Over fifty finder charts and images and updated feature lists are presented to aid the amateur lunar observer to locate, image and enjoy dark haloed craters and dark mantle regions.
In November 2006, the ALPO Lunar Observing Section suggested reviving its dark haloed crater (DHC) observing program. (Benton 2006). Benton suggested a literature review update to the 1976 ALPO DHC observing list. (Id). The 1976 ALPO Dark Haloed Crater observing list was republished and has been previously digitized. (Dembowski 2006, UAI 2004). The 1976 ALPO observing list of 83 known and suspected DHCs contains feature positions in a data format; no feature was associated with letter satellite names. It was felt that a more natural language feature table, an updated a post-1976 literature search and finder charts, might aid amateur interest in DHC observing generally and the ALPO announcement.
A 194 entry, updated DHC observing list was developed.
In professional journal literature, two whole nearside lunar maps showing the distribution of known dark-haloed craters have been produced, but no DHC catalogues were published. Fig. 6 in Schultz and Spudis 1979, Fig. 2 in Salisbury, Alder and Smalley 1968). A further journal literature review located a supplemental catalogue of over 100 DHCs on the western limb and three miscellaneous DHC identifications. (Antonenko 1999a, Giguere et al 1998).
These sources were consolidated into a feature list of 194 items. (Figures 1, 2 and 3 below, DHC List All by Lat-Long (N=194)). Because the list is provisional, duplications have not been removed. Feature identification numbers were assigned in order to enhance referencing of features. For ease of reading, many of DHC data characteristics listed in the original 1976 ALPO catalogue were converted to natural language comments, e.g. - the shape of the halo and whether it is located on a mare or in a crater. The positions of these features were charted in Virtual Moon Atlas and Mosher's and Bondo's Lunar Terminator Visualization Tool (LTVT) and where applicable, DHC features corresponding to satellite craters were assigned lettered satellite crater catalogue identifications. In the revised list presented here, 78 DHCs are identified either as being inside a crater or by a satellite feature lettered name.
All of the Antonenko designated DHCs on the far western limb may not be telescopically visible from Earth. Antonenko designated as DHCs, some craters where the halo has faded but the dark mare layer is visible inside the crater. Since this list is intended to be provisional - that is a list of potential targets whose telescopic visibility should be resolved - no attempt was made to mark such problematic DHCs. In general, they consist of a few features limited to the far western limb in the West Humorum and Procellarum DHC regions.
DHCs in clusters were assigned informal DHC group names by this author. 21 DHC group names were assigned. (Figure 2).
Thirty-five DHC finder charts were developed using LTVT and Clementine color albedo images as an aid to locating these features. (USGS 2006). These charts and images are presented below. For each DHC region, three aids are provided: a labeled finder chart, an unlabeled USGS Clementine color albedo image for the corresponding region, and observing planning data including selenographic position, lunar age when the terminator crosses the region and the applicable Rükl chart number. Where applicable, a cross-reference to Lunar Aeronautical Chart (LAC), LTO and USGS Geologic Atlas of the Moon charts is provided. See DHC List All by Lat-Long (N=194). DHCs strongly stand out from the background of Clementine color albedo images.
Excluded from the class of dark halo craters are large craters with dark ejecta blankets and bright rays and dark-rayed craters. (Schultz and Spudis 1979). Large craters with dark ejecta blankets and bright rays include Copernicus, Langrenus, Theophilus, Maunder, and Tycho. Dark-rayed craters include Dionysius. These features are not included in the DHC observing list. Giguere, Hawke and Gaddis et al provide a recent in depth study of the dark-rayed crater Dionysius. (Giguere, Hawke and Gaddis et al 2006).
Building the DHCs list naturally led to study of two DHC related features: dark mantle regions and cryptomaria, i.e. - mares hidden by overburden layers.
Seventeen DMR finder charts - in the form of Clementine color albedo images - are compiled here to aid in locating their positions, along with lunar age and Rükl chart data. From a literature search, a list of 15 nearside dark mantle regions (DMRs) and localized dark mantle deposits (LDMDs) was developed. (Gaddis, Pieters and Hawke 1985). Hawke, Cooms and Gaddis et al developed a nearside whole moon map of over 50 localized dark mantle deposits, but no catalogue of their LDMD feature positions was published. (Fig. 1 in Hawke, Coombs and Gaddis et al 1989). Hawke, Cooms and Gaddis et al LDMDs are not included here.
A list of eight nearside cryptomaria regions was also developed. (Antonenko 1999d, Antonenko 1999c, Table 5,, infra).
Some DHC clusters are related to lunar light plains. A comprehensive catalogue of lunar light plains could not be found in journal literature; a light-plains feature list is not presented here.
Dark halo craters form by two primary processes:
Dark mantled regions and localized dark mantle deposits form as a result of pyroclastic deposition from point sources or linear sources (straight and sinuous rimae) (Head 1976 , Schultz and Spudis 1979, Figure 1.27 in Hiesinger and Head 2006 at pp. 35-36, 40-42). An example of point source pyroclastic dark mantling can be seen in the local dark mantle deposit in crater J. Herschel (Figure 57, below). Examples of linear source pyroclastic deposition include the northern rimae of crater Messala (Figure 42 and Figure 43, below), and the dark mantle regions east of Aristoteles that flank C. Baily, (Figure 46, below), the dark mantle region surrounding Rimae Sulpicius Gallus (Figure 48, below) and the dark mantle region west of Rima Bode (Figure 51, below). Dark mantle regions are distinguished from localized deposits by area. Dark mantle regions have more than 1,000 square kilometers in deposition area; localized dark mantle deposits are less than 1,000 square kilometers in deposition area.
Meteor impacts do not uniformly distribute excavated ejecta. Materials ejected at higher velocities travel at a higher angle and to a further distance. Materials ejected at lower velocities travel at a lower angle and for a shorter distance. As the impact excavates the crater deeper, the kinetic energy of the impact is consumed. Materials at ejected from lower levels of a crater receive lower impact energy and travel at lower angles and for shorter distances. (Hiesinger and Head 2006, p. 21). The result on the surface of the Moon is the common pattern of brighter rays - consisting of further traveling surface particles ejected in a curtain early during the impact process - and the ejecta blanket - consisting of deeper excavated materials that travel a shorter distance during the later, lower-energy phase of the impact. Smaller meteors have less energy and excavate smaller, shallower craters; larger meteors have more kinetic energy and excavate larger, deeper craters.
Using these principles of cratering mechanics, dark-haloed craters created by meteoric impacts can be used as indicators of the depth and thickness of subsurface layers on the Moon, where the dark-haloed crater is on a brighter surface plain that overlays a darker subsurface layer. Small craters that do not have a dark halo and that have bright floors have not penetrated the bright surface layer. Larger craters that have dark halos and dark floors have penetrated through the bright surface layer and down into a darker subsurface layer. Still larger craters that have dark halos and bright floors have penetrated both the upper surface layer and through the darker subsurface layer - and down into a third lighter subsurface layer. Craters can become so large that too much light, third deep layer material is excavated. Then the largest crater no longer has a dark halo. (Figure 1 in Antonenko and Head 1995b, Figure 2 in Antonenko, Cintala and Hrz 1999) .
Because the relationship between crater diameter and depth is well known, the diameter of the crater can be used to infer its depth. In this manner, the depth and extent of surface and subsurface layers can be mapped. (E.g. Antonenko and Yingst 2002).
As discussed above, DHCs informally were grouped by this author in 20 regions for ease of reference and observing:
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In the following list, click on the thumbnails to see a higher-resolution image.
Endymion DHC Group. |
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N054.6, E055.2 Rising Age: 2.8 Setting Age: 17.6 Rükl 7 |
Mare Crisium DHC Group |
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Peirce - N018.3,E053.5 Rising Age: 3.0 Setting Age: 17.8 Rükl 26, 37 |
Atlas and Hercules DHC Groups |
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Atlas - N046.3, E044.6 Rising Age: 3.7 Setting Age: 18.5 Rükl 14, 15 |
Mare Nectaris DHC Group |
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Beaumont L - S014.4, E030.0 Rising Age: 4.9 Setting Age: 19.7 Rükl 47, 58 |
Apollo 11 DHC Group |
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Maskelyene B - N002.0, E028.9 Rising Age: 5.0 Setting Age: 19.8 Rükl 47 - See also Rükl 35, 36, 46 |
Maurolycus Basin DHC Group |
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Maurolycus A - S043.5, E014.2 Rising Age: 6.2 Setting Age: 21.0 Rükl 66 |
Rimae Menelaus DHC Group |
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Menelaus A - N017.1, E013.4 Rising Age: 6.3 Setting Age: 21.0 Rükl 23, 24 |
Manilus DHC Group |
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N014.4, E007.5 Rising Age: 6.8 Setting Age: 21.5 Rükl 23, 34 |
Rimae Theaetetus DHC Group |
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Autolycus K - N031.2, E005.4 Rising Age: 6.9 Setting Age: 21.7 Rükl 12, 13 |
Triesnecker DHC Group |
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N004.2, E002.2 Rising Age: 7.2, Setting Age: 22.0 Rükl 33, 34 |
Alphonsus DHC Group |
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Alphonsus R - S014.4, W001.9 Rising Age: 7.5 Setting Age: 22.3 Rükl 44 |
Eratosthenes DHC Group |
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Eratosthenes D - N017.5, W010.9 Rising Age: 8.28 Setting Age: 23.04 Rükl 21 |
Copernicus DHC Group |
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Copernicus H - N006.9, W018.3 Rising Age: 8.9 Setting Age: 23.6 Rükl 31, 32 |
Reinhold and Hortensius DHC Groups |
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Hortensius C - N006.0, W026.7 Rising Age: 9.6 Setting Age: 24.3 Rükl 30, 31 |
Schiller-Schickard and Lacus Excellantiae DHC Groups |
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Mee C - S045.3, W028.7 Rising Age: 9.7 Setting Age: 24.5 Rükl 62, 61, 70
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Schickard C - S045.8, W055.8 Rising Age: 12.0 Setting Age: 26.7 Rükl 62 |
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West Humorum DHC Group |
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Gassendi G - S016.8, W044.6 Rising Age: 11.04 Setting Age: 25.8 Rükl 51, 52, 50
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Porcellarum DHC Group |
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Lohrmann M - S000.5, W068.9 Rising Age: 13.0 Setting Age: 27.8 Rükl 39, 28 |
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In the following list, click on the thumbnails to see a higher-resolution image.
Gauss Dark Mantle Localized Deposit |
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N036.0, E079.0 Rising Age: 0.9 Setting Age: 15.7 Rükl 16 |
Messala Dark Mantle Localized Deposit |
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N039.0, E060.0 Rising Age: 2.5 Setting Age: 17.2 Rükl 16 |
Altas and Franklin Dark Mantle Localized Deposits |
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N047.0, E045.0 Rising Age: 3.7 Setting Age: 18.5 Rükl 15 |
Bohnenberger and Nectaris Northeast Mantle Localized Deposits |
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S016.0, E040.0 Rising Age: 4.1 Setting Age: 18.9 Rükl 58 |
Aristoteles East B and East A Dark Mantle Localized Deposits |
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N050.0, E035.0 Rising Age: 4.5 Setting Age: 19.2 Rükl 6 |
Taurus-Littrow Dark Mantle Region |
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N020.0, E030.0 Rising Age: 4.9 Setting Age: 19.7 Rükl 24 |
Sulpicius Gallus Dark Mantle Region |
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N020.0, E010.0 Rising Age: 6.6 Setting Age: 21.3 Rükl 23 |
Vaporum Dark Mantle Region |
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N010.0, E007.0 Rising Age: 6.8 Setting Age: 21.6 Rükl 34 |
Palus Putredinis Dark Mantle Region |
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N025.0, E000.0 Rising Age: 7.4 Setting Age: 22.2 Rükl 22 |
Rima Bode Dark Mantle Region |
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N013.0, W003.0 Rising Age: 7.6 Setting Age: 22.4 Rükl 33 |
Southern Sinus Aestuum East and West Dark Mantle Regions |
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Sinus Aestuum East - N005.0, W007.0 Rising Age: 8.0 Setting Age: 22.7 Rükl 32 |
Mt. Carpatus Dark Mantle Region |
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N015.0, W025.0 Rising Age: 9.43 Setting Age: 24.2 Rükl 31 |
Humorum Dark Mantle Region |
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S030.0, W040.0 Rising Age: 10.7 Setting Age: 25.4 Rükl 52, 51 |
J. Herschel Dark Mantle Localized Deposit |
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N062.0, W041.0 Rising Age: 10.7 Setting Age: 25.5 Rükl 6 |
Aristarchus and Montes Harbinger Dark Mantle Regions |
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N024.0, W048.0 Rising Age: 11.3 Setting Age: 26.1 Rükl 19, 18 |
This section presents a chart and list of cryptomaria, limited to those nearside cryptomaria accessible by Earth-based amateur telescopes.
Name | Lat_dec | Long_dec | OtherSourceSizeDepth | Size_maj_source | Rükl Chart | Lunar Chart | Comments_________________________________________ | |
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Balmer Basin Cryptomare Region | -20.1 | 70.6 | Virtual Moon Atlas | 300 | 60 | See Figure 9 in Antonenko and Head 1995a for schematic of basin. Region designation from Antonenko 1999c and Giguere et al 1998. Sq. area = 17,000 km. Diameter take-off using Virtual Moon Atlas. | ||
Taruntius Cryptomare Region | 7 | 47 | Rükl 2004 | 100 | 37 | I722, LAC61 | Region designation from Antonenko 1999c and Giguere et al 1998. Sq. area = 8.700 km. Size based on rough Rükl chart take-off. | |
Hercules Cryptomare Region | 44 | 38 | Rükl 2004 | 100 | 14 | I841, LAC27 | Region designation from Antonenko 1999c. Sq. area = 6,200 km. Size based on rough Rükl chart take-off and light plain region between C. Williams C and Hercules D mapped by Grolier on Geologic Atlas Chart I841 (1974). | |
East Figoris Cryptomare Region | 65 | 35 | Virtual Moon Atlas | 350 | 6 | I725, LAC13 | Region designation from Antonenko 1999c and Giguere et al 1998. Sq. area = 37,000 km. | |
Maurolycus Basin Cryptomare Region | -41.8 | 14 | Virtual Moon Atlas | 370 | 66 | I695, LAC113 | Region designation from Antonenko 1999c. Sq. area = 16,000 km. Diameter take-off using Virtual Moon Atlas. | |
Shickard-Schiller Basin Cryptomare Region | -44.4 | -54.6 | Antonenko1999 | 700 | 62 | I823, LAC110 | See Figure 7, Chap. 1, in Antonenko and Head 1999 for map. Region designation from Antonenko 1999c and Giguere et al 1998. Sq. area = 38,000 km. | |
West Humorum Cryptomare Region | -22 | -56 | Antonenko1999 | 700 | 51 | I495, I755, LAC92, LAC93 | See Figure 10, Chap. 1, in Antonenko and Head 1999 for map. Region designation from Antonenko 1999c and Giguere et al 1998. Sq. area = 23,000 km. | |
West Procellarum Cryptomare Region | 5 | -70 | Antonenko1999 | 300 | 28 | See Figure 14, Chap. 1, in Antonenko and Head 1999 for map. Region designation from Antonenko 1999c and Giguere et al 1998. Sq. area = 3,800 km. |
Table 6 provides links to LTVT data files that plot DHC and DMR features discussed above.
Description | Download | Version date | Distribution |
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DHCs - All lists (N=194) | Link | 1/28/2007 | Figure 1, above |
DHCs - ALPO 1976 (N=83) | Link | 1/28/2007 | Figure 2, above |
DHCs - Antonenko 1999a and Giguere et al 1998 | Link | 1/28/2007 | Figure 3, above |
Dark Mantle and LDMDs (N=15) | Link | 1/28/2007 | Figure 40, above |
Right-click to download files. |
DHCs and LDMDs are a unique class of difficult to image lunar features. They represent a good observing and imaging challenge for the intermediate to advanced lunar amateur. All nearside telescopically observable DHCs probably have not been discovered despite the detailed NASA review during the Apollo era of Lunar Orbiter IV images. DHCs graphically shown on Fig. 6 in Schultz and Spudis 1979 are in need of recovery.
An opportunity exists to expand the observing list presented here based on Fig. 2 in Salisbury, Alder and Smalley 1968. Examining a clear original copy of an original issue of MNRAS containing the article, it is apparent that there at least 30 DHCs identified on Salisbury et al's whole Moon map that are not in the ALPO observing list. An amateur spending one or two weekends with a good reproduction of Salisbury's Figure 2, U.S.G.S. Map-A-Planet, a copy of Rükls, and Virtual Moon Atlas could probably recover these features' positions.
This note is amateur astronomer work product. Corrections to any errors are welcomed and appreciated.
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Antonenko, I. 1999b. Stratigraphy of the Schickard Crater Area, from Clementine Multispectral Data. Chap. 3 in Antonenko 1999a. Thesis.
Antonenko, I. 1999c. Implications for Lunar Volcanism from Studies of Cryptomafic Deposits. Chap. 4 in Antonenko 1999a. Thesis.
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Antonenko, I. and Head, J.W. 1999. Cryptomafic Deposits on the Western Limb of the Moon: Areal Distribution and Volumetric Significance of Early Imbrian Volcanism as Determined from Dark-Haloed Impact Craters. Chap. 1 in Antonenko 1999a. Thesis.
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Dembowski, W.M., Assoc. of Lunar and Planetary Observers. 2006. 1976 ALPO Catalogue of Dark Haloed-Craters. Originally published J. ALPO 26(3-4):77-79 (1976).
Giguere, T. A., Hawke, B. R., Taylor, G. J. and Lucey, P. G. 1998. Infra.
Head, J. W. and Wilson, L. 1979. Alphonsus-Type Dark-Halo Craters: Morphology, Morphometry, and Eruption Conditions. X Lunar and Planetary Science, Abstract, pp. 525-527. 1979LPI....10..525H
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Evidence for ancient mare volcanism
. X Lunar and Planetary Science Conference, Houston, Tex., March 19-23, 1979, pp. 2899-2918. 1979LPSC...10.2899S. (Key Apollo era map of DHCs)
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Antonenko, I. and Yingst, R. A. 2002. Mare and Cryptomare Deposits in the Schickard Region of the Moon: New Measurements Using Clementine FeO Data. XXXIII Annual Lunar and Planetary Science Conference, March 11-15, 2002, Houston, Texas, Abstract No.1438. 2002LPI....33.1438A
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Hawke, B. R., Gillis, J. J., Giguere, T. A., Blewett, D. T., Lawrence, D. J., Lucey, P. G., Smith, G. A., Spudis, P. D. and Taylor, G. J. 2004. XXXV Lunar and Planetary Science Conference, March 15-19, 2004, League City, Texas, Abstract No.1190 2004LPI....35.1190H
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Giguere, T. A., Hawke, B. Ray, Gaddis, L. R., Blewett, D. T., Gillis-Davis, J. J., Lucey, P. G., Smith, G. A., Spudis, P. D., and Taylor, G. J. 2006. Remote sensing studies of the Dionysius region of the Moon. J. Geophys. Res. 111:E06009. 2006JGRE..11106009G.
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Prepared by K. Fisher fisherka@csolutions.net Org. 1/31/2007