adsabs/AstroCLIMB huggingface dataset:
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Stellar structure profiles for the 18M ⊙ MESA model presented in Figure 2. Plotted are the specific nuclear energy generation rate (in units of 105​​​​​​ erg g−1 s−1), the convective velocity according to mixing length theory (in units of 105 cm s−1), and the H and He mass-fraction profiles as a function of radial coordinate. The left and right panels show the interior properties of the companion as inferred “today” by M. Falanga et al. (2015) and at the time of mapping into the FLASH simulation, respectively. The radial coordinate at which the α = 1 condition is satisfied is shown as a green vertical dashed line in the left panel.
Paper: Rethinking Thorne–Żytkow Object Formation: The Fate of X-Ray Binary LMC X-4 and Implications for Ultra-long Gamma-Ray Bursts
Authors: Tenley Hutchinson-Smith, Rosa Wallace Everson, Angela A. Twum, Aldo Batta, Ricardo Yarza, Jamie A. P. Law-Smith, Alejandro Vigna-Gómez, Enrico Ramirez-Ruiz
Figure caption: Luminosity as a function of the duration of high-energy transients adapted from A. J. Levan et al. (2014). For the GRB and ULGRB sources, we plot t 90 as the duration and the peak isotropic luminosity. The duration of the event assumes the ejection timescale determined by accretion feedback in Figure 9. The properties of the high-energy transient roughly coincide with those of the emerging class of ultra-long GRBs, such as GRB 101225A, GRB 111209A, and GRB 121027A.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Alignment of SN 2019oyw’s late-time spectral features. Both panels show rest-frame wavelength on the x-axis, and on the y-axis the flux densities which are scaled for visual clarity. Upper panel: Redshift z = 0.0785 is assumed for SN 2019oyw on epoch 2019 October 26 (red, phase 53 days) as the source. The letters “A” and “B” mark two prominent peaks in the spectrum. Spectra of both objects were extinction corrected. SN 1998bw is chosen as the standard GRB-SN template (Z. Cano et al. 2014; M. Modjaz et al. 2016). Epochs 1998 June 12 (black dashed line, 47 days) and 1998 June 24 (black solid line, 59 days) cover rest-frame wavelengths comparable to our observations in G102 and G141 grisms, and are comparable in phase to our observations of SN 2019oyw. The Ca II NIR triplet λλ8498, 8542, 8662 (CaIR3) and He I λ10830 are markers close to A and B, respectively. For SN 2019oyw, we adopted values E(B − V) = 0.049, 0.757 for Galactic (E. F. Schlafly & D. P. Finkbeiner 2011; Y. D. Hu et al. 2021) and extragalactic (Milky Way model) reddening (L.-L. Zhang et al. 2021), respectively. For SN 1998bw, we adopted E(B − V) = 0.059 and its host’s A  V  = 0.17 assuming Small Magellanic Cloud dust model (see L. Li et al. 2018 and references therein). Lower panel: Similar to the upper panel but assuming z* = 0.1051 for SN 2019oyw instead (blue, phase 52 days). By comparing between the two cases, it is evident that assuming z* improves the alignment.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Evolution of CaIR3 peaks from samples of SNe Ic-BL. Rest-frame wavelengths are shown on the x-axis and phases are on the y-axis. The samples include SNe Ic-BL with associated GRBs (cross data points), and without GRB (dot data points). Phase is referred from the GRB trigger. The samples show the evolution of CaIR3 peaks from blue to red with ages, and the peaks are well constrained within the CaIR3 constraint if considering late-photospheric phases between 30 and 100 days; see Section 4 for more discussion. SN 2019oyw’s CaIR3 peaks are also shown in red (assuming z = 0.0785) and blue (assuming z* = 0.1051). We noted that early data of SN 2019oyw from VLT/FORS (see Section 2.3). The plot shows that assuming z* = 0.1051 improves the feature alignment better than z = 0.0785.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Spectral energy distribution of SN 2019oyw from several grism spectra taken between 2019 September 28 and 2020 January 12 using HST/WFC3. The plot shows raw spectra (faint lines) and their smoothed versions (solid lines). (We applied the generalized Savitzky–Golay method (R. M. Quimby et al. 2018) in smoothing the spectra. The resolution parameter was set to 60 (which is equivalent to the half width of 5000 km s−1), and the polynomial order was set to n = 2, except the spectrum on 2020 January 12 using n = 0 because of low SNR.) Each spectrum was scaled vertically for visual clarity, and the corresponding scale factor is provided. The data points shown with crosses are the photometric observations (see Table 2) shown for comparison. “A” and “B” mark two prominent features (at about 9500 and 12000 Å, respectively) observed more clearly on 2019 October 26 spectrum. The observed flux densities are shown and are not corrected for the extinction.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Evolution of SN 1998bw’s CaIR3 emission. This figure shows rest-frame wavelengths on x-axis and flux densities on y-axis are scaled for visual clarity. SN 1998bw’s spectra from 1998 May 14 (18 days) to 1998 September 12 (138 days) are shown in order from top to bottom by epoch (F. Patat et al. 2001). This figure features peaks of CaIR3 (marked by crosses). The evolution shows that the peaks become redder with age. They started to be inside the constraint starting at phase 25 days and stayed inside the constraint until at least 138 days. We discuss more about the evolution in Section 4. Spectra of SN 2019oyw on epochs 2019 September 28 and 2019 October 26 (black dotted lines) are also shown in the figure (assuming z* = 0.1051) for comparisons with SN 1998bw at similar phases. These spectra were smoothed by the generalized Savitsky–Golay method (R. M. Quimby et al. 2018; see Section 2.2 for details) and extinction corrected. We also note that the small oscillation (also known as “fringing”) observed on some of SN 1998bw’s spectra (e.g., 18 and 23 days) is the feature seen in the original data, and is not an artifact from our process.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Similar to Figure 13 but with a sample of SNe Ic (square data points) instead. We note that phase is referred from the date of discovery for these SNe without associated GRB.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Cross correlation matching CaIR3 peaks. Left-hand panel: The cross-correlation technique was performed using SN 2019oyw on epoch 2019 October 26 (source, blue) and SN 1998bw on epoch 1998 June 24 (template, black). For the template, this peak was identified as CaIR3 (F. Patat et al. 2001). For the source, only included data points around the peak (blue crosses) were used in the computation. For more details, see Appendix. Right-hand panel: The optimal solution z* from the cross correlation (red dot) is estimated by the second-order polynomial fit to the cross-correlation score curve.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Alignment of SN 2019oyw’s late-time spectral features assuming z* = 0.1051. The figure shows rest-frame wavelength on the x-axis, and on the y-axis the flux densities which are scaled for visual clarity. Spectra on epochs 2019 September 28 (magenta, 26 days) and 2019 October 26 (blue, 52 days) are shown (omitting epochs 2019 November 29 and 2020 January 12 spectra due to low signals). Spectra of SN 1998bw at similar phases are shown for comparisons. These spectra were extinction corrected. The figure supports consistency of the feature alignment assuming z*.
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Evolution of SN 2019oyw’s CaIR3 feature. The spectra in this plot show the evolution of the CaIR3 feature from 4 days after burst to 52 days after burst (in rest frame, assuming z* = 0.1051). The spectra are scaled for legibility and do not represent the evolution of the spectral flux; the scaling factors are provided in the legend. The peak evolves from the blue back toward the rest-frame wavelengths of the CaIR3 interval as the expansion of the photosphere slows. As we will discuss, this is a common feature of Type Ic and Ic-BL supernovae, and understanding this time evolution is critical for accurately estimating the true redshift of SN 20190yw. These spectra are extinction corrected and smoothed (see Section 2.2 for details).
Paper: The Redshift of GRB 190829A/SN 2019oyw: A Case Study of GRB-SN Evolution
Authors: Kornpob Bhirombhakdi, Andrew S. Fruchter, Andrew J. Levan, Elena Pian, Paolo Mazzali, Luca Izzo, Tuomas Kangas, Stefano Benetti, Kyle Medler, Nial Tanvir
Figure caption: Two-dimensional spectrum at the location of GRB 190829A/SN 2019oyw taken by X-shooter. The location of the transient was placed at the center of the slit (horizontal magenta dotted lines). X-axis is shown in observed wavelengths. The spectrum is shown in the middle, and line markers are shown at the top for assuming z = 0.0785 (red) and bottom for z* = 0.1051 (blue). These markers include Hα λ6563​​​​​, [N II] λλ6548, 6583, and [S II] λλ6717, 6731. The image is shown in inverse color, i.e., black = bright. The observed lines are consistent with the SDSS  J025810.28–085719.2 at the redshift z = 0.0785. See more details about this observation in Izzo et al. (2024, in preparation).
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: The L bol vs. z distribution of our core sample. Our X-ray detected (undetected) DOGs are shown as blue (orange)-empty circles. Among them, sources classified as reliable SED AGNs in F. Zou et al. (2022) (see text in Section 3.1) are shown as filled stars for X-ray detected DOGs and filled squares for X-ray undetected DOGs. For comparison, the L bol vs. z distributions of X-ray AGNs in XMM-SERVS, Hot DOGs in C.-W. Tsai et al. (2015), and DOGs in F. Zou et al. (2020) are shown in gray, red, and green circles, respectively. The distributions of z and L bol for sources mentioned above are shown in the top and right-hand subpanels, respectively, with the same colors as those in the legend (we do not further plot the distributions for our reliable SED AGNs). Note that for better visibility, in the top and right-hand subpanels the number of X-ray detected DOGs, Hot DOGs in C.-W. Tsai et al. (2015), and DOGs in F. Zou et al. (2020) are multiplied by factors of 20, 60, and 100, respectively.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Example best-fit SED results for X-ray undetected (top row) and X-ray detected (bottom row) DOGs. All of the six sources have reliable redshifts (spec-zs or photo-zs with ﹩{Q}_{z}^{\mathrm{good}}\lt 1﹩, as shown in each panel). The blue points and downward triangles are the observed photometry and upper limits, respectively. The thick-gray lines are the best-fit total models. The cyan-dashed lines and the red-solid lines represent galaxy and AGN components, respectively. For sources where the statistically preferred model is the AGN model, we also show the intrinsic AGN disk SEDs, which are only modeled at λ ≥ 0.008 μm (G. Yang et al. 2022). The sharp peaks at rest-frame <0.1 μm are strong nebular emission lines, as modeled by the templates from A. K. Inoue (2011). All sources shown with best-fit AGN models are classified as reliable SED AGNs. See Section 3 of F. Zou et al. (2022) for more details about our source classification. We also show the coordinates (R.A. and decl.) of each source at the top of each panel.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Illustrations of four DOGs in our full sample. For each source, we show the XMM-Newton 0.5–10 keV(first column; 60″ × 60″), HSC r-band (second column; 20″ × 20″), VIDEO K  S band (third column; 20″ × 20″), DeepDrill IRAC 3.6 μm (fourth column; 20″ × 20″), and MIGHTEE 1.4 GHz (last column; 60″ × 60″) images. The first two sources are detected in all five bands. The third source is not detected in X-rays, and the fourth source is not detected in radio. The VIDEO position and the redshift are shown in the last column for each source. X-ray positions are marked as cyan circles with a 68% error radius (C.-T. J. Chen et al. 2018); VIDEO positions are marked as red circles with a 1″ radius; and MIGHTEE positions are marked as orange circles with a 68% error radius (S. Zhu et al. 2023).
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Comparison between the photo-zs and spec-zs for sources with spec-z measurements. The brown solid circles represent sources with ﹩{Q}_{z}^{\mathrm{good}}\lt 1﹩. The gray empty circles are sources with ﹩{Q}_{z}^{\mathrm{good}}\gt 1﹩. The ﹩{Q}_{z}^{\mathrm{good}}\lt 1﹩ cut significantly reduces the outlier fraction. The solid line indicates the z phot = z spec relation. The dashed lines represent the ∣z phot − z spec∣/(1 + z spec) > 0.15 relation.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption:  L X,obs (blue) and absorption-corrected L X (gray) distributions for X-ray detected DOGs in the core sample. The red-dashed histogram represents the L X,obs distribution of general X-ray AGNs in XMM-SERVS. X-ray detected DOGs generally have high observed and absorption-corrected X-ray luminosity.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: The f 24μm/f  R  vs. f 24μm distribution. The dashed lines represent our color-selection thresholds, and sources in the upper right-hand region are selected as DOGs. The blue points represent DOGs with positive measured R-band flux. The brown up-triangles represent DOGs with nonpositive R-band flux measured via forced photometry, whose R-band flux is estimated from the best-fit SED. The grayscale cells are the 2D histogram for all 24 μm-detected galaxies in XMM-SERVS, with darker cells representing more galaxies.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Fraction of sources in our full sample with ﹩{Q}_{z}^{\mathrm{good}}\lt 1﹩ as a function of R-mag. Each magnitude bin has a width of 0.45 mag except for the last one showing all sources with R − mag > 26. The number above each bin shows the number of sources in the bin. The y-axis error bar represents the 1σ binomial confidence interval.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption:  M ⋆ distribution for the core sample. Blue and orange histograms represent X-ray detected and X-ray undetected DOGs, respectively. Note that the number of X-ray detected DOGs in each bin is multiplied by a factor of 10 for easier visibility. DOGs generally have high M ⋆, and X-ray detected DOGs have slightly higher M ⋆. The distributions for our full sample are similar.
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: VSFs of the simulated tail for different inclinations (top to bottom) at different snapshots. The VSFs reported here are derived without prior reprocessing of the simulated velocity maps. The continuous and dashed lines indicate the slopes expected in the case of, respectively, rotation (∝ l) and turbulence (∝ l 1/3).
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: Parameter space of η, computed according to Equation (1), for n  e  = 10−4–10−2 cm−3, kT = 0.1–10 keV, and reference values l = 3 kpc and 〈∣δ V∣〉3 kpc = 44 km s−1, which is the average value measured in this work. We report the ICM conditions of the cluster sample (gray points, see Table 2) and the one reported in Y. Li et al. (2023) (green point), the η = 1 kpc and η = 0.2 kpc (black continuous and dashed lines), and the typical temperature range of the mixing layers, 0.8–1.2 keV (red band).
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: Correction procedure applied on the simulated tail W45-y at 300 Myr after stripping. Left-hand panels: Phase-space density plot for the simulated tail; Middle panels: Comparison between the original (top panel), model (center panel), and residual (bottom panel) velocity maps; Right-hand panel: VSF before (orange) and after (blue) the correction procedure (Section 2.3.2). The continuous and dashed lines indicate the slopes expected in the case of, respectively, rotation (∝ l) and turbulence (∝ l 1/3).
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: Comparison of the VSF of the entire sample. The black-dashed line indicates the l 1/3 trend. The gray-filled region marks l < 1″ below which the signal is affected by the spaxel correlation (See Section 2.2).
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: VSFs at increasing distance from the disk for JO147, JO204, JO206, and JW100. The VSFs are computed within a moving frame along the tail direction, color-coded by the distance of the frame center from the stellar disk edge. The dashed line indicates the Kolmogorov slope. In the inserts, we report the average VSF value between 2 and 3 kpc at increasing distances from the disk.
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: VSFs rescaled to the corresponding η reported in Table 2. Below l = 1 kpc, the rescaled VSFs are reported with the dashed lines. JO113, JO147, and JO162 are rescaled for the lower limit of η. The gray-dashed line indicates the l 1/3 Kolmogorov scaling, and the vertical red line points out the l/η = 1 scale.
Paper: Investigating the Intracluster Medium Viscosity Using the Tails of GASP Jellyfish Galaxies
Authors: Alessandro Ignesti, Gianfranco Brunetti, Marco Gullieuszik, Nina Akerman, Antonino Marasco, Bianca M. Poggianti, Yuan Li, Benedetta Vulcani, Myriam Gitti, Alessia Moretti, Eric Giunchi, Neven Tomičić, Cecilia Bacchini, Rosita Paladino, Mario Radovich, Anna Wolter
Figure caption: (a) Phase-space density plots for JO113, JO147, JO162, and JO171. (b) Phase-space density plots for JO175, JO204, JW39, and JW56. (c) Phase-space density plots for JW100.
Paper: NIHAO-RiNG: A Comparison of Simulated Disk Galaxies from GASOLINE and GIZMO
Authors: Hou-Zun Chen, 厚尊 陈, Xi Kang, 熙 康, Andrea V. Macciò, Tobias Buck, Renyue Cen
Figure caption: Comparison of density–temperature diagram of gas particles within 3R vir in the g8.26e11 system. The regions for HOT, WARM, and COLD are divided by horizontal dashed lines. The colors of the dots in the left and right panels denote the distance (in logarithm) to the galaxy center and metallicity (in mass fraction and also in logarithm), respectively. Thus, the gas in the ISM, CGM, and IGM is approximately depicted in red, cyan, and blue hues in the left panels. The left contour maps give the mass distribution of gas particles on the diagram, while the right contour maps show the cooling time of gas with solar metallicity under the assumption of collisional ionization equilibrium. The mean cosmic baryon density and its 200 times value are marked on the x-axis. The black dashed line in the lower panels demonstrates the best-fitting polytropic state of the cold ISM.