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LIS94 - Star Formation in the Galactic Center Dust Ridge

Short title: Lis et al. (1994)
Authors: Lis, D. C.Menten, K. M.Serabyn, E.Zylka, R.
Journal: Astrophysical Journal Letters v.423, p.L39
Bibcode:

Target type: YSO
Transitions: H2O_22

Abstract
We present multiwavelength submillimeter and radio continuum, as well as 22 GHz H2O line observations of the giant molecular cloud core M0.25 + 0.01 located in the 'dust ridge' near the Galactic center radio arc. At lambda = 350 micrometer the continuum emission region is spatially resolved by our 12 sec beam, and we find no evidence for compact dust sources similar to those found in Sgr B2. Although existing far-infrared data do not allow for accurate determination of the dust temperature, the steep rise of the submillimeter spectrum between 800 and 350 micrometer suggests that the grain emissivity law in the M0.25 + 0.01 core may be significantly steeper than in previously studied Galactic center dust sources. The detection of an H2O maser source located near the 350 micrometer emission peak implies the presence of at least some ongoing low-mass star formation. However, in spite of the relatively large molecular mass of the core implied by the submillimeter observations (approximately equals 1.6 x 10⁵ solar mass), our 8.4 GHz continuum data show that current star formation in the M0.25 + 0.01 core is limited to stars with spectral types later than B0 there is no evidence for more massive young stars. This Greater Magellanic Cloud (GMC) core thus appears distinctly different from the Sgr C and D cores, which, although much less massive, harbor O-type stars.

Abstract

We present multiwavelength submillimeter and radio continuum, as well as 22 GHz H2O line observations of the giant molecular cloud core M0.25 + 0.01 located in the 'dust ridge' near the Galactic center radio arc. At lambda = 350 micrometer the continuum emission region is spatially resolved by our 12 sec beam, and we find no evidence for compact dust sources similar to those found in Sgr B2. Although existing far-infrared data do not allow for accurate determination of the dust temperature, the steep rise of the submillimeter spectrum between 800 and 350 micrometer suggests that the grain emissivity law in the M0.25 + 0.01 core may be significantly steeper than in previously studied Galactic center dust sources. The detection of an H2O maser source located near the 350 micrometer emission peak implies the presence of at least some ongoing low-mass star formation. However, in spite of the relatively large molecular mass of the core implied by the submillimeter observations (approximately equals 1.6 x 10⁵ solar mass), our 8.4 GHz continuum data show that current star formation in the M0.25 + 0.01 core is limited to stars with spectral types later than B0 there is no evidence for more massive young stars. This Greater Magellanic Cloud (GMC) core thus appears distinctly different from the Sgr C and D cores, which, although much less massive, harbor O-type stars.

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Detection table from Lis et al. (1994)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	V_range	V_peak	F_peak	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					H₂O	(km/s)	(km/s)	(Jy)		(km/s)	(mJy/beam)	(arcsec)	Yes/No		(kpc)
1	+17 46 8.5857	-28 42 37.4979	0.2524	0.0197	G0.2534+0.0207	M0.25 + 0.01	Image	Descr	22 GHz;	-70;120	35	2.55	NRAOVLA	1.32	7.400	1	+H₂O +CH₃OH I	SFR		1993 June 6

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.line) as line,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' LEFT JOIN transitions ON h2o_data_all.line=transitions."Line"  WHERE ref ilike 'LIS94' 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.line,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' LEFT JOIN transitions ON h2o_data_all.line=transitions."Line"  WHERE ref ilike 'LIS94' AND detected=true AND hide=false ORDER BY detected DESC,id

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LIS94 - Star Formation in the Galactic Center Dust Ridge

View as list of objects

Detection table from Lis et al. (1994)