1080i, Broadcast standard
Within the designation "1080i", the i stands for interlaced scan. A frame of 1080i video consists of two sequential fields of 1920 horizontal and 540 vertical pixels. The first field consists of all odd-numbered TV lines and the second all even numbered lines. Consequently, the horizontal lines of pixels in each field are captured and displayed with a one-line vertical gap between them, so the lines of the next field can be interlaced between them, resulting in 1080 total lines.


1080i, Broadcast standard
1080i differs from 1080p, where the p stands for progressive scan, where all lines in a frame are captured at the same time. In native or pure 1080i, the two fields of a frame correspond to different instants (points in time), so motion portrayal is good (50 or 60 motion phases/second). This is true for interlaced video in general and can be easily observed in still images taken of fast motion scenes. However, when 1080p material is captured at 25 or 30 frames/second, it is converted to 1080i at 50 or 60 fields/second, respectively, for processing or broadcasting. In this situation both fields in a frame do correspond to the same instant. The field-to-instant relation is somewhat more complex for the case of 1080p at 24 frames/second converted to 1080i at 60 fields/second.


1080i, Broadcast standard
The field rate of 1080i is typically 60 Hz (i.e., 60 fields per second) for countries that use or used System M (NTSC and Brazilian PAL-M) as analog television system with 60 fields/sec (such as United States, Canada, Mexico, Japan, South Korea, Taiwan and Philippines), or 50 Hz for regions that use or used 625-lines (PAL or SECAM) television system with 50 fields/sec (such as most of Europe, most of Africa, China, India, Australia, New Zealand, Middle East, and others). Both field rates can be carried by major digital television broadcast formats such as ATSC, DVB, and ISDB-T International.


1080i, Broadcast standard
The frame rate can be implied by the context, while the field rate is generally specified after the letter i, such as "1080i60". In this case 1080i60 refers to 60 fields per second. The European Broadcasting Union (EBU) prefers to use the resolution and frame rate (not field rate) separated by a slash, as in 1080i/30 and 1080i/25, likewise 480i/30 and 576i/25. Resolutions of 1080i60 or 1080i50 often refers to 1080i/30 or 1080i/25 in EBU notation.


1080i, Broadcast standard
1080i is directly compatible with some CRT HDTVs on which it can be displayed natively in interlaced form, but for display on progressive-scan—e.g., most new LCD and plasma TVs, it must be deinterlaced. Depending on the television's video processing capabilities, the resulting video quality may vary, but may not necessarily suffer. For example, film material at 25fps may be deinterlaced from 1080i50 to restore a full 1080p resolution at the original frame rate without any loss. Preferably video material with 50 or 60 motion phases/second is to be converted to 50p or 60p before display.


1080i, Broadcast standard
Worldwide, most HD channels on satellite and cable broadcast in 1080i. In the United States, 1080i is the preferred format for most broadcasters, with Discovery, Inc., ViacomCBS, WarnerMedia, and Comcast owned networks broadcasting in the format, along with most smaller broadcasters. Only Fox- and Disney-owned television networks, along with MLB Network and a few other cable networks, use 720p as the preferred format for their networks; A+E Networks channels converted from 720p to 1080i sometime in 2013 due to acquired networks already transmitting in the 1080i format.


1080i, Broadcast standard
Many ABC affiliates owned by Hearst Television and former Belo Corporation stations owned by TEGNA, along with some individual affiliates of those three networks, air their signals in 1080i and upscale network programming for master control and transmission purposes, as most syndicated programming and advertising is produced and distributed in 1080i/p, removing a downscaling step to 720p. This also allows local newscasts on these ABC affiliates to be produced in the higher resolution (especially for  weather forecasting presentation purposes for map clarity) to match the picture quality of their 1080i competitors.


1080i, Broadcast standard
Some cameras and broadcast systems that use 1080 vertical lines per frame do not actually use the full 1920 pixels of a nominal 1080i picture for image capture and encoding. Common subsampling ratios include 3/4 (resulting in 1440x1080i frame resolution) and 1/2 (resulting in 960x1080i frame resolution). Where used, the lower horizontal resolution is scaled to capture or display a full-sized picture. Using half horizontal resolution and only one field of each frame (possibly with added anti-alias filtering or progressive capture) results in the format known as qHD, which has frame resolution 960x540 and 30 or 25 frames per second.


1080i, Broadcast standard
Due to the chosen 16x16 pixel size for a compressed video packet known as a macroblock as used in ITU H.261 to H.264 video standards, a 1080-line video must be encoded as 1088 lines and cropped to 1080 by the de-compressor. The 720-line video format divides perfectly by 16 and therefore does not require any lines to be wasted.


1080p
1080p (1920×1080 progressively displayed pixels; also known as Full HD or FHD, and BT.709) is a set of HDTV high-definition video modes characterized by 1,920 pixels displayed across the screen horizontally and 1,080 pixels down the screen vertically; the p stands for progressive scan, i.e. non-interlaced. The term usually assumes a widescreen aspect ratio of 16:9, implying a resolution of 2.1 megapixels. It is often marketed as Full HD or FHD, to contrast 1080p with 720p resolution screens. Although 1080p is sometimes informally referred to as 2K, these terms reflect two distinct technical standards, with differences including resolution and aspect ratio.


1080p
1080p video signals are supported by ATSC standards in the United States and DVB standards in Europe. Applications of the 1080p standard include television broadcasts, Blu-ray Discs, smartphones, Internet content such as YouTube videos and Netflix TV shows and movies, consumer-grade televisions and projectors, computer monitors and video game consoles. Small camcorders, smartphones and digital cameras can capture still and moving images in 1080p resolution.


1080p, Broadcasting standards
Any screen device that advertises 1080p typically refers to the ability to accept 1080p signals in native resolution format, which means there are a true 1920 pixels in width and 1080 pixels in height, and the display is not over-scanning, under-scanning, or reinterpreting the signal to a lower resolution. The HD ready 1080p logo program, by DIGITALEUROPE, requires that certified TV sets support 1080p 24 fps, 1080p 25 fps, 1080p 50 fps, and 1080p 60 fps formats, among other requirements, with fps meaning frames per second.


1080p, Broadcasting standards
For live broadcast applications, a high-definition progressive scan format operating at 1080p at 50 or 60 frames per second is currently being evaluated as a future standard for moving picture acquisition. Although 24 frames per second is used for shooting the movies. EBU has been endorsing 1080p50 as a future-proof production format because it improves resolution and requires no deinterlacing, allows broadcasting of standard 1080i50 and 720p50 signal alongside 1080p50 even in the current infrastructure and is compatible with DCI distribution formats.


1080p, Broadcasting standards
1080p50/p60 production format requires a whole new range of studio equipment including cameras, storage and editing systems, and contribution links (such as Dual-link HD-SDI and 3G-SDI) as it has doubled the data rate of current 50 or 60 fields interlaced 1920x1080 from 1.485 Gbit/s to nominally 3 Gbit/s using uncompressed RGB encoding. Most current revisions of SMPTE 372M, SMPTE 424M and EBU Tech 3299 require YCbCr color space and 4:2:2 chroma subsampling for transmitting 1080p50 (nominally 2.08 Gbit/s) and 1080p60 signal.


1080p, Broadcasting standards
Studies from 2009 show that for digital broadcasts compressed with H.264/AVC, transmission bandwidth savings of interlaced video over fully progressive video are minimal even when using twice the frame rate; i.e., 1080p50 signal (50 progressive frames per second) actually produces the same bit rate as 1080i50 signal (25 interlaced frames or 50 sub-fields per second).


1080p, Broadcasting standards, ATSC
In the United States, the original ATSC standards for HDTV supported 1080p video, but only at the frame rates of 23.976, 24, 25, 29.97 and 30 frames per second (colloquially known as 1080p24, 1080p25 and 1080p30). In July 2008, the ATSC standards were amended to include H.264/MPEG-4 AVC compression and 1080p at 50, 59.94 and 60 frames per second (1080p50 and 1080p60). Such frame rates require H.264/AVC High Profile Level 4.2, while standard HDTV frame rates only require Level 4.0. This update is not expected to result in widespread availability of 1080p60 programming, since most of the existing digital receivers in use would only be able to decode the older, less-efficient MPEG-2 codec, and because there is a limited amount of bandwidth for subchannels.


1080p, Broadcasting standards, DVB
In Europe, 1080p25 signals have been supported by the DVB suite of broadcasting standards. The 1080p50 format is considered to be a future-proof production format and, eventually, a future broadcasting format. 1080p50 broadcasting should require the same bandwidth as 1080i50 signal and only 15–20% more than that of 720p50 signal due to increased compression efficiency, though 1080p50 production requires more bandwidth or more efficient codecs such as JPEG 2000, high-bitrate MPEG-2, or H.264/AVC and HEVC.


1080p, Broadcasting standards, DVB
In September 2009, ETSI and EBU, the maintainers of the DVB suite, added support for 1080p50 signal coded with MPEG-4 AVC High Profile Level 4.2 with Scalable Video Coding extensions or VC-1 Advanced Profile compression; DVB also supports 1080p encoded at ATSC frame rates of 23.976, 24, 29.97, 30, 59.94 and 60.


1080p, Broadcasting standards, DVB
EBU requires that legacy MPEG-4 AVC decoders should avoid crashing in the presence of SVC or 1080p50 (and higher resolution) packets. SVC enables forward compatibility with 1080p50 and 1080p60 broadcasting for older MPEG-4 AVC receivers, so they will only recognize baseline SVC stream coded at a lower resolution or frame rate (such as 720p60 or 1080i60) and will gracefully ignore additional packets, while newer hardware will be able to decode full-resolution signal (such as 1080p60).


1080p, Broadcasting standards, DVB
In June 2016, EBU  announced the "Advanced 1080p" format which will include UHD Phase A features such as high-dynamic-range video (using PQ and HLG) at 10 and 12 bit color and BT.2020 color gamut, and optional HFR 100, 120/1.001 and 120 Hz; an advanced 1080p video stream can be encoded alongside baseline HDTV or UHDTV signal using Scalable HEVC. The ITU-T BT.2100 standard that includes Advanced 1080p video was subsequently published in July 2016.


1080p, Resolutions
In practice, 1080p typically refers to a 1920×1080 raster with a 16:9 picture aspect ratio. The following is a list of other resolutions with a picture height of 1080 lines that are sometimes referred as 1080p.


1080p, Availability, Broadcasts
In the United States, 1080p over-the-air broadcasts are currently available in select stations in some cities in the US via ATSC 3.0 multiplex stations where as ATSC 3.0 is currently rolling out throughout the U.S. The majority of the stations that broadcast at 1080p are CBS and NBC stations and affiliates. All other stations do not broadcast at 1080p and usually broadcast at 720p60 (including when simulcasting in ATSC 3.0) or 1080i60 (outside of ATSC 3.0) encoded with MPEG-2. There is also technical restrictions with ATSC 3.0 multiplex stations that prevent stations from airing at 1080p.


1080p, Availability, Broadcasts
While converting to ATSC 3.0 is voluntary by TV Stations, there is no word when any of the major networks will consider airing at 1080p in the foreseeable future on a national scale, although they are required to broadcast ATSC signals for at least five years thereafter. However, satellite services (e.g., DirecTV, XstreamHD and Dish Network) utilize the 1080p/24-30 format with MPEG-4 AVC/H.264 encoding for pay-per-view movies that are downloaded in advance via satellite or on-demand via broadband.


1080p, Availability, Broadcasts
At this time, no pay service channel such as USA, HDNET, etc. nor premium movie channel such as HBO, etc., stream their services live to their distributors (MVPD) in this format because many MVPDs, especially DBS and cable, do not have sufficient bandwidth to provide the format streaming live to their subscribers without negatively impacting their current services.


1080p, Availability, Broadcasts
For material that originates from a progressive scanned 24 frame/s source (such as film), MPEG-2 lets the video be coded as 1080p24, irrespective of the final output format. These progressively-coded frames are tagged with metadata (literally, fields of the PICTURE header) instructing a decoder how to perform a 3:2 pulldown to interlace them. While the formal output of the MPEG-2 decoding process from such stations is 1080i60, the actual content is coded as 1080p24 and can be viewed as such (using a process known as inverse telecine) since no information is lost even when the broadcaster performs the 3:2 pulldown.


1080p, Availability, Broadcasts
In June 2016, Germany commenced terrestrial broadcasts of eight 1080p50 high-definition channels, using DVB-T2 protocol with HEVC encoding; a total of 40 channels will be available by March 2017.


1080p, Availability, Blu-ray Disc
Blu-ray Discs are able to hold 1080p HD content, and most movies released on Blu-ray Disc produce a full 1080p HD picture when the player is connected to a 1080p HDTV via an HDMI cable. The Blu-ray Disc video specification allows encoding of 1080p23.976, 1080p24, 1080i50, and 1080i59.94. Generally this type of video runs at 30 to 40 megabits per second, compared to the 3.5 megabits per second for conventional standard definition broadcasts.


1080p, Availability, Smartphones
Smartphones with 1080p FullHD display have been available on the market since 2012. As of late-2014, it is the standard for mid-range to high-end smartphones and many of the flagship devices of 2014 used even higher resolutions, either Quad HD (1440p) or Ultra HD (2160p) resolutions.


1080p, Availability, Internet content
Several websites, including YouTube, allow videos to be uploaded in the 1080p format. YouTube streams 1080p content at approximately 4 megabits per second compared to Blu-ray's 30 to 40 megabits per second. Digital distribution services like Hulu and HBO Max also deliver 1080p content, such as movies available on Blu-ray Disc or from broadcast sources. This can include distribution services like peer-to-peer websites and public or private tracking networks. Netflix has been offering high quality 1080p content in the US and other countries through select internet providers since 2013.


1080p, Availability, Consumer televisions and projectors
As of 2012, most consumer televisions being sold provide 1080p inputs, mainly via HDMI, and support full high-definition resolutions. 1080p resolution is available in all types of television, including plasma, LCD, DLP front and rear projection and LCD projection. For displaying film-based 1080i60 signals, a scheme called 3:2 pulldown reversal (reverse telecine) is beginning to appear in some newer 1080p displays, which can produce a true 1080p quality image from film-based 1080i60 programs. Similarly, 25fps content broadcast at 1080i50 may be deinterlaced to 1080p content with no loss of quality or resolution.


1080p, Availability, Consumer televisions and projectors
AV equipment manufacturers have adopted the term Full HD to mean a set can display all available HD resolutions up to 1080p. The term is misleading, however, because it does not guarantee the set is capable of rendering digital video at all frame rates encoded in source files with 1920 X 1080 pixel  resolution. Most notably, a "Full HD" set is not guaranteed to support the 1080p24 format, leading to consumer confusion. DigitalEurope (formerly EICTA) maintains the HD ready 1080p logo program that requires the certified TV sets to support 1080p24, 1080p50, and 1080p60, without overscan/underscan and picture distortion.


1080p, Availability, Computer monitors
Most widescreen cathode-ray tube (CRT) and liquid-crystal display (LCD) monitors can natively display 1080p content. For example, widescreen WUXGA monitors support 1920x1200 resolution, which can display a pixel for pixel reproduction of the 1080p (1920×1080) format. Additionally, many 23, 24, and 27-inch (690 mm) widescreen LCD monitors use 1920×1200 as their native resolution; 30 inch displays can display beyond 1080p at up to 2560×1600 (1600p). Many 27" monitors have native resolutions of 2560×1440 and hence operate at 1440p.


1080p, Availability, Computer monitors, Laptops
Sony has their first and formerly VAIO 1080p laptop, VPCCB17FG, in 2011, and since Asus also has their first 4K laptop GL502 which was formerly branded Republic of Gamers in 2017, 1080p has also become the nowadays lowest standard for laptops.


1080p, Availability, Video game consoles
Whilst Microsoft's original Xbox, launched as part of the sixth generation of video game consoles in 2001, could support a 1080i output in limited circumstances, support for 1080p began with the launch of the seventh generation of home video game consoles in 2005. Both the Xbox 360 and PlayStation 3 were capable of outputting at 1080p, with only the Nintendo Wii unable to support the resolution. All home video game consoles launched as part of the eighth generation, which began in 2012 with the launch of the Wii U, were capable of 1080p outputs. Mid


1080p, Availability, Video game consoles
-generation hardware revisions and new models introduced by Sony and Microsoft to their respective PlayStation 4 and Xbox One consoles added the capability of outputting at 4K UHD — well beyond 1080p. Moreover, this mid-generational improvement in computing power also represented a leap in the ability of video game consoles to render gaming content at a 1080p resolution or higher, rather than relying on upscaling. This trend continued with the launch of the current ninth generation of video game consoles in 2020, in which Sony's PlayStation 5 and Microsoft's Xbox Series X also introduced 8K UHD support.


1080p, Availability, Cameras
Many cameras—professional and consumer still, action and video cameras, including DSLR cameras—and other devices with built-in cameras such as laptops, smartphones and tablet computers, can capture 1080p24, 1080p25, 1080p30 or 1080p60 video, often encoding it in progressive segmented frame format.


1080s
The 1080s was a decade of the Julian Calendar which began on January 1, 1080, and ended on December 31, 1089.


1080s BC
The 1080s BC was a decade which lasted from 1089 BC to 1080 BC.


1080s in art
The decade of the 1080s in art involved some significant events.


1080s in poetry
Nationality words link to articles with information on the nation's poetry or literature (for instance, Irish or France).


1080s in poetry, Births
Death years link to the corresponding "[year] in poetry" article. There are conflicting or unreliable sources for the birth years of many people born in this period; where sources conflict, the poet is listed again and the conflict is noted:


1080s in poetry, Deaths
Birth years link to the corresponding "[year] in poetry" article:


1080° Avalanche
1080° Avalanche is a snowboarding video game for the GameCube, developed by Nintendo's in-house development studio, Nintendo Software Technology, and published by Nintendo. It released in Europe on November 28, 2003, in North America on December 1, 2003, and in Japan on January 22, 2004. Avalanche is a sequel to the 1998 video game 1080° Snowboarding for the Nintendo 64.


1080° Avalanche
In contrast to similar snowboarding games such as the SSX series, the game emphasizes racing rather than doing tricks. Gameplay can output in 480p and Dolby Pro Logic II and supports four players on one GameCube as well as LAN play with up to four GameCubes.


1080° Avalanche, Gameplay
Similar to 1080° Snowboarding, gameplay focuses on racing more than performing stunts. There are differences between this game and Snowboarding, with one being the Avalanche - the final event of every Match Race challenge is a daredevil run through an avalanche-prone trail where the player has to outrun an avalanche that starts in the middle of the run or even at the very start. In over 20 courses, the players can compete in the main Match mode, along with Trick Attack, Time Trial and Gate modes.


1080° Avalanche, Gameplay
Unlike the first game, each rider has unique boards, and up to three new boards for each character can be unlocked along with bonus boards, which are surreal objects replacing the snowboard, such as a penguin or a NES controller.


1080° Avalanche, Development and release
In 1999, a sequel to 1080° Snowboarding was announced for the Nintendo 64. Second-party studio Left Field was responsible for development, but when the studio revoked its status as a second-party studio to focus on multi-format titles, the game failed to materialize. Development of the game was handed to Nintendo's American development studio, Nintendo Software Technology Corporation (NST), who would migrate the title to Nintendo's newest venture, the GameCube.


1080° Avalanche, Development and release
1080°: Avalanche was released in both single-disc and double-disc versions. The second disc is a standard miniDVD featuring a half-hour of snowboarding footage alongside gameplay footage set to soundtracks from the game. This version was exclusively available at Wal-Mart and can be differentiated by the presence of a red sash on the front cover.


1080° Avalanche, Reception
It received a score of 7.5/7/5.5 from Electronic Gaming Monthly: Dan Hsu, the first reviewer, said: "You can't beat its cornea-stripping sense of speed". While Hsu found fault with the game's trick system, it was severely criticized by third reviewer Shawn Elliott, who believed that "Avalanche [...] can't compete with SSX 3".


1080° Snowboarding
1080° Snowboarding is a 1998 snowboarding video game developed by Nintendo EAD and published by Nintendo. It was released for the Nintendo 64 and re-released in 2008 for the Wii's Virtual Console. In the game, the player controls one of five snowboarders from a third-person perspective, using a combination of buttons to jump and perform tricks over eight levels.


1080° Snowboarding
1080° was announced in November 1997 and developed over the course of nine months; it garnered critical acclaim and won an Interactive Achievement Award from the Academy of Interactive Arts & Sciences. 1080° sold over two million units, and a second installment, 1080° Avalanche, was released for the GameCube in November 2003.


1080° Snowboarding, Gameplay
The player controls a snowboarder in one of several modes. 1080° has two trick modes (trick attack and contest), three race modes (race, time attack, and 2 players), a training mode, and an options mode. The objective of the game is either to arrive quickly at a level's finish line or to receive maximum points for trick combinations.


1080° Snowboarding, Gameplay
In 1080°'s two trick modes, trick attack and contest, players accrue points from completed tricks. In contest mode, players perform tricks and snowboard past flags for points. Trick attack mode requires players to perform a series of tricks throughout a designated level. The game features 24 tricks and 5 secret tricks, all of which are performed by using a combination of circular positions of the control stick, the R button, the Z button and the B button; point values are allocated based on complexity, combos, and required time. The two types of tricks are grab tricks, in which the board is grabbed in a specific way, or spin tricks, in which the snowboarder spins the board a certain number of degrees. The 1080° spin requires nine actions, the most of any trick in the game.


1080° Snowboarding, Gameplay
1080° has three race modes; in these modes, victory can be achieved by taking separate routes within a course and balancing the snowboarder after a jump to avoid speed loss. Tricks are scored in race modes, but do not count toward victory. In match race mode, the player competes in a series of races against AI-controlled snowboarders. The game times the player throughout the level and players receive a damage meter which fills if the snowboarder falls down or is knocked over. The difficulty level in match races can be set to normal, hard, or expert, adjusting the complexity and number of races. If the player fails at defeating an AI competitor, they must retire. The player is given three chances to beat the computer before the game is over.


1080° Snowboarding, Gameplay
Players may initially choose from five snowboarding characters: two from Japan, and one each from Canada, the United States, and the United Kingdom. Each snowboarder has different abilities and is suited for different levels and modes, since each has varying statistics in fields such as technique, speed, and weight. Three additional snowboarders are unlocked by completing certain game levels and modes. Eight snowboards are initially available for every character, and one additional snowboard may be unlocked later in the game. Each board also excels in different situations, since each has different strengths in categories such as balance and edge control.


1080° Snowboarding, Development
1080°'s release was announced on 21 November 1997 at Nintendo's Space World trade show; the game's working title had previously been Vertical Edge Snowboarding. 1080° was one of several snowboarding games released for the Nintendo 64 in 1998, others being Big Mountain 2000 and Snowboard Kids. Before the game's release, journalists were able to play 1080° at the January 1998 Nintendo Gamers' Summit.


1080° Snowboarding, Development
1080° was directed by Masamachi Abe and Misthuro Tanako, programmed by Englishmen Giles Goddard and Colin Reed, developed and published by Nintendo, and produced by Shigeru Miyamoto. Abe had previously directed Tekken 3 for Namco. Goddard had previously programmed the Mario face in Super Mario 64, which was released two years prior to critical acclaim and was a huge commercial success, while Reed had programmed Stunt Race FX. When developing 1080°, Goddard and Reed used a technique called "skinning" to eliminate joints between the polygons composing the characters.


1080° Snowboarding, Development
Their programming used a combination of standard animation and inverse kinematics, creating characters whose appearance during collisions is affected by what object is hit, what direction the collision occurs in, and the speed at which the collision takes place. Tommy Hilfiger outfits and Lamar snowboards appear throughout 1080° as product placement. 1080°'s soundtrack of "techno and rappy beats" with "thrashy, foozed-out vocals" was composed by Kenta Nagata.


1080° Snowboarding, Development
1080°'s development took place from April or May 1997 to March 1998. The game was released on 28 February 1998 in Japan and on 1 April in North America. Nintendo delayed the game's European release because they hoped to boost sales with a winter release; 1080° was eventually released on 30 November in Europe and the PAL region.


1080° Snowboarding, Reception
1080° Snowboarding received "generally favorable reviews", just two points shy of "universal acclaim", according to review aggregator website Metacritic. In Japan, Famitsu gave it a score of 31 out of 40. Nintendo Power gave the Japanese import a favorable review, over a month before it was released Stateside. It was called "one of the best values in both sports and racing gaming" by Josh Smith of GameSpot. 1080° Snowboarding has been perceived to be a leader among snowboarding titles at the time, with IGN's Levi Buchanan stating: "Every single snowboarding game that followed 1080 borrows from Nintendo's formula". Edge hailed it as the "most convincing video game emulation of the snowboarding experience so far" with an "atmosphere of sobriety" unlike any other Nintendo game at the time.


1080° Snowboarding, Reception
The game's graphics were of the highest quality for the Nintendo 64 at the time. Smith praised general aspects of the game's graphics such as their crispness, detail, smoothness, and lack of polygon dropout. Reviewers praised the game's camera use, the game's "very solid" physics model, the impression of racers' speed, and the game's snow effects (sun reflected in the snow as appropriate, and fluffy snow and packed snow appeared and behaved differently). Graphical faults included occasional pop-up, misplaced shadows, and lag when racers passed through on-track trees; these problems were generally identified as minor.


1080° Snowboarding, Reception
Although writing a positive review, Edge found faults in the game's AI, saying the game suffered from "cheating" CPU opponents. They criticized the AI's simplicity and ability to quickly catch up to the player near the end of a race; they also noted the AI's "limited series of predetermined routes" and the possibility of a player learning where and when an AI falls over, "offering an opportunity to pass [the computer], but conveying little satisfaction with it". Edge also said the PAL release delay "is frankly ludicrous". They believed that, due to Nintendo's slump of noteworthy releases, "any quality title is likely to top the charts with little difficulty".


1080° Snowboarding, Reception
Next Generation said: "With 1080° Snowboarding, Nintendo delivers another system seller and once again sets the standard for an entire genre". Kevin Cheung of Hyper gave the game 90%: "There is little else more to say save that 1080 captures the true essence of the thrill of snowbaording. [ ...] Just as Waverace [sic] brought a new dimension to water-based racing, 1080 brings N64 owners an equally innovative game".


1080° Snowboarding, Reception
Writing for AllGame, Shawn Sackenheim considered the "highly technical" control scheme of 1080° Snowboarding one of the game's strengths despite its initial difficulty. Alex Huhtala of Computer and Video Games positively reviewed the control scheme, but disagreed on its difficulty, noting "the controls have been implemented so brilliantly that you're able to play perfectly well with just one hand on the stick and Z button". GameSpot called the game's control "thoroughly involving" and said that "[t]he crouch move alone –  which makes for supertight turns –  makes this fun to play". The music was also generally praised, with Matt Casamassina of IGN calling it "a shining example of what can be achieved on the format" and Sackenheim calling it "one of the best N64 soundtracks to date". Sackenheim also praised the game's sound effects.


1080° Snowboarding, Reception
In a retrospective review by the Official Nintendo Magazine in 2006, Steve Jarratt commented that 1080° Snowboarding "boasted the best video game representation of snow" and was complemented by "swooshy" sound effects. Positive comments were also made about handling and the quality of the multiplayer. In summary, Jarratt believed "this was a straight-up snowboarder, stunt-free but fast and fun". The magazine also ranked it the 87th best game available on Nintendo platforms. The staff felt it was the most realistic snowboarding game ever made.


1080° Snowboarding, Reception
The game won the Academy of Interactive Arts & Sciences' 1999 Console Sports Game of the Year award.


1080° Snowboarding, Reception
PC Data, which tracked sales in the United States, reported that 1080° Snowboarding sold 817,529 units and earned $40.9 million in revenues by the end of 1998. This made it the country's seventh-best-selling Nintendo 64 release of the year. The game ultimately sold 1,230,000 units in the United States, and over 23,000 in Japan. It did not, however, match the success of the developers' first game, Wave Race 64 which sold 1,950,000 units in the United States and 154,000 in Japan. 1080° Snowboarding was re-released on the Wii's Virtual Console service in 2008.


1080° Snowboarding, Sequel
1080° Avalanche, a sequel to 1080° Snowboarding, was released for the GameCube in 2003. Greg Kasarvin of GameSpot gave the sequel a harsher critical reception due to "frame rate issues and limited gameplay".


1081
Year 1081 (MLXXXI) was a common year starting on Friday (link will display the full calendar) of the Julian calendar.


1081 Reseda
1081 Reseda (prov. designation: 1927 QF) is a dark background asteroid from the outer regions of the asteroid belt. It was discovered on 31 August 1927, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid has a rotation period of 7.3 hours and measures approximately 37 kilometers (23 miles) in diameter. It was named after the herbaceous plant Reseda.


1081 Reseda, Orbit and classification
Reseda is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.7–3.6 AU once every 5 years and 6 months (1,997 days; semi-major axis of 3.10 AU). Its orbit has an eccentricity of 0.15 and an inclination of 4° with respect to the ecliptic. The body's observation arc begins at Heidelberg in September 1927, or 26 days after its official discovery observation.


1081 Reseda, Naming
This minor planet was named after the herbaceous plant Reseda (also known as "weld", "dyer's rocket" and "bastard rocket") a genus of Old World herbs of the mignonette family. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 102).


1081 Reseda, Naming, Reinmuth's flowers
Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200). This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants).


1081 Reseda, Physical characteristics, Rotation period
In August 2008, a rotational lightcurve of Reseda was obtained from photometric observations. Lightcurve analysis gave a well-defined rotation period of 7.3002 hours with a brightness amplitude of 0.34 magnitude (U=3).


1081 Reseda, Physical characteristics, Poles
A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database, gave a concurring period of 7.30136 hours, as well as two spin axis of (92.0°, −69.0°) and (256.0°, −76.0°) in ecliptic coordinates (λ, β).


1081 Reseda, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Reseda measures between 31.60 and 40.462 kilometers in diameter and its surface has an albedo between 0.0326 and 0.09. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0488 and a diameter of 37.97 kilometers based on an absolute magnitude of 11.0.


1082
Year 1082 (MLXXXII) was a common year starting on Saturday (link will display the full calendar) of the Julian calendar.


1082 Pirola
1082 Pirola /ˈpɪrələ/ is a dark Themistian asteroid from the outer regions of the asteroid belt. It was discovered on 28 October 1927, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in Germany, and assigned the provisional designation 1927 UC. The carbonaceous C-type asteroid has a rotation period of 15.9 hours and measures approximately 41 kilometers (25 miles) in diameter. It was named after the herbaceous plant Pyrola (wintergreen).


1082 Pirola, Orbit and classification
When applying the hierarchical clustering method to its proper orbital elements, Pirola is a Themistian asteroid that belongs to the Themis family (602), a large family of nearly 6,000 known carbonaceous asteroids, named after 24 Themis. It orbits the Sun in the outer main belt at a distance of 2.6–3.7 AU once every 5 years and 6 months (2,013 days; semi-major axis of 3.12 AU). Its orbit has an eccentricity of 0.18 and an inclination of 2° with respect to the ecliptic. The asteroid was first identified as A916 UP at Simeiz Observatory in October 1916. The body's observation arc begins with its official discovery observation at Heidelberg in October 1927.


1082 Pirola, Naming
This minor planet was named after Pyrola, also known as wintergreen, a herbaceous plant (mostly evergreen), that belongs to the flowering herbs. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 102).


1082 Pirola, Naming, Reinmuth's flowers
Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200). This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants).


1082 Pirola, Physical characteristics
In the Tholen classification, Pirola is a carbonaceous C-type asteroid, which matches the overall spectral type of the Themis family.


1082 Pirola, Physical characteristics, Rotation period
In 2010, three rotational lightcurves of Pirola were obtained from photometric observations. Lightcurve analysis gave a rotation period of 15.85, 15.851 and 15.8525 hours with a brightness amplitude between 0.53 and 0.62 magnitude (U=3-/2/3).


1082 Pirola, Physical characteristics, Rotation period
A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database, gave a concurring period of 15.8540 hours, as well as two spin axis of (123.0°, −42.0°) and (300.0°, −38.0°) in ecliptic coordinates (λ, β).


1082 Pirola, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Pirola measures between 37.363 and 44.67 kilometers in diameter and its surface has an albedo between 0.052 and 0.0867. The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0655 and a diameter of 41.06 kilometers based on an absolute magnitude of 10.51.


1083
Year 1083 (MLXXXIII) was a common year starting on Sunday (link will display the full calendar) of the Julian calendar.


1083 Salvia
1083 Salvia (prov. designation: 1928 BC) is a stony background asteroid from the inner regions of the asteroid belt. It was discovered on 26 January 1928, by astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The assumed S-type asteroid has a rotation period of 4.2 hours and measures approximately 10 kilometers (6.2 miles) in diameter. It was named after the flowering plant Salvia (sage).


1083 Salvia, Orbit and classification
Located in the region of the Flora family, Salvia is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.9–2.8 AU once every 3 years and 7 months (1,298 days; semi-major axis of 2.33 AU). Its orbit has an eccentricity of 0.18 and an inclination of 5° with respect to the ecliptic. The asteroid was first observed as A910 AA at Heidelberg Observatory on 7 January 1910, where the body's observation arc begins 18 years later, with its official discovery observation on 26 January 1928.


1083 Salvia, Naming
This minor planet was named after the flowering plant Salvia (sage), a genus of herbs or shrubs that belong to the mint family. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 102).


1083 Salvia, Naming, Reinmuth's flowers
Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200). This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants).


1083 Salvia, Physical characteristics
Salvia is an assumed stony S-type asteroid, which corresponds to its observed albedo (see below).


1083 Salvia, Physical characteristics, Rotation period and poles
In March 1992, a rotational lightcurve of Salvia was obtained from photometric observations by Polish astronomer Wiesław Wiśniewski. Lightcurve analysis gave a well-defined rotation period of 4.23 hours with a brightness amplitude of 0.61 magnitude (U=3). A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database, gave a concurring period of 4.281429±0.000001 hours, as well as two spin axis of (165.0°, −59.0°) and (358.0°, −58.0°) in ecliptic coordinates (λ, β).


1083 Salvia, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), Salvia measures between 8.927 and 10.283 kilometers in diameter and its surface has an albedo between 0.2103 and 0.2184. The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE data, that is an albedo of 0.2103 and a diameter of 10.28 kilometers based on an absolute magnitude of 12.25.


10830 Desforges
10830 Desforges, provisional designation 1993 UT6, is a background or Eunomian asteroid from the central regions of the asteroid belt, approximately 7 kilometers (4 miles) in diameter. It was discovered on 20 October 1993, by Belgian astronomer Eric Elst at the La Silla Observatory in northern Chile. The likely elongated S-type asteroid has a rotation period of 8.8 hours. It was named after French priest and aviation visionary Jacques Desforges.


10830 Desforges, Orbit and classification
Desforges is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Eunomia family (502), a prominent family of stony S-type asteroid and the largest one in the intermediate main belt with more than 5,000 members.


10830 Desforges, Orbit and classification
It orbits the Sun in the central main-belt at a distance of 2.2–3.1 AU once every 4 years and 4 months (1,585 days; semi-major axis of 2.66 AU). Its orbit has an eccentricity of 0.18 and an inclination of 11° with respect to the ecliptic. The body's observation arc begins with its first observations as 1982 FS2 at Klet Observatory in March 1982, more than 11 years prior to its official discovery observation at La Silla.


10830 Desforges, Physical characteristics
Desforges is an assumed stony S-type asteroid, which is the overall spectral type for members of the Eunomia family. Observations with the Wide-field Infrared Survey Explorer (WISE), however, gave a low geometric albedo more typical for an X- or C-type asteroid (see below).


10830 Desforges, Physical characteristics, Rotation period
In August 2010, a rotational lightcurve of Desforges was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 8.804 hours with a high brightness amplitude of 0.69 magnitude, which indicates that the body has a non-spherical shape (U=2).


10830 Desforges, Physical characteristics, Diameter and albedo
According to the survey carried out by the NEOWISE mission of NASA's WISE telescope, Desforges measures between 7.692 and 9.390 kilometers in diameter and its surface has an albedo between 0.0635 and 0.080.


10830 Desforges, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.21 – derived from the Eunomia family's parent body, 15 Eunomia – and calculates a diameter of 4.21 kilometers based on an absolute magnitude of 14.19.


10830 Desforges, Naming
This minor planet was named after a French priest Jacques Desforges (1723–1791), who was imprisoned for eight months in 1758 in the Bastille, during which time he planned the construction of a flying machine. The official naming citation was published by the Minor Planet Center on 18 March 2003 (M.P.C. 48156).


1084
Year 1084 (MLXXXIV) was a leap year starting on Monday (link will display the full calendar) of the Julian calendar.


1084 Tamariwa
1084 Tamariwa, provisional designation 1926 CC, is a carbonaceous background asteroid approximately 27 kilometres in diameter from the central regions of the asteroid belt. It was discovered on 12 February 1926, by Soviet astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. The asteroid was named after female paratrooper Tamara Ivanova, who died at an early age.


1084 Tamariwa, Orbit and classification
Tamariwa is a non-family asteroid from the main belt's background population. It orbits the Sun in the central asteroid belt at a distance of 2.3–3.0 AU once every 4 years and 5 months (1,610 days; semi-major axis of 2.69 AU). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic.


1084 Tamariwa, Orbit and classification
The body's observation arc begins at Simeiz with its identification as 1927 JB in May 1927, more than 14 months after its official discovery observation.


1084 Tamariwa, Physical characteristics, Rotation period
Several rotational lightcurves of Tamariwa with a rotation period between 6.153 and 7.08 hours have been obtained from photometric observations since 1984. Analysis of the best-rated lightcurve by French amateur astronomer Pierre Antonini gave a period of 6.1961 hours with a brightness amplitude of 0.42 magnitude (U=3).


1084 Tamariwa, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Tamariwa measures between 24.71 and 30.681 kilometers in diameter and its surface has an albedo between 0.0916 and 0.15.


1084 Tamariwa, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.1165 and a diameter of 27.19 kilometers based on an absolute magnitude of 10.78.


1084 Tamariwa, Naming
This minor planet was named "Tamariwa" after Soviet parachutist Tamara Ivanova (1912–1936). The minor planets 1062 Ljuba and 1086 Nata were also named after Soviet female paratroopers Lyuba Berlin (1915–1936) and Nata Babushkina (1915–1936), respectively.


1085
Year 1085 (MLXXXV) was a common year starting on Wednesday (link will display the full calendar) of the Julian calendar.


1085 Amaryllis
1085 Amaryllis /æməˈrɪlɪs/, provisional designation 1927 QH, is a background asteroid from the outer regions of the asteroid belt, approximately 69 kilometers in diameter. It was discovered on 31 August 1927, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after the flowering planet Amaryllis.


1085 Amaryllis, Orbit and classification
Amaryllis is a non-family asteroid from the main belt's background population. It orbits the Sun in the outer asteroid belt at a distance of 3.1–3.3 AU once every 5 years and 8 months (2,076 days). Its orbit has an eccentricity of 0.04 and an inclination of 7° with respect to the ecliptic.


1085 Amaryllis, Orbit and classification
The asteroid was first identified as A908 HB at Taunton Observatory (803) in April 1908. A few days later, the body's observation arc begins at the United States Naval Observatory  (786) in May 1908, or more than 19 years prior to its official discovery observation at Heidelberg.


1085 Amaryllis, Physical characteristics
Amaryllis has been characterized as an X-type asteroid by Pan-STARRS photometric survey. It is also an assumed carbonaceous C-type asteroid.


1085 Amaryllis, Physical characteristics, Rotation period
In March 2004, a first rotational lightcurve of Amaryllis was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a rotation period of 18.2 hours with a brightness variation of 0.20 magnitude (U=2). In May 2016, the Spanish amateur astronomer group OBAS (Asteroid Observers, Spanish: Observadores de Asteroids) measured a refined period of 18.111 hours with an amplitude of 0.19 magnitude (U=3-).


1085 Amaryllis, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Amaryllis measures between 65.55 and 72.93 kilometers in diameter and its surface has an albedo between 0.04 and 0.067.


1085 Amaryllis, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0437 and a diameter of 69.68 kilometers based on an absolute magnitude of 9.8.


1085 Amaryllis, Naming
This minor planet was named after the flowering planet Amaryllis, also known as belladonna lily, Jersey lily, naked lady, or amarillo. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 102).


1085 Amaryllis, Naming, Reinmuth's flowers
Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200) and also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were named after plants, in particular flowering plants (also see list of minor planets named after animals and plants § Plants).


1086
Year 1086 (MLXXXVI) was a common year starting on Thursday (link will display the full calendar) of the Julian calendar.


1086 Nata
1086 Nata, provisional designation 1927 QL, is a carbonaceous Veritasian asteroid from the outer regions of the asteroid belt, approximately 68 kilometers in diameter. It was discovered on 25 August 1927, by Russian astronomers Sergey Belyavsky and Nikolaj Ivanov at the Simeiz Observatory on the Crimean peninsula. The asteroid was named in memory of Soviet female parachutist Nata Babushkina (1915–1936).


1086 Nata, Orbit and classification
Nata is a member of the Veritas family, a young family of carbonaceous asteroids, that formed approximately 8.5±0.5 million years ago. The family is named after 490 Veritas and consists of nearly 1,300 members.


1086 Nata, Orbit and classification
Nata orbits the Sun in the outer main-belt at a distance of 3.0–3.3 AU once every 5 years and 7 months (2,054 days). Its orbit has an eccentricity of 0.05 and an inclination of 8° with respect to the ecliptic.


1086 Nata, Orbit and classification
The body's observation arc begins with its first identification as A900 YB at Heidelberg Observatory in December 1900, almost 27 years prior to its official discovery observation at Simeiz.


1086 Nata, Physical characteristics
In the SMASS classification, Nata is a Ch-subtype, a "hydrated" carbonaceous C-type asteroid.


1086 Nata, Physical characteristics, Rotation period
In November 2011, a rotational lightcurve of Nata was obtained from photometric observations by American astronomer Edwin E. Sheridan at the Crescent Butte Observatory (682). Lightcurve analysis gave a rotation period of 18.074 hours with a brightness amplitude of 0.17 magnitude (U=2).


1086 Nata, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Spitzer Space Telescope, the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Nata measures between 66.27 and 79.867 kilometers in diameter  and its surface has an albedo between 0.04 and 0.0767.


1086 Nata, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0641 and a diameter of 66.10 kilometers based on an absolute magnitude of 9.5.


1086 Nata, Naming
This minor planet was named in memory of Nadezhda Vasilievna Babushkina (1915–1936), nicknamed "Nata", a Soviet female parachutist who died in an accident at the age of 21. The minor planets (1062) and (1084), were named after paratroopers Tamara Ivanova (1912–1936) and Lyuba Berlin (1915–1936), respectively, which died just three months earlier.


1086 papal election
The 1086 papal election (held 24 May) ended with the election of Desiderius, abbot of Monte Cassino as Pope Gregory VII's successor after a year-long period of sede vacante.


1086 papal election, Death of Gregory VII
Pope Gregory VII died in exile in Salerno on 25 May 1085. Before his death, the Pope nominated three canons as his preferred successors. They were the cardinal-bishop of Ostia Odo of Châtillon, Bishop Anselm of Lucca,  and Archbishop Hugh of Lyon. Rome was at that time under the control of antipope Clement III, supported by the emperor Henry IV, so almost a year before they proceeded to the election of the successor of Gregory VII.


1086 papal election, Cardinal electors
The papal bull In nomine Domini of 1059 changed electoral law to permit only the seven cardinal-bishops of the suburbicarian sees to participate in papal elections. Doubts were harboured about the papal bull had been called into question by the cardinals priests who demanded admission to the election. The antagonism between the cardinal-bishops and cardinal-priests was intensified by the fact that Gregory VII clearly favored the latter. When in Antipope Clement III was installed in Rome, he sentenced Gregory VII to exile. Gregory was joined by seven of eighteen so-called "Gregorian" cardinal-priests and only one cardinal bishop.


1086 papal election, Cardinal electors
One of the reasons for the rebellion was that Gregory VII allowed only cardinal-priests in the circle of advisors for the Holy See. Soon the schismatic clergy who supported the antipope controlled 17 of 28 titular churches in Rome. Even those cardinal-priests who remained loyal to Gregory protested against the cardinal-bishops. A "Gregorian", Cardinal Deusdedit of San Pietro in Vincoli began to distribute a doctored version of the papal bull In nomine Domini, in which the word "cardinals-bishops" was replaced by "cardinals", which according to the nomenclature of the time meant only cardinal-priests. This allowed them to participate in the election of Gregory VII's successor. This was presumed to be the first time cardinal-priests were admitted, although the dominant role of cardinal-bishops was retained.


1086 papal election, Cardinal electors, Cardinal-bishops
In 1086, in the obedience of Gregory VII were six cardinal-bishops:


1086 papal election, Cardinal electors, Cardinal-priests
Based on available data, it can also be inferred that there were only ten cardinal-priests in the obedience of Gregory VII, although it is possible that the data are incomplete:


1086 papal election, Cardinal electors, Cardinal-priests
Nothing is known of the deacons of the Holy Roman Church participating in this election. It seems that these deacons, obedient to Gregory, were not even considered cardinals. It was not until about 1088 that the deacons of the palace (around seven deacons) joined the College as cardinal-deacons. This change occurred due to the schismatic Antipope Clement III. When, in 1084, three of the seven deacons of the palace joined the antipope they, in their records, began to refer to themselves as "cardinal-deacons". This concept was later borrowed by Urban II.


1086 papal election, Election of Victor III
After Gregory VII's death, the people expelled Antipope Clement III from Rome allowing for the return of Gregory's supporters. In May 1086, Norman troops arrived in Rome with the "Gregorian" cardinals, who proceeded to begin the papal elections. On 24 May 1086, meeting in the Chiesa di Santa Lucia in Sepitisolio, the cardinals elected Desiderius, Abbot of Montecassino and cardinal-priest of Santa Cecilia, as pope despite not being among the candidates nominated by Gregory. Desiderius, however, refused to accept the tiara, threatening the electors with a return to the monastery.


1086 papal election, Election of Victor III
Consul Cencius suggested Cardinal-bishop of Ostia, Otho de Lagery, the only dissenting cardinal, and the only cardinal forced to accept Desiderius' selection. de Lagery's candidacy was, however, met with opposition from one of the cardinals (probably Deusdedit), who referred to old canon law prohibiting the translation of a bishop from one diocese to another.


1086 papal election, Election of Victor III
In this situation, the choice of Desiderius was upheld and he was forced to accept it by force under the name of Victor III. Four days later, the "Gregorian" fled from Rome to Terracina before the imperial prefect of Rome, a supporter of Clement III. In Terracina, the pope-elect left the papal insignia and retired to Monte Cassino, where he remained in persistent refusal for ten months. It was only in March 1087, at the Synod of Capua, that he accepted his election as head of the Catholic Church. Soon after, the Normans once again removed Antipope Clement III from Rome. On 9 May 1087, Victor III was consecrated and crowned in St Peter's Basilica.


1087
Year 1087 (MLXXXVII) was a common year starting on Friday (link will display the full calendar) of the Julian calendar.


1087 Arabis
1087 Arabis /ˈærəbɪs/ is a stony Eoan asteroid from the outer regions of the asteroid belt, approximately 35 kilometers in diameter. It was iscovered by Karl Reinmuth at the Heidelberg Observatory in 1927 and assigned the provisional designation 1927 RD. The asteroid was named after the flowering plant Arabis (rockcress).


1087 Arabis, Discovery
Arabis was officially discovered on 2 September 1927, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. On the same night, it was independently discovered by Soviet-Russian astronomers Sergey Belyavsky and Nikolaj Ivanov at the Simeiz Observatory on the Crimean peninsula. The Minor Planet Center does not acknowledge these independent discoverers.


1087 Arabis, Discovery
The asteroid was first identified as A917 UE at the Simeiz Observatory in October 1917, almost 10 years prior to its official discovery observation at Heidelberg.


1087 Arabis, Orbit and classification
Arabis is a member the Eos family (606), the largest asteroid family in the outer main belt consisting of nearly 10,000 known asteroids. It orbits the Sun at a distance of 2.7–3.3 AU once every 5 years and 3 months (1,911 days). Its orbit has an eccentricity of 0.09 and an inclination of 10° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Heidelberg.


1087 Arabis, Physical characteristics
In the Tholen classification, Arabis is a common S-type asteroid.


1087 Arabis, Physical characteristics, Rotation period
During the early 1990s, a rotational lightcurve was obtained in a photometric survey of small asteroids by European astronomers at the Chilean La Silla Observatory using the ESO 1-metre telescope. In November 2006, another lightcurve of Arabis was obtained by astronomers at the Oakley Observatory in Indiana, United States. Lightcurve analysis gave two well-defined rotation periods of 5.794 and 5.797 hours with a brightness variation of 0.14 and 0.40 magnitude, respectively (U=3/3).


1087 Arabis, Physical characteristics, Spin axis
Between 2011 and 2017, an international collaboration modeled three lightcurves with a period of 5.794995, 5.79500 and 5.79501 hours, respectively. The more recent studies also determined two spin axis of (155.0°, 25.0°) and (331.0°, 5.0°) in ecliptic coordinates (λ, β).


1087 Arabis, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Arabis measures between 31.75 and 47.98 kilometers in diameter and its surface has an albedo between 0.098 and 0.2248.


1087 Arabis, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2137 and a diameter of 31.67 kilometers based on an absolute magnitude of 9.79.


1087 Arabis, Naming
This minor planet was named after the flowering plant Arabis (rockcress), a genus of herbs of the brassicaceae (known as the mustards, the crucifers, or the cabbage family). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 102).


1087 Arabis, Naming, Reinmuth's flowers
Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between (1009) and (1200). This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants).


1088
Year 1088 (MLXXXVIII) was a leap year starting on Saturday (link will display the full calendar) of the Julian calendar.


1088 Mitaka
1088 Mitaka (prov. designation: 1927 WA) is a bright background asteroid from the inner regions of the asteroid belt. It was discovered on 17 November 1927, by Japanese astronomer Okuro Oikawa at the old Tokyo Astronomical Observatory in Japan. The stony S-type asteroid has a notably short rotation period of 3.0 hours and measures approximately 15 kilometers (9.3 miles) in diameter. It was named after the Japanese village of Mitaka.


1088 Mitaka, Orbit and classification
Mitaka is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the inner asteroid belt at a distance of 1.8–2.6 AU once every 3 years and 3 months (1,194 days). Its orbit has an eccentricity of 0.20 and an inclination of 8° with respect to the ecliptic. The asteroid was first observed as A917 RA at the Simeiz Observatory on 11 September 1917. The body's observation arc begins at Tokyo in December 1927, one month after its official discovery observation.


1088 Mitaka, Naming
This minor planet was named after the Japanese village of Mitaka, where the discovering Tokyo Astronomical Observatory was located. Nowadays the city of Mitaka hosts the headquarters of the National Astronomical Observatory of Japan with the Tokyo Photoelectric Meridian Circle, public relation and data centers, and several telescopes. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 103).


1088 Mitaka, Physical characteristics
Mitaka is a common, stony S-type asteroid in both the Tholen and Bus–Binzel SMASS classification.


1088 Mitaka, Physical characteristics, Rotation period and poles
Several rotational lightcurves of Mitaka have been obtained from photometric observations since 1989. Analysis of the best rated lightcurve by French amateur astronomer Pierre Antonini gave a rotation period of 3.0361 hours with a consolidated brightness variation of 0.23 to 0.62 magnitude (U=3).


1088 Mitaka, Physical characteristics, Rotation period and poles
In 2009 and 2011, modelling of Mitaka's lightcurve using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue (UAPC), the Palmer Divide Observatory's archive, the Palomar Transient Factory survey, and from individual observers, gave a concurring rotation period of 3.035377 and 3.035378 hours. The modeled lightcurves also gave a spin axis of (115.0°, 46.0°) and (278.0°, −72.0°), as well as (280.0°, −71.0°) in ecliptic coordinates (λ, β).


1088 Mitaka, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Mitaka measures between 11.33 and 16.016 kilometers in diameter and its surface has an albedo between 0.1549 and 0.37. The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE results with an albedo of 0.1549 and takes a diameter of 16.02 kilometers based on an absolute magnitude of 11.62.


1088 Tmogvi earthquake
The 1088 Tmogvi earthquake (Georgian: თმოგვის მიწისძვრა) occurred on April 16 or April 22, 1088, on Easter Sunday, in the southern provinces of the Kingdom of Georgia. It takes its name from the castle of Tmogvi, in Javakheti, whose destruction is specifically noted in the medieval annals of Georgia. Its magnitude is estimated as 6.5 on the surface wave magnitude scale.


1088 Tmogvi earthquake, History
The Tmogvi earthquake was one of the largest recorded earthquakes in the history of Georgia, and was associated with the active faults of the Javakheti Plateau in the Lesser Caucasus.


1088 Tmogvi earthquake, History
According to the anonymous 12th-century Life of King of Kings David, the earthquake shook Georgia on the "last day of Holy Week, on the very resurrection of our Lord Jesus Christ". The chronicle reports widespread destruction and many casualties and adds that "fearsome trembling of the earth lasted for a year". The author specifically notes the collapse of the castle of Tmogvi, trapping its lord Kakhaber, son of Niania, and his wife underneath.


1088 papal election
A papal election subsequent to the death of Pope Victor III in 1087 was held on 12 March 1088. Six cardinal-bishops, assisted by two lower-ranking cardinals, elected Cardinal-Bishop of Ostia Odon de Lagery as the new Pope. He assumed the name Urban II.


1088 papal election, Background
Pope Victor III died on 16 September 1087 at Montecassino. Shortly before his death he recommended the election of Cardinal Odon de Lagery as his successor. Rome at that time was under control of Antipope Clement III, who was supported by the Emperor Henry IV of Germany, and there was no hope for its quick recovery. In this situation the adherents of Victor III assembled on 9 March 1088 at Terracina, under the protection of the Norman army, to elect the new Pope.


1088 papal election, Background
Besides Cardinal-Bishops, who were the sole electors of the Pope, at the electoral assembly in the episcopal church of SS. Pietro e Cesareo there were present also the representatives of the two lower orders of cardinals, over 40 bishops and abbots, as well as Benedetto, prefect of Rome and Countess Matilda of Tuscany.


1088 papal election, Background
The usual three days of fasting and prayer were proclaimed, and the meeting adjourned until Sunday 12 March. On that day the cardinals and the rest of the present churchmen and laymen reassembled in the same church. The Cardinal-Bishops of Albano, Tusculum and Porto together proposed the election of Odon de Lagery, Cardinal-Bishop of Ostia, who had been designated by Victor III. He accepted his election and took the name Urban II. The election was publicly announced by Cardinal Peter Igneus of Albano. On the same day, the new Pope was enthroned and celebrated the inauguration mass. However, it was not until November 1088 that Urban II was able to travel to Rome.


1088 papal election, Cardinal-electors
According to the decree of Nicholas II In Nomine Domini (1059) Cardinal-Bishops of the suburbicarian sees were the sole electors of the Pope. In March 1088 there were six Cardinal Bishops:


1088 papal election, Assistant electors
Two Cardinals of the lower ranges, one Cardinal-Priest and one Cardinal Deacon assisted at the election:


1089
Year 1089 (MLXXXIX) was a common year starting on Monday (link will display the full calendar) of the Julian calendar.


1089 (number)
1089 is the integer after 1088 and before 1090. It is a square number (33 squared), a nonagonal number, a 32-gonal number, a 364-gonal number, and a centered octagonal number. 1089 is the first reverse-divisible number. The next is 2178 (= 1089 × 2 = 8712/4), and they are the only four-digit numbers that divide their reverse.


1089 (number), In magic
1089 is widely used in magic tricks because it can be "produced" from any two three-digit numbers. This allows it to be used as the basis for a Magician's Choice. For instance, one variation of the book test starts by having the spectator choose any two suitable numbers and then apply some basic math to produce a single four-digit number. That number is always 1089. The spectator is then asked to turn to page 108 of a book and read the 9th word, which the magician has memorized. To the audience it looks like the number is random, but through manipulation, the result is always the same.


1089 (number), In magic, Explanation
The spectator's 3-digit number can be written as 100 × A + 10 × B + 1 × C, and its reversal as 100 × C + 10 × B + 1 × A, where 1 ≤ A ≤ 9, 0 ≤ B ≤ 9 and 1 ≤ C ≤ 9. Their difference is 99 × (A − C) (For convenience, we assume A > C; if A < C, we first swap A and C.). Note that if A − C is 0, the difference is 0, and we do not get a 3-digit number for the next step. If A − C is 1, the difference is 99. Using a leading 0 gives us a 3-digit number for the next step.


1089 (number), In magic, Explanation
99 × (A − C) can also be written as 99 × [(A − C) − 1] + 99 = 100 × [(A − C) − 1] − 1 × [(A − C) − 1] + 90 + 9 = 100 × [(A − C) − 1] + 90 + 9 − (A − C) + 1 = 100 × [(A − C) − 1] + 10 × 9 + 1 × [10 − (A − C)]. (The first digit is (A − C) − 1, the second is 9 and the third is 10 − (A − C). As 2 ≤ A − C ≤ 9, both the first and third digits are guaranteed to be single digits.)


1089 (number), In magic, Explanation
Its reversal is 100 × [10 − (A − C)] + 10 × 9 + 1 × [(A − C) − 1]. The sum is thus 101 × [(A − C) − 1] + 20 × 9 + 101 × [10 − (A − C)] = 101 × [(A − C) − 1 + 10 − (A − C)] + 20 × 9 = 101 × [−1 + 10] + 180 = 1089.


1089 (number), In magic, Other properties
Multiplying the number 1089 by the integers from 1 to 9 produces a pattern: multipliers adding up to 10 give products that are the digit reversals of each other:


1089 (number), In magic, Other properties
Numbers formed analogously in other bases, e.g. octal 1067 or hexadecimal 10EF, also have these properties.


1089 (number), Extragalactic astronomy
The numerical value of the cosmic microwave background radiation redshift is about z = 1089 (z = 0 corresponds to present time)


1089 Tama
1089 Tama, provisional designation 1927 WB, is an elongated Florian asteroid and synchronous binary system from the inner regions of the asteroid belt, approximately 12 kilometers in diameter.


1089 Tama
It was discovered by Japanese astronomer Okuro Oikawa at the old Tokyo Astronomical Observatory (389) on 17 November 1927. The asteroid was named after the Tama River in Japan. Its minor-planet moon was discovered in December 2003 and measures approximately 9 kilometers.


1089 Tama, Orbit and classification
Tama is a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt. It is, however, a non-family asteroid from the main belt's background population when applying the Hierarchical Clustering Method to its proper orbital elements.


1089 Tama, Orbit and classification
The asteroid orbits the Sun in the inner main-belt at a distance of 1.9–2.5 AU once every 3 years and 3 months (1,203 days). Its orbit has an eccentricity of 0.13 and an inclination of 4° with respect to the ecliptic. Tama was first identified as A894 VA at Heidelberg Observatory in November 1894. The body's observation arc begins with its identification as A904 VD at Heidelberg in November 1904, or 23 years prior to its official discovery observation at Tokyo.


1089 Tama, Physical characteristics, Rotation period
A large number of rotational lightcurves of Tama were obtained from photometric observations since it has been identified as a binary asteroid (see below). Lightcurve analysis gave a rotation period between 16.4 and 16.464 hours with a brightness variation between 0.08 and 0.41 magnitude (U=2-/2-3-/3), superseding a period of 4 hours from a fragmentary lightcurve obtained in the 1990s (U=1).


1089 Tama, Physical characteristics, Rotation period
Tama appears to be somewhat elongated in shape. LCDB's consolidated result gives a period of 16.44 hours and an amplitude of 0.41 magnitude (U=3).


1089 Tama, Physical characteristics, Diameter and albedo
According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, the Spitzer Space Telescope and the NEOWISE mission of the Wide-field Infrared Survey Explorer, Tama measures between 11.33 and 13.32 kilometers in diameter and its surface has an albedo between 0.216 and 0.32.


1089 Tama, Physical characteristics, Diameter and albedo
The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2048 and a diameter of 12.82 kilometers based on an absolute magnitude of 11.8.


1089 Tama, Physical characteristics, Satellite
In 2004, it was announced that Tama has a minor-planet moon, provisionally designated S/2003 (1089) 1. The satellite was identified based on lightcurve observations with mutual occultation and eclipsing events from 24 December 2003 to 5 January 2004 by Raoul Behrend, René Roy, Claudine Rinner, Pierre Antonini, Petr Pravec, Alan Harris, Stefano Sposetti, Russell Durkee, and Alain Klotz. The moon measures approximately 9 kilometers in diameter. It may orbits 20 km away in a period of 16.4442 hours (synchronously).


1089 Tama, Physical characteristics, Spin axis
Tamas lightcurve has also been modeled. In 2013, modelling by an international study using photometric data from the US Naval Observatory, the Uppsala Asteroid Photometric Catalogue (UAPC) and the Palmer Divide Observatory, gave a concurring rotation period of 16.4655 hours. Another modeled lightcurve using data from UAPC, the Palomar Transient Factory survey, and individual observers, gave a period of 16.4461 hours as well as two spin axes of (193.0°, 32.0°) and (9.0°, 28.0°) in ecliptic coordinates (λ, β).


1089 Tama, Naming
This minor planet was named after Tama River near the discovering Tokyo Astronomical Observatory (389) in Japan. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 103).


108: Kaiba Gorō no Fukushū to Bōken
108: Kaiba Gorō no Fukushū to Bōken (108〜海馬五郎の復讐と冒険〜, Ichi Maru Hachi ~Kaiba Gorō no Fukushū to Bōken~, lit. 108: Revenge and Adventure of Gorō Kaiba) is a 2019 Japanese dark comedy film written, directed by, and starring Suzuki Matsuo, based on his 2018 novel 108. The film also stars Miho Nakayama, Shunsuke Daitō, Shori Doi, Louis Kurihara, and LiLiCo.


108: Kaiba Gorō no Fukushū to Bōken, Synopsis
Screenwriter Gorō Kaiba discovers a Facebook post revealing that his wife, former actress Ayako, is having an extramarital affair. Furthermore, he notices that the post has 108 likes. Gorō can easily divorce Ayako, but he would end up paying her half of his assets, which total an estimated 10 million yen. Instead, he uses that money on a one-month womanizing streak, aiming to have sex with 108 women.


108: Kaiba Gorō no Fukushū to Bōken, Music
Gen Hoshino wrote and recorded the theme song "Yoru no Boat" (夜のボート, Yoru no Bōto, "Boat at Night").


108: Kaiba Gorō no Fukushū to Bōken, Release
The film was released in Japan by on October 25, 2019.


108th (Madras Infantry) Regiment of Foot
The 108th Regiment of Foot (Madras Infantry) was an infantry regiment of the British Army. However, it was raised initially as part of the Madras Army, by the East India Company (EIC) in 1766.


108th (Madras Infantry) Regiment of Foot
In the aftermath of the Indian Rebellion (1857), the British government took control of the Presidency Armies and the 108th became als known by the name 3rd Madras Infantry. Finally, under the Childers Reforms of 1881, the regiment was amalgamated with the 27th (Inniskilling) Regiment of Foot, to form the Royal Inniskilling Fusiliers.


108th (Madras Infantry) Regiment of Foot, History, East India Company
The regiment as first raised by the East India Company as the 3rd Madras European Regiment, when it was formed from the 1st Madras Europeans in 1766.


108th (Madras Infantry) Regiment of Foot, History, East India Company
It served in India until 1774, when it was absorbed by the 1st and 2nd Madras Europeans in 1774. Re -raised as a separate regiment in 1777, the 108th was disbanded in 1796. The regiment was re-raised as the 3rd Madras (European) Regiment in 1854, and then saw action in India in 1857 during the Indian Rebellion.


108th (Madras Infantry) Regiment of Foot, History, British Army
After the Crown took control of the Presidency armies in the aftermath of the Indian Rebellion, the regiment became the 3rd Madras Infantry in November 1859. It was then renumbered as the 108th Regiment of Foot (Madras Infantry) on transfer to the British Army in September 1862. It embarked for England in 1876. As part of the Cardwell Reforms of the 1870s, where single-battalion regiments were linked together to share a single depot and recruiting district in the United Kingdom, the 108th was linked with the 27th (Inniskilling) Regiment of Foot, and assigned to district no. 64 at St Lucia Barracks, Omagh.


108th (Madras Infantry) Regiment of Foot, History, British Army
On 1 July 1881 the Childers Reforms came into effect and the 108th amalgamated with the 27th (Inniskilling) Regiment of Foot to form the Royal Inniskilling Fusiliers.


108th Air Defense Artillery Brigade (United States)
The 108th Air Defense Artillery Brigade is an air defense artillery brigade of the United States Army. The mission of the brigade is to train and maintain a strategic crisis response air defense artillery brigade capable of deploying worldwide, on short notice, to provide air defense force protection from air-breathing threats and tactical ballistic missiles, as well as allow freedom of maneuver for XVIII Airborne Corps operations.


108th Air Defense Artillery Brigade (United States), History, World War II
The 108th Air Defense Artillery Brigade traces its lineage to the 514th Coast Artillery Regiment (Antiaircraft), which was formed in Schenectady, New York in October, 1923. The Regiment was reorganized as the 108th Coast Artillery Group (Antiaircraft) on 3 January 1943 at Camp Davis, North Carolina, and again reorganized as the 108th Antiaircraft Artillery Group, in May of the same year. The 108th was then moved to Camp Stewart, Georgia on 14 October 1943. Two months later, the 108th staged at Camp Shanks, New York on 22 December and remained there until they deployed from the New York Port of Embarkation on 6 days later, and arrived in England on 7 January 1944.


108th Air Defense Artillery Brigade (United States), History, World War II
The brigade deployed to Europe during World War II, and participated in the landings at Normandy, going ashore at Utah Beach on 28 June 1944. The 108th then went on to provide antiaircraft defense for the city and port of Cherbourg, for eleven months, and then moved forward to the cities of Rheims and Rouen. The brigade was moved forward to Germany on 2 May 1945, and was stationed in Kaufhueren on 20 August. The Group was deactivated there on 14 December 1945, and returned to the Army reserve. The personnel and equipment from the brigade were dispersed to the occupation units.


108th Air Defense Artillery Brigade (United States), History, World War II
1/514th CAR (AA) became 217th Coast Artillery Battalion on 20 January 1943, and was again redesignated as 217th Anti Aircraft Artillery Battalion on 28 June 1943. The 217th deployed from the Boston Port of Embarkation on 7 April 1944 and arrived in England on 17 April 1944. The 217th moved forward to France on 25 June 1944, where they remained until they moved forward to participate in the Ardennes-Alsace Offensive. The 217th was relocated to Stubenag, Germany on 20 August 1945. The 217th returned to the continental US via the Hampton Roads Port of Embarkation on 2 February 1946, and was deactivated and returned to the US Army Reserve the same day.


108th Air Defense Artillery Brigade (United States), History, World War II
2/514th CAR (AA) became 639th Coast Artillery Battalion (Auto Weapons) on 20 January 1943, And was again redesignated as the 639th Anti Aircraft Artillery Battalion (Auto Weapons) on 15 May. The 639th deployed from the New York Port of Embarkation on 29 September 1944, and landed in France on 10 October 1944. The 639th was then relocated to Braunfels, Germany on 20 August 1945. The 639th returned to the continental US via the New York Port of Embarkation on 2 February 1946, and was deactivated at Camp Kilmer, and returned to the US Army Reserve on the same day.


108th Air Defense Artillery Brigade (United States), History, World War II
3/514th CAR (AA) became 363rd Coast Artillery Battalion (Search Light) on 20 January 1943, and was redesignated as the 363rd Anti Aircraft Artillery Battalion (Searchlight) on 3 March 1943. The 363rd did not deploy, but remained at Fort Gordon, Georgia until 31 October 1944, whereupon the unit was deactivated and returned to the US Army Reserve, with the personnel and equipment transferred elsewhere as required.


108th Air Defense Artillery Brigade (United States), History, Post-War
In September, 1956, the 108th AA Group was reactivated in Los Angeles, California. It was again redesignated as the 108th Artillery Group (Air Defense). The 108th was deactivated in April 1960, in Fort MacArthur, California.


108th Air Defense Artillery Brigade (United States), History, Vietnam War
In May 1967, the group was reactivated at Fort Riley, Kansas as the 108th Artillery Group and deployed to the Republic of Vietnam in October 1967. The Group participated in every major operation conducted in the I Corps area of operations and credited with participation in eleven different campaigns while in Vietnam. The Group notably supported the Operation Lam Son 719 raid into Laos during  February–March  1971.


108th Air Defense Artillery Brigade (United States), History, Vietnam War
For its service it was awarded the Vietnam Cross of Gallantry with Palm. The 108th departed from Vietnam on 22 November 1971 for Fort Lewis, Washington, where the unit was again inactivated.


108th Air Defense Artillery Brigade (United States), History, Vietnam War
The 1st Battalion, 83rd Field Artillery Regiment served with the Group.


108th Air Defense Artillery Brigade (United States), History, Post-Vietnam
On 26 August 1974, the group was again reactivated at Kapaun Barracks, Kaiserslautern, West Germany, as the 108th Air Defense Group, the only Chaparral/Vulcan Group in the US Army. In September 1975 the group moved to Kleber Kaserne and on 1 October 1982 it was redesignated the 108th Air Defense Artillery Brigade. On 15 April 1992 the Brigade was moved to Fort Polk, Louisiana, commanding the Patriot (2–43rd) battalion, an Avenger (1–2nd) unit and the newly activated (16 December 1992) 208th Signal Company. On 15 August 1996 the brigade moved to Fort Bliss, Texas.


108th Air Defense Artillery Brigade (United States), History, Post-Vietnam
At Fort Polk the brigade was aligned under the Fort Bragg-based XVIII Airborne Corps and, because of this alignment, added an Airborne tab above its patch; however, according to the U.S. Army Institute of Heraldry, the alignment with XVIII Airborne Corps does not serve as authorization to add the Airborne tab. While the brigade did wear the tab, it was done without Department of the Army authorization.


108th Air Defense Artillery Brigade (United States), History, Post-Vietnam
The IOH also notes the brigade asked to be authorized a beret, flash and parachute wing trimming (aka "oval") but was turned down because the brigade is not an Airborne unit and is not authorized either a flash or wing trimming. The brigade's only unit to serve on jump status was the Stinger Platoon of 2–52nd ADA. This platoon, under the command of 1LT Evan Phelps, had the distinction of being the first ADA unit to be deployed in the opening days of the Gulf War. 2–52 ADA was disbanded shortly after the Gulf War in the early 1990s. Later in 2007, the brigade would again have Airborne units assigned to its command with the addition of the 3–4th ADA when it was reassigned from the 82d Airborne Division. Under the ongoing reorganization, only Battery E of 3–4th ADA is on jump status.


108th Air Defense Artillery Brigade (United States), History, Post-Vietnam
In 2007–2008, the unit was to be moved to Fort Bragg as part of the 2005 BRAC realignment. The 108th saw its 1–7th ADA deployed to South Korea (the first U.S. deployment since the Korean War) and gained 3–4th ADA, previously an Avenger battalion. The 3–4th ADA is now organized as an "Air and Missile Defense" battalion.


108th Air Refueling Squadron
The 108th Air Refueling Squadron (108 ARS) is a unit of the Illinois Air National Guard 126th Air Refueling Wing located at Scott Air Force Base, Belleville, Illinois. The 108th is equipped with the KC-135R Stratotanker.


108th Air Refueling Squadron
The squadron is a descendant organization of the World War I 108th Aero Squadron, established on 27 August 1917. It was reformed on 1 July 1927, as the 108th Observation Squadron, and is one of the 29 original National Guard Observation Squadrons of the United States Army National Guard formed before World War II.


108th Air Refueling Squadron, History, World War I
The 108th Air Refueling Squadron origins date to 27 August 1917 when the 108th Aero Squadron was formed at Kelly Field, Texas. The personnel at the time was composed primarily of men from the upper Southern and Midwest, coming from the recruit depot at Fort Thomas, Kentucky. At Kelly, the squadron was put in a military indoctrination course of training until being ordered for overseas service on 26 October. It was moved to the Aviation Concentration Center, Garden City, Long Island. It arrived at Mineola Field on 3 November 1917 where it was prepared and equipped for overseas duty.


108th Air Refueling Squadron, History, World War I
On 7 December, it was ordered to proceed by train to St. John's, Newfoundland where, on 10 December, it boarded the SS Tuscania, and proceeded across the Atlantic and arrived at Liverpool, England on 26 December. It then moved by train to the English Channel port of Southampton, where it waited at a Rest Camp for several days before crossing to Le Havre, France on 28 December. It again waited for transportation at Le Havre before finally arriving at the Replacement Concentration Center, AEF, St. Maixent Replacement Barracks, France, arriving on 2 January 1918.


108th Air Refueling Squadron, History, World War I
At St. Maixent, the squadron was placed in quarantine for several weeks due to the presence of mumps. Finally, on 20 February, it was ordered to proceed to the 3d Air Instructional Center (3d AIC), Issoudun Aerodrome, in Central France, arriving on 21 February. It was first assigned to Field No. 2 where it was put to work in the Aero Repair Department while its permanent buildings were under construction at the main field. In May, the squadron was moved to its permanent quarters and buildings where it remained until after the Armistice with Germany in November 1918. It returned to the United States in late May 1918. Arrived at Mitchel Field, New York, where the squadron members were demobilized and returned to civilian life.


108th Air Refueling Squadron, History, Illinois National Guard
In June 1927 the 108th Aero Squadron was re-activated, and designated the 108th Observation Squadron, 33d Division Aviation at Chicago Municipal Airport, Illinois. In July 1927 the unit received federal recognition; the squadron was authorized 16 officers, 74 enlisted and was assigned PT-1 Trusty aircraft. During the ensuing years, membership in the 108th Observation Squadron was a coveted assignment. Applicants were said to have been on waiting lists for as much as four years prior to being called.


108th Air Refueling Squadron, History, Illinois National Guard
In 1930, Douglas O-2H biplanes were assigned to the 108th Observation Squadron, followed by Douglas O-38 biplanes in 1935. No less than George C. Marshall was a member of the 33d Division from November 1933 to August 1936 as a senior instructor. During the next 10 years, the 108th performed outstanding civic service to the State of Illinois, dropping medicine and relief supplies to many of the towns in central and southern Illinois that were isolated by floodwaters, tornadoes, and fires. Captain Wilson V. Newhall, later to become the first chief of staff of the Illinois Air National Guard was awarded the Distinguished Service Medal during flood duty, in 1937, as a member of the 108th Observation Squadron.


108th Air Refueling Squadron, History, World War II
After war broke out in Europe in 1939, preparedness for war increased in the United States. As part of the preparedness program, 4,800 members of the 33d Division, including the 108th Squadron were mobilized and placed on active duty in February 1941. The unit reequipped with the North American O-47 biplanes and initially trained at Chicago Municipal Airport in Chicago. The unit remained in Chicago until 14 January 1942 when it was assigned to the Caribbean Air Force after the Japanese attack on Pearl Harbor and arrived at Río Hato Army Air Base, Panama. The stay at Rio Hato was brief, however, as the squadron was moved to Howard Field in the Canal Zone on 19 January.


108th Air Refueling Squadron, History, World War II
At Howard Field, the squadron was kept very busy on a myriad of patrol and communications flights along the Atlantic and Pacific Panamanian coast lines and within the far-flung command. The 108th also acquired several Stinson L-1's during this period along with a P-36A, one A-18, two L- l's and two L-4A's all based at Howard Field.


108th Air Refueling Squadron, History, World War II
One of the L-4A's was transferred to the dedicated Tow Target Squadron at Howard Field on 28 February 1943, while the rare Curtiss A-18, to the relief of the hard-pressed maintenance crews, was transferred to the Technical School at Rio Hato on 3 April 1943. This was the only A-18 to serve operationally with a line combat unit during World War II.


108th Air Refueling Squadron, History, World War II
The units first Douglas B-18 Bolo was added in February 1943. The squadron conducted one operational mission with this aircraft, along the "Pacific coast of Colombia" on 24 February. By 25 June 1943, by which time the designation had been changed to a more realistic 108th Reconnaissance Squadron (Special), the mission handed the Squadron were ever more complex and demanding, and the alterations to the equipment reflected this. Another Douglas B-18 (36-275) had been added in May 1943, the Squadron also gained small numbers of Piper L-4A's, Curtiss 0-52's (undocumented but recalled by Squadron members), and four Bell P-39N Airacobras.


108th Air Refueling Squadron, History, World War II
In November 1943, the threat to the Panama Canal had decreased sufficiently that the 108th Reconnaissance Squadron was inactivated in the Canal Zone, and the personnel were reassigned to other units in one of the combat theaters.


108th Air Refueling Squadron, History, Illinois Air National Guard
The wartime 108th Reconnaissance Squadron (Special) was re-designated the 108th Bombardment Squadron (Light), and was allocated to the Illinois Air National Guard on 21 June 1945. It was organized at Chicago Municipal Airport, and was extended federal recognition on 29 June 1947 by the National Guard Bureau. The 108th Bombardment Squadron was bestowed the history, honors, and colors of the wartime 108th and predecessor units. The squadron was equipped with B-26 Invader light bombers and was assigned to the Illinois ANG 126th Bombardment Group.


108th Air Refueling Squadron, History, Illinois Air National Guard, Korean War Activation
The unit was ordered to active service on 1 April 1951 as a result of the Korean War. The unit was initially assigned to Tactical Air Command at Langley AFB, Virginia. The wing moved to Bordeaux-Merignac Air Base, France with the first elements arriving in November 1951. The 126th BW was assigned to United States Air Forces in Europe. By 10 November, Bordeaux was considered an operational base and was assigned to the 12th Air Force.


108th Air Refueling Squadron, History, Illinois Air National Guard, Korean War Activation
At Bordeaux, the 126th BW consisted of the 108th, 168th and 180th Bomb Squadrons (Light). The aircraft were marked by various color bands on the vertical stabilizer and rudder. Black/Yellow/Blue for the 108th; Black/Yellow/Red for the 168th, and Black/Yellow/Green for the 180th. It flew B-26's for training and maneuvers and stayed at Bordeaux AB until being transferred Laon AB, France on 25 May 1952 where it remained for the balance of the year.


108th Air Refueling Squadron, History, Illinois Air National Guard, Cold War
After returning from France, was re-equipped with F-51D Mustangs due to the limited availability of jets which were being used by the USAF in the Korean War. In early 1955, was upgraded to new F-84F Thunderstreak jet fighters. In 1957 the 108th participated in the Ricks Trophy Race. In 1958, the 126th was re-designated as the 126th Air Defense Group and was transferred from TAC to Air Defense Command (ADC). ADC re-equipped the 108th, now a Fighter-Interceptor Squadron with day/nigh/all-weather F-86L Sabre Interceptor aircraft, and the squadron stood a 24/7 air defense alert at O'Hare IAP.


108th Air Refueling Squadron, History, Illinois Air National Guard, Cold War
In July 1961, the 126th was realigned from an air defense mission to becoming the first Air National Guard air refueling group under Tactical Air Command. It was re-equipped with KC-97 Stratotankers and began worldwide aerial refueling operations. In 1963, the 108th was the first squadron to mid-air refuel the elite Air Force Thunderbirds, and in 1964, it participated in Operation "Ready Go", the first all United States Air National Guard (ANG) non-stop deployment of fighter aircraft to Europe.


108th Air Refueling Squadron, History, Illinois Air National Guard, Cold War
In 1966 the squadron began a rotational deployment to Rhein-Main Air Base in support of Operation Creek Party. Which provided USAFE an air refueling capability. The Creek Party deployment rotations lasted until 1976, and over the decade the 108th saw millions of pounds of jet fuel off-loaded and millions of miles flown, all accident free.


108th Air Refueling Squadron, History, Illinois Air National Guard, Cold War
In July 1976 the KC-97s were retired and the parent 126th was transferred to Strategic Air Command, receiving jet KC-135A Stratotankers. These aircraft were later upgraded to "E" models in 1983 and finally replaced with "R" models in 2008.


108th Air Refueling Squadron, History, Illinois Air National Guard, Cold War
On 19 December 1990, President Bush ordered 268 members of the 126th Air Refueling Wing, the 108th Air Refueling Squadron and elements of the 126th Consolidated Aircraft Maintenance Squadron federalized for active duty during the 1991 Gulf Crisis. During Operation Desert Storm, the squadron performed air refueling operations as part of the 1709th Air Refueling Wing (Provisional), stationed at King Abdul Aziz Air Base, Jeddah, Saudi Arabia, and as part of the 1712th Air Refueling Wing (Provisional), stationed at Abu Dhabi, UAE, until being returned to Illinois state control on 22 March 1991.


108th Air Refueling Squadron, History, Illinois Air National Guard, Modern era
The 126th ARW relocated to Scott Air Force Base in 1999 from Chicago's O'Hare International Airport as part of the recommendations for base closure made by the Base Realignment and Closure Commission.


108th Air Refueling Squadron, History, Illinois Air National Guard, Modern era
As part of the Global War on Terrorism, the 126th Air Refueling Wing has been tasked on several occasions for deployment to United States Air Forces Central. Elements of the wing have been assembled and deployed as the 108th Expeditionary Air Refueling Squadron as part of AEF packages, providing air refueling to combat aircraft in Operation Enduring Freedom (OEF) and Operation Iraqi Freedom (OIF) during the 2000s.


108th Air Refueling Squadron, History, Illinois Air National Guard, Modern era
In its 2005 BRAC Recommendations, DoD recommended to realign Grand Forks Air Force Base, North Dakota. It would distribute the 319th Air Refueling Wing's KC-135R aircraft to the 126th Air Refueling Wing (ANG), Scott AFB, IL (12 aircraft) and several other institutions. The 126th would retire its eight KC-135E aircraft. Scott would receive KC-135R model aircraft to replace older, higher maintenance KC-135E models.


108th Air Refueling Squadron, History, Lineage
* * This unit is not related to another 108th Aero Squadron (Service) that was activated in March 1918 at Rich Field, Waco, Texas.


108th Anti-Aircraft Missile Regiment (Ukraine)
The 108th Anti- Aircraft Missile Regiment (Ukrainian: 108-й зенітний ракетний полк (108 ЗРП); Military Unit Number A4527) was an air defense regiment of the Ukrainian Air Force, based at Zolotonosha until its 2012 disbandment. The regiment began as the 22nd Anti- Aircraft Artillery Division of the Red Army formed during World War II.


108th Anti-Aircraft Missile Regiment (Ukraine), World War II
The 22nd Anti- Aircraft Artillery Division of the Reserve of the High Command (RGK) began its formation in the Moscow Military District during December 1942 and on 15 January 1943 Colonel Igor Danshin (promoted to major general 18 November 1944) was appointed commander. The division included the 1335th, 1341st, 1347th, and 1353rd Anti- Aircraft Artillery Regiments. After completing its formation, the division was sent to the Southwestern Front, which became the 3rd Ukrainian Front on 20 October of that year.