A 5 × 10<sup>9</sup> M<sub>⊙</sub> BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY

Walsh, Jonelle L.; Bosch, Remco C. E. van den; Gebhardt, Karl; Yıldırım, Akın; Richstone, D. O.; Gültekin, Kayhan; Husemann, B.

doi:10.3847/0004-637x/817/1/2

Cited by 61 publications

(101 citation statements)

References 88 publications

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“…Intriguingly, while the median M bh /M sph ratio has increased, two points should be made. As warned by Merritt (2013), the importance of being able to better resolve the black hole's sphere-of-influence was illustrated with NGC 1277, whose black hole mass measurement dropped by an order of magnitude as the spatial resolution increased by an order of magnitude (van den Bosch et al 2012;Emsellem 2013;Walsh et al 2016;. Second, Batcheldor (2010) and Shankar et al (2016) have suggested that the sample of galaxies with directly measured black hole masses may reflect the upper envelope of points in the M bh -M sph diagram, because it is preferentially galaxies with a bigger black hole and thus a bigger sphere-of-influence that can have their black hole mass measured.…”

Section: Updatesmentioning

confidence: 99%

Galaxy Bulges and Their Massive Black Holes: A Review

Graham

2016

Astrophysics and Space Science Library

122

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With references to both key and oft-forgotten pioneering works, this article starts by presenting a review into how we came to believe in the existence of massive black holes at the centres of galaxies. It then presents the historical development of the near-linear (black hole)-(host spheroid) mass relation, before explaining why this has recently been dramatically revised. Past disagreement over the slope of the (black hole)-(velocity dispersion) relation is also explained, and the discovery of substructure within the (black hole)-(velocity dispersion) diagram is discussed. As the search for the fundamental connection between massive black holes and their host galaxies continues, the competing array of additional black hole mass scaling relations for samples of predominantly inactive galaxies are presented.

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Section: Updatesmentioning

confidence: 99%

Galaxy Bulges and Their Massive Black Holes: A Review

Graham

2016

Astrophysics and Space Science Library

122

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“…A recent example is NGC 1277, where claims of a ∼ 2 × 10 10 M SBH [53] were subsequently found to be too large by factors of 3-5 [46,66]. Indeed, beyond the Local Group, few if any galaxies show evidence for a central increase in the rms stellar velocities on the relevant spatial scales (see Figure 2.5 in [21]).…”

Section: Sbh Demographicsmentioning

confidence: 99%

Evolution of massive black hole binaries in rotating stellar nuclei: Implications for gravitational wave detection

Rasskazov

Merritt

2017

Phys. Rev. D

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We compute the isotropic gravitational wave (GW) background produced by binary supermassive black holes (SBHs) in galactic nuclei. In our model, massive binaries evolve at early times via gravitational-slingshot interaction with nearby stars, and at later times by the emission of GWs. Our expressions for the rate of binary hardening in the "stellar" regime are taken from the recent work of Vasiliev et al., who show that in the non-axisymmetric galaxies expected to form via mergers, stars are supplied to the center at high enough rates to ensure binary coalescence on Gyr timescales. We also include, for the first time, the extra degrees of freedom associated with evolution of the binary's orbital plane; in rotating nuclei, interaction with stars causes the orientation and the eccentricity of a massive binary to change in tandem, leading in some cases to very high eccentricities (e > 0.9) before the binary enters the GW-dominated regime. We argue that previous studies have overestimated the mean ratio of SBH mass to galaxy bulge mass by factors of 2 -3. In the frequency regime currently accessible to pulsar timing arrays (PTAs), our assumptions imply a factor 2 -3 reduction in the characteristic strain compared with the values computed in most recent studies, removing the tension that currently exists between model predictions and the non-detection of GWs.

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“…NGC 1277 and NGC 1271 are two such compact galaxies, with NGC 1277 being widely studied over the last few years (e.g., van den Bosch et al 2012;Emsellem 2013;Walsh et al 2016;Scharwächter et al compact (R e = 2.8 kpc, M ⋆ = 1.6 × 10 11 M ⊙ ), highdispersion (σ ⋆ = 308 km s −1 ) galaxy found through the HET Massive Galaxy Survey. Yıldırım et al (2015) presented wide-field integral-field spectroscopy of Mrk 1216, and constructed axisymmetric Schwarschild models in order to learn about the galaxy's dynamical stellar massto-light ratio and dark matter halo.…”

Section: Introductionmentioning

confidence: 99%

A Black Hole Mass Determination for the Compact Galaxy Mrk 1216

Walsh

Bosch

Gebhardt

et al. 2017

ApJ

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Mrk 1216 is a nearby, early-type galaxy with a small effective radius of 2.8 kpc and a large stellar velocity dispersion of 308 km s −1 for its K-band luminosity of 1.4 × 10 11 L ⊙ . Using integral-field spectroscopy assisted by adaptive optics from Gemini North, we measure spatially resolved stellar kinematics within ∼450 pc of the galaxy nucleus. The galaxy exhibits regular rotation with velocities of ±180 km s −1 and a sharply peaked velocity dispersion profile that reaches 425 km s −1 at the center. We fit axisymmetric, orbit-based dynamical models to the combination of these high angular resolution kinematics, large-scale kinematics extending to roughly three effective radii, and Hubble Space Telescope imaging, resulting in a constraint of the mass of the central black hole in Mrk 1216. After exploring several possible sources of systematics that commonly affect stellar-dynamical black hole mass measurements, we find a black hole mass of M BH = (4.9±1.7)×10 9 M ⊙ and a H-band stellar mass-to-light ratio of Υ H = 1.3±0.4 Υ ⊙ (1σ uncertainties). Mrk 1216 is consistent with the local black hole mass -stellar velocity dispersion relation, but is a factor of ∼5 − 10 larger than expectations from the black hole mass -bulge luminosity and black hole mass -bulge mass correlations when conservatively using the galaxy's total luminosity or stellar mass. This behavior is quite similar to the extensively studied compact galaxy NGC 1277. Resembling the z ∼ 2 quiescent galaxies, Mrk 1216 may be a passively evolved descendant, and perhaps reflects a previous era when galaxies contained over-massive black holes relative to their bulge luminosities/masses, and the growth of host galaxies had yet to catch up.

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A 5 × 10⁹ M_⊙ BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY

Cited by 61 publications

References 88 publications

Galaxy Bulges and Their Massive Black Holes: A Review

Galaxy Bulges and Their Massive Black Holes: A Review

Evolution of massive black hole binaries in rotating stellar nuclei: Implications for gravitational wave detection

A Black Hole Mass Determination for the Compact Galaxy Mrk 1216

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A 5 × 109 M⊙ BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY

Cited by 61 publications

References 88 publications

Galaxy Bulges and Their Massive Black Holes: A Review

Galaxy Bulges and Their Massive Black Holes: A Review

Evolution of massive black hole binaries in rotating stellar nuclei: Implications for gravitational wave detection

A Black Hole Mass Determination for the Compact Galaxy Mrk 1216

Contact Info

Product

Resources

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A 5 × 10⁹ M_⊙ BLACK HOLE IN NGC 1277 FROM ADAPTIVE OPTICS SPECTROSCOPY