gaia era Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP) What we think our Galaxy looks like GCS data (Hipparcos satellite) - the only pre-gaia sample with good proper
The Thick Thin Disk and the Thin Thick Disk: a New Paradigm from Gaia
The Thick Thin Disk and the Thin Thick Disk: a New Paradigm from Gaia Michael Hayden Alejandra Recio-Blanco, Patrick de Laverny, Sarunas Mikolaitis, Guillaume Guiglion, Anastasia Titarenko Observatoire
The Structure and Substructure of the Milky Way Galaxy Discs. Rosemary Wyse
The Structure and Substructure of the Milky Way Galaxy Discs Rosemary Wyse Hiroshima, 30 th November 2016 The Fossil Record: Galactic Archaeology Studying low-mass old stars near-field cosmology There
The Apache Point Observatory Galactic Evolution Experiment. Ricardo Schiavon
The Apache Point Observatory Galactic Evolution Experiment Ricardo Schiavon CS20, Boston, August 1st, 2018 Overview paper: Majewski, Schiavon et al. (2017) APOGEE at a Glance Dual hemisphere spectroscopic
Action-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE
IAU Symposium 330 Nice, 27. April 2017 Action-based Dynamical Modeling of the Milky Way Disk with Gaia & RAVE Wilma Trick (MPIA, Heidelberg) Hans-Walter Rix (MPIA) Jo Bovy (Uni Toronto) Open Questions
Characterization of the exoplanet host stars. Exoplanets Properties of the host stars. Characterization of the exoplanet host stars
Characterization of the exoplanet host stars Exoplanets Properties of the host stars Properties of the host stars of exoplanets are derived from a combination of astrometric, photometric, and spectroscopic
THE CHEMICAL EVOLUTION OF THE MILKY WAY DISK
THE CHEMICAL EVOLUTION OF THE MILKY WAY DISK 1. The simple picture of disk evolution: independent ring evolution, successes and failures 2. The dynamical picture: stars (and gas) moving around 3. A model
Abundance distribution in the Galactic thick disk
Abundance distribution in the Galactic thick disk omas Bensby Lund Observatory, Department of Astronomy and eoretical Physics Discovery of thick disks (Burstein 1979, ApJ, 234, 829) Discovery of the Galactic
Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee
![Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee](/thumbs/83/87302303.jpg "Determination of [α/fe] and its Application to SEGUE F/G Stars. Young Sun Lee")
Determination of [α/fe] and its Application to SEGUE F/G Stars Young Sun Lee Research Group Meeting on June 16, 2010 Outline Introduction Why [α/fe]? Determination of [α/fe] Validation of estimate of [α/fe]
Milky Way S&G Ch 2. Milky Way in near 1 IR H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/
Why study the MW? its "easy" to study: big, bright, close Allows detailed studies of stellar kinematics, stellar evolution. star formation, direct detection of dark matter?? Milky Way S&G Ch 2 Problems
Exploring the structure and evolu4on of the Milky Way disk
Exploring the structure and evolu4on of the Milky Way disk Results from the Gaia-ESO survey and plans for 4MOST Thomas Bensby Dept. of Astronomy and Theore3cal Physics Lund University Sweden Chemistry
The HERMES project. Reconstructing Galaxy Formation. Ken Freeman RSAA, ANU. The metallicity distribution in the Milky Way discs Bologna May 2012
The HERMES project Reconstructing Galaxy Formation Ken Freeman RSAA, ANU The metallicity distribution in the Milky Way discs Bologna May 2012 HERMES is a new high-resolution fiber-fed multi-object spectrometer
Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles
Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Ling Zhu, Jie Wang Contents 1
ON THE CHEMICAL EVOLUTION OF THE MILKY WAY. The Metallicity distribution of the halo in the hierarchical merging paradigm
ON THE CHEMICAL EVOLUTION OF THE MILKY WAY The Metallicity distribution of the halo in the hierarchical merging paradigm Halo abundance patterns and stellar yields Standard chemical evolution of solar
The role of radial migration in shaping the stellar populations of spiral galaxies
Mem. S.A.It. Suppl. Vol. 25, 64 c SAIt 2013 Memorie della Supplementi The role of radial migration in shaping the stellar populations of spiral galaxies R. Roškar Insititute for Theoretical Physics, University
Galactic archaeology with the RAdial Velocity Experiment
Galactic archaeology with the RAdial Velocity Experiment Georges Kordopatis & RAVE collaboration Leibniz-Institute for Astrophysics, Potsdam Multi-Object Spectroscopy in the next decade: Big questions,
Astronomisches Rechen-Institut Heidelberg, Germany. The evolution history of the extended solar neighbourhood
Astronomisches Rechen-Institut Heidelberg, Germany The evolution history of the extended solar neighbourhood Andreas Just Kseniia Sysoliatina, Ioanna Koutsouridou Content Dynamical disc model Local model
Age- Abundance Trends in the Solar Neighborhood. Diane Feuillet MPIA April 25, 2017 IAUS 330 Nice, France
Age- Abundance Trends in the Solar Neighborhood Diane Feuillet MPIA April 25, 2017 IAUS 330 Nice, France GalacNc Chemical EvoluNon Alpha elements Fe type elements [O/Fe] [Na/Fe] [Mg/Fe] [Cr/Fe] [Ca/Fe]
Gaia-LSST Synergy. A. Vallenari. INAF, Padova
Gaia-LSST Synergy A. Vallenari INAF, Padova The Galaxy view Unveiling the complex history of the MW assembly and internal evolution is still one of the main interest of astrophysics However the specific
Distribution of Mass in the Milky Way Galaxy, Leiden, July Laura V. Sales. Kapteyn Astronomical Institute, Groningen, The Netherlands
Distribution of Mass in the Milky Way Galaxy, Leiden, 13-17 July 2009 Laura V. Sales Kapteyn Astronomical Institute, Groningen, The Netherlands Outline - Brief review of thick disk formation scenarios:
Chemical evolution of the Galactic disk using Open Clusters
Chemical evolution of the Galactic disk using Open Clusters ICC Winter Meeting Feb 2017 1. Galactic Archaeology Unravel the formation and evolution of the Milky Way (MW) Resolved stars provide a fossil
Dynamics of the Milky Way
Jason Sanders (Oxford IoA) with James Binney Dynamics of the Milky Way Tidal streams & Extended Distribution Functions for the Galactic Disc Whistle-stop tour of a PhD Where is the dark matter? We can
TheGalacticDisk and Halo in the. Carlos Allende Prieto Instituto de Astrofísica de Canarias
TheGalacticDisk and Halo in the GaiaEra Carlos Allende Prieto Instituto de Astrofísica de Canarias Introduction Hierarchical galaxy formation Galaxy disks Doubledisks seenin manydisk galaxies observed
JINA Observations, Now and in the Near Future
JINA Observations, Now and in the Near Future Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics Examples SDSS-I, II, and III
Gaia Revue des Exigences préliminaires 1
Gaia Revue des Exigences préliminaires 1 Global top questions 1. Which stars form and have been formed where? - Star formation history of the inner disk - Location and number of spiral arms - Extent of
Gaia ITNG2013 School, Tenerife. Ken Freeman, Lecture 2: the thin disk
Gaia ITNG2013 School, Tenerife Ken Freeman, Lecture 2: the thin disk September 2013 The Thick Disk Thick disk Most spirals (including our Galaxy) have a second thicker disk component The thick disk and
Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution
Chap.3 The nature of Galactic components Overview of (old) Galactic components bulge, thick disk, metal-weak halo Globular clusters metallicity & age distribution Satellite galaxies spatial and metallicity
GALAXIES 626. The Milky Way II. Chemical evolution:
GALAXIES 626 The Milky Way II. Chemical evolution: Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which
From theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, give the prediction of the
The structure and formation of the Milky Way disks
Mem. S.A.It. Suppl. Vol. 25, 11 c SAIt 2013 Memorie della Supplementi The structure and formation of the Milky Way disks M. Haywood GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place
(Present and) Future Surveys for Metal-Poor Stars
(Present and) Future Surveys for Metal-Poor Stars Timothy C. Beers Department of Physics & Astronomy Michigan State University & JINA: Joint Institute for Nuclear Astrophysics SDSS 1 Why the Fascination
Oxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto!
Oxygen in red giants from near-infrared OH lines: 3D effects and first results from Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Overview! 1. APOGEE: status and prospects! 2. A first look at
DOES THE MILKY WAY HAVE AN ACCRETED DISK COMPONENT?
DOES THE MILKY WAY HAVE AN ACCRETED DISK COMPONENT? Gregory Ruchti Lund Observatory!!!! in collaboration with: Justin Read, Sofia Feltzing, Thomas Bensby, Antonio Pipino ACCRETED STARS Our current cosmology
Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator)
Overview of Gaia-ESO Survey results based on high-resolution spectra of FGK-type stars Rodolfo Smiljanic! (Gaia-ESO WG11 co-coordinator) The Gaia-ESO Survey http://www.gaia-eso.eu Public spectroscopic
Gaia DR2 and/versus RAVE DR5: application for the semi-analytic thin disk model
Gaia DR2 and/versus RAVE DR5: application for the semi-analytic thin disk model Speaker: Supervisor: Kseniia Sysoliatina (ARI) Prof. Dr. Andreas Just Gaia DR2 workshop Heidelberg, Outline (1) Comparison
Review of the Bulge Stellar Population And Comparison to the Nuclear Bulge
Review of the Bulge Stellar Population And Comparison to the Nuclear Bulge David M. Nataf, Australian National University 22 July, 2016 IAU Symposium 322, 'The Multi- Messenger Astrophysics of the Galactic
Stellar Populations in the Galaxy
Stellar Populations in the Galaxy Stars are fish in the sea of the galaxy, and like fish they often travel in schools. Star clusters are relatively small groupings, the true schools are stellar populations.
Asterseismology and Gaia
Asterseismology and Gaia Asteroseismology can deliver accurate stellar radii and masses Huber et al 2017 compare results on distances from Gaia and asteroseismology for 2200 Kepler stars Asteroseismology
The Gaia-ESO Spectroscopic Survey. Survey Co-PIs. Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs
The Gaia-ESO Spectroscopic Survey Survey Co-PIs Gerry Gilmore (IoA, Cambridge) & Sofia Randich (INAF/Arcetri) >300 CoIs Gaia-ESO survey context and motivations (conclusions and key words of several talks)
Chapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
Following the evolution of the Galactic disc with Open Clusters
Following the evolution of the Galactic disc with Open Clusters Laura Magrini INAF-Osservatorio Astrofisico di Arcetri With Nikos Prantzos and the GES collaboration (in particular Lorenzo Spina, Sofia
WEAVE Galactic Surveys
WEAVE Galactic Surveys A. Vallenari INAF, Padova On behalf of the Science Team Overview WEAVE Surveys Milky Way Surveys WEAVE Characteristics Project structure Primary Science Surveys There are six primary
The Besançon Galaxy Model development
The Besançon Galaxy Model development Annie C. Robin and collaborators Institut UTINAM, OSU THETA, Université Bourgogne-Franche-Comté, Besançon, France Outline Population synthesis principles New scheme
Phys/Astro 689: Lecture 11. Tidal Debris
Phys/Astro 689: Lecture 11 Tidal Debris Goals (1) We ll explore whether we can trace the accretion events that should have formed the Milky Way. (2) We ll discuss the impact of tidal debris on direct detection
arxiv: v1 [astro-ph.ga] 12 Dec 2018
![arxiv: v1 [astro-ph.ga] 12 Dec 2018](/thumbs/92/110901457.jpg "arxiv: v1 [astro-ph.ga] 12 Dec 2018")
DRAFT VERSION DECEMBER 13, 2018 Preprint typeset using LATEX style emulateapj v. 01/23/15 APOGEE ABUNDANCES ACROSS THE GALAXY: MIGRATION AND INFALL FROM RED GIANT AGES arxiv:1812.05092v1 [astro-ph.ga]
Spatial distribution of stars in the Milky Way
Spatial distribution of stars in the Milky Way What kinds of stars are present in the Solar neighborhood, and in what numbers? How are they distributed spatially? How do we know? How can we measure this?
From theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Update date: December 13, 2010 Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle,
Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia
Milky Way s Anisotropy Profile with LAMOST/SDSS and Gaia Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Chengqun Yang Contents 1 Stellar Halo
The Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution
I S I The Milky Way s rotation curve out to 100 kpc and its constraint on the Galactic mass distribution Yang Huang (LAMOST Fellow, yanghuang@pku.edu.cn) N G U N I V E R P E K T Y 1 8 9 8 Peking University
The Accretion History of the Milky Way
The Accretion History of the Milky Way Julio F. Navarro The Milky Way as seen by COBE Collaborators Mario Abadi Amina Helmi Matthias Steinmetz Ken Ken Freeman Andres Meza The Hierarchical Formation of
l about Ralph Schönrich (MPA, Hubble Fellow, OSU)
Al l about n io t a t ro Ralph Schönrich (MPA, Hubble Fellow, OSU) with Martin Asplund, James Binney Thomas Bilitewski, Luca Casagrande Walter Dehnen, Heather Morrison Model direct onflow ~ 75% of feed
The halo is specially interesting because gravitational potential becomes dominated by the dark matter halo
Evidence for dark matter in the Milky Way Astr 511: Galactic Astronomy Winter Quarter 2015 University of Washington Željko Ivezić The halo is specially interesting because gravitational potential becomes
THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy
THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS B. Barbuy IAG - Universidade de São Paulo Outline: Interest of studies on Galactic bulge and globulars Data available on metallicity,, kinematics in field
Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia
Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia J. Andersen 1,2, B. Nordström 1,2 1 Dark Cosmology Centre, The Niels Bohr Institute, University of Copenhagen, Denmark 2 Stellar Astrophysics
Overview of Dynamical Modeling. Glenn van de Ven
Overview of Dynamical Modeling Glenn van de Ven glenn@mpia.de 1 Why dynamical modeling? -- mass total mass stellar systems key is to their evolution compare luminous mass: constrain DM and/or IMF DM radial
Coordinate Systems! The geometry of the stream requires an oblate near-spherical halo!
Milky Way Galaxy (blue/ white points and orange bulge) with the Sun (yellow sphere), inner and outer Sgr stream models (yellow/red points respectively), Monoceros tidal stream model(violet points), and
Estimating the mass of our Milky Way from the LAMOST Galactic spectroscopic survey
2 nd LAMOST KEPLER WORKSHOP LAMOST in the era of large spectroscopic surveys July 31-August 3, 2017, @ Brussels Estimating the mass of our Milky Way from the LAMOST Galactic spectroscopic survey Yang Huang
Galactic Bulge Science
Galactic Bulge Science Ken Freeman Australian National University ngcfht meeting Hilo, Mar 27-29 2013 NGC 5746 1 The Galactic bulge was long thought to be a merger product. We now know that boxy bulges
Surface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
Classical observations of stellar properties
Classical observations of stellar properties Luca Casagrande M. Bessell - J. Meléndez - I. Ramírez / M. Asplund R. Schönrich / V. Silva Aguirre Spectroscopy F(l) : lots of info, but also model dependent
The chemical evolution of the Galactic Bulge seen through micro-lensing events
The chemical evolution of the Galactic Bulge seen through micro-lensing events Sofia Feltzing Lund Observatory Main collaborators: Martin Asplund (MPA),Thomas Bensby (Lund), Andy Gold (Ohio), Jennifer
Combining Gaia DR1, DR2 and Matthias Steinmetz (AIP) a preview on the full Gaia dataset. Matthias Steinmetz (AIP)
Combining Gaia DR, DR and Matthias Steinmetz (AIP) a preview on the full Gaia dataset Matthias Steinmetz (AIP) a t a d h AS t 5 - TG E V & A R ase e l e r Ga lact ic D app y lica nam tion ics s Towards
Radial Velocity Surveys. Matthias Steinmetz (AIP)
Radial Velocity Surveys Matthias Steinmetz (AIP) The Galactic case for RV surveys Information on how galaxies form is locked in n the phase-space (position,velocities) Information is locked in stars (abundances)
The Gaia-ESO Public Spectroscopic Survey a lesson for our community in use of limited telescope access. Gerry Gilmore Sofia Randich Gaia-ESO Co-PIs
The Gaia-ESO Public Spectroscopic Survey a lesson for our community in use of limited telescope access Gerry Gilmore Sofia Randich Gaia-ESO Co-PIs 1 We have Gaia! We want more Gaia will provide 60 million
Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars
Astr 5465 Feb. 5, 2018 Kinematics of Nearby Stars Properties of Nearby Stars Most in orbit with the Sun around Galactic Center Stellar Kinematics Reveal Groups of Stars with Common Space Motion (Moving
Age and abundance structure of the central sub-kpc of the Milky Way
Age and abundance structure of the central sub-kpc of the Milky Way Thomas Bensby Department of Astronomy and THeoretical Physics Sweden MBD collaboration (Microlensed Bulge Dwarf) Sofia Feltzing Thomas
Tristan Cantat-Gaudin
Open Clusters in the Milky Way with Gaia ICCUB Winter Meeting 1-2 Feb 2018, Barcelona Tristan Cantat-Gaudin Carme Jordi, Antonella Vallenari, Laia Casamiquela, and Gaia people in Barcelona and around the
M31 Color Mag Diagram Brown et al 592:L17-L20!
The physical origin of the form of the IMF is not well understood Use the stellar mass-luminosity relation and present day stellar luminosity function together with a model of how the star formation rate
Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.
![Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.](/thumbs/94/121056697.jpg "Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.")
More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column
The Star Clusters of the Magellanic Clouds
The Dance of Stars MODEST-14 The Star Clusters of the Magellanic Clouds Eva K. Grebel Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Star Clusters in the Magellanic Clouds!
Cosmologia locale: origine e storia della Via Lattea
Cosmologia locale: origine e storia della Via Lattea Mario G. Lattanzi (OATo) & Michele Bellazzini (OABo) Roma, 14 feb 2013 L Italia in Gaia, INAF Hq Collaborators Anna Curir Alessandro Spagna Francesca
Outline. c.f. Zhao et al. 2006, ChJA&A, 6, 265. Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey
KIAA-CambridgeJoint Workshop on Near-Field Cosmology and Galactic Archeology ZHAO Gang National Astronomical Observatories, Chinese Academy of Sciences Dec 1-5, 2008 Beijing Outline LAMOST stellar spectroscopic
Quantitative chemical tagging, stellar ages and the chemo-dynamical evolution of the Galactic disc
Advance Access publication 2014 January 24 doi:10.1093/mnras/stt2320 Quantitative chemical tagging, stellar ages and the chemo-dynamical evolution of the Galactic disc A. W. Mitschang, 1,2 G. De Silva,
disk (kinematics) (Ivans & Schiavon 2009) Connie Rockosi UC Santa Cruz, UCO/Lick Obs. Herschel 1785
disk (kinematics) (Ivans & Schiavon 2009) Connie Rockosi UC Santa Cruz, UCO/Lick Obs. Herschel 1785 disk (kinematics) (Ivans & Schiavon 2009) Connie Rockosi UC Santa Cruz, UCO/Lick Obs. old (no moving
Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient
Advance Access publication 2016 September 16 doi:10.1093/mnras/stw2363 Impacts of a flaring star-forming disc and stellar radial mixing on the vertical metallicity gradient Daisuke Kawata, 1 Robert J.
Migration and kinematics in growing disc galaxies with thin and thick discs
MNRAS, 1 22 (217) Preprint 12 November 217 Compiled using MNRAS LATEX style file v3. Migration and kinematics in growing disc galaxies with thin and thick discs Michael Aumer, James Binney and Ralph Schönrich
Review of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
PE#4: It contains some useful diagrams and formula which we ll use today
Sep 6, 2017 Overview of the MW PE#4: It contains some useful diagrams and formula which we ll use today HW#2 is due next Wed and is now posted. Don t wait for the last minute to start it. Includes a short
ASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney
ASTRO 310: Galactic & Extragalactic Astronomy Prof. Jeff Kenney Class 3 January 23, 2017 The Milky Way Galaxy: Vertical Distributions of Stars & the Stellar Disk disks exist in many astrophysical systems
The cosmic distance scale
The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,
Basics of Galactic chemical evolution
Basics of Galactic chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. Astronomers usually refer to chemical elements other than hydrogen
Astronomy 330 Lecture 7 24 Sep 2010
Astronomy 330 Lecture 7 24 Sep 2010 Outline Review Counts: A(m), Euclidean slope, Olbers paradox Stellar Luminosity Function: Φ(M,S) Structure of the Milky Way: disk, bulge, halo Milky Way kinematics Rotation
arxiv: v1 [astro-ph.ga] 20 Jun 2013
![arxiv: v1 [astro-ph.ga] 20 Jun 2013](/thumbs/85/91551292.jpg "arxiv: v1 [astro-ph.ga] 20 Jun 2013")
IAUS298 Setting the scene for Gaia and LAMOST Proceedings IAU Symposium No. 298, 2014 S. Feltzing, G. Zhao, N.A. Walton & P.A. Whitelock, eds. c 2014 International Astronomical Union DOI: 00.0000/X000000000000000X
Renegades in the Solar neighborhood
Title Renegades in the Solar neighborhood Ana Bonaca ITC Fellow Harvard University // Charlie Conroy // // Andrew Wetzel // Origin of the halo stars: In situ Eggen, Lynden-Bell & Sandage (1962) Accretion
THE GALACTIC BULGE AS SEEN BY GAIA
143 THE GALACTIC BULGE AS SEEN BY GAIA C. Reylé 1, A.C. Robin 1, M. Schultheis 1, S. Picaud 2 1 Observatoire de Besançon, CNRS UMR 6091, BP 1615, 25010 Besançon cedex, France 2 IAG/USP Departamento de
Matthias Steinmetz. 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1
Matthias Steinmetz 16 Oct 2012 Science from the Next Generation Imaging and Spectroscopic Surveys 1 The RAVE Survey Spectroscopic high latitude survey of the MW 9 < I < 13 GAIA spectral range and resolution
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies?
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies? Temperature Determines the λ range over which the radiation is emitted Chemical Composition metallicities
Building the cosmic distance scale: from Hipparcos to Gaia
The Fundamental Distance Scale: state of the art and the Gaia perspectives 3-6 May 2011 Building the cosmic distance scale: from Hipparcos to Gaia Catherine TURON and Xavier LURI 1 ESA / ESO-H. Heyer Fundamental
Basics of chemical evolution
Basics of chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. H and He were present very early on in the Universe, while all metals (except
arxiv: v1 [astro-ph.ga] 23 May 2018
![arxiv: v1 [astro-ph.ga] 23 May 2018](/thumbs/84/89182466.jpg "arxiv: v1 [astro-ph.ga] 23 May 2018")
Draft version May 24, 218 Preprint typeset using L A TEX style emulateapj v. 12/16/11 MEASURING RADIAL ORBIT MIGRATION IN THE GALACTIC DISK Neige Frankel 1, Hans-Walter Rix 1, Yuan-Sen Ting 2,3,4, Melissa
Asteroseismology for Galactic Archaeology: bridging two fields
Asteroseismology for Galactic Archaeology: bridging two fields Luca Casagrande Victor Silva Aguirre Dennis Stello, Aldo Serenelli Daniel Huber, Katie Schlesinger, Ralph Schönrich, Sofia Feltzing Asteroseismology
Taking the census of the Milky Way Galaxy. Gerry Gilmore Professor of Experimental Philosophy Institute of Astronomy Cambridge
Taking the census of the Milky Way Galaxy Gerry Gilmore Professor of Experimental Philosophy Institute of Astronomy Cambridge astrophysics cannot experiment merely observe and deduce: so how do we analyse
Lessons learnt from the Solar neighbourhood and the Kepler field
Astronomische Nachrichten, 9 December 2015 Lessons learnt from the Solar neighbourhood and the Kepler field Luca Casagrande 1,, Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, The
Dark Matter. ASTR 333/433 Spring Today Stars & Gas. essentials about stuff we can see. First Homework on-line Due Feb. 4
Dark Matter ASTR 333/433 Spring 2016 Today Stars & Gas essentials about stuff we can see First Homework on-line Due Feb. 4 Galaxies are made of stars - D. Silva (1990) private communication Stars Majority
Substructure in the Galaxy
Substructure in the Galaxy Amina Helmi Kapteyn Astronomical Institute Groningen, NL Is this how our Galaxy formed? Jeffrey Gardner Hierarchical paradigm Main characteristic of model: mergers Can we find
Bridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome
Bridging the near and the far: constraints on first star formation from stellar archaeology Raffaella Schneider Sapienza University of Rome Kyoto,First Stars IV 2012 Kyoto,First Stars IV 2012 "As we extend
Data-driven models of stars
Data-driven models of stars David W. Hogg Center for Cosmology and Particle Physics, New York University Center for Data Science, New York University Max-Planck-Insitut für Astronomie, Heidelberg 2015
Galactic Projects at ESO Disk and halo. Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark
Galactic Projects at ESO Disk and halo Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark B. Nordstrom Prague 15 April 2014 1980: Milky Way Structure was Known - the formation and evolution
Astronomy. Astrophysics. The age structure of stellar populations in the solar vicinity. Clues of a two-phase formation history of the Milky Way disk
DOI: 10.1051/0004-6361/201321397 c ESO 2013 Astronomy & Astrophysics The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk Misha Haywood