성간 분자와 주변 분자 목록

List of interstellar and circumstellar molecules
HH 46/47의 적외선 스펙트럼(이미지 삽입), 여러 분자의 진동 밴드가 색상으로 표시됨

이것은 성분 원자의 수에 따라 분류된 성간매질과 주위 성간 포락선에서 검출된 분자 목록입니다.화학식은 또한 관찰된 이온화된 형태와 함께 각 검출된 화합물에 대해 나열됩니다.

배경

아래에 나열된 분자들은 천문학적 분광학을 통해 탐지되었습니다.그들의 스펙트럼 특징은 분자들이 두 분자 에너지 준위 사이에서 전이할 때 빛의 광자를 흡수하거나 방출하기 때문에 발생합니다.광자의 에너지(그리고 따라서 파장)는 관련된 수준 간의 에너지 차이와 일치합니다.분자 전자 전이는 분자의 전자 중 하나가 분자 궤도 사이를 이동할 때 발생하며, 전자기 스펙트럼의 자외선, 광학 또는 근적외선 부분에서 스펙트럼 라인을 생성합니다.또는 진동 전이는 분자 결합의 진동으로 양자의 에너지를 전달하여 중적외선 또는 원적외선에서 신호를 생성합니다.기체 분자는 또한 양자화된 회전 수준을 가지며, 마이크로파 또는 무선 파장에서 전이를 일으킵니다.[1]

때때로 전환에는 이러한 에너지 레벨 중 하나 이상이 포함될 수 있습니다. 예를 들어, ro-vibrational spectroscopy는 회전 에너지 레벨과 진동 에너지 레벨을 모두 바꿉니다.때때로2 C(이원자 탄소)의 필립스 밴드에서처럼, 전자 전이가 근적외선에서 선을 생성하고 진동 수준의 동시 변화에 의해 여러 개의 비브로닉 밴드로 분할되어 다시 회전 가지로 분할됩니다.[2]

특정 분자의 스펙트럼은 양자 화학의 선택 규칙과 분자 대칭에 의해 지배됩니다.어떤 분자들은 식별하기 쉬운 단순한 스펙트럼을 가지고 있는 반면, 다른 분자들은 (심지어 작은 분자들도) 많은 다른 선들 사이에 플럭스가 퍼져 있는 극도로 복잡한 스펙트럼을 가지고 있어서 검출하기가 훨씬 더 어렵습니다.[3]원자핵과 전자 사이의 상호작용은 때때로 스펙트럼 선의 초미세 구조를 야기합니다.분자가 여러 개의 동위원소(다른 원자 동위원소를 포함하는 버전)에 존재하는 경우 동위원소 이동으로 스펙트럼이 더욱 복잡해집니다.

새로운 성간 또는 주변부 분자의 탐지는 그것이 존재할 가능성이 있는 적절한 천체를 확인한 다음 필요한 파장, 스펙트럼 해상도 및 민감도에서 작동하는 분광기가 장착된 망원경으로 그것을 관찰해야 합니다.성간매질에서 처음으로 발견된 분자는 1937년 4300 옹스트롬(광학에서)에서 강한 전자 전이를 통해 메틸리딘 라디칼(CH•)이었습니다.[4]천문학 장비의 발전은 새로운 탐지의 수를 증가시켰습니다.1950년대부터 전파천문학이 새로운 탐지를 주도하기 시작했고, 1990년대부터는 서브mm 천문학도 중요해졌습니다.[3]

탐지된 분자의 목록은 탐지하기 쉬운 특정 유형에 매우 치우쳐 있습니다. 예를 들어 전파 천문학은 분자 쌍극자가 높은 작은 선형 분자에 가장 민감합니다.[3]우주에서 가장 일반적인 분자인2 H(분자 수소)는 쌍극자가 없기 때문에 전파망원경에 완전히 보이지 않습니다.[3] H의 전자적 전이는 광학망원경에 비해 너무 에너지가 넘치기 때문에 H를 탐지하기2 위해서는 소리를 내는 로켓을 사용한 자외선 관측이 필요했습니다.[5]진동선은 종종 개별 분자에 특정되지 않으므로 일반적인 부류만 식별할 수 있습니다.예를 들어, 다환 방향족 탄화수소(PAH)의 진동선은 1984년에 확인되었으며,[6] 이는 분자의 종류가 우주에서 매우 흔하다는 것을 보여주었지만,[7] 회전선을 통해 특정 PAH를 확인하는 데는 2021년까지 시간이 걸렸습니다.[8][9]

성간 분자를 탐지하는 가장 풍부한 원천 중 하나는 은하수 중심 근처에 있는 거대 분자 구름인 궁수자리 B2 (Sgr B2)입니다.아래에 나열된 분자의 약 절반은 Sgr B2에서 처음 발견되었고, 다른 많은 분자들은 그 뒤에 그곳에서 발견되었습니다.[10]주변 항성 분자의 풍부한 공급원은 근처에 있는 탄소별인 CW 레오니스(IRC +10216으로도 알려짐)로, 약 50개의 분자가 확인되었습니다.[11]성간매질과 주변매질 사이에 명확한 경계가 없으므로 둘 다 아래 표에 포함됩니다.

천체화학의 학문은 이 분자들이 어떻게 형성되는지 이해하고 그것들의 풍부함을 설명하는 것을 포함합니다.성간매질의 극도로 낮은 밀도는 분자의 형성에 도움이 되지 않으며, 중성 종(원자 또는 분자) 사이의 기존의 기상 반응을 비효율적으로 만듭니다.많은 지역들은 또한 매우 낮은 온도(일반적으로 분자 구름 내부에서 10 켈빈)를 가지고 있어서 반응 속도를 더욱 감소시키거나, 광화학을 통해 분자를 파괴하는 높은 자외선 영역을 가지고 있습니다.[12]관측된 성간 분자의 양을 설명하기 위해서는 가스상 이온 화학(종종 우주선에 의해 구동됨), 우주 먼지에 대한 표면 화학, 성간 소멸을 포함한 복사 전달 및 정교한 반응 네트워크를 사용하여 형성과 파괴 속도 사이의 균형을 계산해야 합니다.[13]분자선을 이용하여 천체의 물리적 성질을 결정하는 것을 분자천체물리학이라고 합니다.

몰레큘스

다음 표는 성간매질이나 주변 물질에서 검출된 분자를 성분 원자의 수로 분류한 것입니다.중성 분자와 분자 이온은 별도의 열에 나열되어 있으며, 분자 열에 항목이 없으면 이온화된 형태만 검출되었습니다.지정(분자의 이름)은 탐지를 설명하는 과학 문헌에 사용되는 지정입니다. 해당 필드가 주어지지 않은 경우에는 해당 필드를 비워 둡니다.질량은 원자 질량 단위로 나열되어 있습니다.적어도 하나의 2중수소(H) 원자를 포함하는 중수소화된 분자는 약간 다른 질량을 가지며 별도의 표에 나열됩니다.각 섹션 헤더에는 구별화 상태를 포함한 고유종의 총 수가 표시됩니다.

지금까지 검출된 대부분의 분자는 유기물질입니다.검출된 5개 이상의 원자를 가진 무기 분자는4 SiH뿐입니다.[14]그보다 더 큰 분자는 모두 N-N 또는 O-O 결합이 없는 적어도 하나의 탄소 원자를 가지고 있습니다.[14]

일산화탄소는 분자 구름의 질량 분포를 추적하는 데 자주 사용됩니다.[15]

규조 (43)

분자 지정 덩어리 이온
AlCl 단염화알루미늄[16][17] 62.5 —
알프 모노플루오라이드 알루미늄[16][18] 46 —
알로 일산화알루미늄[19] 43 —
— 아르고늄[20][21] 37[note 1] ArH+
다2 이원자 탄소[22][23] 24 —
— 플루오로메틸이디늄 31 CF+[24]
CH 메틸리딘 라디칼[25][26] 13 CH+[27]
CN 키아노 라디칼[16][26][28][29] 26 CN+,[30]CN−[31]
CO 일산화탄소[16][32][33] 28 CO+[34]
CP 일인산화탄소[29] 43 —
CS 단황화탄소[16] 44 —
FeO 산화철(II)[35] 82 —
— 수소화 헬륨 이온[36][37] 5 히히+
ㅇ2 분자수소[5] 2 —
HCl 염화수소[38] 36.5 HCl+[39]
HF 불화수소[40] 20 —
HO 하이드록실 라디칼[16] 17 오+[41]
KCl 염화칼륨[16][17] 75.5 —
NH 이미도겐 라디칼[42][43] 15 —
ㄴ2 분자질소[44][45] 28 —
아니요. 산화질소[46] 30 아니오+[30]
NS 황화질소[16] 46 —
NaCl 염화나트륨[16][17] 58.5 —
— 마그네슘 일무수물 양이온 25.3 MgH+[30]
오2 분자산소[47] 32 —
PN 모노나이트라이드인[48][49] 45 —
PO 일산화인[50] 47 —
SH 황일무수물[51] 33 SH+[52]
그렇게 일산화황[16] 48 SO+[27]
SiC 카르보룬덤[16][53] 40 —
SiN –[54] 42 —
SiO 일산화규소[16] 44 —
SiS 단황화규소[16] 60 —
TiO 티타늄()II) 산화물[55] 63.9 —
양이온은+
3 우주에서 가장 풍부한 이온 중 하나입니다.그것은 1993년에 처음으로 발견되었습니다.[56][57]

삼원자 (44)

분자 지정 덩어리 이온
알엔씨 이소시아나이드 알루미늄[16] 53 —
AlOH 수산화알루미늄[58] 44 —
다3 트리카본[59][60] 36 —
C2H 에티닐 라디칼[16][28] 25 —
CCN 시아노메틸리딘[61] 38 —
C2O 일산화탄소[62] 40 —
C2S 티옥소에틸렌[63] 56 —
C2P —[64] 55 —
CO2 이산화탄소[65] 44 —
CaNC 칼슘이소시아니드[66] 92 —
FeCN 시안화철[67] 82 —
— 양성자화된 분자 수소 3 ㅇ+
3[56][57]
H2C 메틸렌 라디칼[68] 14 —
— 클로로늄 37.5 H2Cl+[69]
H2O 물.[70] 18 H2O+[71]
HO2 히드로페록실[72] 33 —
H2S 황화수소[16] 34 —
HCN 시안화수소[16][28][73] 27 —
HNC 이소시아나이드수소[74][75] 27 —
HCO 포밀 라디칼[76] 29 HCO+[27][76][77]
HCP 포스파에틴[78] 44 —
HCS 티오포르밀[79] 45 HCS+[27][77]
— 디아제닐륨[77][27][80] 29 HN+
2
HNO 니트로실[81] 31 —
— 이소포르밀 29 HOC+[28]
HSC 이소티오포르밀[79] 45 —
KCN 시안화칼륨[16] 65 —
MgCN 시안화마그네슘[16] 50 —
MgNC 이소시아나이드 마그네슘[16] 50 —
NH2 아미노기[82] 16 —
아니오2 아산화질소[83] 44 —
NaCN 시안화나트륨[16] 49 —
NaOH 수산화나트륨[84] 40 —
OCS 황화카르보닐[85] 60 —
오3 오존[86] 48 —
SO2 이산화황[16][87] 64 —
c-SiC2 c-실리콘 디카르바이드[16][53] 52 —
SiCSI 탄화규소[88] 68 —
SiCN 탄화규소[89] 54 —
SiNC [90] 54 —
TiO2 이산화티타늄[55] 79.9 —
포름알데히드는 성간매질에 널리 분포하는 유기 분자입니다.[91]

원자 4개(30개)

분자 지정 덩어리 이온
CH3 메틸 라디칼[92] 15 CH3+[93]
l-C3H 프로피닐리딘[16][94] 37 l-C3H+[95]
c-C3H 사이클로프로피닐리딘[96] 37 —
C3N 시아노에틸닐[97] 50 C3N−[98]
C3O 일산화탄소[94] 52 —
C3S 황화삼탄[16][63] 68 —
— 하이드로늄 19 H3O+[99]
C2H2 아세틸렌[100] 26 —
H2CN 메틸렌 아미도겐[101] 28 H2CN+[27]
H2NC 아미노카빈[102] 28 —
H2CO 포름알데히드[91] 30 —
H2CS 티오포름알데히드[103] 46 —
HCCN —[104] 39 —
HCCO 케테닐[105] 41 —
— 시안화수소 양성자 28 HCNH+[77]
— 양성자화된 이산화탄소 45 HOCO+[106]
HCNO 풀민산[107] 43 —
HOCN 사이안산[108] 43 —
CNCN 이소시아노겐[109] 52 —
헉 과산화수소[110] 34 —
HNCO 이소시아네산[87] 43 —
HNCN 시아노미딜 라디칼[111] 41 —
HNCS 이소티오시안산[112] 59 —
NH3 암모니아[16][113] 17 —
HSCN 티오시안산[114] 59 —
SiC3 삼탄화규소[16] 64 —
HMgNC 이소시아니드 마그네슘[115] 51.3 —
HNO2 아질산[116] 47 —
천연가스의 주성분인 메탄은 혜성과 태양계의 몇몇 행성 대기에서도 발견되었습니다.[117]

원자 5개(20개)

분자 지정 덩어리 이온
— 암모늄 이온 18 NH+
4[118][119]
CH4 메탄[120] 16 —
CH3O 메톡시 라디칼[121] 31 —
c-C3H2 사이클로페닐리덴[28][122][123] 38 —
l-H2C3 프로파디에닐리덴[123] 38 —
H2CCN 시아노메틸[124] 40 —
H2C2O 케텐[87] 42 —
H2CNH 메틸에니민[125] 29 —
HNCNH 카르보디이미드[126] 42 —
— 양성자화된 포름알데히드 31 H2COH+[127]
C4H 부타디닐[16] 49 C4H−[128]
HC3N 시아노아세틸렌[16][28][77][129][130] 51 —
HCC-NC 이소시아노아세틸렌[131] 51 —
HCOOH 포름산[132][129] 46 —
NH2CN 키아나마이드[133][134] 42 —
NH2OH 하이드록실아민[135] 37 —
— 양성자화된 시아노겐 53 NCCNH+[136]
HC(O)CN 시아노포름알데히드[137] 55 —
다5 선형5 C[138] 60 —
SiC4 탄화규소 클러스터[53] 92 —
SiH4 실란[139] 32 —
ISM에서, 포름아미드(위)는 메틸렌과 결합하여 아세트아미드를 형성할 수 있습니다.[140]

원자 6개(16개)

분자 지정 덩어리 이온
c-H2C3O 사이클로프로페논[141] 54 —
E-HNCCN 이시아노메탄니민[142] 54 —
C2H4 에틸렌[143] 28 —
CH3CN 아세토니트릴[87][144][145] 40 —
CH3NC 메틸이소시아나이드[144] 40 —
CH3OH 메탄올[87][146] 32 —
CH3SH 메탄티올[147] 48 —
l-H2C4 디아세틸렌[16][148] 50 —
— 양성자화된 시아노아세틸렌 52 HC3NH+[77]
HCONH2 포름아미드[140] 44 —
HOCOOH 탄산[149] —
C5H 펜티닐리딘[16][63] 61 —
C5N 시아노부타디닐기[150] 74 —
HCHO2 프로피날[151] 54 —
HC4N —[16] 63 —
CH2CNH 케테니민[122] 40 —
C5S —[152] 92 —
아세트알데히드(위)와 그 이성질체인 비닐알코올과 에틸렌옥사이드가 모두 성간 공간에서 검출됐습니다.[153]

원자 7개 (13)

분자 지정 덩어리 이온
c-C2H4O 산화에틸렌[154] 44 —
CH3C2H 메틸아세틸렌[28] 40 —
H3CNH2 메틸아민[155] 31 —
CH2CHCN 아크릴로니트릴[87][144] 53 —
HCCCHNH 프로파길리민[156] 53 —
H2CHCOH 비닐알코올[153] 44 —
C6H 헥사트리닐 라디칼[16][63] 73 C6H−[123][157]
HC4CN 시아노디아세틸렌[87][130][144] 75 —
HC4NC 이소시아노디아세틸렌[158] 75 —
HC5O —[159] 77 —
CCHOCHO3 아세트알데히드[16][154] 44 —
CH3NCO 메틸이소시아네이트[160] 57 —
HOCH2CN 글리콜로니트릴[161] 57 —
식초에서 발견되는 화합물인 아세트산의 무선 신호는 1997년에 확인되었습니다.[162]

원자 8개 (14)

분자 지정 덩어리
H3CC2CN 메틸시아노아세틸렌[163] 65
HC3H2CN 시안화 프로파길[164] 65
H2COHCHO 글리콜알데히드[165][166] 60
(CHOH)2 1,2-에틸렌디올[167] 60
HCOOCH3 포름산메틸[87][129][166] 60
CH3COOH 아세트산[162] 60
H2C6 헥사펜타에닐리덴[16][148] 74
CHCHCHOCHO2 프로페날[122] 56
CHCHCN2 시아노알렌[122][163] 65
CH3CHNH 에타니민[168] 43
C2H3NH2 비닐아민[169] 43
C7H 헵타트리에닐 라디칼[170] 85
NH2CH2CN 아미노아세토니트릴[171] 56
(NH2)2CO 요소[172] 60

원자 9개 (10)

분자 지정 덩어리 이온
CH3C4H 메틸디아세틸렌[173] 64 —
COCH33 디메틸에테르[174] 46 —
CH3CH2CN 프로피오니트릴[16][87][144] 55 —
CH3CONH2 아세트아미드[122][140][134] 59 —
CCHHOH32 에탄올[175] 46 —
C8H 옥타테트라닐 라디칼[176] 97 C8H−[177][178]
HC7N 시아노헥사트리엔 또는 시아노트리아세틸렌[16][113][179][180] 99 —
CH3CHCH2 프로필렌(프로펜)[181] 42 —
CH3CH2SH 에틸메르캅탄[182] 62 —
CH3NHCHO N-메틸포름아미드[134]
Diacetylene, HCCCCH
Methyldiacetylene, HCCCCCH3
Cyanotetraacetylene, HCCCCCCCCCN
여러 폴리인에서 파생된 화학물질들은 성간매질에서 발견되는 가장 무거운 분자들 중 하나입니다.

원자수 10개 이상(21개)

아톰스 분자 지정 덩어리 이온
10 (CH3)2CO 아세톤[87][183] 58 —
10 (CH2OH)2 에틸렌글리콜[184][185] 62 —
10 CHCHCHOCHO32 프로파날[122] 58 —
10 CHOOCHOH32 메톡시메탄올[186] 62 —
10 CH3C5N 메틸시아노디아세틸렌[122] 89 —
10 CHCHCHOCHO32 프로필렌 옥사이드[187] 58 —
11 NHCHCHHOH222 에탄올아민[188] 61 —
11 HC8CN 시아노테트라아세틸렌[16][179] 123 —
11 초쵸25 포름산에틸[189] 74 —
11 CHOOCH33 아세트산메틸[190] 74 —
11 CH3C6H 메틸트리아세틸렌[122][173] 88 —
12 C6H6 벤젠[148] 78 —
12 C3H7CN 시안화 n-프로필[189] 69 —
12 (CH3)2CHCN 시안화 아이소프로필[191][192] 69 —
13 C
6H
5CN		 벤조니트릴[193] 104 —
13 HC10CN 시아노펜타아세틸렌[179] 147 —
17 C9H8 인데네[9] 116 —
19 C10H7CN 1-cyan오나프탈렌[8] 153 —
19 C10H7CN 2-cyan로나프탈렌[8] 153 —
27 C11H12N2O2 트립토판[194] —
60 다60 벅민스터풀러렌
(플러렌60)[195]		 720 다+
60[196][197][198]
70 다70 풀러렌70[195] 840 —

탈수소화 분자(22)

이 분자들은 모두 수소의 더 무거운 동위 원소인 하나 이상의 중수소 원자를 포함하고 있습니다.

아톰스 분자 지정
2 HD 수소탈수소[199][200]
3 H2D+, HD+
2		 삼수소 양이온[199][200]
3 HDO, D2O 중수[201][202]
3 DCN 시안화수소[203]
3 DCO 포밀 라디칼[203]
3 DNC 이소시아나이드수소[203]
3 N2D+ —[203]
3 NHD, ND2 아미도겐[204]
4 NH2D, NHD2, ND3 암모니아[200][205][206]
4 HDCO, D2CO 포름알데히드[200][207]
4 DNCO 이소시아네산[208]
5 NH3D+ 암모늄 이온[209][210]
6 NH
2CDO; NHDCHO		 포름아미드[208]
7 CH2DCCH, CH3CCD 메틸아세틸렌[211][212]

확인되지 않음 (13)

다음 분자의 존재에 대한 증거는 과학 문헌에 보고되었지만, 그 검출은 저자들에 의해 잠정적으로 기술되거나 다른 연구자들에 의해 이의가 제기되었습니다.그들은 독자적인 확인을 기다립니다.

아톰스 분자 지정
2 SiH 실릴리딘[74]
4 PH3 포스핀[213]
4 MgCCH 모노아세틸화마그네슘[152]
4 NCCP 시아노포스파에틴[152]
5 H2NCO+ —[214]
6 SiH3CN 시안화 실릴[152]
10 H2NCH2COOH 글리신[215][216]
10 C2H5NH2 에틸아민[169]
12 CO(CH2OH)2 디하이드록시아세톤[217][218]
12 COCH253 에틸메틸에테르[219]
18 C
10H+
8		 나프탈렌 양이온[220]
24 다24 그래핀[221]
24 C14H10 안트라센[222][223]
26 C16H10 피렌[222]

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메모들

  1. ^ 지구에서 아르곤의 지배적인 동위 원소는 Ar이므로, ArH의+ 질량은 41 amu일 것입니다.그러나 성간 탐지는 질량이 37 amu인 ArH+ 동위원소였습니다.

외부 링크