adsabs/AstroCLIMB huggingface dataset:
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: PDFs for the intensity at 2800 Å (upper photosphere, top), the O I 1355 Å intensity I peak (second from top), the O I 1355 Å line width (third from top), and quantity A that is proportional to ﹩{I}_{\mathrm{peak}}^{\displaystyle \frac{-1}{8}}﹩, all as a function of the distance from the solar limb, with positive values of the latter for off-limb positions. The vertical dashed line is the location of the photospheric limb, as determined from the solar radius and IRIS headers. The solid vertical lines show the range of distances from the limb for which I peak decreases with height. The value of A is scaled so that it is equal to the line broadening at the distance from the solar limb indicated by the leftmost solid vertical line.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: PDF of the O I 1355 Å line width as function of the cosine of the viewing angle (μ) for quiet-Sun internetwork areas (top panel), network areas (middle panel), and for areas 1″ limbward of network areas (bottom panel). In all panels, the least-squares quadratic fit is shown with a solid line and the fits for the two other area types as dashed lines.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: IRIS spectroheliograms of NOAA AR 12920 as it traverses the disk between 2015 September 25 and 2015 September 28. The top row shows the O I 1355 Å intensity, while the bottom row shows the line-of-sight magnetic field as deduced from HMI magnetograms stitched together to replicate the IRIS raster timings and locations. The red circles indicate locations with neutral lines between opposite polarities and increased O I 1355 Å intensities, as described in the text.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: IRIS spectroheliograms of NOAA AR 12920 as it traverses the disk between 2015 September 22 and 2015 September 24. The top row shows the O I 1355 Å intensity, while the bottom row shows the line-of-sight magnetic field as deduced from HMI magnetograms stitched together to replicate the IRIS raster timings and locations. The red circles indicate locations with neutral lines between opposite polarities and increased O I 1355 Å intensities, as described in the text.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: IRIS spectroheliograms of the quiet Sun taken along the meridian from the north pole (top left) to the south pole (bottom right). The top two rows show the O I 1355 Å intensity, while the bottom two rows show the O I 1355 Å line broadening. The O I 1355 Å intensity is scaled between 0 and 60 DN for all panels. Regions with bad fits and/or low peak counts (below 4 DN) are masked out in the O I 1355 Å line-width maps.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: PDF of the O I 1355 Å line core intensity (from the fit) as a function of the cosine of the viewing angle (μ) for the AR 12290 data sets (top panel) and the QS data sets (bottom panel). The color scale is linear.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: Upper panel: the SGRB true event rate distributions (﹩{{\mathfrak{R}}}_{\mathrm{true}}﹩) derived from the opening angle measurements, ﹩\langle {{\mathfrak{R}}}_{\mathrm{true},\mathrm{meas}}\rangle =1786[-1507,+6346]﹩ Gpc−3 yr−1 (orange), and mock, ﹩\langle {{\mathfrak{R}}}_{\mathrm{true},\mathrm{mock}}\rangle =361[-217,+4367]﹩ Gpc−3 yr−1 (yellow) samples using the observed rate of ﹩{{\mathfrak{R}}}_{\mathrm{obs}}=10﹩ Gpc−3 yr−1. The median value of each distribution is indicated by a black vertical line. Bottom panel: we present a more realistic range of values of ﹩{{\mathfrak{R}}}_{\mathrm{true}}﹩ that extends between the median values of the true event rate distributions derived from the opening angle measurements (vertical black dashed line) and mock samples (vertical gray dashed line). Other published rates are also shown for comparison. In particular, these rates are derived from the detection of gravitational waves generated by BNS and NS–BH mergers (Abbott et al. 2023) computed over the whole O3 run, SGRBs (Fong et al. 2015a; Jin et al. 2018; Dichiara et al. 2020), Galactic BNSs (O’Shaughnessy & Kim 2010; Pol et al. 2020; Grunthal et al. 2021), and the estimates for the BNS and NS–BH merger rates derived from population synthesis simulations by Sarin et al. (2022). 68% confidence levels are represented.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: Distribution of the jet-break times for 10 SGRBs with jet-break detections (gray histogram) derived from the individual jet-break time posteriors. The gray arrow indicates the median jet-break time of 〈t j〉 = 1.5[−1.2, +7.7] days. The distribution at t j > 20 days is clearly dominated by a peak which represents the late-time detection of the GRB 211106A jet break in the radio band. For the 19 lower limits, the times of the last X-ray detections are indicated with color-coded lower limits, which roughly correspond to the time out to which we are sensitive to jet breaks for each event. A significant fraction (10/19) of the lower limits are found at times of t j > 〈t j〉, and specifically there are six events with final X-ray detections at t j > 10 days. This shows the existence of an SGRB group with jet breaks located at very late times (and potential wide opening angles), as in the case of GRB 211106A.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: Left: the normalized probability distribution for each of the 10 SGRBs with detected jet opening angles (color-coded open histograms), along with the total distribution of all 10 events (gray histogram). For this sample, we find a median value of ﹩\langle {\theta }_{{\rm{j}},\det }\rangle =6.1^\circ [-3.2^\circ ,+9.3^\circ ]﹩ (gray arrow). The inferred core jet opening angle for SGRB 170817A, ﹩{\theta }_{{\rm{j}},{\rm{core}}}={2}^{\circ }-{4}^{\circ }﹩ (Margutti & Chornock 2021), is indicated as a green bar. Right: the total probability distribution for the sample of 19 lower limits (red dashed histogram) in comparison with the total distribution of detected opening angles (dark gray histogram). The red arrow indicates that this distribution represents lower limit values. There is a distinctive group of SGRB lower limits composed of six events with wider minimum opening angles of ﹩{\theta }_{{\rm{j}},\min }\gtrsim 10^\circ ﹩. Thus, this indicates a possible population of SGRBs with wider opening angles than described from the distribution of measurements alone.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: Unabsorbed X-ray flux (0.3–10 keV) afterglow light curves of the 29 SGRBs in our sample. Swift observations are represented as follows: WT-mode data with light gray thin diamonds and PC-mode data with dark gray circles. Chandra and XMM-Newton detections are depicted with dark blue squares and pink diamonds, respectively. The X-ray flux upper limits (3σ) for both observatories are shown with light blue and light pink triangles, respectively.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: 0.3–10 keV unabsorbed X-ray flux light curves of SGRBs with detected jet breaks. All SGRBs are color coded with their corresponding best-fit models (solid lines). Symbols indicate each set of observations obtained by the different observatories or observing modes (top legend). In addition, we note that the afterglow light curve of GRB 211106A exhibits evidence for a jet in the radio band; however it is wide enough to elude detection in the X-rays. Triangles indicate 3σ upper limits. Vertical lines from the top show the times of the jet breaks for each SGRB. Calculated uncertainties correspond to 1σ.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: X-ray imaging panel of GRB 130603B. The XMM-Newton/PN observations (left and middle) at δ t ∼ 2.7 and ∼7.0 days in the 0.3–10 keV energy band, and merged Chandra/ACIS-S observation (right) obtained at δ t ∼ 6.7 yr in the 0.5–7 keV energy band. The blue circle indicates the XMM-Newton source region. The small dashed red region in the images shows the contaminating source (X1), which is resolved in the Chandra observation. The final X-ray flux afterglow light curve is corrected against the extra contribution of this contaminant with unabsorbed X-ray flux of ﹩({9.2}_{-2.4}^{+2.8})\times {10}^{-15}﹩ erg s−1 cm−2, which was not taken into account in earlier works.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: The CDFs of true event rates for the opening angle measurement sample (orange solid line) and the mock sample including wide jets (yellow dashed line) assuming an observed local rate of ﹩{{\mathfrak{R}}}_{\mathrm{obs}}\approx 10﹩ Gpc−3 yr−1. Comparing both distributions, we see that a larger number of wider jet opening angles in our sample would lead to a more constrained true event rate median value.
Paper: The Jet Opening Angle and Event Rate Distributions of Short Gamma-Ray Bursts from Late-time X-Ray Afterglows
Authors: A. Rouco Escorial, W. Fong, E. Berger, T. Laskar, R. Margutti, G. Schroeder, J. C. Rastinejad, D. Cornish, S. Popp, M. Lally, A. E. Nugent, K. Paterson, B. D. Metzger, R. Chornock, K. Alexander, Y. Cendes, T. Eftekhari
Figure caption: The F-test flow chart followed to determine the best-fit model of the SGRB X-ray afterglow light curve.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Top: S-PLUS magnitudes for SPLUS J1424−2542 compared to the values for SPLUS J2104−0049. Also shown are the S-PLUS filter transmission curves. The second panel from top to bottom shows the Gemini/Gemini Multi-Object Spectrograph (GMOS) spectrum, highlighting absorption features of interest. The remaining color panels show sections of the GHOST spectra and features used for the chemical abundance determinations. The 12 side panels show the S-PLUS images for SPLUS J1424−2542. The RGB colors in all panels are assigned based on the central wavelength of each filter. See text for further details.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Same as Figure 2, for the heavy elements highlighted in each panel.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Spectral synthesis for the determination of the carbon abundance. The red solid line shows the best-fit synthesis and uncertainties (±0.1 and ±0.2 dex—shaded regions) compared to the observed spectra (filled squares). Also shown is a synthetic spectrum after removing all contributions from carbon (gray line).
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Same as Figure 2 for the samarium, calcium, and Eu abundance determinations.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: Examples of O I 1355 Å profiles from four locations of Figure 1. The observed profile is given with symbols and the single Gaussian fit with a solid line. The positions and reduced χ 2 of the fit are given in the upper left with the 1/e width and its 1σ error in the upper right. The increased intensity in the red part of the window is due to an emission line from C I at 1355.8 Å.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: IRIS spectroheliograms of NOAA AR 12920 as it traverses the disk between 2015 September 22 and 2015 October 02. The top two rows show the O I 1355 Å intensity, while the bottom two rows show the O I 1355 Å line broadening. The O I 1355 Å intensity is scaled between 0 and 60 DN for all panels. Regions with bad fits and/or low peak counts (below 4 DN) are masked out in the O I 1355 Å line-width maps.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Chemical (stellar metallicity) enrichment history of star-forming central galaxies (SFGs, blue) and passive central galaxies (PGs, red) for MaNGA sample. Each panel shows the median values of galaxies in a different range of present-day stellar mass: ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=9.0\mbox{--}10.0﹩ (M1), 10.0–10.5 (M2), 10.5–11.0 (M3), and 11.0–12.0 (M4), respectively. In each panel, the SFGs and PGs are further divided into young (age < 4 Gyr: “SFG-y,” green/“PG-y,” purple) and old (age > 4 Gyr: “SFG-o,” brown/“PG-o,” orange) subsamples based on their mass-weighted age in MaNGA Pipe3D catalog. The shaded regions represent 1σ  error on the median value.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Stellar metallicity difference between passive central galaxies (PGs) and star-forming central galaxies (SFGs) as a function of the stellar mass at z ∼ 0 (blue), 0.5 (orange), 1 (green), 2 (red) for MaNGA sample. The median values are calculated in the sliding box of 0.5 dex in stellar mass, and the shaded regions are errors with 1σ uncertainty. The purple line and brown line indicate the stellar metallicity difference between passive galaxies and star-forming galaxies obtained in Peng et al. (2015; labeled as “P+15”) and Trussler et al. (2020; labeled as “T+20”), with shaded regions corresponding to the 1σ  error on the mean value and median value, respectively.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Stellar mass growth history of star-forming central galaxies (SFGs, blue) and passive central galaxies (PGs, red) for the MaNGA sample, normalized to the stellar mass at z = 0. Each panel corresponds to a different range of present-day stellar mass: ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=9.0\mbox{--}10.0﹩ (M1), 10.0–10.5 (M2), 10.5–11.0 (M3), and 11.0–12.0 (M4), respectively. The solid curves depict the median growth history, with shaded regions representing 1σ  error on the median value in the x-axis. Dashed lines mark half of the present-day stellar mass.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Stellar mass and star formation rate for MaNGA sample. The thick black solid line indicates the Star-forming Main Sequence (SFMS), and the thin dashed and dotted lines represent the downward offset of 0.5 and 1.5 dex from the SFMS, respectively. The galaxies with ΔMS > −0.5 are classified as SFGs (blue dots), whereas those with ΔMS < −1.5 are classified as PGs (red dots). The galaxies that fall between the two thin lines are green valley galaxies (gray dots), which are not the focus of this study.
Paper: Branching Fractions and Transition Probabilities for UV Transitions in the Spectrum of Cr II 
Authors: Jacob W. Ward, Jacqueline J. Li, Jared Schwartz, Gillian Nave, Ton A. J. J. Raassen, Peter H. M. Uylings
Figure caption: Comparison of the intensity of strong lines from five levels of the z 4 G and y 4 D terms in Cr II in spectrum 7, I #7, to the weighted mean intensity, I mean, of the same line in spectra 1–6, 8, and 9 in Table 1. The line intensities in each spectrum from each upper level were scaled so that the line nearest 34,000 cm−1 from each upper energy level had an intensity of 1. The dashed line shows the 15% change in response between 35,000 and 45,000 cm−1 that was used to derive the correction to the response derived from spectrum 6. The error bars represent one standard uncertainty. The line intensities and wavenumbers used to create this plot are available as data behind the figure in the online version of this article.(The data used to create this figure are available.)
Paper: Branching Fractions and Transition Probabilities for UV Transitions in the Spectrum of Cr II 
Authors: Jacob W. Ward, Jacqueline J. Li, Jared Schwartz, Gillian Nave, Ton A. J. J. Raassen, Peter H. M. Uylings
Figure caption: Relative response of the spectrometer for the spectra in Table 1. The response curve for spectrum 7 is not shown, but was derived from the response curve for spectra 5 and 6 as described in Section 2 and Figure 1. Irregularities in the response curves at wavenumbers greater than 50,000 cm−1 are caused by air in the path between the source and the spectrometer and BFs were thus not calculated in this region.
Paper: Branching Fractions and Transition Probabilities for UV Transitions in the Spectrum of Cr II 
Authors: Jacob W. Ward, Jacqueline J. Li, Jared Schwartz, Gillian Nave, Ton A. J. J. Raassen, Peter H. M. Uylings
Figure caption: Comparison of the transition probabilities from this work, AThiswork, with those of Gurell et al. (2010), AGurell. The transition probabilities and wavenumbers used to create this plot are available as data behind the figure in the online version of this article.(The data used to create this figure are available.)
Paper: Branching Fractions and Transition Probabilities for UV Transitions in the Spectrum of Cr II 
Authors: Jacob W. Ward, Jacqueline J. Li, Jared Schwartz, Gillian Nave, Ton A. J. J. Raassen, Peter H. M. Uylings
Figure caption: Comparison of our experimental and calculated branching fractions. The error bars are the one standard uncertainty of the experimental branching fractions and do not include estimated uncertainties on the calculated values. The branching fraction ratios and values used to create this plot are available as data behind the figure in the online version of this article.(The data used to create this figure are available.)