adsabs/AstroCLIMB huggingface dataset:
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G351.0−5.4 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G355.9−2.5 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G350.0−2.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the PWN and its pulsar near SNR G343.1−2.3. Our flux density measurements are shown at 1335 MHz in red. Other flux density values were taken from Giacani et al. (2001).
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the PWN of SNR G343.1−2.3 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner. The pulsar is seen as a bright point source in the center of the PWN.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G356.2+4.5 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G353.9−2.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G343.1−2.3 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The distributions of 39,445 BHB star candidates with (S/N) g  > 10 and ∣Glat∣ > 20° on the EWCa II K vs. (BP − RP)0 plane. The red solid lines represent EWCa II K as a function of (BP − RP)0 for stars with [Fe/H] = −1 and −3, respectively, which are adopted from Wilhelm et al. (1999a).
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: Distributions of 7955 + 143, 8955 + 163, and 4283 + 23 BHB candidates (gray dots) and BS stars (blue dots) from left to right for Hδ, Hγ, and Hβ in the b vs. c plane. b is an effective indicator of the surface gravity and c represents the temperature. The BHB candidates and BS stars are selected from Figure 5. There is a clear gap between them. The enclosed green boxes represent the criteria for selecting BHB stars.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The contours of the LAMOST DR5 spectra with (S/N) g  > 10 and ∣Glat∣ > 20° on the EWG4300 vs. EWHγ  plane. The blue dashed line with the asterisks and the red dashed line with the unfilled circles represent the loci of the main-sequence and giant stars provided by Liu et al. (2015), respectively. The red solid lines are the line indices’ cuts of Hγ at 4341 Å and G4300 around 4300 Å for the selection of BHB candidates (mainly A-type stars).
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: Distributions of the 23,528 + 552 BHB candidates (the contours) on the D 0.2 vs. f  m  plane for the Hδ, Hγ, and Hβ lines, from left to right, respectively. The red box represents the criteria to further select BHB stars (see the text for details).
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The Hδ, Hγ and Hβ regions in their normalized spectrum of a BHB star (solid line) and a BS star (dotted line) with similar effective temperatures. It is clear that the Balmer lines of the BHB star are narrower than those of the BS star at 20% below the local continuum, which is mainly due to the lower surface gravity of BHB stars.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The distributions of 765 (Xue et al. 2011) (the top panel) and 5198 BHB stars (Vickers et al. 2021; the bottom panel) on the EWCa II K vs. (BP − RP)0 plane. These BHB stars have (S/N) g  ≤ 10 and ∣Glat∣ > 20° and are cut by line indices. The red solid lines are the same in Figure 2.
Paper: Identification of Blue Horizontal-branch Stars from LAMOST DR5
Authors: Jie Ju, Wenyuan Cui, Zhenyan Huo, Chao Liu, Xiangxiang Xue, Jiaming Liu, Shuai Feng, Mingxu Sun, Linlin Li
Figure caption: The spectrum of a typical BHB star with high S/N (top) and the Hδ, Hγ, and Hβ regions of the same star in its normalized spectrum (bottom). We also show the (f  m , D 0.2) parameters of the above three Balmer lines, which are used to select this sample spectrum and, are labeled.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the PWN inside SNR G326.3−1.8. Our flux density measurement is shown at 1335 MHz in red. We also integrated the PWN emission at 935 MHz from the observations of Ball et al. (2023). Other flux density values were taken from Dickel et al. (2000).
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G327.6+14.6 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G296.5+10.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 12″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G315.4−2.3 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the SNR G292.0+1.8's core and plateau. Our flux density measurements are shown at 1335 MHz in red. Other flux density values were taken from Gaensler & Wallace (2003) and are shown in black.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G332.5−5.6 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G299.2−2.9 at 1335 MHz in Galactic coordinates. The resolution of the image is 15″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G326.3−1.8 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G312.5−3.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G4.2−3.5 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of Kepler’s SNR (G4.5+6.8) at 1335 MHz in Galactic coordinates. The resolution of the image is 8″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G4.8+6.2 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G5.2−2.6 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G6.4+4.0 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G5.9+3.1 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G7.7−3.7 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the SNR G55.7+3.4. Our flux density measurement is shown at 1335 MHz (red). Other flux density values (black) were taken from Caswell & Goss (1970), Goss et al. (1977), Bhatnagar et al. (2011), and Sun et al. (2011).
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G55.7+3.4 at 1335 MHz in Galactic coordinates. The resolution of the image is 15′ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Radio continuum spectrum of the SNR G272.2−3.2. Our flux density measurement is shown at 1335 MHz in red. Other flux density values (black) were taken from Duncan et al. (1997a).
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G292.0+1.8 at 1335 MHz in Galactic coordinates. The resolution of the image is 15″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G284.3−1.8 at 1335 MHz in Galactic coordinates. The resolution of the image is 15″ as indicated by the white circle in the lower-left corner. The location of the young pulsar J1016−5857 is indicated by the white asterisk.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G53.6−2.2 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G272.2−3.2 at 1335 MHz in Galactic coordinates. The resolution of the image is 15″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G57.2+0.8 at 1335 MHz in Galactic coordinates. The resolution of the image is 15″ as indicated by the white circle in the lower-left corner.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Total power MeerKAT image of the SNR G261.9+5.5 at 1335 MHz in Galactic coordinates. The resolution of the image is 10″ as indicated by the white circle in the lower-left corner.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: Left panel: the black dots are the MCCF vs. time difference of the between GECAM-C and GBM observations of Crab Pulsar profiles in one year; the red dotted line represents the best time difference. Right panel: distribution of time differences obtained by MC; the red line is obtained by fitting a Gaussian function. Therefore, the time difference is 3.37 ± 3.27 μs, which is consistent with the result obtained by fitting each month (i.e., 2.02 ± 3.02 μs) within the error.
Paper: Calibration of the Timing Performance of GECAM-C
Authors: Shuo Xiao, Ya-Qing Liu, Ke Gong, Zheng-Hua An, Shao-Lin Xiong, Xin-Qiao Li, Xiang-Yang Wen, Wen-Xi Peng, Da-Li Zhang, You-Li Tuo, Shi-Jie Zheng, Li-Ming Song, Ping Wang, Xiao-Yun Zhao, Yue Huang, Xiang Ma, Xiao-Jing Liu, Rui Qiao, Yan-Bing Xu, Sheng Yang, Fan Zhang, Yue Wang, Yan-Qiu Zhang, Wang-Chen Xue, Jia-Cong Liu, Chao Zheng, Chen-Wei Wang, Wen-Jun Tan, Ce Cai, Qi-Bin Yi, Peng Zhang, Xi-Hong Luo, Jiao-Jiao Yang, Qi-Jun Zhi, Ai-Jun Dong, Shi-Jun Dang, Lun-Hua Shang, Shuang-Nan Zhang
Figure caption: Spectral lags of Crab profiles at different energies observed by GECAM-C (red), GECAM-B (blue), and GBM (black). Note that for GECAM-C and GBM the lag is compared to 8–14 keV and for GECAM-B the lag is compared to 14–23 keV. The dotted lines represent the results obtained by fitting them with a linear function.
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: The brief architecture of our model. The meaning of all types of signs is marked on the right of the figure. Top: Res-UNet consists of an encoder and a decoder both composed by five convolutional blocks (vertical blocks in blue) and four skip connections (virtual arrow in gray). Bottom: DexiNed consists of an encoder composed by six main blocks and a decoder composed by six upsample blocks (horizontal blocks in gray). More details are given in Section 2.
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: (a) The coronal loop image observed by TRACE 171 Å of 1998 May 19, 22:21 UT (Handy et al. 1999). (b) The black–white color reversal result. The black areas show the observed coronal loops and other noncoronal structures, with black indicating high fluxes in this image so as to show the details.
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: A labeled example of coronal loop image observed by TRACE 171 Å of 1998 May 19, 22:21 UT. The red mask represents the labeled area where we have artificially added the presence of coronal loop structures, while black represents the background.
Paper: Coronal Loop Detection Using Multiscale Convolutional Neural Networks
Authors: Yunzhi Wang, Bo Liang, Song Feng
Figure caption: Image of the coronal loop detection result in this paper. All of the black curves in Figure 4 represent coronal loops identified by the proposed method.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G358.0+3.8. Peak Faraday depth in color given by scale bar at the top labeled in radians per square meter with Stokes I contours (nearly invisible white on dark background, black on bright) at −0.05, 0.05, 0.2, 0.8, 3.2, 12.8, and 51.2 mJy beam−1. The SNR itself has only very weak total and polarized intensity. The restoring beam is 7.″4 × 7.″3 at position angle = −6.°8.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: G356.2+4.5. Peak Faraday depth in color given by scale bar at the top labeled in radians per square meter with Stokes I contours at −0.1, 0.1, 0.4, 1.6, 6.4, 25.6, and 102.4 mJy beam−1. The restoring beam is 7.″6 × 7.″2 at position angle = −71.°4. The SNR itself has only weak polarization.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Like Figure 46 but showing G4.8+6.2. The restoring beam is 7.″9 × 7.″3 at position angle = −47.°5.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Like Figure 46 but showing G355.9−2.5. The restoring beam is 7.″7 × 7.″3 at position angle = −66.°4.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Like Figure 46 but showing G7.7−3.7. The restoring beam is 7.″6 × 7.″5 at position angle = −44.°3.
Paper: MeerKAT 1.3 GHz Observations of Supernova Remnants
Authors: W. D. Cotton, R. Kothes, F. Camilo, P. Chandra, S. Buchner, M. Nyamai
Figure caption: Like Figure 46 but for G53.6−1.8. The restoring beam is 8.″1 × 7.″7 at position angle = 6.°0.
Paper: Molecular Deuterations in Massive Starless Clump Candidates
Authors: Kai Yang, Junzhi Wang, Keping Qiu, Tianwei Zhang
Figure caption: Line profiles of the 46 DCO+ J = 1−0 detected clumps. The Gaussian-fitting result for each spectrum is shown in magenta. The blue dashed vertical line represents the LSR velocity of NH3 for each SCC derived from Svoboda et al. (2016). The x-axis is velocity in kilometers per second and the y-axis is T mb in kelvin.
Paper: Molecular Deuterations in Massive Starless Clump Candidates
Authors: Kai Yang, Junzhi Wang, Keping Qiu, Tianwei Zhang
Figure caption: Line profiles of the 51 DNC J = 1−0 detected clumps. The Gaussian-fitting result for each spectrum is shown in magenta. The blue dashed vertical line represents the LSR velocity of NH3 for each SCC derived from Svoboda et al. (2016). The x-axis is velocity in kilometers per second, and the y-axis is T mb in kelvin.
Paper: Molecular Deuterations in Massive Starless Clump Candidates
Authors: Kai Yang, Junzhi Wang, Keping Qiu, Tianwei Zhang
Figure caption: Line profiles of the 12 DCN J = 1−0 detected clumps. The Gaussian-fitting result for each spectrum is shown in magenta. The blue dashed vertical line represents the LSR velocity of NH3 for each SCC derived from Svoboda et al. (2016). The x-axis is velocity in kilometers per second, and the y-axis is T mb in kelvin.
Paper: Molecular Deuterations in Massive Starless Clump Candidates
Authors: Kai Yang, Junzhi Wang, Keping Qiu, Tianwei Zhang
Figure caption: The velocity-integrated maps of deuterated and 13C isotopic molecular lines for BGPS 4402. The integrated-velocity range, shown at the bottom-right corner, is derived after combining the Gaussian-fitting line widths for each deuterated molecular line and 13C isotopologue. For H13CO+, DCO+, HN13C, DNC, H13CN, N2D+ J = 1−0, and DCO+ J = 2−1, the contours start from 3σ in steps of 1σ, with σ = 0.14, 0.10, 0.17, 0.10, 0.13, 0.05, and 0.05 K km s−1, respectively. The crosses represent peaks in the velocity-integrated maps of different molecular lines and the red star represents the 1.1 mm continuum peak obtained from Svoboda et al. (2016). The beam sizes for H13CO+, DCO+ J = 1−0, and DCO+ J = 2−1 of ∼28″, ∼34″, and ∼16″ are shown as red circles at the bottom-left corners in their integrated-intensity maps. The averaged spectra for column density estimation are derived in the regions enclosed by blue squares.
Paper: Molecular Deuterations in Massive Starless Clump Candidates
Authors: Kai Yang, Junzhi Wang, Keping Qiu, Tianwei Zhang
Figure caption: The velocity-integrated maps of deuterated and 13C isotopic molecular lines for BGPS 3125. The integrated-velocity range, shown at the bottom-right corner, is derived after combining the Gaussian-fitting line widths for each deuterated molecular line and 13C isotopologue. For H13CO+, DCO+, HN13C, DNC, H13CN, DCN J = 1−0, and DCO+, DCN J = 2−1, the contours start from 3σ in steps of 1σ, with σ = 0.12, 0.07, 0.12, 0.05, 0.13, 0.08, 0.11, and 0.12 K km s−1, respectively. The crosses represent peaks in the velocity-integrated maps of different molecular lines and the red star represents the 1.1 mm continuum peak obtained from Svoboda et al. (2016). The beam sizes for H13CO+, DCO+ J = 1−0, and DCO+ J = 2−1 of ∼28″, ∼34″, and ∼16″ are shown as red circles at the bottom-left corners in their integrated-intensity maps. The averaged spectra for column density estimation are derived in the regions enclosed by blue squares.