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1. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -XIV. Properties of resolved UC Hii regions

Author

Zhang, C., Zhu, Feng-Yao, Liu, Tie, Ren, Z. -Y., Liu, H. -L., Wang, Ke, Wu, J. -W., Zhang, Y., Zhou, J. -W., Tatematsu, K., Garay, Guido, Tej, Anandmayee, Li, Shanghuo, Xu, W. F., Lee, Chang Won, Bronfman, Leonardo, Soam, Archana, Li, D., Zhang, C., Zhu, Feng-Yao, Liu, Tie, Ren, Z. -Y., Liu, H. -L., Wang, Ke, Wu, J. -W., Zhang, Y., Zhou, J. -W., Tatematsu, K., Garay, Guido, Tej, Anandmayee, Li, Shanghuo, Xu, W. F., Lee, Chang Won, Bronfman, Leonardo, Soam, Archana, and Li, D.

Abstract

Hydrogen recombination lines (RRLs) are one of the major diagnostics of the physical properties of H{\sc ii} regions. We use RRL H40$\alpha$, He40$\alpha$ and 3 mm continuum emission to investigate the properties of a large sample of resolved UC H{\sc ii} regions identified in the ATOMS survey. In total, we identify 94 UC H{\sc ii} regions from H40$\alpha$ emission. The basic parameters for these UC H{\sc ii} regions such as electron density, emission measure, electron temperature, ionic abundance ratio (n$_{\rm He^+}$/n$_{\rm H^+}$), and line width are derived. The median electron density and the median n$_{\rm He^+}$/n$_{\rm H^+}$ ratio of these UC H{\sc ii} regions derived from RRLs are $\sim$9000 cm$^{-3}$ and 0.11, respectively. Within UC H{\sc ii} regions, the n$_{\rm He^+}$/n$_{\rm H^+}$ ratios derived from the intensity ratio of the He40$\alpha$ and H40$\alpha$ lines seems to be higher in the boundary region than in the center. The H40$\alpha$ line width is mainly broadened by thermal motion and microturbulence. The electron temperature of these UC H{\sc ii} regions has a median value of $\sim$6700 K, and its dependence on galactocentric distance is weak.

Published
2023
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2. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- IV. Radio Recombination Lines and evolution of star formation efficiencies

Author

Zhang, C., Evans II, Neal J., Liu, T., Wu, J. -W., Wang, Ke, Liu, H. -L., Zhu, F. -Y., Ren, Z. -Y., Dewangan, L. K., Lee, Chang Won, Li, Shanghuo, Bronfman, L., Tej, A., Li, D., Zhang, C., Evans II, Neal J., Liu, T., Wu, J. -W., Wang, Ke, Liu, H. -L., Zhu, F. -Y., Ren, Z. -Y., Dewangan, L. K., Lee, Chang Won, Li, Shanghuo, Bronfman, L., Tej, A., and Li, D.

Abstract

We report detection of radio recombination line (RRL) H$_{40\alpha}$ toward 75 sources, with data obtained from ACA observations in the ATOMS survey of 146 active Galactic star forming regions. We calculated ionized gas mass and star formation rate with H40U line emission. The mass of ionized gas is significantly smaller than molecular gas mass, indicating that ionized gas is negligible in the star forming clumps of the ATOMS sample. The star formation rate (SFR$_{{\rm H}_{40\alpha}}$) estimated with RRL H$_{40\alpha}$ agrees well with that (SFR$_{\rm L_{bol}}$) calculated with the total bolometric luminosity (L$_{\rm bol}$) when SFR $\gtrsim 5 {\rm M_\odot My}r^{-1}$, suggesting that millimeter RRLs could well sample the upper part of the initial mass function (IMF) and thus be good tracers for SFR. We also study the relationships between L$_{\rm bol}$ and the molecular line luminosities (L0mol) of CS J=2-1 and HC$_3$N J=11-10 for all the 146 ATOMS sources. The Lbol-L0mol correlations of both the CS J=2-1 and HC3N J=11-10 lines appear approximately linear and these transitions have success in predicting L$_{\rm bol}$ similar to that of more commonly used transitions. The L$_{\rm bol}$-to-L$_{\rm mol}$ ratios or SFR-to-mass ratios (star formation efficiency; SFE) do not change with galactocentric distances (R$_{\rm GC}$). Sources with H$_{40\alpha}$ emission (or H$_{\rm II}$ regions) show higher L$_{\rm bol}$-to-L$_{\rm mol}$ than those without H$_{40\alpha}$ emission, which may be an evolutionary effect.

Published
2021
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3. Chemically Fresh Gas Inflows Detected in a Nearby High-mass Star-forming Region

Author

Chen, X., Ren, Z. -Y., Li, D. -L., Liu, T., Wang, K., Shen, Z. -Q., Ellingsen, S. P., Sobolev, A. M., Mei, Y., Li, J. -J., Wu, Y. -F., Kim, K. -T., Chen, X., Ren, Z. -Y., Li, D. -L., Liu, T., Wang, K., Shen, Z. -Q., Ellingsen, S. P., Sobolev, A. M., Mei, Y., Li, J. -J., Wu, Y. -F., and Kim, K. -T.

Abstract

We report the detection of a chemically fresh inflow that is feeding high-mass young-stellar-object (HMYSO) growth in the nearby high-mass star-forming region G352.63 made with both the Atacama Large Millimeter/submillimeter Array (ALMA) and the Submillimeter Array (SMA). High-quality images of the dust and molecular lines from both ALMA and SMA have consistently revealed a gravitationally controlled cold (∼10 K) gas inflow of chemically fresh molecules (e.g., CCH and HC3N) toward the central HMYSO and its surrounding dense gas structure, which has a possible torus- or disk-like morphology. The HMYSO is also observed to have an outflow, which is nearly perpendicular to the torus and its parental filament, and thus can be clearly separated from the inflows. These kinematic features provide observational evidence to support the conjecture that the infalling streamers in high-mass star-forming regions could proceed in a similar process to that observed in low-mass counterparts. The chemically fresh infalling streamers could also be involved in the disk or torus configuration, fragmentation, and accretion bursts that occur in both simulations and observations. © 2021. The Author(s). Published by the American Astronomical Society.

Published
2021

4. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- IV. Radio Recombination Lines and evolution of star formation efficiencies

Author

Zhang, C., Evans II, Neal J., Liu, T., Wu, J. -W., Wang, Ke, Liu, H. -L., Zhu, F. -Y., Ren, Z. -Y., Dewangan, L. K., Lee, Chang Won, Li, Shanghuo, Bronfman, L., Tej, A., Li, D., Zhang, C., Evans II, Neal J., Liu, T., Wu, J. -W., Wang, Ke, Liu, H. -L., Zhu, F. -Y., Ren, Z. -Y., Dewangan, L. K., Lee, Chang Won, Li, Shanghuo, Bronfman, L., Tej, A., and Li, D.

Abstract

We report detection of radio recombination line (RRL) H$_{40\alpha}$ toward 75 sources, with data obtained from ACA observations in the ATOMS survey of 146 active Galactic star forming regions. We calculated ionized gas mass and star formation rate with H40U line emission. The mass of ionized gas is significantly smaller than molecular gas mass, indicating that ionized gas is negligible in the star forming clumps of the ATOMS sample. The star formation rate (SFR$_{{\rm H}_{40\alpha}}$) estimated with RRL H$_{40\alpha}$ agrees well with that (SFR$_{\rm L_{bol}}$) calculated with the total bolometric luminosity (L$_{\rm bol}$) when SFR $\gtrsim 5 {\rm M_\odot My}r^{-1}$, suggesting that millimeter RRLs could well sample the upper part of the initial mass function (IMF) and thus be good tracers for SFR. We also study the relationships between L$_{\rm bol}$ and the molecular line luminosities (L0mol) of CS J=2-1 and HC$_3$N J=11-10 for all the 146 ATOMS sources. The Lbol-L0mol correlations of both the CS J=2-1 and HC3N J=11-10 lines appear approximately linear and these transitions have success in predicting L$_{\rm bol}$ similar to that of more commonly used transitions. The L$_{\rm bol}$-to-L$_{\rm mol}$ ratios or SFR-to-mass ratios (star formation efficiency; SFE) do not change with galactocentric distances (R$_{\rm GC}$). Sources with H$_{40\alpha}$ emission (or H$_{\rm II}$ regions) show higher L$_{\rm bol}$-to-L$_{\rm mol}$ than those without H$_{40\alpha}$ emission, which may be an evolutionary effect.

Published
2021
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5. Applying saliency-map analysis in searches for pulsars and fast radio bursts

Author

Zhang, C., Wang, C., Hobbs, G., Russell, C. J., Li, D., Zhang, S. -B., Dai, S., Wu, J. -W., Pan, Z. -C., Zhu, W. -W., Toomey, L., Ren, Z. -Y., Zhang, C., Wang, C., Hobbs, G., Russell, C. J., Li, D., Zhang, S. -B., Dai, S., Wu, J. -W., Pan, Z. -C., Zhu, W. -W., Toomey, L., and Ren, Z. -Y.

Abstract

To investigate the use of saliency-map analysis to aid in searches for transient signals, such as fast radio bursts and individual pulses from radio pulsars. We aim to demonstrate that saliency maps provide the means to understand predictions from machine learning algorithms and can be implemented in piplines used to search for transient events. We have implemented a new deep learning methodology to predict whether or not any segment of the data contains a transient event. The algorithm has been trained using real and simulated data sets. We demonstrate that the algorithm is able to identify such events. The output results are visually analysed via the use of saliency maps. We find that saliency maps can produce an enhanced image of any transient feature without the need for de-dispersion or removal of radio frequency interference. Such maps can be used to understand which features in the image were used in making the machine learning decision and to visualise the transient event. Even though the algorithm reported here was developed to demonstrate saliency-map analysis, we have detected, in archival data, a single burst event with dispersion measure of $41$\,cm$^{-3}$pc that is not associated with any currently known pulsar., Comment: 16 pages, 6 figures, accepted for publication in A&A

Published
2020
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6. 13CH3OH Masers Associated with a Transient Phenomenon in a High-mass Young Stellar Object

Author

Chen, X., Sobolev, A. M., Breen, S. L., Shen, Z. -Q., Ellingsen, S. P., MacLeod, G. C., Li, B., Voronkov, M. A., Kaczmarek, J. F., Zhang, J., Ren, Z. -Y., Wang, J., Linz, H., Hunter, T. R., Brogan, C., Sugiyama, K., Burns, R. A., Menten, K., Sanna, A., Stecklum, B., Hirota, T., Kim, K. -T., Chibueze, J., Heever, S. P. V. D., Chen, X., Sobolev, A. M., Breen, S. L., Shen, Z. -Q., Ellingsen, S. P., MacLeod, G. C., Li, B., Voronkov, M. A., Kaczmarek, J. F., Zhang, J., Ren, Z. -Y., Wang, J., Linz, H., Hunter, T. R., Brogan, C., Sugiyama, K., Burns, R. A., Menten, K., Sanna, A., Stecklum, B., Hirota, T., Kim, K. -T., Chibueze, J., and Heever, S. P. V. D.

Abstract

We report the first detection of isotopic methanol (13CH3OH) maser emission in interstellar space. The emission was detected toward the high-mass young stellar object G358.93-0.03 during monitoring of a flare in the 6.7 GHz methanol (CH3OH) maser emission in this source. We find that the spectral and spatial distribution of the 13CH3OH masers differs from the CH3OH masers imaged at the same epoch, contrary to expectations from similarity of their pumping. This conclusively demonstrates that isotopic methanol masers are bright under different physical conditions and suggests that they can provide additional, complementary information to the CH3OH masers from the same source. We detect a rapid decay of the 13CH3OH maser lines suggesting that they are transient phenomena (masing for only a few months), likely associated with rapid changes in radiation field due to an accretion burst induced by massive disk fragmentation. Changes in the line flux density are faster than required to achieve equilibrium in the energy level populations, indicating that the pumping of these masers is likely variable. © 2020. The American Astronomical Society. All rights reserved..

Published
2020

7. Applying saliency-map analysis in searches for pulsars and fast radio bursts

Author

Zhang, C., Wang, C., Hobbs, G., Russell, C. J., Li, D., Zhang, S. -B., Dai, S., Wu, J. -W., Pan, Z. -C., Zhu, W. -W., Toomey, L., Ren, Z. -Y., Zhang, C., Wang, C., Hobbs, G., Russell, C. J., Li, D., Zhang, S. -B., Dai, S., Wu, J. -W., Pan, Z. -C., Zhu, W. -W., Toomey, L., and Ren, Z. -Y.

Abstract

To investigate the use of saliency-map analysis to aid in searches for transient signals, such as fast radio bursts and individual pulses from radio pulsars. We aim to demonstrate that saliency maps provide the means to understand predictions from machine learning algorithms and can be implemented in piplines used to search for transient events. We have implemented a new deep learning methodology to predict whether or not any segment of the data contains a transient event. The algorithm has been trained using real and simulated data sets. We demonstrate that the algorithm is able to identify such events. The output results are visually analysed via the use of saliency maps. We find that saliency maps can produce an enhanced image of any transient feature without the need for de-dispersion or removal of radio frequency interference. Such maps can be used to understand which features in the image were used in making the machine learning decision and to visualise the transient event. Even though the algorithm reported here was developed to demonstrate saliency-map analysis, we have detected, in archival data, a single burst event with dispersion measure of $41$\,cm$^{-3}$pc that is not associated with any currently known pulsar., Comment: 16 pages, 6 figures, accepted for publication in A&A

Published
2020
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8. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution – Survey Description and Compact Source Catalogue

Author

Eden, D J, Liu, Tie, Kim, Kee-Tae, Juvela, M, Liu, S -Y, Tatematsu, K, Di Francesco, J, Wang, K, Wu, Y, Thompson, M A, Fuller, G A, Li, Di, Ristorcelli, I, Kang, Sung-ju, Hirano, N, Johnstone, D, Lin, Y, He, J H, Koch, P M, Sanhueza, Patricio, Qin, S -L, Zhang, Q, Goldsmith, P F, Evans, N J, Yuan, J, Zhang, C -P, White, G J, Choi, Minho, Won Lee, Chang, Toth, L V, Mairs, S, Yi, H -W, Tang, M, Soam, A, Peretto, N, Samal, M R, Fich, M, Parsons, H, Malinen, J, Bendo, G J, Rivera-Ingraham, A, Liu, H -L, Wouterloot, J, Li, P S, Qian, L, Rawlings, J, Rawlings, M G, Feng, S, Wang, B, Li, Dalei, Liu, M, Luo, G, Marston, A P, Pattle, K M, Pelkonen, V -M, Rigby, A J, Zahorecz, S, Zhang, G, Bőgner, R, Aikawa, Y, Akhter, S, Alina, D, Bell, G, Bernard, J -P, Blain, A, Bronfman, L, Byun, D -Y, Chapman, S, Chen, H -R, Chen, M, Chen, W -P, Chen, X, Chen, Xuepeng, Chrysostomou, A, Chu, Y -H, Chung, E J, Cornu, D, Cosentino, G, Cunningham, M R, Demyk, K, Drabek-Maunder, E, Doi, Y, Eswaraiah, C, Falgarone, E, Fehér, O, Fraser, H, Friberg, P, Garay, G, Ge, J X, Gear, W K, Greaves, J, Guan, X, Harvey-Smith, L, Hasegawa, T, He, Y, Henkel, C, Hirota, T, Holland, W, Hughes, A, Jarken, E, Ji, T -G, Jimenez-Serra, I, Kang, Miju, Kawabata, K S, Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S, Koo, B -C, Kwon, Woojin, Kuan, Y -J, Lacaille, K M, Lai, S -P, Lee, C F, Lee, J -E, Lee, Y -U, Li, H, Lo, N, Lopez, J A P, Lu, X, Lyo, A -R, Mardones, D, McGehee, P, Meng, F, Montier, L, Montillaud, J, Moore, T J T, Morata, O, Moriarty-Schieven, G H, Ohashi, S, Pak, S, Park, Geumsook, Paladini, R, Pech, G, Qiu, K, Ren, Z -Y, Richer, J, Sakai, T, Shang, H, Shinnaga, H, Stamatellos, Dimitris, Tang, Y -W, Traficante, A, Vastel, C, Viti, S, Walsh, A, Wang, H, Wang, J, Ward-Thompson, Derek, Whitworth, A, Wilson, C D, Xu, Y, Yang, J, Yuan, Y -L, Yuan, L, Zavagno, A, Zhang, C, Zhang, H -W, Zhou, C, Zhou, J, Zhu, L, Zuo, P, Eden, D J, Liu, Tie, Kim, Kee-Tae, Juvela, M, Liu, S -Y, Tatematsu, K, Di Francesco, J, Wang, K, Wu, Y, Thompson, M A, Fuller, G A, Li, Di, Ristorcelli, I, Kang, Sung-ju, Hirano, N, Johnstone, D, Lin, Y, He, J H, Koch, P M, Sanhueza, Patricio, Qin, S -L, Zhang, Q, Goldsmith, P F, Evans, N J, Yuan, J, Zhang, C -P, White, G J, Choi, Minho, Won Lee, Chang, Toth, L V, Mairs, S, Yi, H -W, Tang, M, Soam, A, Peretto, N, Samal, M R, Fich, M, Parsons, H, Malinen, J, Bendo, G J, Rivera-Ingraham, A, Liu, H -L, Wouterloot, J, Li, P S, Qian, L, Rawlings, J, Rawlings, M G, Feng, S, Wang, B, Li, Dalei, Liu, M, Luo, G, Marston, A P, Pattle, K M, Pelkonen, V -M, Rigby, A J, Zahorecz, S, Zhang, G, Bőgner, R, Aikawa, Y, Akhter, S, Alina, D, Bell, G, Bernard, J -P, Blain, A, Bronfman, L, Byun, D -Y, Chapman, S, Chen, H -R, Chen, M, Chen, W -P, Chen, X, Chen, Xuepeng, Chrysostomou, A, Chu, Y -H, Chung, E J, Cornu, D, Cosentino, G, Cunningham, M R, Demyk, K, Drabek-Maunder, E, Doi, Y, Eswaraiah, C, Falgarone, E, Fehér, O, Fraser, H, Friberg, P, Garay, G, Ge, J X, Gear, W K, Greaves, J, Guan, X, Harvey-Smith, L, Hasegawa, T, He, Y, Henkel, C, Hirota, T, Holland, W, Hughes, A, Jarken, E, Ji, T -G, Jimenez-Serra, I, Kang, Miju, Kawabata, K S, Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S, Koo, B -C, Kwon, Woojin, Kuan, Y -J, Lacaille, K M, Lai, S -P, Lee, C F, Lee, J -E, Lee, Y -U, Li, H, Lo, N, Lopez, J A P, Lu, X, Lyo, A -R, Mardones, D, McGehee, P, Meng, F, Montier, L, Montillaud, J, Moore, T J T, Morata, O, Moriarty-Schieven, G H, Ohashi, S, Pak, S, Park, Geumsook, Paladini, R, Pech, G, Qiu, K, Ren, Z -Y, Richer, J, Sakai, T, Shang, H, Shinnaga, H, Stamatellos, Dimitris, Tang, Y -W, Traficante, A, Vastel, C, Viti, S, Walsh, A, Wang, H, Wang, J, Ward-Thompson, Derek, Whitworth, A, Wilson, C D, Xu, Y, Yang, J, Yuan, Y -L, Yuan, L, Zavagno, A, Zhang, C, Zhang, H -W, Zhou, C, Zhou, J, Zhu, L, and Zuo, P

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-μm continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of N H 2 NH2 > 5 × 1021 cm−2. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other.

Published
2019

9. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution – Survey Description and Compact Source Catalogue

Author

Eden, D J, Liu, Tie, Kim, Kee-Tae, Juvela, M, Liu, S -Y, Tatematsu, K, Di Francesco, J, Wang, K, Wu, Y, Thompson, M A, Fuller, G A, Li, Di, Ristorcelli, I, Kang, Sung-ju, Hirano, N, Johnstone, D, Lin, Y, He, J H, Koch, P M, Sanhueza, Patricio, Qin, S -L, Zhang, Q, Goldsmith, P F, Evans, N J, Yuan, J, Zhang, C -P, White, G J, Choi, Minho, Won Lee, Chang, Toth, L V, Mairs, S, Yi, H -W, Tang, M, Soam, A, Peretto, N, Samal, M R, Fich, M, Parsons, H, Malinen, J, Bendo, G J, Rivera-Ingraham, A, Liu, H -L, Wouterloot, J, Li, P S, Qian, L, Rawlings, J, Rawlings, M G, Feng, S, Wang, B, Li, Dalei, Liu, M, Luo, G, Marston, A P, Pattle, K M, Pelkonen, V -M, Rigby, A J, Zahorecz, S, Zhang, G, Bőgner, R, Aikawa, Y, Akhter, S, Alina, D, Bell, G, Bernard, J -P, Blain, A, Bronfman, L, Byun, D -Y, Chapman, S, Chen, H -R, Chen, M, Chen, W -P, Chen, X, Chen, Xuepeng, Chrysostomou, A, Chu, Y -H, Chung, E J, Cornu, D, Cosentino, G, Cunningham, M R, Demyk, K, Drabek-Maunder, E, Doi, Y, Eswaraiah, C, Falgarone, E, Fehér, O, Fraser, H, Friberg, P, Garay, G, Ge, J X, Gear, W K, Greaves, J, Guan, X, Harvey-Smith, L, Hasegawa, T, He, Y, Henkel, C, Hirota, T, Holland, W, Hughes, A, Jarken, E, Ji, T -G, Jimenez-Serra, I, Kang, Miju, Kawabata, K S, Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S, Koo, B -C, Kwon, Woojin, Kuan, Y -J, Lacaille, K M, Lai, S -P, Lee, C F, Lee, J -E, Lee, Y -U, Li, H, Lo, N, Lopez, J A P, Lu, X, Lyo, A -R, Mardones, D, McGehee, P, Meng, F, Montier, L, Montillaud, J, Moore, T J T, Morata, O, Moriarty-Schieven, G H, Ohashi, S, Pak, S, Park, Geumsook, Paladini, R, Pech, G, Qiu, K, Ren, Z -Y, Richer, J, Sakai, T, Shang, H, Shinnaga, H, Stamatellos, Dimitris, Tang, Y -W, Traficante, A, Vastel, C, Viti, S, Walsh, A, Wang, H, Wang, J, Ward-Thompson, Derek, Whitworth, A, Wilson, C D, Xu, Y, Yang, J, Yuan, Y -L, Yuan, L, Zavagno, A, Zhang, C, Zhang, H -W, Zhou, C, Zhou, J, Zhu, L, Zuo, P, Eden, D J, Liu, Tie, Kim, Kee-Tae, Juvela, M, Liu, S -Y, Tatematsu, K, Di Francesco, J, Wang, K, Wu, Y, Thompson, M A, Fuller, G A, Li, Di, Ristorcelli, I, Kang, Sung-ju, Hirano, N, Johnstone, D, Lin, Y, He, J H, Koch, P M, Sanhueza, Patricio, Qin, S -L, Zhang, Q, Goldsmith, P F, Evans, N J, Yuan, J, Zhang, C -P, White, G J, Choi, Minho, Won Lee, Chang, Toth, L V, Mairs, S, Yi, H -W, Tang, M, Soam, A, Peretto, N, Samal, M R, Fich, M, Parsons, H, Malinen, J, Bendo, G J, Rivera-Ingraham, A, Liu, H -L, Wouterloot, J, Li, P S, Qian, L, Rawlings, J, Rawlings, M G, Feng, S, Wang, B, Li, Dalei, Liu, M, Luo, G, Marston, A P, Pattle, K M, Pelkonen, V -M, Rigby, A J, Zahorecz, S, Zhang, G, Bőgner, R, Aikawa, Y, Akhter, S, Alina, D, Bell, G, Bernard, J -P, Blain, A, Bronfman, L, Byun, D -Y, Chapman, S, Chen, H -R, Chen, M, Chen, W -P, Chen, X, Chen, Xuepeng, Chrysostomou, A, Chu, Y -H, Chung, E J, Cornu, D, Cosentino, G, Cunningham, M R, Demyk, K, Drabek-Maunder, E, Doi, Y, Eswaraiah, C, Falgarone, E, Fehér, O, Fraser, H, Friberg, P, Garay, G, Ge, J X, Gear, W K, Greaves, J, Guan, X, Harvey-Smith, L, Hasegawa, T, He, Y, Henkel, C, Hirota, T, Holland, W, Hughes, A, Jarken, E, Ji, T -G, Jimenez-Serra, I, Kang, Miju, Kawabata, K S, Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S, Koo, B -C, Kwon, Woojin, Kuan, Y -J, Lacaille, K M, Lai, S -P, Lee, C F, Lee, J -E, Lee, Y -U, Li, H, Lo, N, Lopez, J A P, Lu, X, Lyo, A -R, Mardones, D, McGehee, P, Meng, F, Montier, L, Montillaud, J, Moore, T J T, Morata, O, Moriarty-Schieven, G H, Ohashi, S, Pak, S, Park, Geumsook, Paladini, R, Pech, G, Qiu, K, Ren, Z -Y, Richer, J, Sakai, T, Shang, H, Shinnaga, H, Stamatellos, Dimitris, Tang, Y -W, Traficante, A, Vastel, C, Viti, S, Walsh, A, Wang, H, Wang, J, Ward-Thompson, Derek, Whitworth, A, Wilson, C D, Xu, Y, Yang, J, Yuan, Y -L, Yuan, L, Zavagno, A, Zhang, C, Zhang, H -W, Zhou, C, Zhou, J, Zhu, L, and Zuo, P

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-μm continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of N H 2 NH2 > 5 × 1021 cm−2. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other.

Published
2019

10. Discovery of a New Class i Methanol Maser Transition at 266.8 GHz

Author

Chen, X., Ellingsen, S. P., Ren, Z. -Y., Sobolev, A. M., Parfenov, S., Shen, Z. -Q., Chen, X., Ellingsen, S. P., Ren, Z. -Y., Sobolev, A. M., Parfenov, S., and Shen, Z. -Q.

Abstract

We report the detection of a new class I methanol maser candidate from the 52-41 E transition (266.8 GHz). This methanol transition has been detected toward a nearby high-mass star-forming region G352.630-1.067 (distance ∼0.7 kpc), in Submillimeter Array (SMA) observations. The new candidate transition has a similar spatial distribution as the 42-31 E (218.4 GHz) and 8-1-70 E (229.7 GHz) transitions, which are known class I maser transitions. Thermal methanol emission in this source is confined to a central hot core, while the three class I maser transitions are detected in two additional regions. These two maser-only emission regions are clearly associated with shocked gas traced by 2 μm Ks-band and thermal v = 0, J = 5-4 SiO molecular emission. In contrast to the thermal methanol emission from the hot core, the three class I maser transitions show an positive trend in the rotation diagram for the two maser regions. Large velocity gradient modeling of the 266.8, 218.4, and 229.7 GHz transitions shows that the 266.8 GHz transition can be a maser for a wide range of conditions. The intensity ratios for the three methanol transitions detected in maser regions can be reproduced under conditions that are typical for class I methanol maser sites. These facts all support the hypothesis that the detected emission from the 266.8 GHz methanol (52-41 E) transition is masing. © 2019. The American Astronomical Society.

Published
2019

11. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution - Survey Description and Compact Source Catalogue

Author

Eden, D. J., Liu, Tie, Kim, Kee-Tae, Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans II, N. J., Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, Miju, Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhu, J. Zhou. L., Zuo, P., Eden, D. J., Liu, Tie, Kim, Kee-Tae, Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans II, N. J., Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, Miju, Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhu, J. Zhou. L., and Zuo, P.

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-um continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of $N_{H_{2}}$ $>$ 5 $\times$ 10$^{21}$ cm$^{-2}$. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other., Comment: 16 pages, 13 figures, 1 table. Accepted for publication in MNRAS

Published
2019
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12. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution - survey description and compact source catalogue

Author

Eden, D. J., Liu, Tie, Kim, Kee-Tae, Juvela, M., Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans, N. J., II, Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, M., Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. -E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhou, J., Zhu, L., Zuo, P., Eden, D. J., Liu, Tie, Kim, Kee-Tae, Juvela, M., Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans, N. J., II, Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, M., Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. -E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhou, J., Zhu, L., and Zuo, P.

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850 mu m continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353 GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having three or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of N-H2 > 5 x10(21) cm(-2). By positionally associating the SCOPE compact sources with young stellar objects, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other.

Published
2019

13. High-mass star formation in the nearby region G352.630-1.067. I. parallax

Author

Chen, X., Li, J. -J., Zhang, B., Ellingsen, S. P., Xu, Y., Ren, Z. -Y., Shen, Z. -Q., Sobolev, A. M., Chen, X., Li, J. -J., Zhang, B., Ellingsen, S. P., Xu, Y., Ren, Z. -Y., Shen, Z. -Q., and Sobolev, A. M.

Abstract

Young or forming high-mass stars that are nearby and not within a cluster environment have the potential to provide fundamental insights into star formation. In this paper we report such a candidate (G352.630-1.067), for which we have measured the distance through very long baseline interferometry parallax observations of the associated 6.7 GHz class II methanol maser. We determine the distance to the source to be 0.69 -0.08 +0.10 kpc, which makes it the second nearest highmass star formation region (HMSFR) known, with only the Orion Nebula being closer. This may place this source, not within a Galactic spiral arm, but in the region between the Local and Sagittarius arms, indicating that molecular clouds in interarm regions may also generate high-mass stars. Kinematic association between this source and the Sagittarius Arm suggests that it may be located in a spur extending outward from this arm. Comparison with the known, nearby HMSFRs (distances less than 1 kpc), reveal that G352.630-1.067 is in a more isolated environment than others, hence providing an excellent candidate for investigations of the processes that form individual high-mass stars. We find a good spatial correlation between the 6.7 GHz methanol maser and high angular resolution images of the infrared outflow, suggesting that the class II methanol masers are closely associated with a jet/outflow in this source. © 2019 The American Astronomical Society.

Published
2019

14. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution - survey description and compact source catalogue

Author

Eden, D. J., Liu, Tie, Kim, Kee-Tae, Juvela, M., Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans, N. J., II, Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, M., Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. -E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhou, J., Zhu, L., Zuo, P., Eden, D. J., Liu, Tie, Kim, Kee-Tae, Juvela, M., Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans, N. J., II, Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, M., Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. -E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhou, J., Zhu, L., and Zuo, P.

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850 mu m continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353 GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having three or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of N-H2 > 5 x10(21) cm(-2). By positionally associating the SCOPE compact sources with young stellar objects, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other.

Published
2019

15. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution - Survey Description and Compact Source Catalogue

Author

Eden, D. J., Liu, Tie, Kim, Kee-Tae, Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans II, N. J., Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, Miju, Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhu, J. Zhou. L., Zuo, P., Eden, D. J., Liu, Tie, Kim, Kee-Tae, Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans II, N. J., Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, Miju, Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhu, J. Zhou. L., and Zuo, P.

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-um continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of $N_{H_{2}}$ $>$ 5 $\times$ 10$^{21}$ cm$^{-2}$. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other., Comment: 16 pages, 13 figures, 1 table. Accepted for publication in MNRAS

Published
2019
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16. Measurements of (XcJ)-> K+K-K+K- decays

Author

Ablikim, M., Bai, J. Z., Ban, Y., Bian, J. G., Cai, X., Chen, H. F., Chen, H. S., Chen, H. X., Chen, J. C., Chen, Jin, Chen, Y. B., Chi, S. P., Chu, Y. P., Cui, X. Z., Dai, Y. S., Diao, L. Y., Deng, Z. Y., Dong, Q. F., Du, S. X., Fang, J., Fang, S. S., Fu, C. D., Gao, C. S., Gao, Y. N., Gu, S. D., Gu, Y. T., Guo, Y. N., Guo, Y. Q., Guo, Z. J., Harris, F. A., He, K. L., He, M., Heng, Y. K., Hu, H. M., Hu, T., Huang, G. S., Huang, X. T., Ji, X. B., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jin, D. P., Jin, S., Jin, Yi, Lai, Y. F., Li, G., Li, H. B., Li, H. H., Li, J., Li, R. Y., Li, S. M., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, H. B., Liu, B. J., Liu, C. X., Liu, F., Liu, Fang, Liu, H. H., Liu, H. M., Liu, J., Liu, J. B., Liu, J. P., Liu, Q., Liu, R. G., Liu, Z. A., Lou, Y. C., Lu, F., Lu, G. R., Lu, J. G., Luo, C. L., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, X. B., Mao, Z. P., Mo, X. H., Nie, J., Olsen, S. L., Peng, H. P., Ping, R. G., Qi, N. D., Qin, H., Qiu, J. F., Ren, Z. Y., Rong, G., Shan, L. X., Shang, L., Shen, C. P., Shen, D. L., Shen, X. Y., Sheng, H. Y., Sun, H. S., Sun, J. F., Sun, S. S., Sun, Y. Z., Sun, Z. J., Tan, Z. Q., Tang, X., Tong, G. L., Varner, G. S., Wang, D. Y., Wang, L., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, W. F., Wang, Y. F., Wang, Z., Wang, Z. Y., Wang, Zhe, Wang, Zheng, Wei, C. L., Wei, D. H., Wiedner, Ulrich, Wu, N., Xia, X. M., Xie, X. X., Xu, G. F., Xu, X. P., Xu, Y., Yan, M. L., Yang, H. X., Yang, Y. X., Ye, M. H., Ye, Y. X., Yi, Z. Y., Yu, G. W., Yuan, C. Z., Yuan, J. M., Yuan, Y., Zang, S. L., Zeng, Y., Zeng, Yu, Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. Q., Zhang, H. Y., Zhang, J. W., Zhang, J. Y., Zhang, S. H., Zhang, X. M., Zhang, X. Y., Zhang, Yiyun, Zhang, Z. P., Zhao, D. X., Zhao, J. W., Zhao, M. G., Zhao, P. P., Zhao, W. R., Zhao, Z. G., Zheng, H. Q., Zheng, J. P., Zheng, Z. P., Zhou, L., Zhou, N. F., Zhu, K. J., Zhu, Q. M., Zhu, Y. C., Zhu, Y. S., Zhu, Yingchun, Zhu, Z. A., Zhuang, B. A., Zhuang, X. A., Zou, B. S., Ablikim, M., Bai, J. Z., Ban, Y., Bian, J. G., Cai, X., Chen, H. F., Chen, H. S., Chen, H. X., Chen, J. C., Chen, Jin, Chen, Y. B., Chi, S. P., Chu, Y. P., Cui, X. Z., Dai, Y. S., Diao, L. Y., Deng, Z. Y., Dong, Q. F., Du, S. X., Fang, J., Fang, S. S., Fu, C. D., Gao, C. S., Gao, Y. N., Gu, S. D., Gu, Y. T., Guo, Y. N., Guo, Y. Q., Guo, Z. J., Harris, F. A., He, K. L., He, M., Heng, Y. K., Hu, H. M., Hu, T., Huang, G. S., Huang, X. T., Ji, X. B., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jin, D. P., Jin, S., Jin, Yi, Lai, Y. F., Li, G., Li, H. B., Li, H. H., Li, J., Li, R. Y., Li, S. M., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, H. B., Liu, B. J., Liu, C. X., Liu, F., Liu, Fang, Liu, H. H., Liu, H. M., Liu, J., Liu, J. B., Liu, J. P., Liu, Q., Liu, R. G., Liu, Z. A., Lou, Y. C., Lu, F., Lu, G. R., Lu, J. G., Luo, C. L., Ma, F. C., Ma, H. L., Ma, L. L., Ma, Q. M., Ma, X. B., Mao, Z. P., Mo, X. H., Nie, J., Olsen, S. L., Peng, H. P., Ping, R. G., Qi, N. D., Qin, H., Qiu, J. F., Ren, Z. Y., Rong, G., Shan, L. X., Shang, L., Shen, C. P., Shen, D. L., Shen, X. Y., Sheng, H. Y., Sun, H. S., Sun, J. F., Sun, S. S., Sun, Y. Z., Sun, Z. J., Tan, Z. Q., Tang, X., Tong, G. L., Varner, G. S., Wang, D. Y., Wang, L., Wang, L. L., Wang, L. S., Wang, M., Wang, P., Wang, P. L., Wang, W. F., Wang, Y. F., Wang, Z., Wang, Z. Y., Wang, Zhe, Wang, Zheng, Wei, C. L., Wei, D. H., Wiedner, Ulrich, Wu, N., Xia, X. M., Xie, X. X., Xu, G. F., Xu, X. P., Xu, Y., Yan, M. L., Yang, H. X., Yang, Y. X., Ye, M. H., Ye, Y. X., Yi, Z. Y., Yu, G. W., Yuan, C. Z., Yuan, J. M., Yuan, Y., Zang, S. L., Zeng, Y., Zeng, Yu, Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. Q., Zhang, H. Y., Zhang, J. W., Zhang, J. Y., Zhang, S. H., Zhang, X. M., Zhang, X. Y., Zhang, Yiyun, Zhang, Z. P., Zhao, D. X., Zhao, J. W., Zhao, M. G., Zhao, P. P., Zhao, W. R., Zhao, Z. G., Zheng, H. Q., Zheng, J. P., Zheng, Z. P., Zhou, L., Zhou, N. F., Zhu, K. J., Zhu, Q. M., Zhu, Y. C., Zhu, Y. S., Zhu, Yingchun, Zhu, Z. A., Zhuang, B. A., Zhuang, X. A., and Zou, B. S.

Abstract

Using 14M psi(2S) events taken with the BESII detector, chi(cJ) -> 2(K+K-) decays are studied. For the four-kaon final state, the branching fractions are B(chi(c0,1,2) ->.2(K+K-)) = (3.48 +/- 0.23 +/- 0.47) x 10(-3), (0.70 +/- 0.13 +/- 0.10) x 10(-3), and (2.17 +/- 0.20 +/- 0.31) x 10(-3). For the phi K+K- final state, the branching fractions, which are measured for the first time, are B(chi(c0,1,2) -> phi K+K-) = (1.03 +/- 0.22 +/- 0.15) x 10(-3), (0.46 +/- 0.16 +/- 0.06) x 10(-3), and (1.67 +/- 0.26 +/- 0.24) x 10(-4). For the phi phi final state, B(chi(c0,2) -> phi phi) = (0.94 +/- 0.21 +/- 0.13) x 10(-3) and (1.70 +/- 0.30 +/- 0.25) x 10(-3).

Published
2006
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17. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution – Survey Description and Compact Source Catalogue

Author

Eden, D J, Liu, Tie, Kim, Kee-Tae, Juvela, M, Liu, S -Y, Tatematsu, K, Di Francesco, J, Wang, K, Wu, Y, Thompson, M A, Fuller, G A, Li, Di, Ristorcelli, I, Kang, Sung-ju, Hirano, N, Johnstone, D, Lin, Y, He, J H, Koch, P M, Sanhueza, Patricio, Qin, S -L, Zhang, Q, Goldsmith, P F, Evans, N J, Yuan, J, Zhang, C -P, White, G. J., Choi, Minho, Won Lee, Chang, Toth, L V, Mairs, S, Yi, H -W, Tang, M, Soam, A, Peretto, N, Samal, M R, Fich, M, Parsons, H, Malinen, J, Bendo, G J, Rivera-Ingraham, A, Liu, H -L, Wouterloot, J, Li, P S, Qian, L, Rawlings, J, Rawlings, M G, Feng, S, Wang, B, Li, Dalei, Liu, M, Luo, G, Marston, A P, Pattle, K M, Pelkonen, V -M, Rigby, A J, Zahorecz, S, Zhang, G, Bőgner, R, Aikawa, Y, Akhter, S, Alina, D, Bell, G, Bernard, J -P, Blain, A, Bronfman, L, Byun, D -Y, Chapman, S, Chen, H -R, Chen, M, Chen, W -P, Chen, X, Chen, Xuepeng, Chrysostomou, A, Chu, Y -H, Chung, E J, Cornu, D, Cosentino, G, Cunningham, M R, Demyk, K, Drabek-Maunder, E, Doi, Y, Eswaraiah, C, Falgarone, E, Fehér, O, Fraser, Helen, Friberg, P, Garay, G, Ge, J X, Gear, W K, Greaves, J, Guan, X, Harvey-Smith, L, Hasegawa, T, He, Y, Henkel, C, Hirota, T, Holland, W, Hughes, A, Jarken, E, Ji, T -G, Jimenez-Serra, I, Kang, Miju, Kawabata, K S, Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S, Koo, B -C, Kwon, Woojin, Kuan, Y -J, Lacaille, K M, Lai, S -P, Lee, C F, Lee, J -E, Lee, Y -U, Li, H, Lo, N, Lopez, J A P, Lu, X, Lyo, A -R, Mardones, D, McGehee, P, Meng, F, Montier, L, Montillaud, J, Moore, T J T, Morata, O, Moriarty-Schieven, G H, Ohashi, S, Pak, S, Park, Geumsook, Paladini, R, Pech, G, Qiu, K, Ren, Z -Y, Richer, J, Sakai, T, Shang, H, Shinnaga, H, Stamatellos, D, Tang, Y -W, Traficante, A, Vastel, C, Viti, S, Walsh, A, Wang, H, Wang, J, Ward-Thompson, D, Whitworth, A, Wilson, C D, Xu, Y, Yang, J, Yuan, Y -L, Yuan, L, Zavagno, A, Zhang, C, Zhang, H -W, Zhou, C, Zhou, J, Zhu, L, Zuo, P, Eden, D J, Liu, Tie, Kim, Kee-Tae, Juvela, M, Liu, S -Y, Tatematsu, K, Di Francesco, J, Wang, K, Wu, Y, Thompson, M A, Fuller, G A, Li, Di, Ristorcelli, I, Kang, Sung-ju, Hirano, N, Johnstone, D, Lin, Y, He, J H, Koch, P M, Sanhueza, Patricio, Qin, S -L, Zhang, Q, Goldsmith, P F, Evans, N J, Yuan, J, Zhang, C -P, White, G. J., Choi, Minho, Won Lee, Chang, Toth, L V, Mairs, S, Yi, H -W, Tang, M, Soam, A, Peretto, N, Samal, M R, Fich, M, Parsons, H, Malinen, J, Bendo, G J, Rivera-Ingraham, A, Liu, H -L, Wouterloot, J, Li, P S, Qian, L, Rawlings, J, Rawlings, M G, Feng, S, Wang, B, Li, Dalei, Liu, M, Luo, G, Marston, A P, Pattle, K M, Pelkonen, V -M, Rigby, A J, Zahorecz, S, Zhang, G, Bőgner, R, Aikawa, Y, Akhter, S, Alina, D, Bell, G, Bernard, J -P, Blain, A, Bronfman, L, Byun, D -Y, Chapman, S, Chen, H -R, Chen, M, Chen, W -P, Chen, X, Chen, Xuepeng, Chrysostomou, A, Chu, Y -H, Chung, E J, Cornu, D, Cosentino, G, Cunningham, M R, Demyk, K, Drabek-Maunder, E, Doi, Y, Eswaraiah, C, Falgarone, E, Fehér, O, Fraser, Helen, Friberg, P, Garay, G, Ge, J X, Gear, W K, Greaves, J, Guan, X, Harvey-Smith, L, Hasegawa, T, He, Y, Henkel, C, Hirota, T, Holland, W, Hughes, A, Jarken, E, Ji, T -G, Jimenez-Serra, I, Kang, Miju, Kawabata, K S, Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S, Koo, B -C, Kwon, Woojin, Kuan, Y -J, Lacaille, K M, Lai, S -P, Lee, C F, Lee, J -E, Lee, Y -U, Li, H, Lo, N, Lopez, J A P, Lu, X, Lyo, A -R, Mardones, D, McGehee, P, Meng, F, Montier, L, Montillaud, J, Moore, T J T, Morata, O, Moriarty-Schieven, G H, Ohashi, S, Pak, S, Park, Geumsook, Paladini, R, Pech, G, Qiu, K, Ren, Z -Y, Richer, J, Sakai, T, Shang, H, Shinnaga, H, Stamatellos, D, Tang, Y -W, Traficante, A, Vastel, C, Viti, S, Walsh, A, Wang, H, Wang, J, Ward-Thompson, D, Whitworth, A, Wilson, C D, Xu, Y, Yang, J, Yuan, Y -L, Yuan, L, Zavagno, A, Zhang, C, Zhang, H -W, Zhou, C, Zhou, J, Zhu, L, and Zuo, P

Abstract

We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-μm continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of NH2 > 5 × 1021 cm−2. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other.

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