adsabs/AstroCLIMB huggingface dataset:
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: The CHARA Array data for W Ser are plotted as black points, while the best-fit results from gridsearch are overplotted in red. The visibilities are plotted in the left column, the closure phases are plotted in the second column, the positions associated with the best-fit result from gridsearch are plotted in the third column (R.A. on the x-axis, and decl. on the y-axis), and the spatial frequency (u, v) coverage is plotted in the final column. The brighter component (not shown) is located at the origin in the position diagrams. Since we fixed the fluxes of each component, the code generally finds two solutions for the companion that differ by 180° in position angle. The red circle in the χ 2 maps identifies the solution with the lowest χ 2 and gives the preferred position of the fainter companion relative to the brighter component. The first four rows show data from MIRC-X, and the bottom row shows data from MYSTIC on the best night. From top to bottom, the data were obtained on 2021 July 28, 2023 July 26, 2023 July 27, and 2023 July 28 (for MIRC-X and MYSTIC). Note that there are two pairs of solutions for the 2023 July 26 data set. We selected the better χ 2 solution that was also more consistent with the predicted angular orbit (Figure 9).
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: A graphical representation of the configuration of W Ser as seen from above. The mass donor is on the right and is filling its Roche lobe. The mass gainer (gray) is on the left and is surrounded by its accretion torus (light blue). The mass-transfer stream lies between the stars, but its trajectory and point of impact with the torus may be time variable and related to the stochastic variability of the light curve. The center of mass is indicated by a tick mark. Material leaking out of the region near the mass gainer forms a spiral structure starting at the L3 point. This spiral gradually progresses outward until it joins the circumbinary disk. The size of the CBD relative to the inner binary is not to scale. Numbers on the periphery refer to the orbital phases for different lines of sight.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: Mass of the donor and the gainer based upon the donor star spectroscopic mass function ﹩{ \mathcal F }(M)﹩. The curved lines correspond to the best-fit inclination of i = 79.°1 (solid line) and the lower limit for i = 90° (dashed–dotted line). The dotted lines represent the range given the uncertainty in ﹩{ \mathcal F }(M)﹩. The dashed diagonal line indicates a mass ratio of q = 0.36 ± 0.09 (dotted lines for uncertainty). The intersection point of the solid and dashed lines marks the best fit, and the gray shaded region indicates the error limited range of solutions.
Paper: A Spectroscopic and Interferometric Study of W Serpentis Stars. I. Circumbinary Outflow in the Interacting Binary W Serpentis
Authors: Katherine Shepard, Douglas R. Gies, Gail H. Schaefer, Narsireddy Anugu, Fabien R. Baron, Cyprien Lanthermann, John D. Monnier, Stefan Kraus, Theo ten Brummelaar
Figure caption: MACIM image reconstructions (M. J. Ireland et al. 2006) of the three 2023 nights of data for W Ser made by J. D. Monnier. Each image has 0.04 mas pixel−1. These images illustrate not only the change in position angle that is related to binary motion, but also how difficult it is to resolve this system.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Sizes of the proximity zones (R p) as a function of M UV. The red filled circle indicates the potential AGN source of ID10646, and the red open circle represents the dusty BL AGN of ID20466 after the dust correction. The blue circles indicate the previous measurements for luminous quasars at z ∼ 6 (A.-C. Eilers et al. 2018; R. Ishimoto et al. 2020). The blue and black curves are the best-fit relations for the observations (R. Ishimoto et al. 2020) and the radiative transfer simulations (A.-C. Eilers et al. 2017), respectively. ID10646 and ID20466 show remarkable gaps compared to the previous measurements and theoretical trends. In line with the bright Lyα line detection from the dusty BL AGN of ID20466, one interpretation is that the IGM gas density around these two sources is lower than the environment around the luminous quasars at z ∼ 6 and illuminated by ionizing (and Lyα) photons that escaped from the dusty cloud with a low covering fraction around the AGN. Together with the high AGN abundance from the UV LF measurements at z ∼ 9–10 (Section 4), the identification of one of the largest ionized bubbles to date around a dusty BL AGN and a possible AGN source indicates the nonnegligible contributions of AGNs to cosmic reionization.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Zoom-in 1D + 2D prism spectra of ID10646 (left) and ID20466 (right). The magenta vertical line and dashed curve indicate the expected Lyα line wavelength and the best-fit spline model using msaexp based on z line, respectively. Blueward of the Lyα continuum or line is clearly detected in both sources. The red curve in ID10646 represents our best-fit IGM absorbed model with an ionized bubble, yielding a best-fit R p value of 7.69 ± 0.18 pMpc. The red vertical line corresponds to the expected wavelength of the Lyα line based on the redshift of the ionization front of the ionized bubble along the line of sight. Because of the lack of the blueward Lyα continuum and the difficulty in modeling the intrinsic Lyα line profile in ID20466, we perform the R p measurement only for ID10466. For reference, the red dashed vertical line in ID20466 is drawn at the same wavelength as the red vertical line in the left panel.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Schematic illustration of the relative 3D positions of ID20466 and ID10646 in the source plane. The source plane coordinates of ID20466 and ID10646 are (R.A., decl.) = (3.63506157, −30.44818861) and (3.63209972, −30.46295758), respectively. The light blue shaded sphere denotes an isotropic sphere of the ionized bubble with R p = 7.7 pMpc measured from the blueward Lyα line and continuum emission in the prism spectrum of ID10646. Their physical distance of 0.38 pMpc indicates that ID20466 also resides in the same ionized bubble, which facilitates the blueward Lyα emission also observed from ID20466, and the AGN activity in ID20466 (and ID10646) may contribute to forming this ionized bubble.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top: a partial-amplitude spectrum of the light curve. Bottom: the amplitude spectrum of the envelope. Both plots are designed with the same scale on the x-axis to facilitate alignment. Specifically, the x-axis of the upper figure starts from f 3, and the x-axis of the lower figure starts from −f  m2, both adjustments aiming to align f 0 with f  m1. Red dashed lines, spaced at intervals of f  m1, are drawn across the plots.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Corrected and smoothed light curves of KIC 10407873. Top panel: the entire light curve spanning 1470.5 days, showing long-period amplitude modulation with a period of 73.46 days. Bottom panel: local light curve over a span of 6 days, showcasing short-period amplitude modulation with a period of 1.40 days.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The Fourier amplitude spectrum of the corrected and smoothed light curve of KIC 10407873. The dashed line represents the Nyquist frequency f  N  = 24.469 day−1. The pulsation main frequency and the splitting frequencies caused by amplitude modulation are marked in the figure.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: A portion of KIC’s light curve and its envelope. The black line represents the corrected light curve, while the blue points represent the envelope obtained after applying the Hilbert transform.
Paper: Hilbert Transform Reveals Unusual Modulation in Delta Scuti Star KIC 10407873
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The amplitude spectra and phase-folded light curves of each segment.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Upper panels: predicted minimum IR (8–1000 μm) luminosity of SFGs detected by the reference survey at 30, 100, and 350 μm (blue curves) as a function of redshift. The dotted–dashed green line shows, for comparison, the minimum luminosity corresponding to the 80% completeness of the PEP survey of the COSMOS field (9 mJy; S. Berta et al. 2011) at 100 μm and that corresponding to the Herschel SPIRE 5σ confusion limit at 350 μm (31.5 mJy; H. T. Nguyen et al. 2010). The points with error bars show the characteristic luminosity, L ⋆(z), of the Schechter fit of the IR LF by C. Gruppioni et al. (2013); the point at 4.5 ≤ z ≤ 6 is from C. Gruppioni et al. (2020). The dashed red line shows an estimate of the IR luminosity of the SFG hosting an AGN having a 2–10 keV X-ray luminosity at the 90% completeness detection limit of the Chandra COSMOS legacy survey (7.8 × 10−15 erg cm−2 s−1;  Table 2 of S. Puccetti et al. 2009), as a function of z. To compute the K-correction, we assumed a power-law energy spectrum with a spectral index of −0.4, the slope of the cosmic X-ray background in this energy range; this represents an effective spectral index, taking into account both obscured and unobscured AGNs. Lower panels: minimum bolometric luminosity of AGNs detectable by the reference survey at the three wavelengths as a function of redshift (solid blue line). The dashed red line shows, for comparison, an estimate of the minimum bolometric luminosity of AGNs detected in X-rays by the Chandra COSMOS legacy survey, as a function of z; it was obtained by applying the bolometric correction of 22.4 (from C.-T. J. Chen et al. 2013) to the 2–10 keV luminosity, computed as described above. The data points show the characteristic AGN bolometric luminosity up to z = 6 derived by X. Shen et al. (2020). Similar to the upper panels, the dotted–dashed green line shows, for comparison, the minimum bolometric luminosity corresponding to the 80% completeness of the PEP survey of the COSMOS field (9 mJy; S. Berta et al. 2011) at 100 μm and that corresponding to the Herschel SPIRE 5σ confusion limit at 350 μm (31.5 mJy; H. T. Nguyen et al. 2010).
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: (a) Blue: spectrum extracted from the convolved maps integrated over the same aperture area as that containing 48 galaxies—from which the spectra of the brightest sources are shown in Figure 5—with the “known” model foreground emission subtracted. Red: the summed spectrum of all 48 galaxies in the aperture multiplied by a factor of 3 to offset the resulting spectrum from the lower curve. Six galaxies—those at redshifts 0.11, 0.45, 0.56, 1.39, 1.40, and 3.04—contribute significantly to the emission seen in the summed spectrum, and a single galaxy at z = 0.56 dominates. The PAH feature seen at ∼30 μm is primarily attributable to the ultraluminous galaxy at z = 3.04. (b) The difference between the convolved spectrum (lower/blue curve in (a)) and the sum of the galaxy spectra in the analyzed aperture (upper/red curve in (a)). (c) The corresponding fractional difference between the two spectra. Spectral line blending is most severe at the long-wavelength end of the spectrum, due to the larger beam size at longer wavelengths. Line intensities can be either underestimated or overestimated in a spectrum obtained with a 2 m telescope. At wavelengths ≳70 μm, the shape of the continuum is distorted, suggesting that efforts to ascribe continuum emission to individual galaxies are subject to bias from sources outside the aperture area. While not apparent in (b), the fractional difference in (c) shows that broadband PAH features from high-redshift galaxies merge at wavelengths ≲50 μm.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Spatially integrated spectra of the 22 brightest of 48 simulated galaxies in the analyzed aperture area, shown in order of increasing redshift in raster fashion from top left to bottom right. The remaining galaxies are at best barely brighter than 10 μJy. The same foreground spectrum was subtracted from each galaxy's spectrum. The foreground spectrum is extracted from the data cube at the location of the darkest pixel at 25 μm. The three numbers in each panel indicate the galaxy's redshift, the base-10 logarithm of its disk-integrated IR (8–1000 μm) luminosity in solar units, and the galaxy's AGN luminosity in the same units, respectively. Only one bright galaxy, as indicated, has a Type 1 AGN, while all the others have Type 2 AGNs. The galaxy at redshift z = 3.04 is the only one in the aperture area with a luminosity greater than 1012 L ⊙ and would be considered “ultraluminous.”
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Predicted integral number counts (left) and redshift distributions (right) for sources detected in line emission by the reference survey. In the top left panel, the integral counts of the [Si II] line are superimposed on those of the [O I] line. The dotted–dashed vertical black lines in the left-hand panels show the 5σ detection limit (the mean detection limit for the reference survey and for the fine-structure lines among the four spectral bands). Upper panels: SFGs detected in one or more bright lines, with spectral resolution R = 500 for fine-structure lines and R = 50 for the PAH band. The inflection points of the redshift distributions are due to the transition from the first band (25–50 μm) to the more sensitive second band (50–100 μm). Lower panels: same as in the upper panels, but for AGN lines. The transition from the first to the second band is responsible for the bump at z ≳ 1.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Confusion limit, S conf (5σ), at 30, 100, and 350 μm as a function of the effective telescope diameter or maximum interferometer baseline, D. The diamonds show the measured confusion limits of Herschel SPIRE at 350 μm (31.5 mJy; black diamond; H. T. Nguyen et al. 2010) and of Herschel PACS at 100 μm (0.75 mJy; red diamond; B. Magnelli et al. 2013). The improved resolution of the interferometer results in a dramatic fall of confusion limits. The stars represent the confusion limits for the proposed survey. The model, used to compute S conf as a function of D at the three wavelengths, shown by the solid blue line, by the dotted red line, and by the dotted–dashed black line, yields S conf = 2.3 × 10−7, 8.3 × 10−5, and 0.14 μJy at 30, 100, and 350 μm, respectively. Confusion is negligible at these levels.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Template SEDs of dusty proto-spheroids with L IR = 1012 L ⊙ (left) and obscured AGNs with bolometric luminosity L bol = 1013 L ⊙ (right), at z = 1, 2, 3, 4, and 6, from Z.-Y. Cai et al. (2013), compared with the 5σ detection limits for 1 hr exposures of the FIR interferometer, of JWST MIRI, of the Spitzer Multiband Imaging Photometer for Spitzer, of Herschel PACS and SPIRE, and of ALMA. The luminosity of 1012 L ⊙ corresponds to an SFR of ≃100 M ⊙ yr−1, typical of SFGs at cosmic noon (z ≃ 2–3).
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: The predicted intensities of key spectral lines, compared to 5σ detection limits for 1 hr exposures with the FIR interferometer, JWST MIRI, Spitzer IRS, Herschel PACS and SPIRE, and ALMA. Left: lines powered by star formation from galaxies with L IR = 1013 L ⊙ at z = 1, 2, 3, 4, and 6 (filled symbols connected by solid lines, from left to right). Right: lines powered by AGNs with bolometric luminosity L bol = 1014 L ⊙ at the same redshifts.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Integral counts per square degree at 30, 100, and 350 μm (from left to right) predicted by our model. The vertical black lines correspond to the 5σ reference survey detection limits of 0.14, 0.21, and 0.33 mJy, respectively. The vertical dotted–dashed cyan lines show, at 100 μm, the 80% completeness limit (9 mJy) of the Herschel PACS PEP survey of the COSMOS field (S. Berta et al. 2011) and, at 350 μm, the Herschel SPIRE 5σ confusion noise (31.5 mJy; H. T. Nguyen et al. 2010).
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Predicted redshift distributions at 30, 100, and 350 μm (from left to right) at the detection limits of the reference survey (0.14, 0.21, 0.33) mJy, respectively. The deep hollow at z ∼ 2 in the 30 μm distribution is due to the strong silicate absorption around 9.7 μm. The inflection point at z ≃ 2–2.5, seen at 100 and 350 μm, corresponds to the transition from starburst to proto-spheroid dominance.
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: The SFHs and the evolution of the radial distance of randomly selected stars in two galaxies (g7.08e11 and g7.55e11). The right panel shows the evolution of radial distance to the galactic center of 10,000 randomly selected star particles in each galaxy, which clearly show a bimodal distribution with a characteristic radius of R  g  ∼ 5 kpc, which roughly classifies the stars into the inner and outer region of the galaxies. The left panel shows the total SFH, as well as SFHs in the inner and outer regions of the galaxies. For reference, we mark the epoch for the LMM of each galaxy in each panel.
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 feedback gas in different phase states. Subplots (a) and (b) feature two galaxies, g7.08e11 and g7.55e11, run by GIZMO and GASOLINE, respectively. For each galaxy, the upper panel is the mass fraction of feedback gas in different outermost phase states (see the text for the meaning of outermost phase state), as labeled in each panel, and the lower panel is the duration of feedback gas in each phase.
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: Whereabouts of the final cold disk of the g7.08e11 and g7.55e11 galaxies in two simulations across cosmic time. The upper and lower panels of each subplot display comparisons of the mass and angular momentum fraction in different phases, respectively.