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Home Antarctic MeteoritesAntarctic Meteorite NewslettersAMN 41,1 Program News
Volume 41 No. 1 – February 2018

Program News

Curator Comments

Kevin Righter, NASA-JSC

This newsletter reports 234 new meteorites from the 2014, 2015, and 2016 ANSMET seasons from the Dominion Range (DOM 14), Miller Range (MIL 15), and Elephant Moraine (EET 16) areas. Meteorites include a IIIAB iron, an L chondrite impact melt, a lodranite (?), and 6 unequilibrated ordinary chondrites. We also reclassified a number of meteorites (see below) and remind requestors that some of our samples are small and rare and require stronger than usual justification when submitting a request (also see below).

Requesting small and special samples

The US Antarctic meteorite collection has many rare samples that are preserved for scientific study. Many of these samples have been in the collection since the first years of the program, and have less material available for study. Others are simply small, and there is limited material available. Finally, some have been disaggregated during sample preparation and handling due to their degree of weathering, fracturing, and overall physical state. These samples will be preserved as best as possible, which also means that not all requests can be honored. For severe cases, sample requests may be rejected to save material for future studies of the most compelling nature. For example, requests for multiple members of a meteorite group as part of a cursory survey are unlikely to be honored for samples of this small and rare nature. This message is simply a reminder that requestors should do the necessary background research on such samples to ensure that their request has as much specific justification as possible. Resources for obtaining information about our samples include the Antarctic Meteorite Newsletters, our online database, and the online bibliography which lists over 1600 peer reviewed publications through 2017:

In addition, detailed information is available in our sample compendia:

Reminder to Sign and Return Your Annual Inventory

US Antarctic meteorite inventories were mailed to all PIs in November 2017. You received a list of samples with a header at the top for two signatures — one for you (the PI) and one for an institutional official. Thanks to all of those who have returned their inventories to us, but if you haven't already, please follow these instructions:

  • Print the list
  • Compare your sample list to samples in your possession
  • Confirm samples are in your possession unless consumed during research (if approval was obtained during original sample request), and note any discrepancies
  • Sign/date top of first inventory page
  • Institutional official must sign/date top of first page
  • Scan and email it back to us (JSC-ARES-MeteoriteRequest@nasa.gov)

PIs that do not respond to inventory queries by the NASA Curator will not receive samples from the collection.

Reminder to acknowledge samples received from NASA-JSC

When publishing results of your research, please include the split numbers used in the research. We also request that scientists use the following acknowledgement statement when reporting the results of their research in peer reviewed journals: "US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Astromaterials Curation Office at NASA Johnson Space Center and the Department of Mineral Sciences of the Smithsonian Institution." Such an acknowledgement will broaden the awareness of the funding mechanisms that make this program and these samples possible.

We suggest you find out how to acknowledge samples received from all the collections/museums from which you have received materials so that all the institutions making samples available to you receive proper credit and acknowledgement.

Reclassifications

1) Reclassification of PCA 82500 currently a CK5, but should be a CK3. The observations supporting the low petrologic grade include (1) lack of ilmenite exsolution from magnetite, a property typically seen in type 3 CKs and (2) olivine zoning observed in BSE within the largest chondrule in the type section. Taken together, these suggest classification as a type 3.

2) Reclassification of various unusual carbonaceous chondrites

The compositional, mineralogical, and petrological characteristics of a number of carbonaceous chondrites in our collection has been recognized by our PIs. To draw a distinction between these samples and the more standard members of their groups, we have reclassified the following samples due to observations made by Davidson et al. (2015) and Floss and Brearley (2014) for MIL 07687, and by Choe et al. (2010) for all the rest:

DOM 03238 : CO3 chondrite (anomalous) (Choe et al., 2010)
EET 90043 : CO3 chondrite (anomalous) (Choe et al., 2010)

MIL 07687 : C2 chondrite ungrouped (Davidson et al., 2015; Floss and Brearley, 2014)
GRA 98025 : C2 chondrite ungrouped (Choe et al., 2010)

GRO 95566 : CM chondrite (anomalous) (Choe et al., 2010)
LEW 85311 : CM chondrite (anomalous) (Choe et al., 2010) (paired with LEW 85306, 85307, 85309, and 85312)
PCA 91008 : CM chondrite (anomalous) (Choe et al., 2010)
QUE 99038 : CM chondrite (anomalous) (Choe et al., 2010)
WIS 91600 : CM chondrite (anomalous) (Choe et al., 2010) (paired with WIS 91608)

Choe, W. H., Huber, H., Rubin, A. E., Kallemeyn, G. W., & Wasson, J. T. (2010) . “Compositions and taxonomy of 15 unusual carbonaceous chondrites. ” Meteoritics & Planetary Science 45, 531-554.

Davidson, J., Nittler, L. R., Stroud, R. M., Takigawa, A., De Gregorio, B. T., Alexander, C. M., ... & Cody, G. D. (2015) . “Organic matter in the unique carbonaceous chondrite Miller Range 07687: a coordinated in situ NanoSIMS, FIB-TEM, and XANES study. ” 46th Lunar and Planetary Science Conference, Abstract # 1609.

Floss, C., & Brearley, A. J. (2014) . “Presolar grain abundance variations in the unique carbonaceous chondrite MIL 07687. ” 77th Annual Meeting of the Meteoritical Society, Abstract # 5183.

3) Reclassification of equilibrated ordinary chondrites

A) MAC 88122

This sample was originally announced as an LL5 chondrite in newsletter 13, number 2 (March 1990), and then reclassified as an L/LL5 chondrite in newsletter 30, number 2 (August 2007). The 2007 reclassification was a mistake – we find no evidence for the L/LL classification, and thus re-classify this sample back to its original LL5 classification based on the olivine content (Heggy et al., 2012, Icarus 221, 925-939) and the Ni and Co content of the metal (Table of reclassifications from AMN 30, no. 2, data provided by Welten and Nishiizumi in 2007).

B) GRO 85 and 03 samples

The ANSMET 2003-2004 field team recovered meteorites from the Grosvenor Mountains region of the TransAntarctic Mountains. Within this area was a small collection of ~80 meteorites that appeared to be pieces of the same fall, based on their weathering state, hand specimen appearance, and the fact that they were found in a narrow ellipse with a long axis of 1.7 km, with the largest fragments at one end (Kress et al., 2007).

Subsequent classification of these samples included a wide range of chondrites including LL, L and H, but detailed chemical analyses of 6 larger specimens from the field yielded metal content and composition consistent with H chondrite samples (Welten et al., 2009) . Because of the discrepancy between the original classification and the subsequent studies, and the fact that this small strewnfield may be of special interest to meteoriticists, we have measured the magnetic susceptibility of all samples from this proposed strewnfield. The results indicate that most are indeed H chondrites, and we present the full dataset here, and propose re-classification of those that were classified previously as L or LL, as indicated in the table. Values > 4.8 are consistent with H chondrites, and those < 4.5 are consistent with LL chondrites. After reclassification, only two remain that are consistent with L chondrites (GRO 03005 and GRO 03036), and there are no LL chondrites.

Welten, K. C.; Nishiizumi, K.; Caffee, M. W.; Leclerc, M. D.; Jull, A. J. T. (2009). “Cosmogenic Radionuclides in Chondrite Shower from Otway Massif. ” 40th Lunar and Planetary Science Conference, (Lunar and Planetary Science XL), held March 23-27, 2009 in The Woodlands, Texas, Abstract # 1488.

Kress, M. E.; Benedix, G. K.; Schutt, J.; Harvey, R. P. (2007) . “An Unusual Strewn Field at the Otway Massif, Grosvenor Mountains, Antarctica. ” 70th Annual Meteoritical Society Meeting, held in August 13-17, 2007, Tucson, Arizona. Meteoritics and Planetary Science Supplement, Vol. 42, Abstract # 5270.

Grosvenor Mountains 85 and 03 Sample Reclassifications

SampleM0 (10-3 )Mass (g)Log χ (10-9 m3/kg)AMN Classification New Classification
GRO 85203 226 999.67 5.07 H5 -
GRO 03001 240 29895 5 L5 H5
GRO 03002 154 27995.21 4.8 L5 H5
GRO 03003 219 10625 4.96 L5 H5
GRO 03004 148.5 2406.1 4.81 L5 H5
GRO 03005 86.55 2489.3 4.57 L5 -
GRO 03006 179 1099 4.96 L5 H5
GRO 03008 157.5 1674.1 4.87 L5 H5
GRO 03009 187.5 1095.7 4.98 L5 H5
GRO 03010 163 1292.9 4.91 L5 H5
GRO 03011 249 1253.9 5.09 L5 H5
GRO 03012 205.5 1138.4 5.02 L5 H5
GRO 03013 145 1030 4.87 L5 H5
GRO 03014 185.5 1105 4.98 L5 H5
GRO 03016 186 905.5 4.99 L5 H5
GRO 03017 116.5 194.9 4.93 LL5 H5
GRO 03018 198 1414.6 4.98 L5 H5
GRO 03019 222 1240 5.04 L5 H5
GRO 03020 206.5 550 5.08 L5 H5
GRO 03021 215 603.5 5.09 L5 H5
GRO 03022 171 613.2 4.99 H5 -
GRO 03023 201 878.3 5.03 L5 H5
GRO 03024 166.5 639.5 4.98 L5 H5
GRO 03025 158 592.195 4.96 L5 H5
GRO 03026 123.5 557.7 4.86 L5 H5
GRO 03027 111.5 76.9 5.07 L5 H5
GRO 03028 225 439.4 5.14 L5 H5
GRO 03029 217 513.7 5.11 L5 H5
GRO 03030 182 872.4 4.99 L5 H5
GRO 03031 324 766.5 5.25 L5 H5
GRO 03033 189 330 5.09 L5 H5
GRO 03035 172 354.9 5.04 L5 H5
GRO 03036 74.35 334 4.69 L5 -
GRO 03037 150.5 527.2 4.95 L5 H5
GRO 03038 152.5 387.5 4.98 L5 H5
GRO 03039 159.5 382.9 5 L5 H5
GRO 03041 82.4 111.601 4.85 L5 H5
GRO 03042 202 285.7 5.13 L5 H5
GRO 03043 116.95 271.4 4.9 L5 H5
GRO 03044 128 181.64 4.92 L5 H5
GRO 03045 147.5 213.613 5.03 L5 H5
GRO 03047 167 278.3 5.05 L5 H5
GRO 03048 172 391.2 5.03 L5 H5
GRO 03049 132.5 307.9 4.94 L5 H5
GRO 03050 207.5 234.4 5.17 L5 H5
GRO 03051 161 157.25 5.06 H5 -
GRO 03054 79.3 58.9 4.98 LL5 H5
GRO 03056 159 419.6 4.99 H5 -
GRO 03057 163.5 657.6 4.97 L5 H5
GRO 03058 197.5 417.4 5.09 L5 H5
GRO 03059 182 614.1 5.02 L5 H5
GRO 03060 234 343.2 5.18 L5 H5
GRO 03062 172.5 431.708 5.03 L5 H5
GRO 03065 159.5 301.3 5.03 L5 H5
GRO 03068 163 284.2 5.04 L5 H5
GRO 03069 165.5 217.3 5.07 L5 H5
GRO 03071 135.5 253.9 4.97 L5 H5
GRO 03072 133 153.99 4.98 L5 H5
GRO 03073 96.1 144.514 4.85 L5 H5
GRO 03074 130.5 243.3 4.96 LL5 H5
GRO 03077 135 197.6 5 L5 H5
GRO 03080 124 133.73 4.98 L5 H5
GRO 03081 109.25 209.978 4.9 L5 H5
GRO 03082 124.5 169.549 4.93 L5 H5
GRO 03083 95.3 129.699 4.87 LL5 H5
GRO 03089 158 143.2 5.07 H5 -
GRO 03090 131 122.3 5.03 L5 H5
GRO 03091 103 237.2 4.86 L5 H5
GRO 03092 30.6 11.8 5.08 L5 H5
GRO 03093 77.2 67.45 4.94 L5 H5
GRO 03094 83.2 68.8 4.97 LL5 H5
GRO 03095 86.75 93.297 4.91 H6 -
GRO 03096 110 119.7 4.96 L5 H5
GRO 03097 134.5 93.6 5.1 L5 H5
GRO 03098 66.85 39.6 5 L5 H5
GRO 03099 163 202 5.08 H5 -
GRO 03100 96.15 52.3 5.1 L5 H5
GRO 03101 119.5 70.4 5.12 L5 H5
GRO 03102 107 101.8 4.98 L5 H5
GRO 03103 133 156.3 4.97 H5 -
GRO 03104 77.9 91.638 4.87 H5 -
GRO 03106 114.5 105.7 5 L5 H5
GRO 03109 44.1 23.3 4.98 L5 H5
GRO 03117 100.8 57.4 5.09 L5 H5
GRO 03118 51.25 42.8 4.87 L5 H5
GRO 03119 50.6 33.4 4.92 L5 H5
GRO 03120 154.5 100.354 5.15 H5 -
GRO 03121 89.05 80.839 4.96 H5 -
GRO 03122 67.65 46.766 4.97 L5 H5
GRO 03123 108 57 5.13 L5 H5
GRO 03162 17.8 7.2 5.03 L5 H5
GRO 03165 36.95 17.6 5.01 L5 H5

C) DOM 85 and 03 samples

The Dominion Range has been visited by ANSMET teams during the 1985-86, 2003-04, 2008-09, 2010-11, 2014-15 seasons. A large ordinary chondrite shower dominates the collection in this area. Initial characterization of the samples was yielding ~60% LL chondrites. Several years ago we began to suspect this classification because we weren't seeing any LL chondrite in random thin section sampling, and targeted microprobe analysis of 15 LL chondrites from the DOM 08 and DOM 10 season revealed they are actually L chondrites. We decided a systematic reclassification of this field is necessary to have accurate statistics. In the continued efforts to reclassify, we report magnetic susceptibility data for 142 samples from the 2003-04 and 1985-86 seasons. As suspected, the majority of these samples are L chondrites, with very few LL chondrites. The samples requiring reclassification are indicated in the table as well. Values > 4.8 are consistent with H chondrites, and those < 4.5 are consistent with LL chondrites.

Dominion Range 85 and 03 Sample Reclassifications

SampleM0 (10-3 )Mass (g)Log χ (10-9 m3/kg)AMN Classification New Classification
DOM 03180 166.5 148.4 5.08 H5 -
DOM 03184 0.502 0.7 4.37 LL5 -
DOM 03185 111 745.1 4.79 LL5 L5
DOM 03186 280 1374.5 5.14 L5 H5
DOM 03187 107.6 800.9 4.77 LL5 L5
DOM 03188 177 586.3 5.01 L5 H5
DOM 03189 121.5 991.6 4.8 L5 -
DOM 03190 113 455 4.84 L5 -
DOM 03191 224 550.8 5.12 H5 -
DOM 03192 377.5 217.8 5.43 L5 H5
DOM 03193 128 275.7 4.94 H5 -
DOM 03195 42.35 154.232 4.48 LL6 -
DOM 03196 72.8 89.5 4.85 LL6 L6
DOM 03197 42.95 131.8 4.52 LL5 L5
DOM 03198 68.75 250.5 4.68 LL5 L5
DOM 03199 50.1 99.3 4.66 H5 L5
DOM 03200 64.15 134.154 4.69 L5 -
DOM 03202 105.5 89.6 5.01 L5 H5
DOM 03203 40.35 65.6 4.66 L5 -
DOM 03204 84.95 63.6 4.99 L5 H5
DOM 03205 80.25 38 5.09 H5 -
DOM 03207 60.6 39.1 4.96 H5 -
DOM 03208 140.5 84.9 5.14 LL5 H5
DOM 03209 86 48.3 5.07 H5 -
DOM 03210 61.35 30.8 5.02 L5 H5
DOM 03211 36.65 52.7 4.67 L5 -
DOM 03212 50.9 18.5 5.13 L5 H5
DOM 03213 13.65 26.1 4.43 LL5 -
DOM 03214 45.4 29.887 4.9 H5 -
DOM 03215 10 3.2 5.09 H5 -
DOM 03216 26.5 6.1 5.27 H5 -
DOM 03217 2.585 14 3.94 LL5 -
DOM 03218 43 17.1 5.09 H5 -
DOM 03220 109 29.5 5.28 H6 -
DOM 03221 67.8 32.7 5.06 H5 -
DOM 03222 39.25 13.5 5.14 H6 -
DOM 03223 1 2.2 4.23 LL4 -
DOM 03224 10.03 2.4 5.2 L5 H5
DOM 03225 13.95 4 5.15 L5 H5
DOM 03226 10.1 2.8 5.15 L5 H5
DOM 03227 0.349 1.7 3.88 LL5 -
DOM 03228 0.65 2.1 4.07 LL5 -
DOM 03229 6.755 1.8 5.14 L5 H5
DOM 03230 0.1895 1.7 3.61 LL5 -
DOM 03231 0.798 2 4.17 LL6 -
DOM 03232 9.37 2.4 5.17 L4 H4
DOM 03233 3.655 3.2 4.65 L5 -
DOM 03234 10.7 9.5 4.71 L5 -
DOM 03235 46.35 18.2 5.1 H4 -
DOM 03236 17 5.5 5.12 H5 -
DOM 03237 110.85 69.8 5.09 H6 -
DOM 03239 29.35 57.204 4.56 L6 -
DOM 03240 98.6 277.7 4.83 LL5 L5
DOM 03241 23.55 67.5 4.42 LL6 -
DOM 03242 88.5 55.232 5.05 H5 -
DOM 03243 35.6 41.7 4.72 H5 L5
DOM 03244 130.5 82.3 5.12 LL5 H5
DOM 03245 71.35 216.6 4.71 LL5 L5
DOM 03246 66.4 39.7 5 L5 H5
DOM 03247 115.5 87.3 5.05 H5 -
DOM 03248 137.5 47 5.28 LL5 H5
DOM 03249 6.605 14.92 4.32 LL5 -
DOM 03250 60 465.1 4.56 LL5 L5
DOM 03251 438 631.2 5.4 LL5 H5
DOM 03252 98.55 351.2 4.8 H6 L6
DOM 03253 477 1130.4 5.38 H5 -
DOM 03254 112 484.7 4.83 LL5 L5
DOM 03255 192.5 341.4 5.1 L5 H5
DOM 03256 234 213.9 5.23 L5 H5
DOM 03257 94.4 277.2 4.81 LL5 L5
DOM 03258 385 342.4 5.4 LL5 H5
DOM 03259 37.8 179 4.4 LL6 -
DOM 03260 185 183.6 5.08 LL5 H5
DOM 03261 115 173 4.89 LL5 L5
DOM 03262 38.5 92.3 4.56 LL5 L5
DOM 03263 33.85 69.5 4.57 LL6 L6
DOM 03264 38.2 36.2 4.78 L5 -
DOM 03265 29.25 58.828 4.55 LL5 L5
DOM 03266 90.15 40.9 5.13 L5 H5
DOM 03267 37.5 43.3 4.73 LL5 L5
DOM 03268 21.9 24.7 4.65 LL5 L5
DOM 03269 31.35 39 4.68 LL5 L5
DOM 03270 15.75 19 4.61 LL5 L5
DOM 03271 61.75 19.6 5.19 LL5 H5
DOM 03272 42.4 72.843 4.66 LL5 L5
DOM 03273 27.65 22.6 4.79 LL5 L5
DOM 03274 20.85 26.086 4.61 LL5 L5
DOM 03275 11.75 10.5 4.71 LL5 L5
DOM 03276 5.69 13.396 4.3 LL5 -
DOM 03277 8.825 7.7 4.7 LL5 L5
DOM 03278 21.3 23.2 4.67 LL5 L5
DOM 03279 23.9 20.6 4.76 LL5 L5
DOM 03280 38.55 31.3 4.82 LL6 L5
DOM 03281 3.215 3 4.62 LL6 L6
DOM 03282 4.52 4.4 4.63 LL5 L5
DOM 03283 6.575 6.3 4.65 L6 -
DOM 03284 4.72 4.1 4.67 L5 -
DOM 03285 22.1 11 4.97 L6 H6
DOM 03286 7.02 3.4 4.91 H5 -
DOM 03288 25.7 16.8 4.87 L6 -
DOM 03289 87.85 59.9 5.02 H5 -
DOM 03290 7.915 12.259 4.48 L5 -
DOM 03291 51.7 40.61 4.89 L5 -
DOM 03292 43.6 20.6 5.02 H5 -
DOM 03293 15.4 16.3 4.66 LL5 L5
DOM 03294 27.5 18.7 4.86 L5 -
DOM 03295 8.78 7.6 4.71 L5 -
DOM 03296 55.7 22.9 5.09 L5 H5
DOM 03297 7.235 5.2 4.77 LL6 L6
DOM 03298 6.895 4.8 4.78 L6 -
DOM 03299 34.55 13.1 5.09 L5 H5
DOM 03300 4.705 3.6 4.72 L5 -
DOM 03301 4.575 3.9 4.68 L5 -
DOM 03302 1.995 2 4.57 L5 -
DOM 03303 5.705 4.1 4.75 LL5 L5
DOM 03304 9.275 6.6 4.78 L5 -
DOM 03305 6.99 11.043 4.46 LL5 -
DOM 03306 9.31 2.9 5.1 H4 -
DOM 03307 4.72 3.7 4.71 L5 -
DOM 03308 39.9 20.7 4.98 LL5 H5
DOM 03309 52.9 22.7 5.07 H5 -
DOM 03310 5.48 3.6 4.79 LL5 L5
DOM 03311 12.45 12.5 4.67 LL5 L5
DOM 03312 12.45 4.5 5.06 H5 -
DOM 03313 11.05 5.1 4.96 H5 -
DOM 03314 8.95 2.6 5.12 L5 H5
DOM 03315 7.26 5.5 4.75 LL5 L5
DOM 03317 8.435 4.2 4.91 L5 -
DOM 03318 176.5 2932.5 4.87 H5 L5
DOM 03319 573.5 3397.7 5.38 L5 H5
DOM 03320 92.5 2174.1 4.62 L5 -

DOM 85500 112 53.795 5.16 H5 -
DOM 85501 67.6 29.9 5.07 H5 -
DOM 85502 39.75 229.45 4.45 L6 -
DOM 85503 50.6 579.4 4.47 L6 -
DOM 85504 36.2 90.61 4.54 L4 -
DOM 85505 0.74 1.6 4.23 LL5 -
DOM 85506 0.6805 1.5 4.21 LL5 -
DOM 85507 90.55 79.7 4.97 H5 -
DOM 85508 13.2 2.6 5.29 H6 -
DOM 85509 12.1 14.4 4.6 L6 -
DOM 85510 48.05 13.3 5.23 L6 H6


Rob Wardell
Dominion Range 85 and 03 Samples
Rob Wardell
Dominion Range 14 Samples


ANSMET 2017-2018 Field Season

Jim Karner, Ralph Harvey and John Schutt
Case Western Reserve University

The 2017-18 season included both reconnaissance and systematic work. The season started on Dec. 12, 2017 as a group of eight (see pic) plus gear flew to Shackleton Glacier Camp (SHG), which was situated in the southern Transantarctic Mountains. Once at SHG the group split into two teams of four (i.e., Team A and B) and proceeded to be shuttled to their respective work sites by Twin Otter. Team A, consisting of Jim Karner, Brian Rougeux, Barbara Cohen and Julianne Gross conducted systematic searches of the Mt. Cecily/Mt. Raymond (MC/MR) icefields in the Grosvenor Mountains. The area had been visited in 1995-96, but plenty of unsearched ice remained. The MC/MR area was visually stunning with its huge rolling seas of blue ice at the bases of the mountains and nunataks, but it was really, really cold. And windy. Most days the temps were below zero (F) or just slightly above that- and the winds constantly blew at 15 knots or greater. Team A spent a total of 34 days at MC/MR, and despite the tough conditions recovered a total of 211 meteorites. The bulk of the meteorites were found by snowmobile sweeps of the large icefields, but several dozen were also found by meticulous foot-searching of the many and heavy moraines in the area.

2017-18 ANSMET Team

2017-18 ANSMET team: (l-r) Scott Van Bommel, Jim Karner, James Day, Juli Gross, Barbara Cohen, Brian Rougeux, John Schutt, Ioannis Baziotis

The reconnaissance team (Team B) consisted of John Schutt, James Day, Scott Van Bommel, and Ioannis Baziotis. The team worked in the Amundsen Glacier region and evaluated six bare ice areas for potential meteorite concentrations. Their first stop was the Mt. Wisting and Mt. Prestrud area, which was first visited in 1995-96. The team spent just a few days in the area and recovered about ten meteorites through both snowmobile sweeps and moraine searching. The next move took the team to Nodvedt Nunataks, where they recovered forty meteorites; their final move took them to the Amundsen Glacier icefield where one possible meteorite was collected. Team B also spent a day performing helicopter reconnaissance of two relatively small bare ice patches in the region. The helos transported the team to both the Upper Amundsen Glacier and Devils Glacier icefields where quick foot-searches of the ice were performed. Two meteorites were recovered from the Devils Glacier ice while no rocks (of any kind) were even seen on the ice at Upper Amundsen! In summary, the reconnaissance team evaluated six bare ice areas for meteorite concentrations. Two of the sites had been previously visited (Mt. Wisting and Mt. Prestrud), but the others were first visits. A total of 52 specimens were recovered, but no significant meteorite concentrations were realized.

Report from the Smithsonian

Cari Corrigan, Geologist (Dept. of Mineral Sci.)

Rob Wardell

New laboratory staff member Rob Wardell

Things continue to evolve and adapt as necessary in the Division of Meteorites at the Smithsonian. Our new microprobe (a JEOL JXA 8530f+ Hyperprobe) is still running beautifully, and it is a good thing! Our SEM EDS detector hit a major snag, rendering it useless since the holidays. It is now the instrument we use to classify the Antarctic equilibrated ordinary chondrites, so that left us with a bit of a problem. Never fear, the Hyperprobe is here! We were able to use its state of the art capabilities to perform the EDS analyses generally the same way as we do on the SEM. Therefore, we bring you the entire newsletter with data obtained using the new instrument. Tada! It was a lot of fun figuring out how to make it happen (despite the struggles due to our learning curve)! In personnel news, we have hired another member to our laboratory staff. We would like to welcome Rob Wardell to the crew! Rob comes to us with an engineering degree and a lot of great lab experience. We welcome the addition of another capable body to our lab staff!