adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-4201: An Early M Dwarf Hosting a Massive Transiting Jupiter Stretching Theories of Core Accretion 
Authors: Megan Delamer, Shubham Kanodia, Caleb I. Cañas, Simon Müller, Ravit Helled, Andrea S. J. Lin, Jessica E. Libby-Roberts, Arvind F. Gupta, Suvrath Mahadevan, Johanna Teske, R. Paul Butler, Samuel W. Yee, Jeffrey D. Crane, Stephen Shectman, David Osip, Yuri Beletsky, Andrew Monson, Leslie Hebb, Luke C. Powers, John P. Wisniewski, Jaime A. Alvarado-Montes, Chad F. Bender, Jiayin Dong, Te Han, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Guđmundur Stefánsson, Jason T. Wright
Figure caption: The radius evolution of a planet with the same mass and equilibrium temperature as TOI-4201 b assuming different core (heavy-element) masses, following the model described in Müller & Helled (2021). The gray shaded region represents ±1σ for TOI-4201 b, a region substantially above the radius expected for a planet composed purely of H/He. As there are no indications that this is a particularly young system, we include a dashed line at 1 Gyr to suggest a lower limit on the age of the planet.
Paper: JWST Directly Images Giant Planet Candidates Around Two Metal-polluted White Dwarf Stars
Authors: Susan E. Mullally, John Debes, Misty Cracraft, Fergal Mullally, Sabrina Poulsen, Loic Albert, Katherine Thibault, William T. Reach, J. J. Hermes, Thomas Barclay, Mukremin Kilic, Elisa V. Quintana
Figure caption: Image of each star and its candidate before and after subtracting a PSF modeled from a nearby bright star. Image cutouts are 65 × 65 pixels and the flux density units are in MJy per steradian. Left: original calibrated MIRI image cutout centered on the WD. The north and east directions are specified with blue arrows. Middle: the same image after scaling and subtracting the PSF centered on the WD. The location of the removed star is shown as a blue star. Right: the MIRI image after subtracting both the WD and the candidate using the same PSF. In both cases the candidate is removed cleanly, indicating it is point source in nature. Note that the bright object north of WD 1202−232 is a galaxy.
Paper: JWST Directly Images Giant Planet Candidates Around Two Metal-polluted White Dwarf Stars
Authors: Susan E. Mullally, John Debes, Misty Cracraft, Fergal Mullally, Sabrina Poulsen, Loic Albert, Katherine Thibault, William T. Reach, J. J. Hermes, Thomas Barclay, Mukremin Kilic, Elisa V. Quintana
Figure caption: Photometric measurements for all four bands for both planet candidates (black circles) compared to low-mass planet models (squares) using the BEX (Linder et al. 2019a) and the models published by Burrows, Sudarsky, and Lunine (Burrows et al. 2003, hereafter BSL). WD 1202−232 b is shown on the left compared to models of 5.25 Gyr, and WD 2105−82 b is shown on the right compared to models at 1.6 Gyr for BEX and 1.0 Gyr for BSL (due to the available grid). While the photometry does not exactly match the models, the flux in all four bands is consistent with a giant-mass planet at the age of the WD and shows increasing flux with wavelength.
Paper: JWST Directly Images Giant Planet Candidates Around Two Metal-polluted White Dwarf Stars
Authors: Susan E. Mullally, John Debes, Misty Cracraft, Fergal Mullally, Sabrina Poulsen, Loic Albert, Katherine Thibault, William T. Reach, J. J. Hermes, Thomas Barclay, Mukremin Kilic, Elisa V. Quintana
Figure caption: Projected orbital separation vs. the age of the star the companion is orbiting for directly imaged planets less than 12  M Jup (black circles). The two WD planet candidates are presented with brown triangles. The solar system giant planets are shown as blue stars. The candidates are significantly older than all previously reported directly imaged, low-mass companions, except the Y+Y dwarf binary system (WISE J033605.05-014350.4) recently found using JWST by Calissendorff et al. (2023).
Paper: The First Robust Evidence Showing a Dark Matter Density Spike Around the Supermassive Black Hole in OJ 287
Authors: Man Ho Chan, Chak Man Lee
Figure caption: The shaded region bounded by the black lines is the total energy decay rate constrained by observations (the thick black line indicates the average value). The shaded region bounded by the red lines is the predicted energy decay rate combining the effects of GW and dynamical friction (DF) of the dark matter density spike (the thick red line indicates the average value). The green dotted line indicates the energy decay rate due to GW emission only. The blue vertical dashed line indicates the spike index γ sp = 2.333 predicted by the adiabatic SMBH growing model. Dynamical friction in a dark matter density spike with spike index ﹩{\gamma }_{\mathrm{sp}}={2.351}_{-0.045}^{+0.032}﹩ can account for the large orbital period decay rate measured by Dey et al. (2018).
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: Probability distribution of apparent ﹩v\sin i﹩, similar to Figure 3 but inferred from simulation B.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: Effects of spatial resolution on the observed intensity map and radial velocity map in mock observations. From the left to the right, spatial resolution increases with decreasing beam size (indicated by gray circles). The second column ((b) and (f)) uses the standard resolution of FWHM = 18 mas adopted in ALMA observations of Betelgeuse (K18), the same as shown in Figure 2. In comparison, the beam size of the first column ((a) and (e)) is increased by a factor of 2 (36 mas), whereas the beam size of the third column ((c) and (g)) is reduced by a factor of 2 (9 mas). The last column ((d) and (h)) is the same original simulation image shown in Figure 2. Physical quantities marked in white are defined the same way as in Table 1 using the method in Section 2.3.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: Probability distribution of apparent ﹩v\sin i﹩ resulting from turbulent motions above the surface of a nonrotating stellar model. The gray vertical lines indicate the observed values based on SiO and CO lines (K18), with their uncertainties indicated by the widths and the SiO line we have modeled shown darker. The blue curve illustrates the kernel-smoothed probability density function of the inferred ﹩v\sin i﹩. The 50% probability interval around the peak is shaded in gray. The orange curve shows the cumulative distribution function.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: The equatorial rotational velocity inferred for Betelgeuse (K18) is 2–3 orders of magnitude higher than single-star models predict. To illustrate this point, we show MESA predictions for the rotational velocities of massive stars (12, 15, 18, and 21 M ⊙, shown in lines with increasing color saturation) with typical initial rotation rates as a function of their fractional age, i.e., time divided by their main-sequence lifetime. The steep drop in rotation rates marks the rapid expansion as stars transition from the core H-burning phase (blue background) to the core He-burning RSGs (red background). The red box labeled “Betelgeuse” shows the measured rotational velocity of the star, where the bottom, middle, and top black lines correspond to different assumptions for the inclination with respect to the observer. See Appendix A for details.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: Examples of emission line profiles from synthetic ALMA images. Four small subplots show the simulated line profiles (blue) and fitted Gaussian (orange) in four pixels (shaded in black) of the synthetic ALMA image. In each pixel, the mean value (orange dashed vertical line) of the fitted Gaussian is taken to be the radial velocity from the Doppler shift. From the same snapshot of the simulation shown in Figure 2.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: Three interpretations of Betelgeuse’s dipolar radial velocity map observed by ALMA. The physical pictures and their observational consequences are explained in Section 4.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: Comparison of number densities from interpolated results of the precalculated FASTCHEM2table (squares) against those from MARCS (curves). The colors indicate the number densities of atomic hydrogen, electrons, CO molecules, and SiO molecules.
Paper: Is Betelgeuse Really Rotating? Synthetic ALMA Observations of Large-scale Convection in 3D Simulations of Red Supergiants
Authors: Jing-Ze Ma, 竟泽 马, Andrea Chiavassa, Selma E. de Mink, Ruggero Valli, Stephen Justham, Bernd Freytag
Figure caption: 2D middle slice of SiO number density in the simulated RSG envelope. The green circle is the radio photosphere of the star. From the same snapshot of the simulation shown in Figure 2.
Paper: Formation of Fan-spine Magnetic Topology through Flux Emergence and Subsequent Jet Production
Authors: Yadan Duan, Hui Tian, Hechao Chen, Yuandeng Shen, Zheng Sun, Zhenyong Hou, Chuan Li
Figure caption: The accumulation of helicity injection and the AIA 171 Å light curve calculated within the white box shown in Figure 1(A) from 00:59 UT to 09:00 UT. In (A), the black and red curves represent the shear and emergence terms of the magnetic helicity, respectively. The temporal evolution of AIA 171 Å flux is indicated by the blue curve. The red arrow points to the sharp increase in the injected helicity, respectively. (B) time–distance plot along the direction of the white dashed line in Figure 1(A). (C) close-up view of the red dashed box in (B).
Paper: Formation of Fan-spine Magnetic Topology through Flux Emergence and Subsequent Jet Production
Authors: Yadan Duan, Hui Tian, Hechao Chen, Yuandeng Shen, Zheng Sun, Zhenyong Hou, Chuan Li
Figure caption: Sequential images of AIA 131 Å displaying the current sheet. (A)–(B): the solid red and green dots represent the positions of the north and south magnetic null points, respectively. (E)–(F): extrapolated magnetic field lines over the magnetogram as viewed from two different perspectives. In (E) locations with log (Q) > 5 within the white box are illustrated. In (F), a 2D distribution of factor Q on a vertical slice passing through both nulls is presented.
Paper: Formation of Fan-spine Magnetic Topology through Flux Emergence and Subsequent Jet Production
Authors: Yadan Duan, Hui Tian, Hechao Chen, Yuandeng Shen, Zheng Sun, Zhenyong Hou, Chuan Li
Figure caption: The Doppler maps and spectra obtained from CHASE showing the plasma motions of the homologous jets at different times. (D)–(I) represent the line profiles of selected points in different regions, marked with cross symbols in (A)–(C). The line profiles in green and pink show excess absorptions in the red and blue wings, respectively. The dashed line represents the average Hα profile. The solid black line indicates the line profile of the inner bright patch.
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: Left: the gray lines in all panels are total light curves of Insight-HXMT/HE (0.6–3 MeV), Fermi/GBM N4 (20–900 keV), N8 (20–900 keV), B0 (0.4–45 MeV), B1 (0.4–45 MeV), and GECAM-C GRD05 (20–6000 keV) during the observation of GRB 221009A. The black light curves are the background of the parametric model (a) and the revisit orbit ((b)–(f)) after the trigger time when the satellites were almost in the same orbital locations and orientations. The red lines show the background fitted with the 4th-order polynomial. The orange shaded area in each panel marks the time windows that are confirmed as the early afterglow and are used for spectral analysis. Right: the net light curves of GRB 221009A, for which the background is estimated from the parametric model (a) and the averaged revisit orbital background ((b)–(f)).
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: During the observations of GRB 221009A afterglow, incident angles of Insight-HXMT; Fermi/GBM N4, N8; Fermi/GBM B0, B1; and GECAM-C GRD05 are shown with red lines. The dashed lines with green and blue represent the incident angle of Fermi/GBM N4, N8, B0, and B1 in the pre-revisit orbit and post-revisit orbit, respectively.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: (left) The six apertures along the jet, where we measure the extinction and jet properties, overlaid on top of the [Fe II] jet at 5.34 μm shown in gray scale. The center of aperture 3 (blue circle) marks the position of the protostar. (right) The measured extinction value along in each of the aperture as a function of their position along the jet (from the northeast to southwest).
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: Nomogram from the MAPPINGS shock model grid showing the line ratios of three [Fe II] and [Ne II] lines. The ratio of [Ne II] at 12.81 μm and [Fe II] at 5.34 μm in blue runs along the y-axis and is sensitive to the shock speed, while the ratio of [Fe II] lines at 17.93 and 5.34 μm in green that almost runs parallel to the x-axis is sensitive to the pre-shock density. The dashed green curve is the approximate position of the low-density limit to the [Fe II] flux ratio, below which this ratio is insensitive to pre-shock density. The colored regions represent the de-reddened line ratios from our observations with uncertainties. The colors correspond to those of the apertures in Figure 8. The red half-shaded circle represents aperture 1, where the northern knot is not entirely covered by the MIRI channel 1 field of view (FOV) that has the [Fe II] 5.34 μm line, resulting in overestimated flux ratios.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: The H2 rotation diagram for all apertures shown in Figure 8. Also shown are the observed points (red), the de-reddened points (blue), as well as the fit to them. The extinction value A V as well as the rotation temperatures are listed in the figure. The y-error bars on the observed (red) points are computed based on the uncertainties in the integrated flux determined by a Gaussian fit to the lines using the measured uncertainties from the IFU error cubes. The y-error bars on the de-reddened (blue) points also incorporate the error in A V from the fit.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: The H2 rotation diagram for aperture 3 (centered on the protostar) from Figure 8. Also shown are the observed points (red), the de-reddened points (blue), and a fit to these points. The extinction value A V as well as the rotation temperatures are listed in the figure. The y-error bars on the observed (red) points are computed based on the uncertainties in the integrated flux determined by a Gaussian fit to the lines using the measured uncertainties from the IFU error cubes. The y-error bars on the de-reddened (blue) points also incorporate the error in A V from the fit.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: Left: image showing the line map of the [Fe II] line at 5.34 μm for comparison to the PV diagram. The width of the image gives the range over which we averaged the jet emission. The circle shows the 14 μm MIRI continuum position of the protostar. Right: the PV diagram for the [Fe II] line at 5.34 μm. The white circles represent the center of the Gaussian fit to the velocity channels, while the error bars represent the error in determining the center of the Gaussian fit. The white bar in the top left corner is the FWHM of the JWST MIRI PSF at 5.34 μm (0″28 or 39.2 au).
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: The PV diagrams of the [Fe II] lines detected in MIRI MRS aligned to a common average velocity.
Paper: Detection of Metal Enrichment by SN 2011jm in NGC 4809
Authors: Yulong Gao, Qiusheng Gu, Ping Zhou, Yong Shi, Xiangdong Li
Figure caption: Top: pseudo-color image of 8″ × 8″ region around the SN 2011jm (red star) in dwarf galaxy NGC 4809 combined with the r-, i −, and y -band images from the HSC-SSP (left panel). Integrated-intensity map of the attenuation-corrected Hα emission (right panel). Bottom: the intensity ratio [N II]λ6583/Hα (left) and [S II]λ λ6717, 6731/Hα (right) maps. The red stars represent the SN 2011jm site.
Paper: Detection of Metal Enrichment by SN 2011jm in NGC 4809
Authors: Yulong Gao, Qiusheng Gu, Ping Zhou, Yong Shi, Xiangdong Li
Figure caption: The left panel shows the oxygen abundance (O/H) vs. the distance of pixels from the SN 2011jm site, with gray points representing values for all pixels. Distance values are grouped into seven bins, with average values denoted by black points and 1σ distributions marked by error bars. The black solid line represents the best-fitted relation between average O/H values and distances. In the right panel, a similar representation is shown for N/O ratios. The blue dashed line indicates the constant value of log(N/O) ∼ −1.43 when 12 + log(O/H) < 8.5 (Andrews & Martini 2013).
Paper: Detection of Metal Enrichment by SN 2011jm in NGC 4809
Authors: Yulong Gao, Qiusheng Gu, Ping Zhou, Yong Shi, Xiangdong Li
Figure caption: Spectra from a region with a size of r = 1.″5 around the SN 2011jm site, as observed by SDSS on 2001 April 26. The gray dashed lines indicate the absence of W-R features around ﹩4650\mathring{{\rm{A}}}﹩ (WN stars) and ﹩5808\mathring{{\rm{A}}}﹩ (WC stars).