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Difference from Background: Limit of Detection01:05

Difference from Background: Limit of Detection

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The limit of detection (LOD) is the smallest amount of analyte that can be distinguished from the background noise. The LOD value corresponds to the concentration at which the analyte signal is three times larger than the standard deviation of the blank signal. Below this value, the analyte signal cannot be differentiated from the background noise. It is calculated by dividing the calibration slope by 3 times the standard deviation of the blank signals.
The LOD indicates the presence or absence...
7.9K
Detection of Black Holes01:10

Detection of Black Holes

2.4K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
2.4K
Atomic Emission Spectroscopy: Interference01:30

Atomic Emission Spectroscopy: Interference

511
In atomic emission spectroscopy (AES), high-temperature atomizers excite a broad range of elements and molecules that generate complex emissions from sources such as oxides, hydroxides, and flame combustion products in the flame or plasma. Several strategies can be employed to minimize spectral interferences caused by overlapping emission lines or bands. These include increasing instrument resolution, choosing alternative emission lines, optimally placing the detector in low-background regions,...
511
Emission Spectra02:39

Emission Spectra

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When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
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Atomic Emission Spectroscopy: Lab01:29

Atomic Emission Spectroscopy: Lab

469
AES is a powerful analytical technique, especially effective when used with plasma sources, producing abundant spectra in characteristic emission lines. The Inductively Coupled Plasma (ICP), in particular, yields superior quantitative analytical data due to its high stability, low noise, low background, and minimal interferences under optimal experimental conditions. However, newer air-operated microwave sources are emerging as promising alternatives that could be more cost-effective than...
469
Atomic Emission Spectroscopy: Instrumentation01:22

Atomic Emission Spectroscopy: Instrumentation

1.0K
The instrumentation of atomic emission spectrometry (AES) involves various components, including atomization devices that convert samples into gas-phase atoms and ions. There are two main types of atomization devices: continuous and discrete atomizers.  Continuous atomizers, like plasmas and flames, introduce samples in a constant stream, while discrete atomizers inject individual samples using syringes or autosamplers. The most common discrete atomizer is the electrothermal atomizer.
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Related Experiment Video

Updated: Dec 17, 2025

Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
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Surface Mapping of Earth-like Exoplanets using Single Point Light Curves

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Testing the Sensitivity of the Galactic Center Excess to the Point Source Mask.

Yi-Ming Zhong1, Samuel D McDermott2, Ilias Cholis3

  • 1Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA.

Physical Review Letters
|July 1, 2020
PubMed
Summary
This summary is machine-generated.

The Fermi Large Area Telescope

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Area of Science:

  • Astrophysics
  • Gamma-ray astronomy

Background:

  • The Galactic Center exhibits an excess of gamma rays in Fermi-LAT data.
  • The Fermi Large Area Telescope (Fermi-LAT) has released an updated point source catalog (4FGL).

Purpose of the Study:

  • To investigate the nature of the Galactic Center excess using the new 4FGL catalog.
  • To assess the contribution of point sources to the observed gamma-ray excess.

Main Methods:

  • Performed the first template fit utilizing a mask based on the 4FGL catalog.
  • Searched for point sources and masked them out to analyze remaining emission.

Main Results:

  • The gamma-ray excess at the Galactic Center persists even with the 4FGL catalog mask.
  • Masking 4FGL point sources eliminates a sizable excess of bright pixels in the inner Galaxy.
  • Identified bright sources lacking known counterparts.

Conclusions:

  • Point sources have a restricted ability to account for the Galactic Center excess.
  • Strong constraints are placed on point source luminosity functions that could explain the smooth emission.