adsabs/AstroCLIMB huggingface dataset:
Paper: The GAPS Programme at TNG XXXIX. Multiple Molecular Species in the Atmosphere of the Warm Giant Planet WASP-80 b Unveiled at High Resolution with GIANO-B 
Authors: Ilaria Carleo, Paolo Giacobbe, Gloria Guilluy, Patricio E. Cubillos, Aldo S. Bonomo, Alessandro Sozzetti, Matteo Brogi, Siddharth Gandhi, Luca Fossati, Diego Turrini, Katia Biazzo, Francesco Borsa, Antonino F. Lanza, Luca Malavolta, Antonio Maggio, Luigi Mancini, Giusi Micela, Lorenzo Pino, Ennio Poretti, Monica Rainer, Gaetano Scandariato, Eugenio Schisano, Gloria Andreuzzi, Andrea Bignamini, Rosario Cosentino, Aldo Fiorenzano, Avet Harutyunyan, Emilio Molinari, Marco Pedani, Seth Redfield, Hristo Stoev
Figure caption: As Figure 2 but with v rest interval between [−99, 99] km s−1.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: Each panel shows the map of the superflat on a certain part of a CCD, the number of which is given in the corners with the band name.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The residual of the e 1 component of the PSF ellipticity from polynomial fitting up to the first (left plot), second (middle plot), and third order (right). The data is from the z band.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The residual of the PSF area from polynomial fitting up to the third order. From left to the right are the results for the g, r, and z band, respectively.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: Same as Figure 3, but for the e 2 component.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The distribution of the 62 CCD chips on the focal plane. Inside each chip, we show the CCD number on the upper side, and the detector position ID on the lower side.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The distribution of the PSF FWHM for the g, r, z bands.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The results of the FD test for galaxies of two catagories in z-band: those with PSF FWHM greater (upper panels) or smaller (lower panels) than 1.″4. In each plot, the black solid line is the “y = x” reference, and the red dashed line is the best fit of the data points. The multiplicative and additive biases are shown in the upper-left corner of each plot. The results for the g 1 and g 2 components are shown in the left and right panels respectively.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The distribution of ν  F  in the z-band shear catalog.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: Distribution of the number of images per galaxy in the g, r, and z bands.
Paper: Shear Measurement with Poorly Resolved Images
Authors: Jun Zhang, Cong Liu, Pedro Alonso Vaquero, Hekun Li, Haoran Wang, Zhi Shen, Fuyu Dong
Figure caption: The distribution of the source galaxies in the g, r, and z bands.
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: Comparisons of radii from the asteroseismic scaling relations with linear radii from interferometry across literature for 16 oscillating giants from the HD-TESS catalog. The lower panels show the fractional difference between radii estimates, where ΔR = R interferometric − R seismic. The median ΔR/R seismic for each comparison is quoted in each lower panel, with standard errors as the reported uncertainty. The color of each star’s label along the x-axis reflects its evolutionary state, with red for RGB and blue for CHeB. (a) R seismic uses (T eff, [M/H]) adopted in this study and applies the Sharma et al. (2016) correction to compute the correction factor f Δν  (see Equation (2)). (b) R seismic uses T eff values adopted in this work, with f Δν  = 1. (c) R seismic uses the literature (i.e., interferometric) T eff values reported from each cited work, with f Δν  = 1.
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: (a1) ECDFs for the HD-TESS and Kepler asteroseismic mass proxy values, ﹩{\nu }_{\max }^{0.75}/{\rm{\Delta }}\nu ﹩. The quantity D measures the maximum vertical distance between any two ECDFs. Here, the plotted ECDFs (HD-TESS vs. Kepler) are constructed using the mean values of ﹩{\nu }_{\max }﹩ and Δν. (a2) The distribution of D Proxy across 105 different noise realizations. The black, dashed histogram is a “self-similarity” D Proxy distribution for the Kepler data set, created by repeatedly comparing one instance of a Kepler ECDF to another having a different noise realization. The dashed–dotted green histogram is the self-similarity distribution for the HD-TESS data set. The blue, solid histogram measures similarity between HD-TESS and Kepler data sets and its large offset from the other histograms indicates a strong dissimilarity between the underlying Kepler and TESS seismic mass proxy distributions that is unlikely to be explained by random uncertainties in Kepler or TESS data sets alone. Panels (b1) and (b2) are similar to panels (a1) and (a2), respectively, but for reported values of mass.
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: Gaia color–magnitude diagrams showing the 99 oscillating giants in our sample known to be astrometric binaries from the El-Badry et al. (2021) catalog. Only binary systems that have a chance alignment probability less than 0.1 from the catalog are identified. The blue points mark the brighter, primary component (oscillating giant) of each binary system, while the magenta points mark the corresponding fainter, secondary component. The black points are a random subset of stars from Gaia EDR3 (Gaia Collaboration et al. 2021). Panel (a) shows all identified binary systems, which are further categorized in panels (b-f) based on the location of their secondary components in the color–magnitude diagram: (b) on the upper main sequence (MS); (c) on the main sequence; (d) on the lower main sequence; (e) in the subdwarf regime; (f) along the white dwarf (WD) sequence.
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: (Top) Kernel density estimates comparing the masses of HD-TESS giants (shaded) with those from a population of giants observed by Kepler (Yu et al. 2018). Compared to the Kepler giants, our TESS sample has a greater fraction of stars above 1.5M ⊙, which is consistent with comparisons of the seismic mass proxy ﹩{\nu }_{\max }^{0.75}/{\rm{\Delta }}\nu ﹩ between both samples in Figure 4. (Bottom) A comparison of distances between the two giant star samples. TESS probes stellar populations mainly within the solar neighborhood, whereas Kepler probes populations much farther into the Milky Way disk.
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: The relative popularity of bright, oscillating red giants in our TESS sample, visualized as the number of references registered on the SIMBAD astronomical database (Wenger et al. 2000) as of 2022 January. Bright stars with Bayer designations are annotated in the plot, while blue points indicate interesting giants flagged as “peculiar” by SIMBAD, which here comprises either halo stars or known barium stars (Bidelman & Keenan 1951).
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: Seismic visual diagnostic plots for the 16 oscillating giants benchmarked against interferometric measurements in Section 5.2, categorized by their evolutionary state (RGB = hydrogen shell burning, CHeB = core helium burning). The stars are ordered in decreasing Δν from the top left to the bottom right in each category. The blue horizontal line in each panel corresponds to ﹩{\nu }_{\max }﹩, while the green vertical line corresponds to the location of the radial mode ridge in the échelle diagrams.
Paper: HD-TESS: An Asteroseismic Catalog of Bright Red Giants within TESS Continuous Viewing Zones
Authors: Marc Hon, James S. Kuszlewicz, Daniel Huber, Dennis Stello, Claudia Reyes
Figure caption: Comparisons of radii from the asteroseismic scaling relations with linear radii from interferometry across literature for 16 oscillating giants from our TESS giant sample. This Figure is identical to Figure 10, except that the interferometric radii are derived using Hipparcos parallaxes as opposed to Gaia EDR3 parallaxes.
Paper: A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System 
Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger
Figure caption: PDFs of the stellar parameters of HD 33142 derived by applying the Bayesian inference scheme of Stock et al. (2018) and using the parallax, B and V photometry, and the spectroscopic metallicity estimate provided in Table 1. The vertical dashed lines show the 0.16, 0.5 (median), and 0.84 quantiles of the posterior samples.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: The evolution of the flip ratio for m 1 = 5, 9, 11, and 15 M Jup over a timescale of 100 Myr. As in Figure 8, ﹩{{ \mathcal H }}_{1}﹩, ﹩{{ \mathcal H }}_{2}﹩, and ﹩{{ \mathcal H }}_{3}﹩ correspond to the selected perturbation Hamiltonian. In each panel, the evolution before 2 Myr is given as a subfigure. In these subfigures, dotted–dashed lines with an equilibrium value f > 0.5 represent prograde orbits that have been transformed from retrograde orbits, while solid lines with f < 0.5 have been transformed from prograde orbits to retrograde orbits.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: The contour maps of the total angular momentum G tot and the perturbation Hamiltonian ﹩{ \mathcal H }﹩ for m 1 = 5 and 15 M Jup in the initial conditions plane of (e 1, i mut). The white dashed lines represent the constant values of G tot for e 2 ∈ [0.35, 0.45], while the color bars on the right indicate the different values of the perturbation Hamiltonian. In panel (a), when e 2 selects five different values, there will be five level curves of G tot. We also mark out the initial conditions for G tot = 1.75318 (the black dashed lines) and ﹩{ \mathcal H }=-8.06\times {10}^{-8}﹩ (the solid line) with black dots, corresponding to data points with red error bars in Figure 8(a).
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Ranges of i mut for m 1 = 5, 9, 11, and 15 M Jup over a timescale of 100 Myr. The black dots represent the positions of the initial parameters {e 1,0, i mut,0}. The upper and lower limits of the error bars represent the maximum and minimum values of the mutual orbital inclination i mut, respectively. The different colors correspond to specific values of the perturbation Hamiltonian.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Geometry of the invariable plane and the reference plane system. G 1 and G 2 are angular momentum vectors of the inner and outer orbits; G tot is the total angular momentum vector of the system, with the invariable plane being perpendicular to G tot; i 1,2 is the angle between the orbital angular momentum vector and  G  tot, where i mut is the mutual inclination between the inner and outer orbit; and I 1,2 represents the observed inclination of the inner and outer orbit, which is the angle between the orbital plane and reference plane (the sight plane).
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Corner diagram of our N-body best-fitting solutions, with χ 2 = 1.44. Here, ﹩m\sin I﹩, P, ﹩\sqrt{e}sin{\omega }﹩,﹩\sqrt{e}\cos \omega ﹩, and M with subscripts 1 and 2, denote the minimum mass, orbital period, ﹩\sqrt{e}﹩ vector, and mean anomaly of γ Cep Ab and γ Cep AB, respectively. The figure illustrates the one- and two-dimensional projections of the posterior probability distributions of the parameters, with the structure directly showing the covariances between the two parameters. The distribution histograms of each parameter are listed on the diagonal.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: The blue dots with red error bars are the residuals after subtracting the calculated RV of γ Cep AB from the observations (O-AB). The derived RV signals induced by γ Cep Ab from the N-body fitting are shown by the black solid curve, where all the orbital elements change over time.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: The best-fitting RV signals of the γ Cep Ab B system. Upper panel: the red triangles and squares show published observations (Walker et al. 1992; Hatzes et al. 2003), where the black solid line denotes the RV signals of the N-body model, with mutual perturbation between the companion and planet b. Lower panel: O-C for the N-body model.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: Lomb–Scargle periodogram analysis of γ Cep Ab. The value of the power is the maximum power of the periodic signals, while the dashed lines of false alarm probability (FAP)1, FAP2, and FAP3 represent 1%, 0.1%, and 0.01% of the FAP, respectively. There is a significant periodic signal of roughly 900 days, which means that this signal is truly periodic.
Paper: Extremely Inclined Orbit of the S-type Planet γ Cep Ab Induced by the Eccentric Kozai–Lidov Mechanism
Authors: Xiumin Huang, Jianghui Ji
Figure caption: One of the contour maps of the total angular momentum and the perturbation Hamiltonian in the representative plane of (﹩\sqrt{1-{e}_{1}^{2}}﹩, ﹩\sqrt{1-{e}_{2}^{2}}﹩). The black dashed lines indicate the level curves of the Hamiltonian and the red solid line is the conserved G tot.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: Variation in [C/H] as a function of T eff(a), log g (b) and [Fe/H] (c) after CKS correction. Giant-planet host stars (red), small-planet host stars (black), field stars (gray), and Sun (yellow). Variation in [C/H] error (shifted for visual purpose at different x-values plotted in blue. In Figure 9(c), the black dashed line show the 1:1 correlation. (d) shows [C/Fe] as a function of [Fe/H] and the solid lines indicating the mean value of [C/Fe] in [Fe/H] bin of 0.2 dex for giant-planet host stars (red), Small-planet host stars (black) and field stars (gray).
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: (a) Occurrence rate of exoplanets as a function of the planetary radius and the host star metallicity. (b) The total occurrence rate of the sample without subdividing it into different metallicity bins. (c) Normalized occurrence rate of the exoplanets as a function of the planetary radius and the host star metallicity. The error bars in these plots are the Poissonian errors based on the number of planets in each bin.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: Distribution of carbon among small-planet(R  p  ≤ 4R ⊕) host, giant-planet(R  p  > 4R ⊕) host stars and field stars. Dashed vertical line represents the mean value of each distribution.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: Comparison of ﹩\delta {[{\rm{C}}/{\rm{H}}]={[{\rm{C}}/{\rm{H}}]}_{\mathrm{CKS}}-[{\rm{C}}/{\rm{H}}]}_{\mathrm{LAMOST}}﹩ as a function of T eff. A linear fit is established and the best-fit coefficients are﹩\delta [{\rm{C}}/{\rm{H}}]=-0.762\ast \mathrm{ln}({T}_{\mathrm{eff}}(\mathrm{lamost}))+6.820﹩.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: Comparison of the [Fe/H] values from CKS and the LAMOST pipeline. A linear fit is established between the CKS and the LAMOST [Fe/H] values. The best-fit coefficients are [Fe/H]new = [Fe/H]lamost∗0.791 + 0.005. The blue dashed line is the 1:1 line and black dashed line is the best-fit line.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: Comparison of the [C/H] values from CKS and the LAMOST as a function of T eff. The black dashed line is the 1:1 line and blue dashed line is the best-fit line.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: Comparison of the T eff values from CKS and the LAMOST. The black line is the 1:1 line.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: (a) Occurrence rate of exoplanets as a function of the planetary radius and the host star [C/Fe]. (b) Normalized occurrence rate of exoplanets as a function of the planetary radius and the host star [C/Fe].
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: (a) Occurrence rate of exoplanets as a function of the planetary radius and the host star [C/H]. (b) Normalized occurrence rate of the exoplanets as a function of the planetary radius and the host star [C/H].
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Overlay of cluster positions (solid circles) on the UVIT F148W image of the central and northeast parts of M31 (Leahy et al. 2020). Log(Z/Z ⊙) values are shown by the size of the circles with radius proportional to log(Z/Z ⊙), with blue indicating positive values and red indicating negative values, and the total range is −2.3 to +0.3.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: The cluster model fit to UVIT and PHAT magnitudes for source 1596 in the catalog of Johnson et al. (2015; it is number 84 in our catalog). The black dots with error bars are the data, and the black line connects the best-fit cluster model photometry points. The other six lines are for cluster models with the best-fit parameters fixed, except for the labeled parameter: i.e., age increased (red) or decreased (magenta) by a factor of 2; log(Z/Z ⊙) increased (yellow) or decreased (pink) by 0.6; or E(B–V) increased (blue) or decreased (cyan) by 0.08. The six model curves with altered parameters were normalized to the data at 336 nm in order to illustrate changes in shape.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Overlay of cluster positions (solid circles) on the UVIT F148W image of the central and northeast parts of M31. Log(age/yr) values are shown by the size of the circles with radius proportional to log(age/yr) and total range 6.6 to 9.7. Clusters with log(age/yr) < 6.75 are plotted in red, 6.75 < log(age/yr) < 8.55 are shown in blue, and log(age/yr) > 8.55 are presented in magenta.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Top panel: Metallicity vs. age with errors, illustrating that most clusters have log(Z/Z ⊙) between −0.3 and +0.3. Bottom panel: Mass vs. age with errors, showing a monotonically increasing average mass with age.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Histograms of the best-fit parameters for the UVIT-PHAT clusters. E(B–V) is multiplied by 10 so that it is on a similar x-axis scale to the other parameters.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Number of clusters in bins (0.°1 width) of distance, R, in the disk plane from the center of M31.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Histograms of the best-fit χ 2 for the UVIT-PHAT clusters.
Paper: Search for Extraterrestrial Intelligence with the ngVLA
Authors: C. Ng, L. Rizk, C. Mannion, E. F. Keane
Figure caption: The sky coverage vs. maximum distance of detection of an Arecibo-like transmitter. We obtain the parameters for other SETI projects from Enriquez et al. (2017). We categorize four levels of SETI sensitivity based on the maximum possible detection distance on the bottom x-axis, with ≤25 pc being low sensitivity (light blue), ≤75 pc being mid sensitivity (yellow), ≤250 pc being high sensitivity (red), and anything above being very high sensitivity (purple). The ngVLA is the only SETI project that can detect an Arecibo-like transmitter beyond 250 pc.