Poster Quiz

Below are some questions on the posters, ordered by their poster numbers. Please answer these questions using your own paper (labeled with your name) and turn in at the Registration Desk by the end of Thursday.

The winner of the poster quiz will receive a bottle of port!

  1. (#1, Alvarez-Marquez): Which is the name of the MIRI instrument simulator?
  2. (#2, Bridge): How many very bright (m_H < 25.5) z ~ 8 galaxies (the so-called Super Eights) have been found in the latest BoRG search?
  3. (#4, Jones): Above what redshift does the F275W filter on HST/WFC3 probe only the rest-frame Lyman continuum?
  4. (#6, Larson): How many z = 4-6 galaxies do we expect to find in the SHELA field?
  5. (#7, Leung): How do the physical scales of molecular cloud structures at the Epoch of Reionization differ from those observed in the nearby Universe and high-z galaxies (in terms of their velocity dispersions, masses, and sizes)?
  6. (#8, Mestric): How many LCG candidates are reported in the work “LyC radiation from 3.4 < z < 5 galaxies”?
  7. (#10, Sobral): What does “S-SC4K” stand for?
  8. (#11, Anthony Taylor): What is the name of the most luminous Lyman-alpha emitter at z = 6.6 in the HEROES Survey?
  9. (#12, Tang): Which systems in the survey are the most efficient ionizing agents and likely linked to large ionizing photon escape fraction?
  10. (#14, Amarantidis): Which is one of the main limitations of cosmological models in predicting the most massive SMBHs?
  11. (#15, Çatmabacak): How many large volume high resolution MassiveFIRE cosmological simulations were used to reproduce SMBH-galaxy scaling relations in a post-processing analysis?
  12. (#16, Dopcke): Is it possible to observe CO emission from the star forming gallaxy I Zwicky 18 with ALMA or NOEMA?
  13. (#17, Hviding): What two quantities do you trade off between when using color cuts on high redshift galaxies?
  14. (#18, Jin): What is the spatial resolution of our 3D model?
  15. (#19, Kobayashi): What is the main production source of carbon?
  16. (#20, Lehmann): What process destroys molecular hydrogen in intermediate velocity shock waves?
  17. (#21, Li): What are the key mechanisms implemented in the simulations for destroying dust?
  18. (#24, Song): Our empirical model of galaxy evolution at 0 < z < 8 (Song et al.), which is constrained solely by the evolution of the observed galaxy stellar mass functions, suggests that at z > 2-3, the ratio of stellar mass to halo mass at a given halo mass is _____ for higher-redshift galaxies.
  19. (#25, Yung): Name one advantage of the semi-analytic modeling approach.
  20. (#26, Battisti): What had to be added to the dust attenuation curve in MAGPHYS+photo-z to remove a systematic bias in photo-z values?
  21. (#28,Cardoso): What is the typical maximum uncertainty on the stellar properties of the star-forming galaxy models when using the spectral synthesis code FADO?
  22. (#30, Chu): The spectral energy distribution models for a complete sample of 201 local luminous infrared galaxies will be released soon for the wider astronomical community to use. What is the wavelength range of these models?
  23. (#32, Pappalardo): In this poster the code used to create synthetic spectra is also a kind of music with Byzantine origin: what is its name?
  24. (#34, Vidal Garcia): How does the effect of the stochasticity of the stellar IMF depend on the star cluster mass in the luminosity and EW of CIII] 1908 doublet distributions?
  25. (#36, Breda): According to the proposed scenario, in LTGs what is the physical property that drives bulge formation (pace and predominance)?
  26. (#37, Ceraj): At what redshift (roughly) does the number density peak for the population of radio detected radiatively efficient AGN (called moderate-to-high radiative efficiency AGN) in the COSMOS field?
  27. (#38, Champagne): What are the expected final halo masses of the z = 2.5 galaxy protocluster and its core?
  28. (#39, D’Amato): How many spectra are reported on the poster?
  29. (#41, Glazebrook): The poster presents at the bottom a set of real and fake galaxy spectra, the latter were created using a Generative Adversarial Network. Which ones are the real galaxies?
  30. (#42, Hill): How many galaxies will merge to form a ‘brightest cluster galaxy’ in the redshift 4 galaxy cluster SPT2349?
  31. (#43, Ji): According to the stacking of the VLT/VIMOS U-band images of a sample of 69 Lyman Break Galaxies at z > 3.4, how bright (magnitude) do you expect the Lyman-continuum of galaxies at the similar redshift?
  32. (#45, Pensabene): For how many objects have we been able to measure dynamical mass through kinematical modelling of high-z galaxy disk?
  33. (#46, Santini): What does the stacking of ALMA archival data reveal about the nature of the high-z passive candidates?
  34. (#47, Schindler): What is our best fit slope (beta) for the quasar luminosity function at z = 2.8-4.5?
  35. (#48, Sherman): How many more massive star-forming galaxies are found in the SHELA survey footprint compared to previous observational results?
  36. (#50, Stanley): Should we expect all z~6 quasars to have observable outflow signatures?
  37. (#51, Zhou): What is the mass of the candidate BcG in the protocluster at z ~ 3.5?
  38. (#52, Bakx): What tuning set-up is most optimal for blind spectroscopic redshift searches with ALMA for z ~ 2 – 5 galaxies?
  39. (#53, Dale): Which nitrogen line is used to decompose the [CII] emission into its ionized and neutral components?
  40. (#54, Ferkinhoff) : What is the radio spectral index of the non-thermal emission in galaxy W2246?
  41. (#55, Hatsukade): What is the survey area of ASAGAO?
  42. (#56, Kaasinen): Which rest-frame wavelength must one extrapolate to in order to convert a single-band, dust-continuum flux to a molecular gas mass following the Scoville et al. (2016) prescription?
  43. (#57, Kovács): What was the effect of including AKARI data in the SED fits of the selected galaxies?
  44. (#58, Manning): What is the maximum baseline length of e-MERLIN?
  45. (#60, McKinney): At what redshift did we detect [C II] in a PAH-selected galaxy?
  46. (#61, Rieke): The widely used modified blackbody fit to high redshift galaxy far infrared measurements may, if based only on ALMA Band 7 data, underestimate the true luminosity by ______.
  47. (#64, Butler): Why have I ruled out a flat outflow geometry?
  48. (#65, Jones): What is the largest dynamical class of strong [CII] emitters in the ALPINE sample?
  49. (#66, Pirzkal): What does MAP2D enable over standard wide field slitless spectroscopy?
  50. (#67, Puglisi): Do we find a correlation between the molecular gas size and the Main Sequence position?
  51. (#69, Rybak): Which other line is used to interpret the strong [CII]/FIR deficit?
  52. (#70, Tergolina): Which methods are we using in this work?
  53. (#72, Yang): Which component of the source (R, B or G) has the lowest dust temperature?
  54. (#74, Gonzalez): What is the spectral resolution of the MagE Echellette spectrograph on Las Campanas? (for a 1 arcsec slit).
  55. (#75, Jameson): Is the average cold neutral gas temperature in the low metallicity Small Magellanic Cloud colder or warmer than the Milky Way?
  56. (#76, Menendez-Delmestre): Preliminary results suggest that as one cranks up the AGN in a galaxy, the population of polycyclic aromatic hidrocarbons (PAHs) may be affected. In what way?
  57. (#77, Roman de Oliveira): What are the trail vectors and how can they be defined objectively?
  58. (#78, Schnorr-Muller): What are relic galaxies?
  59. (#80, Wofford): If a model spectrum of a galaxy is able to simultaneously reproduce all of the observed emission-line fluxes of high-ionization UV emission lines, can we trust the physical properties extracted from it?
  60. (#84, Grasha): How much younger are star clusters associated with molecular gas than clusters unassociated with molecular gas?
  61. (#85, Jolly: Cite one tool available in Line-Stacker (aside from stacking).
  62. (#86, Matute): What observational feature was used as a proxy to increase the chances for the radio candidates to be at high redshift?
  63. (#87, Messias): Name four JWST filters which will allow you to select AGN up to z = 6.
  64. (#89, Urrutia): How many Lyman Alpha Emitters has MUSE-Wide found so far?
  65. (#90, van der Vlugt): Which correlation is used to select star-forming galaxies in the COSMOS-XS survey?
  66. (#91, Willmer): How are sources simulated in Guitarra?
  67. (#92, Zavala): How many 3mm-selected galaxies have been confirmed to lie at z < 2?