Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/29080
Titolo: | A NuSTAR view of powerful γ-ray loud blazars | Autori: | GHISELLINI, Gabriele PERRI, Matteo Costamante, L. TAGLIAFERRI, Gianpiero Sbarrato, Tullia Campitiello, S. Madejski, G. TAVECCHIO, Fabrizio GHIRLANDA, Giancarlo |
Data pubblicazione: | 2019 | Rivista: | ASTRONOMY & ASTROPHYSICS | Numero: | 627 | Abstract: | We observed three blazars at z > 2 with the NuSTAR satellite. These were detected in the γ-rays by Fermi/LAT and in the soft X-rays, but have not yet been observed above 10 keV. The flux and slope of their X-ray continuum, together with Fermi/LAT data allows us to estimate their total electromagnetic output and peak frequency. For some of them we were able to study the source in different states, and investigate the main cause of the different observed spectral energy distribution. We then collected all blazars at redshifts greater than 2 observed by NuSTAR, and confirm that these hard and luminous X-ray blazars are among the most powerful persistent sources in the Universe. We confirm the relation between the jet power and the disk luminosity, extending it at the high-energy end. | URI: | http://hdl.handle.net/20.500.12386/29080 | URL: | https://www.aanda.org/articles/aa/abs/2019/07/aa35750-19/aa35750-19.html | ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201935750 | Bibcode ADS: | 2019A&A...627A..72G | Fulltext: | open |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
File in questo documento:
File | Descrizione | Dimensioni | Formato | |
---|---|---|---|---|
A-NuSTAR-view2019.pdf | A NuSTAR view | 779.78 kB | Adobe PDF | Visualizza/apri |
A-NuSTAR-view2019.pdf | PDF editoriale | 779.78 kB | Adobe PDF | Visualizza/apri |
Page view(s)
55
controllato il 25-mag-2024
Download(s)
27
controllato il 25-mag-2024
Google ScholarTM
Check
Altmetric
Altmetric
Tutti i documenti in DSpace sono pubblicati ad Accesso Aperto, salvo diversa indicazione per alcuni documenti specifici.