adsabs/AstroCLIMB huggingface dataset:
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Stellar types of merging stars for mergers following any type of triple RLOF. Gray-scale shading indicates the fraction of a particular combination of stellar types (see Hurley et al. 2000), relative to all mergers involving triple RLOF.
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Changes in the triple system between formation and the onset of triple RLOF. The top panel shows the fractional changes in a 1 and a 2 from birth until triple RLOF. The middle panel shows distributions of the inner and outer eccentricities for systems undergoing triple RLOF, i.e., their initial distributions (dotted lines), as well as their distributions at the moment of triple RLOF (solid lines). The bottom panel shows fractional changes in the three masses between birth and the beginning of triple RLOF.
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Stellar types of merging stars following triple CE evolution (within 1 Myr of the onset of triple RLOF). Gray scale indicates the fraction of a particular combination of stellar types (see Hurley et al. 2000), relative to all mergers involving triple CE.
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Distributions of the semimajor axes (top panel) and eccentricities (bottom panel) of the surviving binaries in the case that triple CE leads to a binary+single configuration (within 1 Myr). Each panel shows the initial distributions for all systems (black dotted lines), the initial distributions for all systems leading to triple CE evolution (black dashed lines), and the distributions of the new binary orbital properties (blue solid lines). In the bottom panel, the red dashed line shows a thermal distribution, ﹩{dN}/{de}=2e﹩.
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Distributions of escape speeds (relative to the initial triple center of mass) for escaping stars following (within 1 Myr of) triple CE evolution. Black solid lines show all unbound objects. Other colors and line styles indicate distributions for different types of stars.
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Fractional changes in the three masses during stable triple RLOF. Distributions for positive (negative) changes are shown with solid (dashed) lines.
Paper: A Statistical View of the Stable and Unstable Roche Lobe Overflow of a Tertiary Star onto the Inner Binary in Triple Systems
Authors: Adrian S. Hamers, Hila Glanz, Patrick Neunteufel
Figure caption: Distributions of the masses of merging (He and CO) WDs in our simulations. Top panel: primary and secondary masses; bottom panel: total mass. In both panels, the dashed lines correspond to all systems in the population synthesis simulations, whereas the solid lines correspond to those systems involving triple RLOF (both stable and unstable). The black vertical dotted lines indicate the Chandrasekhar mass, 1.44 M ⊙.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: The distribution of the observed dippers. The length of the arrows is proportional to the tangential velocities (km s−1) calculated from Gaia DR2 data. The arrow corresponding to 10 km s−1 velocity is shown at the bottom. The background picture is synthesized from images from AKARI (Takita et al. 2015).
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: Left column: TESS FFI light curves for observed targets. Middle column: the folded light curve for each object with the period corresponding to the peak of the power spectrum. The black dots represent all data, and the red line is the smoothed signal by convolving the box kernel. Right column: Lomb–Scargle periodogram of the TESS light curve. Because the dip appears only once in the light curve of TIC 34397579 and we cannot measure the periodicity, we do not show the folded light curve or its power spectrum.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: Classification of the light-curve morphology, using the definitions of Q and M defined by Cody et al. (2014). Targets of this paper are plotted with red circles compared to the K2 light curves of variable stars in Upper Scorpius and ρ Ophiuchus star-forming regions as determined by Cody & Hillenbrand (2018). Markers are scaled by the square root of the variability amplitude. The dashed lines divide the different classes suggested by Cody & Hillenbrand (2018).
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: SEDs for each target built using Virtual Observatory (VOSA). The orange lines are the best-fit theoretical model for data at wavelengths below 3.4 μm except for TIC 317873721. Because there might be a contribution from the companion star in the SED of TIC 317873721, we adopt the theoretical model with the effective temperature from the TESS input catalog as the stellar component. The blue and green lines are blackbody radiations from multiple point sources, which are fitted by using the least-squares method. Two points at 450 μm and 850 μm of the SED for TIC 434229695 are obtained from our observation with JCMT. For TIC 317873721, we show 3σ upper limits.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: JCMT 850 μm map around TIC 317873721. The position of the object is marked with a white circle, and the point sources S1–S4 identified by the pipeline are marked with black crosses. The position of IRAS 05555–1405 is marked with the cyan diamond.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: The EWs of Li and the effective temperatures (see Gaidos et al. 2019). Comparing these parameters of the dippers (plotted pink diamonds with error bars) to those of the nearby young star clusters, the ages for each target can be estimated. Because there exist fewer samples around T eff > 7000 K, we exclude TIC 457231768 (T eff = 8785 K from TICv8) from this figure.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: Observed spectrum around the Hα emission line. The vertical dashed line is at the rest wavelength (6562.8 Å). To show the line profiles clearly, observed spectra of TICs 434229695 and 317873721 are smoothed by convolving a Gaussian function. See Table 3 for observational instruments.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: Posterior distribution of the RV model (τ[day], P orb [day], K [km s−1], e, ω [radians], γ [km s−1], ln jitter). The parameter of “ln jitter” is the natural log of the σ jitter—see the text for more information.
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: The mean (solid line) and standard deviation (shaded region) of the fitted models from MCMC sampling (top), and the difference from the fitted curve (bottom).
Paper: Dippers from TESS Full-frame Images. II. Spectroscopic Characterization of Four Young Dippers
Authors: Yui Kasagi, Takayuki Kotani, Hajime Kawahara, Tomoyuki Tajiri, Takayuki Muto, Masataka Aizawa, Michiko S. Fujii, Kohei Hattori, Kento Masuda, Munetake Momose, Ryou Ohsawa, Satoshi Takita
Figure caption: Sketches based on the plausible scenarios for dippers introduced in this paper. The key properties of each target corresponding to the dimming mechanism are summarized in Table 5. (c) Because TIC 317873721 is in a close-in binary system, the circumstellar dust structures may coalesce around both stars.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Top: the F factor vs. the source size (θ  s  or θ  d ), where the solid and dashed curves represent those calculated assuming Gaussian and disk brightness distributions, respectively. Bottom: the velocity-integrated intensity ratios of the lines detected by the IRAM 30 m and ARO 12 m telescopes, after correcting for the beam dilution effect. See the text for details.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Spectra of our observations with all lines marked. The rms values are 6.6, 11.0, 10.4, and 24.7 mK after smoothing to a frequency resolution of 13.5, 10.9, 6.5, and 5.8 MHz at the rest frequency of 78.0, 96.9, 163.1, and 182.0 GHz, respectively. Newly detected transition lines are indicated in blue.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: The rotation diagrams. The filled and open cycles represent the data obtained in this work and those taken from the literature (see the text for details), respectively.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Overview of the full spectra of CRL 2688 obtained in current observations with strong lines marked.(The data used to create this figure are available.)
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Quasi-continuum of the corotating SARIs for the same parameters as for Figure 14, except that r 0 is varied to follow the radial variation of Ω0 (the dashed curve in the top panel). Every point of the black area corresponds to a quasi-discrete “eigenmode” with ∣W com∣ < c 1 ≡ 10−12, and every point of the gray area corresponds to a quasi-discrete “eigenmode” with c 1 <∣W com∣ ≤ c 2 ≡ 10−8. The labels (a)–(f) refer to the solutions presented in Figure 16.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: (a) Quasi-continuum “eigenfunction” of the corotating SARI for the same parameters as in Figure 14, i.e., ϵ ≡ B 1 = 0.045, μ 1 ≡ B  θ1/B  z1 = 10, ﹩\beta \equiv 2{p}_{1}/{B}_{1}^{2}=10﹩, δ ≡ r 2/r 1 − 1 = 1, m = 1, k = 50, σ = 0.6, but ν = 0.001. (b) Perpendicular current density perturbation ﹩{\tilde{j}}_{\perp }﹩. (c) Period-averaged perpendicular current density distribution.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Quasi-continuum “eigenfunctions” corresponding to Figure 15. Left column: fixed growth rate ν = 0.03 but varying frequency, (a) σ = 0.5, (b) σ = 0.6, (c) σ = 0.7. Right column: fixed frequency σ = 0.6 but varying growth rate, (d) ν = 0.2, (e) ν = 0.05, (f) ν = 0.005. Similar pictures of χ 2, Π1, and Π2 have been omitted; the amplitudes of Π1 are indicated in red.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: (a) Perpendicular current density perturbation ﹩{\tilde{j}}_{\perp }﹩ corresponding to the quasi-continuum “eigenfunction” shown in Figure 17, σ = 0.6, ν = 0.01. (b) The same plot blown up with a factor of 103 to focus on the currents flowing close to the singularities. (c) Period-averaged perpendicular current density distribution.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Quasi-continuum SARIs and discrete MRIs for the same equilibrium as in Figures 14–19; ϵ = 0.045, μ 1 = 10, β = 10, δ = 1. (a) Contra-rotating m = −3, −2, −1 SARIs for k/∣m∣ = 50, and m = 0 MRIs for k = 50 with n = 1, 2, …82. (b) MRIs and corotating m = 1, 2, 3 SARIs. The overlapping continua are colored green; the ranges of ﹩{{\rm{\Omega }}}_{{\rm{A}}}^{-}﹩ (red), ﹩{{\rm{\Omega }}}_{0}^{-}﹩ (gray), and ﹩{{\rm{\Omega }}}_{{\rm{A}}}^{+}﹩ (black) are indicated above the figures.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: (a) Quasi-continuum “eigenfunction” of the corotating SARI for the same parameters as in Figure 14, σ = 0.6, ν = 0.01. For clarity of the oscillations, the plots of the associated variables Π1,2 are suppressed, but their amplitudes are indicated in red. The eigenfunction is blown up (b) with a factor of 1010 to highlight the “explosion” at the singularities and (c) with a factor of 1062 to demonstrate satisfaction of the BCs at the actual boundaries.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Comparison between the observed (black) and modeled (red) column densities of the molecules in CRL 2688 (left panel) and the observed-to-modeled column density ratios of the molecules in CRL 2688 and IRC +10216 (right panel). For some molecules in IRC +10216, diverse abundances have been reported in different observations, which are denoted by open circles linked by straight lines. The vertical lines in the right panel mark the ranges within which the observed and modeled values are in agreement within one order of magnitude.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Rotation diagram of AlF, NaCN, and MgNC, for which the source sizes have been assumed to be 5″, 5″, and 30″, respectively. The measurements of AlF (triangles), NaCN (cycles), and MgNC (squares) taken by us and those by Highberger et al. (2001) are denoted by filled and open symbols, respectively.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: The modeled abundances of molecules in CRL 2688 as a function of radius. The observed abundances are denoted by squares, which are located at different radii for viewing convenience. The open and filled squares represent those within and beyond the modeling results in the radius range from 1.5 × 1016 cm to 1.5 × 1018 cm, respectively. The vertical lines show the level of disagreement between the observed and the maximum modeled abundances.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Comparison of molecular line intensities between CRL 2688 (red) and IRC +10216 (blue), which is ordered by increasing carbon atoms from top to bottom.
Paper: Molecules in the Carbon-rich Protoplanetary Nebula CRL 2688
Authors: Jian-Jie Qiu, 建杰 邱, Yong Zhang, 泳 张, Jiang-Shui Zhang, 水 张江, Jun-ichi Nakashima, 淳一 中岛
Figure caption: Column densities as a function of assumed source sizes. The measurements of AlF (triangles), NaCN (circles), and MgNC (squares) taken by us and those by Highberger et al. (2001) are denoted by filled and open symbols, respectively.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Spectral Web of the counterrotating incompressible SARIs for an accretion disk with parameters ϵ ≡ B 1 = 0.0141, μ 1 ≡ B  θ1/B  z1 = 1, ﹩\beta \equiv 2{p}_{1}/{B}_{1}^{2}=100﹩, δ ≡ r 2/r 1 − 1 = 0.1, and mode numbers m = − 10, k = 70. The radial profiles of the overlapping continua are shown above the main panel. Their real frequencies are indicated in green in the main panel. The “inner” modes cluster toward the tip of the forward Alfvén continuum ﹩\{{{\rm{\Omega }}}_{{\rm{A}}}^{+}\}﹩ at r = r 1, and the “outer” modes cluster toward the tip of the backward Alfvén continuum ﹩\{{{\rm{\Omega }}}_{{\rm{A}}}^{-}\}﹩ at r = r 2.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Spectral Web of the incompressible MRIs for an accretion disk with equilibrium parameters ϵ ≡ B 1 = 0.0141, μ 1 ≡ B  θ1/B  z1 = 1, ﹩\beta \equiv 2{p}_{1}/{B}_{1}^{2}=100﹩, δ ≡ r 2/r 1 − 1 = 1, and mode numbers m = 0 (axisymmetric!), k = 70. The top panel shows the radial profiles of the continuum frequencies and the continua themselves (in green), as well as the stable modes n = 30…126 and ﹩30^{\prime} \ldots 126^{\prime} ﹩ (skipping with Δn = 4). Note the different horizontal scale of the top panel: the continua are located far away from the 29 MRIs of the bottom panel!
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Eigenfunctions corresponding to the Spectral Web depicted in Figure 3. MRIs: (a) n = 1 (σ = − 8.288 × 10−3, ν = 0.6208); (b) n = 10 (σ = − 5.249 × 10−3, ν = 0.3810). Stable modes: (c) n = 30 (σ = 4.502 × 10−2); (d) n = 130 (σ = 0.4609). In the latter panel, the function Π has been omitted for clarity.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Cylindrical slice model (annulus r 1 ≤ r ≤ r 2 of height Δz) of an accretion disk rotating about a compact object in the origin. The dimensionless radial coordinate x ≡ r/r 1 is used for the equilibria and eigenfunctions depicted in this paper.
Paper: The Super-Alfvénic Rotational Instability in Accretion Disks about Black Holes
Authors: Hans Goedbloed, Rony Keppens
Figure caption: Radial equilibrium distributions (in black and red) for ϵ ≡ B 1 = 0.0141, μ 1 ≡ B  θ1/B  z1 = 1, ﹩\beta \equiv 2{p}_{1}/{B}_{1}^{2}=100﹩, and δ ≡ r 2/r 1 − 1 = 1, of (a) density and derivative of the gravitational potential, (b) pressure and azimuthal velocity, (c) longitudinal magnetic field and associated current density, and (d) azimuthal magnetic field and associated current density.
Paper: The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A
Authors: Aleksandra Leśniewska, M. J. Michałowski, P. Kamphuis, K. Dziadura, M. Baes, J. M. Castro Cerón, G. Gentile, J. Hjorth, L. K. Hunt, C. K. Jespersen, M. P. Koprowski, E. Le Floc'h, H. Miraghaei, A. Nicuesa Guelbenzu, D. Oszkiewicz, E. Palazzi, M. Polińska, J. Rasmussen, P. Schady, D. Watson
Figure caption: Atomic gas emission of the GRB 111005A host from GMRT with a resolution of 7.″4 × 5.″7 (black contours) overlaid on maps of physical properties derived from MUSE observations by Tanga et al. (2018). (Top left) Dust reddening E(B ‒ V). (Top right) Velocity map (first moment) based on the Hα line, with respect to the redshift z = 0.01326. (Middle left) Equivalent width of Hα. (Middle right) Star formation rate surface density derived from the Hα emission. (Bottom left) Metallicity using the diagnostic of Dopita et al. (2016). (Bottom right) Metallicity based on the O3N2 method (Pettini & Pagel 2004). The position of GRB 111005A is marked by the red arrow. The beam of H I observations is shown as a gray dotted ellipse. The image size is 2.′5 × 2.′5, corresponding to 40.5 kpc × 40.5 kpc.
Paper: The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A
Authors: Aleksandra Leśniewska, M. J. Michałowski, P. Kamphuis, K. Dziadura, M. Baes, J. M. Castro Cerón, G. Gentile, J. Hjorth, L. K. Hunt, C. K. Jespersen, M. P. Koprowski, E. Le Floc'h, H. Miraghaei, A. Nicuesa Guelbenzu, D. Oszkiewicz, E. Palazzi, M. Polińska, J. Rasmussen, P. Schady, D. Watson
Figure caption: 1.4 GHz continuum emission of the GRB 111005A host (black contours) at three different resolutions: 29.″7 × 22.″5 (top left), 8.″4 × 6.″5 (top right), and 4.″7 × 3.″2 (bottom; the beams are shown as gray dotted ellipses). The contours are 3σ, 5σ, 7σ, and 9σ, where σ = 176, 66, and 40  μJy beam−1 for low-, medium-, and high-resolution images, respectively. The background is the UV image from Michałowski et al. (2018a). The position of GRB 111005A is marked by the arrow. The image size is 2.′5 × 2.′5, corresponding to 40.5 kpc × 40.5 kpc.
Paper: The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A
Authors: Aleksandra Leśniewska, M. J. Michałowski, P. Kamphuis, K. Dziadura, M. Baes, J. M. Castro Cerón, G. Gentile, J. Hjorth, L. K. Hunt, C. K. Jespersen, M. P. Koprowski, E. Le Floc'h, H. Miraghaei, A. Nicuesa Guelbenzu, D. Oszkiewicz, E. Palazzi, M. Polińska, J. Rasmussen, P. Schady, D. Watson
Figure caption: Profiles of properties derived using the MUSE data (Figure 7) as a function of the distance from the galaxy center (red dashed line).
Paper: The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A
Authors: Aleksandra Leśniewska, M. J. Michałowski, P. Kamphuis, K. Dziadura, M. Baes, J. M. Castro Cerón, G. Gentile, J. Hjorth, L. K. Hunt, C. K. Jespersen, M. P. Koprowski, E. Le Floc'h, H. Miraghaei, A. Nicuesa Guelbenzu, D. Oszkiewicz, E. Palazzi, M. Polińska, J. Rasmussen, P. Schady, D. Watson
Figure caption: 1.4 GHz continuum emission profiles of the GRB 111005A host, using the maps with a resolution of 29.″7 × 22.″5, 8.″4 × 6.″5, and 4.″7 × 3.″2.