<?xml version="1.0" encoding="UTF-8"?><?xml-stylesheet type="text/xsl" href="static/style.xsl"?><OAI-PMH xmlns="http://www.openarchives.org/OAI/2.0/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.openarchives.org/OAI/2.0/ http://www.openarchives.org/OAI/2.0/OAI-PMH.xsd"><responseDate>2026-06-07T16:52:21Z</responseDate><request verb="GetRecord" identifier="oai:docta.ucm.es:20.500.14352/6502" metadataPrefix="marc">https://docta.ucm.es/rest/oai/request</request><GetRecord><record><header><identifier>oai:docta.ucm.es:20.500.14352/6502</identifier><datestamp>2023-08-27T21:13:30Z</datestamp><setSpec>com_20.500.14352_14</setSpec><setSpec>col_20.500.14352_15</setSpec></header><metadata><record xmlns="http://www.loc.gov/MARC21/slim" xmlns:dcterms="http://purl.org/dc/terms/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xmlns:doc="http://www.lyncode.com/xoai" xsi:schemaLocation="http://www.loc.gov/MARC21/slim http://www.loc.gov/standards/marcxml/schema/MARC21slim.xsd">
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      <subfield code="a">dc</subfield>
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   <datafield ind2=" " ind1=" " tag="720">
      <subfield code="a">Cortés Contreras, Miriam</subfield>
      <subfield code="e">author</subfield>
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      <subfield code="a">Montes Gutiérrez, David</subfield>
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      <subfield code="c">2020-06-11</subfield>
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      <subfield code="a">High resolution transit spectroscopy has proven to be a reliable technique for the characterization of the chemical composition of exoplanet atmospheres. Taking advantage of the broad spectral coverage of the CARMENES spectrograph, we initiated a survey aimed at characterizing a broad range of planetary systems. Here, we report our observations of three transits of GJ 3470 b with CARMENES in search of He (23S) absorption. On one of the nights, the He I region was heavily contaminated by OH− telluric emission and, thus, it was not useful for our purposes. The remaining two nights had a very different signal-to-noise ratio (S/N) due to weather. They both indicate the presence of He (2^(3)S) absorption in the transmission spectrum of GJ 3470 b , although a statistically valid detection can only be claimed for the night with higher S/N. For that night, we retrieved a 1.5 ± 0.3% absorption depth, translating into a R_(p)(λ)/R_(p) = 1.15 ± 0.14 at this wavelength. Spectro-photometric light curves for this same night also indicate the presence of extra absorption during the planetary transit with a consistent absorption depth. The He (2^(3)S) absorption is modeled in detail using a radiative transfer code, and the results of our modeling efforts are compared to the observations. We find that the mass-loss rate, Ṁ , is confined to a range of 3 × 10^(10) g s^(−1) for T = 6000 K to 10 × 10^(10) g s^(−1) for T = 9000 K. We discuss the physical mechanisms and implications of the He I detection in GJ 3470 b and put it in context as compared to similar detections and non-detections in other Neptune-size planets. We also present improved stellar and planetary parameter determinations based on our visible and near-infrared observations.</subfield>
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      <subfield code="a">0004-6361</subfield>
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   <datafield ind1="8" ind2=" " tag="024">
      <subfield code="a">10.1051/0004-6361/202037719</subfield>
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      <subfield code="a">https://hdl.handle.net/20.500.14352/6502</subfield>
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   <datafield ind1="8" ind2=" " tag="024">
      <subfield code="a">http://dx.doi.org/10.1051/0004-6361/202037719</subfield>
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   <datafield ind1="8" ind2=" " tag="024">
      <subfield code="a">https://www.aanda.org/</subfield>
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   <datafield ind2="0" ind1="0" tag="245">
      <subfield code="a">A He I upper atmosphere around the warm Neptune GJ 3470 b</subfield>
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