adsabs/AstroCLIMB huggingface dataset:
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: (a) A two-color composite integrated intensity map of 12CO (1–0), integrated from −5 km s−1 to 0 km s−1 (depicted in blue color and contours ranging over 16–24 K km s−1 with a step of 2 K km s−1) and from 0 km s−1 to 4 km s−1 (in red, contours ranging over 12–20 K km s−1 with a step of 2 K km s−1) of the G178 cloud. The cuts labeled A, B, and C identify the paths along which PV slices, with a width of one pixel, were extracted, sampling the core regions A2-5, A2-7, and the filament, respectively. (b) Similar to (a) but for 13CO (1–0). The contours for the blueshifted cloud range over 8–16 K km s−1 with a step of 2 K km s−1, and for redshifted cloud are 4–10 K km s−1 with a step of 2 K km s−1. Panel (c), (e), (g) PV diagrams of 12CO (1–0), along cuts A, B, and C. (d), (f), (h) PV diagrams of 13CO (1–0). The two horizontal dashed lines represent the systemic velocities of the blueshifted cloud (−1.2 km s−1) and redshifted cloud (0.8 km s−1). The bridging features are detected within the intermediate velocity range between the dashed lines, marked with black boxes. The peak positions of red and blue clouds are highlighted by white arrows on the PV cuts. Panels (g) and (h) show V-shaped structures noted by white arrows, indicating collisional interactions (T. J. Haworth et al. 2015). The positions of possible collisional interactions are marked out by filled cyan circles in panels (a) and (b).
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: Molecular spectra at 10 continuum peaks. From bottom to top of each subplot, the spectra of HCO+, H2O, N2H+, CH3OH, and H2CO are added by 0, 2, 4, 6, and 8 K, respectively. The intensity of H2CO, N2H+, and HCO+ is multiplied by a factor of 2, 4, and 2, respectively. The green lines show one-component fitting for H2CO, HCO+, and hyperfine structure fitting for N2H+. No detections of CH3OH and H2O are found for 10 peaks.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: Pixel-by-pixel spectra of 12CO (1–0), 13CO (1–0), and C18O (1–0) in black, red, and blue, respectively. In each subplot, the x-axis spans −5 km s−1 to 5 km s−1, and the y-axis extends from −1 K to 12 K for 12CO (1–0), −1–8 K for 13CO (1–0), and −1–6 K for C18O (1–0). The spectra exhibit two discernible velocity components, with their systemic velocities marked by blue dashed lines at −1.2 km s−1 and 0.8 km s−1. From east to west, 13CO (1–0) velocity structure transits from blue- to redshifted components, with broad dual peaks at the central region that coincide with the 850 μm continuum shown as the background. The C18O lines behave similar to the 13CO and peak at analogous velocities.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: CO J = 1–0 and J = 2–1 spectra at 10 continuum peaks, except A1, which was not observed by CO J = 2–1. For each plot, the three lines of 12CO, 13CO, and C18O with corresponding single-component Gaussian fitting results are colored blue, green, and red, respectively. The velocity ranges from −6 km s−1 to 6 km s−1 for all plots.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: Upper panel: WISE three-color composite image (RGB: 22 μm, 12 μm, 3.4 μm), overlaid with associated YSOs and 850 μm continuum contours. Class I YSOs are depicted in open yellow diamonds, Class II YSOs in open squares, and shock knots in open circles. The black cross shows the IRAS point source. The continuum peaks are marked as white crosses and names on the side. Lower panel: the color–color diagram for the bands 3.4 μm, 4.6 μm, and 12 μm used to classify YSOs associated with G178. The dashed lines denote the criteria used by X. P. Koenig et al. (2012) and X. P. Koenig & D. T. Leisawitz (2014) to delineate the YSO classes.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: (a) The 13CO (1–0) integrated intensity map is shown in color scale, and C18O (1–0) map is shown in black contours at levels of 0.3–1.5 K km s−1, increasing in steps of 0.2 K km s−1. The positions of the ten 850 μm continuum peaks are indicated with crosses and labeled. (b) The 13CO (2–1) integrated intensity map is shown in color scale, and the C18O (2–1) map is shown in black contours from 1.4 to 2.2 K km s−1, in steps of 0.2 K km s−1. The corresponding beam sizes are plotted as filled white circles. (c), (d) Integrated intensity ratios of 12CO (1–0) to 13CO (1–0) and 12CO (2–1) to 13CO (2–1). The 850 μm continuum peaks are labeled.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: Moment 1 maps of 13CO (1–0) (left panel) and 12CO (2–1) (right panel) in color scale, with corresponding moment 2 maps overlaid as green contours. The contours for the line widths of 13CO (1–0) are 1.7–2.5 km s−1 with a step of 0.2 km s−1, and for 12CO (2–1) are 3.4–4.0 km s−1 with a step of 0.2 km s−1. The continuum peaks are labeled and found to locate at the intermediate velocity region. The beam sizes are shown as filled white circles.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: The channel maps of 12CO (1–0) (in color) and 13CO (1–0) (black contours) are shown. The color scale is in units of K km s−1. Each map features a channel width of 0.5 km s−1, with the corresponding velocities (in units of kilometers per second) marked at the bottom left corner of each subplot. The overlay of 10 continuum peaks in white crosses effectively delineates the boundaries of the two colliding clouds.
Paper: An S-shaped Filament Formed Due to Cloud–Cloud Collision in Molecular Cloud G178.28-00.61
Authors: Tianwei Zhang, 天惟 张, Tie Liu, Yuefang Wu, Linjing Feng, Sihan Jiao, Derek Ward-Thompson, Alessio Traficante, Helen J Fraser, James Di Francesco, Doug Johnstone, Paul F. Goldsmith, Yasuo Doi, Xunchuan Liu, Chang Won Lee, Fengwei Xu, Ram K. Yadav, Glenn J White, Leonardo Bronfman, Yi-Jehng Kuan, Kee-Tae Kim, Donghui Quan
Figure caption: Schematic illustrations of possible CCC in G178 as presented in the Z–Y plane (left panel) and in the X–Y plane (right), where the Z-axis is along the line of sight. The collision axis is inclined at an angle of relative motion to the line of sight of θ = 50° (see Section 4.1.3).
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Comparison of ATOMS 3 mm and QUARKS 1.3 mm continuum images for two protocluster clumps. The black dashed circle in each panel defines the field of view of the QUARKS survey. Left panels ((a), (c)): ATOMS 3 mm continuum emission. The dashed contour levels are [3, 6, 12, 24, 48, 96] rms, with rms ∼1.4 and ∼0.4 mJy beam−1 for I17271-3439 and I17244-3536, respectively. Red contours correspond to integrated emission of the H40α recombination line representative of ionized gas from the ATOMS survey, with rms ∼0.2 and ∼0.1 Jy beam−1 km s−1 for I17271-3439 and I17244-3536, respectively. Right panels ((b), (d)): QUARKS TM2+ACA 1.3 mm continuum emission. The contour levels are the same as in the left panels, but with rms ∼2.1 and ∼0.4 mJy beam−1 for I17271-3439 and I17244-3536, respectively. The cross symbols correspond to the cores extracted from 1.3 mm continuum emission using the getsf algorithm, where black markers denote those detected by the algorithm at a configuration with a minimum source size employing the beam size, while red markers correspond to relatively faint cores detected at the other configuration employing half-beam. The beam sizes of ATOMS and QUARKS TM2+ACA continuum emission are shown on the lower left, and the 0.1 pc scale bar is on the upper right of each panel.
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Distributions of core separation within all QUARKS protocluster clumps. To visualize the distance effect on the distribution, the clumps were devided into four quartile groups based on their measured distances: ≤2.85, (2.85–3.76), (3.76–5.67), and ≥5.67 kpc, with each quartile coded by a distinct color. The count of the corresponding groups is 36, 35, 35, and 35 protocluster clumps, respectively. (a) Distribution of the angular separation. The number of core separation measurements for each group of protocluster clumps is 375, 363, 366, and 317, respectively, as shown in upper-right legend. The black and red dashed lines indicate the peak of the distribution (∼2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5), and the typical beam size (∼1″) of our observations, respectively. (b) Distribution of the linear core separation. The median value of the distribution for each group of protocluster clumps is 0.03, 0.05, 0.07, and 0.12 pc, respectively, as shown in upper-right legend. The black dashed line indicates the peak of this distribution.
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Demonstration of core-averaged spectra covered in the four spectral windows of the QUARKS survey for dense cores representative of different stages of evolution, including candidates of (a) starless cores, (b) warm cores, (c) hot cores, (d) UCHII-h cores, and (e) UCHII-l cores. The upper-left corner of each panel displays the count of molecular spectral lines tentatively detected in each core. The horizontal dashed line represents the noise level of the spectra. Several common molecular line transitions are labeled.
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Flow chart for ALMA-QUARKS ACA and TM2 combined data reduction. The elliptical boxes denote the raw data and the final reduced data. The rectangle indicates a specific processing step, while the parallelogram indicates an intermediate product during the data reduction.
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Emission of the H30α line toward I12320-6122 Core 1. (a) The black histogram represents the observed core-averaged spectrum while the red line is the Gaussian fitting. (b) QUARKS TM2+ACA continuum image of I12320-6122 Core 1. The contour levels are the same as in Figure 2, but with rms = 1 mJy beam−1. The red contours show velocity-integrated emission of H30α over [–90, 10] km s−1, with rms = 0.5 Jy beam−1 km s−1. The black circle delineates I12320-6122 Core 1. The beam size of the TM2+ACA observations is shown on the lower left, and the 0.05 pc scale bar is on the upper-right corner.
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Pie chart for statistics of core classifications.
Paper: The ALMA-QUARKS Survey. III. Clump-to-core Fragmentation and Searches for High-mass Starless Cores
Authors: Dongting Yang, Hong-Li Liu, Tie Liu, Xunchuan Liu, Fengwei Xu, Sheng-Li Qin, Anandmayee Tej, Guido Garay, Lei Zhu, Xiaofeng Mai, Wenyu Jiao, Siju Zhang, Sami Dib, Amelia M. Stutz, Aina Palau, Patricio Sanhueza, Annie Zavagno, A. Y. Yang, Xindi Tang, Mengyao Tang, Yichen Zhang, Pablo García, Tianwei Zhang, Anindya Saha, Shanghuo Li, Paul F. Goldsmith, Leonardo Bronfman, Chang Won Lee, Kotomi Taniguchi, Swagat Ranjan Das, Prasanta Gorai, Ariful Hoque, Li Chen, Zhiping Kou, Jianjun Zhou, Yankun Zhang, L. Viktor Tóth, Tapas Baug, Xianjin Shen, Chuanshou Li, Jiahang Zou, Ankan Das, Hafiz Nazeer, L. K. Dewangan, Jihye Hwang, James O. Chibueze
Figure caption: Example of the MST results (green segments). QUARKS TM2+ACA 1.3mm continuum emission is shown in a color scale with dense cores (i.e., cross symbols) overlaid. The contour levels are the same as in Figures 2(b) and (d). The beam size of the QUARKS data is shown on the lower left, and the 0.1 pc scale bar is on the upper right.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Examples of six individual spectra that exhibit emission of at least one CL in the optical. The SDSS data, corrected for redshift and galactic extinction, are plotted in black, while the model and each of its components (AGN power law, host galaxy, and emission lines) are overlaid on the spectra. Each CL is labeled, and the object’s SDSS Spec Object ID and coordinates are labeled in each plot’s title.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Bolometric luminosity, black hole mass, and Eddington ratio distributions of our sample compared with the parent sample of quasars from Y. Shen et al. (2011). Quantities displayed are taken directly from the catalog values provided by Y. Shen et al. (2011).
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Example spectral fits for galaxies that show outflows in the [O III] λ5007 line.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Distributions of each CL over the luminosity (L), FWHM, and velocity shift (voff) organized by the critical density in cubic centimeters. The luminosity is in ergs per second, and FWHM and voff are in kilometers per second. Each line is annotated on the right side of the corresponding ﹩{\mathrm{log}}\,\rho ﹩ bin. Note that the vertical axes are not scaled logarithmically; each critical density is shown categorically.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Distributions of each CL over the luminosity (L), FWHM, and velocity shift (voff) organized by the IP in eV. The luminosity is in ergs per second, and FWHM and voff are in kilometers per second. Each line is annotated on the right side of the corresponding IP bin. Note that the vertical axes are not scaled linearly; each ionization potential is shown categorically.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Distributions of each CL over the EW and CL to [O III] λ5007 luminosity ratio, organized by the critical density in cubic centimeters. The EW is in angstroms. Each line is annotated on the right side of the corresponding ﹩{\mathrm{log}}\,\rho ﹩ bin. Note that the vertical axes are not scaled logarithmically; each critical density is shown categorically.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Distributions of each CL over the EW and CL to [O III] λ5007 luminosity ratio, organized by the IP in eV. The EW is in angstroms. Each line is annotated on the right side of the corresponding IP bin. Note that the vertical axes are not scaled linearly; each ionization potential is shown categorically.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: A series of logarithmic scatter plots showing correlations between individual CL fluxes and the WISE 2 band fluxes. Each panel has identical vertical and horizontal scales. Best-fit power laws are plotted with dashed lines over the data, and the best-fit parameters are shown in the legend of each plot as a function of FW2, the W2 flux. The points are colored according to the W1 − W2 color (in magnitudes). Each panel lists the Spearman correlation coefficient r and the corresponding p-value of the distribution.
Paper: The CLASS Quasar Catalog: Coronal Line Activity in Type 1 SDSS Quasars
Authors: Sara Doan, Shobita Satyapal, Michael Reefe, Remington O. Sexton, William Matzko, Jeffrey D. McKaig, Nathan J. Secrest, Jenna M. Cann, Ari Laor, Gabriela Canalizo
Figure caption: Histograms of detection fractions for the various CLs indicated as a function of bolometric luminosity. Number counts are listed for each bin, and error bars are calculated using binomial statistics using a 68% confidence interval.