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{{short description|European X-ray space observatory}}
{{short description|European X-ray space observatory}}
{{Use British English|date=March 2021}}
{{Use dmy dates|date=September 2019}}
{{Use dmy dates|date=September 2019}}
{{EngvarB|date=July 2019}}
{{Infobox spaceflight
{{Infobox spaceflight
| name = Advanced Telescope for High Energy Astrophysics
| name = Advanced Telescope for High-ENergy Astrophysics
| names_list =
| names_list = ''Athena''
| image =
| image =
| image_caption =
| image_caption =
| image_size = 300px
| image_alt = <!--image alt text-->
| image_size = <!--include px/em; defaults to 220px-->

| mission_type = [[Space telescope]]
| mission_type = [[Space telescope]]
| operator = [[European Space Agency]]
| operator = [[European Space Agency]] (ESA)
| COSPAR_ID =
⚫
| website = {{url|http://www.the-athena-x-ray-observatory.eu/ }}
| SATCAT =
⚫
| mission_duration = 4 years plus possible extensions
⚫
| website = {{url|http://www.the-athena-x-ray-observatory.eu/}}
⚫
| launch_date = 2030s<ref name="athena-summary">{{cite web |url=http://sci.esa.int/athena/59896-mission-summary/ |title=Athena: Mission Summary |publisher=[[European Space Agency|ESA]] |date=4 October 2018 |access-date=19 December 2018}}</ref>
⚫
| mission_duration = 4 years (planned)
| launch_rocket = [[Ariane 64]]<ref name="athena-summary">{{cite web |url=http://sci.esa.int/athena/59896-mission-summary/ |title=Athena: Mission Summary |publisher=[[European Space Agency|ESA]] |date=4 October 2018 |access-date=19 December 2018}}</ref>
⚫
| launch_date = 2035 (planned)<ref name="athena-summary">{{cite web|url=https://sci.esa.int/web/athena/-/59896-mission-summary|title=Athena: Mission Summary|publisher=ESA|date=2 May 2022|access-date=4 May 2022}}</ref>

| launch_rocket = [[Ariane 64]]
<!--orbit parameters-->
| launch_site = [[Guiana Space Centre|Centre Spatial Guyanais]]
| launch_contractor = [[Arianespace]]
| orbit_reference = {{L2|pt=yes}} (baseline)
| orbit_reference = {{L2|pt=yes}} (baseline)

<!--Telescope parameters-->
| instrument_type = <!--converts telescope fields to suit a camera or other similar instrument-->
| telescope_name = <!--name, if different to the satellite-->
| telescope_type = [[X-ray telescope]]
| telescope_type = [[X-ray telescope]]
| telescope_diameter = <!--diameter of telescope-->
| telescope_diameter =
| telescope_focal_length = {{cvt|12|m}}
| telescope_focal_length = {{cvt|12|m}}
| telescope_wavelength =
| telescope_area = <!--collecting area-->
| telescope_wavelength = <!--wavelengths at which the telescope operates-->
| telescope_resolution = <!--resolution of telescope-->
| instruments = X-ray Integral Field Unit, Wide Field Imager
| instruments = X-ray Integral Field Unit, Wide Field Imager
| instruments_list = {{Infobox spaceflight/Instruments
| instruments_list = {{Infobox spaceflight/Instruments
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| acronym2 = WFI | name2 = Wide Field Imager
| acronym2 = WFI | name2 = Wide Field Imager
}}
}}
| insignia =

⚫
| insignia_caption =
<!--mission insignia or patch-->
| insignia_size = 200px
| insignia = <!--omit the "file" prefix-->
⚫
| insignia_caption = <!--image caption-->
| insignia_alt = <!--image alt text-->
| insignia_size = <!--include px/em; defaults to 180px-->

| programme = '''[[Cosmic Vision]]'''
| programme = '''[[Cosmic Vision]]'''
| previous_mission = [[Comet Interceptor]]
| previous_mission = [[Comet Interceptor]]
| next_mission = [[Laser Interferometer Space Antenna|LISA]]
| next_mission = [[Laser Interferometer Space Antenna]] (LISA)
}}
}}


'''Advanced Telescope for High-ENergy Astrophysics''' (''Athena'')<ref name="athena-summary">{{cite web |url=http://sci.esa.int/athena/59896-mission-summary/ |title=Athena: Mission Summary |publisher=[[European Space Agency|ESA]] |date=4 October 2018 |access-date=19 December 2018}}</ref><ref>{{Cite web|url=https://www.the-athena-x-ray-observatory.eu/|title=The Athena X-ray Observatory: Community Support Portal}}</ref> is an X-ray observatory mission selected by [[European Space Agency|ESA]] within its [[Cosmic Vision|Cosmic Vision Program]] <ref name="l2mission">{{Cite web | title = ESA's new vision to study the invisible universe| publisher = ESA | url = http://www.esa.int/Our_Activities/Space_Science/ESA_s_new_vision_to_study_the_invisible_Universe |access-date = 29 November 2013}}</ref> to address the Hot and Energetic Universe scientific theme. ''Athena'' will operate in the energy range of 0.2–12keV and will offer spectroscopic and imaging capabilities exceeding those of currently operating [[X-ray astronomy satellite|X-ray astronomy satellites]] – e.g. the [[Chandra X-ray Observatory]] and [[XMM-Newton]] – by at least one order of magnitude on several parameter spaces simultaneously.
'''Advanced Telescope for High-ENergy Astrophysics''' ('''''Athena''''')<ref name="athena-summary"/><ref>{{cite web|url=https://www.the-athena-x-ray-observatory.eu/|title=The Athena X-ray Observatory: Community Support Portal|publisher=ESA|date=8 March 2021|access-date=14 March 2021}}</ref> is an X-ray observatory mission selected by [[European Space Agency]] (ESA) within its [[Cosmic Vision|Cosmic Vision program]]<ref name="l2mission">{{cite web|title=ESA's new vision to study the invisible universe|publisher=ESA|url=https://www.esa.int/Our_Activities/Space_Science/ESA_s_new_vision_to_study_the_invisible_Universe |date=8 March 2021|access-date=14 March 2021}}</ref> to address the Hot and Energetic Universe scientific theme. ''Athena'' will operate in the energy range of 0.2–12 [[Electronvolt|keV]] and will offer spectroscopic and imaging capabilities exceeding those of currently operating [[X-ray astronomy satellite]]s – e.g. the [[Chandra X-ray Observatory]] and [[XMM-Newton]] – by at least one order of magnitude on several parameter spaces simultaneously.


== Mission ==
The primary goals of the mission are to map hot gas structures, determine their physical properties, and search for [[supermassive black hole]]s.
The primary goals of the mission are to map hot gas structures, determine their physical properties, and search for [[supermassive black hole]]s.


==History and development==
== History and development ==
The mission has its roots in two concepts from the early 2000s, ESA’s [[XEUS]] and NASA’s [[Constellation-X]]. Around 2008, these two proposals were merged into the joint NASA/ESA/JAXA [[International X-ray Observatory]] (IXO) proposal. In 2011, IXO was withdrawn and then ESA decided to proceed with a cost-reduced modification, which became known as ATHENA.<ref>{{cite web|url=http://sci.esa.int/ixo/48729-about-athena/|title=About ATHENA|date=2 April 2012|publisher=[[ESA]]|access-date=19 October 2014}}</ref> ''Athena'' was selected in 2014 to become the second (L2) L-class Cosmic Vision mission,<ref name="athenaReboot">{{cite web|url=http://sci.esa.int/cosmic-vision/54241-athena-to-study-the-hot-and-energetic-universe/|title=ESA Science & Technology: Athena to study the hot and energetic Universe|date=27 June 2014|publisher=[[ESA]]|access-date=23 August 2014}}</ref> addressing the Hot and Energetic Universe science theme.
The mission has its roots in two concepts from the early 2000s, [[XEUS]] of ESA and [[Constellation-X Observatory]] (Con-X) of [[NASA]]. Around 2008, these two proposals were merged into the joint NASA/ESA/JAXA [[International X-ray Observatory]] (IXO) proposal. In 2011, IXO was withdrawn and then ESA decided to proceed with a cost-reduced modification, which became known as ATHENA.<ref name="About ATHENA">{{cite web |url=http://sci.esa.int/ixo/48729-about-athena/|title=About ATHENA|publisher=ESA|date=1 September 2019|access-date=14 March 2021}}</ref> ''Athena'' was selected in 2014 to become the second (L2) L-class Cosmic Vision mission,<ref name="athenaReboot">{{cite web|url=https://sci.esa.int/cosmic-vision/54241-athena-to-study-the-hot-and-energetic-universe/|title=ESA Science & Technology: Athena to study the hot and energetic Universe|publisher=ESA|date=27 June 2014|access-date=14 March 2021}}</ref> addressing the Hot and Energetic Universe science theme.


The scientific advice for the ''Athena'' mission is provided by the ''Athena'' Science Study Team (ASST) composed of expert scientists from the community. The ASST was appointed by ESA on 16 July 2014. The ESA Study Scientist and Study Manager are Dr Matteo Guainazzi and Dr Mark Ayre respectively.
The scientific advice for the ''Athena'' mission is provided by the ''Athena'' Science Study Team (ASST) composed of expert scientists from the community. The ASST was appointed by ESA on 16 July 2014. The ESA Study Scientist and Study Manager are Dr Matteo Guainazzi and Dr Mark Ayre respectively. ''Athena'' completed successfully its Phase A with the Mission Formulation Review on 12 November 2019. The next key milestone will be the mission adoption by ESA's Science Programme Committee (SPC) expected in 2023{{update inline|date=August 2024}}, leading to launch in 2035.<ref name="athena-summary" />


In 2023, the mission was rescoped as NewAthena, with launch date moved to 2037.<ref name=2023upd>{{cite web |title=Final three for ESA's next medium science mission |publisher=ESA|url=https://www.esa.int/Science_Exploration/Space_Science/Final_three_for_ESA_s_next_medium_science_mission }}</ref>
''Athena'' completed successfully its Phase A with the Mission Formulation Review on 12 November 2019. The next key milestone will be the mission adoption by ESA’s Science Programme Committee (SPC) expected in the second half of 2022, leading to launch in the early 2030s.


==Orbit==
== Orbit ==
In the early 2030s, an [[Ariane 6]].4  launch vehicle will lift ''Athena'' into a large amplitude [[halo orbit]] around the [[Lagrangian point#L2|L2 point]] of the Sun-Earth system (although an alternative L1 halo orbit is also under consideration). The orbit around L2 was selected due to its stable thermal environment, good sky visibility, and high observing efficiency.  ''Athena'' will perform pre-planned scheduled observations of up to 300 celestial locations per year. A special Target of Opportunity mode will allow a re-point manoeuvre within 4 hours for 50% of any randomly occurring events in the sky.
In 2035, an [[Ariane 6|Ariane 64]] [[launch vehicle]] will lift ''Athena'' into a large amplitude [[halo orbit]] around the {{L2}} point of the [[Earth's orbit|Sun-Earth system]].<ref>{{cite web |url=https://www.the-athena-x-ray-observatory.eu/mission.html |title=Athena mission |work=Athena Community Office |access-date=10 November 2021 |archive-date=6 February 2022 |archive-url=https://web.archive.org/web/20220206080904/https://www.the-athena-x-ray-observatory.eu/mission.html |url-status=dead }}</ref><ref name="athena-summary" /> The orbit around {{L2}} was selected due to its stable thermal environment, good sky visibility, high observing efficiency, and stable particle background. ''Athena'' will perform pre-planned scheduled observations of up to 300 celestial locations per year. A special [[Target of opportunity|Target of Opportunity]] mode will allow a re-point manoeuvre within 4 hours for 50% of any randomly occurring events in the sky.


==Optics and instruments==
== Optics and instruments ==
The ''Athena'' X-ray observatory consists of a single X-ray telescope<ref>{{Cite journal|display-authors=3|vauthors=Bavdaz M, Wille E, Ayre M, Ferreira I, Shortt B, Fransen S, Collon M, Vacanti G, Barrière N, Landgraf B, Sforzini J, Booysen K, van Baren C, Zuknik KH, Della Monica Ferreira D, Massahi S, Christensen F, Krumrey M, Müller P, Burwitz V, Pareschi G, Spiga D, Valsecchi G, Vernani D, Oliver P, Seidel A|title=Development of the ATHENA mirror|journal=Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray|date=6 July 2018|volume=106990X|pages=32|doi=10.1117/12.2313296|bibcode=2018SPIE10699E..0XB|isbn=9781510619517|s2cid=54028845|url=https://backend.orbit.dtu.dk/ws/files/154679591/106990X.pdf|editor1-last=Nikzad|editor1-first=Shouleh|editor2-last=Nakazawa|editor2-first=Kazuhiro|editor3-last=Den Herder|editor3-first=Jan-Willem A}}</ref><ref>{{Cite web|url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Bavdaz.pdf|title=Bavdaz, M. "Mirror development status" PDF Talk at the 2nd Athena conference, Palermo (Italy)|date=October 2018}}</ref> with a 12 m [[focal length]], with an effective area of approx. 1.4 m<sup>2</sup> (at 1 keV) and a spatial resolution of 5 [[Minute and second of arc|arcseconds]] on-axis, degrading gracefully to less than 10 arcseconds at 30 arcminutes off-axis. The mirror is based on ESA’s Silicon Pore Optics (SPO) technology.<ref>{{Cite journal|display-authors=3|vauthors=Collon MJ, Vacanti G, Barrière NM, Landgraf B, Günther R, Vervest M, Voruz L, Verhoex S, Babic L, van der Hoeven R, van Straeten K, Chatbi A, Girou D, Beijersbergen MW, Bavdaz M, Wille E, Fransen S, Shortt B, Ferreira I, Haneveld J, Koelewijn A, Booysen K, Wijnperle M, Lankwarden JJ, van Baren C, Eigenraam A, den Herder JW, Müller P, Krumrey M, Burwitz V, Pareschi G, Massahi S, Della Monica Ferreira D, Christensen FE, Valsecchi G, Oliver P, Chequer I, Ball K, Zuknik KH, Vernani D|date=12 July 2019|title=Silicon pore optics mirror module production and testing|journal=Proceedings Volume 11180, International Conference on Space Optics — ICSO 2018; 1118023 (2019)|volume=11180|pages=74|doi=10.1117/12.2535994|bibcode=2019SPIE11180E..23C|isbn=9781510630772|editor1-last=Karafolas|editor1-first=Nikos|editor2-last=Sodnik|editor2-first=Zoran|editor3-last=Cugny|editor3-first=Bruno|doi-access=free}}</ref><ref>{{Cite web|url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Collon.pdf|title=SPO development" PDF. Talk at the 2nd Athena Conference, Palermo (Italy)|last=Bavdaz|first=Marcos|date=October 2018}}</ref> SPO provides an excellent ratio of collecting area to mass, while still offering a good angular resolution. It also benefits from a high Technology Readiness Level and a modular design highly amenable to mass production necessary to achieve the unprecedented telescope collecting area. A movable mirror assembly can focus X-rays onto either one of ''Athena'''s two instruments (WFI and X-IFU, see below) at any given time.
The ''Athena'' X-ray observatory consists of a single X-ray telescope <ref name="ATHENA Mirror">{{cite conference |url=https://backend.orbit.dtu.dk/ws/files/154679591/106990X.pdf |last1=Bavdaz |first1=Marcos |last2=Wille |first2=Eric |last3=Ayre |first3=Mark |last4=Ferreira |first4=Ivo |last5=Shortt |first5=Brian |last6=Fransen |first6=Sebastiaan |last7=Collon |first7=Maximilien |last8=Vacanti |first8=Giuseppe |last9=Barrière |first9=Nicolas |last10=Landgraf |first10=Boris |title=Development of the ATHENA mirror |editor-first1=Shouleh |editor-first2=Kazuhiro |editor-first3=Jan-Willem A |editor-last1=Nikzad |editor-last2=Nakazawa |editor-last3=Den Herder |conference=Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray|volume=106990X|page=32|doi=10.1117/12.2313296|bibcode=2018SPIE10699E..0XB |isbn=9781510619517|s2cid=54028845|publisher=DTU|date=4 October 2018|access-date=14 March 2021 |archive-url=https://web.archive.org/web/20230412075251/https://backend.orbit.dtu.dk/ws/files/154679591/106990X.pdf |archive-date=12 April 2023 |url-status=live }}</ref><ref name="Mirror">{{cite web |url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Bavdaz.pdf|title=Mirror development status|work=Talk at the 2nd Athena conference, Palermo, Italy|publisher=ESA|date=25 September 2018|access-date=14 March 2021}}</ref> with a 12 m [[focal length]], with an effective area of approx. 1.4 m<sup>2</sup> (at 1 keV) and a spatial resolution of 5 [[Minute and second of arc|arcseconds]] on-axis, degrading gracefully to less than 10 arcseconds at 30 arcminutes off-axis. The mirror is based on ESA's Silicon Pore Optics (SPO) technology.<ref name="Silicon">{{cite book |author=Maximillien J. Collon |author2=Giuseppe Vacanti |author3=Nicolas M. Barrière|title=International Conference on Space Optics — ICSO 2018 |chapter=Silicon pore optics mirror module production and testing |editor-first1=Nikos |editor-first2=Zoran |editor-first3=Bruno |editor-last1=Karafolas |editor-last2=Sodnik |editor-last3=Cugny |volume=11180|pages=74|doi=10.1117/12.2535994|bibcode=2019SPIE11180E..23C|isbn=9781510630772|doi-access=free|publisher=SPIE|date=12 July 2019}}</ref><ref name="SPO">{{cite web |url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Collon.pdf|title=SPO development|work=Talk at the 2nd Athena Conference, Palermo, Italy|last=Collon|first=Maximillien |date=25 September 2018|access-date=14 March 2021}}</ref> SPO provides an excellent ratio of collecting area to mass, while still offering a good angular resolution. It also benefits from a high [[technology readiness level]] and a modular design highly amenable to mass production necessary to achieve the unprecedented telescope collecting area. A movable mirror assembly can focus X-rays onto either one of ''Athena''{{'s}} two instruments (WFI and X-IFU, see below) at any given time.


Both the WFI and X-IFU successfully passed their Preliminary Requirements Reviews, on 31 October 2018 and 11 April 2019 respectively.
Both the WFI and X-IFU successfully passed their Preliminary Requirements Reviews, on 31 October 2018 and 11 April 2019 respectively.


=== Wide Field Imager===
=== Wide Field Imager (WFI)===
The Wide Field Imager (WFI)<ref>{{Cite web|url=http://www.mpe.mpg.de/ATHENA-WFI/|title=The Wide Field Imager for the Athena X-Ray Observatory}}</ref><ref>{{Cite journal|last1=Meidinger|first1=Norbert|last2=Nandra|first2=Kirpal|last3=Plattner|first3=Markus|date=6 July 2018|title=Development of the Wide Field Imager instrument for ATHENA|journal=Proceedings Volume 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray; 106991F (2018)|volume=10699|pages=50|doi=10.1117/12.2310141|bibcode=2018SPIE10699E..1FM|isbn=9781510619517|s2cid=66404115|editor1-last=Nikzad|editor1-first=Shouleh|editor2-last=Nakazawa|editor2-first=Kazuhiro|editor3-last=Den Herder|editor3-first=Jan-Willem A}}</ref><ref>{{Cite web|url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Rau.pdf|title=The Wide Field Imager. Talk at the 2nd Athena conference, Palermo (Italy)|last=Rau|first=Arne|date=October 2018}}</ref> is a large field of view spectral-imaging camera based on the unique [https://www.the-athena-x-ray-observatory.eu/outreach/nuggets/54-outreach/nuggets/689-athenanuggets-29-a-depfet-detector-for-athena%E2%80%99s-wide-field-imager-wfi-instrument.html Silicon DEPFET technology] developed in the semiconductor laboratory of the [[Max Planck Society]]. The DEPFETs provide an excellent energy resolution (<170eV at 7keV), low noise, fast readout and high time resolution, with good radiation hardness.  The instrument combines the Large Detector Array, which is optimized for a wide field of view observations over a 40’ x 40’ instantaneous sky area, with a separate Fast Detector tailored to observe the brightest point sources of the X-ray sky with high throughput and low pile-up. These capabilities, in combination with the unprecedented effective area and wide field of the ''Athena'' telescope, will provide breakthrough capabilities in X-ray imaging spectroscopy.
The Wide Field Imager (WFI) <ref name="WFI">{{cite web|url=https://www.mpe.mpg.de/ATHENA-WFI/|title=The Wide Field Imager for the Athena X-Ray Observatory|publisher=WFI ATHENA|date=30 April 2020|access-date=14 March 2021}}</ref><ref name="Imager">{{cite book |chapter-url=https://ui.adsabs.harvard.edu/abs/2018SPIE10699E..1FM/abstract|last1=Meidinger|first1=Norbert|last2=Nandra|first2=Kirpal|last3=Plattner|first3=Markus|title=Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray |chapter=Development of the wide field imager instrument for ATHENA |editor-first1=Shouleh |editor-first2=Kazuhiro |editor-first3=Jan-Willem A |editor-last1=Nikzad |editor-last2=Nakazawa |editor-last3=Den Herder |volume=10699|page=50|doi=10.1117/12.2310141|bibcode=2018SPIE10699E..1FM |isbn=9781510619517|s2cid=66404115|publisher=ads|date=6 July 2018|access-date=14 March 2021}}</ref><ref name="ISDC">{{cite web |url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Rau.pdf|title=The Wide Field Imager - Talk at the 2nd Athena conference, Palermo, Italy|last=Rau|first=Arne|date=24 September 2018|access-date=14 March 2021}}</ref> is a large field of view spectral-imaging camera based on the unique [https://www.the-athena-x-ray-observatory.eu/outreach/nuggets/54-outreach/nuggets/689-athenanuggets-29-a-depfet-detector-for-athena%E2%80%99s-wide-field-imager-wfi-instrument.html Silicon DEPFET technology]{{Dead link|date=August 2023 |bot=InternetArchiveBot |fix-attempted=yes }} developed in the semiconductor laboratory of the [[Max Planck Society]]. The DEPFETs provide an excellent energy resolution (<170eV at 7keV), low noise, fast readout and high time resolution, with good radiation hardness. The instrument combines the Large Detector Array, which is optimized for a wide field of view observations over a 40' x 40' instantaneous sky area, with a separate Fast Detector tailored to observe the brightest point sources of the X-ray sky with high throughput and low pile-up. These capabilities, in combination with the unprecedented effective area and wide field of the ''Athena'' telescope, will provide breakthrough capabilities in X-ray imaging spectroscopy.


The WFI is developed by an international consortium composed of ESA member states. It is led by the [[Max Planck Institute for Extraterrestrial Physics|Max Planck Institute for extraterrestrial Physics MPE]] (DEU) with partners in Germany (ECAP, IAA Tübingen), Austria (University of Vienna), Denmark (DTU), France (CEA Saclay, Strasbourg), Italy (INAF, Bologna, Palermo), Poland (SRC PAS, NCAC PAS), the United Kingdom (University Leicester, Open University), the United States (Penn State, SLAC, MIT, SAO), Switzerland (University of Geneva), Portugal (IA), and Greece (Athens Observatory, University of Crete). The Principal Investigator is Prof. Kirpal Nandra, Director of the High-Energy Group at MPE.
The WFI is developed by an international consortium composed of ESA member states. It is led by the [[Max Planck Institute for Extraterrestrial Physics]] (DEU) with partners in Germany (ECAP, IAA Tübingen), Austria ([[University of Vienna]]), [[Denmark]] (DTU), France ([[Saclay Nuclear Research Centre|CEA Saclay]], [[Strasbourg]]), Italy ([[INAF]], [[Bologna]], [[Palermo]]), Poland (SRC PAS, NCAC PAS), the United Kingdom ([[University of Leicester]], [[Open University]]), the United States ([[Pennsylvania State University]] (Penn State), SLAC, [[Massachusetts Institute of Technology]] (MIT), SAO), Switzerland ([[University of Geneva]]), Portugal (IA), and [[Greece]] (Athens Observatory, [[University of Crete]]). The principal investigator is Prof. Kirpal Nandra, Director of the High-Energy Group at MPE.


=== X-ray Integral Field Unit ===
=== X-ray Integral Field Unit (X-IFU) ===
The X-ray Integral Field Unit<ref>{{Cite web|url=http://x-ifu.irap.omp.eu/|title=The Athena X-ray Integral Field Unit (X-IFU)}}</ref><ref>{{Cite journal|display-authors=3|vauthors=Barret D, Trong TL, den Herder JW, Piro L, Cappi M, Houvelin J, Kelley R, Mas-Hesse JM, Mitsuda K, Paltani S, Rauw G, Rozanska A, Wilms J, Bandler S, Barbera M, Barcons X, Bozzo E, Ceballos MT, Charles I, Costantini E, Decourchelle A, den Hartog R, Duband L, Duval JM, Fiore F, Gatti F, Goldwurm A, Jackson B, Jonker P, Kilbourne C, Macculi C, Mendez M, Molendi S, Orleanski P, Pajot F, Pointecouteau E, Porter F, Pratt GW, Prêle D, Ravera L, Sato K, Schaye J, Shinozaki K, Thibert T, Valenziano L, Valette V, Vink J, Webb N, Wise M, Yamasaki N, Douchin F, Mesnager JM, Pontet B, Pradines A, Branduardi-Raymont G, Bulbul E, Dadina M, Ettori S, Finoguenov A, Fukazawa Y, Janiuk A, Kaastra J, Mazzotta P, Miller J, Miniutti G, Naze Y, Nicastro F, Scioritino S, Simonescu A, Torrejón JM, Frezouls B, Geoffray H, Peille P, Aicardi C, André J, Daniel C, Clénet A, Etcheverry C, Gloaguen E, Hervet G, Jolly A, Ledot A, Paillet I, Schmisser R, Vella B, Damery JC, Boyce K, Dipirro M, Lotti S, Schwander D, Smith S, Van Leeuwen BJ, van Weers H, Clerc N, Cobo B, Dauser T, Kirsch C, Cucchetti E, Eckart M, Ferrando P, Natalucci L|date=31 July 2018|title=The Athena X-ray Integral Field Unit (X-IFU)|journal=Proc. SPIE 10699, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray, 106991G|volume=10699|pages=51|arxiv=1807.06092|doi=10.1117/12.2312409|bibcode=2018SPIE10699E..1GB|isbn=9781510619517|s2cid=173185994|editor1-last=Nikzad|editor1-first=Shouleh|editor2-last=Nakazawa|editor2-first=Kazuhiro|editor3-last=Den Herder|editor3-first=Jan-Willem A}}</ref><ref>{{Cite web|url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Barret.pdf|title=The Athena X-ray Integral Field Unit (X-IFU) Talk at the 2nd Athena Conference, Palermo (Italy)|last=Barret|first=Didier|date=October 2018}}</ref> is the cryogenic X-ray spectrometer of ''Athena''. X-IFU will deliver spatially resolved X-ray spectroscopy, with a spectral resolution requirement of 2.5 eV up to 7 keV over a hexagonal field of view of 5 arc minutes (equivalent diameter). The prime detector of X-IFU is made of a large format array of Molybdenum Gold [[Transition-edge sensor|transition-edge sensors]] coupled to absorbers made of Au and Bi to provide the required stopping power. The pixel size corresponds to slightly less than 5 arc seconds on the sky, thus matching the angular resolution of the X-ray optics. A large part of the X-IFU related ''Athena'' science objectives relies on the observation of faint extended sources (e.g. hot gas in [[Galaxy cluster|cluster of galaxies]] to measure bulk motions and turbulence or its chemical composition), imposing the lowest possible instrumental background. This is achieved by the addition of a second cryogenic detector underneath the prime focal plane array. This way non-X-ray events such as particles can be vetoed using the temporal coincidence of detecting energy in both detectors simultaneously. The focal plane array, the sensors and the cold front end electronics are cooled at a stable temperature less than 100 mK by a multi-stage cryogenic chain, assembled by a series of mechanical coolers, with interface temperatures at 15 K, 4K and 2K and 300 mK, pre-cooling a sub Kelvin cooler made of a 3He adsorption cooler coupled with an [https://cryo.gsfc.nasa.gov/introduction/ADR_intro/ADR_intro.html Adiabatic Demagnetization Refrigerator]. Calibration data are acquired along with each observation from modulated X-ray sources to enable the energy calibration required to reach the targeted spectral resolution. Although an integral field unit where each and every pixel delivers a high resolution X-ray spectrum, the defocussing capability of the ''Athena'' mirror will enable the focal beam to be spread over hundreds of sensors. The X-IFU will thus be able to observe very bright X-ray sources. It will do so either with the nominal resolution, e.g. for detecting the baryons thought to reside in the [[Warm–hot intergalactic medium|Warm Hot Intergalactic Medium]], using bright gamma-ray burst afterglows, as background sources shining through the cosmic web, or with a spectral resolution of 3–10 eV, e.g. for measuring the spins and characterizing the winds and outflows of bright [[X-ray binary|X-ray binaries]] at energies where their spectral signatures are the strongest (above 5 keV).
The X-ray Integral Field Unit <ref name="X-IFU">{{cite web|url=http://x-ifu.irap.omp.eu/|title=The Athena X-ray Integral Field Unit (X-IFU)|publisher=X-IFU home page|date=11 February 2021|access-date=14 March 2021}}</ref><ref name="Harward">{{cite conference |url=https://ui.adsabs.harvard.edu/abs/2018SPIE10699E..1GB/abstract |last1=Barret |first1=Didier |last2=Lam Trong |first2=Thien |last3=den Herder |first3=Jan-Willem |conference=Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray |title=The ATHENA x-ray integral field unit (X-IFU) |editor-first1=Shouleh |editor-first2=Kazuhiro |editor-first3=Jan-Willem A |editor-last1=Nikzad |editor-last2=Nakazawa |editor-last3=Den Herder |volume=10699 |page=51 |arxiv=1807.06092 |doi=10.1117/12.2312409|bibcode=2018SPIE10699E..1GB |isbn=9781510619517|s2cid=173185994|publisher=ads|date=July 2018|hdl=10261/239684 |access-date=14 March 2021}}</ref><ref name="IRAP">{{cite web |url=https://www.isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/Barret.pdf|title=The Athena X-ray Integral Field Unit (X-IFU) Talk at the 2nd Athena Conference, Palermo, Italy|last=Barret |first=Didier|publisher=IRAP|date=25 September 2018|access-date=14 March 2021}}</ref> is the cryogenic X-ray spectrometer of ''Athena'' X-IFU will deliver spatially resolved [[X-ray spectroscopy]], with a spectral resolution requirement of 2.5 eV up to 7 keV over a hexagonal field of view of 5 arc minutes (equivalent diameter). The prime detector of X-IFU is made of a large format array of Molybdenum Gold [[transition-edge sensor]]s coupled to absorbers made of [[Gold|Au]] and [[Bismuth|Bi]] to provide the required stopping power. The pixel size corresponds to slightly less than 5 arc seconds on the sky, thus matching the angular resolution of the X-ray optics. A large part of the X-IFU related ''Athena'' science objectives relies on the observation of faint extended sources (e.g. hot gas in [[Galaxy cluster|cluster of galaxies]] to measure bulk motions and turbulence or its chemical composition), imposing the lowest possible instrumental background. This is achieved by the addition of a second cryogenic detector underneath the prime focal plane array. This way non-X-ray events such as particles can be vetoed using the temporal coincidence of detecting energy in both detectors simultaneously. The focal plane array, the sensors and the cold front end electronics are cooled at a stable temperature less than 100 mK by a multi-stage cryogenic chain, assembled by a series of mechanical coolers, with interface temperatures at 15 K, 4 K and 2 K and 300 mK, pre-cooling a sub Kelvin cooler made of a [[Helium-3|3He]] adsorption cooler coupled with an [https://cryo.gsfc.nasa.gov/introduction/ADR_intro/ADR_intro.html Adiabatic Demagnetization Refrigerator]. Calibration data are acquired along with each observation from modulated X-ray sources to enable the energy calibration required to reach the targeted spectral resolution. Although an integral field unit where each and every pixel delivers a high resolution X-ray spectrum, the defocussing capability of the ''Athena'' mirror will enable the focal beam to be spread over hundreds of sensors. The X-IFU will thus be able to observe very bright X-ray sources. It will do so either with the nominal resolution, e.g. for detecting the baryons thought to reside in the [[Warm–hot intergalactic medium|Warm Hot Intergalactic Medium]], using bright gamma-ray burst afterglows, as background sources shining through the cosmic web, or with a spectral resolution of 3–10 eV, e.g. for measuring the spins and characterizing the winds and outflows of bright [[X-ray binary|X-ray binaries]] at energies where their spectral signatures are the strongest (above 5 keV).


As of December 2018, when the X-IFU consortium was formally endorsed by ESA as being responsible for the procurement of the instrument to ''Athena'', the X-IFU consortium gathered 11 European countries (Belgium, Czech Republic, Finland, France, Germany, Ireland, Italy, Netherlands, Poland, Spain, Switzerland), plus Japan and the United States. More than 50 research institutes are involved in the X-IFU consortium. The principal investigator of X-IFU is Dr Didier Barret, Director of research at the research institute in astrophysics and planetology of Toulouse ([[L'Institut de Recherche en Astrophysique et Planétologie|IRAP]]-OMP, CNRS UT3-Paul Sabatier/CNES, France). Dr Jan-Willem den Herder ([[Netherlands Institute for Space Research|SRON]], The Netherlands) and Dr Luigi Piro ([[INAF]]-IAPS, Italy) are co-principal investigators of the X-IFU. [[CNES]] manages the project, and on behalf of the X-IFU consortium, is responsible for the delivery of the instrument to ESA.
As of December 2018, when the X-IFU consortium was formally endorsed by ESA as being responsible for the procurement of the instrument to ''Athena'', the X-IFU consortium gathered 11 European countries ([[Belgium]], [[Czech Republic]], [[Finland]], France, Germany, Ireland, Italy, Netherlands, Poland, Spain, Switzerland), plus Japan and the United States. More than 50 research institutes are involved in the X-IFU consortium. The principal investigator of X-IFU is Dr Didier Barret, Director of research at the research institute in astrophysics and planetology of [[Toulouse]] ([[L'Institut de Recherche en Astrophysique et Planétologie|IRAP]]-OMP, [[French National Centre for Scientific Research|CNRS]] UT3-Paul Sabatier/[[CNES]], France). Dr Jan-Willem den Herder ([[Netherlands Institute for Space Research|SRON]], The Netherlands) and Dr Luigi Piro ([[INAF]]-IAPS, Italy) are co-principal investigators of the X-IFU. [[CNES]] manages the project, and on behalf of the X-IFU consortium, is responsible for the delivery of the instrument to ESA.


== ''Athena'' science goals ==
== ''Athena'' science goals ==
The "Hot and Energetic Universe" science theme<ref>{{Cite journal|vauthors=Barcons X, Barret D, Decourchelle A, den Herder JW, Fabian AC, Matsumoto H, Lumb D, Nandra K, Piro L, Smith RK, Willingale R|date=21 March 2017|title=Athena: ESA's X‐ray observatory for the late 2020s|journal=Astronomische Nachrichten|volume=338|issue=2–3|pages=153–158|doi=10.1002/asna.201713323|bibcode=2017AN....338..153B}}</ref> revolves around two fundamental questions in [[astrophysics]]: How does ordinary matter assemble into the large-scale structures that we see today? And how do [[Black hole|black holes]] grow and shape the [[Universe]]? Both questions can only be answered using a sensitive X-ray space observatory. Its combination of scientific performance exceeds any existing or planned X-ray missions by over one order of magnitude on several parameter spaces: effective area, weak line sensitivity, survey speed, just to mention a few. ''Athena'' will perform very sensitive measurements on a wide range of celestial objects. It will investigate the chemical evolution of the hot plasma permeating the intergalactic space in cluster of galaxies, search for elusive observational features of the [[Warm–hot intergalactic medium|Warm-Hot Intergalactic Medium]], investigate powerful outflows ejected from accreting black holes across their whole mass spectrum, and study their impact on the host galaxy, and identify sizeable samples of  comparatively rare populations of [[Active galactic nucleus|Active Galactic Nuclei (AGN)]]  that are key to understanding the concurrent cosmological evolution of accreting black holes and galaxies. Among them are highly obscured and high-redshift (z≥6) AGN. Furthermore, ''Athena'' will be an X-ray observatory open to the whole astronomical community, poised to provide wide-ranging discoveries in almost all fields of modern astrophysics, with a large discovery potential of still unknown and unexpected phenomena. It represents the X-ray contribution to the fleet of large-scale observational facilities to be operational in the 2030s (incl. [[Square Kilometre Array|SKA]], [[Extremely Large Telescope|ELT]], [[Atacama Large Millimeter Array|ALMA]], [[Laser Interferometer Space Antenna|LISA]]...)
The "Hot and Energetic Universe" science theme <ref name="Harvad2">{{cite journal|url=https://ui.adsabs.harvard.edu/abs/2017AN....338..153B/abstract|vauthors=Barcons X, Barret D, Decourchelle A|title=ATHENA: ESA's X-ray observatory for the late 2020s|journal=Astronomische Nachrichten|volume=338|issue=2–3|pages=153–158|doi=10.1002/asna.201713323|bibcode=2017AN....338..153B|publisher=ads|date=21 March 2017|access-date=14 March 2021}}</ref> revolves around two fundamental questions in [[astrophysics]]: How does ordinary matter assemble into the large-scale structures that we see today? And how do [[black hole]]s grow and shape the [[Universe]]? Both questions can only be answered using a sensitive X-ray space observatory. Its combination of scientific performance exceeds any existing or planned X-ray missions by over one order of magnitude on several parameter spaces: effective area, weak line sensitivity, survey speed, just to mention a few. ''Athena'' will perform very sensitive measurements on a wide range of celestial objects. It will investigate the chemical evolution of the hot plasma permeating the intergalactic space in cluster of galaxies, search for elusive observational features of the [[Warm–hot intergalactic medium|Warm-Hot Intergalactic Medium]], investigate powerful outflows ejected from accreting black holes across their whole mass spectrum, and study their impact on the host galaxy, and identify sizeable samples of comparatively rare populations of [[Active galactic nucleus|Active Galactic Nuclei (AGN)]]  that are key to understanding the concurrent cosmological evolution of accreting black holes and galaxies. Among them are highly obscured and high-redshift (z≥6) AGN. Furthermore, ''Athena'' will be an X-ray observatory open to the whole astronomical community, poised to provide wide-ranging discoveries in almost all fields of modern astrophysics, with a large discovery potential of still unknown and unexpected phenomena. It represents the X-ray contribution to the fleet of large-scale observational facilities to be operational in the 2030s (incl. [[Square Kilometre Array|SKA]], [[Extremely Large Telescope|ELT]], [[Atacama Large Millimeter Array|ALMA]], [[Laser Interferometer Space Antenna|LISA]]...).


== The ''Athena'' Community Office ==
== The ''Athena'' Community Office ==
The ''Athena'' Science Study Team (ASST) established the ''Athena'' Community Office (ACO)<ref>{{Cite web|url=http://isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/ACO.pdf|title=The Athena Community Office Talk at the 2nd Athena conference, Palermo (Italy)|date=October 2018}}</ref> to obtain support in performing its tasks assigned by ESA, and most especially in the ASST role as “a focal point for the interests of the broad scientific community”. Currently, this community is formed by more than [https://www.google.com/maps/d/viewer?mid=1sW7NjYAS5qkM3nkEyZ6uFbC3ef4NulfH&ll=46.761827688518224%2C3.924673271191409&z=5 800 members spread around the world].
The ''Athena'' Science Study Team (ASST) established the ''Athena'' Community Office (ACO)<ref name="ACO">{{cite web|url=http://isdc.unige.ch/athena/Repository/Open_access/Second_Athena_Conference/ACO.pdf |title=The Athena Community Office Talk at the 2nd Athena conference, Palermo, Italy|publisher=ACO home page|date=26 September 2018|access-date=14 March 2021}}</ref> to obtain support in performing its tasks assigned by ESA, and most especially in the ASST role as "a focal point for the interests of the broad scientific community". Currently, this community is formed by more than [https://www.google.com/maps/d/viewer?mid=1sW7NjYAS5qkM3nkEyZ6uFbC3ef4NulfH&ll=46.761827688518224%2C3.924673271191409&z=5 800 members spread around the world].


The ACO is meant to become a focal point to facilitate the scientific exchange between the ''Athena'' activities and the scientific community at large, and to disseminate the ''Athena'' science objectives to the general public. The main tasks of the ACO can be divided into three categories:
The ACO is meant to become a focal point to facilitate the scientific exchange between the ''Athena'' activities and the scientific community at large, and to disseminate the ''Athena'' science objectives to the general public. The main tasks of the ACO can be divided into three categories:


* Organisational aspects and optimisation of the community efforts assisting the ASST in several aspects, as for instance helping to the promotion of  ''Athena'' science capabilities in the research world, through Conferences & Workshops or supporting the production of ASST documents, including the White Papers identifying the scientific synergies of ''Athena'' with other observational facilities in the early 2030s
* Organisational aspects and optimisation of the community efforts assisting the ASST in several aspects, as for instance helping to the promotion of ''Athena'' science capabilities in the research world, through Conferences & Workshops or supporting the production of ASST documents, including the White Papers identifying the scientific synergies of ''Athena'' with other observational facilities in the early 2030s
* Keep the ''Athena'' community informed on the status of the project with the regular release of the [https://www.the-athena-x-ray-observatory.eu/resources/newsletter-archive.html newsletter], brief news, weekly news on the ''Athena'' web portal and in the social channels.
* Keep the ''Athena'' community informed on the status of the project with the regular release of the [https://www.the-athena-x-ray-observatory.eu/resources/newsletter-archive.html newsletter] {{Webarchive|url=https://web.archive.org/web/20220308171820/https://www.the-athena-x-ray-observatory.eu/resources/newsletter-archive.html |date=8 March 2022 }}, brief news, weekly news on the ''Athena'' web portal and in the social channels.
* Develop communication and outreach activities, of particular interest, are the [https://www.the-athena-x-ray-observatory.eu/outreach/nuggets.html ''Athena'' nuggets].
* Develop communication and outreach activities, of particular interest, are the [https://www.the-athena-x-ray-observatory.eu/outreach/nuggets.html ''Athena'' nuggets] {{Webarchive|url=https://web.archive.org/web/20180909234349/https://www.the-athena-x-ray-observatory.eu/outreach/nuggets.html |date=9 September 2018 }}.

The ACO is led by the [https://ifca.unican.es/en-us Instituto de Física de Cantabria (CSIC-UC)]. Further ACO contributors are the [[University of Geneva]], [[Max Planck Institute for Extraterrestrial Physics|MPE]] and [[L'Institut de Recherche en Astrophysique et Planétologie|IRAP]].
The ACO is led by the [https://ifca.unican.es/en-us Instituto de Física de Cantabria (CSIC-UC)]. Further ACO contributors are the [[University of Geneva|Université de Genève]], [[Max Planck Institute for Extraterrestrial Physics]] (MPE) and [[L'Institut de Recherche en Astrophysique et Planétologie]] (IRAP).
⚫
==See also==

⚫
*[[Spektr-RG]]
⚫
== See also ==
⚫
*[[List of proposed space observatories]]
{{Portal|Spaceflight}}
⚫
*[[Lynx X-ray Observatory]], a proposed space telescope with greater angular resolution, sensitivity, and spectroscopic power
⚫
* [[Spektr-RG]]
⚫
*[[X-Ray Imaging and Spectroscopy Mission|XRISM]], pathfinder mission for ''Athena''
⚫
* [[List of proposed space observatories]]
⚫
* [[Lynx X-ray Observatory]], a proposed space telescope with greater angular resolution, sensitivity, and spectroscopic power
⚫
* [[X-Ray Imaging and Spectroscopy Mission|XRISM]], pathfinder mission for ''Athena''


==References==
== References ==
{{Reflist|colwidth=30em}}
{{Reflist|30em}}


==External links==
== External links ==
* [http://www.the-athena-x-ray-observatory.eu/ The ''Athena'' X-ray observatory: ''Community Support Portal'']
* [http://www.the-athena-x-ray-observatory.eu/ The ''Athena'' X-ray observatory: ''Community Support Portal'']
*[https://sci.esa.int/web/athena/ ''Athena'' on ESA Cosmic Vision website]
* [https://sci.esa.int/web/athena/ ''Athena'' on ESA Cosmic Vision website]
*[https://www.youtube.com/watch?v=1DtzdbFfk14 ''Athena'' mission proposal video on YouTube]
* [https://www.youtube.com/watch?v=1DtzdbFfk14 ''Athena'' mission proposal video on YouTube]
*[http://www.mpe.mpg.de/ATHENA-WFI/ The ''Athena'' Wide Field Imager website]
* [http://www.mpe.mpg.de/ATHENA-WFI/ The ''Athena'' Wide Field Imager website]
*[http://x-ifu.irap.omp.eu/ The ''Athena'' X-ray Integral Field Unit website]
* [http://x-ifu.irap.omp.eu/ The ''Athena'' X-ray Integral Field Unit website]
*[https://www.youtube.com/watch?v=mOf6WIDmi30 X-IFU, unveiling the secrets of the hot and energetic Universe video on YouTube]
* [https://www.youtube.com/watch?v=mOf6WIDmi30 X-IFU, unveiling the secrets of the hot and energetic Universe video on YouTube]
*[https://www.youtube.com/watch?v=OrB2VaAXfdA Silicone pore optics mirror video]
* [https://www.youtube.com/watch?v=OrB2VaAXfdA Silicon pore optics mirror video]
*[https://www.youtube.com/watch?v=PdwN_VeUaak Silicone pore optics mirror animation]
* [https://www.youtube.com/watch?v=PdwN_VeUaak Silicon pore optics mirror animation]


{{Space observatories}}
{{Space observatories}}
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[[Category:Space telescopes]]
[[Category:Space telescopes]]
[[Category:X-ray telescopes]]
[[Category:X-ray telescopes]]
[[Category:European Space Agency]]
[[Category:European Space Agency facilities]]
[[Category:Future spaceflights]]
[[Category:Future spaceflights]]
[[Category:Cosmic Vision]]
[[Category:Cosmic Vision]]
[[Category:2031 in science]]
[[Category:2035 in science]]

Latest revision as of 13:15, 6 December 2024

Advanced Telescope for High-ENergy Astrophysics
NamesAthena
Mission typeSpace telescope
OperatorEuropean Space Agency (ESA)
Websitewww.the-athena-x-ray-observatory.eu
Mission duration4 years (planned)
Start of mission
Launch date2035 (planned)[1]
RocketAriane 64
Launch siteCentre Spatial Guyanais
ContractorArianespace
Orbital parameters
Reference systemL2 point (baseline)
Main telescope
TypeX-ray telescope
Focal length12 m (39 ft)

Advanced Telescope for High-ENergy Astrophysics (Athena)[1][2] is an X-ray observatory mission selected by European Space Agency (ESA) within its Cosmic Vision program[3] to address the Hot and Energetic Universe scientific theme. Athena will operate in the energy range of 0.2–12 keV and will offer spectroscopic and imaging capabilities exceeding those of currently operating X-ray astronomy satellites – e.g. the Chandra X-ray Observatory and XMM-Newton – by at least one order of magnitude on several parameter spaces simultaneously.

Mission

[edit]

The primary goals of the mission are to map hot gas structures, determine their physical properties, and search for supermassive black holes.

History and development

[edit]

The mission has its roots in two concepts from the early 2000s, XEUS of ESA and Constellation-X Observatory (Con-X) of NASA. Around 2008, these two proposals were merged into the joint NASA/ESA/JAXA International X-ray Observatory (IXO) proposal. In 2011, IXO was withdrawn and then ESA decided to proceed with a cost-reduced modification, which became known as ATHENA.[4] Athena was selected in 2014 to become the second (L2) L-class Cosmic Vision mission,[5] addressing the Hot and Energetic Universe science theme.

The scientific advice for the Athena mission is provided by the Athena Science Study Team (ASST) composed of expert scientists from the community. The ASST was appointed by ESA on 16 July 2014. The ESA Study Scientist and Study Manager are Dr Matteo Guainazzi and Dr Mark Ayre respectively. Athena completed successfully its Phase A with the Mission Formulation Review on 12 November 2019. The next key milestone will be the mission adoption by ESA's Science Programme Committee (SPC) expected in 2023[needs update], leading to launch in 2035.[1]

In 2023, the mission was rescoped as NewAthena, with launch date moved to 2037.[6]

Orbit

[edit]

In 2035, an Ariane 64 launch vehicle will lift Athena into a large amplitude halo orbit around the L2 point of the Sun-Earth system.[7][1] The orbit around L2 was selected due to its stable thermal environment, good sky visibility, high observing efficiency, and stable particle background. Athena will perform pre-planned scheduled observations of up to 300 celestial locations per year. A special Target of Opportunity mode will allow a re-point manoeuvre within 4 hours for 50% of any randomly occurring events in the sky.

Optics and instruments

[edit]

The Athena X-ray observatory consists of a single X-ray telescope [8][9] with a 12 m focal length, with an effective area of approx. 1.4 m2 (at 1 keV) and a spatial resolution of 5 arcseconds on-axis, degrading gracefully to less than 10 arcseconds at 30 arcminutes off-axis. The mirror is based on ESA's Silicon Pore Optics (SPO) technology.[10][11] SPO provides an excellent ratio of collecting area to mass, while still offering a good angular resolution. It also benefits from a high technology readiness level and a modular design highly amenable to mass production necessary to achieve the unprecedented telescope collecting area. A movable mirror assembly can focus X-rays onto either one of Athena's two instruments (WFI and X-IFU, see below) at any given time.

Both the WFI and X-IFU successfully passed their Preliminary Requirements Reviews, on 31 October 2018 and 11 April 2019 respectively.

Wide Field Imager (WFI)

[edit]

The Wide Field Imager (WFI) [12][13][14] is a large field of view spectral-imaging camera based on the unique Silicon DEPFET technology[permanent dead link‍] developed in the semiconductor laboratory of the Max Planck Society. The DEPFETs provide an excellent energy resolution (<170eV at 7keV), low noise, fast readout and high time resolution, with good radiation hardness. The instrument combines the Large Detector Array, which is optimized for a wide field of view observations over a 40' x 40' instantaneous sky area, with a separate Fast Detector tailored to observe the brightest point sources of the X-ray sky with high throughput and low pile-up. These capabilities, in combination with the unprecedented effective area and wide field of the Athena telescope, will provide breakthrough capabilities in X-ray imaging spectroscopy.

The WFI is developed by an international consortium composed of ESA member states. It is led by the Max Planck Institute for Extraterrestrial Physics (DEU) with partners in Germany (ECAP, IAA Tübingen), Austria (University of Vienna), Denmark (DTU), France (CEA Saclay, Strasbourg), Italy (INAF, Bologna, Palermo), Poland (SRC PAS, NCAC PAS), the United Kingdom (University of Leicester, Open University), the United States (Pennsylvania State University (Penn State), SLAC, Massachusetts Institute of Technology (MIT), SAO), Switzerland (University of Geneva), Portugal (IA), and Greece (Athens Observatory, University of Crete). The principal investigator is Prof. Kirpal Nandra, Director of the High-Energy Group at MPE.

X-ray Integral Field Unit (X-IFU)

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The X-ray Integral Field Unit [15][16][17] is the cryogenic X-ray spectrometer of Athena X-IFU will deliver spatially resolved X-ray spectroscopy, with a spectral resolution requirement of 2.5 eV up to 7 keV over a hexagonal field of view of 5 arc minutes (equivalent diameter). The prime detector of X-IFU is made of a large format array of Molybdenum Gold transition-edge sensors coupled to absorbers made of Au and Bi to provide the required stopping power. The pixel size corresponds to slightly less than 5 arc seconds on the sky, thus matching the angular resolution of the X-ray optics. A large part of the X-IFU related Athena science objectives relies on the observation of faint extended sources (e.g. hot gas in cluster of galaxies to measure bulk motions and turbulence or its chemical composition), imposing the lowest possible instrumental background. This is achieved by the addition of a second cryogenic detector underneath the prime focal plane array. This way non-X-ray events such as particles can be vetoed using the temporal coincidence of detecting energy in both detectors simultaneously. The focal plane array, the sensors and the cold front end electronics are cooled at a stable temperature less than 100 mK by a multi-stage cryogenic chain, assembled by a series of mechanical coolers, with interface temperatures at 15 K, 4 K and 2 K and 300 mK, pre-cooling a sub Kelvin cooler made of a 3He adsorption cooler coupled with an Adiabatic Demagnetization Refrigerator. Calibration data are acquired along with each observation from modulated X-ray sources to enable the energy calibration required to reach the targeted spectral resolution. Although an integral field unit where each and every pixel delivers a high resolution X-ray spectrum, the defocussing capability of the Athena mirror will enable the focal beam to be spread over hundreds of sensors. The X-IFU will thus be able to observe very bright X-ray sources. It will do so either with the nominal resolution, e.g. for detecting the baryons thought to reside in the Warm Hot Intergalactic Medium, using bright gamma-ray burst afterglows, as background sources shining through the cosmic web, or with a spectral resolution of 3–10 eV, e.g. for measuring the spins and characterizing the winds and outflows of bright X-ray binaries at energies where their spectral signatures are the strongest (above 5 keV).

As of December 2018, when the X-IFU consortium was formally endorsed by ESA as being responsible for the procurement of the instrument to Athena, the X-IFU consortium gathered 11 European countries (Belgium, Czech Republic, Finland, France, Germany, Ireland, Italy, Netherlands, Poland, Spain, Switzerland), plus Japan and the United States. More than 50 research institutes are involved in the X-IFU consortium. The principal investigator of X-IFU is Dr Didier Barret, Director of research at the research institute in astrophysics and planetology of Toulouse (IRAP-OMP, CNRS UT3-Paul Sabatier/CNES, France). Dr Jan-Willem den Herder (SRON, The Netherlands) and Dr Luigi Piro (INAF-IAPS, Italy) are co-principal investigators of the X-IFU. CNES manages the project, and on behalf of the X-IFU consortium, is responsible for the delivery of the instrument to ESA.

Athena science goals

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The "Hot and Energetic Universe" science theme [18] revolves around two fundamental questions in astrophysics: How does ordinary matter assemble into the large-scale structures that we see today? And how do black holes grow and shape the Universe? Both questions can only be answered using a sensitive X-ray space observatory. Its combination of scientific performance exceeds any existing or planned X-ray missions by over one order of magnitude on several parameter spaces: effective area, weak line sensitivity, survey speed, just to mention a few. Athena will perform very sensitive measurements on a wide range of celestial objects. It will investigate the chemical evolution of the hot plasma permeating the intergalactic space in cluster of galaxies, search for elusive observational features of the Warm-Hot Intergalactic Medium, investigate powerful outflows ejected from accreting black holes across their whole mass spectrum, and study their impact on the host galaxy, and identify sizeable samples of comparatively rare populations of Active Galactic Nuclei (AGN)  that are key to understanding the concurrent cosmological evolution of accreting black holes and galaxies. Among them are highly obscured and high-redshift (z≥6) AGN. Furthermore, Athena will be an X-ray observatory open to the whole astronomical community, poised to provide wide-ranging discoveries in almost all fields of modern astrophysics, with a large discovery potential of still unknown and unexpected phenomena. It represents the X-ray contribution to the fleet of large-scale observational facilities to be operational in the 2030s (incl. SKA, ELT, ALMA, LISA...).

The Athena Community Office

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The Athena Science Study Team (ASST) established the Athena Community Office (ACO)[19] to obtain support in performing its tasks assigned by ESA, and most especially in the ASST role as "a focal point for the interests of the broad scientific community". Currently, this community is formed by more than 800 members spread around the world.

The ACO is meant to become a focal point to facilitate the scientific exchange between the Athena activities and the scientific community at large, and to disseminate the Athena science objectives to the general public. The main tasks of the ACO can be divided into three categories:

  • Organisational aspects and optimisation of the community efforts assisting the ASST in several aspects, as for instance helping to the promotion of Athena science capabilities in the research world, through Conferences & Workshops or supporting the production of ASST documents, including the White Papers identifying the scientific synergies of Athena with other observational facilities in the early 2030s
  • Keep the Athena community informed on the status of the project with the regular release of the newsletter Archived 8 March 2022 at the Wayback Machine, brief news, weekly news on the Athena web portal and in the social channels.
  • Develop communication and outreach activities, of particular interest, are the Athena nuggets Archived 9 September 2018 at the Wayback Machine.

The ACO is led by the Instituto de Física de Cantabria (CSIC-UC). Further ACO contributors are the Université de Genève, Max Planck Institute for Extraterrestrial Physics (MPE) and L'Institut de Recherche en Astrophysique et Planétologie (IRAP).

See also

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References

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  1. ^ a b c d "Athena: Mission Summary". ESA. 2 May 2022. Retrieved 4 May 2022.
  2. ^ "The Athena X-ray Observatory: Community Support Portal". ESA. 8 March 2021. Retrieved 14 March 2021.
  3. ^ "ESA's new vision to study the invisible universe". ESA. 8 March 2021. Retrieved 14 March 2021.
  4. ^ "About ATHENA". ESA. 1 September 2019. Retrieved 14 March 2021.
  5. ^ "ESA Science & Technology: Athena to study the hot and energetic Universe". ESA. 27 June 2014. Retrieved 14 March 2021.
  6. ^ "Final three for ESA's next medium science mission". ESA.
  7. ^ "Athena mission". Athena Community Office. Archived from the original on 6 February 2022. Retrieved 10 November 2021.
  8. ^ Bavdaz, Marcos; Wille, Eric; Ayre, Mark; Ferreira, Ivo; Shortt, Brian; Fransen, Sebastiaan; Collon, Maximilien; Vacanti, Giuseppe; Barrière, Nicolas; Landgraf, Boris (4 October 2018). Nikzad, Shouleh; Nakazawa, Kazuhiro; Den Herder, Jan-Willem A (eds.). Development of the ATHENA mirror (PDF). Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray. Vol. 106990X. DTU. p. 32. Bibcode:2018SPIE10699E..0XB. doi:10.1117/12.2313296. ISBN 9781510619517. S2CID 54028845. Archived (PDF) from the original on 12 April 2023. Retrieved 14 March 2021.
  9. ^ "Mirror development status" (PDF). Talk at the 2nd Athena conference, Palermo, Italy. ESA. 25 September 2018. Retrieved 14 March 2021.
  10. ^ Maximillien J. Collon; Giuseppe Vacanti; Nicolas M. Barrière (12 July 2019). "Silicon pore optics mirror module production and testing". In Karafolas, Nikos; Sodnik, Zoran; Cugny, Bruno (eds.). International Conference on Space Optics — ICSO 2018. Vol. 11180. SPIE. p. 74. Bibcode:2019SPIE11180E..23C. doi:10.1117/12.2535994. ISBN 9781510630772.
  11. ^ Collon, Maximillien (25 September 2018). "SPO development" (PDF). Talk at the 2nd Athena Conference, Palermo, Italy. Retrieved 14 March 2021.
  12. ^ "The Wide Field Imager for the Athena X-Ray Observatory". WFI ATHENA. 30 April 2020. Retrieved 14 March 2021.
  13. ^ Meidinger, Norbert; Nandra, Kirpal; Plattner, Markus (6 July 2018). "Development of the wide field imager instrument for ATHENA". In Nikzad, Shouleh; Nakazawa, Kazuhiro; Den Herder, Jan-Willem A (eds.). Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray. Vol. 10699. ads. p. 50. Bibcode:2018SPIE10699E..1FM. doi:10.1117/12.2310141. ISBN 9781510619517. S2CID 66404115. Retrieved 14 March 2021.
  14. ^ Rau, Arne (24 September 2018). "The Wide Field Imager - Talk at the 2nd Athena conference, Palermo, Italy" (PDF). Retrieved 14 March 2021.
  15. ^ "The Athena X-ray Integral Field Unit (X-IFU)". X-IFU home page. 11 February 2021. Retrieved 14 March 2021.
  16. ^ Barret, Didier; Lam Trong, Thien; den Herder, Jan-Willem (July 2018). Nikzad, Shouleh; Nakazawa, Kazuhiro; Den Herder, Jan-Willem A (eds.). The ATHENA x-ray integral field unit (X-IFU). Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray. Vol. 10699. ads. p. 51. arXiv:1807.06092. Bibcode:2018SPIE10699E..1GB. doi:10.1117/12.2312409. hdl:10261/239684. ISBN 9781510619517. S2CID 173185994. Retrieved 14 March 2021.
  17. ^ Barret, Didier (25 September 2018). "The Athena X-ray Integral Field Unit (X-IFU) Talk at the 2nd Athena Conference, Palermo, Italy" (PDF). IRAP. Retrieved 14 March 2021.
  18. ^ Barcons X, Barret D, Decourchelle A (21 March 2017). "ATHENA: ESA's X-ray observatory for the late 2020s". Astronomische Nachrichten. 338 (2–3). ads: 153–158. Bibcode:2017AN....338..153B. doi:10.1002/asna.201713323. Retrieved 14 March 2021.
  19. ^ "The Athena Community Office Talk at the 2nd Athena conference, Palermo, Italy" (PDF). ACO home page. 26 September 2018. Retrieved 14 March 2021.
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