Large Interferometer For Exoplanets (LIFE): III. Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth
Temperate terrestrial exoplanets are likely common objects, but their discovery and characterization is very challenging. Concepts for optimized space missions to overcome these challenges are being studied. The LIFE initiative focuses on the development of a space-based mid-infrared (MIR) nulling i...
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creator | Konrad, B S Alei, E Angerhausen, D Carrión-González, Ó tney, J J Grenfell, J L Kitzmann, D Mollière, P Rugheimer, S Wunderlich, F Quanz, S P the LIFE Collaboration |
description | Temperate terrestrial exoplanets are likely common objects, but their discovery and characterization is very challenging. Concepts for optimized space missions to overcome these challenges are being studied. The LIFE initiative focuses on the development of a space-based mid-infrared (MIR) nulling interferometer probing the thermal emission of a large sample of exoplanets. We derive first estimates for the signal-to-noise (S/N), spectral resolution (R), and wavelength requirements for LIFE. Using an Earth-twin exoplanet as reference case, we quantify how well planetary/atmospheric properties can be constrained from MIR spectra of different quality. We simulate LIFE observations of an Earth-twin orbiting a G2V star at 10 pc from the Sun with different levels of exozodiacal dust emissions. We combine a cloud-free 1D radiative transfer model and the nested sampling algorithm to retrieve planetary/atmospheric properties from input spectra of different wavelength coverage, R, and S/N. We find that H2O, CO2, and O3 are detectable if S/N\(\geq\)10 (uncertainty \(\leq\pm1.0\) dex). We find upper limits for N2O (abundance \(\leq10^{-3}\)). CO, N2, and O2 are unconstrained in all cases. The limit for a CH4 detection is R \(= 50\), S/N \(=10\). We further correctly determine the exoplanet radius (uncertainty \(\leq\pm10\%\)), surface temperature (uncertainty \(\leq\pm20\)K), and surface pressure (uncertainty \(\leq\pm0.5\) dex). With the current LIFE design, the observation time required to reach the specified S/N amounts to \(\sim7\) weeks with 4x2m apertures. We conclude that a minimum wavelength coverage of \(4-18.5\mu\)m, a R of 50 and an S/N of 10 is required. With the current assumptions, the atmospheric characterization of several Earth-like exoplanets at a distance of 10 pc and within a reasonable amount of observing time will require apertures \(\geq2\) meters. |
doi_str_mv | 10.48550/arxiv.2112.02054 |
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Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Konrad, B S ; Alei, E ; Angerhausen, D ; Carrión-González, Ó ; tney, J J ; Grenfell, J L ; Kitzmann, D ; Mollière, P ; Rugheimer, S ; Wunderlich, F ; Quanz, S P ; the LIFE Collaboration</creator><creatorcontrib>Konrad, B S ; Alei, E ; Angerhausen, D ; Carrión-González, Ó ; tney, J J ; Grenfell, J L ; Kitzmann, D ; Mollière, P ; Rugheimer, S ; Wunderlich, F ; Quanz, S P ; the LIFE Collaboration</creatorcontrib><description>Temperate terrestrial exoplanets are likely common objects, but their discovery and characterization is very challenging. Concepts for optimized space missions to overcome these challenges are being studied. The LIFE initiative focuses on the development of a space-based mid-infrared (MIR) nulling interferometer probing the thermal emission of a large sample of exoplanets. We derive first estimates for the signal-to-noise (S/N), spectral resolution (R), and wavelength requirements for LIFE. Using an Earth-twin exoplanet as reference case, we quantify how well planetary/atmospheric properties can be constrained from MIR spectra of different quality. We simulate LIFE observations of an Earth-twin orbiting a G2V star at 10 pc from the Sun with different levels of exozodiacal dust emissions. We combine a cloud-free 1D radiative transfer model and the nested sampling algorithm to retrieve planetary/atmospheric properties from input spectra of different wavelength coverage, R, and S/N. We find that H2O, CO2, and O3 are detectable if S/N\(\geq\)10 (uncertainty \(\leq\pm1.0\) dex). We find upper limits for N2O (abundance \(\leq10^{-3}\)). CO, N2, and O2 are unconstrained in all cases. The limit for a CH4 detection is R \(= 50\), S/N \(=10\). We further correctly determine the exoplanet radius (uncertainty \(\leq\pm10\%\)), surface temperature (uncertainty \(\leq\pm20\)K), and surface pressure (uncertainty \(\leq\pm0.5\) dex). With the current LIFE design, the observation time required to reach the specified S/N amounts to \(\sim7\) weeks with 4x2m apertures. We conclude that a minimum wavelength coverage of \(4-18.5\mu\)m, a R of 50 and an S/N of 10 is required. With the current assumptions, the atmospheric characterization of several Earth-like exoplanets at a distance of 10 pc and within a reasonable amount of observing time will require apertures \(\geq2\) meters.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2112.02054</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Algorithms ; Apertures ; Extrasolar planets ; Interferometers ; Nulling interferometry ; Physics - Earth and Planetary Astrophysics ; Physics - Instrumentation and Methods for Astrophysics ; Pressure ; Radiative transfer ; Space missions ; Spectra ; Spectral resolution ; Terrestrial planets ; Thermal emission ; Uncertainty</subject><ispartof>arXiv.org, 2022-03</ispartof><rights>2022. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27904</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2112.02054$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1051/0004-6361/202141964$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Konrad, B S</creatorcontrib><creatorcontrib>Alei, E</creatorcontrib><creatorcontrib>Angerhausen, D</creatorcontrib><creatorcontrib>Carrión-González, Ó</creatorcontrib><creatorcontrib>tney, J J</creatorcontrib><creatorcontrib>Grenfell, J L</creatorcontrib><creatorcontrib>Kitzmann, D</creatorcontrib><creatorcontrib>Mollière, P</creatorcontrib><creatorcontrib>Rugheimer, S</creatorcontrib><creatorcontrib>Wunderlich, F</creatorcontrib><creatorcontrib>Quanz, S P</creatorcontrib><creatorcontrib>the LIFE Collaboration</creatorcontrib><title>Large Interferometer For Exoplanets (LIFE): III. Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth</title><title>arXiv.org</title><description>Temperate terrestrial exoplanets are likely common objects, but their discovery and characterization is very challenging. Concepts for optimized space missions to overcome these challenges are being studied. The LIFE initiative focuses on the development of a space-based mid-infrared (MIR) nulling interferometer probing the thermal emission of a large sample of exoplanets. We derive first estimates for the signal-to-noise (S/N), spectral resolution (R), and wavelength requirements for LIFE. Using an Earth-twin exoplanet as reference case, we quantify how well planetary/atmospheric properties can be constrained from MIR spectra of different quality. We simulate LIFE observations of an Earth-twin orbiting a G2V star at 10 pc from the Sun with different levels of exozodiacal dust emissions. We combine a cloud-free 1D radiative transfer model and the nested sampling algorithm to retrieve planetary/atmospheric properties from input spectra of different wavelength coverage, R, and S/N. We find that H2O, CO2, and O3 are detectable if S/N\(\geq\)10 (uncertainty \(\leq\pm1.0\) dex). We find upper limits for N2O (abundance \(\leq10^{-3}\)). CO, N2, and O2 are unconstrained in all cases. The limit for a CH4 detection is R \(= 50\), S/N \(=10\). We further correctly determine the exoplanet radius (uncertainty \(\leq\pm10\%\)), surface temperature (uncertainty \(\leq\pm20\)K), and surface pressure (uncertainty \(\leq\pm0.5\) dex). With the current LIFE design, the observation time required to reach the specified S/N amounts to \(\sim7\) weeks with 4x2m apertures. We conclude that a minimum wavelength coverage of \(4-18.5\mu\)m, a R of 50 and an S/N of 10 is required. 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Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth</title><author>Konrad, B S ; Alei, E ; Angerhausen, D ; Carrión-González, Ó ; tney, J J ; Grenfell, J L ; Kitzmann, D ; Mollière, P ; Rugheimer, S ; Wunderlich, F ; Quanz, S P ; the LIFE Collaboration</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a527-bdfad30f2ba16b1edd11c29f46928edbffcaca78a0c003aa54755df4009837283</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Algorithms</topic><topic>Apertures</topic><topic>Extrasolar planets</topic><topic>Interferometers</topic><topic>Nulling interferometry</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Pressure</topic><topic>Radiative transfer</topic><topic>Space missions</topic><topic>Spectra</topic><topic>Spectral resolution</topic><topic>Terrestrial planets</topic><topic>Thermal emission</topic><topic>Uncertainty</topic><toplevel>online_resources</toplevel><creatorcontrib>Konrad, B S</creatorcontrib><creatorcontrib>Alei, E</creatorcontrib><creatorcontrib>Angerhausen, D</creatorcontrib><creatorcontrib>Carrión-González, Ó</creatorcontrib><creatorcontrib>tney, J J</creatorcontrib><creatorcontrib>Grenfell, J L</creatorcontrib><creatorcontrib>Kitzmann, D</creatorcontrib><creatorcontrib>Mollière, P</creatorcontrib><creatorcontrib>Rugheimer, S</creatorcontrib><creatorcontrib>Wunderlich, F</creatorcontrib><creatorcontrib>Quanz, S P</creatorcontrib><creatorcontrib>the LIFE Collaboration</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Konrad, B S</au><au>Alei, E</au><au>Angerhausen, D</au><au>Carrión-González, Ó</au><au>tney, J J</au><au>Grenfell, J L</au><au>Kitzmann, D</au><au>Mollière, P</au><au>Rugheimer, S</au><au>Wunderlich, F</au><au>Quanz, S P</au><au>the LIFE Collaboration</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Large Interferometer For Exoplanets (LIFE): III. Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth</atitle><jtitle>arXiv.org</jtitle><date>2022-03-03</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>Temperate terrestrial exoplanets are likely common objects, but their discovery and characterization is very challenging. Concepts for optimized space missions to overcome these challenges are being studied. The LIFE initiative focuses on the development of a space-based mid-infrared (MIR) nulling interferometer probing the thermal emission of a large sample of exoplanets. We derive first estimates for the signal-to-noise (S/N), spectral resolution (R), and wavelength requirements for LIFE. Using an Earth-twin exoplanet as reference case, we quantify how well planetary/atmospheric properties can be constrained from MIR spectra of different quality. We simulate LIFE observations of an Earth-twin orbiting a G2V star at 10 pc from the Sun with different levels of exozodiacal dust emissions. We combine a cloud-free 1D radiative transfer model and the nested sampling algorithm to retrieve planetary/atmospheric properties from input spectra of different wavelength coverage, R, and S/N. We find that H2O, CO2, and O3 are detectable if S/N\(\geq\)10 (uncertainty \(\leq\pm1.0\) dex). We find upper limits for N2O (abundance \(\leq10^{-3}\)). CO, N2, and O2 are unconstrained in all cases. The limit for a CH4 detection is R \(= 50\), S/N \(=10\). We further correctly determine the exoplanet radius (uncertainty \(\leq\pm10\%\)), surface temperature (uncertainty \(\leq\pm20\)K), and surface pressure (uncertainty \(\leq\pm0.5\) dex). With the current LIFE design, the observation time required to reach the specified S/N amounts to \(\sim7\) weeks with 4x2m apertures. We conclude that a minimum wavelength coverage of \(4-18.5\mu\)m, a R of 50 and an S/N of 10 is required. With the current assumptions, the atmospheric characterization of several Earth-like exoplanets at a distance of 10 pc and within a reasonable amount of observing time will require apertures \(\geq2\) meters.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2112.02054</doi><oa>free_for_read</oa></addata></record> |
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subjects | Algorithms Apertures Extrasolar planets Interferometers Nulling interferometry Physics - Earth and Planetary Astrophysics Physics - Instrumentation and Methods for Astrophysics Pressure Radiative transfer Space missions Spectra Spectral resolution Terrestrial planets Thermal emission Uncertainty |
title | Large Interferometer For Exoplanets (LIFE): III. Spectral resolution, wavelength range and sensitivity requirements based on atmospheric retrieval analyses of an exo-Earth |
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