Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/30710
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Graham, Alister W. | en_US |
dc.contributor.author | Durré, Mark | en_US |
dc.contributor.author | Savorgnan, Giulia A. D. | en_US |
dc.contributor.author | Medling, Anne M. | en_US |
dc.contributor.author | Batcheldor, Dan | en_US |
dc.contributor.author | Scott, Nicholas | en_US |
dc.contributor.author | Watson, Beverly | en_US |
dc.contributor.author | Marconi, Alessandro | en_US |
dc.date.accessioned | 2021-03-15T12:39:58Z | - |
dc.date.available | 2021-03-15T12:39:58Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30710 | - |
dc.description.abstract | The identification of galaxies with “overly massive” black holes requires two measurements: a black hole mass (M<SUB>bh</SUB>) and a host spheroid mass ({M}<SUB>{{sph,\ast </SUB>}}). Here we provide our measurements for NGC 1277. Our structural decomposition reveals that NGC 1277 is dominated by a “classical” spheroid with a Sérsic index n = 5.3, a half-light radius {R}<SUB>{{e,major</SUB>}}=2.1 {{kpc}}, and a stellar mass of 2.7× {10}<SUP>11</SUP>\quad {M}<SUB>☉ </SUB> (using {M}<SUB>*</SUB>/{L}<SUB>V</SUB>=11.65, Martín-Navarro et al.). This mass is an order of magnitude greater than originally reported. Using the latest M<SUB>bh</SUB>-n, M<SUB>bh</SUB>-{M}<SUB>{{sph,\ast </SUB>}}, and M<SUB>bh</SUB>-σ relations, the expected black hole mass is, respectively, ({0.57}<SUB>-0.40</SUB><SUP>+1.29</SUP>)× {10}<SUP>9</SUP>\quad {M}<SUB>☉ </SUB>, ({1.58}<SUB>-1.13</SUB><SUP>+4.04</SUP>)× {10}<SUP>9</SUP>\quad {M}<SUB>☉ </SUB>, and ({2.27}<SUB>-1.44</SUB><SUP>+4.04</SUP>)× {10}<SUP>9</SUP>\quad {M}<SUB>☉ </SUB> (using σ = 300 km s<SUP>-1</SUP>) for which the “sphere-of-influence” is 0.″31. Our new kinematical maps obtained from laser guide star assisted, adaptive optics on the Keck I Telescope dramatically reaffirm the presence of the inner, nearly edge-on, disk seen in the galaxy image. We also report that this produces a large velocity shear (∼400 km s<SUP>-1</SUP>) across the inner 0.″2 (70 pc) plus elevated values of \sqrt{{σ }<SUP>2</SUP>+{V}<SUP>2</SUP>} across the inner (+/- 3\buildrel{\prime\prime}\over{.} 8)× (+/- 0\buildrel{\prime\prime}\over{.} 6) region of the galaxy. Our new multi-Gaussian expansion (MGE) models and Jeans Anisotropic MGE analysis struggled to match this extended component. Our optimal black hole mass, albeit a probable upper limit because of the disk is 1.2 × 10<SUP>9</SUP> M<SUB>☉</SUB> (M/{L}<SUB>V</SUB>=12.3). This is an order of magnitude smaller than originally reported and 4 times smaller than recently reported. It gives an {M}<SUB>{{bh</SUB>}}/{M}<SUB>{{sph,\ast </SUB>}} ratio of 0.45% in agreement with the median (≈0.5%) and range (0.1%-5.0%) observed in non-dwarf, early-type galaxies. This result highlights the need for caution with inner disks. | en_US |
dc.language.iso | eng | en_US |
dc.title | A Normal Supermassive Black Hole in NGC 1277 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0004-637X/819/1/43 | en_US |
dc.identifier.scopus | 2-s2.0-84960983639 | en_US |
dc.identifier.isi | 000372303400043 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-637X/819/1/43 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 819 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 43 | 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 | 2016ApJ...819...43G | 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_8 Formation and evolution of galaxies | 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.languageiso639-1 | en | - |
item.grantfulltext | open | - |
item.openairetype | Article | - |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | O.A. Arcetri | - |
crisitem.author.orcid | 0000-0002-9889-4238 | - |
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