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YOO14 - SiO and H2O Maser Survey toward Post-asymptotic Giant Branch and Asymptotic Giant Branch Stars

Short title: Yoon et al. (2014)
Authors: Yoon, Dong-Hwan Cho, Se-Hyung Kim, Jaeheon Yun, Young joo Park, Yong-Sun
Journal: The Astrophysical Journal Supplement, Volume 211, Issue 1, article id. 15, 27 pp. (2014).
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Target type: pAGB_PN
Observations category: star.general

Abstract
We performed simultaneous observations of SiO v = 1, 2, ²⁹SiO v = 0, J = 1-0 and H₂O 6₁₆-5₂₃ maser lines toward 143 AGB and 164 post-asymptotic giant branch (AGB) stars in order to investigate how evolutionary characteristics from AGB to post-AGB stars appear in both SiO and H₂O maser emissions. The observations were carried out from 2011 February to 2012 March using the Korean VLBI Network single-dish telescopes. We have detected SiO and/or H₂O maser emission from 21 sources out of 164 post-AGB stars including 12 new detections. Of 143 AGB stars, we detected SiO and/or H₂O maser emission from 44 stars including 24 new detections. SiO v = 2, J = 1-0 maser emission without a SiO v = 1 maser was detected from 7 sources among 14 SiO-detected post-AGB stars, and the intensity of the SiO v = 2, J = 1-0 maser tends to be much stronger than that of SiO v = 1, which is different from those of AGB stars. This may be related to the development of hot dust shells according to the evolutionary processes of post-AGB stars. We also found that both SiO and H₂O masers were detected in the blue group (LI, or Left of IRAS), while only the H₂O maser was detected in the red group (RI, or Right of IRAS) for post-AGB stars. These different detection rates between SiO and H₂O masers may originate from the different abundances of masing molecules in the circumstellar envelope according to the different mass and expansion velocity between LI and RI regions together with their evolutionary stages.

Abstract

We performed simultaneous observations of SiO v = 1, 2, ²⁹SiO v = 0, J = 1-0 and H₂O 6₁₆-5₂₃ maser lines toward 143 AGB and 164 post-asymptotic giant branch (AGB) stars in order to investigate how evolutionary characteristics from AGB to post-AGB stars appear in both SiO and H₂O maser emissions. The observations were carried out from 2011 February to 2012 March using the Korean VLBI Network single-dish telescopes. We have detected SiO and/or H₂O maser emission from 21 sources out of 164 post-AGB stars including 12 new detections. Of 143 AGB stars, we detected SiO and/or H₂O maser emission from 44 stars including 24 new detections. SiO v = 2, J = 1-0 maser emission without a SiO v = 1 maser was detected from 7 sources among 14 SiO-detected post-AGB stars, and the intensity of the SiO v = 2, J = 1-0 maser tends to be much stronger than that of SiO v = 1, which is different from those of AGB stars. This may be related to the development of hot dust shells according to the evolutionary processes of post-AGB stars. We also found that both SiO and H₂O masers were detected in the blue group (LI, or Left of IRAS), while only the H₂O maser was detected in the red group (RI, or Right of IRAS) for post-AGB stars. These different detection rates between SiO and H₂O masers may originate from the different abundances of masing molecules in the circumstellar envelope according to the different mass and expansion velocity between LI and RI regions together with their evolutionary stages.

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Detection table from Yoon et al. (2014)

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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(sio_data_all.ra_hms) as ra_hms,MAX(sio_data_all.dec_dms) as dec_dms,MAX(sio_data_all.source_name) as source_name,MAX(sio_data_all.ra) as ra,MAX(sio_data_all.dec) as dec,MAX(sio_data_all.l) as l,MAX(sio_data_all.b) as b,MAX(sio_data_all.grp) as grp,MAX(sio_data_all.other_name) as other_name,MAX(sio_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(sio_data_all.line) as line,MAX(sio_data_all.vrange) as vrange,MAX(sio_data_all.vpeak) as vpeak,MAX(sio_data_all.peak) as peak,MAX(sio_data_all.fwhm) as fwhm,MAX(sio_data_all.int) as int,MAX(sio_data_all.rms) as rms,MAX(sio_data_all.units) as units,MAX(sio_data_all.units_rms) as units_rms,MAX(sio_data_all.date_txt) as date_txt,MAX(sio_data_all.telescope_ref) as telescope_ref,MAX(sio_data_all.telescope_conf) as telescope_conf,MAX(sio_data_all.v_step) as v_step,MAX(sio_data_all.beam) as beam,MAX(sio_data_all.beam_maj) as beam_maj,MAX(sio_data_all.beam_min) as beam_min,MAX(sio_data_all.beam_pa) as beam_pa,MAX(sio_data_all.ref) as ref,MAX(sio_data_all.list_ref) as list_ref,MAX(sio_data_all.ascii) as ascii,MAX(sio_data_all.url) as url,MAX(sio_data_all.image) as image,MAX(sio_data_all.image2) as image2,MAX(sio_data_all.image3) as image3,MAX(sio_data_all.descr) as descr,MAX(sio_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(sio_data_all.dist) as dist,1 as dist_parallax,MAX(sio_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 sio_data_all  LEFT JOIN all_objects_withmet ON sio_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' WHERE ref ilike 'YOO14' AND detected=true AND hide=false GROUP BY ref

select sio_data_all.ra_hms,sio_data_all.dec_dms,sio_data_all.source_name,sio_data_all.ra,sio_data_all.dec,sio_data_all.l,sio_data_all.b,sio_data_all.grp,sio_data_all.other_name,sio_data_all.other_desc,sio_data_all.thermal,sio_data_all.line,sio_data_all.vrange,sio_data_all.vpeak,sio_data_all.peak,sio_data_all.fwhm,sio_data_all.int,sio_data_all.rms,sio_data_all.units,sio_data_all.units_rms,sio_data_all.date_txt,sio_data_all.telescope_ref,sio_data_all.telescope_conf,sio_data_all.v_step,sio_data_all.beam,sio_data_all.beam_maj,sio_data_all.beam_min,sio_data_all.beam_pa,sio_data_all.ref,sio_data_all.list_ref,sio_data_all.ascii,sio_data_all.url,sio_data_all.image,sio_data_all.image2,sio_data_all.image3,sio_data_all.descr,sio_data_all.id,sio_data_all.mjy_flag,sio_data_all.rms_mjy_flag,sio_data_all.dist,sio_data_all.dist_parallax,sio_data_all.date_txt,line_det,type,simbad_types_cat FROM sio_data_all   LEFT JOIN all_objects_withmet ON sio_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' WHERE ref ilike 'YOO14' AND detected=true AND hide=false ORDER BY detected DESC,id

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YOO14 - SiO and H2O Maser Survey toward Post-asymptotic Giant Branch and Asymptotic Giant Branch Stars

View as list of objects

Detection table from Yoon et al. (2014)