Large Interferometer For Exoplanets (LIFE): XIV. Finding terrestrial protoplanets in the galactic neighborhood

Lorenzo Cesario; Tim Lichtenberg; Eleonora Alei; Óscar Carrión-González; Felix A. Dannert; Denis Defrère; Steve Ertel; Andrea Fortier; A. García Muñoz; Adrian M. Glauser; Jonah T. Hansen; Ravit Helled; Philipp A. Huber; Michael J. Ireland; Jens Kammerer; Romain Laugier; Jorge Lillo-Box; Franziska Menti; Michael R. Meyer; Lena Noack; Sascha P. Quanz; Andreas Quirrenbach; Sarah Rugheimer; Floris van der Tak; Haiyang S. Wang; Marius Anger; Olga Balsalobre-Ruza; Surendra Bhattarai; Marrick Braam; Amadeo Castro-González; Charles S. Cockell; Tereza Constantinou; Gabriele Cugno; Jeanne Davoult; Manuel Güdel; Nina Hernitschek; Sasha Hinkley; Satoshi Itoh; Markus Janson; Anders Johansen; Hugh R. A. Jones; Stephen R. Kane; Tim A. van Kempen; Kristina G. Kislyakova; Judith Korth; Andjelka B. Kovačević; Stefan Kraus; Rolf Kuiper; Joice Mathew; Taro Matsuo; Yamila Miguel; Michiel Min; Ramon Navarro; Ramses M. Ramirez; Heike Rauer; Berke Vow Ricketti; Amedeo Romagnolo; Martin Schlecker; Evan L. Sneed; Vito Squicciarini; Keivan G. Stassun; Motohide Tamura; Daniel Viudez-Moreiras; Robin D. Wordsworth

doi:10.1051/0004-6361/202450764

Large Interferometer For Exoplanets (LIFE): XIV. Finding terrestrial protoplanets in the galactic neighborhood

Lorenzo Cesario^*, Tim Lichtenberg^*, Eleonora Alei, Óscar Carrión-González, Felix A. Dannert, Denis Defrère, Steve Ertel, Andrea Fortier, A. García Muñoz, Adrian M. Glauser, Jonah T. Hansen, Ravit Helled, Philipp A. Huber, Michael J. Ireland, Jens Kammerer, Romain Laugier, Jorge Lillo-Box, Franziska Menti, Michael R. Meyer, Lena NoackSascha P. Quanz, Andreas Quirrenbach, Sarah Rugheimer, Floris van der Tak, Haiyang S. Wang, Marius Anger, Olga Balsalobre-Ruza, Surendra Bhattarai, Marrick Braam, Amadeo Castro-González, Charles S. Cockell, Tereza Constantinou, Gabriele Cugno, Jeanne Davoult, Manuel Güdel, Nina Hernitschek, Sasha Hinkley, Satoshi Itoh, Markus Janson, Anders Johansen, Hugh R. A. Jones, Stephen R. Kane, Tim A. van Kempen, Kristina G. Kislyakova, Judith Korth, Andjelka B. Kovačević, Stefan Kraus, Rolf Kuiper, Joice Mathew, Taro Matsuo, Yamila Miguel, Michiel Min, Ramon Navarro, Ramses M. Ramirez, Heike Rauer, Berke Vow Ricketti, Amedeo Romagnolo, Martin Schlecker, Evan L. Sneed, Vito Squicciarini, Keivan G. Stassun, Motohide Tamura, Daniel Viudez-Moreiras, Robin D. Wordsworth

^*Corresponding author af dette arbejde

Centre for Star and Planet Formation

Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › peer review

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Abstract

Context. The increased brightness temperature of young rocky protoplanets during their magma ocean epoch makes them potentially amenable to atmospheric characterization at distances from the Solar System far greater than thermally equilibrated terrestrial exoplanets, offering observational opportunities for unique insights into the origin of secondary atmospheres and the near surface conditions of prebiotic environments. Aims. The Large Interferometer For Exoplanets (LIFE) mission will employ a space-based midinfrared nulling interferometer to directly measure the thermal emission of terrestrial exoplanets. In this work, we seek to assess the capabilities of various instrumental design choices of the LIFE mission concept for the detection of cooling protoplanets with transient high-temperature magma ocean atmospheres at the tail end of planetary accretion. In particular, we investigate the minimum integration times necessary to detect transient magma ocean exoplanets in young stellar associations in the Solar neighborhood. Methods. Using the LIFE mission instrument simulator (LIFEsim), we assessed how specific instrumental parameters and design choices, such as wavelength coverage, aperture diameter, and photon throughput, facilitate or disadvantage the detection of protoplan-ets. We focused on the observational sensitivities of distance to the observed planetary system, protoplanet brightness temperature (using a blackbody assumption), and orbital distance of the potential protoplanets around both G- and M-dwarf stars. Results. Our simulations suggest that LIFE will be able to detect (S/N ≥ 7) hot protoplanets in young stellar associations up to distances of 100 pc from the Solar System for reasonable integration times (up to a few hours). Detection of an Earth-sized protoplanet orbiting a Solar-sized host star at 1 AU requires less than 30 minutes of integration time. M-dwarfs generally need shorter integration times. The contribution from wavelength regions smaller than 6 μm is important for decreasing the detection threshold and discriminating emission temperatures. Conclusions. The LIFE mission is capable of detecting cooling terrestrial protoplanets within minutes to hours in several local young stellar associations hosting potential targets. The anticipated compositional range of magma ocean atmospheres motivates further architectural design studies to characterize the crucial transition from primary to secondary atmospheres.

Originalsprog	Engelsk
Artikelnummer	A172
Tidsskrift	Astronomy and Astrophysics
Vol/bind	692
Antal sider	18
ISSN	0004-6361
DOI	https://doi.org/10.1051/0004-6361/202450764
Status	Udgivet - 2024

Bibliografisk note

Funding Information:
The authors thank the anonymous reviewer and Daniel Angerhausen and Alycia Weinberger for comments and discussions that improved the paper. T.L. acknowledges support from the Branco Weiss Foundation and the Alfred P. Sloan Foundation (AEThER project, G202114194). Parts of this work have been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. The results reported herein benefited from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program \"Alien Earths\". S.P.Q. acknowledges the financial support of the SNSF. A.Fo. acknowledges support from the Swiss Space Office through the ESA PRODEX program. A.J. thanks the Danish National Research Foundation (DNRF Chair Grant DNRF159) and the Carlsberg Foundation (Semper Ardens: Advance grant FIRSTATMO). D.D. acknowledges the support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement CoG - 866070). V.S. acknowledges the support of the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (COBREX; grant agreement no. 885593). C.C. acknowledges support from the Science and Technology Facilities Council (Grant ST/Y001788/1). J.L.-B. is funded by the Spanish MICIU/AEI/10.13039/501100011033 and NextGenerationEU/PRTR grants PID2019-107061GB-C61 and CNS2023- 144309. A.C.-G. is funded by the Spanish Ministry of Science through MCIN/AEI/10.13039/501100011033 grant PID2019-107061GB-C61. J.K. gratefully acknowledges the support of the Swedish Research Council (VR: Etableringsbidrag 2017-04945) O.B.-R. is supported by INTA grant PRE-MDM-07, Spanish MCIN/AEI/10.13039/501100011033 grant PID2019-107061GB-C6, and CNS2023-144309. R.K. acknowledges financial support via the Heisenberg Research Grant funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grant no. KU 2849/9, project no. 445783058. This work has received funding from the Research Foundation - Flanders (FWO) under the grant number 1234224N. G.C. thanks the Swiss National Science Foundation for financial support under grant number P500PT_206785 RR edited the paper and provided feedback and analysis of results. M.T. is supported by JSPS KAKENHI grant No.18H05442. M.B. acknowledges funding from the European Union H2020-MSCA-ITN-2019 under grant agreement no. 860470 (CHAMELEON). S.K. acknowledges support by the European Research Council (ERC Consolidator grant, No. 101003096). A.B.K. is supported by the Ministry of Science, Technological Development, and Innovation of R. Serbia through projects of the University of Belgrade - Faculty of Mathematics (contract 451-03-68/2023-14/200104).

Funding Information:
The authors thank the anonymous reviewer and Daniel Angerhausen and Alycia Weinberger for comments and discussions that improved the paper. T.L. acknowledges support from the Branco Weiss Foundation and the Alfred P. Sloan Foundation (AEThER project, G202114194). Parts of this work have been carried out within the framework of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. The results reported herein benefited from collaborations and/or information exchange within NASA\u2019s Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA\u2019s Science Mission Directorate under Agreement No. 80NSSC21K0593 for the program \u201CAlien Earths\u201D. S.P.Q. acknowledges the financial support of the SNSF. A.Fo. acknowledges support from the Swiss Space Office through the ESA PRODEX program. A.J. thanks the Danish National Research Foundation (DNRF Chair Grant DNRF159) and the Carlsberg Foundation (Semper Ardens: Advance grant FIRSTATMO). D.D. acknowledges the support from the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation program (grant agreement CoG - 866070). V.S. acknowledges the support of the European Research Council (ERC) under the European Union\u2019s Horizon 2020 research and innovation program (COBREX; grant agreement no. 885593). C.C. acknowledges support from the Science and Technology Facilities Council (Grant ST/Y001788/1). J.L.-B. is funded by the Spanish MICIU/AEI/10.13039/501100011033 and NextGenerationEU/PRTR grants PID2019-107061GB-C61 and CNS2023-144309. A.C.-G. is funded by the Spanish Ministry of Science through MCIN/AEI/10.13039/501100011033 grant PID2019-107061GB-C61. J.K. gratefully acknowledges the support of the Swedish Research Council (VR: Etab-leringsbidrag 2017-04945) O.B.-R. is supported by INTA grant PRE-MDM-07, Spanish MCIN/AEI/10.13039/501100011033 grant PID2019-107061GB-C6, and CNS2023-144309. R.K. acknowledges financial support via the Heisenberg Research Grant funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grant no.KU 2849/9, project no. 445783058. This work has received funding from the Research Foundation - Flanders (FWO) under the grant number 1234224N. G.C. thanks the Swiss National Science Foundation for financial support under grant number P500PT_206785 RR edited the paper and provided feedback and analysis of results. M.T. is supported by JSPS KAKENHI grant No.18H05442. M.B. acknowledges funding from the European Union H2020-MSCA-ITN-2019 under grant agreement no. 860470 (CHAMELEON). S.K. acknowledges support by the European Research Council (ERC Consolidator grant, No. 101003096). A.B.K. is supported by the Ministry of Science, Technological Development, and Innovation of R. Serbia through projects of the University of Belgrade - Faculty of Mathematics (contract 451-03-68/2023-14/200104).

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Citationsformater

Cesario, L., Lichtenberg, T., Alei, E., Carrión-González, Ó., Dannert, F. A., Defrère, D., Ertel, S., Fortier, A., Muñoz, A. G., Glauser, A. M., Hansen, J. T., Helled, R., Huber, P. A., Ireland, M. J., Kammerer, J., Laugier, R., Lillo-Box, J., Menti, F., Meyer, M. R., ... Wordsworth, R. D. (2024). Large Interferometer For Exoplanets (LIFE): XIV. Finding terrestrial protoplanets in the galactic neighborhood. Astronomy and Astrophysics, 692, Artikel A172. https://doi.org/10.1051/0004-6361/202450764

Cesario, L, Lichtenberg, T, Alei, E, Carrión-González, Ó, Dannert, FA, Defrère, D, Ertel, S, Fortier, A, Muñoz, AG, Glauser, AM, Hansen, JT, Helled, R, Huber, PA, Ireland, MJ, Kammerer, J, Laugier, R, Lillo-Box, J, Menti, F, Meyer, MR, Noack, L, Quanz, SP, Quirrenbach, A, Rugheimer, S, van der Tak, F, Wang, HS, Anger, M, Balsalobre-Ruza, O, Bhattarai, S, Braam, M, Castro-González, A, Cockell, CS, Constantinou, T, Cugno, G, Davoult, J, Güdel, M, Hernitschek, N, Hinkley, S, Itoh, S, Janson, M, Johansen, A, Jones, HRA, Kane, SR, van Kempen, TA, Kislyakova, KG, Korth, J, Kovačević, AB, Kraus, S, Kuiper, R, Mathew, J, Matsuo, T, Miguel, Y, Min, M, Navarro, R, Ramirez, RM, Rauer, H, Vow Ricketti, B, Romagnolo, A, Schlecker, M, Sneed, EL, Squicciarini, V, Stassun, KG, Tamura, M, Viudez-Moreiras, D & Wordsworth, RD 2024, 'Large Interferometer For Exoplanets (LIFE): XIV. Finding terrestrial protoplanets in the galactic neighborhood', Astronomy and Astrophysics, bind 692, A172. https://doi.org/10.1051/0004-6361/202450764

@article{ffbc45bde36d4770a441e86b30f8ea85,

title = "Large Interferometer For Exoplanets (LIFE): XIV. Finding terrestrial protoplanets in the galactic neighborhood",

abstract = "Context. The increased brightness temperature of young rocky protoplanets during their magma ocean epoch makes them potentially amenable to atmospheric characterization at distances from the Solar System far greater than thermally equilibrated terrestrial exoplanets, offering observational opportunities for unique insights into the origin of secondary atmospheres and the near surface conditions of prebiotic environments. Aims. The Large Interferometer For Exoplanets (LIFE) mission will employ a space-based midinfrared nulling interferometer to directly measure the thermal emission of terrestrial exoplanets. In this work, we seek to assess the capabilities of various instrumental design choices of the LIFE mission concept for the detection of cooling protoplanets with transient high-temperature magma ocean atmospheres at the tail end of planetary accretion. In particular, we investigate the minimum integration times necessary to detect transient magma ocean exoplanets in young stellar associations in the Solar neighborhood. Methods. Using the LIFE mission instrument simulator (LIFEsim), we assessed how specific instrumental parameters and design choices, such as wavelength coverage, aperture diameter, and photon throughput, facilitate or disadvantage the detection of protoplan-ets. We focused on the observational sensitivities of distance to the observed planetary system, protoplanet brightness temperature (using a blackbody assumption), and orbital distance of the potential protoplanets around both G- and M-dwarf stars. Results. Our simulations suggest that LIFE will be able to detect (S/N ≥ 7) hot protoplanets in young stellar associations up to distances of 100 pc from the Solar System for reasonable integration times (up to a few hours). Detection of an Earth-sized protoplanet orbiting a Solar-sized host star at 1 AU requires less than 30 minutes of integration time. M-dwarfs generally need shorter integration times. The contribution from wavelength regions smaller than 6 μm is important for decreasing the detection threshold and discriminating emission temperatures. Conclusions. The LIFE mission is capable of detecting cooling terrestrial protoplanets within minutes to hours in several local young stellar associations hosting potential targets. The anticipated compositional range of magma ocean atmospheres motivates further architectural design studies to characterize the crucial transition from primary to secondary atmospheres.",

keywords = "Instrumentation: interferometers, Planets and satellites: detection, Planets and satellites: terrestrial planets",

author = "Lorenzo Cesario and Tim Lichtenberg and Eleonora Alei and {\'O}scar Carri{\'o}n-Gonz{\'a}lez and Dannert, {Felix A.} and Denis Defr{\`e}re and Steve Ertel and Andrea Fortier and Mu{\~n}oz, {A. Garc{\'i}a} and Glauser, {Adrian M.} and Hansen, {Jonah T.} and Ravit Helled and Huber, {Philipp A.} and Ireland, {Michael J.} and Jens Kammerer and Romain Laugier and Jorge Lillo-Box and Franziska Menti and Meyer, {Michael R.} and Lena Noack and Quanz, {Sascha P.} and Andreas Quirrenbach and Sarah Rugheimer and {van der Tak}, Floris and Wang, {Haiyang S.} and Marius Anger and Olga Balsalobre-Ruza and Surendra Bhattarai and Marrick Braam and Amadeo Castro-Gonz{\'a}lez and Cockell, {Charles S.} and Tereza Constantinou and Gabriele Cugno and Jeanne Davoult and Manuel G{\"u}del and Nina Hernitschek and Sasha Hinkley and Satoshi Itoh and Markus Janson and Anders Johansen and Jones, {Hugh R. A.} and Kane, {Stephen R.} and {van Kempen}, {Tim A.} and Kislyakova, {Kristina G.} and Judith Korth and Kova{\v c}evi{\'c}, {Andjelka B.} and Stefan Kraus and Rolf Kuiper and Joice Mathew and Taro Matsuo and Yamila Miguel and Michiel Min and Ramon Navarro and Ramirez, {Ramses M.} and Heike Rauer and {Vow Ricketti}, Berke and Amedeo Romagnolo and Martin Schlecker and Sneed, {Evan L.} and Vito Squicciarini and Stassun, {Keivan G.} and Motohide Tamura and Daniel Viudez-Moreiras and Wordsworth, {Robin D.}",

note = "Publisher Copyright: {\textcopyright} The Authors 2024.",

year = "2024",

doi = "10.1051/0004-6361/202450764",

language = "English",

volume = "692",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "E D P Sciences",

}

TY - JOUR

T1 - Large Interferometer For Exoplanets (LIFE)

T2 - XIV. Finding terrestrial protoplanets in the galactic neighborhood

AU - Cesario, Lorenzo

AU - Lichtenberg, Tim

AU - Alei, Eleonora

AU - Carrión-González, Óscar

AU - Dannert, Felix A.

AU - Defrère, Denis

AU - Ertel, Steve

AU - Fortier, Andrea

AU - Muñoz, A. García

AU - Glauser, Adrian M.

AU - Hansen, Jonah T.

AU - Helled, Ravit

AU - Huber, Philipp A.

AU - Ireland, Michael J.

AU - Kammerer, Jens

AU - Laugier, Romain

AU - Lillo-Box, Jorge

AU - Menti, Franziska

AU - Meyer, Michael R.

AU - Noack, Lena

AU - Quanz, Sascha P.

AU - Quirrenbach, Andreas

AU - Rugheimer, Sarah

AU - van der Tak, Floris

AU - Wang, Haiyang S.

AU - Anger, Marius

AU - Balsalobre-Ruza, Olga

AU - Bhattarai, Surendra

AU - Braam, Marrick

AU - Castro-González, Amadeo

AU - Cockell, Charles S.

AU - Constantinou, Tereza

AU - Cugno, Gabriele

AU - Davoult, Jeanne

AU - Güdel, Manuel

AU - Hernitschek, Nina

AU - Hinkley, Sasha

AU - Itoh, Satoshi

AU - Janson, Markus

AU - Johansen, Anders

AU - Jones, Hugh R. A.

AU - Kane, Stephen R.

AU - van Kempen, Tim A.

AU - Kislyakova, Kristina G.

AU - Korth, Judith

AU - Kovačević, Andjelka B.

AU - Kraus, Stefan

AU - Kuiper, Rolf

AU - Mathew, Joice

AU - Matsuo, Taro

AU - Miguel, Yamila

AU - Min, Michiel

AU - Navarro, Ramon

AU - Ramirez, Ramses M.

AU - Rauer, Heike

AU - Vow Ricketti, Berke

AU - Romagnolo, Amedeo

AU - Schlecker, Martin

AU - Sneed, Evan L.

AU - Squicciarini, Vito

AU - Stassun, Keivan G.

AU - Tamura, Motohide

AU - Viudez-Moreiras, Daniel

AU - Wordsworth, Robin D.

PY - 2024

Y1 - 2024

N2 - Context. The increased brightness temperature of young rocky protoplanets during their magma ocean epoch makes them potentially amenable to atmospheric characterization at distances from the Solar System far greater than thermally equilibrated terrestrial exoplanets, offering observational opportunities for unique insights into the origin of secondary atmospheres and the near surface conditions of prebiotic environments. Aims. The Large Interferometer For Exoplanets (LIFE) mission will employ a space-based midinfrared nulling interferometer to directly measure the thermal emission of terrestrial exoplanets. In this work, we seek to assess the capabilities of various instrumental design choices of the LIFE mission concept for the detection of cooling protoplanets with transient high-temperature magma ocean atmospheres at the tail end of planetary accretion. In particular, we investigate the minimum integration times necessary to detect transient magma ocean exoplanets in young stellar associations in the Solar neighborhood. Methods. Using the LIFE mission instrument simulator (LIFEsim), we assessed how specific instrumental parameters and design choices, such as wavelength coverage, aperture diameter, and photon throughput, facilitate or disadvantage the detection of protoplan-ets. We focused on the observational sensitivities of distance to the observed planetary system, protoplanet brightness temperature (using a blackbody assumption), and orbital distance of the potential protoplanets around both G- and M-dwarf stars. Results. Our simulations suggest that LIFE will be able to detect (S/N ≥ 7) hot protoplanets in young stellar associations up to distances of 100 pc from the Solar System for reasonable integration times (up to a few hours). Detection of an Earth-sized protoplanet orbiting a Solar-sized host star at 1 AU requires less than 30 minutes of integration time. M-dwarfs generally need shorter integration times. The contribution from wavelength regions smaller than 6 μm is important for decreasing the detection threshold and discriminating emission temperatures. Conclusions. The LIFE mission is capable of detecting cooling terrestrial protoplanets within minutes to hours in several local young stellar associations hosting potential targets. The anticipated compositional range of magma ocean atmospheres motivates further architectural design studies to characterize the crucial transition from primary to secondary atmospheres.

AB - Context. The increased brightness temperature of young rocky protoplanets during their magma ocean epoch makes them potentially amenable to atmospheric characterization at distances from the Solar System far greater than thermally equilibrated terrestrial exoplanets, offering observational opportunities for unique insights into the origin of secondary atmospheres and the near surface conditions of prebiotic environments. Aims. The Large Interferometer For Exoplanets (LIFE) mission will employ a space-based midinfrared nulling interferometer to directly measure the thermal emission of terrestrial exoplanets. In this work, we seek to assess the capabilities of various instrumental design choices of the LIFE mission concept for the detection of cooling protoplanets with transient high-temperature magma ocean atmospheres at the tail end of planetary accretion. In particular, we investigate the minimum integration times necessary to detect transient magma ocean exoplanets in young stellar associations in the Solar neighborhood. Methods. Using the LIFE mission instrument simulator (LIFEsim), we assessed how specific instrumental parameters and design choices, such as wavelength coverage, aperture diameter, and photon throughput, facilitate or disadvantage the detection of protoplan-ets. We focused on the observational sensitivities of distance to the observed planetary system, protoplanet brightness temperature (using a blackbody assumption), and orbital distance of the potential protoplanets around both G- and M-dwarf stars. Results. Our simulations suggest that LIFE will be able to detect (S/N ≥ 7) hot protoplanets in young stellar associations up to distances of 100 pc from the Solar System for reasonable integration times (up to a few hours). Detection of an Earth-sized protoplanet orbiting a Solar-sized host star at 1 AU requires less than 30 minutes of integration time. M-dwarfs generally need shorter integration times. The contribution from wavelength regions smaller than 6 μm is important for decreasing the detection threshold and discriminating emission temperatures. Conclusions. The LIFE mission is capable of detecting cooling terrestrial protoplanets within minutes to hours in several local young stellar associations hosting potential targets. The anticipated compositional range of magma ocean atmospheres motivates further architectural design studies to characterize the crucial transition from primary to secondary atmospheres.

KW - Instrumentation: interferometers

KW - Planets and satellites: detection

KW - Planets and satellites: terrestrial planets

U2 - 10.1051/0004-6361/202450764

DO - 10.1051/0004-6361/202450764

M3 - Journal article

AN - SCOPUS:85212458349

SN - 0004-6361

VL - 692

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A172

ER -