adsabs/AstroCLIMB huggingface dataset:
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption: Power-law fit to Mrk 841. We show the best fit (black solid line) to the data in the top panel and the ratio between model and data in the bottom panel. The gold dots and dark cyan diamonds show the data from XMM-Newton and NuSTAR, respectively. The top panel shows the result of plotting UFSPEC in the XSPEC language. The data points plotted are calculated by D*UM/FM, where D is the observed data, UM is the theoretical model integrated over the plot bin, and FM is the model times the response.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption: Scheme of reflection models used, accounting the scenarios described in Section 3.2.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption:                         Best fit to the two objects that prefer the ionized model. The description is the same as that given in Figure 4.
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Integrated CO (3–2) blueshifted and redshifted emission contours from −18.0 to 0 km s−1 and 20.0 to 28.0 km s−1, respectively. The peaks for the blueshifted and redshifted emission are 275.3 mJy beam−1 km s−1 and 191.6 mJy beam−1 km s−1. Contours begin at 10% of the peak emission and continue at increments of 10%. The continuum emission shown in background is identical to that in Figure 1. The two dashed arrows indicated the direction of the bipolar outflow from Hunter et al. (1994). The three solid arrows are from Shepherd et al. (2003). Compact sources are labeled as filled triangles. The green segments are the magnetic field from Figure 2. The dashed ellipses in magenta show the dense cores from Figure 1(b).
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Contour map of the dust emission superposed on the color image of the flux-weighted velocity map (moment 1) of the H13CO+ (4–3) line. The color scale is in units of km s−1. Red segments indicate the directions of the magnetic field. The path in white color shows the slice position on MM1 for position–velocity analysis.
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Dispersion function ﹩1-\left\langle \cos ({\rm{\Delta }}\phi )\right\rangle ﹩ for W75N using the 345 GHz SMA data. (a) Angular dispersion data (symbols) plotted as a function of distance ℓ; the dashed curve from Gaussian fitting represents contribution from the large-scale component. (b) The resulting turbulence correlation function b 2(ℓ) and its fitting curve.
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Relevant angles for magnetic field strength derivation. (a) The map of field significance Σ B . The black curves are the intensity contours as shown in Figure 1. (b) The histogram of Σ B .
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Relevant angles for magnetic field strength derivation. (a) The sin ω-map, where ω is the difference between the magnetic field and local gravity orientations. The black curves are the intensity contours as shown in Figure 1. (b) The histogram of sin ω.
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Relevant angles for magnetic field strength derivation. (a) The sin ψ-map, where ψ is the difference between the orientations of the intensity gradient and local gravity. The black curves are the intensity contours as shown in Figure 1. (b) The histogram of sin ψ.
Paper: Submillimeter Observations of Magnetic Fields in Massive Star-forming Region W75N
Authors: Lingzhen Zeng, Qizhou Zhang, Felipe O. Alves, Tao-Chung Ching, Josep M. Girart, Junhao Liu
Figure caption: Position–velocity map of the center region from the slice path shown in Figure 9. The purple ellipse shows the best fit to velocity gradient.
Paper: Lithium in Turnoff Stars in the Globular Cluster M5: A Quest for Primordial Lithium
Authors: Ann Merchant Boesgaard, Constantine P. Deliyannis
Figure caption: Color–magnitude diagram for M5 from Sandquist et al. (1996). Left: the full diagram showing their best fit to the observations. The stars we observed are shown as red stars. Right: an enlargement of the main-sequence and turnoff sections of their color–magnitude diagram with our stars as red stars. Note the faintness of our five stars and their similarity.
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Criteria for the radial collapse displayed on the plane (λ tot, β 0). The circles and cross points represent the radial collapse and stable models, respectively. The enclosed symbols correspond to models with large initial velocities (V int = 10). Color represents different line masses normalized by λ crit,B(β 0): λ tot/λ crit,B(β 0) = 1.8 (red), 1.5 (green), 1.2 (blue), and 1.0 (black). The solid line corresponds to the magnetized critical line mass (Tomisaka 2014). The dashed horizontal line represents the critical line mass of the nonmagnetized filament (Stodółkiewicz 1963; Ostriker 1964). The dashed line represents the critical line mass obtained by considering the geometric mean of the lightest line mass in the radial collapse and stable models. We also show the dimensional quantities for λ tot[M ⊙ pc−1](right) and B 0[μ G](upper), where the sound speed is 190 m s−1 at T = 10 K and the filament surface number density is n  s  = 103 cm−3.
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Same as Figure 4, but for the comparison of models with different β 0 values. Panels (a) and (b) show the maximum density evolution for the radial collapse and stable models, respectively. Color represents different plasma beta values: β 0 = 1 (red), 0.1 (blue), and 0.01 (yellow).
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: The density profiles on the x- and y-axes for the radial collapse models with varying plasma beta values (β 0) are presented in panels (a) and (b), respectively. The colored solid lines show the results of different values of β 0: β 0 = 1 (red), 0.1 (yellow), and 0.01 (blue). The black solid and dashed curves indicate the hydrostatic equilibrium solutions for the gas disk and filament, respectively.
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Same as Figure 8, but for the comparison of models with different V int values. The maximum density is plotted against the time. Panels (a) and (b) show the results for β01M and β01M_highV, and β01S and β01S_highV, respectively. Color represents the initial relative velocity as V int = 1 (red) and V int = 10 (blue). The plasma beta value is set to β 0 = 0.1.
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Same as Figure 9, but for the comparison of models β01M and β01M_highV with different initial relative velocities of V int = 1 (red) and V int = 10 (blue). Other parameters are the same: λ tot = 2.87 and β 0 = 0.1. Images are captured for the final epoch with ﹩{\rho }_{c}={\rho }_{\mathrm{lim}}=1.66\,\times \,{10}^{6}﹩.
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Density profiles on the x- and y-axes for the stable model β01S at time t = 6.500, which corresponds to the epoch after the oscillation of two cycles. The magenta-colored solid and dashed lines correspond to the density profiles on the x- and y-axes, respectively. The cyan-colored solid (ρ eq(x)) and dashed (ρ eq(y)) lines correspond to the density profiles on the x- and y-axes, respectively, for the magnetohydrostatic equilibrium state (Tomisaka 2014).
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Density profiles on the x- and y-axes for the radial collapse models (β1 M), in which β 0 = 1 and V int = 1. The ordinate denotes ϱ and the abscissa denotes x- and y-components of  χ .
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Same as Figure 7, but for a model with an initial relative velocity of V int = 10 (β01S_highV). The density profile at t = 7.10 is illustrated. The other parameters are the same as the model β01S shown in Figure 7: λ tot = 1.91 and β 0 = 0.1.
Paper: Simulation of Head-on Collisions between Filamentary Molecular Clouds Threaded by a Lateral Magnetic Field and Subsequent Evolution
Authors: Raiga Kashiwagi, Kazunari Iwasaki, Kohji Tomisaka
Figure caption: Same as Figure 7, but for the comparison of models with different β 0 values. Panels (a), (b), and (c) correspond to the models with β 0 = 1, 0.1, and 0.01, respectively.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The distribution of stars in the [Mg/Fe] vs. [Fe/H] plane as a function of R and ∣Z∣, as a contour map of point density. Spatial bins move from closest to the Galactic plane (bottom row, 0.0 <∣Z∣ < 0.5 kpc) to farthest above the Galactic plane (top row, 1.0 <∣Z∣ < 2.0 kpc), and from close to the Galactic center (left column, 0.0 <∣R∣ < 3.0 kpc) to farthest out in the disk (right column, 15.0 <∣R∣ < 25.0 kpc). The number in the top-right corner of each panel is the number of stars in our sample in that spatial bin. For reference, the gray background shape and black line are the same in each panel, to highlight how the sequence changes across location in the Galaxy. The black line is the boundary between high- and low-α populations defined in Equation (1), and the gray shape is the contour containing 90% of the points in the full sample. The typical uncertainties in abundance measurements as a function of metallicity are shown as a ±1σ value at the bottom of each panel for reference.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Global maps of the Milky Way, showing the average distribution of [Fe/H] (left), [Mg/Fe] (middle), and stellar age (right) across the Galaxy. The top row of panels shows a face-on view (X–Y plane), integrated through the disk with ∣Z∣ ≤ 1.0 kpc. The bottom row of panels shows an edge-on view (R–Z plane, with R preserving the sign of X to show the opposite side of the Galaxy), integrated through the whole disk. Colors encode the median quantities in each or X − Y or R − Z pixel. In the face-on views, the age and metallicity gradients are visible, with the Galactic bar standing out as metal-rich and α-poor. The location of the Sun at X = − 8.3 kpc is denoted by the solar symbol (⊙), and the Galactic center is marked with a plus (+). The approximate location of the Galactic bar is also shown as an ellipse with major axis length 10 kpc, a 0.4 axis ratio, and rotated 25°.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The spatial distribution of stars in our sample shown as a face-on view of the Galaxy (X–Y plane; top panel), and an edge-on view (R–Z plane; bottom panel). Each spatial bin of ΔX = ΔY = ΔZ=0.5 kpc is colored by the number of stars in that location. The position of the Sun at X = −8.3 kpc is denoted by the solar symbol (⊙), and the Galactic center is marked with a plus (+). The ellipse around the Galactic center marks the approximate location of the bar, as an ellipse with major axis length 10 kpc, a 0.4 axis ratio, and rotated 25°.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Face-on maps of the Galactic disk, showing the median metallicity ([Fe/H]) of stars in spatial bins of ΔX = ΔY = 0.5 kpc. The different panels are slices in vertical space, from closest to the Galactic plane (top panel; ∣Z∣ < 0.5 kpc) to increasing heights above the plane (bottom panel; 1 < ∣Z∣ <2 kpc). The Sun's position is marked by the solar symbol (⊙), and the position of the Galactic center is indicated by a plus (+).
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The [Mg/Fe]–[Fe/H] plane for stars in our red giant sample (black points), demonstrating the adopted definition of the low-α (blue) and high-α (red) sequence defined in Equation (1). The gray region is an added buffer zone of [Fe/H] = ±0.025 dex around the line to remove overlap between the two sequences due to abundance uncertainties. The typical uncertainties associated with each measurement of [Fe/H] and [Mg/Fe] are shown in the error bars near the bottom of the plot (as the ±1σ value), for several selected metallicities.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The reported ±1σ uncertainty in stellar age estimates from the distmass value added catalog. The light-gray histogram shows the lower uncertainty values for the sample, and the dark-gray histogram shows the upper uncertainties for the sample. The median of each distribution is plotted as a vertical line and labeled to highlight a “typical” uncertainty value.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The T eff–﹩\mathrm{log}g﹩ distribution of stars in the sample described in Section 2. Our adopted red giant sample is outlined in black and plotted by color (metallicity), while the full APOGEE sample is shown in gray in the background for reference.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Same as Figure 6, but colored by the median age (in gigayears) of stars in each spatial bins of ΔX = ΔY = 0.5 kpc.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Spectra within central 0.5 kpc (solid black line), 1 kpc (dash–dotted red line), and 2 kpc (dotted blue line) regions. The abscissa is the observed frequency in GHz, and the ordinate is flux density in mJy. (Left) J = 2–1 of HCN and HCO+. (Middle) J = 3–2 of HCN and HCO+. (Right) J = 4–3 of HCN and HCO+. The expected frequency of the HCN and HCO+ J = 2–1, J = 3–2, and J = 4–3 lines at the adopted redshift of each (U)LIRG (column (2) of Table 1; also displayed at the top of each plot) is indicated with the vertical arrow. The straight horizontal dotted thin black line indicates the zero-flux level. For LIRG NGC 1614, ≲2 kpc spectra are not extracted because no meaningful information about the molecular line emission at ≳1 kpc is obtained from our ALMA data.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption:                         Spectra within the central 0.5 kpc (solid black line), 0.5–1 kpc annular (dash–dotted red line), and 1–2 kpc annular (dotted blue line) regions, displayed in the same way as in Figure 2. The 1–2 kpc spectra of LIRG NGC 1614 are not shown for the same reason as explained in the caption to Figure 2.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Curve of growth of HCN (filled symbol) and HCO+ (open symbol) emission line flux, based on our adopted Gaussian fit (Appendix C), with increasing beam size from 0.5 kpc through 1 kpc to 2 kpc. Red square: J = 2–1. Green circle: J = 3–2. Blue triangle: J = 4–3.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Integrated-intensity (moment 0) map of HCN and HCO+ lines created from the original beam-sized data (Table 3, columns (2)–(4)) taken in ALMA Cycle 7. Simultaneously obtained continuum emission is overplotted as contours. The continuum peak position is shown as a cross. The continuum contours start from 4σ and increase by a factor of 2 (i.e., 8σ, 16σ, 32σ, and 64σ) for all sources. The length of the vertical solid white bar in the first image of each object corresponds to 1 kpc. The beam size for each moment 0 map is shown as a filled white circle in the lower left region. Coordinates are in ICRS.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: ALMA 0.88 mm (Band 7 340 GHz) continuum image of MG J0414+0434 overlaid with the HST NIR/optical (F814W+F675W) image (in contours; Falco et al. 1999). “G” is the primary lensing galaxy and “X” is an “object X,” a possible companion galaxy. The ALMA image was obtained from our ALMA Cycle 2 (project ID: 2013.1.01110.S, PI: K.T. Inoue) and Cycle 4 (project ID: 2016.1.00281.S, PI: S. Matsushita) observations. The imaging was conducted with a Briggs weighting of robust = 0.5. The synthesized beam size is 0.″051 × 0.″047 and the position angle (P.A.) is 25.°7. The rms background noise is 23 μJy beam−1.