adsabs/AstroCLIMB huggingface dataset:
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Distribution functions of the pairs (blue) and the ions (orange) for both the uncooled (a) and the strongly cooled (b) simulations. The dashed lines show parts of the distributions contributed by the particles having experienced E > B during their lifetime in the sheet. The inset panels show the distribution of energy gains, Δγ, of particles during their contiguous presence in these regions. The nonideal electric field in the X-points only accelerates particles to Lorentz factors of a fraction of σ. At the same time, this process is essential to promote the particles (pairs and ions) for further acceleration up to the highest energies: in relativistic outflows along the layer and the large-scale reconnection electric field upstream. As a result, the high-energy tail of the spectrum is fully formed by the particles passed through E > B.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Time evolution of the reconnection rate in simulations with different cooling regimes. Measured rates are of order β rec ≈ 0.06...0.14, and are systematically larger for the case of strongest cooling, γ syn/σ = 0.2.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Volume rendering of the plasma density in the current sheet with weak (a) and strong (b) cooling at t ∼ 2.2L  x /c. Magnetic field lines are also displayed, with the color representing the strength, ∣ B ∣. From the field lines, one can easily identify the nonideal regions—the X-points (selected ones are shown by blue arrows)–where the magnetic field vanishes (this corresponds to regions where the field lines are blue). The sizes of the plasmoids (selected ones shown by green arrows) are significantly different in these two simulations, with the strong cooling run displaying smaller structures and larger compression (note that the colorbars for the two plots have different scales).
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Distribution functions of pairs (dashed) and ions (solid) in simulations containing a different fraction of ions, f  i  = n  i /n up = 1%,  10%,  49% (panels (a)–(c)), and different mass ratio m  i /m  e  = 5,  25 (panel (d)). As long as the mass density fraction of ions is relatively small, n  i  m  i /(n  e  m  e ) ≪ 1 (which is not the case in panel (c)), the power-law index of their distribution is insensitive to either f  i , or the m  i /m  e . The x-axis of panel (d) is normalized by the mass of the particles.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Spatial distribution of regions producing the synchrotron radiation shown together with the total plasma density for the same snapshots as in Figure 1. Green volume rendering corresponds to the total synchrotron intensity, while the blue one shows the emission intensity above the burnoff limit, ε  c . Panel (a) corresponds to the weak cooling, while panel (b) corresponds to the strong cooling. The emission in the strongly cooled current sheet is mainly associated with the peaks of the RDKI and the outer shells of the plasmoids (both for the total emission and the emission above the burnoff). The much fainter emission from the weakly cooled current sheet (note the difference in color scales between the two regimes) is significantly more uniform, with the emission above the burnoff being essentially absent.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Estimates for burnoff limit of protons, ﹩{\gamma }_{\mathrm{syn}}^{i}﹩, (blue lines) and the Lorentz factor of protons accelerated in the full potential drop near the light cylinder, ﹩{\gamma }_{\max }^{i}﹩, (red lines) for the pulsars in the ATNF catalog. Axes correspond to the rotation period of the star, P ⋆, and the magnetic field strength near the surface of the star. The shaded region corresponds to the regime, when the synchrotron cooling of protons becomes dynamically important: ﹩{\gamma }_{\max }^{i}\gt {\gamma }_{\mathrm{syn}}^{i}﹩. Evidently, for all of the observed pulsars, the radiation drag of ions is negligible in the context of ion acceleration.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Angular anisotropy of the radiation at different photon energies for different cooling regimes. The angle is measured with respect to the direction of the upstream magnetic field ﹩{{\boldsymbol{B}}}_{\mathrm{up}}\equiv {B}_{x}\hat{{\boldsymbol{x}}}﹩. In the weak cooling case, γ syn = 5σ, emission above the burnoff limit is significantly suppressed, and most of the high-energy photons are emitted perpendicular to the upstream magnetic field. However, in the strong cooling regime, most of the high-energy photons above the burnoff limit are emitted along the upstream magnetic field.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Normalized flux density of the emitted radiation for different cooling regimes. The additional panel shows the position of the exponential cutoff of the spectra as a function of the cooling strength. Current sheets with stronger cooling produce a more extended emission spectrum, with significant power above the burnoff limit, ε c, and a cutoff being in good agreement with the prediction of Equation (8): ε cut ∼ ε c(σ/γ syn). However, current sheets with weak cooling produce almost no emission above the burnoff limit.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Comparison of 2D plasma density slices ((a) and (b)) and normalized particle distributions ((c), and(d)) for different numerical resolutions d  e /Δx = 1,  3. Dark and bright lines correspond to ions and pairs, while blue and orange correspond to high- and low-resolution runs. The acceleration mechanisms, the statistics of the energy gains in E > B regions, and thus the resulting distributions are largely insensitive to numerical resolution. However, the compression of plasmoids is somewhat smaller for the low-resolution run.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: The effective perpendicular magnetic field, ﹩{\tilde{B}}_{\perp }﹩, experienced by the pairs of different energies, γ. The 2D histograms are shown for all the cooling regimes, from weak, γ syn/σ = 5, to strong, γ syn/σ = 0.1. The red-dashed lines show the estimated critical magnetic field, ﹩{\tilde{B}}_{\perp }\gamma ={B}_{\mathrm{up}}{\gamma }_{\mathrm{syn}}﹩. Notably, the acceleration of the highest-energy pairs is inhibited by the synchrotron cooling and, as a result, most of the pairs do not cross the critical line.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Distribution of the lifetimes of strongly cooled pairs at high energies (γ ≳ 2γ syn and γ ≳ σ) for different sizes of the simulation domain. For both thresholds, the lifetime is close to one gyro-period of the most energetic particles, ﹩{r}_{L}^{\mathrm{up}}(\sigma )/c﹩ and, importantly, is independent of the domain size.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Atomic diffusion correction. Top left: CMD of all stars with HST photometry colored by their metallicity. Top right: a grid of the median metallicity correction when considering isochrones that model atomic diffusion. Bottom: CMD of all stars from the top left panel, now with the relevant atomic diffusion correction applied. Stars with S/N < 10 and less reliable photometry are plotted with transparency in each panel.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Comparison to literature values. On the left is the [Fe/H] distribution for Johnson & Pilachowski (2010), Johnson et al. (2020), the black solid line, and from the MUSE results, the black dashed line, for all the matched stars in both catalogs. In red is the [M/H] distribution for the matched stars of the Mészáros et al. (2021) data, solid line, and the MUSE data. On the right, we plot the literature values against the difference between the two [Fe/H] or [M/H] values. The black dashed line indicates where both values agree.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: The discrepancy between spectral parameters with free and fixed log(g). (a) The one-to-one comparison between the [M/H] values, the red line as the 1 to 1 ratio. (b)–(e) The σ deviations for [M/H], vlos, T eff, and log(g). We divide the difference between the two results with the scale error in our catalog, except for the log(g), where we take the SPEXXY error for the free log(g) run. The dashed red line is at 0, the solid red lines are at the 3σ limits, and the orange solid line is the median of all stars, while the red shaded area is the S/N limit of 10.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: [M/H] of RGB vs. MSTO post AD correction. The figure shows how the atomic diffusion correction causes the [M/H] distribution to be more consistent between the MSTO and the RGB (when considering both to have MSTO-like errors).
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: S/N test. The left plot shows on the y-axis the σ difference between the original result and the different [M/H] results after adding noise to the spectra, and the x-axis is the new S/N with the added noise. Similar for the right plot but for the vlos values. The light red shaded areas indicate S/N below 10, the red solid horizontal lines are the 3σ difference, the red dashed horizontal lines are at 0, and the orange solid lines are the median values for our measurements as a function of S/N.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Metal rich. On the left plot, the one-to-one comparison of the [M/H] is shown, with the red solid line being the 1 to 1 ratio. On the right is the difference in log(g) between the two isochrones, with the dashed line indicating no difference at all, the orange line the median difference of our data, and the red shaded area the S/N limit of 10.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Literature comparison log(g). We plot the literature values against the difference between the literature and our log(g) values.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: Perspective rotation. The figure shows the position of the data color coded with the perspective rotation value for each star. The red cross indicates the center, and the velocity values increase from the bottom left to the top right corner of the plot.
Paper: oMEGACat. I. MUSE Spectroscopy of 300,000 Stars within the Half-light Radius of ω Centauri
Authors: M. S. Nitschai, N. Neumayer, C. Clontz, M. Häberle, A. C. Seth, T.-O. Husser, S. Kamann, M. Alfaro-Cuello, N. Kacharov, A. Bellini, A. Dotter, S. Dreizler, A. Feldmeier-Krause, M. Latour, M. Libralato, A. P. Milone, R. Pechetti, G. van de Ven, K. Voggel, Daniel R. Weisz
Figure caption: S/N in the catalog. The CMD of the stars in the catalog color coded with their S/N as calculated from SPEXXY.
Paper: Tracing the Total Stellar Mass and Star Formation of High-redshift Protoclusters
Authors: Roxana Popescu, Alexandra Pope, Kyoung-Soo Lee, Stacey Alberts, Yi-Kuan Chiang, Sowon Lee, Mark Brodwin, Jed McKinney, Vandana Ramakrishnan
Figure caption: Input vs. measured FWHMs of simulated protocluster stacks are shown in orange. A one-to-one relation is shown in blue while the red vertical line indicates the FWHM of the Planck beam. The solid gray horizontal line marks the measured FWHM from our data. The vertical dashed line and the shaded region, both in gray, show the range of the inferred protocluster size after correcting for the broadening effect.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: Relations between the escape fraction (f esc,m and f esc,c) and other galaxy properties, including Lyα emission line luminosity and EW, M UV, SFR, and UV slope β. The solid circles represent the five individual LyC galaxies, and the empty ones are the two possible detections. The triangles represent the upper limits from the stacked images for nondetections in U J. For Lyα emission and EW, the triangles show their median values (see Table 1).
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: SED modeling of LAE3 and the composite SED. In each panel, the purple circles with error bars represent observed broadband photometry, the black spectrum is the best-fit model, and the red dots are the photometry from the best-fit model. The green curve is the best-fit model without correction for the IGM absorption. We have excluded the Lyα emission line in the fitting process.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: Five LyC galaxies in the V, narrowband (NB497 or NB503), and U J bands. Nearby objects in the U J images have been modeled and subtracted. The size of the images is 8″ × 8″. The red circles in the third column are the aperture used for photometry.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: Example of our measurement of the Lyα and continuum emission. The red dots show the photometric data points and the horizontal bars indicate their wavelength coverages. The solid line is the best-fit model that combines the Lyα and continuum emission.
Paper: Lyman Continuum Emission from Spectroscopically Confirmed Lyα Emitters at z ∼ 3.1
Authors: Yuchen Liu, Linhua Jiang, Rogier A. Windhorst, Yucheng Guo, Zhen-Ya Zheng
Figure caption: Median stack of the five LyC candidates in the U J band. The image size is 13.″5 × 13.″5. Nearby objects have been subtracted. The right panel is a smoothed image.
Paper: X-Ray Spectral Variations of Circinus X-1 Observed with NICER throughout an Entire Orbital Cycle
Authors: Mayu Tominaga, Masahiro Tsujimoto, Ken Ebisawa, Teruaki Enoto, Kimitake Hayasaki
Figure caption: Spectra (black) and best-fit model in the top panels and residuals to the fit in the bottom panels for the six snapshot spectra representing the dip ((a) and (b)), flaring ((c), (d), and (e)), and stable ((f)) phases. Different colors are used for different model components: red for total, cyan for covered disk blackbody, blue for uncovered disk blackbody, orange for Gaussian models, and green for soft excess. The insets give a close-up view of the energy bands with apparent spectral line features.
Paper: X-Ray Spectral Variations of Circinus X-1 Observed with NICER throughout an Entire Orbital Cycle
Authors: Mayu Tominaga, Masahiro Tsujimoto, Ken Ebisawa, Teruaki Enoto, Kimitake Hayasaki
Figure caption: Light curves of the NICER AO2 observation covering the orbital phase of 0.54–1.48 (top) and the MAXI observation of the preceding five cycles of the same phase in different colors (bottom). In the top panel, the Bayesian-blocked phase boundaries are shown with blue dashed lines, while the data used for the spectral analysis representing each phase are shown with red solid lines with their snapshot numbers. Three orange arrows show the short dips.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: The DM densities within each Latte CDM galaxy. The red arrow indicates the direction of the stellar minor axis. The blue arrows indicate the directions of the DM halo minor axis, with the lengths scaled to the radii at which the axes are determined. The dashed green inner circle indicates a radius of 100 kpc.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: 〈v  ϕ 〉/σ  v,ϕ  ratios for CDM+baryon galaxies. The vertical red line indicates the time when the thin disk becomes roughly assembled. The vertical black line indicates the time of the LMC analog pericenter. The reference frame is defined as the cylindrical principal axes, where the z-direction is defined by the minor axis of the moment of inertia of young stellar particles.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: Halo triaxiality as a function of time at different scale lengths. Each galaxy’s LMC pericenter is indicated with a vertical black line, and the time at which the disk is formed is shown with the vertical red line.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: Position of the LMC satellite (circle) relative to the galaxy (origin; in the principal/disk axis frame) and the direction of the galaxy’s major axis (crosshair, exaggerated scale). The color indicates the cosmic time at which the major axes and LMC positions were measured.
Paper: X-Ray Spectral Variations of Circinus X-1 Observed with NICER throughout an Entire Orbital Cycle
Authors: Mayu Tominaga, Masahiro Tsujimoto, Ken Ebisawa, Teruaki Enoto, Kimitake Hayasaki
Figure caption: Long-term light curve of Cir X-1 observed with the Ginga, RXTE, and MAXI all-sky monitors. Data points are sampled randomly for clarity. Vertical lines show the epochs of pointing observations with various X-ray telescopes.
Paper: Orientations of Dark Matter Halos in FIRE-2 Milky Way–mass Galaxies
Authors: Jay Baptista, Robyn Sanderson, Dan Huber, Andrew Wetzel, Omid Sameie, Michael Boylan-Kolchin, Jeremy Bailin, Philip F. Hopkins, Claude-André Faucher-Giguere, Sukanya Chakrabarti, Drona Vargya, Nondh Panithanpaisal, Arpit Arora, Emily Cunningham
Figure caption: The same as Figure 11, except with the axes fixed in the latest tracked reference frame of the disk.