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SAN17 - Planar infall of CH₃OH gas around Cepheus A HW2

Short title: Sanna et al. (2017)
Authors: Sanna, A.Moscadelli, L.Surcis, G.van Langevelde, H. J.Torstensson, K. J. E.Sobolev, A. M.
Journal: Astronomy & Astrophysics, Volume 603, id.A94, 9 pp.
Bibcode:

Target type: Known_Class_II
Transitions: CH3OH_6(II)

Abstract
Aims. In order to test the nature of an (accretion) disk in the vicinity of Cepheus A HW2, we measured the three-dimensional velocity ﬁeld of the CH3OH maser spots, which are projected within 1000 au of the HW2 object, with an accuracy on the order of 0.1 km/s. Methods. We made use of the European VLBI Network (EVN) to image the 6.7 GHz CH3OH maser emission toward Cepheus A HW2 with 4.5 milliarcsec resolution (3 au). We observed at three epochs spaced by one year between 2013 and 2015. During the last epoch, in mid-March 2015, we beneﬁted from the newly deployed Sardinia Radio Telescope. Results. We show that the CH3OH velocity vectors lie on a preferential plane for the gas motion with only small deviations of 12 9 away from the plane. This plane is oriented at a position angle of 134 east of north, and inclined by 26 with the line of sight, closely matching the orientation of the previously reported disk-like structure. Knowing the orientation of the equatorial plane, we can reconstruct a face-on view of the CH3OH gas kinematics onto the plane. CH3OH maser emission is detected within a radius of 900 au from HW2, and down to a radius of about 300 au, the latter coincident with the extent of the dust emission at 0.9 mm. The velocity ﬁeld is dominated by an infall component of about 2 km/s down to a radius of 300 au, where a rotational component of 4 km/s becomes dominant. We discuss the nature of this velocity ﬁeld and the implications for the enclosed mass. Conclusions. These ﬁndings directly support the interpretation that the high-density gas and dust emission that surrounds Cepheus A HW2 traces an accretion disk

Abstract

Aims. In order to test the nature of an (accretion) disk in the vicinity of Cepheus A HW2, we measured the three-dimensional velocity ﬁeld of the CH3OH maser spots, which are projected within 1000 au of the HW2 object, with an accuracy on the order of 0.1 km/s. Methods. We made use of the European VLBI Network (EVN) to image the 6.7 GHz CH3OH maser emission toward Cepheus A HW2 with 4.5 milliarcsec resolution (3 au). We observed at three epochs spaced by one year between 2013 and 2015. During the last epoch, in mid-March 2015, we beneﬁted from the newly deployed Sardinia Radio Telescope. Results. We show that the CH3OH velocity vectors lie on a preferential plane for the gas motion with only small deviations of 12 9 away from the plane. This plane is oriented at a position angle of 134 east of north, and inclined by 26 with the line of sight, closely matching the orientation of the previously reported disk-like structure. Knowing the orientation of the equatorial plane, we can reconstruct a face-on view of the CH3OH gas kinematics onto the plane. CH3OH maser emission is detected within a radius of 900 au from HW2, and down to a radius of about 300 au, the latter coincident with the extent of the dust emission at 0.9 mm. The velocity ﬁeld is dominated by an infall component of about 2 km/s down to a radius of 300 au, where a rotational component of 4 km/s becomes dominant. We discuss the nature of this velocity ﬁeld and the implications for the enclosed mass. Conclusions. These ﬁndings directly support the interpretation that the high-density gas and dust emission that surrounds Cepheus A HW2 traces an accretion disk

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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(met2_data_all.ra_hms) as ra_hms,MAX(met2_data_all.dec_dms) as dec_dms,MAX(met2_data_all.source_name) as source_name,MAX(met2_data_all.ra) as ra,MAX(met2_data_all.dec) as dec,MAX(met2_data_all.l) as l,MAX(met2_data_all.b) as b,MAX(met2_data_all.grp) as grp,MAX(met2_data_all.other_name) as other_name,MAX(met2_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(met2_data_all.line) as line,MAX(met2_data_all.vrange) as vrange,MAX(met2_data_all.vpeak) as vpeak,MAX(met2_data_all.peak) as peak,MAX(met2_data_all.fwhm) as fwhm,MAX(met2_data_all.int) as int,MAX(met2_data_all.rms) as rms,MAX(met2_data_all.units) as units,MAX(met2_data_all.units_rms) as units_rms,MAX(met2_data_all.date_txt) as date_txt,MAX(met2_data_all.telescope_ref) as telescope_ref,MAX(met2_data_all.telescope_conf) as telescope_conf,MAX(met2_data_all.v_step) as v_step,MAX(met2_data_all.beam) as beam,MAX(met2_data_all.beam_maj) as beam_maj,MAX(met2_data_all.beam_min) as beam_min,MAX(met2_data_all.beam_pa) as beam_pa,MAX(met2_data_all.ref) as ref,MAX(met2_data_all.list_ref) as list_ref,MAX(met2_data_all.ascii) as ascii,MAX(met2_data_all.url) as url,MAX(met2_data_all.image) as image,MAX(met2_data_all.image2) as image2,MAX(met2_data_all.image3) as image3,MAX(met2_data_all.descr) as descr,MAX(met2_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(met2_data_all.dist) as dist,1 as dist_parallax,MAX(met2_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 met2_data_all  LEFT JOIN all_objects_withmet ON met2_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 met2_data_all.line=transitions."Line"  WHERE ref ilike 'SAN17' AND detected=true AND hide=false GROUP BY ref

select met2_data_all.ra_hms,met2_data_all.dec_dms,met2_data_all.source_name,met2_data_all.ra,met2_data_all.dec,met2_data_all.l,met2_data_all.b,met2_data_all.grp,met2_data_all.other_name,met2_data_all.other_desc,met2_data_all.thermal,met2_data_all.line,met2_data_all.vrange,met2_data_all.vpeak,met2_data_all.peak,met2_data_all.fwhm,met2_data_all.int,met2_data_all.rms,met2_data_all.units,met2_data_all.units_rms,met2_data_all.date_txt,met2_data_all.telescope_ref,met2_data_all.telescope_conf,met2_data_all.v_step,met2_data_all.beam,met2_data_all.beam_maj,met2_data_all.beam_min,met2_data_all.beam_pa,met2_data_all.ref,met2_data_all.list_ref,met2_data_all.ascii,met2_data_all.url,met2_data_all.image,met2_data_all.image2,met2_data_all.image3,met2_data_all.descr,met2_data_all.id,met2_data_all.mjy_flag,met2_data_all.rms_mjy_flag,met2_data_all.dist,met2_data_all.dist_parallax,met2_data_all.date_txt,line_det,type,simbad_types_cat FROM met2_data_all   LEFT JOIN all_objects_withmet ON met2_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 met2_data_all.line=transitions."Line"  WHERE ref ilike 'SAN17' AND detected=true AND hide=false ORDER BY detected DESC,id

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SAN17 - Planar infall of CH3OH gas around Cepheus A HW2

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Detection table from Sanna et al. (2017)

SAN17 - Planar infall of CH₃OH gas around Cepheus A HW2