| Records |
| Author |
Martin슠Harwit |
| Title |
The Herschel mission |
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Journal Article |
| Year |
2004 |
Publication |
Advances in Space Research |
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| Volume |
34 |
Issue  |
3 |
Pages |
568-572 |
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RPLAB @ s @ herschel_mission |
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375 |
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Yu, B; Zeng, F; Yang, Y; Xing, Q; Chechin, A; Xin, X; Zeylikovich, I; Alfano R. R. |
| Title |
Torsional vibrational modes of tryptophan studied by terahertz time-domain spectroscopy |
Type |
Journal Article |
| Year |
2004 |
Publication |
Biophys. J. |
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| Volume |
86 |
Issue |
3 |
Pages |
1649-1654 |
| Keywords |
THz applications |
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no |
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491 |
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Slysz, W.; Wegrzecki, M.; Papis, E.; Gol'tsman, G. N.; Verevkin, A.; Sobolewski, R. |
| Title |
A method of optimization of the NbN superconducting single-photon detector |
Type |
Miscellaneous |
| Year |
2004 |
Publication |
INIS |
Abbreviated Journal |
INIS |
| Volume |
36 |
Issue |
27 |
Pages |
1-2 |
| Keywords |
NbN SSPD, SNSPD |
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5-th International Symposium Ion Implantation and Other Applications of Ions and Electrons, ION |
| Notes |
Reference num. 36060124 |
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1485 |
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Korneev, A.; Kouminov, P.; Matvienko, V.; Chulkova, G.; Smirnov, K.; Voronov, B.; Gol'tsman, G. N.; Currie, M.; Lo, W.; Wilsher, K.; Zhang, J.; Słysz, W.; Pearlman, A.; Verevkin, A.; Sobolewski, Roman |
| Title |
Sensitivity and gigahertz counting performance of NbN superconducting single-photon detectors |
Type |
Journal Article |
| Year |
2004 |
Publication |
Appl. Phys. Lett. |
Abbreviated Journal |
Appl. Phys. Lett. |
| Volume |
84 |
Issue |
26 |
Pages |
5338-5340 |
| Keywords |
SSPD, NEP, QE |
| Abstract |
We have measured the quantum efficiencysQEd, GHz counting rate, jitter, and noise-equivalentpowersNEPdof nanostructured NbN superconducting single-photon detectorssSSPDsdin thevisible to infrared radiation range. Our 3.5-nm-thick and 100- to 200-nm-wide meander-typedevices(total area 10310mm2), operating at 4.2 K, exhibit an experimental QE of up to 20% inthe visible range and,10% at 1.3 to 1.55mm wavelength and are potentially sensitive up tomidinfrareds,10mmdradiation. The SSPD counting rate was measured to be above 2 GHz withjitter,18 ps, independent of the wavelength. The devices’ NEP varies from,10−17W/Hz1/2for1.55mm photons to,10−20W/Hz1/2for visible radiation. Lowering the SSPD operatingtemperature to 2.3 K significantly enhanced its performance, by increasing the QE to,20% andlowering the NEP level to,3310−22W/Hz1/2, both measured at 1.26mm wavelength. |
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0003-6951 |
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532 |
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| Author |
Krasnopolsky, Vladimir A.; Maillard, Jean Pierre; C. Owen, Tobias |
| Title |
Detection of methane in the martian atmosphere: evidence for life? |
Type |
Journal Article |
| Year |
2004 |
Publication |
Icarus |
Abbreviated Journal |
Icarus |
| Volume |
172 |
Issue |
2 |
Pages |
537-547 |
| Keywords |
FTS, Mars atmosphere, methane absorption lines, IR spectroscopy, infrared spectroscopy, landfill gas |
| Abstract |
Using the Fourier Transform Spectrometer at the Canada–France–Hawaii Telescope, we observed a spectrum of Mars at the P-branch of the strongest CH4 band at 3.3 μm with resolving power of 180,000 for the apodized spectrum. Summing up the spectral intervals at the expected positions of the 15 strongest Doppler-shifted martian lines, we detected the absorption by martian methane at a 3.7 sigma level which is exactly centered in the summed spectrum. The observed CH4 mixing ratio is 10±3 ppb. Total photochemical loss of CH4 in the martian atmosphere is equal to View the MathML source, the CH4 lifetime is 340 years and methane should be uniformly mixed in the atmosphere. Heterogeneous loss of atmospheric methane is probably negligible, while the sink of CH4 during its diffusion through the regolith may be significant. There are no processes of CH4 formation in the atmosphere, so the photochemical loss must therefore be balanced by abiogenic and biogenic sources. Outgassing from Mars is weak, the latest volcanism is at least 10 million years old, and thermal emission imaging from the Mars Odyssey orbiter does not reveal any hot spots on Mars. Hydrothermal systems can hardly be warmer than the room temperature at which production of methane is very low in terrestrial waters. Therefore a significant production of hydrothermal and magmatic methane is not very likely on Mars. The calculated average production of CH4 by cometary impacts is 2% of the methane loss. Production of methane by meteorites and interplanetary dust does not exceed 4% of the methane loss. Methane cannot originate from an extinct biosphere, as in the case of “natural gas†on Earth, given the exceedingly low limits on organic matter set by the Viking landers and the dry recent history which has been extremely hostile to the macroscopic life needed to generate the gas. Therefore, methanogenesis by living subterranean organisms is a plausible explanation for this discovery. Our estimates of the biomass and its production using the measured CH4 abundance show that the martian biota may be extremely scarce and Mars may be generally sterile except for some oases. |
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