TheHubble Deep Field (HDF) is an image of a small region in theconstellationUrsa Major, constructed from a series of observations by theHubble Space Telescope. It covers an area about 2.6arcminutes on a side, about one 24-millionth of the whole sky, which is equivalent inangular size to atennis ball at a distance of 100 metres.[1] The image was assembled from 342 separate exposures taken with the Space Telescope'sWide Field and Planetary Camera 2 over ten consecutive days between December 18 and 28, 1995.[2][3]
The field is so small that only a few foregroundstars in theMilky Way lie within it; thus, almost all of the 3,000 objects in the image aregalaxies, some of which are among the youngest and most distant known. By revealing such large numbers of very young galaxies, the HDF has become a landmark image in thestudy of the early universe.
Three years after the HDF observations were taken, a region in the south celestial hemisphere was imaged in a similar way and named theHubble Deep Field South. The similarities between the two regions strengthened the belief that theuniverse is uniform over large scales and that the Earth occupies a typical region in the Universe (thecosmological principle). A wider but shallower survey was also made as part of theGreat Observatories Origins Deep Survey. In 2004 a deeper image, known as theHubble Ultra-Deep Field (HUDF), was constructed from a few months of light exposure. The HUDF image was at the time the most sensitiveastronomical image ever made at visible wavelengths, and it remained so until theHubble eXtreme Deep Field (XDF) was released in 2012.
One of the key aims of the astronomers who designed the Hubble Space Telescope was to use its highoptical resolution to study distant galaxies to a level of detail that was not possible from the ground. Positioned above theatmosphere, Hubble avoids atmosphericairglow allowing it to take more sensitivevisible andultraviolet light images than can be obtained withseeing-limited ground-based telescopes (when goodadaptive optics correction at visible wavelengths becomes possible, 10 m ground-based telescopes may become competitive). Although the telescope's mirror suffered fromspherical aberration when the telescope was launched in 1990, it could still be used to take images of more distant galaxies than had previously been obtainable. Becauselight takes billions of years to reach Earth from very distant galaxies, we see them as they were billions of years ago; thus, extending the scope of such research to increasingly distant galaxies allows a better understanding of how they evolve.[2]
After the spherical aberration was corrected duringSpace Shuttle missionSTS-61 in 1993,[4] the improved imaging capabilities of the telescope were used to study increasingly distant and faint galaxies. TheMedium Deep Survey (MDS) used the Wide Field and Planetary Camera 2 (WFPC2) to take deep images of random fields while other instruments were being used for scheduled observations. At the same time, other dedicated programs focused on galaxies that were already known through ground-based observation. All of these studies revealed substantial differences between the properties of galaxies today and those that existed several billion years ago.[5]
Up to 10% of the HST's observation time is designated as Director's Discretionary (DD) Time, and is typically awarded to astronomers who wish to study unexpected transient phenomena, such assupernovae. Once Hubble's corrective optics were shown to be performing well,Robert Williams, the then-director of theSpace Telescope Science Institute, decided to devote a substantial fraction of his DD time during 1995 to the study of distant galaxies. A special Institute Advisory Committee recommended that the WFPC2 be used to image a "typical" patch of sky at a highgalactic latitude, using severaloptical filters. Aworking group was set up to develop and implement the project.[6]
The field selected for the observations needed to fulfill several criteria. It had to be at a high galactic latitude becausedust and obscuring matter in the plane of theMilky Way's disc prevents observations of distant galaxies at low galactic latitudes (seeZone of Avoidance). The target field had to avoid known bright sources ofvisible light (such as foreground stars), andinfrared,ultraviolet, andX-ray emissions, to facilitate later studies at many wavelengths of the objects in the deep field, and also needed to be in a region with a low backgroundinfrared cirrus, the diffuse, wispy infrared emission believed to be caused by warm dust grains in cool clouds ofhydrogen gas (H I regions).[6]
These criteria restricted the field of potential target areas. It was decided that the target should be in Hubble's continuous viewing zones: the areas of sky that are notocculted by the Earth or themoon during Hubble's orbit.[6] The working group decided to concentrate on the northern continuous viewing zone, so that northern-hemisphere telescopes such as theKeck telescopes, theKitt Peak National Observatory telescopes, and theVery Large Array (VLA) could conduct follow-up observations.[7]
Twenty fields satisfying these criteria were identified, from which three optimal candidate fields were selected, all within the constellation ofUrsa Major.Radio snapshot observations with the VLA ruled out one of these fields because it contained a bright radio source, and the final decision between the other two[clarification needed] was made on the basis of the availability of guide stars near the field: Hubble observations normally require a pair of nearby stars on which the telescope's Fine Guidance Sensors can lock during an exposure, but given the importance of the HDF observations, the working group required a second set of back-up guide stars. The field that was eventually selected is located at aright ascension of12h 36m 49.4s and adeclination of +62° 12′ 58″;[6][7] it is about 2.6arcminutes in width,[2][8] or 1/12 the width of the Moon. The area is about 1/24,000,000 of the total area of the sky.
Once a field was selected, an observing strategy was developed. An important decision was to determine whichfilters the observations would use; WFPC2 is equipped with 48 filters, includingnarrowband filters isolating particularemission lines ofastrophysical interest, andbroadband filters useful for the study of the colors of stars and galaxies. The choice of filters to be used for the HDF depended on thethroughput of each filter—the total proportion of light that it allows through—and the spectral coverage available. Filters withbandpasses overlapping as little as possible were desirable.[6]
In the end, four broadband filters were chosen, centred atwavelengths of 300nm (near-ultraviolet), 450 nm (blue light), 606 nm (red light) and 814 nm (near-infrared). Because thequantum efficiency of Hubble's detectors at 300 nm wavelength is quite low, the noise in observations at this wavelength is primarily due toCCD noise rather than sky background; thus, these observations could be conducted at times when high background noise would have harmed the efficiency of observations in other passbands.[6]
Between December 18 and 28, 1995—during which time Hubble orbited the Earth about 150 times—342 images of the target area in the chosen filters were taken. The total exposure times at each wavelength were 42.7 hours (300 nm), 33.5 hours (450 nm), 30.3 hours (606 nm) and 34.3 hours (814 nm), divided into 342 individual exposures to prevent significant damage to individual images bycosmic rays, which cause bright streaks to appear when they strike CCD detectors. A further 10 Hubble orbits were used to make short exposures of flanking fields to aid follow-up observations by other instruments.[6]
The production of a final combined image at eachwavelength was a complex process. Brightpixels caused by cosmic ray impacts during exposures were removed by comparing exposures of equal length taken one after the other, and identifying pixels that were affected bycosmic rays in one exposure but not the other. Trails ofspace debris andartificial satellites were present in the original images, and were carefully removed.[6]
Scattered light from the Earth was evident in about a quarter of the data frames, creating a visible "X" pattern on the images. This was removed by taking an image affected by scattered light, aligning it with an unaffected image, and subtracting the unaffected image from the affected one. The resulting image was smoothed, and could then be subtracted from the bright frame. This procedure removed almost all of the scattered light from the affected images.[6]
Once the 342 individual images were cleaned of cosmic-ray hits and corrected for scattered light, they had to be combined. Scientists involved in the HDF observations pioneered a technique called 'drizzling', in which the pointing of the telescope was varied minutely between sets of exposures. Each pixel on the WFPC2 CCD chips recorded an area of sky 0.09arcseconds across, but by changing the direction in which the telescope was pointing by less than that between exposures, the resulting images were combined using sophisticated image-processing techniques to yield a final angular resolution better than this value. The HDF images produced at each wavelength had final pixel sizes of 0.03985 arcseconds.[6]
The data processing yielded fourmonochrome images (at 300 nm, 450 nm, 606 nm and 814 nm), one at each wavelength.[9] One image was designated as red (814 nm), the second as green (606 nm) and the third as blue (450 nm), and the three images were combined to give a color image.[3] Because the wavelengths at which the images were taken do not correspond to the wavelengths of red, green and blue light, the colors in the final image only give an approximate representation of the actual colors of the galaxies in the image; the choice of filters for the HDF (and the majority of Hubble images) was primarily designed to maximize the scientific utility of the observations rather than to create colors corresponding to what thehuman eye would actually perceive.[9]
The final images were released at a meeting of theAmerican Astronomical Society in January 1996,[10] and revealed a plethora of distant, faint galaxies. About 3,000 distinct galaxies could be identified in the images,[11] with bothirregular andspiral galaxies clearly visible, although some galaxies in the field are only a few pixels across. In all, the HDF is thought to contain fewer than twenty galactic foreground stars; by far the majority of objects in the field are distant galaxies.[12]
There are about fifty blue point-like objects in the HDF. Many seem to be associated with nearby galaxies, which together form chains and arcs: these are likely to be regions of intensestar formation. Others may be distantquasars. Astronomers initially ruled out the possibility that some of the point-like objects arewhite dwarfs, because they are too blue to be consistent with theories of white dwarf evolution prevalent at the time. However, more recent work has found that many white dwarfs become bluer as they age, lending support to the idea that the HDF might contain white dwarfs.[13]
The HDF data provided extremely rich material for cosmologists to analyse and by late 2014 the associated scientific paper for the image had received over 900 citations.[15] One of the most fundamental findings was the discovery of large numbers of galaxies with highredshift values.
As the Universe expands, more distant objects recede from the Earth faster, in what is called theHubble Flow. The light from very distant galaxies is significantly affected by thecosmological redshift. Whilequasars with high redshifts were known, very few galaxies with redshifts greater than one were known before the HDF images were produced.[10] The HDF, however, contained many galaxies with redshifts as high as six, corresponding to distances of about 12 billionlight-years. Due to redshift the most distant objects in the HDF (Lyman-break galaxies) are not actually visible in the Hubble images; they can only be detected in images of the HDF taken at longer wavelengths by ground-based telescopes.[16] One of the first observations planned for theJames Webb Space Telescope was a mid-infrared image of the Hubble Ultra-Deep Field.[17]
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The HDF galaxies contained a considerably larger proportion of disturbed and irregular galaxies than the local universe;[10] galaxy collisions and mergers were more common in the young universe as it was much smaller than today. It is believed that giantelliptical galaxies form when spirals and irregular galaxies collide.
The wealth of galaxies at different stages of their evolution also allowed astronomers to estimate the variation in the rate ofstar formation over the lifetime of the Universe. While estimates of the redshifts of HDF galaxies are somewhat crude, astronomers believe that star formation was occurring at its maximum rate 8–10 billion years ago, and has decreased by a factor of about 10 since then.[19]
Another important result from the HDF was the very small number of foreground stars present. For years astronomers had been puzzling over the nature ofdark matter, mass which seems to be undetectable but which observations implied made up about 85% of all matter in the Universe by mass.[20] One theory was that dark matter might consist of Massive Astrophysical Compact Halo Objects (MACHOs)—faint but massive objects such asred dwarfs andplanets in the outer regions of galaxies.[21] The HDF showed, however, that there were not significant numbers of red dwarfs in the outer parts of our galaxy.[10][12]
Very-high redshift objects (Lyman-break galaxies) cannot be seen in visible light and generally are detected ininfrared orsubmillimetre wavelength surveys of the HDF instead.[16] Observations with theInfrared Space Observatory (ISO) indicated infrared emission from 13 galaxies visible in the optical images, attributed to large quantities of dust associated with intense star formation.[22] Infrared observations have also been made with theSpitzer Space Telescope.[23] Submillimeter observations of the field have been made withSCUBA on theJames Clerk Maxwell Telescope, initially detecting 5 sources, although with very low resolution.[11] Observations have also been made with theSubaru telescope in Hawaii.[24]
X-ray observations by theChandra X-ray Observatory revealed six sources in the HDF, which were found to correspond to three elliptical galaxies, one spiral galaxy, oneactive galactic nucleus and one extremely red object, thought to be a distant galaxy containing a large amount ofdust absorbing its blue light emissions.[25]
Ground-based radio images taken using the VLA revealed seven radio sources in the HDF, all of which correspond to galaxies visible in the optical images.[26] The field has also been surveyed with theWesterbork Synthesis Radio Telescope and theMERLIN array of radio telescopes at 1.4 GHz;[27][28] the combination of VLA and MERLIN maps made at wavelengths of 3.5 and 20 cm have located 16 radio sources in the HDF-N field, with many more in the flanking fields.[11] Radio images of some individual sources in the field have been made with theEuropean VLBI Network at 1.6 GHz with a higher resolution than the Hubble maps.[29]
An HDF counterpart in the southern celestial hemisphere was created in 1998: theHDF-South (HDF-S).[30] Created using a similar observing strategy,[30] the HDF-S was very similar in appearance to the original HDF.[31] This supports thecosmological principle that at its largest scale the Universe ishomogeneous. The HDF-S survey used theSpace Telescope Imaging Spectrograph (STIS) and theNear Infrared Camera and Multi-Object Spectrometer (NICMOS) instruments installed on the HST in 1997; the region of the original Hubble Deep Field (HDF-N) has since been re-observed several times using WFPC2, as well as by the NICMOS and STIS instruments.[8][11] Severalsupernova events were detected by comparing the first and second epoch observations of the HDF-N.[11]
A wider survey, but less sensitive, was carried out as part of theGreat Observatories Origins Deep Survey; a section of this was then observed for longer to create theHubble Ultra-Deep Field, which was the most sensitive optical deep field image for years[32] until theHubble eXtreme Deep Field was completed in 2012.[33] Images from the Extreme Deep Field, or XDF, were released on September 26, 2012, to a number of media agencies. Images released in the XDF show galaxies which are now believed to have formed in the first 500 million years following the Big Bang.[34][35]
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