adsabs/AstroCLIMB huggingface dataset:
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Monopole in configuration space for both the CMASS NGC and the mock catalogs, using the optimal values of σ scat obtained through the SHAM procedure. Top: the case of COLA mocks with different z init, where da is chosen as da = 1/(1 + z init). Bottom left: the case of COLA mocks with different z init, while setting da to a constant value of 1/120. Bottom right: the case of COLA mocks with a fixed initial redshift of z init = 29 while varying the value of da. In all panels, the black line corresponds to the monopole of the CMASS NGC catalog, with 2σ  uncertainties (gray shaded) computed from 1000 PATCHY mocks. The monopoles of the GADGET mock catalog (solid triangle) and the COLA mocks (empty squares) are shown for comparison.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Top: comparison of the power spectrum multipoles of ℓ = 0, 2, and 4 for CMASS NGC and GADGET mock as well as COLA  mock with z init = 29, 49, 59, and 119 when the time stride da = 1/N step. The shaded region represents the 2σ statistical uncertainty obtained from measuring 1000 PATCHY mocks for each multipole. Bottom: relative error between the mocks and CMASS NGC with respect to the 1σ statistical uncertainty, defined by ﹩({P}_{{\ell }}^{\mathrm{mock}}-{P}_{{\ell }}^{\mathrm{NGC}})/\sigma ﹩ for ℓ = 0, 2, 4.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Comparison of three-point statistics ζ(r 1, r 2, r 3) between the observation data CMASS NGC and mock catalogs. The shaded area in the top panels represents the 2σ uncertainties originating from the initial randomness, which are estimated using PATCHY mock. r 1 and r 2 are both fixed at 15.5 h −1 Mpc, and r 3 varies from 5 to 31 h −1 Mpc.The bottom panels show the relative errors between the mock catalogs and CMASS NGC with respect to the 1σ statistical uncertainty, defined by (ζ mock − ζ NGC)/σ. Same as in Figure 9, three different COLA settings are used for comparison.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Top: comparison of the power spectrum multipoles of ℓ = 0, 2, and 4 for CMASS NGC and GADGET mock as well as COLA mock with z init = 29, 59, and 119 when da = 1/120. The shaded region represents the 2σ statistical uncertainty obtained from measuring 1000 PATCHY mocks for each multipole. Bottom: relative error between the mocks and CMASS NGC with respect to the 1σ statistical uncertainty, defined by ﹩({P}_{{\ell }}^{\mathrm{mock}}-{P}_{{\ell }}^{\mathrm{NGC}})/\sigma ﹩ for ℓ = 0, 2, 4.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Top: comparison of the power spectrum multipoles of ℓ = 0,  2, and 4 for CMASS NGC, GADGET mock and COLA mock with da = 1/30,  1/60, and 1/120 when z init = 29. The shaded region represents the 2σ statistical uncertainty obtained from measuring 1000 PATCHY mocks for each multipole. Bottom: relative error between the mocks and CMASS NGC with respect to the 1σ statistical uncertainty, defined by ﹩({P}_{{\ell }}^{\mathrm{mock}}-{P}_{{\ell }}^{\mathrm{NGC}})/\sigma ﹩ for ℓ = 0,  2,  4.
Paper: Fast Generation of Mock Galaxy Catalogs with COLA
Authors: Jiacheng Ding, Shaohong Li, Yi Zheng, Xiaolin Luo, Le Zhang, Xiao-Dong Li
Figure caption: Angular dependence of ξ on μ according to Equation (18), with s integrated out. The results are only presented for ﹩\mu \gt {\mu }_{\min }﹩, where ﹩{\mu }_{\min }=0.12﹩. For comparison, the gray shaded area represents the 2σ statistical uncertainty estimated using 1000 PATCHY mocks. The bottom panels are the relative errors between the mock catalogs and the observation with respect to the 1σ statistical uncertainty, defined by ﹩({\xi }_{{\rm{\Delta }}s}^{\mathrm{mock}}-{\xi }_{{\rm{\Delta }}s}^{\mathrm{NGC}})/\sigma ﹩. The angular dependence for GADGET mock and the three different COLA settings are displayed from left to right for comparison.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: The histograms for the redshift (left) and r-band magnitude (right) from the DESI Legacy survey are shown. The top panels display the total parent sample (gray) and the three crossmatched groups (blue, orange, and green). The middle panels represent the distributions of CL AGNs found in the three crossmatched groups. The bottom panels show the distributions of CL AGNs with the transition states of turn-on (dark blue) and turn-off (maroon). Note that the r-band magnitude refers to the mean magnitude obtained from the image of the DESI Legacy Survey, which encompasses the period from 2014 to 2018.
Paper: Changing-look Active Galactic Nuclei from the Dark Energy Spectroscopic Instrument. I. Sample from the Early Data
Authors: Wei-Jian Guo, Hu Zou, Victoria A. Fawcett, Rebecca Canning, Stephanie Juneau, Tamara M. Davis, David M. Alexander, Linhua Jiang, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Satya Gontcho A Gontcho, Klaus Honscheid, Theodore Kisner, Anthony Kremin, Martin Landriau, Aaron Meisner, Ramon Miquel, John Moustakas, Jundan Nie, Zhiwei Pan, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Małgorzata Siudek, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Jipeng Sui, Gregory Tarlé, Zhimin Zhou
Figure caption: Distribution of CL AGNs in parameter spaces of Max(N  σ ) vs. R (left panel) and parameter spaces of R vs. ﹩{F}_{\sigma ,\dim }﹩ (right panel). The solid scatters represent the measurements of all AGN parameters (the Hβ or Mg II lines in the spectrum). The hollow triangles and pentagons represent the final CL AGNs and CL candidates after the second stage of VI. The gray shading shows the parameter thresholds for CL AGNs. The dashed gray lines are the corresponding boundaries.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: The rms measured at 1 and 2 times the primary beam FWHM, i.e., σ 1 (left panels) and σ 2 (right panels), respectively, as a function of peak flux density (S  p ) of the brightest source in primary beam-uncorrected SPW9 (top panels) and SPW2 (bottom panels) images. In the cases for which an off-axis source is brighter than the central radio source (i.e., Class-B pointings), the points have been color coded with respect to the distance of the source from the pointing center. In each panel, the three vertical lines from left to right mark median flux densities for (i) central source in Class-B, (ii) central source in all (391), and (iii) off-axis source in Class-B pointings. Horizontal dashed lines mark theoretical and observed rms noise values. For clarity, in the top- and bottom-left panels, three and four points with σ 1 greater than 100 and 200 μJy beam−1 have been omitted, respectively.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Cumulative distribution function (CDF) of pixels in the rms maps of 391 pointings, arranged as per Class-A.1 to Class-A.4, and Class-B (top five panels). The profiles from mean- and median-stacked rms images are shown in the bottom two panels. The dashed–dotted lines in the top five panels correspond to ‘representative’ pointings selected (see the end of Section 3.1). The curves with lowest rms for Class-A.1, -A.3, and -B correspond to four pointings with double the integration time (see the text for details).
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Sky distribution of the 391 MALS pointings observed in the L band shown in Mollweide projection in equatorial coordinates (J2000). The dotted line marks the Galactic plane.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Image cutouts (﹩3^{\prime} \times 3^{\prime} ﹩) exhibiting typical morphology of radio sources detected in primary beam-corrected SPW9 images. The contour levels are shown at 3 × isl_rms × (−1, 1, 2, 4, 8, 16,...) mJy beam−1. The FWHM of major and minor axes of the fit to the source are shown using solid yellow, for S_Code=S, and dashed orange ellipse, for S_Code=M (see Table 3 for details). The individual Gaussian components fitted—six in A, one in B, seven in C, and four in D—to model the emission are shown as solid magenta ellipses. Note that in panel B, for an S_Code=S type source, the yellow ellipse coincides with the magenta ellipse representing the fitted single-Gaussian component. In panels A and B, another unrelated compact source, in a different island, is also detected. The isl_rms used for plotting contours in these panels is the average of the two islands. The restoring beams are shown as filled ellipses at the bottom-left corner of the images.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: The reliability envelope used to select compact sources from a sample of isolated, single-component sources (S/N > 8) detected in MALS SPW9 images. The black “×” symbols mark the lower envelope encompassing 95% of these sources with total-to-peak flux density ratio < 1. The solid red line represents the fit to “×” and the reflected envelope. Out of 22,425 sources, 15,834 (∼70%) lie inside the envelope.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Astrometric comparison of 345 targets and 64 gain calibrators from MALS with NVSS (left) and 1150 compact sources detected in four twice-observed MALS fields (right). The dashed lines mark median offsets. The circle represents half of the average SPW9 restoring beam FWHM (8″). For clarity, three points have been omitted from the left panel (see the text for details). In the right panel, sources with 8 ≤ S/N ≤15 are color coded. The histogram distributions of ΔR.A. and Δdecl. and Gaussian fits to these are also shown.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Median-stacked rms maps for various pointing classes (indicated in the top-right labels) based on primary beam-uncorrected SPW9 images. The blue and red dotted circles represent diameters of one and two times the primary beam FWHM where σ 1 and σ 2 are measured. The color-bar range is saturated at the peak intensity (95 μJy beam−1) of stacked Class-A.1 map. The contours correspond to 25% (green), 30% (gray), 50% (cyan), and 80% (yellow) of the same peak intensity.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: The fraction of “negative” sources with respect to the sources from actual images as a function of distance in three different S/N bins. The bin size is 2′. Error bars denote 1σ Poissonian uncertainties. The shaded portion marks regions with a high false detection rate. Note the absence of artifacts with S/N > 15 in most of the bins, except near the center and at the edges.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Examples of S/N distribution of pixels in the residual images generated by PyBDSF for each class of pointings discussed in Section 3.1. The sigma-clipped Gaussian (﹩{{Ae}}^{-{(x-c)}^{2}/2{\sigma }^{2}}﹩) fitted to the distribution using only the S/N range marked using the dotted vertical lines is also shown.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: MeerKAT primary beam-corrected L-band SPW9 image centered on the radio source J095123.18-325554.8 (Class-A.1; S p  ∼ 153.0 mJy beam−1), with robust=0 weighting. The rms in the vicinity of the central source is 40 μJy beam−1, and the restoring beam is 7.″7 × 6.″2 with a position angle of −16°. The dynamic range is ∼3800.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: MeerKAT primary beam-corrected L-band image centered on the radio source J121211.89-373826.9 (Class-A.3; S p  ∼ 351.9 mJy beam−1), with robust=0 weighting. The rms in the vicinity of the central source is 50 μJy beam−1, and the restoring beam is 9.″0 × 6.″5 with a position angle of −24°. The dynamic range is ∼7000.
Paper: The MeerKAT Absorption Line Survey (MALS) Data Release. I. Stokes I Image Catalogs at 1–1.4 GHz
Authors: P. P. Deka, N. Gupta, P. Jagannathan, S. Sekhar, E. Momjian, S. Bhatnagar, J. Wagenveld, H.-R. Klöckner, J. Jose, S. A. Balashev, F. Combes, M. Hilton, D. Borgaonkar, A. Chatterjee, K. L. Emig, A. N. Gaunekar, G. I. G. Józsa, D. Y. Klutse, K. Knowles, J.-K. Krogager, A. Mohapatra, K. Moodley, Sébastien Muller, P. Noterdaeme, P. Petitjean, P. Salas, S. Sikhosana
Figure caption: Astrometric comparison of 4506 compact and isolated field sources from MALS with NVSS. The dominant fraction (∼95%) is within the restoring beam (∼8″; circle). The dashed lines mark the median offsets.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-2169 (Kepler-1130). Left: the best-fit model includes a long-period, highly eccentric stellar-mass companion that moved through periastron in 2022. The automated KGPS algorithm detects this companion but does not find the optimal orbital period because the full phase curve of the eccentric orbit has not been sampled yet. Right: periodograms of the RVs after removing a model of the transiting planets only (top) and our best-fit model of the stellar companion (bottom).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1925 (Kepler-409). Left: a nontransiting planet is detected with low significance (orbital parameters inset). Right: periodograms of the RVs after removing a model of the transiting planet only (top) and the best-fit two-planet model (bottom).
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-2732 (Kepler-403). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-3179 (Kepler-1911). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-2687 (Kepler-1869). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-3083. No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-2720 (KIC 8176564). No nontransiting companions are detected.
Paper: The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory
Authors: Lauren M. Weiss, Howard Isaacson, Andrew W. Howard, Benjamin J. Fulton, Erik A. Petigura, Daniel Fabrycky, Daniel Jontof-Hutter, Jason H. Steffen, Hilke E. Schlichting, Jason T. Wright, Corey Beard, Casey L. Brinkman, Ashley Chontos, Steven Giacalone, Michelle L. Hill, Molly R. Kosiarek, Mason G. MacDougall, Teo Močnik, Alex S. Polanski, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt
Figure caption: Same as Figure 8, but for KOI-1930 (Kepler-338). No nontransiting companions are detected.