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QIA16 - Unusual Shock-excited OH Maser Emission in a Young Planetary Nebula

Short title: Qiao et al. (2016)
Authors: Qiao, Hai-Hua Walsh, Andrew J. Gómez, José F. Imai, Hiroshi Green, James A. Dawson, Joanne R. Shen, Zhi-Qiang Ellingsen, Simon P. Breen, Shari L. Jones, Paul A. Gibson, Steven J. Cunningham, Maria R.
Journal: The Astrophysical Journal, Volume 817, Issue 1, article id. 37, 7 pp. (2016).
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Abstract
We report on OH maser emission toward G336.644-0.695 (IRAS 16333-4807), which is a H₂O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3-35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H₂O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s^-1). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of &tilde2 to &tilde10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN. eprintid: arXiv:1512.00592

Abstract

We report on OH maser emission toward G336.644-0.695 (IRAS 16333-4807), which is a H₂O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3-35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H₂O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s^-1). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of &tilde2 to &tilde10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN. eprintid:

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Detection table from Qiao et al. (2016)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Frequency	V_peak	F_peak	∫F dv	Telescope	Detection	Type
	(J2000)	(J2000)	(deg.)	(deg.)			(MHz)	(km/s)	(Jy)	(Jy*km/s)		Yes/No
1	16 37 6.6	-48 13 42.4	336.6438	-0.6954	G336.644-0.695	IRAS 16333-4807	1612	-45.2	0.19	0.43	PRS	+H₂O +OH	EVOLVED
2	16 37 6.6	-48 13 42.3	336.6438	-0.6954	G336.644-0.695	IRAS 16333-4807	1667	-45.5	0.32	0.6	PRS	+H₂O +OH	EVOLVED
3	16 37 6.6	-48 13 42.4	336.6438	-0.6955	G336.644-0.695	IRAS 16333-4807	1720	-60.73	0.79	0.71	PRS	+H₂O +OH	EVOLVED
4	16 37 6.6	-48 13 42.6	336.6438	-0.6956	G336.644-0.695	IRAS 16333-4807	1720	-55.3	0.13	0.16	PRS	+H₂O +OH	EVOLVED
5	16 37 6.5	-48 13 42.4	336.6437	-0.6954	G336.644-0.695	IRAS 16333-4807	1720	-49	0.16	0.2	PRS	+H₂O +OH	EVOLVED
6	16 37 6.6	-48 13 42.5	336.6439	-0.6956	G336.644-0.695	IRAS 16333-4807	1720	-24.7	0.27	0.48	PRS	+H₂O +OH	EVOLVED
7	16 37 6.6	-48 13 41.5	336.6441	-0.6954	G336.644-0.695	IRAS 16333-4807	1720	-22.9	0.16	0.33	PRS	+H₂O +OH	EVOLVED
8	16 37 6.6	-48 13 43.3	336.6437	-0.6957	G336.644-0.695	IRAS 16333-4807	1612	-45.2	0.12	0.27	PRS	+H₂O +OH	EVOLVED
9	16 37 6.5	-48 13 42.3	336.6437	-0.6952	G336.644-0.695	IRAS 16333-4807	1667	-45.4	0.14	0.31	PRS	+H₂O +OH	EVOLVED
10	16 37 6.6	-48 13 43	336.6437	-0.6956	G336.644-0.695	IRAS 16333-4807	1720	-55.1	0.26	0.66	PRS	+H₂O +OH	EVOLVED
11	16 37 6.7	-48 13 42.9	336.6438	-0.6957	G336.644-0.695	IRAS 16333-4807	1720	-23.2	0.29	0.78	PRS	+H₂O +OH	EVOLVED

DSS colored	2MASS colored	WISE colored
SDSS color	IRAC color I1,I2,I4	GLIMPSE 360
PACS color (70-160 um)	SPIRE color (250-500 um)	NVSS (1.4GHz)
ATLASGAL 870 um	ATLASGAL 870 um + Planck	Bolocam 1.1 mm
UKIDSS K	2MASS K

select MAX(oh_data_all.ra_hms) as ra_hms,MAX(oh_data_all.dec_dms) as dec_dms,MAX(oh_data_all.source_name) as source_name,MAX(oh_data_all.ra) as ra,MAX(oh_data_all.dec) as dec,MAX(oh_data_all.l) as l,MAX(oh_data_all.b) as b,MAX(oh_data_all.grp) as grp,MAX(oh_data_all.other_name) as other_name,MAX(oh_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(oh_data_all.freq) as freq,MAX(oh_data_all.vrange) as vrange,MAX(oh_data_all.vpeak) as vpeak,MAX(oh_data_all.peak) as peak,MAX(oh_data_all.fwhm) as fwhm,MAX(oh_data_all.int) as int,MAX(oh_data_all.rms) as rms,MAX(oh_data_all.units) as units,MAX(oh_data_all.units_rms) as units_rms,MAX(oh_data_all.date_txt) as date_txt,MAX(oh_data_all.telescope_ref) as telescope_ref,MAX(oh_data_all.telescope_conf) as telescope_conf,MAX(oh_data_all.v_step) as v_step,MAX(oh_data_all.beam) as beam,MAX(oh_data_all.beam_maj) as beam_maj,MAX(oh_data_all.beam_min) as beam_min,MAX(oh_data_all.beam_pa) as beam_pa,MAX(oh_data_all.ref) as ref,MAX(oh_data_all.list_ref) as list_ref,MAX(oh_data_all.ascii) as ascii,MAX(oh_data_all.image) as image,MAX(oh_data_all.descr) as descr,MAX(oh_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(oh_data_all.dist) as dist,MAX(oh_data_all.date_txt) as date_txt,MAX(line_det) as line_det,MAX(type) as type,MAX(simbad_types_cat) as simbad_types_cat FROM oh_data_all  LEFT JOIN all_objects_withmet ON oh_data_all.grp=all_objects_withmet.group_name LEFT JOIN object_categories ON all_objects_withmet.group_name = object_categories.group_name_cat AND object_categories.tbl_cat = 'all_objects_withmet' LEFT JOIN transitions ON oh_data_all.line=transitions."Line"  WHERE ref ilike 'QIA16' AND detected=true AND hide=false GROUP BY ref

select oh_data_all.ra_hms,oh_data_all.dec_dms,oh_data_all.source_name,oh_data_all.ra,oh_data_all.dec,oh_data_all.l,oh_data_all.b,oh_data_all.grp,oh_data_all.other_name,oh_data_all.other_desc,oh_data_all.thermal,oh_data_all.freq,oh_data_all.vrange,oh_data_all.vpeak,oh_data_all.peak,oh_data_all.fwhm,oh_data_all.int,oh_data_all.rms,oh_data_all.units,oh_data_all.units_rms,oh_data_all.date_txt,oh_data_all.telescope_ref,oh_data_all.telescope_conf,oh_data_all.v_step,oh_data_all.beam,oh_data_all.beam_maj,oh_data_all.beam_min,oh_data_all.beam_pa,oh_data_all.ref,oh_data_all.list_ref,oh_data_all.ascii,oh_data_all.image,oh_data_all.descr,oh_data_all.id,oh_data_all.mjy_flag,oh_data_all.rms_mjy_flag,oh_data_all.dist,oh_data_all.date_txt,line_det,type,simbad_types_cat FROM oh_data_all   LEFT JOIN all_objects_withmet ON oh_data_all.grp=all_objects_withmet.group_name LEFT JOIN object_categories ON all_objects_withmet.group_name = object_categories.group_name_cat AND object_categories.tbl_cat = 'all_objects_withmet' LEFT JOIN transitions ON oh_data_all.line=transitions."Line"  WHERE ref ilike 'QIA16' AND detected=true AND hide=false ORDER BY detected DESC,id

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QIA16 - Unusual Shock-excited OH Maser Emission in a Young Planetary Nebula

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Detection table from Qiao et al. (2016)