adsabs/AstroCLIMB huggingface dataset:
Paper: Do High-spin High-mass X-Ray Binaries Contribute to the Population of Merging Binary Black Holes?
Authors: Monica Gallegos-Garcia, Maya Fishbach, Vicky Kalogera, Christopher P L Berry, Zoheyr Doctor
Figure caption: Same as Figure 2 but for the model using q crit values following Neijssel et al. (2019) and BBH mergers within a Hubble time are shown in gray. Binaries with donor masses in the range of M donor = (30 ± 2.5)M ⊙ are shown in the left panel and M donor = (45 ± 2.5)M ⊙ are shown in the middle panel. Although this model results in BBHs in the same parameter space as our grid of MESA simulations, this outcome contributes only 0.01% to the total outcome of Case-A HMXBs.
Paper: Do High-spin High-mass X-Ray Binaries Contribute to the Population of Merging Binary Black Holes?
Authors: Monica Gallegos-Garcia, Maya Fishbach, Vicky Kalogera, Christopher P L Berry, Zoheyr Doctor
Figure caption: Illustration of the method. The evolution of all binaries, from an initial ZAMS population, through Case-A MT, while both stars are on the MS, to the formation of Case-A HMXBs, is simulated entirely with COSMIC. Starting from this population of Case-A HMXBs, we match each Case-A HMXBs to the nearest binary simulation in terms of orbital period and mass ratio from our grids of MESA simulations. For comparison, we use COSMIC to simulate the remaining evolution.
Paper: Do High-spin High-mass X-Ray Binaries Contribute to the Population of Merging Binary Black Holes?
Authors: Monica Gallegos-Garcia, Maya Fishbach, Vicky Kalogera, Christopher P L Berry, Zoheyr Doctor
Figure caption: Contours showing the population from our COSMIC simulations of all BBHs regardless of their formation path (gray contours) and Case-A HMXBs (pink contours) for the model using q crit following Neijssel et al. (2019) for systems with donor mass M donor = (45 ± 2.5)M ⊙. These populations are shown as a function of mass ratio q and orbital period when the system became a BH–H-rich star. The overlapping region corresponds to BBHs that had Case-A HMXBs progenitors.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Ratios of the column density of pure hydrocarbon species to their ﹩-\mathrm{CN}﹩ substituted counterparts as predicted by our chemical models (red diamonds; Burkhardt et al. 2021) compared to those measured by the GOTHAM and QUIJOTE surveys (black circles with error bars). Table B1 provides the values used and specific references. †For ﹩{{\rm{C}}}_{9}{{\rm{H}}}_{7}\mathrm{CN}﹩, the measured value takes only 2-﹩{{\rm{C}}}_{9}{{\rm{H}}}_{7}\mathrm{CN}﹩ into account, while the model-predicted value includes all of the isomers.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Corner plot for C9H8 showing parameter covariances and marginalized posterior distributions for the C9H8 MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: An Empirical Approach to Selecting the First Growing Black Hole Seeds with JWST/NIRCam
Authors: Andy D. Goulding, Jenny E. Greene
Figure caption: Comparison between the F200W–F444W color for JAGUAR z = 7–10 AGN+galaxies with no extinction and A  V  = 0.7 (blue and red histograms, respectively) and pure galaxy emission (black dashed histogram) presented in this work to those found from theoretical BH formation models for obese BHs (Natarajan et al. 2017; N17; gray shaded region), heavy seed mechanisms (e.g., Valiante et al. 2018; N18; green dashed line), and direct-collapse BHs (Whalen et al. 2020; W20; yellow dashed line).
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Chemical structure of indene (A) and 2-cyanoindene (B; 2-﹩{{\rm{C}}}_{9}{{\rm{H}}}_{7}\mathrm{CN}﹩). Sites 1–7 label the nitrile substitution positions of the seven possible isomers of cyanoindene.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Corner plot for 2-﹩{{\rm{C}}}_{9}{{\rm{H}}}_{7}\mathrm{CN}﹩ showing parameter covariances and marginalized posterior distributions for the 2-﹩{{\rm{C}}}_{9}{{\rm{H}}}_{7}\mathrm{CN}﹩ MCMC fit. The 16th, 50th, and 84th confidence intervals (corresponding to ±1σ for a Gaussian posterior distribution) are shown as vertical lines.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Velocity stacked and matched filter spectra of C9H8. The intensity scales are the signal-to-noise ratios of the response functions when centered at a given velocity. The “zero” velocity corresponds to the channel with the highest intensity to account for blended spectroscopic transitions and variations in velocity component source sizes. (Left) The stacked spectra from the GOTHAM DR4 data are displayed in black, overlaid with the expected line profile in red from our MCMC fit to the data. The signal-to-noise ratio is on a per-channel basis. (Right) Matched filter response obtained from cross-correlating the simulated and observed velocity stacks in the left panel; the value annotated corresponds to the peak impulse response of the matched filter.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Potential energy surface ((U)B3LYP-G3/def2-TZVP) for the CN addition–H elimination channels for the reaction between CN and indene. Two possible channels occur via CN addition at carbon positions 2 and 3 for the five-membered ring.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Same as Figure 2 but for 2-﹩{{\rm{C}}}_{9}{{\rm{H}}}_{7}\mathrm{CN}﹩.
Paper: Discovery of Interstellar 2-Cyanoindene (2-C9H7CN) in GOTHAM Observations of TMC-1
Authors: Madelyn L. Sita, P. Bryan Changala, Ci Xue, Andrew M. Burkhardt, Christopher N. Shingledecker, Kin Long Kelvin Lee, Ryan A. Loomis, Emmanuel Momjian, Mark A. Siebert, Divita Gupta, Eric Herbst, Anthony J. Remijan, Michael C. McCarthy, Ilsa R. Cooke, Brett A. McGuire
Figure caption: Potential energy surface ((U)B3LYP-G3/def2-TZVP) for the CN addition–H elimination channels for the reaction between CN and indene. Four possible channels occur via CN addition at carbon positions 5, 6, 7, and 8 for the six-membered ring.
Paper: Broadband Electrostatic Waves near the Lower-hybrid Frequency in the Near-Sun Solar Wind Observed by the Parker Solar Probe
Authors: Jinsong Zhao, David M. Malaspina, T. Dudok de Wit, Viviane Pierrard, Yuriy Voitenko, Giovanni Lapenta, Stefaan Poedts, Stuart D. Bale, Justin C. Kasper, Davin Larson, Roberto Livi, Phyllis Whittlesey
Figure caption: Overview of broadband electrostatic waves and the plasma environment. (a) DC-coupled spectra of the potential difference dV 12 between V 1 and V 2, ﹩{P}_{{{dV}}_{12}};﹩ (b) the normalized DC-coupled spectra ﹩{P}_{{{dV}}_{12}}/{P}_{{{dV}}_{12}}^{\max }﹩, where ﹩{P}_{{{dV}}_{12}}^{\max }﹩ denotes the maximum ﹩{P}_{{{dV}}_{12}}﹩ at each time; (c) DC-coupled spectra of the magnetic field component B  v , ﹩{P}_{{B}_{v}};﹩ (d) the magnetic field  B  in radial–tangential–normal (RTN) coordinates and magnetic field strength ∣ B ∣; (e) the solar wind speed  V  in RTN coordinates; (f) the proton number density, n  p ; (g) the proton temperature, T  p ; (h) the plasma beta β  p  defined as the ratio between the proton thermal pressure and the magnetic pressure; and (i) the pitch angle distribution of electrons in the energy channel with E  e  ≃ 314 eV. The orange bars in the top of panel (a) label the two time intervals: 02:00:00–24:00:00 UT on 2021 April 27 (Interval I) and from 14:00:00 UT on 2021 April 28 to 24:00:00 UT on 2021 April 29 (Interval II). The yellow bars in the bottom of panel (a) and in the top of panel (b) highlight that PSP entered the extended corona below the Alfvén surface during the time intervals 09:33–14:42 on 2021 April 28, 07:18–07:52 on 2021 April 29, and from 23:40 UT on 2021 April 29 to 01:24 on 2021 April 30. The lower-hybrid frequency is denoted by the white curves in panels (a) and (c) and by the black curve in panel (b).
Paper: Broadband Electrostatic Waves near the Lower-hybrid Frequency in the Near-Sun Solar Wind Observed by the Parker Solar Probe
Authors: Jinsong Zhao, David M. Malaspina, T. Dudok de Wit, Viviane Pierrard, Yuriy Voitenko, Giovanni Lapenta, Stefaan Poedts, Stuart D. Bale, Justin C. Kasper, Davin Larson, Roberto Livi, Phyllis Whittlesey
Figure caption: The electric field and its power spectral density in four different events: (a) Event #1; (b) Event #2; (c) Event #3; and (d) Event #4. Panel (I) shows two-dimensional electric fields  E  in the spacecraft frame, panel (II) shows the spectrogram of E  x , panel (III) shows the spectrogram of E  y , panel (IV) shows the filtered electric field  E  fil, and panel (V) shows the mean PSD of  E . Panel (d-VI) zooms in  E  in the time interval 18:51:25:32–47 UT (shaded gray in panel (d-I)). The dotted lines in spectrograms of  E  denote the lower-hybrid frequency.
Paper: Broadband Electrostatic Waves near the Lower-hybrid Frequency in the Near-Sun Solar Wind Observed by the Parker Solar Probe
Authors: Jinsong Zhao, David M. Malaspina, T. Dudok de Wit, Viviane Pierrard, Yuriy Voitenko, Giovanni Lapenta, Stefaan Poedts, Stuart D. Bale, Justin C. Kasper, Davin Larson, Roberto Livi, Phyllis Whittlesey
Figure caption: Statistical results of primary wave parameters. (a) The joint distribution of the wave amplitude δ E and the weighted wave frequency f  w , (b) the joint distribution of δ E and the normalized wave frequency f  w /f LH, and (c) the joint distribution of δ E and the normalized wave frequency band Δf/f LH, where the crosses and circles highlight data belonging to Intervals I and II, respectively. Histograms of (d) δ E, (e) f  w , (f) f  w /f LH, and (g) Δf/f LH, where the blue and red curves denote the wave data sets in Intervals I and II, respectively.
Paper: Broadband Electrostatic Waves near the Lower-hybrid Frequency in the Near-Sun Solar Wind Observed by the Parker Solar Probe
Authors: Jinsong Zhao, David M. Malaspina, T. Dudok de Wit, Viviane Pierrard, Yuriy Voitenko, Giovanni Lapenta, Stefaan Poedts, Stuart D. Bale, Justin C. Kasper, Davin Larson, Roberto Livi, Phyllis Whittlesey
Figure caption: Dependence of statistical results on primary plasma parameters. (a) The joint distribution of n  p  and β  p , and (b) histogram of β  p , where the wave data sets in Intervals I and II are denoted by blue and red, respectively. (c) Histograms of θ  BR  (the angle between the magnetic field  B  and the radial vector  R ), and (d) histograms of θ  BV  (the angle between the magnetic field  B  and the radial vector  V ), where the orange and purple curves denote the data of wave events and data for all time, respectively.
Paper: Broadband Electrostatic Waves near the Lower-hybrid Frequency in the Near-Sun Solar Wind Observed by the Parker Solar Probe
Authors: Jinsong Zhao, David M. Malaspina, T. Dudok de Wit, Viviane Pierrard, Yuriy Voitenko, Giovanni Lapenta, Stefaan Poedts, Stuart D. Bale, Justin C. Kasper, Davin Larson, Roberto Livi, Phyllis Whittlesey
Figure caption: Analyses of the wave nature. (a) The joint distribution of B  z /B 0 and δ E. (b) The joint distribution of V/V  A  and f sc/f cp, where the solid triangles denote the data with V/V A < 1 and circles denote the events with θ BV = 42.°5–47.°5. (c) The joint distribution between V/C  S  and f sc/f cp, where the squares denote the events with θ  BV  = 0°–10°. Real frequencies ω  r  (normalized by ω cp = 2π f cp), damping rates ω  i  (normalized by ω  r ), and phase speeds v  p  = ω  r /k of the fast-magnetosonic whistler waves (FW) and ion Bernstein wave (IBW) at two wave-normal angles: (d) θ = 75°; and (e) θ = 89.°9. Oblique slow mode waves are also overlaid in panels (d) and (e), where the purple solid curves correspond to the numerical solution of the complete dispersion equation in the linear kinetic theory, and the purple dashed curves come from the analytical prediction ω  r  = C  S  k ∥ (Verscharen et al. 2017). The black dotted curves denote the highly oblique fast-magnetosonic whistler wave predicted by the two-fluid model (Zhao 2015). The inset in panel (e) shows two parts of the wave between 2ω cp and 3ω cp: the FW part (v  g  > V A, v  g  denoting the group velocity) and the IBW part with v  g  < 0. Note that the data with ∣ω  i ∣ > ω  r /2 are discarded in panels (d) and (e), and only the harmonic waves below 50f cp are shown in panel (e).
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: Plots showing the morphological evolution of the galaxies found in the SMACS 0723 field up to z = 6. These show the fraction of the total number of galaxies, within a given redshift bin, which has the given type as determined by visual morphologies. We also include the morphological evolution, which has been derived from HST observations of the CANDELS fields in Mortlock et al. (2013). Circled markers denote the JWST observations at higher redshifts. We note that the increase in spheroids can be attributed to smaller sizes with increasing redshift z as discussed in Section 3.1.1.
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: Comparison HST vs. JWST images for nine objects in each class within our sample. Left columns shows the HST F160W image, while the middle panel shows the JWST view at the same orientation, in the rest-frame optical. The far right panel shows the color image of this system as seen through the JWST NIRCam F277W, F356W, and F444W filters, generated by TRINITY (Coe et al. 2012). The IDs refer to the original RELICs catalogs identification.
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: Plot showing the Sérsic index evolution in bins of redshift. Shown are the morphological types and their mean values for these indices alongside error bars representing the 15% and 85% percentiles of the distribution. We can see that the average hovers about n = 1, but that the spheroids appear to have higher values even at the higher redshifts.
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: JWST color image of SMACS 0723 showing the overall distribution of galaxy shapes and morphologies, including the lensing arcs. This image was produced from our reduced data products via a composite of data in six bands: F090W, F150W, F200W, F277W, F356W, and F444W. F090W and F150W were assigned blue colors, F200W and F277W green, and F356W and F444W orange and red, respectively.
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: Rest-frame wavelength at a given redshift for the F200W, F277W, F356W, and F444W filters. The hatched regions show the areas where NIRCam filters probe the optical rest-frame for z > 3, with the color corresponding to the respective optimal filter for the redshift range. To follow galaxies’ optical rest-frames we use F277W for 3 < z < 4, F356W for 4 < z < 6, and F444W for 6 < z < 8.
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: Concentration vs. asymmetry. The abundance of disks results in their populating the area originally used for selecting late-type galaxies. Decision thresholds shown here are drawn from (Bershady et al. 2000).
Paper: Panic! at the Disks: First Rest-frame Optical Observations of Galaxy Structure at z > 3 with JWST in the SMACS 0723 Field
Authors: Leonardo Ferreira, Nathan Adams, Christopher J. Conselice, Elizaveta Sazonova, Duncan Austin, Joseph Caruana, Fabricio Ferrari, Aprajita Verma, James Trussler, Tom Broadhurst, Jose Diego, Brenda L. Frye, Massimo Pascale, Stephen M. Wilkins, Rogier A. Windhorst, Adi Zitrin
Figure caption: The distribution of redshifts across the SMACS 0723 field. Different redshift regimes, where we use our methodology to investigate the morphological evolution, are shown as differently colored markers.
Paper: Measuring Periods in Aperiodic Light Curves—Applying the GPS Method to Infer the Rotation Periods of Solar-like Stars
Authors: Timo Reinhold, Alexander I. Shapiro, Sami K. Solanki, Gibor Basri
Figure caption: Dependence of α on the activity cycle. The gray data show the underlying model light curve (with 90° inclination and solar metallicity) from which we picked 4 yr segments, computed the power spectrum, its gradient, and finally the inflection point period (i.e., α). The blue (noise-free) and red (noisy) curves show the yearly averages of α − 〈α〉 for 5000 randomly drawn samples. We subtracted the mean value 〈α〉 here to show the overlay with the activity cycle.
Paper: Measuring Periods in Aperiodic Light Curves—Applying the GPS Method to Infer the Rotation Periods of Solar-like Stars
Authors: Timo Reinhold, Alexander I. Shapiro, Sami K. Solanki, Gibor Basri
Figure caption: Upper panel: Keplerized model light curve (including noise) with an inclination of i = 70° and solar metallicity [Fe/H] = 0.0 dex. Individual spot transits are visible but there is no obvious periodicity. Middle panel: global wavelet power spectrum. The vertical blue line indicates the model rotation period of 27 days. The power spectrum does not show any peak at this period. Lower panel: GPS. The highest peak indicates the period at the inflection point P IP = 5.41 days. This period can be used to infer the rotation period.
Paper: Measuring Periods in Aperiodic Light Curves—Applying the GPS Method to Infer the Rotation Periods of Solar-like Stars
Authors: Timo Reinhold, Alexander I. Shapiro, Sami K. Solanki, Gibor Basri
Figure caption: Dependence of α on inclination (first panel), metallicity (second panel), and Kepler magnitude Kp (third panel) for 5000 samples. The dashed blue line indicates the median α of all models, and the red dots and error bars indicate the mean and standard deviation of α in the considered bins. We note that the upper and middle panels show the noise-free models, whereas the lower panel shows the results for the noisy model light curves.
Paper: Measuring Periods in Aperiodic Light Curves—Applying the GPS Method to Infer the Rotation Periods of Solar-like Stars
Authors: Timo Reinhold, Alexander I. Shapiro, Sami K. Solanki, Gibor Basri
Figure caption: Dependence of the derived rotation periods on starspot lifetimes. Upper panel: histograms of derived rotation periods for a model set with different lifetimes utilizing the GPS method. Lower panel: the same but with periods derived using the autocorrelation method. The vertical dashed line in both panels indicates the model rotation period.
Paper: Measuring Periods in Aperiodic Light Curves—Applying the GPS Method to Infer the Rotation Periods of Solar-like Stars
Authors: Timo Reinhold, Alexander I. Shapiro, Sami K. Solanki, Gibor Basri
Figure caption: Distribution of the measured inflection point period divided by the model rotation period of 27 days (i.e., α) for the noise-free (blue) and the noisy (red) models for 5000 random samples. Adding noise to the light curves shifts the inflection point toward longer periods (i.e., larger values of α).