A ∼50,000
                    <i>M</i>
                    <sub>⊙</sub>
                    SOLAR MASS BLACK HOLE IN THE NUCLEUS OF RGG 118

Baldassare, Vivienne; Reines, Amy E.; Gallo, Elena; Greene, Jenny E.

doi:10.1088/2041-8205/809/1/l14

Cited by 222 publications

(249 citation statements)

References 47 publications

Supporting

Mentioning

236

Contrasting

Order By: Relevance

“…The isolation of the system, however, implies that whatever morphological changes Was 49b underwent happened during the beginning of its encounter with Was 49a, and so it has not been severely tidally stripped (unlike, for example, the SMBH-hosting ultracompact dwarf galaxy M60-UCD1; Seth et al 2014), suggesting that the SMBH was intrinsically overmassive or that perhaps the black hole's growth during the early phase of the merger happened well before the buildup of its host galaxy (e.g., Medling et al 2015; see also the Discussion in van Loon & Sansom 2015). If Was 49b was originally a late-type/dwarf galaxy, its SMBH is a factor of 10 2 -10 4 as massive as other black holes found in this galaxy type, which are typically between 10 4 and 10 6   M (e.g., Filippenko & Ho 2003;Barth et al 2004;Izotov & Thuan 2008;Shields et al 2008;Reines et al 2011Reines et al , 2013Dong et al 2012;Secrest et al 2012Secrest et al , 2013Secrest et al , 2015Maksym et al 2014;Moran et al 2014;Baldassare et al 2015Baldassare et al , 2016Mezcua et al 2016;Satyapal et al 2016), potentially giving new insight into how SMBHs form and grow in isolated systems. For example, recent work has suggested that black hole mass growth at higher redshifts precedes bulge growth (e.g., Zhang et al 2012), while other work has found no such effect (e.g., Schulze & Wisotzki 2014).…”

Section: Discussionmentioning

confidence: 99%

Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?

Secrest

Schmitt

Blecha

et al. 2017

ApJ

View full text Add to dashboard Cite

We present a combined morphological and X-ray analysis of Was49, an isolated, dual-AGN system notable for the presence of a dominant AGN, Was 49b, in the disk of the primary galaxy, Was 49a, at a projected radial distance of 8kpc from the nucleus. Using X-ray data from Chandra, the Nuclear Spectroscopic Telescope Array, and Swift, we find that this AGN has a bolometric luminosity of L bol ∼ 10 45 erg s −1 , with a black hole mass of. Despite the large mass, our analysis of optical data from the Discovery Channel Telescope shows that the supermassive black hole (SMBH) is hosted by a stellar counterpart with a mass of only , which makes the SMBH potentially larger than expected from SMBH-galaxy scaling relations, and the stellar counterpart exhibits a morphology that is consistent with dwarf elliptical galaxies. Our analysis of the system in the r and K bands indicates that Was49 is a minor merger, with the mass ratio of Was 49b to Was 49a between ∼1:7 and ∼1:15. This is in contrast with findings that the most luminous merger-triggered AGNs are found in major mergers and that minor mergers predominantly enhance AGN activity in the primary galaxy.

show abstract

Section: Discussionmentioning

confidence: 99%

Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?

Secrest

Schmitt

Blecha

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…4, for the (M BH -M sph ) relation. Y on X-axis regression, dashed lines: symmetric regression), the data that the authors used to obtain them as triangles with error bars (black/gray for ellipticals/spirals), the empty diamonds are two other IMBH candidates (LEDA87300: e.g., Baldassare et al 2015;Graham et al 2016 and Pox52: e.g., Barth et al 2004;Thornton et al 2008;Ciambur 2016), and the colored data points are our results. The green stars come from the Sérsic index, the blue squares from pitch angle and the red circles from the FP-BH.…”

Section: Discussionmentioning

confidence: 99%

Searching for intermediate-mass black holes in galaxies with low-luminosity AGN: a multiple-method approach

Koliopanos

Ciambur

Graham

et al. 2017

A&A

View full text Add to dashboard Cite

Aims. This work is the first stage of a campaign to search for intermediate-mass black holes (IMBHs) in low-luminosity active galactic nuclei (LLAGN) and dwarf galaxies. An additional and equally important aim of this pilot study is to investigate the consistency between the predictions of several popular black hole scaling relations and the fundamental plane (FP) of black-hole activity (FP-BH). Methods. We used well established X-ray and radio luminosity relations in accreting black holes, along with the latest scaling relations between the mass of the central black hole (M BH ) and the properties of its host spheroid, to predict M BH in seven LLAGN, that were previously reported to be in the IMBH regime. Namely, we used the recently re-evaluated M BH − M sph (M sph : spheroid absolute magnitude at 3.6 µm) scaling relation for spiral galaxies, the M BH − n sph (n sph : major axis Sérsic index of the spheroid component) relation, the M BH − PA (PA: spiral pitch angle) relation, and a recently re-calibrated version of the FP-BH for weakly accreting BHs, to independently estimate M BH in all seven galaxies. Results. We find that all LLAGN in our list have low-mass central black holes with log M BH /M ≈ 6.5 on average, but that they are, most likely, not IMBHs. All four methods used predicted consistent BH masses in the 1σ range. Furthermore, we report that, in contrast to previous classification, galaxy NGC 4470 is bulge-less, and we also cast doubts on the AGN classification of NGC 3507. Conclusions. We find that our latest, state-of-the-art techniques for bulge magnitude & Sérsic index computations and the most recent updates of the M BH − L sph , M BH − n sph , and M BH − PA relations and the FP-BH produce consistent results in the low-mass regime. We thus establish a multiple-method approach for predicting BH masses in the regime where their spheres of gravitational influence cannot be spatially resolved. Our approach mitigates against outliers from any one relation and provides a more robust average prediction. We will use our new method to revisit more IMBH candidates in LLAGN.

show abstract

“…The handful of identified dwarf IMBH lie on the usual M BH − σ scaling relation, where M BH is the black hole mass and σ is the dwarf stellar velocity dispersion. However these same dwarfs fall below the M BH −M * scaling relation where M * is the stellar mass (Baldassare et al 2015;Reines & Volonteri 2015). One can possibly interpret this as IMBH-induced suppression of star formation in dwarfs that occurred in the early gas-rich phase of dwarf evolution.…”

Section: Introductionmentioning

confidence: 90%

“…Active galactic nuclei are found in about 1% of dwarfs, with the x-ray luminosities well in excess of an x-ray binary contribution as predicted from the star formation rate (Baldassare et al 2016). For any reasonable duty cycle, there must be IMBH in at least 10% of dwarfs, and one cannot exclude a larger fraction because of the special circumstances required for the shallow gravitational potentials of dwarfs to retain gas as effectively as their massive counterparts.…”

Section: Introductionmentioning

confidence: 99%

Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

Silk¹

2017

ApJL

109

View full text Add to dashboard Cite

Could there be intermediate mass black holes in essentially all old dwarf galaxies? I argue that current observations of Active Galactic Nuclei in dwarfs allow such a radical hypothesis which provides early feedback and potentially provides a unifying explanation for many if not all of the apparent dwarf galaxy anomalies, such as the abundance, core-cusp, "too big to fail", ultra-faint and baryon-fraction issues. I describe the supporting arguments, which are largely circumstantial in nature, and discuss a number of tests. There is no strong motivation for modifying the nature of cold dark matter in order to explain any of the dwarf galaxy "problems".

show abstract

A ∼50,000 M _⊙ SOLAR MASS BLACK HOLE IN THE NUCLEUS OF RGG 118

Cited by 222 publications

References 47 publications

Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?

Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?

Searching for intermediate-mass black holes in galaxies with low-luminosity AGN: a multiple-method approach

Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

Contact Info

Product

Resources

About

A ∼50,000 M ⊙ SOLAR MASS BLACK HOLE IN THE NUCLEUS OF RGG 118

Cited by 222 publications

References 47 publications

Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?

Was 49b: An Overmassive AGN in a Merging Dwarf Galaxy?

Searching for intermediate-mass black holes in galaxies with low-luminosity AGN: a multiple-method approach

Feedback by Massive Black Holes in Gas-rich Dwarf Galaxies

Contact Info

Product

Resources

About

A ∼50,000 M _⊙ SOLAR MASS BLACK HOLE IN THE NUCLEUS OF RGG 118