 A model ofPlanck | |||||||
| Names | COBRAS/SAMBA | ||||||
|---|---|---|---|---|---|---|---|
| Mission type | Space telescope | ||||||
| Operator | ESA | ||||||
| COSPAR ID | 2009-026B | ||||||
| SATCATno. | 34938 | ||||||
| Website | www | ||||||
| Mission duration | Planned: >15 months Final: 4 years, 5 months, 8 days | ||||||
| Spacecraft properties | |||||||
| Manufacturer | Thales Alenia Space | ||||||
| Launch mass | 1,950 kg (4,300 lb)[1] | ||||||
| Payload mass | 205 kg (452 lb) | ||||||
| Dimensions | Body: 4.20 m × 4.22 m (13.8 ft × 13.8 ft) | ||||||
| Start of mission | |||||||
| Launch date | 14 May 2009, 13:12:02 UTC (2009-05-14UTC13:12:02) | ||||||
| Rocket | Ariane 5 ECA | ||||||
| Launch site | Guiana Space Centre, French Guiana | ||||||
| Contractor | Arianespace | ||||||
| Entered service | 3 July 2009 | ||||||
| End of mission | |||||||
| Disposal | Decommissioned | ||||||
| Deactivated | 23 October 2013, 12:10:27 UTC (2013-10-23UTC12:10:28) | ||||||
| Orbital parameters | |||||||
| Reference system | Sun-Earth L2 orbit (1,500,000 km / 930,000 mi) | ||||||
| Regime | Lissajous | ||||||
| Main telescope | |||||||
| Type | Gregorian | ||||||
| Diameter | 1.9 m × 1.5 m (6.2 ft × 4.9 ft) | ||||||
| Wavelengths | 300 μm – 11.1 mm (frequencies between 27 GHz and 1 THz) | ||||||
| |||||||
 ESA astrophysics insignia forPlanck | |||||||
Planck was a space observatory operated by the European Space Agency (ESA) from 2009 to 2013. The project aimed to map theanisotropies of thecosmic 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 NASAWilkinson 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 physicistMax Planck (1858–1947), who is widely regarded as the originator of quantum theory by deriving the formula forblack-body radiation.
Built at theCannes Mandelieu Space Center byThales Alenia Space, Planck was created as a medium-sized mission forESA'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 includedpolarization 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 aheliocentricgraveyard orbit andpassivated 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 anddark matter in the Universe, and other important characteristics of the cosmos.
The mission had a wide variety of scientific aims, including:[2]
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 ninefrequency bands rather than WMAP's five, with the goal of improving the astrophysical foreground models.
It is expected that mostPlanck 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 thepolarization measurements.[needs update] The dominant foreground radiation depends on frequency, but could include synchrotron radiation from the Milky Way at low frequencies, and dust at high frequencies.[needs update]
The spacecraft carries two instruments: the Low Frequency Instrument (LFI) and the High Frequency Instrument (HFI).[2] Both instruments can detect both the total intensity andpolarization 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 −273.05 °C (−459.49 °F), or 0.1 °C aboveabsolute zero.[3] From August 2009,Planck was the coldest known object in space, until its active coolant supply was exhausted in January 2012.[4]
NASA played a role in the development of this mission and contributes to the analysis of scientific data. ItsJet Propulsion Laboratory built components of the science instruments, includingbolometers for the high-frequency instrument, a 20-kelvincryocooler for both the low- and high-frequency instruments, and amplifier technology for the low-frequency instrument.[5]
| Frequency (GHz) | Bandwidth (Δν/ν) | Resolution (arcmin) | Sensitivity (total intensity) ΔT/T, 14-month observation (10−6) | Sensitivity (polarization) ΔT/T, 14-month observation (10−6) |
|---|---|---|---|---|
| 30 | 0.2 | 33 | 2.0 | 2.8 |
| 44 | 0.2 | 24 | 2.7 | 3.9 |
| 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 usehigh-electron-mobility transistors.[2]
| Frequency (GHz) | Bandwidth (Δν/ν) | Resolution (arcmin) | Sensitivity (total intensity) ΔT/T, 14-month observation (10−6) | Sensitivity (polarization) ΔT/T, 14-month observation (10−6) |
|---|---|---|---|---|
| 100 | 0.33 | 10 | 2.5 | 4.0 |
| 143 | 0.33 | 7.1 | 2.2 | 4.2 |
| 217 | 0.33 | 5.0 | 4.8 | 9.8 |
| 353 | 0.33 | 5.0 | 14.7 | 29.8 |
| 545 | 0.33 | 5.0 | 147 | N/A |
| 857 | 0.33 | 5.0 | 6700 | N/A |
The HFI was sensitive between 100 and 857 GHz, using 52bolometric detectors, manufactured by JPL/Caltech,[6] optically coupled to the telescope through cold optics, manufactured by Cardiff University's School of Physics and Astronomy,[7] consisting of a triple horn configuration and optical filters, a similar concept to that used in theArcheops 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.[2]
On 13 January 2012, it was reported that the on-board supply ofhelium-3 used inPlanck'sdilution refrigerator had been exhausted, and that the HFI would become unusable within a few days.[8] By this date,Planck had completed five full scans of the CMB, exceeding its target of two. The LFI (cooled byhelium-4) was expected to remain operational for another six to nine months.[8]
A commonservice module (SVM) was designed and built by Thales Alenia Space in itsTurin plant, for both theHerschel Space Observatory andPlanck missions, combined into one single program.[2]
The overall cost is estimated to be€700 million for thePlanck[9] and€1,100 million for theHerschel mission.[10] Both figures include their mission's spacecraft and payload, (shared) launch and mission expenses, and science operations.
Structurally, theHerschel andPlanck 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 theavionics, 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.
On each spacecraft, the power subsystem consists of asolar array, employing triple-junctionsolar cells, abattery 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.
ForPlanck, the circular solar array is fixed on the bottom of the satellite, always facing the Sun as the satellite rotates on its vertical axis.
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 theHerschel andPlanck payloads.
ThePlanck satelliterotates at one revolution per minute, with an aim of an absolute pointing error less than 37 arc-minutes. AsPlanck 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 bothHerschel andPlanck is thestar tracker.
The satellite was successfully launched, along with theHerschel Space Observatory, at 13:12:02 UTC on 14 May 2009 aboard anAriane 5 ECA heavy launch vehicle from theGuiana Space Centre. The launch placed the craft into a very elliptical orbit (perigee: 270 km [170 mi],apogee: more than 1,120,000 km [700,000 mi]), bringing it near theL2 Lagrangian point of theEarth-Sun system, 1,500,000 kilometres (930,000 mi) from the Earth.
The manoeuvre to injectPlanck into its final orbit aroundL2 was successfully completed on 3 July 2009, when it entered aLissajous orbit with a 400,000 km (250,000 mi) radius around theL2 Lagrangian point.[11] The temperature of the High Frequency Instrument reached just a tenth of a degree above absolute zero (0.1K) on 3 July 2009, placing both the Low Frequency and High Frequency Instruments within their cryogenic operational parameters, makingPlanck fully operational.[12]
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 itsL2 point, placing it into aheliocentric 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.[13] The final deactivation command, which switched off the spacecraft's transmitter, was sent toPlanck on 23 October 2013 at 12:10:27 UTC.[14]
Planck started its First All-Sky Survey on 13 August 2009.[16] In September 2009, theEuropean Space Agency announced the preliminary results from thePlanck 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.[17]
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.[11]
Some planned pointing list data from 2009 has been released publicly, along with a video visualization of the surveyed sky.[16]
On 17 March 2010, the firstPlanck photos were published, showing dust concentration within 500 light years from the Sun.[18][19]
On 5 July 2010, thePlanck mission delivered its first all-sky image.[20]
The first public scientific result ofPlanck is the Early-Release Compact-Source Catalogue, released during the January 2011Planck conference in Paris.[21][22]
On 5 May 2014 a map of the galaxy's magnetic field created usingPlanck was published.[23]
The Planck team andprincipal investigatorsNazzareno Mandolesi andJean-Loup Puget shared the 2018Gruber Prize in Cosmology.[24] Puget was also awarded the 2018Shaw Prize in Astronomy.[25]
On 21 March 2013, the European-led research team behind thePlanck cosmology probe released the mission's all-sky map of the cosmic microwave background.[26][27] 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 vastcosmic web ofgalactic clusters anddark 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",[28] more commonly known as theAxis of evil (cosmology). According to the team, the Universe is13.798±0.037 billion-years-old, and contains4.82%±0.05% ordinary matter,26.8%±0.4% dark matter and69%±1%dark energy.[29][30][31] TheHubble constant was also measured to be67.80±0.77 (km/s)/Mpc.[26][29][32][33][34]
| 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 | 0.022068 | 0.02207±0.00033 | 0.022242 | 0.02217±0.00033 | 0.022032 | 0.02205±0.00028 | 0.022069 | 0.02207±0.00027 | 0.022199 | 0.02218±0.00026 | 0.022161 | 0.02214±0.00024 | |
| Colddark matter density | 0.12029 | 0.1196±0.0031 | 0.11805 | 0.1186±0.0031 | 0.12038 | 0.1199±0.0027 | 0.12025 | 0.1198±0.0026 | 0.11847 | 0.1186±0.0022 | 0.11889 | 0.1187±0.0017 | |
| 100x approximation to rs / DA (CosmoMC) | 1.04122 | 1.04132±0.00068 | 1.04150 | 1.04141±0.00067 | 1.04119 | 1.04131±0.00063 | 1.04130 | 1.04132±0.00063 | 1.04146 | 1.04144±0.00061 | 1.04148 | 1.04147±0.00056 | |
| Thomson scatteringoptical depth due toreionization | 0.0925 | 0.097±0.038 | 0.0949 | 0.089±0.032 | 0.0925 | 0.089+0.012 −0.014 | 0.0927 | 0.091+0.013 −0.014 | 0.0943 | 0.090+0.013 −0.014 | 0.0952 | 0.092±0.013 | |
| Power spectrum of curvature perturbations | 3.098 | 3.103±0.072 | 3.098 | 3.085±0.057 | 3.0980 | 3.089+0.024 −0.027 | 3.0959 | 3.090±0.025 | 3.0947 | 3.087±0.024 | 3.0973 | 3.091±0.025 | |
| Scalar spectral index | 0.9624 | 0.9616±0.0094 | 0.9675 | 0.9635±0.0094 | 0.9619 | 0.9603±0.0073 | 0.9582 | 0.9585±0.0070 | 0.9624 | 0.9614±0.0063 | 0.9611 | 0.9608±0.0054 | |
| Hubble's constant (km Mpc−1 s−1) | 67.11 | 67.4±1.4 | 68.14 | 67.9±1.5 | 67.04 | 67.3±1.2 | 67.15 | 67.3±1.2 | 67.94 | 67.9±1.0 | 67.77 | 67.80±0.77 | |
| Dark energy density | 0.6825 | 0.686±0.020 | 0.6964 | 0.693±0.019 | 0.6817 | 0.685+0.018 −0.016 | 0.6830 | 0.685+0.017 −0.016 | 0.6939 | 0.693±0.013 | 0.6914 | 0.692±0.010 | |
| Density fluctuations at 8h−1 Mpc | 0.8344 | 0.834±0.027 | 0.8285 | 0.823±0.018 | 0.8347 | 0.829±0.012 | 0.8322 | 0.828±0.012 | 0.8271 | 0.8233±0.0097 | 0.8288 | 0.826±0.012 | |
| Redshift ofreionization | 11.35 | 11.4+4.0 −2.8 | 11.45 | 10.8+3.1 −2.5 | 11.37 | 11.1±1.1 | 11.38 | 11.1±1.1 | 11.42 | 11.1±1.1 | 11.52 | 11.3±1.1 | |
| Age of the Universe (Gy) | 13.819 | 13.813±0.058 | 13.784 | 13.796±0.058 | 13.8242 | 13.817±0.048 | 13.8170 | 13.813±0.047 | 13.7914 | 13.794±0.044 | 13.7965 | 13.798±0.037 | |
| 100× angular scale of sound horizon at last-scattering | 1.04139 | 1.04148±0.00066 | 1.04164 | 1.04156±0.00066 | 1.04136 | 1.04147±0.00062 | 1.04146 | 1.04148±0.00062 | 1.04161 | 1.04159±0.00060 | 1.04163 | 1.04162±0.00056 | |
| Comoving size of the sound horizon at z = zdrag | 147.34 | 147.53±0.64 | 147.74 | 147.70±0.63 | 147.36 | 147.49±0.59 | 147.35 | 147.47±0.59 | 147.68 | 147.67±0.50 | 147.611 | 147.68±0.45 |
Results from an analysis ofPlanck's full mission were made public on 1 December 2014 at a conference inFerrara, Italy.[35] A full set of papers detailing the mission results were released in February 2015.[36] Some of the results include:
Project scientists worked too withBICEP2 scientists to release joint research in 2015 answering whether a signal detected by BICEP2 was evidence of primordialgravitational waves, or was simplebackground noise from dust in the Milky Way galaxy.[35] Their results suggest the latter.[37]
| 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 | 0.02222±0.00023 | 0.02226±0.00023 | 0.02227±0.00020 | 0.02225±0.00016 | 0.02226±0.00016 | 0.02230±0.00014 | |
| Colddark matter density | 0.1197±0.0022 | 0.1186±0.0020 | 0.1184±0.0012 | 0.1198±0.0015 | 0.1193±0.0014 | 0.1188±0.0010 | |
| 100x approximation to rs / DA (CosmoMC) | 1.04085±0.00047 | 1.04103±0.00046 | 1.04106±0.00041 | 1.04077±0.00032 | 1.04087±0.00032 | 1.04093±0.00030 | |
| Thomson scatteringoptical depth due toreionization | 0.078±0.019 | 0.066±0.016 | 0.067±0.013 | 0.079±0.017 | 0.063±0.014 | 0.066±0.012 | |
| Power spectrum of curvature perturbations | 3.089±0.036 | 3.062±0.029 | 3.064±0.024 | 3.094±0.034 | 3.059±0.025 | 3.064±0.023 | |
| Scalar spectral index | 0.9655±0.0062 | 0.9677±0.0060 | 0.9681±0.0044 | 0.9645±0.0049 | 0.9653±0.0048 | 0.9667±0.0040 | |
| Hubble's constant (km Mpc−1 s−1) | 67.31±0.96 | 67.81±0.92 | 67.90±0.55 | 67.27±0.66 | 67.51±0.64 | 67.74±0.46 | |
| Dark energy density | 0.685±0.013 | 0.692±0.012 | 0.6935±0.0072 | 0.6844±0.0091 | 0.6879±0.0087 | 0.6911±0.0062 | |
| Matter density | 0.315±0.013 | 0.308±0.012 | 0.3065±0.0072 | 0.3156±0.0091 | 0.3121±0.0087 | 0.3089±0.0062 | |
| Density fluctuations at 8h−1 Mpc | 0.829±0.014 | 0.8149±0.0093 | 0.8154±0.0090 | 0.831±0.013 | 0.8150±0.0087 | 0.8159±0.0086 | |
| Redshift ofreionization | 9.9+1.8 −1.6 | 8.8+1.7 −1.4 | 8.9+1.3 −1.2 | 10.0+1.7 −1.5 | 8.5+1.4 −1.2 | 8.8+1.2 −1.1 | |
| Age of the Universe (Gy) | 13.813±0.038 | 13.799±0.038 | 13.796±0.029 | 13.813±0.026 | 13.807±0.026 | 13.799±0.021 | |
| Redshift atdecoupling | 1090.09±0.42 | 1089.94±0.42 | 1089.90±0.30 | 1090.06±0.30 | 1090.00±0.29 | 1089.90±0.23 | |
| Comoving size of the sound horizon at z = z* | 144.61±0.49 | 144.89±0.44 | 144.93±0.30 | 144.57±0.32 | 144.71±0.31 | 144.81±0.24 | |
| 100× angular scale of sound horizon at last-scattering | 1.04105±0.00046 | 1.04122±0.00045 | 1.04126±0.00041 | 1.04096±0.00032 | 1.04106±0.00031 | 1.04112±0.00029 | |
| Redshift with baryon-drag optical depth = 1 | 1059.57±0.46 | 1059.57±0.47 | 1059.60±0.44 | 1059.65±0.31 | 1059.62±0.31 | 1059.68±0.29 | |
| Comoving size of the sound horizon at z = zdrag | 147.33±0.49 | 147.60±0.43 | 147.63±0.32 | 147.27±0.31 | 147.41±0.30 | 147.50±0.24 | |
| Legend |
| ||||||
![[icon]](/mt/?noimg=&dark=on&url=http%3a%2f%2fen.wikipedia.org%2fwiki%2fFile%3aWiki_letter_w_cropped.svg) | This sectionneeds expansion. You can help byadding to it.(January 2019) |
| 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 | 0.02212±0.00022 | 0.02249±0.00025 | 0.0240±0.0012 | 0.02236±0.00015 | 0.02237±0.00015 | 0.02242±0.00014 | |
| Colddark matter density | 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) | 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 scatteringoptical depth due toreionization | 0.0522±0.0080 | 0.0496±0.0085 | 0.0527±0.0090 | 0.0544+0.0070 −0.0081 | 0.0544±0.0073 | 0.0561±0.0071 | |
| Power spectrum of curvature perturbations | 3.040±0.016 | 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 | 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) | 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 | 0.679±0.013 | 0.699±0.012 | 0.711+0.033 −0.026 | 0.6834±0.0084 | 0.6847±0.0073 | 0.6889±0.0056 | |
| Matter density | 0.321±0.013 | 0.301±0.012 | 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 =(/0.3)0.5 | 0.840±0.024 | 0.794±0.024 | 0.781+0.052 −0.060 | 0.834±0.016 | 0.832±0.013 | 0.825±0.011 |
| Redshift ofreionization | 7.50±0.82 | 7.11+0.91 −0.75 | 7.10+0.87 −0.73 | 7.68±0.79 | 7.67±0.73 | 7.82±0.71 | |
| Age of the Universe (Gy) | 13.830±0.037 | 13.761±0.038 | 13.64+0.16 −0.14 | 13.800±0.024 | 13.797±0.023 | 13.787±0.020 | |
| Redshift atdecoupling | 1090.30±0.41 | 1089.57±0.42 | 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) | 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 | 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 | 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 | 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 |
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