adsabs/AstroCLIMB huggingface dataset:
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: XMM-Newton RGS 1, RGS 2, and EPIC pn spectra from the high state part of observation 0865440101. Only narrow energy bands around the strongest disk wind absorption lines N VII, O VIII, Ne X, and Fe XXV I are shown. The first three subplots contain RGS 1 and RGS 2 data only, the fourth subplot only contains EPIC pn data. The fourth subplot shows the effect of applying or removing the EPIC pn gain-shift correction, described in Appendix A. The Fe XXVI residual can be correctly aligned with the residuals in RGS spectra by applying a blueshift to the EPIC spectral model of about −0.016 c (a linear shift of 110 eV at 7 keV).
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: Gain-shift value (as a fraction of the speed of light) for each observation or observation segment vs. raw EPIC pn count rate (no pile-up corrections applied). The 2020 August XMM-Newton observations are shown in black, and older archival observations are in blue. We highlight the two oldest observations carried out in 2001 and 2002.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: EPIC pn 9–13 keV spectra of the Her X-1 High flux states from the three 2020 August XMM-Newton observations. The spectra are fitted with simple power-law models, and all show strong residuals around the instrumental Au M-edge (11.9 keV, blue dotted line), indicating a significant gain shift at these energies.
Paper: A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Authors: Ling-Lin Zheng, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Sen-Yu Qi, Fan Yang, Song Wang, Liang Wang, Zhong-Rui Bai, Haotong Zhang, Chun-Qian Li, Jian-Rong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Figure caption: The pink triangles represent the sources with detailed parameters measured by Hernandez et al. (2021). The green triangles show the A-, F-, G-, and K-type WD-MS systems collected by Hernandez et al. (2021). The red star denotes the source J1729+6529. The black dashed line shows the lower limit of the orbital period.
Paper: A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Authors: Ling-Lin Zheng, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Sen-Yu Qi, Fan Yang, Song Wang, Liang Wang, Zhong-Rui Bai, Haotong Zhang, Chun-Qian Li, Jian-Rong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Figure caption: The distributions of the SED fitting parameters. The black dots represent the nested MCMC samples, and the black curves are the contours with 1σ, 2σ, and 3σ probabilities, respectively. The red points are the best-fitted values.
Paper: A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Authors: Ling-Lin Zheng, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Sen-Yu Qi, Fan Yang, Song Wang, Liang Wang, Zhong-Rui Bai, Haotong Zhang, Chun-Qian Li, Jian-Rong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Figure caption: TESS light curves folded with an orbital period of 0.6003 days. The light curves in the phases of [1, 2] are the duplicates of those of [0, 1] for clarity. The marker in each panel indicates the observed sector (e.g., S15 represents Sector 15). The gray curves show the folded light curves, and the blue dots are the mean values over ten gray points.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: 6 cm radio peak luminosities compared with 2–10 keV X-ray luminosities for our total volume-complete sample, and VLBI observations of a sample of local Seyfert galaxies from Panessa & Giroletti (2013). The blue dotted line indicates the separation between radio-loud and radio-quiet AGNs as introduced by Panessa et al. (2007) and separates Seyferts from LLRGs of L R/L X = 10−2.755. The green dashed–dotted line indicates the well established relation for coronally active cool stars of L R/L X = 10−5 (Guedel & Benz 1993). The black solid line represents the fit line including our nondetection upper limits and the gray shading indicates the 1σ confidence region around the best-fit line.
Paper: Unveiling the Interplay between the GASP Jellyfish Galaxy JO194 and Its Environment with Chandra
Authors: Chiara Bartolini, Alessandro Ignesti, Myriam Gitti, Fabrizio Brighenti, Anna Wolter, Alessia Moretti, Benedetta Vulcani, Bianca M. Poggianti, Marco Gullieuszik, Jacopo Fritz, Neven Tomičić
Figure caption: Ratio between the observed X-ray luminosities, L X,obs, of the total and disk region shown in the Table 4, and the X-ray luminosity associated to the SFR, L X,SFR (Equation (5)). The first four models refer to the Total region of the galaxy and the others to the Disk. The first apec  ICM  represents the contribution of the ICM emission, except for the last two that represent the contribution of the galaxy’s disk emission. The apec  GAL  component describes the X-ray emission of a single-temperature plasma, cemekl  GAL  represents a multitemperature plasma, and mkcflow  GAL  represents a multiphase gas in radiative cooling. The dashed gray line points L X,obs/L X,SFR = 1.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption:  C-band (5.8 GHz) parsec-scale radio detections for the VLBA additional snapshot observations (red boxes) and for the VLBA deep integration observed sources (blue boxes). The outermost contour represents the 5σ flux limit above rms, and the interior contours increase as σ × (10, 15, 20). The gray ellipses to the lower left of each frame represent the synthesized beam size for that observation. The top left image shows the C-band (4.9 GHz) subkiloparsec-scale radio morphology of NGC 3147 from the VLA archive, demonstrating the huge difference in spatial scales and structures between VLA and VLBA observations.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: Radio luminosity vs. the physical scale/beam size (pc mas−1) for all the detected and nondetected sources (5σ upper limits). The downward arrows are five times the 1σ radio noise level in each cleaned image, and the black solid line is the fit for all the nondetections. It denotes the average noise level at a given scale derived from our calibrated images. The black dotted line represents the nondetection upper limit across the whole distance range of the sample.
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: Comparison between the soft X-ray (2–10 keV) luminosity of NuSTAR and XRT data from the X-ray scaling method and indirect optical methods. The black dashed line is the one-to-one line for comparison. Three sources of errors are added in quadrature for each data point as they are all independent: the statistical error of the fit, the error due to interepoch variability (previously estimated at 0.1–0.2 dex), and the absolute flux calibration error (typically about 10% for X-ray data).
Paper: FRAMEx. III. Radio Emission in the Immediate Vicinity of Radio-quiet AGNs
Authors: Onic I. Shuvo, Megan C. Johnson, Nathan J. Secrest, Mario Gliozzi, Travis C. Fischer, Phillip J. Cigan, Luis C. Fernandez, Bryan N. Dorland
Figure caption: Redshift vs. hard X-ray (14−195 keV) luminosity for AGNs from the 105 month Swift BAT catalog. Green filled circles are the sources observed in our initial snapshot observation from Paper I and green squares denote the detections. The red filled circles are the additional snapshot targets and blue rings identify the nine deep integration sources.
Paper: Unveiling the Interplay between the GASP Jellyfish Galaxy JO194 and Its Environment with Chandra
Authors: Chiara Bartolini, Alessandro Ignesti, Myriam Gitti, Fabrizio Brighenti, Anna Wolter, Alessia Moretti, Benedetta Vulcani, Bianca M. Poggianti, Marco Gullieuszik, Jacopo Fritz, Neven Tomičić
Figure caption: Deprojected radial profiles of (from top to bottom): temperature, metallicity, fitted electron density, and pressure in log scale. In red we show the best-fit β-model profile (β = 0.46 ± 0.06 and r  c  = 70 ± 13 kpc), which describes the deprojected electron density radial profile.
Paper: Unveiling the Interplay between the GASP Jellyfish Galaxy JO194 and Its Environment with Chandra
Authors: Chiara Bartolini, Alessandro Ignesti, Myriam Gitti, Fabrizio Brighenti, Anna Wolter, Alessia Moretti, Benedetta Vulcani, Bianca M. Poggianti, Marco Gullieuszik, Jacopo Fritz, Neven Tomičić
Figure caption: Total, disk, and arms’ surface brightness ratios. The magenta and blue vertical ranges are, respectively, the ratio predicted by the SFR calibrators (Equation (7)) and the one presented in Sun et al. (2022).
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Left panel: relationship between extreme modulation and exoplanet magnetic field strength for the short-orbit scenario. Right panel: relationship between extreme modulation and exoplanet magnetic field strength for the long-orbit scenario. Extreme modulation is defined as the difference between the maximum and minimum radio intensity values during the transit.
Paper: Exoplanet Radio Transits as a Probe for Exoplanetary Magnetic Fields—Time-dependent MHD Simulations
Authors: Soumitra Hazra, Ofer Cohen, Igor V. Sokolov
Figure caption: Left panel: synthetic light curves for different EUV frequencies. Right panel: synthetic light curves for different X-ray frequencies. Al-mesh, Al-poly, and Ti-poly correspond to different X-ray filters.
Paper: Black Hole Hyperaccretion in Collapsars. III. GRB Timescale
Authors: Yun-Feng Wei, Tong Liu
Figure caption: Panel (a): GRB duration t GRB as function of r 1 and k 2 for the first jet model. The black line corresponds to t GRB = 2 s. The red line corresponds to collapsar mass M col = 10 M ⊙. Panel (b): isotropic energy E  γ,iso as function of r 1 and k 2.
Paper: Black Hole Hyperaccretion in Collapsars. III. GRB Timescale
Authors: Yun-Feng Wei, Tong Liu
Figure caption: The artificial density profile of a collapsar. The density profile is divided into two parts: star core and envelope. The density of the core is approximated as a power law with index −k 1. The density of the envelope is approximated as a power law with index −k 2. r 1 is the boundary between them. The outer boundary of the collapsar r 2 is defined as the radius at which the density decreases to 10−10 g cm−3. r 0 is the radius where the enclosed mass reaches 3 M ⊙, and ρ 0 is the density at this radius.
Paper: Black Hole Hyperaccretion in Collapsars. III. GRB Timescale
Authors: Yun-Feng Wei, Tong Liu
Figure caption: Constrained collapsar density profiles of GRB 200826A. The black and blue lines correspond to t GRB = 2 s and E  γ,iso = 7.1 × 1051 erg s−1, respectively. The red line corresponds to collapsar mass M col = 10 M ⊙. Panels (a) and (b) show the results of the first and second jet models, respectively. The location of GRB 200826A is marked with green pentagram.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: FT of PG 1159-035 for the years of 1983, 1985, 1989, 1993, 2002, 2016, and 2021, from 1700 to 2300 μHz. Their respective spectral windows are shown on the right side. Frequencies are in microhertz and amplitude units use 1 mma = 1/1.086 mmag = 1 ppt = 0.1%; see, e.g., Bognar & Sodor (2016).
Paper: Black Hole Hyperaccretion in Collapsars. III. GRB Timescale
Authors: Yun-Feng Wei, Tong Liu
Figure caption: Same as Figure 2 but for the second jet model case.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: FT of the original K2 light curve of PG 1159-035. The red dashed line indicates the false-alarm probability fap(1/1000) = 0.119 mma we obtained randomizing the input times 1000 times. Frequencies are in microhertz and amplitudes in parts per thousand.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: FT of first half and second half of the K2 data, showing amplitude changes during the 69 d observations, especially for peaks between 1100 and 1400 μHz.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: FT of the original TESS light curve of PG 1159-035. The red dashed line indicates the false-alarm probability fap(1/1000) = 2.537 mma we obtained randomizing the input times 1000 times.
Paper: GRB 190829A—A Showcase of Binary Late Evolution
Authors: Yu Wang, J. A. Rueda, R. Ruffini, R. Moradi, Liang Li, Y. Aimuratov, F. Rastegarnia, S. Eslamzadeh, N. Sahakyan, Yunlong Zheng
Figure caption: The luminosity of GRB 190829A in the X-ray (0.3–10 keV), optical (i band; Hu et al. 2021), and radio (5.5 and 15.5 GHz) energy bands (Rhodes et al. 2020).
Paper: GRB 190829A—A Showcase of Binary Late Evolution
Authors: Yu Wang, J. A. Rueda, R. Ruffini, R. Moradi, Liang Li, Y. Aimuratov, F. Rastegarnia, S. Eslamzadeh, N. Sahakyan, Yunlong Zheng
Figure caption: The luminosity of GRB 190829A, including the data from HESS (yellow) for TeV; Fermi-GBM (orange dots); Swift-BAT (purple triangles) for the prompt emission of hard X-rays and gamma-rays; Swift-XRT (blue crosses) for the soft X-rays (absorbed); GTC (green diamonds) for the optical i band, from which the SN 2019yw is extracted (red diamonds)—the optical signal of the SN overshoots the synchrotron optical emission; and AMI-LA (brown stars) for the radio observation.
Paper: GRB 190829A—A Showcase of Binary Late Evolution
Authors: Yu Wang, J. A. Rueda, R. Ruffini, R. Moradi, Liang Li, Y. Aimuratov, F. Rastegarnia, S. Eslamzadeh, N. Sahakyan, Yunlong Zheng
Figure caption: Top: the spectrum of the first pulse observed by Fermi-GBM. The blue points are the data and the orange curve indicates the fitting by a cutoff power law with power-law index α = −1.45 and the peak energy E  p  = 144.28 keV. Bottom: the spectrum of the second pulse. The blue points are the data and the orange curve indicates a band function fitting, with the low-energy index α = 0.50, the high-energy index β = −2.53, and the peak energy E  p  = 13.58 keV.
Paper: GRB 190829A—A Showcase of Binary Late Evolution
Authors: Yu Wang, J. A. Rueda, R. Ruffini, R. Moradi, Liang Li, Y. Aimuratov, F. Rastegarnia, S. Eslamzadeh, N. Sahakyan, Yunlong Zheng
Figure caption: The count rate of the GRB 190829A prompt emission from the raw data of Fermi-GBM: the first pulse is from −0.75 s to 8.05 s, indicated by the orange dotted line, and the second pulse is from 46.50 s to 64.00 s, indicated by the green dashed line.
Paper: GRB 190829A—A Showcase of Binary Late Evolution
Authors: Yu Wang, J. A. Rueda, R. Ruffini, R. Moradi, Liang Li, Y. Aimuratov, F. Rastegarnia, S. Eslamzadeh, N. Sahakyan, Yunlong Zheng
Figure caption: The synchrotron and SSC spectra of the first HESS observational epoch. The synchrotron spectrum well fits the optical and X-ray data. Neither the synchrotron nor the SSC spectra are able to reproduce the HESS observations.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Left: ratio of ﹩{L}_{\mathrm{HCN}}^{{\prime} }/{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }﹩                       J = 2 → 1 as a function of IR luminosity surface density. Right: ratio of ﹩{L}_{\mathrm{HCN}}^{{\prime} }/{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }﹩                       J = 2 → 1 as a function of cold component dust temperature. The sample in this work is shown with circles, while the ALMA ULIRG sample from Imanishi et al. (2022) is shown with triangles. The AGN-dominated galaxies are shown with blue filled points, and SF-dominated galaxies are shown with red open points. The gray square points are HCN and HCO+ J = 1 → 0 from the literature for comparison (Nguyen et al. 1992; Solomon et al. 1992; Gao & Solomon 2004b; Wang et al. 2004; García-Burillo et al. 2006; Baan et al. 2008; Krips et al. 2008).
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Left: correlation between ﹩{L}_{\mathrm{HCN}\,{\text{}}{\rm{J}}=2\to 1}^{{\prime} }﹩ and L IR. Right: correlation between ﹩{L}_{{\mathrm{HCO}}^{+}\,{\text{}}{\rm{J}}=2\to 1}^{{\prime} }﹩ and L IR. The AGN- and SF-dominated galaxies are shown in blue and red points, respectively. The fitting results of OLS and MCMC are shown in black and cyan lines, respectively. The green dashed line shows a linear relation for reference. The insets present the probability density distributions of the slope sampling.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Correlations including the ALMA ULIRG sample from Imanishi et al. (2022). Top: correlations of ﹩{L}_{\mathrm{HCN}}^{{\prime} }-{L}_{\mathrm{IR}}﹩ (left) and ﹩{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }-{L}_{\mathrm{IR}}﹩ (right). Bottom: correlations of ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{HCN}}^{{\prime} }}-{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩ (left) and ﹩{{\rm{\Sigma }}}_{{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }}-{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩ (right). The AGN- and SF-dominated galaxies are shown in blue and red points, respectively. The fitting results of OLS and MCMC are shown in black and cyan lines, respectively. The green dashed line shows a linear relation for reference. The insets present the probability density distributions of the fitted slopes. Data points from Imanishi et al. (2022) are shown in purple and not included in the fitting. The purple dashed lines are the fitting results of ﹩\mathrm{HCN}﹩                       J = 4 → 3 and HCO+ J = 4 → 3 obtained from Tan et al. (2018).
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Top: correlations of ﹩{L}_{\mathrm{HCN}}^{{\prime} }-{L}_{\mathrm{IR}}﹩ (left) and ﹩{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }-{L}_{\mathrm{IR}}﹩ (right). Bottom: correlations of ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{HCN}}^{{\prime} }}-{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩ (left) and ﹩{{\rm{\Sigma }}}_{{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }}-{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩ (right). The correlations include dense molecular clouds from the Magellanic Clouds (Galametz et al. 2020), which are shown in orange circles. The total luminosity and averaged luminosity surface density of detected targets in the Magellanic Clouds are also shown for comparison. Luminosity upper limits of nondetection clouds are shown in gray arrows. The purple dashed lines are taken from Figures 2 and 3 and present the fitting results of galaxies.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Left: correlation between ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{HCN}\,{\text{}}{\rm{J}}=2\to 1}^{{\prime} }}﹩ and ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩. Right: correlation between ﹩{{\rm{\Sigma }}}_{{L}_{{\mathrm{HCO}}^{+}\,{\text{}}{\rm{J}}=2\to 1}^{{\prime} }}﹩ and ﹩{{\rm{\Sigma }}}_{{L}_{\mathrm{IR}}}﹩. The AGN- and SF-dominated galaxies are shown in blue and red points, respectively. The fitting results of OLS and MCMC are shown in black and cyan lines, respectively. The green dashed line shows a linear relation for reference. The insets present the probability density distributions of the fitted slopes.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Top left: SFR/M dense traced by HCN J = 2 → 1 as a function of IR luminosity. Top right: SFR/M dense traced by HCO+ J = 2 → 1 as a function of IR luminosity. Bottom left: SFR/M dense traced by HCN J = 2 → 1 as a function of cold dust temperature. Bottom right: SFR/M dense traced by HCN J = 2 → 1 as a function of cold dust temperature. The AGN- and SF-dominated galaxies are shown in blue and red points, respectively.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Example of the dust SED of NGC 1808. The orange and blue dashed lines represent the warm and cold components, respectively. The gray data points represent bands not in the fitting, including WISE 3.4, 4.6, and 12 μm and IRAS 25 μm, due to short wavelength or low resolution.
Paper: Dense Gas and Star Formation in Nearby Infrared-bright Galaxies: APEX Survey of HCN and HCO+ J = 2 → 1
Authors: Jing Zhou, Zhi-Yu Zhang, Yu Gao, Junzhi Wang, Yong Shi, Qiusheng Gu, Chentao Yang, Tao Wang, Qing-Hua Tan
Figure caption: Left: ﹩{L}_{\mathrm{HCN}}^{{\prime} }/{L}_{\mathrm{CO}}^{{\prime} }﹩ as a function of IR surface density. Right: ﹩{L}_{{\mathrm{HCO}}^{+}}^{{\prime} }/{L}_{\mathrm{CO}}^{{\prime} }﹩ as a function of IR surface density. The AGN- and SF-dominated galaxies are shown with blue filled points and red open points, respectively. The best-fit results are shown with solid lines. Nondetections are not included in the fitting.