Observations of nitrogen isotope fractionation in deeply embedded protostars

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Volume 572 (December 2014)

A&A, 572 (2014) A24

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Table B.1

Measurements of the ¹⁴N/¹⁵N ratio in solar system materials from the literature. (B) Stands for “bulk” measurements and (HS) for “hotspot”.

Object	¹⁴N/¹⁵N	δ¹⁵N	Ref.	Remarks
		[%0]

Sun	441 ± 6	− 383 ± 8	^a, ^⋆	Genesis
Lunar soils	≥358	≤ −240	^b	trapped solar wind
Meteorite (CAI)	424 ± 3	− 359 ± 6	^c, ^⋆	Isheyevo, osbornite (TiN)
Jupiter	526	− 423	^d	ISO, NH₃, ¹⁵N/¹⁴N =
Jupiter	435 ± 57	− 375 ± 82	^e, ^⋆	Galileo, NH₃
Jupiter	448 ± 62	− 393 ± 84	^f	Cassini-CIRS, NH₃
Jupiter	450 ± 106	− 396 ± 142	^g	Cassini-CIRS, NH₃
Saturn	≥357	≤−238	^h	ground-based, NH₃
Titan	183 ± 5	486 ± 41	ⁱ	Huygens, N₂, secondary origin

Earth (atmo.)	272	0	^j, ^⋆
Venus (atmo.)	272 ± 54	0 ± 200	^k, ^⋆
Mars (rock)	280	-30	^l, ^⋆	ALH84001 meteorite
Mars (atmo.)	173 ± 11	572 ± 82	^m	Curiosity, secondary origin
Comets	130 to 220	230 to 1100	ⁿ, ^⋆	approx. range, CN
Comet	139 ± 26	957 ± 366	^o	17P/Holmes, HCN
Comet	165 ± 40	648 ± 400	^o	17P/Holmes, CN
Comet	139 ± 38	957 ± 535	^p	Comet C/2012 S1 (ISON), NH₃
Comets	127 (80−190)	1142	^q	avg. spectrum (12 comets), NH₃
Comet (B)	181 to 272	0 to 500	^r	Comet 81P/Wild2, Stardust
Comet (HS)	118 to 368	-260 to 1300 ± 400	^r	Comet 81P/Wild2, Stardust
IDPs (B)	180.7 ± 2.3 to 305.1 ± 3.0	− 108 ± 9 to 500 ± 20	^s	IDPs “Kipling”, “Eliot”
IDPs (HS)	118 ± 6 to 171 ± 4	590 ± 40 to 1300 ± 120	^s	IDPs “Kipling”, “Pirandello”
Cluster IDPs	184 to 300	− 93 ± 4 to 480 ± 40	^t	IDPs “Porky”, “Dragonfly”
Meteorites (B)	192 to 237	146 to 415	^u, ^⋆
Meteorites (HS)	65 to 193	410 ± 130 to 3200 ± 700	^u
Meteorites	192 to 291	− 65.6 ± 2.9 to 415.3 ± 1.6	^v, ^⋆	insoluble organic matter (IOM)
Meteorite (HS)	50	4450	^w, ^⋆	Isheyevo clast
Meteorite (HS)	46	4900 ± 300	^x	Isheyevo clast

Notes. Boldface indicates the unit(s) reported in the original publication (if none of the values is in boldface, the original publication reports ¹⁵N/¹⁴N). Values marked with a star were used for Fig. 4.

Reference.

^(a)

Marty et al. (2011);

^(b)

Hashizume et al. (2000);

^(c)

Meibom et al. (2007);

^(d)

Fouchet et al. (2000);

^(e)

Owen et al. (2001);

^(f)

Abbas et al. (2004);

^(g)

Fouchet et al. (2004);

^(h)

Fletcher et al. (2014);

⁽ⁱ⁾

Niemann et al. (2005);

^(j)

Junk & Svec (1958); Coplen et al. (1992); Böhlke et al. (2005);

^(k)

Hoffman et al. (1979);

^(l)

Mathew & Marti (2001);

^(m)

Wong et al. (2013);

⁽ⁿ⁾

Manfroid et al. (2009); Jehin et al. (2009); Mumma & Charnley (2011) and references therein;

^(o)

Bockelée-Morvan et al. (2008);

^(p)

Shinnaka et al. (2014);

^(q)

Rousselot et al. (2014);

^(r)

McKeegan et al. (2006);

^(s)

Floss et al. (2006);

^(t)

Messenger (2000);

^(u)

Busemann et al. (2006);

^(v)

Alexander et al. (2007);

^(w)

Bonal et al. (2010);

^(x)

Briani et al. (2009).

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