adsabs/AstroCLIMB huggingface dataset:
Paper: Study of Advective Energy Transport in the Inflow and Outflow of Super-Eddington Accretion Flows
Authors: Cheng-Liang Jiao, 承亮 焦
Figure caption: Left panel: total torque and advection of angular momentum, normalized by GM/r. Right panel: the comparison of angular momentum per unit mass normalized by r, ﹩l/r=\sin \theta {v}_{\phi }﹩, and the rotational velocity v  ϕ , for the solution presented in Figure 1. In the left panel, the solid line represents the total torque, the dotted line represents the total advection of angular momentum, and the dashed and dotted–dashed lines represent the advection of angular momentum in the r and θ directions, respectively. Positive values of advection represent loss and negative values represent gain of angular momentum. The total torque is always negative, indicating that viscosity tends to reduce the angular momentum for a fixed region. The solid and dotted lines coincide with each other, indicating that angular momentum conservation is maintained in our steady solution. The solid gray line indicates where the function values equal 0. In the right panel, the solid line represents l/r, and the dashed line represents v  ϕ .
Paper: Study of Advective Energy Transport in the Inflow and Outflow of Super-Eddington Accretion Flows
Authors: Cheng-Liang Jiao, 承亮 焦
Figure caption: Comparison of emergent radiative fluxes. The solid line represents the emergent radiative flux in the θ direction on the surface of the accretion flow in our model, F  θs, for the solution presented in Figure 1, the dotted line represents ﹩{F}_{\theta {\rm{s}}}\sin {\theta }_{{\rm{s}}}﹩, with a factor ﹩\sin {\theta }_{{\rm{s}}}﹩ to keep the luminosity formula the same as models in cylindrical coordinates such as the slim disk, and the dashed line represents the emergent radiative flux of the slim-disk model for the mass-supply rate from the environment, ﹩{\dot{M}}_{\mathrm{supply}}﹩.
Paper: Study of Advective Energy Transport in the Inflow and Outflow of Super-Eddington Accretion Flows
Authors: Cheng-Liang Jiao, 承亮 焦
Figure caption: Components of forces in the r direction (left panel) and θ direction (right panel) for the solution presented in Figure 1. In each panel, the solid line represents the total force, the dotted line represents the radiative force (i.e., pressure gradient), the dashed line represents the centrifugal force, and the dotted–dashed line represents the gravitational force. The directions are in the typical definition of spherical coordinates (except for the gravitational force, which we present as the absolute value here), so that positive values in the r direction point outward, away from the accretor, and positive values in the θ direction point downward, away from the polar axis. Note that in spherical coordinates, the gravitational force has no component in the θ direction, while the centrifugal force has components in both the r and θ directions.
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: Total intensity contour maps of Hydra A, showing the inner tails (left) and jets at 11.1 GHz with 2.″65 resolution, and the low-brightness extended tails (right) at 1.04 GHz with 28″ resolution. The colored box in the right panel shows the extent of the left panel image. These images are from the Very Large Array (VLA) Calibrator Monitoring Program observations taken with the VLA in 2013. Left plot: the peak brightness is 0.59 Jy beam−1 and contour levels are 0.0059 × (−0.2, 0.2, 0.5, 0.75, 1, 1.5, 2, 2.5, 3, 4, 5, 7.5, 10, 15, 20, 25, 30, 40, 50, 60, 70, 80, 90) Jy beam−1. Right plot: the peak brightness is 20.1 Jy beam−1 and contour levels are 0.0201 × (−0.1, 0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.8, 1, 1.25, 1.5, 2, 3, 5, 7.5, 10, 15, 20, 25, 30, 35, 40, 50, 60, 70, 80, 90) Jy beam−1.
Paper: Study of Advective Energy Transport in the Inflow and Outflow of Super-Eddington Accretion Flows
Authors: Cheng-Liang Jiao, 承亮 焦
Figure caption: Velocity field diagram for the solution presented in Figure 1. The abscissa is ﹩x=r\sin \theta ﹩, and the ordinate is ﹩z=r\cos \theta ﹩. The arrows denote the directions of the velocity vectors in the r θ plane. The solid line represents where the radial velocity v  r  = 0 (θ = 1.03 rad), and the dashed line represents the calculation boundary of our self-similar solution (θ = 0.75 rad).
Paper: A Wideband Polarization Observation of Hydra A with the Jansky Very Large Array
Authors: Lerato Baidoo, Richard A. Perley, Jean Eilek, Oleg Smirnov, Valentina Vacca, Torsten Enßlin
Figure caption: False-color total intensity map at 2.051 GHz with 1.″5 × 1.″0 resolution, showing the inner jets and tails more clearly. This image utilizes data taken for this paper.
Paper: Ion Loss within a Reconnection Exhaust near Mars: MAVEN Observations
Authors: Xiaojun Xu, 军 徐晓, Xing Wang, 星 王, Zilu Zhou, 露 周梓, Qing Chang, 清 常, Lei Luo, 磊 罗, Peishan He, 珊 何佩, Siqi Yi, 琦 易思, Hui Li, 晖 李
Figure caption: Event overview: MAVEN observed a reconnection exhaust in the dayside magnetosheath of Mars on 2019 February 9. (a) The trajectory of MAVEN in the Y–Z MSO plane. (b) The trajectory of MAVEN in the X–R MSO plane. 19:24 UT indicates the time when the exhaust center was detected. The “[” and “]” roughly mark the boundaries of the exhaust. (c) The magnetic field strength. (d) Magnetic components in MSO coordinates. (e) Proton speed. (f) Proton velocity components in MSO coordinates. (g) Mass spectrum. (h) Energy–time plot of electrons. The altitudes, solar zenithal angles (SZAs), longitudes, and latitudes are displayed at the bottom. The black vertical dashed lines indicate the boundaries of the reconnection exhaust. The purple dashed line marks the ICB, which separates the solar wind protons from the ionospheric heavy ions. Anticorrelated/correlated variations in B and V can be seen in the red/blue boxes in Panels (d) and (f).
Paper: Ion Loss within a Reconnection Exhaust near Mars: MAVEN Observations
Authors: Xiaojun Xu, 军 徐晓, Xing Wang, 星 王, Zilu Zhou, 露 周梓, Qing Chang, 清 常, Lei Luo, 磊 罗, Peishan He, 珊 何佩, Siqi Yi, 琦 易思, Hui Li, 晖 李
Figure caption: Magnetic field and selected plasma parameters in the LMN system around the exhaust. (a)–(f) Magnetic field components and proton velocity components from MAVEN/SWIA in the LMN system. (g) Proton density. (h) Proton temperature. (i) Heavy-ion densities. (j) ﹩{{\rm{O}}}_{2}^{+}﹩ velocity components in the LMN system. The ﹩{{\rm{O}}}_{2}^{+}﹩ velocity was not in the –X MSO direction, which also indicates that the heavy ions are not simply accelerated by the draped magnetic field lines. The L, M, and N directions in MSO coordinates and the eigenvalue ratios are plotted. No obvious bipolar B  M  is detected, suggesting the absence of Hall effects. The black vertical dashed lines indicate the boundaries of the exhaust.
Paper: Ion Loss within a Reconnection Exhaust near Mars: MAVEN Observations
Authors: Xiaojun Xu, 军 徐晓, Xing Wang, 星 王, Zilu Zhou, 露 周梓, Qing Chang, 清 常, Lei Luo, 磊 罗, Peishan He, 珊 何佩, Siqi Yi, 琦 易思, Hui Li, 晖 李
Figure caption: Magnetic topology analysis around the exhaust. (a) The mass spectrum is replotted to mark the heavy-ion distributions within the exhaust. (b) The shape parameters. (d)–(f) Electron energy spectra corresponding to the most dense heavy ions within the exhaust. The absence of photoelectron peaks during 20–30 eV in both the parallel and antiparallel (to the magnetic field) directions in all three spectra suggests that the magnetic field lines associated with most of the escaped heavy ions are draped.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Left: density slices of the 2D and 3D runs for κ = 0.2 at 250 days. Their respective resolutions are 4.88 × 1012 and 9.76 × 1012 cm. The shell is at r ∼ 8 × 1015 cm in both runs. More fine structure is visible in 2D than in 3D. Right: LCs for the 3D κ = 0.2 model. The colors represent 100 LCs from ten random azimuthal angles, θ and ten polar angles, ϕ = 0°–90° in 10° increments. These LCs sample luminosity variations due to the viewing angle. The luminosity peaks at 1.9–2.1 × 1043 erg s−1 for ∼50 days and then plateaus at 2–3 × 1043 erg s−1 for ∼200 days. As in 2D, the 3D LCs do not have a second peak.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Left: angle-averaged density profiles for the 1D, 2D, and 3D κ = 0.2 runs at 250 days, each offset by a factor of 10 for clarity. The density spike in 1D splits into multiple bumps in 2D and 3D. Right: angle-averaged mass fractions and velocities for the 2D κ = 0.2 run at 135 days when the P2+P3 shell begins to form. The dark gray band shows where 12C and 16O-rich ejecta in the shell mix with 1H and 4He in the wake of P1.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: NICER 0.3–10 keV light curve during the 2021 outburst (black dots) compared with the Swift 0.3–10 keV light curve from the previous outburst in 2006 (red dots). The Swift curve was obtained from the online tool at https://www.swift.ac.uk/user_objects/ (Evans et al. 2007). We used PIMMS for the count rate comparison.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: The 1–10 keV NICER light curve is plotted in black, and the 3–10 keV light curve in red.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Comparison of 1D angle-averaged profiles of gas density, temperature, and velocity for the 2D and 3D runs with the 1D run at 50, 150, and 250 days, respectively, for κ = 0.2 at the highest resolutions. The vertical dashed yellow and green lines indicate the locations of the photosphere at 50, 150, and 250 days, respectively. There is only one yellow line because the photosphere has not moved from 50 to 150 days.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Snapshot of the 3D κ = 0.2 run at 282 days. The four quadrants show radial velocity, gas temperature, radiation flux, and gas density. The pink arrows in the radiation flux show its direction. The white dashed circle marks where the shell begins to deviate from spherical symmetry.
Paper: Multidimensional Radiation Hydrodynamics Simulations of Pulsational Pair-instability Supernovae
Authors: Ke-Jung Chen, Daniel J. Whalen, S. E. Woosley, Weiqun Zhang
Figure caption: Comparison of our 1D, 2D, and 3D LCs κ = 0.2 CASTRO runs with the highest resolutions to those of previous studies. The absence of secondary peaks in our 2D and 3D simulations highlights that multidimensional RHD simulations are required for realistic PPI SN LCs.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: The NICER light curve since optical maximum in the 0.2–10 keV range (black symbols, and red symbols for light curve in the 0.3–10 keV range from 2021 October 15 to avoid contamination from the Sun) and in the 1–10 keV range (blue symbols).
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: The enlarged integrated flux (moment-0) view of the CND for 23 molecular lines, which are obtained with high spectral resolution (synthesized beam <1″) and include the newly detected lines (see Section 3.1). The unit of the color scale is Jy beam−1 km s−1, and the minimum color levels are set to a 1σ noise level for each molecular line. The contour maps are 3σ, 6σ, and 12σ of 12CO (J = 1–0); the integrated flux indicates a typical gas distribution. Three magenta cross marks represent the positions of the E-knot, AGN, and W-knot from the left side (the coordinates are explained in the text of Section 3.2). The dual cone structure with a 30° P.A. (dashed–dotted-dash line) and 40° outer opening angle (dashed line) from the location of the supermassive black hole is represented in all images (Das et al. 2006).
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: The images of integrated flux (moment-0) for 23 molecular lines, which are clearly detected both in the CND and the SBR in NGC 1068. The unit of the color scale is Jy beam−1 km s−1, and the minimum color levels are set to 1σ noise level for each molecular line. The contour maps are 3σ and 9σ of 12CO (J = 1–0); the integrated flux indicates a typical gas distribution. The positions of the AGN (Gallimore et al. 2004) and the southwestern region in the SBR (Takano et al. 2014) are indicated using yellow cross marks.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption:                         The extracted positions of spectral data are indicated by crosses on (a) the 13CO moment-0 map for the CND and SBR, and on (b) the HCN moment-0 map for the AGN, E-, and W-knots. These coordinates are explained in Section 3.2. The contour map shows a 12CO distribution (see the captions of Figures 3 and 4 for detail). The dashed-line circles in (a) and (b) represent the convolved beam sizes of 5.″0 (∼350 pc) and 0.″9 (∼60 pc), respectively. These beams do not overlap and the samples are spatially independent.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: The spectra and Gaussian fitting curves of the first detection or the first observation with the interferometer in NGC 1068 include (a) HC18O+, (b) 29SiO, (c) HC15N, and (d) HN13C. The vertical axis is the flux density per convolved beam. The spatial resolution is 5.″0 (∼350 pc) for (a) and (d) centered at the AGN position, and 0.″9 (∼60 pc) for (b) and (c) centered at the E-knot position (coordinates are explained in the text of Section 3.2). The horizontal axes represent the velocity (V LSR; lower) and rest frequency (upper).
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Enlarged spectra with a spatial resolution of 5.″0 (∼350 pc) from 85–100 GHz in the CND (upper panel) and the SBR (lower panel). The vertical and horizontal axes are the beam-averaged flux density and rest frequency, respectively. The velocity resolution is 20 km s−1, and the primary beam correction is applied. The shaded regions refer to the range of ± 1σ noise level. The names of the molecular line carriers, which have a peak flux of more than 1σ, are indicated above the spectra.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: The obtained spectra with spatial resolution of 5.″0 (∼350 pc) from 85–114 GHz in the CND (upper panel) and the SBR (lower panel). The vertical and horizontal axes are the beam-averaged flux density and rest frequency, respectively. The velocity resolution is 20 km s−1, and the primary beam correction is applied. The names of major molecular line carriers are indicated above the spectra.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Enlarged spectra with a spatial resolution of 5.″0 (∼350 pc) from 100–114 GHz in the CND (upper panel) and the SBR (lower panel).
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Left: WISE color–color plot for the spectroscopically classified samples of galaxies (1325; red points) and QSOs (4135; blue points). Right: the galaxy sample is divided into two subsamples, normal galaxies (638; red) and XBONGs (460; cyan). Two horizontal lines are overplotted to separate AGNs and galaxies at W1–W2 = 0.8 (blue dashed) applied by Stern et al. (2012) to select AGNs above this line, and at W1–W2 = 0.4 (red dashed) applied by Kim et al. (2023) to select normal galaxies below this line. Also overplotted is the AGN selection wedge (green dashed) from Mateos et al. (2012). Many XBONGs lie outside the AGN wedge and between the two regions occupied by AGNs and galaxies.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: The X-ray luminosities of normal galaxies (red), XBONGs (cyan), and QSOs (blue) are plotted against the 20 cm radio luminosities. The blue line is the best-fit relation of QSOs, and the red line is from Richards et al. (2007) for SF galaxies with L X < 1042 erg s−1. The thin black line indicates the boundary between radio-loud and radio-quiet QSOs (Terashima & Wilson 2003). The yellow line is the best-fit relation between L X(ICM) of groups and clusters and L 20 cm(AGN) of brightest cluster galaxies from Pasini et al. (2022).
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Top: the X-ray luminosities of galaxies (red) and QSOs (blue) are plotted against (a) 2MASS K-band, (b) SDSS r-band luminosities. (bottom) The galaxies are separated into normal galaxies (red) and XBONGs (cyan). The black dashed line indicates L X from LXMBs for a given L  K  (Boroson et al. 2011).
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: HR(hm) is plotted against z for (left) XBONGs, and (right) QSOs. The lines indicate 1.7 power-law models N H = 1021, 1022, 1023, 1024 cm−2 from bottom to top.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Same as Figure 12, but showing only the XBONGs of each subclass.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Same as Figure 15, but with (a) GALEX NUV and (b) GALEX FUV luminosities. The vertical line indicates the maximum limit of normal galaxies, L NUV = 2.5 ×  1011 L ⊙.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: An example of extended XBONG candidates. Left: 2CXO J102155.7+344102 at 14′ from the aim point of a 5K observation. Right: the corresponding Chandra PSF at the same location. The vertical bar indicates 1′.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Same as Figure 12 but only with (left) unobscured XBONGs (N H < 1022 cm−2) and (right) obscured XBONGs (N H > 1022 cm−2).
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Same as the left panel of Figure 7, but (left) with only sources flagged as extended in CSC2; (right) with only sources flagged as variable in CSC2.
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Moment 1 maps of HCO+ (4–3) toward high-mass YSOs in the LMC. The angular resolution, ∼0.″39 × 0.″32, is given by the white ellipse in the lower left corner of the bottom left panel. Black plus signs represent the position of the YSOs (Seale et al. 2009). The systemic velocities (V sys) for each source are listed in Table 3. Black lines show the identified spines of the filament that we used to derive the physical properties (see the text in Section 3.2).
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Same as those in Figure 7, but for moment 2 maps.