adsabs/AstroCLIMB huggingface dataset:
Paper: The Dipole Instability in Gravitational N-body Systems: A Natural Explanation for Lopsidedness and Off-centered Nuclei in Galaxies
Authors: Shashank Dattathri, Frank C. van den Bosch, Martin D. Weinberg, Uddipan Banik
Figure caption: Mock kinematic maps of our fiducial simulation at three key snapshots, showing the mean velocity v0 (top panels), velocity dispersion σ (bottom panels), and the location of the cusp (white cross in all panels). At T = 0, the system is isotropic with v0 ≈ 0 everywhere, and the central minimum in the σ map corresponds to the cusp. Once the cusp is dislodged from the center due to the l = 1 mode, the local minimum in σ is now off-centered, as seen in the subsequent two panels. In addition, the cusp’s line-of-sight motion is clearly visible as a positive (at T = 150) or negative (at T = 153) v0 feature.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: CMD for the ≈400 candidate members in our initial Coma Ber catalog, a merger of preexisting catalogs for which we updated the astrometry and photometry to the Gaia DR3 values. Spectral types are indicated along the top axis for reference. The filled cyan stars appear in more than one of these catalogs. As discussed in the text, this CMD shows important contamination from background giants lacking parallaxes that were included in the A. L. Kraus & L. A. Hillenbrand (2007) catalog. These stars are identified as nonmembers in Figure 3.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: An illustration of the discriminating power of Gaia data: DR3 parallax distribution for the 379 stars in our initial Coma Ber catalog. Stars to the left of the ϖ = 8 mas line are likely nonmembers, with the clump with ϖ ≲ 2 mas likely to be background giants that contaminated the A. L. Kraus & L. A. Hillenbrand (2007) catalog because of the cluster’s relatively low proper motion compared to other field stars.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Flowchart illustrating our approach to classifying the 379 stars in our initial Coma Ber catalog. We first followed the path indicated by the thick arrows, which allowed us to define a velocity core of 140 high-confidence members for the cluster, before considering the membership status of stars either lacking RVs or whose RVs have large errors (>5 km s−1).
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Period analysis for Gaia DR3 3957357582063045120. Panels on the top row show TESS data (Cycles 23 and 49); those on the bottom row show ZTF data. The leftmost panels show all available photometric data for both surveys (at the time of our analysis), highlighting the years-long coverage provided by ZTF. The center-left panels show representative segments of length equal to a single TESS sector (≈27 days), highlighting the relative sparseness of the ZTF light curves. The center-right panels show Lomb–Scargle periodograms for TESS Sector 23 and for the full ZTF light curve. The rightmost panels present the phase-folded light curves. Despite differences in data quality (total baseline, duration of each observing sector/season, cadence, precision, angular resolution), we obtain a Prot = 9.17 days for these M3 stars from both data sets.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Top—Positions for the 140 stars confirmed as high-confidence members of Coma Ber based on their UVW velocities (see Figure 4). We used this distribution to test the membership of the 143 stars with ϖ > 8 mas but lacking or having unreliable RVs in our sample. Bottom—Positions for those 143 stars. The 122 stars whose positions and proper motions all fell within the range defined by the astrometry for the UVW high-confidence members were also classified as high-confidence members and are shown as filled gold stars. The 21 purple points are positional and/or proper-motion outliers, and are classified as candidate members until their RVs can be obtained.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: U, V, and W velocities for the 181 stars with ϖ > 8 mas and Gaia RV measurements in our initial catalog. The filled gold stars are the 140 stars that form the cluster’s velocity core and are classified as high-confidence members, while the nine light blue points are UVW outliers and therefore candidate nonmembers. We used the proper motions of the 140 high-confidence members to select members from the 119 stars with ϖ > 8 mas but lacking RVs, and from the 24 stars having RVs with RVerr > 5 km s−1 (see Figure 5).
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Color–period diagram for Coma Ber members before (left panel) and after (right) our TESS and ZTF measurements. In the left panel, the purple points are stars with Prot measured by A. Collier Cameron et al. (2009), the beige crosses are Prot from R. C. Terrien et al. (2014), and the two filled cyan squares are stars with periods published by both sets of authors. There are 24 stars on this plot, mostly G and K stars. In the right panel, we show the updated Prot distribution for the cluster, which now includes 161 stars. We highlight single members with orange stars, and candidate/confirmed binaries with filled gray triangles.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Updated Gaia CMD for Coma Ber. Using velocity and astrometric cuts, we identify 262 stars as high-confidence members (filled gold stars), 29 stars as candidate members (purple points), nine as likely nonmembers (green pluses), and 79 as nonmembers (gray crosses).
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Coma Ber CMD showing likely single stars (filled star symbols) and known/possible binaries (filled triangles). The orange symbols are high-confidence members, and the purple ones are candidate members. In addition to spectroscopic binaries (SBs) identified in the literature, we flag as possible binaries stars for which the Gaia RUWE ≥ 1.4. In total, 230 of our Coma Ber members are likely single stars, and 61 are spectroscopic and/or candidate binaries.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Prot from TESS vs. Prot from ZTF (open black stars), A. Collier Cameron et al. (2009, purple points), and R. C. Terrien et al. (2014, beige crosses) for the 66 Coma Ber stars with more than one Prot measurement. The solid gray line is the 1:1 match, and the shaded area is the ±10% difference range. The overall agreement between the measurements is excellent, with a median difference <1%.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: PARSEC 675 Myr isochrone overlaid on the CMD for likely single high-confidence members of Coma Ber. We zoom in on the main-sequence turnoff, where the distinction between the different isochrone predictions is most evident.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: wdwarfdate outputs for Gaia DR3 4008511467191955840: its progenitor’s main-sequence age, its cooling age, its total age, its progenitor’s initial mass, and its mass.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: LHα/Lbol (left) and LX/Lbol (right) as a function of Ro for likely single members of Coma Ber. Stars are color coded by their M⋆ according to the color bar in the left panel. The solid black line is the maximum a posteriori MCMC fit, and the gray lines are 200 random samples from the posterior probability distributions. We assumed a flat saturated regime described by ﹩{({L}_{i}/{L}_{{\rm{bol}}})}_{{\rm{sat}}}﹩ (where Li is either LHα or LX) and Ro,sat, and an unsaturated regime described by a power law of index β. The results of the fit for these three parameters are given in each panel. The dashed black lines are the results of a similar analysis for single members of Praesepe (A. Núñez et al. 2024), which in the right panel also includes a supersaturated regime (Ro ≲ 0.01). We show in Appendix B the marginalized posterior probability distributions from the MCMC analysis for our fits.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Color–period (left column) and mass–period (right column) diagrams for likely single members of Coma Ber (filled orange stars) and Praesepe (open white squares; data from A. Núñez et al. 2024). In each column, the bottom and top panels show the same data; we plot the Prot linearly at the bottom and logarithmically on the top. The agreement in the Prot distributions for the hotter (F through early M) stars in our samples is very clear in both panels on the left; the offset in the distributions for the mid and late M dwarfs is most obvious in the top left panel. To produce the two panels in the right column, we have transformed the Gaia colors into masses. The M dwarf Prot distributions now agree (as is most evident in the top right panel), whereas the distributions for the ≈solar-mass stars are offset, as is most clearly visible for the 0.6–0.9 M⊙ stars in the bottom right panel.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Measured Hα EW as a function of (GBP − GRP) for low-mass stars in Coma Ber. Negative EW values correspond to emission. The left panel distinguishes between likely single stars (filled orange stars) and known and candidate binaries (filled gray triangles). Blue × symbols denote stars for which we could not measure an EW and to which we assigned EW = 0 Å. The right panel distinguishes between single members with known Prot (filled colored stars, following the inset color bar) and single members without a measured Prot (gray circles). For clarity, we excluded from the panels one outlier star with (GBP − GRP) = 2.8 mag and EW = −76 Å. We also excluded stars with (GBP − GRP) < 0.5 (spectral types earlier than ≈F5), as they are not relevant to our analysis.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Measured Hα EW as a function of (GBP − GRP) for single members of Coma Ber (orange stars) and of Praesepe (white squares; data from A. Núñez et al. 2024). We exclude the same outlier in Coma Ber as in Figure 15. The distributions for the two clusters are remarkably similar, with stars earlier than ≈M2 being inactive, and later stars showing a comparable range of Hα emission at a given color. Interestingly, the relative shift in the Prot distribution for the later M dwarfs seen in the top left panel of Figure 16 does not appear to have an equivalent in this space.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Top—Spectral energy distribution for Gaia DR3 4001560041148002432. The error bars are the photometry available for the WD, including GALEX far- and near-ultraviolet (in red, and not used for fitting), SDSS u, and Pan-STARSS griz. The black dots are the derived flux values from the best-fit model to the ugriz data, and the numbers shown correspond to the parameters for this best-fit pure-hydrogen model atmosphere. These parameters were used to create a model spectrum for the WD. Middle—The model spectrum is plotted in red, with the LAMOST spectrum in black, for a window centered on the Hα line. The match is clearly poor, with the model predicting a far broader absorption feature than what is observed. Bottom—The LAMOST spectrum for the WD.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Color–period (left panel) and color–EW (right panel) diagrams for likely single members of Coma Ber (filled colored stars) and Praesepe (open white squares). In the left panel, Coma Ber stars are color coded by their Hα EW, and in the right panel, by their Ro. Stars shaded in gray do not have an EW measurement (left panel) or a calculated Ro (right panel). In the left panel, the dashed line and shaded area indicate Ro,sat and one standard deviation, respectively (see Figure 19), which separates saturated stars (Ro < Ro,sat) from unsaturated stars (Ro > Ro,sat) in LHα/Lbol space. The white shade in the color bar of the right panel corresponds to Ro,sat (log Ro,sat = −0.80 ± 0.09).
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: LX/Lbol as a function of (GBP − GRP) for likely single members of Coma Ber (filled orange stars) and of Praesepe (open white squares; data from A. Núñez et al. 2024). For most stars, the uncertainty in LX/Lbol is smaller than the size of the symbol. While there are clear gaps in the X-ray coverage for Coma Ber, the measurements for the F and G stars on one hand and for the mid and late M dwarfs on the other appear consistent with those for these same stars in Praesepe. And, as with the Hα measurements in Figure 17, the distributions for those cooler stars do not appear offset from each other, unlike for their Prot.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Five representative spectra obtained with the Hiltner 2.4 m telescope at MDM Observatory, each labeled with the instrument used and the star’s DR3 identifier and our estimate of its mass. The spectra are normalized to the flux at 6555 Å and offset for plotting purposes. The right panel shows close-ups of the Hα line; the dotted line is at 6563 Å, the position of the line core. These spectra illustrate the change from Hα absorption to strong emission as we go from solar-like to late M stars.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Stacked histogram illustrating our excellent optical spectral coverage for Coma Ber. The orange bars correspond to the stars for which we have at least one good quality optical spectrum with which to measure the Hα EW (246 of 291 cluster members). Gray bars indicate the members without spectra.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: From top to bottom: observed 2−4 GHz luminosity (L2−4; from Epoch 1, if in both epochs), projected physical offset from the host galaxy centroid (ΔS), and host galaxy stellar mass (M⋆,Host) against host galaxy redshift (z) for the parent AGN (gray-scale color map) and offset AGN candidate (red dots) samples. The solid (orange) lines indicate (from top to bottom) the limits imposed by the VLASS imaging sensitivity (completeness limit of 3 mJy beam−1), the VLASS spatial resolution (2﹩\mathop{.}\limits^{^{\prime\prime} }﹩5), and the stellar mass completeness based on the SDSS imaging sensitivity. The redshift distributions are shown at the top for the parent AGN (black, dashed) and offset AGN candidates (red, solid).
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Optical counterpart stellar masses (M⋆,OA) against host galaxy stellar masses (M⋆,Host) for the offset AGN candidates (Section 2.4). The circles and downward-facing triangles denote the sources with detections and upper limits, respectively, color coded by host galaxy redshift (z). The dashed (black) line denotes the median M⋆,Host/M⋆,OA value for the subset with optical detections, and values of 1/1, 10/1, 100/1, and 1000/1 are indicated by dotted (gray) lines. The M⋆,OA upper limits imply mass ratios up to 100/1 or larger, demonstrating how the selection is not biased toward major mergers.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Observed 2–4 GHz luminosities (L2−4) vs. those predicted from the matched host galaxy (from star formation and supernovae/supernovae remnants: ﹩{L}_{2-4,{\rm{SF}}+{\rm{SN}}}﹩) for the VLASS AGN selected in Section 2.3 from Epochs 1 (left) and 2 (right). The (red) solid, dashed, and dotted lines denote L2−4 = [1, 10, 100] × ﹩{L}_{2-4,{\rm{SF}}+{\rm{SN}}}﹩, respectively. For both epochs, 99% and 99% exceed the predictions by factors of 10 and 100, respectively. In each of Epochs 1 and 2, all AGN exceed the predictions by a factor of >5 and 6, respectively.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Observed 2−4 GHz luminosities normalized by host galaxy stellar mass (L2−4/M⋆,Host) against the 4000 Å break index (D4000) for the subset of VLASS AGN selected in Section 2.3 with measurements of D4000 (J. Brinchmann et al. 2004; C. A. Tremonti et al. 2004) for Epochs 1 (left) and 2 (right). The dashed (red) line shows the AGN selection threshold used in P. N. Best & T. M. Heckman (2012), where 90% of the AGN from our selection pass this threshold for both epochs.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Cutouts of the WD’s Balmer lines fit using a 1D model for the WD atmosphere. The three-dimensional corrections in both Teff and log g given in P.-E. Tremblay et al. (2013) have been applied to take into account hydrodynamical effects. This fit produces significantly different values for the WD’s fundamental properties.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Marginalized posterior probability distributions from the MCMC analysis of our Ro–LHα/Lbol model using emcee for single members in Coma Ber. The parameter values of the a posteriori model are the peaks of the 1D distributions; the vertical dashed lines approximate the median and 16th, 50th, and 84th percentiles. The 2D distributions illustrate covariances between parameters; the contour lines approximate the 1σ and 2σ levels of the distributions.
Paper: Crowning the Queen: Membership, Age, Rotation, and Activity for the Open Cluster Coma Berenices
Authors: M. A. Agüeros, J. L. Curtis, A. Núñez, C. Burhenne, P. Rothstein, B. J. Shaham, K. Singh, P. Bergeron, M. Kilic, K. R. Covey, S. T. Douglas
Figure caption: Same as Figure 23, but for our Ro–LX/Lbol model.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Fraction of galaxies with an offset AGN (fOA = NOA/NGal; corrected for background/foreground contamination; Section 4.1) against observed AGN 2−4 GHz luminosity (L2−4). In each bin, NGal is the number of parent sample galaxies for which a VLASS detection could be made down to the lower luminosity limit of the bin (L2−4,Lo), and NOA is the number of offset AGN in the parent sample with L2−4 > L2−4,Lo. Vertical error bars denote binomial uncertainties, and horizontal errorbars denote the bin widths. The results are divided into bins of discrete host galaxy stellar mass (M⋆,Host). Separate panels show subsets for three limiting redshifts for which the parent samples are mass-complete (Figure 4). At all values of z and M⋆,Host, the occupation fraction declines with luminosity, reflecting the distribution of radio AGN in galaxies. The values of fOA (and their errors) that are shown in this figure are available as the Data behind the Figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)