Display data from paper

Select data type:

GOM90 - H2O and SiO maser emission in OH/IR stars.

Short title: Gomez et al. (1990)
Authors: Gómez, Y. Moran, J. M. Rodríguez, L. F.
Journal: Revista Mexicana de Astronomia y Astrofisica, Vol. 20, No. 1, p. 55 - 66
Bibcode:

Target type: IRAS

Abstract
The authors searched for H₂O and SiO maser emission in 84 OH/IR stars that have measured IRAS fluxes at 12, 25, and 60 mum. They detected four new H₂O sources and eight new SiO sources. The authors have used previous detections reported in the literature to determine the percentage of OH/IR stars with H₂O and SiO maser emission as a function of [25-12] color. The percentage of objects with detectable H₂O and SiO maser emission decreases with increasing [25-12] color. This color is believed to be an age indicator. The statistical analysis of the data suggests that the percentage of OH/IR stars with SiO maser emission decrease as the [25-12] color increases. Current models for the time evolution of OH/IR stars suggest that it is around [25-12] &cong +0.2 that the mass loss ceases or decreases significantly. The percentage of OH/IR stars with H₂O maser emission decreases significantly at [25-12] &cong -0.2, before mass loss ceases. The reasons for the early drop in H₂O maser percentage are not known.

Abstract

The authors searched for H₂O and SiO maser emission in 84 OH/IR stars that have measured IRAS fluxes at 12, 25, and 60 mum. They detected four new H₂O sources and eight new SiO sources. The authors have used previous detections reported in the literature to determine the percentage of OH/IR stars with H₂O and SiO maser emission as a function of [25-12] color. The percentage of objects with detectable H₂O and SiO maser emission decreases with increasing [25-12] color. This color is believed to be an age indicator. The statistical analysis of the data suggests that the percentage of OH/IR stars with SiO maser emission decrease as the [25-12] color increases. Current models for the time evolution of OH/IR stars suggest that it is around [25-12] &cong +0.2 that the mass loss ceases or decreases significantly. The percentage of OH/IR stars with H₂O maser emission decreases significantly at [25-12] &cong -0.2, before mass loss ceases. The reasons for the early drop in H₂O maser percentage are not known.

Download as: Table (CSV)
View as list of objects

Detection table from Gomez et al. (1990)

Export table to csv

Hide / Show individual components

ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	V_range	V_peak	F_peak	RMS	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(km/s)	(km/s)	(Jy)	(Jy)		Yes/No		(kpc)
1	18 09 25	+34 46 17.3	61.4728	23.1625	G61.473+23.164	*IRAS 18076+3445	0.00	4.2	9	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
2	18 20 36.7	-18 47 9.4	12.7689	-1.9401	G12.769-1.941	OH 12.8-1.9	0.00	10.9	39.7	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
3	18 21 06	-15 03 24.1	16.1148	-0.2875	G16.117-0.291	OH 16.1-0.3	0.00	22	51	9.000	ENG_SIO	+H₂O -CH₃OH I +CH₃OH II +OH +SiO	SFR_MIXED		GOM90
4	18 35 29.9	-07 13 10.3	24.6940	0.2324	G24.693+0.235	*OH 24.7 +0.3	0.00	47.5	10.7	9.000	ENG_SIO	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		GOM90
5	18 45 52.7	-01 46 43.3	30.7150	0.4255	G30.715+0.427	OH 30.7 +0.4	0.00	68.9	14.8	9.000	ENG_SIO	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		GOM90
6	19 21 36.4	+09 27 51.4	44.7933	-2.3066	G44.795-2.307	OH 44.8-2.3	0.00	-71.6	14.2	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
7	19 30 50.2	+29 29 56.8	63.4817	5.2799	G63.482+5.280	*IRAS 19288+2923	0.00	-37.8	6.1	9.000	ENG_SIO	+H₂O +OH +SiO	EVOLVED		GOM90
8	19 40 54.1	+15 20 8.5	52.2137	-3.6244	G52.218-3.627	IRAS 19386+1513	0.00	1.7	7.3	9.000	ENG_SIO	+H₂O -CH₃OH II +OH +SiO	EVOLVED		GOM90

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 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 'GOM90' 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 'GOM90' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

GOM90 - H2O and SiO maser emission in OH/IR stars.

View as list of objects

Detection table from Gomez et al. (1990)