adsabs/AstroCLIMB huggingface dataset:
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The distribution for our standard-star network on the sky. Stars are categorized by whether they are included in our set of primary CALSPEC standards or are treated as secondary standards to be recalibrated. Additionally, stars that entered our sample via the Southern Spectrophotometric Standards (SSPS) sample are highlighted; these were originally on the Hayes (1985) system and so are likely to change the most when transformed to the CALSPEC system. The standard stars that we ultimately rejected (see Table 1) are also shown. The green dashed line indicates the decl. corresponding to zenith for Maunakea. The primary and secondary standard stars are both well distributed on the sky.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Results of simulations to test the linearity of our extract_star2 software that measures 1D spectra from SNIFS data cubes. On the left is shown a simulation in which a PSF vs. wavelength is fit to the data cubes using as weights the photon and readout noise variance spectrum estimated directly from the signal. On the right is shown the cases where the initial signal-estimated variance spectrum is smoothed in wavelength, leaving out the target wavelength and the two adjacent from the kernel, thereby decorrelating the signal and the weights. Using the variance spectrum directly results in a strong bias with S/N, whereas using the smoothed variance does not. The simulations used to produce these results take high S/N standard-star data cubes and add noise that simulates fainter and fainter stars. Overall, this test spans a factor of 5000× in brightness, corresponding to a range of 9.25 mag. We performed ∼16,200 of these simulations across all spectra for 10 different standard stars in order to sample over a wide range of PSF shapes.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The per-transit rms of the Gaia G magnitude vs. the G magnitude. The rms includes Gaia measurement errors and any stellar variability that may be present. The legend identifies stars in order of their G-band magnitude. The cyan-shaded regions indicate the 3σ and 5σ measurement uncertainty ranges expected from the typical Gaia measurement accuracy (taken from Riello et al. 2021). Stars with significant rms—larger than 0.015 mag and 3σ larger than the expected measurement uncertainty—are labeled.
Paper: GWFAST: A Fisher Information Matrix Python Code for Third-generation Gravitational-wave Detectors
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Comparison of the results obtained using GWFAST for some selected events from GWTC–2 and GWTC–3: GW170817, GW190412, GW190814, GW200208_130117, GW200224_222234, and GW200311_115853. Each row contains the histogram of the S/N, 90% relative credible intervals on the source-frame chirp mass and luminosity distance, and 90% credible sky area for 1000 samples of the posterior distributions of the events for all of the parameters. Lines of different colors refer to different waveform models, and the vertical dashed lines denote the errors inferred by LVC with a full Bayesian parameter estimation (Abbott et al. 2021b, 2021a).
Paper: GWFAST: A Fisher Information Matrix Python Code for Third-generation Gravitational-wave Detectors
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Ratio of the time needed to compute S/Ns (left) and Fisher matrices (right) vectorizing on N events, and the time needed to perform the computation serially, with a for loop (equivalent to N times the time needed for a single evaluation). The different colors refer to the results obtained using machines with different characteristics, as reported in the legend.
Paper: GWFAST: A Fisher Information Matrix Python Code for Third-generation Gravitational-wave Detectors
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Relative difference of the Fisher matrix diagonal elements computed on a sample of 100 events with GWFAST and an independent Wolfram Mathematica code. The labels of the x-axes refer to the parameters whose diagonal elements are plotted.
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the Na D2 (5891.58 Å) and D1 (5897.56 Å) lines and (b) the solar spectrum in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Na.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the Ca 4227.92 Å line and (b) the solar spectrum in the region of the line. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Ca.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the Mg 2852.96 Å line and (b) the solar spectrum in the region of the line. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Mg.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: Mercury’s radial velocity relative to the Sun as a function of Mercury’s true anomaly angle.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption:  3He/4He ratios at 0.64–1.28 MeV nucleon−1 vs. 0.32–0.45 MeV nucleon−1 with a dashed line of symmetry. The 1D ratio distributions for each spacecraft are shown along their respective axis, matching colors accordingly. The mean, median, and standard deviation of 3He/4He for each spacecraft are shown in the top right of the figure.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: Mass histogram of 1–7 amu between 0.32 and 0.45 MeV nucleon−1 (a) and 0.64–1.28 MeV nucleon−1 (b) of a reference period observed by STEREO-A. This reference period has significant enhancement in 4He and H, but it does not show any 3He enhancement. We take the mean and standard deviation of the best-fitted Gaussians (shown in blue and red, matching their respective curve) and use them as approximate parameters when separating masses for 3He-rich time periods.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: Fe/O abundances ratios at 0.64–1.28 MeV nucleon−1 vs. 0.32–0.45 MeV nucleon−1 with a line of symmetry. Colored vertical and horizontal lines show the nominal Fe/O ratios of commonly observed heliospheric populations as a comparison. Again, the mean, median, and standard deviation of Fe/O for each spacecraft are shown in the top right of the figure, noting that (1) the median Fe/O ratios are a factor of 10 higher than GSEPs, CIRs, and the slow solar wind, and (2) the standard deviation of the Fe/O ratios is substantially smaller than that of 3He/4He.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: Mass histograms of the 3He event (see Figure 2) observed by STEREO-A with 3He and 4He separated. The mean and standard deviation of H, 3He, and 4He are listed in the same color as their respective curves. Integrating the best-fitted Gaussian, normalizing to a standard bin size, and accounting for the detector efficiency yields an abundance ratio of 0.25 ± 0.03 between 0.32 and 0.45 MeV nucleon−1 (a). The same method yields an abundance ratio of 0.37 ± 0.08 between 0.64 and 1.28 MeV nucleon−1 (b).
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption:  3He/4He vs. Fe/O for 0.32–0.45 MeV nucleon−1 (a) and 0.64–1.28 MeV nucleon−1 (b). At low 3He/4He ratios, there is a moderate correlation with the Fe/O values ((a) r = 0.49; (b) r = 0.46). Above 3He/4He = 0.3, the correlation tends to zero ((a) r = −0.01; (b) r = 0.06).
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: Mass histograms highlighting the separation of 3He and 4He for the 3He-rich SEP event that occurred on 1999 September 30 observed by ACE. The black line shows the separation mass of 3.3 amu. Anything greater is considered 4He up to 5 amu, less is considered 3He down to 2.2 amu (vertical dashed lines). We measure 3He/4He abundance ratios of 0.94 ± 0.04 (a) for 0.32–0.45 MeV nucleon−1 and 2.02 ± 0.18 (b) for 0.64–1.28 MeV nucleon−1.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: A 4 day plot of the reference period observed by STEREO-A. There are no signatures of a 3He enhancement, evident in (b). We use the mass distributions of reference events to resolve the 3He fluences of 3He-rich time periods.
Paper: Statistical Study and Live Catalog of Multispacecraft 3He-rich Time Periods over Solar Cycles 23, 24, and 25
Authors: S. T. Hart, M. A. Dayeh, R. Bučík, M. I. Desai, R. W. Ebert, G. C. Ho, G. Li, G. M. Mason
Figure caption: Heavy-ion abundances during the 1999 September 30 event observed by ACE (a) and 2010 August 24 observed by STEREO-A (b) between 0.32 and 0.45 MeV nucleon−1. We measure the Fe and O abundances by summing incident ion observations with masses between 45–80 and 14–19 amu, respectively.
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption: Energy of the high-energy component plotted as a function of ﹩{\nu }_{\mathrm{pk}}^{{\prime} \mathrm{syn}}﹩, both estimated in the rest frame, for the different blazar classes. The source selection is described in the text. The blue line represents a linear fit to the BL Lac object data and the orange one (restricted to ﹩{\rm{log}}({\nu }_{\mathrm{pk}}^{{\prime} \mathrm{syn}})\lt 13.6﹩) to the FSRQ data. The black dashed–dotted line corresponds to the prescription from Abdo et al. (2010a).
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption:  ν F ν of the high-energy peak as a function of the peak energy for sources fulfilling the conditions given in the text. Error bars have been omitted for clarity. The dashed curve corresponds to an estimated average threshold.
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption: Distributions of ﹩{\nu }_{\mathrm{pk}}^{\mathrm{syn}}﹩ (top) and photon index (bottom) of the new (DR2 and DR3) BCUs (green, solid) compared to the arbitrarily normalized sum of the FSRQ and BL Lac object distributions (solid, black). The relative weight between FSRQs and BL Lac objects has been multiplied by 2.5 with respect to that found in 4FGL.
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption: Compton dominance plotted as a function of ﹩{\nu }_{\mathrm{pk}}^{{\prime} \mathrm{syn}}﹩ for the same sources as in Figure 6. The dashed line corresponds to an estimate of the average threshold for BL Lac objects (derived from the threshold plotted in Figure 5) and the solid line to an exponential fit to the BL Lac object data.
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption: Comparison between the photon-index distributions of 4LAC-DR1 and new (DR2 and DR3) blazars for different classes.
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption: Photon-index distributions for the new BCUs and the subset of sources showing significant variability.
Paper: The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3
Authors: M. Ajello, L. Baldini, J. Ballet, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, A. Berretta, E. Bissaldi, R. Bonino, A. Brill, P. Bruel, S. Buson, R. Caputo, P. A. Caraveo, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, M. Crnogorcevic, S. Cutini, F. D'Ammando, S. De Gaetano, N. Di Lalla, L. Di Venere, A. Domínguez, V. Fallah Ramazani, E. C. Ferrara, A. Fiori, Y. Fukazawa, S. Funk, P. Fusco, V. Gammaldi, F. Gargano, S. Garrappa, D. Gasparrini, N. Giglietto, F. Giordano, M. Giroletti, D. Green, I. A. Grenier, S. Guiriec, D. Horan, X. Hou, T. Kayanoki, M. Kuss, S. Larsson, L. Latronico, T. Lewis, J. Li, I. Liodakis, F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, G. M. Madejski, S. Maldera, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, I. Mereu, P. F. Michelson, N. Mirabal, W. Mitthumsiri, T. Mizuno, M. E. Monzani, A. Morselli, I. V. Moskalenko, M. Negro, R. Ojha, M. Orienti, E. Orlando, J. F. Ormes, Z. Pei, H. Peña-Herazo, 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, L. Scotton, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, D. J. Suson, H. Tajima, D. F. Torres, J. Valverde, H. Yassin, G. Zaharijas
Figure caption: Comparison between the redshift distributions of 4LAC-DR1 and new (DR2 and DR3) blazars for different classes.