adsabs/AstroCLIMB huggingface dataset:
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of CH3CCH for different values of the CH2CCH + H rate constant. The dashed lines are networks where this rate constant has been modified by the factors in the legend. The base network (presented in this paper) is shown for comparison as a solid line, as well as a network where this reaction is removed entirely. The color gradient corresponds with the magnitude of the factor of change. The dotted line represents the observed column density in TMC-1, with the shaded area signifying an error of 1σ.
Paper: Kinematics and Collimation of the Two-sided Jets in NGC 4261: VLBI Study on Subparsec Scales
Authors: Xi Yan, Ru-Sen Lu, Wu Jiang, Thomas P. Krichbaum, Zhi-Qiang Shen
Figure caption: Top: the radial intensity profiles of the jet (green) and counterjet (blue) are shown, along with their corresponding brightness ratio R (red). The brightness ratio within the shaded area was used to constrain the jet viewing angle. Bottom: the allowed range of the viewing angle and intrinsic velocity of NGC 4261 jet.
Paper: Kinematics and Collimation of the Two-sided Jets in NGC 4261: VLBI Study on Subparsec Scales
Authors: Xi Yan, Ru-Sen Lu, Wu Jiang, Thomas P. Krichbaum, Zhi-Qiang Shen
Figure caption: Self-calibrated images of the NGC 4261 jet obtained from VLBA observations at 43, 44, and 88 GHz. The synthesized beam is shown at the bottom left corner of each image. Contours start at 3 times the rms value and increase by a factor of ﹩\sqrt{2}﹩.
Paper: Kinematics and Collimation of the Two-sided Jets in NGC 4261: VLBI Study on Subparsec Scales
Authors: Xi Yan, Ru-Sen Lu, Wu Jiang, Thomas P. Krichbaum, Zhi-Qiang Shen
Figure caption: Radial distance from the core vs. time for the cross-identified components.
Paper: Kinematics and Collimation of the Two-sided Jets in NGC 4261: VLBI Study on Subparsec Scales
Authors: Xi Yan, Ru-Sen Lu, Wu Jiang, Thomas P. Krichbaum, Zhi-Qiang Shen
Figure caption: Top: power-law fit of the jet width vs. de-projected distance (assuming a viewing angle of 63°) from the core using data at 15, 43, 44, and 88 GHz. Bottom: same as the top panel but including the 1, 2, 5, 8, and 22 GHz data. The black solid line represents the radial width profile fit from Nakahara et al. (2018). The vertical dashed line indicates the location of the structural transition. The black and gray areas represent the size of the event horizon surface for black holes with maximum spin and no spin, respectively.
Paper: Kinematics and Collimation of the Two-sided Jets in NGC 4261: VLBI Study on Subparsec Scales
Authors: Xi Yan, Ru-Sen Lu, Wu Jiang, Thomas P. Krichbaum, Zhi-Qiang Shen
Figure caption: Images of NGC 4261 at 15 GHz. These images are centered on the bright core position. The fitted circular Gaussian components are represented by dark violet circles superimposed on the contours. The cross-identified components are labeled at the bottom. The dark violet lines depict the best-fit line of proper motion. The slate gray filled ellipses on the left indicate the synthesized beam for each image. Contours begin at 3 times the rms value and increase by a factor of ﹩\sqrt{2}﹩.
Paper: GRB 221009A with an Unconventional Precursor: A Typical Two-stage Collapsar Scenario?
Authors: Xin-Ying Song, Shuang-Nan Zhang
Figure caption: A scenario for the “two-stage” model of precursors.
Paper: GRB 221009A with an Unconventional Precursor: A Typical Two-stage Collapsar Scenario?
Authors: Xin-Ying Song, Shuang-Nan Zhang
Figure caption: The relation between Γb and L j in Equation (2) in red dotted lines of different L iso. The violet shadow denotes the possible Γb − L j only with Constraint (1) if t b ≲ 10 s. The dark blue shadow denotes the region of possible Γb and L j.
Paper: GRB 221009A with an Unconventional Precursor: A Typical Two-stage Collapsar Scenario?
Authors: Xin-Ying Song, Shuang-Nan Zhang
Figure caption: The light curves of Na I 7, 8, and BGO 0 from T 0 − 1100 s to T 0 + 2500 s and nearby orbits in different energy bands.
Paper: GRB 221009A with an Unconventional Precursor: A Typical Two-stage Collapsar Scenario?
Authors: Xin-Ying Song, Shuang-Nan Zhang
Figure caption: The light curves of BGO, Na I 7, and Na I 8 from T 0 − 1100 s to T 0 + 2500 s and nearby orbits.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Our LRG sample compared with the COS-Halos sample. Left panel: color u − r vs. absolute r-magnitude, for our LRGs with (red squares) and without (red diamonds) Mg II. COS-Halos are shown as blue circles. Right panel: impact parameter scaled to the virial radius vs. stellar mass for our LRGs with (red squares) and without (red diamonds) Mg II. For reference, we also show the COS-Halos galaxies (blue circles) and the LRG samples from Chen et al. (2018) and Berg et al. (2019; orange triangles).
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Our LRG sample compared against subsets of the overall LRG population. Left panel: QSO NUV magnitude vs. impact parameter for QSO–LRG pairs with bright (in GALEX NUV and FUV bands) background QSOs. Marked are our QSO–LRGs with (red squares) and without Mg II (red diamonds), and QSO–LRGs pairs with (orange circles) and without Mg II (open gray circles) in the overall LRGs population. Larger symbols correspond to QSOs brighter in FUV. Right panel: EW(Mg II) vs. impact parameter, for the SDSS data. The measurements are provided by Huang et al. (2016). Marked are our LRGs with Mg II (red squares). The blue dashed line shows the average EW(Mg II), when it is detected.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: CGM of LRGs traced by EW(H I 1215) as a function of impact parameter. Data points that lie below the y-axes limits are shown as upper limits at a fixed value of EW =10−1Å. We note that there is no clear decrease of LRG–CGM EW(H I 1215) with increasing impact parameter.
Paper: GRB 221009A with an Unconventional Precursor: A Typical Two-stage Collapsar Scenario?
Authors: Xin-Ying Song, Shuang-Nan Zhang
Figure caption: (a) The light curve and BG shape from the data of Na I 8. (b) The BG-subtracted light curves in different energy bands of Na I 8. (c) The light curve from T 0 to T 0 + 200 s. (d) The spectrum of the first pulse. (e) The light curves from the GBM Na I 8 detector and HXMT, α, and E p values of the precursor. (f) The spectrum of T 0 + 50 s to T 0 + 115 s. (g) The spectrum of T 0 + 115 s to T 0 + 172 s.
Paper: Toward Interpreting the IBEX Ribbon with Mirror Diffusion in Interstellar Turbulent Magnetic Fields
Authors: Siyao Xu, 思遥 徐, Hui Li, 晖 李
Figure caption: The rate of mirroring Γ m  by the interstellar mean magnetic field and the rate of scattering Γsc by the turbulent magnetic fluctuations in the outer heliosheath for keV protons. The turbulence parameters are adopted (see text) to reach an approximate balance between Γ m  and Γsc. For the magnetic mirroring to be effective, the turbulence parameters should satisfy Γ m  > Γsc.
Paper: Toward Interpreting the IBEX Ribbon with Mirror Diffusion in Interstellar Turbulent Magnetic Fields
Authors: Siyao Xu, 思遥 徐, Hui Li, 晖 李
Figure caption: The rate of mirroring Γtm (Equations (16) and (20)) and the rate of scattering Γsc (Equations (6) and (7)) by the turbulent magnetic fluctuations in the outer heliosheath for keV protons. The same parameters as in Figure 1 are used, except for δ B  f /B 0 values. The vertical dashed lines denote μ  c .
Paper: Toward Interpreting the IBEX Ribbon with Mirror Diffusion in Interstellar Turbulent Magnetic Fields
Authors: Siyao Xu, 思遥 徐, Hui Li, 晖 李
Figure caption: Illustration for the ribbon width. The shaded regions, after projection along the line of sight, correspond to the ENA flux distribution transverse to the ribbon structure in the sky. The width W corresponds to the region in the outer heliosheath where pickup ions undergo the slow mirror diffusion in interstellar turbulent magnetic fields. The misalignment between red and green shaded regions shows the additional broadening of the ribbon ΔW due to the field line wandering caused by Alfvénic modes over a radial distance ∼λ.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of (a) CH2CCH, (b) CH3CCH, and (c) CH2CCH2 for different initial abundances of elemental oxygen. The solid line indicates the base model with a C/O ratio of 1.1, while the dashed lines indicate models with variations in C/O ratio. The color gradient corresponds with the magnitude of the C/O ratio. The dotted line represents the observed column density in TMC-1, with the shaded area signifying an error of 1σ.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: (a) The gradient from a least-squares linear fit, γ, of the magnetic spectral index, α B, against absolute cross helicity, ∣σ c∣, for sets of intervals binned by heliocentric distance, r. (b) γ of α B against r for sets of intervals binned by ∣σ c∣. (c) γ of α B against absolute residual energy, ∣σ r∣, for sets of intervals binned by r. (d) γ of α B against r for sets of intervals binned by ∣σ r∣. The 95% confidence intervals for each γ are marked. In each case a dashed line marks γ = 0 to illustrate the statistical significance, or lack thereof, of each γ. The data points for bins containing fewer than 10 intervals are not shown.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: (a) The dependence of the nonlinear time, τ nl, on heliocentric distance, r. (b) The dependence of the turbulence age, A t, on r with the age calculated using Equation (8). (c) The mean spectral index, α B, for intervals binned by A t with associated standard errors. (d) The gradient from a least-squares linear fit, γ, of α B against A t for sets of intervals binned by r with 95% confidence intervals.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: The dependence of the residual energy, σ r, on the cross helicity, σ c. The circle marks ﹩{\sigma }_{{\rm{c}}}^{2}+{\sigma }_{{\rm{r}}}^{2}=1﹩. Note that a positive σ c does not always correspond to an excess of energy in the Elsässer variable propagating away from the Sun, as the direction of  B  has not been altered in the calculation of σ c to ensure this.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: (a) The gradient from a least-squares linear fit, γ, of the spectral index, α B, against absolute cross helicity, ∣σ c∣, for sets of intervals binned by absolute residual energy, ∣σ r∣. (b) γ of α B against ∣σ r∣ for sets of intervals binned by ∣σ c∣. The 95% confidence intervals for each γ are marked. The data points for bins containing fewer than 10 intervals are not shown.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: (a) The absolute cross helicity,∣σ c∣, dependence and (b) the absolute residual energy,∣σ r∣, dependence on heliocentric distance, r. (c) The mean magnetic spectral index, α B, for intervals binned by ∣σ c∣ with associated standard errors. The dashed lines mark α B values of −3/2 and −5/3. (d) The equivalent for ∣σ r∣ bins.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: The trace magnetic field spectral index, α B, of 6 hr PSP intervals against the heliocentric distance, r, with α B calculated in the frequency range 10−2 Hz < f sc < 10−1 Hz. The red line is a 75-point running mean. The dashed lines mark the spectral index values commonly predicted from theory, −3/2 and −5/3.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: Example smoothed, 6 hr magnetic field power spectra, E, colored by the heliocentric distance, r, of the intervals the spectra are calculated from. The solid black lines mark slopes corresponding to spectral index values of −3/2 and −5/3.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of propargyl radical (green), methylacetylene (red), and allene (purple) as a function of time. The dotted lines represent the observed column densities in TMC-1, with the shaded areas signifying an error of 1σ. The dashed lines represent modeled abundances obtained from GOTHAM DR1, and the solid lines are the modeled abundances with the updated model presented in this work.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Reaction rates for key CH3CCH formation pathways as a function of time. Each color represents a different reaction, with the reactants given in the legend (“s-” denotes a grain species, and “CRP” denotes a cosmic-ray-induced photon). For more information on these reactions, including product channels, refer to Tables 4–8 in the appendices.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Reaction rates for key CH2CCH formation pathways as a function of time. Each color represents a different reaction, with the reactants given in the legend (“s-” denotes a grain species). For more information on these reactions, including product channels, refer to Tables 4–8 in the appendices.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of propargyl cyanide (blue), methylcyanoacetylene (yellow), and cyanoallene (brown) as a function of time. The dotted lines represent the observed column densities in TMC-1, with the shaded areas signifying an error of 1σ. The dashed lines represent modeled abundances from GOTHAM DR1, and the solid lines are the modeled abundances with the updated model presented in this work.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Reaction rates for key CH2CCH2 formation pathways as a function of time. Each color represents a different reaction, with the reactants given in the legend (“s-” denotes a grain species). For more information on these reactions, including product channels, refer to Tables 4–8 in the appendices.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Resonance structures of CH2CCH.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Chemical structures of the three isomers of C4H3N that have been detected in TMC-1: methylcyanoacetylene (left), cyanoallene (middle), and propargyl cyanide (right).
Paper: GTC Follow-up Observations of Very Metal-poor Star Candidates from DESI
Authors: Carlos Allende Prieto, David S. Aguado, Jonay I. González Hernández, Rafael Rebolo, Joan Najita, Christopher J. Manser, Constance Rockosi, Zachary Slepian, Mar Mezcua, Monica Valluri, Rana Ezzeddine, Sergey E. Koposov, Andrew P. Cooper, Arjun Dey, Boris T. Gänsicke, Ting S. Li, Katia Cunha, Siwei Zou, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Shaun Cole, Sarah Eftekharzadeh, Kevin Fanning, Jaime Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Pascale Jablonka, Robert Kehoe, Theodore Kisner, Martin Landriau, Axel de la Macorra, Aaron Meisner, Ramón Miquel, John Moustakas, Jundan Nie, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Eusebio Sánchez, Michael Schubnell, Ray Sharples, Malgorzata Siudek, Verne V. Smith, Gregory Tarlé, Fiorenzo Vincenzo, Benjamin Alan Weaver, Zhimin Zhou, Hu Zou
Figure caption: The DESI spectra of three of the candidates in our sample (blue lines) and the best fits (red) from the RVS pipeline. Two of the targets have been observed more than once, under different conditions or target selection schemes. The numerical DESI target identifications are indicated, as well as the survey (sv1 and sv3 stand for the first and third phases of the Survey Validation), observing conditions or program (bright/dark sky), and healpix number (Górski et al. 1999). All the data shown in this figure, and all the other figures of the paper, are available from the Zenodo repository at doi:10.5281/zenodo.8020840 (Version 2).
Paper: GTC Follow-up Observations of Very Metal-poor Star Candidates from DESI
Authors: Carlos Allende Prieto, David S. Aguado, Jonay I. González Hernández, Rafael Rebolo, Joan Najita, Christopher J. Manser, Constance Rockosi, Zachary Slepian, Mar Mezcua, Monica Valluri, Rana Ezzeddine, Sergey E. Koposov, Andrew P. Cooper, Arjun Dey, Boris T. Gänsicke, Ting S. Li, Katia Cunha, Siwei Zou, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Shaun Cole, Sarah Eftekharzadeh, Kevin Fanning, Jaime Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Pascale Jablonka, Robert Kehoe, Theodore Kisner, Martin Landriau, Axel de la Macorra, Aaron Meisner, Ramón Miquel, John Moustakas, Jundan Nie, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Eusebio Sánchez, Michael Schubnell, Ray Sharples, Malgorzata Siudek, Verne V. Smith, Gregory Tarlé, Fiorenzo Vincenzo, Benjamin Alan Weaver, Zhimin Zhou, Hu Zou
Figure caption: OSIRIS/GTC spectra (3750–4500 Å) of our stellar sample (black lines) and the best fits calculated with FERRE, color-coded by T eff (the bluer the hotter) and sorted by decreasing [Fe/H]. The Balmer lines (yellow) and main metallic absorptions (purple) are highlighted. Above each spectrum the metallicity, effective temperature, and carbon ratios are displayed. We also show the OSIRIS spectrum of SDSS J1313–0019 for comparison.
Paper: GTC Follow-up Observations of Very Metal-poor Star Candidates from DESI
Authors: Carlos Allende Prieto, David S. Aguado, Jonay I. González Hernández, Rafael Rebolo, Joan Najita, Christopher J. Manser, Constance Rockosi, Zachary Slepian, Mar Mezcua, Monica Valluri, Rana Ezzeddine, Sergey E. Koposov, Andrew P. Cooper, Arjun Dey, Boris T. Gänsicke, Ting S. Li, Katia Cunha, Siwei Zou, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Shaun Cole, Sarah Eftekharzadeh, Kevin Fanning, Jaime Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Pascale Jablonka, Robert Kehoe, Theodore Kisner, Martin Landriau, Axel de la Macorra, Aaron Meisner, Ramón Miquel, John Moustakas, Jundan Nie, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Eusebio Sánchez, Michael Schubnell, Ray Sharples, Malgorzata Siudek, Verne V. Smith, Gregory Tarlé, Fiorenzo Vincenzo, Benjamin Alan Weaver, Zhimin Zhou, Hu Zou
Figure caption: Carbon-to-iron ratio vs. iron abundance in the 10 stars from our sample (red stars) together with metal-poor stars with carbon abundances from the JINA database (blue circles; Abohalima & Frebel 2018). We also include the 14 stars already known in the [Fe/H] < −4.5 regime (Christlieb et al. 2004; Frebel et al. 2005; Norris et al. 2007; Caffau et al. 2011, 2016; Hansen et al. 2014; Keller et al. 2014; Allende Prieto et al. 2015b; Bonifacio et al. 2015; Aguado et al. 2018a, 2018b, 2019a; Nordlander et al. 2019; González Hernández et al. 2020). The fraction of carbon-enhanced metal-poor stars (CEMPs) in each regime are also shown.
Paper: GTC Follow-up Observations of Very Metal-poor Star Candidates from DESI
Authors: Carlos Allende Prieto, David S. Aguado, Jonay I. González Hernández, Rafael Rebolo, Joan Najita, Christopher J. Manser, Constance Rockosi, Zachary Slepian, Mar Mezcua, Monica Valluri, Rana Ezzeddine, Sergey E. Koposov, Andrew P. Cooper, Arjun Dey, Boris T. Gänsicke, Ting S. Li, Katia Cunha, Siwei Zou, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Shaun Cole, Sarah Eftekharzadeh, Kevin Fanning, Jaime Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Pascale Jablonka, Robert Kehoe, Theodore Kisner, Martin Landriau, Axel de la Macorra, Aaron Meisner, Ramón Miquel, John Moustakas, Jundan Nie, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Eusebio Sánchez, Michael Schubnell, Ray Sharples, Malgorzata Siudek, Verne V. Smith, Gregory Tarlé, Fiorenzo Vincenzo, Benjamin Alan Weaver, Zhimin Zhou, Hu Zou
Figure caption: The continuum-normalized spectra of the same stars as in Figure 1 (blue lines) and the best fits (red) from the SP pipeline, limited in this case to the 375–450 nm region.
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Mutual relation between the dust opacity in the V band (A  V ) and the slopes of the attenuation curve in the optical (A  B /A  V ; left) and NUV (A  w 2 /A  w 1 ; middle), with the mutual relation between A  B /A  V  and A  w 2 /A  w 1  shown in the right panel. The black line shows the median values of the results obtained from individual pixels, with gray shaded regions indicating 1σ and 2σ scatters of the data points. The stars are the results from the 1Re  stacks of each galaxy, with color codes showing the total stellar mass of the galaxy (from NSA). In the left and middle panels, the slopes for the Milky Way and Calzetti curves are indicated by blue and red dashed lines, while in the right panel, they are marked as blue and red dots, respectively.
Paper: Mapping Dust Attenuation and the 2175 Å Bump at Kiloparsec Scales in Nearby Galaxies
Authors: Shuang Zhou, Cheng Li, Niu Li, Houjun Mo, Renbin Yan, Michael Eracleous, Mallory Molina, Caryl Gronwall, Nikhil Ajgaonkar, Zhuo Cheng, Ruonan Guo
Figure caption: Attenuation caused by the 2175 Å bump (A bump; top) and normalized bump strength (B; bottom) in our sample as a function of A  V  (left) and the slopes of the attenuation curve in the optical (A  B /A  V ; middle) and NUV (A  w 2 /A  w 1 ; right). The black line shows the median values of the results obtained from individual pixels, with gray shaded regions indicating 1σ and 2σ scatters of the data points. The stars are the results from the 1Re  stacks of each galaxy, with color codes showing the total stellar mass of the galaxy (from NSA). In the panels from left to right, colored triangles/lines show the results of subsamples of spaxels selected by A  V  (left), b/a (middle), and galactocentric distance (right). Values for the Milky Way and Calzetti dust curve are indicated in red and blue, respectively.