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Title:
The Stellar Halo of M104. I. A Survey for Planetary Nebulae and the Planetary Nebula Luminosity Function Distance
Authors:
Ford, H. C.; Hui, X.; Ciardullo, R.; Jacoby, G. H.; Freeman, K. C.
Publication:
Astrophysical Journal v.458, p.455 (ApJ Homepage)
Publication Date:
02/1996
Origin:
APJ
Astronomy Keywords:
COSMOLOGY: DISTANCE SCALE, GALAXIES: CLUSTERS: INDIVIDUAL NAME: VIRGO, GALAXIES: DISTANCES AND REDSHIFTS, GALAXIES: INDIVIDUAL MESSIER NUMBER: M104, GALAXIES: STELLAR CONTENT, ISM: PLANETARY NEBULAE: GENERAL
DOI:
10.1086/176828
Bibliographic Code:
1996ApJ...458..455F

Abstract

We used the CTIO 4 m telescope to make a complete and kinematically unbiased survey of M 104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9±0.6 Mpc to the galaxy. The luminosity-specific PN number alpha2.5 in the halo of M104 is approximately 21.7 × 10-9 Lsun, which for its color (B-V) = 0.95, is comparable to the values in other galaxies.

We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M 104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H0 = 91±8 km s-1 Mpc-1. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall.

The values of H0 for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster The unweighted mean of the four values is H0 = 84±4. The value of H0 derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.


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