adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: R Lep Band 10 HCN maser at 890.8 GHz, from the J = 10−9 transition between the (1110) and (0400) vibrationally excited states, using the HCN maser cube averaged over the velocity range between −0.5 and 20.3 km s−1 in the image cube with the velocity width of 0.3 km s−1 (yellow contours). The Band 10 continuum emission is shown as a background grayscale gradation. Phase and amplitude self-cal solutions for the HCN maser channel at v LSRK = 9.4 km s−1 were applied both to the HCN maser and the continuum data. The solid line contours start from the 5σ level, increased by a factor of a power of 2. The dashed line contours start from the −5σ level, increased by a factor of a power of 2. The contour levels are shown on the upper side. The image rms noise of the continuum emission and HCN maser are 0.9 and 497 mJy beam−1, respectively. The synthesized beam size is shown on the lower left and right corners for the HCN maser (5.4 × 4.9 mas) and continuum (5.3 × 4.8 mas), respectively.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Top: R Lep continuum images calibrated with B2B phase referencing alone, adopting the calibrator morphology model as shown in Figure 10. From the left, B-08–B-10. The solid line contours start from the 3σ level of R Lep continuum image without modeling the calibrator morphology, increased by a factor of a power of 2, and the dashed line contour denotes the −3σ level. The contour levels are shown on the upper side of each panel. Bottom: differential images of the R Lep continuum calibrated with B2B phase referencing alone between the calibrators’ point-source assumption and morphology modeling, normalized by the image rms noise. From the left, B-08–B-10. The color scale ranges between −8σ and 8σ. The contours are −4σ, −2σ, and −σ (dashed lines), and σ, 2σ, and 4σ(solid lines).
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Synthesized images of the calibrators observed in the HF-LBC-2021 experiment. The top, middle, and bottom rows show the images at B-08–B-10, respectively. Left, middle, and right panels show the images of (a) J0504-1512 (phase calibrator) in the LF band, (b) J0522-3627 (DGC source) in the LF band, and (c) J0522-3627 (DGC source) in the HF band, respectively. The solid line contours start from 3σlevel, increasing by a factor of a power of 4. The dashed line contours start from −3σ level, increased by a factor of a power of 4. The image peak and rms noise are given at the top and bottom of each panel, respectively. The ellipse in the lower left represents the synthesized beam of the image.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Check source images of J0516-1603 (3.°0 from the phase calibrator) in Band 8 (left), J0438-1251 (6.°7) in Band 9 (middle), and J0423-0120 (17.°2) in Band 10 (right). The horizontal and vertical axes represent relative R.A. and decl. in mas, respectively. The synthesized beam is drawn at the bottom left corner. Contours start from the 3σ level, increasing by a factor of a power of 4. The dashed line contours start from the −3σ level, increased by a factor of a power of 4. The image peak value and rms noise are listed at the top and bottom of each panel, respectively. It is clear that for larger separation angles from the phase calibrator that the check sources cannot be correctly calibrated.
Paper: ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
Authors: Yoshiharu Asaki, Luke T. Maud, Harold Francke, Hiroshi Nagai, Dirk Petry, Edward B. Fomalont, Elizabeth Humphreys, Anita M. S. Richards, Ka Tat Wong, William Dent, Akihiko Hirota, Jose Miguel Fernandez, Satoko Takahashi, Antonio S. Hales
Figure caption: Distribution of the target scans within the switching cycle time used during the observations. The horizontal axis is the switching cycle time between visits to the phase calibrators. The longer switching cycle times are due to system noise temperature measurement or check source scans being inserted in between phase calibrator scans. From the left, B-08–B-10.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: The stellar mass, distance, and Hubble type of the 33 NSC sample galaxies (circles) selected from the 53 galaxy CBS survey (triangles). The MW-like subsample of 20 galaxies are shown as squares.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: Top panel: color–magnitude diagram with the NSC UVIS color vs. F814W band absolute magnitude. The circles denote the NSCs in our sample. The MW-like subsample is denoted by the squares. The open circles represent the dusty galaxies with an NSC quality fit = 2. Bottom panel: NSC color–color plot (UVIS vs. IR). Colored pluses and squares show PARSEC 1.2S SSP models (Bressan et al. 2012) at two metallicities (−1.0 and +0.3) and with ages from 1–13 Gyr (indicated by the color). An extinction vector of corresponding to A  V  = 1 is also shown. All plotted magnitudes in both panels are foreground extinction corrected.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: The mass–size relation of our NSCs compared to previous literature measurements. The circles denote our NSC sample galaxies, with surrounding squares indicating the MW-like subsample. Open circles indicate uncertain measurements due to dust (i.e., quality flag = 2 in Table 3). The points are colored red or blue based on their Hubble type (early and late type, respectively). The literature sample of NSCs from early- (red stars) and late-type (blue stars) galaxies is obtained from Côté et al. (2006), Erwin & Gadotti (2012), Georgiev & Böker (2014), Spengler et al. (2017), Eigenthaler et al. (2018), Sánchez-Janssen et al. (2019), and Pechetti et al. (2020).
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: 2D image modeling of an example galaxy, NGC 4689, using IMFIT. Each row describes fits on a different scale: the top row shows the largest-scale fits to the Spitzer IRAC1 image, the middle row shows an HST/WFC3/IR F160W image, while the bottom row shows the smallest-scale and highest-resolution fits to the HST/WFC3/UVIS F814W image. The left column shows the data, the next column to the right shows the best-fit model, and the right-most columns show the residuals. In the bottom row, three residual images are shown, the left one is from a fit with no NSC, the middle with a point-source NSC component, and the right with the best-fit model image shown; the stretch of all three of these residual images is identical and clearly shows the need for a resolved NSC component in this galaxy.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: The ratios of BH mass to NSC mass are plotted against the host galaxy masses (left panel) and against the NSC masses (right panel) based on plots from Neumayer et al. (2020) but adding in data from the new NSC masses in our sample. The circles denote our NSC sample galaxies, with surrounding squares indicating the MW-like subsample. Open circles indicate uncertain measurements due to dust (i.e., quality flag = 2 in Table 3). The points are colored red or blue based on their Hubble type (early and late type, respectively). The literature sample from early- (red stars) and late-type (blue stars) galaxies are obtained from Seth et al. (2008a), Graham & Spitler (2009), Neumayer & Walcher (2012), Georgiev et al. (2016), and Nguyen et al. (2018). Literature results with upper and lower limits for the BH and NSC masses are represented by the arrows. The solid horizontal line indicates equal NSC and BH masses in the galaxies.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: Top panel: an example 1D surface brightness profile of NGC 4689 from our F814W imaging and modeling. Note this is the same galaxy shown in Figure 2. The data are shown as green crosses, the best-fit model is shown as the blue solid line, and the best-fit NSC component is shown as the purple solid line. Lower panel: the residuals (model – data) in magnitudes. Three different residuals are shown corresponding to the right three panels in Figure 2. The best-fit model with a resolved NSC, point-source NSC model, and no NSC model are shown as blue, orange, and red lines, respectively.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: The NSC masses are plotted against the host galaxy masses. The markings are the same as in Figure 5. The literature sample contains both early- and late-type galaxies from Côté et al. (2006), Turner et al. (2012), Georgiev et al. (2016), and Sánchez-Janssen et al. (2019).
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: Left panel: galaxy ellipticity vs. NSC ellipticity. The population of NSCs is typically rounder than their host galaxy disks, suggesting a less flattened distribution. Circles denote the NSC sample with squares showing the MW-like subsample. The galaxies are colored red and blue based on their Hubble type (early and late type, respectively). The NSCs with quality flag = 2, i.e., dusty centers, are denoted by open circles. Right panel: difference between NSC and galaxy PAs, δPA. We plot the difference for all those NSCs whose ϵ > 0.05. There is a clear preference for near-alignment between the NSCs and their host galaxies’ disks.
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: Top panel: NSC mass vs. NSC Sérsic index. Bottom panel: NSC mass vs. NSC ellipticity. The solid circles denote our NSC sample galaxies, with squares indicating the MW-like subsample. All dusty galaxies (i.e., quality flag = 2) are denoted by open circles. The points are colored red or blue based on their Hubble type (early and late type, respectively).
Paper: Composite Bulges. III. A Study of Nuclear Star Clusters in Nearby Spiral Galaxies
Authors: Aishwarya Ashok, Anil Seth, Peter Erwin, Victor P. Debattista, Adriana de Lorenzo-Cáceres, Dmitri A. Gadotti, Jairo Méndez-Abreu, John E. Beckman, Ralf Bender, Niv Drory, Deanne Fisher, Ulrich Hopp, Matthias Kluge, Tutku Kolcu, Witold Maciejewski, Kianusch Mehrgan, Taniya Parikh, Roberto Saglia, Marja Seidel, Jens Thomas
Figure caption: The NSC masses plotted against the photometric bulge to total ratios (top panel) and the bar luminosities (bottom panel). The markings are the same as in Figure 4.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: GCS reconstructions of the three different subparts—(a) streamer blowout, (b) large loop, and (c) three-part cavity—of the complex 2015 July 9 CME using the single LASCO/C3 viewpoint. The panels to the left show 2 hr difference images, and the panels to the right display the corresponding GCS wireframe projection overlaid.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: The 2015 July 9 CME observed in situ by the Wind and ACE spacecraft, together with its geomagnetic response. The panels show: (a) magnetic field magnitude, (b) Cartesian components of the magnetic field, (c) latitudinal and (d) longitudinal angles of the magnetic field, (e) solar wind speed, (f) proton density, (g) proton temperature, (h) plasma beta, (i) total pressure (proton and electron gas pressure plus magnetic pressure), (j) pitch-angle spectrogram of suprathermal 265 eV electrons, (k) oxygen charge state ratio, (l) average iron charge state, and (m) Dst index. The gray vertical line indicates the arrival of the shock-like disturbance, while the gray shaded areas highlight the ICME ejecta (dark gray) and the magnetic cloud interval (light gray) within it. A Lundquist flux rope fitting has been plotted in pink over the magnetic cloud interval.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: Simulated magnetic field and plasma time series for (a) all EUHFORIA simulations and (b) the EUHFORIA+FRi3D simulation, shown against the corresponding measurements taken by the Wind spacecraft. The panels show, from top to bottom: Magnetic field magnitude, magnetic field components in Cartesian coordinates, solar wind bulk speed, proton density, proton temperature, plasma beta, and Dst index (where the red profile features WDC Kyoto data and the black profile displays the modeled Dst based on Wind in situ measurements using the algorithm of O’Brien & McPherron 2000). The solid vertical lines mark the arrival of the shock-like disturbance, while the dashed vertical lines mark the leading and trailing edges of the ICME ejecta (i.e., the beginning and end of the gray shaded area in Figure 3). The results in (a) show the simulated time series at Earth only, while the results in (b) show simulation outputs at Earth as well as in the ±5° and ±10° latitudinal and longitudinal offsets around Earth.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: Overall modeling results of the 2015 July 9 CME. The figure shows the three heliospheric simulations performed with EUHFORIA compared with each other and with the Paper I coronal simulation modeled with ARMS+STITCH. (a) ARMS+STITCH simulation. (b) EUHFORIA+Spheroid simulation. (c) EUHFORIA+Spheromak simulation. (d) EUHFORIA+FRi3D simulation. Each panel shows (left) the −20° latitude plane and (right) the 0° longitude plane in Stonyhurst coordinates. The latitudinal plane shows the radial velocity V  r , and the longitudinal plane shows the B  z  component of the magnetic field. Representative magnetic field lines are shown in the simulations with magnetized CME ejecta, and the black contours in panel (b) highlight the merged density enhancement of the nonmagnetized spheroid CMEs.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: Pre-eruptive configuration of the filament. (a) Hα image from BBSO, with left-bearing filament barbs (signatures of a right-handed filament) indicated by arrows. (b) SDO/HMI magnetogram with the global PILs marked in orange. The approximate locations of the positive and negative filament footpoints with respect to the PIL involved in the eruption are marked with ⊕  and ⊖  symbols, respectively.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: Overview of the GCS geometry in the (left) face-on and (right) edge-on projections, adapted from Thernisien (2011). The half-angular face-on (R maj) and edge-on (R min) widths of the croissant are highlighted in magenta.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: Dependence of the GCS face-on width R maj on model parameters α and κ. (a) R maj computed numerically via Equation (A4) using the procedure outlined in Thernisien (2011). (b) The empirical fit ﹩{\widehat{R}}_{\mathrm{maj}}﹩ given by Equation (A5). (c) The residual ﹩({R}_{\mathrm{maj}}-{\widehat{R}}_{\mathrm{maj}})﹩ between the numerical (a) and empirical (b) formulations.
Paper: Modeling a Coronal Mass Ejection from an Extended Filament Channel. II. Interplanetary Propagation to 1 au
Authors: Erika Palmerio, Anwesha Maharana, Benjamin J. Lynch, Camilla Scolini, Simon W. Good, Jens Pomoell, Alexey Isavnin, Emilia K. J. Kilpua
Figure caption: Comparison of a (b) GCS vs. a (c) FRi3D fitting of the 2017 July 9 CME applied to (a) SOHO/LASCO/C3 imagery from July 10 at 12:54 UT.
Paper: CWISE J105512.11+544328.3: A Nearby Y Dwarf Spectroscopically Confirmed with Keck/NIRES
Authors: Grady Robbins, Aaron M. Meisner, Adam C. Schneider, Adam J. Burgasser, J. Davy Kirkpatrick, Jonathan Gagné, Chih-Chun Hsu, Leslie Moranta, Sarah Casewell, Federico Marocco, Roman Gerasimov, Jacqueline K. Faherty, Marc J. Kuchner, Dan Caselden, Michael C. Cushing, Sherelyn Alejandro
Figure caption:  J-band absolute magnitude (M  JMKO) plotted against Spitzer ch1−ch2 color for the LTY dwarfs in Kirkpatrick et al. (2021), where the blue star is W1055+5443, the purple star is WISEA J153429.75−104303.3 (a.k.a. The Accident), the green star is WISEA J114156.67−332635.5, and the black star is Y dwarf WISE 0855−0714. Cases of objects with Spitzer and/or J-band limits rather than detections are excluded, as are dwarfs without parallax measurements available. The WISEA J153429.75−104303.3 data point makes use of its Gemini J-band detection from Meisner et al. (2023).
Paper: CWISE J105512.11+544328.3: A Nearby Y Dwarf Spectroscopically Confirmed with Keck/NIRES
Authors: Grady Robbins, Aaron M. Meisner, Adam C. Schneider, Adam J. Burgasser, J. Davy Kirkpatrick, Jonathan Gagné, Chih-Chun Hsu, Leslie Moranta, Sarah Casewell, Federico Marocco, Roman Gerasimov, Jacqueline K. Faherty, Marc J. Kuchner, Dan Caselden, Michael C. Cushing, Sherelyn Alejandro
Figure caption: Comparison of the W1055+5443 near-infrared spectrum normalized between 1.27 and 1.29 μm (black) vs. various fitted models (red). The left models are the top three best-fitting LOWZ models from Meisner et al. (2021). The right models are the top three best-fitting Sonora Bobcat models from Marley et al. (2021). Both of these model grids explore multiple values of T eff, log(g), and [m/H]. The LOWZ models shown have log(K  zz ) = 2.0, while the Sonora Bobcat models are not parameterized in terms of K  zz .
Paper: CWISE J105512.11+544328.3: A Nearby Y Dwarf Spectroscopically Confirmed with Keck/NIRES
Authors: Grady Robbins, Aaron M. Meisner, Adam C. Schneider, Adam J. Burgasser, J. Davy Kirkpatrick, Jonathan Gagné, Chih-Chun Hsu, Leslie Moranta, Sarah Casewell, Federico Marocco, Roman Gerasimov, Jacqueline K. Faherty, Marc J. Kuchner, Dan Caselden, Michael C. Cushing, Sherelyn Alejandro
Figure caption: CatWISE2020 and AllWISE W2 − W3 color vs. CatWISE2020 W1 − W2 color for the LTY dwarfs in Kirkpatrick et al. (2021) with CatWISE detections in W1 and W2 and AllWISE detections in W3. The blue star is W1055+5443, the green star is Y0 dwarf WISEA J114156.67−332635.5, and the black star is Y dwarf WISE 0855−0714 (Luhman 2014). The WISE 0855−0714 data point makes use of this object’s W3 detection reported in Leggett et al. (2017). We note that the W1 photometry of WISEA J114156.67−332635.5 is likely contaminated (resulting in an artificially blue W1 − W2 color), given that the AllWISE epoch and the Spitzer ch1 epoch for this source are similar (see Section 2.1 for discussion of the Spitzer ch1 contamination of this source).