adsabs/AstroCLIMB huggingface dataset:
Paper: Searching for C II Emission from the First Sample of z ∼ 6 O I Absorption-associated Galaxies with the Atacama Large Millimeter/submillimeter Array
Authors: Yunjing Wu, Zheng Cai, Jianan Li, Kristian Finlator, Marcel Neeleman, J. Xavier Prochaska, Bjorn H. C. Emonts, Shiwu Zhang, Feige Wang, Jinyi Yang, Ran Wang, Xiaohui Fan, Dandan Xu, Emmet Golden-Marx, Laura C. Keating, Joseph F. Hennawi
Figure caption: The impact parameter between absorber-galaxy pairs. The unfilled dots are C IV absorber–LAE pairs reported by Cai et al. (2017) and Díaz et al. (2021). The filled gray star is the identified O I absorber-[C II] emitter pair, while the nonfilled stars are emitters in our data cube but get ruled out because of large impact parameters. The solid and dashed lines are calculated based on the projected outflow velocities of 100 and 200 km s−1, respectively. Different colors indicate different launching times of galactic outflow ranging from z = 7–10.
Paper: Searching for C II Emission from the First Sample of z ∼ 6 O I Absorption-associated Galaxies with the Atacama Large Millimeter/submillimeter Array
Authors: Yunjing Wu, Zheng Cai, Jianan Li, Kristian Finlator, Marcel Neeleman, J. Xavier Prochaska, Bjorn H. C. Emonts, Shiwu Zhang, Feige Wang, Jinyi Yang, Ran Wang, Xiaohui Fan, Dandan Xu, Emmet Golden-Marx, Laura C. Keating, Joseph F. Hennawi
Figure caption: Left: Cumulative number distribution of emitters in six O I absorber fields as the function of S/N. Blue and orange lines are the measured numbers in six fields, respectively. The red dashed line shows a fitted error function to the number of negative targets. This fitting is in order to avoid the small number of statistics at the high-S/N end. Right: The measured fidelity as the function of S/N. The gray bars show the measured fidelity. The fitted fidelity is shown in dark red.
Paper: Searching for C II Emission from the First Sample of z ∼ 6 O I Absorption-associated Galaxies with the Atacama Large Millimeter/submillimeter Array
Authors: Yunjing Wu, Zheng Cai, Jianan Li, Kristian Finlator, Marcel Neeleman, J. Xavier Prochaska, Bjorn H. C. Emonts, Shiwu Zhang, Feige Wang, Jinyi Yang, Ran Wang, Xiaohui Fan, Dandan Xu, Emmet Golden-Marx, Laura C. Keating, Joseph F. Hennawi
Figure caption: Velocity offsets vs. impact parameters of [C II] candidates in this work. These targets are all color-coded by their signal-to-noise ratios. The dark and light gray regions show our major and relaxed selection criteria, respectively.
Paper: Searching for C II Emission from the First Sample of z ∼ 6 O I Absorption-associated Galaxies with the Atacama Large Millimeter/submillimeter Array
Authors: Yunjing Wu, Zheng Cai, Jianan Li, Kristian Finlator, Marcel Neeleman, J. Xavier Prochaska, Bjorn H. C. Emonts, Shiwu Zhang, Feige Wang, Jinyi Yang, Ran Wang, Xiaohui Fan, Dandan Xu, Emmet Golden-Marx, Laura C. Keating, Joseph F. Hennawi
Figure caption: Completeness as a function of S/N. Circles are the field-averaged completeness, while error bars represent the field-to-field variance in five QSO fields. The red line is the best-fit function.
Paper: Latitudinal Propagation of Thermal Rossby Waves in Stellar Convection Zones
Authors: Rekha Jain, Bradley W. Hindman
Figure caption: Propagation diagram for a neutrally stable polytropic atmosphere in a semi-infinite domain. The positive (negative) frequencies indicate waves propagating in prograde (retrograde) direction in the rotating frame. The lightly shaded region indicates the frequencies of waves that are radially propagating (﹩{k}_{z}^{2}\gt 0﹩) at the indicated height in the atmosphere. The purple curves denote those frequencies and radii for which a radial turning point occurs (i.e., ﹩{k}_{z}^{2}=0﹩). Thus, at a given frequency, an inertial wave cavity exists in the shaded region between two turning points. Such a cavity for thermal Rossby waves is formed purely by the stratification. We have indicated the eigenfrequencies for such modes for a semi-infinite atmosphere using the blue horizontal dotted lines. The green horizontal lines denote the critical frequencies—see Equation (19)—that separate the low-frequency waves that lack a lower turning point from the higher frequency waves that have two turning points (an upper and a lower turning point).
Paper: Latitudinal Propagation of Thermal Rossby Waves in Stellar Convection Zones
Authors: Rekha Jain, Bradley W. Hindman
Figure caption: Eigenfrequencies of modes trapped latitudinally and radially in the millstone domain are illustrated in Figure 4. The frequencies are plotted as a function of the azimuthal order. Each distinct color corresponds to a different latitudinal order λ, as indicated in the legend. The solid curves show the prograde-propagating thermal Rossby waves, whereas the dashed curves are for the retrograde inertial waves. The dotted curves indicate the frequency where the lower turning point passes through the bottom boundary. Wave frequencies above the appropriate dotted curve have two turning points in the radial domain and have a wave cavity that is screened from the lower boundary condition. Frequencies below the dotted curve possess only an upper turning point in the domain and are reflected off the lower boundary.
Paper: Latitudinal Propagation of Thermal Rossby Waves in Stellar Convection Zones
Authors: Rekha Jain, Bradley W. Hindman
Figure caption: Dimensionless eigenfrequencies as a function of harmonic degree k  h   R ⊙ for a neutrally stable polytropic atmosphere with a finite depth of D = 200 Mm. The green solid line is the same as in Figure 1. For waves with latitudinal propagation (χ > 0), the uppermost and lowermost curves are for n = 0 modes lacking radial nodes in their pressure eigenfunctions. Each subsequent radial overtone (n = 1, n = 2, and so forth) lies slightly closer to zero frequency. Thus, there is a retrograde and prograde branch for each radial overtone. The solid cone of blue color is artificial and arises because the curves become so close together that they cannot be resolved in the image. The leftmost panel, which corresponds to pure zonal propagation, lacks the retrograde lower curves altogether.
Paper: Latitudinal Propagation of Thermal Rossby Waves in Stellar Convection Zones
Authors: Rekha Jain, Bradley W. Hindman
Figure caption: Illustration of two types of eigenfunction. The two curves show the normalized Lagrangian pressure fluctuation as a function of dimensionless height for a naturally trapped (red curve) and an untrapped thermal Rossby wave (blue curve). The trapped mode corresponds to a radial order of n = 3 and has two turning points in radius: an upper turning point that lies very near the upper surface and a lower turning point near k  h  z ≈ = −5. The wave cavity exists between these two turning points, and the eigenfunction decays exponentially with depth below the lower turning point. The untrapped wave has only a single turning point. It corresponds to a continuum mode that is launched from infinite depth, travels upwards, reflects off the upper turning point near the origin, and then travels back downwards. This specific continuum mode is prograde with a frequency ω/Ω = 0.5. Both eigenfunctions are computed for an angle of propagation of χ = 45°.
Paper: Latitudinal Propagation of Thermal Rossby Waves in Stellar Convection Zones
Authors: Rekha Jain, Bradley W. Hindman
Figure caption: Sketch showing the finite domain considered in Section 5.2. The outer surface of the Sun and the bottom of the convection zone are indicated in the meridional plane as orange circles. The waves are confined within the convection zone of depth D and within a latitudinal band of length L, which is the length of the chord that is tangent to the bottom of the Sun’s convection zone. The domain is periodic in the azimuthal direction with a circumference length of 2π  R ⊙. A meridional slice through the domain is shown as the gray box.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: (A) Summary of this work. We take the Schlegel et al. (1998, SFD) Galactic dust-reddening E(B − V) map (lower left) and reconstruct the extragalactic LSS, or the CIB (upper), which we subtract to obtain CSFD, a cleaned dust map with improved accuracy (lower right). The maps are in full-sky Galactic Mollweide projection with the Galactic center in the center and a histogram equalization color stretch. In the CIB map, gray areas mark regions without reconstruction (Galactic plane, Magellanic clouds, and M31), and the nontransparent areas indicate the most reliable regions for precision cosmology analyses. (B) Tomographic 1D (upper) and 2D (lower) statistics of the LSS imprints in SFD via cross-correlating with a set of reference galaxies and quasars in SDSS. The 1D estimator extracts the CIB-induced excess E(B − V) within 10′ of the references, and the 2D estimator measures the differential excess E(B − V) at a given characteristic scale θ  C  with a compensated filter, both as a function of redshift. (C) Same as panel (B), but for CSFD, showing no detectable LSS imprint.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Comparison between SFD, the corrected SFD (CSFD), the LSS correction term, and its error from left to right panels, respectively, over a 20° field centered on the Galactic coordinates (l, b) = (−50°, −80°) in Gnomonic projection. All maps are in the SFD E(B − V) unit, with a decreasing dynamic range from the left to right panels. The CSFD map is made to be LSS-free, i.e., CSFD = SFD − CIB. The white masks in the last panel, mostly around bright, red stars in this field, indicate the “noncosmology” areas where the LSS reconstruction, and thus SFD correction, is less reliable (Appendix A.3.1).
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Tomographic cross-correlation statistics, same as Figure 1(B) and (C), but for the reconstructed LSS/CIB map. The 1D statistics for SFD (from Figure 1(B)) are overlaid using blue data points in the upper panel. By construction, the reconstructed CIB map reproduces all statistics of the CIB embedded in SFD. Furthermore, the S/Ns in the former are much higher, highlighting the value of this foreground-free LSS product as a probe of the matter density field in the Universe.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Probability distributions of the per-beam, or per-resolution, element map values for the best reconstructed LSS map (black, and that without the AKARI point-source contribution in gray) and its corresponding error map (blue) in our cosmology area. Independent resolution elements are approximated using HEALPix N side = 512 pixels of ﹩6\buildrel{\,\prime}\over{.} 9﹩ each, similar to the beam size of SFD. The typical LSS correction is at the millimagnitude level, and the mean S/N is ∼2.5 for every resolution element.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Error map of the LSS/CIB reconstruction in the SFD reddening unit in full-sky Galactic Mollweide projection. The typical error is 0.2 mmag and slightly increases toward low latitudes due to increasing uncertainties in mostly the WISE-based LSS templates.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: (Left) HST F160W (H-band) image (black contours) with the dust-masked MGE model (red contours) overlaid. (Middle, top) The central 5″ of the HST H-band image. (Right, top) The inner 5″ of the HST F814W (I-band) image. The dust disk (with a diameter of ∼3.″9) is clearly visible in the I-band image, particularly to the east/northeast of the nucleus. (Middle, bottom) Contours of the inner 5″ of the HST H-band image (black) and the dust-masked MGE (red). The gray-shaded region was masked for the dust-masked MGE fit. The black contours are asymmetric on the east/northeast side of the disk, indicating that dust clearly diminishes the stellar surface brightness within the masked region. The asymmetry is no longer present in the red model contours. (Right, bottom) The inner 5″ of the ALMA CO(2−1) emission (blue) with the HST I − H image (black contours) overplotted. The blue ellipse in the lower left of the panel displays the size of the synthesized ALMA beam. The dust disk and CO(2−1) emission are co-spatial, with the dust disk’s diameter (∼3.″9) approximately the same size as the CO disk.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Location of the local compact galaxies with dynamical BH masses relative to the M BH–σ ⋆ (left), M BH–L bul (middle), and M BH–M bul (right) relationships (Kormendy & Ho 2013; McConnell & Ma 2013; Läsker et al. 2014; van den Bosch 2016; Saglia et al. 2016; Savorgnan 2016). The ALMA-based M BH for PGC 11179 measured in this work is shown as a blue diamond, along with the molecular gas-dynamical M BH determination for UGC 2698 (Cohn et al. 2021). The stellar-dynamical BH masses from integral field spectroscopy assisted by adaptive optics are displayed as red squares (Walsh et al. 2015, 2016, 2017). The shaded regions indicate the intrinsic scatter of the scaling relations. All of the galaxies are consistent with M BH–σ ⋆. We conservatively use the total luminosity and mass for each of the compact galaxies when plotting “bulge” quantities. As such, these estimates are upper bounds on the bulge measurements. NGC 1271, NGC 1277, and Mrk 1216, as well as PGC 11179, are positive outliers from the M BH–L bul and M BH–M bul relations. However, UGC 2698 is consistent with the M BH–L bul and M BH–M bul correlations within their intrinsic scatter.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: (Top row) PVDs built from the observed data cube (left), the best-fit fiducial model (middle), and the best-fit model with M BH fixed to 0 (right). (Bottom row) PVD residuals for the best-fit fiducial model (left) and the best-fit model with M BH fixed to 0 (right). The residuals are normalized by the noise and calculated as the standard deviation of an emission-free region of the observed data cube’s PVD. The PVDs were extracted along the major axis of the disk at a PA of 335.°7 east of north, with a width of 0.″22 that matches the geometric mean of the synthesized beam dimensions. The panels are mapped linearly to the colors of the scale bar. Our dynamical models are fit directly to the data cube, not to these PVDs. The PVDs are not used in the fit and are simply extracted from the data cube and the best-fit model cube.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Zeroth, first, and second moments from the PGC 11179 ALMA data cube (left) and the best-fit model (middle) within the fiducial elliptical fitting region. The synthesized ALMA beam is shown as a white ellipse in the upper left panel. The uncertainty of the moment one map, calculated from a 1000-iteration Monte Carlo simulation, is shown in the upper right, and the residual (data−model) of the first moment normalized by the uncertainty is shown in the bottom right. These maps are constructed on the original 0.″03 pixel−1 ALMA pixel scale. All panels are linearly mapped to colors given by the scale bars, with data and model maps for each moment shown on the same scale. Note that our dynamical models are fit directly to the data cube, not to these moment maps. The maps here are thus not used in the fit and are simply extracted from the data cube and the best-fit model cube.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Flux maps for each channel in the data cube, showing the data (black) with the best-fit fiducial model contours overlaid (cyan). The line-of-sight velocity, with the systemic velocity subtracted, is shown in the top left of each panel. The minimum and maximum fluxes plotted for both data and model are listed in the top left panel. The data and model are shown on the same logarithmic scale. The top left panel also displays a 1″ bar and a black ellipse showing the ALMA synthesized beam. Low levels of model flux extend beyond the data in a few of the highest velocity channels, matching the low-signal upturns seen in Figure 4. Nevertheless, in general, the model matches the observations quite well.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Corner plot of parameters from the fiducial model, showing their one-dimensional (1D; top edge) and 2D posteriors. Medians and 3σ confidence intervals are displayed with the 1D posteriors with a black solid line and dashed blue lines, respectively, with values listed above the 1D panels for each parameter. Contours in the 2D posterior panels correspond to 1σ, 2σ, and 3σ confidence levels. Our best-fit BH mass is M BH = (1.91 ± 0.04[ ± 0.11]) × 109 M ⊙ (1σ [3σ] statistical uncertainties). For the best-fit model, we take the median of each parameter’s posterior, resulting in ﹩{\chi }_{\nu }^{2}=1.458﹩.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Central surface brightness profiles of PGC 11179 along the major and minor axes as a function of the projected radius based on the H-band image (black circles), the minimally masked MGE (blue triangles), and the dust-masked MGE (pink pluses). We use the dust-masked MGE in our fiducial dynamical model.
Paper: ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, Akın Yıldırım, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Line profiles built from the down-sampled data cubes (black) and the best-fit model cubes (blue) at each pixel location in the fitting ellipse region. The noise in each channel is displayed as a shaded gray region. The velocity and flux ranges of each line profile panel are labeled on the x- and y-axis, respectively. The physical extent of the fitting region is also labeled on each axis. The black star labels the best-fit BH location. The model matches the observations quite well throughout the disk.
Paper: Constraining the Binarity of Black Hole Candidates: A Proof-of-concept Study of Gaia BH1 and Gaia BH2
Authors: Toshinori Hayashi, 利憲 林, Yasushi Suto, 靖 須藤, Alessandro A. Trani, 虎似 三努郎
Figure caption: Schematic illustration of a triple system configuration that we consider in the present paper. The orbital angles are defined with respect to the reference Cartesian frame whose origin is set to be the barycenter of the inner orbit. The left panel shows the inner and outer orbits, and the right panel defines various angles specifying the orientations of the total ( G  tot), inner ( G  in), and outer orbital angular momenta of the system ( G  out); the mutual inclination between the inner and outer binaries (i mut); the orbital inclinations of the inner (i in) and outer (i out) binaries with respect to  G  tot; the inclination of the line of sight with respect to  G  tot (I los); and the inclination of the outer orbit with respect to the observer’s line of sight (I obs). The time-dependent azimuthal angle of  G  out relative to the line of sight is ϕ(t).
Paper: Constraining the Binarity of Black Hole Candidates: A Proof-of-concept Study of Gaia BH1 and Gaia BH2
Authors: Toshinori Hayashi, 利憲 林, Yasushi Suto, 靖 須藤, Alessandro A. Trani, 虎似 三努郎
Figure caption: Examples of simulated RV curves and the residuals after removing the best-fit Kepler motion. The fittings are performed with RadVel (Fulton et al. 2018). We assume an equal-mass inner binary (m 1 = m 2 = m c/2) for both systems. The left and right plots assume Gaia BH1 with P in = 10 days and Gaia BH2 with P in = 50 days. The top panels show the total RV curve with e in = 0 (red) and e in = 0.2 (blue), and the middle and bottom panels plot the corresponding RV residuals, respectively.
Paper: Constraining the Binarity of Black Hole Candidates: A Proof-of-concept Study of Gaia BH1 and Gaia BH2
Authors: Toshinori Hayashi, 利憲 林, Yasushi Suto, 靖 須藤, Alessandro A. Trani, 虎似 三努郎
Figure caption: Contours of the characteristic semi-amplitude K short (black dotted), Equation (4) in the q 21 ≡ m 2/m 1−P in plane for Gaia BH1 (left) and Gaia BH2 (right). We assume coplanar triples (i mut = 0). The shaded region indicates dynamically unstable triples according to Equation (6). More accurate empirical predictions near the pericenter passage, ﹩{K}_{\mathrm{short}}{(1-{e}_{\mathrm{obs}})}^{-7/2}﹩, are plotted in red solid lines.
Paper: Constraining the Binarity of Black Hole Candidates: A Proof-of-concept Study of Gaia BH1 and Gaia BH2
Authors: Toshinori Hayashi, 利憲 林, Yasushi Suto, 靖 須藤, Alessandro A. Trani, 虎似 三努郎
Figure caption: Contours of the RV semi-amplitude changes Δ K  (red solid) and the mutual inclination i mut (black dotted) from nodal precession on P Ω—P in plane for Gaia BH1 (left) and Gaia BH2 (right). The light blue regions correspond to the dynamically unstable region from MA01. The green regions are excluded from the observed value of I obs; see Equation (24). For relatively large mutual inclination, i mut ≳ 50°, the predictions of these plots become less reliable because the ZKL oscillations become important.
Paper: Constraining the Binarity of Black Hole Candidates: A Proof-of-concept Study of Gaia BH1 and Gaia BH2
Authors: Toshinori Hayashi, 利憲 林, Yasushi Suto, 靖 須藤, Alessandro A. Trani, 虎似 三努郎
Figure caption: Mass ratio of inner BBH q 21 (dashed) and the corresponding planet mass M pl (solid) in RV signal semi-amplitude K s–period P s plane for Gaia BH1. We note that K s and P s are interpreted as RV semi-amplitude and period induced by a planet for the planet interpretation, while they are interpreted as ﹩{K}_{{\rm{s}}}={K}_{\mathrm{short}}{(1-{e}_{\mathrm{obs}})}^{-7/2}﹩ and P s = P in/2 for the BBH interpretation.