J/ApJ/871/17ivo://CDS.VizieR/J/ApJ/871/17doi:10.26093/cds/vizier.18710017CDSUtomo D.Blitz L.Falgarone E.2020-10-12T12:22:50Z2020-08-10T06:59:25ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesmolecular-cloudsinterstellar-mediumco-line-emissionh-i-line-emissiongalaxy-kinematicsWe utilize the multi-wavelength data of M33 to study the origin of turbulence in its interstellar medium. We find that the HI turbulent energy surface density inside 8kpc is ~1-3x10^46^erg/pc^2^, and has no strong dependence on galactocentric radius because of the lack of variation in HI surface density and HI velocity dispersion. Then, we consider the energies injected by supernovae (SNe), the magneto-rotational instability (MRI), and the gravity-driven turbulence from accreted materials as the sources of turbulent energy. For a constant dissipation time of turbulence, the SNe energy can maintain turbulence inside ~4kpc radius (equivalent to ~0.5R_25_), while the MRI energy is always smaller than the turbulent energy within 8kpc radius. However, when we let the dissipation time to be equal to the crossing time of turbulence across the HI scale height, the SNe energy is enough to maintain turbulence out to 7kpc radius, and the sum of SNe and MRI energies is able to maintain turbulence out to 8kpc radius. Due to lack of constraint in the mass accretion rate through the disk of M33, we cannot rule out the accretion driven turbulence as a possible source of energy. Furthermore, by resolving individual giant molecular clouds in M33, we also show that the SNe energy can maintain turbulence within individual molecular clouds with ~1% of coupling efficiency. This result strengthens the proposition that stellar feedback is an important source of energy to maintain turbulence in nearby galaxies.2019ApJ...871...17Uhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/871/17CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJS/149/343 : Giant molecular clouds in M33 (Engargiola+, 2003)J/A+A/417/421 : WSRT wide-field HI survey. II. (Braun+, 2004)J/ApJS/173/185 : GALEX UV atlas of nearby galaxies (Gil de Paz+, 2007)J/ApJ/658/1006 : Radial profiles for face-on spirals (Munoz-Mateos+, 2007)J/ApJ/661/830 : Giant molecular clouds of M33 (Rosolowsky+, 2007)J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)J/ApJ/675/1213 : Abundances in M33 HII regions (Rosolowsky+, 2008)J/AJ/136/2563 : HI Nearby Galaxy Survey, THINGS (Walter+, 2008)J/ApJ/703/517 : The Spitzer Local Volume Legacy: IR photometry (Dale+, 2009)J/ApJ/699/1092 : Giant molecular clouds (SRBY) (Heyer+, 2009)J/A+A/522/A3 : M33 CO(2-1) & HI integrated intensity maps (Gratier+, 2010)J/A+A/542/A108 : Giant molecular clouds in M33 (Gratier+, 2012)J/A+A/548/A52 : Molecular cloud formation in M33 (Braine+, 2012)J/ApJ/761/37 : CO obs. in giant molecular clouds of M33 (Miura+, 2012)J/A+A/549/A17 : IRAM spectra toward M33 Molecular Clouds (Buchbender+, 2013)J/ApJ/803/16 : Giant molecular clouds in NGC4526 from ^12^CO (Utomo+, 2015)J/A+A/601/A146 : M33 molecular clouds & stellar clusters (Corbelli+, 2017)J/MNRAS/468/3965 : SAMI Galaxy Survey. Gas surface densities (Federrath+, 2017)J/ApJ/846/71 : M51 ISM structures from the CO maps of PAWS (Leroy+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/871/17https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/871/17http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/871/17https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/871/17https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/871/17http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/871/17GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapRadiodefaultJ/ApJ/871/17/table1The radial profile of energy per unit arearecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRad[0.05/8] Radiuskpcphys.size.radiusfloate_Rad[0.05] Error in Radkpcstat.errorfloatKin[1.7/4.4] Kinetic energy surface density1e+39J.pc**-2src.densityfloate_Kin[0.3/1.8] Lower limit in Kin1e+39J.pc**-2stat.errorfloatE_Kin[0.3/1.8] Upper limit in Kin1e+39J.pc**-2stat.error;stat.maxfloatTherm[0.4/0.9] Thermal energy surface density1e+39J.pc**-2src.densityfloate_Therm[0.1/0.4] Lower limit in Therm1e+39J.pc**-2stat.errorfloatE_Therm[0.05/0.3] Upper limit in Therm1e+39J.pc**-2stat.error;stat.maxfloatTurb[1.3/3.7] Turbulent energy surface density1e+39J.pc**-2src.densityfloate_Turb[0.4/2] Lower limit in Turb1e+39J.pc**-2stat.errorfloatE_Turb[0.5/2] Upper limit in Turb1e+39J.pc**-2stat.error;stat.maxfloatMRI[0.07/1.1] The magneto-rotational instability (MRI) energy surface density1e+39J.pc**-2src.densityfloate_MRI[0.04/1] Lower limit in MRI1e+39J.pc**-2stat.errorfloatE_MRI[0.06/2.3] Upper limit in MRI1e+39J.pc**-2stat.error;stat.maxfloatSNeC[0.1/26.7] Supernovae energy surface density with constant dissipation time of 9.8Myr1e+39J.pc**-2src.densityfloate_SNeC[0.08/9.7] Lower limit in SNeC1e+39J.pc**-2stat.errorfloatE_SNeC[0.2/51.2] Upper limit in SNeC1e+39J.pc**-2stat.error;stat.maxfloatSNeV[1.1/34.8] Supernovae energy surface density with variable dissipation time1e+39J.pc**-2src.densityfloate_SNeV[0.8/22.3] Lower limit in SNeC1e+39J.pc**-2stat.errorfloatE_SNeV[2.4/193] Upper limit in SNeC1e+39J.pc**-2stat.error;stat.maxfloatEffC[0.1/3.3] Total coupling efficiency; Turb/(MRI+SNeC)stat.fit.omcfloate_EffC[0.02/2.1] Lower limit in EffCstat.errorfloatE_EffC[0.03/9.2] Upper limit in EffCstat.error;stat.maxfloatEffV[0.08/0.9] Total coupling efficiency; Turb/(MRI+SNeV)stat.fit.omcfloate_EffV[0.02/0.6] Lower limit in EffVstat.errorfloatE_EffV[0.02/2.1] Upper limit in EffVstat.error;stat.maxfloatJ/ApJ/871/17/table2The radial profile of surface densities, velocity dispersion, and scale-heightrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRad[0.05/8] Radiuskpcphys.size.radiusfloate_Rad[0.05] Error in Radkpcstat.errorfloatAtomSB[4.5/9.8] Atomic gas mass surface densitysolMass.pc**-2phys.densityfloate_AtomSB[0.5/3.7] Lower limit in AtomSBsolMass.pc**-2stat.errorfloatE_AtomSB[0.5/4.3] Upper limit in AtomSBsolMass.pc**-2stat.error;stat.maxfloatMolSB[0.2/6] Molecular gas mass surface densitysolMass.pc**-2phys.densityfloate_MolSB[0.2/3.1] Lower limit in MolSBsolMass.pc**-2stat.errorfloatE_MolSB[0.8/5.2] Upper limit in MolSBsolMass.pc**-2stat.error;stat.maxfloatStarSB[3.8/1019] Stellar mass surface densitysolMass.pc**-2phys.densityfloate_StarSB[0.04/19]? Lower limit in StarSB (1)solMass.pc**-2stat.errorfloatnullableE_StarSB[0.1/19]? Upper limit in StarSB (1)solMass.pc**-2stat.error;stat.maxfloatnullableSFRSB[0.05/13.4] Star formation rate surface densitysolMass.pc**-2.Gyr**-1phys.SFRfloate_SFRSB[0.04/5] Lower limit in SFRSBsolMass.pc**-2.Gyr**-1stat.errorfloatE_SFRSB[0.1/26] Upper limit in SFRSBsolMass.pc**-2.Gyr**-1stat.error;stat.maxfloatVDisp[9.9/13.7] Atomic gas velocity dispersionkm/sphys.veloc.dispersionfloate_VDisp[0.2/1.2] Lower limit in VDispkm/sstat.errorfloatE_VDisp[0/2.3] Upper limit in VDispkm/sstat.error;stat.maxfloatHeight[72/628] Scale-height of the atomic gaspcphys.sizefloate_Height[19/416] Lower limit in Heightpcstat.error;pos.cartesian.zfloatE_Height[20/929] Upper limit in Heightpcstat.error;stat.maxfloatJ/ApJ/871/17/table3The properties of molecular clouds in M33recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/124] Cloud number, ordered from center of M33meta.id;meta.mainintRad[0.2/6.7] Cloud distance from M33 centerkpcpos.distancefloate_Rad[0.02/0.2] Uncertainty in Radkpcstat.errorfloatSize[36/140] Effective cloud radius defined as (area/{pi})^0.5pcphys.size.radiusfloate_Size[16.66] Uncertainty in Size (1)pcstat.error;phys.angSizefloatMass[0.1/6.8] Cloud mass derived using a variable {alpha}_CO100000solMassphys.massfloate_Mass[0.01/0.4] Uncertainty in Mass (2)100000solMassstat.error;phys.massfloatVDisp[1/5.4]? Mean cloud velocity dispersionkm/sphys.veloc.dispersionfloatnullablee_VDisp[0/9.4]? Uncertainty in VDisp (3)km/sstat.errorfloatnullablelogTEng[-4.3/-0.4]? Log cloud turbulent energy surface density in units of 10^51^erg/pc^2^log(1e+44J.pc**-2)src.densityfloatnullablee_logTEng[0.04/1.2]? Lower limit in logTEnglog(1e+44J.pc**-2)stat.errorfloatnullableE_logTEng[0.04/0.5]? Upper limit in logTEnglog(1e+44J.pc**-2)stat.error;stat.maxfloatnullablelogSNe[-1.5/1.71] Log cloud supernovae energy surface density in units of 10^51^erg/pc^2^log(1e+44J.pc**-2)src.densityfloate_logSNe[0.01/0.2] Lower limit in logSNelog(1e+44J.pc**-2)stat.errorfloatE_logSNe[0.01/0.2] Upper limit in logSNelog(1e+44J.pc**-2)stat.error;stat.maxfloat