A new method of spectra acquisition and exact mass determination of resolved peaks in high mass resolution ion microscopy

1988 ◽  
Vol 11 (4) ◽  
pp. 189-197 ◽  
Author(s):  
N. A. Thorne ◽  
F. Degrève
Keyword(s):  
Mass Resolution ◽  
New Method ◽  
High Mass ◽  
Mass Determination ◽  
Exact Mass ◽  
High Mass Resolution ◽  
Ion Microscopy

scholarly journals Concurrent Determination of U‐Pb Age and REE Mass Fractions of Zircon by High Mass Resolution SIMS

2020 ◽  
Vol 44 (3) ◽  
pp. 421-437
Author(s):  
Yu Liu ◽  
Qiu‐Li Li ◽  
Guo‐Qiang Tang ◽  
Xian‐Hua Li
Keyword(s):  
Mass Resolution ◽  
High Mass ◽  
High Mass Resolution ◽  
Mass Fractions

Simultaneous quantitative determination of the distribution of dopants in silicon by high mass resolution secondary ion mass spectrometry

1989 ◽  
Vol 61 (5) ◽  
pp. 412-416 ◽  
Author(s):  
Gerhard. Stingeder ◽  
Kurt. Piplits ◽  
Stefan. Gara ◽  
Manfred. Grasserbauer ◽  
Matthias. Budil ◽  
...  
Keyword(s):  
Mass Spectrometry ◽  
Quantitative Determination ◽  
Secondary Ion Mass Spectrometry ◽  
Mass Resolution ◽  
High Mass ◽  
High Mass Resolution ◽  
Ion Mass Spectrometry ◽  
Secondary Ion

scholarly journals Hipparcos, Three Years After Launch

1993 ◽  
Vol 156 ◽  
pp. 1-10
Author(s):  
J. Kovalevsky ◽  
M. Froeschlé
Keyword(s):  
Standard Error ◽  
Present Status ◽  
Double Star ◽  
New Method ◽  
Standard Errors ◽  
First Year ◽  
Mass Determination ◽  
Mission Duration ◽  
The Mean

In a first part, the present status of the HIPPARCOS mission is described. Despite the degradations and failures of gyroscopes, it is still hoped that a 4 1/2 mission duration will be reached. The first-year of data has been reduced by both FAST and NDAC consortia. For the best 46200 observed stars, the distribution of standard errors in positions has a maximum of 1.5 mas in latitude and 1.8 mas in longitude and the mean standard error for parallaxes is of the order of 3 mas. The comparison of results obtained by both consortia shows that the differences are small and quite consistent with the announced internal precisions. Magnitude measurements are precise to 0.02 magnitude for a 4 second observation. The precision to be expected for double star observations is also given. The main new result is that the magnitudes of the components are obtained with a few hundredths of a magnitude precision. This allows to devise a new method of mass determination based upon the parallax and a recalibrated mass-luminosity diagram. The parallax dependence of the results is much more favourable than in the case of the classical determination of masses using orbital motions.

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