ALMA Receiver Bands

ALMA telescope dishesThe Atacama Large Millimeter/submillimeter Array (ALMA) observes the Universe over a range of radio wavelengths within the millimetre and submillimetre region of the electromagnetic spectrum. To capture such a broad range of light from distant cosmic sources, each of ALMA’s 66 antennas are equipped with an arsenal of detectors, which are highly sensitive radio receivers. Each receiver type is sensitive to a particular "band", or range of wavelengths of the electromagnetic spectrum, and data can only be taken in one band at a time.

To date, eight out of a planned ten receivers have been installed on each ALMA antenna. These bands range from band 3, starting at wavelengths of 3.6 mm, to band 10, ending at 0.3 mm. Band 1 is under construction (covering wavelengths between 6 and 8.5 millimetres), and band 2 (covering 3.3 to 4.5 millimetres) might be added in the future.

ALMA Band

Wavelength coverage (mm)

Noise Temperature (K) Specification

Frequency (GHz)

Produced by

Receiver Technology

First light

1

6–8.5

26

35 – 50

TBD

HEMT

TBD

2

3.3–4.5

47

65 – 90

TBD

HEMT

TBD

3

2.6–3.6

60

84 – 116

HIA

SIS

2009

4

1.8–2.4

82

125 – 163

NAOJ

SIS

2013

5

1.4–1.8

105

163 – 211

OSO / NOVA

SIS

2016

6

1.1–1.4

136

211 – 275

NRAO

SIS

2009

7

0.8–1.1

219

275 – 373

IRAM

SIS

2009

8

0.6–0.8

292

385 – 500

NAOJ

SIS

2013

9

0.4–0.5

261

602 – 720

NOVA

SIS

2011

10

0.3–0.4

344

787 – 950

NAOJ

SIS

2012

Band 3

Produced by the Herzberg Institute of Astrophysics in Canada, band 3 covers the longest wavelength range of the bands initially installed, between 2.6–3.6 mm.

Band 3 is of crucial importance to ALMA. It was used during the testing and commissioning of the antennas, because its low frequency minimises the effects of atmospheric variations. During science operations, band 3 is routinely used to perform phase calibration of observations taken at both band 3 and higher frequencies.

Within our galaxy, band 3 can be used to observe small scale structure in molecular clouds, to search for new and exotic molecules (including carbon-based, pre-biotic molecules necessary for building life), and to detect molecular gas in disks around young stars. Beyond our own galaxy, band 3 can be used to image molecules in nearby galaxies at high resolution, to probe the cold interstellar medium of galaxies, and to peer into dust-obscured galaxies to observe star formation.

Band 3 has already helped to produce spectacular science results, such as finding an ingredient of life around infant Sun-like stars (eso1718) and observing the Sun (eso1703).

Band 4

Developed by National Astronomical Observatory of Japan (NAOJ), band 4 covers a wavelength range of 1.8–2.4 mm. ALMA observations with the band 4 receiver provide data about interstellar matter and increase our understanding of the formation of stars and galaxies.

The very first target of band 4 was the protostar system IRAS16293-2422. About 400 light-years away, this system is surrounded by a large amount of gas that served as a seedbed for these stars. This test observation captured radio emission from carbon sulfide (CS) molecules contained in the gas. Many other interesting molecules also emit in the frequency range covered by the band 4 receiver, including formaldehyde (H2CO), deuterium compounds, and carbon chain molecules (a linkage of carbon atoms). These substances are found in large quantities in cold star-forming regions.

Band 5

Band 5 ALMA receiverBand 5 saw first light in 2016 (eso1645) and extended ALMA’s coverage to a new range of the electromagnetic spectrum, seeing radio waves with wavelengths between 1.4–1.8 millimetres. This is a particularly exciting band because it allows astronomers to detect faint signals of water in the nearby Universe.

The European ALMA Programme Scientist, Leonardo Testi, explains the significance of band 5: “The band 5 receivers make it much easier to detect water, a prerequisite for life as we know it, in our Solar System and in more distant regions of our galaxy and beyond. They also allow ALMA to search for ionised carbon in the primordial Universe.”

The high sensitivity and angular resolution of ALMA allows astronomers to make detailed studies of water in a wide range of objects, including forming and evolved stars, the interstellar medium, and regions close to supermassive black holes. With band 5, ALMA is able to detect the emission from ionised carbon from objects seen soon after the Big Bang, opening up the possibility of probing the earliest epoch of galaxy formation.

The band 5 receiver was developed by the Group for Advanced Receiver Development (GARD) at Onsala Space Observatory, Chalmers University of Technology, Sweden. The production of the 66 receivers for the ALMA observatory was done jointly by GARD and NOVA.

Band 6

Band 6 was produced by the National Radio Astronomy Observatory (NRAO) and covers the wavelength range of 1.1–1.4 mm. This allows it to study a variety of astronomical objects, such as the molecular gas in planetary nebulae, molecules on active comets, the heating mechanisms of red giants and the afterglows of gamma-ray bursts. Along with band 3, astronomers have also used band 6 to reveal otherwise invisible details of our Sun, including a new view of the dark, contorted centre of a sunspot that is nearly twice the diameter of the Earth (eso1703).

Band 7

Covering a wavelength range of 0.8–1.1 mm, the band 7 receivers were delivered by the Institut de Radio Astronomie Millimétrique (IRAM). At these wavelengths, astronomers can peer at the disks of gas and dust around newborn stars, see into star-forming clouds, and observe early galaxies that are bright in submillimetre wavelengths but obscured by dust in optical light. Band 7 has also been used for astronomy a bit closer to home, measuring the global wind patterns on Mars and the water content in the atmosphere of Venus.

Band 8

Developed by NAOJ, ALMA’s band 8 receivers span a wavelength range of 0.6–0.8 mm, opening another window to the Universe. This band covers a wide range of radio emission lines from various atoms and molecules, and one of the most attractive targets is the emission from atomic carbon at 0.6 mm. Using ALMA’s band 8, astronomers took the world’s first interferometric image at 0.6 mm, synthesising the distribution of atomic carbon around a planetary nebula. Before this, all observations at this wavelength were made with single dish radio telescopes.

Band 9

Band 9 receiver cartridges for ALMAThe band 9 receivers, produced by the Nederlandse Onderzoekschool voor Astronomie (NOVA), cover the wavelength range 0.4–0.5 mm. It is one of the highest frequency bands in the baseline ALMA project, and offers some of the telescope's highest spatial resolution. The observations made possible by the band 9 receivers allow astronomers to study molecular clouds — the dense regions of gas and dust where new stars are being born — at higher temperatures and densities, and with higher angular resolution, thus complementing the longer wavelength bands.

Astronomers have also used band 9 to study a "comet factory" around a new star, solving a long-standing planet formation mystery (eso1325).

Six of the Band 9 receiver cartridges delivered by NOVA (the Netherlands Research School for Astronomy) under contract to ESO for the Atacama Large Millimeter/submillimeter Array project.

Band 10

The addition of the band 10 receivers extended ALMA’s vision fully into the realm of the submillimetre, the wavelengths of cosmic light that hold intriguing information about the cold, dark, and distant Universe. The effort to develop and produce band 10 was led by NAOJ. Band 10 covers the wavelength range of 0.3–0.4 mm.

Band 10 brings to ALMA a broad range of capabilities, which — among other things — enables astronomers and planetary scientists to study and monitor temperature changes at different altitudes above the clouds of Uranus and other giant planets in our Solar System.