adsabs/AstroCLIMB huggingface dataset:
Paper: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Authors: Sayantan Auddy, Ramit Dey, Min-Kai Lin, Daniel Carrera, Jacob B. Simon
Figure caption: This schematic diagram shows the workflow of a typical BNN, along with how the uncertainty/errors propagate.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Total system W  r (Ca II K) (left) and W  r (Na I 5891) (right) versus projected distance from the associated host galaxy. Colored points show constraints from our ESI spectroscopy. Upper limits, indicated with open squares, are shown in cases for which W  r  < 3 ﹩{\sigma }_{{W}_{r}}﹩ and represent 3σ limits. Gray points show measurements reported in Straka et al. (2015) from their analysis of SDSS spectroscopy probing the parent sample of GOTOQs. We exclude absorbers that were flagged as blended by Straka et al. (2015). We also exclude any systems in which the Ca II K transition falls more than 20 Å blueward of the Lyα emission line of the corresponding QSO to avoid blending from the Lyα forest. Black solid lines show best-fit linear relations between log W  r  and R ⊥ (see Section 5.1), and medium gray contours show the inner ±34% of the locus of fits drawn at random from the posterior probability density function of each linear model. The light gray region extends the boundaries of the medium gray 1σ region by the best-fit value of σ  C  to approximately indicate the degree of intrinsic scatter implied by the data. Our W  r  measurements exhibit no apparent anticorrelation with increasing projected distance from the foreground host.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Left: distribution of log M */M ⊙ vs. R ⊥ for our sample. Points are color-coded by the R ⊥ value for each system across all panels, as indicated by the color bar at right. Middle: distribution of log M */M ⊙ vs. R ⊥/R eff,est for our foreground GOTOQ sample. Right: distribution of SFRlocal vs. log M */M ⊙ for our foreground GOTOQ sample. The SFR values shown here should be considered lower limits on the total SFR of each system due to fiber losses. The grayscale histogram shows the distribution of total SFR versus M * for all galaxies included in the MPA-JHU catalog of these values for SDSS DR7 (Brinchmann et al. 2004). The turquoise line shows a linear fit to the minimum in the galaxy distribution between star-forming and quiescent systems by Moustakas et al. (2013) for z = 0.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Absorption velocity offsets relative to z Hα  for Ca II (left) and Na I (middle) for each securely detected absorption system versus projected distance from the galaxy host. Systems fit with single velocity components are shown with solid light blue and orange squares. The primary and secondary components of systems fit with two velocity components are shown with light blue/orange squares outlined with dark blue/red and open squares outlined with dark blue/red, respectively. Error bars show the span of velocities included in the Δv 90 measurement for the Ca II K and Na I 5891 lines. The gray curves indicate the radial velocity required to escape an M  h  = 1010 M ⊙ halo (a conservative minimum escape velocity given the stellar mass distribution of our sample) as a function of total distance from the halo center. The projected velocity of all detected absorption is well below this threshold. The rightmost panel shows the distribution of best-fit b D values for all components in our Ca II (cyan) and Na I (orange) absorbers. The median value of each distribution is shown with a vertical dashed line.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Regions of five of our ESI GOTOQ spectra showing the locations of Ca II H & K and Na I λλ5891, 5897 transitions associated with the foreground galaxy. The velocity is defined relative to the GOTOQ redshift estimated from a Gaussian fit to its Hα emission as described in Section 4.1 (z Hα ). The gray horizontal line indicates the continuum level, and the gray shaded region shows the velocity window selected for computation of W  r , N aod, and Δv 90. The blue and red bars show the pixels that contain >5% of the total apparent optical depth of the line (determined by stepping inward from the profile edges), and the length of these bars corresponds to Δv 90. Best-fit profile models are shown with cyan (for Ca II) and orange (for Na I) curves for systems with significantly detected absorption (see Section 4.2 for details).
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Total system W  r (Ca II K) (left) and W  r (Na I 5891) (right) versus projected distance from the associated host galaxy, normalized by the galaxy’s estimated effective radius. Symbols, lines, and contours are as described in the Figure 4 caption. The relation between log W  r (Ca II K) and R ⊥/R eff,est for the combined ESI and SDSS sample has a slope m = −0.035+0.028 −0.030, indicative of a weak anticorrelation between these quantities. The relation between log W  r (Na I 5891) and R ⊥/R eff,est exhibits no significant anticorrelation.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Fitted absorption velocity offsets relative to z Hα  for securely detected Ca II systems versus those for securely detected Na I systems. Error bars show the uncertainties in these fitted values. Absorbers fit with single velocity components in both transitions are shown with solid blue squares. Absorbers in which Ca II was fit with one component and Na I was fit with two components are indicated with solid blue and open squares outlined in orange. Absorbers in which Na I was fit with one component and Ca II was fit with two components are indicated in a similar fashion, as listed in the legend. Velocities for absorbers in which both ions were fit with two components are shown with open red squares.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Top row: total system column density of Ca II (left) and Na I (right) versus projected distance from the associated GOTOQs. Open squares with downward arrows represent 3σ upper limits calculated using the apparent optical depth method. The filled boxes indicate the ±34th percentile Wilson score confidence intervals, with respect to the right axes, for the covering fraction of absorbers having ﹩\mathrm{log}\,N(\mathrm{Ca}\,{\rm\small{II}})\gt 12.5﹩ and ﹩\mathrm{log}\,N(\mathrm{Na}\,{\rm\small{I}})\gt 12.0﹩, respectively. Bottom row: same as above, vs. R ⊥/R eff,est.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: SDSS gri color imaging of all GOTOQs for which we have obtained Echellette Spectrograph and Imager (ESI) spectroscopy (York et al. 2000). Each panel is 25″ × 25″. The images are labeled with the corresponding GOTOQ ID at the upper left. The dashed white circle indicates the size of the 3″ diameter fiber used for the SDSS spectroscopy of each system.
Paper: On the Kinematics of Cold, Metal-enriched Galactic Fountain Flows in Nearby Star-forming Galaxies
Authors: Kate H. R. Rubin, Christian Juarez, Kathy L. Cooksey, Jessica K. Werk, J. Xavier Prochaska, John M. O'Meara, Joseph N. Burchett, Ryan J. Rickards Vaught, Varsha P. Kulkarni, Lorrie A. Straka
Figure caption: Total system column density of Ca II versus that of Na I in individual GOTOQ sight lines. Sight lines along which we do not securely detect one or both of these ions are indicated with open squares placed at the corresponding 3σ upper limit. The purple filled region indicates the range in the average ratio N(Na I)/N(Ca II) observed toward high Galactic latitude sight lines probing the Milky Way by Murga et al. (2015).
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Detailed portions of the K2 data power spectrum of PG 1159-035 illustrating some Lorentzian fits as red lines. The frequency is in microhertz and the power is in units of mma2 (1 mma = 1 ppt). All plots have the same frequency range of 4 μHz, but different power ranges. In the top panel, we show some modes whose HWHMs are very close to the frequency resolution and, in the bottom panel, we show those modes with the widest HWHMs.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Asymmetry of the ℓ=1 modes as a function of the radial node k. The height of the square markers corresponds to the internal uncertainties calculated by MCMC simulation. The error bars indicate the uncertainties obtained by the Lorentzian fit.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Normalized weight function of the k = 16 mode (in black) vs. the normalized stellar radius. The chemical composition profiles are also indicated by lines with different colors. Inset: the same quantities as in the main figure, but as a function of the negative logarithm of the outer mass fraction.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: HWHM of the Lorentzian fit to the significant peaks in the FT of PG 1159-035 in microhertz vs. their periods in seconds. The horizontal blue dashed indicates the spectral window HWHM of the K2 data.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: K2 data FT in the range of asymmetric modes. Vertical blue lines indicate the component m = 0 of the ℓ = 1 model calculated in Section 6.1; similarly, the red ones indicate the component m = 0 of the ℓ = 2 model. The red horizontal dashed line indicates the fap limit.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: The panels show detailed portions of the K2 FT centered in the m = 0 frequency of the asymmetric modes. The red dashed lines indicate the 〈δ ν rot,1〉 frequency spacing averages.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: K-S test applied to our list of independent frequencies. There are six significant peaks: two of them correspond to ΔΠ1 and ΔΠ2 values, and the others are multiples of these.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Observed periods sequences for ℓ = 1 (blue line) and ℓ = 2 (red line) modes from K2 data.
Paper: Kepler and TESS Observations of PG 1159-035
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, Alejandro H. Córsico, J. E. S. Costa, J. J. Hermes, S. D. Kawaler, Keaton J. Bell, M. H. Montgomery, J. L. Provencal, D. E. Winget, G. Handler, Bart Dunlap, J. C. Clemens, Murat Uzundag
Figure caption: Same as Figure 12, but for the k = 56 mode.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The best-fitting wavelength of the O VIII line (top subplot) and the N VII line (bottom subplot) vs. the super-orbital phase. The observations with XMM-Newton during the 2020 campaign, and previously, are shown in distinct colors. The red dashed horizontal lines indicate the rest-frame wavelengths of the two transitions.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The 1D velocity (left y-axes) and FWHM widths (right y-axes) of the Fe XXV (top panel) and O VIII/N VII (bottom panel) lines vs. the super-orbital phase. The right y-axis on the bottom panel only contains the FWHM width of the O VIII line. The observations with XMM-Newton during the 2020 campaign are shown in black, archival XMM-Newton observations are shown in blue, and Chandra observations are shown in red.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: RGS spectrum (RGS 1 and 2 stacked for visual purposes) from the full 100 ks long observation 0865440401 (top panel), fitted with the full spectral model. Notable spectral components and features are described with labels. The red shaded region was ignored in this analysis (Appendix B). The bottom subpanel shows the ratio residuals to the best-fitting model.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The observed luminosity of the broad Fe K line with respect to the super-orbital phase (left subplot) and the observed Her X-1 luminosity (right subplot). The observations with XMM-Newton during the 2020 campaign, or previously, are shown in distinct colors. The line could not be constrained in any Chandra observation.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The broad Fe L line (1 keV residual) width vs. the super-orbital phase (left subplot) and the observed Her X-1 luminosity (right subplot). The observations with XMM-Newton during the 2020 campaign, previously, and with Chandra are shown in distinct colors.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: Left panel: the best-fitting FWHM line width of the O VII(i) line vs. its observed luminosity. Right panel: FWHM line width of the N VI(i) line vs. its observed luminosity. The left y-axes on each panel show the line widths in Å, while the right y-axes show the velocity widths in kilometers per second.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The observed luminosity of the narrow Fe I line vs. the super-orbital phase. The observations with XMM-Newton during the 2020 campaign, or previously, as well as Chandra observations, are shown in distinct colors.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The observed luminosity of the broad Fe L line vs. the observed luminosity of the broad Fe K line. The observations with XMM-Newton during the 2020 campaign, and previous observations, are shown in distinct colors.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: The broad Fe K line width vs. the observed Her X-1 luminosity. The observations with XMM-Newton during the 2020 campaign, or previously, are shown in distinct colors. The line could not be constrained in any Chandra observation.
Paper: A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Authors: Ling-Lin Zheng, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Sen-Yu Qi, Fan Yang, Song Wang, Liang Wang, Zhong-Rui Bai, Haotong Zhang, Chun-Qian Li, Jian-Rong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Figure caption: The first panel (from top to bottom) shows the Lomb–Scargle power peak. The second panel displays the TESS light curve folded with an orbital period of 0.600303 days. The black dots are binned over ten violet dots. The third panel shows the radial velocities folded by the period of 0.600303 days. The black curve is the best-fitting radial-velocity curve with a semi-amplitude of ﹩K\,=\,{124.4}_{-1.1}^{+1.0}﹩ km s−1. The pink dots represent the data collected from LAMOST, and the dark red dots are from P200. The errors of the photometric data are too small to be shown in the light curve, and the errors of the radial velocities are shown with the short bars over the dots (see the third panel). The residuals in the fourth panel are obtained by subtracting the observed radial velocities from the best-fit model (Equation (3)). It should be noted that the eccentricity is fixed to zero when fitting the radial velocities.
Paper: A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Authors: Ling-Lin Zheng, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Sen-Yu Qi, Fan Yang, Song Wang, Liang Wang, Zhong-Rui Bai, Haotong Zhang, Chun-Qian Li, Jian-Rong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Figure caption: The SED of J1729+6529. The dark violet dots are the photometric data collected from GALEX, SDSS, APASS g and r bands, APASS Johnson B and V, Pan-STARRS, Gaia, TESS, 2MASS, and ALLWISE. The gray circles are the synthetic fluxes from the best-fitting theoretical spectral template. The black arrow indicates an upper limit of the WISE W4 band. The green curve is the best-fitting model. The lower panel shows the residuals calculated by the difference between the photometric and the synthetic fluxes divided by the synthetic fluxes. It should be noted that NUV, W3, and W4 were not involved in the SED fitting process. The residual value of the NUV flux is too large to be displayed properly in the lower panel.
Paper: A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Authors: Ling-Lin Zheng, Wei-Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Sen-Yu Qi, Fan Yang, Song Wang, Liang Wang, Zhong-Rui Bai, Haotong Zhang, Chun-Qian Li, Jian-Rong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Figure caption: The LAMOST coadd spectrum (blue and pink curves) of J1729+6529 and the best-matching template (black curves). The upper and lower panels are for the blue and red arms, respectively.