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2018 NYC Gaia Sprint wrap-up slides

2018 NYC Gaia Sprint wrap-up slides

90-ish authors; presented on 2018-06-08 at the Gaia Sprint

David W Hogg

June 08, 2018

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  1. Sergey Koposov Did: Talked a lot, learned a lot, looked

    at streams/binaries/substructures/RRlyrae, Got distracted by ‘weird RRlyrae’. Didn’t quite do what/as much as I was planning to do. Great meeting -- thank you!
  2. TLDR: “this looks cool” ⇒ “where am I?!” ⇒ “this

    looks strange” Learned - should have known: Can’t look for GW in DR2 (need residuals from epoch-astrometry, not motion fits) - not surprising: Gaia doesn’t share scanning solution (but it’s not too hard to extract; thanks @SihaoCheng!) - surprise: spin-2 spherical-harmonics are our friends (and emcee can calculate them quite well!) Accomplished - Many additions to simulated GW-detection pipeline - Realish scanning law for “observations” (almost done) - Incorporate model of Basic-Angle modulations (``) - Use real DR2 magnitudes and uncertainties - `` DR2 proper-motions, and positions Luke Zoltan Kelley [email protected] Harvard CfA ⇒ Northwestern CIERA Gaia Astrometric Gravitational Wave Detection Thanks So Much!! CCA, SOC, GAIA & Sprint Attendees
  3. 1. Distribution of q (mass-ratio) of unresolved binaries (m1<1 Msun)

    as a function of m1 and [Fe/H] 2. (with Xiangxiang Xue) Identify new OB associations Chao Liu (National Astronomical Observatories, CAS) p(q|m1) p(q|[Fe/H]) Single Single New spiral arm? q q
  4. Gabriel Torrealba ASIAA - Used RR Lyrae as tracers of

    satellite galaxies - Learned a lot from an amazing group of people!
  5. Daniel Michalik ( & ) Met fantastic people, discussed amazing

    projects Computation of spectroscopic parallaxes (Eilers et al): understood individual outliers due to astrometric quality, photometric quality, variability Explored the identification of multiplicity from Gaia-DR2 and DR1-TGAS ◦ Goals: TGAS 2.0, long-period (>25 yr) binaries, dynamical masses from orbital fits ◦ People involved: Brandt, Faherty, Hernandez, Michalik, Mora, etc Intended to confirm/reject kinematic cluster members in chemical space ◦ Too little overlap with APOGEE, GALAH ◦ Learned about Hypatia (Hinkel et al.) - to be continued! Visiting the Netherlands? Say hi at ESTEC - standing invitation for all sprint participants! Email address is in the running notes of the sprint
  6. Keith Hawkins (UT Austin) Can we measure Eu (r-process) in

    APOGEE spectra? A (photometric) metallicity Map of the MW w/ N. Hinkel w/ Y. S. Ting YS Ting + shows can measure [Fe/H] from WISE+Gaia+2MASS+Panstarrs photemotry to ~0.20 dex (NN, Ting) and (PM, Hawkins) HYPOGEE: APOGEE+Hypatia (111 stars) [Eu/Fe] in GALAH+APOGEE: -0.14 (0.15 dex) [Eu/Fe] in Gaia-ESO+APOGEE: 0.02 (0.18 dex) Line identification underway w/ N Hinkel Maybe wrong?
  7. Sanjib Sharma (University of Sydney) • I computed the anisotropy

    profile of the stellar halo using BHB and K Giants from SEGUE (Xue et al.). • I used a non-parametric Bayesian scheme, along with a model for outliers. I take into account uncertainties in radial velocity, proper motion and distance. The model had about 120 free parameters. • While most N-body simulations suggest outer stellar halo to be radial ( >0) we find the MW halo to be non radial ( <0). Bullock & Johnston 2005 (Kafle et al. 2012)
  8. Natalie Price-Jones (UToronto) What worked: - Developing normed distance metric

    for patchy/uncertain data - Chemical clustering on APOGEE spectra/GALAH abundances in Gaia overlap - Abundance trends in R, z with Gaia positions What didn’t: - Verifying clusters with chemical space alone - Distinguishing open clusters in chemical space with DBSCAN Next steps/new ideas: - Implement FOPTICS in Python (thanks: Joris de Ridder) - Look for chemistry of nearby young associations (thanks: Jonathan Gagné) - Action-angle space clustering (thanks: 4th floor library)
  9. Francisca Concha-Ramírez Leiden Observatory ❄ ✅ Learned to better represent

    my (simulated) open clusters to be compared with observational data ✅ Used Boquan Chen’s clustering algorithm, adapted it for my simulations ✅ Learned about arcane topics such as parallaxes and proper motions ✅ Talked to a lot of people, got new ideas for my project ✅ Preached about AMUSE ✅ Tweeted a lot #GaiaSprint Did not feel judged about my usual excessive emoji use ✅ Wrote a script to run an open cluster moving through the galaxy and interacting with giant molecular clouds… ❌ ...to see if it would yield something similar to Semyeong’s object. It didn’t http://francisca.cr @franconchar franciscaconcha Let’s a k u p lu r !✨
  10. Tried to do: Classify QSOs/BHBs/WDs using Gaia-GALEX-WISE. SDSS spectroscopic training

    set of 4,000 BHBs ---> Gaia catalogue of 400,000 Needs to be cleaned (a lot), but can be used to map halo in proper motions! Douglas Boubert (IoA, Cambridge -> Magdalen College, Oxford) What is next: Map these stars in velocity, add in GALEX and WISE, go to lower latitudes, extend to classifying quasars as well. What I learnt: 1. Only write code if you are sure that it isn’t in Bovy’s back-catalogue. 2. You are only as good as your internet connection to the Gaia archive.
  11. Hans-Walter Rix (MPIA) Plan: finish 1 paper, start 2 papers.

    Result: finished 0, sniffed out or co-started >5. I am happy Learned: • that global kinematic disk maps can be made! (from Inno, Eilers, Hogg, ..) • how the disk heats (from Ting) • how to find massive stars (from Cantiello,Mora) • infinitely more from many others Took away: Gaia + Sprinters sowed 1000 scientific flowers. Let’s await the bloom The gently warping young disk (courtesy Laura Inno)
  12. Federica Spoto • Combine Gaia + ground-based obs ~ 190

    millions of obs with their catalogs ~ 2 millions of Gaia obs How does it work? For each observation: 1. Cross-match 2. Correction
  13. Matthew Buckley: Mass through Phase Space Goal: calculate the mass

    of gravitational objects by calculating their phase space volume in the Gaia data. Test this using M4 Problem: too far for radial position/velocity measurements to be accurate. But! It’s a spherical system, so just rotate the projected positions/velocities (this cannot increase the phase space volume). I calculate a mass within 10-20% of the accepted answer (with caveats) Accepted mass My best-fit mass Range of masses using range of concentration parameters of globular clusters Thanks to Katelin, Lina, Hamish, Oren, Colin, Adrian, and Hogg for help this week
  14. Jeans Analysis of the Local MW Katelin Schutz, Hamish Silverwood,

    Oren Slone Measurable with DR2 Unknown Radial + Vertical Forces And Disequilibria X R X Z Zero Disequilibria: X R = -K R X Z = -K Z Comparing Populations i and j, extracting time term T X Ri - X Rj = T Ri - T Rj X Zi - X Zj = T Zi - T Zj
  15. Jeans Analysis of the Local MW Katelin Schutz, Hamish Silverwood,

    Oren Slone Outlook: • Performing same analysis on tracers with different dynamical mixing timescales • Find regions that are relatively in equilibrium • Model time-dependent terms • Measure properties of the DM halo (triaxiality, radial profile, mass, local density) • Measure correlation of DM/acceleration with baryonic profile/acceleration • Compare with simulations of various DM models 10-13 km s-2
  16. 2. DR2 pm compared to TGAS pm -> pm_accel: Trying

    to find accelerating objects Wrapping up Gaia Sprint! LMC 4. PSA: Don’t forget radial velocity is in heliocentric frame SMC 1. Comoving Objects Collector: Group by patches of sky, only take objects with low variance on proper motion. Insights: 1. LMC is rotating and spinning 2. SMC also; but has satellites 3. I think we can use this to find streams 3. Lensing: Ken will talk about our ongoing analysis!
  17. Eddie Schlafly (LBL) • Fit photometry of ~50k sources seen

    in Gaia+APOGEE+PS1+2MASS+WISE • Learned absolute magnitudes as a function of APOGEE spectroscopic parameters, reproduced observations to ~10 mmag • New extinction curve measurements with Gaia!
  18. Kareem El-Badry (UC Berkeley) • Separation distributions of wide binaries

    bear imprints of disruption and common envelope! • Binary fraction does not depend on [Fe/H] for wide binaries! • Learned about binary evolution, Gaia sensitivity limits, white dwarfs • Good discussion with Badenes, Price-Whelan, Rix, Liu, Widmark, Oh, Koposov ++ • Met many nice people!
  19. Daniella Bardalez Gagliuffi Things I did: - Crossmatched spectral binary

    sample to Gaia for: - Understanding astrometric flags (with Richard Galvez) - Comovers, i.e. triple systems (with Megan Bedell) - Cleaned 25pc sample way too much so killed all binaries Things I learned: - Tricks and quirks of the Gaia data - Brown dwarfs in Gaia too faint to find even fainter things around them for now :( Maybe next DR - My cleanish 25pc sample is way too clean! Need to relax quality cuts. Most importantly, quality cuts depend on the kind of objects you’re interested in. Thank you everyone! astrometric_excess_noise
  20. Chervin Laporte (UVic) Refined colour magnitude diagram and proper motion

    selection for the AntiCenter Stream - to select targets from MSTO to RGB for stream modeling.. Saw that Monoceros and ACS appear as “distinct” kinematic components in mul vs mub space ACS looks very much like the remnant of a tidal tail from Sgr perturbation to disc. Had conversations with HWR and DH about outer disc (perhaps some stars in APOGEE fall on the structure or Monoceros - will need to discss further when I select all the M-giants in the field). Also some conversations with Colin Slater on Anticenter! Had conversations with Ron + Hamish about disc disequilibrium in simulations and data. Had problems with proper motion subtractions in the edge of the disc - will have to write own routines to figure what is going on. Was hoping to learn more about modeling, but will be in touch with members. Thanks for the invitation!!!
  21. Josh Peek – STScI/JHU I tried to find the dust

    around post(-post) AGB stars… and failed to fail... so far? I tried a lot of stuff with varying levels of stupidity • constructing absolute magnitude incorrectly, like 3 times • selecting post-AGB stars from Gaia (hard to tell from reddened hot stars) • using catalogs of post AGB stars (dust likely way to close in & opaque) • trying to use the a_g_val (scary systematics) I learned about the HRD and WD cooling curves ~300, d < 1kpc Hot WDs ~1 Myr past tp 0.02 mag of reddening ~ 1% decrease in star counts Few M⊙ of dusty gas?? I remain skeptical
  22. Lina Necib, Caltech • Learned a lot!!!! • Played with

    the completeness function from Ronald Drummel and Jan Rybizki. • Failed multiple times at getting the density distribution of the metal poor stars (all by myself!). • Joris De Ridder taught me how to query data (now I know that I hate it). • Jackie Faherty and Jonathan Gagne visualized my sample! • Keith Hawkins suggested ways to test the validity of the chemical abundances of my sample of stars. • Got faster MCMC code from Lachlan Lancaster. • Discussed new datasets of metal poor stars with Juna Kollmeier. • Discussed the density distribution with Vasily Belokurov. • Talked to the particle physicists: Mariangela, Matt, Neal, Ken, Katelin, Oren, and Hamish. • Did not manage to get a decent plot of the density distribution before we have to present the wrap up slides. R [kpc] M_sun/kpc^3 Slope = ?
  23. • Calculated bayesian distances with Kepler zero point • Found

    extinction probabilities for each star and applied these to calculate absolute magnitudes, empirical radii and bolometric luminosities • Learned so much about dust extinction, data validation, data storage, integers and more! • Great discussions with so many people including Josh Peek, Eddie Schlafly, Boris Leistedt, Alcione Mora, Megan Bedell, Jonathan Gagne, Adrian Price Whelan, Rocio Kiman + it was lovely to meet everyone! Ellie Schwab Abrahams (AMNH, UC Berkeley)
  24. Rachael Beaton (Princeton & Carnegie) ★ Course BP, RP, and

    G Period-Luminosity Relationship for RR Lyrae ◦ Use MG = 0.5 mag -- look for paper by Jill Neeley soon. ★ Collated 200+ RRL spectra into phase-curves in Temp, log(g), & [(Fe, Si, Al)/H] -- We can & will do RR Lyrae Chemistry in APOGEE! (left) ◦ Bounced it to students at UVa to finish polishing the line list :-). ★ Cross Match OGLEIV (Sgr + Bulge) with Berry’s master Gaia RRL Catalog. Sgr OGLE IV RRL ★ Use 1% mean distance to Sgr from SMHASH (MIR RRL) an assume that the scatter in mag = line-of-sight depth. Coarsely, agrees with what we get using MIR PL. ★ Convert PM to Vtan for each star. ★ Remove “bulk” motion (just the PM components) Super Preliminary
  25. Eileen Gonzales, CUNY GC Subdwarfs with parallaxes Pre-Gaia Thing that

    I did this week: • Completed my catalog of subdwarfs type sdM6 and later • Updated absolute magnitude relations for JHK vs SpT • Started to play around with the sample • Found an awesome spot to work all week! Post-Gaia
  26. Neige Frankel (MPIA) -- WORK IN “PROGRESS” -- Had the

    pleasure to meet the authors of my favourite papers -- Adapted a radial migration model (##) from p([Fe/H], age | R_gal, model) to p([Fe/H], age, R_gal | model) → can now predict a density profile. to plug in a spatial selection function. -- Received tips for APOGEE selection function from Melissa N. -- Was stuck for 24h on a 4D integral connecting model predictions to selected data, until Dan F.M. pointed out it should be a 3D integral! -- Working on a 3D integral.
  27. David W Hogg (NYU) (MPIA) (Flatiron) • My project: spectroscopic

    parallaxes with APOGEE and Eilers ◦ (side conversation: radial-velocity binaries with Price-Whelan and Casey) ◦ (side conversation: velocity-marginalized parallax likelihoods with Leistedt) • I learned: L1-regularized linear regression is incredible: We beat full spectral modeling in spectroscopic-parallax precision, and our data-driven model is literally a projection of the spectral (and photometric) data onto a single linear basis vector! ◦ Take that, deep learning! ◦ Model is interpretable and uncertainties can be propagated; not true for deep learning! • Now we can: Make precise maps of the Milky Way in abundances and kinematics. ◦ (out to 30 kpc from the Galactic Center; much further than red-clump stars)
  28. Jason Hunt (Dunlap Institute, Toronto) Chatted to people about the

    structure in the velocity distribution, and potential causes for it - e.g. Spirals, phase mixing after passage of dwarf / merger. Finished this paper On (arXiv tomorrow!) Then I (mostly) learned actions! (Thanks Wilma & Adrian) And, with 4th floor library: Action space clustering (credit: Natalie P-J) Searching for resonance conditions in action / angle / frequency space (credit: Ted)
  29. Ronald Drimmel [email protected] Learned lots. Helped others. Shared data. Talked

    about completeness. Found >8400 EHB stars. Questions: • • • •
  30. Cicero Lu (JHU) • Giants misclassified (these two are 5.7kpc,

    & 46 kpc away)? • Giant stars hosting sub-Neptune planets? • Matthew Wilde told me he also see similar stuff for Kepler Could there be potential metallicity offset between Exoplanet host and non-host? Done: X-matched Gaia x K2 x APASS x 2MASS for M dwarfs
  31. Alcione Mora (ESA-ESAC) 1. Learnt how people use the data

    2. Prepared for ESAC Exploration Lab 3. Done some multiples: Hipparcos vs Gaia DR2 4. Wanted to do more on catalogue debiasing 5. Enjoyed a lot
  32. Stephen Feeney, Flatiron Institute What I’ve done: Initiated one wild

    goose chase :/ Talked to very interesting people \o/ Downloaded ~10K Gaia Cepheids :O Downloaded ~50 HST Cepheids :) Moved from Python 2.7→3.6 >:( Discovered Astropy’s awesomeness \o/ Matched all but 6 Cepheids… O.o
  33. Boquan Chen, UWisconsin-Madison => USydney [email protected] 1. Classification of Orion

    with 5d information in Gaia 2.Chemo-Dynamical Tagging with APOGEE-Gaia (Refound open and globular clusters and some features) 3.Fe-Dynamical Tagging with LAMOST-Gaia (locally) 4. Did not have time to apply the SNN algorithm to Gaia DR2 beyond Orion. To be continued…….
  34. Ken Van Tilburg (NYU & IAS) => A DM subhalo/blob

    heavier than 2 * 10^7 solar masses with a scale radius of 0.4 pc and line-of-sight distance of 2 kpc would have shown up as an outlier larger than any measured test statistic Astrometric, weak, gravitational lensing by completely dark, compact, dark matter clumps in the LMC foreground
  35. Sihao Cheng (JHU) RR Lyrae distraction with Sergey Got Help

    to calibrate RR Lyrae color First action distribution in my life Learnt useful knowledge of Gaia, lightcurve data, RR Lyrae property, dynamics Co m=4 m=2 Assume Flat rotation curve Omega_p ~ 1.5 R_co ~ 5.3 kpc Thanks to Wilma and Johanna JR Lz
  36. Andy Casey Monash University (Melbourne, Australia) • I learned a

    tonne of stuff this week, and formed new collaborations. • Inferring binarity for ~10 million stars in Gaia: detection, characterisation (period, semi-amplitude, inclination). • Built a non-parametric model of binarity across the H-R diagram using astrometry, radial velocity (absence/scatter), colours, systematics, photometric variability, etc. (~210 million parameters) • Found a few candidate stellar-mass black hole binary systems. • Used Gaia data to kill off multi-modality in APOGEE binary solutions. • Made a Python tool to query Gaia forecast tool. Through collaboration and discussions with Badenes, El-Badry, Foreman-Mackey, Hogg, Holl, Michalik, Hernandez, Koposov, and Price-Whelan. Slide design by Adrian Price-Whelan
  37. Natalie Hinkel (Vanderbilt -> Southwest Research Institute) I did: Some

    awesome visualizations with AMNH and Jonathan Gagné, Jackie Faherty, & Keith Hawkins. Young moving groups -- hint of a chemical stream? Still working on: HYPOGEE...111 stars I also am using (tried? still trying?): Elements = [-0.25, 0, 0.25] Fe, C, O, Ti, Mg, Na, Al [Eu/Fe] in GALAH+APOGEE: -0.14 (0.15 dex) [Eu/Fe] in Gaia-ESO+APOGEE: 0.02 (0.18 dex)
  38. We found 4 new coeval groups ! • Distances 70

    ‒ 180 pc • Ages 100 ‒ 400 Myr Jonathan Gagné (Carnegie DTM)
  39. Joris De Ridder KU Leuven - DPAC CU7 Ceci n'est

    pas un 'spectrum' Order OPTICS clustering 35K RRab 4h download time 50K RRL SMC Sgr stream Bump NGC 6229 Sgr dSph M3 M72 IC 4499 M53
  40. Mercè Romero-Gómez (Institute of Cosmos Sciences, University of Barcelona -

    ICCUB, DPAC-CU9) • I used J. Gagné’s selection of YLAs to re-compute dynamical ages via traceback analysis (backward orbital integration). • For most of the YLAs we are able to provide an estimated age or a range, improving GDR1-TGAS results. • For TW-Hya, we now have 22 members and give an age estimate of 4-11Myr. TW - Hya, estimated age from literature: 3-15Myr Not available using GDR1-TGAS __ observed __ estimated ... errors
  41. I was searching for this “blob” in Gaia DR2 to

    check if it’s associated with Pal 5’s leading arm My project on Pal 5: Sarah Pearson (Columbia University) As predicted by my simulations of Pal 5 in a barred Galactic potential CMD of red blob region CMD of Pal 5 and blob CMD of Pal 5 (shifted) to closer distance and the blob Pal 5 in DR2:
  42. Christina Eilers (MPIA) • linear model to obtain spectroscopic parallaxes

    from APOGEE spectra + 3 colors • distances to ~50,000 RGB stars out to ~30 kpc with < 10% uncertainties In collaboration with David W Hogg, Melissa Ness, Hans-Walter Rix, Daniel Michalik & Sven Buder! Thank you!!
  43. Daniel Hestroffer (Paris obs. +DPAC) • I did this: ◦

    New connections! (Dank U Santiago and the Leiden Sterrewacht group ;) & Co. ◦ Discussions on stellar perturbations on Solar System, and brown dwarfs ◦ Start astrometric reductions from stellar catalogue • I didn’t yet do that ◦ Looking forward to DR3 and next GaiaSprint (this was my 1st one) & more Solar System Science? (SSO rocks!) Thanks to NYC GaiaSprint organizers and Flatiron inst. [email protected]
  44. I did/learned that: • finding stars in MC stream is

    truly amazing (thanks Elena D'Onghia) though very difficult (thanks (?) Vasily Belokurov) ◦ Found that one suggested leading stream star is in the disk (hence discarded) • people seem extremely interested using the variable star samples (especially RR Lyrae) ◦ Our partially disjoint classifier and detailed analyses tables successfully confused people, so we provided above link to get unconfused) ◦ Many people hack first / read later (is reading papers overrated?) • That it was very useful&pleasing to contribute in people’s understanding of the data • This sprint was the best scientific experience I had (so far ;)
  45. I did/learned that: • finding stars in MC stream is

    truly amazing (thanks Elena D'Onghia) though very difficult (thanks (?) Vasily Belokurov) ◦ Found that one suggested leading stream star is in the disk (hence discarded) • people seem extremely interested using the variable star samples (especially RR Lyrae) ◦ Our partially disjoint classifier and detailed analyses tables successfully confused people, so we provided above link to get unconfused. ◦ Many people hack first / read later (is reading papers overrated?) • That it was very useful & pleasing to contribute in people’s understanding of the data • This sprint was the best scientific experience I ever had! • Flatiron Institute: many thanks for the travel support, great facilities and super tasty food
  46. Axel Widmark Unresolved multiple stellar systems White dwarfs population statistics

    Unresolved WD binaries Some WD binaries are not found when looking at a 2D at a parameter space. Complications: inaccuracies in WD color models (data-driven corrections with Boris Leistedt)
  47. Eleonora Zari Leiden Observatory • I made a 3D density

    map of PMS stars within d = 500 pc • I studied the kinematics of the stars within the contours and rediscovered the Sun motion!
  48. • I consulted with various people about the morphology of

    the group. • I found that 14 of these stars are bright X-ray sources. • I learned that one can measure acceleration and constrain orbit with Hipparcos+Gaia astrometry. Semyeong Oh (Princeton)
  49. Ana Bonaca (Harvard) Members of the Jhelum stream (proper motion-selected

    along the main sequence): Possible origins: • Caustic shell • Two progenitors • Precession of the orbital plane • Chaos!
  50. Went looking for structure in the outer disk. Stepping PM

    in Galactic longitude coord; mostly showing “normal” disk behavior + Mon + ACS + EBS + Etc. No big surprises(?) Lots of thanks to Chervin Laporte for the ideas and for doing a more proper job Colin Slater (University of Washington) MSTO stars, 20.5 > G > 19, low parallax
  51. Boris Leistedt (NYU) Hierarchical inference of velocity distribution Application to

    halo stars: improved parallaxes with PMs marginalized (+5/10 points in SNR!) Weak dust constraints from HRD only
  52. Sven Buder (MPIA) Gaia/GALAH@Hayden planetarium Thanks: - For using GALAH

    DR2 - To Gaia and DPAC - To Flatiron [Ba/Fe] as age indicator
  53. Borja Anguiano (University of Virginia) • • • • single

    point = 1000 stars Z - vz Ratio between semi-axes of the velocity ellipsoid
  54. Jacob Hamer (Johns Hopkins University) • Went from 140 Hot

    Jupiters to ~340 for which I could calculate UVW velocities (!) • Learned many things that made it all that easier (thanks Adrian and others!) • Future: ◦ Disentangle metallicity-age effect ◦ Select a better control sample to do that ◦ Extinction correction ◦ Better MS selection
  55. Elena D’Onghia (UW-Madison) The MW in Action space Simulation of

    Milky Way galaxy with a buckling bar of 5 kpc. Stars selected within 1 kpc from the Sun. At the time of the buckling of the bar there is an empty region in JR- Lz (thanks Wilma) Test to look for corotation in Action Space: we can look at Perseus, Outer Arm Vr Vphi See Chao Liu’s plots eccentricity
  56. Carles Badenes (University of Pittsburgh) • Talked to LOTS of

    people, learned A TON. Special thanks to Andy Casey, Adrian Price-Whelan, Kareem El-Badry, and Josh Peek! • Stellar multiplicity with Gaia RV dispersions: doable but needs more work. Andy Casey’s approach is more powerful (but potentially harder to interpret). • Many cool systems (bunnies) in the censored zone!
  57. Megan Bedell (Flatiron) Things I did: • Many ADQL queries

    • Looked at kinematics + stellar age + composition connections with solar twins • Found co-moving Gaia sources in the Kepler field • Fun science with excellent people! One cool result: (with Ben Montet (UChicago)) This star is 4 Gyr old (from isochrones + Gaia plx) These stars are comoving in Gaia DR2! This star has a Hot Jupiter and a 4-day rotation period (from Kepler PSF modeling)
  58. Jose Hernandez (ESAC) I did this: Learned a lot, got

    a few odd sources which I’d like to investigate, explained the astrometry flags, good some ideas of what could be helpful to try improving, enjoyed seeing how Gaia data gets used in very imaginative and surprising ways. Got many new ideas of things to look at… so may be DR3 will get delayed a bit :-) I did that: Worked with Jackie, Tim, Daniel and Alcione on possible binaries found comparing DR1/DR2 proper motions, investigated DR2 pm systematics in the RF.
  59. Ted Mackereth (Liverpool John Moores University, UK) - I DIDNT

    do my proposed project! - I learned stuff about actions and angles (thanks to Wilma Trick: Action Woman), learned stuff about the bar (and some bars) from Jason - and made a .gif, because thats what we do now, right? (thanks Adrian) - Once again, had a great week with all you great folks.
  60. Rocio Kiman (The Graduate Center, CUNY) Want I did •

    Defined color cuts for M dwarfs in G-RP and BP-G. • With some cut to keep good photometry, G-RP is a proxy for spt. • Added cut in absolute magnitude to remove giants contamination.
  61. Denis Erkal (University of Surrey) Did: Had fun, learned a

    lot, struggled with streams near GCs. -> Sagittarius Sgr on sky Sgr PM Traced bifurcation closer in 3d Sgr in RR Lyrae Across stream direction
  62. Mark Fardal (STScI) Did: messed with Sagittarius RR Lyraes and

    measured their tangential motion. Looked at lots of awesome Sag plots by Denis and Vasily. Failed: detecting fainter streams in proper motion space. But at least now I’ve learned how to do it. And learned a lot from many awesome people!
  63. Kathryn V Johnston (Columbia University) I did this: • Provided

    (?helpful?) thoughts for projects with Sarah Pearson, David Hendel, Chervin Laporte; Ana Bonaca • Appreciated being surrounded by exciting science; • Interrupted Wilma too many times as she imparted great action-intuition; THANKS: • Gaia team • Sprint leaders - Hogg! Ana! Adrian! ….. • Jackie for AMNH immersion • And fellow sprinters/ramblers…...
  64. Cecilia Mateu • Remember to use the filter astro_excess_noise<2 •

    Distances to ALL SOS RRLyrae computed with PMG from R. Beaton @ Gaia Sprint (available online) • In progress: testing RRL catalogue from Classifier Table (Berry Holl) -> 195,780 (RR*) matched to compilation of (~12) RRLyrae surveys from literature -> advantage: sky uniformity, at cost of higher contamination SOS RR (~120K, astro_excess_noise<2) with (lots of) help from Berry Holl and Joris de Ridder