Observational Selection Bias Affecting the Determination of the Extragalactic Distance Scale

Teerikorpi, P.

doi:10.1146/annurev.astro.35.1.101

Cited by 102 publications

(89 citation statements)

References 73 publications

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“…The median deviates from the line of the equal distance starting from about 100 pc and this deviation increases toward the larger distances. This trend is in the sense expected from the Malmquist bias of the 2nd kind (Teerikorpi 1997), due to the magnitude limit which at a fixed true distance cuts away stars from the faint side of the luminosity function. (Hill et al 1982) and HIPPARCOS distances for the stars in the NGP area.…”

Section: Distance Estimatesmentioning

confidence: 54%

Interstellar polarization at high galactic latitudes from distant stars

Berdyugin¹,

Teerikorpi²,

Haikala³

et al. 2001

A&A

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Abstract. We present a catalog of interstellar polarization measurements for the North Galactic Pole area (b > 70 • ). Our list contains 336 stars of spectral classes from A to K for which the linear polarization has been measured by us and other researchers. The data are useful for investigation of the distribution of dust, to estimate the amount of interstellar extinction and to map Galactic magnetic field at high galactic latitudes. We discuss also the data selection, sampling and completeness of the catalog.

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Section: Distance Estimatesmentioning

confidence: 54%

Interstellar polarization at high galactic latitudes from distant stars

Berdyugin¹,

Teerikorpi²,

Haikala³

et al. 2001

A&A

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“…It is caused to the fact that faint galaxies are missing in the sample because of the limiting apparent magnitude (see the review paper by Teerikorpi 1997). To reach large distances with limited bias, we have to consider only intrinsically bright galaxies.…”

Section: Selection Of Primary Calibratorsmentioning

confidence: 99%

“…Two methods exist to detect unbiased galaxies: the method of normalized distances (Bottinelli et al 1986) and the Spaenhauer diagram (Spaenhauer 1978) used by Sandage (1994). A detailed discussion about these methods is given by Teerikorpi (1997). In the case of galaxies which are sosie of a same calibrator, both diagrams are equivalent.…”

Section: Correction For the Malmquist Biasmentioning

confidence: 99%

Local velocity field from sosie galaxies

Terry

Paturel

Ekholm

2002

A&A

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Abstract. Pratton et al. (1997) showed that the velocity field around clusters could generate an apparent distortion that appears as tangential structures or radial filaments. In the present paper we determine the parameters of the Peebles' model (1976) describing infall of galaxies onto clusters with the aim of testing quantitatively the amplitude of this distortion. The distances are determined from the concept of sosie galaxies (Paturel 1984) using 21 calibrators for which the distances were recently calculated from two independent Cepheid calibrations. We use both B and I-band magnitudes. The Spaenhauer diagram method is used to correct for the Malmquist bias. We give the equations for the construction of this diagram. We analyze the apparent Hubble constant in different regions around Virgo and obtain simultaneously the Local Group infall and the unperturbed Hubble constant. We found:The front side and backside infalls can be seen around Virgo and Fornax. In the direction of Virgo the comparison is made with the Peebles' model. We obtain:with C Virgo = 2800 for Virgo and C Fornax = 1350 for Fornax, with the adopted units (km s −1 and Mpc). We obtain the following mean distance moduli:µ Virgo = 31.3 ± 0.2 r = 18 Mpc µ Fornax = 31.7 ± 0.3 r = 22 Mpc .All these quantities form an accurate and coherent system.

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“…However, it has been convincingly shown that such deviations from linearity are easily produced by the Malmquist bias in magnitude limited samples [201,202,194] and when one by-passes this problem using suitable methods, the linearity is recovered. The second main advancement is concerned with measurement of the value of the Hubble constant H 0 .…”

Section: Observed Hubble Lawmentioning

confidence: 99%

Scale-invariance of galaxy clustering

1998

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Some years ago we proposed a new approach to the analysis of galaxy and cluster correlations based on the concepts and methods of modern statistical Physics. This led to the surprising result that galaxy correlations are fractal and not homogeneous up to the limits of the available catalogs. The usual statistical methods, which are based on the assumption of homogeneity, are therefore inconsistent for all the length scales probed so far, and a new, more general, conceptual framework is necessary to identifythe real physical properties of these structures. In the last few years the 3-d catalogs have been significatively improved and we have extended our methods to the analysis of number counts and angular catalogs. This has led to a complete analysis of all the available data that we present in this review. The result is that galaxy structures are highly irregular and self-similar: all the available data are consistent with each other and show fractal correlations (with dimension $D \simeq 2$) up to the deepest scales probed so far ($1000 \hmp$) and even more as indicated from the new interpretation of the number counts. The evidence for scale-invariance of galaxy clustering is very strong up to $150 \hmp$ due to the statistical robustness of the data but becomes progressively weaker (statistically) at larger distances due to the limited data. In These facts lead to fascinating conceptual implications about our knowledge of the universe and to a new scenario for the theoretical challenge in this field.Comment: Latex file 165 pages, 106 postscript figures. This paper is also available at http://www.phys.uniroma1.it/DOCS/PIL/pil.html To appear in Physics Report (Dec. 1997

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Observational Selection Bias Affecting the Determination of the Extragalactic Distance Scale

Cited by 102 publications

References 73 publications

Interstellar polarization at high galactic latitudes from distant stars

Interstellar polarization at high galactic latitudes from distant stars

Local velocity field from sosie galaxies

Scale-invariance of galaxy clustering

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