Identification and characterization of nascent planetary nebulae with OH and H2O masers

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Table 2

List of all known maser-emitting PNe and candidates.

			Maser emission^a					References^b
Name	Alt. name	Galactic coordinates	SiO	H₂O	OH	Status^c	SiO	H₂O	OH	Nature
IRAS 07027–7934	Vo 1	291.375–26.294	−	No	Yes	IP	−	1	TW	2, 3
IRAS 15103–5754	GLMP 405	320.907–00.293	No	Yes	−	IP	4	5	−	5, 6
IRAS 16029–5055	SCHD 68	331.158+00.781	−	−	Yes	IC	−	−	7	TW
IRAS 16333–4807		336.644–00.696	No	Yes	Yes	IP	4	8	9	8, 9
IRAS 16372–4808	SCHD 117	337.064–01.173	No	No	Yes	IC	4	10	11	12
IRAS 17150–3754	PBZ 1	349.351–00.211	−	No	Yes	IC	−	−	13	13
IRAS 17347–3139	RPZM 28	356.801–00.055	No	Yes	Yes	IP	4	14	15	14, 16, 15, TW
IRAS 17371–2747	JaSt 23	000.340+01.574	No	−	Yes	IP	4	−	17	18, 19
IRAS 17375–2759	PBOZ 26	000.208+01.412	−	−	Yes	IC	−	−	20	19, TW
IRAS 17393–2727	OH 0.9+1.3	000.892+01.341	No	−	Yes	IP	4	−	13	13, 21, TW
IRAS 17487–1922	OH 008.9+03.7	008.905+03.712	−	No	Yes	IC	−	TW	TW	TW
IRAS 17494–2645	SCHB 220	002.640–00.191	−	No	Yes	IC	−	TW	22	12, TW
IRAS 18019–2216	SCHB 281	007.958–00.393	−	Yes	Yes	IC	−	TW	23	12, TW
IRAS 18061–2505	MaC 1-10	005.974–02.611	No	Yes	No	IP	4	24	24	24, 25
IRAS 18213–1245A		018.526+00.150	−	Yes	Yes	IC	−	26	27	TW
IRAS 18443–0231	RFS 505	030.234–00.138	−	Yes	No	IC	−	TW	TW	TW
IRAS 18464–0140	OH 31.21–0.18	031.213–00.180	−	Yes	Yes	IC	−	28	28	TW
IRAS 18480+0008		033.023+00.279	−	Yes	Yes	IC	−	TW	27	TW
IRAS 18508+0047	GPSR5 33.906–0.044	033.906–00.043	−	No	Yes	IC	−	TW	27	TW
IRAS 19035+0801	PM 1-279	041.787+00.488	−	No	Yes	IC	−	TW	TW	TW
IRAS 19176+1251	GLMP 898	047.688–00.302	−	No	Yes	IC	−	29	27	TW
IRAS 19194+1548		050.480+00.705	−	No	Yes	IC	−	TW	27	30, TW
IRAS 19219+0947	Vy 2-2	045.498–02.703	No	No	Yes	IP	4	31	32	33, 32
IRAS 19255+2123	K 3-35	056.096+02.094	No	Yes	Yes	IP	4	34	34	35, 34, TW
OH 25.646–0.003		025.646–00.003	−	No	Yes	IC	−	27	TW	TW
OH 341.681+00.264		341.681+00.263	No	−	Yes	IC	4	−	11	12

Notes. ^a ‘−’: no interferometric observations available. ^b Reference for the interferometric maser emission detected. In the nature column, we provide references that have contributed to classifying the source as a PN candidate or confirmed PN. TW: This work. ^c As defined in Table 1. 1. Suárez et al. (2009). 2. Menzies & Wolstencroft (1990). 3. Surendiranath (2002). 4. Cala et al. (2024a). 5. Gómez et al. (2015b). 6. Suárez et al. (2015). 7. Sevenster et al. (1997). 8. Uscanga et al. (2014). 9. Qiao et al. (2016a). 10. Deacon et al. (2007). 11. Qiao et al. (2016b). 12. Cala et al. (2022). 13. Pottasch et al. (1987). 14. de Gregorio-Monsalvo et al. (2004). 15. Tafoya et al. (2009). 16. Gómez et al. (2005). 17. Sevenster (2002). 18. Jacoby & Van de Steene (2004). 19. Uscanga et al. (2012). 20. Zijlstra et al. (1989). 21. García-Hernández et al. (2007). 22. Qiao et al. (2018). 23. Qiao et al. (2020). 24. Gómez et al. (2008). 25. Miranda et al. (2021). 26. Walsh et al. (2014). 27. Beuther et al. (2019). 28. Forster & Caswell (1999). 29. Gómez et al. (2015a). 30. Sabin et al. (2014). 31. Gómez et al. (1990). 32. Seaquist & Davis (1983). 33. Vyssotsky et al. (1945). 34. Miranda et al. (2001). 35. Miranda et al. (2000). IC: interferometrically confirmed maser-emitting PN candidate. IP: interferometrically confirmed maser-emitting PN.

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