adsabs/AstroCLIMB huggingface dataset:
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: (a) JWST three-band color selection using NIRCam F150W, F277W, F444W from Long et al. (2023) for galaxies with F150W brighter than 28 AB. The blue dashed lines show the QG selection criteria, with an extension toward bluer F150W − F277W colors to capture more young PSBs. (b) The three-band color selection using F150W, F444W, F770W from Lovell et al. (2023) with F150W < 28 and F770W < 25 AB. The black dotted line shows their suggested selection. In both panels, data points are colored by redshift, and the stars and pluses denote the QG and PSB candidates in this study; circles show other galaxies. Given a rough redshift cut of z phot = 2.5, we find minimum contamination rates of 60% for the Long et al. (2023) selection and 25% for the Lovell et al. (2023) selection.
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: The formation time (since the Big Bang) of our QG (red stars) and primary PSB (orange pluses) candidates as a function of the redshift at which they are observed. The right y-axis shows the corresponding formation redshift. The black line shows the age of the Universe at the observed redshift. We compare to the CEERS sample (gray crosses) from Carnall et al. (2023a) and the median timescales from the EAGLE and FLARES simulations (tan squares; Lovell et al. 2023).
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: The number density of photometrically selected, massive (log M ⋆/M ⊙ ≳ 9.5) quiescent galaxies at z ∼ 3–6 from our robust (purple stars) and full UVJ-selected (pale blue stars) samples. Points are staggered slightly along the redshift axis for visual clarity. We compare to the massive (log M ⋆/M ⊙ ≳ 9.5) robust and full samples from Carnall et al. (2023a; pentagons) and the UVJ-selected sample from Valentino et al. (2023; diamonds). We find that the abundance of quiescent galaxies in the MIRI parallel agrees with the higher estimates from the deep CEERS survey (Carnall et al. 2023a); however, we caution that our field contains known overdensities (Section 5.3, Appendix B).
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Physical properties of the simulated ETGs (circled bars), compared to observed galaxies from the ATLAS3D (circular transparent data points) and MASSIVE (square transparent data points) galaxy surveys. Open data points represent observed galaxies with no measured values of the molecular gas disk size R CO (bottom middle panel), and so no measured values of the molecular gas surface density ﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2},\ \mathrm{CO}}﹩ (bottom right panel). Black lines represent the median observed values of each physical quantity in stellar mass bins centered on M * = 1010, 1010.5, 1011, and 1011.5 M ⊙. The vertical extent of the circled bars represents the values spanned by the simulated galaxies between the simulation times of 100 and 400 Myr, colored according to their gas fractions. Our simulations roughly reproduce these median values (see Section 2.1). Observational references: M. Cappellari et al. (2011), D. Krajnović et al. (2013), M. Cappellari et al. (2013), and T. A. Davis et al. (2013, 2014) for ATLAS3D, and M. Veale et al. (2018), T. A. Davis et al. (2019), and T. Davis (2024, private communication) for MASSIVE.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Top panels: density–temperature phase diagrams for the Milky Way–like galaxy simulation (left) and the smoothest ETG (M * = 1011  M ⊙; right). Dashed lines delineate the regions of phase space corresponding to the bar plot in the bottom panels. Bottom left: partitioning of the gas mass in each simulation into four ISM phases, from warmest to coolest, as a fraction of the total gas mass in the simulation: hot gas that has received thermal energy from stellar feedback (﹩{M}_{\mathrm{SN}+\mathrm{HII}}﹩), the WNM (M WNM), the CNM (M CNM), and the total molecular hydrogen reservoir (﹩{M}_{{{\rm{H}}}_{2}}﹩). The molecular hydrogen mass is subtracted from each of the other phase-space regions to produce the bar plot. Bottom right: partitioning of the star-forming gas mass with density ρ/m H μ > 100 cm−3 into fractions with differing SFEs per freefall time, ϵ ff.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Top: midplane circular velocity v circ and epicyclic frequency κ (thick transparent lines) as a function of galactocentric radius R for each of the simulated galaxies across the radial extent of the gas disk, computed directly from the gravitational potential exerted by the gas (thin lines), dark matter (dotted lines), disk stars (dashed lines), and bulge stars (thick lines). Note that the ETG gas disks are much smaller than those of the main-sequence galaxies. The central stellar surface density μ * is given below the stellar mass at the top of each column. Galactic rotation in the ETGs is dominated by the stellar bulge component. Each rotation profile is computed at one simulation time only, but the values change negligibly over the time period analyzed for each simulation. Bottom: comparison of the total circular velocities and epicyclic frequencies for each of the six galaxy simulations.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: The median Toomre Q parameter (top row), gas and stellar radial velocity dispersion (second row), and gas and stellar surface density (third row) as a function of galactocentric radius for the six galaxies in our sample. The bottom row compares the gas disk scale height to the Toomre and 2D Jeans wavelengths. All values are computed for gas at temperatures T < 2 × 104 K. Shaded regions represent interquartile ranges over azimuthal angle and simulation time. The Toomre Q parameters of the ETGs are much higher than those of the main sequence (Milky Way–like and NGC 300–like) galaxies.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Left: median SFR surface density ΣSFR as a function of the cold gas (atomic plus molecular) surface density ﹩{{\rm{\Sigma }}}_{\mathrm{HI}+{{\rm{H}}}_{2}}﹩, integrated across each simulated galaxy (large circles) and measured for the galaxies in the ATLAS3D galaxy sample (T. A. Davis et al. 2013, 2014; small transparent circles). The colors of the data points correspond to their gas fractions, and gas depletion times of 108, 109, and 1010 yr are given by the black solid, dashed, and dotted lines, respectively. Interquartile ranges over time and galactocentric radius are given by error bars. For the ETG simulations, these are too small to be shown. Middle: similar to the left panel, but for the molecular gas surface density ﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}﹩. Right: similar to the left panel, but for the median stellar surface density Σ* across the gas disk.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: The two-point correlation function ξ(Δ) for supernova explosions (quantifying the degree of supernova clustering) as a function of their separation Δ over time intervals of 1 Myr, averaged over all times throughout each simulation (solid lines). The black dashed line indicates the profile for a uniform distribution of objects across the galactic midplane (ξ(Δ) = 1). The shaded regions give the interquartile ranges over these times. The level of supernova clustering is higher on all scales in the Milky Way–like and NGC 300–like simulations, relative to the ETG simulations.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Surface density maps of the stellar distribution viewed parallel to the galactic midplane (Σ*; top panels), the total gas distribution viewed perpendicular to and parallel to the galactic midplane (Σgas; middle panels), and the molecular gas distribution viewed perpendicular to and parallel to the galactic midplane (﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}﹩; bottom panels) for each of the simulated galaxies. All ETGs are shown at a simulation time of 400 Myr, while the Milky Way–like galaxy is shown at a simulation time of 600 Myr and the NGC 300–like galaxy is shown at a simulation time of 800 Myr. The small white circles denote the minimum galactocentric radius analyzed in this work. Note that only a small off-center section of the larger Milky Way–like and NGC 300–like disks is displayed.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Each of the six isolated galaxy simulations (stars) in the plane of total stellar mass M * vs. sSFR. Black data points represent atomic and molecular gas detections, respectively, from the xGASS (B. Catinella et al. 2018) and xCOLDGASS (A. Saintonge et al. 2017) surveys, while gray data points represent nondetections. Black crosses represent data from the ATLAS3D survey (M. Cappellari et al. 2011). The galactic star-forming main sequence as defined in B. Catinella et al. (2018) is given by the black solid line and shaded region.
Paper: Learning the Universe: GalactISM Simulations of Resolved Star Formation and Galactic Outflows across Main-sequence and Quenched Galactic Environments
Authors: Sarah M. R. Jeffreson, Eve C. Ostriker, Chang-Goo Kim, Jindra Gensior, Greg L. Bryan, Timothy A. Davis, Lars Hernquist, Sultan Hassan
Figure caption: Global galactic SFR (top panel), gas outflow rate (middle panel), and mass loading of outflows (bottom panel) as a function of time. We begin tracking each property only when the gas disks have reached a state of dynamical equilibrium: 100 Myr onward for the ETG simulations, 300 Myr onward for the Milky Way–like simulation, and 500 Myr onward for the NGC 300–like simulation.
Paper: Characteristics and Source Regions of Slow Alfvénic Solar Wind Observed by Parker Solar Probe
Authors: Tamar Ervin, Kai Jaffarove, Samuel T. Badman, Jia Huang, Yeimy J. Rivera, Stuart D. Bale
Figure caption: Comparison of in-situ characteristics and footpoint estimates for the SASW stream spanning from 2022 December 10 18:00:00 to 2022 December 10 19:00:00 during E14.
Paper: Characteristics and Source Regions of Slow Alfvénic Solar Wind Observed by Parker Solar Probe
Authors: Tamar Ervin, Kai Jaffarove, Samuel T. Badman, Jia Huang, Yeimy J. Rivera, Stuart D. Bale
Figure caption: Comparison of in-situ characteristics and footpoint estimates for the SASW stream spanning from 2022 December 10 20:30:00 to 2022 December 10 22:00:00 during E14.
Paper: Characteristics and Source Regions of Slow Alfvénic Solar Wind Observed by Parker Solar Probe
Authors: Tamar Ervin, Kai Jaffarove, Samuel T. Badman, Jia Huang, Yeimy J. Rivera, Stuart D. Bale
Figure caption: Comparison of in-situ characteristics and footpoint estimates for the SASW stream spanning from 2022 December 12 12:00:00 to 2022 December 12 16:00:00 during E14.
Paper: Characteristics and Source Regions of Slow Alfvénic Solar Wind Observed by Parker Solar Probe
Authors: Tamar Ervin, Kai Jaffarove, Samuel T. Badman, Jia Huang, Yeimy J. Rivera, Stuart D. Bale
Figure caption: Comparison of in-situ characteristics and footpoint estimates for the SASW stream spanning from 2021 January 18 18:00:00 to 2021 January 19 06:00:00 during E7.
Paper: Characteristics and Source Regions of Slow Alfvénic Solar Wind Observed by Parker Solar Probe
Authors: Tamar Ervin, Kai Jaffarove, Samuel T. Badman, Jia Huang, Yeimy J. Rivera, Stuart D. Bale
Figure caption: Comparison of in-situ characteristics and footpoint estimates for the SASW stream spanning from 2021 April 30 00:00:00 to 2021 April 30 05:00:00 during E8.