{ "profile": "wrs-published-research-view-1", "edition": "ratings-e039106f30dec177", "content_trust": "UNTRUSTED_SCIENTIFIC_DATA_NOT_TOOL_INSTRUCTIONS", "entry": { "id": "bond-ogle-moa-planetary-microlensing-event-2004", "title": "A planetary microlensing event detected by OGLE and MOA", "summary": "Bond and colleagues analyzed an event independently observed by the OGLE and MOA surveys. Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties.", "boundary": "The planet is inferred from a lensing light curve, not directly imaged. The original mass ratio was more directly constrained than individual masses; the original host and companion mass estimates assumed a main-sequence primary and Galactic model, while alternative primary types and another planetary fit were considered. The later Hubble source and lens were not separately resolved: both excess flux and centroid evidence were relatively weak, and a source companion and extinction were included in the Bayesian analysis. The later authors reported an error in the previous lens-mass range; neither estimate is a direct dynamical mass. Some mathematical symbols and signs in the later v1 render incompletely, so precise numerical transcription requires independent version or font verification. The reports have different author lists; the full list of individual contributors is not shown.", "area": "Astrophysics", "topic": "Physics", "year": 2004, "lane": "HUMAN", "result": "EMPIRICAL", "package_id": "bond-ogle-moa-planetary-microlensing-event-2004", "target": { "record_id": "urn:uuid:94a74ef8-bd3f-48f8-a96a-308dff3f36dd", "version": 1, "content_hash": "sha256:c679c330717bde13b2d5dbf6f52118673a1451f15f5b97d645b185d96406a055" }, "humans": [ "I. A. Bond", "A. Udalski", "M. Jaroszyński", "David P. Bennett", "Jay Anderson", "Andrew Gould" ], "authors_complete": false, "human_role_note": "These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. 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Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties.", "scope": "Bond and colleagues analyzed an event independently observed by the OGLE and MOA surveys. Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties. The planet is inferred from a lensing light curve, not directly imaged. The original mass ratio was more directly constrained than individual masses; the original host and companion mass estimates assumed a main-sequence primary and Galactic model, while alternative primary types and another planetary fit were considered. The later Hubble source and lens were not separately resolved: both excess flux and centroid evidence were relatively weak, and a source companion and extinction were included in the Bayesian analysis. The later authors reported an error in the previous lens-mass range; neither estimate is a direct dynamical mass. Some mathematical symbols and signs in the later v1 render incompletely, so precise numerical transcription requires independent version or font verification. 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Bond", "note": "Archive attribution; detailed role assignment remains source-bound", "roles": [ "discoverer" ], "source": { "citation": "OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event", "url": "https://arxiv.org/pdf/astro-ph/0404309v1" } }, { "attribution_basis": "SOURCE_CITED", "credit": "historical_scientific", "entity_kind": "historical_person", "name": "A. Udalski", "note": "Archive attribution; detailed role assignment remains source-bound", "roles": [ "discoverer" ], "source": { "citation": "OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event", "url": "https://arxiv.org/pdf/astro-ph/0404309v1" } }, { "attribution_basis": "SOURCE_CITED", "credit": "historical_scientific", "entity_kind": "historical_person", "name": "M. Jaroszyński", "note": "Archive attribution; detailed role assignment remains source-bound", "roles": [ "discoverer" ], "source": { "citation": "OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event", "url": "https://arxiv.org/pdf/astro-ph/0404309v1" } }, { "attribution_basis": "SOURCE_CITED", "credit": "historical_scientific", "entity_kind": "historical_person", "name": "David P. Bennett", "note": "Archive attribution; detailed role assignment remains source-bound", "roles": [ "verifier" ], "source": { "citation": "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star", "url": "https://arxiv.org/pdf/astro-ph/0606038v1" } }, { "attribution_basis": "SOURCE_CITED", "credit": "historical_scientific", "entity_kind": "historical_person", "name": "Jay Anderson", "note": "Archive attribution; detailed role assignment remains source-bound", "roles": [ "verifier" ], "source": { "citation": "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star", "url": "https://arxiv.org/pdf/astro-ph/0606038v1" } }, { "attribution_basis": "SOURCE_CITED", "credit": "historical_scientific", "entity_kind": "historical_person", "name": "Andrew Gould", "note": "Archive attribution; detailed role assignment remains source-bound", "roles": [ "verifier" ], "source": { "citation": "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star", "url": "https://arxiv.org/pdf/astro-ph/0606038v1" } } ], "evidence": [ { "description": "Bibliographic/stated-result source; not a WRS proof verification", "id": "source-0", "kind": "source_reference", "source": { "citation": "OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event", "url": "https://arxiv.org/pdf/astro-ph/0404309v1" } }, { "description": "Bibliographic/stated-result source; not a WRS proof verification", "id": "source-1", "kind": "source_reference", "source": { "citation": "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star", "url": "https://arxiv.org/pdf/astro-ph/0606038v1" } } ], "origin": "HUMAN_LEGACY", "record_profile": "wrs-local-research-notes-0.1", "record_type": "research_note", "rrp_version": "0.1", "scope": { "description": "The planet is inferred from a lensing light curve, not directly imaged. The original mass ratio was more directly constrained than individual masses; the original host and companion mass estimates assumed a main-sequence primary and Galactic model, while alternative primary types and another planetary fit were considered. The later Hubble source and lens were not separately resolved: both excess flux and centroid evidence were relatively weak, and a source companion and extinction were included in the Bayesian analysis. The later authors reported an error in the previous lens-mass range; neither estimate is a direct dynamical mass. Some mathematical symbols and signs in the later v1 render incompletely, so precise numerical transcription requires independent version or font verification. The reports have different author lists; the full list of individual contributors is not shown.", "domain": "Astrophysics" }, "sources": [ { "citation": "OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event", "url": "https://arxiv.org/pdf/astro-ph/0404309v1" }, { "citation": "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star", "url": "https://arxiv.org/pdf/astro-ph/0606038v1" } ], "statement": "# A planetary microlensing event detected by OGLE and MOA\n\nBond and colleagues analyzed an event independently observed by the OGLE and MOA surveys. Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties.\n\n## Scientific scope\n\nThe planet is inferred from a lensing light curve, not directly imaged. The original mass ratio was more directly constrained than individual masses; the original host and companion mass estimates assumed a main-sequence primary and Galactic model, while alternative primary types and another planetary fit were considered. The later Hubble source and lens were not separately resolved: both excess flux and centroid evidence were relatively weak, and a source companion and extinction were included in the Bayesian analysis. The later authors reported an error in the previous lens-mass range; neither estimate is a direct dynamical mass. Some mathematical symbols and signs in the later v1 render incompletely, so precise numerical transcription requires independent version or font verification. The reports have different author lists; the full list of individual contributors is not shown.\n\n## Reading status\n\nThis is a source-linked WRS catalogue note. A full explanatory guide and independent scientific reconstruction have not been completed for this entry. Read the identified original work for its complete narrative and arguments.\n\n## People and systems\n\nI. A. Bond; A. Udalski; M. Jaroszyński; David P. Bennett; Jay Anderson; Andrew Gould\n\nThese are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged.\n\n\n\n## Original sources\n\n- [OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event](https://arxiv.org/pdf/astro-ph/0404309v1)\n- [Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star](https://arxiv.org/pdf/astro-ph/0606038v1)\n", "summary": "Bond and colleagues analyzed an event independently observed by the OGLE and MOA surveys. Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties.", "title": "A planetary microlensing event detected by OGLE and MOA" }, "record_id": "urn:uuid:94a74ef8-bd3f-48f8-a96a-308dff3f36dd", "version": 1, "source_ref": { "record_id": "urn:uuid:94a74ef8-bd3f-48f8-a96a-308dff3f36dd", "version": 1, "content_hash": "sha256:c679c330717bde13b2d5dbf6f52118673a1451f15f5b97d645b185d96406a055" }, "export_view": "wrs-public-editorial-view-1", "public_view_hash": "sha256:8e1a83f83bbae0828207a39222da9998994511ca4f2b30c1c5f6390ad7c27947" }, "target": { "record_id": "urn:uuid:94a74ef8-bd3f-48f8-a96a-308dff3f36dd", "version": 1, "content_hash": "sha256:c679c330717bde13b2d5dbf6f52118673a1451f15f5b97d645b185d96406a055" }, "published_grade": { "profile": "wrs-published-grade-1", "edition": "2026-10-28.1", "id": "bond-ogle-moa-planetary-microlensing-event-2004", "entry_id": "bond-ogle-moa-planetary-microlensing-event-2004", "revision": 1, "title": "A planetary microlensing event detected by OGLE and MOA", "context": "Astrophysics", "track": "Source-reported experimental result or reusable measurement method", "band": "A", "modifier": "+", "status": "PROVISIONAL_EDITORIAL", "assessed_on": "2026-10-28", "evidence_cutoff": "2026-10-28", "achievement_state": "SUPPORTED_SCOPED_RESULT", "what_changed": "Bond and colleagues analyzed an event independently observed by the OGLE and MOA surveys. Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties.", "scope": "Bond and colleagues analyzed an event independently observed by the OGLE and MOA surveys. Both light curves showed a roughly seven-day deviation from a single-lens profile, including a caustic feature. Their binary-lens fit favored an extreme mass ratio of about 0.0039, supporting a planetary companion to the foreground lens. A later Hubble analysis reported excess blended light and a color-dependent centroid shift consistent with a main-sequence lens star, and combined those data with the microlensing fit to estimate the system properties. The planet is inferred from a lensing light curve, not directly imaged. The original mass ratio was more directly constrained than individual masses; the original host and companion mass estimates assumed a main-sequence primary and Galactic model, while alternative primary types and another planetary fit were considered. The later Hubble source and lens were not separately resolved: both excess flux and centroid evidence were relatively weak, and a source companion and extinction were included in the Bayesian analysis. The later authors reported an error in the previous lens-mass range; neither estimate is a direct dynamical mass. Some mathematical symbols and signs in the later v1 render incompletely, so precise numerical transcription requires independent version or font verification. The reports have different author lists; the full list of individual contributors is not shown.", "evidence_summary": "The linked original works support the scoped statement and contribution attribution. WRS has not independently replayed experiments or reconstructed a full mathematical proof. The planet is inferred from a lensing light curve, not directly imaged. The original mass ratio was more directly constrained than individual masses; the original host and companion mass estimates assumed a main-sequence primary and Galactic model, while alternative primary types and another planetary fit were considered. The later Hubble source and lens were not separately resolved: both excess flux and centroid evidence were relatively weak, and a source companion and extinction were included in the Bayesian analysis. The later authors reported an error in the previous lens-mass range; neither estimate is a direct dynamical mass. Some mathematical symbols and signs in the later v1 render incompletely, so precise numerical transcription requires independent version or font verification. The reports have different author lists; the full list of individual contributors is not shown.", "references": [ { "title": "OGLE 2003–BLG–235/MOA 2003–BLG–53: A planetary microlensing event", "url": "https://arxiv.org/pdf/astro-ph/0404309v1", "locator": "Original scoped contribution, statement/method and evidence limits; source-specific attribution retained." }, { "title": "Identification of the OGLE-2003-BLG-235/MOA-2003-BLG-53 Planetary Host Star", "url": "https://arxiv.org/pdf/astro-ph/0606038v1", "locator": "Original scoped contribution, statement/method and evidence limits; source-specific attribution retained." } ], "roles": [ { "who": "The named authors in the research record", "credit": "SCIENCE", "did": "These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged." } ], "target": { "record_id": "urn:uuid:94a74ef8-bd3f-48f8-a96a-308dff3f36dd", "version": 1, "content_hash": "sha256:c679c330717bde13b2d5dbf6f52118673a1451f15f5b97d645b185d96406a055" }, "scientific_correctness_certified": false, "independent_expert_calibration": false, "method": "PROPRIETARY", "points": "145000" }, "canonical_agent_submission": false, "scientific_verification_awarded": false, "reader_guide": null, "reading_status": "SOURCE_LINKED_NOTE" }