The Cepheid distance to the narrow-line Seyfert 1 galaxy NGC 4051
Autor: | R. W. Pogge, C. J. Grier, Gagandeep S. Anand, Wenlong Yuan, G. De Rosa, Bradley M. Peterson, E. Dalla Bontà, Misty C. Bentz, Marianne Vestergaard, Laura Ferrarese, Lucas M. Macri, Ric Davies, E. K. S. Hicks, Thaisa Storchi-Bergmann, Adam G. Riess, Michael Fausnaugh, Christopher A. Onken, S. L. Hoffmann |
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Jazyk: | angličtina |
Rok vydání: | 2021 |
Předmět: |
Cepheid variable stars
Cepheid variable Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Hubble space telescope Hubble Space Telescope Astrophysics::Solar and Stellar Astrophysics HST photometry Astrophysics::Galaxy Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) AGN host galaxies Line (formation) Physics distance measure Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Galaxy Cepheid distance near infrared astronomy Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) time series analysis galaxy distances distance indicators |
Popis: | We derive a distance of $D = 16.6 \pm 0.3$~Mpc ($\mu=31.10\pm0.04$~mag) to the archetypal narrow-line Seyfert 1 galaxy NGC 4051 based on Cepheid Period--Luminosity relations and new Hubble Space Telescope multiband imaging. We identify 419 Cepheid candidates and estimate the distance at both optical and near-infrared wavelengths using subsamples of precisely-photometered variables (123 and 47 in the optical and near-infrared subsamples, respectively). We compare our independent photometric procedures and distance-estimation methods to those used by the SH0ES team and find agreement to 0.01~mag. The distance we obtain suggests an Eddington ratio $\dot{m} \approx 0.2$ for NGC 4051, typical of narrow-line Seyfert 1 galaxies, unlike the seemingly-odd value implied by previous distance estimates. We derive a peculiar velocity of $-490\pm34$~km~s$^{-1}$ for NGC 4051, consistent with the overall motion of the Ursa Major Cluster in which it resides. We also revisit the energetics of the NGC 4051 nucleus, including its outflow and mass accretion rates. Comment: 15 pages, 12 figures, 6 tables, accepted for publication in ApJ |
Databáze: | OpenAIRE |
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