Jove
Visualize
Contact Us
JoVE
x logofacebook logolinkedin logoyoutube logo
ABOUT JoVE
OverviewLeadershipBlogJoVE Help Center
AUTHORS
Publishing ProcessEditorial BoardScope & PoliciesPeer ReviewFAQSubmit
LIBRARIANS
TestimonialsSubscriptionsAccessResourcesLibrary Advisory BoardFAQ
RESEARCH
JoVE JournalMethods CollectionsJoVE Encyclopedia of ExperimentsArchive
EDUCATION
JoVE CoreJoVE BusinessJoVE Science EducationJoVE Lab ManualFaculty Resource CenterFaculty Site
Terms & Conditions of Use
Privacy Policy
Policies

Related Concept Videos

Distribution of Molecular Speeds01:27

Distribution of Molecular Speeds

6.0K
The motion of molecules in a gas is random in magnitude and direction for individual molecules, but a gas of many molecules has a predictable distribution of molecular speeds. This predictable distribution of molecular speeds is known as the Maxwell-Boltzmann distribution. The distribution of molecular speeds in liquids is comparable to that of gases but not identical and can help to understand the phenomenon of the boiling and vapor pressure of a liquid. Consider that a molecule requires a...
6.0K
Doppler Effect - II01:05

Doppler Effect - II

5.1K
The Doppler effect has several practical, real-world applications. For instance, meteorologists use Doppler radars to interpret weather events based on the Doppler effect. Typically, a transmitter emits radio waves at a specific frequency toward the sky from a weather station. The radio waves bounce off the clouds and precipitation and travel back to the weather station. The radio frequency of the waves reflected back to the station appears to decrease if the clouds or precipitation are moving...
5.1K
Doppler Effect - I00:56

Doppler Effect - I

6.9K
The Doppler effect and Doppler shift were named after the Austrian physicist and mathematician Christian Johann Doppler in 1842, who conducted experiments with both moving sources and moving observers. Consider an observer standing on a street corner, observing an ambulance with a siren sound passing by at a constant speed. The observer experiences two characteristic changes in the sound of the siren. Initially, the sound increases in loudness as the ambulance approaches and decreases in...
6.9K
IR Spectroscopy: Hooke's Law Approximation of Molecular Vibration01:16

IR Spectroscopy: Hooke's Law Approximation of Molecular Vibration

3.6K
A covalently bonded heteronuclear diatomic molecule can be modeled as two vibrating masses connected by a spring. The vibrational frequency of the bond can be expressed using an equation derived from Hooke's law, which describes how the force applied to stretch or compress a spring is proportional to the displacement of the spring. In this case, the atoms behave like masses, and the bond acts like a spring.
According to Hooke's law, the vibrational frequency is directly proportional to...
3.6K
UV–Vis Spectroscopy: Molecular Electronic Transitions01:16

UV–Vis Spectroscopy: Molecular Electronic Transitions

3.5K
In Ultraviolet–Visible (UV–Vis) spectroscopy, the absorption of electromagnetic radiation is used to probe the electronic structure of molecules. This technique provides insights into molecular electronic transitions, particularly the movement of electrons between different molecular orbitals. Radiation is absorbed if the energy of the electromagnetic radiation passing through the molecule is precisely equal to the energy difference between the excited and ground states. During this...
3.5K
IR Spectroscopy: Molecular Vibration Overview01:24

IR Spectroscopy: Molecular Vibration Overview

6.0K
When Infrared (IR) radiation passes through a covalently bonded molecule, the bonds transition from lower to higher vibrational levels. The fundamental vibrational motions that result in infrared absorption can be classified as stretching or bending vibrations.
Stretching vibrations are vibrational motions that occur along the bond line, changing the bond length or distance between two bonded atoms. They are further distinguished as symmetric or asymmetric. In symmetric stretching, the...
6.0K

You might also read

Related Articles

Articles linked to this work by shared authors, journal, and citation graph.

Sort by
Same author

Sub-GeV Dark Matter Direct Detection with Neutrino Observatories.

Physical review letters·2025
Same author

TeV Solar Gamma Rays as a Probe for the Solar Internetwork Magnetic Fields.

Physical review letters·2025
Same author

Enhancing DUNE's Solar Neutrino Capabilities with Neutral-Current Detection.

Physical review letters·2025
Same author

Can LIGO Detect Nonannihilating Dark Matter?

Physical review letters·2023
Same author

Toward Powerful Probes of Neutrino Self-Interactions in Supernovae.

Physical review letters·2023
Same author

Low Mass Black Holes from Dark Core Collapse.

Physical review letters·2021
Same journal

Erratum: Bacterial Turbulence at Compressible Fluid Interfaces [Phys. Rev. Lett. 136, 138301 (2026)].

Physical review letters·2026
Same journal

Unveiling Light-Quark Yukawa Flavor Structure via Dihadron Fragmentation at Lepton Colliders.

Physical review letters·2026
Same journal

Adaptable Route to Fast Coherent State Transport via Bang-Bang-Bang Protocols.

Physical review letters·2026
Same journal

Topological Transition and Emergence of Elasticity of Dislocation in Skyrmion Lattice: Beyond Kittel's Magnetic-Polar Analogy.

Physical review letters·2026
Same journal

Pound-Drever-Hall Method for Superconducting-Qubit Readout.

Physical review letters·2026
Same journal

Coupling a ^{73}Ge Nuclear Spin to an Electrostatically Defined Quantum Dot in Silicon.

Physical review letters·2026
See all related articles

Related Experiment Video

Updated: Mar 26, 2026

High-speed Particle Image Velocimetry Near Surfaces
11:59

High-speed Particle Image Velocimetry Near Surfaces

Published on: June 24, 2013

34.0K

Dark Matter Velocity Spectroscopy.

Eric G Speckhard1,2, Kenny C Y Ng1,2, John F Beacom1,2,3

  • 1Center for Cosmology and AstroParticle Physics (CCAPP), Ohio State University, Columbus, Ohio 43210, USA.

Physical Review Letters
|February 6, 2016
PubMed
Summary
This summary is machine-generated.

Velocity spectroscopy can distinguish dark matter signals from astrophysical or instrumental mimics. Upcoming missions like Astro-H will have the precision to use this technique for identifying dark matter decay or annihilation signatures.

More Related Videos

Molecular Beam Mass Spectrometry With Tunable Vacuum Ultraviolet VUV Synchrotron Radiation
09:53

Molecular Beam Mass Spectrometry With Tunable Vacuum Ultraviolet VUV Synchrotron Radiation

Published on: October 30, 2012

13.7K
Quantitative Analysis of Vacuum Induction Melting by Laser-induced Breakdown Spectroscopy
03:49

Quantitative Analysis of Vacuum Induction Melting by Laser-induced Breakdown Spectroscopy

Published on: June 10, 2019

7.7K

Related Experiment Videos

Last Updated: Mar 26, 2026

High-speed Particle Image Velocimetry Near Surfaces
11:59

High-speed Particle Image Velocimetry Near Surfaces

Published on: June 24, 2013

34.0K
Molecular Beam Mass Spectrometry With Tunable Vacuum Ultraviolet VUV Synchrotron Radiation
09:53

Molecular Beam Mass Spectrometry With Tunable Vacuum Ultraviolet VUV Synchrotron Radiation

Published on: October 30, 2012

13.7K
Quantitative Analysis of Vacuum Induction Melting by Laser-induced Breakdown Spectroscopy
03:49

Quantitative Analysis of Vacuum Induction Melting by Laser-induced Breakdown Spectroscopy

Published on: June 10, 2019

7.7K

Area of Science:

  • Astrophysics
  • Particle Physics
  • Cosmology

Background:

  • Dark matter (DM) decays or annihilations may produce distinctive linelike spectra.
  • These signals can be mimicked by astrophysical phenomena or instrumental effects.
  • Distinguishing true DM signals is crucial for understanding DM properties.

Purpose of the Study:

  • To demonstrate how velocity spectroscopy can differentiate between DM signals and background sources.
  • To highlight the potential of upcoming experiments in achieving the necessary energy resolution.
  • To apply this method to a specific case, such as the 3.5-keV line observed in the Milky Way.

Main Methods:

  • Velocity spectroscopy measures energy shifts caused by relative motion between source and observer.
  • This technique allows for the separation of signals based on their kinematic properties.
  • Analysis of spectral line profiles to identify unique velocity signatures.

Main Results:

  • Velocity spectroscopy can effectively separate dark matter signals from astrophysical and instrumental backgrounds with minimal theoretical uncertainty.
  • Upcoming experiments will possess the required energy resolution for precise velocity measurements.
  • The Astro-H mission can utilize Milky Way observations to resolve the origin of the 3.5-keV line using this method.

Conclusions:

  • Velocity spectroscopy is a powerful tool for confirming dark matter signals.
  • Technological advancements in energy resolution are enabling new observational strategies.
  • This method has broad applications for identifying and characterizing dark matter.