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Mercury has never been an easy planet to observe. It never appears further from the sun than 28^o, hence it is virtually never observed in a dark sky. Although it is less difficult to locate in the sky than commonly assumed, it is always observed low in the sky and is greatly affected by air turbulence. The surface markings then have a low contrast to the sky background and are visible only at an observer's threshold of vision.

In addition, Mercury elongations vary in favorability. Indeed, for mid-northern latitudes, spring evening (eastern) elongations are the most favorable, with respect to the maximum angular distance from the sun, length of visibility (usually less than about 20 days) and height above the horizon. The same is true for the autumn morning (western) elongations; the entire situation is reversed for the southern hemisphere. The primary factor controlling favorability is the inclination of the ecliptic to the horizon.

The earliest observations of Mercurian detail were those of cusp truncation by Schroter, in 1800. Occasional truncations were observed by others but little surface detail was recorded until the 1880's, by Denning in England and Schiaparelli at Milan. Schiaparelli published no individual drawings to this writer's knowledge but did publish the first planisphere (single hemisphere) of Mercury's surface (1889). He believed the planet to rotate synchronously with a period equal to its orbital period, namely 87.969 days. This opinion was not at first universally accepted. Schroter's assistant, Harding, and the astronomer Prince concluded that the Mercurian day was approximately that of the Earth's (Sandner, 1963). Leo Brenner (1896) concluded that it was actually 33 to 35 hours. These opinions lapsed after various observers would observe a feature as motionless over a period of several hours (of date-time observing)(see, for example, McEwen, 1909).

The first third of this century found the observations of Mercury confined principally to three groups:

The English, as reported by Henry McEwen for the British Astronomical Association (BAA),
the French, principally at Meudon and the Jarry-Desloges Observatories,
and in America by Lowell.

The BAA created a Mercury observation section, which did, and still does, periodically publish drawings and analyses of observations. The observers were few in number and confined almost completely to observers in the British Isles, the principle exception being one Captain Molesworth in Ceylon. Approxmiately 50 percent of all observations from this time are to be found in theJournal of the British Astronomical Association (JBAA). The other 50 percent is to be found inObservatoires Jarry-Desloges: Observations des Surfaces Planetaries (1909-1946), perhaps the single largest and most important piece of amateur work in this century. The drawings of R. Jarry-Desloges, G. and V. Fournier, and P. Briault are among the finest ever made. In ten volumes, there are found 139 drawings of Mercury from 1909 to 1926. At the same time, at Meudon and at other sites in France, Danjon and others made occasional observations of the planet. This French research culminated in the work of E. M. Antoniadi, which is described below. During this period, the first quality photograph was taken by Quenisset (1931). The American contributions are meager. The drawings by Pickering (1892)( and Douglas) are the only useful ones. Percival Lowell made an extensive series of drawings (1898), which show linear markings like martiancanali and resemble other planispheres only with the greatest stretch of the imagination. Lowell's work will be consider no further.

The most important work of the period is that of Antoniadi (1934). Working at Meudon, Antoniadi observed Mercury from 1924 to 1929, firmly established (as he thought) an 88--day rotation period, and gave nomenclature to the various bright and dark areas. Although not the first to do so, he had truly mastered the art of daylight observations. The drawings, being so excellent, if small in number, firmly entrenched various markings into Mercury observation lore, such as his famous "figure 5" (See Sandner, 1963, page 36), so much so that observational bias imitative of Antoniadi is quite strong in many later drawings.

Mercury observation became sporadic after Antoniadi's work. Only a rather well-observed elongation in 1936 (McEwen, 1936) was reported in the 1930's plus a few French contributions (Danjon 1937, Quenisset 1931). In 1942 and 1944 Lyot and Camichel at Pic du Midi Observatory observed Mercury and made the first good photographic series of observations (see Dollfus, 1953). In 1950, Dollfus also obtained a very fine series of drawings (1953) using filters for increasing the visibility of features. The French efforts effectively ended, in terms of published material, at this time and theJBAA has published a scant nine observations for the 1950's and 1960's.

Most of the post-World War II drawings are to be found in the American journal,The Strolling Astronomer, of the Association of the Lunar and Planetary Observers. Created by Walter Haas, who originally published in theJBAA, this journal also has a Mercury section, which publishes selected drawings for each year. Unfortunately, many, if not most, of the drawings are inaccurate and unusable.

A short discussion of the Mercury observations is appropriate here. As noted previously, the markings are at the limit of visual perception, due somewhat to their own soft nature but more to the observing constraints. The personal equations (personal styles and tendancies) of the observers are quite significant. Often, general features agree between observers observing the same apparition but the detail and placement of the markings often show little, if any, agreement (see, for example, the drawings of the Fournier brothers (Jarry-Desloges, 1910)). Once the 88-day rotation period was "confirmed" by Antoniadi, it became rather easy for an observer to "see" Antoniadi's markings in the fleeting images of steady seeing.

Still, discrepancies were reported from time to time. Major dark areas disappeared, bright areas of the disk and limb would appear, even polar caps were recorded on both poles. Some Mercury observers, especially Haas (1947), ascribed these occurences to clouds and haze in a Mercurian atmosphere. Most of such phenomena may be ascribed to the personal equation of the observer (where or not he was Antoniadi-biased), others imply poor observing and/or poor observer. Some short-lived phenomena have been ascribed possibly to luminescence (Cruikshank 1966), but the aforementioned factors may still play a role. Any apparent motion of the features was considered as librations, a rocking of about 23 degrees amplitude in longitude and about seven degrees in latitude. But the major cause of discrepancies is the true nonsynchronous rotation of Mercury, so that observers were really viewing more than just the one hemisphere they thought they were seeing!

The 88-day rotation period seemed quite secure, both observationally and theoretically. Tidal friction from the sun's pull caused Mercury to have one face eternally sunward, a situation similar to the Earth-Moon system (so it was thought). It, therefore, was a considerable jolt when Pettengill and Dyce (1965), using radar doppler techniques, found that they couuld fit their measures only to a 59 +/- 5 day Mercurian "day." Peale and Gold (1965) proposed immediately that Mercury was locked into a exact 2/3 resonance with the orbital period. Other astronomers quickly proved the strong resonance theoretically (Columbo 1965, Columbo and Shapiro 1966), which immediately created new consequences. The motion of the Sun in the Mercurian sky caused the formation of "hot poles" 180 degrees apart (Soter and Ulrichs (1967)) and reinterpretation of the infrared data was necessary to evaluate light and dark side temperatures (Morrison 1970, Section 7.1). *Our* most important concern would be how much of the old visual observations are still accurate and useful. Indeed the question "Why was the 59-day period not discovered visually?" immediately begs an answer.

The answer lies in several interesting coincidences. A point on Mercury at a noon position will be at the noon position exactly 3 Mercurian days later, which is also exactly 2 Mercurian years. Now, the synodic (phases) period is 116 days, which is 4/3 the orbital period, twice the Mercurian day,and about one-third of an Earth year. The synodic period means that there are 116 days between similar apparitions but not all of these are favorable in mid-northern latitudes, where the observers were.

This situation, for a particular face of Mercury, will exist for six years after which the favorable apparitions will shift by 1 synodic period, for the synodic period is slightly out of phase with the calendar year.

There is one more coincidence to the puzzle. Maps made by the best observers, computer digitized and placed upon a map based on a 59 day rotation, still show the famous "Figure 5", a set of dark markings that resemble the numeral. The problem is....the "5" is replicated in three places! Though one is by far the most prominent, the three together, each 120 degrees in hermographic longitude apart mean that once more, an observer could be fooled into believing he has seen the same feature!

An analysis of Antoniadi's excellent drawings was published by Larry Krumenaker in 1978 in Academic Press' "Icarus," a journal on planetary sciences, Vol 34, #1, P. 215. It was also briefly alluded to in an article by Jonathan Eberhart in "Science News" for May 20, 1978, Vol 113, No.20, "Old Bottle, New Wine."

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