Mapping of ozone and water in the atmosphere of Mars near the 1997 aphelion

Robert E. Novak; Michael J. Mumma; Michael A. DiSanti; Neil Dello Russo; Karen Magee-Sauer

doi:10.1006/icar.2002.6863

Mapping of ozone and water in the atmosphere of Mars near the 1997 aphelion

Robert E. Novak, Michael J. Mumma, Michael A. DiSanti, Neil Dello Russo, Karen Magee-Sauer

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Abstract

We present absolute abundances and latitudinal variations of ozone and water in the atmosphere of Mars during its late northern spring (L_s = 67.3°) shortly before aphelion. Long-slit maps of the a¹Δ_g state of molecular oxygen (O₂) and HDO, an isotopic form of water, were acquired on UT January 21.6 1997 using a high-resolution infrared spectrometer (CSHELL) at the NASA Infrared Telescope Facility. O₂(a¹Δ_g) is produced by ozone photolysis, and the ensuing dayglow emission at 1.27 μm is used as a tracer for ozone. Retrieved vertical column densities for ozone above ∼20 km ranged between 1.5 and 2.8 μm-atm at mid- to low latitudes (30°S-60°N) and decreased outside that region. A significant decrease in ozone density is seen near 30°N (close to the subsolar latitude of 23.5°N). The rotational temperatures retrieved from O₂(a-X) emissions show a mean of 172±2.5 K, confirming that the sensed ozone lies in the middle atmosphere (∼24 km). The ν₁ fundamental band of HDO near 3.67 μm was used as a proxy for H₂O. The retrieved vertical column abundance of water varies from 3 precipitable microns (pr-μm) at ∼30°S to 24 pr-μm at ∼60°N. We compare these results with current photochemical models and with measurements obtained by other methods.

Original language	English (US)
Pages (from-to)	14-23
Number of pages	10
Journal	Icarus
Volume	158
Issue number	1
DOIs	https://doi.org/10.1006/icar.2002.6863
State	Published - Jul 2002

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1006/icar.2002.6863

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@article{4a7446a83983412490c3beac6ea0fb43,

title = "Mapping of ozone and water in the atmosphere of Mars near the 1997 aphelion",

abstract = "We present absolute abundances and latitudinal variations of ozone and water in the atmosphere of Mars during its late northern spring (Ls = 67.3°) shortly before aphelion. Long-slit maps of the a1Δg state of molecular oxygen (O2) and HDO, an isotopic form of water, were acquired on UT January 21.6 1997 using a high-resolution infrared spectrometer (CSHELL) at the NASA Infrared Telescope Facility. O2(a1Δg) is produced by ozone photolysis, and the ensuing dayglow emission at 1.27 μm is used as a tracer for ozone. Retrieved vertical column densities for ozone above ∼20 km ranged between 1.5 and 2.8 μm-atm at mid- to low latitudes (30°S-60°N) and decreased outside that region. A significant decrease in ozone density is seen near 30°N (close to the subsolar latitude of 23.5°N). The rotational temperatures retrieved from O2(a-X) emissions show a mean of 172±2.5 K, confirming that the sensed ozone lies in the middle atmosphere (∼24 km). The ν1 fundamental band of HDO near 3.67 μm was used as a proxy for H2O. The retrieved vertical column abundance of water varies from 3 precipitable microns (pr-μm) at ∼30°S to 24 pr-μm at ∼60°N. We compare these results with current photochemical models and with measurements obtained by other methods.",

author = "Novak, {Robert E.} and Mumma, {Michael J.} and DiSanti, {Michael A.} and Russo, {Neil Dello} and Karen Magee-Sauer",

note = "Funding Information: This work was supported by the NASA–JOVE Program under Grant NAG8-1273 to R. Novak, by the NASA Planetary Astronomy Program under RTOP 344-32-30-07 to M. J. Mumma and Grant NAG5-7905 to M. A. DiSanti, and by the NASA Planetary Atmospheres Program under Grant NAG5-7753 to N. Dello Russo. K. Magee-Sauer gratefully acknowledges support from the National Science Foundation under Grant AST-9619461. We thank Fred Espenak for constructing the aspect diagram of Mars (Fig. 2) and Michael Smith and John Pearl for providing us with atmospheric temperature and water profiles from TES. We thank and acknowledge Vladimir Krasnopolsky for his conversations at the beginning of the project. Data presented herein were obtained at the NASA Infrared Telescope Facility (IRTF), which is operated for NASA by the University of Hawaii. We gratefully acknowledge the support of the IRTF Director, Dr. Robert Joseph, and the expert assistance of the IRTF telescope operators and staff.",

year = "2002",

month = jul,

doi = "10.1006/icar.2002.6863",

language = "English (US)",

volume = "158",

pages = "14--23",

journal = "Icarus",

issn = "0019-1035",

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TY - JOUR

T1 - Mapping of ozone and water in the atmosphere of Mars near the 1997 aphelion

AU - Novak, Robert E.

AU - Mumma, Michael J.

AU - DiSanti, Michael A.

AU - Russo, Neil Dello

AU - Magee-Sauer, Karen

N1 - Funding Information: This work was supported by the NASA–JOVE Program under Grant NAG8-1273 to R. Novak, by the NASA Planetary Astronomy Program under RTOP 344-32-30-07 to M. J. Mumma and Grant NAG5-7905 to M. A. DiSanti, and by the NASA Planetary Atmospheres Program under Grant NAG5-7753 to N. Dello Russo. K. Magee-Sauer gratefully acknowledges support from the National Science Foundation under Grant AST-9619461. We thank Fred Espenak for constructing the aspect diagram of Mars (Fig. 2) and Michael Smith and John Pearl for providing us with atmospheric temperature and water profiles from TES. We thank and acknowledge Vladimir Krasnopolsky for his conversations at the beginning of the project. Data presented herein were obtained at the NASA Infrared Telescope Facility (IRTF), which is operated for NASA by the University of Hawaii. We gratefully acknowledge the support of the IRTF Director, Dr. Robert Joseph, and the expert assistance of the IRTF telescope operators and staff.

PY - 2002/7

Y1 - 2002/7

N2 - We present absolute abundances and latitudinal variations of ozone and water in the atmosphere of Mars during its late northern spring (Ls = 67.3°) shortly before aphelion. Long-slit maps of the a1Δg state of molecular oxygen (O2) and HDO, an isotopic form of water, were acquired on UT January 21.6 1997 using a high-resolution infrared spectrometer (CSHELL) at the NASA Infrared Telescope Facility. O2(a1Δg) is produced by ozone photolysis, and the ensuing dayglow emission at 1.27 μm is used as a tracer for ozone. Retrieved vertical column densities for ozone above ∼20 km ranged between 1.5 and 2.8 μm-atm at mid- to low latitudes (30°S-60°N) and decreased outside that region. A significant decrease in ozone density is seen near 30°N (close to the subsolar latitude of 23.5°N). The rotational temperatures retrieved from O2(a-X) emissions show a mean of 172±2.5 K, confirming that the sensed ozone lies in the middle atmosphere (∼24 km). The ν1 fundamental band of HDO near 3.67 μm was used as a proxy for H2O. The retrieved vertical column abundance of water varies from 3 precipitable microns (pr-μm) at ∼30°S to 24 pr-μm at ∼60°N. We compare these results with current photochemical models and with measurements obtained by other methods.

AB - We present absolute abundances and latitudinal variations of ozone and water in the atmosphere of Mars during its late northern spring (Ls = 67.3°) shortly before aphelion. Long-slit maps of the a1Δg state of molecular oxygen (O2) and HDO, an isotopic form of water, were acquired on UT January 21.6 1997 using a high-resolution infrared spectrometer (CSHELL) at the NASA Infrared Telescope Facility. O2(a1Δg) is produced by ozone photolysis, and the ensuing dayglow emission at 1.27 μm is used as a tracer for ozone. Retrieved vertical column densities for ozone above ∼20 km ranged between 1.5 and 2.8 μm-atm at mid- to low latitudes (30°S-60°N) and decreased outside that region. A significant decrease in ozone density is seen near 30°N (close to the subsolar latitude of 23.5°N). The rotational temperatures retrieved from O2(a-X) emissions show a mean of 172±2.5 K, confirming that the sensed ozone lies in the middle atmosphere (∼24 km). The ν1 fundamental band of HDO near 3.67 μm was used as a proxy for H2O. The retrieved vertical column abundance of water varies from 3 precipitable microns (pr-μm) at ∼30°S to 24 pr-μm at ∼60°N. We compare these results with current photochemical models and with measurements obtained by other methods.

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DO - 10.1006/icar.2002.6863

M3 - Article

AN - SCOPUS:0036639470

SN - 0019-1035

VL - 158

SP - 14

EP - 23

JO - Icarus

JF - Icarus

IS - 1

ER -

Mapping of ozone and water in the atmosphere of Mars near the 1997 aphelion

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