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2019_SB_Gaia_Sprint_pitch_slides.pdf

David W Hogg
March 25, 2019
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 2019_SB_Gaia_Sprint_pitch_slides.pdf

David W Hogg

March 25, 2019
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  1. 2019 SB Gaia Sprint
    pitch slides
    KITP — 2019 March 25

    View Slide

  2. plan to do:
    1. Infer true spatial (on sky) density structure of GD-1
    2. Improve phase-space models of known stellar streams (e.g., GD-1, Pal 5)
    3. Confirm / re-discover some other “known” streams
    want to learn:
    How to construct a very specific selection function in the GD-1 footprint
    will bring:
    Expertise in Python/Astropy; Gaia data access and use; galactic dynamics
    and practical tools; stellar streams; Bayesian inference
    want to discuss:
    Stellar populations of globular clusters vs. ultra-faint dwarf galaxies;
    dynamical inference / dark matter; star / globular clusters
    Adrian Price-Whelan (Princeton)

    View Slide

  3. Want to do:
    - use mixture models in parallax+PM+colour space for membership selection
    - search for extended structures around star clusters
    - build dynamical models of star clusters using Gaia+other data(?)
    Want to learn:
    - how to find and access other sources of astronomical data besides Gaia
    Can share:
    - how to cope with systematics in Gaia astrometry
    - galaxy modelling framework Agama: potentials, actions, dynamical models...
    Eugene Vasiliev (Institute of Astronomy, Cambridge)

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  4. Alice Quillen
    University of Rochester, Rochester NY
    What I want to do:
    ○ Look for kinematic patterns associated with recent
    star formation.
    ○ Improve models for the stellar phase space
    distribution function that are sensitive to
    relaxation and resonance
    What I want to learn:
    ○ How to create and work with nice databases of
    stars
    What I bring:
    ○ Multidisciplinary approach to dynamics modeling,
    dynamics theory and particle based numerical
    simulation. Javascript, python, rebound
    What I want to discuss:
    ○ How to create a better 3D and time dependent
    model Milky Way
    ○ Classification projects for future large data sets

    View Slide

  5. What I want to do:
    1. Classify variable objects without time series: how far can we go?
    2. Any δ Scuti or SX Phoenicis fans to validate the Gaia DR2 candidates?
    3. How to best exploit the public time series of unpublished variability classes?
    What I want to learn: complementary data sets; streams; local dark matter density
    What I bring:
    1. Gaia DR2 variable stars + Classification of high-amplitude pulsators
    2. How to access, crossmatch, and get started with the Gaia DR2 data
    3. (Semi-)supervised classification and all what is needed to make it work
    What I would like to discuss: variability phenomena; unsupervised classification; quasars; gravity
    Lorenzo Rimoldini (University of Geneva, CH)

    View Slide

  6. Zhen Yuan (Shanghai Astronomical Observatory)
    plan to do:

    Finding tails of existing GCs

    Dynamical Evolution of GCs in the MW
    What I bring::
    A new clustering method StarGO based on self-organizing-map
    (unsupervised neural network learning)
    Applications: Substructures, Star Clusters, Any Clustering Projects
    Example:
    Member Identification
    For NGC 5824
    want to learn:

    Statistical tools (e.g. non-parametric way
    to decompose multiple Gaussians)

    A variety of ways to download Gaia data

    Mock MW from Latte Simulations
    want to discuss:

    Archeological Fossils: Dwarfs & GCs

    What can we learn from abundances?

    View Slide

  7. Giuliano Iorio
    ● Look for halo structures in phase-space using RRLs
    ● RRLs around GCs, RRLs in known streams
    RRLs in Pal-5 stream
    (Institute of Astronomy, Cambridge) RRLs around M5
    4 Rt
    Want to do:
    Want to learn:
    Ask me about / What I bring:
    Want to discuss:
    ● Methods to estimate the phase-space density
    ● Clustering methods / Associate stars to known GC/Sats/streams
    ● MW stellar halo
    ● RRLs in Gaia
    (I bring catalogs of all RRLs classified in Gaia DR2 with additional information)
    ● (non cosmological) N-body simulations
    (I bring catalogs of an LMC-like destroyed in the MW, credit D. Erkal)
    ● Gaia selection function / completeness
    ● How to find shells in the MW halo
    ● Can we improve distance estimate for
    RRLs?

    View Slide

  8. Timothy Brandt
    UCSB
    ● Want to do: calibrate uncertainties for the medium/faint end
    of Gaia astrometry: Tycho, WFPC2? ACS?
    ● Want to learn: how else can we understand Gaia
    uncertainties and systematics?
    ● What I bring: Cross-calibration of Gaia DR2 to Hipparcos
    (HGCA), fitting orbits with the HGCA, RV, imaging
    ● Want to discuss: how can we get the best handle on
    spatially correlated systematics, external uncertainties?
    P~100-400 years

    View Slide

  9. Paolo Tanga - Observatoire de la Côte d’Azur
    What I want to do:
    a. Exploit ~200 million asteroid positions reduced with pre-Gaia
    catalogs
    b. Optimize my brand new approach to correct zonal errors for
    those catalogs
    c. Study the results and start writing an article!
    What I want to learn: write better ADQL queries, launch python
    parallel threads, and all that you can share about systematics in ancient
    catalogs.
    What I bring: Solar System data expertise. Zonal error corrections for
    ~3000 asteroids, ~20 catalogues. Independent cross-match approach.
    What I would like to discuss: Spatially correlated errors.
    Clustering algorithms for multi-dimensional data. Good beers.

    View Slide

  10. Larry Widrow Queen’s University
    Want to do: Apply methods such as Gaussian process regression to Gaia
    data to build models for the phase space DF.
    Want to learn: Better methods for GPR including application of sparse GP
    to problems in 3-6 dimensions and with observational errors.
    What I bring: Preliminary success modelling 3D velocity field via GPR.
    Familiarity with GPy. Have also worked on building equilibrium disk models
    and embedding them in cosmological halos.
    What I want to discuss: Theoretical underpinning of phase space structure
    in stellar DF and other methods to analyse both data and simulations.

    View Slide

  11. View Slide

  12. Alexa Villaume (University of California Santa Cruz)
    What I want to do:
    What you can ask me about:
    SQL databases
    Stellar population
    synthesis models
    ● Cross-match E-IRTF
    library with Gaia
    ● Normalize spectra
    to Gaia photometry
    ● Infer luminosity for
    each E-IRTF star in
    manner similar to
    Hawkins et al. 2017
    What I want to learn:
    How to choose informative
    priors when using the
    parallax measurements
    Use Gaia to turn the E-IRTF
    stellar spectra library into new
    SPS models
    E-IRTF

    View Slide

  13. View Slide

  14. Kathryn V Johnston (Columbia University/CCA)
    DO
    dynamics-driven data analysis of PS-spiral
    LEARN
    prior work and best data for this
    python tips and toolkits
    BRING
    direct experience in prehistoric times
    DISCUSS
    anything and everything
    Images from Aaron Tran (Columbia)

    View Slide

  15. Andy Casey (Monash)
    What I want to do >> use eclipsing binaries to translate excess astrometric noise
    to tangential motion, and estimate inclination angles for non-eclipsing binaries
    What I want to learn >> is the distribution of inclination angles isotropic?
    What I bring >> Zen. My time (for your Sprint problems). Experience in data
    analysis, some knowledge about stars
    What I’d like to discuss >> astrometry >> (other things….) >> thoughts about next
    Gaia data release

    View Slide

  16. What I want to do: apply our method for modeling a 3D dust map to real data, profile the python code to
    minimize compute time, sprint with Juna
    What I want to learn: data viz with yt (3d rendering and sim reconstruction), limits of GP method with
    real data, more intuition for how approximate GP methods work
    What I’d like to chat about: interpreting structures in a 3D dust map, including velocity in the dust map,
    non-parametric representations of galactic potentials, inference of the MW halo shape/accretion history
    from stellar streams, structures in the CMD, modeling and interpreting the phase space distribution
    function of stars
    What I bring: GP 101 description, data-driven models, curiosity and optimism
    Lauren Anderson (Flatiron Institute)

    View Slide

  17. Sarah Pearson
    Credit: Eilers & Hogg
    Gaia/APOGEE
    v_r vs v_phi correlation
    What I want to do:
    Re-compute Eilers’ plot for galactic bars formed through two
    different scenarios:
    1) In-situ (E. D’Onghia’s simulations)
    2) Sagittarius impact (C. Laporte simulations)
    What I hope to learn:
    How long is the Milky Way’s Galactic bar?
    How did it form? (optimistic question)
    Which orbits support the bar? (using APOGEE/Gaia 6D info)
    What can we learn about the bar from APOGEE metallicities?
    You can ask me about:
    - Galactic dynamics/the Galactic bar
    - Orbit integration
    - Using Price-Whelan’s Gala package
    I’d like to chat about:
    - APOGEE selection function
    - The Galactic bar in general
    Flatiron Institute,
    Center for Computational Astrophysics

    View Slide

  18. View Slide

  19. Luis Quiroga-Nuñez (Leiden Observatory/JIVE)
    ❖ Cross-matches at different λ
    ❖ Variability for evolved stars.
    ❖ Galactic structures
    characterization (arms & bar)
    What I want to do What I want to learn
    What I bring What I like to discuss
    ❖ Radio astrometry at 1μas
    resolution.
    ❖ Experience generating
    simulated astrometric data.
    ❖ Radio data that complements Gaia results in the GP
    ❖ How variability can be obtained from Gaia ?
    ❖ How extinction maps are used
    over Gaia data?
    ❖ Generate MLE to test the Gaia
    limits
    ❖ Members of stellar association
    ❖ Synergies between astro-
    metric campaigns at different λ
    ❖ Stellar population across the GP
    ❖ Future missions in IR?...plausible?

    View Slide

  20. View Slide

  21. Jason Hunt (Dunlap Institute - Toronto)
    What I want to do: Explore the non-axisymmetric &
    disequilibria structure in the Gaia data
    What I want to learn: How to differentiate between
    signatures of bars/spirals/external perturbers
    What I bring: Dynamical Galaxy modelling methods /
    knowledge; N-body, Test particle, Action-Angle (and
    models themselves), with various bars+spirals
    What I’d like to discuss: Reconciling long/short bar
    evidence, I don’t mind who’s right, I’d just like to know!

    View Slide

  22. to do
    ★ understand origin (and lack thereof!) of alpha/Fe bimodality in
    Latte simulations, connection with stellar kinematics (and ages),
    test this formation scenario with Gaia++
    ★ convince you to use our (really Robyn’s) Ananake synthetic Gaia
    DR2 catalogs from our Latte simulations
    to learn
    ★ how better to compare kinematics, abundances, and ages from
    Gaia + APOGEE + ??? against simulations
    bringing/sharing
    ★ Ananake synthetic Gaia DR2 catalogs and full snapshots of Latte
    simulations (i.e. I am happy to point you in Robyn’s direction)
    ★ sarcasm
    to discuss
    ★ joint analysis of abundances + kinematics + ages
    Andrew Wetzel (UC Davis)

    View Slide

  23. Christophe Pichon IAP/Paris
    Interests
    ● Galactic/DM dynamics
    ● Secular evolution/kinetic theory
    ● Impact of LSS on galaxies
    Would like to learn more about
    ● GAIA’s constrain on DHs
    ● Who wins, when, where in driving galaxies’ fate?
    What I bring
    ● Understanding(?) of LSS + secular. dynamics
    Do discuss
    ● What can be done with GAIA streams/ridges?
    Happy to work with anybody interested...
    What I want to do
    ● Modify kinetic theory for streams
    ● Map ridges in Gaia coordinates
    ● Convince people quasi-linear theory rocks

    View Slide

  24. Patrick LaChance
    What I want to do:
    ● Disentangle the qualities of the kinematic background in the solar
    neighborhood from the nearby clusters
    University of Wisconsin-Madison;
    4th year undergraduate student working with Elena D’Onghia
    What I bring:
    ● I bring a clustering algorithm (SNN) that can group stars together
    based on a variety of attributes (position, velocity, chemistry, etc.)
    that was developed in our group.
    ● I bring some data structures and analysis experience from my CS
    background.
    What I want to learn:
    ● I want to learn about the kinematic features of our solar
    neighborhood, and spiral galaxies in general.
    ● I would like to learn the ages and metallicities of the clusters in the
    solar neighborhood to differentiate them from the background

    View Slide

  25. Alexandra Borukhovetskaya University of Wisconsin - Madison
    undergraduate student working with Elena D’Onghia
    What I want to do:
    I am interested in understanding the Arcturus moving
    group - its members and origin. I am hoping to be able to
    rebuild the group so that I may argue for either in situ or
    extragalactic formation.
    What I want to learn:
    Ages and metallicities of known Arcturus members as
    well as other clustering techniques.
    What I bring:
    Clustering algorithm (SNN) developed in our group, previously used for kinematic and chemical
    clustering for globular clusters and now modified for clustering in Gaia data - proper motion, ra,
    dec, and parallaxes.

    View Slide

  26. Elena D’Onghia (University of Wisconsin-Madison/Flatiron Institute)
    I will work on understanding the formation of
    moving Pleaides, Coma Berenice (with Patrick
    LaChance) and on Arcturus moving group
    (with Alexandra Borukhovetskaya)
    I want to learn about ages and metallicities of
    moving groups and the open clusters
    I bring dynamical models with N-body
    simulations and experience on galactic
    dynamics

    View Slide

  27. Juna Kollmeier (Carnegie Observatories)
    What I want to do: I would like to produce useful “Gaia Gold Catalogs” for
    quasars, single stars and white dwarfs. Or something cooler with Anderson.
    Maybe some BHBs?
    What I want to learn: The pitfalls of producing such catalogs; particularly how to
    best cut the Gaia data
    What I bring: broad interests and expertise
    What I want to discuss: I will want to discuss anything

    View Slide

  28. Hamish Silverwood
    ICC, University of Barcelona
    Do:
    -Gaussian Process Regression on binned velocity and tracer
    density data →
    -Apply to Jeans Equations to derive force maps and/or
    disequilibria maps (Δ-Jeans method from Sprint 2018), working
    with Lauren Anderson & Larry Widrow.
    Learn:
    Anything GP related. Selection functions.
    Bring:
    Broad Dark Matter knowledge (indirect, direct detection etc).
    Expertise in Jeans Modelling. Oscar - brute force tool for
    binning Gaia data incorporating full uncertainties.
    Discuss:
    Dark matter. GPs. Future measurements of stellar accelerations
    with high precision spectrographs & nano-arcsecond
    astrometry (1812.07581).
    V
    R
    V
    R
    V
    R
    V
    Z
    V
    Z
    V
    Z

    View Slide

  29. Harshil Kamdar
    Harvard
    Plan to do: can angles between very wide co-moving
    pairs in data (>2 pc) tell us about whether stars are
    born together?
    Want to learn about: hierarchical star formation.
    Can help with: the lifecycle of star clusters born in the
    disk, clustering algorithms.
    Would like to discuss: the ISM! And what we can learn
    about clustered star formation from Gaia.
    A simulation of all stars born in star clusters in the Milky Way disk
    in the last 5 Gyr that includes a realistic potential (bar + spiral +
    GMCs) and a subgrid model for cluster birth and evolution

    View Slide

  30. Cecilia Mateu (UdelaR, Uruguay)
    What I bring:

    RR Lyrae stuff + Gaia RR Lyrae completeness maps, PyMGC3,
    Galstreams library - compilation of MW stream footprints
    What I want to do:

    Calibrate MG
    for RR Lyrae stars as a
    function of period-shift (location on
    Period-Amplitude diagram)
    OoII RRLs
    are brighter
    than OoI:
    ~0.25mag
    = 10% in
    Distance
    What I want to learn:

    Statistical tools to deal with error
    systematics & correlations
    What I want to discuss:

    New analytical models for the disc’s density profile to
    replace double exp+flare+warp

    View Slide

  31. Anthony Brown (Leiden Observatory)
    What I want to do
    ● Build a “Gaia for beginners” catalogue, intended for use
    in, e.g., astronomy education (thanks Juna for suggesting
    this!)
    ● Gaia DR2 sub-sample cleaned from the nasty bits,
    documentation, warnings on limitations
    What I want to learn
    ● Can the “phase spiral” really be explained as due to
    moving groups (arXiv:1903.08325)?
    What I bring
    ● Gaia expertise: all aspects of the data, quality filtering, archive access, ...
    What I want to discuss
    ● Your thoughts on future Gaia data releases
    ● How to preserve sufficient likelihood information in long term Gaia archive
    ● Gaia selection function: your inputs on a good proposal to fund this effort
    ● Uncertainties/systematics: how will these affect cross-calibration of other/future surveys against Gaia?

    View Slide

  32. Christina Eilers (Max Planck Institute for Astronomy)
    you can ask me about: distances to APOGEE
    red giant stars, Gaussian processes, the
    Milky Way’s circular velocity.
    sprint idea: find, map & model non-axisymmetric
    features of the Milky Way.
    I hope to learn about: Galactic bar, spiral arms,
    how to install galpy & calculate actions.

    View Slide

  33. Hans-Walter Rix Max Planck Institute for Astronomy, Heidelberg
    you should ask me about: SDSS-V
    the perfect spectroscopic match to Gaia...
    seeking collaboration on Gaia (DR2) as a time-domain survey:
    DR2 provides rms variations in flux, astrometric wobble, and v
    los
    (non-)variable WD candidates/contaminants
    rms fractional flux variation in G
    and their light-centroid wobble

    View Slide

  34. to do
    - Identify chemo-dynamical substructure in the stellar halo using clustering algorithms
    - Estimate the shape of dark matter halo using hyper-velocity stars
    - Use orbits of runaway stars to identify their natal star clusters
    to learn
    - Clustering algorithms
    - Density distribution of young stars (<10Myr) in simulations.
    - Chemistry/age of known young massive clusters (e.g., Westerlund 1).
    - Basics on photometric metallicity
    - Why sometimes, two mathematically equivalent ADQL queries take very different times.
    - (E.g., “Select ra from AAA where (ra < 10)” and “Select ra from AAA where (ra - 0.5 < 9.5)”)
    - Any tips for reducing the ADQL query times.
    - Does anyone use astroquery? Is there any ways to run ADQL queries other than Gaia archive?
    to bring
    - Knowledge on hyper-velocity stars / runaway stars
    - Practical use of AGAMA code
    to discuss
    - Gaia Sausage / Disc substructure (e.g., Hercules stream)
    - Any bold ideas using Gaia data
    Kohei Hattori (University of Michigan)

    View Slide

  35. Siddharth Mishra-Sharma (NYU)
    What I want to do:
    ● Understand collective effect of Galactic dark matter substructure on
    stellar velocity/acceleration fields (dynamical + lensing-induced)
    ● Look for this pattern in Gaia DR2
    What I want to learn:
    ● Working with Gaia data!
    ● Estimators and techniques to look for structure in 3D vector fields,
    accounting for uncertainties (e.g., extensions of 2-point correlations)
    What I bring:
    ● Background in astrophysical signatures + particle physics properties
    of dark matter
    ● Experience in writing fast Python code
    What I’d like to discuss:
    ● Particle physics implications of DM substructure (population)
    measurements
    Substructure lens-induced...
    … velocity field
    … acceleration field

    View Slide

  36. Jackie Faherty, American Museum of Natural History
    Do: Figure out what the end of the main sequence in Gaia looks
    like and find new objects (young especially!)
    Learn: About hypervelocity stars in vtan space
    Bring: The end of the main sequence and science visualization
    Discuss: Visualizing our data!

    View Slide

  37. Sihao Cheng Johns Hopkins University What I want to do >> white dwarf H-R diagram
    ● Explain the Q branch
    ● WD-WD merger rate
    What I want to learn >>
    optimal quality cuts; selection function; dust
    within 250 pc
    What I bring >>
    ● white dwarf knowledge:
    cooling, merger, spectra, ...
    ● experience in DR2 light-curves (effect of
    extended sources)
    ● scanning directions of Gaia
    What I’d like to discuss >>
    ● Gaia selection function
    ● Gaia-Panstarrs cross-matching
    ● bifurcation of Sagittarius Stream
    ● spiral arms in stellar mass / gas
    ...

    View Slide

  38. May Gade Pedersen (KU Leuven, Belgium)
    Plan to do:
    ★ Determine luminosities of pulsating stars
    ★ Search for stellar clusters w. EMSTOs and fit
    isochrone clouds
    Johnston+2019
    Victoria Antoci
    Want to learn
    ★ Application of Gaia astrometry and photometry
    to stellar clusters
    ★ Cluster membership verification
    Ask me about
    ★ Asteroseismology/seismic modelling
    of pulsating (massive) stars
    ★ Internal mixing and impact on stellar
    evolution and surface abundances
    Isochrone
    Cloud

    View Slide

  39. Heidi Newberg (Rensselaer Polytechnic Institute)
    plan to do:
    Explore the shell structure in Virgo and related halo substructure
    want to learn:
    Is the shell structure in Virgo the same as the
    Gaia-Enceladus/Gaia-sausage merger and how old is
    that structure?
    bringing:
    Expertise in structure of the Milky Way halo and disk.
    want to discuss:
    How do we fit N-body simulations to Milky Way shell
    structure?

    View Slide

  40. David W. Hogg
    (NYU) (MPIA) (Flatiron)
    What I want to do >> Map non-axisymmetries in the disk with red-giant stars.
    >> Dynamically model the GD-1 spur.
    What I want to learn >> How to classify stellar variables using Gaia noise
    information.
    What I bring >> Expertise in computational data analysis, linear algebra, Bayesian
    inference, model building, MCMC. >> Knowledge about SDSS, BOSS, APOGEE,
    HARPS, Kepler, and Gaia.
    What I’d like to discuss >> Hierarchical models. >> The Gaia likelihood function.
    >> Mapping the dark matter. >> Chemodynamics. >> Binary stars.

    View Slide

  41. Jason Sanders
    (Institute of Astronomy, Cambridge)
    What I want to do - 3d bulge (chemo-)
    dynamics with Gaia RVS M giants.
    Photometric metallicities → distances.
    What I want to learn - kinematic differences
    between metal-rich & metal-poor
    populations across bulge.
    What I bring - knowledge on ages/distances
    from Gaia+spectro, action-angles, streams,
    bar/bulge.
    What I want to discuss - 3d extinction
    mapping, photometric metallicity/ages, RVS
    selection fn, bar’s impact on SN kinematics.
    Li et al. 2016
    Metallicity
    WISE colour

    View Slide

  42. Borja Anguiano - University of Virginia
    What I want to do: Characterize the kinematic signature of the
    Galactic stellar warp using APOGEE and Gaia data-sets.
    What I want to learn: I noticed that recent works are pointing out
    new ways of using Gaia flags. I would be interested to have a
    discussion with Gaia experts about it.
    What I bring: Knowledge and experience working with APOGEE,
    GALAH and RAVE data, this can be useful for this meeting.
    What I want to discuss: Stellar multiplicity using different RV visits
    in RAVE.

    View Slide

  43. Sukanya Chakrabarti
    (RIT)
    Plan to do:
    ● How do MW satellites
    affect the gas &
    stellar disk ?
    Including new
    satellites discovered
    by Gaia
    Expertise:
    ● SPH & test particle
    simulations, galactic
    dynamics, variable stars
    Want to discuss: happy
    to discuss anything!
    Levine, Blitz & Heiles 06
    Chakrabarti & Blitz 09

    View Slide

  44. Josh Simon (Carnegie Observatories)
    What I want to do: Photometrically select
    metal-poor stars by combining broadband colors
    from Gaia and other all-sky surveys
    What I want to learn about: Efficiently
    cross-matching large catalogs, spectroscopic
    surveys covering bright (V<14) stars
    What I bring: Knowledge of dwarf galaxies and
    stellar streams (in Gaia and elsewhere).
    Beginner’s ability to model orbits with galpy.
    Other things I want to talk about and/or work
    on: Dwarf galaxies, stellar streams
    1962 version:
    Wallerstein (1962)
    2019 version?

    View Slide

  45. Ellianna Schwab Abrahams (UC Berkeley, CTDI)
    Plan To:
    ★ Search for anomalous RV measurements using ensemble learning
    ★ Predict RV measurements for stars without measurements
    ★ Also very interested in the DR2 Time-Series Catalog and variable star classification
    Hope to Learn:
    ★ Systematics in the Gaia RV Catalog ★ Edge detection and clustering methods
    Bringing/Ask me About:
    ★ ADQL Queries ★ Database Crossmatching ★ Representation ML ★ Time Series
    Featurization
    Want to Discuss:
    ★ Gaia in the time domain, in DR2 and future DRs ★ Detecting variability using static data

    View Slide

  46. What I want to do this week
    ● Dynamics of M31 HII regions using biased Gaia astrometry
    ● Star cluster properties accounting for small field correlations
    Morgan Fouesneau Max-Planck Institute
    for Astronomy
    What I would like to learn this week
    ● Estimating Gaia’s small field of view correlations
    ● Feedback on Gaia mock and GDR2.
    ● Crossmatching catalogs including SED information
    I Can help with
    ● Gaia data, crossmatch & data query helpdesk
    ● Gaia Mock / Gaia classification & APs
    ● GDR3 BP/RP spectra
    [email protected] @mfouesneau
    mfouesneau.github.io

    View Slide

  47. LV in gas
    [sim]
    Interested in:
    ● Large scale [G/g]alactic structure. Impact of
    spirals/bars/companions on ISM/SF processes.
    Aim to do:
    ● Look at galactic scale velocity fields, how they
    compare to sims. with different
    asymmetries/underpinning physics.
    Specific knowledge of:
    ● Hydro+N-body simulations of galaxies, ISM
    physics.
    Would be keen to know more about:
    ● Any aspect of the obs. data really
    (not touched it before!), phase spirals,
    models people are desperate in need of.
    ...What I don’t want to talk about:
    ● Brexit. Please... just let it end.
    Do ISM
    features align
    with any stellar
    pops?
    ISM in
    a spiral Makes some
    stars...
    Alex Pettitt
    ?

    View Slide

  48. Kareem El-Badry
    (UC Berkeley)
    Ideas:
    - What’s going on with wide binary
    luminosity ratios?
    - Hardening of close binaries in
    hierarchical triples
    - Test MOND with wide binaries
    Bring: binaries, white dwarfs,
    cosmological simulations, enthusiasm,
    short attention span
    Learn: how to use Gaia as a
    time-domain survey

    View Slide

  49. Plan to do: Look at known streams in Gaia - measure proper motions, map
    density, look for extensions in RR Lyrae
    Want to learn: More about Gaia systematics, RR Lyrae, reliable density mapping
    of streams
    Bringing: Experience working with DES data, cross-matched dataset, tools for
    working with streams, experience with stream detection, photometric filtering,
    proper motion measurement
    Want to discuss: Dark matter constraints with streams, differences in globular
    cluster/dwarf stream populations
    Nora Shipp (UChicago)

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  50. Emily Cunningham (UCSC)
    What I want to do: Look for spatial variation of kinematic
    properties in the halo with RR Lyrae
    What I want to learn: Modeling Gaia systematics;
    computationally efficient Bayesian inference methods for use
    with large datasets
    What I bring: Expertise in proper motions with HST;
    spectroscopic analysis; Bayesian inference (incl. hierarchical
    and mixture modeling)
    What I’d like to discuss: Methods for combining multiple
    datasets; chemodynamics; data-model comparison tools

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  51. David Mykytyn (New York University)
    What I want to do: *joint with Alex Malz (NYU; he is remote due
    to impending thesis defense but will Skype in when possible)
    ➔ Improve HR Diagrams for open clusters by identifying
    and correcting double stars, with the goal of creating a
    fully probabilistic model for HRD
    What I want to learn:
    ➔ A lot more about good models for HRD and also some
    stellar models that could be combined?
    ➔ Stuff about open clusters? -> What generates the HRD
    for clusters
    What I bring:
    ➔ A lot of knowledge about Gaussian Processes, especially
    for time-series analysis. Some crazy ideas about using GPs
    to speed up monte carlo, or even to get better
    information out of simulations (keywords: Multifidelity
    Monte Carlo, metamodels/emulators/simulators/etc.)
    (Want to get at what 1801.08547
    marginalized over)
    [Widmark, et. al 2018]
    (First stab
    at PGM)

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  52. Ana Bonaca
    Center for Astrophysics
    Harvard & Smithsonian
    Do: constrain the orbit of a
    possible perturber of the GD-1
    stream based on the kinematics of
    the perturbed region
    Bring: Python3 API for C, expertise in the detection
    and modeling of structures in the stellar halo
    Discuss: dating accretion events based on their
    structure in the space of conserved orbital properties

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  53. Jatan Buch
    (Brown U.)
    > Discuss:
    - (Passively): DF modeling in action-angle space; inferring MW dust maps with DR2 + MA, age-abundance
    relations, realistic pipeline for time-series data; zoom-in simulations;
    - (Passionately): outline of a SOTA analysis, hierarchical inference, banish closed-form likelihoods?
    > Intend to:
    - (Warmup) DR2-APOGEE/SDSS x-matched data-sets to study chemo-dynamic
    properties of velocity ‘substructure’ (h/t: Myeong+’18, TCR’18).
    - Develop criteria for qualifying stellar population in a given volume patch as
    phase-mixed (h/t: BMH’09).
    > Experience:
    - with DR2 data and selection function based on gaia_tools (Bovy’16);
    - particle physics: indirect and direct DM detection; cooling rates for dissipative DM.
    - (Audaciously): Explore disequilibria with a semi-analytic forward modeling
    approach using simulations; toy n-body code that includes DM self-interactions.

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  54. Semyeong Oh
    Institute of Astronomy, Cambridge
    I am doing:
    kinematic modelling of a cluster
    - evidence beyond small (isotropic) dispersion?
    I want to learn about:
    ○ stellar binaries and clusters
    ○ hierarchical inference and clustering
    ○ future data
    I bring experience with:
    Gaia data access and exploration and
    making interactive visualizations

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  55. Joel C. Zinn
    Ohio State University
    What I want to do:
    Explore TESS-K2-Gaia synergy
    What I want to learn more about:
    Binaries in Gaia
    Gaia parallax systematics
    I bring experience with:
    Parallaxes beyond ~2-3kpc with red
    giants, asteroseismology, stellar models,
    APOGEE, Kepler, K2

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  56. Chervin F.P Laporte (University of Victoria / CITA)
    DO 1) Finish paper from last year’s Sprint. 2) Test+Map PS-spiral beyond
    10 kpc without WEAVE or 4MOST with RC and a model to generate RVs
    complementing 5D data.
    LEARN Bayesian inference methods, data driven techniques, adaptive
    smoothing/filterning methods, AGAMA.
    BRING My pre-Gaia DR2 N-body models of Sgr impacting disc (free
    data). Useful for anyone doing disc-kinematics/bar kinematics? Familiar with
    studying kinematic substructure in SN, i.e. happy to help people (e.g. Elena’s
    team on Arcturus) if I can/it’s cool with y’all.
    DISCUSS
    “Existence of moving groups is not a physical explanation for the origin of
    the PS-spiral.” Happy to discuss/philosophise with Anthony Brown (maybe do
    a project?). Analogy: If I put re-assemble KFC chicken pieces (drum, breast,
    wings) into something looking like a chicken it doesn’t mean that KFC
    explains why chickens exist.
    Pre-Gaia simulations
    Gaia DR2
    ??????????
    ??????????

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  57. Andreea Font (Liverpool John Moores U., UK)
    What I want to do:
    Look for substructure signature in the Solar neighborhood using
    various tracer stars.
    Compare with results of cosmological simulations. Think about
    implications for dark matter detection.
    What I want to learn:
    Combining different catalogues (Gaia, RAVE, APOGEE).
    Modeling Gaia systematics.
    Knowledge of:
    hydro-dynamical simulations, chemo-dynamical models of the
    Milky Way and dwarf galaxies.

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  58. Robyn Sanderson
    UPenn/Flatiron
    ananke.hub.yt
    Doing: evaluating basis-expansion models of the Latte halos for orbit studies, prep
    for public release of models
    Learning: how well we need to represent the MW to study its orbit structure; what
    else people want from mock observations
    Sharing: the ananke mock catalogs, dynamics expertise generally

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  59. Philip Chang (University of Wisconsin - Milwaukee, Flatiron Institute)
    What I want to do: See what everyone is up to; extract physics from
    test particle simulations.
    What I want to learn: am currently GAIA curious - ready to take the
    next step.
    What I bring: Expertise in theoretical and computational astrophysics;
    some experience in test particle dynamics; a bit more in
    SPH/Moving-mesh/Eulerian hydro.
    What I want to discuss: Phase space mixing of stars, perturbation
    theory, etc.

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