adsabs/AstroCLIMB huggingface dataset:
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The spectrum of the SGR J1935+2154 burst whose spectrum resembles that of FRB 200428-Associated Burst. Data from LE, ME, and HE of Insight-HXMT are represented in different colors (LE: black; ME: red; HE: purple). The X-ray spectrum of the burst described by the CPL model is shown in the top panel. The five lower panels are the residuals of the data from the individual models of CPL, BB+BB, BB+PL, PL, and BB.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The evolution of the fitting models for CPL and BB+BB. The blue and green lines mark BB+BB models (13) and CPL models (24), respectively, for which the bursts are fit with the minimum BIC value. The triangles and circles that represent the preferred models are BB+BB models (3) and CPL models (11) using a BIC of Δ > 10 (see Section 3.2).
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The scatter plot of E cut and photon index. Orange circles represent the saturated bursts. The red and purple stars are the time-integral and peak spectra of FRB 200428-Associated Burst, respectively.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The light curves of the burst whose spectrum resembles that of the FRB 200428-Associated Burst. The light curves observed with LE (1–10 keV), ME (10–30 keV), and HE (28–250 keV) with a time resolution of 10 ms are shown in the top, middle, and bottom panels, respectively.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The evolution of fluence (top panel) and flux (bottom panel) in 1–250 keV. The stars represent the FRB 200428-Associated Burst. The gray shadow is the time gap of the monitoring of SGR J1935+2154 of Insight-HXMT.
Paper: An Insight-HXMT Dedicated 33 day Observation of SGR J1935+2154. II. Burst Spectral Catalog
Authors: Ce Cai, Shao-Lin Xiong, Lin Lin, Cheng-Kui Li, Shuang-Nan Zhang, Wang-Chen Xue, You-Li Tuo, Xiao-Bo Li, Ming-Yu Ge, Hai-Sheng Zhao, Li-Ming Song, Fang-Jun Lu, Shu Zhang, Qing-Xin Li, Shuo Xiao, Zhi-Wei Guo, Sheng-Lun Xie, Yan-Qiu Zhang, Qi-Bin Yi, Yi Zhao, Zhen Zhang, Jia-Cong Liu, Chao Zheng, Ping Wang
Figure caption: The evolution of the parameters of the BB+BB model. Low kT and high kT are marked as red and blue circles, respectively. The gray shadow is the time gap of the monitoring of SGR J1935+2154.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: (a) Abundances of elements from Ga to Te in the solar system (Lodders et al. 2009; black triangles), excluding elements that are not detected in HD 222925. The AGB s-process contribution to the solar abundances (Bisterzo et al. 2011 for Ga through Se, Bisterzo et al. 2014 for all others) is shown with blue circles; the r-process abundances derived from HD 222925, scaled by +0.40 dex, are shown as red squares; and the sum of the r-process and s-process abundances, with ±1σ uncertainties, are shown as the purple band. (b) The difference between the summed r-process and s-process abundances (the purple line and band) and the total solar abundances (the black line). (c) Percentage contributions by the r-process (red) and s-process (blue) to the total solar abundances. The dotted line marks 100%. (d) Percentage contributions (yellow band) that are unaccounted for by either the r-process or s-process. The dotted line marks 100%.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: Top: the r-process abundance pattern in HD 222925. The solar s-process pattern (the thin blue line, scaled to match the Ba abundance) and the r-process residuals (the thick red line, scaled to match the Eu abundance) are shown for comparison (Sneden et al. 2008, except Y, which is adopted from Bisterzo et al. 2014). The detected elements are marked by the filled black squares, and the upper limits derived from nondetections are marked by arrows. The light red line at Th and U accounts for 13 Gyr of radioactive decay; i.e., 8.5 Gyr of additional decay relative to the solar abundances. Bottom: the difference between the HD 222925 abundances and the solar r-process residuals when scaled to Eu.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: Histogram showing the magnitude distribution of highly r-process-enhanced stars, here defined as those with [Eu/Fe] ≥ +0.7 (Holmbeck et al. 2020). The three stars brighter than HD 222925 in the V band, HD 115444 (Westin et al. 2000), HD 120559 (Hansen et al. 2012), and HD 221170 (Ivans et al. 2006), are all fainter than HD 222925 in the GALEX NUV band. Data for these 181 stars have been compiled from more than 40 literature sources, including Barklem et al. (2005), Ezzeddine et al. (2020), Hansen et al. (2018), Holmbeck et al. (2020), Howes et al. (2016), Ishigaki et al. (2013), Jacobson et al. (2015), Rasmussen et al. (2020), Roederer et al. (2014a), Sakari et al. (2018), and Yong et al. (2021b).
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: Abundances near the Fe peak in the solar system and four metal-poor stars. The abundance patterns are normalized to logε(Fe) = 0.0. [Eu/Fe] ratios are indicated for the four metal-poor stars next to their Se abundances. The data are taken from Roederer et al. (2012a, 2014d) for HD 108317 and HD 128279 and Roederer & Lawler (2012) for HD 160617. The dashed lines approximately follow the decline in the abundances of the even-Z elements on either side of the Fe peak. The Se abundances in the metal-poor stars, especially HD 222925, are far in excess of this extrapolation.
Paper: The R-process Alliance: A Nearly Complete R-process Abundance Template Derived from Ultraviolet Spectroscopy of the R-process-enhanced Metal-poor Star HD 222925 
Authors: Ian U. Roederer, James E. Lawler, Elizabeth A. Den Hartog, Vinicius M. Placco, Rebecca Surman, Timothy C. Beers, Rana Ezzeddine, Anna Frebel, Terese T. Hansen, Kohei Hattori, Erika M. Holmbeck, Charli M. Sakari
Figure caption: Periodic table showing the elements examined in HD 222925. Elements with no long-lived isotopes are indicated using the light gray font. He was previously detected in NIR spectra by Navarrete et al. (2015).
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: WISE [3.4]–[4.6] vs. 22 μm color−magnitude diagram for sources associated with the 6035 MHz ex-OH masers, 6.7 GHz CH3OH masers, and RRLs. WISE point sources associated with different maser species are shown in the legend. The distributions of sources associated with RRLs are given with red histograms, those with 6.7 GHz CH3OH masers are given with green histograms, and those with ex-OH masers are given with blue histograms. The red, green, and blue lines mark the average positions of the corresponding distributions.
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Statistical histograms of the RRL luminosities in different subsamples. The red, green, and blue histograms represent the RRL luminosity distributions for sources associated with RRLs only, CH3OH masers, and ex-OH masers, respectively. The RRL luminosity is in units of K kpc2 km s−1 (for integrated luminosity) or K kpc2 (for peak luminosity).
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: The IR three-color images around the newly detected ex-OH maser sources. Blue, green, and red represent the 3.4, 4.6, and 12 μm band emission in WISE, respectively. The circle in the center of each panel represents the maser targeted positions in our observations (Table 2). The newly detected transitions are given in the upper left corner of each source.
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Spectra of the 6035.09 MHz (2∏3/2, J−5/2, F = 3−3) OH masers detected in the TMRT survey. Blue and red lines denote the spectra on the LHCP and RHCP, respectively.
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Color–color diagram of the WISE point sources associated with different MSFR tracers. The red dots in the left panel represent the 3348 WISE point sources we selected to be observed. The WISE point sources associated with different tracers of MSFR are shown in the legend. The dashed lines represent the WISE color criteria: [3.4]–[4.6] = 2 and [12]–[22] = 2 (see Yang et al. 2017).
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: The RRL FWHM line width distributions for different subsamples. The red, green, and blue histograms represent the sources associated with RRLs only, CH3OH masers, and ex-OH masers, respectively.
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Flux density variations of the 12 6035 MHz ex-OH masers that have high positional accuracy measurements with the ATCA provided in Avison et al. (2016).
Paper: An Excited-state OH Maser Survey toward WISE Point Sources
Authors: Xu-Jia Ouyang, Xi Chen, Zhi-Qiang Shen, Bin Li, Ya-Jun Wu, Hong-Ying Chen, Xiao-Qiong Li, Kai Yang, Shi-Min Song, Hai-Hua Qiao
Figure caption: Long-term variability of the peak flux densities of the 6035 MHz ex-OH masers on the LHCP and RHCP for the three sources that have high positional accuracy measurements.
Paper: Incremental Fermi Large Area Telescope Fourth Source Catalog
Authors: S. Abdollahi, F. Acero, L. Baldini, J. Ballet, D. Bastieri, R. Bellazzini, B. Berenji, A. Berretta, E. Bissaldi, R. D. Blandford, E. Bloom, R. Bonino, A. Brill, R. J. Britto, P. Bruel, T. H. Burnett, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, D. Castro, S. Chaty, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, J. Coronado-Blázquez, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, S. W. Digel, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, V. Fallah Ramazani, S. J. Fegan, E. C. Ferrara, A. Fiori, H. Fleischhack, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, F. Giacchino, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, D. Green, I. A. Grenier, M.-H. Grondin, L. Guillemot, S. Guiriec, M. Gustafsson, A. K. Harding, E. Hays, J. W. Hewitt, D. Horan, X. Hou, G. Jóhannesson, C. Karwin, T. Kayanoki, M. Kerr, M. Kuss, D. Landriu, S. Larsson, L. Latronico, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, D. Paneque, Z. Pei, J. S. Perkins, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, T. Reposeur, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, D. A. Smith, G. Spandre, P. Spinelli, K. Sueoka, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, E. Troja, J. Valverde, K. Wood, G. Zaharijas
Figure caption: Left: fraction of spectrally curved sources as a function of significance, outside the Galactic plane. The error bars are based on the source counts in each bin, assuming a binomial distribution. The sharp increase followed by a plateau at low significance (instead of the expected regular increase) is due to the fact that the source significance is boosted (moved to the right) for curved sources, combined with the detection threshold and a decreasing dN/dlogTS. Right: impact of changing the TScurv threshold from 1 to 9 on the global source spectrum (sum of all sources, excluding the diffuse model) in three regions of the sky; high (∣b∣ > 10°) in blue, ridge (∣b∣ ≤ 2° and ∣l∣ < 60°) in black, and plane (∣b∣ ≤ 10° excluding the ridge) in green. This test was carried out on the 10 yr data set and DR2 sources. The plot starts at 10 MeV, lower than the data (50 MeV).
Paper: Incremental Fermi Large Area Telescope Fourth Source Catalog
Authors: S. Abdollahi, F. Acero, L. Baldini, J. Ballet, D. Bastieri, R. Bellazzini, B. Berenji, A. Berretta, E. Bissaldi, R. D. Blandford, E. Bloom, R. Bonino, A. Brill, R. J. Britto, P. Bruel, T. H. Burnett, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, D. Castro, S. Chaty, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, J. Coronado-Blázquez, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, S. W. Digel, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, V. Fallah Ramazani, S. J. Fegan, E. C. Ferrara, A. Fiori, H. Fleischhack, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, F. Giacchino, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, D. Green, I. A. Grenier, M.-H. Grondin, L. Guillemot, S. Guiriec, M. Gustafsson, A. K. Harding, E. Hays, J. W. Hewitt, D. Horan, X. Hou, G. Jóhannesson, C. Karwin, T. Kayanoki, M. Kerr, M. Kuss, D. Landriu, S. Larsson, L. Latronico, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, D. Paneque, Z. Pei, J. S. Perkins, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, T. Reposeur, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, D. A. Smith, G. Spandre, P. Spinelli, K. Sueoka, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, E. Troja, J. Valverde, K. Wood, G. Zaharijas
Figure caption: Comparison of the pointlike localizations of uw1216 seeds (for DR3) with those of uw8606 (for DR1). The abscissa is the ratio of TS values, whereas the ordinate is the inverse of the ratio of the areas of the error ellipses (such that larger is better). Sources in the upper right corner (materialized by the dashed lines) are stronger and much better localized in uw1216, and their positions and error ellipses were updated in DR3. The source at TS ratio around 300 is the bright γ-ray binary LS 5039, which appeared double in uw8606 because of its complex spectrum (resulting in low TS) but was well localized.
Paper: Incremental Fermi Large Area Telescope Fourth Source Catalog
Authors: S. Abdollahi, F. Acero, L. Baldini, J. Ballet, D. Bastieri, R. Bellazzini, B. Berenji, A. Berretta, E. Bissaldi, R. D. Blandford, E. Bloom, R. Bonino, A. Brill, R. J. Britto, P. Bruel, T. H. Burnett, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, D. Castro, S. Chaty, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, J. Coronado-Blázquez, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, S. W. Digel, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, V. Fallah Ramazani, S. J. Fegan, E. C. Ferrara, A. Fiori, H. Fleischhack, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, F. Giacchino, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, D. Green, I. A. Grenier, M.-H. Grondin, L. Guillemot, S. Guiriec, M. Gustafsson, A. K. Harding, E. Hays, J. W. Hewitt, D. Horan, X. Hou, G. Jóhannesson, C. Karwin, T. Kayanoki, M. Kerr, M. Kuss, D. Landriu, S. Larsson, L. Latronico, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, D. Paneque, Z. Pei, J. S. Perkins, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, T. Reposeur, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, D. A. Smith, G. Spandre, P. Spinelli, K. Sueoka, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, E. Troja, J. Valverde, K. Wood, G. Zaharijas
Figure caption: Ratio between the energy flux (0.1 to 100 GeV) in the PL approximation and that in the LP or PLEC representation, for those sources that are considered significantly curved, outside the Galactic plane. Plus signs refer to the LP model, diamonds to the PLEC model. The scatter increases toward low significance because of the larger statistical fluctuations.
Paper: Incremental Fermi Large Area Telescope Fourth Source Catalog
Authors: S. Abdollahi, F. Acero, L. Baldini, J. Ballet, D. Bastieri, R. Bellazzini, B. Berenji, A. Berretta, E. Bissaldi, R. D. Blandford, E. Bloom, R. Bonino, A. Brill, R. J. Britto, P. Bruel, T. H. Burnett, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, D. Castro, S. Chaty, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, J. Coronado-Blázquez, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, S. W. Digel, N. Di Lalla, F. Dirirsa, L. Di Venere, A. Domínguez, V. Fallah Ramazani, S. J. Fegan, E. C. Ferrara, A. Fiori, H. Fleischhack, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, G. Galanti, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, F. Giacchino, N. Giglietto, F. Giordano, M. Giroletti, T. Glanzman, D. Green, I. A. Grenier, M.-H. Grondin, L. Guillemot, S. Guiriec, M. Gustafsson, A. K. Harding, E. Hays, J. W. Hewitt, D. Horan, X. Hou, G. Jóhannesson, C. Karwin, T. Kayanoki, M. Kerr, M. Kuss, D. Landriu, S. Larsson, L. Latronico, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, M. Meyer, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, D. Paneque, Z. Pei, J. S. Perkins, M. Persic, M. Pesce-Rollins, V. Petrosian, R. Pillera, H. Poon, T. A. Porter, G. Principe, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, T. Reposeur, M. Sánchez-Conde, P. M. Saz Parkinson, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, D. A. Smith, G. Spandre, P. Spinelli, K. Sueoka, D. J. Suson, H. Tajima, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, E. Troja, J. Valverde, K. Wood, G. Zaharijas
Figure caption: Distribution of spectral fit quality over all DR3 sources (histogram). The χ 2 distributions for 4 (dashed line, good fit) and 6 (solid line, bad fit) degrees of freedom are overlaid. The vertical lines correspond to a p-value of 10−3. The threshold for Flag 10 in Table 4 corresponds to the dashed vertical line (for 4 dof).