TY - JOUR
T1 - An Unbiased CO Survey Toward the Northern Region of the Small Magellanic Cloud with the Atacama Compact Array. II. CO Cloud Catalog
AU - Ohno, Takahiro
AU - Tokuda, Kazuki
AU - Konishi, Ayu
AU - Matsumoto, Takeru
AU - Sewiło, Marta
AU - Kondo, Hiroshi
AU - Sano, Hidetoshi
AU - Tsuge, Kisetsu
AU - Zahorecz, Sarolta
AU - Goto, Nao
AU - Neelamkodan, Naslim
AU - Wong, Tony
AU - Fukushima, Hajime
AU - Takekoshi, Tatsuya
AU - Muraoka, Kazuyuki
AU - Kawamura, Akiko
AU - Tachihara, Kengo
AU - Fukui, Yasuo
AU - Onishi, Toshikazu
N1 - Funding Information:
We would like to thank the anonymous referee for useful comments that improved the manuscript. This paper makes use of the following ALMA data: ADS/ JAO. ALMA#2017.A.00054.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work was supported by NAOJ ALMA Scientific Research grant Nos. 2022-22B and Grants-in-Aid for Scientific Research (KAKENHI) of Japan Society for the Promotion of Science (JSPS; grant Nos. JP18K13582, JP18H05440, JP21K13962, and JP21H00049). The material is based upon work supported by NASA under award numbers 80GSFC21M0002 and 80NSSC22K0168 (M.S.). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. T.W. acknowledges support from collaborative NSF AAG award 2009849. T. Ohno was supported by the ALMA Japan Research Grant of NAOJ ALMA Project, NAOJ-ALMA-286. We thank Dr. Masato I.N. Kobayashi for the discussion on the cloud mass spectrum from theoretical aspects.
Funding Information:
We would like to thank the anonymous referee for useful comments that improved the manuscript. This paper makes use of the following ALMA data: ADS/ JAO. ALMA#2017.A.00054.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work was supported by NAOJ ALMA Scientific Research grant Nos. 2022-22B and Grants-in-Aid for Scientific Research (KAKENHI) of Japan Society for the Promotion of Science (JSPS; grant Nos. JP18K13582, JP18H05440, JP21K13962, and JP21H00049). The material is based upon work supported by NASA under award numbers 80GSFC21M0002 and 80NSSC22K0168 (M.S.). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. T.W. acknowledges support from collaborative NSF AAG award 2009849. T. Ohno was supported by the ALMA Japan Research Grant of NAOJ ALMA Project, NAOJ-ALMA-286. We thank Dr. Masato I.N. Kobayashi for the discussion on the cloud mass spectrum from theoretical aspects.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/6/1
Y1 - 2023/6/1
N2 - The nature of molecular clouds and their statistical behavior in subsolar metallicity environments are not fully explored yet. We analyzed data from an unbiased CO (J = 2-1) survey at the spatial resolution of ∼2 pc in the northern region of the Small Magellanic Cloud with the Atacama Compact Array to characterize the CO cloud properties. A cloud-decomposition analysis identified 426 spatially/velocity-independent CO clouds and their substructures. Based on the cross-matching with known infrared catalogs by Spitzer and Herschel, more than 90% CO clouds show spatial correlations with point sources. We investigated the basic properties of the CO clouds and found that the radius-velocity linewidth (R-σ v ) relation follows the Milky Way-like power-law exponent, but the intercept is ∼1.5 times lower than that in the Milky Way. The mass functions (dN/dM) of the CO luminosity and virial mass are characterized by an exponent of ∼1.7, which is consistent with previously reported values in the Large Magellanic Cloud and in the Milky Way.
AB - The nature of molecular clouds and their statistical behavior in subsolar metallicity environments are not fully explored yet. We analyzed data from an unbiased CO (J = 2-1) survey at the spatial resolution of ∼2 pc in the northern region of the Small Magellanic Cloud with the Atacama Compact Array to characterize the CO cloud properties. A cloud-decomposition analysis identified 426 spatially/velocity-independent CO clouds and their substructures. Based on the cross-matching with known infrared catalogs by Spitzer and Herschel, more than 90% CO clouds show spatial correlations with point sources. We investigated the basic properties of the CO clouds and found that the radius-velocity linewidth (R-σ v ) relation follows the Milky Way-like power-law exponent, but the intercept is ∼1.5 times lower than that in the Milky Way. The mass functions (dN/dM) of the CO luminosity and virial mass are characterized by an exponent of ∼1.7, which is consistent with previously reported values in the Large Magellanic Cloud and in the Milky Way.
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U2 - 10.3847/1538-4357/accadb
DO - 10.3847/1538-4357/accadb
M3 - Article
AN - SCOPUS:85161274672
SN - 0004-637X
VL - 949
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 63
ER -