adsabs/AstroCLIMB huggingface dataset:
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Size of torus (Rtor) as a function of 5100 Å luminosity for W1 (left) and W2 (right) for the merged sample. The black circles illustrate the sample from A. K. Mandal et al. (2024), while the red circles indicate the sample of this study. The blue solid line shows our best fit with a free slope, and the shaded regions represent the 1σ–3σ confidence intervals around the best fit. The purple lines show the regression results from A. K. Mandal et al. (2024), while the black dashed lines mark the best fit with a fixed slope of 0.5.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Comparison of lag measurements obtained using ICCF and MICA in the observed frame for WISE W1 (left) and W2 (right). Colors follow the same convention as in Figure 3. The shaded areas show ±1σint, ±2σint, and ±3σint intrinsic scatter around the one-to-one line, illustrating the agreement between the two methods.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: Examples of true lag detection probability as a function of input lag from Monte Carlo simulations for AGNs without measured lags. The green dashed line indicates the expected lag from the dust size–luminosity relation assuming a slope of 0.5.
Paper: Scaling Relations of the Dusty Torus with Luminosity and the Broad-line Region
Authors: Ashraf Ayubinia, Jong-Hak Woo, Shu Wang, Amit Kumar Mandal, Donghoon Son
Figure caption: The same as Figure 1, showing lag analysis for PG 1322+659, an example from the SAMP sample.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Terminal velocity v∞,dust of a radiation-driven superwind, accelerated by a cluster with radius Rc, mass M*, and M*/L* ratio of Mrk 71-A, assuming dust opacity κ = 103 cm2 g−1 (Equation (1)). We limit the displayed cluster parameter combinations to those that do not exceed the maximum stellar density Σ < 105M⊙ pc−2.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Power-law [O III]λ5007 fits for galaxies classified with power-law wing morphologies. The blue- and red-wing fits are shown with their corresponding colors, and the respective best-fit slopes are shown in the legend. The red wing is arbitrarily offset on the y-axis for display purposes. The best-fit local continuum is shown as a gray dashed line, and the maximum wing velocity ﹩{V}_{{\rm{Max}}}﹩ is shown as dashed–dotted brown lines.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Blue slope αblue vs. r90,Lyα/r20,Lyα for objects with measured power-law wing slopes. The symbols indicate the wing morphology as shown in the legend, and the points are color-coded by EW(Hβ).
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption: Multi-Gaussian [O III]λ5007 fits for the four galaxies classified as showing Gaussian wing morphologies. The Gaussian parameters are indicated in the legends with the following units: amplitudes A in 10−15 erg s−1 cm−2 Å−1, centroids V0 and widths σ in km s−1. The best-fit local continuum is shown as a gray dashed line, and the maximum wing velocity ﹩{V}_{{\rm{Max}}}﹩ is shown as dashed–dotted brown lines.
Paper: Power-law Emission-line Wings and Radiation-driven Superwinds in Local Lyman Continuum Emitters
Authors: Lena Komarova, M. S. Oey, Rui Marques-Chaves, Ricardo Amorín, Alaina Henry, Daniel Schaerer, Alberto Saldana-Lopez, Alexandra Le Reste, Claudia Scarlata, Matthew J. Hayes, Omkar Bait, Sanchayeeta Borthakur, Cody Carr, John Chisholm, Harry C. Ferguson, Vital Gutierrez Fernandez, Brian Fleming, Sophia R. Flury, Mauro Giavalisco, Andrea Grazian, Timothy Heckman, Anne E. Jaskot, Zhiyuan Ji, Göran Östlin, Laura Pentericci, Swara Ravindranath, Trinh Thuan, Jose M. Vílchez, Gabor Worseck, Xinfeng Xu
Figure caption:  ﹩{V}_{{\rm{Max}}}﹩ vs. Lyα halo fraction (see the text). The points are color-coded by wing morphology.
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: I-band TFR of the FGLR galaxies using FGLR distance moduli for the calculation of absolute magnitudes. The green line corresponds to the zero-point obtained with these galaxies. The pink dashed line is the old regression from Figure 1. The galaxy in gray is NGC 3109. As in the work by R. B. Tully & H. M. Courtois (2012), it is not used for the zero-point fit.
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: I-band TFR of the R. B. Tully & H. M. Courtois (2012) zero-point calibration sample. The galaxies shown in red are the subsample for which we have determined FGLR distances.
Paper: Blue Supergiants and the Zero-point of the Tully–Fisher Relation: A Path to a New Independent Test of the Hubble Constant
Authors: Rolf-Peter Kudritzki, Fabio Bresolin, Miguel A. Urbaneja, Eva Sextl
Figure caption: Distance moduli obtained with the FGLR method versus the distance moduli used in R. B. Tully & H. M. Courtois (2012).
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Multispacecraft measurements of event #7. (a) Wind/WAVES dynamic radio spectrogram. Color-coding indicates electric field intensity (dB above background). The vertical black arrow marks the type III radio burst associated with the event; the subsequent slow-drifting feature corresponds to a type II burst. The locations of STEREO-A (A), STEREO-B (B), and near-Earth (E) spacecraft (Wind, SOHO) at the time of the type III burst are shown in HEE X–Y coordinates next to panel (a). The tilted arrow indicates the flare longitude (W47). (b) 2 hr proton intensities from STEREO-B/HET, STEREO-A/HET, and SOHO/ERNE in the indicated energy ranges. (c) 1 hr ion intensities from ACE/ULEIS in the 0.23–0.32 MeV nucleon−1 energy range. (d) Mass versus time spectrogram from ACE/ULEIS covering 0.4–10 MeV nucleon−1. (e) Inverse ion speed versus arrival time for ions with mass 10–70 AMU. Slanted lines indicate expected arrival times for scatter-free propagation along a nominal Parker spiral path of 1.2 au. The magenta polygon marks the region, defined in inverse speed–time space, over which elemental abundance ratios were calculated.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Left: element abundances relative to O for events #1, #2, #4, and #12 in this study (blue shaded triangles). Right: survey-averaged elemental abundances relative to O (blue triangles). For comparison, GSEP and ISEP reference abundances are shown as red circles and orange squares, respectively.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: Helium mass histograms for events #8 (left) and #19 (right). The vertical red lines mark the 3He mass range. The 3He/4He ratios are shown in the upper right corner. Left: the two tilted black lines are the least-squares fits of the background and 4He spillover. The extrapolations to the 3He range are marked by blue.
Paper: Helium-3 Enrichment in Gradual Solar Energetic Particle Events: Evidence for a Jet-supplied Seed Population
Authors: Radoslav Bučík, Samuel T. Hart, Maher A. Dayeh, Mihir I. Desai, Glenn M. Mason, Mark E. Wiedenbeck
Figure caption: ACE/ULEIS 3 hr 3He (2.8–3.1 AMU) and 1 hr 4He (3.5–6.0 AMU) 0.4–10 MeV nucleon−1 count rates for events #1 (left) and #22 (right). Error bars with arrows denote ULEIS single-count data points. SOHO/ERNE 2 hr proton fluxes (in arbitrary units) in two energy ranges are overplotted as black dotted and solid curves.