adsabs/AstroCLIMB huggingface dataset:
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Top: frequency-dependent absorption opacity per dust mass employed for stellar irradiation. Bottom: Planck- and Rosseland-averaged absorption opacities per dust mass used to compute radiation−matter interaction terms (Equation (10)).
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Same as Figure 2, but showing color maps of the reduced flux f = ∣∣ F   r ∣∣/E  r  in log scale. Arrows indicate the direction of  F   r .
Paper: Extremely Low-mass White Dwarf Stars Observed in Gaia DR2 and LAMOST DR8
Authors: Kun Wang, 坤 王, Péter Németh, Yangping Luo, 杨平 罗, Xiaodian Chen, 孝钿 陈, Qingquan Jiang, 青权 蒋, Xingmei Cao, 星梅 曹
Figure caption: Best model-atmosphere fits to the 23 LAMOST spectra for the 21 new high-probability ELM WDs. The black and red lines are the observed and synthetic spectra, respectively. The residuals are shown as dark gray lines. The vertical blue lines mark the locations of the Ca II K (3934.8 Å), the Mg II (4481 Å), the Mg I (5167 Å), and the Na D (5895.6 Å) absorption lines. The target name and the besting-fitting atmospheric parameters are given for each spectrum.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Density (top) and irradiation power (bottom) hydrostatic distributions after 35 iterations for each f dg in the t iter = 100 yr runs.
Paper: No Self-shadowing Instability in 2D Radiation Hydrodynamical Models of Irradiated Protoplanetary Disks
Authors: Julio David Melon Fuksman, Hubert Klahr
Figure caption: Midplane temperature profiles in the hydrostatic runs between iterations 15 and 25 for each f dg.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Left panel: distance to the center of the Per-Tau Shell as a function of traceback time. The dashed and dotted lines are stellar traceback lines from Zucker et al. (2022) for IC 348 and NGC 1333, respectively. The horizontal solid line corresponds to a distance of 78 pc, the radius of the shell (Bialy et al. 2021). The circles are individual members in the remaining cloud regions, shifted horizontally with random values to avoid overlap. Right panel: the distribution of separation angles between the velocity vectors and the radial vectors (pointing from the center of the shell to the star) of individual stars. The vertical dashed line indicates a separation angle of 90°.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Left panel: infrared color–color plot for members and candidates in IC 348. The blue circles, red squares, and orange diamonds mark known members, new members, and candidate members, respectively. The black solid line is the locus of dwarfs from Pecaut & Mamajek (2013), and the dashed lines correspond to the extinction law from Wang & Chen (2019), enclosing the color space of dwarfs due to reddening. The dashed–dotted line is 0.15 mag (about 3 times the typical uncertainties in K  S  − W2 colors) redder than the right border of the dwarf locus, serving as the boundary between disk and diskless YSOs. The middle and right panels are the same as the left panel, but for NGC 1333 and the remaining cloud regions, respectively.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Left: histograms of the stellar surface densities for members in different cloud regions, i.e., IC 348 (black open histogram), NGC 1333 (hatched histogram), the remaining cloud regions (gray open histogram), and Autochthe (blue bars). Right: the same as in the left panel, but for densities including candidate members. The red bars indicate the Barnard 1 group found in Section 5.2 and marked in Figure 3, stacked on top of that for Autochthe.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Pan-STARRS1 r − i vs. r CMDs for known (blue circles) and new (red squares) members of the Perseus molecular cloud, divided into three regions, IC 348 (left), NGC 1333 (middle), and the remaining cloud regions (right). The points have been dereddened and distance corrected. In each panel, the black lines are 1, 3, 10, 30, and 100 Myr isochrones, from top to bottom, from the PARSEC stellar model (Bressan et al. 2012), with solar metallicity, and the red solid line is the best-fitting isochrone. The resulting ages are labeled.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Distance changes along the R.A. direction. The known members and the new members are marked with blue circles and red squares, respectively. The two vertical dashed lines show the locations of the two clusters. The orange-filled diamonds with error bars, connected with the solid line show the median distances in individual R.A. bins. The horizontal error bars are the corresponding R.A. ranges, the vertical error bars are the standard deviations of the median values in individual R.A. bins. The standard deviations are calculated from 10,000 realizations assuming Gaussian errors (Curran 2014).
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: H-R diagram of members identified in this work. Members with and without Hα emission lines or Li I λ 6707 Å absorption lines in their optical spectra are marked with gray circles and black pluses, respectively. The solid line is the 10 Myr isochrone and the dashed line is the stellar birth line, from the PARSEC stellar model (Bressan et al. 2012), with solar metallicity. The open diamonds and the square denote stars well below the 10 Myr isochrone and well above the stellar birth line, respectively.
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption:  H − K  S  vs. J − H CCD for the candidates in the Perseus molecular cloud. The solid line shows the intrinsic colors for main-sequence stars of K5-M6 types (Bessell & Brett 1988), and the dashed–dotted line is the locus of T Tauri stars from Meyer et al. (1997). The dashed lines are the reddening vectors from Wang & Chen (2019).
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: Histograms showing the extinction distributions for previously known members (open histogram), new members (light gray bars), and candidates (dark gray bars).
Paper: Distributed YSOs in the Perseus Molecular Cloud from the Gaia and LAMOST Surveys
Authors: Xiao-Long Wang, Min Fang, Yu Gao, Hong-Xin Zhang, Gregory J. Herczeg, Hong-Jun Ma, En Chen, Xing-Yu Zhou
Figure caption: 2D projections of 3D locations of the five groups identified by Pavlidou et al. (2021) in a heliocentric Galactic Cartesian reference frame. The two famous clusters IC 348 and NGC 1333 are also shown for comparison. Different colors correspond to different regions as indicated in the legend. The arrows are the velocity vectors of individual groups or clusters. The large circle marks the Per-Tau Shell.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Fiducial model with α t = 10−3 for both compact (sa3g) and fractal (fa3g) growth at, from left to right, 104, 105, and 5 × 105 yr. Plotted in each panel is a snapshot of the particle mass distribution as a function of semimajor axis. The color scale on the right indicates the particle solids mass volume density per bin of width Δm, m 2 f(m). The brown curves overlaying the distributions are the mass that corresponds to the mean-free path m  λ  (dotted), and estimates for the bouncing m b, fragmentation m f, and radial drift m d curve masses (above which growth times are longer than drift times, see text and Section 2.4.2) as indicated in the leftmost panels. When and where present, the dashed black curve corresponds to locations where the actual fragmentation barrier has been reached. Growth beyond the fragmentation barrier occurs to varying degrees, up to lucky particles, which are few in number and contain little mass. When the mass distribution extends beyond the fragmentation barrier, the mass-dominant particle (particle size containing most of the mass) is shown by the black solid curve. We note that in the fractal models, the m d increases very steeply to masses well beyond the plotted range. We have chosen to have a break in the curves (m f as well) so that they do not cut through the upper right label and legend. The particle size distributions for models sa3g and fa3g after 0.5 Myr can be seen in Appendix A.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Left panel: disk midplane temperature for the compact model sa3g (dashed curves) and fractal model fa3g (solid curves) at the same times given in Figure 2. Flat regions seen in some parts of the profile are EFs, which migrate inward considerably over the course of the simulation. The blue curve is a standard MMSN temperature profile (Hayashi 1981) for comparison, which beyond 10 au is steeper than our profile, which has an∼ R −3/7 dependence due to our flared disk geometry. Inside the water snowline, the mean slope of T has roughly an ∼R −1 dependence. Right panel: total solids surface density at the same times. Both compact and fractal growth models are characterized by a sharp decrease in surface density outside the snowline and beyond, as growth proceeds quickly to large particles there, which drift in. This is visible by the shift from yellow to orange color in Figure 2, for fractals at 105 yr, and for both by 5 × 105 yr. However, the fractal case retains much more material outside starting outside of ∼20 au because aggregates are increasingly more underdense. Note that in the fiducial model, the water snowline migrates inward from outside 10 to ∼4 au after 0.5 Myr. Kinks in Σsolids seen at ∼50 and ∼125 au at 0.5 Myr most notable in the compact growth case correspond to enhancements at the CO2 and CH4 EFs.
Paper: Global Modeling of Nebulae with Particle Growth, Drift, and Evaporation Fronts. II. The Influence of Porosity on Solids Evolution
Authors: Paul R. Estrada, Jeffrey N. Cuzzi, Orkan M. Umurhan
Figure caption: Evolution of the internal density ρ int = ρ p/ψ of the largest (mass-dominant) aggregate for a static MMSN model at 5 au. Perfect sticking is assumed. Models are shown in which only collisional compaction is included (dashed curve) employing the compaction formulae from Equation (37), and with both collisional and non-collisional compaction effects (solid curve) using Equations (39) and (40), and assuming α t = 10−3. In both cases, aggregates begin as monomers, which grow fractally (D ∼ 2) with decreasing internal density until either E imp ≳ E roll and/or gas ram pressure begins to compact the aggregate. When non-collisional compaction effects are included, aggregates will generally continue to compact as they grow, whereas if only collisional compaction is considered, aggregates can remain very underdense even at planetesimal masses.
Paper: The Missing Satellite Problem outside of the Local Group. II. Statistical Properties of Satellites of Milky Way–like Galaxies
Authors: Masashi Nashimoto, Masayuki Tanaka, Masashi Chiba, Kohei Hayashi, Yutaka Komiyama, Takashi Okamoto
Figure caption: Normalized cumulative angular distribution of dwarf galaxies. Solid and dashed lines represent observed dwarf galaxies divided into the secure and possible group, respectively. The black line is for all stacked galaxies, and the colored lines are for each galaxy. The dark- and light-green (yellow) shaded regions indicate the variation of the MW (M31) satellite galaxies and only those brighter than M  V  = −10 (McConnachie 2012), respectively, which take into account the projection effects (see text for details). The magenta dotted line is estimated using random points in the 3D uniform distribution.
Paper: The Missing Satellite Problem outside of the Local Group. II. Statistical Properties of Satellites of Milky Way–like Galaxies
Authors: Masashi Nashimoto, Masayuki Tanaka, Masashi Chiba, Kohei Hayashi, Yutaka Komiyama, Takashi Okamoto
Figure caption: Normalized cumulative distributions of the projected distance from each host galaxy, stacked for all galaxies (black lines), and the LG satellites around the MW and M31 (green and yellow lines; McConnachie 2012). For the MW (M31), the green (yellow) shaded region represents the variation of the number count due to projection effects (see text for details). The red and blue lines show the best-fit models of the NFW profile and Einasto profile, respectively. The solid line is for secure satellites, and the dashed line includes both secure and possible dwarfs. Note that the blue solid curve overlaps the red solid curve. The shaded region shows the predicted radial distribution with IllustrisTNG-100 (Carlsten et al. 2020).
Paper: The Missing Satellite Problem outside of the Local Group. II. Statistical Properties of Satellites of Milky Way–like Galaxies
Authors: Masashi Nashimoto, Masayuki Tanaka, Masashi Chiba, Kohei Hayashi, Yutaka Komiyama, Takashi Okamoto
Figure caption: The g − i color plotted against absolute magnitude. The red and black circles are the secure and possible satellites, respectively. The gray circles show the satellite galaxies outside the LG provided by the ELVES survey (Carlsten et al. 2021).
Paper: The Missing Satellite Problem outside of the Local Group. II. Statistical Properties of Satellites of Milky Way–like Galaxies
Authors: Masashi Nashimoto, Masayuki Tanaka, Masashi Chiba, Kohei Hayashi, Yutaka Komiyama, Takashi Okamoto
Figure caption: Effective radius vs. absolute magnitude. The dark- and light-gray circles are the secure and possible satellites, respectively. The circles indicate the satellite galaxies in the LG provided by McConnachie (2012).
Paper: The Missing Satellite Problem outside of the Local Group. II. Statistical Properties of Satellites of Milky Way–like Galaxies
Authors: Masashi Nashimoto, Masayuki Tanaka, Masashi Chiba, Kohei Hayashi, Yutaka Komiyama, Takashi Okamoto
Figure caption: Images of 93 satellite galaxies. The label on each image shows the host galaxy, the serial number of detected objects, and the confidence flag, which are the same as in Table 4. Each cutout size is 1′ × 1′.
Paper: Energy Conversion and Partition in Plasma Turbulence Driven by Magnetotail Reconnection
Authors: Xinmin Li, Rongsheng Wang, Can Huang, Quanming Lu, San Lu, J. L. Burch, Shui Wang
Figure caption: Overview of the reconnection event. (a) Electron omnidirectional spectrogram. (b) Magnetic field. (c) The ion bulk flows. (d) The electron bulk flows. (e) Electric field. (f) The magnitude of current density. (g) Energy conversion rate ( J • E ).
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: Cloud column optical depth (τ cld) posteriors for two different representative targets from our 50-target sample. The optical depth is calculated by integrating the retrieved opacity profile. The central dashed line indicates where τ cld = 1. The histograms sharply decline as we approach this value, suggesting that the data are not affected by optically thick clouds. Profiles for all 50 objects are available via the Zenodo link in Section 4.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: TP profile comparisons of the limited and full log(g) range retrievals for 2MASS-J07290002 and WISE-J032547. The restrictions in the gravity ranges influence the shapes of the thermal profiles.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: A continuation of Figure 3, showing the retrieved (red) and grid model (blue) TP profiles, overlaid with relevant condensate curves, for all the objects in our sample.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: Corner plot posteriors of 2MASS-J072290002 (the highest-gravity object) and WISE-J032547.72 (the lowest-gravity object). This is based on a test of constraining the prior ranges of the gravity for the two objects. The gravity range restrictions affect the gravity’s correlation with the other gas species. The limited log g prior results for surface gravity lean more toward the full log(g) prior results.
Paper: A Uniform Retrieval Analysis of Ultra-cool Dwarfs. IV. A Statistical Census from 50 Late-T Dwarfs
Authors: Joseph A. Zalesky, Kezman Saboi, Michael R. Line, Zhoujian Zhang, Adam C. Schneider, Michael C. Liu, William M. J. Best, Mark S. Marley
Figure caption: A continuation of Figure 2, showing the SpeX spectra (black), the best-fit spectra (blue), and the residuals (red) for all the objects in our sample.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Near-infrared J, H, and K spectrum of V1515 Cyg. Gray and red colors present the spectra observed with IRTF (Connelley & Reipurth 2018) and NOTCam, respectively. The first panel shows the full JHK spectrum, the second the J, the third the H, and then the K-band spectrum.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Spectral energy distribution of V1515 Cyg at different representative epochs. The data points are from Figure 1, as well as from space-based (IRAS, Spitzer, WISE, Herschel) and airborne (SOFIA) missions, as indicated in the legend. Solid curves show the results of our accretion disk models for the individual epochs.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Optical V-band and near-infrared K-band light curves of V1515 Cyg (upper panel), temporal evolution of the accretion rate (middle panel), and extinction toward the star (bottom panel) derived from our accretion disk modeling described in Section 4.2.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Multiple velocity components observed in V1515 Cyg in 2021 May: Na D 5889, Hα 6562, K I 7664, and Ca II 8542 Å. The dashed line indicates zero velocity, and dotted lines mark blueshifted velocity components of about −141, −65, −44, and −16 km s−1. The spectra are smoothed by 5 pixels to show line profiles clearly.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Averaged metallic absorption profiles of V1515 Cyg in 2021 May (black) and standard star (red) convolved with a rotational velocity of 15 km s−1.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Broad blueshifted absorption lines of V1515 Cyg in 2021 May: Na I D doublet (5889 and 5895 Å), Mg I 5167 and 5184 Å, and K I (7664 and 7698 Å) doublet.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Broad blueshifted absorption lines: Ba II 4934, M I 5183, Na D 5889/5895, K I 7664, and K I 7698 Å.