adsabs/AstroCLIMB huggingface dataset:
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: The DESI focal plane has over 675,000 individual parts. It was installed in 2019 on the Mayall Telescope, located atop Iolkam Du’ag (Kitt Peak) in the Tohono O’odham Nation (near Tucson, Arizona). Commissioning took place in 2020; survey operations began in 2021.
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: Each of the 10 petals on DESI is a complete instrument with 502 robots, 12–14 fiducial point sources, a guide or wave front camera, a protective enclosure for fiber splices, power supplies, and control electronics. At left, a fully assembled petal is viewed from the front, looking toward the robotically controlled fiber tips. Fiducial sources are mounted in cylindrical housings and interspersed throughout the robot array. A guide camera (covered by a protective plate in this image) is mounted at the upper-right corner, and the whole assembly here is surrounded by a protective metal enclosure (which is removed just prior to installation in the telescope). At the right, a side view shows the layout of fibers, electronics, and the support structure.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: (a) q PAH vs. ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ for 373 non-AGN MIR-selected galaxies (same plot as the panel (4,0) in Figure 6). Symbols are color-coded according to the sSFR. Typical error bar in oxygen abundance and q PAH is marked in the corner. The mean value of the q PAH is 2.3 and 3.7 for galaxies with ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})\lt 8.5﹩ and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})\geqslant 8.5﹩, respectively (horizontal lines). The black line is the linear regression describing the relationship between ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ and q PAH, while gray lines are possibilities of linear correlation determined based on Bayesian methods considering uncertainties in ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ and q PAH. (b) q PAH vs. stellar mass. For galaxies in stellar mass bins of ﹩\mathrm{log}({M}_{\mathrm{star}}/{M}_{\odot })=﹩[9.0, 9.5], [9.5, 10.0], [10.0, 10.5], and [10.5, 11.0], galaxies are divided into the low metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})\lt 8.5﹩) and high metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})\geqslant 8.5﹩) subgroups and the mean q PAH for each subgroup are plotted (note that points for the low metallicity subgroups are slightly shifted in x-direction for clarity). Overplotted are (1) q PAH values measured from the stacked SEDs of 0.3 < z < 0.7 star-forming galaxies in different stellar mass bins (black horizontal lines; Schreiber et al. 2018), and (2) 〈q PAH〉 values for different stellar mass bins of z < 0.7 MIR/FIR-selected galaxies (gray horizontal lines; Kovács et al. 2019). The linear relationship between the ﹩\mathrm{log}({M}_{\mathrm{star}})﹩ and q PAH and its posterior distribution is overplotted as black and gray lines.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: (a) Comparison between the parent AKARI MIR-selected sources (dots) and sources with optical spectroscopic observations (crosses). Histograms on the top and the right show the number fractions of the sources with optical spectra among the entire MIR-selected sources, i.e., the completeness of the spectroscopic observations, for different magnitude bins. Optical spectra are available for more than 50% of the MIR-selected sources with f S9W > 0.4 mJy (corresponds to f S11 > 0.6 mJy and/or f L15 > 0.9 mJy). (b) Redshift distributions of (i) AKARI MIR galaxies with optical identification (photometric redshifts from Ho et al. 2021), (ii) AKARI galaxies with r-band magnitude cut (r < 21.5), (iii) MIR-selected sources targeted for optical spectroscopic observations using MMT/Hectospec and WIYN/Hydra, and (iv) z spec < 0.4 sources studied in this work. All histograms are normalized to have equal areas. (c) Star-formation rate vs. stellar mass from SED fitting for AKARI galaxies with z phot < 0.4 (dots), spectroscopic sample of galaxies with z spec < 0.4 (open circles), and subsample of spectroscopic sample that also satisfy MIR and FIR detection criteria (crosses; see Section 2.4 for sample selection in this work). Overplotted solid lines represent star-forming main sequences at z ∼ 0 and z ∼ 0.4 (Speagle et al. 2014) with ±0.2 dex scatter as shaded regions. Short vertical and horizontal bars with different colors indicate median values of ﹩\mathrm{log}\,{M}_{\mathrm{star}}﹩ and ﹩\mathrm{log}\,\mathrm{SFR}﹩ for different samples, respectively.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: Correlation between different physical parameters: gas-phase metallicity ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩, stellar mass, specific SFR (sSFR), total IR luminosity, and mass fraction of PAH particles (q PAH). Spearman rank coefficients (ρ) between two variables in the x- and y-axis are specified in each panel. The sample is divided into three subsamples according to the redshift (z < 0.1, 0.1 ≤ z < 0.25, and 0.25 ≤ z < 0.4), which results in a similar number of galaxies in each subsample. The distribution of each physical parameter is illustrated using a stacked histogram (in order of 0.25 ≤ z < 0.4, 0.1 ≤ z < 0.25, and z < 0.1 bins) in order to better represent the difference between different subsamples.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: (a) BPT diagram (Baldwin et al. 1981) for MIR-selected sources. Objects with sufficient MIR and FIR photometric data points (at least four in MIR wavelengths and one in FIR wavelengths) are marked as coral squares. Typical values of errors in x- and y-axes are plotted as an error bar at the bottom right. Overplotted are criteria to separate AGN and star-forming galaxies (Kewley et al. 2001 and Kauffmann et al. 2003 for solid and dashed lines, respectively). (b) MIR color–color diagram for AGN selection using WISE 3-bands (3.4, 4.6, and 12 μm) photometry. Dots are WISE-detected sources with spectroscopic redshifts of z < 0.4. Objects that are classified by the BPT diagram as star-forming (H II), composite, and AGN subgroups are plotted using different symbols. Typical error bar in both axes is shown in the right. Solid and dashed lines represent AGN selection criteria suggested by Mateos et al. (2012) and Jarrett et al. (2011), respectively, based on the assumption that AGN contribution is described by a power-law-shaped hot dust emission at 3–12 μm.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: Test results to reproduce values of physical parameters based on the CIGALE run using mock catalog constructed from the best-fit SEDs. 373 non-AGN objects with estimated metallicity values are used to construct these plots. The x-axis represents the total IR luminosity, dust mass, mass fraction of PAH particles (q PAH), SFR, stellar mass, and IR excess (defined as the ratio between IR and UV luminosity) determined from the best-fit SED. A mock catalog is constructed using the expected flux density (based on the best-fit SED) and the observed flux uncertainty in each filter, which is to be used as an input in the CIGALE run with the same configuration to derive output (y-axis) value for each physical parameter. Gray dashed lines are y = x lines, while the correlations between the input and output values are described as linear functions (blue solid lines) with the determination coefficients r 2. All properties are relatively well reproduced with strong correlation (r 2 > 0.9), supporting the robustness of the derived properties.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: (a) Comparison between the oxygen abundance values derived using O3N2 index and N2 index (Pettini & Pagel 2004). The uncertainties of ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ implemented in two methods are 0.14 dex and 0.18 dex (at 1σ) for O3N2 and N2, respectively. Such systematic uncertainty and uncertainty in the measured line flux ratio are quadratically summed to produce a typical error bar, marked in the corner. For HII galaxies, ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ values from O3N2 and N2 are consistent within 0.02. (b) Distribution of the ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ values for spectroscopically observed objects (after the AGN exclusion), estimated using O3N2 index (371 objects) and N2 index (747 objects). Filled histograms are the metallicity distributions of objects satisfying criteria for availability of FIR and MIR photometric points (179 and 369 for O3N2 and N2 methods, respectively; the number of total objects with measured metallicity that meets other criteria is 373).
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: Example MIR-FIR SED of MIR-selected galaxies (best-fit template from CIGALE run). Blue solid and orange dashed lines represent (unattenuated) stellar component and dust emission component, respectively. Oxygen abundance ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩, PAH mass fraction derived from SED fitting, and redshift are indicated.
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: (a) Molecular gas mass for MIR-selected galaxies as a function of stellar mass. In order to calculate the molecular gas mass (﹩{M}_{{{\rm{H}}}_{2}}﹩), total gas mass is estimated using δ GDR-metallicity calibration (De Vis et al. 2019), dust mass from SED fitting, and metallicity-dependent H2/HI mass ratio (Boselli et al. 2014). Error bar in the left corner represents typical uncertainties in the derived ﹩{M}_{{{\rm{H}}}_{2}}﹩. Overplotted symbols are 0.05 < z < 0.5 star-forming galaxies with measured molecular gas mass through CO observations (squares and triangles; Bauermeister et al. 2013). Linear regression fit between the gas mass and stellar mass of our sample galaxies is plotted as a thick black line, along with thin gray lines covering a possible range of linear relation. (b) Gas depletion time (M gas/SFR) vs. sSFR (SFR/M star) for our sample of MIR-selected galaxies. Error bar in the corner represents typical uncertainties in x- and y-axis parameters, reflecting the estimation errors as well as scatter in a conversion formula. Again, the CO-detected samples from Bauermeister et al. (2013) and Villanueva et al. (2017) are plotted for comparison. The thick black line and thin gray lines show linear regression results. Dot-dashed and dashed lines indicate depletion time vs. sSFR relation for nearby (z < 0.05) galaxies measured either using global gas mass (COLD GASS; Saintonge et al. 2011) or gas mass derived for 1 kpc grids (HERACLES; Huang & Kauffmann 2014). Dotted line is such a relation for local (with distance <25 Mpc) “gas-rich” galaxies among the Herschel reference survey galaxies (Boselli et al. 2014).
Paper: Metallicity–PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
Authors: Hyunjin Shim, Ho Seong Hwang, Woong-Seob Jeong, Yoshiki Toba, Minjin Kim, Dohyeong Kim, Hyunmi Song, Tetsuya Hashimoto, Takago Nakagawa, Ambra Nanni, William J. Pearson, Toshinobu Takagi
Figure caption: (a) Comparison between q PAH derived from SED fitting and luminosity (ν L  ν ) ratio between 8 and 4.5 μm—the former stands for PAH emission and the latter for stellar continuum (Murata et al. 2014). Blue solid line is the best-fit linear correlation with specified determination coefficient r 2. (b) Comparison between q PAH and IR8, defined as ﹩{L}_{\mathrm{IR}}^{\mathrm{total}}/\nu {L}_{\nu }(8\mu {\rm{m}})﹩. Overplotted curve is the correlation between the two suggested by Schreiber et al. (2018). (c) Comparison between luminosity fraction of PAH features (relative to total IR emission) and mass fraction q PAH. PAH luminosity is calculated by the sum of luminosities of 6.2 μm and 7.7 μm features from Ohyama et al. (2018).
Paper: Astrometric Accelerations as Dynamical Beacons: Discovery and Characterization of HIP 21152 B, the First T-dwarf Companion in the Hyades 
Authors: Kyle Franson, Brendan P. Bowler, Mariangela Bonavita, Timothy D. Brandt, Minghan Chen, Matthias Samland, Zhoujian Zhang, Anna Lueber, Kevin Heng, Daniel Kitzmann, Trevor Wolf, Brandon A. Jones, Quang H. Tran, Daniella C. Bardalez Gagliuffi, Beth Biller, Jeffrey Chilcote, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Clémence Fontanive, Tyler D. Groff, Raffaele Gratton, Olivier Guyon, Rebecca Jensen-Clem, Nemanja Jovanovic, N. Jeremy Kasdin, Julien Lozi, Eugene A. Magnier, Koraljka Mužić, Aniket Sanghi, Christopher A. Theissen
Figure caption: Keck/NIRC2 ﹩L^{\prime} ﹩ (top) and SCExAO/CHARIS 1.15–2.39 μm (bottom) imaging of HIP 21152 B. The left panels show the PSF-subtracted images for each data set, while the right panels shows the corresponding S/N maps. Each frame is oriented so that north is up and east is to the left. The S/N maps are generated by measuring the flux in 0.5 FWHM-radius circular apertures at different separations and comparing the flux to noise estimated through additional nonoverlapping apertures at the same separation. We apply a Gaussian filter with a standard deviation of 1.5 px to the Keck/NIRC2 ﹩L^{\prime} ﹩ imaging to enhance features at the scale of the recovered FWHM of the companion.
Paper: Astrometric Accelerations as Dynamical Beacons: Discovery and Characterization of HIP 21152 B, the First T-dwarf Companion in the Hyades 
Authors: Kyle Franson, Brendan P. Bowler, Mariangela Bonavita, Timothy D. Brandt, Minghan Chen, Matthias Samland, Zhoujian Zhang, Anna Lueber, Kevin Heng, Daniel Kitzmann, Trevor Wolf, Brandon A. Jones, Quang H. Tran, Daniella C. Bardalez Gagliuffi, Beth Biller, Jeffrey Chilcote, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Clémence Fontanive, Tyler D. Groff, Raffaele Gratton, Olivier Guyon, Rebecca Jensen-Clem, Nemanja Jovanovic, N. Jeremy Kasdin, Julien Lozi, Eugene A. Magnier, Koraljka Mužić, Aniket Sanghi, Christopher A. Theissen
Figure caption: Predicted mass as a function of projected separation for HIP 21152 B based on the 8.4 ± 0.8 m s−1 yr−1 Hipparcos-Gaia acceleration of its host star in the HGCA. Colors indicate the relative probability of agreement; companions with separations and masses below the blue curve cannot produce the observed change in proper motion. HIP 21152's astrometric acceleration indicates the presence of a substellar companion within 1″ or a star at wider separations. The dotted lines denote the hydrogen-burning limit (HBL; ∼75 M Jup) and the deuterium-burning limit (DBL; ∼13 M Jup). The yellow star on the plot shows the dynamical mass (﹩{24}_{-4}^{+6}\,{M}_{\mathrm{Jup}}﹩) and separation (0.″37) of HIP 21152 B, which agrees with the prediction.
Paper: Astrometric Accelerations as Dynamical Beacons: Discovery and Characterization of HIP 21152 B, the First T-dwarf Companion in the Hyades 
Authors: Kyle Franson, Brendan P. Bowler, Mariangela Bonavita, Timothy D. Brandt, Minghan Chen, Matthias Samland, Zhoujian Zhang, Anna Lueber, Kevin Heng, Daniel Kitzmann, Trevor Wolf, Brandon A. Jones, Quang H. Tran, Daniella C. Bardalez Gagliuffi, Beth Biller, Jeffrey Chilcote, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Clémence Fontanive, Tyler D. Groff, Raffaele Gratton, Olivier Guyon, Rebecca Jensen-Clem, Nemanja Jovanovic, N. Jeremy Kasdin, Julien Lozi, Eugene A. Magnier, Koraljka Mužić, Aniket Sanghi, Christopher A. Theissen
Figure caption: Reduced chi-square (﹩{\chi }_{\nu }^{2},﹩ left) and goodness-of-fit (G, right) values for model spectra from Saumon & Marley (2008) compared with HIP 21152 B’s spectra and photometry. Lower values of ﹩{\chi }_{\nu }^{2}﹩ or G signify a better fit to the data. Colors indicate different values of f sed, while symbols correspond to different values of ﹩\mathrm{log}g﹩. Reduction 2 is used for the SPHERE/IFS spectrum. The two metrics yield the same best-fitting spectrum, with T eff = 1400 K, ﹩\mathrm{log}g=4.5﹩, and f sed = 2.
Paper: Astrometric Accelerations as Dynamical Beacons: Discovery and Characterization of HIP 21152 B, the First T-dwarf Companion in the Hyades 
Authors: Kyle Franson, Brendan P. Bowler, Mariangela Bonavita, Timothy D. Brandt, Minghan Chen, Matthias Samland, Zhoujian Zhang, Anna Lueber, Kevin Heng, Daniel Kitzmann, Trevor Wolf, Brandon A. Jones, Quang H. Tran, Daniella C. Bardalez Gagliuffi, Beth Biller, Jeffrey Chilcote, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Clémence Fontanive, Tyler D. Groff, Raffaele Gratton, Olivier Guyon, Rebecca Jensen-Clem, Nemanja Jovanovic, N. Jeremy Kasdin, Julien Lozi, Eugene A. Magnier, Koraljka Mužić, Aniket Sanghi, Christopher A. Theissen
Figure caption: Orbit fit of HIP 21152 B compared with relative astrometry (top panels), HGCA proper motions (middle panels), sky-projected orbit (bottom-left panel), and RVs (bottom-right panel). The gray curves show 150 randomly drawn orbits from the MCMC chains. The maximum-likelihood orbit is highlighted in black. The middle proper motion (diamond) in the proper-motion panels is a joint proper motion from the difference in sky position between Hipparcos and Gaia EDR3. It is an average proper motion that reflects the reflex motion over the entire 25 yr between the missions.
Paper: Astrometric Accelerations as Dynamical Beacons: Discovery and Characterization of HIP 21152 B, the First T-dwarf Companion in the Hyades 
Authors: Kyle Franson, Brendan P. Bowler, Mariangela Bonavita, Timothy D. Brandt, Minghan Chen, Matthias Samland, Zhoujian Zhang, Anna Lueber, Kevin Heng, Daniel Kitzmann, Trevor Wolf, Brandon A. Jones, Quang H. Tran, Daniella C. Bardalez Gagliuffi, Beth Biller, Jeffrey Chilcote, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Clémence Fontanive, Tyler D. Groff, Raffaele Gratton, Olivier Guyon, Rebecca Jensen-Clem, Nemanja Jovanovic, N. Jeremy Kasdin, Julien Lozi, Eugene A. Magnier, Koraljka Mužić, Aniket Sanghi, Christopher A. Theissen
Figure caption: Comparison between two independent reductions of the SPHERE/IFS data. Reduction 1 uses the DRH pipeline complemented with additional steps described in Langlois et al. (2021) and the SpeCal software to extract spectral cubes from the raw data, subtract the host-star PSF, and obtain the companion’s spectrum. Reduction 2 uses a modified version of the CHARIS pipeline and the TRAP post-processing pipeline to measure the companion’s spectrum from the raw data. These two independent reductions produce similar results for λ ≳ 1.15 μm. Reduction 2 tends to yield lower values for the companion flux blueward of 1.15 μm than Reduction 1. Due to this discrepancy, we exclude points with λ < 1.15 μm from this analysis.