antarctic meteorite newsletter
Newsletter 31,1
Program News

Curator's Comments
Kevin Righter, NASA-JSC

New Meteorites and Meteorite Enclosed in Ice

This newsletter reports 418 new meteorites from the 2004 and 2006 ANSMET seasons from the Cumulus Hills (CMS), LaPaz Ice Field (LAP), Graves Nunataks (GRA), Grosvenor Mountains (GRO), Larkman Nunatak (LAR), MacAlpine Hills (MAC), Miller Range (MIL), Roberts Massif (RBT), and Scott Glacier (SCO).  These new samples include one iron, 1 eucrite, 1 mesosiderite, 6 CK chondrites (2 with pairing), 2 CV3 chondrites, 1 CM1, 7 CM2 (4 with pairing), 3 CR2 (2 with pairing), and one each of a type 3 L and H chondrites.  The CK6 chondrites (LAR 06869, 06872, 06873) are unusual in that they have no discernable chondrules, extremely fine-grained texture, and are full of veins.  This newsletter represents a break from recent newsletters in which we have announced many unusual and popular samples, including new lunar and martian meteorites, an unusual achondrite (GRA 06128 and 06129 – the topic of a special session at this years LPSC). 

Last fall we received the third highest number of requests for samples since the start of the program in 1977 (73), yet we also continue to announce >300 new meteorites in newsletters.  This combined level of activity from the field teams, Smithsonian and NASA-JSC has resulted in the allocation of >600 samples to 87 PI's, including thin sections, since last year at this time.  With such a high load of samples, there can be temporary delays, and we appreciate everyone's patience during these busy periods.    

This newsletter also marks the completion of characterization and announcement of the 2004 season samples.  To see a summary of the seasons finds, you can search "2004" in our Classification database online.


Meteorite Fully Enclosed in Ice:  A Call for Proposals

During the recently completed 2007-2008 ANSMET field season the field team recovered a specimen (presumably a meteorite) fully enclosed within blue ice.  Although specimens partially enclosed in ice have been recovered and studied before, the 2007 specimen is unique in two important ways.  First,   it is fully enclosed by ice and thus potentially sealed off from any anthropogenic contamination; second, it is larger than any previously discovered "in-ice" specimen (4-5 cm in longest dimension), making it easier to work with. The block of ice (roughly 30x45x60 cm) containing the new specimen is currently en route to the Meteorite Processing Laboratory at JSC, sealed in a double set of nylon bags and kept frozen since recovery.  It should arrive at JSC in early April.  

Presumed meteorite enclosed in ice
Presumed meteorite enclosed in ice

The Meteorite Working Group would like to receive proposals from researchers interested in joining a consortium that will extract this specimen from the ice and conduct in situ sampling of the ice or the meteorite specimen at the moment of extraction. The following ground rules apply:

If you would like to be involved in the extraction of this meteorite, please prepare a short (1 page) proposal describing exactly what you’d like to do (sample or direct measurement needs, samples sizes, etc) and your willingness to participate. Proposals should be sent to Ralph Harvey via email (rph@case.edu) no later than March 21, 2008. The Meteorite Working Group will review these proposals in late March and the consortium will be formed shortly thereafter. We anticipate extracting the meteorite in mid- to late-summer.


Antarctic Meteorite Workshop - July 26-27, 2008 at Matsue Meteoritical Society

At the upcoming Meteoritical Society meeting in Matsue, Japan (July 28 - August 1, 2008), there will be a pre-meeting Antarctic Meteorite Workshop hosted by the NIPR and MetSoc. The purpose of the workshop is to gather meteoriticists to discuss issues relating to these collections, and how to allow these new discoveries to have the largest impact on our field. The workshop format will allow discussion of topics not usually covered during the regular sessions of the Meteoritical Society meeting. Specifically, the topics of interest will include the search, recovery, classification, weathering and curation of Antarctic Meteorites. Information about the workshop will be distributed soon.


Changes and Additions to the US Antarctic Meteorite Webpage

Some substantial changes and additions have been made to our webpage recently, including an updated sample request form, addition of an updated master list and spreadsheet for all samples in the US Antarctic meteorite collection (cross-checked against the Meteoritical Bulletin announcements), and a summary of bandsawing at NASA-JSC and the Smithsonian Institution. Also, augmentation of photographic information available about the US Antarctic meteorite collection continues on our webpage. You will notice many new photos of achondrites announced in pre-1996 newsletters. These photos will be added for all classes of meteorites over the next few months, so please watch for updates. There are some beautiful photos taken of samples from the period 1977 to 1995 that have only been available in hard copy through JSC. Now many of these will be available electronically on our webpage in the "Classification Database" section.


Availability of Possible Impact Crater Feature in LAP 02200

NASA-JSC scientist, Mark Cintala received four ~400 g bandsawed pieces of the large LL6 chondrite LAP 02200 in May 2007 for shock experiments in his lab at JSC. After sandblasting the fusion crust off of the samples, which is customary for these shock experiments, Cintala observed what looks like a pre-existing impact crater and spallation zone in this chondrite sample. In order to preserve this feature for study by other researchers, he has traded two pieces with these features for two different pieces of LAP 02200. Below are several photos of this sample, before and after sandblasting, and then after one shock experiment, showing the artificial crater as well as the potential natural crater. If you are interested in studying these samples, please contact us through the normal request channel, but it may be beneficial to speak with the curator in advance of such a request to discuss sample dimensions, sampling needs, etc.

 
Split ,18 before sandblasting 
 
Post gun experiment of split
Split ,18 before sandblasting 
(white pad is ~ 10 cm in length
 
Post gun experiment of split showing artificial crater (obliquely) on top surface and possible natural crater on lower front surface.
   
Split ,18 after sandblasting and crater feature is already visible at lower right hand side of sample
   

(All photos courtesy of Mark Cintala, JSC/NASA)

 

Staff Changes at the Smithsonian

This newsletter announces the end of the classification of the 04’s and continues working through the 06’s. It also marks a significant transition at the Smithsonian. The staff of the Div. of Meteorites is growing and changing. LuElla Speakman has joined our staff as a Collections Technician and will assume responsibility for samples that are permanently transferred to the Smithsonian. Also joining our staff as a trust-funded Geologist is Cari Corrigan, who has twice traveled to Antarctica to collect meteorites and previously worked as a postdoctoral fellow with us. She joins us in what we anticipate to be an ongoing position funded in part by an endowment generously provided by former curator Ed Henderson. Cari will assume the day-to-day responsibilities in the classification of Antarctic meteorites and will serve as the Smithsonian’s representative to the Meteorite Working Group. Linda Welzenbach continues as Collection Manager and serves as the Fall Secretary for the Meteorite Working Group. Finally, I am moving from the MWG, where I have served for a decade, to the Meteorite Steering Group, replacing Glenn MacPherson who served on the Steering Group. We are extremely pleased to welcome LuElla and Cari and will continue to make sure the high level of service you have come to expect from the Smithsonian continues.

Results From the 2007-2008 ANSMET Field Season
Ralph Harvey, ANSMET

Sometimes it starts with just one little find. Back in 1985 the US Antarctic Research Program established a remote helicopter camp on the Bowden Névé (Beardmore South Camp), an effort designed to promote field explorations in the mid-Transantarctic Mountains. It worked, at least for us; with a bit of helicopter support and some snowmobile traversing, during that season my predecessor (Bill Cassidy) and his team discovered the meteorite concentrations near Lewis Cliff, the Queen Alexandra Range, the Grosvenor Mountains, the Geologists Range, and the Miller Range.  More than 8000 LEW, QUE, GRO, GEO and MIL meteorites have been recovered over the past 22 years as a result, and there are more to come.

During that prodigal season, Bill and company found only a single meteorite on ice near the Miller Range; that find took a back seat to the dense concentrations found at Lewis Cliff and nearby areas.  But that lone H5 wasn’t forgotten.  In 1999 we sent a two person team back to the Miller Range, where 30 meteorites found in a day and vast extents of blue ice revealed enormous potential.  A four-person team found another 100 or so meteorites in 2003, and in 2005 a full 8-person, 6-week and weather-confounded expedition found about 170 more.  The Miller Range icefields yielded many meteorites of unique interest as a result of these efforts, including lunar and martian specimens; so while the numbers weren't huge, the potential of the Miller Range icefields continued to grow.  

The just-completed 2007-2008 field season was the first to really exploit that potential.  Good weather and lighter snow cover allowed more than 700 meteorites to be recovered, including a good number of non-OC specimens.   Our efforts were concentrated on the informally-named Middle Icefields, sitting (rather obviously) between the North icefields partially searched in 2005, and the as-yet unsearched South icefields.  Searching conditions were interesting, to say the least.  Around the north and east ends of the Middle Icefield are myriad separate patches of exposed ice and hard firn, with both meteorites and terrestrial rocks unevenly scattered on their surfaces. We set ourselves to search all the potential stranding surfaces, not just the convenient ones, and meteorites were found in some very unexpected settings, including the steep slopes of local nunataks.  We also used special techniques to recover several "ultraclean" meteorite samples to support detailed chemical and biological investigations;   these will be fully described and made available in a future newsletter.  Another meteorite (at least we think it's a meteorite) was found while still fully submerged in the ice.  The block of ice containing this specimen was collected; look elsewhere in this newsletter for a description of what we hope to do with this sample.

My thanks to the field team, which consisted of Les Bleamaster III, Marc Caffee, Marc Fries, Marie Keiding, Lucy McFadden, John Schutt, Tim Swindle, Dejun Tan and me.  Several future seasons will be required to complete the harvest of meteorites from the Miller Range and I think they'll all agree it's something to look forward to.    

Group photo of 07-08 team: From left to right Les Bleamaster, Marc Fries, Marie Keiding, Lucy McFadden,Marc Caffee, Dejun Tan, Tim Swindle not pictured: Ralph Harvey and John Schutt (Photo courtesy of Lucy McFadden.)
Presumed meteorite enclosed in ice

Reclassifications

In the last newsletter (AMN 30, no. 2) we announced 10 reclassifications of various chondrites and achondrites. Continuing to update our database, here are listed re-classifications of various carbonaceous, enstatite and R chondrites. These are based on either new published information or correction of terminology. Also, R chondrites were rare about a decade ago, and now we have 20 in the US collection making the subtypes more important for distinction. We anticipate more in future newsletters, and we thank Jeff Grossman for his aid in identifying many of these.

Sample

Previous

New

References

 

 

 

 

ALH 85005

C2

CM2

See notes below

ALH 85007

C2

CM2

"

ALH 85008

C2

CM2

"

ALH 85009

C2

CM2

"

ALH 85010

C2

CM2

"

ALH 85011

C2

CM2

"

ALH 85012

C2

CM2

"

ALH 85013

C2

CM2

"

ALH 85106

C2

CM2

"

ALH 90407

C2

CM2

"

ALHA 81312

C2

CM2

"

EET 83224

C2

CM2

"

EET 83250

C2

CM2

"

EET 83389

C2

CM2

"

EET 90021

C2

CM2

"

EET 90043

C2

CM2

"

EET 92005

C2

CM2

"

EET 92007

C2

CM2

"

EET 92008

C2

CM2

"

EET 92009

C2

CM2

"

EET 92010

C2

CM2

"

EET 96005

C2

CM2

"

EET 96006

C2

CM2

"

EET 96007

C2

CM2

"

EET 96011

C2

CM2

"

EET 96012

C2

CM2

"

EET 96013

C2

CM2

"

EET 96014

C2

CM2

"

EET 96016

C2

CM2

"

EET 96017

C2

CM2

"

EET 96019

C2

CM2

"

EET 96096

C2

CM2

"

EET 96097

C2

CM2

"

EET 96098

C2

CM2

"

EET 96226

C2

CM2

"

GRO 85202

C2

CM2

"

LEW 85306

C2

CM2

"

LEW 85307

C2

CM2

"

LEW 85309

C2

CM2

"

LEW 85311

C2

CM2

"

LEW 85312

C2

CM2

"

LEW 86004

C2

CM2

"

LEW 86005

C2

CM2

"

LEW 86007

C2

CM2

"

LEW 86008

C2

CM2

"

LEW 86009

C2

CM2

"

LEW 87016

C2

CM2

"

LEW 87148

C2

CM2

"

LEW 87271

C2

CM2

"

LEW 88001

C2

CM2

"

LEW 88002

C2

CM2

"

LEW 88003

C2

CM2

"

LEW 90500

C2

CM2

"

MAC 88101

C2

CM2

"

MAC 88176

C2

CM2

"

PCA 91008

C2

CM2

"

QUE 93005

C2

CM2

"

QUE 93018

C2

CM2

"

WIS 91608

C2

CM2

"

 

 

 

 

EET 90047

C2

CM1/2

1

EET 83334

CM1-2

CM1

1

LAP 031214

CM1-2

CM1/2

It is intermediate between 1 and 2

MAC 02820

CM1-2

CM1/2

It is intermediate between 1 and 2

ALH 83100

CM2

CM1/2

1

GRO 95566

C2

C2-ung

2

 

 

 

 

QUE 94411

CB

CBb

3

QUE 94627

CB

CBb

3

QUE 99309

CB

CBb

3

 

 

 

 

PCA 82500

CK4-5

CK4/5

It is intermediate between 4 and 5

EET 87860

CK5-6

CK5/6

It is intermediate between 5 and 6

 

 

 

 

ALH 82101

CO3

CO3.4

4

ALH 83108

CO3

CO3.5

5

ALH 85003

CO3

CO3.5

4

ALHA 77003

CO3

CO3.6

6,7

ALHA 77029

CO3

CO3.4

6

MET 00694

CO3

CO3.6

AMN 26, no. 1

MET 00737

CO3

CO3.6

AMN 26, no. 1

ALHA 77307

CO3 (?)

CO3.0

8

 

 

 

 

ALH 82132

E4

EH4

9

QUE 93513

E4

EH4

9

QUE 94368

E5

EL4

10

TIL 91714

E5

EL5

11

LON 94100

E6

EL6

12

QUE 99473

EH

EH-imp melt

AMN 25, no.2

EET 87746

EH3

EH4

13

EET 96135

EH4-5

EH4/5

It is intermediate between 4 and 5

EET 96202

EH4-5

EH4/5

It is intermediate between 4 and 5

EET 96217

EH4-5

EH4/5

It is intermediate between 4 and 5

EET 96223

EH4-5

EH4/5

It is intermediate between 4 and 5

EET 96299

EH4-5

EH4/5

It is intermediate between 4 and 5

EET 96309

EH4-5

EH4/5

It is intermediate between 4 and 5

EET 96341

EH4-5

EH4/5

It is intermediate between 4 and 5

LEW 88180

EH6

EH5

11

LEW 87119

EL6 (7?)

EL6

7 not verified

QUE 97289

E-ungr

Aubrite-an

Paired with QUE94204

QUE 97348

E-ungr

Aubrite-an

Paired with QUE94204

LAP 03780

Aub (Anom)

Aubrite

AMN 27, no. 3

 

 

 

 

ALH 85151

R

R3.6

14

PCA 91002

R

R3.8-6

15

PCA 91241

R

R3.8-6

15

PRE 95410

R

R3

AMN 20, no. 2

PRE 95411

R

R3

AMN 20, no. 2

PRE 95412

R

R3

AMN 20, no. 2

LAP 031135

R

R4

AMN 29, no. 1

LAP 031144

R

R4

AMN 29, no. 2

LAP 031156

R

R4

AMN 29, no. 1

LAP 031275

R

R5

AMN 29, no. 2

LAP 031387

R

R4

AMN 29, no. 2

LAP 03639

R

R4

AMN 29, no. 2

LAP 03731

R

R4

AMN 29, no. 2

LAP 03793

R

R4

AMN 29, no. 2

LAP 03902

R

R4

AMN 29, no. 2

LAP 04840

R

R6

AMN 29, no. 1

LAP 04845

R

R4

AMN 29, no. 2

PRE 95404

CV3

R3

16


Notes and references: Many carbonaceous chondrites were initially classified as C2 in early newsletters. These are mostly CM2, based on matrix properties, chondrules abundance and sizes, and therefore all these samples have been reclassified more specifically here as CM2. References for other samples: 1) Zolensky et al., 1997, GCA 61, 5099-5115; 2) Clayton and Mayeda, 1999, GCA 63, 2089-2104; 3) Weisberg et al., 2001, MAPS 36, 401-418; 4) D.W.G.Sears et al., 1991, Proc. NIPR Symp. Ant. Met. 4, 319; 5) R.H.Jones, 1997, Workshop on Modification of Chondritic Materials, LPI Tech. Rpt. 97-02, Part 1, p.30 (abs.); 6) subtype classification, E.R.D.Scott and R.H.Jones, 1990, GCA 54, 2485; 7) TL data, petrologic type 3.4, D.W.G.Sears et al., 1991, Proc. NIPR Symp. Ant. Met. 4, 319; 8) Grossman, J.N. and Brearley, A. (2005) MaPS 40, 87-122; 9) A.E.Rubin and E.R.D.Scott, 1997, GCA 61, 425; 10) A.E.Rubin, 1997, LPSC 28, 1201; 11) A.E.Rubin et al., 1995, LPSC 26, 1197; 12) A.E.Rubin et al., 1997, GCA 61, 849; 13) Y.Zhang et al., 1995, J. Geophys. Res. 100, 9417–9438; 14) A.E.Rubin and G.W.Kallemeyn, 1989, GCA 53, 3035; 15) Rubin, A.E. and Kallemeyn, 1994, Meteoritics 29, 255-264; 16) G.W.Kallemeyn, 1998, MAPS 33, p.A80 (abs.).

Terrestrial Age Survey of Antarctic Meteorites
Kuni Nishiizumi and Kees Welten

We are continuing a terrestrial age survey of Antarctic meteorites, based on the concentration of cosmogenic   36Cl (half-life = 3.01x105 yr) in the metal fraction. After separation of clean metal and chemical separation of Cl at the Space Sciences Laboratory, University of California, Berkeley, the 36Cl concentrations were measured by accelerator mass spectrometry (AMS) at PRIME Lab, Purdue University (mcaffee@purdue.edu). Table 1 shows the results of 36Cl concentrations and terrestrial ages in 100 Antarctic meteorites that were measured since our last report in Antarctic Meteorite Newsletter (Volume 29, Number 1, 2006). Since the 36Cl saturation values in the metal phase of small to medium-sized meteorites are in a relatively narrow range of 19-25 dpm/kg (2σ), the measured 36Cl concentrations yield a direct measure of the terrestrial age (Nishiizumi et al. 1989). The apparent terrestrial age, T(terr), (in kyr) can be calculated using the following equation:

T(terr) = -434 x ln(A/A0)

where A is the measured 36Cl concentration and A0 is the average 36Cl saturation value of 22.1±2.8 dpm/kg (2s) (Nishiizumi 1995). For meteorites with 36Cl concentrations >22.1 dpm/kg we only report an upper limit of the terrestrial age, whereas for meteorites with 36Cl concentrations between 19.3 and 22.1 dpm/kg, we report the possible range of terrestrial ages, with the age and error in Table 1 having the same value, e.g. 37±37 kyr instead of 8±57 kyr for ALHA 79016. For meteorites with 36Cl concentrations <19 dpm/kg there is a small possibility that these low values are due to unusually high shielding conditions or a short exposure age, but this can only be verified by measuring additional cosmogenic nuclides.

For more information about the 36Cl results, or the terrestrial ages, please contact Kees Welten (kcwelten@berkeley.edu) or Kuni Nishiizumi (kuni@ssl.berkeley.edu). This work was supported by NASA’s Cosmochemistry Program.

References
Nishiizumi K., Elmore D. and Kubik P. W. (1989) Update on terrestrial ages of Antarctic meteorites Earth Planet. Sci. Lett. 93, 299-313.
Nishiizumi K. 1995. Terrestrial ages of meteorites from cold and cold regions. In Workshop on meteorites from cold and hot deserts. (eds. L. Schultz, J. O. Annexstad and M. E. Zolensky) pp. 53-55. LPI Technical Report No. 95-02, Lunar and Planetary Institute, Houston, Texas.

Table 1. Measured 36Cl concentrations (in dpm/kg-metal) and 36Cl-derived terrestrial ages (in kyr) of Antarctic meteorites.

Meteorite

Type

36Cl

T(terr)

 

Meteorite

Type

36Cl

T(terr)

ALHA 79012

H5

23.1±0.5

<43

 

LAR 04328

H5

18.6±0.7

76±57

ALHA 79016

H6

21.7±0.7

37±37

 

MAC 87307

H4

17.6±0.3

98±55

ALHA 79018

L6

21.1±0.5

42±42

 

MAC 88119

H5

15.5±0.4

150±60

ALH 94001

L4

17.9±0.8

91±58

 

MAC 88175

LL6

13.0±0.5

230±60

ALH 97100

L6

13.6±0.5

210±60

 

MAC 02452

LL5

17.6±0.6

99±57

ALH 97101

H5

16.5±0.5

125±60

 

MAC 02454

L4

24.8±1.6

<31

ALH 99506

L5

14.8±0.5

175±60

 

MAC 02458

LL6

22.6±0.9

<60

CMS 04001

L5

22.5±0.5

<53

 

MAC 02601

L4

23.9±0.7

<30

CMS 04002

LL6

22.4±0.8

<63

 

MAC 02832

H5

20.2±0.7

53±53

CMS 04010

LL5

22.3±0.6

<60

 

MAC 02918

L4

22.8±0.8

<27

CMS 04019

H6

21.5±0.5

38±38

 

MET 00437

L6

15.2±0.4

160±60

DOM 03195

LL6

24.0±0.5

<28

 

MET 00442

H4

17.4±0.7

100±60

DOM 03260

LL5

20.5±0.5

51±51

 

MET 00444

LL6

16.9±0.7

120±60

FIN 01602

H5

24.3±0.5

<26

 

MET 00445

L5

17.7±0.7

96±58

FIN 01604

H5

25.5±0.5

< 5

 

MET 00447

L5

18.1±0.7

88±57

GEO 99102

H4

23.3±0.5

<40

 

MET 00449

LL6

21.7±0.6

36±36

GEO 99104

L6

20.3±0.5

53±53

 

MET 00461

L6

20.3±0.7

52±52

GEO 99109

H4

23.4±0.5

<53

 

MIL 99310

L5

23.6±0.9

<40

GRA 98013

H4

14.2±0.5

190±60

 

MIL 03362

LL5

19.9±0.8

55±55

GRA 98118

L6

22.2±0.5

<64

 

PCA 02002

L5

19.7±0.7

60±60

GRO 95526

L6

18.7±0.8

73±60

 

PCA 02003

H5

20.4±0.6

50±50

GRO 95528

L6

7.4±0.2

470±60

 

QUE 93019

L6

24.8±0.7

<14

GRO 95529

L5

21.9±0.5

34±34

 

QUE 93046

H5

22.7±0.5

<51

GRO 95532

H6

18.4±0.7

79±57

 

QUE 93182

L5

21.0±0.5

43±43

GRO 95537

H5

19.9±1.0

59±59

 

QUE 93264

L6

20.2±0.5

50±50

GRO 95538

H5

18.6±0.7

75±57

 

QUE 93572

H5

19.7±0.5

57±57

GRO 95540

L5

14.7±0.6

180±60

 

QUE 93711

H5

21.2±0.5

40±40

GRO 95541

H4

19.6±0.8

60±60

 

QUE 93724

L6

15.1±0.3

165±55

GRO 95547

H6

18.6±0.9

74±59

 

QUE 94237

H5

18.1±0.5

86±56

GRO 95552

LL4

20.5±0.6

49±49

 

QUE 94243

H6

20.3±0.7

52±52

GRO 95553

L6

18.9±0.9

69±59

 

QUE 94501

H6

19.7±0.3

54±54

GRO 95556

LL6

19.7±0.5

56±56

 

QUE 94719

L6

21.8±0.4

32±32

GRO 95557

LL5

16.0±0.4

140±56

 

RBT 03531

H5

23.5±0.5

<35

GRO 95590

LL4

18.9±0.6

68±57

 

SAN 03453

LL5

11.3±1.4

290±80

GRO 95607

L6

20.8±1.0

50±50

 

SAN 03458

LL6

19.9±0.4

55±55

GRO 95616

L4

17.6±0.6

99±57

 

SAN 03461

L6

20.7±0.6

46±46

GRO 03017

LL5

13.8±0.5

200±70

 

SAN 03480

L5

19.5±0.5

59±59

GRO 03032

H5

17.6±0.5

98±57

 

SAN 03487

LL4

15.8±0.6

150±60

GRO 03051

H5

23.1±0.5

<46

 

SAN 03488

H5

21.1±0.5

41±41

GRO 03063

L4

24.2±0.5

<26

 

TIL 82400

L5

23.1±0.6

22±22

GRO 03104

H5

22.5±0.5

<56

 

TIL 82404

L4

17.5±0.3

100±55

GRO 03105

LL6

22.5±0.5

<57

 

TIL 82405

H6

21.7±0.8

38±38

GRO 03114

H5

20.1±0.5

58±58

 

TIL 82409

H5

15.5±0.5

155±60

GRO 03138

L5

23.1±1.1

<53

 

WIS 90300

L5

15.9±0.3

140±60

LAP 02204

L5

19.4±0.8

63±63

 

WIS 91602

L5

15.5±0.4

155±60

LAP 02218

L4

21.3±0.7

42±42

 

WIS 91603

L4

18.2±0.5

85±56

LAP 02230

LL6

17.6±0.8

100±60

 

WIS 91610

H6

23.4±1.1

<47

LAP 02231

H5

20.7±0.8

49±49

 

WIS 91612

L6

21.2±0.5

40±40

LAP 02266

LL4

19.8±0.5

55±55

 

WIS 91617

H5

22.5±0.5

<53

LAP 02353

L6

23.0±1.3

<59

 

WIS 91618

LL4

20.7±0.5

45±45