Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30189
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Mori, Kaya | en_US |
dc.contributor.author | Hailey, Charles J. | en_US |
dc.contributor.author | Krivonos, Roman | en_US |
dc.contributor.author | Hong, Jaesub | en_US |
dc.contributor.author | PONTI, GABRIELE | en_US |
dc.contributor.author | Bauer, Franz | en_US |
dc.contributor.author | Perez, Kerstin | en_US |
dc.contributor.author | Nynka, Melania | en_US |
dc.contributor.author | Zhang, Shuo | en_US |
dc.contributor.author | Tomsick, John A. | en_US |
dc.contributor.author | Alexander, David M. | en_US |
dc.contributor.author | Baganoff, Frederick K. | en_US |
dc.contributor.author | Barret, Didier | en_US |
dc.contributor.author | Barrière, Nicolas | en_US |
dc.contributor.author | Boggs, Steven E. | en_US |
dc.contributor.author | Canipe, Alicia M. | en_US |
dc.contributor.author | Christensen, Finn E. | en_US |
dc.contributor.author | Craig, William W. | en_US |
dc.contributor.author | Forster, Karl | en_US |
dc.contributor.author | Giommi, Paolo | en_US |
dc.contributor.author | Grefenstette, Brian W. | en_US |
dc.contributor.author | Grindlay, Jonathan E. | en_US |
dc.contributor.author | Harrison, Fiona A. | en_US |
dc.contributor.author | Hornstrup, Allan | en_US |
dc.contributor.author | Kitaguchi, Takao | en_US |
dc.contributor.author | Koglin, Jason E. | en_US |
dc.contributor.author | Luu, Vy | en_US |
dc.contributor.author | Madsen, Kristen K. | en_US |
dc.contributor.author | Mao, Peter H. | en_US |
dc.contributor.author | Miyasaka, Hiromasa | en_US |
dc.contributor.author | PERRI, Matteo | en_US |
dc.contributor.author | Pivovaroff, Michael J. | en_US |
dc.contributor.author | Puccetti, Simonetta | en_US |
dc.contributor.author | Rana, Vikram | en_US |
dc.contributor.author | Stern, Daniel | en_US |
dc.contributor.author | Westergaard, Niels J. | en_US |
dc.contributor.author | Zhang, William W. | en_US |
dc.contributor.author | Zoglauer, Andreas | en_US |
dc.date.accessioned | 2021-02-03T10:30:19Z | - |
dc.date.available | 2021-02-03T10:30:19Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30189 | - |
dc.description.abstract | We present the first sub-arcminute images of the Galactic Center above 10 keV, obtained with NuSTAR. NuSTAR resolves the hard X-ray source IGR J17456-2901 into non-thermal X-ray filaments, molecular clouds, point sources, and a previously unknown central component of hard X-ray emission (CHXE). NuSTAR detects four non-thermal X-ray filaments, extending the detection of their power-law spectra with Γ ∼ 1.3-2.3 up to ∼50 keV. A morphological and spectral study of the filaments suggests that their origin may be heterogeneous, where previous studies suggested a common origin in young pulsar wind nebulae (PWNe). NuSTAR detects non-thermal X-ray continuum emission spatially correlated with the 6.4 keV Fe Kα fluorescence line emission associated with two Sgr A molecular clouds: MC1 and the Bridge. Broadband X-ray spectral analysis with a Monte-Carlo based X-ray reflection model self-consistently determined their intrinsic column density (∼10^23 cm^-2), primary X-ray spectra (power-laws with Γ ∼ 2) and set a lower limit of the X-ray luminosity of Sir A* flare illuminating the Sgr A clouds to L_X ≳ 10^38 erg s^-1. Above ∼20 keV, hard X-ray emission in the central 10 pc region around Sgr A* consists of the candidate PWN G359.95-0.04 and the CHXE, possibly resulting from an unresolved population of massive CVs with white dwarf masses M_WD ∼ 0.9 M_☉. Spectral energy distribution analysis suggests that G359.95-0.04 is likely the hard X-ray counterpart of the ultra-high gamma-ray source HESS J1745-290, strongly favoring a leptonic origin of the GC TeV emission. | en_US |
dc.language.iso | eng | en_US |
dc.title | NuSTAR Hard X-Ray Survey of the Galactic Center Region I: Hard X-Ray Morphology and Spectroscopy of the Diffuse Emission | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1088/0004-637X/814/2/94 | en_US |
dc.identifier.scopus | 2-s2.0-84948770091 | en_US |
dc.identifier.isi | 000365317300012 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.1088/0004-637X/814/2/94 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 814 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 94 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015ApJ...814...94M | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_10 High energy and particle astronomy – X-rays, cosmic rays, gamma rays, neutrinos | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0003-0293-3608 | - |
crisitem.author.orcid | 0000-0003-3613-4409 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
1510.04631.pdf | postprint | 4.25 MB | Adobe PDF | View/Open |
Mori_2015_ApJ_814_94.pdf | Pdf editoriale | 4.41 MB | Adobe PDF | View/Open |
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