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ROL99 - A search for methanol masers at 9.978 GHz and 10.058 GHz

Short title: Rollig et al. (1999)
Authors: Röllig, M. Kegel, W. H. Mauersberger, R. Doerr, C.
Journal: Astronomy and Astrophysics, v.343, p.939-942 (1999)
Bibcode:

Target type: Class_II(6)
Transitions: CH3OH_9(I),CH3OH_25-30_GHz(I),CH3OH_36(I),CH3OH_44(I),CH3OH_84(I),CH3OH_95(I),CH3OH_104(I),CH3OH_132(I),CH3OH_6(II),CH3OH_107(II),CH3OH_157(II)

Abstract
We performed NLTE-radiative transfer calculations for interstellar A-type methanol maser lines in order to find out under which physical conditions the level populations show strong inversion. In our model we considered collisional as well as radiative pumping and accounted for line overlap as well as for torsional excitation of the methanol molecules. The radiation field was calculated using a simple on-the-spot approximation. Our results show that torsional excitation can be essential for the maser pumping mechanism while line overlap appears to be of minor importance. In addition to the well known Class I and Class II maser lines, we found two new transitions which possibly may show up as strong masers. These are the 4_3-5_2 {A}(-) and {A}(+) transitions at 10.058 {GHz} and 9.978 {GHz} respectively. These masers are radiatively pumped by IR radiation, i.e. they should be found near IR sources similar to the classical Class II methanol masers. 88 galactic CH₃OH maser sources were searched for emission in these two lines, but no detection was made. Upper limits are given and discussed.

Abstract

We performed NLTE-radiative transfer calculations for interstellar A-type methanol maser lines in order to find out under which physical conditions the level populations show strong inversion. In our model we considered collisional as well as radiative pumping and accounted for line overlap as well as for torsional excitation of the methanol molecules. The radiation field was calculated using a simple on-the-spot approximation. Our results show that torsional excitation can be essential for the maser pumping mechanism while line overlap appears to be of minor importance. In addition to the well known Class I and Class II maser lines, we found two new transitions which possibly may show up as strong masers. These are the 4_3-5_2 {A}(-) and {A}(+) transitions at 10.058 {GHz} and 9.978 {GHz} respectively. These masers are radiatively pumped by IR radiation, i.e. they should be found near IR sources similar to the classical Class II methanol masers. 88 galactic CH₃OH maser sources were searched for emission in these two lines, but no detection was made. Upper limits are given and discussed.

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Detection table from Rollig et al. (1999)

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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(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.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' WHERE ref ilike 'ROL99' 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.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' WHERE ref ilike 'ROL99' AND detected=true AND hide=false ORDER BY detected DESC,id

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ROL99 - A search for methanol masers at 9.978 GHz and 10.058 GHz

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Detection table from Rollig et al. (1999)