adsabs/AstroCLIMB huggingface dataset:
Paper: Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections
Authors: Stephan G. Heinemann, Chaitanya Sishtla, Simon Good, Maxime Grandin, Jens Pomoell
Figure caption: MHD simulation of an HSS interacting with a magnetic obstacle in cartesian coordinates comoving with the magnetic obstacle. The dashed lines indicate the initial condition of the simulation while solid lines present the solar wind plasma at ≈19.4 hr simulation time. Panel (a) shows the solar wind v  x  velocity component (in blue), the Alfvén velocity ﹩{v}_{a}=B/\sqrt{{\mu }_{0}\rho }﹩ (in red), and the number density n (in green). The magnetic fields are presented in panel (b). Panel (c) presents the plasma temperature T (in red), and the plasma beta β (in purple). Finally, in panel (d) we show the simulated geomagnetic activity index DST (in red) according to B.3. The shaded regions mark the solar wind structures corresponding to the magnetic obstacle, HSS, and the compressed BL at ≈19.4 hr simulation time.
Paper: Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections
Authors: Stephan G. Heinemann, Chaitanya Sishtla, Simon Good, Maxime Grandin, Jens Pomoell
Figure caption: Distribution of flux tube orientations. The orientations are labeled according to the convention in Bothmer & Schwenn (1998). N, S, E, and W correspond to north (B  z  > 0), south (B  z  < 0), east (B  y  > 0), and west (B  y  < 0). In the abbreviation, the first to third letters represent the variation of the magnetic field vector in the respective component, and the middle letter indicates the direction of the magnetic field on the flux tube axis. The inset shows the distribution of the flux rope helicity between left-handed (LH) and right-handed (RH) flux ropes.
Paper: Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections
Authors: Stephan G. Heinemann, Chaitanya Sishtla, Simon Good, Maxime Grandin, Jens Pomoell
Figure caption: Correlation matrix depicting the properties of the HSS–ICME interaction. The Spearman correlation coefficient is presented above the diagonal. The size of the circle indicates the significance of the correlation (p-value), with larger circles denoting p < 0.001 and the absence of circles indicating p > 0.05, respectively. Corresponding scatterplots are displayed below the diagonal. The distribution of the parameters is shown along the diagonal.
Paper: Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections
Authors: Stephan G. Heinemann, Chaitanya Sishtla, Simon Good, Maxime Grandin, Jens Pomoell
Figure caption: Superposed epoch analysis of solar wind velocity (v  p ; top panel) and the geomagnetic activity index (SymH, bottom panel) centered on the time when the HSS velocity reaches its maximum. The colored lines and shaded areas (velocity in blue, geomagnetic index in red) denoted with "Grandin et al." represent the median and the 95th percentiles of the 478 SIRs with ﹩{{SymH}}_{\min }\lt -30\,\mathrm{nT}﹩ detailed in Grandin et al. (2019). Overlaid in green and purple are the results from our 23 events.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: LyC leakers having off-centered or extended emission in FUV 154W band. The sequence and symbols are the same as in Figure 1. Spurious sources (see Section 4) are highlighted by dashed black squares in the F154W band. We quote the magnitude (S/N) of such sources from top to bottom. On the first row, peaks in the north and northeast are due to sources observed in HST F435W (not seen in the 10″ × 10″) cutouts shown; third row in the northwest, southwest, and southeast have magnitudes (S/N): 26.61 (2.56), 26.42 (2.88), and 27.0 (2.01) respectively.
Paper: Classification of Enhanced Geoeffectiveness Resulting from High-speed Solar Wind Streams Compressing Slower Interplanetary Coronal Mass Ejections
Authors: Stephan G. Heinemann, Chaitanya Sishtla, Simon Good, Maxime Grandin, Jens Pomoell
Figure caption: Example of an HSS interacting with a slower ICME leading to an intensified geomagnetic response in 2011 February. Panel (a) displays the solar wind velocity (in blue) and number density (in orange), while panel (b) presents the total magnetic field strength and its components in GSM coordinates. Panel (c) exhibits proton temperature (in red) and plasma beta (in green), followed by (d) the dynamic solar wind pressure and (f) the geomagnetic activity index, SymH (in red). The dashed and dotted lines in panel (f) correspond to the predicted DSTs according to Appendix A. The vertical sections mark the boundaries of the magnetic structure, BL, and HSS.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: The LyC absolute f esc estimated using Bassett et al. (2021) IGM model in black open circles for the ten leakers in our sample compared to individual LyC leakers at lower (z < 1, blue filled circles) and higher redshifts (z > 2, red filled circles). The low-z leakers are taken from Leitet et al. (2013), Borthakur et al. (2014), Leitherer et al. (2016), Izotov et al. (2016, 2018, 2021), and Flury et al. (2022). The high-z leakers are taken from Shapley et al. (2016), Vanzella et al. (2010, 2016), Bian et al. (2017), Fletcher et al. (2019), Rivera-Thorsen et al. (2019), and Marques-Chaves et al. (2021, 2022). The individual detection at z = 1.42 from Saha et al. (2020) is indicated by the gray filled circle.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: Top: the UVIT F154W-weighted IGM transmission distributions of I14 and B21 for the redshifts corresponding to the LyC leakers. Each curve was binned according to Freedman–Diaconis. The I14 simulations resulted in more clear sight lines compared to B21 for the same redshifts, which would result in lower f esc (see Equations (2) and (3)). Bottom: escape fraction distribution of the LyC leakers using IGM attenuation models from I14 on left and B21 on the right.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: LyC leakers indicated by red circles in the UVIT AUDFn field. Blue polygon is the 3D-HST GOODS North spectral coverage.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: Left: redshift histogram of sources having Hα and O[III] flux S/N > 3 and redshift <2 (Blue) and those having detection in UVIT FUV (39 sources) out of 178 sources selected from 3D-HST. Right: SFR–stellar mass plot of the LyC leakers (blue filled circles) along with other non-leaker galaxies (gray filled circles) at 1 < z < 1.5. The solid black line is a linear fit to the sample with a slope of 0.46.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: Left: FUV magnitude distribution of clean sources having detection in UVIT FUV (39 sources) out of 178 sources selected from 3D-HST. Right: FUV S/N distribution of 39 clean sources.
Paper: Lyman Continuum Leakers in the AstroSat Ultraviolet Deep Field: Extreme-ultraviolet Emitters at the Cosmic Noon
Authors: Suraj Dhiwar, Kanak Saha, Soumil Maulick, Brent M. Smith, Chayan Mondal, Harry I. Teplitz, Marc Rafelski, Rogier A. Windhorst
Figure caption: The stacked image of LyC (FUV F154W) of the six LyC leakers having emission within UVIT PSF FWHM ∼ 1.″6.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: Left panel: the grids of sSFR vs. EW(Hα) from a set of delayed SFH models overlaid on the 2D histograms of sSFR vs. EW(Hα) for all pixels. The diamonds show expectations from SED models with delayed-τ SFHs at different ages and with different τ values. The colors of the crosses correspond to models of different ages and τ values. The models with the same age are linked with a solid colored line. The τ values are labeled by each model: τ = 0.1, 0.2, 5, 1, 2 Gyr. The 2D histogram is the same as in Figure 4, but in gray. All models assume solar metallicity. The arrows on models at an age = 0.5 Gyr show the shift in the models if we adopt a gas-phase metallicity Z/Z ⊙ = 0.6 and a stellar metallicity Z/Z ⊙ = 0.16 (see Section 5.2.2). The black error bar shows the median error of individual, spatially resolved pixels. Right panels: the 2D histograms for pixels in four bins of galactocentric radius, normalized by the galaxies’ effective radii (r eff) measured at rest frame 1.2 μm (see text). The radii of each bin are listed in each panel. The colored lines show the same models as in the left panel.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: The radial gradients of EW(Hα) vs. sSFR (left), and the radial gradients of EW(Hα) vs. stellar-mass-weighted age (right). Here the gradients are the slope measured for the radial gradients for each galaxy (see Figure 5). In each plot, the histograms show the distribution of EW(Hα), sSFR, and age gradients for the individual galaxies. The markers in the scatter plots are color-coded by the distance of the galaxies from the SFMS (positive/negative values are above/below the SFMS). Galaxies identified with an AGN are marked by open red diamonds and orange squares. The best-fit linear relations are shown as the purple dashed lines, along with 400 random draws from the posterior (faint gray lines).
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: Example of the EW(Hα), sSFR, and age spatial maps and their radial gradients for galaxies in our sample. The sSFR and age maps use the Voronoi tessellation (see Section 3.2). In the left panels, the red crosses mark the luminosity-weighted galaxy centroid derived from the F160W image. Orange contours are 5σ, 10σ, 25σ, 50σ, and 100σ in the F160W image. The example here shows a galaxy with no AGN indication (NGDEEP_01614). The middle panels show the radial gradient of the EW(Hα), sSFR, and age. The purple solid lines show best-fit linear relations, along with 400 random draws from the posterior. Gray circles in the sSFR and age panels show Voronoi bins that lack EW(Hα) measurements, which are excluded in the linear fitting. The right panels show SED fits at three different radial bins (“inner,” “middle,” and “outer” regions, from top to bottom), indicated by the red boxes in the middle panels. Each panel shows the observed photometric fluxes with errors (purple), the CIGALE-derived best-fitted model (black curve), and model photometry (red circles). The best-fitted CIGALE model is the sum of the contributions from a dust-attenuated stellar emission and nebular emission (the unattenuated stellar model is shown in blue). A galaxy with an AGN is shown in Figure 6. The maps and radial gradients of the remainder of our galaxies are shown in the Appendix.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: Same as Figure 5, but for a galaxy flagged with an AGN (NGDEEP_02071). For all galaxies with an AGN, we mask the central 3 × 3 pixels to remove possible contamination (see Section 2.4, as seen in this galaxy). The maps and radial gradients of the remainder of our galaxies are shown in the Appendix.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: The EW(Hα), sSFR, and age spatial maps for galaxies with atypical gradients. The top row shows NGDEEP_00922, which shows a large offset from the relationship in both EW(Hα)–sSFR and EW(Hα)–age gradients (Section 4.2). The middle and bottom rows show the two galaxies with negative EW(Hα) gradients (NGDEEP_01831 and NGDEEP_01948, respectively; Section 5.3).
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: The EW(Hα), sSFR, and age maps and their radial gradients for five galaxies in our sample. The same as Figure 5 for each galaxy.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: The EW(Hα), sSFR, and age maps and their radial gradients for six galaxies in our sample. The same as Figure 5 for each galaxy.
Paper: The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE
Authors: Ying Li, Zhichen Jing, De-Chao Song, Qiao Li, Jun Tian, Xiaofeng Liu, Ya Wang, M. D. Ding, Andrea Francesco Battaglia, Li Feng, Hui Li, Weiqun Gan
Figure caption: Overview of the on-disk X2.1 flare on 2023 March 3. (a) Light curves of GOES SXR 1–8 Å flux, its time derivative, and available HXR fluxes from Fermi. (b) Emission curves of WST continuum at 3600 Å, HMI continuum at ∼6173 Å, CHASE continuum at ∼6569 Å, and CHASE Fe I λ6569 line (integrated over ± 0.5 Å) for the flaring region marked by the black dashed box in panels (c)–(h). The vertical dashed and dashed–dotted lines in panels (a) and (b) indicate the peak times (∼17:50 and ∼17:52 UT) of SXR time derivative and SXR 1–8 Å flux, respectively. (c)–(h) Multiwavelength images of the flaring AR at ∼17:50 UT. The black dashed box marks the flaring region that is integrated over for the emission curves in Figure 1(b). The yellow dotted box in panel (f) is used to estimate the uncertainties of white-light emission enhancements. The pink and cyan contours in panel (h) represent the positive and negative magnetic polarities at ± 200 G, respectively.
Paper: The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE
Authors: Ying Li, Zhichen Jing, De-Chao Song, Qiao Li, Jun Tian, Xiaofeng Liu, Ya Wang, M. D. Ding, Andrea Francesco Battaglia, Li Feng, Hui Li, Weiqun Gan
Figure caption: (a) and (b) Maps of relative enhancements of HMI continuum, CHASE Fe I line center, CHASE continuum, and WST continuum emissions at ∼17:50 and ∼17:52 UT for the X2.1 flare. The solar limb is marked by a white line. In each panel, the yellow contours indicate an enhancement level of 20% and the three colored plus symbols denote three representative brightening kernels. (c) and (d) Line profiles of CHASE Fe I and Hα at three selected kernels at ∼17:50 UT (the second column, corresponding to the Fe I and Hα intensity maps shown in the first column) as well as the temporal evolution of line profiles at the two most brightened kernels (the third and fourth columns, corresponding to the green and magenta pluses, respectively). A gray plus symbol in the first column indicates a quiet-Sun location where the Fe I and Hα line profiles are displayed in the second column for comparison. The pink and cyan contours in the first column of panel (c) represent the positive and negative magnetic polarities at ± 200 G, respectively.
Paper: The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE
Authors: Ying Li, Zhichen Jing, De-Chao Song, Qiao Li, Jun Tian, Xiaofeng Liu, Ya Wang, M. D. Ding, Andrea Francesco Battaglia, Li Feng, Hui Li, Weiqun Gan
Figure caption: (a) and (b) AIA 1700 Å, WST 3600 Å, WST and HMI base-difference images at ∼21:03 and ∼21:33 UT for the X1.5 flare. The base-difference images are in a reversed color. The magenta and green squares in panel (b) indicate two selected loop locations showing white-light emissions, which are the same as the ones in panel (c). The insets in the third and fourth columns of panel (b) display the temporal evolution of the average intensities of WST and HMI continua at the two selected locations. (c) AIA 131 Å image, temperature and EM maps at ∼21:33 UT, and DEM curves at the two loop locations marked by magenta and green squares. The gray DEM curve in the last column is from the location marked by green square before the flare for comparison. (d) CHASE Hα image, Hα Doppler velocity map, Hα line profiles at different locations marked by colored plus symbols in the image, and temporal evolution of Hα profiles at the location denoted by magenta plus.
Paper: The White-light Emissions in Two X-class Flares Observed by ASO-S and CHASE
Authors: Ying Li, Zhichen Jing, De-Chao Song, Qiao Li, Jun Tian, Xiaofeng Liu, Ya Wang, M. D. Ding, Andrea Francesco Battaglia, Li Feng, Hui Li, Weiqun Gan
Figure caption: Overview of the off-disk X1.5 flare on 2023 August 7. (a) Light curves of GOES SXR 1–8 Å, its time derivative, HXR fluxes from STIX and Fermi/GBM. (b) and (c) Multiwavelength emission curves integrated over the loop region marked by the dashed box in panels (d), (e), and (g)–(i). The vertical dashed line indicates the flare peak time. (d)–(i) Multiwavelength images for the flaring region during the decay phase. The AIA, WST, and HMI images are observed from Earth view while the EUI/FSI image at 174 Å is obtained from another perspective. The red and blue contours in panel (f) indicate the loop and footpoint sources from STIX imaging. The dashed box in panels (d), (e), and (g)–(i) denotes the southern loops where show white-light emissions. The WST and HMI base-difference images are subtracted by a preflare image. The stripes visible above the limb in the WST image are caused by residuals of flat field.
Paper: On the Scarcity of Dense Cores (n > 105 cm−3) in High-latitude Planck Galactic Cold Clumps
Authors: Fengwei Xu, Ke Wang, Tie Liu, David Eden, Xunchuan Liu, Mika Juvela, Jinhua He, Doug Johnstone, Paul Goldsmith, Guido Garay, Yuefang Wu, Archana Soam, Alessio Traficante, Isabelle Ristorcelli, Edith Falgarone, Huei-Ru Vivien Chen, Naomi Hirano, Yasuo Doi, Woojin Kwon, Glenn J. White, Anthony Whitworth, Patricio Sanhueza, Mark G. Rawlings, Dana Alina, Zhiyuan Ren, Chang Won Lee, Ken'ichi Tatematsu, Chuan-Peng Zhang, Jianjun Zhou, Shih-Ping Lai, Derek Ward-Thompson, Sheng-Yuan Liu, Qilao Gu, Eswaraiah Chakali, Lei Zhu, Diego Mardones, L. Viktor Tóth
Figure caption: The sky distribution of 70 high-latitude Planck Galactic cold clumps (HLPCs). The background color map is Planck 353 GHz (850 μm) emission in cylinder projection. The 70 HLPCs are marked with green crosses. Three foreground subregions are zoomed in toward the Orion Frontier, the MBM 12 Complex, and the L134 Complex. The HLPCs in these regions cover the high column density end (﹩{N}_{{{\rm{H}}}_{2}}\gt 1.0\times {10}^{21}﹩ cm−2). In the zoomed-in subregions, HLPCs are marked with green open circles whose sizes are equivalent to the size of the observing fields. The identifiers in each subregion are marked as green text. The names of the subregions and the number of HLPCs are marked with white text on the upper left. The white rectangles are the CO emission regions.
Paper: On the Scarcity of Dense Cores (n > 105 cm−3) in High-latitude Planck Galactic Cold Clumps
Authors: Fengwei Xu, Ke Wang, Tie Liu, David Eden, Xunchuan Liu, Mika Juvela, Jinhua He, Doug Johnstone, Paul Goldsmith, Guido Garay, Yuefang Wu, Archana Soam, Alessio Traficante, Isabelle Ristorcelli, Edith Falgarone, Huei-Ru Vivien Chen, Naomi Hirano, Yasuo Doi, Woojin Kwon, Glenn J. White, Anthony Whitworth, Patricio Sanhueza, Mark G. Rawlings, Dana Alina, Zhiyuan Ren, Chang Won Lee, Ken'ichi Tatematsu, Chuan-Peng Zhang, Jianjun Zhou, Shih-Ping Lai, Derek Ward-Thompson, Sheng-Yuan Liu, Qilao Gu, Eswaraiah Chakali, Lei Zhu, Diego Mardones, L. Viktor Tóth
Figure caption: The distribution of column density corrected by beam-filling factor ﹩{N}_{{{\rm{H}}}_{2}}^{{\prime} }﹩ for low-latitude SCOPE fields (gray), HLPC fields (blue), and Taurus SCOPE fields (orange), respectively. The connected data points in corresponding colors depict the DCDR in various ﹩{N}_{{{\rm{H}}}_{2}}﹩ bins.