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GRE04 - A Survey for Water Maser Emission toward Planetary Nebulae: New Detection in IRAS 17347-3139

Short title: de Gregorio-Monsalvo et al. (2004)
Authors: de Gregorio-Monsalvo, Itziar Gómez, Yolanda Anglada, Guillem Cesaroni, Riccardo Miranda, Luis F. Gómez, José F. Torrelles, José M.
Journal: The Astrophysical Journal, Volume 601, Issue 2, pp. 921-929.
Bibcode:

Target type: pAGB_PN

Abstract
We report on a water maser survey toward a sample of 27 planetary nebulae (PNe) using the Robledo de Chavela and Medicina single-dish antennas, as well as the Very Large Array (VLA). Two detections have been obtained: the already known water maser emission in K3-35, and a new cluster of masers in IRAS 17347-3139. This low rate of detections is compatible with the short lifetime of water molecules in PNe (~100 yr). The water maser cluster at IRAS 17347-3139 are distributed on a ellipse of size ~=0.2""ࡦ.1"", spatially associated with compact 1.3 cm continuum emission (simultaneously observed with the VLA). From archive VLA continuum data at 4.9, 8.4, and 14.9 GHz, a spectral index alpha=0.76+/-0.03 (S_nu~nu^alpha) is derived for this radio source, which is consistent with either a partially optically thick ionized region or an ionized wind. However, the latter scenario can be ruled out by mass-loss considerations, thus indicating that this source is probably a young PN. The spatial distribution and the radial velocities of the water masers are suggestive of a rotating and expanding maser ring, tracing the innermost regions of a torus formed at the end of the asymptotic giant branch phase. Given that the 1.3 cm continuum emission peak is located near one of the tips of the major axis of the ellipse of masers, we speculate on a possible binary nature of IRAS 17347-3139, where the radio continuum emission could belong to one of the components and the water masers would be associated with a companion. eprintid: arXiv:astro-ph/0310415

Abstract

We report on a water maser survey toward a sample of 27 planetary nebulae (PNe) using the Robledo de Chavela and Medicina single-dish antennas, as well as the Very Large Array (VLA). Two detections have been obtained: the already known water maser emission in K3-35, and a new cluster of masers in IRAS 17347-3139. This low rate of detections is compatible with the short lifetime of water molecules in PNe (~100 yr). The water maser cluster at IRAS 17347-3139 are distributed on a ellipse of size ~=0.2""ࡦ.1"", spatially associated with compact 1.3 cm continuum emission (simultaneously observed with the VLA). From archive VLA continuum data at 4.9, 8.4, and 14.9 GHz, a spectral index alpha=0.76+/-0.03 (S_nu~nu^alpha) is derived for this radio source, which is consistent with either a partially optically thick ionized region or an ionized wind. However, the latter scenario can be ruled out by mass-loss considerations, thus indicating that this source is probably a young PN. The spatial distribution and the radial velocities of the water masers are suggestive of a rotating and expanding maser ring, tracing the innermost regions of a torus formed at the end of the asymptotic giant branch phase. Given that the 1.3 cm continuum emission peak is located near one of the tips of the major axis of the ellipse of masers, we speculate on a possible binary nature of IRAS 17347-3139, where the radio continuum emission could belong to one of the components and the water masers would be associated with a companion. eprintid: arXiv:astro-ph/0310415

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Detection table from de Gregorio-Monsalvo et al. (2004)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_range	V_peak	F_peak	Detection	Class	Dist. (parallax)
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(km/s)	(km/s)	(Jy)	Yes/No		(kpc)
1	17 38 0.7	-31 40 54	356.8016	-0.0554	G356.802-0.055	IRAS 17347-3139	22 GHz;	-68.2;-61.8	-68.1	0.7	+H₂O +OH	SFR_MIXED
	17 38 0.7	-31 40 54	356.8016	-0.0554	G356.802-0.055	IRAS 17347-3139	22 GHz;	-68.2;-61.8	-61.8	1.36	+H₂O +OH	SFR_MIXED
	17 38 0.7	-31 40 54	356.8016	-0.0554	G356.802-0.055	IRAS 17347-3139	22 GHz;	-68.2;-61.8	-68.2	1.7	+H₂O +OH	SFR_MIXED
	17 38 0.7	-31 40 54	356.8016	-0.0554	G356.802-0.055	IRAS 17347-3139	22 GHz;	-68.2;-61.8	-62.1	2.1	+H₂O +OH	SFR_MIXED
5	19 27 44	+21 30 3.4	56.0960	2.0937	G56.096+2.094	K3-35	22 GHz;		22.4	0.27	+H₂O +OH	EVOLVED
	19 27 44	+21 30 3.4	56.0960	2.0937	G56.096+2.094	K3-35	22 GHz;		22.6	0.933	+H₂O +OH	EVOLVED
	19 27 44	+21 30 3.4	56.0960	2.0937	G56.096+2.094	K3-35	22 GHz;		22.4	1.33	+H₂O +OH	EVOLVED
	19 27 44	+21 30 3.4	56.0960	2.0937	G56.096+2.094	K3-35	22 GHz;		22.4	1.41	+H₂O +OH	EVOLVED
	19 27 44	+21 30 3.4	56.0960	2.0937	G56.096+2.094	K3-35	22 GHz;		22.4	1.33	+H₂O +OH	EVOLVED
	19 27 44	+21 30 3.4	56.0960	2.0937	G56.096+2.094	K3-35	22 GHz;		22.4	2.1	+H₂O +OH	EVOLVED

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

select MAX(h2o_data_all.ra_hms) as ra_hms,MAX(h2o_data_all.dec_dms) as dec_dms,MAX(h2o_data_all.source_name) as source_name,MAX(h2o_data_all.ra) as ra,MAX(h2o_data_all.dec) as dec,MAX(h2o_data_all.l) as l,MAX(h2o_data_all.b) as b,MAX(h2o_data_all.grp) as grp,MAX(h2o_data_all.other_name) as other_name,MAX(h2o_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(h2o_data_all.line) as line,MAX(h2o_data_all.vrange) as vrange,MAX(h2o_data_all.vpeak) as vpeak,MAX(h2o_data_all.peak) as peak,MAX(h2o_data_all.fwhm) as fwhm,MAX(h2o_data_all.int) as int,MAX(h2o_data_all.rms) as rms,MAX(h2o_data_all.units) as units,MAX(h2o_data_all.units_rms) as units_rms,MAX(h2o_data_all.date_txt) as date_txt,MAX(h2o_data_all.telescope_ref) as telescope_ref,MAX(h2o_data_all.telescope_conf) as telescope_conf,MAX(h2o_data_all.v_step) as v_step,MAX(h2o_data_all.beam) as beam,MAX(h2o_data_all.beam_maj) as beam_maj,MAX(h2o_data_all.beam_min) as beam_min,MAX(h2o_data_all.beam_pa) as beam_pa,MAX(h2o_data_all.ref) as ref,MAX(h2o_data_all.list_ref) as list_ref,MAX(h2o_data_all.ascii) as ascii,MAX(h2o_data_all.url) as url,MAX(h2o_data_all.image) as image,MAX(h2o_data_all.image2) as image2,MAX(h2o_data_all.image3) as image3,MAX(h2o_data_all.descr) as descr,MAX(h2o_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(h2o_data_all.dist) as dist,1 as dist_parallax,MAX(h2o_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 h2o_data_all  LEFT JOIN all_objects_withmet ON h2o_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 h2o_data_all.line=transitions."Line"  WHERE ref ilike 'GRE04' AND detected=true AND hide=false GROUP BY ref

select h2o_data_all.ra_hms,h2o_data_all.dec_dms,h2o_data_all.source_name,h2o_data_all.ra,h2o_data_all.dec,h2o_data_all.l,h2o_data_all.b,h2o_data_all.grp,h2o_data_all.other_name,h2o_data_all.other_desc,h2o_data_all.thermal,h2o_data_all.line,h2o_data_all.vrange,h2o_data_all.vpeak,h2o_data_all.peak,h2o_data_all.fwhm,h2o_data_all.int,h2o_data_all.rms,h2o_data_all.units,h2o_data_all.units_rms,h2o_data_all.date_txt,h2o_data_all.telescope_ref,h2o_data_all.telescope_conf,h2o_data_all.v_step,h2o_data_all.beam,h2o_data_all.beam_maj,h2o_data_all.beam_min,h2o_data_all.beam_pa,h2o_data_all.ref,h2o_data_all.list_ref,h2o_data_all.ascii,h2o_data_all.url,h2o_data_all.image,h2o_data_all.image2,h2o_data_all.image3,h2o_data_all.descr,h2o_data_all.id,h2o_data_all.mjy_flag,h2o_data_all.rms_mjy_flag,h2o_data_all.dist,h2o_data_all.dist_parallax,h2o_data_all.date_txt,line_det,type,simbad_types_cat FROM h2o_data_all   LEFT JOIN all_objects_withmet ON h2o_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 h2o_data_all.line=transitions."Line"  WHERE ref ilike 'GRE04' AND detected=true AND hide=false ORDER BY detected DESC,id

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GRE04 - A Survey for Water Maser Emission toward Planetary Nebulae: New Detection in IRAS 17347-3139

View as list of objects

Detection table from de Gregorio-Monsalvo et al. (2004)