Physics:List of interstellar and circumstellar molecules

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Infrared spectrum of HH 46/47 (image in inset), with vibrational bands of several molecules labelled in colour

This is a list of molecules that have been detected in the interstellar medium and circumstellar envelopes, grouped by the number of component atoms. The chemical formula is listed for each detected compound, along with any ionized form that has also been observed.

Background

Idealised example of the rotational spectrum (bottom) produced by transitions between different rotational energy levels (top) of a simple linear molecule. B is the rotational constant of the molecule, J is the rotational quantum number, J′ is the upper level and J″ is the lower level.

The molecules listed below were detected through astronomical spectroscopy. Their spectral features arise because molecules either absorb or emit a photon of light when they transition between two molecular energy levels. The energy (and thus the wavelength) of the photon matches the energy difference between the levels involved. Molecular electronic transitions occur when one of the molecule's electrons moves between molecular orbitals, producing a spectral line in the ultraviolet, optical or near-infrared parts of the electromagnetic spectrum. Alternatively, a vibrational transition transfers quanta of energy to (or from) vibrations of molecular bonds, producing signatures in the mid- or far-infrared. Gas-phase molecules also have quantised rotational levels, leading to transitions at microwave or radio wavelengths.[1]

Sometimes a transition can involve more than one of these types of energy level e.g. ro-vibrational spectroscopy changes both the rotational and vibrational energy level. Occasionally all three occur together, as in the Phillips band of C2 (diatomic carbon), in which an electronic transition produces a line in the near-infrared, which is then split into several vibronic bands by a simultaneous change in vibrational level, which in turn are split again into rotational branches.[2]

The spectrum of a particular molecule is governed by the selection rules of quantum chemistry and by its molecular symmetry. Some molecules have simple spectra which are easy to identify, whilst others (even some small molecules) have extremely complex spectra with flux spread among many different lines, making them far harder to detect.[3] Interactions between the atomic nuclei and the electrons sometimes cause further hyperfine structure of the spectral lines. If the molecule exists in multiple isotopologues (versions containing different atomic isotopes), the spectrum is further complicated by isotope shifts.

Detection of a new interstellar or circumstellar molecule requires identifying a suitable astronomical object where it is likely to be present, then observing it with a telescope equipped with a spectrograph working at the required wavelength, spectral resolution and sensitivity. The first molecule detected in the interstellar medium was the methylidyne radical (CH•) in 1937, through its strong electronic transition at 4300 angstroms (in the optical).[4] Advances in astronomical instrumentation have led to increasing numbers of new detections. From the 1950s onwards, radio astronomy began to dominate new detections, with sub-mm astronomy also becoming important from the 1990s.[3]

The inventory of detected molecules is highly biased towards certain types which are easier to detect. For example, radio astronomy is most sensitive to small linear molecules with a high molecular dipole.[3] The most common molecule in the Universe, H2 (molecular hydrogen), is completely invisible to radio telescopes because it has no dipole;[3] its electronic transitions are too energetic for optical telescopes, so detection of H2 required ultraviolet observations with a sounding rocket.[5] Vibrational lines are often not specific to an individual molecule, allowing only the general class to be identified. For example, the vibrational lines of polycyclic aromatic hydrocarbons (PAHs) were identified in 1984,[6] showing the class of molecules is very common in space,[7] but it took until 2021 to identify any specific PAHs through their rotational lines.[8][9]

The carbon star CW Leonis. The visible shells of circumstellar material were ejected by the central star over thousands of years.

One of the richest sources for detecting interstellar molecules is Sagittarius B2 (Sgr B2), a giant molecular cloud near the centre of the Milky Way. About half of the molecules listed below were first found in Sgr B2, and many of the others have been subsequently detected there.[10] Many of the largest molecules were first detected in another molecular cloud, TMC-1. A rich source of circumstellar molecules is CW Leonis (also known as IRC +10216), a nearby carbon star, where about 50 molecules have been identified.[11] There is no clear boundary between interstellar and circumstellar media, so both are included in the tables below.

The discipline of astrochemistry includes understanding how these molecules form and explaining their abundances. The extremely low density of the interstellar medium is not conducive to the formation of molecules, making conventional gas-phase reactions between neutral species (atoms or molecules) inefficient. Many regions also have very low temperatures (typically 10 kelvin inside a molecular cloud), further reducing the reaction rates, or high ultraviolet radiation fields, which destroy molecules through photochemistry.[12] Explaining the observed abundances of interstellar molecules requires calculating the balance between formation and destruction rates using gas-phase ion chemistry (often driven by cosmic rays), surface chemistry on cosmic dust, radiative transfer including interstellar extinction, and sophisticated reaction networks.[13] The use of molecular lines to determine the physical properties of astronomical objects is known as molecular astrophysics.

Molecules

The following tables list molecules that have been detected in the interstellar medium or circumstellar matter, grouped by the number of component atoms. Neutral molecules and their molecular ions are listed in separate columns; if there is no entry in the molecule column, only the ionized form has been detected. Designations (names of molecules) are those used in the scientific literature describing the detection; if none was given that field is left empty. Mass is listed in daltons. Deuterated molecules, which contain at least one deuterium (2H) atom, have slightly different masses and are listed in a separate table. The total number of unique species, including distinct ionization states, is indicated in each section header.

Most of the molecules detected so far are organic. The only detected inorganic molecule with five or more atoms is SiH4.[14] Molecules larger than that all have at least one carbon atom, with no N−N or O−O bonds.[14]

Diatomic (45)

Carbon monoxide is frequently used to trace the distribution of mass in molecular clouds.[15]
Molecule Designation Mass Ions
AlCl Aluminium monochloride[16] 62.5 —
AlF Aluminium monofluoride[17] 46 —
AlO Aluminium monoxide[18] 43 —
— Argonium[19][20] 37[note 1] ArH+
C2 Diatomic carbon[21][22] 24 —
— Fluoromethylidynium 31 CF+[23]
CH Methylidyne radical[24][25] 13 CH+[26]
CN Cyano radical[25][27][28] 26 CN+,[29] CN−[30]
CO Carbon monoxide[31][32] 28 CO+[33]
CP Carbon monophosphide[28] 43 —
CS Carbon monosulfide[34] 44 —
FeO Iron(II) oxide[35] 82 —
— Helium hydride ion[36][37] 5 HeH+
H2 Molecular hydrogen[5] 2 —
HCl Hydrogen chloride[38] 36.5 HCl+[39]
HF Hydrogen fluoride[40] 20 —
HO Hydroxyl radical[34] 17 OH+[41]
KCl Potassium chloride[16] 75.5 —
NH Imidogen radical[42][43] 15 —
N2 Molecular nitrogen[44][45] 28 —
NO Nitric oxide[46] 30 NO+[29]
NS Nitrogen sulfide[34] 46 —
NaCl Sodium chloride[16] 58.5 —
— Magnesium monohydride cation
O2 Molecular oxygen[47] 32 —
PN Phosphorus mononitride[48][49] 45 —
PO Phosphorus monoxide[50] 47 —
SH Sulfur monohydride[51] 33 SH+[52]
SO Sulfur monoxide[34] 48 SO+[26]
SiC Carborundum[53] 40 —
SiN –[54] 42 —
SiO Silicon monoxide[34] 44 —
NaS Sodium sulfide[55] 55 —
MgS Magnesium sulfide[55] 56 —
SiS Silicon monosulfide[34] 60 —
TiO Titanium(II) oxide[56] 64[note 2] —

Triatomic (45)

The H+3 cation is one of the most abundant ions in the universe. It was first detected in 1993.[57][58]
Molecule Designation Mass Ions
AlNC Aluminium isocyanide[34] 53 —
AlOH Aluminium hydroxide[59] 44 —
C3 Tricarbon[60][61] 36 —
C2H Ethynyl radical[27] 25 —
CCN Cyanomethylidyne[62] 38 —
C2O Dicarbon monoxide[63] 40 —
C2S Thioxoethenylidene[64] 56 —
C2P —[65] 55 —
CO2 Carbon dioxide[66] 44 —
CaNC Calcium(I) isocyanide[67] 66 —
FeCN Iron(I) cyanide[68] 82 —
— Protonated molecular hydrogen 3 H+3[57][58]
H2C Methylene radical[69] 14 —
— Chloronium 37.5 H2Cl+[70]
H2O Water[71] 18 H2O+[72]
HO2 Hydroperoxyl[73] 33 —
H2S Hydrogen sulfide[34] 34 —
HCN Hydrogen cyanide[27][74] 27 —
HNC Hydrogen isocyanide[75][76] 27 —
HCO Formyl radical[77] 29 HCO+[26][77][78]
HCP Phosphaethyne[79] 44 —
HCS Thioformyl[80] 45 HCS+[26][78]
— Diazenylium[78][26][81] 29 HN+2
HNO Nitroxyl[82] 31 —
— Isoformyl 29 HOC+[27]
HSC Isothioformyl[80] 45 —
KCN Potassium cyanide[34] 65 —
MgCN Magnesium(I) cyanide[34] 50 —
MgNC Magnesium(I) isocyanide[34] 50 —
NH2 Amino radical[83] 16 —
N2O Nitrous oxide[84] 44 —
NaCN Sodium cyanide[34] 49 —
NaOH Sodium hydroxide[85] 40 —
OCS Carbonyl sulfide[86] 60 —
O3 Ozone[87] 48 —
SO2 Sulfur dioxide[88] 64 —
c-SiC2 c-Silicon dicarbide[53] 52 —
SiCSi Disilicon carbide[89] 68 —
SiCN Silicon carbonitride[90] 54 —
SiNC [91] 54 —
CaC2 Calcium dicarbide[92] 64 —
TiO2 Titanium dioxide[56] 79.9 —

Four atoms (31)

Formaldehyde is an organic molecule that is widely distributed in the interstellar medium.[93]
Molecule Designation Mass Ions
CH3 Methyl radical[94] 15 CH+
3[95]
l-C3H Propynylidyne[96] 37 l-C3H+[97]
c-C3H Cyclopropynylidyne[98] 37 —
C3N Cyanoethynyl[99] 50 C3N−[100]
C3O Tricarbon monoxide[96] 52 —
C3S Tricarbon sulfide[64] 68 —
— Hydronium 19 H3O+[101]
C2H2 Acetylene[102] 26 —
H2CN Methylene amidogen[103] 28 H2CN+[26]
H2NC Aminocarbyne[104] 28 —
H2CO Formaldehyde[93] 30 —
H2CS Thioformaldehyde[105] 46 —
HCCN —[106] 39 —
HCCO Ketenyl[107] 41 —
— Protonated hydrogen cyanide 28 HCNH+[78]
— Protonated carbon dioxide 45 HOCO+[108]
HCNO Fulminic acid[109] 43 —
HOCN Cyanic acid[110] 43 —
CNCN Isocyanogen[111] 52 —
HOOH Hydrogen peroxide[112] 34 —
HNCO Isocyanic acid[88] 43 —
HNCN Cyanomidyl radical[113] 41 —
HNCS Isothiocyanic acid[114] 59 —
NH3 Ammonia[115] 17 —
HSCN Thiocyanic acid[116] 59 —
HNSO Thionylimide[117] 63 —
SiC3 Silicon tricarbide[34] 64 —
HMgNC Hydromagnesium isocyanide[118] 51.3 —
HNO2 Nitrous acid[119] 47 —

Five atoms (21)

Methane, the primary component of natural gas, has also been detected in molecular clouds.[120]
Molecule Designation Mass Ions
— Ammonium ion 18 NH+4[121][122]
CH4 Methane[123] 16 —
CH3O Methoxy radical[124] 31 —
c-C3H2 Cyclopropenylidene[27][125][126] 38 —
l-H2C3 Propadienylidene[126] 38 —
H2CCN Cyanomethyl[127] 40 —
H2C2O Ketene[88] 42 —
H2CNH Methylenimine[128] 29 —
HNCNH Carbodiimide[129] 42 —
— Protonated formaldehyde 31 H2COH+[130]
C4H Butadiynyl[34] 49 C4H−[131]
HC3N Cyanoacetylene[27][78][132][133] 51 —
HCC-NC Isocyanoacetylene[134] 51 —
HCOOH Formic acid[135][132] 46 —
NH2CN Cyanamide[136][137] 42 —
NH2OH Hydroxylamine[138] 37 —
— Protonated cyanogen 53 NCCNH+[139]
HC(O)CN Cyanoformaldehyde[140] 55 —
C5 Linear C5[141] 60 —
HCS2H dithioformic acid[142] 78 —
SiC4 Silicon-carbide cluster[53] 92 —
SiH4 Silane[143] 32 —

Six atoms (16)

In the ISM, formamide (above) can combine with methylene to form acetamide.[144]
Molecule Designation Mass Ions
c-H2C3O Cyclopropenone[145] 54 —
E-HNCHCN E-Cyanomethanimine[146] 54 —
C2H4 Ethylene[147] 28 —
CH3CN Acetonitrile[88][148][149] 40 —
CH3NC Methyl isocyanide[148] 40 —
CH3OH Methanol[88][150] 32 —
CH3SH Methanethiol[151] 48 —
l-H2C4 Diacetylene[152] 50 —
— Protonated cyanoacetylene 52 HC3NH+[78]
HCONH2 Formamide[144] 44 —
HOCOOH Carbonic acid[153] —
C5H Pentynylidyne[64] 61 —
C5N Cyanobutadiynyl radical[154] 74 —
HC2CHO Propynal[155] 54 —
HC4N —[34]  63 —
CH2CNH Ketenimine[125] 40 —
C5S —[156] 92 —

Seven atoms (16)

Acetaldehyde (above) and its isomers vinyl alcohol and ethylene oxide have all been detected in interstellar space.[157]
Molecule Designation Mass Ions
c-C2H4O Ethylene oxide[158] 44 —
CH3C2H Methylacetylene[27] 40 —
H3CNH2 Methylamine[159] 31 —
CH2CHCN Acrylonitrile[88][148] 53 —
53 —
H2CHCOH Vinyl alcohol[157] 44 —
C6H Hexatriynyl radical[64] 73 C6H−[126][160]
HC4CN Cyanodiacetylene[88][133][148] 75 —
HC4NC Isocyanodiacetylene[161] 75 —
HC5O —[162] 77 —
CH3CHO Acetaldehyde[158] 44 —
CH3CHS Thioacetaldehyde[163] 60 —
CH3NCO Methyl isocyanate[164] 57 —
HOCH2CN Glycolonitrile[165] 57 —
HC3HCN 1-cyano propargyl radical[166] 64 —
CH2C3N 3-cyano propargyl radical[167] 64 —

Eight atoms (14)

The radio signature of acetic acid, a compound found in vinegar, was confirmed in 1997.[168]
Molecule Designation Mass
H3CC2CN Methylcyanoacetylene[169] 65
HC3H2CN Propargyl cyanide[170] 65
H2COHCHO Glycolaldehyde[171] 60
(CHOH)2 1,2-ethenediol[172] 60
HCOOCH3 Methyl formate[88][132] 60
CH3COOH Acetic acid[168] 60
H2C6 Hexapentaenylidene[152] 74
CH2CHCHO Propenal[125] 56
CH2CCHCN Cyanoallene[125][169] 65
CH3CHNH Ethanimine[173] 43
C2H3NH2 Vinylamine[174] 43
C7H Heptatrienyl radical[175] 85
NH2CH2CN Aminoacetonitrile[176] 56
(NH2)2CO Urea[177] 60

Nine atoms (11)

Molecule Designation Mass Ions
CH3C4H Methyldiacetylene[178] 64 —
CH3OCH3 Dimethyl ether[179] 46 —
CH3CH2CN Propionitrile[88][148] 55 —
CH3CONH2 Acetamide[125][144][137] 59 —
CH3CH2OH Ethanol[180] 46 —
C8H Octatetraynyl radical[181] 97 C8H−[182][183]
HC7N Cyanohexatriyne or Cyanotriacetylene[115][184][185] 99 —
CH3CHCH2 Propylene (propene)[186] 42 —
CH3CH2SH Ethyl mercaptan[187] 62 —
CH3SCH3 Dimethyl sulfide[188] 62 —
CH3NHCHO N-methylformamide[137] 59 —

Ten or more atoms (24)

Diacetylene, HCCCCH
Methyldiacetylene, HCCCCCH3
Cyanotetraacetylene, HCCCCCCCCCN
A number of polyyne-derived chemicals are among the heaviest molecules found in the interstellar medium.
Atoms Molecule Designation Mass Ions
10 (CH3)2CO Acetone[88][189] 58 —
10 (CH2OH)2 Ethylene glycol[190][191] 62 —
10 CH3CH2CHO Propanal[125] 58 —
10 CH3OCH2OH Methoxymethanol[192] 62 —
10 CH3C5N Methylcyanodiacetylene[125] 89 —
10 CH3CHCH2O Propylene oxide[193] 58 —
11 NH2CH2CH2OH Ethanolamine[194] 61 —
11 HC8CN Cyanotetraacetylene[184] 123 —
11 C2H5OCHO Ethyl formate[195] 74 —
11 CH3COOCH3 Methyl acetate[196] 74 —
11 CH3C6H Methyltriacetylene[125][178] 88 —
12 C6H6 Benzene[152] 78 —
12 C3H7CN n-Propyl cyanide[195] 69 —
12 (CH3)2CHCN iso-Propyl cyanide[197][198] 69 —
13 CH3OCH2CH2OH 2-methoxyethanol[199] 76 —
13 C6H5CN Benzonitrile[200] 104 —
13 HC10CN Cyanopentaacetylene[184] 147 —
17 C9H8 Indene[9] 116 —
19 C10H7CN 1-cyanonaphthalene[8] 153 —
19 C10H7CN 2-cyanonaphthalene[8] 153 —
21 C12H7CN 1-cyanoacenaphtylene[201] 177 —
21 C12H7CN 5-cyanoacenaphtylene[201] 177 —
27 C16H9CN 1-cyanopyrene[202] 227 —
27 C16H9CN 2-cyanopyrene[203] 227 —
27 C16H9CN 4-cyanopyrene[203] 227 —
37 C24H11CN cyanocoronene[204] 325 —
60 C60 Buckminsterfullerene
(C60 fullerene)[205]		 720 C+60[206][207][208]
70 C70 C70 fullerene[205] 840 —

Deuterated molecules (22)

These molecules all contain one or more deuterium atoms, a heavier isotope of hydrogen.

Atoms Molecule Designation
2 HD Hydrogen deuteride[209][210]
3 H2D+, HD+2 Trihydrogen cation[209][210]
3 HDO, D2O Heavy water[211][212]
3 DCN Hydrogen cyanide[213]
3 DCO Formyl radical[213]
3 DNC Hydrogen isocyanide[213]
3 N2D+ —[213] 
3 NHD, ND2 Amidogen[214] 
4 NH2D, NHD2, ND3 Ammonia[210][215][216]
4 HDCO, D2CO Formaldehyde[210][217]
4 DNCO Isocyanic acid[218]
5 NH3D+ Ammonium ion[219][220]
6 NH2CDO; NHDCHO Formamide[218]
7 CH2DCCH, CH3CCD Methylacetylene[221][222]

Unconfirmed (16)

Evidence for the existence of the following molecules has been reported in the scientific literature, but the detections either are described as tentative by the authors, or have been challenged by other researchers. They await independent confirmation.

Atoms Molecule Designation
2 SiH Silylidine[75]
2 CaO Calcium oxide[55]
4 PH3 Phosphine[223]
4 MgCCH Magnesium monoacetylide[156]
4 NCCP Cyanophosphaethyne[156]
5 H2NCO+ —[224]
6 SiH3CN Silyl cyanide[156]
10 H2NCH2COOH Glycine[225][226]
10 C2H5NH2 Ethylamine[174]
12 CO(CH2OH)2 Dihydroxyacetone[227][228]
12 C2H5OCH3 Ethyl methyl ether[229]
18 C10H+8 Naphthalene cation[230]
24 C24 Graphene[231]
24 C14H10 Anthracene[232][233]
26 C16H10 Pyrene[232]
27 C11H12N2O2 Tryptophan[234][235][236]

See also

Notes

  1. ↑ On Earth, the dominant isotope of argon is 40Ar, so ArH+ would have a mass of 41 amu. However, the interstellar detection was of the 36ArH+ isotopologue, which has a mass of 37 amu.
  2. ↑ Although titanium has several stable isotopes, only the 48Ti16O isotopologue was detected,[56] which has a molecular mass of 64 amu.

References

  1. ↑ Shu, Frank H. (1982). The Physical Universe: An Introduction to Astronomy. University Science Books. ISBN 978-0-935702-05-7. https://books.google.com/books?id=v_6PbAfapSAC. 
  2. ↑ Chaffee, Frederick H.; Lutz, Barry L.; Black, John H.; Vanden Bout, Paul A.; Snell, Ronald L. (1980). "Rotational fine-structure lines of interstellar C2 toward Zeta Persei". The Astrophysical Journal 236: 474. doi:10.1086/157764. Bibcode: 1980ApJ...236..474C. 
  3. ↑ 3.0 3.1 3.2 3.3 McGuire, Brett A. (2018). "2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules". The Astrophysical Journal Supplement Series 239 (2): 17. doi:10.3847/1538-4365/aae5d2. Bibcode: 2018ApJS..239...17M. 
  4. ↑ Woon, D. E. (May 2005), Methylidyne radical, The Astrochemist, http://www.astrochymist.org/AMOTM/amotm_0505.html, retrieved 2007-02-13 
  5. ↑ 5.0 5.1 Carruthers, George R. (1970), "Rocket Observation of Interstellar Molecular Hydrogen", Astrophysical Journal 161: L81–L85, doi:10.1086/180575, Bibcode: 1970ApJ...161L..81C 
  6. ↑ Leger, A.; Puget, J. L. (1984). "Identification of the "unidentified" IR emission features of interstellar dust ?". Astronomy and Astrophysics 137: L5. Bibcode: 1984A&A...137L...5L. 
  7. ↑ Tielens, A.G.G.M. (2008). "Interstellar Polycyclic Aromatic Hydrocarbon Molecules". Annual Review of Astronomy and Astrophysics 46: 289–337. doi:10.1146/annurev.astro.46.060407.145211. Bibcode: 2008ARA&A..46..289T. https://zenodo.org/record/1234931. 
  8. ↑ 8.0 8.1 8.2 McGuire, Brett A. et al. (19 March 2021). "Detection of two interstellar polycyclic aromatic hydrocarbons via spectral matched filtering". Science 371 (6535): 1265–1269. doi:10.1126/science.abb7535. PMID 33737489. Bibcode: 2021Sci...371.1265M. 
  9. ↑ 9.0 9.1 Burkhardt, Andrew M. et al. (1 June 2021). "Discovery of the Pure Polycyclic Aromatic Hydrocarbon Indene (c-C9H8) with GOTHAM Observations of TMC-1". The Astrophysical Journal Letters 913 (2): L18. doi:10.3847/2041-8213/abfd3a. Bibcode: 2021ApJ...913L..18B. 
  10. ↑ Cummins, S. E.; Linke, R. A.; Thaddeus, P. (1986), "A survey of the millimeter-wave spectrum of Sagittarius B2", Astrophysical Journal Supplement Series 60: 819–878, doi:10.1086/191102, Bibcode: 1986ApJS...60..819C 
  11. ↑ Kaler, James B. (2002). The hundred greatest stars. Copernicus Series. Springer. ISBN 978-0-387-95436-3. https://books.google.com/books?id=Aq24O7B4ehoC&pg=PA107. Retrieved 2011-05-09. 
  12. ↑ Brown, Laurie M.; Pais, Abraham; Pippard, A. B. (1995), "The physics of the interstellar medium", Twentieth Century Physics (2nd ed.), CRC Press, p. 1765, ISBN 978-0-7503-0310-1 
  13. ↑ Dalgarno, A. (2006), "Interstellar Chemistry Special Feature: The galactic cosmic ray ionization rate", Proceedings of the National Academy of Sciences 103 (33): 12269–12273, doi:10.1073/pnas.0602117103, PMID 16894166, Bibcode: 2006PNAS..10312269D 
  14. ↑ 14.0 14.1 Klemperer, William (2011), "Astronomical Chemistry", Annual Review of Physical Chemistry 62: 173–184, doi:10.1146/annurev-physchem-032210-103332, PMID 21128763, Bibcode: 2011ARPC...62..173K 
  15. ↑ The Structure of Molecular Cloud Cores, Centre for Astrophysics and Planetary Science, University of Kent, http://astro.kent.ac.uk/gw/molcloud.html, retrieved 2007-02-16 
  16. ↑ 16.0 16.1 16.2 Cernicharo, J.; Guelin, M. (1987), "Metals in IRC+10216 - Detection of NaCl, AlCl, and KCl, and tentative detection of AlF", Astronomy and Astrophysics 183 (1): L10–L12, Bibcode: 1987A&A...183L..10C 
  17. ↑ Ziurys, L. M.; Apponi, A. J.; Phillips, T. G. (1994), "Exotic fluoride molecules in IRC +10216: Confirmation of AlF and searches for MgF and CaF", Astrophysical Journal 433 (2): 729–732, doi:10.1086/174682, Bibcode: 1994ApJ...433..729Z 
  18. ↑ Tenenbaum, E. D.; Ziurys, L. M. (2009), "Millimeter Detection of AlO (X2Σ+): Metal Oxide Chemistry in the Envelope of VY Canis Majoris", Astrophysical Journal 694 (1): L59–L63, doi:10.1088/0004-637X/694/1/L59, Bibcode: 2009ApJ...694L..59T 
  19. ↑ Barlow, M. J. et al. (2013), "Detection of a Noble Gas Molecular Ion, 36ArH+, in the Crab Nebula", Science 342 (6164): 1343–1345, doi:10.1126/science.1243582, PMID 24337290, Bibcode: 2013Sci...342.1343B 
  20. ↑ Quenqua, Douglas (13 December 2013). "Noble Molecules Found in Space". The New York Times. https://www.nytimes.com/2013/12/17/science/space/noble-molecules-found-in-space.html. 
  21. ↑ Souza, S. P; Lutz, B. L (1977). "Detection of C2 in the interstellar spectrum of Cygnus OB2 number 12 /VI Cygni number 12/". The Astrophysical Journal 216: L49. doi:10.1086/182507. Bibcode: 1977ApJ...216L..49S. 
  22. ↑ Lambert, D. L.; Sheffer, Y.; Federman, S. R. (1995), "Hubble Space Telescope observations of C2 molecules in diffuse interstellar clouds", Astrophysical Journal 438: 740–749, doi:10.1086/175119, Bibcode: 1995ApJ...438..740L 
  23. ↑ Neufeld, D. A. et al. (2006), "Discovery of interstellar CF+", Astronomy and Astrophysics 454 (2): L37–L40, doi:10.1051/0004-6361:200600015, Bibcode: 2006A&A...454L..37N 
  24. ↑ Landau, Elizabeth (12 October 2016). "Building Blocks of Life's Building Blocks Come From Starlight". NASA. http://www.jpl.nasa.gov/news/news.php?feature=6645. 
  25. ↑ 25.0 25.1 Adams, Walter S. (1941), "Some Results with the COUDÉ Spectrograph of the Mount Wilson Observatory", Astrophysical Journal 93: 11–23, doi:10.1086/144237, Bibcode: 1941ApJ....93...11A 
  26. ↑ 26.0 26.1 26.2 26.3 26.4 26.5 Smith, D. (1988), "Formation and Destruction of Molecular Ions in Interstellar Clouds", Philosophical Transactions of the Royal Society of London 324 (1578): 257–273, doi:10.1098/rsta.1988.0016, Bibcode: 1988RSPTA.324..257S 
  27. ↑ 27.0 27.1 27.2 27.3 27.4 27.5 27.6 Fuente, A. et al. (2005), "Photon-dominated Chemistry in the Nucleus of M82: Widespread HOC+ Emission in the Inner 650 Parsec Disk", Astrophysical Journal 619 (2): L155–L158, doi:10.1086/427990, Bibcode: 2005ApJ...619L.155F 
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  220. ↑ Doménech, J. L. et al. (2013), "Improved Determination of the 10-00 Rotational Frequency of NH3D+ from the High-Resolution Spectrum of the ν4 Infrared Band", Astrophysical Journal Letters 771 (1): L11, doi:10.1088/2041-8205/771/1/L10, Bibcode: 2013ApJ...771L..11D 
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  222. ↑ Markwick, A. J.; Charnley, S. B.; Butner, H. M.; Millar, T. J. (2005), "Interstellar CH3CCD", The Astrophysical Journal 627 (2): L117–L120, doi:10.1086/432415, Bibcode: 2005ApJ...627L.117M. 
  223. ↑ Agúndez, M. et al. (2008-06-04), "Tentative detection of phosphine in IRC +10216", Astronomy & Astrophysics 485 (3): L33, doi:10.1051/0004-6361:200810193, Bibcode: 2008A&A...485L..33A 
  224. ↑ Gupta, H. et al. (2013), "Laboratory Measurements and Tentative Astronomical Identification of H2NCO+", Astrophysical Journal Letters 778 (1): L1, doi:10.1088/2041-8205/778/1/L1, Bibcode: 2013ApJ...778L...1G, http://authors.library.caltech.edu/43247/1/2041-8205_778_1_L1.pdf 
  225. ↑ Snyder, L. E. et al. (2005), "A Rigorous Attempt to Verify Interstellar Glycine", Astrophysical Journal 619 (2): 914–930, doi:10.1086/426677, Bibcode: 2005ApJ...619..914S. 
  226. ↑ Kuan, Y. J. et al. (2003), "Interstellar Glycine", Astrophysical Journal 593 (2): 848–867, doi:10.1086/375637, Bibcode: 2003ApJ...593..848K. 
  227. ↑ Widicus Weaver, S. L.; Blake, G. A. (2005), "1,3-Dihydroxyacetone in Sagittarius B2(N-LMH): The First Interstellar Ketose", Astrophysical Journal Letters 624 (1): L33–L36, doi:10.1086/430407, Bibcode: 2005ApJ...624L..33W 
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  231. ↑ García-Hernández, D. A. et al. (2011), "The Formation of Fullerenes: Clues from New C60, C70, and (Possible) Planar C24 Detections in Magellanic Cloud Planetary Nebulae", Astrophysical Journal Letters 737 (2): L30, doi:10.1088/2041-8205/737/2/L30, Bibcode: 2011ApJ...737L..30G. 
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  233. ↑ Iglesias-Groth, S. et al. (May 2010), "A search for interstellar anthracene toward the Perseus anomalous microwave emission region", Monthly Notices of the Royal Astronomical Society 407 (4): 2157–2165, doi:10.1111/j.1365-2966.2010.17075.x, Bibcode: 2010MNRAS.407.2157I 
  234. ↑ Iglesias-Groth, S. (August 2023). "A search for tryptophan in the gas of the IC 348 star cluster of the Perseus molecular cloud". Monthly Notices of the Royal Astronomical Society 523 (2): 2876–2886. doi:10.1093/mnras/stad1535. Bibcode: 2023MNRAS.523.2876I. 
  235. ↑ Hudson, Reggie L. (2023). "Interstellar tryptophan revisited". Monthly Notices of the Royal Astronomical Society 526 (3): 4051–4053. doi:10.1093/mnras/stad3058. Bibcode: 2023MNRAS.526.4051H. https://academic.oup.com/mnras/article/526/3/4051/7310867. "there is no firm support for the tryptophan assignment". 
  236. ↑ Dhariwal, Aditya et al. (June 2024). "On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348". The Astrophysical Journal Letters 968 (1): L9. doi:10.3847/2041-8213/ad4d9a. ISSN 2041-8205. Bibcode: 2024ApJ...968L...9D. "there is no compelling evidence for the tryptophan assignment". 



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