adsabs/AstroCLIMB huggingface dataset:
Paper: Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae
Authors: Tin Long Sunny Wong, Lars Bildsten
Figure caption: Fractional mass loss of the donor, ﹩{\rm{\Delta }}{M}_{\star }/{M}_{\star }^{i}﹩, as a function of the ratio between ejecta ram pressure and initial donor central pressure, ﹩{P}_{{\rm{ej}}}/{P}_{{\rm{c}}}^{i}﹩ (left), and ratio between ejecta ram pressure and initial donor volume-averaged pressure, ﹩{P}_{{\rm{ej}}}/{P}_{{\rm{avg}}}^{i}﹩ (right). The left panel includes models from this work (pink stars) and T. L. S. Wong et al. (2024, gray diamonds; Γ = 5/3). Roche lobe filling donors with lower ﹩{M}_{\star }^{i}﹩ are toward the right. In the right panel, we include the main-sequence models from E. Marietta et al. (2000, their HCV model; yellow squares), the n = 1.5 (blue circles) and n = 3 (orange crosses) polytrope models from R. Hirai et al. (2018), our n = 3 polytrope models (purple plus signs), and our fitted power-law relation (gray dashed line; Equation (2)) in the right panel. The scatter in the data spans a factor of ≈3.
Paper: Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae
Authors: Tin Long Sunny Wong, Lars Bildsten
Figure caption: Time evolution of the density (left) and temperature (right) at the midplane for the ﹩{M}_{\star }^{i}=0.08\,{M}_{\odot }﹩, ﹩{s}_{{\rm{c}}}^{i}=3.9\,{N}_{{\rm{A}}}{k}_{{\rm{B}}}﹩ simulation. Time stamps in the left column give the time since explosion. The insets in the top row show zoomed-in views around the donor. In the first row, the outer edge of the ejecta consists of swept-up, shocked floor material, which is unimportant to the ejecta–companion interaction.
Paper: Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae
Authors: Tin Long Sunny Wong, Lars Bildsten
Figure caption: Velocity distribution of donor mass loss (top), total donor mass loss above a given velocity (middle), and the fraction of mixed donor mass loss above a given velocity (bottom), for selected models. Dotted lines show the escape velocity of the unperturbed donor.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Comparison between the CIGALE-estimated ages of the optical YSC population in NGC 4449 (see Section 2.3) and the age estimates from the LEGUS survey (B. C. Whitmore et al. 2020). In the left panel, LEGUS ages are derived using only broadband filters, while in the right panel, the Hα recombination line is included. The color bar indicates the Hα morphology (from 1: strong Hα emission, to 4: no Hα), as described in B. C. Whitmore et al. (2020).
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Same as the top right panel of Figure 6, but adopting radii of 4 (∼3.6 pc, left) and 6 pixels (∼5.5 pc, right) for the aperture photometry measurements.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Same as Figure 9, but with adopted metallicity Z = 0.4 Z⊙. Black and gray pentagons represent the eYSCI and optically identified YSC younger than 10 Myr and with a fitted E(B − V) < 0.1 populations in NGC 4449, respectively.
Paper: The Near Infrared Spectral Energy Distribution of Young Star Clusters in the FEAST Galaxies: Missing Ingredients at 1–5 μm
Authors: Alex Pedrini, Angela Adamo, Arjan Bik, Daniela Calzetti, Sean T. Linden, Benjamin Gregg, Varun Bajaj, Jenna E. Ryon, Anne S. M. Buckner, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey E. Johnson, Mark R. Krumholz, Drew Lapeer, Thomas S.-Y. Lai, Matteo Messa, Göran Östlin, Linn Roos, Linda J. Smith, Monica Tosi
Figure caption: Same as Figure 8, but for the YSC populations in M83 (left), NGC 628 (center), NGC 4449 (right).
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Comparisons of our SSP-based distance and extinction measurements with literature values. Upper panel: comparison of our distance moduli with RR Lyrae results from P. Nagarajan et al. (2022, filled blue triangles) and A. K. Vivas et al. (2020, orange inverted triangles). Error bars reflect only the RR Lyrae distances’ uncertainties, as we do not calculate formal uncertainties on ours. Average differences between respective distance moduli are shown as horizontal lines, and standard deviations as horizontal bars. Lower panel: comparison of our AV with values from the maps of D. J. Schlegel et al. (1998, filled blue diamonds), with RV from E. F. Schlafly & D. P. Finkbeiner (2011), and L. Delchambre et al. (2023, filled orange hexagons). As above, averages and standard deviations are marked with horizontal lines and bars.
Paper: Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae
Authors: Tin Long Sunny Wong, Lars Bildsten
Figure caption: Evolution on the H-R diagram of the shocked donors with initial masses ﹩{M}_{\star }^{i}=0.15\mbox{--}0.45\,{M}_{\odot }﹩ (left) and 0.08−0.126 M⊙ (right), starting from 102 yr. Models on the right have initial central specific entropies ﹩{s}_{{\rm{c}}}^{i}=3.9﹩ (solid lines) and 2.7 kBNA (dashed lines), and we show their final masses in the legend. For each model we label ages of 102 (pentagons), 103 (squares), 104 (upright triangles), 105 (circles), and 106 yr (downright triangles). We also show lines of constant radius (dashed) and several hypervelocity stars (black diamonds).
Paper: Mass Loss and Subsequent Thermal Evolution of Surviving Helium White Dwarfs Shocked by Thermonuclear Supernovae
Authors: Tin Long Sunny Wong, Lars Bildsten
Figure caption: Time evolution of the luminosity (left) and F555W absolute magnitude for shocked donors with initial masses ﹩{M}_{\star }^{i}=0.15\mbox{--}0.45\,{M}_{\odot }﹩. For comparison, we show the light curve of SN 2011fe from M. A. Tucker & B. J. Shappee (2024), including the 1σ and 3σ (filled triangles) nondetection limits at 11.5 yr postexplosion, and we adopt distance modulus of μ = 29.03 mag. The nondetection limit of SN 1972E (μ = 27.49 mag; A. Do et al. 2021) at 33 yr after explosion is shown as a gray open triangle.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: CMDs of all galaxies, with all photometric quality and membership cuts applied. The integrated magnitudes in each panel reflect the effective luminosity, i.e., the luminosity within HST’s field of view for each galaxy.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Application of successive culling criteria to CMDs of Hercules, with the fourth panel showing the final version of the catalog used in the remainder of this work. The stellar population signal of the galaxy remains constant throughout, whereas noise, artifacts, and contaminant populations are dramatically reduced.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: As Figure 4, but using absolute magnitudes (based on the distances and reddenings reported in Table 2) and zooming in on the few magnitudes around the oMSTO, subgiant branch, and base of the red giant branch.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Footprints of all HST observations used in this work (blue filled patches) overlaid on DSS2 imaging cutouts. Open black ellipses show the galaxy profiles at one half-light radius.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Size–magnitude relation for known Local Group dwarf galaxies within 1.5 Mpc. Filled blue points are the galaxies used in this work, and open orange circles are other local galaxies not studied here, either because they are too massive to be considered UFDs or because they lack HST imaging. Data obtained from the Local Volume Database (A. B. Pace 2024).
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Best-fit SFHs for all UFDs (blue lines) with 68% confidence intervals (light blue shaded regions). The epoch of reionization is marked with the gray vertical bands (12.87–13.33 Gyr ago in ΛCDM; Planck Collaboration et al. 2020; M. Boylan-Kolchin & D. R. Weisz 2021). Uncertainties are from random errors only, and do not include systematic uncertainties on models or on galaxy parameters such as distance and reddening.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Example foreground and background components for Hercules, shown as blue density maps with scatter plots of the CMD overlaid. The color–magnitude box we use for SFH fitting is outlined in black on each panel. In this case, the NSC (left panel) is too shallow to reach Hercules’ MSTO, so that foreground component has a weight of zero in the resulting SFH fit, and the MATCH foreground model (center panel) is used instead. However, this is not the case for all galaxies. Similarly, the background component (right panel) is negligible here, but in more distant galaxies, it carries more weight.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Average SFHs by kinematic group for our full galaxy sample (left column) and galaxies with MVeff less than −2.5 (right column), computed as simple averages (upper row) and inverse variance-weighted averages (lower row). We see significant differences in τ80 and τ90 (black dashed lines) between the long-term MW sample and the other two kinematic groups only in the weighted averages, whereas the unweighted averages show largely marginal differences.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Error on τ80 (half the width of the 68% confidence interval) against the effective V magnitude of the HST observations, ﹩{M}_{V{\rm{eff}}}={M}_{V}-2.5{\mathrm{log}}\,_{10}({f}_{\star })﹩ (left), and the number of stars within ±1 mag of the F606W oMSTO (right; 2.5 < MF606W < 4.5), colored by S/N at the F606W oMSTO. From these, we infer MVeff ≤ −2.5 or 100 oMSTO stars as the limits for which one can derive precise SFHs, with S/N as a minor secondary factor.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: As Figure 11, with the SFHs reported by E. Sacchi et al. (2021) as black lines. Again, we see generally excellent agreement with some exceptions. The two galaxies with the strongest disagreement, Tri II and Tuc II, have large error bars in our fits.
Paper: The HST Legacy Archival Uniform Reduction of Local Group Imaging (LAURELIN). I. Photometry and Star Formation Histories for 36 Ultra-faint Dwarf Galaxies
Authors: Meredith J. Durbin, Yumi Choi, Alessandro Savino, Daniel R. Weisz, Andrew E. Dolphin, Julianne J. Dalcanton, Myoungwon Jeon, Nitya Kallivayalil, Ting S. Li, Andrew B. Pace, Ekta Patel, Elena Sacchi, Evan D. Skillman, Sangmo Tony Sohn, Roeland P. van der Marel, Andrew Wetzel, Benjamin F. Williams
Figure caption: Comparison of the SFHs derived in this work (blue) with the SFHs reported by T. M. Brown et al. (2014, gray patches). We find excellent agreement in most cases, with only minor exceptions.
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: The distribution of LPV stars in the galaxies NGC 147 and NGC 185. Stars identified as LPVs from the observations of D. Lorenz et al. (2011) are highlighted in red. Among these, stars with reported mid-infrared magnitudes for each galaxy are marked in green.
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Mass-loss rate as a function of luminosity for LPV stars. Low-mass M-type AGB stars (green triangles) and intermediate-mass AGB carbon stars (red squares) are represented in the mass-loss rate vs. luminosity model using DUSTY. The DESK code outcomes for these stars are displayed as black pluses and blue crosses, respectively. If the carbon stars are assumed to be oxygen-rich instead, the results are displayed as open red squares. The diagonal dotted line indicates the mass consumption rates by the CNO cycle burning on the AGB, the vertical dashed–dotted line indicates the tip luminosity of the RGB, and the diagonal dashed line indicates the classical limit of the mass-loss rate in dust-driven winds due to single scattering (J. T. van Loon et al. 1999).
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: (Right) Bolometric correction in the i band vs. color, and (left) optical depth in the K band vs. color, for stars in NGC 147 and NGC 185. In this illustration, carbon stars are represented by red squares, while M-type stars are denoted by green triangles. The plot also illustrates the best-fit trends for oxygen LPV stars, represented by the green dashed line, and carbon LPVs, shown by the red dashed line. The parameters of the fitted curves are listed in Table 5.
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: The associations between optical depth in the K-band filter and near-infrared colors for carbon stars are represented by red squares, while empty red squares in the plot represent carbon stars that were modeled assuming an oxygen-rich atmosphere. Red circles correspond to carbon stars modeled using synthetic SED calculations. The blue crosses correspond to the results obtained from the DESK code applied to the stars found in the catalogs of A. Kang et al. (2005) and Y. J. Sohn et al. (2006).
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Mass-loss rate as a function of color. It is important to note that the observational data, represented by squares, pertain exclusively to carbon stars. In contrast, the data depicted as circles are derived from the synthetic SED calculations rather than direct observations.
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Mass-loss rate as a function of period. Green and red colors represent oxygen- and carbon-rich stars, respectively. The plot showcases the best-fit trends for oxygen LPV stars (green line) and carbon LPVs (red line). For comparison, the black line represents the results reported by E. Vassiliadis & P. R. Wood (1993). Refer to Table 4 for the fit parameters.
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Relationship between the combination of optical depth, stellar luminosity, gas-to-dust mass ratio, and mass-loss rate (as defined by Equation (2)) and the derived mass-loss rate. Red markers represent carbon-rich stars, while green markers indicate oxygen-rich stars. The dashed lines denote the 1σ deviation from the mean value.
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Spatial distribution maps of the number surface density of carbon-rich (C-type), oxygen-rich (M-type), and combined (M+C-type) stars within the galaxies NGC 147 and NGC 185, displayed individually. White arrows indicate the approximate direction toward the center of M31, while the black arrow (shown only for NGC 147) indicates the approximate direction of the tidal stream, as adapted from J. Preston et al. (2025).
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: K-band color–magnitude diagrams showing theoretical isochrones from P. Marigo et al. (2008) for an age of log(t) = 9.3 (equivalent to 2 Gyr) and metallicity Z = 0.0015. The left plots display the distribution of LPV stars, adapted from D. Lorenz et al. (2011), while the right plots represent carbon-rich stars, adapted from A. Kang et al. (2005) and Y. J. Sohn et al. (2006).
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Mass-loss rate as a function of amplitude in the i filter band. Oxygen-rich stars are represented by the color green, while carbon-rich stars are depicted in red. Amplitudes are adopted from D. Lorenz et al. (2011).
Paper: Long-period Variable Stars in NGC 147 and NGC 185. II. Their Dust Production
Authors: Hamidreza Mahani, Atefeh Javadi, Jacco Th. van Loon, Francisca Kemper, Roya Hamedani Golshan, Iain McDonald, Habib G. Khosroshahi, Hedieh Abdollahi, Sajjad Mahdizadeh
Figure caption: Grid results for four stars within the NGC 147 galaxy. The solid green line depicts the oxygen models, while the red dashed line illustrates the carbon models. Error bars represent the photometric uncertainties for each band, as provided in the original catalogs.