The Cepheid Distance to the Seyfert 1 Galaxy NGC 4151

Yuan, Wenlong; Fausnaugh, Michael; Hoffmann, Samantha; Macri, Lucas M.; Peterson, B. M.; Riess, Adam G.; Bentz, Misty C.; Brown, J. S.; Bontà, E. Dalla; Davies, R. I.; Rosa, Gisella De; Ferrarese, Laura; Grier, C. J.; Hicks, E. K. S.; Onken, Christopher A.; Pogge, Richard W.; Storchi‐Bergmann, Thaisa; Vestergaard, M.

doi:10.3847/1538-4357/abb377

Cited by 39 publications

(28 citation statements)

References 70 publications

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“…Onken et al (2014) found M BH = (3.76 ± 1.15) × 10 7 M but assumed a distance of D = 13.9 Mpc. When adjusted for the recently published Cepheid distance to NGC 4151 of D = 15.8 ± 0.4 Mpc (Yuan et al 2020), their best-fit mass becomes M BH = (4.27±1.31)× 10 7 M . Our range of M BH values is somewhat lower, which may be attributed to a somewhat lower velocity dispersion σ in the central parts inferred from our reanalysis of the observational data.…”

Section: Comparison With Previous Resultsmentioning

confidence: 98%

The Black Hole Mass of NGC 4151 from Stellar Dynamical Modeling

Roberts,

Bentz,

Vasiliev

et al. 2021

Preprint

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The mass of a supermassive black hole (M BH ) is a fundamental property that can be obtained through observational methods. Constraining M BH through multiple methods for an individual galaxy is important for verifying the accuracy of different techniques, and for investigating the assumptions inherent in each method. However, there exist only a few galaxies where multiple M BH measurement techniques can be applied. NGC 4151 is one of these rare galaxies for which multiple methods can be used: stellar and gas dynamical modeling because of its proximity (D = 15.8 ± 0.4 Mpc from Cepheids), and reverberation mapping because of its active accretion. In this work, we re-analyzed H−band integral field spectroscopy of the nucleus of NGC 4151 from Gemini NIFS, improving the analysis at several key steps. We then constructed a wide range of axisymmetric dynamical models with the new orbit-superposition code FORSTAND. One of our primary goals is to quantify the systematic uncertainties in M BH arising from different combinations of the deprojected density profile, inclination, intrinsic flattening, and mass-to-light ratio. As a consequence of uncertainties on the stellar luminosity profile arising from the presence of the AGN, our constraints on M BH are rather weak. Models with a steep central cusp are consistent with no black hole; however, in models with more moderate cusps, the black hole mass lies within the range of 0.25 × 10 7 M M BH 3 × 10 7 M . This measurement is somewhat smaller than the earlier analysis presented by Onken et al. ( 2014), but agrees with previous M BH values from gas dynamical modeling and reverberation mapping. Future dynamical modeling of reverberation data, as well as IFU observations with JWST, will aid in further constraining the mass of the central supermassive black hole in NGC 4151.

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Section: Comparison With Previous Resultsmentioning

confidence: 98%

The Black Hole Mass of NGC 4151 from Stellar Dynamical Modeling

Roberts,

Bentz,

Vasiliev

et al. 2021

Preprint

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“…The calculations for M BARY are detailed in Paper I, M DYN and M DM are described in Sec. 6. which found 15.8 ± 0.4 Mpc (Yuan et al 2020b). Almost all of the TF studies underpredict the distance, which seems to be caused by the adoption of an axis ratio of 0.6 when constraining the galaxy inclination.…”

Section: Notes On Individual Objectsmentioning

confidence: 93%

“…Cepheids measurement (Yuan et al 2020a), 5. Cepheids measurement (Yuan et al 2020b), 6. Cepheids measurement (Bentz et al 2019), 7.…”

Section: Notes On Individual Objectsmentioning

confidence: 99%

Tully-Fisher Distances and Dynamical Mass Constraints for 24 Host Galaxies of Reverberation-Mapped AGN

Robinson,

Bentz,

Courtois

et al. 2021

Preprint

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We present Tully-Fisher distances for 24 AGN host galaxies with black hole mass (M BH ) measurements from reverberation mapping, as well as the first calibration of the V −band Tully-Fisher relation. Combining our measurements of HI 21 cm emission with HST and ground-based optical and near-infrared images allows multiple distance measurements for 19 galaxies and single measurements for the remaining 5. Separation of the nucleus from its host galaxy via surface brightness decomposition yields galaxy-only luminosities, thus allowing measurements of the distance moduli free of contamination from the AGN. For 14 AGN hosts, these are the first reported distances independent of redshift, and hence independent of peculiar velocities. For the remaining galaxies, we show good agreement between our distances and those previously reported from surface brightness fluctuations (SBF) and Cepheids. We also determine the total galaxy mass enclosed within the estimated HI radius, which when compared to the baryonic content allows for constraints on the dark matter masses. We find a typical mass fraction of M DM /M DYN = 62%, and find significant correlations between M BH − M DYN and M BH − M DM . Finally, we scale our galaxy radii based on estimated relationships between visible and halo radii and assume a flat rotation curve out to the halo radius to approximate M HALO . Over the range of M BH and M HALO in this sample, we find good agreement with observationally-constrained relationships between M BH and M HALO and with hydrodynamical simulations.

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“…A new search of possible ULPs not classified as ULPs, but present in CC samples was carried out. Ten new candidates were found: two ULPs in M33, Pellerin and Macri [22], five new ULPs in M31 Kodric et al [23], one ULP in Yuan et al [24] and one in Bentz et al [25] (gP1, rP1 and iP1 ULP mean magnitudes obtained by Kodric et al [23] and WFC3 magnitudes by Yuan et al [24] and Bentz et al [25] were converted in the Johnson V and I magnitudes adopting transformation by Tonry et al [26] and Harris [27], respectively). In particular, the five new ULPs in M31 were identified in the framework of the Pandromeda survey [23], with a minimum period of 79.35 d. In the Kodric et al [23] sample are also included the bf two M31 variables by Ngeow et al [18], but 8-1498 (with period longer than 80 days) is listed as unclassified.…”

Section: Literature Samplesmentioning

confidence: 99%

“…The metal abundances of the all M31 ULPs are obtained from their position [19,23,32], taking into account the metallicity gradient of this galaxy derived in the framework of the PHAT survey [33]. Distances for NGC 4151 and NGC 6814 are those derived by Yuan et al [24] and Bentz et al [25], respectively. For NGC 4151, in the literature, there is no reliable metallicity determination, whereas NGC 6814 has approximately a solar average abundance [34].…”

Section: Literature Samplesmentioning

confidence: 99%

Ultra Long Period Cepheids: Observation and Theory

Musella

2022

Universe

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Ultra Long Period Cepheids are becoming a very interesting and important topic thanks to the contribution that they can give to understanding the current tension existing between the early-universe and local Hubble constant measurements. These bright pulsating variables are observable up to cosmological distances (larger than 100 Mpc) allowing us, in principle, to measure the Hubble constant without the need for secondary indicators, thus reducing the possible systematic errors in the calibration of the extragalactic distance scale. The Ultra Long Period Cepheids also represent a useful tool for obtaining information on the star formation history of the host galaxy and a challenge for the evolutionary and pulsational models, particularly in the very metal poor regime. In this paper, the largest known ULP sample, consisting of 72 objects, including 10 new candidates, is analyzed to give an observational and theoretical overview of their role as distance indicators and of their evolutionary properties.

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The Cepheid Distance to the Seyfert 1 Galaxy NGC 4151

Cited by 39 publications

References 70 publications

The Black Hole Mass of NGC 4151 from Stellar Dynamical Modeling

The Black Hole Mass of NGC 4151 from Stellar Dynamical Modeling

Tully-Fisher Distances and Dynamical Mass Constraints for 24 Host Galaxies of Reverberation-Mapped AGN

Ultra Long Period Cepheids: Observation and Theory

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