adsabs/AstroCLIMB huggingface dataset:
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: The green line is a blackbody model, while the red line is a DA-type white dwarf of 1.0M ⊙ with T eff,WD = 12,000K.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: SuperWASP, HATNet, CCS, and ASAS-SN photometry for J1527 from 2004 May 2 to 2018 July 22. No evidence for outbursts appears in the total 5193 day time span.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: Left: H α  emission-line profiles as a function of orbital phase in the rest frame of the K9-M0 type star. Right: H α  emission-line profiles in the rest frame of the compact object.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: The best-fitting SED model for J1527 after fixing the extinction parameters A v = 0. The black curve is the best-fitting model. The green pluses and circles are the retrieved photometric measures. The blue diamonds are synthetic photometry. Here, the GALEX FUV and NUV (two green pluses) were not included in the SED fitting.
Paper: An X-Ray-dim “Isolated” Neutron Star in a Binary?
Authors: Jie Lin, Chunqian Li, Weiyang Wang, Heng Xu, Jinchen Jiang, Daoye Yang, Shahidin Yaqup, Abdusamatjan Iskanda, Shuguo Ma, Hubiao Niu, Ali Esamdin, Shuai Liu, Gavin Ramsay, Jose I. Vines, Jianrong Shi, Renxin Xu
Figure caption: Low-resolution LAMOST spectrum from 2020 January 22, showing the K9-M0 spectral type star and the clear Ca II H&K and Balmer H α  and H β  emission lines.
Paper: A Second Earth-sized Planet in the Habitable Zone of the M Dwarf, TOI-700
Authors: Emily A. Gilbert, Andrew Vanderburg, Joseph E. Rodriguez, Benjamin J. Hord, Matthew S. Clement, Thomas Barclay, Elisa V. Quintana, Joshua E. Schlieder, Stephen R. Kane, Jon M. Jenkins, Joseph D. Twicken, Michelle Kunimoto, Roland Vanderspek, Giada N. Arney, David Charbonneau, Maximilian N. Günther, Chelsea X. Huang, Giovanni Isopi, Veselin B. Kostov, Martti H. Kristiansen, David W. Latham, Franco Mallia, Eric E. Mamajek, Ismael Mireles, Samuel N. Quinn, George R. Ricker, Jack Schulte, S. Seager, Gabrielle Suissa, Joshua N. Winn, Allison Youngblood, Aldo Zapparata
Figure caption: Signal-to-noise ratio of TOI-700 e’s transit detection as a function of number of observed transits. The main panel shows matched-filter response functions of a filter shaped like TOI-700 e’s transit convolved with the TOI-700 light curve. The individual curves show the response of the light curve as additional data were collected. Curves with only a small number of transits (light pink) show a relatively weak detection of the planet’s signal, while curves with many observed transits show a convincing detection, with greater than 10σ significance. The inset shows the peak signal-to-noise ratio of the planet’s signal as a function of the number of observed transits. The purple curve is a best-fit curve with a square root power law, which describes the growth of the signal strength well, as expected for an astrophysical transit signal. The consistent growth of the signal-to-noise ratio as additional data was collected is evidence that the signal of TOI-700 e is not dominated by occasional instrumental artifacts, and instead is caused by a periodic signal with a period of 27.8 days. We note that, in the parlance of Kepler exoplanet detection literature, this type of metric is known as a “mod-shift” test.
Paper: A Second Earth-sized Planet in the Habitable Zone of the M Dwarf, TOI-700
Authors: Emily A. Gilbert, Andrew Vanderburg, Joseph E. Rodriguez, Benjamin J. Hord, Matthew S. Clement, Thomas Barclay, Elisa V. Quintana, Joshua E. Schlieder, Stephen R. Kane, Jon M. Jenkins, Joseph D. Twicken, Michelle Kunimoto, Roland Vanderspek, Giada N. Arney, David Charbonneau, Maximilian N. Günther, Chelsea X. Huang, Giovanni Isopi, Veselin B. Kostov, Martti H. Kristiansen, David W. Latham, Franco Mallia, Eric E. Mamajek, Ismael Mireles, Samuel N. Quinn, George R. Ricker, Jack Schulte, S. Seager, Gabrielle Suissa, Joshua N. Winn, Allison Youngblood, Aldo Zapparata
Figure caption: Here, we present the light curves for the TOI-700 planets, phase-folded to each of their orbital periods. The gray dots are the TESS 2 minutes cadence data, the pink dots are the data binned to 10 minutes cadence, and the purple lines show our transit fit generated using EXOFASTv2.
Paper: A Second Earth-sized Planet in the Habitable Zone of the M Dwarf, TOI-700
Authors: Emily A. Gilbert, Andrew Vanderburg, Joseph E. Rodriguez, Benjamin J. Hord, Matthew S. Clement, Thomas Barclay, Elisa V. Quintana, Joshua E. Schlieder, Stephen R. Kane, Jon M. Jenkins, Joseph D. Twicken, Michelle Kunimoto, Roland Vanderspek, Giada N. Arney, David Charbonneau, Maximilian N. Günther, Chelsea X. Huang, Giovanni Isopi, Veselin B. Kostov, Martti H. Kristiansen, David W. Latham, Franco Mallia, Eric E. Mamajek, Ismael Mireles, Samuel N. Quinn, George R. Ricker, Jack Schulte, S. Seager, Gabrielle Suissa, Joshua N. Winn, Allison Youngblood, Aldo Zapparata
Figure caption: The distribution of periods of the TCEs shows that there is no significant pileup at the period of TOI-700 e (27.8 days) in this cutaway figure. The lack of overdensity at this period implies that there is no instrumental effect inducing planet signals at the period of TOI-700 e.
Paper: A Second Earth-sized Planet in the Habitable Zone of the M Dwarf, TOI-700
Authors: Emily A. Gilbert, Andrew Vanderburg, Joseph E. Rodriguez, Benjamin J. Hord, Matthew S. Clement, Thomas Barclay, Elisa V. Quintana, Joshua E. Schlieder, Stephen R. Kane, Jon M. Jenkins, Joseph D. Twicken, Michelle Kunimoto, Roland Vanderspek, Giada N. Arney, David Charbonneau, Maximilian N. Günther, Chelsea X. Huang, Giovanni Isopi, Veselin B. Kostov, Martti H. Kristiansen, David W. Latham, Franco Mallia, Eric E. Mamajek, Ismael Mireles, Samuel N. Quinn, George R. Ricker, Jack Schulte, S. Seager, Gabrielle Suissa, Joshua N. Winn, Allison Youngblood, Aldo Zapparata
Figure caption: TOI-700 e (pink) resides in the Optimistic Habitable Zone (light green) around its host star in between the orbits of TOI-700 c and d. The Conservative Habitable Zone is shown in dark green, and planets b, c, and d (from inner to outer) are shown in indigo.
Paper: PHANGS–JWST First Results: The Influence of Stellar Clusters on Polycyclic Aromatic Hydrocarbons in Nearby Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, Sinan Deger, Oleg V. Egorov, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Eric J. Murphy, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: PAH bandpass flux ratios for the compact clusters (top) and stellar associations (bottom). The open blue squares, green triangles, and red circles are for compact stellar clusters, colored according to their ages: 0–10 Myr, 10–100 Myr, and >100 Myr, respectively. Large symbols indicate medians. Overlaid tracks are presented for select subsets of the simulated ratios, and the general trends for these tracks are indicated with the inset arrows/descriptions (see the text for details). The magenta and blue tracks are for small (a 01 = 3 Å) and large (a 01 = 5 Å) modeled PAH distributions, respectively, with both assuming logU = 0, ion=0, 1.2, and age = 10 Myr. The black hook-shaped track spans ﹩\mathrm{log}U﹩ = 0, 7 and fixes ion = 0, size = 2, and age = 10 Myr.
Paper: PHANGS–JWST First Results: The Influence of Stellar Clusters on Polycyclic Aromatic Hydrocarbons in Nearby Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, Sinan Deger, Oleg V. Egorov, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Eric J. Murphy, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Example synthetic spectra drawn from the dust models of Draine et al. (2021) and generated using the CIGALE software (see Section 3 for details). The spectra are shown for maximum differences in the chosen grid for stellar age, PAH size, and interstellar radiation field intensity. The changes in the spectra as a function of PAH ionization are less pronounced and are thus not displayed. The six different colors represent the six different example spectra, with their physical properties indicated by arrows and their descriptors.
Paper: PHANGS–JWST First Results: The Influence of Stellar Clusters on Polycyclic Aromatic Hydrocarbons in Nearby Galaxies
Authors: Daniel A. Dale, Médéric Boquien, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Yixian Cao, Rupali Chandar, Jérémy Chastenet, Mélanie Chevance, Sinan Deger, Oleg V. Egorov, Kathryn Grasha, Brent Groves, Hamid Hassani, Kiana F. Henny, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Janice C. Lee, Adam K. Leroy, Daizhong Liu, Eric J. Murphy, Erik Rosolowsky, Karin Sandstrom, Eva Schinnerer, Jessica Sutter, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: F770W imaging along with the locations of the stellar clusters. A 1 kpc scale bar is included within each panel.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Comparison of intrinsic and measured polarization phase functions, illustrating the effects of multiple scattering and limb-brightening, for two different disk locations (top row with r = 90 au and bottom row with r = 150 au) and two different material compositions (left column with highly absorbing amorphous carbon and right column with less absorbing organic carbon). In each panel, the thick dotted green line shows the intrinsic polarization phase function of FA1.9 with ﹩{N}_{\max }=512﹩ with amc 200 (left panels) and org 200 (right panels) used in the radiative transfer model. That radiative transfer model was then used to produce an image. The solid orange line shows the apparent phase function measured from the image, which differs from the intrinsic function due to multiple scattering and limb brightening. The dotted-dashed lines represent the phase functions obtained by measuring the images from a radiative transfer computation with multiple scattering switched off. The thin solid lines show the analytical estimate for ﹩{Q}_{\phi }﹩ computed from the intrinsic phase function, ignoring multiple scattering and correcting for limb brightening using Equations (C2) and (C8).
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Effect of dust disk mass on the polarized flux and the aspect ratio of the disk. The aspect ratio of each dust disk model was measured at a disk height where the optical depth measured from the star becomes unity. The blue, orange, and green lines represent the results for all fractal models with org 300 (18 models in total, see Table 2) with the dust disk mass M dust = 2 × 10−5 M ☉ (fiducial), 6 × 10−6 M ☉ and 2 × 10−6 M ☉, respectively. The dust disk mass does not include the contribution of pebble-sized grains that settle into the midplane. The black dashed line represents the results for the fiducial disk mass with FA1.5 with ﹩{N}_{\max }=256﹩ with the monomer model of amc 200 (see Section 4.2). The observed faint scattered light and large aspect ratio of the disk surface point toward a highly absorbing composition of each monomer.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Maximum degree of polarization of disk-scattered light for fractal aggregates (left) and compact aggregates (right). Each color represents the maximum polarization of aggregates with a specific monomer radius. For the left panel, the colored region shows the values of the maximum polarization for various aggregate radii, four fractal dimensions (FA1.1, FA1.3, FA1.5, FA1.9), and two monomer compositions (org and amc). For the right panel, the colored region shows the values for various aggregate radii, three porosity models (CA-HP, CA-MP, CA-LP), and two monomer compositions (org and amc). For comparison, we overlaid the observed maximum polarization of various planet-forming disks. References: HD 142527 (Hunziker et al. 2021), HD 169142 (Tschudi & Schmid 2021), HD 34700 A (Monnier et al. 2019), GG Tau (Silber et al. 2000), AB Aur (Perrin et al. 2009), UX Tau A (Tanii et al. 2012), TW Hya (Poteet et al. 2018), and HL Tau nebula region (Murakawa et al. 2008).
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Comparison of polarized scattered light of the IM Lup disk and simulated one for FA1.9 with ﹩{a}_{{\rm{c}}}^{\max }=6.5\pm 0.22\,\mu {\rm{m}}﹩ but consisting of different monomer radii and compositions. The top images show the largest aggregate in the size distribution of each model. Adopted aggregate parameters are (N max, a m) = (2048, 100 nm; dotted–dashed), (512, 200 nm; solid), (256, 300 nm; dashed), (128, 400 nm; dotted). The bottom left and right panels show the polarized flux and the polarization phase function (normalized to 90°) at the H band, respectively. Blue and yellow colors represent the amc and org composition models, respectively.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Dust particle models used to model disk-scattered light around IM Lup: FA1.1 (N = 128, a m = 100 nm), FA1.3 (N = 256, a m = 100 nm), FA1.5 (N = 512, a m = 100 nm), FA1.9 (N = 4096, a m = 100 nm), CA-HP (N = 4096, a m = 100 nm), CA-MP (N = 4096, a m = 100 nm), CA-LP (N = 4096, a m = 100 nm) and an irregular grain with a V = 1.6 μm.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Best dust models for the polarization phase function of the IM Lup disk. The top, middle, and bottom panels represent the results for irregular grains, compact aggregates, and fractal aggregates, respectively. From left to right panels, the disk-polarized flux and the polarization phase functions (normalized to a scattering angle of 90°) at the J and H bands are shown. The thick lines represent the best fit among each particle type: the best irregular grain model (﹩{a}_{{\rm{V}}}^{\max }=0.504\,\mu {\rm{m}}﹩ with amc: a reduced χ 2 = 6.8), the best compact aggregate model (CA-HP with ﹩{N}_{\max }=512﹩ and amc200: a reduced χ 2 = 5.0), the best fractal model (FA1.5 with ﹩{N}_{\max }=256﹩ and amc200: a reduced χ 2 = 3.6). Thin gray lines in each panel are models that are consistent with the disk polarization color (J/H = 0.81 ± 0.12).
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Observed polarized scattered-light image for the IM Lup disk at the H band (scaled with the square of the distance from the central star) overlaid with the extraction regions of the polarization phase function (left), the computed scattering angles at the disk surface (middle), and the extracted polarization phase functions (right). The phase functions were extracted at deprojected radii centered at 90 au, 150 au, and 237 au with the 40 au width for each.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: Comparison of the observed disk image taken by VLT/SPHERE (left) and model images at the H band without/with the phase function extraction regions (middle and right). The color scale shows the azimuthal polarization component Q  ϕ  after correcting the drop-off of stellar light with distance. The assumed dust model is FA1.5 with ﹩{N}_{\max }=256﹩ with the monomer model of amc 200, which is the best particle model derived in this study (Section 4.2).
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: The ratio of the polarization phase function extracted from model images with and without multiple scattering. The curves are normalized to a scattering angle of 90 degrees. The black and gray lines represent the results for the amc and org compositions, respectively. The solid, dashed, and dotted lines represent the results at 90 au, 150 au, and 237 au, respectively.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: A simple model to account for the effect of limb brightening on the phase function. The left cartoon summarizes the geometry of the plane-parallel atmosphere. The right panel shows the limb-brightening factor μ */(μ * + μ) for various disk aspect ratios (h s/r) and flaring indices (χ) at a disk inclination angle of 55°. The limb-brightening effect amplifies the near- and far-side brightness asymmetry of disk-scattered light.
Paper: Fractal Aggregates of Submicron-sized Grains in the Young Planet-forming Disk around IM Lup
Authors: Ryo Tazaki, Christian Ginski, Carsten Dominik
Figure caption: A cartoon of a small patch of the disk surface illustrating the effect of limb brightening on the emergent intensity. The two solid arrows escaping from the disk surface represent scattered light for the near and far sides of the disk. The background color gradient represents the attenuation of stellar radiation from the top of the surface toward the midplane. The green dashed lines represent the location where the optical depth measured from the disk surface is unity. The line of sight for the near-side scattered light is exposed to a high stellar flux for a longer distance than that of the far side, and therefore the emergent intensity is enhanced.
Paper: An Anomalous Cosmic-Ray Mediated Termination Shock: Implications for Energetic Neutral Atoms
Authors: M. Kornbleuth, M. Opher, G. P. Zank, B. B. Wang, J. Giacalone, M. Gkioulidou, K. Dialynas
Figure caption: Ion fluxes inferred from observations and derived from models. Top left: ion flux inferred from IBEX-Hi (blue dots) and INCA (red dots) observations averaged over the years 2009–2012 assuming n H = 0.12 cm−3 in the heliosheath and a heliosheath thickness of 35 au in the Voyager 2 direction (Dialynas et al. 2020). The lines correspond to best-fit model results to the hybrid model of Giacalone et al. (2021; black dots) for a two-kappa approximation of the flux (orange) and using the ZW method with δ = 9.5 (ZW9 method—turquoise) and δ = 7.5 (ZW7 method—green). Also included are relative ion contributions for the ZW7 method relative to the hybrid model for the Voyager 2 direction (top right), flank direction (bottom left), and tail direction (bottom right). In these plots, the black dots correspond to the hybrid model, and the red, blue, green, and black lines correspond to the ion fluxes from the transmitted, reflected, accelerated/reflected, and combined PUIs, respectively.
Paper: An Anomalous Cosmic-Ray Mediated Termination Shock: Implications for Energetic Neutral Atoms
Authors: M. Kornbleuth, M. Opher, G. P. Zank, B. B. Wang, J. Giacalone, M. Gkioulidou, K. Dialynas
Figure caption: Extrapolated parameters as a function of radial distance to the termination shock normalized to the Voyager 2 direction. The red dots correspond to the best-fit parameters for the ZW7 method for the Voyager 2, flank, and tail directions. From top to bottom, the left column shows the transmitted PUI density fraction relative to the plasma, the reflected PUI density fraction, the fraction of PUIs accelerated at the termination shock, and the maximum energy for reflected PUI acceleration. From top to bottom, the right column shows the transmitted PUI energy fraction relative to the plasma, the reflected PUI energy fraction, the minimum energy for reflected PUI acceleration, and the power-law index (δ) for the accelerated PUIs.
Paper: An Anomalous Cosmic-Ray Mediated Termination Shock: Implications for Energetic Neutral Atoms
Authors: M. Kornbleuth, M. Opher, G. P. Zank, B. B. Wang, J. Giacalone, M. Gkioulidou, K. Dialynas
Figure caption: ENA fluxes from the Voyager 2 direction (top left), flank direction (top right), and tail direction (bottom right). The black lines correspond to the modeled ENA flux using the ZW7 method, while the orange and blue lines correspond to the 2009–2012 averages of the IBEX-Hi (orange) and INCA (blue) observations. Bottom left: Global map showing locations of ENA sampling for the figure.
Paper: Precise Empirical Determination of Metallicity Dependence of Near-infrared Period–Luminosity Relations for RR Lyrae Variables
Authors: Anupam Bhardwaj, Marcella Marconi, Marina Rejkuba, Richard de Grijs, Harinder P. Singh, Vittorio F. Braga, Shashi Kanbur, Chow-Choong Ngeow, Vincenzo Ripepi, Giuseppe Bono, Giulia De Somma, Massimo Dall'Ora
Figure caption: Near-infrared PLZ and PWZ relations for RR Lyrae variables in GCs in the JHK  s  bands. In each case, the color-coded solid lines in the top panels correspond to [Fe/H] = [−0.5, −1.5, −2.5] dex. The solid line in the bottom panels shows the best-fitting linear regression while the dashed line displays the predicted relation from Marconi et al. (2015). The average residuals (ΔJ,  ΔH,  ΔK  s ) in a period bin of ﹩\mathrm{log}(P)=0.02﹩ days are shown for visualization purposes. The data points are color coded according to the color bar.
Paper: Precise Empirical Determination of Metallicity Dependence of Near-infrared Period–Luminosity Relations for RR Lyrae Variables
Authors: Anupam Bhardwaj, Marcella Marconi, Marina Rejkuba, Richard de Grijs, Harinder P. Singh, Vittorio F. Braga, Shashi Kanbur, Chow-Choong Ngeow, Vincenzo Ripepi, Giuseppe Bono, Giulia De Somma, Massimo Dall'Ora
Figure caption: Histograms of period distributions (top) of 964 GC RR Lyrae variables and distribution of mean metallicities (bottom) for their parent GCs. The peak and the width of the metallicity distribution represent the mean metallicity and its scatter from Carretta et al. (2009), respectively.