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ING22 - Evolutionary map of the Universe (EMU): 18-cm OH-maser discovery in ASKAP continuum images of the SCORPIO field

Short title: Ingallinera et al. (2022)
Authors: Ingallinera, A.Cavallaro, F.Loru, S.Marvil, J.Umana, G.Trigilio, C.Breen, S.Bordiu, C.Buemi, C. S.Bufano, F.Collier, J.Etoka, S.FilipoviÄ�, M. D.Goldman, S. R.Hopkins, A. M.Koribalski, B. S.Leto, P.Norris, R. P.Riggi, S.SchillirÃ², F.Tremblay, C.van Loon, J. Th
Journal: Monthly Notices of the Royal Astronomical Society: Letters, Volume 512, Issue 1, pp.L21-L26
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Target type: star
Observations category: star.general
Facility type: interferometer
Transitions: OH_1612

Abstract
Low- and intermediate-mass stars end their life dispersing their outer layers into the circumstellar medium, during the asymptotic and post-asymptotic giant branch phases. OH masers at 18 cm offer an effective way to probe their circumstellar environment. In this work, we present the discovery of seven OH maser sources likely associated with such evolved stars from the visual inspection of Australian SKA Pathfinder (ASKAP) continuum images. These seven sources do not emit real continuum emission, but the high sensitivity of our images allows us to detect their maser emission, resembling continuum sources. To confirm their nature, we carried out spectral-line observations with ATCA. All the sources showed the double-peaked spectra at 1612 MHz, typical of evolved stars. The detection of maser emission in continuum images can be a complementary and easy-to-use method to discover new maser sources with the large-area deep surveys conducted with the Square Kilometre Array (SKA) precursors. The implication for radio stars studies are remarkable since pure OH maser sources (i.e. with no continuum associated) represent, at a sensitivity of $100\,\mu \mathrm{Jy\,beam}^{-1}$, about 4 per cent of all Galactic sources and by far the most numerous stellar population.

Abstract

Low- and intermediate-mass stars end their life dispersing their outer layers into the circumstellar medium, during the asymptotic and post-asymptotic giant branch phases. OH masers at 18 cm offer an effective way to probe their circumstellar environment. In this work, we present the discovery of seven OH maser sources likely associated with such evolved stars from the visual inspection of Australian SKA Pathfinder (ASKAP) continuum images. These seven sources do not emit real continuum emission, but the high sensitivity of our images allows us to detect their maser emission, resembling continuum sources. To confirm their nature, we carried out spectral-line observations with ATCA. All the sources showed the double-peaked spectra at 1612 MHz, typical of evolved stars. The detection of maser emission in continuum images can be a complementary and easy-to-use method to discover new maser sources with the large-area deep surveys conducted with the Square Kilometre Array (SKA) precursors. The implication for radio stars studies are remarkable since pure OH maser sources (i.e. with no continuum associated) represent, at a sensitivity of $100\,\mu \mathrm{Jy\,beam}^{-1}$, about 4 per cent of all Galactic sources and by far the most numerous stellar population.

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Detection table from Ingallinera et al. (2022)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Line	Frequency	V_peak	F_peak	Telescope	Beam	Detection	Dist. (parallax)
	(J2000)	(J2000)	(deg.)	(deg.)				OH	(MHz)	(km/s)	(Jy)		(arcsec)	Yes/No	(kpc)
1	16 50 9.7	-44 01 42	341.2969	0.3504	G341.284+0.357	G341.2969+0.3504	G341.2969+0.3504	1612 MHz;	1612	24.1	0.098	ATCA	11.4 x 7.8	+OH
2	16 51 57.1	-44 09 53	341.3970	0.0159	G341.397+0.016	G341.3970+0.0159	G341.3970+0.0159	1612 MHz;	1612	-31.5	0.070	ATCA	11.4 x 7.8	+OH
3	16 55 53	-43 08 07	342.6443	0.1142	G342.644+0.114	G342.6443+0.1142	G342.6443+0.1142	1612 MHz;	1612	-99.0	0.047	ATCA	11.4 x 7.8	+OH
	16 55 53	-43 08 07	342.6443	0.1142	G342.644+0.114	G342.6443+0.1142	G342.6443+0.1142	1612 MHz;	1612	-71.8	0.044	ATCA	11.4 x 7.8	+OH
	16 55 53	-43 08 07	342.6443	0.1142	G342.644+0.114	G342.6443+0.1142	G342.6443+0.1142	1612 MHz;	1612	-63.8	0.046	ATCA	11.4 x 7.8	+OH
6	16 58 46	-42 46 37	343.2533	-0.0749	G343.253-0.075	G343.2533-0.0749	G343.2533-0.0749	1612 MHz;	1612	-102.8	0.067	ATCA	11.4 x 7.8	+OH
7	17 02 19.9	-43 13 24	343.3031	-0.8633	G343.303-0.863	G343.3031-0.8633	G343.3031-0.8634	1612 MHz;	1612	-58.7	0.045	ATCA	11.4 x 7.8	+OH
8	17 01 39.4	-42 16 50	343.9724	-0.1879	G343.972-0.188	G343.9724-0.1879	G343.9724-0.1879	1612 MHz;	1612	-64.1	0.054	ATCA	11.4 x 7.8	+OH
9	17 01 16.4	-41 48 54	344.2963	0.1540	G344.296+0.154	G344.2961+0.1542	G344.2963+0.1540	1612 MHz;	1612	14.8	0.078	ATCA	11.4 x 7.8	+OH

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(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.grpv) as grpv,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.line) as line,MAX(oh_data_all.freq) as freq,MAX(oh_data_all.pol) as pol,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.url) as url,MAX(oh_data_all.image) as image,MAX(oh_data_all.image2) as image2,MAX(oh_data_all.image3) as image3,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,1 as dist_parallax,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 'ING22' 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.grpv,oh_data_all.other_name,oh_data_all.other_desc,oh_data_all.thermal,oh_data_all.line,oh_data_all.freq,oh_data_all.pol,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.url,oh_data_all.image,oh_data_all.image2,oh_data_all.image3,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.dist_parallax,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 'ING22' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

ING22 - Evolutionary map of the Universe (EMU): 18-cm OH-maser discovery in ASKAP continuum images of the SCORPIO field

View as list of objects

Detection table from Ingallinera et al. (2022)