adsabs/AstroCLIMB huggingface dataset:
Paper: Deep-learning Reconstruction of Sunspot Vector Magnetic Fields for Forecasting Solar Storms
Authors: Dattaraj B. Dhuri, Shamik Bhattacharjee, Shravan M. Hanasoge, Sashi Kiran Mahapatra
Figure caption: A comparison of the time evolution of the CNN-estimated vector field features during the 2003 Halloween storms using MDI and GONG LOS magnetograms. The CNN trained with HMI magnetograms is used for the estimation from MDI magnetograms, whereas the CNN trained with GONG magnetograms is used for the estimation from GONG magnetograms. Note that the HMI observations are not available before 2010. The CNN:GONG feature values are generally high compared to the CNN:MDI, showing little variation throughout the storms. The CNN:MDI features appear to capture the variation of these features during the storms expected from the theoretical modeling (e.g., Kazachenko et al. 2010). The 1σ errors are shown. The gaps indicate missing observations. The legend in the rightmost panel applies to all panels.
Paper: Deep-learning Reconstruction of Sunspot Vector Magnetic Fields for Forecasting Solar Storms
Authors: Dattaraj B. Dhuri, Shamik Bhattacharjee, Shravan M. Hanasoge, Sashi Kiran Mahapatra
Figure caption: Comparison of true and CNN-estimated SHARP vector field features. Scatter plots for the distribution of CNN-estimated and true HMI values of total unsigned flux, absolute current helicity, and mean free energy density obtained from HMI and GONG LOS magnetograms. The 45° line is marked for reference.
Paper: Analysis of Thermal Emissions of Exoplanets with Axially Symmetric Temperature Gradients
Authors: Jennifer L. Carter
Figure caption: Illustrated is the geometry of a point P on the exoplanet surface. It may be described in terms of its polar angle η and its azimuthal angle ϕ. The angle between the substellar point S and the subplanetary point E is the phase angle ϵ. The line of sight passes through the subplanetary point and the center of the exoplanet O  p . The angle ﹩\gamma ^{\prime} ﹩ is the angular separation of S and P. Finally, the angle of foreshortening γ is also called the angle of reflection, and measures the angle between P and the subplanetary point. Adapted from K´opal (1954, 1959) as in Carter (2018).
Paper: Analysis of Thermal Emissions of Exoplanets with Axially Symmetric Temperature Gradients
Authors: Jennifer L. Carter
Figure caption: Example spacing for modeling the temperature gradient of an exoplanet using six equally spaced, axially symmetric zones. Shown are polar angles delimiting the starting position of each temperature zone, separated by π/6 radians such that η 1 = η 6 = π/3, η 2 = η 5 = π/6, and η 3 = η 4 = 0.
Paper: Analysis of Thermal Emissions of Exoplanets with Axially Symmetric Temperature Gradients
Authors: Jennifer L. Carter
Figure caption: A depiction of the geometry relating the polar angles η  full , η pen, and η un that delimit the end of the fully illuminated, first, and second penumbral zones, respectively. Points beyond η un are within the unilluminated zone. Adapted from Carter (2018).
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Pressure levels probed by the HST/WFC3 + G141 wavelength range for T dwarfs with temperatures of 900 K (red line) and 600 K (blue line), covering the T5–T8 spectral types according to radiative-transfer models. We shaded in red the most variable wavelength ranges of the spectra, which were used as numerators for J and H indices (see Figure 3). We shaded in blue the least variable wavelength ranges of the spectra, which were used as the denominator for indices J, H, and J-slope.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Upper plot: histogram showing how many synthetic variable spectra fall in variable areas of index–index plots. The histogram shows that most of the variable synthetic spectra fall in at least 11 variable areas in the index–index plots. Bottom plot: histogram showing how many synthetic nonvariable spectra fall in variable areas. The histogram shows that most of the nonvariable synthetic spectra fall in fewer than 10 variable areas. Thus, we mark the threshold on 11 plots to catalog an object as a variable candidate.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Color–magnitude diagrams in the MKO system showing all ultracool dwarfs from Table 3 in Dupuy & Liu (2012) with errors < 0.5 mag. Symbol colors indicate spectral types: M6–L2 (brown), L2.5–L9 (red), L9.5–T4 (purple), >T4.5 (blue), and the brown dwarfs with SpeX/IRTF spectra used in this work (black). J1416B is one of the objects included in our sample of weak variables that have a blue color.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Histogram of the number of variable zones in which the variable synthetic spectra generated with the SpeX spectra are found. Most of the synthetic spectra generated from the SpeX spectra of 2M2228 and J0050–3322 are in more than 11 variable zones in the index plots.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Histogram of the number of times each of the mid- to late-T dwarfs in Table 3 falls in the variability regions in each of the 12 index–index plots.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Histogram of the number of times the synthetic spectra of brown dwarfs are within the 10/12 limit of our variability regions.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Histogram of the number of times in which nonvariable synthetic spectra generated using the SpeX spectra fall. Only J1110+0116 has a few spectra in more than 11 out of 12 regions.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: The ratio of WIBRaLS flux density averaged over a 570-day window to the average flux density outside it. Top: all WIBRaLS sources. Bottom: TXS 0506+056 and PKS 1502+106 are removed from the sample. Definitions of legends are the same as in Figure 4.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Distribution of the simultaneous flaring period (overlap flaring time) ratio in infrared and γ-ray. The blue bars indicate the FIBS sources with flaring in both infrared and γ-ray, and the orange and green bars are the “IceCube Warm Spots” and “IceCube Region” sources, respectively. See text for more details.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: The ratio of orphan flares vs. simultaneous multifrequency flares with observed and simulated data. The stars represent the averaged values of the observed data, while the circles mean those from the simulations. The red, green, and blue points are “IceCube Warm Spots,” “IceCube Region” sources with a distance smaller than 1°, and “IceCube Region” sources with a distance larger than 1°, respectively.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: The ratio of ACC flux density averaged over a 30-day window to the average flux density outside it. The data average and 1σ statistical error are calculated with the observed experimental data, while the trials’ 1σ statistical errors are obtained from random trials of the control samples.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: The ratio of 4FGL flux averaged over a 22-day window to the average flux outside it. Top: with 90% containment region extended by a factor of 1.1. Bottom: factor of 1.5. Definitions of legends are the same as in Figure 4.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Correlation between infrared and Fermi light curves. The time lags of flaring in infrared are estimated with the DCF. The blue and orange bars represent the time lag corresponding to the maximum cross-correlation and the Gaussian fitted mean of the cross-correlated matrix between two light curves, respectively.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption:  P-values with respect to different ΔT (time window) trials. The top panel is for WIBRaLS sources, and the bottom panel is for Fermi 4FGL-DR2 sources.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: The ratio of XRT flux averaged over a 30-day window to the average flux outside it. Definitions of legends are the same as in Figure 4.
Paper: Hunting for Neutrino Emission from Multifrequency Variable Sources
Authors: Yu-Ling Chang, Bruno Arsioli, Wenlian Li, Donglian Xu, Liang Chen
Figure caption: Pretrial p-values of the ratio of averaged flux over a 570-day window to that outside it for WIBRaLS sample.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: Multiscale views of the G28.20-0.05 massive protostar. (a) Top left: Spitzer 8 μm image (1″.9 resolution) of the ∼20 pc scale region. A filamentary IRDC, from which the massive protostar appears to have formed, is visible as a dark shadow. (b) Top middle: Herschel 70 μm image (5″.2 resolution) of the ∼5-pc scale region. The circle shows the aperture used for MIR to FIR SED photometry of the source (see text). (c) Top right: ALMA 1.3 mm compact (C) configuration only continuum map (beam size of 0″.813 × 0″.735), with intensity scale from 0.1σ (σ = 1.29 mJy beam−1) to 316 mJy beam−1. The dashed circle represents the ALMA 12 m primary beam. (d) Bottom left: the same field of view as (c), but now showing the ALMA 1.3 mm compact + intermediate (C+I) configurations continuum map (beam size of 0″.201 × 0″.217), with intensity scale from 0.1σ (σ = 0.358 mJy beam−1) to 316 mJy beam−1. The solid circle shows a 5″ radius aperture enclosing the main continuum structures, which is one scale used for flux measurements. (e) Bottom middle: as (c), but now showing the ALMA 1.3 mm compact + intermediate + extended (C+I+E) configurations continuum map (beam size of 0″.060 × 0″.036), with intensity scale from 0.1σ (σ ∼ 0.170 mJy beam−1). (f) Bottom right: a zoom-in of panel (e) to the inner region of G28.20-0.05, which shows a ring-like structure. The solid circle shows a 0″.5 radius aperture, which is used to measure the flux of the ring.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Top left: ALMA 1.3 mm continuum image (E configuration only) of inner region of G28.20-0.05. The VLA 1.3 cm continuum is shown with contours [0.1, 0.2, 0.4, 0.8, 1.2, 1.6, 2.0, 2.4 Jy arcsec−2]. The beam size of 1.3 mm image is 0″.048 × 0″.026 (see inset), while that at 1.3 cm is 0″.09. An offset of 34.8 mas in the direction of P.A. = 216° is seen between the peaks of the VLA and ALMA images (see red arrow in lower right, while black arrow, almost overlapping, shows the direction to Galactic center). (b) Top right: as (a), but now showing 1.3 mm C+I+E combined image, with beam size 0″.060 × 0″.036 (see inset). (c) Middle left: as (a), but now with the 1.3 cm image translated to align with the 1.3 mm image. (d) Middle right: as (b), but now with the 1.3 cm image translated to align with the 1.3 mm image. (e) Bottom left: map of spectral index, ﹩{\alpha }_{\nu }=\mathrm{log}\left({I}_{{\nu }_{1}}/{I}_{{\nu }_{2}}\right)/\mathrm{log}\left({\nu }_{1}/{\nu }_{2}\right)﹩, where ν 1 = 22.4 GHz and ν 2 = 234 GHz, i.e., evaluated using 1.3 cm and 1.3 mm (E configuration) fluxes. The contours are the 1.3 mm continuum E configuration image, with levels at [0.5, 1, 1.5, 2, 2.5, 3, 3.5, 4, 4.5, 5, 5.5, 6] Jy/arcsec2. (f) Bottom right: as (e), but now using the 1.3 mm C+I+E configuration image. The overlaid contours levels are the same as in (e).
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Top: radio to millimeter SED of the inner 0″.5 (2850 au) radius region of G28.20-0.05. Two data points are shown at 230 GHz (1.3 mm) from the ALMA observations. The higher (blue) point is based on the C+I+E combined image, while the lower (red) one is based on the E-only configuration image. Information about the other data points, which are from VLA observations, is given in Table 3. A power-law fit to the SED (including ALMA C+I+E measurement) is shown, along with 1σ and 2σ confidence intervals, with derived spectral index of α  ν  = 0.118 ± 0.020. (b) Bottom: as (a), but now showing separate in-band ALMA measurements from 43 to 14.7 GHz (C+I+E—blue open squares; E—red open squares). Solid squares show the equivalent average ALMA fluxes with these configurations from (a). Now the power-law fit is only done to the VLA data points and then extrapolated to the ALMA frequencies. This power law has α  ν  = 0.168 ± 0.058.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Top left: moment 0 map of H2CO (32,1 − 22,0, E up = 68.1 K) only considering cells above 1σ of the spectral rms measured over representative emission free channels. The black contours show the 1.3 mm continuum emission (0.5, 1, 1.5, 2, 2.5, 3, 3.5, 4, 4.5, 5, 5.5, 6 Jy arcsec−2). (b) Top right: as (a), but for H2CO (91,8 − 91,9, E up = 174 K). (c) Bottom left: as (a), but for CH3OH (4−2,3 − 3−1,2, E up = 45.46 K). (d) Bottom right: as (a), but for CH3OCH 3(224,19 − 223,20, E up = 253.41 K).
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Top: optical depth (τ) of inner-scale dust around G28.20-0.05, i.e., within a projected radius of 0″.5 (2850 au), vs. assumed dust temperature. The blue dotted line shows τ evaluated from a uniform face-on slab of material in this region, with its mass surface density estimated assuming 0.19 Jy is due to optically thin dust emission at 1.3 mm. The solid blue line shows the equivalent τ, but allowing for optical depth in the slab. The red dotted and solid lines show the equivalent cases when assuming this 1.3 mm continuum emission is concentrated in a 10 times smaller area, e.g., a uniform slab of radius 900 au. (b) Bottom: as (a), but now showing the implied mass surface densities, Σmm, of the slabs.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Top left: 216.575  GHz (spw8) continuum image in E configuration only of the inner region of G28.20-0.05. The beam size is 0″.042 × 0″.021. (b) Top right: as (a), but now for C+I+E combined data. The beam size is 0″.073 × 0″.046. (c) Middle left: as (a), but for 233.926  GHz (spw0). The beam size is 0″.048 × 0″.027. (d) Middle right: as (b), but for 233.926  GHz (spw0). The beam size is 0″.077 × 0″.051. (e) Bottom left: E-only spectral index map between spw8 and spw0, i.e., ﹩{\alpha }_{\nu }=\mathrm{log}\left({I}_{{\nu }_{1}}/{I}_{{\nu }_{2}}\right)/\mathrm{log}\left({\nu }_{1}/{\nu }_{2}\right)﹩, where ν 1 = 216.575 GHz, and ν 2 = 233.926 GHz. The overlaid continuum contours levels are the same as in Figure 2. (f) Bottom right: as (e), but for C+I+E combined data.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: Averaged H2CO (32,1 − 22,0, E up = 68.1 K) (blue), CH3OH (4−2,3 − 3−1,2, E up = 45.46 K) (red), H2CO (91,8 − 91,9, E up = 174 K) (magenta), and CH3OCH 3(224,19 − 223,20, E up = 253.41 K) (cyan) spectrum of G28.20-0.05 over an aperture 3″ radius. We notice the lines both show good Gaussian-like single peak shape. The black dotted line shows the systemic velocity from the literature at 95.6 km s−1, which is consistent to the peaks of both lines. Hence, we adopt the literature value as the systemic velocity of the source and used through this work.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: In-band 1.3 mm SED of the inner 0″.5 (2,850 au) radius region of G28.20-0.05 based on E-only (red points) and C+I+E (blue points) configuration images. Power-law fits to these SEDs are shown with derived spectral indices of α  ν  = 0.255 ± 2.930 for E-only and α  ν  = 2.77 ± 0.71 for C+I+E.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: Moment 0, 1, and 2 maps (left to right) of CH3OCH 3(224,19 − 223,20, E up = 253.41 K) emission, only including pixels that are above 1σ spectral rms (see Table 2, spw7). The black contours show the 1.3 mm continuum emission (0.5, 1, 1.5, 2, 2.5, 3, 3.5, 4, 4.5, 5, 5.5, 6 Jy arcsec−2).
Paper: Magellan/IMACS Spectroscopy of Grus I: A Low Metallicity Ultra-faint Dwarf Galaxy 
Authors: Anirudh Chiti, Joshua D. Simon, Anna Frebel, Andrew B. Pace, Alexander P. Ji, Ting S. Li
Figure caption: Top left: color–magnitude diagram of stars observed in this study. Confirmed nonmembers of Gru I, as determined by their radial velocities and metallicities (see Section 3.3) are shown as red crosses. Confirmed members of Grus I are shown as filled blue circles. Candidate members (those with velocities consistent with membership, but no metallicity information) are shown as hollow blue circles. DES J225643.20−501130.0, the star with a radial velocity consistent with Grus I membership but a high metallicity ([Fe/H] = −0.9 ± 0.38; see Section 3.3) is indicated by a larger red cross. A 10 Gyr, [Fe/H] = −2.2 MIST isochrone (Paxton et al. 2011, 2013, 2015, 2018; Choi et al. 2016; Dotter 2016) is overplotted at the distance modulus of Grus I (m − M = 20.48 mag; Cantu et al. 2021) for reference. Top right: spatial distribution of stars observed in this study. The dashed ellipse denotes the Grus I half-light radius presented in Cantu et al. (2021). Bottom left: histogram of velocities of the stars in our sample. The Grus I members clearly cluster between ∼−150 and ∼−135 km s−1. Note that one star (DES J225643.20-501130.0) has a velocity consistent with membership but is listed as a nonmember due to its high metallicity (see paragraph 2 in Section 3.3). Bottom right: Gaia EDR3 (Gaia Collaboration et al. 2016, 2021) proper motions of stars in our sample. The members and candidate members of the Grus I cluster at a systemic proper motion of ﹩{\mu }_{\alpha }\cos \delta =0.07\,\pm \,0.05﹩ mas yr−1, μ  δ  = 0.25 ± 0.07 mas yr−1.
Paper: Magellan/IMACS Spectroscopy of Grus I: A Low Metallicity Ultra-faint Dwarf Galaxy 
Authors: Anirudh Chiti, Joshua D. Simon, Anna Frebel, Andrew B. Pace, Alexander P. Ji, Ting S. Li
Figure caption: Left panels: corner plot from our Markov Chain Monte Carlo (MCMC) analysis to determine the systemic radial velocity and velocity dispersion of Grus I, while jointly fitting for the velocity offset between the M2FS and IMACS spectrographs (see Section 4.1). We determine a systematic velocity of −143.5 ± 1.2 km s−1 and a velocity dispersion of ﹩{2.5}_{-0.8}^{+1.3}﹩ km s−1, confirming Grus I to be dark-matter dominated (>80 M ⊙/L ⊙ from the 95% CI; see Section 4.1) as is typical of UFDs. Right panels: corner plot from our MCMC analysis to determine the mean metallicity and metallicity dispersion of Grus I. We find that Grus I has a low 〈[Fe/H]〉  = −2.62 ± 0.11, also as is typical of UFDs, and places an upper limit on the metallicity dispersion of σ [Fe/H] < 0.44.
Paper: Magellan/IMACS Spectroscopy of Grus I: A Low Metallicity Ultra-faint Dwarf Galaxy 
Authors: Anirudh Chiti, Joshua D. Simon, Anna Frebel, Andrew B. Pace, Alexander P. Ji, Ting S. Li
Figure caption: [Fe/H] vs. radial velocities for stars in this study. The members of Grus I clearly cluster at low metallicities ([Fe/H] < −2.0) and at a systematic velocity of ∼−143 km s−1. Note that one star has a velocity consistent with membership but a high metallicity ([Fe/H] −0.9 ± 0.38 dex), and is therefore listed as a nonmember. There are additional candidate members in our sample with velocities consistent with membership (see Section 3.3), but are not shown in this plot as the S/N of their spectra is too low for a metallicity determination.
Paper: A Submillimeter Survey of Faint Galaxies behind 10 Strong Lensing Clusters
Authors: L. L. Cowie, A. J. Barger, F. E. Bauer, C.-C. Chen, L. H. Jones, C. Orquera-Rojas, M. J. Rosenthal, A. J. Taylor
Figure caption: Ratio of F160W flux to SCUBA-2 850 μm flux (left) and redshift (right) vs. demagnified SCUBA-2 850 μm flux for the ALMA clusters listed in the legend with either speczs or photzs. We also show SMA sources in the CDF-N from Cowie et al. (2017) (black triangles) and ALMA sources in the CDF-S from Cowie et al. (2018) (black diamonds). In the left panel, we include two SMA-selected sources in MACSJ0717 from Hsu et al. (2017 green circles). We also show our definition of optical/NIR dark SMGs (horizontal line). Finally, we show a power-law fit to the points above 0.5 mJy, log(flux ratio) = (−3.00 ± 0.11)–(0.96 ± 0.23)log (demagnified 850 μm flux), where the errors on the parameters are 1σ. In the right panel, we show the ALMA cluster sources that are not detected in the SCUBA-2 850 μm image at a nominal flux of 0.03 mJy.