adsabs/AstroCLIMB huggingface dataset:
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Comparison between photometric redshifts in this catalog and SDSS spectroscopic redshifts for 13,895 sources. In the left panel, the dashed black line shows where the photometric and spectroscopic redshifts are equal. In the right panel, the black points and error bars show the median and 68% tiles, respectively. Outliers are mainly due to bright and highly resolved sources at z ≤ 1 that are not adequately modeled by the available light profiles and tend to get set to specific values of z phot.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Comparison between the measured magnitudes in this catalog (L23) and the AUTO magnitudes using Kron apertures in Wold et al. (2019; W19). The black dashed lines show the expected 1σ magnitude difference due to photometric uncertainties in both catalogs as a function of magnitude. The photometry in this catalog is generally within 0.1 mag of that in Wold et al. (2019), with an absolute median offset of <0.07 mag.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Difference between the measured magnitudes in this catalog (L23) and DECaLS DR9 (LS) as a function of magnitude in this catalog. The median magnitude difference is shown in each panel. DECaLS covers the grz bands in DECam. Both catalogs employ model-based photometry. The photometry is in excellent agreement between the catalogs with a median offset of ≤0.03 mag.
Paper: The Spitzer–HETDEX Exploratory Large-Area Survey. IV. Model-based Multiwavelength Photometric Catalog
Authors: Gene C. K. Leung, Steven L. Finkelstein, John R. Weaver, Casey Papovich, Rebecca L. Larson, Katherine Chworowsky, Robin Ciardullo, Eric Gawiser, Caryl Gronwall, Shardha Jogee, Lalitwadee Kawinwanichakij, Rachel S. Somerville, Isak G. B. Wold, L. Y. Aaron Yung
Figure caption: Fraction of simulated sources recovered as a function of input magnitude. The simulated sources have zero color, i.e., equal AB magnitudes between bands. The simulations show an 80% (50%) completeness threshold of ∼24.7 (∼25.1) mag.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Comparison between group numbers derived from this study and those in the Vaquero et al. (2016) database. Shown are probability distribution matrices following Chatzistergos et al. (2017). The PMF matrices are color coded with dark blue for a probability of 1 and white of 0. For each column, the mean group count is marked with a circle (red when the column has data for more than 20 days and black otherwise) also giving the asymmetric 1σ intervals. The histogram shows the number of days populating each column. The orange and purple curves are linear and exponential fits following Chatzistergos et al. (2017) to the mean values of the distributions. Within the panel, also listed is the the solar cycle for which there is overlap between the counts of the two compared series, as well as the total number of overlapping days vs. the total number of days for the solar cycle along with the slope of the linear fit. The black-dotted line has a slope of unity.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Comparison between group numbers derived from our study and by Secchi and other observers as reported in the database compiled by Vaquero et al. (2016). In particular, we compare the Secchi records as recounted in our study (left column) and the Secchi records in the Vaquero et al. (2016) database (right column) to the data by Tacchini (fist row), Schmidt (second row), and Wolf (third row). Shown are probability distribution matrices following Chatzistergos et al. (2017). See Section 4.2 and the caption of Figure 16 for more details.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Flux-scaling procedure for W51-E in ALMA-IMF Band 3 and MGPS90. For each of the top (a, before scaling) and bottom (b, after scaling) images: Top left: the ratio between FFT amplitudes for common angular scales between interferometric and single-dish data. Top-right: histogram of these ratios. Bottom: FFT amplitudes from the interferometer (red dots) and single dish (blue dots). The gray-shaded area shows the common scales.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Histograms of effective diameters for the entire sample of dendrogram structures. The top and bottom panels show the structures in Band 3 and Band 6, respectively. The vertical red line marks the 0.1 pc threshold that approximately separates small and large scales. The total number of leaves (blue), structures without internal substructures (orange), and trunks (green) are shown, corresponding to the size indicated by the bin. These numbers refer to the total sample, summing across all fields. Insets highlight structures with diameters <0.1 pc.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Reprojection procedure for W51-E. From top to bottom: (a) MGPS90 image with ALMA-IMF Band 3 mosaic outline in red contours before reprojection. (b) ALMA-IMF Band 3 mosaic. (c) ALMA-IMF Band 3 FOV in red contours and MGPS90 after reprojection in colors. Panels (b) and (c) show the ALMA-IMF Band 3 (barely noticeable red circle) and MGPS90 (larger blue circle) beams in their bottom-left corners.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Alignment correction (ΔR.A. = −6.″49, Δdecl. = −0.″55) for the MGPS90 and ALMA-IMF B3 combination for W51-E. Top left: MGPS90 original (unshifted) data. Top right: MGPS90 data with original (unshifted) astrometry overlaid as contours on the ALMA-IMF image. Bottom left: MGPS90 data with shifted astrometry overlaid as contours on the MGPS90 original image. Bottom right: MGPS90 data with shifted astrometry overlaid as contours on the ALMA-IMF image.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Alignment correction (ΔR.A. = −3.″60, Δdecl. = 0.″31) for the BGPS and ALMA-IMF B6 combination for W43-MM3. Top left: original BGPS astrometry in colors. Top right: original BGPS astrometry (contours) over ALMA-IMF-B6 astrometry (colors). Bottom left: shifted BGPS astrometry (contours) over original BGPS astrometry (colors). Bottom right: shifted BGPS astrometry (contours) over ALMA-IMF-B6 astrometry (colors).
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Flowchart of the procedure to combine the interferometric and single-dish data.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: An example showing the variations of the magnitude offsets between the SCR method and the XPSP method before (top panels) and after (bottom panels) the improvements are applied as a function of G BP − G RP color (left panels) and G magnitude (right panels) for the u band. The color represents the number density of stars in each panel. The comparisons for all the bands are shown in Figure A3 and A4. The gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Variations of stellar loci for different metallicities relative to the corresponding ones of [Fe/H] = 0.0 for the u, J0378, J0395, J0410, J0430, and g bands. The difference between the results of [Fe/H] = −1.0, −0.5, 0.0, and +0.5 and [Fe/H] = 0.0 for each panel is represented by the red, green, orange, and blue curves, respectively.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Variations of the zero-point offsets between the SCR method and the XPSP method as a function of extinction E(G BP − G RP) in all bands. For each panel, the red and blue curves denote the median value of the gray points and the residuals estimated for the low-extinction stars, respectively. The bands are marked in the top right corners. The zero-residual lines are denoted by gray dashed lines.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Correlation plots between the zero-point offsets between the XPSP method and the SCR method for all bands. For each panel, the band and the standard deviation are marked in the top left corner and the bottom right corner, respectively. The black dashed lines denote y = x in each panel.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Variations of the zero-point offsets between the SCR method and the XPSP method as a function of R v in all bands. For each panel, the bands are marked in the top left corners; the gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Spatial variations of the stellar fitting residuals for all bands. For each panel, the band and standard deviation are marked in the top left and top right corners, respectively. The color bar showing the size of the residuals is plotted on the right.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Same as Figure 4 but for the SCR method vs. the XPSP zero-points.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Same as Figure 10 but for the difference between the SCR method and the improved XPSP method. The gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Same as Figure 4 but for the difference between the SCR method and the improved XPSP method. The gray dashed lines denote zero offsets.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Example of notebook’s page with the solar drawing made on 1872 June 22 at 8:50 local time. It shows the sunspots, pores, and faculae observed on the solar surface, as well as the chromospheric spicules and prominences seen at the solar limb. In addition to the observed solar features, there are annotations reporting the date and weather during the observation, identification labels attributed to the observed features, Secchi’s counts of sunspots (﹩n^{\prime} =16﹩), group number (n = 6), and sunspot area (a = 65 in units of square millimeters), as well as reference lines that allow defining the solar disk orientation and position of solar features. The solar disk in the drawing has a diameter of about 24.3 cm.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Examples of drawings with detailed and enlarged views of sunspot groups made on 1859 August 28 (top) and 1865 February 16 (bottom). The first one is inside the full-disk drawing for that day, while the second one is a stand-alone sketch. The region of interest in the top image is the one that gave rise to the Carrington event of 1859 September 1. The same drawing is also shown in Hayakawa et al. (2019).
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Examples of the cover (left) and spine (right) of one notebook. Information about the location in the INAF OAR archive of the document shown in this figure, as well as of the archival documents shown in the following figures, is given in Section 5 of this paper.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Drawing made on 1866 June 22 that shows an enlargement of a sunspot group clearly outlining the facular regions in the group’s surroundings.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Examples of drawings reporting the evolution of sunspot groups from 1865 October 5–8 (top) and from 1869 April 11–13 (bottom).
Paper: A Strong-flare Prediction Model Developed Using a Machine-learning Algorithm Based on the Video Data Sets of the Solar Magnetic Field of Active Regions
Authors: Jingjing Wang, Bingxian Luo, Siqing Liu, Yue Zhang
Figure caption: Forecasts of flaring ARs (false-alarm cases) for some negative samples (C-class-flaring ARs).
Paper: A Strong-flare Prediction Model Developed Using a Machine-learning Algorithm Based on the Video Data Sets of the Solar Magnetic Field of Active Regions
Authors: Jingjing Wang, Bingxian Luo, Siqing Liu, Yue Zhang
Figure caption: Forecasts of flaring ARs (false-alarm cases) for some negative samples (nonflaring ARs).
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Example of a prominence drawing made on 1871 July 23.
Paper: New SB1s with Spectroscopic Orbits from LAMOST-LRS
Authors: Yue Chen, 悦 陈, Fang Xia, 芳 夏, Xiaoli Wang, 晓丽 王, Yanning Fu, 燕宁 傅, Ye Yuan, 烨 袁
Figure caption: Histogram of the number of LAMOST observations per object of sample (empty histogram), sample II (filled orange).
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Group numbers derived from the drawings of the Secchi collection in this study (daily counts are shown in gray and annual mean values in red). Also shown are the annual values of the group number series by Chatzistergos et al. (2017, solid green) and S N  (the values are given in the right axis; dashed light blue) as well as the raw group counts of Secchi (dashed yellow) from the Vaquero et al. (2016) database. The vertical dashed black line separates the sporadic data prior to 1858 December and the regular ones afterward. The numbers at the lower part of the figure denote the conventional solar cycle numbering.
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Example of pages in the handwritten notebooks with measurements of properties of the observed solar features and calculation of quantities related to them. This example refers to pores and sunspot data recorded in early 1871. The tabulated values refer to the date of the observation (January 5, 8, 10, 11; column 1); identification number of the observed sunspot (column 2); SA (umbral, penumbral, and total area given in square millimeters; columns 3–5); total SA daily value (column 6); number of observed pores (column 7); annotations (column 8).
Paper: Solar Observations by Angelo Secchi. I. Digitization of Original Documents and Analysis of Group Numbers over the Period of 1853–1878
Authors: I. Ermolli, T. Chatzistergos, F. Giorgi, V. M. S. Carrasco, A. J. P. Aparicio, I. Chinnici
Figure caption: Comparison of the number of days per year with information on group counts in the Secchi collection (black) and those from Secchi (red) and Ferrari (green) in the Vaquero et al. (2016) database.