{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,9,9]],"date-time":"2026-09-09T00:46:34Z","timestamp":1788914794914,"version":"build-2803163510"},"reference-count":92,"publisher":"American Physical Society (APS)","issue":"5","license":[{"start":{"date-parts":[[2026,7,28]],"date-time":"2026-07-28T00:00:00Z","timestamp":1785196800000},"content-version":"vor","delay-in-days":0,"URL":"https:\/\/creativecommons.org\/licenses\/by\/4.0\/"}],"funder":[{"DOI":"10.13039\/100000001","name":"National Science Foundation","doi-asserted-by":"publisher","award":["PHY-2412701"],"award-info":[{"award-number":["PHY-2412701"]}],"id":[{"id":"10.13039\/100000001","id-type":"DOI","asserted-by":"publisher"}]},{"DOI":"10.13039\/100000001","name":"National Science Foundation","doi-asserted-by":"publisher","award":["PHY-2210452"],"award-info":[{"award-number":["PHY-2210452"]}],"id":[{"id":"10.13039\/100000001","id-type":"DOI","asserted-by":"publisher"}]},{"DOI":"10.13039\/501100001659","name":"Deutsche Forschungsgemeinschaft","doi-asserted-by":"publisher","award":["EXC-2094\u201339078331"],"award-info":[{"award-number":["EXC-2094\u201339078331"]}],"id":[{"id":"10.13039\/501100001659","id-type":"DOI","asserted-by":"publisher"}]},{"DOI":"10.13039\/100007739","name":"Aspen Center for Physics","doi-asserted-by":"publisher","id":[{"id":"10.13039\/100007739","id-type":"DOI","asserted-by":"publisher"}]},{"DOI":"10.13039\/100006230","name":"Fermilab","doi-asserted-by":"publisher","award":["URA-22-F-13"],"award-info":[{"award-number":["URA-22-F-13"]}],"id":[{"id":"10.13039\/100006230","id-type":"DOI","asserted-by":"publisher"}]},{"name":"Tom and Carolyn Marquez Chair Fund"}],"content-domain":{"domain":["journals.aps.org"],"crossmark-restriction":true},"short-container-title":["Phys. Rev. Lett."],"accepted":{"date-parts":[[2026,6,30]]},"abstract":"<jats:p>\n                    A first-order phase transition could occur in the late Universe when vacuum energy begins dominating the energy density (\n                    <a:math xmlns:a=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" display=\"inline\">\n                      <a:mrow>\n                        <a:mi>z<\/a:mi>\n                        <a:mo>\u2272<\/a:mo>\n                        <a:mn>0.3<\/a:mn>\n                      <\/a:mrow>\n                    <\/a:math>\n                    ) and convert some latent heat into other forms such as invisible radiation. This generic possibility also has concrete motivation in particle physics models, which invoke a multitude of vacua to address theoretical puzzles. The na\u00efve constraint on such an event comes from measurements of the Hubble expansion rate, but this can only probe transitions involving\n                    <c:math xmlns:c=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" display=\"inline\">\n                      <c:mrow>\n                        <c:mi mathvariant=\"script\">O<\/c:mi>\n                        <c:mo stretchy=\"false\">(<\/c:mo>\n                        <c:mn>10<\/c:mn>\n                        <c:mo stretchy=\"false\">)<\/c:mo>\n                        <c:mo>%<\/c:mo>\n                      <\/c:mrow>\n                    <\/c:math>\n                    of the dark energy. In this Letter, we show that significantly tighter constraints appear when accounting for phase transition fluctuations affecting CMB photon propagation anisotropically. For instance, if a completed phase transition has\n                    <h:math xmlns:h=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" display=\"inline\">\n                      <h:mrow>\n                        <h:mi>\u03b2<\/h:mi>\n                        <h:mo>\/<\/h:mo>\n                        <h:msub>\n                          <h:mrow>\n                            <h:mi>H<\/h:mi>\n                          <\/h:mrow>\n                          <h:mrow>\n                            <h:mo>\u22c6<\/h:mo>\n                          <\/h:mrow>\n                        <\/h:msub>\n                        <h:mo>\u2272<\/h:mo>\n                        <h:mn>25<\/h:mn>\n                      <\/h:mrow>\n                    <\/h:math>\n                    , current CMB data limit the associated vacuum energy released to less than 1% of the dark energy. A transition to negative vacuum energy (quasi-anti\u2013de Sitter) is allowed only for\n                    <j:math xmlns:j=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" display=\"inline\">\n                      <j:mrow>\n                        <j:mi>\u03b2<\/j:mi>\n                        <j:mo>\/<\/j:mo>\n                        <j:msub>\n                          <j:mrow>\n                            <j:mi>H<\/j:mi>\n                          <\/j:mrow>\n                          <j:mrow>\n                            <j:mo>\u22c6<\/j:mo>\n                          <\/j:mrow>\n                        <\/j:msub>\n                        <j:mo>\u2273<\/j:mo>\n                        <j:mn>300<\/j:mn>\n                      <\/j:mrow>\n                    <\/j:math>\n                    . For\n                    <l:math xmlns:l=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" display=\"inline\">\n                      <l:mrow>\n                        <l:mi>\u03b2<\/l:mi>\n                        <l:mo>\/<\/l:mo>\n                        <l:msub>\n                          <l:mrow>\n                            <l:mi>H<\/l:mi>\n                          <\/l:mrow>\n                          <l:mrow>\n                            <l:mo>\u22c6<\/l:mo>\n                          <\/l:mrow>\n                        <\/l:msub>\n                        <l:mo>\u2272<\/l:mo>\n                        <l:mn>500<\/l:mn>\n                      <\/l:mrow>\n                    <\/l:math>\n                    , the Universe will not crunch for at least 14\u00a0Gyr.\n                  <\/jats:p>","DOI":"10.1103\/1vyz-xdkb","type":"journal-article","created":{"date-parts":[[2026,6,30]],"date-time":"2026-06-30T19:05:00Z","timestamp":1782846300000},"update-policy":"https:\/\/doi.org\/10.1103\/crossmark-policy","source":"Crossref","is-referenced-by-count":1,"title":["Boiling After the Dust Settles: Constraining First-Order Phase Transitions During Dark Energy Domination"],"prefix":"10.1103","volume":"137","author":[{"ORCID":"https:\/\/orcid.org\/0000-0003-2409-4171","authenticated-orcid":true,"given":"Seth","family":"Koren","sequence":"first","affiliation":[{"id":[{"id":"https:\/\/ror.org\/00mkhxb43","id-type":"ROR","asserted-by":"publisher"}],"name":"University of Notre 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