HARD X-RAY MORPHOLOGICAL AND SPECTRAL STUDIES OF THE GALACTIC CENTER MOLECULAR CLOUD SGR B2: CONSTRAINING PAST SGR A<SUP>☆</SUP> FLARING ACTIVITY

Simple item page
dc.contributor.authorZhang, Shuo
dc.contributor.authorHailey, Charles J.
dc.contributor.authorMori, Kaya
dc.contributor.authorClavel, Maica
dc.contributor.authorTerrier, Regis
dc.contributor.authorPonti, Gabriele
dc.contributor.authorGoldwurm, Andrea
dc.contributor.authorBauer, Franz E.
dc.contributor.authorBoggs, Steven E.
dc.contributor.authorChristensen, Finn E.
dc.contributor.authorCraig, William W.
dc.contributor.authorHarrison, Fiona A.
dc.contributor.authorHong, Jaesub
dc.contributor.authorNynka, Melania
dc.contributor.authorSoldi, Simona
dc.contributor.authorStern, Daniel
dc.contributor.authorTomsick, John A.
dc.contributor.authorZhang, William W.
dc.date.accessioned2025-01-23T21:32:46Z
dc.date.available2025-01-23T21:32:46Z
dc.date.issued2015
dc.description.abstractIn 2013, NuSTAR observed the Sgr B2 region and for the first time resolved its hard X-ray emission on subarcminute scales. Two prominent features are detected above 10 keV:. a newly emerging cloud, G0.66-0.13, and the central 90 '' radius region containing two compact cores, Sgr B2(M) and Sgr B2(N), surrounded by diffuse emission. It is inconclusive whether the remaining level of Sgr. B2 emission is still decreasing or has reached a constant background level. A decreasing X-ray emission can be best explained by the X-ray reflection nebula scenario, where the cloud reprocesses a past giant outburst from Sgr A(star). In the X-ray reflection nebula (XRN) scenario, the 3-79 keV Sgr. B2 spectrum allows us to self-consistently test the XRN model using both the Fe K alpha line and the continuum emission. The peak luminosity of the past Sgr A(star) outburst is constrained to L3-79keV similar to 5 x 10(38) ergs s(-1). A newly discovered cloud feature, G0.66-0.13, shows different timing variability. We suggest that it could be a molecular clump located in the Sgr B2 envelope reflecting the same Sgr A(star) outburst. In contrast, if the Sgr. B2 X-ray emission has reached a constant background level, it would imply an origin of low-energy cosmic-ray (CR) proton bombardment. In this scenario, from the NuSTAR measurements we infer a CR ion power of dW/dt = (1 - 4) x 10(39) erg s(-1) and a CR ionization rate of zeta(H) = (6 - 10) x 10(-15) H-1 s(-1). measurements can become powerful tools to constrain the GC CR population.
dc.fuente.origenWOS
dc.identifier.doi10.1088/0004-637X/815/2/132
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.1088/0004-637X/815/2/132
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/101500
dc.identifier.wosidWOS:000367151300052
dc.issue.numero2
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectGalaxy: center
dc.subjectISM: clouds
dc.subjectX-rays: individual (Sgr B2)
dc.subjectX-rays: ISM
dc.titleHARD X-RAY MORPHOLOGICAL AND SPECTRAL STUDIES OF THE GALACTIC CENTER MOLECULAR CLOUD SGR B2: CONSTRAINING PAST SGR A<SUP>☆</SUP> FLARING ACTIVITY
dc.typeartículo
dc.volumen815
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas