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  1. Book ; Online: Gaia Early Data Release 3

    Riello, M. / De Angeli, F. / Evans, D. W. / Montegriffo, P. / Carrasco, J. M. / Busso, G. / Palaversa, L. / Burgess, P. W. / Diener, C. / Davidson, M. / Rowell, N. / Fabricius, C. / Jordi, C. / Bellazzini, M. / Pancino, E. / Harrison, D. L. / Cacciari, C. / van Leeuwen, F. / Hambly, N. C. /
    Hodgkin, S. T. / Osborne, P. J. / Altavilla, G. / Barstow, M. A. / Brown, A. G. A. / Castellani, M. / Cowell, S. / De Luise, F. / Gilmore, G. / Giuffrida, G. / Hidalgo, S. / Holland, G. / Marinoni, S. / Pagani, C. / Piersimoni, A. M. / Pulone, L. / Ragaini, S. / Rainer, M. / Richards, P. J. / Sanna, N. / Walton, N. A. / Weiler, M. / Yoldas, A.

    Photometric content and validation

    2020  

    Abstract: Gaia Early Data Release 3 contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the ESA Gaia satellite during the first 34 months of operations. This paper focuses on the photometric content, ... ...

    Abstract Gaia Early Data Release 3 contains astrometry and photometry results for about 1.8 billion sources based on observations collected by the ESA Gaia satellite during the first 34 months of operations. This paper focuses on the photometric content, describing the input data, the algorithms, the processing, and the validation of the results. Particular attention is given to the quality of the data and to a number of features that users may need to take into account to make the best use of the EDR3 catalogue. The treatment of the BP and RP background has been updated to include a better estimation of the local background, and the detection of crowding effects has been used to exclude affected data from the calibrations. The photometric calibration models have also been updated to account for flux loss over the whole magnitude range. Significant improvements in the modelling and calibration of the point and line spread functions have also helped to reduce a number of instrumental effects that were still present in DR2. EDR3 contains 1.806 billion sources with G-band photometry and 1.540 billion sources with BP and RP photometry. The median uncertainty in the G-band photometry, as measured from the standard deviation of the internally calibrated mean photometry for a given source, is 0.2 mmag at magnitude G=10 to 14, 0.8 mmag at G=17, and 2.6 mmag at G=19. The significant magnitude term found in the Gaia DR2 photometry is no longer visible, and overall there are no trends larger than 1 mmag/mag. Using one passband over the whole colour and magnitude range leaves no systematics above the 1% level in magnitude in any of the bands, and a larger systematic is present for a very small sample of bright and blue sources. A detailed description of the residual systematic effects is provided. Overall the quality of the calibrated mean photometry in EDR3 is superior with respect to DR2 for all bands.
    Keywords Astrophysics - Instrumentation and Methods for Astrophysics
    Subject code 551
    Publishing date 2020-12-03
    Publishing country us
    Document type Book ; Online
    Database BASE - Bielefeld Academic Search Engine (life sciences selection)

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  2. Article ; Online: Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger.

    Pian, E / D'Avanzo, P / Benetti, S / Branchesi, M / Brocato, E / Campana, S / Cappellaro, E / Covino, S / D'Elia, V / Fynbo, J P U / Getman, F / Ghirlanda, G / Ghisellini, G / Grado, A / Greco, G / Hjorth, J / Kouveliotou, C / Levan, A / Limatola, L /
    Malesani, D / Mazzali, P A / Melandri, A / Møller, P / Nicastro, L / Palazzi, E / Piranomonte, S / Rossi, A / Salafia, O S / Selsing, J / Stratta, G / Tanaka, M / Tanvir, N R / Tomasella, L / Watson, D / Yang, S / Amati, L / Antonelli, L A / Ascenzi, S / Bernardini, M G / Boër, M / Bufano, F / Bulgarelli, A / Capaccioli, M / Casella, P / Castro-Tirado, A J / Chassande-Mottin, E / Ciolfi, R / Copperwheat, C M / Dadina, M / De Cesare, G / Di Paola, A / Fan, Y Z / Gendre, B / Giuffrida, G / Giunta, A / Hunt, L K / Israel, G L / Jin, Z-P / Kasliwal, M M / Klose, S / Lisi, M / Longo, F / Maiorano, E / Mapelli, M / Masetti, N / Nava, L / Patricelli, B / Perley, D / Pescalli, A / Piran, T / Possenti, A / Pulone, L / Razzano, M / Salvaterra, R / Schipani, P / Spera, M / Stamerra, A / Stella, L / Tagliaferri, G / Testa, V / Troja, E / Turatto, M / Vergani, S D / Vergani, D

    Nature

    2017  Volume 551, Issue 7678, Page(s) 67–70

    Abstract: The merger of two neutron stars is predicted to give rise to three major detectable phenomena: a short burst of γ-rays, a gravitational-wave signal, and a transient optical-near-infrared source powered by the synthesis of large amounts of very heavy ... ...

    Abstract The merger of two neutron stars is predicted to give rise to three major detectable phenomena: a short burst of γ-rays, a gravitational-wave signal, and a transient optical-near-infrared source powered by the synthesis of large amounts of very heavy elements via rapid neutron capture (the r-process). Such transients, named 'macronovae' or 'kilonovae', are believed to be centres of production of rare elements such as gold and platinum. The most compelling evidence so far for a kilonova was a very faint near-infrared rebrightening in the afterglow of a short γ-ray burst at redshift z = 0.356, although findings indicating bluer events have been reported. Here we report the spectral identification and describe the physical properties of a bright kilonova associated with the gravitational-wave source GW170817 and γ-ray burst GRB 170817A associated with a galaxy at a distance of 40 megaparsecs from Earth. Using a series of spectra from ground-based observatories covering the wavelength range from the ultraviolet to the near-infrared, we find that the kilonova is characterized by rapidly expanding ejecta with spectral features similar to those predicted by current models. The ejecta is optically thick early on, with a velocity of about 0.2 times light speed, and reaches a radius of about 50 astronomical units in only 1.5 days. As the ejecta expands, broad absorption-like lines appear on the spectral continuum, indicating atomic species produced by nucleosynthesis that occurs in the post-merger fast-moving dynamical ejecta and in two slower (0.05 times light speed) wind regions. Comparison with spectral models suggests that the merger ejected 0.03 to 0.05 solar masses of material, including high-opacity lanthanides.
    Language English
    Publishing date 2017-11-02
    Publishing country England
    Document type Journal Article
    ZDB-ID 120714-3
    ISSN 1476-4687 ; 0028-0836
    ISSN (online) 1476-4687
    ISSN 0028-0836
    DOI 10.1038/nature24298
    Database MEDical Literature Analysis and Retrieval System OnLINE

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  3. Book ; Online: Gaia Early Data Release 3

    Gaia Collaboration / Brown, A. G. A / Vallenari, A. / Prusti, T. / de Bruijne, J. H. J. / Babusiaux, C. / Biermann, M. / Creevey, O. L. / Evans, D. W. / Eyer, L. / Hutton, A. / Jansen, F. / Jordi, C. / Klioner, S. A. / Lammers, U. / Lindegren, L. / Luri, X. / Mignard, F. / Panem, C. /
    Pourbaix, D. / Randich, S. / Sartoretti, P. / Soubiran, C. / Walton, N. A. / Arenou, F. / Bailer-Jones, C. A. L. / Bastian, U. / Cropper, M. / Drimmel, R. / Katz, D. / Lattanzi, M. G. / van Leeuwen, F. / Bakker, J. / Cacciari, C. / Castañeda, J. / De Angeli, F. / Ducourant, C. / Fabricius, C. / Fouesneau, M. / Frémat, Y. / Guerra, R. / Guerrier, A. / Guiraud, J. / Piccolo, A. Jean-Antoine / Masana, E. / Messineo, R. / Mowlavi, N. / Nicolas, C. / Nienartowicz, K. / Pailler, F. / Panuzzo, P. / Riclet, F. / Roux, W. / Seabroke, G. M. / Sordo, R. / Tanga, P. / Thévenin, F. / Gracia-Abril, G. / Portell, J. / Teyssier, D. / Altmann, M. / Andrae, R. / Bellas-Velidis, I. / Benson, K. / Berthier, J. / Blomme, R. / Brugaletta, E. / Burgess, P. W. / Busso, G. / Carry, B. / Cellino, A. / Cheek, N. / Clementini, G. / Damerdji, Y. / Davidson, M. / Delchambre, L. / Dell'Oro, A. / Fernández-Hernández, J. / Galluccio, L. / García-Lario, P. / Garcia-Reinaldos, M. / González-Núñez, J. / Gosset, E. / Haigron, R. / Halbwachs, J. -L. / Hambly, N. C. / Harrison, D. L. / Hatzidimitriou, D. / Heiter, U. / Hernández, J. / Hestroffer, D. / Hodgkin, S. T. / Holl, B. / Janßen, K. / de Fombelle, G. Jevardat / Jordan, S. / Krone-Martins, A. / Lanzafame, A. C. / o}ffler, W. L\"{ / Lorca, A. / Manteiga, M. / Marchal, O. / Marrese, P. M. / Moitinho, A. / Mora, A. / Muinonen, K. / Osborne, P. / Pancino, E. / Pauwels, T. / Petit, J. -M. / Recio-Blanco, A. / Richards, P. J. / Riello, M. / Rimoldini, L. / Robin, A. C. / Roegiers, T. / Rybizki, J. / Sarro, L. M. / Siopis, C. / Smith, M. / Sozzetti, A. / Ulla, A. / Utrilla, E. / van Leeuwen, M. / van Reeven, W. / Abbas, U. / Aramburu, A. Abreu / Accart, S. / Aerts, C. / Aguado, J. J. / Ajaj, M. / Altavilla, G. / Álvarez, M. A. / Cid-Fuentes, J. Álvarez / Alves, J. / Anderson, R. I. / Varela, E. Anglada / Antoja, T. / Audard, M. / Baines, D. / Baker, S. G. / Balaguer-Núñez, L. / Balbinot, E. / Balog, Z. / Barache, C. / Barbato, D. / Barros, M. / Barstow, M. A. / Bartolomé, S. / Bassilana, J. -L. / Bauchet, N. / Baudesson-Stella, A. / Becciani, U. / Bellazzini, M. / Bernet, M. / Bertone, S. / Bianchi, L. / Blanco-Cuaresma, S. / Boch, T. / Bombrun, A. / Bossini, D. / Bouquillon, S. / Bragaglia, A. / Bramante, L. / Breedt, E. / Bressan, A. / Brouillet, N. / Bucciarelli, B. / Burlacu, A. / Busonero, D. / Butkevich, A. G. / Buzzi, R. / Caffau, E. / Cancelliere, R. / Cánovas, H. / Cantat-Gaudin, T. / Carballo, R. / Carlucci, T. / Carnerero, M. I / Carrasco, J. M. / Casamiquela, L. / Castellani, M. / Castro-Ginard, A. / Sampol, P. Castro / Chaoul, L. / Charlot, P. / Chemin, L. / Chiavassa, A. / Cioni, M. -R. L. / Comoretto, G. / Cooper, W. J. / Cornez, T. / Cowell, S. / Crifo, F. / Crosta, M. / Crowley, C. / Dafonte, C. / Dapergolas, A. / David, M. / David, P. / de Laverny, P. / De Luise, F. / De March, R. / De Ridder, J. / de Souza, R. / de Teodoro, P. / de Torres, A. / del Peloso, E. F. / del Pozo, E. / Delbo, M. / Delgado, A. / Delgado, H. E. / Delisle, J. -B. / Di Matteo, P. / Diakite, S. / Diener, C. / Distefano, E. / Dolding, C. / Eappachen, D. / Edvardsson, B. / Enke, H. / Esquej, P. / Fabre, C. / Fabrizio, M. / Faigler, S. / Fedorets, G. / Fernique, P. / Fienga, A. / Figueras, F. / Fouron, C. / Fragkoudi, F. / Fraile, E. / Franke, F. / Gai, M. / Garabato, D. / Garcia-Gutierrez, A. / García-Torres, M. / Garofalo, A. / Gavras, P. / Gerlach, E. / Geyer, R. / Giacobbe, P. / Gilmore, G. / Girona, S. / Giuffrida, G. / Gomel, R. / Gomez, A. / Gonzalez-Santamaria, I. / González-Vidal, J. J. / Granvik, M. / Gutiérrez-Sánchez, R. / Guy, L. P. / Hauser, M. / Haywood, M. / Helmi, A. / Hidalgo, S. L. / Hilger, T. / Hładczuk, N. / Hobbs, D. / Holland, G. / Huckle, H. E. / Jasniewicz, G. / Jonker, P. G. / Campillo, J. Juaristi / Julbe, F. / Karbevska, L. / Kervella, P. / Khanna, S. / Kochoska, A. / Kontizas, M. / Kordopatis, G. / Korn, A. J. / Kostrzewa-Rutkowska, Z. / Kruszyńska, K. / Lambert, S. / Lanza, A. F. / Lasne, Y. / Campion, J. -F. Le / Fustec, Y. Le / Lebreton, Y. / Lebzelter, T. / Leccia, S. / Leclerc, N. / Lecoeur-Taibi, I. / Liao, S. / Licata, E. / Lindstrøm, H. E. P. / Lister, T. A. / Livanou, E. / Lobel, A. / Pardo, P. Madrero / Managau, S. / Mann, R. G. / Marchant, J. M. / Marconi, M. / Santos, M. M. S. Marcos / Marinoni, S. / Marocco, F. / Marshall, D. J. / Polo, L. Martin / Martín-Fleitas, J. M. / Masip, A. / Massari, D. / Mastrobuono-Battisti, A. / Mazeh, T. / McMillan, P. J. / Messina, S. / Michalik, D. / Millar, N. R. / Mints, A. / Molina, D. / Molinaro, R. / Molnár, L. / Montegriffo, P. / Mor, R. / Morbidelli, R. / Morel, T. / Morris, D. / Mulone, A. F. / Munoz, D. / Muraveva, T. / Murphy, C. P. / Musella, I. / Noval, L. / Ordénovic, C. / Orrù, G. / Osinde, J. / Pagani, C. / Pagano, I. / Palaversa, L. / Palicio, P. A. / Panahi, A. / Pawlak, M. / Esteller, X. Peñalosa / a}, A. Penttil\"{ / Piersimoni, A. M. / Pineau, F. -X. / Plachy, E. / Plum, G. / Poggio, E. / Poretti, E. / Poujoulet, E. / Prša, A. / Pulone, L. / Racero, E. / Ragaini, S. / Rainer, M. / Raiteri, C. M. / Rambaux, N. / Ramos, P. / Ramos-Lerate, M. / Fiorentin, P. Re / Regibo, S. / Reylé, C. / Ripepi, V. / Riva, A. / Rixon, G. / Robichon, N. / Robin, C. / Roelens, M. / Rohrbasser, L. / Romero-Gómez, M. / Rowell, N. / Royer, F. / Rybicki, K. A. / Sadowski, G. / Sellés, A. Sagristà / Sahlmann, J. / Salgado, J. / Salguero, E. / Samaras, N. / Gimenez, V. Sanchez / Sanna, N. / Santoveña, R. / Sarasso, M. / Schultheis, M. / Sciacca, E. / Segol, M. / Segovia, J. C. / Ségransan, D. / Semeux, D. / Shahaf, S. / Siddiqui, H. I. / Siebert, A. / Siltala, L. / Slezak, E. / Smart, R. L. / Solano, E. / Solitro, F. / Souami, D. / Souchay, J. / Spagna, A. / Spoto, F. / Steele, I. A. / u}ller, H. Steidelm\"{ / Stephenson, C. A. / u}veges, M. S\"{ / Szabados, L. / Szegedi-Elek, E. / Taris, F. / Tauran, G. / Taylor, M. B. / Teixeira, R. / Thuillot, W. / Tonello, N. / Torra, F. / Torra, J. / Turon, C. / Unger, N. / Vaillant, M. / van Dillen, E. / Vanel, O. / Vecchiato, A. / Viala, Y. / Vicente, D. / Voutsinas, S. / Weiler, M. / Wevers, T. / Wyrzykowski, Ł. / Yoldas, A. / Yvard, P. / Zhao, H. / Zorec, J. / Zucker, S. / Zurbach, C. / Zwitter, T.

    Summary of the contents and survey properties

    2020  

    Abstract: We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Gaia EDR3 contains ... ...

    Abstract We present the early installment of the third Gaia data release, Gaia EDR3, consisting of astrometry and photometry for 1.8 billion sources brighter than magnitude 21, complemented with the list of radial velocities from Gaia DR2. Gaia EDR3 contains celestial positions and the apparent brightness in G for approximately 1.8 billion sources. For 1.5 billion of those sources, parallaxes, proper motions, and the (G_BP-G_RP) colour are also available. The passbands for G, G_BP, and G_RP are provided as part of the release. For ease of use, the 7 million radial velocities from Gaia DR2 are included in this release, after the removal of a small number of spurious values. New radial velocities will appear as part of Gaia DR3. Finally, Gaia EDR3 represents an updated materialisation of the celestial reference frame (CRF) in the optical, the Gaia-CRF3, which is based solely on extragalactic sources. The creation of the source list for Gaia EDR3 includes enhancements that make it more robust with respect to high proper motion stars, and the disturbing effects of spurious and partially resolved sources. The source list is largely the same as that for Gaia DR2, but it does feature new sources and there are some notable changes. The source list will not change for Gaia DR3. Gaia EDR3 represents a significant advance over Gaia DR2, with parallax precisions increased by 30 percent, proper motion precisions increased by a factor of 2, and the systematic errors in the astrometry suppressed by 30--40 percent for the parallaxes and by a factor ~2.5 for the proper motions. The photometry also features increased precision, but above all much better homogeneity across colour, magnitude, and celestial position. A single passband for G, G_BP, and G_RP is valid over the entire magnitude and colour range, with no systematics above the 1 percent level.

    Comment: Accepted for A&A Special Issue on Gaia EDR3, 21 pages, 2 figures. This version includes the updates in the erratum (https://doi.org/10.1051/0004-6361/202039657e)
    Keywords Astrophysics - Astrophysics of Galaxies
    Subject code 302
    Publishing date 2020-12-02
    Publishing country us
    Document type Book ; Online
    Database BASE - Bielefeld Academic Search Engine (life sciences selection)

    Full text online

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    Inter-library loan at ZB MED

    Your chosen title can be delivered directly to ZB MED Cologne location if you are registered as a user at ZB MED Cologne.

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