Sentences with phrase «at emission wavelength»

Not exact matches

Rampadarath explains: «Comparing the VLA images at radio wavelengths to Chandra's X-ray observations and the hydrogen - emission detected by Hubble, shows that features are not only connected, but that the radio outflows are in fact the progenitors of the structures seen by Chandra and Hubble.

The picture which emerges is one of a twisting jet whose emission is amplified at different wavelengths at different times, by the «lighthouse effect.»

The instrument is sensitive to near - infrared light, the wavelengths at which the emissions of extremely distant galaxies — stretched by the expansion of space — shine most brightly.

WISE 0855 is too faint for conventional spectroscopy at optical or near - infrared wavelengths, but thermal emission from the deep atmosphere at wavelengths in a narrow window around 5 microns offered an opportunity where spectroscopy would be «challenging but not impossible,» he said.

What is more, because Jupiter's microwave emissions vary in wavelength based on the pressure (as well as temperature) of the atmospheric layers where they originate, observations at multiple wavelengths allow researchers to create a cross-section through the atmosphere.

Now, in a study published in Nature Nanotechnology on January 11th 2016 (online), a team of MIT researchers describes another way to recycle light emitted at unwanted infrared wavelengths while optimizing the emission at useful visible wavelengths.

At short wavelengths the ripples might have been caused by emission from dust in the Galaxy.

But for one lengthy interval during the observations, the team spotted emissions from hydrogen (at a wavelength of 121.6 nanometers) in the same region.

Working at the IRAM Plateau De Bure interferometer in the French Alps, the researchers gathered data in the millimetre band, which allows observation of the emission from the cold gas which is the primary fuel for star formation and main ingredient of galaxies, but is almost invisible at other wavelengths.

These so - called relativistic jets produce strong emission at radio wavelengths.

Beyond the wavelength coverage of the space - borne observatories, the spectra taken in Hawaii even turned up a curious new feature — a boost in emissions of unknown origin at wavelengths of about 3.3 microns.

Marengo said the study looked at two different infrared wavelengths: the shorter was consistent with a typical star and the longer showed some infrared emissions, but not enough to reach a detection threshold.

To prove their concept of this multiplex spectral microgel analysis within a microfluidic flow, the team used «different barcodes corresponding to different emissions at specific wavelengths and the fluorescence intensity of known microRNA concentration,» which was measured for calibrations of the specific microRNA being explored.

The team determined this by detecting two types of carbon monoxide signatures, an absorption signature at a wavelength of about 1.6 micrometers and an emission signature at about 4.5 micrometers.

Los Alamos National Laboratory has produced the first known material capable of single - photon emission at room temperature and at telecommunications wavelengths.

This might indicate that smaller (and warmer) dust grains are responsible for the 100 μm emission than at the longer wavelengths, in agreement with the theoretical predictions of van Marle et al. (2011).

«Ideally, a single photon emitter will provide both room - temperature operation and emission at telecom wavelengths, but this has remained an elusive goal.

Los Alamos National Laboratory researchers have produced the first known material capable of single - photon emission at room temperature and at telecommunications wavelengths, using chemically functionalized carbon nanotubes.

At millimetre wavelengths emission from the CO molecule allows astronomers to obtain high - resolution maps of the gas emission from the strong stellar wind generated by the AGB stars.

Ongoing radio observations (SMA, JCMT, VLA) of Sirius A are being used to set an observationally determined standard for stellar atmosphere modeling and debris disk studies around A stars, as well as to take the first step toward characterizing potential intrinsic uncertainty in stellar emission at these wavelengths.

Natural astronomical masers — the analog of laser emission at microwave wavelengths — are one class of coherent sources, but these emit in specific wavelengths.

Both the temperature and composition determines the star's energy emission at different wavelengths.

Okay, one little nit - picky issue with Q2 is that O2 and N2 actually DO absorb infrared radiation, just at shorter wavelengths than matter for the Earth's infrared emission spectrum (3 - 27 microns, with a peak around 9 microns or so).

The European X-ray Observatory Satellite (EXOSAT), developed by the European Space Agency, was capable of greater spectral resolution than the Einstein Observatory and was more sensitive to X-ray emissions at shorter wavelengths.

Therefore, the research group targeted molecular line emissions from hydrogen cyanide (HCN), formyl ion (HCO +), and hydrogen sulfide (CS) at millimeter / submillimeter wavelengths (* 4) in the galaxy called NGC 1097 (about 50 million light years away) with the ALMA Telescope in the Atacama Desert in Chile.

The new identification method is based on molecular line emission at submillimeter wavelengths.

A number of similar black hole exploration methods have also been proposed in optical / infrared spectra so far, but one crucial problem is that emissions at these wavelengths are absorbed by interstellar dust particles although the more active black holes contain more dust particles.

That first quasar and others identified later puzzled astronomers because, when their light was analyzed to find the characteristic «signature» of emission at specific wavelengths shown by particular atoms, the pattern was at first indecipherable.

Nuclei were stained with Hoechst 33342 (5 μg / ml) and observed by a fluorescence microscope equipped with U-MWU optical filters with a U-MWU optical filter at an excitation wavelength of 355 nm and an emission wavelength of 420 nm.

They observed L1551 NE in the emission from dust at a 0.9 - mm wavelength, a tracer of distribution of interstellar materials, and carbon monoxide molecular emission, which can be used to study gas motion with the Doppler Effect.

The goal of the research group is to establish a new exploration method using as reference various molecular / atomic emission lines which can be observed at millimeter / submillimeter wavelengths (* 3).

However, the original Green Bean population show little to no emission at radio wavelengths.

The fluorescence emitted by Hoechst 33342 was viewed using a fluorescence microscope, equipped with U-MWU optical filters at excitation / emission wavelengths of 330-385/420 nm.

LOS ALAMOS, N.M., July 31, 2017 — Los Alamos National Laboratory has produced the first known material capable of single - photon emission at room temperature and at telecommunications wavelengths.

In Pascucci et al. (2012) we demonstrated that free - free emission from a fully or partially ionized disk surface is detectable with current instruments and appears as emission in excess to the dust thermal emission at centimeter wavelengths.

Calcein - AM and Hoechst were added at the end of the treatment for 10 minutes and the developed fluorescence was measured in assay buffer in a Victor3 plate reader (Hoechst at excitation and emission wavelengths of 355 nm and 465 nm, respectively and calcein at excitation and emission wavelengths of 485 nm and 535 nm, respectively).

The fluorescence emitted by the cells was viewed using a fluorescence microscope, equipped with U-MWB2 optical filters at excitation / emission wavelengths of 460 ~ 490/520 nm.

Abstract: Debris discs are typically revealed through excess emission at infrared wavelengths.

In practice, mono - atomic and symmetrical diatomic gas molecules have negligible emission / absorption at most wavelengths including thermal infrared.

Using the HIgh Precision Polarimetric Instrument (H... ▽ More Debris discs are typically revealed through excess emission at infrared wavelengths.

This excess emission has been suggested to stem from debris di... ▽ More (abridged) Infrared excesses associated with debris disk host stars detected so far peak at wavelengths around ~ 100 -LCB- \ mu -RCB- m or shorter.

Intensity as recorded in zebrafish (crosshairs in Fig. 4a show where measurement took place) at an excitation wavelength of 633 nm and scanned for emission at 11 nm intervals from 654 nm to 794 nm.

Here, f (λex) is the absorption factor at the excitation wavelength λex, F the integral emission intensity, i.e., the area under the blank and spectrally corrected emission spectrum on a wavelength scale, and n the refractive index of the solvent (s) used.

We have clearly detected FIR dust emission extended in the halo of the galaxy; there are two filamentary emission structures extending from the galactic disk up to 9 kpc in the northern and 6 kpc in the northwestern direct... ▽ More We present new far - infrared (FIR) images of the edge - on starburst galaxy NGC253 obtained with the Far - Infrared Surveyor (FIS) onboard AKARI at wavelengths of 90 um and 140 um.

The shifts in emission peaks are significant; however, absorption shows little to no spectral shift, presumably due to the ratio sorting protocol used at a constant excitation wavelength of 568 nm.

The radio emission rose and fell several times, and the relative intensity at different radio wavelengths also changed.

We refer to that thermal radiation at longer wavelengths as «dusty emission» because it's coming from the dust.

Fluorescence intensities were measured at an excitation wavelength of 340 or 380 nm and an emission wavelength of 510 nm, with a fluorescence spectrometer (Hitachi F - 2500) during stimulation as indicated in Fig. 5.

The reason for this is as follows: Carbon dioxide has three absorption bands at wavelengths of 4.26, 7.52, and 14.99 micrometers (microns).13 The Earth's emission spectrum, treated as a black body (no atmospheric absorption), peaks at between 15 and 20 microns, and falls off rapidly with decreasing wavelength.

Okay, one little nit - picky issue with Q2 is that O2 and N2 actually DO absorb infrared radiation, just at shorter wavelengths than matter for the Earth's infrared emission spectrum (3 - 27 microns, with a peak around 9 microns or so).