Effect of Noise Crosscorrelation for a Narrow‐Band Masking Noise on the Detection of a Tonal Signal

1964 ◽  
Vol 36 (5) ◽  
pp. 1042-1042
Author(s):  
Ted L. Langford ◽  
Lloyd A. Jeffress
Keyword(s):  
Narrow Band ◽  
Tonal Signal ◽  
Masking Noise

Stimulus, Response, and Observer Variables in the Auditory Screening of Newborn Infants

1970 ◽  
Vol 13 (1) ◽  
pp. 9-18 ◽  
Author(s):  
Daniel Ling ◽  
Agnes H. Ling ◽  
Donald G. Doehring
Keyword(s):  
High Frequency ◽  
Narrow Band ◽  
Newborn Infants ◽  
Response Strength ◽  
Whole Body ◽  
Stimulus Response ◽  
Narrow Band Noise ◽  
Band Noise ◽  
Masking Noise ◽  
Infant Screening

Behavioral responses of 144 healthy neonates to actual and simulated presentations of three different high-frequency sounds of 85 dB SPL were studied. Stimuli were a narrow-band noise centered at 2000 Hz, a narrow-band noise centered at 3150 Hz, and a pure tone increasing and decreasing in frequency between 2000 and 4000 Hz. A masking noise which prevented knowledge of stimulus events was presented to one member of each observer pair. Results indicated that an observer’s judgments of infant behavior may be significantly influenced by knowledge of stimulus events. More responses were observed with the narrow-band noise centered at 2000 Hz; the most frequently observed responses were strong whole-body movements. A decrement in response strength tended to occur with repeated stimulation. Neither positive nor false positive responses were related to sex, anomalies, gestation period, birth weight, age at test, or body temperature. The inherent complexities of infant screening are discussed in relation to a signal detection paradigm.

Statistical analysis of classification

1966 ◽  
Vol 24 ◽  
pp. 188-189
Author(s):  
T. J. Deeming
Keyword(s):  
Multivariate Analysis ◽  
Statistical Analysis ◽  
Classification Scheme ◽  
Analytical Procedure ◽  
Narrow Band ◽  
Scientific Research ◽  
Maximum Amount ◽  
Amount Of Information

If we make a set of measurements, such as narrow-band or multicolour photo-electric measurements, which are designed to improve a scheme of classification, and in particular if they are designed to extend the number of dimensions of classification, i.e. the number of classification parameters, then some important problems of analytical procedure arise. First, it is important not to reproduce the errors of the classification scheme which we are trying to improve. Second, when trying to extend the number of dimensions of classification we have little or nothing with which to test the validity of the new parameters.Problems similar to these have occurred in other areas of scientific research (notably psychology and education) and the branch of Statistics called Multivariate Analysis has been developed to deal with them. The techniques of this subject are largely unknown to astronomers, but, if carefully applied, they should at the very least ensure that the astronomer gets the maximum amount of information out of his data and does not waste his time looking for information which is not there. More optimistically, these techniques are potentially capable of indicating the number of classification parameters necessary and giving specific formulas for computing them, as well as pinpointing those particular measurements which are most crucial for determining the classification parameters.

Photo-electric Hβ and uvby photometry

1966 ◽  
Vol 24 ◽  
pp. 170-180
Author(s):  
D. L. Crawford
Keyword(s):  
Narrow Band ◽  
Line Strength ◽  
Interference Filter ◽  
B Stars ◽  
Relative Line ◽  
The Mean ◽  
F Stars ◽  
Two Parameters ◽  
Filter Photometry ◽  
The Continuum

Early in the 1950's Strömgren (1, 2, 3, 4, 5) introduced medium to narrow-band interference filter photometry at the McDonald Observatory. He used six interference filters to obtain two parameters of astrophysical interest. These parameters he calledlandc, for line and continuum hydrogen absorption. The first measured empirically the absorption line strength of Hβby means of a filter of half width 35Å centered on Hβand compared to the mean of two filters situated in the continuum near Hβ. The second index measured empirically the Balmer discontinuity by means of a filter situated below the Balmer discontinuity and two above it. He showed that these two indices could accurately predict the spectral type and luminosity of both B stars and A and F stars. He later derived (6) an indexmfrom the same filters. This index was a measure of the relative line blanketing near 4100Å compared to two filters above 4500Å. These three indices confirmed earlier work by many people, including Lindblad and Becker. References to this earlier work and to the systems discussed today can be found in Strömgren's article inBasic Astronomical Data(7).

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