CDMS classic documentation - molecules:extragalactic

arh-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 04 Apr 2022 10:53:14 +0000

2022/04/04 12:45		current
Line 13:		Line 13:
	A. M. Jacob, K. M. Menten, F. Wyrowski, B. Winkel, D. A. Neufeld and B. S. Koribalski<br>		A. M. Jacob, K. M. Menten, F. Wyrowski, B. Winkel, D. A. Neufeld and B. S. Koribalski<br>
	reported on\\		reported on\\
-	[[https://doi.org/10.1051/0004-6361/201527254\|ArH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> Absorption towards Luminous Galaxies]]\\	+	[[https://doi.org/10.1051/0004-6361/202142544\|ArH<sup>+</sup> and H<sub>2</sub>O<sup>+</sup> Absorption towards Luminous Galaxies]]\\
	//Astron. Astrophys.// 659, (2022) Art. No. 152.\\		//Astron. Astrophys.// 659, (2022) Art. No. 152.\\
		+	The //J// = 1 − 0 transition of <sup>36</sup>ArH<sup>+</sup> was detected with the APEX 12 m dish toward the nearby galaxies NGC 253, NGC 4945, and Arp 220. The molecular fraction of the gas traced by ArH<sup>+</sup> was estimated to be ~10<sup>−3</sup> and that it resides in gas volumes with low electon densities.\\
		+	\\

	----		----

benzol_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 25 Feb 2019 21:38:06 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Benzene in Extragalactic Sources =====
	+
	+	J. Bernard-Salas, E. Peeters, G. C. Sloan, J. Cami, S. Guiles, and J. R. Houck\\
	+	obtained\\
	+	[[http://dx.doi.org/10.1086/509777\|The //Spitzer// IRS spectrum of SMP LMC 11]]\\
	+	//Astrophys. J.// 652, (2006) L29.\\
	+	The spectrum resembles that of the protoplanetary nebula V353 Aur, which is somewhat better known as CRL (or AFGL) 618. As in the Galactic source, benzene was detected in absorption by its //ν//<sub>4</sub> band at 674.0 cm<sup>–1</sup> (or 14.84 μm).
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+
	+	----
	+

c-c3h_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 25 Feb 2019 21:38:06 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of C3H =====
	+
	+	S. Martín et al., in preparation.\\
	+
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

c2h_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:44:29 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of C2H =====
	+
	+	C. Henkel, P. Schilke, and R. Mauersberger,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1988A%26A...201L..23H\|Molecules in external galaxies - The detection of CN, C<sub>2</sub>H, and HNC, and the tentative detection of HC<sub>3</sub>N]],\\
	+	//Astron. Astrophys.// 201, L23-L26 (1988).
	+
	+	Source(s): M82\\
	+	Facility: IRAM 30m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

c2h3-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Wed, 13 Mar 2024 11:39:54 +0000

2024/03/13 12:27		current
Line 5:		Line 5:
	[[https://doi.org/10.1051/0004-6361/202348994\|Protonated Acetylene in the //z// = 0.89 Molecular Absorber toward PKS 1830−211]]\\		[[https://doi.org/10.1051/0004-6361/202348994\|Protonated Acetylene in the //z// = 0.89 Molecular Absorber toward PKS 1830−211]]\\
	//Astron. Astrophys.// 683, (2024) Art. No. A62.\\		//Astron. Astrophys.// 683, (2024) Art. No. A62.\\
		+	\\
		+	The molecule C<sub>2</sub>H<sub>3</sub><sup>+</sup> was identified through the //ortho//-transition 2<sub>12</sub> – 1<sub>01</sub> at a rest frequency of 494.034 GHz and through the //para//-transition 1<sub>11</sub> – 0<sub>00</sub> at a rest frequency of 431.315 GHz. Protonated acetylene is less abundant than C<sub>2</sub>H and C<sub>4</sub>H by factors of about 600 and 60, respectively.\\
	\\		\\
		+
		+	----
		+
		+	Contributor(s): H. S. P. Müller; 03, 2024
		+
		+	----

c2h3cn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Fri, 24 Apr 2020 13:34:56 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Propenenitrile, C2H3CN, in Extragalactic Sources =====
	+
	+	B. Tercero, J. Cernicharo, S. Cuadrado, P. de Vicente, and M. Guélin\\
	+	used the Yebes 40 m telescopy in the 7 mm wavelength region (rest frequencies: 58.7 − 93.5 GHz) to study the molecular content of a foreground galaxy at //z// = 0.89 in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\
	+	//Astron. Astrophys.// 636, (2020) Art. No. L7.\\
	+	Propenenitrile, C<sub>2</sub>H<sub>3</sub>CN, also known as vinyl cyanide or acrylonitrile, was identfied by five rotational transitions with //J// = 8 − 7 or 7 − 6 and //K<sub>a</sub>// = 0 to 2. The lines show good (three) to very modest signal-to-noise ratios.
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 4, 2020
	+
	+	----

c2s_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:48:33 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Thioethenylidene, C2S, in Extragalactic Sources =====
	+
	+	S. Martín, R. Mauersberger, J. Martín-Pintado, C. Henkel, and S. García-Burillo\\
	+	used the IRAM 30 m telecope to carry out\\
	+	[[https://doi.org/10.1086/503297\|A 2 Millimeter Spectral Line Survey of the Starburst Galaxy NGC 253]]\\
	+	//Astrophys. J. Suppl. ser.// 164, (2006) 450 – 476.\\
	+	Thioethenylidene, C<sub>2</sub>S, was identified by its four //N<sub>J</sub>// = 10<sub>11</sub> – 9<sub>10</sub> to 11<sub>12</sub> – 10<sub>14</sub> transitions with rest frequencies between 131.5 and 144.3 GHz.
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	The low energy fine structure lines //N<sub>J</sub>// = 5<sub>5</sub> – 4<sub>3</sub>, 6<sub>5</sub> – 5<sub>4</sub>, and 7<sub>6</sub> – 6<sub>5</sub> with rest frequencies near 57.2, 69.3, and 81.5 GHz, respectively, were detected in absorption.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 08, 2017
	+
	+	----
	+

c3h2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:23:02 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of c-C3H2 =====
	+
	+	E. R. Seaquist and M. B. Bell,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1986ApJ...303L..67S\|Detection of the hydrocarbon ring molecule C<sub>3</sub>H<sub>2</sub> in the radio galaxy Centaurus A (= NGC 5128)]],\\
	+	//Astrophys. J.// 303, L67-L70 (1986).
	+
	+	Source(s): NGC5128\\
	+	Facility: NRAO 140 foot (43m)\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

c3n_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Fri, 24 Apr 2020 11:03:08 +0000

2020/04/24 11:54		current
Line 5:		Line 5:
	[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\		[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\
	//Astron. Astrophys.// 636, (2020) Art. No. L7.\\		//Astron. Astrophys.// 636, (2020) Art. No. L7.\\
		+	The cyanoethynyl radical, C<sub>3</sub>N, was identfied by four fine structure components of three rotational transitions with //N// = 6 − 5 to 8 − 7; two fine structure components were severly blended.
		+
		+
		+	----
		+
		+	Contributor(s): H. S. P. Müller; 4, 2020
		+
		+	----

c4h_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:25:52 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of the Butadiynyl Radical, C4H, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	The linear butadiynyl radical, C<sub>4</sub>H, was identified by its //N// = 6 – 5 to 9 – 8 transitions with rest frequencies between 57.0 and 85.7 GHz. All transitions display fine structure splitting of about 40 MHz, whereas the H-hyperfine structure was not resolved. Even though the signal-to-noise ratio appears to be fairly good, it may be the cause of some relative intensity issue in the fine structure components of a respective rotational transition.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

cf-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:36:38 +0000

2026/04/12 12:18	current
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	+	===== Fluoromethylidynium, CF+, in Extragalactic Sources =====
	+
	+	S. Muller, K. Kawaguchi, J. H. Black, and T. Amano,\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/201628494\|Detection of Extragalactic CF<sup>+</sup> toward PKS 1830–211 – Chemical Differentiation in the Absorbing Gas]]\\
	+	//Astron. Astrophys.// 589, (2016) Art. No. L5.\\
	+	The //J// = 2 – 1 transition of CF<sup>+</sup> (rest frequency 205.2 GHz) was observed in absorption in the //z// = 0.89 foreground galaxy toward the quasar PKS 1830–211. The Atacama Large Millimeter Array (ALMA) was used in its Early Science Cycle 2 phase.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 04, 2016
	+
	+
	+	----
	+

ch_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:26:27 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of CH =====
	+
	+	J. B. Whiteoak, F. F. Gardner, and B. Hoglund,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1980MNRAS.190P..17W\|The detection of CH in external galaxies]],\\
	+	//Mon. Not. R. Astron. Soc.// 190, 17P-22P (1980).
	+
	+	Source(s): LMC, NGC4945, NGC5128\\
	+	Facility: Parkes 64m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

ch-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:28:28 +0000

2026/04/12 12:18	current
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	+	===== Extragalactic Methyliumylidene, CH+ =====
	+
	+	P. Magain and D. Gillet\\
	+	reported on the\\
	+	[[https://ui.adsabs.harvard.edu/abs/1987A%26A...184L...5M\|Detection of interstellar CH and CH<sup>+</sup> towards SN 1987a]],\\
	+	//Astron. Astrophys.// 184, L5–L6 (1987).\\
	+	Lowest-//J// optical transitions were observed in absorption with the ESO 1.4 m telescope at La Silla. The velocities correspond to interstellar matter within the Large Magellanic Cloud.
	+
	+	E. Falgarone, M. A. Zwaan, B. Godard, E. Bergin, R. J. Ivison, P. M. Andreani, F. Bournaud, R. S. Bussmann, D. Elbaz, A. Omont, I. Oteo, and F. Walter\\
	+	reported on the\\
	+	[[https://doi.org/10.1038/nature23298\|Large Turbulent Reservoirs of Cold Molecular Gas around High-redshift Starburst Galaxies]],\\
	+	//Nature// 548, (1987) 430–433.\\
	+	The //J// = 1 – 0 transitions of CH<sup>+</sup> was detected in emission and/or absorption toward six galaxies at red-shifts of 2.0 to 2.6 with ALMA.
	+
	+	S. Muller, H. S. P. Müller, J. H. Black, M. Gérin, F. Combes, S. Curran, E. Falgarone, M. Guélin, C. Henkel, S. Martín, K. M. Menten, E. Roueff, S. Aalto, A. Beelen, T. Wiklind, and M. A. Zwaan,\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/201731405\|Detection of CH<sup>+</sup>, SH<sup>+</sup>, and Their <sup>13</sup>C- and <sup>34</sup>S-isotopologues toward PKS 1830–211]]\\
	+	//Astron. Astrophys.// 606, (2017) Art. No. A109.\\
	+	The //J// = 1 – 0 transitions of CH<sup>+</sup> and <sup>13</sup>CH<sup>+</sup> were observed with ALMA redshifted from about 835.1 and 830.2 GHz to about 442.85 and 440.24 GHz. The molecular cations were detected toward both SW and NE images. The intensity ratio appears to suggest the molecular cation resides in gas with at least slightly higher molecular fraction than H<sub>2</sub>O<sup>+</sup> or H<sub>2</sub>Cl<sup>+</sup>. The <sup>12</sup>C/<sup>13</sup>C isotopic ratio is about 100, possibly higher. This is, to the best of our knowledge, the first account on extragalactic <sup>13</sup>CH<sup>+</sup>.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 11, 2017
	+
	+	----
	+

ch2nh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:24:28 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Methanimine, H2CNH, in Extragalactic Sources =====
	+
	+	S. Martín, R. Mauersberger, J. Martín-Pintado, C. Henkel, and S. García-Burillo\\
	+	used the IRAM 30 m telecope to carry out\\
	+	[[https://doi.org/10.1086/503297\|A 2 Millimeter Spectral Line Survey of the Starburst Galaxy NGC 253]]\\
	+	//Astrophys. J. Suppl. ser.// 164, (2006) 450 – 476.\\
	+	Methanimine, H<sub>2</sub>CNH, was identified by the //J<sub>K<sub>a</sub>,K<sub>c</sub></sub>// = 2<sub>1,1</sub> – 1<sub>1,0</sub> transition in emission near 133.27 GHz. A feature near the noise level is present at the 1<sub>1,0</sub> – 1<sub>0,1</sub> transition with rest frequencies near 166.85 GHz.
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	The 1<sub>0,1</sub> – 0<sub>0,0</sub> ground state transition was detected prominently in absorption near 33.9 GHz, corresponding to a rest frequency of about 64.0 GHz.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 08, 2017
	+
	+	----
	+

ch3cch_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:30:40 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of CH3CCH =====
	+
	+	R. Mauersberger, C. Henkel, C. M. Walmsley, L. J. Sage, and T. Wiklind, T.\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...247..307M\|Dense gas in nearby galaxies. V - Multilevel studies of CH<sub>3</sub>CCH and CH<sub>3</sub>CN]],\\
	+	//Astron. Astrophys.// 247, 307-314 (1991).
	+
	+	Source(s): M82, NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

ch3cn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:27:11 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of CH3CN =====
	+
	+	R. Mauersberger, C. Henkel, C. M. Walmsley, L. J. Sage, and T. Wiklind, T.\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...247..307M\|Dense gas in nearby galaxies. V - Multilevel studies of CH<sub>3</sub>CCH and CH<sub>3</sub>CN]],\\
	+	//Astron. Astrophys.// 247, 307-314 (1991).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

ch3oh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:26:43 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of CH3OH =====
	+
	+	C. Henkel, T. Jacq, R. Mauersberger, K. M. Menten, H. Steppe,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1987A%26A...188L...1H\|The detection of extragalactic methanol]],\\
	+	//Astron Astrophys.// 188, L1-L4 (1987).
	+
	+	Source(s): NGC253, IC342, and possibly towards NGC6946\\
	+	Facility: IRAM 30m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

ch3sh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 04 Jan 2022 13:20:46 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Methanethiol, CH3SH, in Extragalactic Sources =====
	+
	+	B. Tercero, J. Cernicharo, S. Cuadrado, P. de Vicente, and M. Guélin\\
	+	used the Yebes 40 m telescopy in the 7 mm wavelength region (rest frequencies: 58.7 − 93.5 GHz) to study the molecular content of a foreground galaxy at //z// = 0.89 in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\
	+	//Astron. Astrophys.// 636, (2020) Art. No. L7.\\
	+	Methanethiol, CH<sub>3</sub>SH, also known as methyl mercaptan, was identfied by three lines of four rotational transitions with //J// = 3 − 2 and //K// = 0 or 1. The lines show good to fairly reasonable signal-to-noise ratios.
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 04, 2020
	+
	+	----

chloronium-extra

anonymous@undisclosed.example.com (Anonymous) — Wed, 26 Nov 2025 13:41:15 +0000

2026/04/12 12:18	current
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	+	===== Chloronium, H2Cl+, in Extragalactic Sources =====
	+
	+	S. Muller, J. H. Black, M. Guélin, C. Henkel, F. Combes, M. Gérin, S. Aalto, A. Beelen, J. Darling, C. Horellou, S. Martín, K. M. Menten, Dinh-V-Trung, and M. A. Zwaan\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/201423947\|Detection of chloronium and measurement of the 35Cl/37Cl isotopic ratio at //z// = 0.89 toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 566, (2014) Art. No. L6.\\
	+	The 1<sub>11</sub> – 0<sub>00</sub> transitions of H<sub>2</sub><sup>35</sup>Cl<sup>+</sup> and H<sub>2</sub><sup>37</sup>Cl<sup>+</sup> were observed with ALMA redshifted from about 485 GHz to about 257 GHz. The <sup>35</sup>Cl/<sup>37</sup>Cl isotopic ratio agrees within error bars with the terrestrial ratio.\\
	+	\\
	+
	+	S. H. J. Wallström, S. Muller, E. Roueff, R. Le Gal, J. H. Black, and M. Gérin\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/201935860\|Chlorine-bearing Molecules in Molecular Absorbers at Intermediate Redshifts]]\\
	+	//Astron. Astrophys.// 566, (2014) Art. No. L6.\\
	+	Both chloronium isotopologs were also detected in the //z// ≈ 0.68 foreground galaxy of the quasar B 0218+357; the <sup>35</sup>Cl/<sup>37</sup>Cl isotopic ratio is about 2.2.\\
	+	\\
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 06, 2014; 11, 2025
	+
	+	----

cn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:28:57 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of CN =====
	+
	+	C. Henkel, P. Schilke, and R. Mauersberger,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1988A%26A...201L..23H\|Molecules in external galaxies - The detection of CN, C<sub>2</sub>H, and HNC, and the tentative detection of HC<sub>3</sub>N]],\\
	+	//Astron. Astrophys.// 201, L23-L26 (1988).
	+
	+	Source(s): NGC253, IC342, M82\\
	+	Facility: IRAM 30m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

co_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:25:24 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of CO =====
	+
	+	L. J. Rickard, P. Palmer, M. Morris, B. E. Turner, and B. Zuckerman,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1975ApJ...199L..75R\|Detection of extragalactic carbon monoxide at millimeter wavelengths]],\\
	+	//Astrophys. J.// 199, L75-L78 (1974).
	+
	+	Source(s): M82, NGC253\\
	+	Facility: NRAO 11m
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of 13CO ====
	+
	+	P. M. Solomon and R. de Zafra\\
	+	[[https://ui.adsabs.harvard.edu/abs/1975ApJ...199L..79S\|Carbon monoxide in external galaxies]],\\
	+	//Astrophys. J.// 199, L79-L83 (1974).
	+
	+	Source(s): M82\\
	+	Facility: NRAO 11m
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of C17O and C18O ====
	+
	+	L. J. Sage, C. Henkel, and R. Mauersberger,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...249...31S\|Extragalactic O-18/O-17 ratios and star formation - High-mass stars preferred in starburst systems?]],\\
	+	//Astron. Astrophys.// 249, 31-35 (1991).
	+
	+	Source(s): M82, NGC253, tentatively: IC 342\\
	+	Facility: IRAM 30m, NRAO 12m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth, 09/2005
	+
	+	----
	+

co-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:30:44 +0000

2026/04/12 12:18	current
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	+	===== Extragalactic Detection of CO+ =====
	+
	+	A. Fuente, S. García-Burillo, M. Gerin, J. R. Rizzo, A. Usero, D. Teyssier, E. Roueff, and J. Le Bourlot\\
	+	[[https://doi.org/10.1086/503605\|Detection of CO<sup>+</sup> in the Nucleus of M82]],\\
	+	//Astrophys. J.// 641, L105–L108 (2006).
	+
	+	Source(s): M82\\
	+	Facility: IRAM 30 m
	+
	+	Comments:\\
	+	Two fine structure components of the //N// = 2 – 1 transition have been detected at 235789.64 and 236062.55 GHz, respectively.\\
	+	A tentative detection of the //N// = 1 – 0 fs components had been recorded few years earlier by:\\
	+	A. Fuente, J. H. Black, J. Martín-Pintado, A. Rodríguez-Franco, S. García-Burillo, P. Planesas, and J. Lindholm\\
	+	[[https://doi.org/10.1086/317879\|Tentative Detection of CO<sup>+</sup> toward Cygnus A]],\\
	+	//Astrophys. J.// 545, L113–L116 (2000).
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller, 07/2010
	+
	+	----
	+

cs_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:27:27 +0000

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	+	===== First Extragalactic Detection of CS =====
	+
	+	C. Henkel and J. Bally,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1985A%26A...150L..25H\|Detection of extragalactic CS]],\\
	+	//Astron. Astrophys.// 150, L25-L27 (1985).
	+
	+	Source(s): M82, IC342\\
	+	Facility: Bell Labs 7m\\
	+
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of C34S ====
	+
	+	R. Mauersberger and C. Henkel,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1989A%26A...223...79M\|Dense gas in nearby galaxies. I - Distribution, kinematics and multilevel studies of CS]],\\
	+	//Astron. Astrophys.// 223, 79-88 (1989).
	+
	+	Source(s): NGC253, M82\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of 13CS ====
	+
	+	C. Henkel, R. Mauersberger, T. Wiklind, S. Huettemeister, C. Lemme, and T. J. Millar,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1993A%26A...268L..17H\|Dense gas in nearby galaxies. VI - A large <sup>12</sup>C/<sup>13</sup>C ratio in a nuclear starburst environment]],\\
	+	//Astron. Astrophys.// 268, L17-L20 (1993).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

dme

anonymous@undisclosed.example.com (Anonymous) — Tue, 04 Jan 2022 13:44:43 +0000

2026/04/12 12:18	current
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	+	===== On Dimethyl Ether in Extragalactic Sources =====
	+
	+	M. Sewiło, R. Indebetouw, S. B. Charnley, S. Zahorecz, J. M. Oliveira, J. T. van Loon, J. L. Ward, C.-H. R. Chen, J. Wiseman, Y. Fukui, A. Kawamura, M. Meixner, T. Onishi, and P. Schilke\\
	+	reported on\\
	+	**[[https://doi.org/10.3847/2041-8213/aaa079\|The Detection of Hot Cores and Complex Organic Molecules
	+	in the Large Magellanic Cloud]]**\\
	+	//Astrophys. J. Lett.// 853, (2018) Art. No. L19.\\
	+	ALMA was used at 1.3 mm to study the N 113 hot core region of the LMC. One line of dimethyl ether near 231.99 GHz was detected with reasonable signal-to-noise ratio toward the A1 and B3 peaks. The derived column densities are about a factor of 8 and 4, respectively, lower than those of methanol.\\
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 01, 2022
	+
	+	----

formamid_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:27:49 +0000

2026/04/12 12:18	current
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	+	===== Detection of Extragalactic Formamide, HC(O)NH2 =====
	+
	+	S. Muller, A. Beelen, J. H. Black, S. J. Curran, C. Horellou, S. Aalto, F. Combes, M. Guélin, and C. Henkel\\
	+	reported on\\
	+	[[https://doi.org/10.1051/0004-6361/201220613\|A precise and accurate determination of the cosmic microwave background temperature at //z// = 0.89]]\\
	+	//Astron. Astrophys.// 551, (2013) Art. No. A109.\\
	+	The famous, but unnamed foreground galaxy in direction of the quasar PKS 1830–211 was studied with the Australia Telecope Compact Array and the Plateau de Bure Interferometer. ATCA observations at 7 mm revealed 2 significant lines of formamide, 4<sub>04</sub> – 3<sub>03</sub> near 44.8 GHz (restfrequency near 84.5 GHz) and 4<sub>13</sub> – 3<sub>12</sub> near 46.6 GHz (restfrequency near 87.8 GHz). Even though rather few transitions have been observed, the detection is probably secure because of the limited line density.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 04, 2013
	+
	+	----
	+

fullerene_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:32:16 +0000

2026/04/12 12:18	current
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	+	===== On the Thus Far Questionable Detection of Fullerenes in Extragalactic Sources =====
	+
	+	\\
	+	\\
	+
	+
	+	==== C60 ====
	+
	+	Fullerenes, and in particular the most stable small fullerene C<sub>60</sub>, were sought for quite extensively. Initially, they appeared to be rather elusive. Shortly after the definitive Galactic detection of C<sub>60</sub> and C<sub>70</sub>, they appeared to be almost ubiquitous. However, a very recent laboratory spectroscopic investigation by\\
	+	W. W. Duley and A. Hu,\\
	+	[[https://doi.org/10.1088/2041-8205/745/1/L11\|Fullerenes and Proto-fullerenes in Interstellar Carbon Dust]],\\
	+	//Astrophys. J.// 659, Art. No. L11 (2012);\\
	+	concluded that the presence of PAH molecules and of fullerenes are mutually exclusive. In fact, the dehydrogenation of PAHs involves pseudo-fullerenes which still contain H atoms and which are not as symmetric as C<sub>60</sub>. Prior to turning to fullerenes, these molecules exhibit IR bands similar to C<sub>60</sub>, but in addition a strong mode near 16.4 μm (610 cm<sup>–1</sup>). Some of the IR bands of fullerenes are apparently less specific than had been thought. This fact, however, had been known for the mid-infrared features of PAHs for a long time. As a consequence, the autors cast doubt on all reported detections of C<sub>60</sub> described in this section and in the Extragalactic section. The only uncontested report appears to be the one in which C<sub>60</sub> and C<sub>70</sub> were detected in Tc 1, see in the Galactic section. However, some of the other detection are probably likely correct, even if some caution is advised.
	+
	+	D. A. García-Hernández, A. Manchado, P. García-Lario, L. Stanghellini, E. Villaver, R. A. Shaw, R. Szczerba, and J. V. Perea-Calderón,\\
	+	studied with //Spitzer//\\
	+	[[https://doi.org/10.1088/2041-8205/724/1/L39\|Formation of Fullerenes in H-containing Planetary Nebulae]],\\
	+	//Astrophys. J.// 724, Art. No. L39 (2010).\\
	+	Besides several Galactic sources, they also studied LHA 115-N 42, also known as SMP SMC 16, in the Small Magellanic Cloud. Strong features attributed to C<sub>60</sub> were detected near 17.4 and 18.9 μm. These features overlap with weaker features of C<sub>70</sub> in the Galactic PN Tc 1. However, a C<sub>70</sub> feature near 14.8 μm is clearly absent. The 8.5 μm feature of C<sub>60</sub> was also observed weakly, the one near 7.0 μm is overlapped by a much stronger Ar<sup>+</sup> line – similar to the situation in Tc 1. Because of the investigation mentioned above, this identification should be viewed with caution, though it appears to be rather likely.
	+
	+
	+	----
	+
	+	\\
	+	\\
	+
	+
	+	==== C70 ====
	+
	+	There are no reports on Extragalactic observations of C<sub>70</sub> thus far.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 06, 2011; 01, 2012
	+
	+
	+	----
	+

h2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:25:54 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of H2 =====
	+
	+	R. I. Thompson, M. J. Lebofsky, G. H. Rieke,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1978ApJ...222L..49T\|The 2-2.5 micron spectrum of NGC 1068 - A detection of extragalactic molecular hydrogen]],\\
	+	//Astrophys. J.// 222, L49-L53 (1978).
	+
	+	Source(s): NGC1068\\
	+	Facility: Steward Observatory 2.3m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

h2ccn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:25:16 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of the Cyanomethyl Radical, H2CCN, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	The cyanomethyl radical shows at low quantum numbers complicated pattern caused by fine structure (FS) and hyperfine structure (HFS) of the N nucleus; at even //K<sub>a</sub>//, HFS of the two equivalent H nuclei occurs. Two //K<sub>a</sub>// = 0 transitions with //J"// = 2 and 3 were detected. The lines were broadened because of FS and HFS.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

h2cco_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:25:35 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Ketene, H2CCO, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	Two pairs of //K<sub>a</sub>// = 1 transitions of ketene with //J"// = 2 and 3 were detected. The //K<sub>a</sub>// = 0 //para// transitions are within the noise level.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

h2cl-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Wed, 26 Nov 2025 20:56:18 +0000

2025/11/26 21:55		current

h2cn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Fri, 24 Apr 2020 11:30:22 +0000

2026/04/12 12:18	current
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	+	===== On the Detection of Methyleneamidogen, H2CN, in Extragalactic Sources =====
	+
	+	B. Tercero, J. Cernicharo, S. Cuadrado, P. de Vicente, and M. Guélin\\
	+	used the Yebes 40 m telescopy in the 7 mm wavelength region (rest frequencies: 58.7 − 93.5 GHz) to study the molecular content of a foreground galaxy at //z// = 0.89 in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\
	+	//Astron. Astrophys.// 636, (2020) Art. No. L7.\\
	+	The methyleneamidogen radical, H<sub>2</sub>CN, also known as methaniminyl, was identfied by four hyperfine components of the 1<sub>01</sub> − 0<sub>00</sub> //ortho// rotational transition. The lines show good to quite reasonable signal-to-noise ratios.
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 4, 2020
	+
	+	----

h2co_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:18:16 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of Formaldehyde, H2CO =====
	+
	+	F. F. Gardner and J. B. Whiteoak,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1974Natur.247..526G\|Detection of formaldehyde in external galaxies]],\\
	+	//Nature// 247, 526 (1974).
	+
	+	Source(s):\\
	+	Facility: Parkes 64m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

h2cs_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:21:13 +0000

2026/04/12 12:18	current
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	+	===== Tentative Extragalactic Detections of H2CS =====
	+
	+	A. Heikkilä, L. E. B. Johansson, and H. Olofsson,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1999A%26A...344..817H\|Molecular abundance variations in the Magellanic Clouds]],\\
	+	//Astron. Astrophys.// 344, 817-847 (1999).
	+
	+	Source(s): LMC\\
	+	Facility: SEST 15m
	+
	+
	+	----
	+
	+	S. Martín, J. Martin-Pintado, R. Mauersberger, C. Henkel, and S. Garcia-Burillo,\\
	+	[[https://ui.adsabs.harvard.edu/abs/2005ApJ...620..210M\|Sulfur Chemistry and Isotopic Ratios in the Starburst Galaxy NGC 253]],\\
	+	//Astrophys. J.// 620, 210-216 (2005).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

h2nc_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 12 Oct 2021 10:53:49 +0000

2026/04/12 12:18	current
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	+	===== On the Extragalactic Detection of Aminomethylidyne, H2NC =====
	+
	+	C. Cabezas, M. Agúndez, N. Marcelino, B. Tercero, S. Cuadrado, and J. Cernicharo\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/202141491\|Interstellar Detection of the Simplest Aminocarbyne H<sub>2</sub>NC: An ignored but Abundant Molecule, ]]\\
	+	//Astron. Astrophys.// 654, art. no. A45 (2021).\\
	+	The aminomethylidyne isomer was observed in the course of monitoring aboservation of of the //z// = 0.89 galaxy in front of the quasar PKS 1830−211 using the Yebes 40 m telescope. The column densities of H<sub>2</sub>CN is about four times that of H<sub>2</sub>NC.\\
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 10, 2021
	+
	+	----

h2o_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:41:30 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of Water, H2O =====
	+
	+	E. Churchwell, A. Witzel, W. Huchtmeier, I. Pauliny-Toth, J. Roland, and W. Sieber,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1977A%26A....54..969C\|Detection of H<sub>2</sub>O maser emission in the Galaxy M 33]],\\
	+	//Astron. Astrophys.// 54, 969-971 (1977).
	+
	+	Source(s): M33\\
	+	Facility: Effelsberg 100m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth, 07/2005
	+
	+	----
	+

h2o-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:49:15 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On Oxydaniumyl, H2O+, in Extragalactic Sources =====
	+
	+	The first substantiated detection of Extragalactic H<sub>2</sub>O<sup>+</sup> involves the //J// = 1.5 – 0.5 fine structure component of the 1<sub>11</sub> – 0<sub>00</sub> transition of //ortho//-oxidaniumyl near 1115 GHz, which has been detected in absorption with the HIFI instrument on board of the //Herschel// satellite toward M 82:\\
	+	A. Weiß, M. A. Requena-Torres, R. Güsten, et al.\\
	+	[[https://doi.org/10.1051/0004-6361/201015078\|HIFI Spectroscopy of Low-Level Water Transitions in M 82]]\\
	+	//Astron. Astrophys.// 521, (2010) Art. No. L1.\\
	+	As may be interpreted from the title, H<sub>2</sub>O<sup>+</sup> was observed by accident because of the proximity of that fine structure component to the 1<sub>11</sub> – 0<sub>00</sub> transition of //para//-H<sub>2</sub>O. However, a detailed analysis of this feature has been presented.
	+
	+	It is worthwhile mentioning that only the weaker //J// = 0.5 – 0.5 fine structure component of the 1<sub>11</sub> – 0<sub>00</sub> transition was reportedly detected with SPIRE///Herschel// in emission toward the ultraluminous infrared galaxy Mrk 231:\\
	+	P. P. van der Werf, K. G. Isaak, R. Meijerink, et al.,\\
	+	[[https://doi.org/10.1051/0004-6361/201014682\|Black Hole Accretion and Star-Formation as Drivers of Gas Excitation and Chemistry in Markarian 231]]\\
	+	//Astron. Astrophys.// 518, (2010) Art. No. L42.\\
	+	The account is somewhat sketchy, the report should therefore be viewed with some caution. On the other hand, the title seems to indicate why the line, provided the identification is correct, is seen in emission, in contrast to all presently known Galactic observations and also in contrast to the Extragalactic detection mentioned above.
	+
	+	E. González-Alfons1 , J. Fischer, S. Bruderer, et al.\\
	+	reported on\\
	+	[[https://doi.org/10.1051/0004-6361/201220466\|Excited OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, and H<sub>3</sub>O<sup>+</sup> in NGC 4418 and Arp 220]],\\
	+	//Astron. Astrophys.// 550, Art. No. A25 (2013);\\
	+	using PACS on board of the //Herschel// satellite. Transitions 4<sub>04</sub> – 3<sub>13</sub> and 3<sub>22</sub> – 2<sub>11</sub> with upper state energies of about 300 K were detected in both sources with no or negligible overlap. Additional transitions with //E//<sub>up</sub> beyond 400 K have also been observed, but are at least partially overlapped.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 10, 2010; 04, 2013.
	+
	+	----
	+

h2s_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:47:19 +0000

2026/04/12 12:18	current
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	+	===== First Extragalactic Detection of H2S =====
	+
	+	A. Heikkilä, L. E. B. Johansson, and H. Olofsson,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1999A%26A...344..817H\|Molecular abundance variations in the Magellanic Clouds]],\\
	+	//Astron. Astrophys.// 344, 817-847 (1999).
	+
	+	Source(s): LMC\\
	+	Facility: SEST 15m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

h3o-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:22:04 +0000

2026/04/12 12:18	current
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	+	===== Oxidanium, H3O+, in Extragalactic Sources =====
	+
	+	F. F. S. van der Tak, S. Aalto, and R. Meijerink,\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361:20078824\|Detection of Extragalactic H<sub>3</sub>O<sup>+</sup>]],\\
	+	//Astron. Astrophys.// 477, L5–L8 (2008).\\
	+	The //J<sub>K</sub><sup>v<sub>t</sub></sup>// = 3<sub>2</sub><sup>+</sup> – 2<sub>2</sub><sup>–</sup> at 364797.427 MHz has been detected unambiguously in emission in the starburst galaxy M 82 and in the ultraluminous infrared galaxy (ULIRG) Arp 220 using the JCMT. Thus far, this is the only transition detected. Thus, the detection may be viewed with some caution. The detection in the ISM (see respective section) started out similarly. Moreover, no line overlap with a line of an unknown seems possible. Therefore, the detection is probably quite secure.
	+
	+	S. Aalto, F. Costagliola, F. F. S. van der Tak, and R. Meijerink,\\
	+	found in addition\\
	+	[[https://doi.org/10.1051/0004-6361/201015878\|H<sub>3</sub>O<sup>+</sup> Line Mmission from Starbursts and AGNs]],\\
	+	//Astron. Astrophys.// 527, Art. No. A69 (2011).\\
	+	Transition and telescope were the same as above. IC 342, NGC 253, and NGC 4418 are members of the former group of galaxies, NGC 1068, also known as M 77, and NGC 6240 belong to the latter.
	+
	+	E. González-Alfonso, J. Fischer, S. Bruderer, et al.\\
	+	reported on\\
	+	[[https://doi.org/10.1051/0004-6361/201220466\|Excited OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, and H<sub>3</sub>O<sup>+</sup> in NGC 4418 and Arp 220]],\\
	+	//Astron. Astrophys.// 550, Art. No. A25 (2013);\\
	+	using PACS on board of the //Herschel// satellite. Very highly excited rotation-inversion transitions were detected in both sources. In addition extensive metastable pure inversion transitions (up to //J// = //K// = 12 with an upper state energy of more than 1500 K) were detected in Arp 220. The hottest components diplay rotational temperatures of about 500 K and 550 K for NGC 4418 and Arp 220, respectively.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller, 01/2008; 04, 2013.
	+
	+	----
	+

hc2nh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:20:19 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of Polyacetylenes in Extragalactic Sources =====
	+
	+	==== Acetylene ====
	+
	+	An early account on Extragalactic acetylene was presented by\\
	+	J. T. van Loon, A. A. Zijlstra, and M. A. T. Groenewegen,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1999A%26A...346..805V\|Luminous Carbon Stars in the Magellanic Clouds]]\\
	+	//Astron. Astrophys.// 346, (1999) 805.\\
	+	Telescopes of ESO and CTIO were used to carry out observations in the L-band (at 3 μm). Broad, strong absorption was found between 3.0 and 3.3 μm which was attributed to HCN and HCCH. As usual also in the later accounts, no spectroscopic information is given and no reference to laboratory spectroscopy. The band is caused by the strong CH stretching mode of both molecules, and the contributions of the molecules can not be disentangled.
	+
	+	[[https://doi.org/10.1086/345680\|Very Large Telescope Spectra of Carbon Stars in the Large Magellanic Cloud and Their Metallicity Dependence]]\\
	+	//Astrophys. J.// 580, (2002) L133,\\
	+	by\\
	+	M. Matsuura, A. A. Zijlstra, J. T. van Loon, I. Yamamura, A. J. Markwick, P. M. Woods, and L. B. F. M. Waters\\
	+	did not only reveal the 3.1 μm band, but also a much weaker one at 3.8 μm which is caused by //ν//<sub>2</sub> + //ν//<sub>5</sub> of acetylene, the combination of the CC stretch with the asymmetric bending mode. The longer wavelength band is comparatively stronger than in spectra of Galactic carbon stars. This, in turn, is interpreted in terms of, on average, larger C/O ratio in carbon stars of the LMC.
	+
	+	Further observations at these and even longer wavelengths of 7.5 μm (//ν//<sub>4</sub> + //ν//<sub>5</sub>) and 13 μm (//ν//<sub>5</sub>) have been carried out by several groups with the //Spitzer// Space Telescope.
	+
	+	==== Di- and Triacetylene ====
	+
	+	J. Bernard-Salas, E. Peeters, G. C. Sloan, J. Cami, S. Guiles, and J. R. Houck\\
	+	obtained\\
	+	[[https://doi.org/10.1086/509777\|The //Spitzer// IRS spectrum of SMP LMC 11]]\\
	+	//Astrophys. J.// 652, (2006) L29.\\
	+	The spectrum resembles that of the protoplanetary nebula V353 Aur, which is somewhat better known as CRL (or AFGL) 618. Butadiyne, HC<sub>4</sub>H, aka diacetylene, and hexatriyne, HC<sub>6</sub>H, aka as triacetylene, were iditified by their unresolved //Q//-branches of the //ν//<sub>8</sub> band of butadiyne at 15.9 μm and the //ν//<sub>11</sub> band of hexatriyne at 16.1 μm, respectively, as in the Galactic source.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

hc3n_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:23:53 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== Extragalactic Detection of HC3N =====
	+
	+	R. Mauersberger, C. Henkel, and L. J. Sage,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1990A%26A...236...63M\|Dense gas in nearby galaxies. III – HC<sub>3</sub>N as an extragalactic density probe]],\\
	+	//Astron. Astrophys.// 236, 63–68 (1990).
	+
	+	Source(s): NGC 253\\
	+	Facility: IRAM 30 m\\
	+
	+
	+	Comments:\\
	+	Six transitions were observed between 81.8 and 236.6 GHz with quantum numbers //J"// = 8, 9, 11, 14, 15, and 25.\\
	+	A tentative detection of the //J// = 10 – 9 transition toward IC342 or M82 with the IRAM 30 m telescope had been reported previously:\\
	+	C. Henkel, R. Mauersberger, and P. Schilke,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1988A%26A...201L..23H\|Molecules in external galaxies – The detection of CN, C<sub>2</sub>H, and HNC, and the tentative detection of HC<sub>3</sub>N]],\\
	+	//Astron. Astrophys.// 201, L23–L26 (1988).
	+
	+
	+	----
	+
	+	==== Detection of Extragalactic Vibrationally Excited HC3N ====
	+
	+	F. Costagliola and S. Aalto,\\
	+	[[https://doi.org/10.1051/0004-6361/200913370\|Vibrationally Excited HC<sub>3</sub>N in NGC 4418]],\\
	+	//Astron. Astrophys.// 515, Art. No. A71 (2010).
	+
	+	Source(s): NGC 4418\\
	+	Facility: IRAM 30 m; JCMT\\
	+
	+
	+	Comments:\\
	+	This seems to be the first report on the detection of a vibrationally excited molecule in an Extragalactic source. The //J"// = 9, 15, 16, 24, 27, 29, and 37 between 90.9 and 345.6 GHz were observed for the ground vibrational state; six of the eight components of //v//<sub>7</sub> = 1, //J"// = 9, 16, 24, and 27 and one component of //v//<sub>6</sub> = 1, //J"// = 24 were detected as well.
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005; H. S. P. Müller, 07, 2010
	+
	+	----
	+

hcl_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 17 Nov 2025 13:13:54 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== HCl in Extragalactic Sources =====
	+
	+	S. H. J. Wallström, S. Muller, E. Roueff, R. Le Gal, J. H. Black, and M. Gérin\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/201935860\|Chlorine-bearing Molecules in Molecular Absorbers at Intermediate Redshifts]]\\
	+	//Astron. Astrophys.// 566, (2014) Art. No. L6.\\
	+	The 1 – 0 transitions of H<sup>35</sup>Cl and H<sup>37</sup>Cl were observed with ALMA in the //z// ≈ 0.89 foreground galaxy of the lensed quasar PKA 1830−211. The isotopologs were both detected in the molecule rich SW image, where a H<sub>2</sub>Cl<sup>+</sup> to HCl ratio of ~1 was obtained, and unsurprisingly not toward the more atomic NE image, where a H<sub>2</sub>Cl<sup>+</sup> to HCl ratio of > 17 was deduced.
	+	HCl was also not observed in the //z// ≈ 0.68 foreground galaxy of the lensed quasar B 0218+357.\\
	+	\\
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 11, 2025
	+
	+	----

hcn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:42:49 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of HCN =====
	+
	+	L. J. Rickard, B. E. Turner, P. Palmer, M. Morris, and B. Zuckerman,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1977ApJ...214..390R\|Observations of extragalactic molecules. II - HCN and CS]],\\
	+	//Astrophys. J.// 214, 390-393 (1977).
	+
	+	Source(s): NGC253, M82\\
	+	Facility: NRAO 11m\\
	+	Comment: CS was searched for but remained undetected here.
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of H13CN ====
	+
	+	R. Mauersberger and C. Henkel\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...245..457M\|Dense gas in nearby galaxies. IV - The detection of N<sub>2</sub>H<sup>+</sup>, SiO, H<sup>13</sup>CO<sup>+</sup>, H<sup>13</sup>CN, and HN<sup>13</sup>C]],\\
	+	//Astron. Astrophys.// 245, 457-466 (1991).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of DCN ====
	+
	+	Y.-N. Chin, C. Henkel, T. J. Millar, J. B. Whiteoak, and R. Mauersberger, R.\\
	+	[[https://ui.adsabs.harvard.edu/abs/1996A%26A...312L..33C\|Molecular abundances in the Magellanic Clouds. II. Deuterated species in the LMC]],\\
	+	//Astron. Astrophys.// 312, L33-L36 (1996).
	+
	+	Source(s): LMC\\
	+	Facility: SEST 15m
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of HC15N ====
	+
	+	Y.-N. Chin, C. Henkel, N. Langer, and R. Mauersberger\\
	+	[[https://ui.adsabs.harvard.edu/abs/1999ApJ...512L.143C\|The Detection of Extragalactic <sup>15</sup>N: Consequences for Nitrogen Nucleosynthesis and Chemical Evolution]] ,\\
	+	//Astrophys. J.// 512, L143-L146 (1999).
	+
	+	Source(s): LMC\\
	+	Facility: SEST 15m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

hco_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:46:52 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of HCO =====
	+
	+	Some evidence for extragalactic HCO has been reported in
	+
	+	L. J. Sage and L. M. Ziurys,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1995ApJ...447..625S\|Toward Extragalactic Chemistry: Detections of N<sub>2</sub>H<sup>+</sup> and SiO in Nearby Galaxies]],\\
	+	//Astrophys. J.// 447, 625-629 (1991).
	+
	+	Source(s): NGC253, M82\\
	+	Facility: NRAO 12m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

hco-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:44:07 +0000

hcooh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Fri, 24 Apr 2020 13:19:19 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of Formic Acid, HCOOH, in Extragalactic Sources =====
	+
	+	B. Tercero, J. Cernicharo, S. Cuadrado, P. de Vicente, and M. Guélin\\
	+	used the Yebes 40 m telescopy in the 7 mm wavelength region (rest frequencies: 58.7 − 93.5 GHz) to study the molecular content of a foreground galaxy at //z// = 0.89 in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\
	+	//Astron. Astrophys.// 636, (2020) Art. No. L7.\\
	+	Formic acid, HCOOH, was identfied by five rotational transitions with //J// = 4 − 3 or 3 − 2 and //K<sub>a</sub>// = 0 or 1. The lines show good (three) to fairly reasonable signal-to-noise ratios.
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 4, 2020
	+
	+	----

hcs-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:49:31 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== Detection of Extragalactic HCS+ =====
	+
	+	S. Muller, A. Beelen, J. H. Black, S. J. Curran, C. Horellou, S. Aalto, F. Combes, M. Guélin, and C. Henkel\\
	+	reported on\\
	+	[[https://doi.org/10.1051/0004-6361/201220613\|A precise and accurate determination of the cosmic microwave background temperature at //z// = 0.89]]\\
	+	//Astron. Astrophys.// 551, (2013) Art. No. A109.\\
	+	The famous, but unnamed foreground galaxy in direction of the quasar PKS 1830–211 was studied with the Australia Telecope Compact Array (ATCA) and with the Plateau de Bure Interferometer (PdBI). ATCA observations at 7 mm revealed one significant line of HCS<sup>+</sup>, 2 – 1 near 45.3 GHz (rest frequency near 85.3 GHz). A detail of the spectrum (S. Muller, private communication) shows that overlap of this line with a much stronger //c//-C<sub>3</sub>H<sub>2</sub> line is almost negligible. Even though only one line was observed, the detection is probably fairly secure because of the limited line density.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 04, 2013
	+
	+	----
	+

hf_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:34:09 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== Hydrogen Fluoride, HF, in Extragalactic Sources =====
	+
	+	The //J// = 1 – 0 transition was observed in emission with the SPIRE instrument of the //Herschel// satellite toward the ultra-luminous infrared galaxie (ULIRG) Mrk 231:\\
	+	P. P. van der Werf, K. G. Isaak, R. Meijerink, et al.,\\
	+	[[https://doi.org/10.1051/0004-6361/201014682\|Black Hole Accretion and Star-Formation as Drivers of Gas Excitation and Chemistry in Markarian 231]]\\
	+	//Astron. Astrophys.// 518, (2010) Art. No. L42.\\
	+	The account is sparse, but a detail of the spectrum (van der Werf, private communication) clearly shows the line well-separated from a near-by water line.
	+
	+	The same transition was seen with the same instrument in absorption toward the ULIRG Arp 220 by\\
	+	N. Rangwala, P. R. Maloney, J. Glenn, et al.,\\
	+	[[https://doi.org/10.1088/0004-637X/743/1/94\|Observations of Arp 220 Using //Herschel//-SPIRE: An Unprecedented View of the Molecular Gas in an Extreme Star Formation Environment]]\\
	+	//Astrophys. J.// 743, (2011) Art. No. 94.
	+
	+	R. R. Monje, T. G. Phillips, R. Peng, D. C. Lis, D. A. Neufeld, and M. Emprechtinger\\
	+	reported on the\\
	+	[[https://doi.org/10.1088/2041-8205/742/2/L21\|Discovery of Hydrogen Fluoride in the Cloverleaf Quasar at //z// = 2.56]]\\
	+	//Astrophys. J.// 743, (2011) Art. No. 94;\\
	+	employing the CSO. Again, the //J// = 1 – 0 transition was observed in absorption.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 12, 2010; 04, 2013
	+
	+	----
	+

hnc_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:45:17 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On Extragalactic HNC =====
	+
	+	C. Henkel, P. Schilke, and R. Mauersberger\\
	+	reported on\\
	+	[[https://ui.adsabs.harvard.edu/abs/1988A%26A...201L..23H\|Molecules in External Galaxies – The Detection of CN, C<sub>2</sub>H, and HNC, and the Tentative detection of HC<sub>3</sub>N]],\\
	+	//Astron. Astrophys.// 201, L23–L26 (1988).\\
	+	The IRAM 30 m telescope was used to detect the //J// = 1 – 0 transition near 90.7 GHz in emission in the starburst galaxy IC 342.
	+
	+	Soon thereafter,\\
	+	R. Mauersberger and C. Henkel\\
	+	reported on\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...245..457M\|Dense Gas in Nearby Galaxies. IV – The Detection of N<sub>2</sub>H<sup>+</sup>, SiO, H<sup>13</sup>CO<sup>+</sup>, H<sup>13</sup>CN, and HN<sup>13</sup>C]],\\
	+	//Astron. Astrophys.// 245, 457–466 (1991).\\
	+	The IRAM 30 m telescope was used to detect the //J// = 1 – 0 transition near 87.1 GHz in emission in the Seyfert galaxy NGC 253.
	+
	+	F. Costagliola, S. Aalto, K. Sakamoto, S. Martín, R. Beswick, S. Muller, and H.-R. Klöckner\\
	+	carried out a\\
	+	[[https://doi.org/10.1051/0004-6361/201220634\|High-resolution mm and cm Study of the Obscured LIRG NGC 4418 – A Compact Obscured Nucleus Fed by In-falling Gas ?]],\\
	+	//Astron. Astrophys.// 565, Art. No. A66 (2013).\\
	+	Vibrationally excited HNC was detected for the first time with the SMA. the //J// = 3 – 2 transition of //v//<sub>2</sub> = 1 was detected. The //e//-component appeared as a weak shoulder to the ground state emission line, whereas the //f//-component was essentially not overlapped.
	+
	+
	+	----
	+
	+	Contributors: S. Thorwirth; 09/2005; H. S. P. Müller; 01, 2014
	+
	+	----
	+

hnco_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:19:30 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of HNCO =====
	+
	+	Nguyen-Q-Rieu, C. Henkel, J. M. Jackson, and R. Mauersberger, R.,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...241L..33N\|Detection of HNCO in external galaxies]],\\
	+	//Astron. Astrophys.// 241, L33-L36 (1990).
	+
	+	Source(s): NGC253, Maffei 2, IC342\\
	+	Facility: IRAM 30m\\
	+
	+
	+	a tentative detection of one transition had been reported previously:
	+
	+	Nguyen-Q-Rieu, N. Nakai, and J. M. Jackson,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1989A%26A...220...57N\|Dense molecular gas in galaxies - HCN, HCO<sup>+</sup>, and CS in M 82 and NGC 253]],\\
	+	//Astron. Astrophys.// 201, L23-L26 (1988).
	+
	+	Source(s): NGC253\\
	+	Facility: Nobeyama 45m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

hoc-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:48:11 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of HOC+ =====
	+
	+	A. Usero, S. García-Burillo, A. Fuente, J. Martín-Pintado, and N. J. Rodríguez-Fernandez,\\
	+	[[https://ui.adsabs.harvard.edu/abs/2004A%26A...419..897U\|Molecular gas chemistry in AGN. I. The IRAM 30 m survey of NGC 1068]],\\
	+	//Astron. Astrophys.// 419, 897-912 (2004).
	+
	+	Source(s): NGC1068\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth, 07/2005
	+
	+	----
	+

hoco-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 25 Feb 2019 21:38:07 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of HOCO+ =====
	+
	+	S. Martín et al., in preparation.\\
	+
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

l-c3h_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:22:28 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of Propynylidyne, l-C3H, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	Propynylidyne, //l//-C<sub>3</sub>H, was identified by its //J// = 7/2 – 5/2 transition of the lower energy fine structure component <sup>2</sup>Π<sub>1/2</sub> with a rest frequency of 76.2 GHz. The Λ-doubling was marginally resolved, the H-hyperfine structure was not resolved. The detection can probably be viewed as secure because of the strong signal and the moderate line number density.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

l-c3h-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Fri, 24 Apr 2020 11:18:12 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of Propynylidynium, //l//-C3H+, in Extragalactic Sources =====
	+
	+	B. Tercero, J. Cernicharo, S. Cuadrado, P. de Vicente, and M. Guélin\\
	+	used the Yebes 40 m telescopy in the 7 mm wavelength region (rest frequencies: 58.7 − 93.5 GHz) to study the molecular content of a foreground galaxy at //z// = 0.89 in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/202037837\|New Molecular Species at Redshift //z// = 0.89]]\\
	+	//Astron. Astrophys.// 636, (2020) Art. No. L7.\\
	+	The propynylidynium cation, //l//-C<sub>3</sub>H<sup>+</sup>, was identfied by three rotational transitions with good to reasonable signal-to-noise ratios and with //J// = 2 − 1 to 4 − 3.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 4, 2020
	+
	+	----

l-c3h2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:24:59 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of Propadienylidene, l-C3H2, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	Propadienylidene, //l//-C<sub>3</sub>H<sub>2</sub>, was identified by three //K<sub>a</sub>// = 1 //ortho// transitions (2 with //J"// = 2 and the lower //J"// = 3) and one with //K<sub>a</sub>// = 0 (//para//) and //J"// = 3. The OPR is compatible with the high temperature limit of 3. The abundance ratio //c//-C<sub>3</sub>H<sub>2</sub> to //l//-C<sub>3</sub>H<sub>2</sub> is about 25, between 3–5 in diffuse clouds, and 70 found in the dark cloud TMC-1.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

mecho_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:31:28 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of Ethanal, CH3CHO, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	5 Δ//K<sub>a</sub>// = 0 transitions with //K<sub>a</sub>// ≤ 1 and //J"// = 2 and 3 were detected between rest frequencies of 57.7 and 79.2 GHz. All transitions show resolved CH<sub>3</sub>-internal rotation splitting. One component of the lowest frequency transition is hidden in the noise.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

menh2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:31:08 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of the Methylamine, CH3NH2, in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	Methylamine, CH<sub>3</sub>NH<sub>2</sub>, is an asymmetric top rotor displaying considerable splitting caused by the internal rotation of the CH<sub>3</sub> group and the inversion of the NH<sub>2</sub> group. Three transitions with //K// = 1 – 0 have been identified; two with //J'// = //J"// = 1 at rest frequencies of 79008 and 89956 MHz, respectively, and one with //J'// = //J"// = 2 at 78135 MHz. Even though the number of lines is a bit small, the detection can probably be viewed as secure because of the moderate line number density.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+	----
	+

methylformiat

anonymous@undisclosed.example.com (Anonymous) — Tue, 04 Jan 2022 13:34:53 +0000

2022/01/04 14:30		current
Line 6:		Line 6:
	in the Large Magellanic Cloud]]**\\		in the Large Magellanic Cloud]]**\\
	//Astrophys. J. Lett.// 853, (2018) Art. No. L19.\\		//Astrophys. J. Lett.// 853, (2018) Art. No. L19.\\
-	ALMA was used at 1.3 mm to study the N 113 hot core region of the LMC. One line near 216.97 GHz was detected with reasonable signal-to-noise ratio toward the A1 peak and two more around 216.835 GHz were close to the noise limit. The derived column density is about a factor of 15 lower than that of methanol.\\	+	ALMA was used at 1.3 mm to study the N 113 hot core region of the LMC. One line of methyl formate near 216.97 GHz was detected with reasonable signal-to-noise ratio toward the A1 peak and two more lines around 216.835 GHz look a bit too strong. The derived column density is about a factor of 15 lower than that of methanol.\\

	----		----

n2h-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:45:43 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of N2H+ =====
	+
	+	R. Mauersberger and C. Henkel\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...245..457M\|Dense gas in nearby galaxies. IV - The detection of N<sub>2</sub>H<sup>+</sup>, SiO, H<sup>13</sup>CO<sup>+</sup>, H<sup>13</sup>CN, and HN<sup>13</sup>C]],\\
	+	//Astron. Astrophys.// 245, 457-466 (1991).
	+
	+	Source(s): NGC253, Maffei 2, IC342, M82, NGC6946\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

nh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:33:13 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== Detection of Imidogen, NH, in Extragalactic Sources =====
	+
	+	The detection of the imidogen radical, NH, with //ISO// LWS in an Extragalactic source was described first by\\
	+	E. González-Alfonso, H, A. Smith, J. Fischer, and J. Cernicharo,\\
	+	[[https://doi.org/10.1086/422868\|The Far-Infrared Spectrum of Arp 220]]\\
	+	//Astrophys. J.// 613, (2004) 247–261.\\
	+	The two overlapping strongest fine structure components of the //N// = 2 – 1 transition were clearly detected near 153.2 μm as well as the overlapping components of 3 – 2 near 102 μm. There is additional evidence near the noise level for the three weaker fine structure components of 2 – 1.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 10, 2010.
	+
	+	----
	+

nh2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:50:01 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On Amidogen, NH2, in Extragalactic Sources =====
	+
	+	Amidogen was detected with ALMA within cycle 0 observations in the unnamed foreground galaxy at //z// ≈ 0.89 toward the blazar PKS 1830–211 by\\
	+	S. Muller, F. Combes, M. Guélin, et al.,\\
	+	[[https://doi.org/10.1051/0004-6361/201423646\|An ALMA Early Science survey of molecular absorption lines toward PKS 1830–211 – Analysis of the absorption profiles]]\\
	+	//Astron. Astrophys.// 566, (2014) Art. No. A112.\\
	+	The strongest //J// = 1.5 – 1.5 and the weaker 1.5 – 0.5 fine structure components of the 1<sub>10</sub> – 1<sub>01</sub> transition of //para//-amidogen at 462446.5 and around 461440 MHz were detected in absorption, the latter with partially resolved <sup>14</sup>N hyperfine splitting.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 07, 2014.
	+
	+
	+	----
	+

nh2cn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 25 Feb 2019 21:38:07 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of NH2CN =====
	+
	+	S. Martín et al., in preparation.\\
	+
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

nh3_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 14:18:37 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of NH3 =====
	+
	+	R. N. Martin and P. T. P. Ho,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1979A%26A....74L...7M\|Detection of Extragalactic Ammonia]],\\
	+	//Astron. Astrophys.// 74, L7-L9 (1979).
	+
	+	Source(s): NGC253, IC342\\
	+	Facility: MPIfR 100m\\
	+
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

no_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:31:09 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of NO =====
	+
	+	S. Martín, R. Mauersberger, J. Martín-Pintado, S. García-Burillo, and C. Henkel,\\
	+	[[https://ui.adsabs.harvard.edu/abs/2003A%26A...411L.465M\|First detections of extragalactic SO<sub>2</sub>, NS and NO]],\\
	+	//Astron. Astrophys.// 411, L465-L468 (2003).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

ns_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:32:56 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of NS =====
	+
	+	S. Martín, R. Mauersberger, J. Martín-Pintado, S. García-Burillo, and C. Henkel,\\
	+	[[https://ui.adsabs.harvard.edu/abs/2003A%26A...411L.465M\|First detections of extragalactic SO<sub>2</sub>, NS and NO]],\\
	+	//Astron. Astrophys.// 411, L465-L468 (2003).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

o2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Sat, 15 Feb 2020 13:44:32 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On Extragalactic molecular Oxygen, O2 =====
	+
	+	J. Wang, D. Li, P. F. Goldsmith, Z.-Y. Zhang, Y. Gao, Y. Shi, S. Li, M. Fang, J. Li, and J. Zhang\\
	+	reported on\\
	+	[[https://doi.org/10.3847/1538-4357/ab612d\|Molecular Oxygen in the Nearest QSO Mrk 231]]\\
	+	//Astrophys. J.// 889, (2020) Art. No. 129.\\
	+	The 1<sub>1</sub> − 1<sub>0</sub> spin-flip transition at a rest frequency of 118750.34 MHz was seen in emission with NOEMA. The authors provide arguments why the detection is quite secure. While these are certainly fine, some caution is still advised because it is only one line thus far.\\
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 02, 2020
	+
	+	----
	+

ocs_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:46:08 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of OCS =====
	+
	+	R. Mauersberger, C. Henkel, and Y.-N. Chin,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1995A%26A...294...23M\|Dense gas in nearby galaxies - VIII. The detection of OCS]],\\
	+	//Astron. Astrophys.// 294, 23-32 (1991).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

oh_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:24:07 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of OH =====
	+
	+	L. Weliachew,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1971ApJ...167L..47W\|Detection of Interstellar OH in Two External Galaxies]],\\
	+	//Astrophys. J.// 167, L47-L52 (1971).
	+
	+	Source(s): NGC253, M82\\
	+	Facility: OVRO
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+
	+	----
	+

oh-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:33:46 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On OH+ in Extragalactic Sources =====
	+
	+	The first firm detection of of oxidaniumylidene or hydroxylium, OH<sup>+</sup>, was reported by\\
	+	P. P. van der Werf, K. G. Isaak, R. Meijerink, et al.,\\
	+	[[https://doi.org/10.1051/0004-6361/201014682\|Black Hole Accretion and Star-Formation as Drivers of Gas Excitation and Chemistry in Markarian 231]]\\
	+	//Astron. Astrophys.// 518, (2010) Art. No. L42.\\
	+	The account is somewhat sketchy, no rest frequencies are given and no references for these. An abundance has been derived, but no details are given. Only a broad overview spectrum is shown. Thus, one may be inclined to view this detection with some caution. On the other hand, all three fine structure components of the //N// = 1 – 0 transition seem to have been observed in emission toward the ultraluminous infrared galaxy Mrk 231with correct relative intensities employing the SPIRE instrument on board of the //Herschel// satellite. Given the ubiquity and high abundance of OH<sup>+</sup> in Galactic sources, the identification is probably correct.
	+
	+	There have been prior reports on the tentative detection of OH<sup>+</sup>:\\
	+	E. González-Alfonso, H, A. Smith, J. Fischer, and J. Cernicharo,\\
	+	[[https://doi.org/10.1086/422868\|The Far-Infrared Spectrum of Arp 220]]\\
	+	//Astrophys. J.// 613, (2004) 247–261\\
	+	discuss the possibility that absorption features of NH observed with //ISO// LWS at 100 and 150 μm may be affected by the //N// = 3 – 2 and 2 – 1 transitions, respectively, of OH<sup>+</sup>. However, they refrain from suggesting that there is strong evidence for OH<sup>+</sup> to be present.\\
	+	E. González-Alfonso, H. A. Smith, M. L. N. Ashby, J. Fischer, L. Spinoglio, and T. W. Grundy,\\
	+	[[https://doi.org/10.1086/527292\|High-excitation OH and H<sub>2</sub>O Lines in Markarian 231: The Molecular Signatures of Compact Far-infrared Continuum Sources]]\\
	+	//Astrophys. J.// 675, (2008) 303–315\\
	+	assigned two barely detected (about 2.5 σ) absorption features detected near 150 μm with //ISO// LWS to the two strongest fine structure components of the //N// = 2 – 1 transition.\\
	+	Detailed modeling may provide clues as to how plausible these observations are.
	+
	+	E. González-Alfonso, J. Fischer, S. Bruderer, et al.\\
	+	reported on\\
	+	[[https://doi.org/10.1051/0004-6361/201220466\|Excited OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, and H<sub>3</sub>O<sup>+</sup> in NGC 4418 and Arp 220]],\\
	+	//Astron. Astrophys.// 550, Art. No. A25 (2013);\\
	+	using PACS on board of the //Herschel// satellite. Transitions up to //N// = 4 – 3 with upper state energy of almost 500 K were detected in both sources. There may be even evidence for the 5 – 4 components (//E//<sub>up</sub> ≈ 700 K) in NGC 4418, but the intensities do not fit the model.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 10, 2010; 04, 2013.
	+
	+	----
	+

pn_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 04 Apr 2022 10:36:51 +0000

2022/04/04 11:39		current
Line 6:		Line 6:
	//Astron. Astrophys.// 659, (2022) Art. No. A158.\\		//Astron. Astrophys.// 659, (2022) Art. No. A158.\\
	\\		\\
-	The //J// = 2 – 1 and //J// = 3 – 2 transitions of PN near 93.980 and 140.968 GHz, respectively, were observed with ALMA in the course of a very extensive molecular line survey (84.2 to 373.2 GHz) of the central molecular zone (CMZ) of the near-by star-burst galaxy NGC 253. \\	+	The //J// = 2 – 1 and //J// = 3 – 2 transitions of PN near 93.980 and 140.968 GHz, respectively, were observed with ALMA in the course of a very extensive molecular line survey (84.2 to 373.2 GHz) of the central molecular zone (CMZ) of the near-by star-burst galaxy NGC 253. Both transitions were detected toward the source GMC 6 with good and fairly good signal-to-noise ratios (S/N), respectively. The //J// = 2 – 1 transition was also detected with reasonable S/N toward the source GMC 4. The two transitions detected toward GMC 6 constrain the excitation temperature to 4.4 ± 1.3 K.\\
	\\		\\
-	The <sup>32</sup>S/<sup>34</sup>S isotopic ratio is 16.2 ± 1.3, lower than the terrestrial ratio of 22, thus suggesting greater importance of supernovae in the elemental synthesis about 7.5 billion years ago compared to today. On the other hand, the <sup>32</sup>S/<sup>34</sup>S isotopic ratios are still lower, about 10.5, for CS and H<sub>2</sub>S in that galaxy, suggesting an even greater importance of higher-mass supernovae in the probably still denser ISM where these two molecules reside.\\	+	Other phosphorus-bearing molecules were searched for, but not detected. The PO/PN ratio was found to be < 1.3 for GMC 6, still compatible with PO/PN > 1 in Galactic sources. The PH<sub>3</sub>/PN ratio was found to be < 2.7 toward the same position.\\
	\\		\\
-

	----		----

sh-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:36:55 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On Extragalactic Sulfanylium, SH+ =====
	+
	+	S. Muller, H. S. P. Müller, J. H. Black, M. Gérin, F. Combes, S. Curran, E. Falgarone, M. Guélin, C. Henkel, S. Martín, K. M. Menten, E. Roueff, S. Aalto, A. Beelen, T. Wiklind, and M. A. Zwaan,\\
	+	reported on the\\
	+	[[https://doi.org/10.1051/0004-6361/201731405\|Detection of CH<sup>+</sup>, SH<sup>+</sup>, and Their <sup>13</sup>C- and <sup>34</sup>S-isotopologues toward PKS 1830–211]]\\
	+	//Astron. Astrophys.// 606, (2017) Art. No. A109.\\
	+	\\
	+	The //N// = 1 – 0, //J// = 2 – 1 fine structure transitions of SH<sup>+</sup> and <sup>34</sup>SH<sup>+</sup> were observed with ALMA redshifted from about 526.0 and 525.1 GHz to about 279.9 and 278.4 GHz. The molecular cations were only detected toward the SW image representing denser material with a fairly high molecular fraction overall. They were not seen toward the NE image representing less dense material with a lower molecular fraction overall. Formation of SH<sup>+</sup> thus appears to require higher densities than that best suited for OH<sup>+</sup> or H<sub>2</sub>O<sup>+</sup>.\\
	+	\\
	+	The <sup>32</sup>S/<sup>34</sup>S isotopic ratio is 16.2 ± 1.3, lower than the terrestrial ratio of 22, thus suggesting greater importance of supernovae in the elemental synthesis about 7.5 billion years ago compared to today. On the other hand, the <sup>32</sup>S/<sup>34</sup>S isotopic ratios are still lower, about 10.5, for CS and H<sub>2</sub>S in that galaxy, suggesting an even greater importance of higher-mass supernovae in the probably still denser ISM where these two molecules reside.\\
	+	\\
	+	The isotopolog <sup>34</sup>SH<sup>+</sup> has not yet been detected in a Galactic source.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 11, 2017
	+
	+	----
	+

sio_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:30:19 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of SiO =====
	+
	+	R. Mauersberger and C. Henkel\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...245..457M\|Dense gas in nearby galaxies. IV - The detection of N<sub>2</sub>H<sup>+</sup>, SiO, H<sup>13</sup>CO<sup>+</sup>, H<sup>13</sup>CN, and HN<sup>13</sup>C]],\\
	+	//Astron. Astrophys.// 245, 457-466 (1991).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

so_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:29:51 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of SO =====
	+
	+	L. E. B. Johansson,\\
	+	[[https://ui.adsabs.harvard.edu/abs/1991IAUS..146....1J\|Interstellar Gas in the Magellanic Clouds: SEST Observations of CO and Other Molecules]],\\
	+	in //Dynamics of Galaxies and Their Molecular Cloud Distributions//:\\
	+	Proceedings of the 146th Symposium of the International Astronomical Union,\\
	+	Edited by F. Combes and Fabienne Casoli. International Astronomical Union. Symposium no. 146,\\
	+	Kluwer Academic Publishers, Dordrecht, 1991, p. 1-8
	+
	+	Source(s): LMC\\
	+	Facility: SEST 15m\\
	+
	+
	+
	+	----
	+
	+	==== First Extragalactic Detection of 34SO ====
	+
	+	One line that may arise from <sup>34</sup>SO
	+
	+	has been reported in
	+
	+	S. Martín, R. Mauersberger, J. Martín-Pintado, S. García-Burillo, and C. Henkel,\\
	+	[[https://ui.adsabs.harvard.edu/abs/2003A%26A...411L.465M\|First detections of extragalactic SO<sub>2</sub>, NS and NO]],\\
	+	//Astron. Astrophys.// 411, L465-L468 (2003).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

so_plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Mon, 25 Feb 2019 21:41:12 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of SO+ in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[http://dx.doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	SO<sup>+</sup> was identified by its //J// = 3/2 – 1/2 transition of the lower energy fine structure component <sup>2</sup>Π<sub>1/2</sub> with rest frequencies of 69.4 and 69.8 GHz because of the Λ-doubling. The lower frequency //e// component was blended with the //F// = 5/2 – 3/2 hyperfine component of the <sup>2</sup>Π<sub>1/2</sub>, //J// = 3/2 – 1/2, //f// transition of NS. The different contributions could be disentangled because of the well-resolved hyperfine structure of NS.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+
	+	----
	+

so-plus_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:34:25 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== On the Detection of SO+ in Extragalactic Sources =====
	+
	+	S. Muller, A. Beelen, M. Guélin, S. Aalto, J. H. Black, F. Combes, S. J. Curran, P. Theule, and S. N. Longmore\\
	+	used the Australia Telescope Compact Array (ATCA) to study the molecular content of a foreground galaxy at //z// = 0.89 (FG0.89 consisting of two subsources, FG0.89SW and FG0.89NO) in absorption toward the quasar PKS 1830-211:\\
	+	[[https://doi.org/10.1051/0004-6361/201117096\|Molecules at //z// = 0.89: A 4-mm-Rest-Frame Absorption-Line Survey toward PKS 1830-211]]\\
	+	//Astron. Astrophys.// 535, (2011) Art. No. A103.\\
	+	SO<sup>+</sup> was identified by its //J// = 3/2 – 1/2 transition of the lower energy fine structure component <sup>2</sup>Π<sub>1/2</sub> with rest frequencies of 69.4 and 69.8 GHz because of the Λ-doubling. The lower frequency //e// component was blended with the //F// = 5/2 – 3/2 hyperfine component of the <sup>2</sup>Π<sub>1/2</sub>, //J// = 3/2 – 1/2, //f// transition of NS. The different contributions could be disentangled because of the well-resolved hyperfine structure of NS.
	+
	+
	+	----
	+
	+	Contributor(s): H. S. P. Müller; 5, 2012
	+
	+
	+	----
	+

so2_extragalactic

anonymous@undisclosed.example.com (Anonymous) — Tue, 22 Oct 2019 11:47:46 +0000

2026/04/12 12:18	current
Line 1:	Line 1:
	+	===== First Extragalactic Detection of SO2 =====
	+
	+	S. Martín, R. Mauersberger, J. Martín-Pintado, S. García-Burillo, and C. Henkel,\\
	+	[[https://ui.adsabs.harvard.edu/abs/2003A%26A...411L.465M\|First detections of extragalactic SO<sub>2</sub>, NS and NO]],\\
	+	//Astron. Astrophys.// 411, L465-L468 (2003).
	+
	+	Source(s): NGC253\\
	+	Facility: IRAM 30m
	+
	+
	+	----
	+
	+	Contributor(s): S. Thorwirth; 09/2005
	+
	+	----
	+

2019/02/25 22:38		current
Line 2:		Line 2:

	A. A. Stark and R. S. Wolff,\\		A. A. Stark and R. S. Wolff,\\
-	[[http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1979ApJ...229..118S&db_key=AST&data_type=HTML&format=&high=42db7152ee04699\|Some observations of extragalactic HCO<sup>+</sup> and HCN]],\\	+	[[https://ui.adsabs.harvard.edu/abs/1979ApJ...229..118S\|Some observations of extragalactic HCO<sup>+</sup> and HCN]],\\
	//Astrophys. J.// 229, 118-120 (1979).		//Astrophys. J.// 229, 118-120 (1979).

Line 15:		Line 15:

	R. Mauersberger and C. Henkel\\		R. Mauersberger and C. Henkel\\
-	[[http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1991A%26A...245..457M&db_key=AST&data_type=HTML&format=&high=42db7152ee09932\|Dense gas in nearby galaxies. IV - The detection of N<sub>2</sub>H<sup>+</sup>, SiO, H<sup>13</sup>CO<sup>+</sup>, H<sup>13</sup>CN, and HN<sup>13</sup>C]],\\	+	[[https://ui.adsabs.harvard.edu/abs/1991A%26A...245..457M\|Dense gas in nearby galaxies. IV - The detection of N<sub>2</sub>H<sup>+</sup>, SiO, H<sup>13</sup>CO<sup>+</sup>, H<sup>13</sup>CN, and HN<sup>13</sup>C]],\\
	//Astron. Astrophys.// 245, 457-466 (1991).		//Astron. Astrophys.// 245, 457-466 (1991).

Line 27:		Line 27:

	Y.-N. Chin, C. Henkel, T. J. Millar, J. B. Whiteoak, and R. Mauersberger, R.\\		Y.-N. Chin, C. Henkel, T. J. Millar, J. B. Whiteoak, and R. Mauersberger, R.\\
-	[[http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1996A%26A...312L..33C&db_key=AST&data_type=HTML&format=&high=42db7152ee14533\|Molecular abundances in the Magellanic Clouds. II. Deuterated species in the LMC]],\\	+	[[https://ui.adsabs.harvard.edu/abs/1996A%26A...312L..33C3\|Molecular abundances in the Magellanic Clouds. II. Deuterated species in the LMC]],\\
	//Astron. Astrophys.// 312, L33-L36 (1996).		//Astron. Astrophys.// 312, L33-L36 (1996).

	Source(s): LMC\\		Source(s): LMC\\
	Facility: SEST 15m		Facility: SEST 15m
-

	----		----

	Contributor(s): S. Thorwirth; 09/2005		Contributor(s): S. Thorwirth; 09/2005
-

	----		----