adsabs/AstroCLIMB huggingface dataset:
Paper: Power Anisotropy, Dispersion Signature and Turbulence Diffusion Region in the 3D Wavenumber Domain of Space Plasma Turbulence
Authors: Rong Lin, Jiansen He, Xingyu Zhu, Lei Zhang, Die Duan, Fouad Sahraoui, Daniel Verscharen
Figure caption: (a–f): reduced 2D distributions of PSD  B  (ω pl,  k ) and ﹩{\mathrm{PSD}}_{{{\boldsymbol{E}}}_{\langle {{\boldsymbol{v}}}_{i}\rangle }^{{\prime} }}﹩ (ω pl,  k ), where P(k ∥, k ⊥1) = ﹩\iint ﹩PSD (ω pl,  k ) dk⊥2dω pl, and so forth. (g–i): ﹩{P}_{{{\boldsymbol{E}}}_{\langle {{\boldsymbol{v}}}_{i}\rangle }^{{\prime} }}/{P}_{{\boldsymbol{B}}}﹩, normalized by the square of the Alfvén speed, ﹩{V}_{{\rm{A}}}^{2}﹩, plotted to present the detail of the spectral bifurcation between P   B   and ﹩{P}_{{{\boldsymbol{E}}}_{\langle {{\boldsymbol{v}}}_{i}\rangle }^{{\prime} }}﹩. The black dashed circles centered at (0,0) with a length of k min denote a region within which there is large uncertainty.
Paper: Experimental Determination of the Dissociative Recombination Rate Coefficient for Rotationally Cold CH+ and Its Implications for Diffuse Cloud Chemistry
Authors: Daniel Paul, Manfred Grieser, Florian Grussie, Robert von Hahn, Leonard W. Isberner, Ábel Kálosi, Claude Krantz, Holger Kreckel, Damian Müll, David A. Neufeld, Daniel W. Savin, Stefan Schippers, Patrick Wilhelm, Andreas Wolf, Mark G. Wolfire, Oldřich Novotný
Figure caption: Relative level-population evolution of CH+ ions in the CSR during DR measurements. The markers represent laser-probed rotational populations ﹩{\mathop{p}\limits^{\unicode{x002C6}}}_{J}﹩ with statistical one-sigma uncertainties. The lines indicate modeled populations p  J  from experimentally benchmarked radiative rotational cooling (Kálosi et al. 2022) and using the J-dependent inelastic electron-collision cross sections for rotational (de)excitation from Hamilton et al. (2015). Initial populations for the model were fixed to the measured values at t = 23 s (leftmost markers). The metastable a 3Π population evolution (p m, dashed–dotted line) was modeled with Equation (A1). All J populations were normalized such that ﹩{\sum }_{J}{\mathop{p}\limits^{\unicode{x002C6}}}_{J}+{p}_{{\rm{m}}}=1﹩ and ∑ J  p  J  + p m = 1.
Paper: Power Anisotropy, Dispersion Signature and Turbulence Diffusion Region in the 3D Wavenumber Domain of Space Plasma Turbulence
Authors: Rong Lin, Jiansen He, Xingyu Zhu, Lei Zhang, Die Duan, Fouad Sahraoui, Daniel Verscharen
Figure caption:                    ﹩{P}_{{{\boldsymbol{E}}}_{\mathrm{local}\,{{\boldsymbol{v}}}_{i}}^{{\prime} }}/{P}_{{{\boldsymbol{E}}}_{\langle {{\boldsymbol{v}}}_{i}\rangle }^{{\prime} }}﹩ of the event, where P denotes PSD integrated over ω pl and different components of  k  as defined in Figure 2. ﹩{P}_{{{\boldsymbol{E}}}_{{\rm{l}}{\rm{o}}{\rm{c}}{\rm{a}}{\rm{l}}{{\boldsymbol{v}}}_{i}}^{{\rm{{\prime} }}}}/{P}_{{{\boldsymbol{E}}}_{\text{\unicode{x02329}}{{\boldsymbol{v}}}_{i}\text{\unicode{x0232A}}}^{{\rm{{\prime} }}}}﹩                    ﹩({k}_{\parallel },{k}_{\perp 1})=\left(\iint {\mathrm{PSD}}_{{{\boldsymbol{E}}}_{\mathrm{local}\,{{\boldsymbol{v}}}_{i}}^{{\prime} }}({\omega }_{\mathrm{pl}},{\boldsymbol{k}}){\rm{d}}{k}_{\perp 2}{\rm{d}}{\omega }_{\mathrm{pl}}\right)﹩                    ﹩/\left(\iint {\mathrm{PSD}}_{{{\boldsymbol{E}}}_{\langle {{\boldsymbol{v}}}_{i}\rangle }^{{\prime} }}({\omega }_{\mathrm{pl}},{\boldsymbol{k}}){\rm{d}}{k}_{\perp 2}{\rm{d}}{\omega }_{\mathrm{pl}}\right)﹩. The black dashed circles centered at (0,0) with the length k min denote a region within which there is large uncertainty.
Paper: Power Anisotropy, Dispersion Signature and Turbulence Diffusion Region in the 3D Wavenumber Domain of Space Plasma Turbulence
Authors: Rong Lin, Jiansen He, Xingyu Zhu, Lei Zhang, Die Duan, Fouad Sahraoui, Daniel Verscharen
Figure caption: Metric of ion demagnetization/diffusion (left), normalized magnetic helicity (middle), and metric of dispersion computed by NHDS. The black line denotes θ kB ∼ 30°.
Paper: Power Anisotropy, Dispersion Signature and Turbulence Diffusion Region in the 3D Wavenumber Domain of Space Plasma Turbulence
Authors: Rong Lin, Jiansen He, Xingyu Zhu, Lei Zhang, Die Duan, Fouad Sahraoui, Daniel Verscharen
Figure caption: Cuts of energy distribution in the ω−k plane. The angular frequencies are (a) in the spacecraft frame and (b) in the plasma frame obtained by the Doppler relation. Panel (c) shows a result after filling the gray part in panel (b) with its mirror counterpart.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Relation between the column densities of COMs and N(H2), which is estimated using 1.3 mm continuum images. The gray empty and black filled circles represent the cores with a number of detected COMs smaller and greater than 5, respectively. The purple solid line is the linear fit in the log–log space for the COM-rich cores, except for an outlier, G49.49-0.39 C3 (sky blue). The red solid line is the same as the purple line but fitted only at log10 N(H2) < 24.7 cm−2, excluding the three densest cores.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Relation for the abundance ratios of COMs relative to CH3OH vs. N(H2), which is estimated using 1.3 mm continuum images. The gray empty and black filled circles represent cores with a number of detected COMs smaller and greater than 5, respectively. The red solid line is the linear fit in the log–log space for the COM-rich cores.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Abundance relative to CH3OH. The gray boxes indicate the abundance estimated in this work. The different symbols and colors are the adopted values in other regions.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Heat maps of the correlation using the column densities (left) and abundances to N(H2) (right) between two species. The colors show the level of correlation, which corresponds to the Pearson r coefficient shown inside each box. The scatter plots with measured slopes are presented in Figures E1 and E2.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: CH3OH emission peak flux vs. T ex(CH3OH). The units of CH3OH emission peak values are the flux density (Jy) for the 6.7 GHz CH3OH maser emission by MMB and VLA observations and the intensity (Jy beam−1) for the 216.946 GHz CH3OH emission by ALMA observation.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Relation between the number of detected COMs and the N(H2). Filled and unfilled symbols present 6.7 GHz CH3OH detected and undetected cores, respectively. The colors of the filled symbols depict the 6.7 GHz maser peak flux in VLA observation (Hu et al. 2016).
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption:  T ex of COMs derived by the rotation diagram analysis. The medians of CH3OH and isotopologues (green), O-bearing COMs (red), and N-bearing COMs (blue) are presented. Error bars depict the minimum and maximum T ex (Table 5).
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: COM detection rates as functions of (top) N(H2) and (bottom) T ex(CH3OH).
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Column density of CH3OH and abundances of COMs with respect to CH3OH obtained by XCLASS fitting.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Isotopic ratios of 13CH3OH/12CH3OH, CH ﹩{}_{3}^{18}﹩ OH/CH ﹩{}_{3}^{16}﹩ OH, and C2H5C15N/C2H5C14N as functions of N(H2) (upper panels) and T ex(CH3OH) (lower panels). The red and black dots indicate the cores with N(H2) > 24.7 and N(H2) < 24.7 cm−2, respectively.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Correlation between the CH3CHO and HCOCH2OH of 11 cores where the two COMs are detected. The solid and dashed lines are the abundance ratios of 3.5 and 1.6, respectively, which imply the branching ratio suggested by the gas-phase formation route including their uncertainty (Vazart et al. 2020).
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Relation between the N(COMs) vs. T ex(CH3OH). The symbols are the same as in Figure 8. The red solid lines are the linear fits in the log–linear space for all COM-rich cores.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Relation between the X(COMs) vs. T ex(CH3OH). The conventions of symbols and colors are identical to those in Figure D1.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Example spectrum of G49.49-0.39 C1. The red and green solid lines show the spectrum at the 1.3 mm continuum and CH3OH peaks, respectively.
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: D/H ratios of CH3OH and NH2CHO, to N(H2) (top) and T ex(CH3OH) (bottom).
Paper: Complex Organic Molecules Detected in 12 High-mass Star-forming Regions with Atacama Large Millimeter/submillimeter Array
Authors: Giseon Baek, Jeong-Eun Lee, Tomoya Hirota, Kee-Tae Kim, Mi Kyoung Kim
Figure caption: Rotation diagram for CH3OH.
Paper: Anisotropic Magnetic Turbulence in the Inner Heliosphere—Radial Evolution of Distributions Observed by Parker Solar Probe
Authors: Rohit Chhiber
Figure caption: Top: ratio of rms magnetic fluctuation to mean magnitude of the magnetic field. Three cases are shown, based on different temporal averaging intervals for computation of mean and fluctuating fields. Black curve shows r 1/4 power-law scaling (see text). Middle: measures of variance anisotropy. Bottom: test of nonaxisymmetry of transverse fluctuations. Here κ refers to the kurtosis. See text for other definitions. In all panels, statistics are computed within radial bins of size 5 R ⊙; error bars (not shown) are smaller than symbols.
Paper: Anisotropic Magnetic Turbulence in the Inner Heliosphere—Radial Evolution of Distributions Observed by Parker Solar Probe
Authors: Rohit Chhiber
Figure caption: Statistical moments of magnetic fluctuation components, computed in radial bins of size 5 R ⊙ by aggregating data from PSP’s first five orbits. Here “std dev” is the standard deviation. Error bars (not shown) are generally smaller than the symbols.
Paper: Anisotropic Magnetic Turbulence in the Inner Heliosphere—Radial Evolution of Distributions Observed by Parker Solar Probe
Authors: Rohit Chhiber
Figure caption: Direction of mean magnetic field  B  0 as a function of radial distance, aggregated from PSP orbits 1–5, and averaged in radial bins of size 10 R ⊙. Horizontal axis represents R coordinate, and vertical direction represents T and N coordinates for blue and green cases, respectively. The sign of components of  B  0 is not taken into account, and length of arrows is arbitrary. Tail of each arrow is placed at center of the respective radial bin. At 30 R ⊙, angles made by  B  0 wrt to the R direction are 13° and 8° in the R–T and R–N planes, respectively, while at 200 R ⊙ these angles are 46° and 32°.
Paper: Anisotropic Magnetic Turbulence in the Inner Heliosphere—Radial Evolution of Distributions Observed by Parker Solar Probe
Authors: Rohit Chhiber
Figure caption: Probability density functions (pdfs) of magnetic fluctuations. Fields have been normalized by their respective standard deviations before computing pdfs. Bins with fewer than 10 counts are discarded. Dashed curve shows the best-fit Gaussian, which is fit to each pdf in the horizontal range ±3 standard deviations. Skewness of each distribution is indicated. The chi-squared goodness of fit to a Gaussian has values (in order of increasing r) 0.003, 0.002, 0.002 for b ∥, and a value of 0.001 for b ⊥1 and b ⊥2, for all r shown.
Paper: Broadband X-Ray Spectral Analysis of the Dual AGN System Mrk 739
Authors: Koki Inaba, Yoshihiro Ueda, Satoshi Yamada, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Claudio Ricci
Figure caption: Relationship between λ Edd and ﹩{C}_{{\rm{T}}}^{(22)}﹩ for Swift/BAT selected AGNs (black line) and 1σ uncertainties (the gray shaded areas) obtained by Ricci et al. (2017b). Our result for Mrk 739E (red diamond; the best-fit value obtained for σ = 15° is adopted) and those for the late-merger U/LIRGs (cyan circles; Yamada et al. 2021) are overplotted. The arrows represent the results reaching the lower boundary.
Paper: Broadband X-Ray Spectral Analysis of the Dual AGN System Mrk 739
Authors: Koki Inaba, Yoshihiro Ueda, Satoshi Yamada, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Claudio Ricci
Figure caption: (Left) Chandra/ACIS-S image of the central region of the Mrk 739 system in the 2.0–8.0 keV band, smoothed with a 2D Gaussian of a σ radius of 1.5 pixels (each pixel is 0.″492). The spectral extraction regions for Mrk 739E and Mrk 739W are marked by the left (red) and right (green) circles, respectively. (Right) The same but in the 0.4–2.0 keV band. The large circle (white) marks the spectral region for the extended emission from which the rectangle region containing a readout streak and the two circular regions in the left panel are excluded.
Paper: Broadband X-Ray Spectral Analysis of the Dual AGN System Mrk 739
Authors: Koki Inaba, Yoshihiro Ueda, Satoshi Yamada, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Claudio Ricci
Figure caption: The best-fit models in units of EI  E , where I  E  is the energy flux at the energy E. The black, magenta, red, blue, and cyan lines represent the total model, direct component, reflection component from the torus, reflection component from the accretion disk, and optically thin thermal emission, respectively. (Left) The best-fit model of Mrk 739E at the epoch of the Chandra observation. (Right) The best-fit model of Mrk 739W.
Paper: Broadband X-Ray Spectral Analysis of the Dual AGN System Mrk 739
Authors: Koki Inaba, Yoshihiro Ueda, Satoshi Yamada, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Claudio Ricci
Figure caption: The observed spectra of Mrk 739 folded with the energy responses but corrected for the effective area (crosses). The best-fit models are overplotted (lines). (Left) The black, light blue, and magenta crosses and lines represent the NuSTAR, XMM-Newton, and Swift/BAT data of the total spectrum of Mrk 739, respectively. (Right) The red, green, and blue crosses and lines represent the Chandra spectra of Mrk 739E, Mrk 739W, and the extended emission, respectively. The residuals are plotted in the lower panels.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: Vector point diagrams (VPDs) showing the relative proper motions for sources in the Boo I field. Left: all sources brighter than m astrom = 25.0 mag, with stars shown as black points and the 113 best-measured background galaxies shown as gray triangles. Center: all sources fainter than m astrom = 25.0 mag that occupy the stellar locus defined in Figure 8. Right: all background galaxies (i.e., sources to the left/above the red curve in the plane of Figure 8) brighter than m astrom = 25 mag. In the left panel, the stars cluster around zero, as expected, as the vast majority of these are members of Boo I. The slight asymmetry in the distribution of sources in the center panel hints at the presence of faint starlike galaxies. The relative proper motions of the galaxies (right) are clearly offset from the majority of stellar relative proper motions (left).
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: The distribution of all sources detected in one of the second-epoch images, in the plane of instrumental magnitude vs. the quality-of-fit parameter qfit. The red curve is based upon the previous analysis of rich stellar fields and separates likely stars (to the right and below the curve) from artifacts and background galaxies (to the left and above the curve). Astrometric measurements were made only for sources with qfit values below unity, indicated in the plot by the horizontal dashed blue line.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: A sample corner plot verifying the ABC MCMC algorithm for a simulated population drawn from a broken power-law IMF. The synthetic population that was used as the “observed data” was simulated using values for the extinction and distance that do not match the synthetic data generated in the ABC MCMC algorithm (15% higher extinction and ∼3% closer distance). The input parameter values (red) are α 1 =− 1.8, α 2 = −2.5, and f  f  = 0.2, and the retrieved best-fit values are given above the one-dimensional histograms (also shown with black dashed lines). Note that we cannot retrieve the binary fraction within the 68% CI.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: A sample corner plot investigating the effect of assuming a uniform binary mass-ratio distribution while fitting a lognormal IMF to the Boo I observational data. The retrieved best-fit values are given above the one-dimensional histograms (also shown with black dashed lines), and to the right, the Chabrier (2005) values for the low-mass single-star IMF of stellar populations of the Milky Way are provided for context.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: A sample corner plot verifying the ABC MCMC algorithm for a simulated population drawn from a broken power-law IMF. Input parameter values (red) are α 1 = −1.8, α 2 = − 2.5, and f  f  = 0.2, and the retrieved best-fit values are given above the one-dimensional histograms (also shown with black dashed lines). As in the analysis of the observed data, the break mass is held fixed at ﹩{{\rm{M}}}_{b}=0.5{{ \mathcal M }}_{\odot }﹩.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: A sample corner plot verifying the performance of the ABC MCMC algorithm for a simulated population with a known single power-law IMF slope and binary fraction. The input parameter values (α = −1.8, f  f  = 0.4) are shown in red, and the retrieved best-fit values are given above the one-dimensional histograms (also shown with black dashed lines).
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: A sample corner plot verifying the ABC MCMC algorithm for a simulated population drawn from a lognormal IMF. Input parameter values (in red) are ﹩{M}_{c}=0.15{{ \mathcal M }}_{\odot }﹩, σ = 0.6, and f  f  = 0.8, and the retrieved best-fit values are given above the one-dimensional histograms (also shown with black dashed lines).
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: The results of the lognormal fit to the Boo I member catalog. The dashed lines on, and text above, the one-dimensional histograms give the best-fit values. The text to the right of the plot gives, for context, the Chabrier (2005) values for the low-mass, single-star IMF of stellar populations of the Milky Way.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: CMDS of all sources that were fit with DAOPHOT photometry. Left: the sources in the HUDF PSF catalog. Right: the sources in the Boo I field, where no quality cuts have been applied. The mean color of the sources in the HUDF PSF catalog is indicated by the vertical dotted line. Two solar-scaled 13 Gyr isochrones ([Fe/H] = [M/H] = −1.7, solid, and [Fe/H] = [M/H] = −2.5, dashed) from the Dartmouth Stellar Evolution Database (Dotter et al. 2008) are overplotted on the Boo I data, after adjustment for distance and extinction. The two metallicities shown correspond to the approximate mean and maximum metallicity in Boo I, and while these isochrones overlap at brighter magnitudes, they diverge at the faint (low-mass) end, illustrating the importance of metallicity information. In both panels, the dashed black lines show our imposed magnitude limits for the final Boo I catalog used to constrain the IMF.
Paper: Faint Stars in a Faint Galaxy. II. The Low-mass Stellar Initial Mass Function of the Boötes I Ultrafaint Dwarf Spheroidal Galaxy
Authors: Carrie Filion, Imants Platais, Rosemary F. G. Wyse, Vera Kozhurina-Platais
Figure caption: CMDs of the NMSs and likely member stars in the Boo I field, as determined by the Bayesian probabilities computed in Section 3.1 and the adopted 50% probability threshold. Left: all NMSs in the Boo I field. Center: all candidate Boo I member stars. The isochrone is as described in Figure 1. Right: all sources (NMSs shown in gray, candidate member stars in black). In all panels, the dashed black lines show our imposed magnitude limits for the final Boo I catalog used to constrain the IMF.