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The Info List - List Of Interstellar And Circumstellar Molecules


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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.

Contents

1 Detection

1.1 History

2 Theoretical models 3 Molecules

3.1 Diatomic (43) 3.2 Triatomic (41) 3.3 Four atoms (27) 3.4 Five atoms (19) 3.5 Six atoms (16) 3.6 Seven atoms (11) 3.7 Eight atoms (11) 3.8 Nine atoms (10) 3.9 Ten or more atoms (17)

4 Deuterated molecules (20) 5 Unconfirmed (13) 6 See also 7 References 8 External links

Detection[edit] The molecules listed below were detected by spectroscopy. Their spectral features are generated by transitions of component electrons between different energy levels, or by rotational or vibrational spectra. Detection usually occurs in radio, microwave, or infrared portions of the spectrum.[1] Interstellar molecules are formed by chemical reactions within very sparse interstellar or circumstellar clouds of dust and gas. Usually this occurs when a molecule becomes ionized, often as the result of an interaction with a cosmic ray. This positively charged molecule then draws in a nearby reactant by electrostatic attraction of the neutral molecule's electrons. Molecules can also be generated by reactions between neutral atoms and molecules, although this process is generally slower.[2] The dust plays a critical role of shielding the molecules from the ionizing effect of ultraviolet radiation emitted by stars.[3] History[edit] The chemistry of life may have begun shortly after the Big Bang, 13.8 billion years ago, during a habitable epoch when the Universe
Universe
was only 10–17 million years old.[4][5] The first carbon-containing molecule detected in the interstellar medium was the methylidyne radical (CH•) in 1937.[6] From the early 1970s it was becoming evident that interstellar dust consisted of a large component of more complex organic molecules (COMs),[7] probably polymers. Chandra Wickramasinghe
Chandra Wickramasinghe
proposed the existence of polymeric composition based on the molecule formaldehyde (H2CO).[8] Fred Hoyle and Chandra Wickramasinghe
Chandra Wickramasinghe
later proposed the identification of bicyclic aromatic compounds from an analysis of the ultraviolet extinction absorption at 2175 Å,[9] thus demonstrating the existence of polycyclic aromatic hydrocarbon molecules in space. In 2004, scientists reported[10] detecting the spectral signatures of anthracene and pyrene in the ultraviolet light emitted by the Red Rectangle nebula (no other such complex molecules had ever been found before in outer space). This discovery was considered a confirmation of a hypothesis that as nebulae of the same type as the Red Rectangle approach the ends of their lives, convection currents cause carbon and hydrogen in the nebulae's core to get caught in stellar winds, and radiate outward.[11] As they cool, the atoms supposedly bond to each other in various ways and eventually form particles of a million or more atoms. The scientists inferred[10] that since they discovered polycyclic aromatic hydrocarbons (PAHs) — which may have been vital in the formation of early life on Earth — in a nebula, by necessity they must originate in nebulae.[11] In 2010, fullerenes (or "buckyballs") were detected in nebulae.[12] Fullerenes
Fullerenes
have been implicated in the origin of life; according to astronomer Letizia Stanghellini, "It's possible that buckyballs from outer space provided seeds for life on Earth."[13] In October 2011, scientists found using spectroscopy that cosmic dust contains complex organic compounds ("amorphous organic solids with a mixed aromatic-aliphatic structure") that could be created naturally, and rapidly, by stars.[14][15][16] The compounds are so complex that their chemical structures resemble the makeup of coal and petroleum; such chemical complexity was previously thought to arise only from living organisms.[14] These observations suggest that organic compounds introduced on Earth by interstellar dust particles could serve as basic ingredients for life due to their surface-catalytic activities.[17][18] One of the scientists suggested that these compounds may have been related to the development of life on Earth and said that, "If this is the case, life on Earth may have had an easier time getting started as these organics can serve as basic ingredients for life."[14] In August 2012, astronomers at Copenhagen University
Copenhagen University
reported the detection of a specific sugar molecule, glycolaldehyde, in a distant star system. The molecule was found around the protostellar binary IRAS 16293-2422, which is located 400 light years from Earth.[19][20] Glycolaldehyde
Glycolaldehyde
is needed to form ribonucleic acid, or RNA, which is similar in function to DNA. This finding suggests that complex organic molecules may form in stellar systems prior to the formation of planets, eventually arriving on young planets early in their formation.[21] In September 2012, NASA
NASA
scientists reported that PAHs, subjected to interstellar medium (ISM) conditions, are transformed, through hydrogenation, oxygenation, and hydroxylation, to more complex organics — "a step along the path toward amino acids and nucleotides, the raw materials of proteins and DNA, respectively".[22][23] Further, as a result of these transformations, the PAHs lose their spectroscopic signature which could be one of the reasons "for the lack of PAH detection in interstellar ice grains, particularly the outer regions of cold, dense clouds or the upper molecular layers of protoplanetary disks."[22][23] PAHs are found everywhere in deep space[24] and, in June 2013, PAHs were detected in the upper atmosphere of Titan, the largest moon of the planet Saturn.[25] In 2013, Dwayne Heard at the University of Leeds suggested[26] that quantum mechanical tunneling could explain a reaction his group observed taking place, at a significantly higher than expected rate, between cold (around 63 kelvins) hydroxyl and methanol molecules, apparently bypassing intramolecular energy barriers which would have to be overcome by thermal energy or ionization events for the same rate to exist at warmer temperatures. The proposed tunneling mechanism may help explain the common observation of fairly complex molecules (up to tens of atoms) in interstellar space. A particularly large and rich region for detecting interstellar molecules is Sagittarius B2 (Sgr B2). This giant molecular cloud lies near the center of the Milky Way
Milky Way
galaxy and is a frequent target for new searches. About half of the molecules listed below were first found near Sgr B2, and nearly every other molecule has since been detected in this feature.[27] A rich source of investigation for circumstellar molecules is the relatively nearby star CW Leonis
CW Leonis
(IRC +10216), where about 50 compounds have been identified.[28] In March 2015, NASA
NASA
scientists reported that, for the first time, complex DNA
DNA
and RNA
RNA
organic compounds of life, including uracil, cytosine and thymine, have been formed in the laboratory under outer space conditions, using starting chemicals, such as pyrimidine, found in meteorites. Pyrimidine, like polycyclic aromatic hydrocarbons (PAHs), the most carbon-rich chemical found in the Universe, may have been formed in red giants or in interstellar dust and gas clouds, according to the scientists.[29] In October 2016, astronomers reported that the very basic chemical ingredients of life—the carbon-hydrogen molecule (CH•, or methylidyne radical), the carbon-hydrogen positive ion (CH+ cation) and the carbon ion (C+ cation)—are the result, in large part, of ultraviolet light from stars, rather than in other ways, such as the result of turbulent events related to supernovae and young stars, as thought earlier.[30][31] Theoretical models[edit] To explain the observed ratios of isomeric compounds, the minimum energy principle has been used. In the majority of cases, it explains that some organic entities have greater abundance than their isomers due to the lower total energies of the first one. However, a few exceptions where the principle fails are also known.[32] Another approach ignores energy and deals only with the molecular complexity estimated by the information entropy index. It speculates that the points of several natural compounds (urea, pyrimidine, dihydroxyacetone, uracil, cytosine, glycine, and alanine) fall into the range of the values typical for the known interstellar molecules that indicates high probability of their detection in interstellar environment. Additionally the molecules with maximal information entropy, i.e. the most complex compounds, make up approximately a half of the interstellar set and their percentage is decreased with the size. This trend may be associated with the different stabilities of the molecules with uniform (usually more stable) and diversified (usually less stable) chemical structures, so the detectable molecules with a large size must possess symmetric structure more probably than non-symmetric. The remarkable detection of low-entropy (highly symmetric) fullerene molecules supports this assumption. It is also noted that information entropy reflects the depth of hydrogenation of interstellar entities: the molecules with maximal information entropy are hydrogen-poor whereas the others are mainly hydrogen-rich.[33] Molecules[edit] The following tables list molecules that have been detected in the interstellar medium, grouped by the number of component atoms. If there is no entry in the molecule column, only the ionized form has been detected. For molecules where no designation was given in the scientific literature, that field is left empty. Mass is given in atomic mass units. The total number of unique species, including distinct ionization states, is listed in parentheses in each section header. Most of the molecules detected so far are organic. Only one inorganic species has been observed in molecules which contain at least five atoms, SiH4.[34] Larger molecules have so far all had at least one carbon atom, with no N−N or O−O bonds.[34]

Carbon monoxide
Carbon monoxide
is frequently used to trace the distribution of mass in molecular clouds.[35]

Diatomic (43)[edit]

Molecule Designation Mass Ions

AlCl Aluminium monochloride[36][37] 62.5 —

AlF Aluminium monofluoride[36][38] 46 —

AlO Aluminium monoxide[39] 43 —

— Argonium[40][41] 41 ArH+

C2 Diatomic carbon[42][43] 24 —

— Fluoromethylidynium 31 CF+[44]

CH Methylidyne radical[30][45] 13 CH+[46]

CN Cyanogen
Cyanogen
radical[36][45][47][48] 26 CN+,[49] CN−[50]

CO Carbon
Carbon
monoxide[36][51][52] 28 CO+[53]

CP Carbon
Carbon
monophosphide[48] 43 —

CS Carbon
Carbon
monosulfide[36] 44 —

FeO Iron(II) oxide[54] 82 —

H2 Molecular hydrogen[55] 2 —

HCl Hydrogen
Hydrogen
chloride[56] 36.5 HCl+[57]

HF Hydrogen
Hydrogen
fluoride[58] 20 —

HO Hydroxyl radical[36] 17 OH+[59]

KCl Potassium chloride[36][37] 75.5 —

NH Nitrogen
Nitrogen
monohydride[60][61] 15 —

N2 Molecular nitrogen[62][63] 28 —

NO Nitric oxide[64] 30 NO+[49]

NS Nitrogen
Nitrogen
sulfide[36] 46 —

NaCl Sodium chloride[36][37] 58.5 —

— Magnesium monohydride cation 25.3 MgH+[49]

NaI Sodium iodide[65] 150 —

O2 Molecular oxygen[66] 32 —

PN Phosphorus mononitride[67] 45 —

PO Phosphorus monoxide[68] 47 —

SH Sulfur monohydride[69] 33 SH+[70]

SO Sulfur monoxide[36] 48 SO+[46]

SiC Carborundum[36][71] 40 —

SiN Silicon mononitride[36] 42 —

SiO Silicon monoxide[36] 44 —

SiS Silicon monosulfide[36] 60 —

TiO Titanium oxide[72] 63.9 —

The H+ 3 cation is one of the most abundant ions in the universe. It was first detected in 1993.[73][74]

Triatomic (41)[edit]

Molecule Designation Mass Ions

AlNC Aluminium isocyanide[36] 53 —

AlOH Aluminium hydroxide[75] 44 —

C3 Tricarbon[43] 36 —

C2H Ethynyl radical[36][47] 25 —

CCN Cyanomethylidyne[76] 38 —

C2O Dicarbon monoxide[77] 40 —

C2S Thioxoethenylidene[78] 56 —

C2P —[79] 55 —

CO2 Carbon
Carbon
dioxide[80] 44 —

FeCN Iron cyanide[81] 82 —

— Protonated molecular hydrogen 3 H+ 3[73][74]

H2C Methylene radical[82] 14 —

— Chloronium 37.5 H2Cl+[83]

H2O Water[84] 18 H2O+[85]

HO2 Hydroperoxyl[86] 33 —

H2S Hydrogen
Hydrogen
sulfide[36] 34 —

HCN Hydrogen
Hydrogen
cyanide[36][47][87] 27 —

HNC Hydrogen
Hydrogen
isocyanide[88][89] 27 —

HCO Formyl
Formyl
radical[90] 29 HCO+[46][90][91]

HCP Phosphaethyne[92] 44 —

HCS Thioformyl[93] 45 HCS+[46][91]

— Diazenylium[91][46][94] 29 HN+ 2

HNO Nitroxyl[95] 31 —

— Isoformyl 29 HOC+[47]

HSC Isothioformyl[93] 45 —

KCN Potassium cyanide[36] 65 —

MgCN Magnesium cyanide[36] 50 —

MgNC Magnesium isocyanide[36] 50 —

NH2 Amino
Amino
radical[96] 16 —

N2O Nitrous oxide[97] 44 —

NaCN Sodium cyanide[36] 49 —

NaOH Sodium hydroxide[98] 40 —

OCS Carbonyl sulfide[99] 60 —

O3 Ozone[100] 48 —

SO2 Sulfur dioxide[36][101] 64 —

c-SiC2 c-Silicon dicarbide[36][71] 52 —

SiCSi Disilicon carbide[102] 68 —

SiCN Silicon carbonitride[103] 54 —

SiNC [104] 54 —

TiO2 Titanium dioxide[72] 79.9 —

Formaldehyde
Formaldehyde
is an organic molecule that is widely distributed in the interstellar medium.[105]

Four atoms (27)[edit]

Molecule Designation Mass Ions

CH3 Methyl radical[106] 15 —

l-C3H Propynylidyne[36][107] 37 l-C3H+[108]

c-C3H Cyclopropynylidyne[109] 37 —

C3N Cyanoethynyl[110] 50 C3N−[111]

C3O Tricarbon
Tricarbon
monoxide[107] 52 —

C3S Tricarbon
Tricarbon
sulfide[36][78] 68 —

— Hydronium 19 H3O+[112]

C2H2 Acetylene[113] 26 —

H2CN Methylene amidogen[114] 28 H2CN+[46]

H2CO Formaldehyde[105] 30 —

H2CS Thioformaldehyde[115] 46 —

HCCN —[116] 39 —

HCCO Ketenyl[117] 41 —

— Protonated hydrogen cyanide 28 HCNH+[91]

— Protonated carbon dioxide 45 HOCO+[118]

HCNO Fulminic acid[119] 43 —

HOCN Cyanic acid[120] 43 —

HOOH Hydrogen
Hydrogen
peroxide[121] 34 —

HNCO Isocyanic acid[101] 43 —

HNCS Isothiocyanic acid[122] 59 —

NH3 Ammonia[36][123] 17 —

HSCN Thiocyanic acid[124] 59 —

SiC3 Silicon tricarbide[36]  64 —

HMgNC Hydromagnesium isocyanide[125]  51.3 —

Methane, the primary component of natural gas, has also been detected on comets and in the atmosphere of several planets in the Solar System.[126]

Five atoms (19)[edit]

Molecule Designation Mass Ions

Ammonium
Ammonium
ion[127][128]  18 NH+ 4

CH4 Methane[129] 16 —

CH3O Methoxy
Methoxy
radical[130] 31 —

c-C3H2 Cyclopropenylidene[47][131][132] 38 —

l-H2C3 Propadienylidene[132] 38 —

H2CCN Cyanomethyl[133] 40 —

H2C2O Ketene[101] 42 —

H2CNH Methylenimine[134] 29 —

HNCNH Carbodiimide[135] 42 —

— Protonated formaldehyde 31 H2COH+[136]

C4H Butadiynyl[36] 49 C4H−[137]

HC3N Cyanoacetylene[36][47][91][138][139] 51 —

HCC-NC Isocyanoacetylene[140] 51 —

HCOOH Formic acid[141][138] 46 —

NH2CN Cyanamide[142] 42 —

— Protonated cyanogen 53 NCCNH+[143]

HC(O)CN Cyanoformaldehyde[144] 55 —

SiC4 Silicon-carbide cluster[71] 92 —

SiH4 Silane[145] 32 —

In the ISM, formamide (above) can combine with methylene to form acetamide.[146]

Six atoms (16)[edit]

Molecule Designation Mass Ions

c-H2C3O Cyclopropenone[147] 54 —

E-HNCHCN E-Cyanomethanimine[148] 54 —

C2H4 Ethylene[149] 28 —

CH3CN Acetonitrile[101][150][151] 40 —

CH3NC Methyl isocyanide[150] 40 —

CH3OH Methanol[101][152] 32 —

CH3SH Methanethiol[153] 48 —

l-H2C4 Diacetylene[36][154] 50 —

— Protonated cyanoacetylene 52 HC3NH+[91]

HCONH2 Formamide[146] 44 —

C5H Pentynylidyne[36][78] 61 —

C5N Cyanobutadiynyl radical[155] 74 —

HC2CHO Propynal[156] 54 —

HC4N —[36]  63 —

CH2CNH Ketenimine[131] 40 —

C5S —[157] 92 —

Acetaldehyde
Acetaldehyde
(above) and its isomers vinyl alcohol and ethylene oxide have all been detected in interstellar space.[158]

Seven atoms (11)[edit]

Molecule Designation Mass Ions

c-C2H4O Ethylene
Ethylene
oxide[159] 44 —

CH3C2H Methylacetylene[47] 40 —

H3CNH2 Methylamine[160] 31 —

CH2CHCN Acrylonitrile[101][150] 53 —

H2CHCOH Vinyl alcohol[158] 44 —

C6H Hexatriynyl radical[36][78] 73 C6H−[132][161]

HC4CN Cyanodiacetylene[101][139][150] 75 —

HC5O —[162] 77 —

CH3CHO Acetaldehyde[36][159] 44 —

CH3NCO Methyl isocyanate[163] 57 —

The radio signature of acetic acid, a compound found in vinegar, was confirmed in 1997.[164]

Eight atoms (11)[edit]

Molecule Designation Mass

H3CC2CN Methylcyanoacetylene[165] 65

H2COHCHO Glycolaldehyde[166] 60

HCOOCH3 Methyl formate[101][138][166] 60

CH3COOH Acetic acid[164] 60

H2C6 Hexapentaenylidene[36][154] 74

CH2CHCHO Propenal[131] 56

CH2CCHCN Cyanoallene[131][165] 65

CH3CHNH Ethanimine[167] 43

C7H Heptatrienyl radical[168] 85

NH2CH2CN Aminoacetonitrile[169] 56

(NH2)2CO Urea[170] 60

Nine atoms (10)[edit]

Molecule Designation Mass Ions

CH3C4H Methyldiacetylene[171] 64 —

CH3OCH3 Dimethyl Ether[172] 46 —

CH3CH2CN Propionitrile[36][101][150] 55 —

CH3CONH2 Acetamide[131][146] 59 —

CH3CH2OH Ethanol[173] 46 —

C8H Octatetraynyl radical[174] 97 C8H−[175][176]

HC7N Cyanohexatriyne or Cyanotriacetylene[36][123][177][178] 99 —

CH3CHCH2 Propylene
Propylene
(propene)[179] 42 —

CH3CH2SH Ethyl mercaptan[180] 62 —

A number of polyyne-derived chemicals are among the heaviest molecules found in the interstellar medium.

Ten or more atoms (17)[edit]

Atoms Molecule Designation Mass Ions

10 (CH3)2CO Acetone[101][181] 58 —

10 (CH2OH)2 Ethylene
Ethylene
glycol[182][183] 62 —

10 CH3CH2CHO Propanal[131] 58 —

10 CH3OCH2OH Methoxymethanol[184] 62 —

10 CH3C5N Methyl-cyano-diacetylene[131] 89 —

10 CH3CHCH2O Propylene
Propylene
oxide[185] 58 —

11 HC8CN Cyanotetra-acetylene[36][177] 123 —

11 C2H5OCHO Ethyl formate[186] 74 —

11 CH3COOCH3 Methyl acetate[187] 74 —

11 CH3C6H Methyltriacetylene[131][171] 88 —

12 C6H6 Benzene[154] 78 —

12 C3H7CN n-Propyl cyanide[186] 69 —

12 (CH3)2CHCN iso-Propyl cyanide[188][189] 69 —

13 C 6H 5CN Benzonitrile[190] 104 —

13 HC10CN Cyanopentaacetylene[177] 147 —

60 C60 Buckminsterfullerene (C60 fullerene)[191] 720 C+ 60[192][193]

70 C70 C70 fullerene[191] 840 —

Deuterated molecules (20)[edit] These molecules all contain one or more deuterium atoms, a heavier isotope of hydrogen.

Atoms Molecule Designation

2 HD Hydrogen
Hydrogen
deuteride[194][195]

3 H2D+, HD+ 2 Trihydrogen cation[194][195]

3 HDO, D2O Heavy water[196][197]

3 DCN Hydrogen
Hydrogen
cyanide[198]

3 DCO Formyl
Formyl
radical[198]

3 DNC Hydrogen
Hydrogen
isocyanide[198]

3 N2D+ —[198] 

4 NH2D, NHD2, ND3 Ammonia[195][199][200]

4 HDCO, D2CO Formaldehyde[195][201]

4 DNCO Isocyanic acid[202]

5 NH3D+ Ammonium
Ammonium
ion[203][204]

6 NH 2CDO; NHDCHO Formamide[202]

7 CH2DCCH, CH3CCD Methylacetylene[205][206]

Unconfirmed (13)[edit] Evidence for the existence of the following molecules has been reported in scientific literature, but the detections are either described as tentative by the authors, or have been challenged by other researchers. They await independent confirmation.

Atoms Molecule Designation

2 SiH Silylidine[88]

4 PH3 Phosphine[207]

4 MgCCH Magnesium monoacetylide[157]

4 NCCP Cyanophosphaethyne[157]

5 C5 Linear C5[43]

5 H2NCO+ —[208]

4 SiH3CN Silyl cyanide[157]

10 H2NH2CCOOH Glycine[209][210]

12 CO(CH2OH)2 Dihydroxyacetone[211]

12 C2H5OCH3 Ethyl methyl ether[212]

18 C 10H+ 8 Naphthalene
Naphthalene
cation[213]

24 C24 Graphene[214]

24 C14H10 Anthracene[10][215]

26 C16H10 Pyrene[10]

See also[edit]

Abiogenesis Astrobiology Astrochemistry Atomic and molecular astrophysics Cosmic dust Cosmic ray Cosmochemistry Diffuse interstellar band Extraterrestrial liquid water Forbidden mechanism Intergalactic dust Interplanetary medium Interstellar medium Lists of molecules Organic compound Outer space Panspermia Polycyclic aromatic hydrocarbon
Polycyclic aromatic hydrocarbon
(PAH) Spectroscopy Tholin

References[edit]

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External links[edit]

Woon, David E. (October 1, 2010). "Interstellar and Circumstellar Molecules". Retrieved 2010-10-04.  "Molecules in Space". Universität zu Köln. August 2010. Retrieved 2010-10-04.  Dworkin, Jason P. (February 1, 2007). "Interstellar Molecules". NASA's Cosmic Ice Lab. Retrieved 2010-12-23.  Wootten, Al (November 2005). "The 129 reported interstellar and circumstellar molecules". National Radio
Radio
Astronomy Observatory. Retrieved 2007-02-13.  Lovas, F. J.; Dragoset, R. A. (February 2004). "NIST Recommended Rest Frequencies for Observed Interstellar Molecular Microwave
Microwave
Transitions, 2002 Revision". National Institute of Standards and Technology. Retrieved 2007-02-13. 

v t e

Molecules detected in outer space

Molecules

Diatomic

Aluminium monochloride Aluminium monofluoride Aluminium monoxide Argonium Carbon
Carbon
monophosphide Carbon
Carbon
monosulfide Carbon
Carbon
monoxide Carborundum Cyanogen
Cyanogen
radical Diatomic carbon Fluoromethylidynium Hydrogen
Hydrogen
chloride Hydrogen
Hydrogen
fluoride Hydrogen
Hydrogen
(molecular) Hydroxyl radical Iron(II) oxide Magnesium monohydride cation Methylidyne radical Nitric oxide Nitrogen
Nitrogen
(molecular) Nitrogen
Nitrogen
monohydride Nitrogen
Nitrogen
sulfide Oxygen
Oxygen
(molecular) Phosphorus monoxide Phosphorus mononitride Potassium chloride Silicon carbide Silicon mononitride Silicon monoxide Silicon monosulfide Sodium chloride Sodium iodide Sulfur monohydride Sulfur monoxide Titanium oxide

Triatomic

Aluminium hydroxide Aluminium isocyanide Amino
Amino
radical Carbon
Carbon
dioxide Carbonyl sulfide CCP radical Chloronium Diazenylium Dicarbon monoxide Disilicon carbide Ethynyl radical Formyl
Formyl
radical Hydrogen
Hydrogen
cyanide (HCN) Hydrogen
Hydrogen
isocyanide (HNC) Hydrogen
Hydrogen
sulfide Hydroperoxyl Iron cyanide Isoformyl Magnesium cyanide Magnesium isocyanide Methylene radical N2H+ Nitrous oxide Nitroxyl Ozone Phosphaethyne Potassium cyanide Protonated molecular hydrogen Sodium cyanide Sodium hydroxide Silicon carbonitride c-Silicon dicarbide Silicon naphthalocyanine Sulfur dioxide Thioformyl Thioxoethenylidene Titanium dioxide Tricarbon Water

Four atoms

Acetylene Ammonia Cyanic acid Cyanoethynyl Cyclopropynylidyne Formaldehyde Fulminic acid HCCN Hydrogen
Hydrogen
peroxide Hydromagnesium isocyanide Isocyanic acid Isothiocyanic acid Ketenyl Methylene amidogen Methyl radical Propynylidyne Protonated carbon dioxide Protonated hydrogen cyanide Silicon tricarbide Thioformaldehyde Tricarbon
Tricarbon
monoxide Tricarbon
Tricarbon
sulfide Thiocyanic acid

Five atoms

Ammonium
Ammonium
ion Butadiynyl Carbodiimide Cyanamide Cyanoacetylene Cyanoformaldehyde Cyanomethyl Cyclopropenylidene Formic acid Isocyanoacetylene Ketene Methane Methoxy
Methoxy
radical Methylenimine Propadienylidene Protonated formaldehyde Protonated formaldehyde Silane Silicon-carbide cluster

Six atoms

Acetonitrile Cyanobutadiynyl radical E-Cyanomethanimine Cyclopropenone Diacetylene Ethylene Formamide HC4N Ketenimine Methanethiol Methanol Methyl isocyanide Pentynylidyne Propynal Protonated cyanoacetylene

Seven atoms

Acetaldehyde Acrylonitrile

Vinyl cyanide

Cyanodiacetylene Ethylene
Ethylene
oxide Hexatriynyl radical Methylacetylene Methylamine Methyl isocyanate Vinyl alcohol

Eight atoms

Acetic acid Aminoacetonitrile Cyanoallene Ethanimine Glycolaldehyde Heptatrienyl radical Hexapentaenylidene Methylcyanoacetylene Methyl formate Propenal

Nine atoms

Acetamide Cyanohexatriyne Cyanotriacetylene Dimethyl ether Ethanol Methyldiacetylene Octatetraynyl radical Propene Propionitrile

Ten atoms or more

Acetone Benzene Benzonitrile Buckminsterfullerene
Buckminsterfullerene
(C60 fullerene, buckyball) C70 fullerene Cyanodecapentayne Cyanopentaacetylene Cyanotetra-acetylene Ethylene
Ethylene
glycol Ethyl formate Methyl acetate Methyl-cyano-diacetylene Methyltriacetylene Propanal n-Propyl cyanide Pyrimidine

Deuterated molecules

Ammonia Ammonium
Ammonium
ion Formaldehyde Formyl
Formyl
radical Heavy water Hydrogen
Hydrogen
cyanide Hydrogen
Hydrogen
deuteride Hydrogen
Hydrogen
isocyanide Methylacetylene N2D+ Trihydrogen cation

Unconfirmed

Anthracene Dihydroxyacetone Ethyl methyl ether Glycine Graphene H2NCO+ Linear C5 Naphthalene
Naphthalene
cation Phosphine Pyrene Silylidine

Related

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Polycyclic aromatic hydrocarbon
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