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List of interstellar and circumstellar molecules

January 01, 1970

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.

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

Background edit

 
Idealised example of the rotational spectrum (bottom) produced by transitions between different rotational energy levels (top) of a simple linear molecule.   is the rotational constant of the molecule,   is the rotational quantum number,   is the upper level and   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: e.g. 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] 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 edit

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 atomic mass units. 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]

 
Carbon monoxide is frequently used to trace the distribution of mass in molecular clouds.[15]

Diatomic (43) edit

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 25.3 MgH+[29]
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 —
SiS Silicon monosulfide[34] 60 —
TiO Titanium(II) oxide[55] 63.9 —
 
The H+
3 cation is one of the most abundant ions in the universe. It was first detected in 1993.[56][57]

Triatomic (44) edit

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

Four atoms (30) edit

Molecule Designation Mass Ions
CH3 Methyl radical[92] 15 CH+3[93]
l-C3H Propynylidyne[94] 37 l-C3H+[95]
c-C3H Cyclopropynylidyne[96] 37 —
C3N Cyanoethynyl[97] 50 C3N−[98]
C3O Tricarbon monoxide[94] 52 —
C3S Tricarbon sulfide[63] 68 —
— Hydronium 19 H3O+[99]
C2H2 Acetylene[100] 26 —
H2CN Methylene amidogen[101] 28 H2CN+[26]
H2NC Aminocarbyne[102] 28 —
H2CO Formaldehyde[91] 30 —
H2CS Thioformaldehyde[103] 46 —
HCCN —[104] 39 —
HCCO Ketenyl[105] 41 —
— Protonated hydrogen cyanide 28 HCNH+[77]
— Protonated carbon dioxide 45 HOCO+[106]
HCNO Fulminic acid[107] 43 —
HOCN Cyanic acid[108] 43 —
CNCN Isocyanogen[109] 52 —
HOOH Hydrogen peroxide[110] 34 —
HNCO Isocyanic acid[87] 43 —
HNCN Cyanomidyl radical[111] 41 —
HNCS Isothiocyanic acid[112] 59 —
NH3 Ammonia[113] 17 —
HSCN Thiocyanic acid[114] 59 —
SiC3 Silicon tricarbide[34]  64 —
HMgNC Hydromagnesium isocyanide[115]  51.3 —
HNO2 Nitrous acid[116] 47 —
 
Methane, the primary component of natural gas, has also been detected on comets and in the atmosphere of several planets in the Solar System.[117]

Five atoms (20) edit

Molecule Designation Mass Ions
— Ammonium ion 18 NH+
4[118][119]
CH4 Methane[120] 16 —
CH3O Methoxy radical[121] 31 —
c-C3H2 Cyclopropenylidene[27][122][123] 38 —
l-H2C3 Propadienylidene[123] 38 —
H2CCN Cyanomethyl[124] 40 —
H2C2O Ketene[87] 42 —
H2CNH Methylenimine[125] 29 —
HNCNH Carbodiimide[126] 42 —
— Protonated formaldehyde 31 H2COH+[127]
C4H Butadiynyl[34] 49 C4H−[128]
HC3N Cyanoacetylene[27][77][129][130] 51 —
HCC-NC Isocyanoacetylene[131] 51 —
HCOOH Formic acid[132][129] 46 —
NH2CN Cyanamide[133][134] 42 —
NH2OH Hydroxylamine[135] 37 —
— Protonated cyanogen 53 NCCNH+[136]
HC(O)CN Cyanoformaldehyde[137] 55 —
C5 Linear C5[138] 60 —
SiC4 Silicon-carbide cluster[53] 92 —
SiH4 Silane[139] 32 —
 
In the ISM, formamide (above) can combine with methylene to form acetamide.[140]

Six atoms (16) edit

Molecule Designation Mass Ions
c-H2C3O Cyclopropenone[141] 54 —
E-HNCHCN E-Cyanomethanimine[142] 54 —
C2H4 Ethylene[143] 28 —
CH3CN Acetonitrile[87][144][145] 40 —
CH3NC Methyl isocyanide[144] 40 —
CH3OH Methanol[87][146] 32 —
CH3SH Methanethiol[147] 48 —
l-H2C4 Diacetylene[148] 50 —
— Protonated cyanoacetylene 52 HC3NH+[77]
HCONH2 Formamide[140] 44 —
HOCOOH Carbonic acid[149] —
C5H Pentynylidyne[63] 61 —
C5N Cyanobutadiynyl radical[150] 74 —
HC2CHO Propynal[151] 54 —
HC4N —[34]  63 —
CH2CNH Ketenimine[122] 40 —
C5S —[152] 92 —
 
Acetaldehyde (above) and its isomers vinyl alcohol and ethylene oxide have all been detected in interstellar space.[153]

Seven atoms (13) edit

Molecule Designation Mass Ions
c-C2H4O Ethylene oxide[154] 44 —
CH3C2H Methylacetylene[27] 40 —
H3CNH2 Methylamine[155] 31 —
CH2CHCN Acrylonitrile[87][144] 53 —
HCCCHNH Propargylimine[156] 53 —
H2CHCOH Vinyl alcohol[153] 44 —
C6H Hexatriynyl radical[63] 73 C6H−[123][157]
HC4CN Cyanodiacetylene[87][130][144] 75 —
HC4NC Isocyanodiacetylene[158] 75 —
HC5O —[159] 77 —
CH3CHO Acetaldehyde[154] 44 —
CH3NCO Methyl isocyanate[160] 57 —
HOCH2CN Glycolonitrile[161] 57 —
 
The radio signature of acetic acid, a compound found in vinegar, was confirmed in 1997.[162]

Eight atoms (14) edit

Molecule Designation Mass
H3CC2CN Methylcyanoacetylene[163] 65
HC3H2CN Propargyl cyanide[164] 65
H2COHCHO Glycolaldehyde[165] 60
(CHOH)2 1,2-ethenediol[166] 60
HCOOCH3 Methyl formate[87][129] 60
CH3COOH Acetic acid[162] 60
H2C6 Hexapentaenylidene[148] 74
CH2CHCHO Propenal[122] 56
CH2CCHCN Cyanoallene[122][163] 65
CH3CHNH Ethanimine[167] 43
C2H3NH2 Vinylamine[168] 43
C7H Heptatrienyl radical[169] 85
NH2CH2CN Aminoacetonitrile[170] 56
(NH2)2CO Urea[171] 60

Nine atoms (10) edit

Molecule Designation Mass Ions
CH3C4H Methyldiacetylene[172] 64 —
CH3OCH3 Dimethyl ether[173] 46 —
CH3CH2CN Propionitrile[87][144] 55 —
CH3CONH2 Acetamide[122][140][134] 59 —
CH3CH2OH Ethanol[174] 46 —
C8H Octatetraynyl radical[175] 97 C8H−[176][177]
HC7N Cyanohexatriyne or Cyanotriacetylene[113][178][179] 99 —
CH3CHCH2 Propylene (propene)[180] 42 —
CH3CH2SH Ethyl mercaptan[181] 62 —
CH3NHCHO N-methylformamide[134]
 
 
 
A number of polyyne-derived chemicals are among the heaviest molecules found in the interstellar medium.

Ten or more atoms (22) edit

Atoms Molecule Designation Mass Ions
10 (CH3)2CO Acetone[87][182] 58 —
10 (CH2OH)2 Ethylene glycol[183][184] 62 —
10 CH3CH2CHO Propanal[122] 58 —
10 CH3OCH2OH Methoxymethanol[185] 62 —
10 CH3C5N Methylcyanodiacetylene[122] 89 —
10 CH3CHCH2O Propylene oxide[186] 58 —
11 NH2CH2CH2OH Ethanolamine[187] 61 —
11 HC8CN Cyanotetraacetylene[178] 123 —
11 C2H5OCHO Ethyl formate[188] 74 —
11 CH3COOCH3 Methyl acetate[189] 74 —
11 CH3C6H Methyltriacetylene[122][172] 88 —
12 C6H6 Benzene[148] 78 —
12 C3H7CN n-Propyl cyanide[188] 69 —
12 (CH3)2CHCN iso-Propyl cyanide[190][191] 69 —
13 CH3OCH2CH2OH 2-methoxyethanol[192] 76 —
13 C
6H
5CN		 Benzonitrile[193] 104 —
13 HC10CN Cyanopentaacetylene[178] 147 —
17 C9H8 Indene[9] 116 —
19 C10H7CN 1-cyanonaphthalene[8] 153 —
19 C10H7CN 2-cyanonaphthalene[8] 153 —
27 C11H12N2O2 Tryptophan[194] —
60 C60 Buckminsterfullerene
(C60 fullerene)[195]		 720 C+
60[196][197][198]
70 C70 C70 fullerene[195] 840 —

Deuterated molecules (22) edit

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

Atoms Molecule Designation
2 HD Hydrogen deuteride[199][200]
3 H2D+, HD+
2		 Trihydrogen cation[199][200]
3 HDO, D2O Heavy water[201][202]
3 DCN Hydrogen cyanide[203]
3 DCO Formyl radical[203]
3 DNC Hydrogen isocyanide[203]
3 N2D+ —[203] 
3 NHD, ND2 Amidogen[204] 
4 NH2D, NHD2, ND3 Ammonia[200][205][206]
4 HDCO, D2CO Formaldehyde[200][207]
4 DNCO Isocyanic acid[208]
5 NH3D+ Ammonium ion[209][210]
6 NH
2CDO; NHDCHO		 Formamide[208]
7 CH2DCCH, CH3CCD Methylacetylene[211][212]

Unconfirmed (13) edit

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[74]
4 PH3 Phosphine[213]
4 MgCCH Magnesium monoacetylide[152]
4 NCCP Cyanophosphaethyne[152]
5 H2NCO+ —[214]
6 SiH3CN Silyl cyanide[152]
10 H2NCH2COOH Glycine[215][216]
10 C2H5NH2 Ethylamine[168]
12 CO(CH2OH)2 Dihydroxyacetone[217][218]
12 C2H5OCH3 Ethyl methyl ether[219]
18 C
10H+
8		 Naphthalene cation[220]
24 C24 Graphene[221]
24 C14H10 Anthracene[222][223]
26 C16H10 Pyrene[222]

See also edit

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January 01, 1970
list, interstellar, circumstellar, molecules, this, list, molecules, that, have, been, detected, interstellar, medium, circumstellar, envelopes, grouped, number, component, atoms, chemical, formula, listed, each, detected, compound, along, with, ionized, form,. 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 Infrared spectrum of HH 46 47 image in inset with vibrational bands of several molecules labelled in colour Contents 1 Background 2 Molecules 2 1 Diatomic 43 2 2 Triatomic 44 2 3 Four atoms 30 2 4 Five atoms 20 2 5 Six atoms 16 2 6 Seven atoms 13 2 7 Eight atoms 14 2 8 Nine atoms 10 2 9 Ten or more atoms 22 3 Deuterated molecules 22 4 Unconfirmed 13 5 See also 6 References 7 Notes 8 External linksBackground edit nbsp Idealised example of the rotational spectrum bottom produced by transitions between different rotational energy levels top of a simple linear molecule B displaystyle B nbsp is the rotational constant of the molecule J displaystyle J nbsp is the rotational quantum number J displaystyle J nbsp is the upper level and J displaystyle J nbsp 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 e g 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 nbsp 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 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 editThe 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 atomic mass units 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 nbsp Carbon monoxide is frequently used to trace the distribution of mass in molecular clouds 15 Diatomic 43 edit 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 25 3 MgH 29 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 SiS Silicon monosulfide 34 60 TiO Titanium II oxide 55 63 9 nbsp The H 3 cation is one of the most abundant ions in the universe It was first detected in 1993 56 57 Triatomic 44 edit Molecule Designation Mass Ions AlNC Aluminium isocyanide 34 53 AlOH Aluminium hydroxide 58 44 C3 Tricarbon 59 60 36 C2H Ethynyl radical 27 25 CCN Cyanomethylidyne 61 38 C2O Dicarbon monoxide 62 40 C2S Thioxoethenylidene 63 56 C2P 64 55 CO2 Carbon dioxide 65 44 CaNC Calcium isocyanide 66 92 FeCN Iron cyanide 67 82 Protonated molecular hydrogen 3 H 3 56 57 H2C Methylene radical 68 14 Chloronium 37 5 H2Cl 69 H2O Water 70 18 H2O 71 HO2 Hydroperoxyl 72 33 H2S Hydrogen sulfide 34 34 HCN Hydrogen cyanide 27 73 27 HNC Hydrogen isocyanide 74 75 27 HCO Formyl radical 76 29 HCO 26 76 77 HCP Phosphaethyne 78 44 HCS Thioformyl 79 45 HCS 26 77 Diazenylium 77 26 80 29 HN 2 HNO Nitroxyl 81 31 Isoformyl 29 HOC 27 HSC Isothioformyl 79 45 KCN Potassium cyanide 34 65 MgCN Magnesium cyanide 34 50 MgNC Magnesium isocyanide 34 50 NH2 Amino radical 82 16 N2O Nitrous oxide 83 44 NaCN Sodium cyanide 34 49 NaOH Sodium hydroxide 84 40 OCS Carbonyl sulfide 85 60 O3 Ozone 86 48 SO2 Sulfur dioxide 87 64 c SiC2 c Silicon dicarbide 53 52 SiCSi Disilicon carbide 88 68 SiCN Silicon carbonitride 89 54 SiNC 90 54 TiO2 Titanium dioxide 55 79 9 nbsp Formaldehyde is an organic molecule that is widely distributed in the interstellar medium 91 Four atoms 30 edit Molecule Designation Mass Ions CH3 Methyl radical 92 15 CH 3 93 l C3H Propynylidyne 94 37 l C3H 95 c C3H Cyclopropynylidyne 96 37 C3N Cyanoethynyl 97 50 C3N 98 C3O Tricarbon monoxide 94 52 C3S Tricarbon sulfide 63 68 Hydronium 19 H3O 99 C2H2 Acetylene 100 26 H2CN Methylene amidogen 101 28 H2CN 26 H2NC Aminocarbyne 102 28 H2CO Formaldehyde 91 30 H2CS Thioformaldehyde 103 46 HCCN 104 39 HCCO Ketenyl 105 41 Protonated hydrogen cyanide 28 HCNH 77 Protonated carbon dioxide 45 HOCO 106 HCNO Fulminic acid 107 43 HOCN Cyanic acid 108 43 CNCN Isocyanogen 109 52 HOOH Hydrogen peroxide 110 34 HNCO Isocyanic acid 87 43 HNCN Cyanomidyl radical 111 41 HNCS Isothiocyanic acid 112 59 NH3 Ammonia 113 17 HSCN Thiocyanic acid 114 59 SiC3 Silicon tricarbide 34 64 HMgNC Hydromagnesium isocyanide 115 51 3 HNO2 Nitrous acid 116 47 nbsp Methane the primary component of natural gas has also been detected on comets and in the atmosphere of several planets in the Solar System 117 Five atoms 20 edit Molecule Designation Mass Ions Ammonium ion 18 NH 4 118 119 CH4 Methane 120 16 CH3O Methoxy radical 121 31 c C3H2 Cyclopropenylidene 27 122 123 38 l H2C3 Propadienylidene 123 38 H2CCN Cyanomethyl 124 40 H2C2O Ketene 87 42 H2CNH Methylenimine 125 29 HNCNH Carbodiimide 126 42 Protonated formaldehyde 31 H2COH 127 C4H Butadiynyl 34 49 C4H 128 HC3N Cyanoacetylene 27 77 129 130 51 HCC NC Isocyanoacetylene 131 51 HCOOH Formic acid 132 129 46 NH2CN Cyanamide 133 134 42 NH2OH Hydroxylamine 135 37 Protonated cyanogen 53 NCCNH 136 HC O CN Cyanoformaldehyde 137 55 C5 Linear C5 138 60 SiC4 Silicon carbide cluster 53 92 SiH4 Silane 139 32 nbsp In the ISM formamide above can combine with methylene to form acetamide 140 Six atoms 16 edit Molecule Designation Mass Ions c H2C3O Cyclopropenone 141 54 E HNCHCN E Cyanomethanimine 142 54 C2H4 Ethylene 143 28 CH3CN Acetonitrile 87 144 145 40 CH3NC Methyl isocyanide 144 40 CH3OH Methanol 87 146 32 CH3SH Methanethiol 147 48 l H2C4 Diacetylene 148 50 Protonated cyanoacetylene 52 HC3NH 77 HCONH2 Formamide 140 44 HOCOOH Carbonic acid 149 C5H Pentynylidyne 63 61 C5N Cyanobutadiynyl radical 150 74 HC2CHO Propynal 151 54 HC4N 34 63 CH2CNH Ketenimine 122 40 C5S 152 92 nbsp Acetaldehyde above and its isomers vinyl alcohol and ethylene oxide have all been detected in interstellar space 153 Seven atoms 13 edit Molecule Designation Mass Ions c C2H4O Ethylene oxide 154 44 CH3C2H Methylacetylene 27 40 H3CNH2 Methylamine 155 31 CH2CHCN Acrylonitrile 87 144 53 HCCCHNH Propargylimine 156 53 H2CHCOH Vinyl alcohol 153 44 C6H Hexatriynyl radical 63 73 C6H 123 157 HC4CN Cyanodiacetylene 87 130 144 75 HC4NC Isocyanodiacetylene 158 75 HC5O 159 77 CH3CHO Acetaldehyde 154 44 CH3NCO Methyl isocyanate 160 57 HOCH2CN Glycolonitrile 161 57 nbsp The radio signature of acetic acid a compound found in vinegar was confirmed in 1997 162 Eight atoms 14 edit Molecule Designation Mass H3CC2CN Methylcyanoacetylene 163 65 HC3H2CN Propargyl cyanide 164 65 H2COHCHO Glycolaldehyde 165 60 CHOH 2 1 2 ethenediol 166 60 HCOOCH3 Methyl formate 87 129 60 CH3COOH Acetic acid 162 60 H2C6 Hexapentaenylidene 148 74 CH2CHCHO Propenal 122 56 CH2CCHCN Cyanoallene 122 163 65 CH3CHNH Ethanimine 167 43 C2H3NH2 Vinylamine 168 43 C7H Heptatrienyl radical 169 85 NH2CH2CN Aminoacetonitrile 170 56 NH2 2CO Urea 171 60 Nine atoms 10 edit Molecule Designation Mass Ions CH3C4H Methyldiacetylene 172 64 CH3OCH3 Dimethyl ether 173 46 CH3CH2CN Propionitrile 87 144 55 CH3CONH2 Acetamide 122 140 134 59 CH3CH2OH Ethanol 174 46 C8H Octatetraynyl radical 175 97 C8H 176 177 HC7N Cyanohexatriyne or Cyanotriacetylene 113 178 179 99 CH3CHCH2 Propylene propene 180 42 CH3CH2SH Ethyl mercaptan 181 62 CH3NHCHO N methylformamide 134 nbsp nbsp nbsp A number of polyyne derived chemicals are among the heaviest molecules found in the interstellar medium Ten or more atoms 22 edit Atoms Molecule Designation Mass Ions 10 CH3 2CO Acetone 87 182 58 10 CH2OH 2 Ethylene glycol 183 184 62 10 CH3CH2CHO Propanal 122 58 10 CH3OCH2OH Methoxymethanol 185 62 10 CH3C5N Methylcyanodiacetylene 122 89 10 CH3CHCH2O Propylene oxide 186 58 11 NH2CH2CH2OH Ethanolamine 187 61 11 HC8CN Cyanotetraacetylene 178 123 11 C2H5OCHO Ethyl formate 188 74 11 CH3COOCH3 Methyl acetate 189 74 11 CH3C6H Methyltriacetylene 122 172 88 12 C6H6 Benzene 148 78 12 C3H7CN n Propyl cyanide 188 69 12 CH3 2CHCN iso Propyl cyanide 190 191 69 13 CH3OCH2CH2OH 2 methoxyethanol 192 76 13 C6 H5 CN Benzonitrile 193 104 13 HC10CN Cyanopentaacetylene 178 147 17 C9H8 Indene 9 116 19 C10H7CN 1 cyanonaphthalene 8 153 19 C10H7CN 2 cyanonaphthalene 8 153 27 C11H12N2O2 Tryptophan 194 60 C60 Buckminsterfullerene C60 fullerene 195 720 C 60 196 197 198 70 C70 C70 fullerene 195 840 Deuterated molecules 22 editThese molecules all contain one or more deuterium atoms a heavier isotope of hydrogen Atoms Molecule Designation 2 HD Hydrogen deuteride 199 200 3 H2D HD 2 Trihydrogen cation 199 200 3 HDO D2O Heavy water 201 202 3 DCN Hydrogen cyanide 203 3 DCO Formyl radical 203 3 DNC Hydrogen isocyanide 203 3 N2D 203 3 NHD ND2 Amidogen 204 4 NH2D NHD2 ND3 Ammonia 200 205 206 4 HDCO D2CO Formaldehyde 200 207 4 DNCO Isocyanic acid 208 5 NH3D Ammonium ion 209 210 6 NH2 CDO NHDCHO Formamide 208 7 CH2DCCH CH3CCD Methylacetylene 211 212 Unconfirmed 13 editEvidence 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 74 4 PH3 Phosphine 213 4 MgCCH Magnesium monoacetylide 152 4 NCCP Cyanophosphaethyne 152 5 H2NCO 214 6 SiH3CN Silyl cyanide 152 10 H2NCH2COOH Glycine 215 216 10 C2H5NH2 Ethylamine 168 12 CO CH2OH 2 Dihydroxyacetone 217 218 12 C2H5OCH3 Ethyl methyl ether 219 18 C10 H 8 Naphthalene cation 220 24 C24 Graphene 221 24 C14H10 Anthracene 222 223 26 C16H10 Pyrene 222 See also editAstrochemistry Cosmic dust Diffuse interstellar band Lists of molecules Molecular astrophysics Molecular spectroscopy Molecules in stars Polycyclic aromatic hydrocarbon PAH TholinReferences edit Shu Frank H 1982 The Physical Universe An Introduction to Astronomy University Science Books ISBN 978 0 935702 05 7 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 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