Planck (spacecraft)

{{Short description|Space observatory}} {{Italic title}} {{Use dmy dates|date=September 2019}} {{Infobox spaceflight | name = ''Planck'' | names_list = COBRAS/SAMBA

| image = Model of the Planck Satellite.jpg | image_caption = A model of ''Planck'' | image_size = 250px

| mission_type = Space telescope | operator = ESA | COSPAR_ID = 2009-026B | SATCAT = 34938 | website = {{URL|http://www.esa.int/planck}} | mission_duration = Planned: >15 months Final: {{time interval|14 May 2009 13:12|23 October 2013 12:10|show=ymd|sep=,}}

| manufacturer = Thales Alenia Space | launch_mass = {{convert|1950|kg|lb|abbr=on}}<ref name="ariane20090424">{{cite web |url=http://www.arianespace.com/news-mission-update/2009/587.asp |title=The Planck space observatory is integrated on Ariane 5 for Arianespace's upcoming launch |publisher=Arianespace |date=24 April 2009 | archiveurl=https://web.archive.org/web/20101213045621/https://www.arianespace.com/news-mission-update/2009/587.asp | archivedate=13 December 2010}}</ref> | dry_mass = | payload_mass = {{convert|205|kg|lb|abbr=on}} | dimensions = Body: {{convert|4.20|x|4.22|m|ft|abbr=on}} | power =

| launch_date = {{start date text|14 May 2009, 13:12:02 UTC}} | launch_rocket = Ariane 5 ECA | launch_site = Guiana Space Centre, French Guiana | launch_contractor = Arianespace | entered_service = 3 July 2009

| disposal_type = Decommissioned | deactivated = {{end date text|23 October 2013, 12:10:27 UTC}}

| orbit_reference = Sun-Earth L2 orbit ({{convert|1500000|km|mi|abbr=on|disp=x| / }}) | orbit_regime = Lissajous | apsis = helion

| telescope_type = Gregorian | telescope_diameter = {{convert|1.9|x|1.5|m|ft|abbr=on}} | telescope_focal_length=  | telescope_area =  | telescope_wavelength = 300 μm – 11.1 mm (frequencies between 27 GHz and 1 THz) | instruments_list = {{Infobox spaceflight/Instruments | acronym1 = HFI | name1 = High Frequency Instrument | acronym2 = LFI | name2 = Low Frequency Instrument }}

| insignia = Planck insignia.png  | insignia_upright = 0.6 | insignia_caption = Contemporary ESA insignia (2000s)

| programme = '''Horizon 2000''' (Science Programme) | previous_mission = ''Herschel'' | next_mission = ''Gaia'' }}

'''''Planck''''' was a space observatory operated by the European Space Agency (ESA) from 2009 to 2013. The project aimed to map the anisotropies of the cosmic microwave background (CMB) at microwave and infrared frequencies, with high sensitivity and angular resolution. The mission provided data that substantially improved upon previous observations made by the NASA Wilkinson Microwave Anisotropy Probe (WMAP).

The Planck observatory was a major source of information relevant to several cosmological and astrophysical issues. One of its key objectives was to test cosmological theories about the early Universe, its composition and evolution, and the origin of cosmic structure.

Planck was initially called COBRAS/SAMBA, which stands for the Cosmic Background Radiation Anisotropy Satellite/Satellite for Measurement of Background Anisotropies. The project started in 1996, and it was later renamed in honor of the German physicist Max Planck (1858–1947), who is widely regarded as the originator of quantum theory by deriving the formula for black-body radiation.

Built at the Cannes Mandelieu Space Center by Thales Alenia Space, Planck was created as a medium-sized mission for ESA's Horizon 2000 long-term scientific program. The observatory was launched in May 2009 and reached the Earth/Sun L2 point by July 2009. By February 2010, it had successfully started a second all-sky survey.

On 21 March 2013, the Planck team released its first all-sky map of the cosmic microwave background. The map allowed researchers to measure temperature variations in the CMB with the highest accuracy then available. In February 2015, an expanded release was published, which included polarization data. The final papers by the Planck team were released in July 2018, marking the end of the mission.

At the end of its mission, Planck was put into a heliocentric graveyard orbit and passivated to prevent it from endangering any future missions. The final deactivation command was sent to Planck in October 2013.

The mission provided the most precise measurements of several key cosmological parameters. Planck's observations helped determine the age of the universe, the average density of ordinary matter and dark matter in the Universe, and other important characteristics of the cosmos.

== Objectives == The mission had a wide variety of scientific aims, including:<ref name="bluebook_c1"/>

* high resolution detections of both the total intensity and polarization of primordial CMB anisotropies, * creation of a catalogue of galaxy clusters through the Sunyaev–Zel'dovich effect, * observations of the gravitational lensing of the CMB, as well as the integrated Sachs–Wolfe effect, * observations of bright extragalactic radio (active galactic nuclei) and infrared (dusty galaxy) sources, * observations of the Milky Way, including the interstellar medium, distributed synchrotron emission and measurements of the Galactic magnetic field, and * studies of the Solar System, including planets, asteroids, comets and the zodiacal light.

''Planck'' had a higher resolution and sensitivity than WMAP, allowing it to probe the power spectrum of the CMB to much smaller scales (×3). It also observed in nine frequency bands rather than WMAP's five, with the goal of improving the astrophysical foreground models.

It is expected that most ''Planck'' measurements have been limited by how well foregrounds can be subtracted, rather than by the detector performance or length of the mission, a particularly important factor for the polarization measurements.{{update after|2017|10|21}} The dominant foreground radiation depends on frequency, but could include synchrotron radiation from the Milky Way at low frequencies, and dust at high frequencies.{{update after|2017|10|21}}

== Instruments ==

thumb|right|The 4 K reference load qualification model

thumb|right|LFI 44 GHz horn and front-end chassis

thumb|right|LFI focal plane model

The spacecraft carries two instruments: the Low Frequency Instrument (LFI) and the High Frequency Instrument (HFI).<ref name="bluebook_c1">{{cite web |url=http://www.rssd.esa.int/SA/PLANCK/docs/Bluebook-ESA-SCI%282005%291_V2.pdf |title=Planck: The Scientific Programme |publisher=European Space Agency |id=ESA-SCI(2005)1 |date=2005 |access-date=6 March 2009}}</ref> Both instruments can detect both the total intensity and polarization of photons, and together cover a frequency range of nearly 830 GHz (from 30 to 857 GHz). The cosmic microwave background spectrum peaks at a frequency of 160.2 GHz.

''Planck''{{'s}} passive and active cooling systems allow its instruments to maintain a temperature of {{convert|-273.05|C|F|2}}, or 0.1 °C above absolute zero.<ref>{{Cite journal | doi = 10.1016/j.cryogenics.2021.103390 |issn=0011-2275| title = Development of Dilution refrigerators – A review | journal = Cryogenics| volume = 121| year = 2022| last1 = Zu | first1 = H.| last2 = Dai | first2 = W.| last3 = de Waele | first3 = A.T.A.M.| s2cid = 244005391 }}</ref> From August 2009, ''Planck'' was the coldest known object in space, until its active coolant supply was exhausted in January 2012.<ref name="space20090707">{{cite news |url=http://www.space.com/6930-coldest-object-space-unnatural.html |title=Coldest Known Object in Space Is Very Unnatural |work=Space.com |date=7 July 2009 |access-date=3 July 2013}}</ref>

NASA played a role in the development of this mission and contributes to the analysis of scientific data. Its Jet Propulsion Laboratory built components of the science instruments, including bolometers for the high-frequency instrument, a 20-kelvin cryocooler for both the low- and high-frequency instruments, and amplifier technology for the low-frequency instrument.<ref>{{cite web |url=http://www.nasa.gov/mission_pages/planck/overview.html |title=Planck: Mission Overview |publisher=NASA |access-date=26 September 2009}}</ref>

=== Low Frequency Instrument ===

{| class="wikitable" |- ! Frequency (GHz) || Bandwidth (Δν/ν) || Resolution (arcmin) || Sensitivity (total intensity) Δ''T''/''T'', 14-month observation (10−6) || Sensitivity (polarization) Δ''T''/''T'', 14-month observation (10−6) |- style="text-align:center;" | 30 || 0.2 || 33 || 2.0 || 2.8 |- style="text-align:center;" | 44 || 0.2 || 24 || 2.7 || 3.9 |- style="text-align:center;" | 70 || 0.2 || 14 || 4.7 || 6.7 |}

The LFI has three frequency bands, covering the range of 30–70 GHz, covering the microwave to infrared regions of the electromagnetic spectrum. The detectors use high-electron-mobility transistors.<ref name="bluebook_c1"/>

=== High Frequency Instrument ===

thumb|right|The High Frequency Instrument qualification model.

{| class="wikitable" |- ! Frequency (GHz) || Bandwidth (Δν/ν) || Resolution (arcmin) || Sensitivity (total intensity) Δ''T''/''T'', 14-month observation (10−6) || Sensitivity (polarization) Δ''T''/''T'', 14-month observation (10−6) |- style="text-align:center;" | 100 || 0.33 || 10 || 2.5 || 4.0 |- style="text-align:center;" | 143 || 0.33 || 7.1 || 2.2 || 4.2 |- style="text-align:center;" | 217 || 0.33 || 5.0 || 4.8 || 9.8 |- style="text-align:center;" | 353 || 0.33 || 5.0 || 14.7 || 29.8 |- style="text-align:center;" | 545 || 0.33 || 5.0 || 147 || N/A |- style="text-align:center;" | 857 || 0.33 || 5.0 || 6700 || N/A |}

The HFI was sensitive between 100 and 857 GHz, using 52 bolometric detectors, manufactured by JPL/Caltech,<ref>{{cite web |url=http://planck.caltech.edu/hfi.html |title=The Planck High Frequency Instrument (HFI) |publisher=Jet Propulsion Laboratory |date=21 March 2013 |access-date=22 March 2013 |archive-date=25 April 2015 |archive-url=https://web.archive.org/web/20150425082904/http://planck.caltech.edu/hfi.html |url-status=dead }}</ref> optically coupled to the telescope through cold optics, manufactured by Cardiff University's School of Physics and Astronomy,<ref>{{cite web |url=http://www.astro.cardiff.ac.uk/research/astro/instr/projects/?page=hfi |title=High Frequency Instrument (HFI) |publisher=Cardiff University |access-date=22 March 2013 |archive-date=12 April 2017 |archive-url=https://web.archive.org/web/20170412051045/http://www.astro.cardiff.ac.uk/research/astro/instr/projects/?page=hfi |url-status=dead }}</ref> consisting of a triple horn configuration and optical filters, a similar concept to that used in the Archeops balloon-borne experiment. These detection assemblies are divided into 6 frequency bands (centred at 100, 143, 217, 353, 545 and 857 GHz), each with a bandwidth of 33%. Of these six bands, only the lower four have the capability to measure the polarisation of incoming radiation; the two higher bands do not.<ref name="bluebook_c1"/>

On 13 January 2012, it was reported that the on-board supply of helium-3 used in ''Planck''{{'s}} dilution refrigerator had been exhausted, and that the HFI would become unusable within a few days.<ref name="BBC-warming">{{cite news |url=https://www.bbc.co.uk/news/science-environment-12065464 |title=Super-cool Planck mission begins to warm |work=BBC News |last=Amos |first=Jonathan |date=13 January 2012 |access-date=13 January 2012}}</ref> By this date, ''Planck'' had completed five full scans of the CMB, exceeding its target of two. The LFI (cooled by helium-4) was expected to remain operational for another six to nine months.<ref name="BBC-warming" />

== Service module ==

[[File:Herschel planck team.jpg|thumb|Some of the ''Herschel''-''Planck'' team, from left to right: Jean-Jacques Juillet, director of scientific programmes, Thales Alenia Space; Marc Sauvage, project scientist for ''Herschel'' PACS experiment, CEA; François Bouchet, ''Planck'' operations manager, IAP; and Jean-Michel Reix, ''Herschel'' & ''Planck'' operations manager, Thales Alenia Space. Taken during presentations of the first results for the missions, Cannes, October 2009.]]

A common service module (SVM) was designed and built by Thales Alenia Space in its Turin plant, for both the ''Herschel Space Observatory'' and ''Planck'' missions, combined into one single program.<ref name="bluebook_c1"/>

The overall cost is estimated to be {{€|700 million}} for the ''Planck''<ref>{{cite web |url=http://esamultimedia.esa.int/docs/planck/Planck-Factsheet.pdf |title=Planck: Fact Sheet |publisher=European Space Agency |date=20 January 2012 |archive-url=https://web.archive.org/web/20120731085438/http://esamultimedia.esa.int/docs/planck/Planck-Factsheet.pdf |archive-date=31 July 2012 |url-status=live}}</ref> and {{€|1,100 million}} for the ''Herschel'' mission.<ref>{{cite web |url=http://esamultimedia.esa.int/docs/herschel/Herschel-Factsheet.pdf |title=Herschel: Fact Sheet |publisher=European Space Agency |date=28 April 2010 |archive-url=https://web.archive.org/web/20121018233814/http://esamultimedia.esa.int/docs/herschel/Herschel-Factsheet.pdf |archive-date=18 October 2012 |url-status=live}}</ref> Both figures include their mission's spacecraft and payload, (shared) launch and mission expenses, and science operations.

Structurally, the ''Herschel'' and ''Planck'' SVMs are very similar. Both SVMs are octagonal in shape and each panel is dedicated to accommodate a designated set of warm units, while taking into account the dissipation requirements of the different warm units, of the instruments, as well as the spacecraft. On both spacecraft, a common design was used for the avionics, attitude control and measurement (ACMS), command and data management (CDMS), power, and tracking, telemetry and command (TT&C) subsystems. All units on the SVM are redundant.

=== Power Subsystem ===

On each spacecraft, the power subsystem consists of a solar array, employing triple-junction solar cells, a battery and the power control unit (PCU). The PCU is designed to interface with the 30 sections of each solar array, to provide a regulated 28 volt bus, to distribute this power via protected outputs, and to handle the battery charging and discharging.

For ''Planck'', the circular solar array is fixed on the bottom of the satellite, always facing the Sun as the satellite rotates on its vertical axis.

=== Attitude and Orbit Control ===

This function is performed by the attitude control computer (ACC), which is the platform for the attitude control and measurement subsystem (ACMS). It was designed to fulfil the pointing and slewing requirements of the ''Herschel'' and ''Planck'' payloads.

The ''Planck'' satellite rotates at one revolution per minute, with an aim of an absolute pointing error less than 37 arc-minutes. As ''Planck'' is also a survey platform, there is the additional requirement for pointing reproducibility error less than 2.5 arc-minutes over 20 days.

The main line-of-sight sensor in both ''Herschel'' and ''Planck'' is the star tracker.

== Launch and orbit == {{multiple image | align =right| direction = vertical| width = | header = Animation of Planck Space Observatory{{'s}} trajectory | image1 = Animation of Planck Space Observatory trajectory - Polar view.gif | caption1 = Polar view | image2 = Animation of Planck Space Observatory trajectory - Equatorial view.gif | caption2 = Equatorial view | image3 = Animation of Planck Space Observatory trajectory viewed from Earth.gif | caption3 = Viewed from the Sun | footer ={{legend2| RoyalBlue| Earth}}{{·}}{{legend2|Magenta| Planck Space Observatory }} }}

The satellite was successfully launched, along with the ''Herschel Space Observatory'', at 13:12:02 UTC on 14 May 2009 aboard an Ariane 5 ECA heavy launch vehicle from the Guiana Space Centre. The launch placed the craft into a very elliptical orbit (perigee: {{convert|270|km|mi|abbr=on|disp=x| [|]}}, apogee: more than {{convert|1120000|km|mi|abbr=on|disp=x| [|]}}), bringing it near the {{L2}} Lagrangian point of the Earth-Sun system, {{convert|1500000|km}} from the Earth.

The manoeuvre to inject ''Planck'' into its final orbit around {{L2}} was successfully completed on 3 July 2009, when it entered a Lissajous orbit with a {{convert|400000|km|abbr=on|adj=on}} radius around the {{L2}} Lagrangian point.<ref name="planck-summary">{{cite web |url=http://www.rssd.esa.int/index.php?project=PLANCK&page=dev_news |archive-url=https://archive.today/20120805125417/http://www.rssd.esa.int/index.php?project=PLANCK&page=dev_news |title=Planck: Mission Status Summary |publisher=European Space Agency |date=19 March 2013 |access-date=22 March 2013| archive-date=5 August 2012}}</ref> The temperature of the High Frequency Instrument reached just a tenth of a degree above absolute zero (0.1 K) on 3 July 2009, placing both the Low Frequency and High Frequency Instruments within their cryogenic operational parameters, making ''Planck'' fully operational.<ref>{{cite web |url=http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=45133 |title=Planck instruments reach their coldest temperature |publisher=European Space Agency |date=3 July 2009 |access-date=5 July 2009}}</ref>

== Decommissioning ==

In January 2012 the HFI exhausted its supply of liquid helium, causing the detector temperature to rise and rendering the HFI unusable. The LFI continued to be used until science operations ended on 3 October 2013. The spacecraft performed a manoeuvre on 9 October to move it away from Earth and its {{L2|pt=yes}}, placing it into a heliocentric orbit, while payload deactivation occurred on 19 October. ''Planck'' was commanded on 21 October to exhaust its remaining fuel supply; passivation activities were conducted later, including battery disconnection and the disabling of protection mechanisms.<ref name="deactivation">{{cite web |url=http://www.esa.int/Our_Activities/Operations/Planck_on_course_for_safe_retirement |title=Planck on course for safe retirement |publisher=European Space Agency |date=21 October 2013 |access-date=23 October 2013}}</ref> The final deactivation command, which switched off the spacecraft's transmitter, was sent to ''Planck'' on 23 October 2013 at 12:10:27 UTC.<ref name="finalcommand">{{cite web |url=http://www.esa.int/Our_Activities/Space_Science/Planck/Last_command_sent_to_ESA_s_Planck_space_telescope |title=Last command sent to ESA's Planck space telescope |publisher=European Space Agency |date=23 October 2013 |access-date=23 October 2013}}</ref>

== Results ==

[[File:PIA16874-CobeWmapPlanckComparison-20130321.jpg|thumb|Comparison of CMB results from COBE, WMAP and ''Planck'']] [[File:Galaxy cluster PLCK G004.5-19.5 A window into the cosmic past.jpg|thumb|left|Galaxy cluster PLCK G004.5-19.5 was discovered through the Sunyaev–Zel'dovich effect.<ref>{{cite web|title=A window into the cosmic past|url=https://www.spacetelescope.org/images/potw1807a/|website=Spacetelescope.org|access-date=12 February 2018}}</ref>]]

''Planck'' started its First All-Sky Survey on 13 August 2009.<ref name="planck-pointing">{{cite web |url=http://www.rssd.esa.int/index.php?project=PLANCK&page=Pointing |title=Simultaneous observations with Planck |publisher=European Space Agency |date=31 August 2009 |access-date=17 August 2012}}</ref> In September 2009, the European Space Agency announced the preliminary results from the ''Planck First Light Survey'', which was performed to demonstrate the stability of the instruments and the ability to calibrate them over long periods. The results indicated that the data quality is excellent.<ref>{{cite web |url=http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=45543 |title=Planck first light yields promising results |publisher=European Space Agency |date=17 September 2009}}</ref>

On 15 January 2010 the mission was extended by 12 months, with observation continuing until at least the end of 2011. After the successful conclusion of the First Survey, the spacecraft started its Second All Sky Survey on 14 February 2010. The last observations for the Second All Sky Survey were made on 28 May 2010.<ref name="planck-summary"/>

Some planned pointing list data from 2009 has been released publicly, along with a video visualization of the surveyed sky.<ref name="planck-pointing"/>

On 17 March 2010, the first ''Planck'' photos were published, showing dust concentration within 500 light years from the Sun.<ref>{{cite news |url=http://www.esa.int/Our_Activities/Space_Science/Planck/Planck_sees_tapestry_of_cold_dust |title=Planck sees tapestry of cold dust |publisher=European Space Agency |date=17 March 2010}}</ref><ref>{{cite web |url=http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=46706 |title=New Planck images trace cold dust and reveal large-scale structure in the Milky Way |publisher=European Space Agency |date=17 March 2010 |access-date=17 August 2012}}</ref>

On 5 July 2010, the ''Planck'' mission delivered its first all-sky image.<ref>{{cite web |url=http://www.esa.int/Our_Activities/Space_Science/Planck/Planck_unveils_the_Universe_now_and_then |title=Planck unveils the Universe – now and then |publisher=European Space Agency |date=5 July 2010 |access-date=22 March 2013}}</ref>

The first public scientific result of ''Planck'' is the Early-Release Compact-Source Catalogue, released during the January 2011 ''Planck conference'' in Paris.<ref>{{cite web |url=http://www.planck2011.fr/ |title=2011 Planck Conference |access-date=22 March 2013}}</ref><ref>{{cite web |url=http://www.sciops.esa.int/index.php?project=planck&page=Planck_Legacy_Archive |title=Planck Legacy Archive |publisher=European Space Agency |url-status=dead |archive-url=https://web.archive.org/web/20121007212449/http://www.sciops.esa.int/index.php?project=planck&page=Planck_Legacy_Archive |archive-date=7 October 2012 }}</ref>

On 5 May 2014 a map of the galaxy's magnetic field created using ''Planck'' was published.<ref>{{cite news |url=https://www.sciencenews.org/article/milky-way%E2%80%99s-magnetic-field-mapped |title=Milky Way's magnetic field mapped |work=Science News |first=Christopher |last=Crockett |date=9 May 2014 |access-date=10 May 2014}}</ref>

The Planck team and principal investigators Nazzareno Mandolesi and Jean-Loup Puget shared the 2018 Gruber Prize in Cosmology.<ref name="gruber2018">{{cite web |url=https://gruber.yale.edu/prize/2018-gruber-cosmology-prize |title=2018 Gruber Cosmology Prize |publisher=Gruber Foundation |date=2018 |access-date=28 May 2018}}</ref> Puget was also awarded the 2018 Shaw Prize in Astronomy.<ref name="shaw2018">{{cite web |url=http://www.shawprize.org/en/shaw.php?tmp=5&twoid=79&threeid=278&fourid=554 |title=Announcement of The Shaw Laureates 2018 |publisher=The Shaw Prize |date=14 May 2018 |access-date=28 May 2018 |archive-date=7 October 2018 |archive-url=https://web.archive.org/web/20181007061234/http://www.shawprize.org/en/shaw.php?tmp=5&twoid=79&threeid=278&fourid=554 |url-status=dead }}</ref> The 2019 Cocconi Prize of the European Physical Society has been awarded to the Planck collaboration (jointly with the WMAP collaboration).<ref>{{Cite web |last=High Energy Particle Physics Division of EPS |title=The Giuseppe and Vanna Cocconi Prize |url=https://eps-hepp.web.cern.ch/cocconi-prize-awards.php |access-date=2026-02-05 |website=eps-hepp.web.cern.ch}}</ref>

=== 2013 data release === On 21 March 2013, the European-led research team behind the ''Planck'' cosmology probe released the mission's all-sky map of the cosmic microwave background.<ref name="NASA-20130321" /><ref name="NYT-20130321g">{{cite news |url=https://www.nytimes.com/interactive/2013/03/21/science/space/0321-universe.html |title=Mapping the Early Universe |work=The New York Times |date=21 March 2013 |access-date=23 March 2013}}</ref> This map suggests the Universe is slightly older than thought: according to the map, subtle fluctuations in temperature were imprinted on the deep sky when the Universe was about 370,000 years old. The imprint reflects ripples that arose as early in the existence of the Universe as the first nonillionth (10−30) of a second. It is theorised that these ripples gave rise to the present vast cosmic web of galactic clusters and dark matter. The 2013 release found an asymmetry in the statistics of the CMB with respect to viewing angle in the sky, determining that "deviations from isotropy have been found and demonstrated to be robust against component separation algorithm, mask choice and frequency dependence",<ref>{{cite journal |arxiv=1303.5083 |doi=10.1051/0004-6361/201321534 |title=''Planck'' 2013 results. XXIII. Isotropy and statistics of the CMB |date=2014 |last1=Ade |first1=P. A. R. |last2=Aghanim |first2=N. |last3=Armitage-Caplan |first3=C. |last4=Arnaud |first4=M. |last5=Ashdown |first5=M. |last6=Atrio-Barandela |first6=F. |last7=Aumont |first7=J. |last8=Baccigalupi |first8=C. |last9=Banday |first9=A. J. |last10=Barreiro |first10=R. B. |last11=Bartlett |first11=J. G. |last12=Bartolo |first12=N. |last13=Battaner |first13=E. |last14=Battye |first14=R. |last15=Benabed |first15=K. |last16=Benoît |first16=A. |last17=Benoit-Lévy |first17=A. |last18=Bernard |first18=J.-P. |last19=Bersanelli |first19=M. |last20=Bielewicz |first20=P. |last21=Bobin |first21=J. |last22=Bock |first22=J. J. |last23=Bonaldi |first23=A. |last24=Bonavera |first24=L. |last25=Bond |first25=J. R. |last26=Borrill |first26=J. |last27=Bouchet |first27=F. R. |last28=Bridges |first28=M. |last29=Bucher |first29=M. |last30=Burigana |first30=C. |journal=Astronomy & Astrophysics |volume=571 |pages=A23 |display-authors=1 |bibcode=2014A&A...571A..23P }}</ref> more commonly known as the Axis of evil (cosmology). According to the team, the Universe is {{val|13.798|0.037}} billion-years-old, and contains {{val|4.82|0.05|u=%}} ordinary matter, {{val|26.8|0.4|u=%}} dark matter and {{val|69|1|u=%}} dark energy.<ref name= "planck_overview">See Table 9 in {{cite journal |author1=Planck Collaboration |date=2013 |title=Planck 2013 results. I. Overview of products and scientific results |arxiv=1303.5062 |doi=10.1051/0004-6361/201321529 |volume=571 |journal=Astronomy & Astrophysics |page=A1 |bibcode=2014A&A...571A...1P|s2cid=218716838 }}</ref><ref name="planck_overview2">{{cite web |url=http://www.sciops.esa.int/index.php?project=PLANCK&page=Planck_Published_Papers |title=Planck 2013 Results Papers |publisher=European Space Agency |url-status=dead |archive-url=https://web.archive.org/web/20130323234553/http://www.sciops.esa.int/index.php?project=PLANCK&page=Planck_Published_Papers |archive-date=23 March 2013 }}</ref><ref name="planck_overview3">{{cite journal |author1=Planck Collaboration |date=2013 |title=Planck 2013 results. XVI. Cosmological parameters |arxiv=1303.5076 |doi=10.1051/0004-6361/201321591 |volume=571 |journal=Astronomy & Astrophysics |page=A16 |bibcode=2014A&A...571A..16P|s2cid=118349591 }}</ref> The Hubble constant was also measured to be {{val|67.80|0.77|u=(km/s)/Mpc}}.<ref name="NASA-20130321">{{cite web |url=http://www.jpl.nasa.gov/news/news.php?release=2013-109 |title=Planck Mission Brings Universe Into Sharp Focus |publisher=Jet Propulsion Laboratory |date=21 March 2013 |access-date=21 March 2013}}</ref><ref name="planck_overview" /><ref name="ESA-20130321">{{cite web |url=http://www.esa.int/Our_Activities/Space_Science/Planck/Planck_reveals_an_almost_perfect_Universe |title=Planck reveals an almost perfect Universe |publisher=European Space Agency |date=21 March 2013 |access-date=21 March 2013}}</ref><ref name="NYT-20130321">{{cite news |url=https://www.nytimes.com/2013/03/22/science/space/planck-satellite-shows-image-of-infant-universe.html?pagewanted=all |title=Universe as an Infant: Fatter Than Expected and Kind of Lumpy |work=The New York Times |last=Overbye |first=Dennis |date=21 March 2013 |access-date=21 March 2013}}</ref><ref name="NBC-20130321">{{cite web |url=http://www.nbcnews.com/science/planck-probes-cosmic-baby-picture-revises-universes-vital-statistics-1C8986034 |title=Planck probe's cosmic 'baby picture' revises universe's vital statistics |work=NBC News |last=Boyle |first=Alan |date=21 March 2013 |access-date=21 March 2013}}</ref> {{Clear}}

<div class="center"> {| border="1" cellpadding="1" cellspacing="0" style="margin: 1em 1em 1em 0; background: #f9f9f9; border: 1px #aaa solid; border-collapse: collapse; font-size: 80%; text-align:center;" |- bgcolor="#B0C4DE" align="center" |+ Cosmological parameters from 2013 Planck results<ref name="planck_overview" /><ref name="planck_overview3" /> ! Parameter !! Symbol !! ''Planck'' Best fit !! ''Planck'' 68% limits !! ''Planck''+lensing Best fit !! ''Planck''+lensing 68% limits !! ''Planck''+WP Best fit !! ''Planck''+WP 68% limits !! ''Planck''+WP +HighL Best fit !! ''Planck''+WP +HighL 68% limits !! ''Planck''+lensing +WP+highL Best fit !! ''Planck''+lensing +WP+highL 68% limits !! ''Planck''+WP +highL+BAO Best fit !! ''Planck''+WP +highL+BAO 68% limits |- | Baryon density || <math>\Omega_b h^2</math> || 0.022068 || {{val|0.02207|0.00033}} || 0.022242 || {{val|0.02217|0.00033}} || 0.022032 || {{val|0.02205|0.00028}} || 0.022069 || {{val|0.02207|0.00027}} || 0.022199 || {{val|0.02218|0.00026}} || 0.022161 || {{val|0.02214|0.00024}} |- | Cold dark matter density || <math>\Omega_c h^2</math> || 0.12029 || {{val|0.1196|0.0031}} || 0.11805 || {{val|0.1186|0.0031}} || 0.12038 || {{val|0.1199|0.0027}} || 0.12025 || {{val|0.1198|0.0026}} || 0.11847 ||{{val|0.1186|0.0022}} || 0.11889 ||{{val|0.1187|0.0017}} |- | 100x approximation to rs / DA (CosmoMC) || <math>100\,\theta_{MC}</math> || 1.04122 || {{val|1.04132|0.00068}} || 1.04150 || {{val|1.04141|0.00067}} || 1.04119 || {{val|1.04131|0.00063}} || 1.04130|| {{val|1.04132|0.00063}} || 1.04146 || {{val|1.04144|0.00061}} || 1.04148 || {{val|1.04147|0.00056}} |- | Thomson scattering optical depth due to reionization || <math>\tau</math> || 0.0925 || {{val|0.097|0.038}} || 0.0949 || {{val|0.089|0.032}} || 0.0925 || {{val|0.089|+0.012|-0.014}} || 0.0927 || {{val|0.091|+0.013|-0.014}} || 0.0943 || {{val|0.090|+0.013|-0.014}}|| 0.0952 || {{val|0.092|0.013}} |- | Power spectrum of curvature perturbations || <math>\ln(10^{10} A_s)</math> || 3.098 || {{val|3.103|0.072}} || 3.098 || {{val|3.085|0.057}} || 3.0980 || {{val|3.089|+0.024|-0.027}} || 3.0959 || {{val|3.090|0.025}} || 3.0947 || {{val|3.087|0.024}} || 3.0973 || {{val|3.091|0.025}} |- | Scalar spectral index || <math>n_s</math> || 0.9624 || {{val|0.9616|0.0094}}|| 0.9675 || {{val|0.9635|0.0094}}|| 0.9619 || {{val|0.9603|0.0073}}|| 0.9582 || {{val|0.9585|0.0070}}|| 0.9624 || {{val|0.9614|0.0063}}|| 0.9611 || {{val|0.9608|0.0054}} |- | Hubble's constant (km Mpc−1 s−1) || <math>H_0</math> || 67.11 || {{val|67.4|1.4}} || 68.14 || {{val|67.9|1.5}} || 67.04 || {{val|67.3|1.2}} || 67.15 || {{val|67.3|1.2}} || 67.94 || {{val|67.9|1.0}}|| 67.77 || {{val|67.80|0.77}} |- | Dark energy density || <math>\Omega_\Lambda</math> || 0.6825 || {{val|0.686|0.020}} || 0.6964 || {{val|0.693|0.019}} || 0.6817 || {{val|0.685|+0.018|-0.016}} || 0.6830 || {{val|0.685|+0.017|-0.016}} || 0.6939 || {{val|0.693|0.013}} || 0.6914 || {{val|0.692|0.010}} |- | Density fluctuations at 8h−1 Mpc || <math>\sigma_8</math> || 0.8344 || {{val|0.834|0.027}} || 0.8285 || {{val|0.823|0.018}} || 0.8347 || {{val|0.829|0.012}} || 0.8322 || {{val|0.828|0.012}} || 0.8271 || {{val|0.8233|0.0097}}|| 0.8288 || {{val|0.826|0.012}} |- | Redshift of reionization || <math>z_{re}</math> || 11.35 ||{{val|11.4|+4.0|-2.8}} || 11.45 || {{val|10.8|+3.1|-2.5}} || 11.37 || {{val|11.1|1.1}} || 11.38 || {{val|11.1|1.1}} || 11.42 || {{val|11.1|1.1}} || 11.52 || {{val|11.3|1.1}} |- | Age of the Universe (Gy) || <math>t_0</math> || 13.819 || {{val|13.813|0.058}} || 13.784 || {{val|13.796|0.058}} || 13.8242 || {{val|13.817|0.048}} || 13.8170 || {{val|13.813|0.047}} || 13.7914 || {{val|13.794|0.044}} || 13.7965 || {{val|13.798|0.037}} |- | 100× angular scale of sound horizon at last-scattering || <math>100\,\theta_*</math> || 1.04139 || {{val|1.04148|0.00066}} || 1.04164 || {{val|1.04156|0.00066}} || 1.04136 || {{val|1.04147|0.00062}} || 1.04146 || {{val|1.04148|0.00062}} || 1.04161 || {{val|1.04159|0.00060}}|| 1.04163 || {{val|1.04162|0.00056}} |- | Comoving size of the sound horizon at z = zdrag || <math>r_{drag}</math> || 147.34 || {{val|147.53|0.64}} || 147.74 || {{val|147.70|0.63}} || 147.36 || {{val|147.49|0.59}} || 147.35 || {{val|147.47|0.59}} || 147.68 || {{val|147.67|0.50}} || 147.611 || {{val|147.68|0.45}} |} </div> {{Clear}}

=== 2015 data release === Results from an analysis of ''Planck''{{'s}} full mission were made public on 1 December 2014 at a conference in Ferrara, Italy.<ref name="nature20141202">{{cite news |url=http://www.nature.com/news/european-probe-shoots-down-dark-matter-claims-1.16462 |title=European probe shoots down dark-matter claims |journal=Nature |first1=Ron |last1=Cowen |first2=Davide |last2=Castelvecchi |date=2 December 2014 |access-date=6 December 2014 |doi=10.1038/nature.2014.16462}}</ref> A full set of papers detailing the mission results were released in February 2015.<ref name="planckesa2015">{{cite web |url=http://www.cosmos.esa.int/web/planck/publications |title=Planck Publications: Planck 2015 Results |publisher=European Space Agency |date=February 2015 |access-date=9 February 2015}}</ref> Some of the results include:

* More agreement with previous WMAP results on parameters such as the density and distribution of matter in the Universe, as well as more accurate results with less margin of error. * Confirmation of the Universe having a 26% content of dark matter. These results also raise related questions about the positron excess over electrons detected by the Alpha Magnetic Spectrometer, an experiment on the International Space Station. Previous research suggested that positrons could be created by the collision of dark matter particles, which could only occur if the probability of dark matter collisions is significantly higher now than in the early Universe. ''Planck'' data suggests that the probability of such collisions must remain constant over time to account for the structure of the Universe, negating the previous theory. * Validation of the simplest models of inflation, thus giving the Lambda-CDM model stronger support. * That there are likely only three types of neutrinos, with a fourth proposed sterile neutrino unlikely to exist.

Project scientists worked too with BICEP2 scientists to release joint research in 2015 answering whether a signal detected by BICEP2 was evidence of primordial gravitational waves, or was simple background noise from dust in the Milky Way galaxy.<ref name="nature20141202"/> Their results suggest the latter.<ref name="planckbicep2015">{{cite journal |title=A Joint Analysis of BICEP2/''Keck Array'' and ''Planck'' Data |arxiv=1502.00612 | last=Ade | first=P. A. R. | collaboration=BICEP2/Keck and Planck Collaborations. |date=February 2015 |doi=10.1103/PhysRevLett.114.101301 |pmid=25815919 |volume=114 |issue=10 |article-number=101301 |journal=Physical Review Letters |bibcode=2015PhRvL.114j1301B|s2cid=218078264 }}</ref>

{{Clear}} <div class="center"> {| border="1" cellpadding="1" cellspacing="0" style="margin: 1em 1em 1em 0; background: #f9f9f9; border: 1px #aaa solid; border-collapse: collapse; font-size: 80%; text-align: center;" |- bgcolor="#B0C4DE" align="center" |+ Cosmological parameters from 2015 ''Planck'' results<ref name="planckesa2015" /><ref name="planckesa20152">{{cite journal |author=Planck Collaboration |year=2016 |title=Planck 2015 results. XIII. Cosmological parameters |arxiv=1502.01589 |doi=10.1051/0004-6361/201525830 |volume=594 |journal=Astronomy & Astrophysics |page=A13 |bibcode=2016A&A...594A..13P|s2cid=119262962 }}</ref> ! Parameter !! Symbol !! TT+lowP 68% limits !! TT+lowP +lensing 68% limits !! TT+lowP +lensing+ext 68% limits !! TT,TE,EE+lowP 68% limits !! TT,TE,EE+lowP +lensing 68% limits !! TT,TE,EE+lowP +lensing+ext 68% limits |- | Baryon density || <math>\Omega_b h^2</math> || {{val|0.02222|0.00023}} || {{val|0.02226|0.00023}} || {{val|0.02227|0.00020}} || {{val|0.02225|0.00016}} || {{val|0.02226|0.00016}} || {{val|0.02230|0.00014}} |- | Cold dark matter density || <math>\Omega_c h^2</math> || {{val|0.1197|0.0022}} || {{val|0.1186|0.0020}} || {{val|0.1184|0.0012}} || {{val|0.1198|0.0015}} || {{val|0.1193|0.0014}} || {{val|0.1188|0.0010}} |- | 100x approximation to rs / DA (CosmoMC) || <math>100\,\theta_{MC}</math> || {{val|1.04085|0.00047}} || {{val|1.04103|0.00046}} || {{val|1.04106|0.00041}} || {{val|1.04077|0.00032}} || {{val|1.04087|0.00032}}|| {{val|1.04093|0.00030}} |- | Thomson scattering optical depth due to reionization || <math>\tau</math> || {{val|0.078|0.019}} || {{val|0.066|0.016}} || {{val|0.067|0.013}} || {{val|0.079|0.017}} || {{val|0.063|0.014}} || {{val|0.066|0.012}} |- | Power spectrum of curvature perturbations || <math>\ln(10^{10} A_s)</math> || {{val|3.089|0.036}} || {{val|3.062|0.029}} || {{val|3.064|0.024}} || {{val|3.094|0.034}} || {{val|3.059|0.025}}|| {{val|3.064|0.023}} |- | Scalar spectral index || <math>n_s</math> || {{val|0.9655|0.0062}}|| {{val|0.9677|0.0060}}|| {{val|0.9681|0.0044}}|| {{val|0.9645|0.0049}}|| {{val|0.9653|0.0048}}|| {{val|0.9667|0.0040}} |- | Hubble's constant (km Mpc−1 s−1) || <math>H_0</math> || {{val|67.31|0.96}} || {{val|67.81|0.92}} || {{val|67.90|0.55}} || {{val|67.27|0.66}} || {{val|67.51|0.64}}|| {{val|67.74|0.46}} |- | Dark energy density || <math>\Omega_\Lambda</math> || {{val|0.685|0.013}} || {{val|0.692|0.012}} || {{val|0.6935|0.0072}} || {{val|0.6844|0.0091 }} || {{val|0.6879|0.0087}} || {{val|0.6911|0.0062}} |- | Matter density || <math>\Omega_m</math> || {{val|0.315|0.013}} || {{val|0.308|0.012}} || {{val|0.3065|0.0072}} || {{val|0.3156|0.0091 }} || {{val|0.3121|0.0087}} || {{val|0.3089|0.0062}} |- | Density fluctuations at 8h−1 Mpc || <math>\sigma_8</math> || {{val|0.829|0.014}} || {{val|0.8149|0.0093}} || {{val|0.8154|0.0090}} || {{val|0.831|0.013}} || {{val|0.8150|0.0087}}|| {{val|0.8159|0.0086}} |- | Redshift of reionization || <math>z_{re}</math> || {{val|9.9|+1.8|-1.6}} ||{{val|8.8|+1.7|-1.4}} ||{{val|8.9|+1.3|-1.2}} ||{{val|10.0|+1.7|-1.5}} ||{{val|8.5|+1.4|-1.2}} ||{{val|8.8|+1.2|-1.1}} |- | Age of the Universe (Gy) || <math>t_0</math> || {{val|13.813|0.038}} || {{val|13.799|0.038}} || {{val|13.796|0.029}} || {{val|13.813|0.026}} || {{val|13.807|0.026}} || {{val|13.799|0.021}} |- | Redshift at decoupling || <math>z_*</math> || {{val|1090.09|0.42}} || {{val|1089.94|0.42}} || {{val|1089.90|0.30}} || {{val|1090.06|0.30}} || {{val|1090.00|0.29}} || {{val|1089.90|0.23}} |- | Comoving size of the sound horizon at z = z* || <math>r_*</math> || {{val|144.61|0.49}} || {{val|144.89|0.44}} || {{val|144.93|0.30}} || {{val|144.57|0.32}} || {{val|144.71|0.31}} || {{val|144.81|0.24}} |- | 100× angular scale of sound horizon at last-scattering || <math>100\,\theta_*</math> || {{val|1.04105|0.00046}} || {{val|1.04122|0.00045}} || {{val|1.04126|0.00041}} || {{val|1.04096|0.00032}} || {{val|1.04106|0.00031}}|| {{val|1.04112|0.00029}} |- | Redshift with baryon-drag optical depth = 1 || <math>z_{drag}</math> || {{val|1059.57|0.46}} || {{val|1059.57|0.47}} || {{val|1059.60|0.44}} || {{val|1059.65|0.31}} || {{val|1059.62|0.31}} || {{val|1059.68|0.29}} |- | Comoving size of the sound horizon at z = zdrag || <math>r_{drag}</math> || {{val|147.33|0.49}} || {{val|147.60|0.43}} || {{val|147.63|0.32}} || {{val|147.27|0.31}} || {{val|147.41|0.30}} || {{val|147.50|0.24}} |- | '''''Legend''''' || colspan="7" align="left" | *'''68% limits''': Parameter 68% confidence limits for the base ΛCDM model *'''TT, TE, EE''': ''Planck'' Cosmic microwave background (CMB) power spectra; here TT represents temperature power spectrum, TE is temperature-polarization cross spectrum, and EE is polarisation power spectrum. *'''lowP''': ''Planck'' polarization data in the low-ℓ likelihood *'''lensing''': CMB lensing reconstruction *'''ext''': External data (BAO+JLA+H0). BAO: Baryon acoustic oscillations, JLA: Joint Light-curve Analysis (of supernovae), H0: Hubble constant |} </div>

=== 2018 final data release === {{expand section|date=January 2019}} <div class="center"> {| border="1" cellpadding="1" cellspacing="0" style="margin: 1em 1em 1em 0; background: #f9f9f9; border: 1px #aaa solid; border-collapse: collapse; font-size: 80%; text-align: center;" |- bgcolor="#B0C4DE" align="center" |+ Cosmological parameters from 2018 ''Planck'' results<ref name="Planck 2018">{{Cite journal|author=Planck Collaboration|year=2020|title=Planck 2018 results. VI. Cosmological parameters (See PDF, page 15, Table 2).|journal=Astronomy & Astrophysics|volume=641|pages=A6|doi=10.1051/0004-6361/201833910|arxiv=1807.06209|bibcode=2020A&A...641A...6P |s2cid=119335614}}</ref><ref>{{Cite web |date=17 July 2018 |title=From an almost perfect Universe to the best of both worlds |url=https://sci.esa.int/web/planck/-/60499-from-an-almost-perfect-universe-to-the-best-of-both-worlds |access-date=2022-06-16 |website=ESA Science & Technology}}</ref> ! Parameter !! Symbol !! TT+lowE 68% limits !! TE+lowE 68% limits !! EE+lowE 68% limits !! TT,TE,EE+lowE 68% limits !! TT,TE,EE+lowE +lensing 68% limits !! TT,TE,EE+lowE +lensing+BAO 68% limits |- | Baryon density || <math>\Omega_b h^2</math> || 0.02212±0.00022 || 0.02249±0.00025|| 0.0240±0.0012 || 0.02236±0.00015 || 0.02237±0.00015 || 0.02242±0.00014 |- | Cold dark matter density || <math>\Omega_c h^2</math> ||0.1206±0.0021|| 0.1177±0.0020 ||0.1158±0.0046|| 0.1202±0.0014|| 0.1200±0.0012 ||0.11933±0.00091 |- | 100x approximation to rs / DA (CosmoMC) || <math>100\,\theta_{MC}</math> ||1.04077±0.00047 | 1.04139±0.00049 || 1.03999±0.00089 || 1.04090±0.00031 || 1.04092±0.00031 ||1.04101±0.00029 |- | Thomson scattering optical depth due to reionization || <math>\tau</math> ||0.0522±0.0080|| 0.0496��0.0085|| 0.0527±0.0090 || {{val|0.0544|+0.0070|−0.0081 }} || 0.0544±0.0073 || 0.0561±0.0071 |- | Power spectrum of curvature perturbations || <math>\ln(10^{10} A_s)</math> || 3.040±0.016 ||{{val|3.018|+0.020|−0.018}} | 3.052±0.022 || 3.045±0.016 || 3.044±0.014 || 3.047±0.014 |- | Scalar spectral index || <math>n_s</math> || 0.9626±0.0057 || 0.967±0.011 || 0.980±0.015 || 0.9649±0.0044 || 0.9649±0.0042 || 0.9665±0.0038 |- | Hubble's constant (km s−1 Mpc−1) ||<math>H_0</math> || 66.88±0.92 || 68.44±0.91 || 69.9±2.7 || 67.27±0.60 || 67.36±0.54 || 67.66±0.42 |- | Dark energy density || <math>\Omega_\Lambda</math> || 0.679±0.013 || 0.699±0.012 ||{{val|0.711|+0.033|−0.026}}|| 0.6834±0.0084 || 0.6847±0.0073 || 0.6889±0.0056 |- | Matter density || <math>\Omega_m</math> || 0.321±0.013 || 0.301±0.012 ||{{val|0.289|+0.026|−0.033}} | 0.3166±0.0084 || 0.3153±0.0073 || 0.3111±0.0056 |- | Density fluctuations at 8h−1 Mpc || S8 = <math>\sigma_8</math>(<math>\Omega_m</math>/0.3)0.5|| 0.840±0.024 || 0.794±0.024 ||{{val|0.781|+0.052|−0.060}}|| 0.834±0.016 || 0.832±0.013 || 0.825±0.011 |- | Redshift of reionization || <math>z_{re}</math> || 7.50±0.82 ||{{val|7.11|+0.91|−0.75}} |{{val|7.10|+0.87|−0.73}} | 7.68±0.79|| 7.67±0.73||7.82±0.71 |- | Age of the Universe (Gy) || <math>t_0</math> ||13.830±0.037 || 13.761±0.038 ||{{val|13.64|+0.16|−0.14}}||13.800±0.024 || 13.797±0.023 || 13.787±0.020 |- | Redshift at decoupling || <math>z_*</math> || 1090.30±0.41 || 1089.57±0.42 ||{{val|1087.8|+1.6|−1.7}} | 1089.95±0.27 || 1089.92±0.25 || 1089.80±0.21 |- | Comoving size of the sound horizon at z = z*(Mpc) |<math>r_*</math> ||144.46±0.48|| 144.95±0.48|| 144.29±0.64 ||144.39±0.30 ||144.43±0.26|| 144.57±0.22 |- | 100× angular scale of sound horizon at last-scattering || <math>100\,\theta_*</math> || 1.04097±0.00046 || 1.04156±0.00049 || 1.04001±0.00086 || 1.04109±0.00030 || 1.04110±0.00031 || 1.04119±0.00029 |- | Redshift with baryon-drag optical depth = 1 || <math>z_{drag}</math> || 1059.39±0.46 || 1060.03±0.54 || 1063.2±2.4 || 1059.93±0.30 || 1059.94±0.30 || 1060.01±0.29 |- | Comoving size of the sound horizon at z = zdrag || <math>r_{drag}</math> || 147.21±0.48 || 147.59±0.49 || 146.46±0.70 || 147.05±0.30 || 147.09±0.26 || 147.21±0.23 |- | '''''Legend''''' || colspan="7" align="left" | *'''68% limits''': Parameter 68% confidence limits for the base ΛCDM model *'''TT, TE, EE''': ''Planck'' Cosmic microwave background (CMB) power spectra; here TT represents temperature power spectrum, TE is temperature-polarization cross spectrum, and EE is polarisation power spectrum. *'''lowP''': ''Planck'' polarization data in the low-ℓ likelihood *'''lensing''': CMB lensing reconstruction *'''ext''': External data (BAO+JLA+H0). BAO: Baryon acoustic oscillations, JLA: Joint Light-curve Analysis (of supernovae), H0: Hubble constant |} </div>

== See also == {{Portal|Physics|Spaceflight}} * DustPedia * Lambda-CDM model * List of cosmological computation software * Observational cosmology * Physical cosmology *Terahertz radiation

== References == {{Reflist|33em}}

== Further reading == * {{cite journal |last=Dambeck |first=Thorsten |date=May 2009 |title=Planck Readies to Dissect the Big Bang |journal=Sky & Telescope |volume=117 |issue=5 |pages=24–28 |bibcode=2009S&T...117e..24D |oclc=318973848}}

== External links == {{Commons category|Planck (spacecraft)}} * ESA ** [http://www.esa.int/planck ''Planck'' mission website] ** [http://sci.esa.int/planck/ ''Planck'' science website] ** [http://www.esa.int/Our_Activities/Operations/Planck ''Planck'' operations website] ** [http://www.cosmos.esa.int/web/planck ''Planck'' science results website] * NASA ** [http://www.nasa.gov/planck/ ''Planck'' mission website] ** [http://irsa.ipac.caltech.edu/Missions/planck.html NASA/IPAC ''Planck'' archive]

{{CMB experiments}} {{Space observatories}} {{European Space Agency}} {{Orbital launches in 2009}} {{Authority control}}

Category:European Space Agency space probes Category:Cosmic microwave background experiments Category:Space telescopes Category:Infrared telescopes Category:Submillimetre telescopes Category:Derelict satellites in heliocentric orbit Category:Spacecraft using Lissajous orbits Category:Space probes launched in 2009 Category:2013 disestablishments Category:Max Planck