J/ApJS/261/13 High-velocity dispersion compact clouds in the CMZ (Oka+, 2022) ================================================================================ Catalog of high-velocity dispersion compact clouds in the central molecular zone of our galaxy. Oka T., Uruno A., Enokiya R., Nakamura T., Yamasaki Y., Watanabe Y., Tokuyama S., Iwata Y. =2022ApJS..261...13O ================================================================================ ADC_Keywords: Molecular clouds; Galactic center; Velocity dispersion; Carbon monoxide Keywords: Galactic center Abstract: This study developed an automated identification procedure for compact clouds with broad velocity widths in the spectral-line data cubes of highly crowded regions. The procedure was applied to the CO J=3-2 line data, obtained using the James Clerk Maxwell Telescope, to identify 184 high-velocity dispersion compact clouds (HVDCCs), which are a category of peculiar molecular clouds found in the central molecular zone of our Galaxy. A list of HVDCCs in the area -1.4{deg}<=l<=+2.0{deg}, -0.25{deg}<=b<=+0.25{deg} was presented with their physical parameters, CO J=3-2/J=1-0 intensity ratios, and morphological classifications. Consequently, the list provides several intriguing sources that may have been driven by encounters with pointlike massive objects, local energetic events, or cloud-to-cloud collisions. Description: To identify high-velocity dispersion compact clouds (HVDCCs) in the central molecular zone (CMZ), the CO J=3-2 (345.796GHz) line data obtained using the James Clerk Maxwell Telescope (JCMT) by the JCMT Galactic plane survey (JPS) team (Parsons+ 2018, J/ApJS/234/22) was utilized. The observations were conducted in the periods ranging from 2013 July-September, in 2014 July, and from 2015 March to June. The Hetrodyne Array Receiver Program was employed to obtain the CO J=3-2 image of the CMZ. In addition, the autocorrelation spectral imaging system (ACSIS) was also employed as a receiver backend with the 1800MHz bandwidth and 0.97MHz spectral resolution mode. The CO J=1-0 (115.271GHz) line data, used to calculate the CO J=1-0 luminosity and CO J=3-2/J=1-0 intensity ratio (R3-2/1-0), was obtained from observations using the 45m telescope at the Nobeyama Radio Observatory (NRO) in 2011 January. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table4.dat 74 184 Catalog of high-velocity dispersion compact clouds (HVDCCs) table5.dat 53 184 Physical parameters of high-velocity dispersion compact clouds (see Appendix A) -------------------------------------------------------------------------------- See also: J/A+A/391/159 : A search for Compact High-Velocity Clouds (De Heij+, 2002) J/AJ/123/873 : HIPASS high-velocity clouds (Putman+, 2002) J/ApJ/623/181 : Compact high-velocity cloud photometry catalog (Siegel+, 2005) J/ApJ/768/77 : Ultra-compact high velocity clouds from ALFALFA (Adams+, 2013) J/ApJ/806/95 : A search for ultra-compact HVC counterparts (Sand+, 2015) J/ApJS/234/22 : SCUBA-2 Galactic Center compact source catalog (Parsons+, 2018) Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq [1/184] Running sequence number 5- 10 F6.3 deg GLON [-1.41/1.8] Galactic longitude 12- 17 F6.3 deg GLAT [-0.25/0.25] Galactic latitude 19- 24 F6.1 km/s Vlsr [-207.4/184.6] Local Standard of Rest velocity 26- 32 A7 --- Morph1 Morphological type, primary class, Type 1 (1) 34- 40 A7 --- Morph2 Morphological type, secondary class, Type 2 42- 68 A27 --- pID Previous identification(s) (see Section 4.1) 70- 74 A5 --- Ref Reference(s) (2) -------------------------------------------------------------------------------- Note (1): Morphological type (see Section 4.2) as follows: complex = few components with complex morphologies and/or kinematics (46 occurrences) simple = generally isolated in the l-b-V space, which has simple kinematics (35 occurrences) bridge = This type of high-velocity dispersion compact clouds (HVDCC) connects two molecular clouds with different velocities in the position-velocity space (18 occurrences) shell = shell-/arc-shaped morphology and expanding kinematics, suggesting an origin related to local explosive events (28 occurrences) wing = a compact broad-velocity-width emission arises from a parent normal-velocity-width cloud in position-velocity maps (57 occurrences) Note (2): Reference as follows: a = Nagai M. 2008, PhD thesis The Univ. of Tokyo b = Oka et al. (1999ApJ...515..249O) c = Oka et al. (2001PASJ...53..787O) d = Oka et al. (2008PASJ...60..429O) e = Oka et al. (2011ApJ...732..120O) f = Oka et al. (2012ApJS..201...14O) g = Oka et al. (2016ApJ...816L...7O) h = Matsumura et al. (2012ApJ...756...87M) i = Tsujimoto et al. (2018ApJ...856...91T) j = Tsujimoto et al. (2021ApJ...910...61T) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq [1/184] Running sequence number 5- 8 F4.2 pc Size [0.23/6] Size, S (3) 10- 13 F4.1 km/s Sigma [20/61.6] Velocity dispersion, {sigma}_V_ 15- 18 F4.1 10+2K.km.s-1.pc2 LCO [0.6/58.3] CO J=3-2 luminosity 20- 24 F5.1 10+2Msun MCO [1.8/178.3] Molecular gas mass 26- 30 F5.1 10+5Msun MVT [2.5/206.8] Virial theorem mass, M_VT_ 32- 37 F6.1 10+41J Ekin [3.1/1064.9] Kinetic energy in 10^48^erg 39- 42 F4.1 10+4yr Texp [0.9/28] Expansion time 44- 48 F5.1 10+29W Pkin [4/751.1] Kinetic power in 10^36^erg/s 50- 53 F4.2 --- RCO [0.66/2.2]? CO J=3-2/J=1-0 intensity ratio, R_3-2/1-0_ -------------------------------------------------------------------------------- Note (3): The size of the cloud can be calculated using the following formula: Equation (A1): S=D.tan({sigma}_l_{sigma}_b_)^0.5^ where {sigma}_x_ is the dispersion in the x-direction, and D represents the distance to the cloud. In addition, D=D_GC_ was employed here. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Emmanuelle Perret [CDS] 22-Sep-2022