The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission

Formisano, V.; Angrilli, Francesco; Arnold, Gabriele; Atreya, S. K.; Bianchini, G.; Biondi, David; Blanco, A.; Błęcka, M. I.; Coradini, A.; Colangeli, L.; Ekonomov, A. P.; Esposito, F.; Fonti, S.; Giuranna, M.; Grassi, D.; Gnedykh, V. I.; Grigoriev, Аlexey; Hansen, G. B.; Hirsh, Hayley; Khatuntsev, I.; Kiselev, Alexander V.; Ignatiev, N.; Jurewicz, A. J. G.; Lellouch, E.; Moreno, J. J. Lopez; Marten, A.; Mattana, A.; Maturilli, Alessandro; Mencarelli, E.; Michalska, Małgorzata; Moroz, V.I.; Moshkin, B. E.; Nespoli, F.; Nikolsky, Yu. V.; Orfei, R.; Orleański, P.; Orofino, V.; Palomba, E.; Patsaev, D.; Piccioni, G.; Rataj, M.; Rodrigo, R.; Rodriguez, J.; Rossi, Maurizio; Saggin, Bortolino; Титов, Д. В.; Zasova, L. V.

doi:10.1016/j.pss.2004.12.006

Cited by 154 publications

(65 citation statements)

References 12 publications

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“…This corresponds to 12 km on Mars surface when viewed from periapsis. A more detailed description of the PFS instrument can be found in Formisano et al (2005).…”

Section: Pfs/lwmentioning

confidence: 99%

A study of the Martian water vapor over Hellas using OMEGA and PFS aboard Mars Express

Encrenaz¹,

Fouchet²,

Melchiorri³

et al. 2008

A&A

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We used the OMEGA imaging spectrometer aboard Mars Express to study the evolution of the water vapor abundance over the Hellas basin, as a function of the seasonal cycle. The H 2 O column density is found to range from very low values (between southern fall and winter) up to more than 15 pr-µm during southern spring and summer. The general behavior is consistent with the expected seasonal cycle of water vapor on Mars, as previously observed by TES and modeled. In particular, the maximum water vapor content is observed around the southern solstice, and is significantly less than its northern couterpart. However, there is a noticeable discrepancy around the northern spring equinox (L s = 330-60• ), where the observed H 2 O column densities are significantly lower than the values predicted by the GCM. Our data show an abrupt enhancement of the water vapor column density (from 3 to 16 pr-µm) on a timescale of 3 days, for L s = 251-254• . Such an increase, not predicted by the GCM, was also occasionally observed by TES over Hellas during previous martian years at the same season; however, its origin remains to be understood.

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“…This corresponds to 12 km on Mars surface when viewed from periapsis. A more detailed description of the PFS instrument can be found in Formisano et al (2005).…”

Section: Pfs/lwmentioning

confidence: 99%

A study of the Martian water vapor over Hellas using OMEGA and PFS aboard Mars Express

Encrenaz¹,

Fouchet²,

Melchiorri³

et al. 2008

A&A

Self Cite

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“…These measurements are achieved by the PFS' short wavelength channel (SWC) [1.25-5 µm] with the spectral resolution allowing the unambiguous identification of many of the CO 2 emission bands. Details on the instrument description, its calibration and inflight performance can be found in Formisano et al (2005), Giuranna et al (2005), and Formisano et al (2006).…”

Section: Introductionmentioning

confidence: 99%

Evidence of a significant rotational non-LTE effect in the CO<sub>2</sub> 4.3 µm PFS-MEX limb spectra

Kutepov

Rezac

2017

Atmos. Meas. Tech.

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Abstract. Since January 2004, the planetary Fourier spectrometer (PFS) on board the Mars Express satellite has been recording near-infrared limb spectra of high quality up to the tangent altitudes ≈ 150 km, with potential information on density and thermal structure of the upper Martian atmosphere. We present first results of our modeling of the PFS short wavelength channel (SWC) daytime limb spectra for the altitude region above 90 km. We applied a ro-vibrational non-LTE model based on the stellar astrophysics technique of accelerated lambda iteration (ALI) to solve the multispecies and multi-level CO 2 problem in the Martian atmosphere. We show that the long-standing discrepancy between observed and calculated spectra in the cores and wings of 4.3 µm region is explained by the non-thermal rotational distribution of molecules in the upper vibrational states 10011 and 10012 of the CO 2 main isotope second hot (SH) bands above 90 km altitude. The redistribution of SH band intensities from band branch cores into their wings is caused (a) by intensive production of the CO 2 molecules in rotational states with j > 30 due to the absorption of solar radiation in optically thin wings of 2.7 µm bands and (b) by a short radiative lifetime of excited molecules, which is insufficient at altitudes above 90 km for collisions to maintain rotation of excited molecules thermalized. Implications for developing operational algorithms for massive processing of PFS and other instrument limb observations are discussed.

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“…During the last twenty years high-resolution (spatial) multispectral imaging systems for photogeologic surface mapping and multi-hyperspectral sensors for thematic mapping have been developed to operate together for planetologic applications on ESA's deep space missions. Planetary spectrometers which were successfully developed, applied and operated on different European planetary projects can be divides into three groups: imaging spectrometers for the 0.25 to 5 µm range 34,35,36,37 , imaging spectrometers in the 7-14 µm region 6,8,9,53 , and interferometers 4,5,41,42,[54][55][56] . Covering the wavelength range from the UV/VIS up to the mid-infrared region, these hyperspectral systems use the reflected sunlight or the thermal emission from the different objects.…”

Section: Introductionmentioning

confidence: 99%

Front Matter: Volume 8160

SPIE¹

2011

SPIE Proceedings

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The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission

Cited by 154 publications

References 12 publications

A study of the Martian water vapor over Hellas using OMEGA and PFS aboard Mars Express

A study of the Martian water vapor over Hellas using OMEGA and PFS aboard Mars Express

Evidence of a significant rotational non-LTE effect in the CO<sub>2</sub> 4.3 µm PFS-MEX limb spectra

Front Matter: Volume 8160

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The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission

Cited by 154 publications

References 12 publications

A study of the Martian water vapor over Hellas using OMEGA and PFS aboard Mars Express

A study of the Martian water vapor over Hellas using OMEGA and PFS aboard Mars Express

Evidence of a significant rotational non-LTE effect in the CO&lt;sub&gt;2&lt;/sub&gt; 4.3 µm PFS-MEX limb spectra

Front Matter: Volume 8160

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Product

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Evidence of a significant rotational non-LTE effect in the CO<sub>2</sub> 4.3 µm PFS-MEX limb spectra