A New Cepheid Distance to the Maser‐Host Galaxy NGC 4258 and Its Implications for the Hubble Constant

Macri, Lucas M.; Stanek, K. Z.; Bersier, D.; Greenhill, L. J.; Reid, M. J.

doi:10.1086/508530

Cited by 303 publications

(487 citation statements)

References 63 publications

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“…In fact, Cepheids have proved to be extremely useful and robust to determine distances to LMC using as reference direct distance determinations to other galaxies. Macri et al (2006) used the Cepheids in NGC 4258, which has a direct maser-based distance (Herrnstein et al 1999), to determine a distance modulus to LMC that is almost identical to the EB value. It follows that the derived distances using EBs are not only fully compatible among themselves, but also with other direct distance determination methods.…”

Section: The Distance To M 31mentioning

confidence: 99%

The distance to the Andromeda galaxy from eclipsing binaries

Vilardell¹,

Ribas²,

Jordi³

et al. 2010

A&A

112

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The cosmic distance scale largely depends on distance determinations to galaxies of the Local Group. In this sense, the Andromeda galaxy (M 31) is a key rung to better constrain the cosmic distance ladder. A project was started in 1999 to firmly establish a direct and accurate distance to M 31 using eclipsing binaries (EBs). After the determination of the first direct distance to M 31 from EBs, the second direct distance to an EB system is presented: M31V J00443610+4129194. Light and radial velocity curves were obtained and fitted to derive the masses and radii of the components. The acquired spectra were combined and disentangled to determine the temperature of the components. The analysis of the studied EB resulted in a distance determination to M 31 of (m − M) 0 = 24.30 ± 0.11 mag. This result, when combined with the previous distance determination to M 31, results in a distance modulus of (m − M) 0 = 24.36 ± 0.08 mag (744 ± 33 kpc), fully compatible with other distance determinations to M 31. With an error of only 4%, the obtained value firmly establishes the distance to this important galaxy and represents the fulfillment of the main goal of our project.

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Section: The Distance To M 31mentioning

confidence: 99%

The distance to the Andromeda galaxy from eclipsing binaries

Vilardell¹,

Ribas²,

Jordi³

et al. 2010

A&A

112

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show abstract

“…Herrnstein et al (1999) obtained the distance of this galaxy by fitting a simple kinematic model to the maser radial velocities and VLBI proper motions (7.3 ± 0.4 Mpc). The Cepheid distance is 7.5 ± 0.3 Mpc (Macri et al 2006). In addition, HST trigonometric parallaxes for a sample of Cepheids have become available (Benedict et al 2007), confirming the Key Project period-luminosity calibration, as shown in Figure 25.…”

Section: Measurement Of the Hubble Constantmentioning

confidence: 88%

Measuring the Hubble Constant With the Hubble Space Telescope

Freedman¹,

Kennicutt²,

Mould³

2009

Proc. IAU

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Ten years ago our team completed the Hubble Space Telescope Key Project on the extragalactic distance scale. Cepheids were detected in some 25 galaxies and used to calibrate four secondary distance indicators that reach out into the expansion field beyond the noise of galaxy peculiar velocities. The result was H0 = 72 ± 8 km s−1 Mpc−1 and put an end to galaxy distances uncertain by a factor of two. This work has been awarded the Gruber Prize in Cosmology for 2009.

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“…Here, we describe some of the refinements to the basic model. The distance determined from the accelerations and proper motions of the maser features under the assumption † Present address: 60 Garden Street, MS-42, Cambridge, MA 02138 USA of circular orbits is 7.2 ± 0.5 Mpc ; compare cepheid distance of 7.5 ±0.25 Mpc for an LMC distance of 50 kpc by Macri et al, 2007). At this (maser distance) 1 mas = 0.035 pc = 1.1 × 10 17 cm.…”

Section: Introductionmentioning

confidence: 93%

The structure of the accretion disk in NGC 4258

Moran¹,

Humphreys²,

Greenhill³

et al. 2007

Proc. IAU

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Abstract. A wealth of new information about the structure of the maser disk in NGC 4258 has been obtained from a series of 18 VLBA observations spanning three years, as well as from 32 additional epochs of spectral monitoring data from 1994 to the present, acquired with the VLA, Effelsberg, and GBT. The warp of the disk has been defined precisely. The thickness of the maser disk has been measured to be 12 microarcseconds (FWHM), which is slightly smaller than previously quoted upper limits. Under the assumption that the masers trace the true vertical distribution of material in the disk, from the condition of hydrostatic equilibrium the sound speed is 1.5 km s −1 , corresponding to a thermal temperature of 600K. The accelerations of the high velocity maser components have been accurately measured for many features on both the blue and red side of the spectrum. The azimuthal offsets of these masers from the midline (the line through the disk in the plane of the sky) and derived projected offsets from the midline based on the warp model correspond well with the measured offsets. This result suggests that the masers are well described as discrete clumps of masing gas, which accurately trace the Keplerian motion of the disk. However, we have continued to search for evidence of apparent motions caused by "phase effects." This work provides the foundation for refining the estimate of the distance to NGC 4258 through measurements of feature acceleration and proper motion. The refined estimate of this distance is expected to be announced in the near future.

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A New Cepheid Distance to the Maser‐Host Galaxy NGC 4258 and Its Implications for the Hubble Constant

Cited by 303 publications

References 63 publications

The distance to the Andromeda galaxy from eclipsing binaries

The distance to the Andromeda galaxy from eclipsing binaries

Measuring the Hubble Constant With the Hubble Space Telescope

The structure of the accretion disk in NGC 4258

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