adsabs/AstroCLIMB huggingface dataset:
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Left: the mass–size distribution of CSSs in TNG50 at z = 0. The blue and red triangles represent the CSSs in TNG50 selected based on our criteria. Blue triangles denote BSF-CSSs, and red triangles represent TS-CSSs. The distribution of ordinary dwarf galaxies is indicated by the gray density scale since they are numerous. Observed CSSs (I. Chilingarian & I. Zolotukhin 2015; A. Guérou et al. 2015; J. Janz et al. 2016; A. Ferré-Mateu et al. 2018; S. Kim et al. 2020) are overlaid using gray crosses. The classifications are described in the text following Figure 2. M32 is represented by a blue star. The black dashed line corresponds to the minimum size limit of stellar systems, and the dark-gray filled region represents the zone of avoidance (﹩{r}_{e}\leqslant 2.24\times 1{0}^{-6}\mathrm{pc}\cdot {\left(\tfrac{{M}_{* }}{{M}_{\odot }}\right)}^{4/5}﹩; see D. Burstein et al. 1997; I. Misgeld & M. Hilker 2011, for details). The horizontal dashed line corresponds to a Plummer-equivalent gravitational softening length at z = 0. In the upper and right subpanels, M* and re distributions are shown as histograms, as well as that of ordinary dwarf galaxies (gray). Right: mass-weighted stellar age vs. metallicity of TNG50 CSSs. The M32-like samples are marked by black circles. Gray contours show the overall distribution of CSSs from observations. The age and shifted metallicity distributions are shown as histograms in the upper and right panels. The gray arrow in the upper corner of the right subpanel indicates that we apply a uniform 0.75 dex rescaling to the metallicities of TNG50 galaxies to align them with the observed scaling relation (E. N. Kirby et al. 2013), as in Figure 2.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Evolution of each CSS recovered from their stellar population at z = 0. Each row represents a galaxy, with panels displaying 100 randomly selected Iso-dwarfs (top), BSF-CSSs (middle), and TS-CSSs (bottom). From left to right, the panels show the star formation history, [Fe/H], and [α/Fe].
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: Sketch of the proposed geometry of GX 13+1 (not to scale). The gray region represents the outer disk rim, the yellow region the ADC, and the blue circle the central X-ray source. The black segments show the PA of the radiation scattered by the ADC. The PA at the observer (given by the average of the PAs) changes from the off-dip state (panel (A)) to the dip state, when a small clump obscures the central source and a negligible part of the ADC (panel (B)) and a large clump obscures the central source a fairly large fraction of the ADC (panel (C)).
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: GX 13+1 HID from the three different IXPE observations where the different colors correspond to different HR and flux bins (top). The bottom panel reports the 90% CL polarization contours corresponding to the four different HR bins.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: GX 13+1 HID from the three different IXPE observations where the different colors correspond to different bins in intensity (top). The bottom panel reports the polarization contours at 90% CL, corresponding to each intensity bin.
Paper: X-Ray Dips and Polarization Angle Swings in GX 13+1
Authors: Alessandro Di Marco, Fabio La Monaca, Anna Bobrikova, Luigi Stella, Alessandro Papitto, Juri Poutanen, Maria Cristina Baglio, Matteo Bachetti, Vladislav Loktev, Maura Pilia, Daniele Rogantini
Figure caption: IXPE HID obtained for GX 13+1 from the different observations (panels (a)–(c)) and when the three observations are combined (d).
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Top panels: the evolutionary pathways of BSF-CSSs (left, panels (a)–(f)) and TS-CSSs (right, panels (g)–(l)). Panels (a)–(f)/(g)–(l) show the evolution, centering at the time of the first pericenter (﹩{t}_{{1}^{{\rm{st}}}{\rm{peri}}}﹩). Mgas is the gas mass. The 〈[Z/H]〉 values of gas and stars represent the mass-weighted average metallicities of star-forming gaseous cells and star particles, respectively. Thin curves represent individual galaxies. The colored lines represent M32-like CSSs. Bottom panels: the orbits and stellar and gaseous surface density maps of examples of a BSF-CSS (left, ID 448833, panels (m)–(n)) and a TS-CSS (right, ID 414930, panels (o)–(p)). Interpolation is used to reconstruct the orbits, with a darker color indicating a later time. The colored stars mark positions in their evolution. The background shows the stellar mass surface density distribution of the host galaxy, shown in both face-on (upper) and edge-on (lower) projections at z = 0. The inset images, showing the stellar and gas mass surface density distribution of the CSS, are overlaid onto the background images in the face-on views. Panel (m) presents these maps at three distinct time points, and panel (o) at five. For better visibility, the stellar and gas maps are projected at a different spatial scale of 15 kpc by 15 kpc centered on the CSS. At each time, the stellar and gas maps are horizontally offset from each other. In the upper right corner of panel (m)/(o), we list the ID for the CSS (IDsat) and the host galaxy (IDhost), along with the stellar mass of the host galaxy (﹩{M}_{* }^{{\rm{host}}}﹩) and the minimum distance to the host ﹩\min \left({d}_{\mathrm{sat}}^{\mathrm{host}}\right)﹩.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: (a) Normalized distribution of the galactocentric distances of CSSs from their hosts at z = 0. BSF-CSSs are represented in blue, while TS-CSSs are depicted in red. Dashed histograms show the median distance of each CSS from its host galaxy during the first orbit. (b) The mass ratio of CSSs to their host galaxies’ stellar mass at z = 0 in TNG50. CSSs selected based on our criteria are exclusively found near massive host galaxies. (c) The cumulative distribution function of the time of the first pericentric passage for BSF-CSSs and TS-CSSs. (d) The probability of central galaxies hosting CSSs in TNG50. The black solid line displays the ratio between the number of central galaxies having at least one CSS satellite of M* = 108–1010 M⊙ and the number of all central galaxies at a given stellar mass. We indicate the stellar mass at z = 0 of the Milky Way (in cyan, based on J. Bland-Hawthorn & O. Gerhard 2016) and M31 (pink, from A. Tamm et al. 2012; J. Sick et al. 2014). (e) The average number of CSSs as a function of the stellar mass of their host galaxies. The number of CSSs hosted by galaxies with a mass around 1012 M⊙ in the Virgo Cluster is indicated by the blue point in this panel.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Illustrative evolution of the gas for a BSF-CSS during the first pericentric passage. The ID of the CSS at z = 0 is 448833. The CSS is centrally positioned within each panel, with time annotated in the lower right corner. Each panel (except for those in the bottom row) covers an area of 400 × 400 kpc2, projected onto a plane perpendicular to the bulk velocity vector direction of the CSS and rendered at a resolution of 800 × 800 pixels. Dashed lines connect the position of the CSS to its host, while arrows denote the velocity direction of the CSS relative to the host. Quiver plots are overlaid on each panel, illustrating the gas velocity field around the CSS. The top row shows the pressure field, measured in dynes per square centimeter, with distance and velocity indicated in the lower left corner of each panel. The second row presents the gas temperature, with the mass of cold gas (identified by a star formation rate of the cell > 0) and the SFR shown in the lower left corner of each panel. The third row shows the evolution of gas metallicity, with the 〈[Z/H]〉 value of stars and 〈[Z/H]〉 value of gas specified in the lower left corner of each panel. The bottom row zooms in on the gas density distribution.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: [α/Fe]–[Fe/H] diagram of stellar populations of CSSs at z = 0 formed by different mechanisms. The α species are 12C, 16O, 20Ne, 24Mg, and 28Si. The contours from light to dark blue represent the maximum density's 20th, 40th, and 80th percentiles, respectively. In the top nine panels, from top to bottom, we present cases of isolated central dwarfs (Iso-dwarfs), TS-CSSs, and BSF-CSSs, with stars color-coded based on the difference between their age and the median age (﹩\widetilde{{\rm{Age}}}﹩) of the stellar populations in their respective galaxies. The ﹩\widetilde{{\rm{Age}}}﹩ for each example is indicated within its corresponding panel. In the bottom six panels, stars are color-coded based on their respective formation periods to illustrate the timing of the formation of distinct stellar populations: red (stars formed before infall), orange (during the first orbit), light blue (during the second orbit), and navy (beyond the second orbit). These distributions exhibit significant differences, with BSF-CSSs exhibiting distinct finger features extending toward high [α/Fe] and [Fe/H].
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Orbital characteristics of CSSs selected based on our criteria in TNG50. The four panels display cumulative distribution functions for various orbital characteristics of CSSs, which include ellipticity, number of orbits, the median distance of each galaxy from its host galaxy during the first orbit (D(1storbit)/Rvir), and the median velocity during the first orbit (V(1storbit)). The cumulative distribution functions for BSF-CSSs and TS-CSSs are shown in blue and red, respectively, which allows for a direct comparison against the background distribution of ordinary satellite dwarf galaxies (excluding isolated dwarfs), shown in gray. The ellipticity, denoted as ϵ, is defined as the median value of ﹩1-\frac{b}{a}﹩, where a and b represent the apocenter and pericenter of the orbit, respectively.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Pram vs. Pwind at two radii, re and Rvir of each CSS, during its first pericentric passage. The figure compares the ram pressure, Pram, experienced by CSSs as they move through the surrounding medium (defined by Equation (1)) with the pressure exerted by galactic winds, Pwind, as defined by Equation (2). The data are shown in blue for BSF-CSSs and red for TS-CSSs. The inset image shows the distribution of log (Pram/Pwind) at Rvir.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Illustrative evolution of the gas for a TS-CSS during the first pericentric passage. The ID of the CSS at z = 0 is 414930. This figure uses the same conventions as those established in Figure 8.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: Formation of the stellar halo in a TS-dominated M31–M32 analog system. Here we select the time when the CSS is interacting with the central host, resembling the M31–M32 system. The first row shows the stellar halo formed through close interactions. The stellar halo is composed of material from both the central galaxy (depicted in blue colors) and the progenitor of the CSS (depicted using yellow and red colors). The second row's detailed images display the stellar surface density of the CSS during these interactions.
Paper: Two Channels of Metal-rich Compact Stellar System Formation: Starbursts under High Ram Pressure versus Tidal Stripping
Authors: Yuan Bian, Min Du, Victor P. Debattista, Dylan Nelson, Mark A. Norris, Luis C. Ho, Shuai Lu, Renyue Cen, Shuo Ma, Chong Ge, Taotao Fang, Hui Li
Figure caption: 〈Age〉 vs. σAge of CSSs. We plot the mass-weighted average age, 〈Age〉, vs. the age dispersion, σAge, for each CSS at z = 0. Red triangles represent TS-CSSs, while blue triangles represent BSF-CSSs. BSF-CSSs are younger and have a narrower age distribution (typically with σAge<1 Gyr) compared to TS-CSSs.
Paper: Late-time Radio Brightening and Emergence of a Radio Jet in the Changing-look AGN 1ES 1927+654
Authors: Eileen T. Meyer, Sibasish Laha, Onic I. Shuvo, Agniva Roychowdhury, David A. Green, Lauren Rhodes, Amelia M. Hankla, Alexander Philippov, Rostom Mbarek, Ari laor, Mitchell C. Begelman, Dev R. Sadaula, Ritesh Ghosh, Gabriele Bruni, Francesca Panessa, Matteo Guainazzi, Ehud Behar, Megan Masterson, Haocheng Zhang, Xiaolong Yang, Mark A. Gurwell, Garrett K. Keating, David Williams-Baldwin, Justin D. Bray, Emmanuel K. Bempong-Manful, Nicholas Wrigley, Stefano Bianchi, Federica Ricci, Fabio La Franca, Erin Kara, Markos Georganopoulos, Samantha Oates, Matt Nicholl, Main Pal, S. Bradley Cenko
Figure caption: The soft X-ray and radio light curves of 1ES 1927+654 since 2021. The top panel shows the 0.3–2 keV flux (in units of 10−12 erg cm−2 s−1) observed by the Swift/XRT (further details in S. Laha et al. 2024). The middle panel shows the total (log scale) VLBA/EVN flux in bands C, X, and K (5, 8.4, and 22.2/23.5 GHz, respectively), along with fluxes from lower-resolution AMI and e-MERLIN observations at 15.5 and 5 GHz, respectively. The bottom panel shows the evolution of the radio spectral index between 5 and 8.4 GHz (light red) and between 8.4 and 22 GHz (dark red); open circles denote two epochs of near-simultaneous observations for the lower band index. While the X-rays have shown considerable variability during the years since the late 2017 CL event, the radio remained quiescent in all bands until exhibiting an exponential rise over a few months in early 2023. The radio evolution since has shown only mild variability at or slightly below the peak radio flux density reached in 2023 June, with the exception of K band.
Paper: Late-time Radio Brightening and Emergence of a Radio Jet in the Changing-look AGN 1ES 1927+654
Authors: Eileen T. Meyer, Sibasish Laha, Onic I. Shuvo, Agniva Roychowdhury, David A. Green, Lauren Rhodes, Amelia M. Hankla, Alexander Philippov, Rostom Mbarek, Ari laor, Mitchell C. Begelman, Dev R. Sadaula, Ritesh Ghosh, Gabriele Bruni, Francesca Panessa, Matteo Guainazzi, Ehud Behar, Megan Masterson, Haocheng Zhang, Xiaolong Yang, Mark A. Gurwell, Garrett K. Keating, David Williams-Baldwin, Justin D. Bray, Emmanuel K. Bempong-Manful, Nicholas Wrigley, Stefano Bianchi, Federica Ricci, Fabio La Franca, Erin Kara, Markos Georganopoulos, Samantha Oates, Matt Nicholl, Main Pal, S. Bradley Cenko
Figure caption: Plots of the radio spectral energy distribution (VLBI and SMA only), from 2020 January through 2024 April. As shown, the source exhibited a flat/hard spectrum during the initial rise in early 2023, but since then it shows a fairly consistent GPS. The peak of the spectrum appears to be at or just below 5 GHz. The SMA observations shown were taken on 2024 June 10 at 225 and 345 GHz and suggest a flat spectrum (α = 0.1 ± 0.6) in the submillimeter band, possibly consistent with a coronal origin. The 225 GHz flux in 2024 June is consistent with the value obtained in 2023 July at the same frequency.
Paper: Late-time Radio Brightening and Emergence of a Radio Jet in the Changing-look AGN 1ES 1927+654
Authors: Eileen T. Meyer, Sibasish Laha, Onic I. Shuvo, Agniva Roychowdhury, David A. Green, Lauren Rhodes, Amelia M. Hankla, Alexander Philippov, Rostom Mbarek, Ari laor, Mitchell C. Begelman, Dev R. Sadaula, Ritesh Ghosh, Gabriele Bruni, Francesca Panessa, Matteo Guainazzi, Ehud Behar, Megan Masterson, Haocheng Zhang, Xiaolong Yang, Mark A. Gurwell, Garrett K. Keating, David Williams-Baldwin, Justin D. Bray, Emmanuel K. Bempong-Manful, Nicholas Wrigley, Stefano Bianchi, Federica Ricci, Fabio La Franca, Erin Kara, Markos Georganopoulos, Samantha Oates, Matt Nicholl, Main Pal, S. Bradley Cenko
Figure caption: Total polarized intensity map at 5.5 GHz for the VLA observation of 2023 May 21. The color scale gives the flux density in mJy beam−1. Contours overlaid in cyan correspond to the total (Stokes I) intensity, with levels at 10, 50, 250, and 1000 times the base value 2.5 × 10−5 Jy beam−1, which is approximately the total intensity image rms. The vectors shown in black correspond to the measured linear polarization EVPA (no rotation applied). The polarized intensity peak appears slightly offset from the total intensity peak and has a value of 0.29 mJy, corresponding to a 0.6% polarization fraction.
Paper: Late-time Radio Brightening and Emergence of a Radio Jet in the Changing-look AGN 1ES 1927+654
Authors: Eileen T. Meyer, Sibasish Laha, Onic I. Shuvo, Agniva Roychowdhury, David A. Green, Lauren Rhodes, Amelia M. Hankla, Alexander Philippov, Rostom Mbarek, Ari laor, Mitchell C. Begelman, Dev R. Sadaula, Ritesh Ghosh, Gabriele Bruni, Francesca Panessa, Matteo Guainazzi, Ehud Behar, Megan Masterson, Haocheng Zhang, Xiaolong Yang, Mark A. Gurwell, Garrett K. Keating, David Williams-Baldwin, Justin D. Bray, Emmanuel K. Bempong-Manful, Nicholas Wrigley, Stefano Bianchi, Federica Ricci, Fabio La Franca, Erin Kara, Markos Georganopoulos, Samantha Oates, Matt Nicholl, Main Pal, S. Bradley Cenko
Figure caption: Core-subtracted K-band VLBA images of 1ES 1927+654 on 2023 June 8 (top left) 2024 February 9 (top right), 2024 April 24 (bottom left), and 2024 May 30 (bottom right). The contours correspond to the non-core-subtracted intensity and are drawn at 5, 10, 15, 20, and 50 times the non-core-subtracted image rms (given in the upper right corner of each panel). The longer 2024 February observation resulted in better UV coverage and a less elongated synthesized beam (green oval in the lower left corner of each panel) than the other observations. The extended structure apparent in early- to mid-2024 is entirely absent at the time of the initial radio outburst in 2023 June.
Paper: Radial Evolution of Interplanetary Shock Properties with Heliospheric Distance: Observations from Parker Solar Probe
Authors: Oksana Kruparova, Adam Szabo, Lan K. Jian, František Němec, Jana Šafránková, Zdeněk Němeček, Jacob Pasanen, Ayris Narock, Vratislav Krupar
Figure caption: Example of an SR shock observed by PSP on 2018 November 7 at 07:50:19 UT, with R-H asymptotic values calculated using the NEWGAP code (A. Szabo 1994). Panels show: (a) proton density, (b)–(d) proton velocity components in RTN coordinates, (e) thermal speed, (f) magnetic field magnitude, and (g)–(i) magnetic field components in RTN coordinates. The vertical dashed orange line marks the shock time. Upstream and downstream intervals used for the R-H analysis are highlighted by horizontal black and colored lines, respectively, with the corresponding R-H results indicated. All parameters fall within the R-H solution error bars, indicating successful asymptotic solutions.
Paper: Radial Evolution of Interplanetary Shock Properties with Heliospheric Distance: Observations from Parker Solar Probe
Authors: Oksana Kruparova, Adam Szabo, Lan K. Jian, František Němec, Jana Šafránková, Zdeněk Němeček, Jacob Pasanen, Ayris Narock, Vratislav Krupar
Figure caption: Scatter plots of key shock parameters vs. heliocentric distance for all 66 IP shocks observed by PSP. (a) Density compression (ncomp), (b) magnetic field compression (Bcomp), (c) change in velocity (ΔV), and (d) shock normal angle (θBn). Different colors represent different shock types: FF (red), FR (green), SF (blue), and SR (magenta). Kendall's tau coefficients (τ) and p-values (p) are indicated in each panel.
Paper: Radial Evolution of Interplanetary Shock Properties with Heliospheric Distance: Observations from Parker Solar Probe
Authors: Oksana Kruparova, Adam Szabo, Lan K. Jian, František Němec, Jana Šafránková, Zdeněk Němeček, Jacob Pasanen, Ayris Narock, Vratislav Krupar
Figure caption: Histogram of radial distances from the Sun for all 66 IP shocks observed by PSP, color coded by shock type: FF (red), FR (green), SF (blue), and SR (magenta).
Paper: Radial Evolution of Interplanetary Shock Properties with Heliospheric Distance: Observations from Parker Solar Probe
Authors: Oksana Kruparova, Adam Szabo, Lan K. Jian, František Němec, Jana Šafránková, Zdeněk Němeček, Jacob Pasanen, Ayris Narock, Vratislav Krupar
Figure caption: Temporal evolution of magnetic field and plasma parameters across four types of IP shocks in the spacecraft frame of reference.
Paper: Shedding Light on the Origin of the Broken Misaligned Circumtriple Disk around GW Ori
Authors: Jeremy L. Smallwood, Stephen H. Lubow, Rebecca G. Martin, Rebecca Nealon
Figure caption: Circumtriple disk evolution around GW Ori with an initial misalignment between the disk and the outer binary of the triple star of i0 = 38∘ (first two columns) and i0 = 28∘ (last two columns) at time t = 2000 Porb. The upper row represents disks with H/r = 0.02, while the bottom row shows those with H/r = 0.05. The triple stars are depicted by blue dots. Columns 1 and 3 show the view looking down onto the outer binary orbital plane (the x–y plane), while columns 2 and 4 present the x–z plane, with the AB-C binary eccentricity aligned along the x-axis. The color indicates gas density, with the yellow regions being about 2 orders of magnitude higher than the purple regions.