adsabs/AstroCLIMB huggingface dataset:
Paper: The Undiscovered Ultradiffuse Galaxies of the Local Group
Authors: Oliver Newton, Arianna Di Cintio, Salvador Cardona–Barrero, Noam I. Libeskind, Yehuda Hoffman, Alexander Knebe, Jenny G. Sorce, Matthias Steinmetz, Elmo Tempel
Figure caption: Lower panel: the whole-sky radial cumulative distributions of UDGs (solid lines) and all field galaxies (dotted lines) with stellar masses, 106 ≤ M */ M⊙ < 109, as a function of the distance to the nearest host galaxy, r nearest, normalized to the host galaxy’s R 200. We overlay the incomplete census of observed field galaxies as points with error bars showing the 68% distance uncertainties (using data compiled by McConnachie 2012). Upper panel: the cumulative distribution function of the UDGs in each HESTIA simulation. To aid the eye, we mark the 50% threshold with a horizontal dotted line.
Paper: The Undiscovered Ultradiffuse Galaxies of the Local Group
Authors: Oliver Newton, Arianna Di Cintio, Salvador Cardona–Barrero, Noam I. Libeskind, Yehuda Hoffman, Alexander Knebe, Jenny G. Sorce, Matthias Steinmetz, Elmo Tempel
Figure caption: The two-dimensional effective radius, R e, as a function of the r-band effective surface brightness, μ e, of the field UDGs in the three high-resolution HESTIA simulations. The size of each marker is inversely proportional to the distance to the nearest host galaxy. The dashed lines show two of our selection criteria applied to the field haloes in the simulations. The galaxies that satisfy all of the selection criteria described in Section 2.1 are plotted with filled symbols, while unfilled symbols show the rest of the field galaxies. The faint filled symbols show galaxies that satisfy less stringent selection criteria (dotted lines) that are often used in the literature.
Paper: The Undiscovered Ultradiffuse Galaxies of the Local Group
Authors: Oliver Newton, Arianna Di Cintio, Salvador Cardona–Barrero, Noam I. Libeskind, Yehuda Hoffman, Alexander Knebe, Jenny G. Sorce, Matthias Steinmetz, Elmo Tempel
Figure caption: The projected mass-weighted densities of DM (red), gas (green), and stars (white) within 2.5 Mpc of the Local Group in the 17_11 simulation. The two bright galaxies at the center are the analogs of the Milky Way and M31 and we mark the projected positions of the UDGs with light-blue circles.
Paper: The Undiscovered Ultradiffuse Galaxies of the Local Group
Authors: Oliver Newton, Arianna Di Cintio, Salvador Cardona–Barrero, Noam I. Libeskind, Yehuda Hoffman, Alexander Knebe, Jenny G. Sorce, Matthias Steinmetz, Elmo Tempel
Figure caption: Mock SDSS observations of the population of field UDGs. The solid and dashed lines show the median predictions obtained by observers in the Milky Way and M31 analogs, respectively. The shaded regions represent the 68% scatter in the Milky Way analog luminosity functions over 15,000 mock observations.
Paper: Accurate Dust Temperature and Star Formation Rate in the Most Luminous z > 6 Quasar in the Hyperluminous Quasars at the Epoch of Reionization (HYPERION) Sample
Authors: Roberta Tripodi, Chiara Feruglio, Francisca Kemper, Francesca Civano, Tiago Costa, Martin Elvis, Manuela Bischetti, Stefano Carniani, Fabio Di Mascia, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Luca Zappacosta
Figure caption: Left panel: SED of J0100+28 using our new ALMA 670.91 GHz data (cyan star); the continuum fluxes from 32 to 353 GHz (Wang et al. 2019) and at 1.5, 6, and 10 GHz (Li et al. 2022; cyan diamonds). The best-fitting curve is shown as a blue solid line. Right panel: corner plot showing the posterior probability distributions of T dust, M dust, and β. Orange solid lines indicate the best-fitting value for each parameter, while the dashed lines mark the 16th and 84th percentiles for each parameter.
Paper: Accurate Dust Temperature and Star Formation Rate in the Most Luminous z > 6 Quasar in the Hyperluminous Quasars at the Epoch of Reionization (HYPERION) Sample
Authors: Roberta Tripodi, Chiara Feruglio, Francisca Kemper, Francesca Civano, Tiago Costa, Martin Elvis, Manuela Bischetti, Stefano Carniani, Fabio Di Mascia, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Luca Zappacosta
Figure caption: 670.9 GHz dust continuum map of QSO J0100+28 (levels −3σ, −2σ, 2σ, 3σ, 5σ, and 8σ, σ = 0.8 mJy beam−1). The clean beam (﹩1.97^{\prime\prime} \times 1.17^{\prime\prime} ﹩) is indicated in the lower left corner of the diagram. The cross indicates the position of the continuum peak.
Paper: Accurate Dust Temperature and Star Formation Rate in the Most Luminous z > 6 Quasar in the Hyperluminous Quasars at the Epoch of Reionization (HYPERION) Sample
Authors: Roberta Tripodi, Chiara Feruglio, Francisca Kemper, Francesca Civano, Tiago Costa, Martin Elvis, Manuela Bischetti, Stefano Carniani, Fabio Di Mascia, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Luca Zappacosta
Figure caption: Left panel: [C II]-to-TIR luminosity ratio vs. TIR luminosity. We show our result for QSO J0100+28 (green star) compared with QSO J2310+18 at z = 6.0028 (red star ); two samples of star-forming galaxies at 5 < z < 6 and 6 < z < 7 (cyan and blue squares, respectively, taken from Lagache et al. 2018); and a sample of QSOs at z > 4.4 (violet diamonds, from Bischetti et al. 2021 and Decarli et al. 2018). Right panel: BH mass vs. dynamical mass for J0100+28 (green star), compared with QSO J2310+18 at z = 6.0028 (red star, Tripodi et al. 2022), WISSH QSOs at z ∼ 2–4 (gray diamonds, Bischetti et al. 2021), and luminous z ∼ 4–7 QSOs (gray circles and gray squares, Mortlock et al. 2011; Willott et al. 2013; De Rosa et al. 2014; Kashikawa et al. 2015; Kimball et al. 2015; Willott et al. 2015; Venemans et al. 2016; Trakhtenbrot et al. 2017; Venemans et al. 2017; Willott et al. 2017; Feruglio et al. 2018; Neeleman et al. 2021). Black dashed line (and shaded area) is the local relation from Kormendy & Ho (2013). For J0100+28 (J2310+18), the slope of the arrow, with its uncertainty, indicates how much the growth efficiency of the SMBH is increasing (slowing down) with respect to the growth of the host galaxy.
Paper: Accurate Dust Temperature and Star Formation Rate in the Most Luminous z > 6 Quasar in the Hyperluminous Quasars at the Epoch of Reionization (HYPERION) Sample
Authors: Roberta Tripodi, Chiara Feruglio, Francisca Kemper, Francesca Civano, Tiago Costa, Martin Elvis, Manuela Bischetti, Stefano Carniani, Fabio Di Mascia, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Luca Zappacosta
Figure caption: Corner plot showing the six-dimensional posterior probability distributions of T dust, M dust, β, n, α, and ν cutoff. Orange solid lines on the posterior probability distributions indicate the best-fitting value for each parameter, while the dashed lines mark the 16th and 84th percentiles for each parameter.
Paper: Ultrafast Variability in AGN Jets: Intermittency and Lighthouse Effect
Authors: Emanuele Sobacchi, Tsvi Piran, Luca Comisso
Figure caption: Cartoon of our scenario for the ultrafast variability of AGN flares. The jet’s energy is dissipated via a turbulent cascade. Due to the intermittency of the cascade, the dissipation is concentrated in a set of reconnecting current sheets with a typical size ℓ cs. Since the guide magnetic field is comparable to the antiparallel component (i.e., B g ∼ δ B), electrons energized by reconnection have a strong pitch-angle anisotropy, i.e., their velocity is nearly aligned with the guide field. Then each current sheet produces a narrow radiation beam with opening angle α ≪ 1 and duration τ cs ∼ ℓ cs/c, which is much shorter than the total duration of the flare, τ ∼ ℓ 0/c (the duration is calculated in the proper frame of the emission region). The gamma-ray light curve is highly variable as a single beam dominates over the whole emission region when it intercepts the line of sight. Our model predicts that ultrafast gamma-ray flares have a faint counterpart at lower frequencies (optical, X-rays) as the synchrotron emission is suppressed due to the pitch-angle anisotropy of the radiating particles.
Paper: Ultrafast Variability in AGN Jets: Intermittency and Lighthouse Effect
Authors: Emanuele Sobacchi, Tsvi Piran, Luca Comisso
Figure caption: Morphology of the gamma-ray light curve for weak beaming (dotted), intermediate beaming (solid), and strong beaming (dashed). The light curve becomes more variable as the beaming of the radiation from the current sheets increases.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: We show snapshots of a vertical slice from the inner regions of the 3D GRMHD simulations with a09rc0 (R  c  = 0, top), a09rc10 (R  c  = 10r  g , middle), or a09rc50 (R  c  = 50r  g , bottom), at different times t = (3000, 35,000, 48,000)r  g /c (left to right). The colors show the gas rest-mass density ρ 0. The black lines indicate the magnetic field lines, of which the thickness represents the magnetic field strength. The pink contours show the boundary of the jet with σ = 1. The blue contours show the disk–wind (i.e., inflow–outflow) boundary, which has u  r  = 0. In all simulations, geometrically thick disk structures (shaded with a light blue color) form close to the BHs. In addition, wide-angle winds and relativistic jets are launched.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: Leakage of magnetic flux: The panels show snapshots at t = 35,000r  g /c in the a09rc0 model (top four panels) and a09rc50 model (bottom four panels) in the vertical plane (panels (a) and (c)) and equatorial plane (panels (b) and (d)). The left column shows the gas density, and the right column shows the electromagnetic energy flux. The inflow regions are shaded with a light blue color, with blue contours marking the inflow–outflow boundaries. The pink contours indicate the jet boundaries with σ = 1. The black lines in the left column are the density-weighted velocity streamlines, and the white lines in the right column are the magnetic field lines. One can see that in the a09rc0 model gas around the midplane can persistently flow out at a large range of angles and carry away large magnetic fluxes. In contrast, in the R  c  = 50r  g  run, a steadier inflow structure forms, which likely plays an important role in retaining the high-level magnetic flux in the inner accretion flow. (Full movies of these models can be seen at https://tomkm.com/madbondi.html.)
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/angle-integrated radial profiles of (a) density ρ, (b) lab-frame radial velocity v  r  (ρ-weighted) over the freefall velocity v ff, (c) lab-frame angular velocity Ω (ρ-weighted) over the relativistic Keplerian angular velocity ΩK, (d) geometric half angular disk thickness H/R, and (e) Lorentz factor of the jet Γ (σ-weighted). The three different colors denote the different models: a09rc0 (red), a09rc010 (yellow), and a09rc50 (blue). The quantities in the inflow and wind regions in (a)–(c) are plotted using solid and dotted–dashed lines, respectively. All models produce sub-Keplerian, sub-freefall, and geometrically thick disks, though the model a09r50 produces the thinnest and fastest-rotating disk among the three. The relativistic jets in the models have a peak Lorentz factor Γ = 3–4, at r ∼ 1000r  g .
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: Time evolution of the mass accretion rate ﹩{\dot{M}}_{H}﹩ (top panel), dimensionless magnetic flux ϕ  H  (middle panel), outflow energy efficiency η  H  (bottom panel, dotted line), and jet efficiency η jet (bottom panel, solid line) of the three models a09rc0 (red), a09rc10 (orange), and a09rc50 (blue). The jet efficiency is measured at r = 100r  g ; the other quantities are measured close to the horizon. The three vertical blue lines indicate the time at which the snapshots in Figure 1 are taken. The light yellow highlight indicates the time interval over which we compute the time-averaged values of the various quantities. The horizontal dashed line in the middle panel indicates the critical value of ϕ  H  ∼ 40 for the disk to enter the MAD state. The smaller the value of R  c  and hence of the initial specific angular momentum, the faster the magnetic fluxes accumulate initially. However, the MAD state and very powerful jet are only sustained in the model a09rc50 with the highest initial specific angular momentum.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/ϕ-averaged θ-profiles of (a) ρ, (b) v  r /v ff (ρ-weighted), and (c) Ω/ΩK (ρ-weighted) for the surface at r = 100r  g . The colors indicate the three models as in Figure 3. In panel (b), solid lines indicate inflow, and dotted–dashed lines indicate outflow. In panel (c), solid lines indicate clockwise rotation, and dotted lines indicate counterclockwise rotation. The vertical dashed lines indicate the northern jet boundary with σ = 1 in the three models. Only the accretion flow in model a09rc50 can develop coherent rotation among the three. Model a09rc50 also produces the highest radial and angular speed of the wind.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/θ/ϕ-averaged radial profiles of (a) the fastest-growing MRI wavelength in the θ-direction, λ  θ,MRI, (b) the fastest-growing MRI wavelength in the ϕ-direction, λ  ϕ,MRI, (c) the quality factor in the θ-direction, Q  θ,MRI, (d) the quality factor in the ϕ-direction, Q  ϕ,MRI, and (e) the MRI suppression factor, S disk,MRI. The colors indicate the three models as in Figure 3. The dashed line indicates the criterion that the MRI is suppressed in the disks if S disk,MRI ≲ 1/2.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/angle-integrated radial profiles of (a) ∣B  R ∣, (b) ∣B  ϕ ∣, and (c) ∣B  z ∣ of the inflow. The colors indicate the three models as in Figure 3. We find the three magnetic field components evolve similarly in the inflow equilibrium regions (r  g  ≲ 100r  g ) in all three models.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The initial conditions of the gas specific angular momentum l and magnetic field of the three runs: (a) a09rc0, (b) a09rc10, and (c) a09rc50. The colors show the initial specific angular momentum. The black lines indicate the initial magnetic field lines.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/ϕ-averaged θ-profiles of the total Maxwell stress W  r ϕ,Maxwell (solid lines), mean-field torque stress W  r ϕ,mean (blue dashed lines), and turbulent field torque stress W  r ϕ,turbulent (red dashed lines) for the surface at r = 6r  g . The light yellow shading highlights the inflow region where u  r  < 0 at r = 6r  g . The Maxwell stress is always positive at all latitudes. In all models, the turbulent component of the Maxwell stress dominates the inflow region toward the midplane, and the mean-field component dominates the outflow region.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: Histograms of the dimensionless magnetic flux around the horizon ϕ  H  of the three models: (a) a09rc0, (b) a09rc10, and (c) a09rc50. We sample ϕ  H  in two different time ranges: (1) the early phase t = (0–20,000)r  g /c, plotted in red, and (2) the late, quasi-equilibrium phase t = (20,000–50,000)r  g /c (when we compute the average values of the quantities), plotted in blue. The orange and green dashed–dotted lines are the lognormal distribution functions fitted on the profiles of ϕ  H  in the early and late phases, respectively.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/angle-integrated radial profiles of (a) the total disk viscosity parameter α of the accretion inflow and its components: (b) the Reynolds viscosity parameter α Reynolds and (c) the Maxwell viscosity parameter α Maxwell. The colors indicate the three models as in Figure 3. The Maxwell viscosity α Maxwell is relatively high in the inner inflow in all simulations, suggesting the Maxwell stress mainly causes the transport of angular momentum and accretion.
Paper: The Effects of Gas Angular Momentum on the Formation of Magnetically Arrested Disks and the Launching of Powerful Jets
Authors: Tom M. Kwan, Lixin Dai, Alexander Tchekhovskoy
Figure caption: The time/ϕ-averaged θ-profiles of (a) B  R , (b) B  ϕ , and (c) B  z  along the surface at r = 6r  g . The colors indicate the three models as in Figure 3. B  R  and B  ϕ  have different signs above and below the midplane.
Paper: PAH Emission from Star-forming Galaxies in JWST Mid-infrared Imaging of the Lensing Cluster SMACS J0723.3-7327
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: F444W−F770W vs. F770W−F1000W color–color diagram for the JWST observations of the SMACS J0723 field. Top panel: simulated diagram for SFGs detected (filled crosses) in an MIRI FOV with the same magnitude limits as those of the SMACS J0723 observations. The large filled circles indicate the entire sample of SFGs in this FOV, most of which are undetected. The color-shaded tracks (small filled circles) are similar to the tracks of Figure 1, with an additional 0.05 mag scatter. The shaded black region shows the expected location of early-type galaxies. We expect to detect 18 SFGs per MIRI FOV. Bottom panel: color–color diagram of 173 galaxies detected in JWST imaging (filled crosses), supplemented with MUSE spectroscopic redshifts where available (color-filled crosses). We identify 23 cluster galaxies with available spectroscopic redshifts (z = 0.387 ± 0.020; yellow-filled crosses). There is only one confirmed cluster galaxy that resembles the color–color diagram location of SFGs (yellow-filled cross at (0.5,1.3); see Section 5).
Paper: PAH Emission from Star-forming Galaxies in JWST Mid-infrared Imaging of the Lensing Cluster SMACS J0723.3-7327
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Color-composite image (F1500W: red; F1000W: green; F770W: blue) of a 320 × 310 pixel (0.″11 per pixel) except of the JWST/MIRI SMACS J0723 observations (see Pontoppidan et al. 2022 for the full FOV). The number next to each circle indicates the ID in the spectroscopic redshift catalog of Caminha et al. (2022). The yellow circles mark two SFGs at z = 0.4233 (ID: 48) and 0.5189 (ID: 49). The light blue circle marks the brightest cluster (elliptical) galaxy (ID: 41). The green circle shows a lensed source at z = 1.4503 (ID: 1.2). We identify one cluster (z = 0.3822; ID: 25) SFG, which is marked with the red circle. The white circles mark three SFGs at estimated z ∼ 0.9–1.3, as indicated by their location in the color–color diagrams.
Paper: PAH Emission from Star-forming Galaxies in JWST Mid-infrared Imaging of the Lensing Cluster SMACS J0723.3-7327
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Same as Figures 2 and 3 but showing the F1000W−F1500W vs. F1500W−F1800W colors for a total of 99 detections.
Paper: PAH Emission from Star-forming Galaxies in JWST Mid-infrared Imaging of the Lensing Cluster SMACS J0723.3-7327
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Same as Figure 2 but showing the F770W−F1000W vs. F1000W−F1500W colors for a total of 129 detections.
Paper: PAH Emission from Star-forming Galaxies in JWST Mid-infrared Imaging of the Lensing Cluster SMACS J0723.3-7327
Authors: Danial Langeroodi, Jens Hjorth
Figure caption: Redshift-dependent tracks of SFGs (thick lines), AGNs (thin lines), and quiescent galaxies (thick lines with thick black filling) in mid-infrared color–color diagrams. From top to bottom: F444W−F770W vs. F770W−F1000W; F770W−F1000W vs. F1000W−F1500W; and F1000W−F1500W vs. F1500W−F1800W color–color diagrams based on SF SED templates from Dale & Helou (2002) and Kirkpatrick et al. (2012); AGN templates from Kirkpatrick et al. (2012); and the early-type SED of NGC 584.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Stacked histograms illustrating the distributions of the rest-frame optical Sérsic Index (n), effective radius (R  e ), and axis ratio (b/a) for the z > 3 galaxy sample. The colors indicate the different combinations of the main morphological class chosen by two out of three people during the visual classifications, as described in Section 4.1 and Figure 2.