The 1994-1995 apparition of Mars was aphelic, in that the planet's apparent size reached only 13.85 arc seconds at opposition. This made the apparition the poorest (in apparent size) since 1980. What this apparition had going for it was Mars being high in the sky for northern observers. Furthermore, since the Martian north pole was tilted earthward observers were able to watch the spring-summer regression of the North Polar Cap and the concomitant increase in meteorological activity. These phenomena formed the main thrust of the observational programs of the Association of Lunar and Planetary Observers' International Mars Patrol (IMP). Despite Mars unfavorable presentation, improved instrumentation and observational techniques permitted quality work to be done. For the hard-core Mars observer this apparition turned out to be very exciting! INTRODUCTION The ALPO Mars Section received 2,364 observations from 66 observers in ten countries as part of the IMP not bad for an aphelic apparition that had Mars at over 100 million kilometers from Earth at its closest approach. Observations covered the period from Ls 261 (T. Stryk) to 127 (H. Ishado), corresponding to Martian northern winter through early summer (Fig. 1). Observers submitted 1297 drawings, 41 photographs, and 444 CCD images. In addition, we received over 400 measurements of the North Polar Cap (NPC) areocentric latitudes obtained between 22 and 122 Ls from bifilar micrometer, CCD and video red-light images. The NPC displayed numerous rifts and web-like features. Some interesting relationships between Martian meteorology and NPC behavior appear to be emerging, with numerous atmospheric features such as limb clouds and hazes, topographic clouds, equatorial band clouds and the Syrtis Blue Cloud increasing in prominence as theNPC progressed. CAN AMATEUR OBSERVATIONS STILL BE WORTHWHILE? The answer is definitely YES!! The Mars Section has assisted a number of professional planetary scientists during the present apparition by responding to requests for ALPO Mars data. One request comes from Fred Espenak of the NASA/Goddard Space Flight Center-Planetary Systems Branch. He observed Mars in March of 1995 in the 10 micron spectroscopic range with NASA's 3 meter telescope (IRTF) on Mauna Kea. He was measuring the distribution of ozone in Mars' atmosphere using the Goddard's IR Heterodyne Spectrometer. In his analysis of this data he needed to know the transparency of the Martian atmosphere at the time of his observation. Our data showed him what clouds or haze activities were present before, during and after his observing run on Mauna Kea. Jim Bell and Jeff Moersch of NASA Planetary Astronomy program at Cornell University hosted the Mars Telescopic Observations (MTO) workshop which was sponsored by the Lunar and Planetary Institute. The theme of this workshop was to explore the role that current and continuing Earth-based observations play in increasing our understanding of Mars. In addition, it brought togetherastronomers who work at different wavelengths (both professionals and amateurs) and don't often have the opportunity to share their ideas with one another. All of the Mars recorders were invited to present papers on the work of our section. Don Parker gave a talk on the NPC regressions, past and present and on the continuing IMP meteorological survey that Jeff Beish and he have been conducting for many years. Dan Joyce substituted for Dan Troiani, who was unable to attend, and presented the ALPO Mars Section results from both the 1992-93 and the 1994-995 Martian apparitions, including numerous drawings, photographs, and videos. All of the ALPO papers were well received and generated a great deal of interest from the professional astronomers present. Abstracts of the MTO Workshop papers have been published in a professional abstract volume [Bell and Moersch 1995]. The work of the IMP (your observations and hard work) has made an impact upon theprofessional planetary scientists' community. Even in this day of space telescopes and planned space missions, planetary scientists are still interested in using amateur's data on Mars. In fact, a significant portion of the MTO workshop was devoted to planning ground-based support programs for the upcoming space probes to Mars, and amateur visible light monitoring was included in these plans. We will keep the readers and our observers informed of these programs, including an E-mail alert network, as they crystallize. THE MARTIAN ARCTIC The North Polar Hood (NPH) was conspicuous and visible from June, 1994, through late October, 1994 (290 - 010 Ls), after which time the hood became fragmented. This agrees well with Ebisawas finding that polarization of the north polar region weakened around 9 Ls [Ebisawa 1995]. Whitby, Warell, Niechoy, and Parker reportedthe NPC largely free of the hood around 358 Ls, but at times high thin arctic clouds were visible in blue light through November (25 Ls) by Will, Stryk, and Schmude. There was an arctic cold front that pushed clouds south of the NPC on the morning limb on Oct. 7, 1994 and again on November 3 (359 and 012 Ls respectively). Lowells Band, the dark collar around the NPC, first appeared around mid-October, as reported by Warell, and persisted throughout the apparition. The NPC Regression The northern spring - early summer (22 - 112 Ls) regression of the NPC was investigated by measuring the areocentric latitudes of the caps edge from 220 bifilar micrometer measurements, 168 CCD images, and 36 video images (Fig. 2). In all cases, red filters were employed and the east-west extent of the cap was measured and corrected for phase and Ds. Areocentric latitudes were computed using the formulae derived by Beish [Dobbins, et al. 1986]. There were no statistically significant differencesbetween the micrometer, CCD, or video determinations, supporting preliminary data obtained during the 1992-1993 apparition. This is good news, since micrometric determinations are tedious and require considerable experience. We anticipate obtaining more NPC data in future apparitions as the number of astronomers submitting CCD and video images grows. It must be stressed, however, that observations must be made through red filters, since even thin arctic hazes and clouds will make the cap appear larger than it really is. Perhaps this is one reason that cap sizes derived from drawings are systematically larger. It must also be stressed that images submitted for NPC measurements be carefully calibrated; that is, flat-fielded and dark subtracted. Initially the NPC was significantly smaller than normal but then exhibited a delayed regression, similar to that observed in 1992-1993. This retardation ceased at approximately 60 Ls, after which the caps edge retreated rapidly to a latitude of 84.8 by 100 Ls. The tiny summer cap remnant remained at approximately this size into early northern summer, when the planets small apparent size precluded further measurements. A slight transient regrowth of the cap was observed between 65 and 72 Ls, corresponding to the aphelic chill. This phenomenon, first described by Dr. Clyde Tombaugh, is a temporary reforming of arctic hazes near aphelion [Capen andCapen 1970]. Overall, the 1994-1995 spring (24 -90 Ls) NPC was slightly (2.4 ) but significantly smaller than those of the 1980 and 1982 (P< 0.05>0.01), suggesting a continuation of the warming trend first observed in 1980 [Parker et al. 1983]. See Fig. 3. The 1984 North Cap exhibited unusual retardations in regression between 60 and 110 Ls, a period coinciding with the appearances of five localized dust storms [Beish and Parker 1990a]. Inclusion of this 1984 data would make the difference between 1995 and the 1980s even greater but could introduce spurious results. Our 1995 data agrees nicely with that obtained by Iwasaki [1995] and with preliminary Hubble Space Telescope (HST) values. NPC Rifts 1. The Chasma Borealis and NPC Outliers. Upon emergence from beneath the polar hood, the NPC displays a rather smooth and uniform border. Later, during the rapid thaw period, the edge of the cap will appear uneven, with numerous small, white, circular detachments along its border. By Martian summer, the NPC retreat slows and three bright projections, termed outliers, appear which detach from the cap as its edge retreats past 80 N. latitude. The white remnants may persist throughout northern summer and autumn, although this has not been the case in recent apparitions. They are named after the areas on Mars that they occupy. Their averaged center-of-area areocentric longitude positions according to G. de Mottini's 1941-52 IAU Mars map are as follows: Ierne 137 , Lemuria (Olympia) 200 , and Cecropia 297 . Lemuria is separated from the cap by a dark conspicuous rift, called the Chasma Borealis. The positions of the outliers vary form one apparition to the next, as can be seen in Table 2. The outliers and the Chasma Borealis were well observed during the 1994-1995 apparition. In January Hiroshi Ishadoh of the OAA Mars Section (Japan) observed a shadowy streak in the NPC that Masatsugu Minami of the OAA believes to be the early start of the Chasma Borealis. Parkers CCD images from late December through mid February (39 -60 Ls) reveal a concentric dark NPC rift, producing a lifesaver effect on the cap that corresponded in orientation and position to the Chasma Borealis. By 17 February the classical NPC peripheral extensions, or outliers, called Lemuria and Ierne had become completely detached from the cap. Lemuria persisted until at least late March (78 Ls) and was possibly detected as late as mid June, at 111 Ls. Ierne was imaged well into May (97 Ls). The third classical outlier, Cecropia, was not detected in its established location at 280 W, but a peripheral deposit was noted near 350 W, close to the location of one of two unnamed bright spots observed in 1982 and 1984 [Beish and Parker 1988]. This feature appeared on images taken between late February (64 Ls) and early March (68 Ls). 2. The Rima Tenuis. Giovanni Schiaparelli, while using a 9-inch refractor in 1888, noted that the north polar cap of Mars was divided in two parts by a dark rift or fissure. This observation was later confirmed by Terby and Perrotin. This rift, crossing the cap at approximate longitudes 135 and 325 , is called the Rima Tenuis and was observed many times from 1901 through 1918. Records from the British Astronomical Association (BAA) reveal that the Rima Tenuis had been observed during 1933 and again in 1950. Then it apparently disappeared for nearly 30 years. C.F. Capen searched unsuccessfully for the feature during the 1960's,even though he employed telescopes of 16, 30 and 82 inches in aperture. The Rima also eluded the Viking orbiters during the 1970s. It was not until late 1979 that the Rima Tenuis reappeared, when D. Troiani detected a dark notch at the south edge of the NPC near 335 areocentric longitude. R. Robotham, J. Dragesco, J. Beish and D. Parker observed the Rima Tenuis within days of the first observations of the notch. Later, on February 22, 1980, P. Moore and C.F. Capen observed the complete Rima Tenuis while using the Lowell Observatory's 24-inch refractor [Capen, 1980]. The first photograph of this elusive feature was obtained by A. MacFarlane on 22 February, 1980. Visibility of the Rima Tenuis has increased since 1979. While this may be due in part to improved observational technology and greater awareness of the feature, there is evidence that the Rima is intrinsically more conspicuous, since observers are detecting it with instruments as small as 6 inches in aperture. 1994-1995 is the fifth consecutive aphelic apparition during which this feature was observed. It may have been detected as early as December 2 (26 Ls), when D. Niechoy of Germany observed an NPC rift corresponding in position to the Rima. A number of reports were made between 20 December and 2 January (34 -40 Ls), when S.R. Whitby, D. Troiani, D. Parker, G. Cameron, T. Stryk, and M. Schmidt (CCD images) independently observed both notches and the rift itself. The notches in the cap edge were located at 80 and 332 areocentric longitudes. The next observations of this rift were reported on January 26 (51 Ls) by D. Joyce and D. Troiani using the Cernan Space Center (Triton College) 10" f/8 Newtonian. Troiani made a drawing showing the complete rift with his 17.5 f/4.5 scope on January 27, when M.. Schmidt and C. Tobias obtained CCD images at the Racine Observatory (Wisconsin) that clearly show the Rima Tenuis notch in the south edge of the NPC. Over the next two nights a number of midwestern observers, including D. Drake, Jesse Carroll, Troiani, and Joyce, saw the Rima Tenuis with telescopes ranging from 6 inches to 17.5 inches in aperture. On January 30th, M. Schmidt obtained excellent CCD images showing the Rima Tenuis starting at the small notch in the NPC at 332 W and cutting across the cap. Images from the HST reveal a faint streak in the cap at the right longitude. After opposition D.L. Lehman obtained quality CCD images of the Rima Tenuis on March 8 (69 Ls), and D. Parker imaged the feature between May 9 and May 23 (96 -102 Ls). METEOROLOGY Clouds, clouds and more clouds. That's what many observers reported on Mars from January through March of '95. It is most gratifying that most observers employed blue filters and thus were able to make quality observations of MarsÆ atmosphere. This is a most important part of the ALPO Mars program and one that provides a valuable source of data for professional astronomers. The following meteorological results for the 1994-1995 apparition are qualitative only, because several hundred blue-light observations are being measured and statistically analyzed by Beish and Parker for inclusion in their ongoing study of Martian clouds [Beish and Parker 1990b]. The study now includes over 24,000 drawings, photographs , and CCD images observed since 1965! Limb Clouds and Hazes. Limb brightenings, or limb arcs, are caused by scattered light from dust and dry ice particles high in the Martian atmosphere. They are often brilliant in blue light but can also be bright in all wavelengths. They were reported throughout the apparition. Morning clouds are bright, isolated patches of surface fog or frosty ground near the morning limb (Mars' western edge as seen on Earth's sky). The fogs usually dissipate by mid-morning, while the frosts may persist most of the Martian day, depending on the season. Evening clouds give the same appearance as morning clouds but are usually larger and more numerous than morning clouds. They appear as isolated bright patches over light desert regions in the late Martian afternoon and grow in size as they rotate into the late evening. Morning and evening limb clouds are distinguished from localized clouds in that they do not rotate with the planet. Limb clouds tend to cluster in the Martian tropical regions, whereas limb hazes/arcs usually extend from pole to pole. There was an abundance of morning and evening limb clouds throughout most of the apparition, with some of these clouds being very bright at times. They became particularly prominent during late northern spring, around 75 Ls, and were still detected during early summer (100 Ls), after which observations became difficult due to Mars small apparent diameter. A bright evening limb cloud appears on Parkers tricolor CCD images taken from March 28 through April 5 (77 -81 Ls). It was interesting to watch the Acidalium and Nilokeras albedo features disappear as they rotated under this cloud. A particularly unusual morning cloud was imaged by Parker between May 9 and May 19 (96 -100 Ls). This cloud had a peanut shape and appeared quite blue in color. Unlike a localized cloud, however, it did not rotate with the planet. Localized Clouds, Topographic Topographic clouds are intense bright patches of limited extent that occur seasonally over certain regions of Mars. Appearing white in integrated light, these features are best viewed and photographed through blue and blue-green filters. Occasionally they become more prominent in green and even yellow-orange light, suggesting that they may be combinations of water-ice and dust. During the 1994-1995 apparition, bright localized clouds became prominent over Libya, Chryse, and Moab starting in late January, around 50 Ls. These clouds persisted and perhaps increased in size and intensity well into northern summer. On February 18 (61 Ls), Beish reported a localized cloud formation over Xanthe-Memnonia that he called the "Capen wedge-cloud". By late February (64 Ls), discrete clouds over Xanthe, Amazonis, Argyre I and Arabia-Moab had become very conspicuous. On February 24th (63 Ls) Cameron saw a small bright spot in the Solis Lacus region and clouds over Tharsis. Hellas had some light fog in early March. On the 16th of March (72 Ls), there were a few very small bright spots in Cebrenia and Utopia. A specialized type of topographic cloud is the famous "Syrtis Blue Cloud. This is a very localized cloud that had been traced for over a century by C.F. Capen. It appears every Martian year around the northern hemisphere summer solstice and persists through early summer. This cloud circulates around the Libya Basin and then crosses over to the Syrtis Major, where it changes the color of this albedo feature to an intense blue. When Syrtis Major is viewed through a yellow filter it turns a vivid green (yellow + blue = green). This cloud was first observed in 1858 by Father Angelo Secchi, who called it the Blue Scorpion. The cloud was next seen by J. N. Lockyear in 1862 and again in 1911 by members of the BAA. C. W. Tombaugh and Capen observed the cloud early in the Martian northern hemisphere summer during the apparition of 1950. It was seen regularly in the 1960's and it was most prominent in 1982. D. Parker and J. Beish first reported the Syrtis Blue Cloud on Jan. 28th (51 Ls), and it was imaged on both morning and evening limbs several times until April 20 (87 Ls). By May 23 (102 Ls) Libya still displayed bright cloud cover with wispy tendrils extending over Syrtis Major, but no coloration was detected. On May 30 (105 Ls), however, Parker again noted the distinctive coloration. The next apparition will again be favorable for viewing the Syrtis Blue Cloud. Since this is one of the most spectacular features on Mars, we hope that observers avail themselves of the opportunity. Localized Clouds, Orographic Orographic clouds, like those that form on Earth, are white discrete clouds that are condensed from the moisture-laden air which is uplifted over a mountain or volcano. They appear bright on Mars when viewed through a blue (W#80A) or a violet (W#47) color filter. Orographic clouds are discreet white clouds which develop as moisture-laden air is uplifted over the peaks of the great volcanoes located in the Martian tropics. They form when the Martian atmosphere is high in water vapor especially in late spring or early summer of the northern hemisphere, assembling as local noon approaches, when they are best seen and photographed in blue and violet light. They continue to expand and brighten throughout the remainder of the Martian day, and by nightfall are best discerned in the violet and ultraviolet regions of the spectrum, suggesting that they are carried further aloft by convection. The most spectacular orographic clouds occur over the volcanoes of the Elysium Shield and the Tharsis Bulge. The latter clouds sometimes appear to coalesce to form the famed "W-cloud," first reported by E.C. Slipher in 1954 [Slipher, 1962]. In 1971 the Mariner 9 spacecraft probe showed them to be water clouds near the large volcanoes Olympus Mons (longitude 133 west, latitude 18 north), Ascraeus Mons (104 W, 11 N), Pavonis Mons (112 W, 0 N), and Arsia Mons (120 W, 9 S). The Elysium cloud usually forms first, and that was the case in the 1994-95 apparition. Early in December (25 Ls) some brightening over Elysium was reported, and by the months end (39 Ls) bright orographic clouds were conspicuous over this volcanic shield. This is rather normal for this region, as opposed to the 1992-93 apparition, during which the Elysium cloud were very well formed by 28 Ls. Interestingly, this appears to parallel the behavior of the NPC, which was considerably smaller during the early northern spring of the 1992-93 apparition. By mid-January (45 Ls), orographics were beginning to appear over the Tharsis volcanoes and had become very conspicuous by mid-February (57 Ls). By February 19 (61 Ls) these clouds had coalesced to form the W-Cloud. The Tharsis and Elysium orographics persisted and became larger and brighter well into northern summer. Polar Clouds, Hazes, and Hoods During northern winter a thick mantle of cloud covers the Martian arctic. Termed the North Polar Hood (NPH), this dull shroud generally breaks up around the time of the vernal equinox, revealing the bright pearly-white spring NPC. It is uncertain whether the NPC is formed from the dissolving hood or was lying fully formed beneath the cloud layer during northern winter. Near-infrared CCD images taken by Parker in October, 1992, suggest the former state of affairs. These images, taken during late northern winter (346 Ls), reveal named albedo features beneath the NPH with no evidence of the large spring cap which appeared a few weeks later when the hood dissipated [Parker and Berry 1993]. Similar evidence was obtained from infrared observations from Tokyo and from the University of Arizonas Catalina Telescope during the period Ls=347 -354 [Ebisawa 1995b]. These investigators also imaged the tiny permanent cap remnant beneath the hood, but found no trace of the large surface cap spring surface cap that was to emerge only a few weeks later. During the 1994-95 apparition the NPH became variable and thin near the vernal equinox. Both Whitby and Niechoy reported a large, dull hood between 346-347 Ls; but, by 354 Ls (Sept. 28), Niechoy detected the cap largely free of the hood. By 356-358 Ls, Whitby, Warell, and Parker all observed the NPC clear of the NPH, bordered by the dark Lowells Band. As the NPC retreated a number of observers spotted polar clouds, especially on the morning side of the cap. These were reported on Dec. 1 (25 Ls), Feb. 3-6 (54 -55 Ls), and on March 8 (68 Ls). J. Beish saw a light haze over the cap, possibly the start of the "aphelic chill" on the 8th of February. Micrometer and CCD measurements revealed a small but significant re-growth of the NPC around the time of aphelion at 70 Ls. Equatorial Cloud Bands (ECBÆs) Perhaps the most interesting formations, however, are the equatorial cloud bands (ECBs). These are faint veils of wispy white clouds with variable shapes and transparencies that extend across the Martian disk within 20 of the equator. Residing at high altitudes and probably composed of CO2 ice crystals, ECBs are best detected with dark blue (W47 or W47B) filters. Until recently, cloud bands were thought to be exceedingly rare phenomena that were most likely to occur during the Martian northern summer. However, systematic tri-color CCD imaging has uncovered evidence that these wisps of cloud bands may be more frequent and may occur in all Martian seasons. They were seen and imaged on numerous occasions during the latter half of the 1992-93 apparition, being much more prominent on CCD images than they were visually or photographically. The ability of the CCD camera to reveal subtle cloud structures that are only 1-2% brighter than the background demonstrates the power of electronic image processing. This did create a problem, however, since it was uncertain whether the increase in ECBs during the last apparition was real or merely due to better imaging techniques. It was hoped that the 1994-95 apparition would clarify the matter. While ECBs were not usually specifically mentioned, they do appear on a few blue-light drawings from a number of observers, including J. Beish, C. Hernandez, D. Lehman, R. McKim, D. Niechoy, , R. Schmude, T. Stryk, and S. Whitby. Parkers CCD images again revealed them on several occasions. These delicate features were most prevalent over Tharsis and Amazonis during February and March. More information on ECB prevalence awaits Beishs statistical analysis. Dust Clouds As expected, no major dust clouds were reported during this apparition; but some very minor dust activity was observed in 1994. Stryk reported a small, transient dust cloud over Argyre on 5 June (290 Ls) [Stryk, 1994]. On 5 October (358 Ls), it appears that there was dust in the atmosphere over Chryse making it very bright at times in red light. In addition, a small thin dust cloud in Xanthe was first observed by Whitby on Nov. 3 (12 Ls). It was again seen on the 13th and 14th by Ted Stryk, who reported some expansion on 14 November. Analysis of color filter observations suggests that there was some dust mixed in the clouds over the Chryse region in March and a small dusty spot near Solis Lacus. This admixture of dust with the prevalent water-ice crystal clouds was verified by polarization measurements of Ebisawa [1995], who detected dust present in the Chryse-Xanthe-Tharsis clouds in late January (50 Ls). In addition, a bar-like dust cloud was seen at the same time over Arcadia-Tempe, similar to the more conspicuous one observed in 1982 around 122 Ls [McKim 1985]. Finally, Ebisawas polarization data revealed dust mixed with the Elysium shield clouds in mid-January (45 Ls). It should be noted, however, that the phase angle (the Earth-Sun angle as seen from Mars) in mid-January was about 25 . This is where the signs of polarization of both water-ice clouds and dust clouds changes, making differentiation of cloud types nearly impossible with this method. SURFACE FEATURES Region I: 250 W-010 W Syrtis Major was dark throughout the apparition, exhibiting little change from 1992- 93. It displayed average width, with a blunted northern border. Osiridis Promontorium, at the northeast border of Syrtis Major was again prominent. Moeris Lacus, a short streak just south of Osiridis, was again seen jutting into Libya. The Thoth-Nepenthes canal, so conspicuous from 1954 to 1967, was not seen. The Laocoontis-Nubis Lacus complex was also absent, as it has been since 1982, although Seigel and Falsarella drew it faintly in March. Nodus Alcyonius, northeast of Syrtis Major, was extremely dark and elongated NE- SW. To the south, Hellas was bright with cloud or fog both before and after opposition. In February, however, the floor of this great basin was cloud-free, revealing the Hellas Cross, consisting of Peneus, Alpheus, and Zea Lacus. West of Syrtis, Astaborae Sinus was faintly seen by Cave, Schmude, and Stryk. To the north, Nilosyrtis and Astusapes were faint to absent, although the former was reported after opposition by Cameron, Haas, Teichert, and Niechoy. Boreosyrtis and Umbra were dark. Moving westward, Protonilus, Ismenius Lacus, and Deuteronilus were fairly well defined on both CCD images and drawings from several observers, including Cameron, Fabian, Teichert, and Troiani. Sabaeus Sinus was quite dark, and its eastern end, which had been faded since 1990, resumed a more normal aspect, as reported by Cave, Lehman, and Cameron. Despite the markedly positive De, Pandorae Fretum was very well seen by most observers. It was very dark and appears to have shifted southward from its usual position. In late January (52 LS), however, Hernandez found only the eastern half of Pandorae Fr. to be dark, with the western portion halftone. He also detected the dark Vulcani Pelagus projecting from the eastern border of Erythraeum M. Classically, Syrtis Major broadens after northern summer solstice (90 Ls). No significant changes in its breadth were observed during this apparition, agreeing with HST data [Lee et al. 1995]. This feature demonstrated a high degree of variability during the 1970s and early 1980s, but it has remained fairly stable since the 1984 apparition. Region II: 010 W-130 W Margaritifer S. And Aurorae S. were well defined and of normal intensity. Oxia Palus was prominent, as it has been for several years. The delicate filament Cantabras, joining the western fork of Meridiani S. With Oxia P. was seen on CCD images. At least four small, dark, round features were seen in southern Chryse-Xanthe, including Hydapsis S., Iamunae S., Hydrae P., and Clytaemnestrae L. These were also conspicuous in the 1992-1993 apparition. These features do not correspond well with those on classical maps it would appear that the areography of the northern Chryse-Xanthe region is somewhat inconsistent. To the west, in Candor, Juventae Fons was again prominent and Ganges was broad but only dusky. McKim reported that Lunae L., so noticeable in the early 1980s, was again faint. Several observers found western Nilokeras to be faint, while at its eastern end it appeared double (Nilokeras I and II). Idaeus Fons and Achillus F. presented as two dark nodules west of Niliacus. Prior to opposition, Niliacus was darker than Acidalium M., but by March Crocker and Parker found that it had lightened somewhat. To the south, Agathadaemon, Melas L., and the Tithonius L. Complex were distinct. Solis Lacus was dark and elongated E-W. It has undergone little change since the 1986 apparition. Gallinaria Silva was a distinct dark dot west of Solis L. The canal Phasis, joining Gallinaria to Aonius S. was not imaged or reported. This variable feature had resumed prominence in May, 1984, darkened in 1986, but had faded during the 1988 apparition. Then, in 1990, it became very prominent after the early November dust storm [McKim 1992] but was barely perceptible during the 1992-93 apparition. Acampsis, linking Solis L. to Gallinaria was drawn and imaged by several observers, and the unnamed dark streak running west from Gallinaria to near Gomer S. was seen and imaged in December and in March. Near opposition it had faded but was still barely perceptible on CCD images. This streak, running along the northern borders of Sirenum M. and Cimmerium M. was first detected in August, 1988 by S. OMeara and D. Parker and has been reported sporadically since. Like Eumenides to the north, this feature seems to be most prominent when Mars phase angle is greatest, and may thus be linked to shadow effects. In addition to the numerous clouds in Tharsis, some albedo feature changes were reported. In early December (28 Ls) Teichert recorded a darkening of Ascraeus Lacus. Again, in late March (75 Ls) Siegel, Warell, Teichert, Lehman found this feature dark, with Cameron and McKim reporting Uranius to be broad and dark. Whitby also observed a darkening in Ceraunius in late January (48 Ls). Region III: 130 W-250 W T. Cave and W. Haas reported Laestrygonum Sinus well-detached from Cimmerium M. in March, when Haas also sighted the canals Cyclops and Cerberus II. The dark patch in eastern Aetheria, prominent since 1977 and termed the Hyblaeus Extension by C. Capen, remained dark during 1994-95. Cerberus I, forming the southern border of the Elysium Shield, displayed some interesting changes, proving that it is a highly variable feature. In fact, this was one of the features targeted for intensive study by the HST. It was a dark and conspicuous feature throughout the 1950s and early 1960s, weakening in 1965 and more in 1967, but returning as a thin but dark feature in 1969. It remained conspicuous until the 1975 apparition, when it reached near invisibility. It recovered somewhat in 1977 and darkened dramatically after opposition in 1980. After the February and May dust storms of 1982, Cerberus weakened, a trend that continued after the 1984 dust events. Since 1984,Cerberus has remained faded, although there has been some variations in its intensity. In 1994-95 Cerberus was fairly dark and conspicuous early in the apparition. However it became fainter by late November and early December (23-25 Ls) when Trivium-Cerberus appeared on CCD images as a halftone streak with 2-3 diffuse nuclei. >From 2-12 January (40-44 Ls) it had weakened considerably, becoming a weak thin streak with Trivium a small dark dot. During mid-February (57-60 Ls) the complex was barely visible, appearing as only three small dots. Parkers March 18-25 CCD images (both tricolor and red light) showed Cerberus still weak, just three small dots, especially after local noon. Interestingly, however, several very experienced ALPO observers independently reported that Cerberus became quite dark and streak-like around March 14. During April the feature darkened considerably as noted on both drawings and CCD images. It maintained that aspect for the remainder of the apparition, but was still not as conspicuous as it had been during the 1970s. CONCLUSIONS Despite the unfavorable aspect that Mars presented during the 1994-1995 apparition, much useful data was obtained. This was largely due to the high quality of the observations submitted. Many IMP astronomers systematically observed Mars when it was less than 6 arc-seconds in apparent size, thus significantly extending the seasonal coverage. Over 50% of observers, both visual and photographic, regularly employed color filters this is the highest proportion to date, and we hope that the trend continues. In addition, the vast majority of the observations submitted were properly documented as to image orientation, dates, times, CMs, etc., and the quality of the reports was, on the average, the highest we have seen. Despite the high tech contributions of CCD imaging and active optics assisted photography, the visual drawing remains the backbone of Mars observations. Cases in point areTroianis 1994-95 Mars maps (Figs. 4-5) that were highly praised by a number of professionals at the MTO Workshop. Even though Troiani generated these on a computer, they were produced entirely from the amateur observations submitted to the A.L.P.O. Mars Section. Many thanks to all our observers! ACKNOWLEDGEMENTS The Mars Section of the Association of Lunar and Planetary Observers wishes to express its gratitude for the contributions of fellow A.L.P.O. members as well as those of the British Astronomical Association and the Oriental Astronomical Association. REFERENCES Beish, J.D. and Parker, D.C. (1988) "The 1983-85 Aphelic Apparition of Mars - Report I", J.A.L.P.O., Vol. 32, Nos. 9-10, p. 192. Beish, J.D. and D.C. Parker (1990a). "The 1983-85 Aphelic Apparition of Mars-Part II" J.A.L.P.O., Vol. 34, Nos. 2, pp 62-79. Beish, J.D., and D.C. Parker 1990b). "Meteorological Survey of Mars, 1968-1985," Journal of Geophysical Research, Vol. 95, B9, pp. 14567-14675. August 20. Bell, J.F. III and J.E. Moersch, eds. (1995). Workshop on Mars Telescopic Observations. LPI Tech. Rpt. 95-04. Order from: Order Dept. Lunar and Planetary Institute, Houston, TX 77058-1113. No charge, but send $5.00 (US) for S&H. Capen, C.F. and V.W. Capen (1970). Martian North Polar Cap, 1962-68. Icarus, 13:1, pp. 100-108. Dobbins, T.A., D.C. Parker, and C.F. Capen (1986). Introduction to Observing and Photographing the Solar System. Richmond: Willmann-Bell, Inc. pp. 193-201. Ebisawa, S. (1995a). Mars Observations During The Period of 1994-1995 Apparition. Dust Storm Displays: A Quick Preliminary Report. Planetary Res. Obs. Contrib. No. 23, Feb. Ebisawa, S. (1995b). Probable Existence of the Martian North Permanent Cap Beneath the Winter Polar Hood and Beneath the Saesonal Ground Cap in Spring-Summer Season: A Preliminary Report. Planetary Res. Obs. Contrib. No. 24, Aug. Iwasaki, K., T. Akabane, R. Sagar, K.K. Ghosh, M. Raharto, and F. Dirghantara (1995). Regression of Martian Polar Cap 1994-1995. Proc. 28th ISAS Lunar and Planetary Symp 1995. Lee, S.W., M.J. Wolff, P.B. James, L.J. Martin, R.T. Clancy, and J.F. Bell (1995). HST Observations of Time-variable Albedo Features on Mars. Workshop on Mars Telescopic Observations, LPI Tech. Rpt. No. 95-04, p.19. McKim, R. (1985). The Opposition of Mars, 1982. J. Brit. Astron. Assoc. 96:1, 36-52. McKim, R. (1992). The Opposition of Mars, 1990. J. Brit. Astron. Assoc. 102:5, 251. Parker, D.C., Capen, C.F., and Beish, J.D. (1983). "Exploring the Martian Arctic", Sky & Telescope Magazine, Vol. 65, No. 3, March. Parker, D.C. and R. Berry (1993). Clear Skies on Mars. Astronomy, 21:7, pp. 72-77, July. Stryk, T. (1994). The Martian Dust Cloud of 1994 Jun 05: Appearance and Implications. J.A.L.P.O., 38:2, 85-86. Table 1. Members of the A.L.P.O. International Mars Patrol for the 1994-1995 Apparition Observer Location Observer Makoto Adachi Ohtsu City, Japan Osczr Arnal Ontario, Canada Greg Banialis Arlington Hts., IL Jeff Beish Miami, FL Phillip Budine Walton, NY Gary Cameron Des Moines, IA Lawrence Carlino Lockport, NY Jesse Carroll Chicago, IL Jim Carroll Chicago, IL Thomas Cave Long Beach, CA Mt. Wilson, CA Vanessa Cave Long Beach, CA John Crocker Chicago, IL Brian Cudnik Flagstaff, AZ Tom Dobbins Coshocton, OH Darren Drake Indian Head Pk., IL Garry Dymond St. John, Canada Karl Fabian Hickory Hills, IL Nelson Falsarella San Jose, Brazil Vincent Giovannone Latham, NY David Graham N. Yorkshire, UK David Gray County Durham, UK Bob Gunnerson Loveland, CO Walter Haas Las Cruces, NM David Hanon Chattanooga, TN Carlos Hernandez Miami, FL Richard Hill Tucson, AZ Hiroshi Ishado Okinawa, Japan Tohru Iwasaki Morodomi, Japan Chuck Jacobson Puyallup, WA Daniel Joyce Chicago, IL David Lehman Pinedale, CA Michael Mattei Littleton, MA Richard McKim Oundle, UK Frank Melillo Holtsville, NY Masatsugu Minami Fukui, Japan Patrick Moore Selsey, UK Yukio Morita Hatssuka, Japan Mike Morrow Ewa Beach, HI Masami Murakami Fujisawa, Japan Takashi Nakajima Fukui, Japan Detlev Niechoy Goettingen, Germany Gary Nowak Essex Jct., VT Yoshio Ohba Yamagata, Japan Don Parker Coral Gables, FL Cecil Post Las Cruces, NM Phil Plante Poland, OH Terry Platt Binfield Berks, UK Robert Robinson Morgantown, WV Mark Schmidt Racine, WI Richard Schmude Barnesville, GA Elisabeth Siegel Agertoften, Denmark Robert Smith Huntville, AK Chester Spell Woodstock, GA Robert Soltis LaJolla, CA Ted Stryk Bristol, VA Gerard Teichert Hattstatt, France Greg Terrance Lima, NY Chris Tobias Racine, WI Daniel Troiani Schaumberg, IL Robert Young Harrisburg, PA Johan Warell Uppsala, Sweden John Westfall San Francisco, CA Samuel Whitby Hopewell, VA Matthew Will Springfield, IL Pat Winemiller Terre Haute, IN Gene Witkowski Buffalo, NY Mike Zweifel Yorkville, WI Table 2. NPC Residuals (Bright Projections, ôOutliers.ö) Observer, Years, Ierne, Lemuria, Cecropia Schiaparelli 1879-88 121 208 310 Lowell 1901-05 122 206 311 Antoniadi 1903-29 122 208 309 Maggini 1918-35 136 213 278 de Mottoni 1941-52 137 200 297 Dollfus 1946-52 142 227 292 Capen 1962-68 140 196 290 Beish/Parker/ 1981-82 132 205 280 Capen/Dragesco Beish/Parker/ 1983-85 142 205 282 Hernandez/Dragesco Mean 133 208 294 Range 121 -142 196 -227 278 -311
1. 1994 June 07, 09:55 UT, CM: 127 , Ls: 290 , 10-in (25-cm) Newt. Filter: None. Ted Stryk. First observation of the apparition showing prominent southern maria. De: -17 . Diameter only 4.45 arc- sec. 2. 1994 Nov 02, 08:15 UT, CM: 106 , Ls: 012 , 16-in (41-cm) Newt. Filter: W47. Don Parker. Prominent evening limb cloud with terminator projection; bright morning limb haze. 3. 1994 Nov 03, 10:45 UT, CM: 133 , Ls: 012 , 7-in. (17.8-cm) Refr. Filter: W21. Samuel Whitby. N. Polar collar dark in orange light; morning limb haze. 4. 1994 Dec 01, 08:31 UT, CM: 194 , Ls: 025 , 16-in (41-cm) Newt. Don Parker. From tricolor CCD image showing dark streak along northern border of Cimmerium M. Hyblaeus extension prominent; Trivium-Cerberus halftone. Lynxx PC camera. 5. 1994 Dec 26, 06:40 UT, CM: 294 , Ls: 037 , 17.5-in (45-cm) Newt. Filter: W25. Dan Troiani. Rima notch at edge of NPC , bright spot in Hellas. 6. 1994 Dec 30, 09:20 UT, Cm: 276 , Ls: 39 , 14.25-in (36-cm) Newt. Gene Witkowski. From video image showing faint Rima Tenuis. 7. 1995 Jan 01, 07:30 UT, CM: 251 Ls: 39 , 8-in (20-cm) Newt. Filter: W30. Carlos Hernandez. Elysium cloud on evening limb. Hyblaeus extension, N. Alcyonius, and Cerberus prominent. 8. 1995 Jan 06, 08:40 UT, CM: 38 , Ls: 42 , 12.8-in (32.5-cm) Newt. Filters: R,O,B. Thomas Cave. Trivium-Cerberus still dark but thin. 9. 1995 Jan 10, 05:45 UT, CM: 144 , Ls: 043 , 8-in (20-cm) Newt. Filter: W30 (magenta). Carlos Hernandez. Tractus Albus noted over Tempe-Tharsis. Propontis complex prominent. 10. 1995 Jan 10, 05:55 UT, CM: 147 , Ls: 043 , 8-in (20-cm) Newt. Filter: W38A. Carlos Hernandez. Equatorial Cloud Band (ECB) over Memnonia-Tharsis. Refer to red light observation Figure 9. 11. 1995 Jan 20, 06:00 UT CM: 059 , Ls: 048 , 4.25-in (11-cm) Schief. Filters: W23A, 80A. Gary Cameron. Chryse-Xanthe bright. Lunae Lacus dusky, not discrete. 12. 1995 Jan 21, 00:25 UT, CM: 328 , Ls: 048 , 15-in (38-cm) Newt. Filters: None. Patrick Moore. Hellas light; Pandorae Fr. noted. 13. 1995 Jan 26, 09:10 UT, CM: 052 , Ls: 050 , 8-in (20-cm) Newt. Filters: None. Robert Smith. Idaeus Fons dark; Lunae L. not noted. 14. 1995 Jan 27, 09:10 UT, CM: 096 , Ls: 048 , 10-in (25-cm) Newt. Filters: None. Daniel Joyce. Rima Tenuis visible. Again, Lunae L. not noted. 15. 1995, Jan 28, 02:45 UT, CM: 300 , Ls: 051 , 8-in (20-cm) Newt. Filters: R,O,G,B. Nelson Falsarella. Sabaeus Sinus dark along its length; Pandorae Fr. prominent. 16. 1995 Jan 29, 05:30 UT, CM: 326 , Ls: 052 , 17.5-in (45-cm) Newt. Filter: None. Dan Troiani. Rima Tenuis prominent. 17. 1995 Feb 02, 23:26 UT, CM: 199 , Ls: 054 , 12.5-in (32-cm) Tri-schief. From color CCD camera (Starlight Xpress). Terry Platt. Orographic clouds Arcadia-Tharsis on evening limb. Propontis complex prominent. 18. 1995 Feb 02, 07:20 UT, CM: 324 , Ls: 054 , 14-in (36-cm) Newt. Filters: W25A. Richard Hill. Numerous canals, including Arosis-Sitacus, Astaboras, and Hiddekel noted. 19. 1995 Feb 03, 05:35 UT, CM: 289 , Ls: 054 , 16-in (41-cm) Newt. Filters: Tricolor CCD image. Lynxx PC camera. Don Parker. Hellas Cross noted. Boreosyrtis prominent. 20. 1995 Feb 05, 05:05 UT, CM: 265 , Ls: 055 , 11-in (28-cm) SCT. Filters: R,O,G.B. Gerard Teichert. Casius dark on CM; Nasamon seen extending from northeastern Syrtis Major. Bright cloud over Aethiopis.
21. 1995 Feb 06, 03:50 UT, CM: 238 , Ls: 055 , 10-in (25-cm) Newt. Filter: W23A. John Crocker. Hyblaeus extension dark, broad; Trivium-Cerberus very weak. 22. 1995 Feb 07, 03:45 UT, CM: 228 , Ls: 056 , 10-in (25-cm) Newt. Filters: R,G,B,Y. Ted Stryk. Detail of NPC outliers, Rima Borealis. 23. 1995 Feb 02, 02:59 UT, CM: 260 , Ls: 054 , 16-in (41-cm) Newt. Greg Terrance. Integrated light Lynxx PC CCD image showing Hyblaeus extension broad and dusky. Cerberus very weak on PM limb. 24. 1995 Feb 11, 06:37 UT, CM: 235 , Ls: 058 , 16-in (41-cm) Newt. Filters: Tricolor CCD image. Lynxx PC camera. Don Parker. Trivium-Cerberus now very weak. 25. 1995 Feb 12, 06:45 UT, CM: 228 , Ls: 058 , 14-in (36-cm) Newt. Filter: W23A. Richard Hill. Trivium-Cerberus more prominent. 26. 1995 Feb 18, 03:03 UT, CM: 122 , Ls: 061 , 16-in (41-cm) Newt. Filters: Tricolor CCD image. Lynxx PC camera. Don Parker. Prominent orographic clouds over Tharsis. 27. 1995 Feb 20, 04:20 UT, CM: 123 , Ls: 062 , 10-in (25-cm) Newt. Filter: W25, 38A. David Lehman. Clouds over Tharsis. Possible polar cloud on CM (Ierne region). 28. 1995 Feb 22, 19:47 UT, CM: 332 , Ls: 062 , 11-in (28-cm) SCT. Filters: R,O,Y,G,B. Gerard Teichert. Sabaeus S. dark throughout its length; Pandorae Fr. strong, broad. 29. 1995 Feb 22, 03:40 UT, CM: 095 , Ls: 062 , 12.8-in (32.5-cm) Newt. Filters: R,O,B. Thomas Cave. Clouds over Xanthe, Arcadia, Tempe, and near Olympus Mons. Lunae Lacus weak. 30. 1995 Feb 26, 01:40 UT, CM: 031 , Ls: 064 , 4.25-in (11-cm) Schief. Filters: W23A, 80A. Gary Cameron. Clouds over Candor on AM limb; clouds over Chryse, Arabia-Moab, and south limb. Lunae Lacus weak. 31. 1995 Feb 26, 04:30 UT, CM: 72 , Ls: 064 , 14-in (36-cm) Newt. Filters: W25A. Richard Hill. Lunae L. very weak; Ganges prominent. Acidalius Fons dark at S. border of NPC with Issedon joining it to Nilokeras. Lunae Lacus not discrete. Blue light observation reveals AM and PM limb clouds. 32. 1995 Feb 28, 02:48 UT, CM: 030 , Ls: 065 , 16-in (41-cm) Newt. Don Parker. From tricolor CCD image. Lynxx PC camera. Bright cloud on AM limb over western Tempe. Hazes across Chryse and Moab. Nuclei in Idaeus F. Lunae L. weak. 33. 1995 Mar 01, 01:58 UT, CM: 009 , Ls: 065 , 7-in (18-cm) Refr. ST-5 camera CCD image. David Hanon. Achillus P. light. Ismenius L., Deuteronilus, Dirce F., and Gehon detected! 34. 1995 Mar 04, 21:00 UT CM: 262 , Ls: 067 , 8-in (20-cm) SCT. Filters: None. Report with W25, 15, 58, 80A, 47. Elisabeth Siegel. Hyblaeus extension prominent. Aeria, Ausonia, and PM limb brightest with W80A. 35. 1995 Mar 04, 00:40 UT, CM: 324 , Ls: 067 , 6-in (15-cm) Refr. Filter: W23A. Lawrence Carlino. Aeria bright (see observation # 34); Sabaeus S. and Hellespontis dark. 36. 1995 Mar 11, 01:45 UT, CM: 278 , Ls: 070 , 7-in (18-cm) Newt. Filters: W25, 23A. Gary Cameron. Rima Tenuis noted. Hellas bright in red and blue light. Clouds reported over Moab, Aethiopis, and Elysium. 37. 1995 Mar 13, 03:00 UT, CM: 274 , Ls: 071 , 100-in (2.5-M) Mt. Wilson Coud. Filters: R,M. Thomas Cave. Bright PM limb cloud (Elysium). Numerous small white areas in desert regions. Edge of NPC scalloped. 38. 1995 Mar 14, 02:25 UT, CM: 261 , Ls: 071 , 6-in (15-cm) Refr. Filters: W25, 12, 80A, 38A. Phillip Budine. Nilosyrtis prominent. Cerberus darkening. 39. 1995 Mar 14, 01:55 UT, CM: 253 , Ls: 071 , 6-in (15-cm) Refr. Filter: Y8, Phil Plante. Aeria very bright on AM limb; Trivium-Cerberus reported as dusky. 40. 1995 Mar 14, 03:00 UT, CM: 267 , Ls: 071 , 12.8-in (32.5-cm) Newt. Filters: R,O. Vanessa Cave. Trivium-Cerberus darkened. Albor bright in NE Elysium.
41. 1995 Mar 21, 20:00 UT, CM: 095 , Ls: 074 , 8-in (20-cm) SCT. Filters: None for drawing. Report with W25, 15, 58, 80A, 47. Elisabeth Siegel. Ascraeus L. and Ceraunius prominent near CM. 42. 1995 Mar 21, 04:45 UT, CM: 231 , Ls: 074 , 12.5-in (32-cm) Newt. Filter: W25A. Walter Haas. NPC peanut-shaped. Cerberus II extending between Pambotis L. and Gomer S. Symplegades Insula bright. 43. 1995 Mar 22, 22:32 UT, CM: 122 , Ls: 075 , 12.5-in (32-cm) Tri-schief. From color CCD camera (Starlight Xpress). Terry Platt. Numerous orographic clouds over Tharsis. 44. 1995 Mar 23, 03:55 UT, CM: 201 , Ls: 075 , 16-in (41-cm) Newt. Filters: Tricolor CCD image. Lynxx PC camera. Don Parker. Trivium-Cerberus strengthening. Tharsis orographics on PM limb. 45. 1995 Mar 31, 01:28 UT, CM: 092 , Ls: 079 , 16-in (41-cm) Newt. Filters: Tricolor CCD image. Lynxx PC camera. Don Parker. Bright cloud on AM limb over Memnonia. Cloud wisps over Tharsis. 46. 1995 Mar 31, 01:15 UT CM: 089 , Ls: 078 , 16-in (41-cm) Newt. Filters: W47, 47B. Jeff Beish. Band cloud and numerous discrete clouds over Tharsis, Xanthe. 47. 1995 Apr 09, 20:05 UT CM: 281 , Ls: 083 , 6.3-in (16-cm) Refr. Filters: W21. Johan Warell. PM limb haze. Hellas bright. Pambotis Lacus noted adjacent to bright PM limb. 48. 1995 Apr 12, 20:00 UT, CM: 252 , Ls: 084 , 8.5-in (21.6-cm) Newt. Filters: None. Richard McKim. Trivium-Cerberus darkened. Brightening over Libya-Isidis R.-Neith R.-Aeria (Blue Syrtis Cloud?). PM limb bright. 49. 1995 Apr 13 20:40 UT, CM: 253 , Ls: 085 , 16-in (42-cm) Dall-Kirk. Filters: I.L., W15. David Gray. Cerberus I and II visible. Elysium complex well-defined. 50. 1995 Apr 28, 21:10 UT, CM: 119 , Ls: 091 , 16-in (42-cm) Dall-Kirk. Filters: I.L., W15. David Gray. Tharsis features noted: Nodus Gordii, Eumenides, Ascraeus L., Ascuris L., and dusky bands. 51. 1995 May 13 21:20 UT, CM: 339 , Ls: 097 , 16-in (42-cm) Dall-Kirk. Filters: I.L., W15. David Gray. Hellas, Chryse bright; Protonilus, Ismenius L., Deuteronilus, Hiddekel, and Gehon noted. 52. May 30, 02:05 UT, CM: 255 , Ls: 105 , 16-in (41-cm) Newt. Filter: W47. Don Parker. ECB over Aethiopis-Isidis. Bright limb clouds. Syrtis Major covered with the Blue Syrtis Cloud. NPC Outliers 53. 1995 Feb 18, 03:15 UT, CM: 125 , Ls: 060 , 16-in (41-cm) Newt. Filters: Red light (Schott RG- 610) CCD image. Lynxx PC camera. Don Parker. Outliers Ierne and Lemuria south of NPC, separated from it by the Chasma Borealis. 54. 1995 Feb 18, 01:50 UT, CM: 104 , Ls: 060 , 16-in (41-cm) Newt. Filters: W25, 22. Don Parker. Ierne west of the NPC; small outlier glimpsed on PM limb. 55. 1995 Feb 25, 02:33 UT, CM: 053 , Ls: 064 , 16-in (41-cm) Newt. Filters: Red light (Schott RG- 610) CCD image. Lynxx PC camera. Ierne west of NPC. Small outlier in northern Ortygia east of NPC. 56. 1995 Mar 23, 01:56 UT, CM: 172 , Ls: 075 , 16-in (41-cm) Newt. Filters: Red light (Schott RG-610) CCD image. Lynxx PC camera. Lemuria southwest of NPC.
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