adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Intracluster Globular Clusters in the First JWST Images of the Gravitational Lens Cluster SMACS J0723.3–7327 at z = 0.39
Authors: Myung Gyoon Lee, Jang Ho Bae, In Sung Jang
Figure caption: Completeness (recovery fraction) vs. F150W (a) and F200W (b) magnitudes of the point sources. Blue solid lines denote the fitting results. The vertical black lines mark 50% completeness limits: ﹩{\rm{F}}150{{\rm{W}}}_{0,{\rm{l}}{\rm{i}}{\rm{m}}}=30.44﹩ and ﹩{\rm{F}}200{{\rm{W}}}_{0,{\rm{l}}{\rm{i}}{\rm{m}}}=30.11﹩ mag.
Paper: GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114
Authors: A. S. Evans, D. T. Frayer, Vassilis Charmandaris, Lee Armus, Hanae Inami, Jason Surace, Sean Linden, B. T. Soifer, Tanio Diaz-Santos, Kirsten L. Larson, Jeffrey A. Rich, Yiqing Song, Loreto Barcos-Munoz, Joseph M. Mazzarella, George C. Privon, Vivian U, Anne M. Medling, Torsten Böker, Susanne Aalto, Kazushi Iwasawa, Justin H. Howell, Paul van der Werf, Philip Appleton, Thomas Bohn, Michael J. I. Brown, Christopher C. Hayward, Shunshi Hoshioka, Francisca Kemper, Thomas Lai, David Law, Matthew A. Malkan, Jason Marshall, Eric J. Murphy, David Sanders, Sabrina Stierwalt
Figure caption: A comparison of the JWST MIRI 5.6, 7.7, and 15 μm images to the HST 0.4 μm, Spitzer IRAC 5.8 μm, MIPS 24 μm, VLA 3.0 GHz (θ FWHM ∼ 0.″7 resolution), and ALMA CO(2-1) emission (θ FWHM ∼ 0.″5: green contours in (i)). The axes are in degrees of R.A. and decl. The HST and JWST images are displayed in a logarithmic stretch to highlight both high and low surface brightness emission. The Spitzer and VLA images are displayed in a linear stretch. The eastern dust lanes visible in the 0.4 μm image cover the bright mid-infrared emission observed with Spitzer and JWST. Both VV 114E cores are also visible in the VLA images, as well as several of the higher surface brightness star-forming regions observed in the JWST images (i). The JWST images show an order-of-magnitude improvement in resolution and a factor of 50 improvement in sensitivity relative to Spitzer, allowing for the identification of ∼40 mid-IR star-forming regions and underlying diffuse emission at resolutions of ∼100–200 pc.
Paper: GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114
Authors: A. S. Evans, D. T. Frayer, Vassilis Charmandaris, Lee Armus, Hanae Inami, Jason Surace, Sean Linden, B. T. Soifer, Tanio Diaz-Santos, Kirsten L. Larson, Jeffrey A. Rich, Yiqing Song, Loreto Barcos-Munoz, Joseph M. Mazzarella, George C. Privon, Vivian U, Anne M. Medling, Torsten Böker, Susanne Aalto, Kazushi Iwasawa, Justin H. Howell, Paul van der Werf, Philip Appleton, Thomas Bohn, Michael J. I. Brown, Christopher C. Hayward, Shunshi Hoshioka, Francisca Kemper, Thomas Lai, David Law, Matthew A. Malkan, Jason Marshall, Eric J. Murphy, David Sanders, Sabrina Stierwalt
Figure caption: A F770W/F560W vs. F1500W/F560W flux density ratio plot of the VV 114E cores (stars) and the mid-IR knots (filled black circles) in VV 114. The diffuse component of VV 114 is plotted as a “+” symbol. Also plotted are LIRGs in the GOALS sample with ratios derived from Spitzer IRS data. The LIRGs are color coded by their 6.2 μm PAH equivalent width, and the triangle is the IRS-derived ratio of VV 114. The MIRI-derived ratios for the total VV 114 emission (the “×”) agree well with the IRS-derived ratio. The MIRI-detected knots and VV 114E NE have MIRI ratios consistent with LIRGs with strong PAH emission, and they are redder in F1500W/F560W relative to the majority of the IRS measured values of the GOALS LIRG sample, indicating that they are reddened star-forming regions. VV 114E SW ratios are consistent with an AGN.
Paper: GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114
Authors: A. S. Evans, D. T. Frayer, Vassilis Charmandaris, Lee Armus, Hanae Inami, Jason Surace, Sean Linden, B. T. Soifer, Tanio Diaz-Santos, Kirsten L. Larson, Jeffrey A. Rich, Yiqing Song, Loreto Barcos-Munoz, Joseph M. Mazzarella, George C. Privon, Vivian U, Anne M. Medling, Torsten Böker, Susanne Aalto, Kazushi Iwasawa, Justin H. Howell, Paul van der Werf, Philip Appleton, Thomas Bohn, Michael J. I. Brown, Christopher C. Hayward, Shunshi Hoshioka, Francisca Kemper, Thomas Lai, David Law, Matthew A. Malkan, Jason Marshall, Eric J. Murphy, David Sanders, Sabrina Stierwalt
Figure caption: A close-up comparison of the VV 114E nucleus at 7.7 μm and 33 GHz (θ FWHM ∼ 0.″2: Song et al. 2022). In the JWST image, the nucleus is separated into an NE and SW core. The SW core is further resolved into two components, with the most southern component (SW-S knot) having a tail of emission extending in the SW direction. In the VLA image, the SW core is resolved into four components.
Paper: GOALS-JWST: Hidden Star Formation and Extended PAH Emission in the Luminous Infrared Galaxy VV 114
Authors: A. S. Evans, D. T. Frayer, Vassilis Charmandaris, Lee Armus, Hanae Inami, Jason Surace, Sean Linden, B. T. Soifer, Tanio Diaz-Santos, Kirsten L. Larson, Jeffrey A. Rich, Yiqing Song, Loreto Barcos-Munoz, Joseph M. Mazzarella, George C. Privon, Vivian U, Anne M. Medling, Torsten Böker, Susanne Aalto, Kazushi Iwasawa, Justin H. Howell, Paul van der Werf, Philip Appleton, Thomas Bohn, Michael J. I. Brown, Christopher C. Hayward, Shunshi Hoshioka, Francisca Kemper, Thomas Lai, David Law, Matthew A. Malkan, Jason Marshall, Eric J. Murphy, David Sanders, Sabrina Stierwalt
Figure caption: (a) False-color optical image of VV 114 constructed with HST WFC3/UVIS F330W (0.3 μm) and the ACS/WFC F435W (0.4 μm) and F814W (0.9 μm) data. Both (a) and (b) have the same spatial scale. The blue “+” symbols mark the location of the VV 114E NE and SW cores detected with MIRI. (b) False-color mid-IR image constructed with F560W, F770W, and F1500W MIRI data. Blue (5.6 μm) diffraction spikes emanate from the VV 114E NE and SW cores. The images are displayed in a logarithmic stretch to highlight both high and low surface brightness emission, and they show NUV/UV starlight ((a)—white knots) and dust lanes ((a)—red), the reddened nucleus and star-forming regions ((b)—pink), and the extended, filamentary 7.7 μm PAH emission ((b)—green), which covers much of the MIRI field of view.
Paper: First Millimeter Flares Detected from ϵ Eridani with the Atacama Large Millimeter/submillimeter Array
Authors: Kiana Burton, Meredith A. MacGregor, Rachel A. Osten
Figure caption: (Left) Natural weighted image of continuum emission from the Atacama Compact Array (ACA). Millimeter emission is detected at the stellar position (center of the image) at 776 ± 103 μJy . The outer debris disk is seen surrounding the star at approximately 16″. The contour levels are in steps of [−2, 2, 4, 6, 8...] × the rms noise of 94 μJy beam−1. The gray ellipse in the lower left corner shows the beam size, which is 7.″4 × 4.″5. (Right) Primary beam corrected, natural weighted continuum image of ϵ Eridani and the northern arc of its outer debris disk from the Atacama Large Millimeter/submillimeter Array (ALMA) 12 m array. Millimeter emission at the stellar position, 794 ± 45 μJy. The contours are in steps of [−3, 3, 6, 9...] × the rms noise of 33 μJy beam−1 (primary beam corrected noise). The beam size is 1.″6 × 1.″1, as indicated by the gray ellipse in the lower left corner of the image.
Paper: Metallicities of Five z > 5 Emission-line Galaxies in SMACS 0723 Revealed by JWST
Authors: A. J. Taylor, A. J. Barger, L. L. Cowie
Figure caption: Gaussian and continuum fits to the 1D spectra for the galaxy sample. In each panel, the blue curve is the coadded 1D spectrum, and the red curves are the best-fit functions to the spectrum. For visual clarity, we normalize the flux scale to be equal to 1 at the peak of the [O III]λ5007 line fit. Note that object 05144 is at too low of redshift for the G395/F290LP observations to capture the [O II]λ3727+H8+[Ne III]λ3869 complex. To avoid introducing errors from comparing lines across both filter/grating observations, we omit the [O II]λ3727+H8+[Ne III]λ3869 fit for this object. Also note that due to limited signal, the [O II]λ3727+H8+[Ne III]λ3869 fit for object 10612 failed to converge.
Paper: First Millimeter Flares Detected from ϵ Eridani with the Atacama Large Millimeter/submillimeter Array
Authors: Kiana Burton, Meredith A. MacGregor, Rachel A. Osten
Figure caption: Images for all three detected flares (E1, top row; E2, middle row; E3, bottom row) in the integration just before the flare (left panels), at the peak of the flares (middle panels), and just after the flare (right panels). A point source is only detected at the stellar position (bottom center of the image toward the edge of the primary beam) at the flare peak for all three events. The flux density from these images (indicated by the color scale bars) is consistent with what we obtain from visibility modeling.
Paper: First Millimeter Flares Detected from ϵ Eridani with the Atacama Large Millimeter/submillimeter Array
Authors: Kiana Burton, Meredith A. MacGregor, Rachel A. Osten
Figure caption: Light curves of the three major flaring events labeled E1, E2, and E3. Each light curve is centered on the flare peak, with the top x-axis indicating time relative to the flare peak in seconds. Each data point represents an individual ALMA integration (6 s in length, indicated by the x error bars). The shaded region in each plot indicates ± the rms noise level centered on a dashed line at 0 mJy.
Paper: Metallicities of Five z > 5 Emission-line Galaxies in SMACS 0723 Revealed by JWST
Authors: A. J. Taylor, A. J. Barger, L. L. Cowie
Figure caption: Gaussian and continuum fits to the weighted aperture extracted 1D spectra for the galaxy sample. In each panel, the blue curve is the coadded and extracted 1D spectrum, and the red curves are the best-fit functions to the spectrum. For visual clarity and ease of comparison, we again normalize the flux scale to be equal to 1 at the peak of the [O III]λ5007 line fit.
Paper: Metallicities of Five z > 5 Emission-line Galaxies in SMACS 0723 Revealed by JWST
Authors: A. J. Taylor, A. J. Barger, L. L. Cowie
Figure caption: Cutouts of the coadded 2D spectra centered on the [O III]λ5007 and [O III]λ4363 lines. The extraction footprints determined by the [O III]λ5007 line shape are shown with black outlines.
Paper: First Millimeter Flares Detected from ϵ Eridani with the Atacama Large Millimeter/submillimeter Array
Authors: Kiana Burton, Meredith A. MacGregor, Rachel A. Osten
Figure caption: Gaussian fits to the light curves of the three flares detected from ϵ Eridani. These flares are similar to millimeter flares detected previously by ALMA in being relatively short-lived.
Paper: Prograde and Retrograde Gas Flow around Disk-embedded Companions: Dependence on Eccentricity, Mass, and Disk Properties
Authors: Yi-Xian Chen, Avery Bailey, James Stone, Zhaohuan Zhu
Figure caption: Flow pattern around the embedded companion. The color shows the specific angular momentum of gas J 0 relative to the companion (red: prograde; blue: retrograde), and the purple arrows represent the flow velocity around the companion. The three columns correspond to e = 0.02, 0.065, 0.067 cases for parameters h 0 = 0.05 and q  t  = 0.2. Upper/lower panels are at the apogee/pergee. The flow quantities are averaged over the last 10 snapshots at the companion’s perigee/apogee passing. The innermost solid black circle is the softening length ϵ, the black dashed circles represent R BHL, while the red dashed circles represent R  H . The x, y coordinates are normalized in R  B . The faint white dashed lines roughly indicate shock fronts.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Comparison between the spectral slopes of the Dhurmsala (LL6) and Tagish Lake (C2) meteorites, Sw-type asteroid 433 Eros, and D-type asteroids as a function of phase angle. The D-type asteroid data set is a combination of multiple D-type asteroids. Gray and yellow areas indicate the slope uncertainty from Marsset et al. (2020) for the meteorites and asteroids, respectively. The solid and dashed lines represent polynomial fits for the meteorites and asteroids, respectively. The D-type data set includes the postimpact spectrum of 596.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Spectra of 203 Pompeja (top panels), 269 Justitia (bottom left panel), and 732 Tjilaki (bottom right panel). Square brackets in these panels indicate the observation dates. Black arrows are present on the right-hand side of the vertical axis in the 269 figure. Arrows indicate the slope uncertainty from Marsset et al. (2020) centered at the reflectance value of the spectra at 2.40 μm, as shown by the black dashed lines.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Spectra of 99942 Apophis (left panel) and 2020 WU5 (right panel). The data of 203 Pompeja, 99942 Apophis, and 2020 WU5 were taken on 2021 January 14. The spectra of 99942 and 2020 WU5 were measured four times and once, respectively (Binzel et al. 2009, 2019; Marsset et al. 2022), in addition to their measurement on the same day as 203 (Hasegawa et al. 2021). The five spectra of 99942 and the two spectra of 2020 WU5 are found to be in agreement. Square brackets in these panels indicate the observation dates. The black arrows indicate the slope uncertainty from Marsset et al. (2020) centered at the reflectance value of the spectra at 2.40 μm, as shown by the black dashed lines.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Spectral slope for 596 Scheila against space weathering time. Blue and orange lines correspond to linear and logarithmic regression of the spectral slope values of DeMeo et al. (2009), Yang & Hsieh (2011), and Hasegawa et al. (2022), respectively.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Comparison of the visible spectra of VROs 203 Pompeja, 269 Justitia, 2019 PR2, and 2019 QR6. The figure shows the spectra in the 0.4–1.0 μm wavelength regions, normalized to 1 at 0.55 μm.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Radial brightness profiles of 203 Pompeja obtained by the Zwicky Transient Facility on 2020 December 10 (top left), 17 (top middle), and 22 (top right) and 2021 January 5 (bottom left), 13 (bottom middle), and 19 (bottom right). These profiles are normalized at 2.″5 from the photocenter and compared with field stars. The FWHM of the images used was roughly 2″–3″. Since 203 was almost saturated, brightness profiles within 2.″5 from the photocenter are not given.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Comparison of 596 Scheila’s NIR spectra before, immediately after, and a decade after the 2010 impact event. The figure shows spectra of 596 in the 0.4–2.5 μm wavelength region, normalized to 1 at 0.55 μm. The black arrows indicate the slope uncertainty from Marsset et al. (2020) centered at the reflectance value of the spectra at 2.40 μm, as shown by the black dashed lines.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Convex shape models of 203 Pompeja. While the left panel represents the pole solution λ 1 = 315 [deg], β 1 = −40 [deg], the right panel shows the pole solution λ 2 = 132 [deg], β 2 = −36 [deg]. The left and middle views are equatorial with a 90° rotation, while the right view is pole-on. Both shape models appear very similar.
Paper: Spectral Evolution of Dark Asteroid Surfaces Induced by Space Weathering over a Decade
Authors: Sunao Hasegawa, Francesca E. DeMeo, Michaël Marsset, Josef Hanuš, Chrysa Avdellidou, Marco Delbo, Schelte J. Bus, Hidekazu Hanayama, Takashi Horiuchi, Driss Takir, Emmanuël Jehin, Marin Ferrais, Jooyeon Geem, Myungshin Im, Jinguk Seo, Yoonsoo P. Bach, Sunho Jin, Masateru Ishiguro, Daisuke Kuroda, Richard P. Binzel, Akiko M. Nakamura, Bin Yang, Pierre Vernazza
Figure caption: Spectra of 212 Medea, 328 Gudrun, and 769 Tatjana. The spectra of these asteroids were obtained at SAO in 2020–2021. Previous spectra were derived from Sergeyev & Carry (2021), Sergeyev et al. (2022), and Gaia Collaboration et al. (2022).
Paper: Corrections to Estimated Accretion Disk Size due to Color Correction, Disk Truncation, and Disk Wind
Authors: Andrzej A. Zdziarski, Bei You, Michał Szanecki
Figure caption: The disk blackbody spectra shown at the observer frame for r b = 6 for the parameters of SDSS 0924+0219 (Morgan et al. 2010) for some models of Table 1. (a) The blue solid and red dashed curves correspond to r in = 6 and f col = 1 and f col of C02, respectively. The green dotted and black dotted–dashed curves give the spectra for r in = 20, f col of C02 and ﹩{\dot{m}}_{\mathrm{out}}/{\dot{m}}_{\mathrm{in}}=1﹩ and 5, respectively. (b) The disk blackbody spectra were obtained with the models of D12 (﹩{\dot{m}}_{\mathrm{out}}/{\dot{m}}_{\mathrm{in}}=1﹩). The blue solid curve is for f col = 1, r in = 6, which was obtained with the optxagn model. The red dashed and green dotted curves are for f col of optxagnf (D12) and r in = 6 and 20, respectively. All of the spectra are normalized to the observed flux at ν 1 = 3.7 × 1014 Hz, where all of the above spectra intersect.
Paper: Corrections to Estimated Accretion Disk Size due to Color Correction, Disk Truncation, and Disk Wind
Authors: Andrzej A. Zdziarski, Bei You, Michał Szanecki
Figure caption: The radial emissivity profiles, ﹩{\rm{d}}{F}_{\nu }/\mathrm{dln}r﹩, at the source-frame wavelength of 2500 Å for some models of Table 1. The dotted cyan curve is for r in = 0, ﹩{\dot{m}}_{\mathrm{out}}/{\dot{m}}_{\mathrm{in}}=1﹩, and f col = 1. The red dashed and magenta solid curves are for r in = 6 and the color corrections of C02 and D12, respectively. The black dotted–dashed curve is for r in = 20, ﹩{\dot{m}}_{\mathrm{out}}/{\dot{m}}_{\mathrm{in}}=5﹩, and the color corrections of C02.
Paper: Metallicities of Five z > 5 Emission-line Galaxies in SMACS 0723 Revealed by JWST
Authors: A. J. Taylor, A. J. Barger, L. L. Cowie
Figure caption: Metallicity vs. rest-frame EW(Hβ) for the Laseter et al. (2022) sample of galaxies at z ≲ 1 with strong emission lines and rest-frame EW(Hβ) > 30 Å (red circles), JWST 1D spectra results (squares, see legend for colors), and JWST 2D spectra results (diamonds, see legend for colors). Note that the 2D spectrum for object 05144 has very faint continuum near the Hβ line. Given the substantial error on the continuum for this object, the upper error bounds on the EW(Hβ) exceed ∼400 Å, so we use a rightward-pointing arrow. Note that as object 08140 only showed an [O III]λ4363 detection with the footprint method, we use that metallicity with the 2D EW(Hβ) (pink diamond). The black dashed curve is the best fit to 12+log(O/H) vs. EW(Hβ) for values of EW(Hβ) > 100 Å from Laseter et al. (2022).
Paper: Corrections to Estimated Accretion Disk Size due to Color Correction, Disk Truncation, and Disk Wind
Authors: Andrzej A. Zdziarski, Bei You, Michał Szanecki
Figure caption: The dependencies of f col on the disk effective temperature using the formula of C02 (blue solid curve) and that of D12 (red dashed curve).
Paper: Prograde and Retrograde Gas Flow around Disk-embedded Companions: Dependence on Eccentricity, Mass, and Disk Properties
Authors: Yi-Xian Chen, Avery Bailey, James Stone, Zhaohuan Zhu
Figure caption: Flow pattern around the embedded companion similar to Figure 1. The three columns correspond to e = 0.012, 0.013, 0.014 cases for parameters h 0 = 0.01 and q  t  = 1.0. Upper/lower panels are for inviscid/viscous simulations. The flow quantities are averaged over the last 10 snapshots at the companion’s perigee passing. The results for apogee are similar and quite centrosymmetric.
Paper: Prograde and Retrograde Gas Flow around Disk-embedded Companions: Dependence on Eccentricity, Mass, and Disk Properties
Authors: Yi-Xian Chen, Avery Bailey, James Stone, Zhaohuan Zhu
Figure caption: Azimuthally averaged J 0 profiles around the embedded companion. The companion-centric distance r is plotted in logarithmic scale to offer a closer-in scrutiny compared to Figure 1. Different colors correspond to different orbital eccentricities. Solid lines plot positive (prograde) rotation whereas dashed lines plot negative (retrograde) rotation. Keplerian profiles are shown for comparison in black holes, which deviate from power laws at small r due to gravitational softening. Left/right panels show the profiles at the perigee/apogee.
Paper: Prograde and Retrograde Gas Flow around Disk-embedded Companions: Dependence on Eccentricity, Mass, and Disk Properties
Authors: Yi-Xian Chen, Avery Bailey, James Stone, Zhaohuan Zhu
Figure caption: Similar to Figure 3, only the e  t  scalings are normalized by h 0. Dotted black line shows the analytical prescription from Equation (12) with parameter λ = 1.3.