adsabs/AstroCLIMB huggingface dataset:
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: B-field orientation and polarization maps of the FIR and submillimeter polarimetric observations of starburst galaxies. The polarized intensity (colormap in log-scale) maps of the starburst galaxies M8˙2 (left-hand), NGC 2146 (middle), and NGC 253 (right-hand) for the FIR (53 − 214 μm; rows 1–4) and submillimeter (850 and 890 μm; last row) polarimetric observations (top of each panel) are displayed. The B-field orientation of the disk (white lines) and outflow (yellow lines) with their lengths proportional to the polarization fraction are displayed. Only polarization measurements with PI/σ PI ≥ 2, P ≤ 20%, and I/σ I ≥ 60 are displayed. The contour levels start at ﹩{\mathrm{log}}_{10}{PI}=3{\sigma }_{\mathrm{PI}}﹩ and increase in steps of 0.2. A legend showing the physical scale of the image is shown in each panel.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: B-field orientation and polarization maps of the FIR and submillimeter polarimetric observations of starburst galaxies. The total intensity (colormap in log-scale) maps of the starburst galaxies M 82 (left-hand), NGC 2146 (middle), and NGC 253 (right-hand) for the FIR (53–214 μm; rows 1–4) and submillimeter (850 and 890 μm; last row) polarimetric observations are displayed. The B-field orientation of the disk (white lines) and outflow (yellow-black lines) with their lengths proportional to the polarization fraction are displayed. Only polarization measurements with PI/σ PI ≥ 2, P ≤ 20%, and I/σ I ≥ 60 are displayed. The contour levels start at ﹩{\mathrm{log}}_{10}I=0﹩ and increase in steps of 0.5. Each panel shows the legends of the physical scale, a 5% polarization fraction, and the beam size (red circle).
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Total and polarized SEDs of the full starburst, and only disk and outflow regions. The total (λ I  ν ;  dashed lines and filled symbols; top panels) and polarized (λ PI  ν ;  dashed lines and open symbols; bottom panels) SEDs for the full galaxy (left-hand), disk (middle), and outflow (right-hand) are shown. The best fit (solid line) and 1σ uncertainty (shadowed region) of the modified blackbody functions with their characteristic dust temperature, mass, and β are shown in each panel.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: B-field morphology of the starburst galaxies studied in this work. The B-field orientation (streamlines) using SOFIA/HAWC+ at 89 μm are displayed over a combination of optical and infrared images. Each panel shows the physical scale of 1 kpc. Credits: M 82: NASA/SOFIA/E. Lopez-Rodriguez and L. Proudfit; NASA/Spitzer/J. Moustakas et al.; NGC 253: ESO and NASA/SOFIA/E. Lopez-Rodriguez and L. Proudfit; NGC 2146: ESA/Hubble & NASA/E. Lopez-Rodriguez and L. Proudfit.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: Left: mock photometry of UVISTA 174150 generated with MAP SFH pushed back by 0 Gyr (blue), 0.5 Gyr (green), 1 Gyr (orange), and 2 Gyr (red). Each colored line shows the mock SED generated with each SFH. We assume the same signal-to-noise ratio of the photometric measurements for each filter used in the UVISTA survey and generate mock noise, shown as error bars. The magenta points are the photometric data provided by the UVISTA catalog. Right: MAP SFH of UVISTA 174150 pushed back to account for passive evolution (the same color code used as for the left panel). The oldest bins are removed to assume the same observed epoch/redshift.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Histograms of the B-field orientation of the outflow and disk of starburst galaxies. The histograms of the B-field orientation of the outflow (blue) and disk (red) in 10° bins, as well as, the PA B,− and PA B,+ from Equation (3) are shown. The spatial location of the polarization measurements associated with the outflow and disk are shown in Figure 2.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: SFHs from the Prospector fitting on mock photometry generated with the SFH shifted back by 0 Gyr (blue), 0.5 Gyr (green), 1 Gyr (orange), and 2 Gyr (red). The dashed line shows the input SFH used to generated the mock photometry, and the solid line is the MAP distribution from the Prospector fit on the mock photometry. The shaded regions include 95% of the posterior distribution.
Paper: The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Enrique Lopez-Rodriguez
Figure caption: Histograms of the polarization fraction of the outflow and disk of starburst galaxies. We use the polarization fraction of the outflow (blue) and disk (red) from the same regions shown in Figures 2 and 4. The histograms are computed in 0.5% bins. The median and 1σ dispersion of the histogram are shown in each panel.
Paper: Continuum Reverberation Mapping of Mrk 876 over Three Years with Remote Robotic Observatories
Authors: Jake A. Miller, Edward M. Cackett, Michael R. Goad, Keith Horne, Aaron J. Barth, Encarni Romero-Colmenero, Michael Fausnaugh, Jonathan Gelbord, Kirk T. Korista, Hermine Landt, Tommaso Treu, Hartmut Winkler
Figure caption: A comparison of the time lags found using PyROA, JAVELIN and PyCCF. The wavelengths have been redshift corrected. The solid black line is the best-fitting ﹩\tau ={\tau }_{0}[{(\lambda /{\lambda }_{0})}^{\beta }-{y}_{0}]﹩, with β fixed to 4/3 while τ 0 and y 0 are free. The red dashed line represents the a = 0.998 analytic prescription for time lags as described by Kammoun et al. (2021b). This fit allows only the X-ray corona height (H) to be a free parameter, while black hole mass, X-ray luminosity, and mass accretion rate (﹩\dot{m}﹩) are fixed. When (﹩\dot{m}﹩) is allowed to be a free parameter, the fit becomes unconstrained for both spin cases. For more details, see Section 3.2.
Paper: Continuum Reverberation Mapping of Mrk 876 over Three Years with Remote Robotic Observatories
Authors: Jake A. Miller, Edward M. Cackett, Michael R. Goad, Keith Horne, Aaron J. Barth, Encarni Romero-Colmenero, Michael Fausnaugh, Jonathan Gelbord, Kirk T. Korista, Hermine Landt, Tommaso Treu, Hartmut Winkler
Figure caption: Flux–flux analysis on the base data set of Mrk 876. (a) Fluxes corrected for redshift and Galactic extinction, in mJy, for each filter. Data points are black, while the colored lines are the model (as described by Equation (4)) overlaid. (b) The flux–flux analysis, with each band having the same colors as shown in (a). X  G  is where the first band’s lower uncertainty crosses the x-axis, which in this case is the u band. This is done so that a value for the constant component can be measured for this band. (c) Maximum (in blue), average (in teal), and minimum (in purple) flux values for each filter. rms values calculated from Equation (4) are given in black. The red dashed line is a f  ν  ∝ λ −1/3 fit to the rms values. The solid orange line labeled “const.” is the constant contribution for the fluxes, measured by where each filter’s line crosses X  G . The values for each filter are listed in Table 6.
Paper: Continuum Reverberation Mapping of Mrk 876 over Three Years with Remote Robotic Observatories
Authors: Jake A. Miller, Edward M. Cackett, Michael R. Goad, Keith Horne, Aaron J. Barth, Encarni Romero-Colmenero, Michael Fausnaugh, Jonathan Gelbord, Kirk T. Korista, Hermine Landt, Tommaso Treu, Hartmut Winkler
Figure caption: The combined light curves of Mrk 876. The CCF is found for each light curve, measured with respect to the g band. The dashed line is at 0 days, and the solid and dotted lines show the PyCCF lag and corresponding uncertainties.
Paper: Continuum Reverberation Mapping of Mrk 876 over Three Years with Remote Robotic Observatories
Authors: Jake A. Miller, Edward M. Cackett, Michael R. Goad, Keith Horne, Aaron J. Barth, Encarni Romero-Colmenero, Michael Fausnaugh, Jonathan Gelbord, Kirk T. Korista, Hermine Landt, Tommaso Treu, Hartmut Winkler
Figure caption: A comparison between the different boxcar detrending widths used and the resultant time lags found using PyCCF. A detrending width of 100 days was chosen due to having the smallest overall uncertainties, and it is shown here as the points with green stars. Widths from 75 to 175 agree to the lags found within uncertainty for all bands. The lags with uncertainties can be found in Table 2. All points have been fitted using the standard ugriz bands, but they have been spatially adjusted on this figure for clarity.
Paper: Continuum Reverberation Mapping of Mrk 876 over Three Years with Remote Robotic Observatories
Authors: Jake A. Miller, Edward M. Cackett, Michael R. Goad, Keith Horne, Aaron J. Barth, Encarni Romero-Colmenero, Michael Fausnaugh, Jonathan Gelbord, Kirk T. Korista, Hermine Landt, Tommaso Treu, Hartmut Winkler
Figure caption: The combined light curves of Mrk 876, detrended by subtracting a moving boxcar average of 100 days. The CCF is displayed following the same format as Figure 1.
Paper: Continuum Reverberation Mapping of Mrk 876 over Three Years with Remote Robotic Observatories
Authors: Jake A. Miller, Edward M. Cackett, Michael R. Goad, Keith Horne, Aaron J. Barth, Encarni Romero-Colmenero, Michael Fausnaugh, Jonathan Gelbord, Kirk T. Korista, Hermine Landt, Tommaso Treu, Hartmut Winkler
Figure caption: Spectra taken on 2019 July 2 of Mrk 876. The data are shown in black, while the fitted model, containing both a continuum and multiple Gaussian and Lorentzian components, is in orange. The dotted line is the throughput of the u, g, r, and i bands. We only find significant emission line contribution from the Hα line present in the i band. The exact contribution from the continuum and emission lines can be found in Table 5.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: (a) Triangulated trajectory of the prominence apex with the PFSS magnetic field lines. White magnetic field lines are closed and blue ones are open lines of positive polarity. Rainbow-colored dots show the prominence triangulation in EUVI images. Black, violet, pink, and beige dots are triangulated in COR1 images at 10:45, 10:55, 11:05, and 11:15 UT, respectively. In purple, the radial direction according to the initial position of the prominence, with markers separated by 0.2 R ☉. In light blue, the plane where the trajectory lies, the pink circle shows the intersection of this POE and solar surface, the teal circle represents the equator. Magnetic structures PS1, PS2, AR, and CH idem Figure 1. (b) Rotated position of the eruption and magnetic field lines. Cartesian axes defined from the POE. (c) Radial magnetic field B  r  at 1 R ☉ in gray scale with isocontours of magnetic field strength in purple shades. The spots of stronger purple show the 3D location of the minimum magnetic field. The magnetic field lines are plotted in blue (open) and white (closed), also the position of the preeruptive filament (light pink line), and the pink circle showing the POE projection over the surface of the plane. The magnetic structures are the same as in panel (a).
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: Magnetic field magnitude (logarithmic scale) and field lines with the prominence and CME trajectory in the POE. The gray star indicates the null point position of PS2. Rainbow-colored dots correspond to the triangulated positions of the prominence with the same timescale as Figure 4 and the last larger red dot being the black one used in Figure 4. White to gray circles represent the cross sections of the nonradial GCS model from 9:25–11:20 UT, and color dots with the same white/gray edges represent the centers of each cross section, up to 10:45 UT.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: (a) Source region and preeruptive filament (pink arrows) seen by STA on 2008 April 7. The white square indicates the AR as in the right panel. (b) Preeruptive filament (pink arrow) seen by STA on 2008 April 9 hours before the eruption, PS1 is located behind the limb (orange arrow), the CH is seen as a dark patch, and some field lines of PS2 (violet arrow) are possibly seen at the limb. (c) Radial magnetic field B  r  at 1 R ☉ in gray scale, open (blue) and closed (white) field lines, the position of the preeruptive filament (pink line) and the magnetic structures surrounding the source region. The white square indicates AR 10989, the pseudostreamers are indicated by circles (in orange PS1, in violet PS2), and the southern CH is delimited by blue dashed lines.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: 2008 April 9 event in STEREO 171, 195, and 304 Å filters at 09:56 UT. Rainbow-colored dots represent the apex position of the prominence from 8:25 UT (violet dot) to 10:40 UT (red dot), triangulated in EUVI images. The left panels show STB FOV, dots with the black center are behind the limb and are triangulated with SOHO/EIT; the right panels show STA FOV. Panel (b) indicates also the prominence position with the pink arrow, and the CME front in white dashed lines.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: Normalized magnetic gradient pressure (﹩{\tilde{G}}_{x}﹩) and normalized acceleration (﹩{\tilde{a}}_{x}﹩) in the x-direction during the observed interaction between the MFR and the CH.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: 2008 April 9 event in STA, SOHO, and STB in the 195 Å filter (left) and coronagraph (right) images. Images are processed with base difference. Color dots represent the position of the CME center from 9:25 UT (violet dot) to 11:45 UT (yellow dot). The GCS reconstruction at 10:05 UT (magenta wire frame) and its central cross section (white circle) is plotted over the 195 images. The cross sections (gray circles) of the GCS reconstruction and centers (color dots) from 9:25–11:45 UT are overplotted on the coronagraph composites in the right panels.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: Angle of misalignment between the magnetic gradient and trajectory (G-T), and the magnetic field and trajectory (B-T). The gray dashed line indicates the height at which the PS spine is crossed.
Paper: Understanding the Deflection of the “Cartwheel CME”: Data Analysis and Modeling
Authors: Abril Sahade, Angelos Vourlidas, Laura A. Balmaceda, Mariana Cécere
Figure caption: Background magnetic field magnitude and lines of the simulated case. The turquoise dot indicates the initial position of the FR, and the gray star indicates the observed PS null point position. The MFR cross section and center are represented by white/gray-scaled circles and blue-scaled dots, respectively.
Paper: Data-constrained 3D Modeling of a Solar Flare Evolution: Acceleration, Transport, Heating, and Energy Budget
Authors: Gregory D. Fleishman, Gelu M. Nita, Galina G. Motorina
Figure caption: (a) Evolution of the plasma temperature in flux tubes I (red) and II (green). The dotted green segment replicates the dotted segment in Figure 8. The dark green line shows the result obtained from the RHESSI OSPEX fit (see Figure 8). The thin red line shows temperature obtained for flux tube I from AIA EM maps (see Figure 8). For the reference, the thin black line shows a conveniently scaled impulsive HXR emission peak recorded by Konus–Wind. (b) Composite evolution of the thermal energy computed for flux tubes I (red) and II (green). The solid portions of the lines show the time range, when the model is constrained by both AIA and RHESSI data starting 06:45:06 UT. Dashed segments show estimates of W obtained using the number density derived from adjustment of the model to AIA EM maps and temperatures derived from the AIA temperature maps directly (shown in Figure 8). The green dotted segment uses the number density derived from adjustment of the model to the AIA EM maps and the temperature shown by the dotted green segment in panel (a). The black line shows the evolution of the total thermal energy obtained by adding up the contributions from both loops. The dashed blue line shows cumulative deposition of the nonthermal energy computed using the injection function determined in Section 3.2.
Paper: Data-constrained 3D Modeling of a Solar Flare Evolution: Acceleration, Transport, Heating, and Energy Budget
Authors: Gregory D. Fleishman, Gelu M. Nita, Galina G. Motorina
Figure caption: Evolution of the spatial peak thermal density (a) and volume-integrated EM (b) in flux tubes I (red colors) and II (green colors). (a) Dark thin lines show the number densities inferred from the model adjusting to AIA EM maps. The green thick line shows the number density in flux tube II obtained from adjusting X-ray RHESSI spectra. The red thick line shows the number density values used to match the X-ray spectra; these values are close to those shown in dark red but shifted to the closest RHESSI time stamp (as the RHESSI and AIA cadences do not match each other). (b) Volume-integrated EM obtained from the AIA EM map match for flux tube I and from the RHESSI spectral match for flux tube II. For the reference, the thin black line shows a conveniently scaled impulsive HXR emission peak recorded by Konus–Wind.
Paper: Data-constrained 3D Modeling of a Solar Flare Evolution: Acceleration, Transport, Heating, and Energy Budget
Authors: Gregory D. Fleishman, Gelu M. Nita, Galina G. Motorina
Figure caption: Evolution of the plasma temperature inferred from the data. The dark green line is the larger temperature (T 2), and the dark red one is the smaller one (T 1) from the two-thermal-component RHESSI spectral fit reported by Fleishman et al. (2021). The RHESSI record started at 06:45:06 UT; the dotted dark green line shows implied temperatures obtained from linear extrapolation of RHESSI data to the earlier time. The red and green lines show mean temperatures over valid pixels in the AIA DEM-weighted temperature maps inside two boxes covering portions of flux tubes I and II (shown in Figure 7). For the reference, the thin black line shows a conveniently scaled impulsive HXR emission peak recorded by Konus–Wind.
Paper: Data-constrained 3D Modeling of a Solar Flare Evolution: Acceleration, Transport, Heating, and Energy Budget
Authors: Gregory D. Fleishman, Gelu M. Nita, Galina G. Motorina
Figure caption: Plasma temperature distribution obtained for time interval 06:46:37–06:46:49 UT inferred from the DEM map (Fleishman et al. 2021). Red and green boxes, respectively, show the areas over which the mean temperatures of flux tubes I and II were evaluated. Only “valid” pixels, where the thermal energy estimated in Fleishman et al. (2021) is above 20% of its peak value, are taken into account.
Paper: ACA CO(J = 2–1) Mapping of the Nearest Spiral Galaxy M33. I. Initial Results and Identification of Molecular Clouds
Authors: Kazuyuki Muraoka, Ayu Konishi, Kazuki Tokuda, Hiroshi Kondo, Rie E. Miura, Tomoka Tosaki, Sachiko Onodera, Nario Kuno, Masato I. N. Kobayashi, Kisetsu Tsuge, Hidetoshi Sano, Naoya Kitano, Shinji Fujita, Atsushi Nishimura, Toshikazu Onishi, Kazuya Saigo, Rin I. Yamada, Fumika Demachi, Kengo Tachihara, Yasuo Fukui, Akiko Kawamura
Figure caption: Virial parameter α as a function of the 12CO luminosity-based mass (M CO). The filled area in blue indicates 1 ≤ α ≤ 3, in which clouds are in virial equilibrium. Red dots indicate high-S/N clouds and open squares indicate low-S/N clouds.
Paper: ACA CO(J = 2–1) Mapping of the Nearest Spiral Galaxy M33. I. Initial Results and Identification of Molecular Clouds
Authors: Kazuyuki Muraoka, Ayu Konishi, Kazuki Tokuda, Hiroshi Kondo, Rie E. Miura, Tomoka Tosaki, Sachiko Onodera, Nario Kuno, Masato I. N. Kobayashi, Kisetsu Tsuge, Hidetoshi Sano, Naoya Kitano, Shinji Fujita, Atsushi Nishimura, Toshikazu Onishi, Kazuya Saigo, Rin I. Yamada, Fumika Demachi, Kengo Tachihara, Yasuo Fukui, Akiko Kawamura
Figure caption: Same as Figure 15, but using the 8 μm flux without diffuse components.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Section of the spectrum dominated by the self-reversed wind lines. The wind spectrum appears stronger in the noncoronal γ Cru (bottom). However, γ Dra (top) has a smaller angular diameter, and our calculations indicate that the chromosphere is more powerful in the hybrid star. The bottom figure compares the ASTRAL spectrum (solid) recorded in 2011 with the GHRS spectrum (dashed–dotted) from 1994. The wind signatures have increased significantly between the two observations.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Comparison of the derived line surface flux for γ Cru and γ Dra Fe II spectra (top). The flux ratio indicates a stronger chromosphere in the hybrid object γ Dra. The bottom panel shows that the surface flux from 1994 (GHRS) was about half of what is measured in 2011 (ASTRAL). The comparison is based on fewer measured lines due to the GHRS spectrum’s limited wavelength coverage. The dashed lines represent the average surface flux ratio of 0.67 (top) and 0.53 (bottom).
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: The SEI fits of Fe II lines in γ Cru for a range of excitation potentials. The observed spectrum (solid) is compared to the modeled profile (dashed). The dotted line is the profile at the base of the chromosphere. The lines are consistently well fit with β = 0.7.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: The SEI fits of Fe II lines in γ Dra for a range of excitation potentials. The observed spectrum (solid) is compared to the modeled profile (dashed). The dotted line is the profile at the base of the chromosphere. The lines are consistently well fit with β = 0.35.