Cosmic Background Explorer

NASA satellite of the Explorer program

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 our 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.

## Mission

[edit]

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

[edit]

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".[9]

## Spacecraft

[edit]

Part of a series on

Physical cosmology

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

Early universe

* Inflation · Nucleosynthesis

Backgrounds

* Gravitational wave (GWB)
* Microwave (CMB) · Neutrino (CNB)

Expansion · Future

* Hubble's law · Redshift
* Expansion of the universe
* FLRW metric · Friedmann equations
* Inhomogeneous cosmology
* Future of an expanding universe
* Ultimate fate of the universe

Components · Structure

|  Components

* Lambda-CDM model
* Dark energy · Dark matter

Structure

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

Experiments

* Black Hole Initiative (BHI)
* BOOMERanG
* Cosmic Background Explorer (COBE)
* Dark Energy Survey
* Planck space observatory
* Sloan Digital Sky Survey (SDSS)
* 2dF Galaxy Redshift Survey ("2dF")
* Wilkinson Microwave Anisotropy
Probe (WMAP)

Scientists

* Aaronson
* Alfvén
* Alpher
* Copernicus
* de Sitter
* Dicke
* Ehlers
* Einstein
* Ellis
* Friedmann
* Galileo
* Gamow
* Guth
* Hawking
* Hubble
* Huygens
* Kepler
* Lemaître
* Mather
* Newton
* Penrose
* Penzias
* Rubin
* Schmidt
* Smoot
* Suntzeff
* Sunyaev
* Tolman
* Wilson
* Zeldovich

* List of cosmologists

Subject history

* Discovery of cosmic microwave
background radiation

* History of the Big Bang theory
* Timeline of cosmological theories

* Category
* Astronomy portal

* 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.[10] 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.[10] 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 .[10] 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.[10] 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.[10]

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

[edit]

#### Differential Microwave Radiometers (DMR)

[edit]

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.[11]

#### Diffuse Infrared Background Experiment (DIRBE)

[edit]

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.[12]

#### Far Infrared Absolute Spectrophotometer (FIRAS)

[edit]

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.[13]

## Scientific findings

[edit]

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.[10]

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

[edit]

Data from COBE showed a perfect fit between the black body curve predicted by big bang theory and that observed in the microwave background. 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[14] 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.[15] 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.[16]

### Intrinsic anisotropy of CMB

[edit]

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.[17]

### Detecting early galaxies

[edit]

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.[18]

### DIRBE

[edit]

Main article: 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.[18] 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.[19]

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.[20]

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

[edit]

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.[21]

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.[21]

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.[21] 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.[22][23]

## See also

[edit]

* Spaceflight portal

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

## References

[edit]

1. ^ "COBE Mission Design, Spacecraft and Orbit". Goddard Space Flight Center. 18 April 2008. Retrieved 21 July 2015. This article incorporates text from this source, which is in the public domain.
2. ^ Crouse, Megan (16 July 2015). "Cosmic Background Explorer". Product Design & Development. Retrieved 21 July 2015.[permanent dead link]
3. ^ "Trajectory: COBE (1989-089A)". NASA. 28 October 2021. Retrieved 27 November 2021. This article incorporates text from this source, which is in the public domain.
4. ^ "The Nobel Prize in Physics 2006". The Royal Swedish Academy of Sciences. 3 October 2006. Retrieved 23 August 2011.
5. ^ a b "Display: COBE (1989-089A)". NASA. 28 October 2021. Retrieved 27 November 2021. This article incorporates text from this source, which is in the public domain.
6. ^ a b c Leverington, David (2000). New Cosmic Horizons: Space Astronomy from the V2 to the Hubble Space Telescope. Cambridge University Press. ISBN 0-521-65833-0.
7. ^ Schewe, Phillip F.; Stein, Ben (24 April 1992). "COBE PICKS OUT PRIMORDIAL SEEDS AT LAST". The AIP Bulletin of Physics News. Vol. 77\. Archived from the original on 23 October 2006. Retrieved 23 July 2023.
8. ^ Wilford, John Noble (24 April 1992). "SCIENTISTS REPORT PROFOUND INSIGHT ON HOW TIME BEGAN". The New York Times. ISSN 0362-4331. Retrieved 23 July 2023.
9. ^ "The Nobel Prize in Physics 2006". Nobel Foundation. Retrieved 9 October 2008.
10. ^ a b c d e f Boggess, N. W.; J. C. Mather; R. Weiss; C. L. Bennett; E. S. Cheng; E. Dwek; S. Gulkis; M. G. Hauser; M. A. Janssen; T. Kelsall; S. S. Meyer; S. H. Moseley; T. L. Murdock; R. A. Shafer; R. F. Silverberg; G. F. Smoot; D. T. Wilkinson & E. L. Wright (1992). "The COBE Mission: Its Design and Performance Two Years after the launch". Astrophysical Journal. 397 (2): 420. Bibcode:1992ApJ...397..420B. doi:10.1086/171797.
11. ^ "Experiment: Differential Microwave Radiometers (DMR)". NASA. 28 October 2021. Retrieved 27 November 2021. This article incorporates text from this source, which is in the public domain.
12. ^ "Experiment: Diffuse Infrared Background Experiment (DIRBE)". NASA. 28 October 2021. Retrieved 27 November 2021. This article incorporates text from this source, which is in the public domain.
13. ^ "Experiment: Far Infrared Absolute Spectrophotometer (FIRAS)". NASA. 28 October 2021. Retrieved 27 November 2021. This article incorporates text from this source, which is in the public domain.
14. ^ Melchiorri, Francesco; Melchiorri, Bianca O.; Pietranera, Luca; Melchiorri, B. O. (November 1981). "Fluctuations in the microwave background at intermediate angular scales" (PDF). The Astrophysical Journal. 250: L1. Bibcode:1981ApJ...250L...1M. doi:10.1086/183662. Retrieved 23 August 2011.
15. ^ Hayakawa, S.; Matsumoto, T.; Matsuo, H.; Murakami, Hiroshi; Sato, S.; Lange A. E. & Richards, P. (1987). "Cosmological implication of a new measurement of the submillimeter background radiation". Publications of the Astronomical Society of Japan. 39 (6): 941–948. Bibcode:1987PASJ...39..941H. ISSN 0004-6264. Retrieved 17 May 2012.
16. ^ Fixsen, D. J.; Cheng, E. S.; Cottingham, D. A.; Eplee, R. E. Jr.; Isaacman, R. B.; Mather, J. C.; Meyer, S. S.; Noerdlinger, P. D.; Shafer, R. A.; Weiss, R.; Wright, E. L.; Bennett, C. L.; Boggess, N. W.; Kelsall, T.; Moseley, S. H.; Silverberg, R. F.; Smoot, G. F.; Wilkinson, D. T. (1994). "Cosmic microwave background dipole spectrum measured by the COBE FIRAS instrument". Astrophysical Journal. 420 (2): 445–449. Bibcode:1994ApJ...420..445F. doi:10.1086/173575.
17. ^ Dick, Steven J. (16 October 2006). "Voyages to the Beginning of Time". nasa.gov. NASA. Archived from the original on 16 June 2022. Retrieved 16 June 2022. This article incorporates text from this source, which is in the public domain.
18. ^ a b T. J. Sodroski (1994). "Large-Scale Characteristics of Interstellar Dust from COBE DIRBE Observations". The Astrophysical Journal. 428 (2): 638–646. Bibcode:1994ApJ...428..638S. doi:10.1086/174274.
19. ^ Spiesman, W. J.; M. G. Hauser; T. Kelsall; C. M. Lisse; S. H. Moseley Jr.; W. T. Reach; R. F. Silverberg; S. W. Stemwedel & J. L. Weiland (1995). "Near and far-infrared observations of interplanetary dust bands from the COBE Diffuse Infrared Background Experiment". Astrophysical Journal. 442 (2): 662. Bibcode:1995ApJ...442..662S. doi:10.1086/175470.
20. ^ Freudenreich, H. T. (1996). "The shape and color of the galactic disk". Astrophysical Journal. 468: 663–678. Bibcode:1996ApJ...468..663F. doi:10.1086/177724. See also Freudenreich, H. T. (1997). "The shape and color of the galactic disk: Erratum". Astrophysical Journal. 485 (2): 920. Bibcode:1997ApJ...485..920F. doi:10.1086/304478.
21. ^ a b c Dwek, E.; R. G. Arendt; M. G. Hauser; D. Fixsen; T. Kelsall; D. Leisawitz; Y. C. Pei; E. L. Wright; J. C. Mather; S. H. Moseley; N. Odegard; R. Shafer; R. F. Silverberg & J. L. Weiland (1998). "The COBE Diffuse Infrared Background Experiment search for the cosmic infrared background: IV. Cosmological Implications". Astrophysical Journal. 508 (1): 106–122. arXiv:astro-ph/9806129. Bibcode:1998ApJ...508..106D. doi:10.1086/306382. S2CID 14706133.
22. ^ Thomas, Christopher (3 April 2013). "Planck's Probe Map - A picture of the Universe". Spider Magazine. Retrieved 28 May 2013.
23. ^ "Planck's HFI Completes Its Survey of the Early Universe". ESA. Retrieved 28 May 2013.

## Sources

[edit]

* Arny, Thomas T. (2002). Explorations: An Introduction to Astronomy (3rd ed.). Dubuque, Iowa: McGraw-Hill. ISBN 978-0-07-241593-3.
* Liddle, A. R.; Lyth, D. H. (1993). "The Cold Dark Matter Density Perturbation". Physics Report. 231 (1–2): 1–105. arXiv:astro-ph/9303019. Bibcode:1993PhR...231....1L. doi:10.1016/0370-1573(93)90114-S. S2CID 119084975.
* Odenwald, S.; J. Newmark & G. Smoot (1998). "A study of external galaxies detected by the COBE Diffuse Infrared Background Experiment". Astrophysical Journal. 500 (2): 554–568. arXiv:astro-ph/9610238. Bibcode:1998ApJ...500..554O. doi:10.1086/305737. S2CID 18799050.

## Further reading

[edit]

* 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.
* Smoot, George; Davidson, Keay (1993). Wrinkles in Time. New York: W. Morrow. ISBN 0-688-12330-9.
* WMAP

## External links

[edit]

Wikimedia Commons has media related to COBE.

* 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
* Diffusion damping
* Recombination
* Sachs–Wolfe effect
* Sunyaev–Zeldovich effect
* Thomson scattering

4-year Planck image (2018) 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
* Atacama Cosmology Telescope
* Arcminute Microkelvin Imager
* AMiBA
* APEX
* ATCA
* BICEP (1,2,3,Array)
* BIMA
* CAPMAP
* Cosmic Anisotropy Telescope
* Cosmic Background Imager
* CLASS
* COSMOSOMAS
* DASI
* GroundBIRD
* Keck Array
* LSPE/STRIP
* Mobile Anisotropy Telescope
* OVRO
* POLARBEAR
* QUaD
* QUBIC
* QUIET
* QUIJOTE
* Saskatoon
* Simons Observatory
* South Pole Telescope
* SZA
* Tenerife
* Very Small Array

* 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-I)
* 44 (Solrad 10)
* 45 (SSS-A)
* 46 (MTS)
* 47 (IMP-H)
* 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
* MUSE
* HelioSwarm
* UVEX

SMEX|

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

UNEX/MO/I|

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

Proposals|

| Proposals|

* FINESSE
* Arcus
* OHMIC
* ASTRE
* EXCEDE
* ESCAPE

|

* 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

NASA Goddard Space Flight Center

Main articles|

* Robert H. Goddard
* GSFC History

Facilities|

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

Notable missions
and programs|

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

People|

| Leadership|

* Dennis J. Andrucyk (Director)
* Anne L. Kinney (Deputy Center Director)
* Christyl Johnson (Deputy Director, Technology and Research Investments)
* Ray Rubilotta (Associate Center Director)

|

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
* Nancy Roman

* v
* t
* e

Space telescopes

Operating|

| Radio and Microwave|

* NCLE (since 2018)
* Solar Orbiter (since 2020)
* STEREO (since 2006)
* Queqiao (since 2018)
* Wind (since 1994)
* Queqiao 2 (since 2024)

|

Infrared|

* James Webb (since 2022)
* Odin (since 2001)
* SOLAR (since 2008)
* WISE (since 2009)

Optical|

* Aoi (since 2018)
* Astrosat (since 2015)
* BRITE constellation (since 2013)
* CHASE (since 2021)
* CHEOPS (since 2019)
* DSCOVR (since 2015)
* Euclid (since 2023)
* Hayabusa2 (since 2021)
* Gaia (since 2013)
* HiRISE (since 2005)
* Hubble (since 1990)
* Hinode (Solar-B) (since 2006)
* NEOSSat (since 2013)
* Odin (since 2001)
* SDO (since 2010)
* SOHO (since 1995)
* SOLAR (since 2008)
* Swift (since 2004)
* TESS (since 2018)

Ultraviolet|

* Aditya-L1 (since 2023)
* ASO-S (since 2022)
* Astrosat (since 2015)
* Hibari (since 2021)
* Hinode (Solar-B) (since 2006)
* IRIS (since 2013)
* SDO (since 2010)
* SOHO (since 1995)
* SOLAR (since 2008)
* Solar Orbiter (since 2020)
* STEREO (since 2006)
* Swift (since 2004)

X-ray and Gamma-ray|

* CALET (since 2015)
* Chandra (AXAF) (since 1999)
* DAMPE (since 2015)
* Einstein Probe (since 2024)
* HXMT (Insight) (since 2017)
* INTEGRAL (since 2002)
* Fermi (since 2008)
* GECAM (since 2020)
* IXPE (since 2021)
* Spektr-RG (since 2019)
* SVOM (since 2024)
* Swift (since 2004)
* Max Valier Sat (since 2017)
* MAXI (since 2009)
* MinXSS-2 (since 2018)
* NICER (since 2017)
* NuSTAR (since 2012)
* LEIA (since 2022)
* XRISM (since 2023)
* XPoSat (since 2024)
* XMM-Newton (since 1999)

Other (particle
or unclassified)|

* ACE (since 1997)
* AMS-02 (since 2011)
* CALET (since 2015)
* DAMPE (since 2015)
* IBEX (since 2008)
* ISS-CREAM (since 2017)
* Mini-EUSO (since 2019)
* SOHO (since 1995)
* Solar Orbiter (since 2020)
* STEREO (since 2006)

Planned|

* SPHEREx (2025)
* K-EUSO (2026)
* Nancy Grace Roman Space Telescope (2026)
* PLATO (2026)
* Xuntian (2026)
* COSI (2027)
* LORD (2027)
* NEO Surveyor (2027)
* JASMINE (2028)
* Solar-C EUVST (2028)
* ARIEL (2029)
* Spektr-UV (2030)
* UVEX (2030)
* Spektr-M (2030+)
* LiteBIRD (2032)
* Taiji (2033)
* Athena (2035)
* LISA (2035)

Proposed|

* Arcus
* Astro-1 Telescope
* AstroSat-2
* EXCEDE
* Fresnel Imager
* FOCAL
* HabEx
* HWO
* Hypertelescope
* ILO-1
* iWF-MAXI
* JEM-EUSO
* LUCI
* LUVOIR
* Lynx
* Nano-JASMINE
* Nautilus Deep Space Observatory
* New Worlds Mission
* NRO donation to NASA
* ORBIS
* OST
* PETREL
* PhoENiX
* Solar-D
* Space Solar Telescope
* THEIA
* THESEUS

Retired|

* AGILE (2007–2024)
* 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)
* ASTERIA (2017–2019)
* ATM (1973–1974)
* ASCA (Astro-D) (1993–2000)
* Astro-1 (1990)
* BBXRT
* HUT
* Astro-2 (HUT) (1995)
* Astron (1983–1991)
* ANS (1974–1976)
* BeppoSAX (1996–2003)
* CHIPSat (2003–2008)
* Compton (CGRO) (1991–2000)
* CoRoT (2006–2013)
* Cos-B (1975–1982)
* COBE (1989–1993)
* CXBN-2 (2017–2019)
* 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)
* Hisaki (SPRINT-A) (2013–2023)
* HEAO-2 (Einstein Obs.) (1978–1982)
* HEAO-3 (1979–1981)
* HETE-2 (2000–2008)
* Hipparcos (1989–1993)
* ILO-X (2024)
* IRAS (1983)
* IRTS (1995–1996)
* ISO (1996–1998)
* IUE (1978–1996)
* IXAE (1996–2004)
* Kepler (2009–2018)
* Kristall (1990–2001)
* LEGRI (1997–2002)
* LISA Pathfinder (2015–2017)
* MinXSS (2015–2017)
* MOST (2003–2019)
* MSX (1996–1997)
* Mikhailo Lomonosov (2016–2019?)
* OAO-2 (1968–1973)
* OAO-3 (Copernicus) (1972–1981)
* Orbiting Solar Observatory
* OSO 1
* 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)
* Spitzer (2003–2020)
* 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/Failed|

* OAO-1 (1966)
* OAO-B (1970)
* CORSA (1976)
* CXBN (2012–2013)
* OSO C (1965)
* ABRIXAS (1999)
* HETE-1 (1996)
* WIRE (1999)
* Astro-E (2000)
* Tsubame (2014–2015)
* Hitomi (Astro-H) (2016)

Cancelled|

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

Related|

* Great Observatories program
* List of space telescopes
* List of proposed space telescopes
* X-ray telescope
* List of heliophysics missions
* List of planetariums

* Category:Space telescopes

* v
* t
* e

NASA

Policy and history|

| History
(creation)|

* 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
* NASA research
* spinoff technologies
* NASA+
* NASA TV
* NASA Social
* Launch Services Program
* Mercury Control Center
* Manned Space Flight Network
* Kennedy Space Center
* Vehicle Assembly Building
* Launch Complex 39
* Launch Complex 48
* Launch Control Center
* Operations and Checkout Building
* Johnson Space Center
* Mission Control
* Lunar Sample Laboratory
* Science Mission Directorate

Human spaceflight
programs|

| Past|

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

|

Current|

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

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 Exploration
* Mars Exploration Rover

|

Current|

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

Individual featured
missions
(human and robotic)|

| Past|

* Apollo 11
* COBE
* Mercury 3
* Mercury-Atlas 6
* Magellan
* Pioneer 10
* Pioneer 11
* Galileo
* timeline
* GALEX
* GRAIL
* WMAP
* Space Shuttle
* Spitzer Space Telescope
* Sojourner rover
* Spirit rover
* LADEE
* MESSENGER
* Aquarius
* Cassini
* Dawn
* Kepler space telescope
* Opportunity rover
* timeline
* observed
* RHESSI
* InSight
* Ingenuity helicopter
* flights

|

Currently
operating|

* Mars Reconnaissance Orbiter
* 2001 Mars Odyssey
* New Horizons
* International Space Station
* Hubble Space Telescope
* Swift
* THEMIS
* Mars Exploration Rover
* Curiosity rover
* timeline
* 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
* Mars 2020
* Perseverance rover
* timeline
* James Webb Space Telescope
* timeline
* PACE

Future|

* Joint Polar Satellite System
* NISAR
* Europa Clipper
* Nancy Grace Roman Space Telescope

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
* Space Shuttle crews
* NASA aircraft
* NASA missions
* uncrewed missions
* Apollo missions
* Space Shuttle missions
* United States rockets
* NASA cancellations
* 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
* Deep fields
* Lunar plaques
* Pioneer plaques
* Voyager Golden Record
* Apollo 11 goodwill messages
* NASA insignia
* Gemini and Apollo medallions
* Mission patches
* Hubble Space Telescope anniversary images

Related|

* "We choose to go to the Moon"
* Apollo 8 Genesis reading
* Apollo 15 postal covers incident
* Space Mirror Memorial
* The Astronaut Monument
* Lunar sample displays
* Moon rocks
* stolen or missing
* U.S. Astronaut Hall of Fame
* Space program on U.S. stamps
* Apollo 17 Moon mice
* Moon tree
* Other primates in space
* NASA International Space Apps Challenge
* Astronauts Day
* National Astronaut Day
* Nikon NASA F4

* Category
* Commons

* v
* t
* e

← 1988

Orbital launches in 1989

1990 →

January|

* Kosmos 1987, Kosmos 1988, Kosmos 1989
* Kosmos 1990
* Kosmos 1991
* Gorizont No.29L
* Kosmos 1992
* Intelsat VA F-15
* Kosmos 1993

February|

* 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

March|

* 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

April|

* Tele-X
* Kosmos 2016
* Kosmos 2017
* Gran' No.33L
* Kosmos 2018
* Foton No.5L

May|

* 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

June|

* 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

July|

* 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

August|

* 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

September|

* 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

October|

* Kosmos 2047
* Kosmos 2048
* STS-34 (Galileo)
* USA-47
* Meteor-3 No.4
* Intelsat VI F-2

November|

* Kosmos 2049
* COBE
* STS-33 (USA-48)
* Kosmos 2050
* Kosmos 2051
* Kvant 2
* Molniya-3 No.46
* Kosmos 2052

December|

* Granat
* USA-49
* Gran' No.36L
* Progress M-2
* Kosmos 2053
* Kosmos 2054

Launches are separated by dots ( • ), payloads by commas ( , ), multiple names for the same satellite by slashes ( / ).
Crewed flights are underlined. Launch failures are marked with the † sign. Payloads deployed from other spacecraft are (enclosed in parentheses).

Authority control databases

International|

* VIAF

National|

* Israel
* United States

*[no.]: number
*[v]: View this template
*[t]: Discuss this template
*[e]: Edit this template
*[MIDEX]: Medium-Class Explorers
*[UNEX]: University-class Explorers
*[MO]: Missions of Opportunity
*[I]: International Missions