Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30706
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Savorgnan, Giulia A. D. | en_US |
dc.contributor.author | Graham, Alister W. | en_US |
dc.contributor.author | Marconi, Alessandro | en_US |
dc.contributor.author | Sani, Eleonora | en_US |
dc.date.accessioned | 2021-03-15T12:32:11Z | - |
dc.date.available | 2021-03-15T12:32:11Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30706 | - |
dc.description.abstract | In our first paper, we performed a detailed (I.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, M<SUB>BH</SUB>, imaged at 3.6 μ {{m}} with Spitzer. Our sample is the largest to date and, for the first time, the decompositions were checked for consistency with the galaxy kinematics. We present correlations between M<SUB>BH</SUB> and the host spheroid (and galaxy) luminosity, L<SUB>sph</SUB> (and L<SUB>gal</SUB>), and also stellar mass, {M}<SUB>*,{sph</SUB>}. While most previous studies have used galaxy samples that were overwhelmingly dominated by high-mass, early-type galaxies, our sample includes 17 spiral galaxies, half of which have {M}<SUB>{BH</SUB>}\lt {10}<SUP>7</SUP> {M}<SUB>☉ </SUB>, and allows us to better investigate the poorly studied low-mass end of the {M}<SUB>{BH</SUB>}{--}{M}<SUB>*,{sph</SUB>} correlation. The bulges of early-type galaxies follow {M}<SUB>{BH</SUB>} \propto \{M}<SUB>*,{sph</SUB>}<SUP>1.04+/- 0.10</SUP> and define a tight red sequence with intrinsic scatter {∊ }<SUB>({M</SUB><SUB>{BH</SUB>}| {M}<SUB>*,{sph</SUB>})}\quad =\quad 0.43\quad +/- \quad 0.06 {dex} and a median {M}<SUB>{BH</SUB>}/{M}<SUB>*,{sph</SUB>} ratio of 0.68 ± 0.04%, I.e., a +/- 2σ range of 0.1%-5%. At the low-mass end, the bulges of late-type galaxies define a much steeper blue sequence, with {M}<SUB>{BH</SUB>} \propto {M}<SUB>*,{sph</SUB>}<SUP>2-3</SUP> and {M}<SUB>{BH</SUB>}/{M}<SUB>*,{sph</SUB>} equal to 0.02% at {M}<SUB>{BH</SUB>} ≈ {10}<SUP>6</SUP> {M}<SUB>☉ </SUB>. We additionally report that (1) our Sérsic galaxy sample follows {M}<SUB>{BH</SUB>} \propto \{M}<SUB>*,{sph</SUB>}<SUP>1.48+/- 0.20</SUP>, a less steep sequence than previously reported; (2) bulges with Sérsic index {n}<SUB>{sph</SUB>}\lt 2, argued by some to be pseudo-bulges, are not offset to lower M<SUB>BH</SUB> from the correlation defined by the current bulge sample with {n}<SUB>{sph</SUB>}\gt 2; and (3) L<SUB>sph</SUB> and L<SUB>gal</SUB> correlate equally well with M<SUB>BH</SUB>, in terms of intrinsic scatter, only for early-type galaxies—once reasonable numbers of spiral galaxies are included, the correlation with L<SUB>sph</SUB> is better than that with Lgal. | en_US |
dc.language.iso | eng | en_US |
dc.title | Supermassive Black Holes and Their Host Spheroids. II. The Red and Blue Sequence in the MBH-M*,sph Diagram | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0004-637X/817/1/21 | en_US |
dc.identifier.scopus | 2-s2.0-84955441722 | en_US |
dc.identifier.isi | 000368872400021 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-637X/817/1/21 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 817 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 21 | 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...817...21S | 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 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
Savorgnan_2016_ApJ_817_21.pdf | PDF editoriale | 638.92 kB | Adobe PDF | View/Open |
Page view(s)
45
checked on Aug 27, 2024
Download(s)
15
checked on Aug 27, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.