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Remarks: We Are Completing an SMA Survey of the Cygnus-X Complex

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Remarks: We Are Completing an SMA Survey of the Cygnus-X Complex Surveys of Clumps, Cores, and Condensations in Cygnus-X Keping Qiu (NJU), Yue Cao (NJU), Yuwei Wang (NJU), Qizhou Zhang (CfA), Junhao Liu (NJU), Bo Hu (NJU) Figure 1 — Pseudo three- Project Overview: color image of the Cygnus-X is the most massive and active high-mass star-forming Cygnus-X complex, with complex at a distance less than 3 kpc from the Sun (Motte et al. 2007, the Herschel 500 µm, 2018). We are performing comprehensive surveys of Clumps, CorEs, 160 µm, and 70 µm maps and CoNdenSations in cygnUS-X (CENSUS, PI: K. Qiu), dedicated to a coded in red, green, and systemic study of the hierarchy of molecular cloud structures and high- blue, respectively. By mass star formation in the complex. The SMA survey, which is the jointly analyzing the central part of the project, has been conducted in the 1.3 mm Herschel, JCMT, and IRAM 30m observations waveband with the Subcompact, Compact, and Extended of the dust continuum configurations. So far we have completed most of the SMA emissions, we identify observations with more than 200 hours of observing time. and characterize more 100 pc than 40 MDCs with sizes The scientific goals of this project are: of order 0.2 pc and to constrain the initial conditions of high-mass star formation by masses of ~20 to 1000 revealing how pc-sized massive molecular clumps form in giant M⨀. These MDCs cover molecular clouds, how they fragment to form ~0.1 pc massive dense a b r o a d r a n g e o f evolutionary stages (Cao, cores (MDCs), and how MDCs further collapse and fragment into Qiu, et al., submitted), ~0.01 pc prestellar and protostellar condensations; and provide targets for to understand to what extent high-mass protostars acquire mass in a our SMA survey. Red way similar to their low-mass counterparts through an unbiased survey circles and crosses mark of a large sample of outflows, rotational toroids and disks within a the 38 fields covered by single molecular cloud complex. our SMA survey. Figure 2 — SMA 1.3 mm SMA single-field observations of MDCs SMA mosaic observations of MDCs continuum observations of the N1/2/3 N05/06 N10 N12/13 N14 DR 15 / IRDC G79.34 MDCs in Cygnus-X. The data DR 21(OH) reveal the fragments of the MDCs with a linear resolution of ~0.01 pc. Upper Left: SMA 0.2pc (30") single-field observations of the N22/24 N30/31/32 N56/57 N58 N63 MDCs. We follow Motte et al. (2007) for the nomenclature of the MDCs. Upper Right: SMA mosaic observations of the M D C s e m b e d d e d w i t h i n N64/65 N68 N69 S7/8 S10 0.5pc remarkable pc-sized clumps. Solid circles approximately show the sizes and locations of S106 IR the MDCs. Dashed circles depict dense cores with masses S15 S29 S30/31 S32 S34 1pc less than 20 M⨀. Lower: SMA observations of the MDCs newly identified around the Cygnus-X OB2 association. A detailed analysis of the S41 S42/43 NW1/2 NW3/4/5 NW14 fragmentation of the MDCs based on the continuum maps is ongoing. We find that most 0.5pc MDCs fragment into a few to more than 10 condensations, but there are also a very few MDCs SMA single-field observations of MDCs around the Cygus-X OB2 association remaining singly peaked down to a size scale of 0.01 pc. Core-1 around OB2 Core-2 around OB2 Core-3 around OB2 Core-4 around OB2 Core-6 around OB2 Core-7 around OB2 Moreover, statistically, the fragmentation level dose not appear to correlate with properties of the MDCs (Qiu et 0.2pc 0.2pc 0.2pc 0.2pc 0.2pc 0.2pc al., in prep.). Remarks: We are completing an SMA survey of the Cygnus-X complex, and the ongoing analysis provides these preliminary results: • We detect ~0.01 pc fragments toward more than 90% of the MDCs, and find that the fragmentation of the MDCs cannot be understood as thermal Jeans or turbulent fragmentation. • We detect high-velocity outflows in the SMA+JCMT CO maps in more than 90% of the MDCs; though most outflows are bipolar and/or collimated, only a few of them are associated with rotational structures seen in typical “disk-tracing” spectral lines, suggesting that (pseudo)disks around high-mass protostars are mostly smaller than 1000 AU. • We find that expanding HII regions, strong UV radiation, and stellar winds are very inefficient in triggering nearby high- mass star formation. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy & Astrophysics.
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