adsabs/AstroCLIMB huggingface dataset:
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: All-sky PS map with “source” settings in Galactic coordinates (Mollweide projection). The color scale corresponds to −4σ to 4σ deviations (accounting for the number of pixels in the map).
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: All-sky PS map with “diffuse” settings in Galactic coordinates (Mollweide projection). The color scale corresponds to −4σ to 4σ deviations (accounting for the number of independent pixels in the map).
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: Variability-index (left) and photon-index (right) distributions of high-latitude unassociated sources and blazars for different bins in Test_Statistic.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Covariance matrix of quantities associated with M BH as derived from the C IV emission line.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Covariance matrix of quantities associated with M BH as derived from the Mg II emission line.
Paper: The US Naval Observatory VLBI Spectroscopic Catalog
Authors: Remington O. Sexton, Nathan J. Secrest, Megan C. Johnson, Bryan N. Dorland
Figure caption: Covariance matrix of quantities associated with M BH as derived from the Hβ emission line.
Paper: Variability of the Sun’s Luminosity Places Constraints on the Thermal Equilibrium of the Convection Zone
Authors: L. E. A. Vieira, G. Kopp, T. Dudok de Wit, L. A. da Silva, F. Carlesso, A. R. Barbosa, A. Muralikrishna, R. Santos
Figure caption: Reconstruction of the solar luminosity for cycles 23 and 24. Panels (a) and (b) present comparisons between the percentage variation of the total solar irradiance observations (blue) and the reconstructed luminosity (red) for 2003 and for solar cycles 23/24, respectively. The reference level for both quantities is the average value for the year 2008 during the solar minimum between cycles 23 and 24. (c) Power enhancement due to bright features (blue) and deficit due to power blocked by sunspots (red). (d) Difference between the TSI composite and our model for each cycle (blue/red for 23/24). The estimated TSI composite uncertainties are shown in yellow. The dashed red lines indicate the 3 month period during which the SoHO spacecraft lost contact (beginning 1998 June 24). The tick labels for the time are in the format dd/mm/yy.
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: The dust extinction curves toward the sight lines with pcFlag = “UVI” are plotted as solid gray lines. The main figure shows the extinction laws from UV (0.15 μm) to 1 μm, and the inset shows those from 0.6 μm to NIR bands (3 μm). The median extinction curve derived in this work (solid red line) is compared with the median attenuation curve derived in Hagen (2017; solid green line) and the attenuation curve of M33 nucleus derived in Gordon et al. (1999; solid cyan line). The black dashed line shows the extinction law toward the diffuse region in the MW. The yellow dashed line is the average extinction curve in M31 derived in Paper I. The orange dashed−dotted line and the blue dashed−dotted line are the extinction curve of the SMC bar and the average LMC extinction curve (Gordon et al. 2003), respectively.
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Influence of lacking UV or NIR data on the derived α,  A  V , ﹩\overline{a}﹩, and E(B − V). The red and blue circles indicate the tracers in the seventh line and the ninth line in Table 3, respectively. The x-axis values for a certain red (blue) circle are the derived parameters ﹩(\alpha ,\,{A}_{V},\,\bar{a},\,E(B-V))﹩ with all available photometric data considered, while the corresponding y-axis values are the derived parameters ﹩(\tilde{\alpha },\,\tilde{{A}_{V}},\,\tilde{a},\,\tilde{E(B-V)})﹩ when repeating the calculation process but without taking the available NIR (UV) data into consideration. The deviation between the red (blue) circles and y = x presents the influence of the lack of NIR (UV) data.
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Dust size distributions for the selected tracers with pcFlag = “UVI.” The solid red line indicates the average dust size distribution for M33 derived in this work. The black dashed line shows the corresponding dust size distribution for the diffuse region in the MW as fitting the model extinction curves to the F19 extinction law (R  V  = 3.1). The yellow dotted line and the solid blue line are the typical MRN dust size distributions for silicate and graphite, respectively (Mathis et al. 1977).
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: Dust extinction curves (gray dotted lines) toward the selected tracers in (a) NGC 6822 and (b) WLM. The solid gray line in panel (a) is the extinction curve toward the sight line with pcFlag = “UVI” in NGC 6822. The solid red lines are the average ones for the derived extinction curves in NGC 6822 and WLM compared with those in the MW and M31 (the symbol convention follows Figure 3), as well as the average extinction curve in M33 derived in this work (cyan dashed line).
Paper: Variability of the Sun’s Luminosity Places Constraints on the Thermal Equilibrium of the Convection Zone
Authors: L. E. A. Vieira, G. Kopp, T. Dudok de Wit, L. A. da Silva, F. Carlesso, A. R. Barbosa, A. Muralikrishna, R. Santos
Figure caption: Reconstruction of the irradiance on the heliographic latitude for an observer at Earth’s heliographic longitude (a) and dependence on heliographic longitude for an observer at the solar equator (b) for 2003. For reference, we show the TSI observations as dashed lines in both panels. The tick labels for the time are in the format dd/mm/yy.
Paper: Dust Extinction Law in Nearby Star-resolved Galaxies. II. M33 Traced by Supergiants
Authors: Yuxi Wang, 钰溪 王, Jian Gao, 健 高, Yi Ren, 逸 任, Bingqiu Chen, 丙秋 陈
Figure caption: The A  V  distribution derived in this work. The background image is taken from the GALEX ultraviolet observation.
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: Galactic distributions of the 6031 and 6035 MHz ex-OH masers. Top panel: Galactic coordinate distribution of the ex-OH maser sources detected in our observations and collected from other maser catalogs. The dotted lines define the Galactic latitude range of ±2°. Bottom panel: Galactic plane distributions of the corresponding ex-OH maser sources. (Background image of the Milky Way credit: Xing-Wu Zheng and Mark Reid BeSSeL/NJU/CFA.) The yellow circle represents the position of the Sun, and the red cross represents the Galactic center.
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: Galactic plane distributions of sources that have magnetic field direction measurements from ground-state or ex-OH masers. The data include our measurements for the ex-OH masers (red filled circles and blue crosses) and those extracted from Figure 6 of Green et al. (2012) for the ground-state OH masers and Figure 9 of Green et al. (2015) for the ex-OH masers (red open circles and blue plus signs). Red represents a source whose magnetic field direction is positive, and blue represents negative. (Background image of Milky Way credit: Xing-Wu Zheng & Mark Reid BeSSeL/NJU/CFA.) The yellow circle represents the position of the Sun, and the red cross represents the Galactic center.
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: Correlation analysis for luminosities of different MFSR tracers. (a) Log–log relations of luminosities between the 6035 and 6031 MHz OH masers. (b) Log–log relations of luminosities between the 6035 MHz OH masers and 6669 MHz CH3OH masers. (c) Log–log relations of luminosities between the RRLs and 6035 MHz OH masers. Maser luminosity is in units of Jy kpc2 km s−1 (for integrated luminosity) or Jy kpc2 (for peak luminosity); RRL luminosity is in units of K kpc2 km s−1 (for integrated luminosity) or K kpc2 (for peak luminosity).
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: Positions of unassociated sources (crosses) around the Galactic center. The background is a count map of 83–228 MeV patch photons simulated over 12 yr with a pixel size of 1°.
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: Same as Figure 15 bottom, but for low-latitude unassociated sources.
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: Photon-index distributions of low-latitude unassociated sources in different sky regions.
Paper: Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory
Authors: Igor Andreoni, Raffaella Margutti, Om Sharan Salafia, B. Parazin, V. Ashley Villar, Michael W. Coughlin, Peter Yoachim, Kris Mortensen, Daniel Brethauer, S. J. Smartt, Mansi M. Kasliwal, Kate D. Alexander, Shreya Anand, E. Berger, Maria Grazia Bernardini, Federica B. Bianco, Peter K. Blanchard, Joshua S. Bloom, Enzo Brocato, Mattia Bulla, Regis Cartier, S. Bradley Cenko, Ryan Chornock, Christopher M. Copperwheat, Alessandra Corsi, Filippo D'Ammando, Paolo D'Avanzo, Laurence Élise Hélène Datrier, Ryan J. Foley, Giancarlo Ghirlanda, Ariel Goobar, Jonathan Grindlay, Aprajita Hajela, Daniel E. Holz, Viraj Karambelkar, E. C. Kool, Gavin P. Lamb, Tanmoy Laskar, Andrew Levan, Kate Maguire, Morgan May, Andrea Melandri, Dan Milisavljevic, A. A. Miller, Matt Nicholl, Samaya M. Nissanke, Antonella Palmese, Silvia Piranomonte, Armin Rest, Ana Sagués-Carracedo, Karelle Siellez, Leo P. Singer, Mathew Smith, D. Steeghs, Nial Tanvir
Figure caption: Simulated KN light curves in the six Rubin filters for different properties of the ejecta (mass and velocity) at four representative distances (30, 100, 200, and 300 Mpc). The models include a “red” and “blue” KN component. We explore three values of the red-component ejecta mass, M ej,R = 0.005, 0.01, and 0.05 M ⊙, with velocity v ej,R = 0.15 c (the KN luminosity is not a strong function of v ej,R and values within 0.1–0.2 c give comparable results). For each combination of these parameters, the blue ejecta component is M ej,B = 0.5 × M ej,R and v ej,B = 1.5 × v ej,R. Open circles depict the expected preferred cadence times postmerger (1, 2, 4, 24, and 48 hr, with the possible addition of data at 8 hr). Dotted and dotted–dashed horizontal lines mark typical 5σ detection thresholds of ZTF and DECam, respectively, assuming 30 s exposure times (although GW follow-up with those instruments is likely to be performed using longer exposure times). Red and purple solid lines: Rubin 5σ detection thresholds for exposure times of 30 and 180 s under ideal observing conditions.
Paper: Target-of-opportunity Observations of Gravitational-wave Events with Vera C. Rubin Observatory
Authors: Igor Andreoni, Raffaella Margutti, Om Sharan Salafia, B. Parazin, V. Ashley Villar, Michael W. Coughlin, Peter Yoachim, Kris Mortensen, Daniel Brethauer, S. J. Smartt, Mansi M. Kasliwal, Kate D. Alexander, Shreya Anand, E. Berger, Maria Grazia Bernardini, Federica B. Bianco, Peter K. Blanchard, Joshua S. Bloom, Enzo Brocato, Mattia Bulla, Regis Cartier, S. Bradley Cenko, Ryan Chornock, Christopher M. Copperwheat, Alessandra Corsi, Filippo D'Ammando, Paolo D'Avanzo, Laurence Élise Hélène Datrier, Ryan J. Foley, Giancarlo Ghirlanda, Ariel Goobar, Jonathan Grindlay, Aprajita Hajela, Daniel E. Holz, Viraj Karambelkar, E. C. Kool, Gavin P. Lamb, Tanmoy Laskar, Andrew Levan, Kate Maguire, Morgan May, Andrea Melandri, Dan Milisavljevic, A. A. Miller, Matt Nicholl, Samaya M. Nissanke, Antonella Palmese, Silvia Piranomonte, Armin Rest, Ana Sagués-Carracedo, Karelle Siellez, Leo P. Singer, Mathew Smith, D. Steeghs, Nial Tanvir
Figure caption: Same as Figure 1, but only the red KN component is considered to simulate the light curves, instead of a combination of a red and a blue component. The KN light curves are adapted from models described in Villar et al. (2017). Since NS–BH mergers are expected to be accompanied by such redder KNe at larger distances, a longer and deeper monitoring is preferred (see Section 2.1.2).