Show simple item record

dc.contributor.authorBeifiori, A.
dc.contributor.authorSarzi, M.
dc.contributor.authorCorsini, E.M.
dc.contributor.authorBonta, E.D.
dc.contributor.authorPizzella, A.
dc.contributor.authorCoccato, L.
dc.contributor.authorBertola, F.
dc.identifier.citationBeifiori , A , Sarzi , M , Corsini , E M , Bonta , E D , Pizzella , A , Coccato , L & Bertola , F 2009 , ' Upper limits on the masses of 105 supermassive black holes from Hubble Space Telescope / space telescope imaging spectrograph archival data ' , The Astrophysical Journal , vol. 692 , no. 1 , pp. 856-868 .
dc.identifier.otherPURE: 152098
dc.identifier.otherPURE UUID: 5386e878-f721-4bc3-951b-b0a9e561e373
dc.identifier.otherdspace: 2299/2994
dc.identifier.otherScopus: 66649107986
dc.descriptionOriginal article can be found at: Copyright American Astronomical Society. DOI: 10.1088/0004-637X/692/1/856 [Full text of this article is not available in the UHRA]
dc.description.abstractBased on the modeling of the central emission-line width measured over subarcsecond apertures with the Hubble Space Telescope, we present stringent upper bounds on the mass of the central supermassive black hole, M •, for a sample of 105 nearby galaxies (D < 100 Mpc) spanning a wide range of Hubble types (E–Sc) and values of the central stellar velocity dispersion, σc (58-419 km s–1). For the vast majority of the objects, the derived M • upper limits run parallel and above the well-known M •-σc relation independently of the galaxy distance, suggesting that our nebular line-width measurements trace rather well the nuclear gravitational potential. For values of σc between 90 and 220 km s–1, 68% of our upper limits falls immediately above the M •-σc relation without exceeding the expected M • values by more than a factor 4.1. No systematic trends or offsets are observed in this σc range as a function of the galaxy Hubble type or with respect to the presence of a bar. For 6 of our 12 M • upper limits with σc <90 km s–1, our line-width measurements are more sensitive to the stellar contribution to the gravitational potential, either due to the presence of a nuclear stellar cluster or because of a greater distance compared to the other galaxies at the low-σc end of the M •-σc relation. Conversely, our M • upper bounds appear to lie closer to the expected M • in the most massive elliptical galaxies with values of σc above 220 km s–1. Such a flattening of the M •-σc relation at its high-σc end would appear consistent with a coevolution of supermassive black holes and galaxies driven by dry mergers, although better and more consistent measurements for σc and K-band luminosity are needed for these kinds of objects before systematic effects can be ruled out.en
dc.relation.ispartofThe Astrophysical Journal
dc.subjectblack hole physics
dc.titleUpper limits on the masses of 105 supermassive black holes from Hubble Space Telescope / space telescope imaging spectrograph archival dataen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionScience & Technology Research Institute
dc.description.statusPeer reviewed
rioxxterms.typeJournal Article/Review

Files in this item


There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record