adsabs/AstroCLIMB huggingface dataset:
Paper: Extreme Tidal Stripping May Explain the Overmassive Black Hole in Leo I: A Proof of Concept
Authors: Fabio Pacucci, Yueying Ni, Abraham Loeb
Figure caption:  M •–M ⋆ plane, displaying (i) the current location of the MW and Leo I (with their 1σ uncertainties in the mass estimates), (ii) the relations by Schutte et al. (2019) (appropriate for dwarf galaxies) and Reines & Volonteri (2015), (iii) the time evolution, in terms of the lookback time (see the color bar), of the stellar mass enclosed within 1 kpc from our N-body simulations, and (iv) the initial location in the M •–M ⋆ plane of our simulated Leo I system, with the total stellar mass enclosed within 10 kpc.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: 2D histograms of β  z , for free (left) and trapped (right) positrons (the corresponding figure for electrons is mirror-symmetric with respect to the β  z  = 0 axis). The Lorentz factor γ on the horizontal axis is the instantaneous value. The histograms are normalized to their respective maxima, and colors span the range [10−3, 1] in logarithmic increments.
Paper: Extreme Tidal Stripping May Explain the Overmassive Black Hole in Leo I: A Proof of Concept
Authors: Fabio Pacucci, Yueying Ni, Abraham Loeb
Figure caption: Fractional mass loss of the progenitor of Leo I, calculated analytically for a single pericenter passage. The color scale shows the fractional mass loss as a function of the pericenter radius and the progenitor’s stellar velocity dispersion. The horizontal and vertical bands show estimates of the pericenter and of the velocity dispersion of Leo I (according to two studies), with 1σ confidence intervals.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: Fraction of particles that have experienced at least one free phase, as a function of the maximum Lorentz factor ﹩{\gamma }_{\max }﹩ attained during the particle life. We only show the γ ≳ 3σ range beyond injection.
Paper: The Origin of Power-law Spectra in Relativistic Magnetic Reconnection
Authors: Hao Zhang, Lorenzo Sironi, Dimitrios Giannios, Maria Petropoulou
Figure caption: From our σ = 10 simulation, particle spectra time-averaged within two time intervals (blue: (3 − 5)L/c; red: (5 − 7)L/c), after reconnection has achieved a statistical steady state (t ≳ 3 L/c). Solid lines show “trapped” particles while dashed lines show “free” particles.
Paper: Unveiling the Nature of Galactic TeV Sources with IceCube Results
Authors: V. Vecchiotti, F. L. Villante, G. Pagliaroli
Figure caption: Differential energy spectra of the all-flavor diffuse neutrino emission from the Galactic region ∣b∣ < 5° and 0° < l < 360°. The magenta region corresponds to the superposition of the three IceCube best fits for the Galactic component with their 1σ uncertainty. The predictions for the diffuse emission (Case B) and the total neutrino flux (Case B + sources) are shown with a cyan band and blue band, respectively. The bands represent the uncertainties on the spatial distributions of CRs in our Galaxy. The solid and dotted lines are obtained by assuming smearing radius infinity and 1 kpc, respectively. We show the effect of different energy cutoffs for the CR source spectra as displayed in the labels. We additionally display an excluded region in gray. The bottom line corresponds to the maximum neutrino contribution from our Galaxy obtained by assuming Case B for the diffuse emission, ξ = 1 and E cut = ∞.
Paper: Unveiling the Nature of Galactic TeV Sources with IceCube Results
Authors: V. Vecchiotti, F. L. Villante, G. Pagliaroli
Figure caption: Differential energy spectra of the all-flavor diffuse neutrino emission from the Galactic region ∣b∣ < 5° and 0° < l < 360°. The magenta region corresponds to the superposition of the three IceCube best fits for the Galactic component with their 1σ uncertainty. The prediction for the diffuse emission (Case C) is shown with a red band. The bands represent the uncertainties on the spatial distributions of CRs in our Galaxy. The solid and dotted lines are obtained by assuming smearing radius infinity and 1 kpc, respectively. We additionally display an excluded region in gray. The bottom line corresponds to the maximum neutrino contribution from our Galaxy obtained by assuming Case C for the diffuse emission, ξ = 1 and E cut = ∞.
Paper: Unveiling the Nature of Galactic TeV Sources with IceCube Results
Authors: V. Vecchiotti, F. L. Villante, G. Pagliaroli
Figure caption: We compare the all-sky, single-flavor expectations provided by different models for the truly diffuse emission due to the CR interactions with the interstellar medium. The diffuse emission due to Case B and Case C are plotted with a blue and a red band, respectively. Predicted nominal values for the π 0, the KRA﹩{}_{\gamma }^{5}﹩, and the KRA﹩{}_{\gamma }^{50}﹩ are also displayed for a comparison.
Paper: Extreme Tidal Stripping May Explain the Overmassive Black Hole in Leo I: A Proof of Concept
Authors: Fabio Pacucci, Yueying Ni, Abraham Loeb
Figure caption: Upper panel: time evolution of the stellar mass of the progenitor of Leo I within 10 kpc, following its evolution of the past 8 Gyr. The final mass in the nuclear region, within ∼1 kpc, is smaller and compatible with observations. Lower panel: radial absolute distance between the MW center and Leo I. The horizontal blue line shows the current distance, reproduced at z = 0. The gray shaded area indicates the range of pericenters estimated with Gaia EDR3 data (Pace et al. 2022).
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Estimated sources of scatter in extragalactic Period–Luminosity relations as indicated (add in quadrature). Scatter from random phase sampling and patchy extinction can be reduced through multiepoch sampling and color measurements and are dominant in the optical. Crowding is an important source of scatter in the NIR, but is greatly reduced by the resolution of JWST. These sources do not include photon statistics and assume low galaxy inclination. Measurements from HST and JWST for NGC 5584 and NGC 4258 are indicated as gold and red symbols, respectively.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: HST and JWST Bandpass systems referenced in this work. The HST filters are F555W, F814W, F350LP, and F160W, and the JWST filters include F090W, F150W, and F277W. There is a good correspondence between F814W and F090W and a very good correspondence between F160W and F150W.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Color–magnitude diagrams for the modules covering Cepheids. Each star has a small black point, while Cepheids are indicated by a cyan star. A color cut in this space is included, 0.3 < F090W–F150W < 1.15 corresponding to a broad range around the instability strip (0.5 < V − I < 1.7). The background CMDs are shown from the first visit. If a Cepheid is observed in only the first or both visits, its location on the CMD is shown from the first visit. Otherwise, if it is observed on only the second visit, its location is shown from the second visit.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: JWST wave front sensing data during the interval of these observations in the first half of 2023. The wave front sensing, drifts, remediations, and wave front errors are shown in the top four panels. The bottom panel shows the change to encircled energy in the core of the PSF in the three passbands used for this program. The dates of our observations are indicated as vertical dashed lines and a star symbol.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: HST and JWST image stamps in NGC 4258 for all Cepheids with a period of 18 to 41 days. The upper row indicates the location of each Cepheid. HST filters are labeled in black, and JWST filters in magenta.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: NIRCAM RGB images (F090W/F150W/F277W) showing positions of Cepheids (cyan circles). Regions without short-wavelength coverage (due to the module gaps) were manually set to gray scale.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: NIRCAM fields superimposed on Sloan Digital Sky Survey gri images (Alam et al. 2015) of NGC 4258 (left) and NGC 5584 (right). North is up, and east is to the left.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Same as Figure 7 but for NGC 5584, and with periods of 39–43 days.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Differences in the photometry of stars observed in two epochs on different positions of the NIRCAM field.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Magnitude differences of two epochs for Cepheids in NGC 5584, Left is F090W and right is F150W. Gray density shows the expected frequency of sampling based on random phase and template light curves. Red points are measurements from JWST, and the errors do not include the crowding error, which effectively cancels in the difference. The asymmetry of Cepheid light curves in F090W produces a structure in this diagram that can be used to constrain the phase. The log of the time interval between epochs produces a negligible difference at a value of ﹩\mathrm{log}P\,=﹩ 1.34.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Comparison between the standard (SH0ES: R22) magnitude ﹩{W}_{V,I}^{H}﹩ period–magnitude relation used to measure distances. The red points use JWST F150W, and the gray points are from HST F160W, including a small transformation F150W–F160W = 0.033+0.036[(V–I)-1.0]. The upper panel is NGC 5584, with the inset showing image stamps of the same Cepheid seen in the H band by each telescope. The lower panel is NGC 4258, with the inset showing the difference in distance moduli between NGC 5584 and NGC 4258 measured with each telescope.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Graphical representation of the correspondence between the Cepheid phase (color bar) and magnitude difference between epochs for F090W. NGC  4258 is on the left, and NGC 5584 is on the right.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Same as Figure 10 but for NGC 4258, with an epoch time difference of ﹩\mathrm{log}P\,=﹩ 1.18.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Period–luminosity relations from bluest (bottom) to least reddened (top). The bottom two, F555W and F814W, are from HST, and the others are from JWST. The top set in black is a dereddened or Wesenheit magnitude, F150W-R(F090W–F150W). Magnitude offsets are applied as indicated for ease of view, and the dispersion for each is given.
Paper: Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: A comparison of Cepheid distance measures to NGC 5584.
Paper: Metallicity and Spectral Evolution of WASP 39b: The Limited Role of Hydrodynamic Escape
Authors: Amy J. Louca, Yamila Miguel, Daria Kubyshkina
Figure caption: The metallicity enhancement after ∼12 Gyr of the WASP-39 b grid simulations when solar initial metallicity is assumed (left) and the evolution of the metal-enhancement factor over time (right) for one specific case when solar initial metallicity is assumed and no metal drag is included (red line). The evolution of the metallicity enhancement factor is plotted for the most extreme case, indicated by the red box in the left plot. For the grid plot (left), the color represents the metal-enhancement factor with respect to the initial metallicity, and the horizontal and vertical axes represent the initial mass and initial envelope fraction, respectively. Note that the grid plot is smoothed using the default anti-aliasing interpolation function. The dashed gray rectangle represents the region within the grid plot where a lower internal luminosity of L int = 5 · 1026 erg s−2 is assumed. For all simulations outside this region, we assume a higher internal luminosity of L int = 1027 erg s−2. The maximum metal enhancement for the solar initial metallicity case is ∼1.23× initial metallicity. The vertical dashed black line in the evolution plot is the current age estimation of the WASP-39 system (Bonomo et al. 2017), with error bars as indicated by the vertical dotted gray lines. The yellow diamonds in the evolution plot represent the time steps at which the transmission spectra are evaluated.
Paper: Discovery of a Planar Black Hole Mass Scaling Relation for Spiral Galaxies
Authors: Benjamin L. Davis, Zehao Jin, 泽灏 金
Figure caption: Plots between the dynamically measured M • on the x-axis and the M • predicted by Equation (1) (blue dots) on the y-axis, compared with the M •–ϕ relation from Davis et al. (2017, Equation (8)) in the left column of plots and the M •–v max relation from Davis et al. (2019c, Equation (10)) in the right column of plots (both depicted with orange squares). The subplots show histograms (spread across eight bins, each 0.41 dex wide) for the Δrms scatter (top subplots) and ﹩\bar{{\rm{\Delta }}}﹩ average residual (bottom subplots) about the 1:1 line for both the planar relation (blue solid lines) and the M •–ϕ (left column) or M •–v max (right column) relations (both depicted with orange solid lines). The red dashed line depicts the 1:1 correlation between observed and predicted masses in the main plots and ﹩\bar{{\rm{\Delta }}}=0.0﹩ dex in the lower subplots. For clarity, predicted errors (along the y-axis) are not shown because they are directly proportional to (and always greater than) the errors along the x-axis.
Paper: Metallicity and Spectral Evolution of WASP 39b: The Limited Role of Hydrodynamic Escape
Authors: Amy J. Louca, Yamila Miguel, Daria Kubyshkina
Figure caption: The evolving mixing ratios (left) and transmission spectra (right) of WASP-39 b for the most extreme metal-enhanced scenario, at different time steps in the simulation. The time step is shown within each transmission evolution plot (right). Highlighted in each plot are CH4 features at 3.3 μm and 7–8 μm, CO2 features around 4–5 μm, and missing SO2 features around 4 μm and 7–8 μm, colored similarly as in the mixing ratio plot. The solid lines in the mixing ratio plots represent the abundances at 0.002 Gyr, the striped lines at 0.5 Gyr, the dotted–striped lines at 6.0 Gyr, and the dotted lines at 9.0 Gyr, as labeled above the left figure. The time stamps for the transmission spectra plot are labeled within the figure.
Paper: Discovery of a Planar Black Hole Mass Scaling Relation for Spiral Galaxies
Authors: Benjamin L. Davis, Zehao Jin, 泽灏 金
Figure caption: The distributions of ϕ (left), v max (middle), and M • (right) for our sample of 41 spiral galaxies. The smoothed histograms (red dashed) are generated from the summation of all 41 respective measurements with their uncertainties for each galaxy (i.e., kernel density estimations). The pdfs (blue solid) are skew–kurtotic–normal distributions fit to each histogram. Left: mean = 13.°7 ± 5.°4, median=13.°2 ± 3.°6, and peak probability at 12.°1 ± 0.°9. Middle: mean = 217 ± 44 km s−1, median = 211 ± 32 km s−1, and peak probability at 213 ± 7 km s−1. Right: mean = 7.30 ± 0.75 dex, median=7.27 ± 0.51 dex, and peak probability at 7.28 ± 0.12 dex.
Paper: Discovery of a Planar Black Hole Mass Scaling Relation for Spiral Galaxies
Authors: Benjamin L. Davis, Zehao Jin, 泽灏 金
Figure caption: This figure is identical to Figure 3, except it includes the Milky Way (marked with a star). The online animated version of Figure 2 also includes the Milky Way.
Paper: Metallicity and Spectral Evolution of WASP 39b: The Limited Role of Hydrodynamic Escape
Authors: Amy J. Louca, Yamila Miguel, Daria Kubyshkina
Figure caption: The evolution of the crossover mass for all simulations (left) and the distribution of the age at which the gradient in mass, ﹩{t}_{{\dot{M}}_{\max }}﹩, is the largest (right). In the evolution plots, the orange lines represent the crossover masses of the simulations while the horizontal purple line represents the atomic mass of oxygen in atomic mass units. This horizontal line marks the threshold for which metal drag should occur.
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: The transmission spectrum of K2-18 b. The observed JWST spectrum and 							retrieved model fits are shown for the one-offset retrieval case 							discussed in Section 3. 							The data in orange show our NIRISS spectrum between 0.9 and 2.8 μm, and those in dark red show our NIRSpec 							G395H spectrum between 2.8 and 5.2 μm. The 							spectra are binned to R 							﹩\approx ﹩ 25 and R 							﹩\approx ﹩ 55 for NIRISS and NIRSpec, respectively, for visual 							clarity. The retrievals are conducted on the native resolution spectra, 							resulting in the best-fit reduced ﹩{\chi }_{\nu }^{2}=1.080﹩. The NIRSpec spectrum is vertically offset by −41 ppm, 							corresponding to the median retrieved offset in the one-offset retrieval 							case. The blue curve shows the median retrieved model spectrum, while 							the medium- and lighter-blue contours denote the 1σ and 2σ intervals, 							respectively. Yellow points correspond to the median spectrum binned to 							match the observations. The prominent molecules responsible for the 							features in different spectral regions are labeled.
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Retrieved posterior probability distributions for the mixing ratios of 							important molecules for the three retrieval cases described in Section 								3. The horizontal 							error bar in the top row denotes each distribution’s median and 							corresponding 1σ interval for the three 							molecules with significant detections. The arrows in the bottom row 							indicate 95% upper limits. We find strong evidence for CH4 							and CO2, at a significance of 5σ and 3σ, respectively. We 							find marginal evidence for DMS and no significant evidence for the 							remaining molecules. The abundance estimates and detection significances 							are shown in Table 2.
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: HST and JWST observations of K2-18 b. The black points show prior 							observations of K2-18 b obtained with HST WFC3 in the 1.1–1.7 μm range, with data from eight transits, 							presented by Benneke et al. (2019b) using data from HST GO 13665 and GO 14682 programs 							(PI: B. Benneke). The orange and dark-red points show our JWST NIRISS 							and NIRSpec observations from one transit each. The data are binned for 							visual clarity to R 							﹩\approx ﹩ 25 and R 							﹩\approx ﹩ 55, respectively, as shown in Figure 3. The dark-blue line 							denotes the median retrieved spectrum (one-offset case), while medium- 							and lighter-blue regions denote the 1σ and 								2σ contours, respectively. The yellow 							points correspond to the median spectrum binned to match the JWST 							observations. Our JWST NIRISS spectrum is in agreement with the HST WFC3 							spectrum for most of the common wavelength range except for two data 							points toward the blue end of the WFC3 band.
Paper: Carbon-bearing Molecules in a Possible Hycean Atmosphere
Authors: Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses
Figure caption: Left: white light curve for the transit of K2-18 b observed with NIRISS 							SOSS. The blue contour shows the 1σ model 							interval. We find evidence of a spot occultation at the start of the 							transit. The bottom panel shows the residuals after subtracting the 							median model. The standard deviation of the residuals is measured to be 							115 ppm, which is 2.2× the expected noise level. The blue line is shown 							to indicate zero. Right: the top panel shows the normalized 							spectroscopic light curves (binned in wavelength for visual clarity). 							The bottom panel shows the transit depth precision obtained from the 							light-curve fitting, binned at two pixel columns per light curve.