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NEON AND $[{\rm{C}}\,{\rm{II}}]$ 158 μ m EMISSION LINE PROFILES IN DUSTY STARBURSTS AND ACTIVE GALACTIC NUCLEI

Sujet: galaxies: active, galaxies: distances and redshifts, galaxies: starburst, infrared: galaxies, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]
Auteur: Samsonyan, Anahit, Weedman, Daniel, Lebouteiller, Vianney, Barry, Donald, Sargsyan, Lusine
Résumé: A sample of 379 extragalactic sources is presented that has mid-infrared, high-resolution spectroscopy from the Spitzer Infrared Spectrograph (IRS) and also spectroscopy of the [C II] 158 μm line from the Herschel Photodetector Array Camera and Spectrometer (PACS). The emission line profiles of [Ne II] 12.81 μm, [Ne III] 15.55 μm, and [C II] 158 μm are presented, and intrinsic line widths are determined (full width half maximum of Gaussian profiles after instrumental correction). All line profiles, together with overlays comparing the positions of PACS and IRS observations, are made available in the Cornell Atlas of Spitzer IRS Sources. Sources are classified from active galactic nucleus (AGN) to starburst based on equivalent widths of the 6.2 μm polycyclic aromatic hydrocarbon feature. It is found that intrinsic line widths do not change among classifications for [C II], with median widths of 207 km s-1 for AGNs, 248 km s-1 for composites, and 233 km s-1 for starbursts. The [Ne II] line widths also do not change with classification, but [Ne III] lines are progressively broader from starburst to AGN. A few objects with unusually broad lines or unusual redshift differences in any feature are identified.
Source: info:eu-repo/semantics/altIdentifier/doi/10.3847/0067-0049/226/1/11
Editeur: HAL CCSD, American Astronomical Society