Detection of Methane in the Atmosphere of Mars

By V. Formisano, S. Atreya, T. Encrenaz, N. Ignatiev, M. Giuranna. Science, 2004

773 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/6ba6590c2d871a0f7db0f568e2ba1e838c4c433b

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Citations in the corpus

Resistance of Microorganisms to Extreme Environmental Conditions and Its Contribution to Astrobiology (2010, background): “Recent discoveries demonstrate trace amounts of methane in the Martian atmosphere [111].”
Astrobiology: The Study of the Living Universe (2005, methodology): “Detection at a 10 ± 5 ppb mixing ratio, with local variations ranging from 0 ppb to 30 ppb, has also been achieved with the Mars Express spacecraft (Formisano et al. 2004).”
Mapping the methane on Mars (2010, methodology): “The same calculation can be applied to TES, given its NESR and spectral resolution, for evaluating how many spectra must be averaged to obtain the detection of methane at 10 ppbv level, which is the mean mixing ratio claimed by Krasnopolsky et al. (2004) and Formisano et al. (2004).”
Titan's methane cycle (2006, background): “Such a process has been studied for Earth, and has been applied to Mars to explain the presence of methane on that planet (Atreya et al., 2004; Formisano et al., 2004; Atreya, 2005; Atreya et al., 2006; Oze and Sharma, 2005).”
Outgassing History and Escape of the Martian Atmosphere and Water Inventory (2015, background): “…from both Earth and spacecraft in orbit around Mars (Planetary Fourier Spectrometer (PFS) on Mars Express, Thermal Emission Spectrometer (TES) on Mars Global Surveyor (MGS)) at an average ∼10–20 ppb level (Krasnopolsky et al. 2004; Formisano et al. 2004; Mumma et al. 2009; Fonti and Marzo 2010).”
The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter (2018, background): “…the first half of the 2000’s) pioneering works that reported for the first time the detection of methane in the Martian atmosphere (the FKM group: Formisano et al. 2004; Krasnopolsky et al. 2004; as well as Mumma et al. 2009; note that the latter observations were reported first in Mumma et al.…”
NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance (2018, background): “2009), from space-borne instruments (Fonti and Marzo 2010; Formisano et al. 2004; Geminale et al. 2011), and in-situ (Webster et al.”
Is there methane on Mars (2010, background): “Methane is inferred indirectly: adding 10-60 ppbv CH4 to their model appears to improve their model’s fit at one wavelength, 3018 cm 1 (Formisano et al., 2004).”
Methane clathrate hydrates as a potential source for martian atmospheric methane (2007, methodology): “It is known that methanogenic archaea actively reduce CO and CO2 to methane in the following reactions (Formisano et al., 2004):”
Circular polarization in scattered light as a possible biomarker (2009, neutral): “On Mars, however, there are surface features that indicate the presence of considerable flows of water in the past, and recent results from the Mars Express and other missions show that substantial quantities of water and perhaps even methane are present [32, 33, 34].”
The Sample Analysis at Mars Investigation and Instrument Suite (2012, methodology): “…and latitude (Smith 2004; Maltagliati et al. 2011) CO ∼1× 10−3 From microwave spectroscopy (Clancy et al. 1983) CH4 10 (±5) ppb From Mars Express (Formisano et al. 2004) or ground based high resolution infrared spectroscopy (Krasnopolsky et al. 2004; Mumma et al. 2009) H2O2 10–800 ppb Ground…”