Cosmic Background Explorer

Artist's concept of the COBE spacecraft

Names| Explorer 66
COBE
Mission type| Cosmic microwave background Astronomy
Operator| NASA
COSPAR ID| 1989-089A
SATCAT no.| 20322
Website| lambda.gsfc.nasa.gov/product/cobe
Mission duration| 6 months (planned)
4 years, 1 month and 4 days (achieved)
Spacecraft properties
Spacecraft| Explorer LXVI
Spacecraft type| Cosmic Background Explorer
Bus| COBE
Manufacturer| Goddard Space Flight Center
Launch mass| 2,206 kg (4,863 lb) [1]
Dry mass| 1,408 kg (3,104 lb) [2]
Dimensions| 5.49 × 2.44 m (18.0 × 8.0 ft)
Power| 750 watts
Start of mission
Launch date| 18 November 1989, 14:34 UTC
Rocket| Delta 5920-8 (Delta 189)
Launch site| Vandenberg, SLC-2W
Contractor| Douglas Aircraft Company
Entered service| 18 November 1989
End of mission
Deactivated| 23 December 1993
Orbital parameters
Reference system| Geocentric orbit[3]
Regime| Sun-synchronous orbit
Perigee altitude| 900 km (560 mi)
Apogee altitude| 900 km (560 mi)
Inclination| 99.00°
Period| 103.00 minutes
Instruments
Differential Microwave Radiometer (DMR)
Diffuse Infrared Background Experiment (DIRBE)
Far-InfraRed Absolute Spectrophotometer (FIRAS)

Cosmic Background Explorer mission patch

Explorer program

<- AMPTE-CCE (Explorer 65)

Extreme Ultraviolet Explorer (Explorer 67) ->

The Cosmic Background Explorer (COBE /ˈkoʊbi/ KOH-bee), also referred to as Explorer 66, was a NASA satellite dedicated to cosmology, which operated from 1989 to 1993. Its goals were to investigate the cosmic microwave background radiation (CMB or CMBR) of the universe and provide measurements that would help shape the understanding of the cosmos.

COBE's measurements provided two key pieces of evidence that supported the Big Bang theory of the universe: that the CMB has a near-perfect black-body spectrum, and that it has very faint anisotropies. Two of COBE's principal investigators, George F. Smoot III and John C. Mather, received the Nobel Prize in Physics in 2006 for their work on the project. According to the Nobel Prize committee, "the COBE project can also be regarded as the starting point for cosmology as a precision science".[4]

COBE was the second cosmic microwave background satellite, following RELIKT-1, and was followed by two more advanced spacecraft: the Wilkinson Microwave Anisotropy Probe (WMAP) operated from 2001 to 2010 and the Planck spacecraft from 2009 to 2013.

## Contents

* 1 Mission
* 2 History
* 3 Spacecraft
* 3.1 Instruments
* 3.1.1 Differential Microwave Radiometers (DMR)
* 3.1.2 Diffuse Infrared Background Experiment (DIRBE)
* 3.1.3 Far Infrared Absolute Spectrophotometer (FIRAS)
* 4 Scientific findings
* 4.1 Black-body curve of CMB
* 4.2 Intrinsic anisotropy of CMB
* 4.3 Detecting early galaxies
* 4.4 DIRBE
* 4.5 Cosmological implications
* 5 Popular culture
* 6 See also
* 7 References
* 8 Sources
* 9 Further reading
* 10 External links

## Mission

The purpose of the Cosmic Background Explorer (COBE) mission was to take precise measurements of the diffuse radiation between 1 micrometre and 1 cm (0.39 in) over the whole celestial sphere. The following quantities were measured: (1) the spectrum of the 3 K radiation over the range 100 micrometres to 1 cm (0.39 in) (2) the anisotropy of this radiation from 3 to 10 mm (0.39 in); and, (3) the spectrum and angular distribution of diffuse infrared background radiation at wavelengths from 1 to 300 micrometres.[5]

## History

In 1974, NASA issued an Announcement of Opportunity for astronomical missions that would use a small- or medium-sized Explorer spacecraft. Out of the 121 proposals received, three dealt with studying the cosmological background radiation. Though these proposals lost out to the Infrared Astronomical Satellite (IRAS), their strength made NASA further explore the idea. In 1976, NASA formed a committee of members from each of 1974's three proposal teams to put together their ideas for such a satellite. A year later, this committee suggested a polar-orbiting satellite called COBE to be launched by either a Delta 5920-8 launch vehicle or the Space Shuttle. It would contain the following instruments:[6]

Instruments  Instrument  | Acronym  | Description  | Principal Investigator

|
|
|

Differential Microwave Radiometer  | DMR  | Microwave instrument that would map variations (or anisotropies) in the Cosmic microwave background (CMB) radiation  | George F. Smoot III
Diffuse Infrared Background Experiment | DIRBE  | Multiwavelength infrared detector used to map dust emission  | Michael G. Hauser
Far-InfraRed Absolute Spectrophotometer  | FIRAS  | Spectrophotometer used to measure the spectrum of the CMB  | John C. Mather
Launch of the COBE spacecraft on 18 November 1989.

NASA accepted the proposal provided that the costs be kept under US$30 million, excluding launcher and data analysis. Due to cost overruns in the Explorer program due to IRAS, work on constructing the satellite at Goddard Space Flight Center (GSFC) did not begin until 1981. To save costs, the infrared detectors and liquid helium dewar on COBE would be similar to those used on Infrared Astronomical Satellite (IRAS).

COBE was originally planned to be launched on a Space Shuttle mission STS-82-B in 1988 from Vandenberg Air Force Base, but the Challenger explosion delayed this plan when the Shuttles were grounded. NASA prevented COBE's engineers from going to other space companies to launch COBE, and eventually a redesigned COBE was placed into Sun-synchronous orbit on 18 November 1989 aboard a Delta launch vehicle.

On 23 April 1992, COBE scientists announced at the APS April Meeting in Washington, D.C. the finding of the "primordial seeds" (CMBE anisotropy) in data from the DMR instrument; until then the other instruments were "unable to see the template."[7] The following day The New York Times ran the story on the front page, explaining the finding as "the first evidence revealing how an initially smooth cosmos evolved into today's panorama of stars, galaxies and gigantic clusters of galaxies."[8]

The Nobel Prize in Physics for 2006 was jointly awarded to John C. Mather, NASA Goddard Space Flight Center, and George F. Smoot III, University of California, Berkeley, "for their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation".[4]

## Spacecraft

Part of a series on

Physical cosmology

* Big Bang · Universe
* Age of the universe
* Chronology of the universe

Early universe

* Planck epoch
* Grand unification epoch
* Electroweak epoch
* Quark epoch
* Hadron epoch
* Lepton epoch
* Photon epoch
* Big Bang nucleosynthesis
* Inflation
* Dark Ages

Backgrounds

* Cosmic background radiation (CBR)
* Gravitational wave background (GWB)
* Cosmic microwave background (CMB) · Cosmic neutrino background (CNB)
* Cosmic infrared background (INB)

Expansion · Future

* Hubble's law · Redshift
* Expansion of the universe
* Accelerating expansion of the universe
* Comoving and proper distances
* FLRW metric · Friedmann equations
* Inhomogeneous cosmology
* Future of an expanding universe
* Ultimate fate of the universe
* Heat death of the universe
* Big Rip
* Big Crunch
* Big Bounce

Components · Structure

|  Components

* Lambda-CDM model
* Baryonic matter
* Energy
* Radiation
* Dark energy
* Quintessence
* Phantom energy
* Dark matter
* Cold dark matter
* Warm dark matter
* Hot dark matter
* Dark radiation

Structure

* Shape of the universe
* Reionization · Structure formation
* Galaxy formation
* Large-scale structure
* Large quasar group
* Galaxy filament
* Supercluster
* Galaxy cluster
* Galaxy group
* Local Group
* Galaxy
* Dark matter halo
* Star cluster
* Solar system
* Planetary system
* Void

Experiments

* BOOMERanG
* Cosmic Background Explorer (COBE)
* Dark Energy Survey
* Euclid
* Illustris project
* Large Synoptic Survey Telescope
* Planck space observatory
* Sloan Digital Sky Survey (SDSS)
* 2dF Galaxy Redshift Survey ("2dF")
* UniverseMachine
* Wilkinson Microwave Anisotropy
Probe (WMAP)

* Scientists

* Aaronson
* Alfvén
* Alpher
* Bharadwaj
* Copernicus
* de Sitter
* Dicke
* Eddington
* Ehlers
* Einstein
* Ellis
* Friedman
* Galileo
* Gamow
* Guth
* Hubble
* Lemaître
* Linde
* Mather
* Newton
* Penzias
* Rubin
* Schmidt
* Schwarzschild
* Smoot
* Starobinsky
* Steinhardt
* Suntzeff
* Sunyaev
* Tolman
* Wilson
* Zeldovich

Subject history

* Discovery of cosmic microwave
background radiation

* History of the Big Bang theory
* Religious interpretations of
the Big Bang theory

* Timeline of cosmological theories

* Category

* v
* t
* e

Diagram of COBE spacecraft

COBE was an Explorer class satellite, with technology borrowed heavily from IRAS, but with some unique characteristics.

The need to control and measure all the sources of systematic errors required a rigorous and integrated design. COBE would have to operate for a minimum of 6 months and constrain the amount of radio interference from the ground, COBE and other satellites as well as radiative interference from the Earth, Sun and Moon.[9] The instruments required temperature stability and to maintain gain, and a high level of cleanliness to reduce entry of stray light and thermal emission from particulates.

The need to control systematic error in the measurement of the CMB anisotropy and measuring the zodiacal cloud at different elongation angles for subsequent modeling required that the satellite rotate at a 0.8 rpm spin rate.[9] The spin axis is also tilted back from the orbital velocity vector as a precaution against possible deposits of residual atmospheric gas on the optics as well against the infrared glow that would result from fast neutral particles hitting its surfaces at extremely high speed.

In order to meet the twin demands of slow rotation and three-axis attitude control, a sophisticated pair of yaw angular momentum wheels were employed with their axis oriented along the spin axis .[9] These wheels were used to carry an angular momentum opposite that of the entire spacecraft in order to create a zero net angular momentum system.

The orbit would prove to be determined based on the specifics of the spacecraft's mission. The overriding considerations were the need for full sky coverage, the need to eliminate stray radiation from the instruments and the need to maintain thermal stability of the dewar and the instruments.[9] A circular Sun-synchronous orbit satisfied all these requirements. A 900 km (560 mi) altitude orbit with a 99° inclination was chosen as it fit within the capabilities of either a Space Shuttle (with an auxiliary propulsion on COBE) or a Delta launch vehicle. This altitude was a good compromise between Earth's radiation and the charged particles in Earth's radiation belts at higher altitudes. An ascending node at 18:00 was chosen to allow COBE to follow the boundary between sunlight and darkness on Earth throughout the year.

The orbit combined with the spin axis made it possible to keep the Earth and the Sun continually below the plane of the shield, allowing a full sky scan every six months.

The last two important parts pertaining to the COBE mission were the dewar and Sun-Earth shield. The dewar was a 650 L (140 imp gal; 170 US gal) superfluid helium cryostat designed to keep the FIRAS and DIRBE instruments cooled during the duration of the mission. It was based on the same design as one used on IRAS and was able to vent helium along the spin axis near the communication arrays. The conical Sun-Earth shield protected the instruments from direct solar and Earth-based radiation as well as radio interference from Earth and the COBE's transmitting antenna. Its multilayer insulating blankets provided thermal isolation for the dewar.[9]

In January 1994, engineering operations concluded and the operation of the spacecraft was transferred to Wallops Flight Facility (WFF) for use as a test satellite.[5]

### Instruments

#### Differential Microwave Radiometers (DMR)

The Differential Microwave Radiometer (DMR) investigation uses three differential radiometers to map the sky at 31.4, 53, and 90 GHz. The radiometers are distributed around the outer surface of the cryostat. Each radiometer employs a pair of horn antennas viewing at 30° from the spin axis of the spacecraft, measuring the differential temperature between points in the sky separated by 60°. At each frequency, there are two channels for dual-polarization measurements for improved sensitivity and for reliability. Each radiometer is a microwave receiver whose input is switched rapidly between the two horn antennas, obtaining the difference in brightness of two fields of view 7° in diameter located 60° apart and 30° from the axis of the spacecraft. High sensitivity is achieved by temperature stabilization (at 300 K for 31.4 GHz and at 140 K for 53 and 90 GHz), by spacecraft spin, and by the ability to integrate over the entire year. Sensitivity to large-scale anisotropies is about 3E-5 K. The instrument weighs 120 kg (260 lb), uses 114 watts, and has a data rate of 500 bit/s.[10]

#### Diffuse Infrared Background Experiment (DIRBE)

The Diffuse Infrared Background Experiment (DIRBE) consists of a cryogenically cooled (to 2 K) multiband radiometer used to investigate diffuse infrared radiation from 1 to 300 micrometres. The instrument measures the absolute flux in 10 wavelength bands with a 1° field of view pointed 30° off the spin axis. Detectors (photoconductors) and filters for the 8 to 100 micrometre channels are the same as for the IRAS mission. Bolometers are used for the longest wavelength channel (120 to 300 micrometres). The telescope is a well baffled, off-axis, Gregorian flux collector with re-imaging. The instrument weighs approximately 34 kg (75 lb), uses 100 W and has a data rate of 1700 bit/s.[11]

#### Far Infrared Absolute Spectrophotometer (FIRAS)

The Far Infrared Absolute Spectrophotometer (FIRAS) is a cryogenically cooled polarizing Michelson interferometer used as a Fourier transform spectrometer. The instrument points along the spin axis and has a 7° field of view. This device measures the spectrum to a precision of 1/1000 of the peak flux at 1.7 mm (0.067 in) for each 7° field of view on the sky (over the range 0.1 to 10 mm (0.39 in)). The FIRAS uses a special flared trumpet horn flux collector having very low sidelobe levels and an external calibrator covering the entire beam; precise temperature regulation and calibration are required. The instrument has a differential input to compare the sky with an internal reference at 3 K. This feature provides immunity from systematic errors in the spectrometer and contributes significantly to the ability to detect small deviations from a blackbody spectrum. The instrument weighs 60 kg (130 lb), uses 84 watts and has a data rate of 1200 bit/s.[12]

## Scientific findings

The map of the CMB anisotropy formed from data taken by the COBE spacecraft.

The science mission was conducted by the three instruments detailed previously: DIRBE, FIRAS and DMR. The instruments overlapped in wavelength coverage, providing consistency check on measurements in the regions of spectral overlap and assistance in discriminating signals from our galaxy, Solar System and CMB.[9]

COBE's instruments would fulfill each of their objectives as well as making observations that would have implications outside COBE's initial scope.

### Black-body curve of CMB

Data from COBE showed a perfect fit between the black body curve predicted by big bang theory and that observed in the microwave background. The error bars are smaller than the width of the blue curve. The red crosses merely locate the data points. Comparison of CMB results from COBE, WMAP and Planck \- 21 March 2013.

During the 15-year-long period between the proposal and launch of COBE, there were two significant astronomical developments:

* First, in 1981, two teams of astronomers, one led by David Wilkinson of Princeton University and the other by Francesco Melchiorri of the University of Florence, simultaneously announced that they detected a quadrupole distribution of CMB using balloon-borne instruments. This finding would have been the detection of the black-body distribution of CMB that FIRAS on COBE was to measure. In particular, the Florence group claimed a detection of intermediate angular scale anisotropies at the level 100 microkelvins[13] in agreement with later measurements made by the BOOMERanG experiment. However, a number of other experiments attempted to duplicate their results and were unable to do so.[6]
* Second, in 1987 a Japanese-American team led by Andrew E. Lange and Paul Richards of University of California, Berkeley and Toshio Matsumoto of Nagoya University made an announcement that CMB was not that of a true black body.[14] In a sounding rocket experiment, they detected an excess brightness at 0.5 and 0.7 mm (0.028 in) wavelengths.

With these developments serving as a backdrop to COBE's mission, scientists eagerly awaited results from FIRAS. The results of FIRAS were startling in that they showed a perfect fit of the CMB and the theoretical curve for a black body at a temperature of 2.7 K, in contrast to the Berkeley-Nagoya results.

FIRAS measurements were made by measuring the spectral difference between a 7° patch of the sky against an internal black body. The interferometer in FIRAS covered between 2 and 95 cm-1 in two bands separated at 20 cm-1. There are two scan lengths (short and long) and two scan speeds (fast and slow) for a total of four different scan modes. The data were collected over a ten-month period.[15]

### Intrinsic anisotropy of CMB

Data obtained at each of the three DMR frequencies — 31.5, 53, and 90 GHz — following dipole subtraction.

The DMR was able to spend four years mapping the detectable anisotropy of cosmic background radiation as it was the only instrument not dependent on the dewar's supply of helium to keep it cooled. This operation was able to create full sky maps of the CMB by subtracting out galactic emissions and dipole at various frequencies. The cosmic microwave background fluctuations are extremely faint, only one part in 100,000 compared to the 2.73 K average temperature of the radiation field. The cosmic microwave background radiation is a remnant of the Big Bang and the fluctuations are the imprint of density contrast in the early universe. The density ripples are believed to have produced structure formation as observed in the universe today: clusters of galaxies and vast regions devoid of galaxies.[16]

### Detecting early galaxies

DIRBE also detected 10 new far-IR emitting galaxies in the region not surveyed by IRAS as well as nine other candidates in the weak far-IR that may be spiral galaxies. Galaxies that were detected at the 140 and 240 μm were also able to provide information on very cold dust (VCD). At these wavelengths, the mass and temperature of VCD can be derived. When these data were joined with 60 and 100 μm data taken from IRAS, it was found that the far-infrared luminosity arises from cold (≈17–22 K) dust associated with diffuse H I region cirrus clouds, 15-30% from cold (≈19 K) dust associated with molecular gas, and less than 10% from warm (≈29 K) dust in the extended low-density H II regions.[17]

### DIRBE

Main article: Astronomy:Diffuse Infrared Background Experiment

Model of the Galactic disk as seen edge-on from Earth's position.

On top of the findings DIRBE had on galaxies, it also made two other significant contributions to science.[17] The DIRBE instrument was able to conduct studies on interplanetary dust (IPD) and determine if its origin was from asteroid or cometary particles. The DIRBE data collected at 12, 25, 50 and 100 μm were able to conclude that grains of asteroidal origin populate the IPD bands and the smooth IPD cloud.[18]

The second contribution DIRBE made was a model of the Galactic disk as seen edge-on from our position. According to the model, if the Sun is 8.6 kpc from the Galactic Center, then it is 15.6% above the midplane of the disk, which has a radial and vertical scale lengths of 2.64 and 0.333 kpc, respectively, and is warped in a way consistent with the HI layer. There is also no indication of a thick disk.[19]

To create this model, the IPD had to be subtracted out of the DIRBE data. It was found that this cloud, which as seen from Earth is Zodiacal light, was not centered on the Sun, as previously thought, but on a place in space a few million kilometers away. This is due to the gravitation influence of Saturn and Jupiter.[6]

### Cosmological implications

In addition to the science results detailed in the last section, there are numerous cosmological questions left unanswered by COBE's results. A direct measurement of the extragalactic background light (EBL) can also provide important constraints on the integrated cosmological history of star formation, metal and dust production, and the conversion of starlight into infrared emissions by dust.[20]

By looking at the results from DIRBE and FIRAS in the 140 to 5000 μm we can detect that the integrated EBL intensity is ≈16 nW/(m2·sr). This is consistent with the energy released during nucleosynthesis and constitutes about 20–50% of the total energy released in the formation of helium and metals throughout the history of the universe. Attributed only to nuclear sources, this intensity implies that more than 5–15% of the baryonic mass density implied by Big Bang nucleosynthesis analysis has been processed in stars to helium and heavier elements.[20]

There were also significant implications into star formation. COBE observations provide important constraints on the cosmic star formation rate and help us calculate the EBL spectrum for various star formation histories. Observation made by COBE require that star formation rate at redshifts of z ≈ 1.5 to be larger than that inferred from UV-optical observations by a factor of 2. This excess stellar energy must be mainly generated by massive stars in yet - undetected dust enshrouded galaxies or extremely dusty star-forming regions in observed galaxies.[20] The exact star formation history cannot unambiguously be resolved by COBE and further observations must be made in the future.

On 30 June 2001, NASA launched a follow-up mission to COBE led by DMR Deputy Principal Investigator Charles L. Bennett. The Wilkinson Microwave Anisotropy Probe has clarified and expanded upon COBE's accomplishments. Following WMAP, the European Space Agency's probe, Planck has continued to increase the resolution at which the background has been mapped.[21][22]

## Popular culture

The Cosmic Background Explorer satellite appeared twice in the season 1 episode of Young Sheldon called "Gluons, Guacamole, and the Color Purple", where a young Sheldon Lee Cooper daydreams of helping NASA save the satellite from crashing back to Earth.[23]

## See also

* 9997 COBE, a minor planet named after the experiment.
* S150 Galactic X-Ray Mapping
* Wilkinson Microwave Anisotropy Probe

## References

1. ↑ "COBE Mission Design, Spacecraft and Orbit". NASA/Goddard Space Flight Center. 18 April 2008. https://lambda.gsfc.nasa.gov/product/cobe/spacecraft_description.html. This article incorporates text from this source, which is in the public domain.
2. ↑ Crouse, Megan (16 July 2015). "Spacecraft of the Week: Cosmic Background Explorer". Product Design & Development. http://www.pddnet.com/article/2015/07/spacecraft-week-cosmic-background-explorer.
3. ↑ "Trajectory: COBE (1989-089A)". NASA. 28 October 2021. https://nssdc.gsfc.nasa.gov/nmc/spacecraft/displayTrajectory.action?id=1989-089A. This article incorporates text from this source, which is in the public domain.
4. ↑ 4.0 4.1 "The Nobel Prize in Physics 2006". Royal Swedish Academy of Sciences. 3 October 2006. https://www.nobelprize.org/prizes/physics/2006/summary/.
5. ↑ 5.0 5.1 "Display: COBE (1989-089A)". NASA. 28 October 2021. https://nssdc.gsfc.nasa.gov/nmc/spacecraft/display.action?id=1989-089A. This article incorporates text from this source, which is in the public domain.
6. ↑ 6.0 6.1 6.2 Leverington, David (2000). New Cosmic Horizons: Space Astronomy from the V2 to the Hubble Space Telescope. Cambridge University Press. ISBN 0-521-65833-0. OCLC 44174182.
7. ↑ Schewe, Phillip F.; Stein, Ben (24 April 1992). "COBE Picks Out Primordial Seeds at Last". The AIP Bulletin of Physics News (American Institute of Physics) 77. https://www.aip.org/pnu/1992/split/pnu077-1.htm.
8. ↑ Wilford, John Noble (24 April 1992). "Scientists Report Profound Insight on How Time Began". The New York Times. ISSN 0362-4331. https://www.nytimes.com/1992/04/24/us/scientists-report-profound-insight-on-how-time-began.html.
9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 Boggess, N. W.; Mather, J. C.; Weiss, R.; Bennett, C. L.; Cheng, E. S.; Dwek, E.; Gulkis, S.; Hauser, M. G. et al. (31 January 1992). "The COBE Mission: Its Design and Performance Two Years after the launch". The Astrophysical Journal (American Astronomical Society) 397 (2): 420-429. 1 October 1992. doi:10.1086/171797. ISSN 0004-637X. Bibcode: 1992ApJ...397..420B.
10. ↑ "Experiment: Differential Microwave Radiometers (DMR)". NASA. 28 October 2021. https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1989-089A-03. This article incorporates text from this source, which is in the public domain.
11. ↑ "Experiment: Diffuse Infrared Background Experiment (DIRBE)". NASA. 28 October 2021. https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1989-089A-02. This article incorporates text from this source, which is in the public domain.
12. ↑ "Experiment: Far Infrared Absolute Spectrophotometer (FIRAS)". NASA. 28 October 2021. https://nssdc.gsfc.nasa.gov/nmc/experiment/display.action?id=1989-089A-01. This article incorporates text from this source, which is in the public domain.
13. ↑ Melchiorri, Francesco; Melchiorri, Bianca Olivo; Ceccarelli, Cecilia; Pietranera, Luca (1 October 1980). "Fluctuations in the microwave background at intermediate angular scales". The Astrophysical Journal (American Astronomical Society) 250: L1-L4. 1 November 1981. doi:10.1086/183662. ISSN 0004-637X. Bibcode: 1981ApJ...250L...1M.
14. ↑ Hayakawa, Satio; Matsumoto, Toshio; Matsuo, Hiroshi; Murakami, Hiroshi; Sato, Shinji; Lange, Andrew E.; Richards (2 November 1987). "Cosmological implication of a new measurement of the submillimeter background radiation". Publications of the Astronomical Society of Japan 39 (6): 941–948. 25 December 1987. doi:10.1093/pasj/39.6.941. ISSN 0004-6264. Bibcode: 1987PASJ...39..941H.
15. ↑ Fixsen, D. J.; Cheng, E. S.; Cottingham, D. A.; Eplee, Jr., R. E.; Isaacman, R. B.; Mather, J. C.; Meyer, S. S.; Noerdlinger, P. D. et al. (5 February 1993). "Cosmic microwave background dipole spectrum measured by the COBE FIRAS instrument". The Astrophysical Journal (American Astronomical Society) 420: 445–449. 10 January 1994. doi:10.1086/173575. ISSN 0004-637X. Bibcode: 1994ApJ...420..445F.
16. ↑ Dick, Steven J. (16 October 2006). "Voyages to the Beginning of Time" (in en). NASA. https://www.nasa.gov/exploration/whyweexplore/Why_We_24.html. This article incorporates text from this source, which is in the public domain.
17. ↑ 17.0 17.1 Sodroski, T. J.; Bennett, C.; Boggess, N.; Dwek, E.; Franz, B. A.; Hauser, M. G.; Kelsall, T.; Moseley, S. H. et al. (11 August 1993). "Large-Scale Characteristics of Interstellar Dust from COBE DIRBE Observations". The Astrophysical Journal (American Astronomical Society) 428: 638–646. 20 June 1994. doi:10.1086/174274. ISSN 0004-637X. Bibcode: 1994ApJ...428..638S.
18. ↑ Spiesman, William J.; Hauser, Michael G.; Kelsall, Thomas; Lisse, Carey M.; Moseley, Jr., S. Harvey; Reach, William T.; Silverberg, Robert F.; Stemwedel, Sally W. et al. (17 May 1994). "Near and far-infrared observations of interplanetary dust bands from the COBE Diffuse Infrared Background Experiment". The Astrophysical Journal (American Astronomical Society) 442: 662. 1 April 1995. doi:10.1086/175470. ISSN 0004-637X. Bibcode: 1995ApJ...442..662S.
19. ↑ Freudenreich, H. T. (14 December 1995). "The Shape and Color of the Galactic Disk". The Astrophysical Journal (American Astronomical Society) 468: 663–678. 10 September 1996. doi:10.1086/177724. ISSN 0004-637X. Bibcode: 1996ApJ...468..663F. See also Freudenreich, H. T. (20 August 1997). "The Shape and Color of the Galactic Disk: Erratum". The Astrophysical Journal (American Astronomical Society) 485 (2): 920. doi:10.1086/304478. ISSN 0004-637X. Bibcode: 1997ApJ...485..920F.
20. ↑ 20.0 20.1 20.2 Dwek, E.; Arendt, R. G.; Hauser, M. G.; Fixsen, D.; Kelsall, T.; Leisawitz, D.; Pei, Y. C.; Wright, E. L. et al. (3 February 1998). "The COBE Diffuse Infrared Background Experiment search for the cosmic infrared background: IV. Cosmological Implications". The Astrophysical Journal (American Astronomical Society) 508 (1): 106–122. 9 June 1998. doi:10.1086/306382. ISSN 0004-637X. Bibcode: 1998ApJ...508..106D.
21. ↑ Thomas, Christopher (3 April 2013). "Planck's Probe Map - A picture of the Universe". Spider Magazine. http://dawn.com/2013/04/03/plank-probes-map-a-picture-of-our-universe/.
22. ↑ "Planck's HFI Completes Its Survey of the Early Universe" (Press release). ESA. 16 January 2012. Archived from the original on 4 January 2026. Retrieved 28 May 2013.
23. ↑ Young Sheldon Saves the WORLD from Satellite CRASH on YouTube

## Sources

* Arny, Thomas T. (2002). Explorations: An Introduction to Astronomy (3rd ed.). Dubuque, Iowa: McGraw-Hill. ISBN 978-0-07-241593-3.
* Liddle, Andrew R.; Lyth, David H. (March 1993). "The Cold Dark Matter Density Perturbation". Physics Reports (Elsevier) 231 (1–2): 1–105. August 1993. doi:10.1016/0370-1573(93)90114-S. Bibcode: 1993PhR...231....1L.
* Odenwald, Sten; Newmark, Jeffrey; Smoot, George (6 October 1995). "A Study of External Galaxies Detected by the COBE Diffuse Infrared Background Experiment". The Astrophysical Journal (American Astronomical Society) 500 (2): 554–568. 20 June 1998. doi:10.1086/305737. ISSN 0004-637X. Bibcode: 1998ApJ...500..554O.

## Further reading

* Mather, John C.; Boslough, John (1996). The Very First Light: The True Inside Story of the Scientific Journey Back to the Dawn of the Universe. New York: BasicBooks. ISBN 0-465-01575-1. https://archive.org/details/veryfirstlight00john.
* Smoot, George; Davidson, Keay (1993). Wrinkles in Time. New York: William Morrow. ISBN 0-688-12330-9. OCLC 28215032.
* WMAP

## External links

* NASA's website on COBE
* NASA informational video prior to COBE launch
* COBE Mission Profile by NASA's Solar System Exploration
* APOD picture of the COBE dipole, showing the 600 km/s motion of the Earth relative to the cosmic background radiation
* Cosmic Background Explorer article from Scholarpedia

* v
* t
* e

Cosmic microwave background radiation (CMB)

* Discovery of CMB radiation
* Timeline of CMB astronomy

Effects|

* Cosmic variance
* Silk damping
* Recombination
* Sachs–Wolfe effect
* Sunyaev–Zel'dovich effect
* Thomson scattering

9-year WMAP image (2012) of the CMB.

9-year WMAP image (2012) of the CMB.

Experiments|

| Space|

* COBE
* LiteBIRD
* Planck
* RELIKT-1
* WMAP

|

Balloon|

* Archeops
* ARCADE
* BOOMERanG
* LSPE/SWIPE
* EBEX
* MAXIMA
* QMAP
* Spider
* TopHat

Ground|

* ABS
* ACBAR
* ACT
* AMI
* AMiBA
* APEX
* ATCA
* BICEP (1,2,3,Array)
* BIMA
* CAPMAP
* CAT
* CBI
* CLASS
* COSMOSOMAS
* DASI
* Keck Array
* LSPE/STRIP
* MAT
* OVRO
* POLARBEAR
* QUaD
* QUBIC
* QUIET
* QUIJOTE
* Saskatoon
* SPT
* SZA
* Tenerife
* VSA

* v
* t
* e

Explorers Program

List of Explorers Program missions

Missions|

| 1958–1992|

* Explorer 1
* 2†
* 3
* 4
* 5†
* S-1†
* 6 (S-2)
* 7 (S-1A)
* S-46A†
* 8
* S-56†
* 9 (S-56A)
* S-45†
* 10
* 11 (S-15)
* S-45A†
* S-55†
* 12 (EPE-A)
* 13 (S-55A)
* 14 (EPE-B)
* 15 (EPE-C)
* 16 (S-55B)
* 17 (AE-A)
* 18 (IMP-A)
* 19 (AD-A)
* S-66A (BE-A)†
* 20 (IE-A)
* 21 (IMP-B)
* 22 (BE-B)
* 23 (S-55C)
* 24 (AD-B)
* 25 (Injun 4, IE-B)
* 26 (EPE-D)
* 27 (BE-C)
* 28 (IMP-C)
* 29 (GEOS-A)
* 30 (Solrad 8)
* 31 (DME-A)
* 32 (AE-B)
* 33 (IMP-D)
* 34 (IMP-F)
* 35 (IMP-E)
* 36 (GEOS-B)
* 37 (Solrad 9)
* 38 (RAE-A)
* 39 (AD-C)
* 40 (Injun 5)
* 41 (IMP-G)
* 42 (Uhuru, SAS-A)
* 43 (IMP-H)
* 44 (Solrad 10)
* 45 (SSS-A)
* 46 (MTS)
* 47 (IMP-I)
* 48 (SAS-B)
* 49 (RAE-B)
* 50 (IMP-J)
* 51 (AE-C)
* 52 (Hawkeye 1)
* 53 (SAS-C)
* 54 (AE-D)
* 55 (AE-E)
* DADE-A†
* DADE-B†
* 56 (ISEE-1)
* 57 (IUE)
* 58 (HCMM)
* 59 (ICE)
* 60 (SAGE)
* 61 (Magsat)
* 62 (DE-1)
* 63 (DE-2)
* 64 (SME)
* 65 (CCE)
* 66 (COBE)
* 67 (EUVE)

|

MIDEX|

* 69 (RXTE)
* 71 (ACE)
* 77 (FUSE)
* 78 (IMAGE)
* 80 (WMAP)
* FAME
* 84 (Swift)
* 85–89 (THEMIS)
* 92 (WISE)
* 95 (TESS)
* 96 (ICON)
* SPHEREx

SMEX|

* 68 (SAMPEX)
* 70 (FAST)
* 73 (TRACE)
* 74 (SWAS)
* 75 (WIRE)†
* 81 (RHESSI)
* 83 (GALEX)
* 90 (AIM)
* 91 (IBEX)
* 93 (NuSTAR)
* 94 (IRIS)
* GEMS
* IXPE
* PUNCH
* TRACERS

UNEX/MO/I|

* HETE-1†
* 72 (SNOE)
* 76 (TERRIERS)†
* 79 (HETE-2)
* INTEGRAL
* 82 (CHIPSat)
* CINDI
* Suzaku
* TWINS
* Hitomi†
* NICER
* GOLD
* XRISM
* GUSTO
* CASE

Proposals|

| Proposals|

* FINESSE
* Arcus
* OHMIC
* ASTRE
* EXCEDE

|

* Green titles indicates active current missions
* Grey titles indicates cancelled missions
* Italics indicate missions yet to launch
* Symbol † indicates failure en route or before intended mission data returned

* v
* t
* e

Cosmology

Background|

* Age of the universe
* Big Bang
* Chronology of the universe
* Universe
* Observable Universe

History of
cosmological theories|

* Discovery of cosmic microwave background
* History of the Big Bang theory
* Religious interpretations of the Big Bang
* Timeline of cosmological theories

Past universe|

* Cosmic microwave background
* Cosmic neutrino background
* Gravitational wave background
* Inflation
* Nucleosynthesis
* Habitable epoch

Present universe|

* FLRW metric
* Friedmann equations
* Hubble's law
* Metric expansion of space
* Accelerating expansion
* Redshift

Future universe|

* Future of an expanding universe
* Ultimate fate of the universe

Components|

* Dark energy
* Dark fluid
* Dark matter
* Lambda-CDM model

Structure formation|

* Galaxy filament
* Galaxy formation
* Large quasar group
* Large-scale structure
* Reionization
* Shape of the universe
* Structure formation

Experiments|

* 2dF
* 6dF
* BOOMERanG
* COBE
* Illustris project
* Observational cosmology
* Planck
* SDSS
* WMAP

* v
* t
* e

NASAGoddard Space Flight Center|Goddard Space Flight Center]]

Main articles|

* Robert H. Goddard
* GSFC History

Facilities|

* Wallops Flight Facility (WFF)
* Goddard Institute for Space Studies (GISS)
* Independent Verification and Validation Facility (IV&V)
* Spacecraft Magnetic Test Facility
* Spacecraft Fabrication Facility
* Columbia Scientific Balloon Facility (CSBF)

Notable missions
and programs|

* James Webb Space Telescope (JWST)
* Cosmic Background Explorer (COBE)
* Space Network
* Near Earth Network
* Landsat program
* Getaway Special
* Compton Gamma Ray Observatory (CGRO)
* Rossi X-ray Timing Explorer (RXTE)
* Explorers program
* Hitchhiker Program
* Solar and Heliospheric Observatory (SOHO)
* Lunar Reconnaissance Orbiter (LRO)
* Solar Dynamics Observatory (SDO)
* Hubble Space Telescope (HST)
* Tracking and Data Relay Satellite (TDRS)

People|

| Leadership|

* Christopher Scolese (Director)
* George Morrow (Deputy Director)
* Christyl Johnson (Deputy Director, Technology and Research Investments)
* Colleen Hartman (Deputy Director, Science, Operations and Performance)

|

Notable scientists
and engineers|

* David Louis Band
* Robert Bindschadler
* Fred Espenak
* Gene Carl Feldman
* Orlando Figueroa
* James Hansen
* Marc Kuchner
* Lissette Martinez
* John C. Mather

* v
* t
* e

Space observatories

Operating|

* AGILE (since 2007)
* AMS-02 (since 2011)
* Aoi (since 2018)
* ASTERIA (since 2017)
* Astrosat (since 2015)
* BRITE constellation (since 2013)
* CALET (since 2015)
* Chandra (AXAF) (since 1999)
* DAMPE (since 2015)
* Fermi (since 2008)
* Gaia (since 2013)
* HXMT (Insight) (since 2017)
* Hinode (Solar-B) (since 2006)
* HiRISE (since 2005)
* Hisaki (SPRINT-A) (since 2013)
* Hubble (since 1990)
* INTEGRAL (since 2002)
* IBEX (since 2008)
* IRIS (since 2013)
* ISS-CREAM (since 2017)
* MAXI (since 2009)
* Mikhailo Lomonosov (since 2016)
* Mini-EUSO (since 2019)
* NCLE (since 2018)
* NEOSSat (since 2013)
* NICER (since 2017)
* NuSTAR (since 2012)
* Odin (since 2001)
* SDO (since 2010)
* SOHO (since 1995)
* SOLAR (since 2008)
* Spektr-RG (since 2019)
* Spitzer (since 2003)
* STEREO (since 2006)
* Swift (since 2004)
* TESS (since 2018)
* WISE (since 2009)
* XMM-Newton (since 1999)

Planned|

* CHEOPS (2019)
* iWF-MAXI (2019)
* Astro-1 Telescope (2020)
* ILO-1 (2020)
* LUCI (2020)
* Nano-JASMINE (2020)
* ORBIS (2020)
* Solar Orbiter (SolO) (2020)
* IXPE (2021)
* James Webb (JWST) (2021)
* LORD (2021)
* SVOM (2021)
* XPoSat (2021)
* Euclid (2022)
* Space Solar Telescope (2022)
* XRISM (2022)
* Xuntian (2022)
* K-EUSO (2023)
* Solar-C (2023)
* SPHEREx (2023)
* Small-JASMINE (2024)
* Near-Earth Object Surveillance Mission (2025+)
* Spektr-UV (2025)
* WFIRST (2025+)
* PLATO (2026)
* LiteBIRD (2027)
* ARIEL (2028)
* Spektr-M (2030+)
* ATHENA (2031)
* LISA (2034)

Proposed|

* Arcus
* AstroSat-2
* EXCEDE
* Fresnel Imager
* FOCAL
* HabEx
* Hibari
* Hypertelescope
* JEM-EUSO
* LUVOIR
* ATLAST
* HDST
* Lynx
* Nautilus Deep Space Observatory
* New Worlds Mission
* NRO donation to NASA
* OST
* PhoENiX
* Solar-D
* SPICA
* THEIA
* THESEUS

Retired|

* Akari (Astro-F) (2006–2011)
* ALEXIS (1993–2005)
* Alouette 1 (1962–1972)
* Ariel 1 (1962, 1964)
* Ariel 2 (1964)
* Ariel 3 (1967–1969)
* Ariel 4 (1971–1972)
* Ariel 5 (1974–1980)
* Ariel 6 (1979–1982)
* ATM (1973–1974)
* ASCA (Astro-D) (1993–2000)
* Astro-1 (1990)
* BBXRT
* HUT
* Astro-2 (HUT) (1995)
* Astron (1983–1989)
* ANS (1974–1976)
* BeppoSAX (1996–2003)
* CHIPSat (2003–2008)
* Compton (CGRO) (1991–2000)
* CoRoT (2006–2013)
* Cos-B (1975–1982)
* COBE (1989–1993)
* DXS (1993)
* EPOCh (2008)
* EPOXI (2010)
* Explorer 11 (1961)
* EXOSAT (1983–1986)
* EUVE (1992–2001)
* FUSE (1999–2007)
* Kvant-1 (1987–2001)
* GALEX (2003–2013)
* Gamma (1990–1992)
* Ginga (Astro-C) (1987–1991)
* Granat (1989–1998)
* Hakucho (CORSA-b) (1979–1985)
* HALCA (MUSES-B) (1997–2005)
* HEAO-1 (1977–1979)
* Herschel (2009–2013)
* Hinotori (Astro-A) (1981–1991)
* HEAO-2 (Einstein Obs.) (1978–1982)
* HEAO-3 (1979–1981)
* HETE-2 (2000–2008)
* Hipparcos (1989–1993)
* IUE (1978–1996)
* IRAS (1983)
* IRTS (1995–1996)
* ISO (1996–1998)
* IXAE (1996–2004)
* Kepler (2009–2018)
* Kristall (1990–2001)
* LEGRI (1997–2002)
* LISA Pathfinder (2015–2017)
* MOST (2003–2019)
* MSX (1996–1997)
* OAO-2 (1968–1973)
* OAO-3 (Copernicus) (1972–1981)
* Orbiting Solar Observatory
* OSO 1
* OSO 2/OSO B
* OSO 3
* OSO 4
* OSO 5
* OSO 6
* OSO 7
* OSO 8
* Orion 1 (1971)
* Orion 2 (1973)
* PAMELA (2006–2016)
* PicSat (2018)
* Planck (2009–2013)
* RELIKT-1 (1983–1984)
* R/HESSI (2002–2018)
* ROSAT (1990–1999)
* RXTE (1995–2012)
* SAMPEX (1992–2004)
* SAS-B (1972–1973)
* SAS-C (1975–1979)
* Solwind (1979–1985)
* Spektr-R (2011–2019)
* Suzaku (Astro-EII) (2005–2015)
* Taiyo (SRATS) (1975–1980)
* Tenma (Astro-B) (1983–1985)
* Uhuru (1970–1973)
* Vanguard 3 (1959)
* WMAP (2001–2010)
* Yokoh (Solar-A) (1991–2001)

Hibernating
(Mission completed)|

* SWAS (1998–2005)
* TRACE (1998–2010)

Lost|

* OAO-1 (1966)
* OAO-B (1970)
* CORSA (1976)
* OSO C (1965)
* ABRIXAS (1999)
* HETE-1 (1996)
* WIRE (1999)
* Astro-E (2000)
* Tsubame (2014–2015)
* Hitomi (Astro-H) (2016)

Cancelled|

* AOSO
* Astro-G
* Constellation-X
* Darwin
* Destiny
* EChO
* Eddington
* FAME
* FINESSE
* GEMS
* HOP
* IXO
* JDEM
* LOFT
* OSO J
* OSO K
* Sentinel
* SIM & SIMlite
* SNAP
* SPOrt
* TAUVEX
* TPF
* XEUS
* XIPE

See also|

* Great Observatories program
* List of space telescopes
* List of proposed space observatories
* List of X-ray space telescopes

* Category

* v
* t
* e

NASA

Policy and history|

| History|

* NACA (1915)
* National Aeronautics and Space Act (1958)
* Space Task Group (1958)
* Paine (1986)
* Rogers (1986)
* Ride (1987)
* Space Exploration Initiative (1989)
* Augustine (1990)
* U.S. National Space Policy (1996)
* CFUSAI (2002)
* CAIB (2003)
* Vision for Space Exploration (2004)
* Aldridge (2004)
* Augustine (2009)

|

General|

* Space Race
* Administrator and Deputy Administrator
* Chief Scientist
* Astronaut Corps
* Ranks and positions
* Chief
* Budget
* Spin-off technologies
* NASA TV
* NASA Social
* Launch Services Program
* Mercury Control Center
* Kennedy Space Center
* Vehicle Assembly Building
* Launch Complex 39
* Launch Control Center
* Operations and Checkout Building
* Johnson Space Center
* Mission Control
* Lunar Sample Laboratory

Robotic programs|

| Past|

* Hitchhiker
* Mariner
* Mariner Mark II
* MESUR
* Mars Surveyor '98
* New Millennium
* Lunar Orbiter
* Pioneer
* Planetary Observer
* Ranger
* Surveyor
* Viking
* Project Prometheus
* Mars Scout
* Mars Exploration Rover

|

Current|

* Living With a Star
* Lunar Precursor Robotic Program
* Earth Observing System
* Great Observatories program
* Explorer
* Small explorer
* Voyager
* Discovery
* New Frontiers
* Solar Terrestrial Probes
* Commercial Lunar Payload Services

Human spaceflight
programs|

| Past|

* X-15 (suborbital)
* Mercury
* Gemini
* Apollo
* Apollo–Soyuz Test Project (with the Soviet space program)
* Skylab
* Space Shuttle
* Shuttle–Mir (with Roscosmos State Corporation)
* Constellation

|

Current|

* International Space Station
* Commercial Orbital Transportation Services
* Commercial Crew Development
* Orion
* Artemis
* Lunar Gateway

Individual featured
missions
(human and robotic)|

| Past|

* COBE
* Mercury 3
* Mercury-Atlas 6
* Magellan
* Pioneer 10
* Pioneer 11
* Galileo
* GALEX
* GRAIL
* WMAP
* Space Shuttle
* Sojourner rover
* Spirit rover
* LADEE
* MESSENGER
* Aquarius
* Cassini
* Dawn
* Kepler space telescope
* Opportunity rover
* RHESSI
* observed

|

Currently
operating|

* Mars Reconnaissance Orbiter
* 2001 Mars Odyssey
* New Horizons
* International Space Station
* Hubble Space Telescope
* Spitzer
* Swift
* THEMIS
* Mars Exploration Rover
* Curiosity rover
* timeline
* InSight
* GOES 14
* Lunar Reconnaissance Orbiter
* GOES 15
* Van Allen Probes
* Solar Dynamics Observatory
* Juno
* Mars Science Laboratory
* timeline
* NuSTAR
* Voyager 1
* Voyager 2
* WISE
* MAVEN
* MMS
* OSIRIS-REx
* Transiting Exoplanet Survey Satellite

Future|

* Joint Polar Satellite System
* James Webb Space Telescope
* Wide Field Infrared Survey Telescope
* Mars 2020
* NISAR
* Europa Clipper

Communications
and navigation|

* Near Earth Network
* Space Network
* Deep Space Network (Goldstone
* Madrid
* Canberra
* Space Flight Operations Facility)
* Deep Space Atomic Clock

NASA lists|

* Astronauts
* by name
* by year
* Gemini astronauts
* Apollo astronauts
* List of NASA aircraft
* List of NASA missions
* uncrewed missions
* List of NASA contractors
* List of United States rockets
* List of NASA cancellations
* List of Space Shuttle missions
* crews
* List of NASA cameras on spacecraft

NASA images
and artwork|

* Earthrise
* The Blue Marble
* Family Portrait
* Pale Blue Dot
* Pillars of Creation
* Mystic Mountain
* Solar System Family Portrait
* The Day the Earth Smiled
* Fallen Astronaut
* Lunar plaques
* Pioneer plaques
* Voyager Golden Record
* Apollo 11 goodwill messages
* NASA insignia
* Gemini and Apollo medallions
* Mission patches

Related|

* Apollo 15 postal covers incident
* Space Mirror Memorial
* The Astronaut Monument
* U.S. Astronaut Hall of Fame
* Space program on U.S. stamps
* Apollo 17 Moon mice
* Other primates in space
* NASA spinoff technologies

* Category

* v
* t
* e

Orbital launches in 1989

Kosmos 1987 * Kosmos 1988 * Kosmos 1989 | Kosmos 1990 | Kosmos 1991 | Gorizont No.29L | Kosmos 1992 | Intelsat VA F-15 | Kosmos 1993 | Progress 40 | Kosmos 1994 * Kosmos 1995 * Kosmos 1996 * Kosmos 1997 * Kosmos 1998 * Kosmos 1999 | Kosmos 2000 | Kosmos 2001 | Kosmos 2002 | USA-35 | Molniya-1 No.84 | Kosmos 2003 | Akebono | Kosmos 2004 | Meteor-2 No.22 | Kosmos 2005 | JCSAT-1 * Meteosat 4 | STS-29 (TDRS-4) | Kosmos 2006 | Progress 41 | Kosmos 2007 | Kosmos 2008 * Kosmos 2009 * Kosmos 2010 * Kosmos 2011 * Kosmos 2012 * Kosmos 2013 * Kosmos 2014 * Kosmos 2015 | USA-36 | Tele-X | Kosmos 2016 | Kosmos 2017 | Gran' No.33L | Kosmos 2018 | Foton No.5L | STS-30 (Magellan) | Kosmos 2019 | USA-37 | Kosmos 2020 | Kosmos 2021 | Resurs-F1 No.45 * Pion 1 * Pion 2 | Kosmos 2022 * Kosmos 2023 * Kosmos 2024 | Kosmos 2025 | Superbird-A * DFS Kopernikus 1 | Kosmos 2026 | Molniya-3 No.45 | Okean-O1 No.4 | USA-38 | Kosmos 2027 | USA-39 | Kosmos 2028 | Globus No.11 | Resurs-F1 No.46 | Nadezhda No.403 | Kosmos 2029 | Gorizont No.27L | Olympus F1 | Kosmos 2030 | Resurs-F1 No.47 * Pion 3 * Pion 4 | Kosmos 2031 | Kosmos 2032 | Kosmos 2033 | Kosmos 2034 | Kosmos 2035 | STS-28 (USA-40 * USA-41) | TV-SAT 2 * Hipparcos | Resurs-F2 No.4 | USA-42 | Kosmos 2036 | Progress M-1 | Marco Polo 1 | Kosmos 2037 | USA-43 * USA-44 | Himawari 4 | Soyuz TM-8 | USA-45 | Resurs-F1 No.48 | Kosmos 2038 * Kosmos 2039 * Kosmos 2040 * Kosmos 2041 * Kosmos 2042 * Kosmos 2043 | Kosmos 2044 | Kosmos 2045 | USA-46 | Molniya-1 No.69 | Kosmos 2046 | Interkosmos 24 * Magion 2 | Gorizont No.31L | Kosmos 2047 | Kosmos 2048 | STS-34 (Galileo) | USA-47 | Meteor-3 No.4 | Intelsat VI F-2 | Kosmos 2049 | COBE | STS-33 (USA-48) | Kosmos 2050 | Kosmos 2051 | Kvant 2 | Molniya-3 No.46 | Kosmos 2052 | Granat | USA-49 | Gran' No.36L | Progress M-2 | Kosmos 2053 | Kosmos 2054

Payloads are separated by bullets ( * ), launches by pipes ( | ). Crewed flights are indicated in bold text. Uncatalogued launch failures are listed in italics. Payloads deployed from other spacecraft are denoted in (brackets).

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Original source: https://en.wikipedia.org/wiki/Cosmic Background Explorer. Read more

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*[MIDEX]: Medium-Class Explorers
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*[MO]: Missions of Opportunity
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